Seite 12 von 17
(571)The Fluorescence Telescope on board EUSO-SPB2 for the detection of Ultra High Energy Cosmic Rays
  • G. Osteria,
  • J. H. Adams,
  • M. Battisti,
  • A. S. Belov,
  • M. E. Bertaina
  • +35
  • F. Bisconti,
  • F. Saverio Cafagna,
  • D. Campana,
  • R. Caruso,
  • M. Casolino,
  • M. Christi,
  • T. Ebisuzaki,
  • J. Eser,
  • F. Fenu,
  • G. Filippatos,
  • C. Fornaro,
  • F. Guarino,
  • P. Klimov,
  • V. Kungel,
  • S. Mackovjak,
  • M. Mese,
  • M. Miller,
  • H. Miyamoto,
  • A. Olinto,
  • Y. Onel,
  • E. Parizot,
  • M. Pech,
  • F. Perfetto,
  • L. Piotrowski,
  • G. Prévôt,
  • P. Reardon,
  • M. Ricci,
  • F. Sarazin,
  • V. Scotti,
  • K. Shinozaki,
  • P. Shovanec,
  • J. Szabelski,
  • Y. Takizawa,
  • L. Valore,
  • L. Wiencke
  • (less)
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin (03/2022)
abstract + abstract -

The Fluorescence Telescope is one of the two telescopes on board the Extreme Universe Space Observatory on a Super Pressure Balloon II (EUSO-SPB2). EUSO-SPB2 is an ultra-long-duration balloon mission that aims at the detection of Ultra High Energy Cosmic Rays (UHECR) via the fluorescence technique (using a Fluorescence Telescope) and of Ultra High Energy (UHE) neutrinos via Cherenkov emission (using a Cherenkov Telescope). The mission is planned to fly in 2023 and is a precursor of the Probe of Extreme Multi-Messenger Astrophysics (POEMMA). The Fluorescence Telescope is a second generation instrument preceded by the telescopes flown on the EUSO-Balloon and EUSO-SPB1 missions. It features Schmidt optics and has a 1-meter diameter aperture. The focal surface of the telescope is equipped with a 6912-pixel Multi Anode Photo Multipliers (MAPMT) camera covering a 37.4 x 11.4 degree Field of Regard. Such a big Field of Regard, together with a flight target duration of up to 100 days, would allow, for the first time from suborbital altitudes, detection of UHECR fluorescence tracks. This contribution will provide an overview of the instrument including the current status of the telescope development.


(570)Expected Performance of the EUSO-SPB2 Fluorescence Telescope
  • G. Filippatos,
  • M. Battisti,
  • M. E. Bertaina,
  • F. Bisconti,
  • J. Eser
  • +4
  • G. Osteria,
  • F. Sarazin,
  • L. Wiencke,
  • JEM-EUSO Collaboration
  • (less)
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin (03/2022)
abstract + abstract -

The Extreme Universe Space Observatory Supper Pressure Balloon 2 (EUSO-SPB2) is under development, and will prototype instrumentation for future satellite-based missions, including the Probe of Extreme Multi-Messenger Astrophysics (POEMMA). EUSO-SPB2 will consist of two telescopes. The first is a Cherenkov telescope (CT) being developed to identify and estimate the background sources for future below-the-limb very high energy (E>10 PeV) astrophysical neutrino observations, as well as above-the-limb cosmic ray induced signals (E>1 PeV). The second is a fluorescence telescope (FT) being developed for detection of Ultra High Energy Cosmic Rays (UHECRs). In preparation for the expected launch in 2023, extensive simulations tuned by preliminary laboratory measurements have been preformed to understand the FT capabilities. The energy threshold has been estimated at $10^{18.2}$ eV, and results in a maximum detection rate at $10^{18.6}$ eV when taking into account the shape of the UHECR spectrum. In addition, onboard software has been developed based on the simulations as well as experience with previous EUSO missions. This includes a level 1 trigger to be run on the computationally limited flight hardware, as well as a deep learning based prioritization algorithm in order to accommodate the balloon's telemetry budget. These techniques could also be used later for future, space-based missions.


(569)Overview of Cherenkov Telescope on-board EUSO-SPB2 for the Detection of Very-High-Energy Neutrinos
  • M. Bagheri,
  • P. Bertone,
  • I. Fontane,
  • E. Gazda,
  • E. G. Judd
  • +10
  • J. F. Krizmanic,
  • E. N. Kuznetsov,
  • M. J. Miller,
  • J. Nachtman,
  • Y. Onel,
  • A. Nepomuk Otte,
  • P. J. Reardon,
  • O. Romero Matamala,
  • L. Wiencke,
  • JEM-EUSO Collaboration
  • (less)
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin (03/2022)
abstract + abstract -

We present the status of the development of a Cherenkov telescope to be flown on a long-duration balloon flight, the Extreme Universe Space Observatory Super Pressure Balloon 2 (EUSO-SPB2). EUSO-SPB2 is an approved NASA balloon mission that is planned to fly in 2023 and is a precursor of the Probe of Extreme Multi-Messenger Astrophysics (POEMMA), a candidate for an Astrophysics probe-class mission. The purpose of the Cherenkov telescope on-board EUSOSPB2 is to classify known and unknown sources of backgrounds for future space-based neutrino detectors. Furthermore, we will use the Earth-skimming technique to search for Very-High-Energy (VHE) tau neutrinos below the limb (E > 10 PeV) and observe air showers from cosmic rays above the limb. The 0.785 m^2 Cherenkov telescope is equipped with a 512-pixel SiPM camera covering a 12.8° x 6.4° (Horizontal x Vertical) field of view. The camera signals are digitized with a 100 MS/s readout system. In this paper, we discuss the status of the telescope development, the camera integration, and simulation studies of the camera response.


CN-1
CN-3
CN-7
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RU-B
(568)How special are black holes?
  • Dvali G.,
  • Kaikov O.,
  • and Valbuena-Bermúdez J.S
Phys. Rev. D (03/2022) doi:10.1103/PhysRevD.105.056013
abstract + abstract -

Black holes are considered to be exceptional due to their time evolution and information processing. However, it was proposed recently that these properties are generic for objects, the so-called saturons, that attain the maximal entropy permitted by unitarity. In the present paper, we verify this connection within a renormalizable SU(N) invariant theory. We show that the spectrum of the theory contains a tower of bubbles representing bound states of SU(N) Goldstones. Despite the absence of gravity, a saturated bound state exhibits a striking correspondence with a black hole: Its entropy is given by the Bekenstein-Hawking formula; semi-classically, the bubble evaporates at a thermal rate with a temperature equal to its inverse radius; the information retrieval time is equal to Page's time. The correspondence goes through a trans-theoretic entity of Poincaré Goldstone. The black hole/saturon correspondence has important implications for black hole physics, both fundamental and observational.


RU-D
(567)EUSO-SPB2 Telescope Optics and Testing
  • V. Kungel,
  • R. Bachman",
  • J. Brewster",
  • M. Dawes",
  • J. Desiato"
  • +12
  • J. Eser",
  • W. Finch",
  • L. Huelett",
  • A. V. Olinto",
  • J. Pace",
  • M. Pech",
  • P. Reardon",
  • P. Schovanek",
  • C. Wang",
  • L. Wiencke",
  • V. Kungel",
  • JEM-EUSO Collaboration
  • (less)
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin (03/2022)
abstract + abstract -

The Extreme Universe Space Observatory - Super Pressure Balloon (EUSO-SPB2) mission will fly two custom telescopes that feature Schmidt optics to measure Čerenkov- and fluorescence-emission of extensive air-showers from cosmic rays at the PeV and EeV-scale, and search for tau-neutrinos. Both telescopes have 1-meter diameter apertures and UV/UV-visible sensitivity. The Čerenkov telescope uses a bifocal mirror segment alignment, to distinguish between a direct cosmic ray that hits the camera versus the Čerenkov light from outside the telescope. Telescope integration and laboratory calibration will be performed in Colorado. To estimate the point spread function and efficiency of the integrated telescopes, a test beam system that delivers a 1-meter diameter parallel beam of light is being fabricated. End-to-end tests of the fully integrated instruments will be carried out in a field campaign at dark sites in the Utah desert using cosmic rays, stars, and artificial light sources. Laser tracks have long been used to characterize the performance of fluorescence detectors in the field. For EUSO-SPB2 an improvement in the method that includes a correction for aerosol attenuation is anticipated by using a bi-dynamic Lidar configuration in which both the laser and the telescope are steerable. We plan to conduct these field tests in Fall 2021 and Spring 2022 to accommodate the scheduled launch of EUSO-SPB2 in 2023 from Wanaka, New Zealand.


(566)Science and mission status of EUSO-SPB2
  • J. Eser,
  • A. V. Olinto,
  • L. Wiencke,
  • JEM-EUSO Collaboration
37th International Cosmic Ray Conference. 12-23 July 2021. Berlin (03/2022)
abstract + abstract -

The Extreme Universe Space Observatory on a Super Pressure Balloon II (EUSO-SPB2) is a second generation stratospheric balloon instrument for the detection of Ultra High Energy Cosmic Rays (UHECRs, E > 1 EeV) via the fluorescence technique and of Very High Energy (VHE, E > 10 PeV) neutrinos via Cherenkov emission. EUSO-SPB2 is a pathfinder mission for instruments like the proposed Probe Of Extreme Multi-Messenger Astrophysics (POEMMA). The purpose of such a space-based observatory is to measure UHECRs and UHE neutrinos with high statistics and uniform exposure. EUSO-SPB2 is designed with two Schmidt telescopes, each optimized for their respective observational goals. The Fluorescence Telescope looks at the nadir to measure the fluorescence emission from UHECR-induced extensive air shower (EAS), while the Cherenkov Telescope is optimized for fast signals ($\sim$10 ns) and points near the Earth's limb. This allows for the measurement of Cherenkov light from EAS caused by Earth skimming VHE neutrinos if pointed slightly below the limb or from UHECRs if observing slightly above. The expected launch date of EUSO-SPB2 is Spring 2023 from Wanaka, NZ with target duration of up to 100 days. Such a flight would provide thousands of VHECR Cherenkov signals in addition to tens of UHECR fluorescence tracks. Neither of these kinds of events have been observed from either orbital or suborbital altitudes before, making EUSO-SPB2 crucial to move forward towards a space-based instrument. It will also enhance the understanding of potential background signals for both detection techniques. This contribution will provide a short overview of the detector and the current status of the mission as well as its scientific goals.


(565)Bubble wall velocities in local equilibrium
  • Wen-Yuan Ai,
  • Björn Garbrecht,
  • Carlos Tamarit
Journal of Cosmology and Astroparticle Physics (03/2022) doi:10.1088/1475-7516/2022/03/015
abstract + abstract -

It is commonly expected that a friction force on the bubble wall in a first-order phase transition can only arise from a departure from thermal equilibrium in the plasma. Recently however, it was argued that an effective friction, scaling as γ2 w (with γ w being the Lorentz factor for the bubble wall velocity), persists in local equilibrium. This was derived assuming constant plasma temperature and velocity throughout the wall. On the other hand, it is known that, at the leading order in derivatives, the plasma in local equilibrium only contributes a correction to the zero-temperature potential in the equation of motion of the background scalar field. For a constant plasma temperature, the equation of motion is then completely analogous to the vacuum case, the only change being a modified potential, and thus no friction should appear. We resolve these apparent contradictions in the calculations and their interpretation and show that the recently proposed effective friction in local equilibrium originates from inhomogeneous temperature distributions, such that the γ2 w -scaling of the effective force is violated. Further, we propose a new matching condition for the hydrodynamic quantities in the plasma valid in local equilibrium and tied to local entropy conservation. With this added constraint, bubble velocities in local equilibrium can be determined once the parameters in the equation of state are fixed, where we use the bag equation in order to illustrate this point. We find that there is a critical value of the transition strength αcrit such that bubble walls run away for α>αcrit.


(564)Revealing the Cosmic History with Gravitational Waves
  • Andreas Ringwald,
  • Carlos Tamarit
arXiv e-prints (03/2022) e-Print:2203.00621
abstract + abstract -

The characteristics of the cosmic microwave background provide circumstantial evidence that the hot radiation-dominated epoch in the early universe was preceded by a period of inflationary expansion. Here, we show how a measurement of the stochastic gravitational wave background can reveal the cosmic history and the physical conditions during inflation, subsequent pre- and re-heating, and the beginning of the hot big bang era. This is exemplified with a particularly well-motivated and predictive minimal extension of the Standard Model which is known to provide a complete model for particle physics -- up to the Planck scale, and for cosmology -- back to inflation.


RU-D
(563)ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT). VI. Accretion shocks in the disk of DG Tau and HL Tau
  • A. Garufi,
  • L. Podio,
  • C. Codella,
  • D. Segura-Cox,
  • M. Vander Donckt
  • +7
  • S. Mercimek,
  • F. Bacciotti,
  • D. Fedele,
  • M. Kasper,
  • J. E. Pineda,
  • E. Humphreys,
  • L. Testi
  • (less)
Astronomy and Astrophysics (02/2022) doi:10.1051/0004-6361/202141264
abstract + abstract -

Planet-forming disks are not isolated systems. Their interaction with the surrounding medium affects their mass budget and chemical content. In the context of the ALMA-DOT program, we obtained high-resolution maps of assorted lines from six disks that are still partly embedded in their natal envelope. In this work, we examine the SO and SO2 emission that is detected from four sources: DG Tau, HL Tau, IRAS 04302+2247, and T Tau. The comparison with CO, HCO+, and CS maps reveals that the SO and SO2 emission originates at the intersection between extended streamers and the planet-forming disk. Two targets, DG Tau and HL Tau, offer clear cases of inflowing material inducing an accretion shock on the disk material. The measured rotational temperatures and radial velocities are consistent with this view. In contrast to younger Class 0 sources, these shocks are confined to the specific disk region impacted by the streamer. In HL Tau, the known accreting streamer induces a shock in the disk outskirts, and the released SO and SO2 molecules spiral toward the star in a few hundred years. These results suggest that shocks induced by late accreting material may be common in the disks of young star-forming regions with possible consequences for the chemical composition and mass content of the disk. They also highlight the importance of SO and SO2 line observations in probing accretion shocks from a larger sample.

The reduced datacubes are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/658/A104


CN-1
(562)Observational properties of puffy discs: radiative GRMHD spectra of mildly sub-Eddington accretion
  • Maciek Wielgus,
  • Debora Lancova,
  • Odele Straub,
  • Wlodek Kluzniak,
  • Ramesh Narayan
  • +5
  • David Abarca,
  • Agata Rozanska,
  • Frederic Vincent,
  • Gabriel Torok,
  • Marek Abramowicz
  • (less)
Mon.Not.Roy.Astron.Soc. (02/2022) e-Print:2202.08831 doi:10.1093/mnras/stac1317
abstract + abstract -

Numerical general relativistic radiative magnetohydrodynamic simulations of accretion discs around a stellar-mass black hole with a luminosity above 0.5 of the Eddington value reveal their stratified, elevated vertical structure. We refer to these thermally stable numerical solutions as puffy discs. Above a dense and geometrically thin core of dimensionless thickness h/r ∼ 0.1, crudely resembling a classic thin accretion disc, a puffed-up, geometrically thick layer of lower density is formed. This puffy layer corresponds to h/r ∼ 1.0, with a very limited dependence of the dimensionless thickness on the mass accretion rate. We discuss the observational properties of puffy discs, particularly the geometrical obscuration of the inner disc by the elevated puffy region at higher observing inclinations, and collimation of the radiation along the accretion disc spin axis, which may explain the apparent super-Eddington luminosity of some X-ray objects. We also present synthetic spectra of puffy discs, and show that they are qualitatively similar to those of a Comptonized thin disc. We demonstrate that the existing xspec spectral fitting models provide good fits to synthetic observations of puffy discs, but cannot correctly recover the input black hole spin. The puffy region remains optically thick to scattering; in its spectral properties, the puffy disc roughly resembles that of a warm corona sandwiching the disc core. We suggest that puffy discs may correspond to X-ray binary systems of luminosities above 0.3 of the Eddington luminosity in the intermediate spectral states.


CN-4
RU-C
(561)Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC galaxies
  • R. Chen,
  • D. Scolnic,
  • E. Rozo,
  • E.S. Rykoff,
  • B. Popovic
  • +80
  • R. Kessler,
  • M. Vincenzi,
  • T.M. Davis,
  • P. Armstrong,
  • D. Brout,
  • L. Galbany,
  • L. Kelsey,
  • C. Lidman,
  • A. Möller,
  • B. Rose,
  • M. Sako,
  • M. Sullivan,
  • G. Taylor,
  • P. Wiseman,
  • J. Asorey,
  • A. Carr,
  • C. Conselice,
  • K. Kuehn,
  • G.F. Lewis,
  • E. Macaulay,
  • M. Rodriguez-Monroy,
  • B.E. Tucker,
  • T.M.C. Abbott,
  • M. Aguena,
  • S. Allam,
  • F. Andrade-Oliveira,
  • J. Annis,
  • D. Bacon,
  • E. Bertin,
  • S. Bocquet,
  • D. Brooks,
  • D.L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • R. Cawthon,
  • M. Costanzi,
  • L.N. da Costa,
  • M.E.S. Pereira,
  • S. Desai,
  • H.T. Diehl,
  • P. Doel,
  • S. Everett,
  • I. Ferrero,
  • B. Flaugher,
  • D. Friedel,
  • J. Frieman,
  • J. García-Bellido,
  • M. Gatti,
  • E. Gaztanaga,
  • D. Gruen,
  • S.R. Hinton,
  • D.L. Hollowood,
  • K. Honscheid,
  • D.J. James,
  • O. Lahav,
  • M. Lima,
  • M. March,
  • F. Menanteau,
  • R. Miquel,
  • R. Morgan,
  • A. Palmese,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A.A. Plazas Malagón,
  • J. Prat,
  • A.K. Romer,
  • A. Roodman,
  • E. Sanchez,
  • M. Schubnell,
  • S. Serrano,
  • I. Sevilla-Noarbe,
  • M. Smith,
  • M. Soares-Santos,
  • E. Suchyta,
  • G. Tarle,
  • D. Thomas,
  • C. To,
  • D.L. Tucker,
  • T.N. Varga
  • (less)
(02/2022) e-Print:2202.10480
abstract + abstract -

Current and future cosmological analyses with Type Ia Supernovae (SNe Ia) face three critical challenges: i) measuring redshifts from the supernova or its host galaxy; ii) classifying SNe without spectra; and iii) accounting for correlations between the properties of SNe Ia and their host galaxies. We present here a novel approach that addresses each challenge. In the context of the Dark Energy Survey (DES), we analyze a SNIa sample with host galaxies in the redMaGiC galaxy catalog, a selection of Luminous Red Galaxies. Photo-$z$ estimates for these galaxies are expected to be accurate to $\sigma_{\Delta z/(1+z)}\sim0.02$. The DES-5YR photometrically classified SNIa sample contains approximately 1600 SNe and 125 of these SNe are in redMaGiC galaxies. We demonstrate that redMaGiC galaxies almost exclusively host SNe Ia, reducing concerns with classification uncertainties. With this subsample, we find similar Hubble scatter (to within $\sim0.01$ mag) using photometric redshifts in place of spectroscopic redshifts. With detailed simulations, we show the bias due to using photo-$z$s from redMaGiC host galaxies on the measurement of the dark energy equation-of-state $w$ is up to $\Delta w \sim 0.01-0.02$. With real data, we measure a difference in $w$ when using redMaGiC photometric redshifts versus spectroscopic redshifts of $\Delta w = 0.005$. Finally, we discuss how SNe in redMaGiC galaxies appear to be a more standardizable population due to a weaker relation between color and luminosity ($\beta$) compared to the DES-3YR population by $\sim5\sigma$; this finding is consistent with predictions that redMaGiC galaxies exhibit lower reddening ratios ($\textrm{R}_\textrm{V}$) than the general population of SN host galaxies. These results establish the feasibility of performing redMaGiC SN cosmology with photometric survey data in the absence of spectroscopic data.


(560)Trade-offs and design principles in the spatial organization of catalytic particles
  • Florian Hinzpeter,
  • Filipe Tostevin,
  • Alexander Buchner,
  • Ulrich Gerland
Nature Physics (02/2022) doi:10.1038/s41567-021-01444-4
abstract + abstract -

Catalytic particles are spatially organized in a number of biological systems across different length scales, from enzyme complexes to metabolically coupled cells. Despite operating on different scales, these systems all feature localized reactions involving partially hindered diffusive transport, which is determined by the collective arrangement of the catalysts. Yet it remains largely unexplored how different arrangements affect the interplay between the reaction and transport dynamics, which ultimately determines the flux through the reaction pathway. Here we show that two fundamental trade-offs arise, the first between efficient inter-catalyst transport and the depletion of substrate, and the second between steric confinement of intermediate products and the accessibility of catalysts to substrate. We use a model reaction pathway to characterize the general design principles for the arrangement of catalysts that emerge from the interplay of these trade-offs. We find that the question of optimal catalyst arrangements generalizes the well-known Thomson problem of electrostatics.


CN-6
(559)Observation of the doubly charmed baryon decay $ {\varXi}_{cc}^{++}\to {\varXi}_c^{\prime +}{\pi}^{+} $
  • Roel Aaij,
  • Ahmed Sameh Wagih Abdelmotteleb,
  • Carlos Abellán Beteta,
  • Fernando Jesus Abudinén,
  • Thomas Ackernley
  • +1006
  • Bernardo Adeva,
  • Marco Adinolfi,
  • Hossein Afsharnia,
  • Christina Agapopoulou,
  • Christine Angela Aidala,
  • Salvatore Aiola,
  • Ziad Ajaltouni,
  • Simon Akar,
  • Johannes Albrecht,
  • Federico Alessio,
  • Michael Alexander,
  • Alejandro Alfonso Albero,
  • Zakariya Aliouche,
  • Georgy Alkhazov,
  • Paula Alvarez Cartelle,
  • Sandra Amato,
  • Jake Lewis Amey,
  • Yasmine Amhis,
  • Liupan An,
  • Lucio Anderlini,
  • Martin Andersson,
  • Aleksei Andreianov,
  • Mirco Andreotti,
  • Dong Ao,
  • Flavio Archilli,
  • Alexander Artamonov,
  • Marina Artuso,
  • Kenenbek Arzymatov,
  • Elie Aslanides,
  • Michele Atzeni,
  • Benjamin Audurier,
  • Sebastian Bachmann,
  • Marie Bachmayer,
  • John Back,
  • Pablo Baladron Rodriguez,
  • Vladislav Balagura,
  • Wander Baldini,
  • Juan Baptista de Souza Leite,
  • Matteo Barbetti,
  • Roger Barlow,
  • Sergey Barsuk,
  • William Barter,
  • Matteo Bartolini,
  • Fedor Baryshnikov,
  • Jan-Marc Basels,
  • Giovanni Bassi,
  • Baasansuren Batsukh,
  • Alexander Battig,
  • Aurelio Bay,
  • Anja Beck,
  • Maik Becker,
  • Franco Bedeschi,
  • Ignacio Bediaga,
  • Andrew Beiter,
  • Vladislav Belavin,
  • Samuel Belin,
  • Violaine Bellee,
  • Konstantin Belous,
  • Ilia Belov,
  • Ivan Belyaev,
  • Giovanni Bencivenni,
  • Eli Ben-Haim,
  • Alexander Berezhnoy,
  • Roland Bernet,
  • Daniel Berninghoff,
  • Harris Conan Bernstein,
  • Claudia Bertella,
  • Alessandro Bertolin,
  • Christopher Betancourt,
  • Federico Betti,
  • Ia. Bezshyiko,
  • Iaroslava Bezshyiko,
  • Srishti Bhasin,
  • Jihyun Bhom,
  • Lingzhu Bian,
  • Martin Stefan Bieker,
  • Nicolo Vladi Biesuz,
  • Simone Bifani,
  • Pierre Billoir,
  • Alice Biolchini,
  • Matthew Birch,
  • Fionn Caitlin Ros Bishop,
  • Alexander Bitadze,
  • Andrea Bizzeti,
  • Mikkel Bjørn,
  • Michele Piero Blago,
  • Thomas Blake,
  • Frederic Blanc,
  • Steven Blusk,
  • Dana Bobulska,
  • Julian Alexander Boelhauve,
  • Oscar Boente Garcia,
  • Thomas Boettcher,
  • Alexey Boldyrev,
  • Alexander Bondar,
  • Nikolay Bondar,
  • Silvia Borghi,
  • Maxim Borisyak,
  • Martino Borsato,
  • Jozef Tomasz Borsuk,
  • Sonia Amina Bouchiba,
  • Themistocles Bowcock,
  • Alexandre Boyer,
  • Concezio Bozzi,
  • Matthew John Bradley,
  • Svende Braun,
  • Alexandre Brea Rodriguez,
  • Jolanta Brodzicka,
  • Arnau Brossa Gonzalo,
  • Davide Brundu,
  • Annarita Buonaura,
  • Laura Buonincontri,
  • Aodhan Tomas Burke,
  • Christopher Burr,
  • Albert Bursche,
  • Anatoly Butkevich,
  • Jordy Sebastiaan Butter,
  • Jan Buytaert,
  • Wiktor Byczynski,
  • Sandro Cadeddu,
  • Hao Cai,
  • Roberto Calabrese,
  • Lukas Calefice,
  • Stefano Cali,
  • Ryan Calladine,
  • Marta Calvi,
  • Miriam Calvo Gomez,
  • Patricia Camargo Magalhaes,
  • Pierluigi Campana,
  • Angel Fernando Campoverde Quezada,
  • Simone Capelli,
  • Lorenzo Capriotti,
  • Angelo Carbone,
  • Giovanni Carboni,
  • Roberta Cardinale,
  • Alessandro Cardini,
  • Ina Carli,
  • Paolo Carniti,
  • Leon David Carus,
  • Kazuyoshi Carvalho Akiba,
  • Adrian Casais Vidal,
  • Rowina Caspary,
  • Gianluigi Casse,
  • Marco Cattaneo,
  • Giovanni Cavallero,
  • Sara Celani,
  • Jacopo Cerasoli,
  • Daniel Cervenkov,
  • Abbie Jane Chadwick,
  • Matthew George Chapman,
  • Matthew Charles,
  • Philippe Charpentier,
  • Ph. Charpentier,
  • Carlos Alberto Chavez Barajas,
  • Maximilien Chefdeville,
  • Chen Chen,
  • Shanzhen Chen,
  • Aleksei Chernov,
  • Veronika Chobanova,
  • Serhii Cholak,
  • Marcin Chrzaszcz,
  • Alexsei Chubykin,
  • Vladimir Chulikov,
  • Paolo Ciambrone,
  • Maria Flavia Cicala,
  • Xabier Cid Vidal,
  • Gregory Ciezarek,
  • P.E. L. Clarke,
  • Marco Clemencic,
  • Harry Cliff,
  • Joel Closier,
  • John Leslie Cobbledick,
  • Victor Coco,
  • Joao A B Coelho,
  • Julien Cogan,
  • Eric Cogneras,
  • Lucian Cojocariu,
  • Paula Collins,
  • Tommaso Colombo,
  • Liliana Congedo,
  • Andrea Contu,
  • Naomi Cooke,
  • George Coombs,
  • Imanol Corredoira,
  • Gloria Corti,
  • Cayo Mar Costa Sobral,
  • Benjamin Couturier,
  • Daniel Charles Craik,
  • Jana Crkovská,
  • Melissa Maria Cruz Torres,
  • Robert Currie,
  • Cesar Luiz Da Silva,
  • Shakhzod Dadabaev,
  • Lingyun Dai,
  • Elena Dall'Occo,
  • Jeremy Dalseno,
  • Carmelo D'Ambrosio,
  • Anna Danilina,
  • Philippe d'Argent,
  • Aigerim Dashkina,
  • Jonathan Edward Davies,
  • Adam Davis,
  • Oscar De Aguiar Francisco,
  • Kristof De Bruyn,
  • Stefano De Capua,
  • Michel De Cian,
  • Ulisses De Freitas Carneiro Da Graca,
  • Erika De Lucia,
  • Jussara De Miranda,
  • Leandro De Paula,
  • Marilisa De Serio,
  • Dario De Simone,
  • Patrizia De Simone,
  • Fabio De Vellis,
  • Jacco de Vries,
  • Cameron Thomas Dean,
  • Francesco Debernardis,
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  • Vlad-George Dedu,
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  • Hans Peter Dembinski,
  • Vadym Denysenko,
  • Denis Derkach,
  • Olivier Deschamps,
  • Francesco Dettori,
  • Biplab Dey,
  • Alessandro Di Cicco,
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  • Sergey Didenko,
  • Lorena Dieste Maronas,
  • Shuchong Ding,
  • Vasyl Dobishuk,
  • Chenzhi Dong,
  • Amanda May Donohoe,
  • Francesca Dordei,
  • Alberto dos Reis,
  • Lauren Douglas,
  • Anatoliy Dovbnya,
  • Anthony Gavin Downes,
  • Maciej Wojciech Dudek,
  • Laurent Dufour,
  • Viacheslav Duk,
  • Paolo Durante,
  • John Matthew Durham,
  • Deepanwita Dutta,
  • Agnieszka Dziurda,
  • Alexey Dzyuba,
  • Sajan Easo,
  • Ulrik Egede,
  • Victor Egorychev,
  • Semen Eidelman,
  • Stephan Eisenhardt,
  • Surapat Ek-In,
  • Lars Eklund,
  • Scott Ely,
  • Alexandru Ene,
  • Eliane Epple,
  • Stephan Escher,
  • Jonas Nathanael Eschle,
  • Sevda Esen,
  • Timothy Evans,
  • Lucas Falcao,
  • Yanting Fan,
  • Bo Fang,
  • Stephen Farry,
  • Davide Fazzini,
  • Mauricio Féo,
  • Antonio Fernandez Prieto,
  • Alex Daniel Fernez,
  • Fabio Ferrari,
  • Lino Ferreira Lopes,
  • Fernando Ferreira Rodrigues,
  • Silvia Ferreres Sole,
  • Martina Ferrillo,
  • Massimiliano Ferro-Luzzi,
  • Sergey Filippov,
  • Rosa Anna Fini,
  • Massimiliano Fiorini,
  • Miroslaw Firlej,
  • Kamil Leszek Fischer,
  • K.M. Fischer,
  • Dillon Scott Fitzgerald,
  • Conor Fitzpatrick,
  • Tomasz Fiutowski,
  • Aristeidis Fkiaras,
  • Frederic Fleuret,
  • Marianna Fontana,
  • Flavio Fontanelli,
  • Roger Forty,
  • Daniel Foulds-Holt,
  • Vinicius Franco Lima,
  • Manuel Franco Sevilla,
  • Markus Frank,
  • Edoardo Franzoso,
  • Giulia Frau,
  • Christoph Frei,
  • David Anthony Friday,
  • Jinlin Fu,
  • Quentin Fuehring,
  • Emmy Gabriel,
  • Giuliana Galati,
  • Abraham Gallas Torreira,
  • Domenico Galli,
  • Silvia Gambetta,
  • Yuyue Gan,
  • Miriam Gandelman,
  • Paolo Gandini,
  • Yuanning Gao,
  • Michela Garau,
  • Luis Miguel Garcia Martin,
  • Paula Garcia Moreno,
  • Julián García Pardiñas,
  • Beatriz Garcia Plana,
  • Felipe Andres Garcia Rosales,
  • Lluis Garrido,
  • Clara Gaspar,
  • Robbert Erik Geertsema,
  • David Gerick,
  • Louis Lenard Gerken,
  • Evelina Gersabeck,
  • Marco Gersabeck,
  • Timothy Gershon,
  • Luca Giambastiani,
  • Valerie Gibson,
  • Henryk Karol Giemza,
  • Alexander Leon Gilman,
  • Matteo Giovannetti,
  • Alessandra Gioventù,
  • Pere Gironella Gironell,
  • Carmen Giugliano,
  • Konstantin Gizdov,
  • Evangelos Leonidas Gkougkousis,
  • Vladimir Gligorov,
  • Carla Göbel,
  • Elisabet Golobardes,
  • Dmitry Golubkov,
  • Andrey Golutvin,
  • Alvaro Gomes,
  • Sergio Gomez Fernandez,
  • Fernanda Goncalves Abrantes,
  • Mateusz Goncerz,
  • Guanghua Gong,
  • Petr Gorbounov,
  • Igor Vladimirovich Gorelov,
  • Claudio Gotti,
  • Jascha Peter Grabowski,
  • Thomas Grammatico,
  • Luis Alberto Granado Cardoso,
  • Eugeni Graugés,
  • Elena Graverini,
  • Giacomo Graziani,
  • Alexandru Grecu,
  • Lex Marinus Greeven,
  • Nathan Allen Grieser,
  • Lucia Grillo,
  • Sergey Gromov,
  • Barak Raimond Gruberg Cazon,
  • Chenxi Gu,
  • Marco Guarise,
  • Manuel Guittiere,
  • Paul Andre Günther,
  • Evgeny Gushchin,
  • Andreas Guth,
  • Yury Guz,
  • Thierry Gys,
  • Thomas Hadavizadeh,
  • Guido Haefeli,
  • Christophe Haen,
  • Jakob Haimberger,
  • Susan Haines,
  • Tabitha Halewood-leagas,
  • Phoebe Meredith Hamilton,
  • Jan Patrick Hammerich,
  • Qundong Han,
  • Xiaoxue Han,
  • Eva Brottmann Hansen,
  • Stephanie Hansmann-Menzemer,
  • Neville Harnew,
  • Thomas Harrison,
  • Christoph Hasse,
  • Mark Hatch,
  • Jibo He,
  • Kevin Heijhoff,
  • Kevin Heinicke,
  • Riley Dylan Leslie Henderson,
  • Arthur Marius Hennequin,
  • Karol Hennessy,
  • Louis Henry,
  • Johannes Heuel,
  • Adlène Hicheur,
  • Donal Hill,
  • Martha Hilton,
  • Sophie Elizabeth Hollitt,
  • Ruiwe Hou,
  • Yingrui Hou,
  • Jiangqiao Hu,
  • Jifeng Hu,
  • Wenhua Hu,
  • Xiaofan Hu,
  • Wenqian Huang,
  • Xiaotao Huang,
  • Wouter Hulsbergen,
  • Ross John Hunter,
  • Mikhail Hushchyn,
  • David Hutchcroft,
  • Daniel Hynds,
  • Philipp Ibis,
  • Marek Idzik,
  • Dmitrii Ilin,
  • Philip Ilten,
  • Alexander Inglessi,
  • Aleksandr Iniukhin,
  • Artur Ishteev,
  • Kuzma Ivshin,
  • Richard Jacobsson,
  • Hendrik Jage,
  • Sune Jakobsen,
  • Eddy Jans,
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  • Xiaojie Jiang,
  • Malcolm John,
  • Daniel Johnson,
  • Christopher Jones,
  • Thomas Peter Jones,
  • Beat Jost,
  • Nathan Jurik,
  • Sergii Kandybei,
  • Youen Kang,
  • Matthias Karacson,
  • Dmitrii Karpenkov,
  • Maksim Karpov,
  • Jacob William Kautz,
  • Floris Keizer,
  • Dustin Michael Keller,
  • Matthew Kenzie,
  • Tjeerd Ketel,
  • Basem Khanji,
  • Anastasiia Kharisova,
  • Sergei Kholodenko,
  • Thomas Kirn,
  • Veronica Soelund Kirsebom,
  • Ouail Kitouni,
  • Suzanne Klaver,
  • Nico Kleijne,
  • Konrad Klimaszewski,
  • Mateusz Rafal Kmiec,
  • Serhii Koliiev,
  • Almagul Kondybayeva,
  • Anatoly Konoplyannikov,
  • Pawel Kopciewicz,
  • Renata Kopecna,
  • Patrick Koppenburg,
  • Mikhail Korolev,
  • Igor Kostiuk,
  • Oleksander Kot,
  • Sofia Kotriakhova,
  • Anastasiia Kozachuk,
  • Polina Kravchenko,
  • Leonid Kravchuk,
  • Rafal Dominik Krawczyk,
  • Michal Kreps,
  • Sophie Katharina Kretzschmar,
  • Pavel Krokovny,
  • Wojciech Krupa,
  • Wojciech Krzemien,
  • Jakub Kubat,
  • Marcin Kucharczyk,
  • Vasily Kudryavtsev,
  • Hilbrand Steffen Kuindersma,
  • Gerd Joachim Kunde,
  • Tengiz Kvaratskheliya,
  • Daniel Lacarrere,
  • George Lafferty,
  • Adriano Lai,
  • Andrea Lampis,
  • Davide Lancierini,
  • John Jake Lane,
  • Richard Lane,
  • Gaia Lanfranchi,
  • Christoph Langenbruch,
  • Jan Langer,
  • Oliver Lantwin,
  • Thomas Latham,
  • Federico Lazzari,
  • Renaud Le Gac,
  • Sook Hyun Lee,
  • Regis Lefèvre,
  • Alexander Leflat,
  • Sergey Legotin,
  • Olivier Leroy,
  • Tadeusz Lesiak,
  • Blake Leverington,
  • Hengne Li,
  • Peilian Li,
  • Shiyang Li,
  • Yiming Li,
  • Zhuoming Li,
  • Xixin Liang,
  • Tai-hua Lin,
  • Rolf Lindner,
  • Vitalii Lisovskyi,
  • Roman Litvinov,
  • Guoming Liu,
  • Huanhuan Liu,
  • Qian Liu,
  • Shuaiyi Liu,
  • Aniol Lobo Salvia,
  • Angelo Loi,
  • Riccardo Lollini,
  • Julian Lomba Castro,
  • Iain Longstaff,
  • Jose Lopes,
  • Saúl López Soliño,
  • George Holger Lovell,
  • Yu Lu,
  • Chiara Lucarelli,
  • Donatella Lucchesi,
  • Stanislav Luchuk,
  • Miriam Lucio Martinez,
  • Valeriia Lukashenko,
  • Yiheng Luo,
  • Anna Lupato,
  • Eleonora Luppi,
  • Oliver Lupton,
  • Alberto Lusiani,
  • Xiao-Rui Lyu,
  • Lishuang Ma,
  • Ruiting Ma,
  • Serena Maccolini,
  • Frederic Machefert,
  • Florin Maciuc,
  • Vladimir Macko,
  • Patrick Mackowiak,
  • Samuel Maddrell-Mander,
  • Lakshan Ram Madhan Mohan,
  • Oleg Maev,
  • Artem Maevskiy,
  • Dmitrii Maisuzenko,
  • Maciej Witold Majewski,
  • Jakub Jacek Malczewski,
  • Sneha Malde,
  • Bartosz Malecki,
  • Alexander Malinin,
  • Timofei Maltsev,
  • Hanna Malygina,
  • Giulia Manca,
  • Giampiero Mancinelli,
  • Daniele Manuzzi,
  • Claudio Andrea Manzari,
  • Daniele Marangotto,
  • Jan Maratas,
  • Jean François Marchand,
  • Umberto Marconi,
  • Saverio Mariani,
  • Carla Marin Benito,
  • Matthieu Marinangeli,
  • Jörg Marks,
  • Alexander Mclean Marshall,
  • Phillip John Marshall,
  • Gabriele Martelli,
  • Giuseppe Martellotti,
  • Loris Martinazzoli,
  • Maurizio Martinelli,
  • Diego Martinez Santos,
  • Fernando Martinez Vidal,
  • André Massafferri,
  • Marcel Materok,
  • Rosen Matev,
  • Abhijit Mathad,
  • Viacheslav Matiunin,
  • Clara Matteuzzi,
  • Kara Renee Mattioli,
  • Andrea Mauri,
  • Emilie Maurice,
  • Juan Mauricio,
  • Michal Kazimierz Mazurek,
  • Michael McCann,
  • Lucas Mcconnell,
  • Tamaki Holly Mcgrath,
  • Niall Thomas Mchugh,
  • Andrew McNab,
  • Ronan McNulty,
  • James Vincent Mead,
  • Brian Meadows,
  • Gerwin Meier,
  • Dmytro Melnychuk,
  • Simone Meloni,
  • Marcel Merk,
  • Andrea Merli,
  • Lucas Meyer Garcia,
  • Mikhail Mikhasenko,
  • Diego Alejandro Milanes,
  • Edward James Millard,
  • Marko Milovanovic,
  • Marie-Noelle Minard,
  • Alessandro Minotti,
  • Sara Elizabeth Mitchell,
  • Biljana Mitreska,
  • Dominik Stefan Mitzel,
  • Antje Mödden,
  • Rizwaan Adeeb Mohammed,
  • Razvan Daniel Moise,
  • Sergei Mokhnenko,
  • Titus Mombächer,
  • Igancio Alberto Monroy,
  • Stephane Monteil,
  • Mauro Morandin,
  • Gianfranco Morello,
  • Michael Joseph Morello,
  • Jakub Moron,
  • Adam Benjamin Morris,
  • Andrew George Morris,
  • Raymond Mountain,
  • Hongjie Mu,
  • Franz Muheim,
  • Mick Mulder,
  • Katharina Müller,
  • Colm Harold Murphy,
  • Donal Murray,
  • Rebecca Murta,
  • Piera Muzzetto,
  • Paras Naik,
  • Tatsuya Nakada,
  • Raja Nandakumar,
  • Tara Nanut,
  • Irina Nasteva,
  • Matthew Needham,
  • Nicola Neri,
  • Sebastian Neubert,
  • Niko Neufeld,
  • Ryan Newcombe,
  • Elisabeth Maria Niel,
  • Simon Nieswand,
  • Nikolay Nikitin,
  • Niklas Stefan Nolte,
  • Camille Normand,
  • Cynthia Nunez,
  • Agnieszka Oblakowska-Mucha,
  • Vladimir Obraztsov,
  • Thomas Oeser,
  • Daniel Patrick O'Hanlon,
  • Shinichi Okamura,
  • Rudolf Oldeman,
  • Federica Oliva,
  • Mario Edgardo Olivares,
  • C.J. G. Onderwater,
  • Ryunosuke Hugo O'Neil,
  • Juan Martin Otalora Goicochea,
  • Tatiana Ovsiannikova,
  • Patrick Owen,
  • Maria Aranzazu Oyanguren,
  • Ozlem Ozcelik,
  • Klaas Ole Padeken,
  • Bhagyashree Pagare,
  • Preema Rennee Pais,
  • Tommaso Pajero,
  • Antimo Palano,
  • Matteo Palutan,
  • Yue Pan,
  • Gennady Panshin,
  • Antonios Papanestis,
  • Marco Pappagallo,
  • Luciano Pappalardo,
  • Cheryl Pappenheimer,
  • William Parker,
  • Christopher Parkes,
  • Barbara Passalacqua,
  • Giovanni Passaleva,
  • Alessandra Pastore,
  • Mitesh Patel,
  • Claudia Patrignani,
  • Christopher James Pawley,
  • Alex Pearce,
  • Antonio Pellegrino,
  • Monica Pepe Altarelli,
  • Stefano Perazzini,
  • Dmitrii Pereima,
  • Asier Pereiro Castro,
  • Pascal Perret,
  • Marko Petric,
  • Konstantinos Petridis,
  • Alessandro Petrolini,
  • Aleksandr Petrov,
  • Stefano Petrucci,
  • Marco Petruzzo,
  • Thi Thuy Hang Pham,
  • Anton Philippov,
  • Roberto Piandani,
  • Lorenzo Pica,
  • Mauro Piccini,
  • Boleslaw Pietrzyk,
  • Guillaume Pietrzyk,
  • Martina Pili,
  • Davide Pinci,
  • Flavio Pisani,
  • Marco Pizzichemi,
  • P.K. Resmi,
  • Vlad-Mihai Placinta,
  • Jonathan Plews,
  • Maximo Plo Casasus,
  • Francesco Polci,
  • Marco Poli Lener,
  • Mariia Poliakova,
  • Anton Poluektov,
  • Natalia Polukhina,
  • Ivan Polyakov,
  • Erica Polycarpo,
  • Sebastien Ponce,
  • Dmitry Popov,
  • Sergei Popov,
  • Stanislav Poslavskii,
  • Kodassery Prasanth,
  • Laura Promberger,
  • Claire Prouve,
  • Valery Pugatch,
  • Veronique Puill,
  • Giovanni Punzi,
  • Hongrong Qi,
  • Wenbin Qian,
  • Ning Qin,
  • Renato Quagliani,
  • Naomi Veronika Raab,
  • Raul Iraq Rabadan Trejo,
  • Bartlomiej Rachwal,
  • Jonas Rademacker,
  • Rohan Rajagopalan,
  • Matteo Rama,
  • Miguel Ramos Pernas,
  • Murilo Rangel,
  • Fedor Ratnikov,
  • Gerhard Raven,
  • Meril Reboud,
  • Federico Redi,
  • Florian Reiss,
  • Clara Remon Alepuz,
  • Zan Ren,
  • Victor Renaudin,
  • Roberto Ribatti,
  • Alessandro Maria Ricci,
  • Stefania Ricciardi,
  • Kurt Rinnert,
  • Patrick Robbe,
  • Gary Robertson,
  • Ana Barbara Rodrigues,
  • Eduardo Rodrigues,
  • Jairo Alexis Rodriguez Lopez,
  • E.R. R. Rodriguez Rodriguez,
  • Alexandra Paige Rollings,
  • Philipp Roloff,
  • Vladimir Romanovskiy,
  • Marcos Romero Lamas,
  • Antonio Romero Vidal,
  • Jordan Daniel Roth,
  • Marcello Rotondo,
  • Matthew Scott Rudolph,
  • Thomas Ruf,
  • Ramon Angel Ruiz Fernandez,
  • Joan Ruiz Vidal,
  • Artem Ryzhikov,
  • Jakub Ryzka,
  • Juan Jose Saborido Silva,
  • Naylya Sagidova,
  • Niladribihari Sahoo,
  • Biagio Saitta,
  • Matteo Salomoni,
  • Cristina Sanchez Gras,
  • Izaac Sanderswood,
  • Roberta Santacesaria,
  • Cibran Santamarina Rios,
  • Marco Santimaria,
  • Emanuele Santovetti,
  • Danila Saranin,
  • Gediminas Sarpis,
  • Mindaugas Sarpis,
  • Alessio Sarti,
  • Celestina Satriano,
  • Alessia Satta,
  • Miroslav Saur,
  • Darya Savrina,
  • Halime Sazak,
  • Luke George Scantlebury Smead,
  • Alessandro Scarabotto,
  • Stefan Schael,
  • Sigrid Scherl,
  • Manuel Schiller,
  • Heinrich Schindler,
  • Michael Schmelling,
  • Burkhard Schmidt,
  • Sebastian Schmitt,
  • Olivier Schneider,
  • Andreas Schopper,
  • Maxime Schubiger,
  • Sebastian Schulte,
  • Marie Helene Schune,
  • Rainer Schwemmer,
  • Barbara Sciascia,
  • Sara Sellam,
  • Alexander Semennikov,
  • Mara Senghi Soares,
  • Antonino Sergi,
  • Nicola Serra,
  • Lorenzo Sestini,
  • Alex Seuthe,
  • Yiduo Shang,
  • Desmond Mzamo Shangase,
  • Mikhail Shapkin,
  • Ivan Shchemerov,
  • Lesya Shchutska,
  • Tara Shears,
  • Lev Shekhtman,
  • Zhihong Shen,
  • Shuqi Sheng,
  • Vladimir Shevchenko,
  • Edward Brendan Shields,
  • Yuya Shimizu,
  • Evgenii Shmanin,
  • Joseph David Shupperd,
  • Benedetto Gianluca Siddi,
  • Rafael Silva Coutinho,
  • Gabriele Simi,
  • Saverio Simone,
  • Minni Singla,
  • Nicola Skidmore,
  • Raphael Skuza,
  • Tomasz Skwarnicki,
  • Mark Slater,
  • Igor Slazyk,
  • Jennifer Clare Smallwood,
  • John Gordon Smeaton,
  • Eluned Smith,
  • Mark Smith,
  • Aleksandra Snoch,
  • Lais Soares Lavra,
  • Michael Sokoloff,
  • F.J. P. Soler,
  • Aleksandr Solovev,
  • Ivan Solovyev,
  • Felipe Luan Souza De Almeida,
  • Bruno Souza De Paula,
  • Bernhard Spaan,
  • Elisabetta Spadaro Norella,
  • Patrick Spradlin,
  • Federico Stagni,
  • Marian Stahl,
  • Sascha Stahl,
  • Seophine Stanislaus,
  • Olaf Steinkamp,
  • Oleg Stenyakin,
  • Holger Stevens,
  • Sheldon Stone,
  • Daria Strekalina,
  • Fidan Suljik,
  • Jiayin Sun,
  • Liang Sun,
  • Yipeng Sun,
  • Peter Svihra,
  • Paul Nathaniel Swallow,
  • Krzysztof Swientek,
  • Adam Szabelski,
  • Tomasz Szumlak,
  • Maciej Pawel Szymanski,
  • Shantam Taneja,
  • Alastair Roger Tanner,
  • Martin Duy Tat,
  • Aleksandr Terentev,
  • Frederic Teubert,
  • Eric Thomas,
  • Daniel James David Thompson,
  • Kayleigh Anne Thomson,
  • Hanae Tilquin,
  • Vincent Tisserand,
  • Stephane T'Jampens,
  • Mark Tobin,
  • Luca Tomassetti,
  • Xingyu Tong,
  • Diego Torres Machado,
  • Da Yu Tou,
  • Ekaterina Trifonova,
  • Stoyan Miroslavov Trilov,
  • Carina Trippl,
  • Giulia Tuci,
  • Alison Tully,
  • Niels Tuning,
  • Artur Ukleja,
  • Daniel Joachim Unverzagt,
  • Eduard Ursov,
  • Andrii Usachov,
  • Andrey Ustyuzhanin,
  • Ulrich Uwer,
  • Alexander Vagner,
  • Vincenzo Vagnoni,
  • Andrea Valassi,
  • Giovanni Valenti,
  • Nuria Valls Canudas,
  • Martinus van Beuzekom,
  • Maarten Van Dijk,
  • Hubert Van Hecke,
  • Eric van Herwijnen,
  • Maarten van Veghel,
  • Ricardo Vazquez Gomez,
  • Pablo Vazquez Regueiro,
  • Carlos Vázquez Sierra,
  • Stefania Vecchi,
  • Jaap Velthuis,
  • Michele Veltri,
  • Aravindhan Venkateswaran,
  • Michele Veronesi,
  • Mika Vesterinen,
  • Daniel Vieira,
  • Maria Vieites Diaz,
  • Harald Viemann,
  • Xavier Vilasis-Cardona,
  • Eva Vilella Figueras,
  • Andrea Villa,
  • Pascal Vincent,
  • Felicia Carolin Volle,
  • Dorothea Vom Bruch,
  • Alexey Vorobyev,
  • Vitaly Vorobyev,
  • Nikolai Voropaev,
  • Kimberley Vos,
  • Roland Waldi,
  • John Walsh,
  • Chishuai Wang,
  • Jialu Wang,
  • Jianchun Wang,
  • Jianqiao Wang,
  • Jike Wang,
  • Mengzhen Wang,
  • Rui Wang,
  • Yilong Wang,
  • Zhenzi Wang,
  • Zirui Wang,
  • Ziyi Wang,
  • Jake Alexander Ward,
  • Nigel Watson,
  • David Websdale,
  • Constantin Weisser,
  • Benedict Donald C Westhenry,
  • Dylan Jaide White,
  • Mark Whitehead,
  • Aidan Richard Wiederhold,
  • Dirk Wiedner,
  • Guy Wilkinson,
  • Michael Kent Wilkinson,
  • Ifan Williams,
  • Mike Williams,
  • Mark Richard James Williams,
  • Fergus Wilson,
  • Wojciech Wislicki,
  • Mariusz Witek,
  • Lukas Witola,
  • Guy Wormser,
  • Stephen Wotton,
  • Hangyi Wu,
  • Kenneth Wyllie,
  • Zhiyu Xiang,
  • Dong Xiao,
  • Yuehong Xie,
  • Ao Xu,
  • Jingyi Xu,
  • Li Xu,
  • Menglin Xu,
  • Qingnian Xu,
  • Zehua Xu,
  • Zhihao Xu,
  • Di Yang,
  • Shuangli Yang,
  • Youhua Yang,
  • Zhenwei Yang,
  • Zishuo Yang,
  • Yuezhe Yao,
  • Lauren Emma Yeomans,
  • Hang Yin,
  • Jiesheng Yu,
  • Xuhao Yuan,
  • Oleg Yushchenko,
  • Ettore Zaffaroni,
  • Mikhail Zavertyaev,
  • Milosz Zdybal,
  • Oleksandr Zenaiev,
  • Ming Zeng,
  • Dongliang Zhang,
  • Liming Zhang,
  • Shulei Zhang,
  • Shunan Zhang,
  • Yanxi Zhang,
  • Yu Zhang,
  • Alina Zharkova,
  • Alexey Zhelezov,
  • Yangheng Zheng,
  • Tianwen Zhou,
  • Xiaokang Zhou,
  • Yixiong Zhou,
  • Valeriia Zhovkovska,
  • Xianglei Zhu,
  • Xiaoyu Zhu,
  • Zhanwen Zhu,
  • Valery Zhukov,
  • Quan Zou,
  • Stefano Zucchelli,
  • Davide Zuliani,
  • Gianluca Zunica
  • (less)
abstract + abstract -

The $ {\varXi}_{cc}^{++}\to {\varXi}_c^{\prime +}{\pi}^{+} $ decay is observed using proton-proton collisions collected by the LHCb experiment at a centre-of-mass energy of 13 TeV, corresponding to an integrated luminosity of 5.4 fb−1. The $ {\varXi}_{cc}^{++}\to {\varXi}_c^{\prime +}{\pi}^{+} $ decay is reconstructed partially, where the photon from the $ {\varXi}_c^{\prime +}\to {\varXi}_c^{+}\gamma $ decay is not reconstructed and the pK$^{−}$π$^{+}$ final state of the $ {\varXi}_c^{+} $ baryon is employed. The $ {\varXi}_{cc}^{++}\to {\varXi}_c^{\prime +}{\pi}^{+} $branching fraction relative to that of the $ {\varXi}_{cc}^{++}\to {\varXi}_c^{+}{\pi}^{+} $ decay is measured to be 1.41 ± 0.17 ± 0.10, where the first uncertainty is statistical and the second systematic.[graphic not available: see fulltext]


(558)The ALPs from the top: searching for long lived axion-like particles from exotic top decays
  • Adrian Carmona,
  • Fatemeh Elahi,
  • Christiane Scherb,
  • Pedro Schwaller
abstract + abstract -

We propose a search for long lived axion-like particles (ALPs) in exotic top decays. Flavour-violating ALPs appear as low energy effective theories for various new physics scenarios such as t-channel dark sectors or Froggatt-Nielsen models. In this case the top quark may decay to an ALP and an up- or charm-quark. For masses in the few GeV range, the ALP is long lived across most of the viable parameter space, suggesting a dedicated search. We propose to search for these long lived ALPs in $ t\overline{t} $ events, using one top quark as a trigger. We focus on ALPs decaying in the hadronic calorimeter, and show that the ratio of energy deposits in the electromagnetic and hadronic calorimeters as well as track vetoes can efficiently suppress Standard Model backgrounds. Our proposed search can probe exotic top branching ratios smaller than 10$^{−4}$ with a conservative strategy at the upcoming LHC run, and potentially below the 10$^{−7}$ level with more advanced methods. Finally we also show that measurements of single top production probe these branching ratios in the very short and very long lifetime limit at the 10$^{−3}$ level.


(557)Irreversibility in linear systems with colored noise
  • Grzegorz Gradziuk,
  • Gabriel Torregrosa,
  • Chase P. Broedersz
Physical Review E (02/2022) doi:10.1103/PhysRevE.105.024118
abstract + abstract -

Time irreversibility is a distinctive feature of nonequilibrium dynamics and several measures of irreversibility have been introduced to assess the distance from thermal equilibrium of a stochastically driven system. While the dynamical noise is often approximated as white, in many real applications the time correlations of the random forces can actually be significantly long-lived compared to the relaxation times of the driven system. We analyze the effects of temporal correlations in the noise on commonly used measures of irreversibility and demonstrate how the theoretical framework for white-noise-driven systems naturally generalizes to the case of colored noise. Specifically, we express the autocorrelation function, the area enclosing rates, and mean phase space velocity in terms of solutions of a Lyapunov equation and in terms of their white-noise limit values.


(556)On phase-space integrals with Heaviside functions
  • Daniel Baranowski,
  • Maximilian Delto,
  • Kirill Melnikov,
  • Chen-Yu Wang
Journal of High Energy Physics (02/2022) doi:10.1007/JHEP02(2022)081
abstract + abstract -

We discuss peculiarities that arise in the computation of real-emission contributions to observables that contain Heaviside functions. A prominent example of such a case is the zero-jettiness soft function in SCET, whose calculation at next-to-next-to-next-to-leading order in perturbative QCD is an interesting problem. Since the zero-jettiness soft function distinguishes between emissions into different hemispheres, its definition involves θ-functions of light-cone components of emitted soft partons. This prevents a direct use of multi-loop methods, based on reverse unitarity, for computing the zero-jettiness soft function in high orders of perturbation theory. We propose a way to bypass this problem and illustrate its effectiveness by computing various non-trivial contributions to the zero-jettiness soft function at NNLO and N3LO in perturbative QCD.


(555)Three-loop helicity amplitudes for diphoton production in gluon fusion
  • Piotr Bargieła,
  • Fabrizio Caola,
  • Andreas von Manteuffel,
  • Lorenzo Tancredi
Journal of High Energy Physics (02/2022) doi:10.1007/JHEP02(2022)153
abstract + abstract -

We present a calculation of the helicity amplitudes for the process gg → γγ in three-loop massless QCD. We employ a recently proposed method to calculate scattering amplitudes in the 't Hooft-Veltman scheme that reduces the amount of spurious non-physical information needed at intermediate stages of the computation. Our analytic results for the three-loop helicity amplitudes are remarkably compact, and can be efficiently evaluated numerically. This calculation provides the last missing building block for the computation of NNLO QCD corrections to diphoton production in gluon fusion.


CN-4
RU-D
(554)The iron and oxygen content of LMC Classical Cepheids and its implications for the extragalactic distance scale and Hubble constant. Equivalent width analysis with Kurucz stellar atmosphere models
  • Martino Romaniello,
  • Adam Riess,
  • Sara Mancino,
  • Richard I. Anderson,
  • Wolfram Freudling
  • +4
  • Rolf-Peter Kudritzki,
  • Lucas Macrì,
  • Alessio Mucciarelli,
  • Wenlong Yuan
  • (less)
Astronomy and Astrophysics (02/2022) doi:10.1051/0004-6361/202142441
abstract + abstract -

Context. Classical Cepheids are primary distance indicators and a crucial stepping stone in determining the present-day value of the Hubble constant H0 to the precision and accuracy required to constrain apparent deviations from the ΛCDM Concordance Cosmological Model.
Aims: We measured the iron and oxygen abundances of a statistically significant sample of 89 Cepheids in the Large Magellanic Cloud (LMC), one of the anchors of the local distance scale, quadrupling the prior sample and including 68 of the 70 Cepheids used to constrain H0 by the SH0ES program. The goal is to constrain the extent to which the luminosity of Cepheids is influenced by their chemical composition, which is an important contributor to the uncertainty on the determination of the Hubble constant itself and a critical factor in the internal consistency of the distance ladder.
Methods: We derived stellar parameters and chemical abundances from a self-consistent spectroscopic analysis based on equivalent width of absorption lines.
Results: The iron distribution of Cepheids in the LMC can be very accurately described by a single Gaussian with a mean [Fe/H] = −0.409 ± 0.003 dex and σ = 0.076 ± 0.003 dex. We estimate a systematic uncertainty on the absolute mean values of 0.1 dex. The width of the distribution is fully compatible with the measurement error and supports the low dispersion of 0.069 mag seen in the near-infrared Hubble Space Telescope LMC period-luminosity relation. The uniformity of the abundance has the important consequence that the LMC Cepheids alone cannot provide any meaningful constraint on the dependence of the Cepheid period-luminosity relation on chemical composition at any wavelength. This revises a prior claim based on a small sample of 22 LMC Cepheids that there was little dependence (or uncertainty) between composition and near-infrared luminosity, a conclusion which would produce an apparent conflict between anchors of the distance ladder with different mean abundance. The chemical homogeneity of the LMC Cepheid population makes it an ideal environment in which to calibrate the metallicity dependence between the more metal-poor Small Magellanic Cloud and metal-rich Milky Way and NGC 4258.

Full Tables 1-8 and Appendix B are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/658/A29

Based on observations collected at the European Southern Observatory under ESO programmes 66.D-0571 and 106.21ML.003.


RU-A
(553)Double copy for Lagrangians at trilinear order
  • M. Beneke,
  • P. Hager,
  • A. F. Sanfilippo
Journal of High Energy Physics (02/2022) doi:10.1007/JHEP02(2022)083
abstract + abstract -

We present a novel double-copy prescription for gauge fields at the Lagrangian level and apply it to the original double copy, couplings to matter and the soft theorem. The Yang-Mills Lagrangian in light-cone gauge is mapped directly to the N = 0 supergravity Lagrangian in light-cone gauge to trilinear order, and we show that the obtained result is manifestly equivalent to Einstein gravity at tree level up to this order. The application of the double-copy prescription to couplings to matter is exemplified by scalar and fermionic QCD and finally the soft-collinear effective QCD Lagrangian. The mapping of the latter yields an effective description of an energetic Dirac fermion coupled to the graviton, Kalb-Ramond, and dilaton fields, from which the fermionic gravitational soft and next-to-soft theorems follow.


(552)Dynamical ejecta of neutron star mergers with nucleonic weak processes I: nucleosynthesis
  • I. Kullmann,
  • S. Goriely,
  • O. Just,
  • R. Ardevol-Pulpillo,
  • A. Bauswein
  • +1
Monthly Notices of the Royal Astronomical Society (02/2022) doi:10.1093/mnras/stab3393
abstract + abstract -

We present a coherent study of the impact of neutrino interactions on the r-process element nucleosynthesis and the heating rate produced by the radioactive elements synthesized in the dynamical ejecta of neutron star-neutron star (NS-NS) mergers. We have studied the material ejected from four NS-NS merger systems based on hydrodynamical simulations which handle neutrino effects in an elaborate way by including neutrino equilibration with matter in optically thick regions and re-absorption in optically thin regions. We find that the neutron richness of the dynamical ejecta is significantly affected by the neutrinos emitted by the post-merger remnant, in particular when compared to a case neglecting all neutrino interactions. Our nucleosynthesis results show that a solar-like distribution of r-process elements with mass numbers $A \gtrsim 90$ is produced, including a significant enrichment in Sr and a reduced production of actinides compared to simulations without inclusion of the nucleonic weak processes. The composition of the dynamically ejected matter as well as the corresponding rate of radioactive decay heating are found to be rather independent of the system mass asymmetry and the adopted equation of state. This approximate degeneracy in abundance pattern and heating rates can be favourable for extracting the ejecta properties from kilonova observations, at least if the dynamical component dominates the overall ejecta. Part II of this work will study the light curve produced by the dynamical ejecta of our four NS merger models.


CN-5
RU-C
(551)Cassiopeia A reveals past interaction with circumstellar shell
  • S. Orlando,
  • A. Wongwathanarat,
  • H. -T. Janka,
  • M. Miceli,
  • S. Nagataki
  • +6
  • M. Ono,
  • F. Bocchino,
  • J. Vink,
  • D. Milisavljevic,
  • D. J. Patnaude,
  • G. Peres
  • (less)
arXiv e-prints (02/2022) e-Print:2202.01643
abstract + abstract -

Observations of the SNR Cassiopeia A (Cas A) show asymmetries in the reverse shock that cannot be explained by models describing a remnant expanding through a spherically symmetric wind of the progenitor star. We investigate whether a past interaction of Cas A with a massive asymmetric shell of the circumstellar medium can account for the observed asymmetries. We performed 3D MHD simulations that describe the remnant evolution from the SN to its interaction with a circumstellar shell. The initial conditions are provided by a 3D neutrino-driven SN model whose morphology resembles Cas A. We explored the parameter space of the shell, searching for a set of parameters able to produce reverse shock asymmetries at the age of 350 years analogous to those observed in Cas A. The interaction of the remnant with the shell can match the observed reverse shock asymmetries if the shell was asymmetric with the densest portion in the nearside to the northwest (NW). According to our models, the shell was thin with radius 1.5 pc. The reverse shock shows the following asymmetries at the age of Cas A: i) it moves inward in the observer frame in the NW region, while it moves outward in other regions; ii) the geometric center of the reverse shock is offset to the NW by 0.1 pc from the geometric center of the forward shock; iii) the reverse shock in the NW region has enhanced nonthermal emission because, there, the ejecta enter the reverse shock with a higher relative velocity (between 4000 and 7000 km/s) than in other regions (below 2000 km/s). Our findings suggest the interaction of Cas A with an asymmetric circumstellar shell between 180 and 240 years after the SN event. We suggest that the shell was, most likely, the result of a massive eruption from the progenitor star that occurred about 10^5 years prior to core-collapse. We estimate a total mass of the shell of approximately 2.6 Msun.


(550)Synthetic galaxy clusters and observations based on Dark Energy Survey Year 3 Data
  • T. N. Varga,
  • D. Gruen,
  • S. Seitz,
  • N. MacCrann,
  • E. Sheldon
  • +75
  • W. G. Hartley,
  • A. Amon,
  • A. Choi,
  • A. Palmese,
  • Y. Zhang,
  • M. R. Becker,
  • J. McCullough,
  • E. Rozo,
  • E. S. Rykoff,
  • C. To,
  • S. Grandis,
  • G. M. Bernstein,
  • S. Dodelson,
  • K. Eckert,
  • S. Everett,
  • R. A. Gruendl,
  • I. Harrison,
  • K. Herner,
  • R. P. Rollins,
  • I. Sevilla-Noarbe,
  • M. A. Troxel,
  • B. Yanny,
  • J. Zuntz,
  • H. T. Diehl,
  • M. Jarvis,
  • M. Aguena,
  • S. Allam,
  • J. Annis,
  • E. Bertin,
  • S. Bhargava,
  • D. Brooks,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • M. Costanzi,
  • L. N. da Costa,
  • M. E. S. Pereira,
  • J. De Vicente,
  • S. Desai,
  • J. P. Dietrich,
  • I. Ferrero,
  • B. Flaugher,
  • J. García-Bellido,
  • E. Gaztanaga,
  • D. W. Gerdes,
  • J. Gschwend,
  • G. Gutierrez,
  • S. R. Hinton,
  • K. Honscheid,
  • T. Jeltema,
  • K. Kuehn,
  • N. Kuropatkin,
  • M. A. G. Maia,
  • M. March,
  • P. Melchior,
  • F. Menanteau,
  • R. Miquel,
  • R. Morgan,
  • J. Myles,
  • F. Paz-Chinchón,
  • A. A. Plazas,
  • A. K. Romer,
  • E. Sanchez,
  • V. Scarpine,
  • M. Schubnell,
  • S. Serrano,
  • M. Smith,
  • M. Soares-Santos,
  • E. Suchyta,
  • M. E. C. Swanson,
  • G. Tarle,
  • D. Thomas,
  • J. Weller,
  • J. Weller,
  • DES Collaboration
  • (less)
Monthly Notices of the Royal Astronomical Society (02/2022) doi:10.1093/mnras/stab3269
abstract + abstract -

We develop a novel data-driven method for generating synthetic optical observations of galaxy clusters. In cluster weak lensing, the interplay between analysis choices and systematic effects related to source galaxy selection, shape measurement, and photometric redshift estimation can be best characterized in end-to-end tests going from mock observations to recovered cluster masses. To create such test scenarios, we measure and model the photometric properties of galaxy clusters and their sky environments from the Dark Energy Survey Year 3 (DES Y3) data in two bins of cluster richness $\lambda \in [30; 45)$, $\lambda \in [45; 60)$ and three bins in cluster redshift ($z\in [0.3; 0.35)$, $z\in [0.45; 0.5)$ and $z\in [0.6; 0.65)$. Using deep-field imaging data, we extrapolate galaxy populations beyond the limiting magnitude of DES Y3 and calculate the properties of cluster member galaxies via statistical background subtraction. We construct mock galaxy clusters as random draws from a distribution function, and render mock clusters and line-of-sight catalogues into synthetic images in the same format as actual survey observations. Synthetic galaxy clusters are generated from real observational data, and thus are independent from the assumptions inherent to cosmological simulations. The recipe can be straightforwardly modified to incorporate extra information, and correct for survey incompleteness. New realizations of synthetic clusters can be created at minimal cost, which will allow future analyses to generate the large number of images needed to characterize systematic uncertainties in cluster mass measurements.


(549)Dynamical ejecta of neutron star mergers with nucleonic weak processes - II: kilonova emission
  • O. Just,
  • I. Kullmann,
  • S. Goriely,
  • A. Bauswein,
  • H. -T. Janka
  • +1
Monthly Notices of the Royal Astronomical Society (02/2022) doi:10.1093/mnras/stab3327
abstract + abstract -

The majority of existing results for the kilonova (or macronova) emission from material ejected during a neutron-star (NS) merger is based on (quasi-) one-zone models or manually constructed toy-model ejecta configurations. In this study, we present a kilonova analysis of the material ejected during the first $\sim 10\,$ ms of a NS merger, called dynamical ejecta, using directly the outflow trajectories from general relativistic smoothed-particle hydrodynamics simulations, including a sophisticated neutrino treatment and the corresponding nucleosynthesis results, which have been presented in Part I of this study. We employ a multidimensional two-moment radiation transport scheme with approximate M1 closure to evolve the photon field and use a heuristic prescription for the opacities found by calibration with atomic-physics-based reference results. We find that the photosphere is generically ellipsoidal but augmented with small-scale structure and produces emission that is about 1.5-3 times stronger towards the pole than the equator. The kilonova typically peaks after $0.7\!-\!1.5\,$ d in the near-infrared frequency regime with luminosities between $3\!-\!7\times 10^{40}\,$ erg s-1 and at photospheric temperatures of $2.2\!-\!2.8\times 10^3\,$ K. A softer equation of state or higher binary-mass asymmetry leads to a longer and brighter signal. Significant variations of the light curve are also obtained for models with artificially modified electron fractions, emphasizing the importance of a reliable neutrino-transport modelling. None of the models investigated here, which only consider dynamical ejecta, produces a transient as bright as AT2017gfo. The near-infrared peak of our models is incompatible with the early blue component of AT2017gfo.


(548)Differentiable Matrix Elements with MadJax
  • Lukas Heinrich,
  • Michael Kagan
arXiv e-prints (02/2022) e-Print:2203.00057
abstract + abstract -

MadJax is a tool for generating and evaluating differentiable matrix elements of high energy scattering processes. As such, it is a step towards a differentiable programming paradigm in high energy physics that facilitates the incorporation of high energy physics domain knowledge, encoded in simulation software, into gradient based learning and optimization pipelines. MadJax comprises two components: (a) a plugin to the general purpose matrix element generator MadGraph that integrates matrix element and phase space sampling code with the JAX differentiable programming framework, and (b) a standalone wrapping API for accessing the matrix element code and its gradients, which are computed with automatic differentiation. The MadJax implementation and example applications of simulation based inference and normalizing flow based matrix element modeling, with capabilities enabled uniquely with differentiable matrix elements, are presented.


MIAPbP
(547)Smearing scale in Laguerre reconstructions of the correlation function
  • Farnik Nikakhtar,
  • Ravi K. Sheth,
  • Idit Zehavi
Physical Review D (02/2022) doi:10.1103/PhysRevD.105.043536
abstract + abstract -

To a good approximation, on large scales, the evolved two-point correlation function of biased tracers is related to the initial one by a convolution with a smearing kernel. For Gaussian initial conditions, the smearing kernel is Gaussian, so if the initial correlation function is parametrized using simple polynomials, then the evolved correlation function is a sum of generalized Laguerre functions of half-integer order. This motivates an analytic "Laguerre reconstruction" algorithm which previous work has shown is fast and accurate. This reconstruction requires as input the width of the smearing kernel. We show that the method can be extended to estimate the width of the smearing kernel from the same dataset. This estimate, and associated uncertainties, can then be used to marginalize over the distribution of reconstructed shapes and hence provide error estimates on the value of the distance scale. This procedure is not tied to a particular cosmological model. We also show that if, instead, we parametrize the evolved correlation function using simple polynomials, then the initial one is a sum of Hermite polynomials, again enabling fast and accurate deconvolution. If one is willing to use constraints on the smearing scale from other datasets, then marginalizing over its value is simpler for this latter, "Hermite" reconstruction, potentially providing further speed-ups in cosmological analyses.


CN-3
CN-4
RU-C
RU-D
(546)Euclid: Forecasts from redshift-space distortions and the Alcock-Paczynski test with cosmic voids
  • N. Hamaus,
  • M. Aubert,
  • A. Pisani,
  • S. Contarini,
  • G. Verza
  • +125
  • M. -C. Cousinou,
  • S. Escoffier,
  • A. Hawken,
  • G. Lavaux,
  • G. Pollina,
  • B. D. Wandelt,
  • J. Weller,
  • M. Bonici,
  • C. Carbone,
  • L. Guzzo,
  • A. Kovacs,
  • F. Marulli,
  • E. Massara,
  • L. Moscardini,
  • P. Ntelis,
  • W. J. Percival,
  • S. Radinović,
  • M. Sahlén,
  • Z. Sakr,
  • A. G. Sánchez,
  • H. A. Winther,
  • N. Auricchio,
  • S. Awan,
  • R. Bender,
  • C. Bodendorf,
  • D. Bonino,
  • E. Branchini,
  • M. Brescia,
  • J. Brinchmann,
  • V. Capobianco,
  • J. Carretero,
  • F. J. Castander,
  • M. Castellano,
  • S. Cavuoti,
  • A. Cimatti,
  • R. Cledassou,
  • G. Congedo,
  • L. Conversi,
  • Y. Copin,
  • L. Corcione,
  • M. Cropper,
  • A. Da Silva,
  • H. Degaudenzi,
  • M. Douspis,
  • F. Dubath,
  • C. A. J. Duncan,
  • X. Dupac,
  • S. Dusini,
  • A. Ealet,
  • S. Ferriol,
  • P. Fosalba,
  • M. Frailis,
  • E. Franceschi,
  • P. Franzetti,
  • M. Fumana,
  • B. Garilli,
  • B. Gillis,
  • C. Giocoli,
  • A. Grazian,
  • F. Grupp,
  • S. V. H. Haugan,
  • W. Holmes,
  • F. Hormuth,
  • K. Jahnke,
  • S. Kermiche,
  • A. Kiessling,
  • M. Kilbinger,
  • T. Kitching,
  • M. Kümmel,
  • M. Kunz,
  • H. Kurki-Suonio,
  • S. Ligori,
  • P. B. Lilje,
  • I. Lloro,
  • E. Maiorano,
  • O. Marggraf,
  • K. Markovic,
  • R. Massey,
  • S. Maurogordato,
  • M. Melchior,
  • M. Meneghetti,
  • G. Meylan,
  • M. Moresco,
  • E. Munari,
  • S. M. Niemi,
  • C. Padilla,
  • S. Paltani,
  • F. Pasian,
  • K. Pedersen,
  • V. Pettorino,
  • S. Pires,
  • M. Poncet,
  • L. Popa,
  • L. Pozzetti,
  • R. Rebolo,
  • J. Rhodes,
  • H. Rix,
  • M. Roncarelli,
  • E. Rossetti,
  • R. Saglia,
  • P. Schneider,
  • A. Secroun,
  • G. Seidel,
  • S. Serrano,
  • C. Sirignano,
  • G. Sirri,
  • J. -L. Starck,
  • P. Tallada-Crespí,
  • D. Tavagnacco,
  • A. N. Taylor,
  • I. Tereno,
  • R. Toledo-Moreo,
  • F. Torradeflot,
  • E. A. Valentijn,
  • L. Valenziano,
  • Y. Wang,
  • N. Welikala,
  • G. Zamorani,
  • J. Zoubian,
  • S. Andreon,
  • M. Baldi,
  • S. Camera,
  • S. Mei,
  • C. Neissner,
  • E. Romelli
  • (less)
Astronomy and Astrophysics (02/2022) doi:10.1051/0004-6361/202142073
abstract + abstract -

Euclid is poised to survey galaxies across a cosmological volume of unprecedented size, providing observations of more than a billion objects distributed over a third of the full sky. Approximately 20 million of these galaxies will have their spectroscopy available, allowing us to map the three-dimensional large-scale structure of the Universe in great detail. This paper investigates prospects for the detection of cosmic voids therein and the unique benefit they provide for cosmological studies. In particular, we study the imprints of dynamic (redshift-space) and geometric (Alcock-Paczynski) distortions of average void shapes and their constraining power on the growth of structure and cosmological distance ratios. To this end, we made use of the Flagship mock catalog, a state-of-the-art simulation of the data expected to be observed with Euclid. We arranged the data into four adjacent redshift bins, each of which contains about 11 000 voids and we estimated the stacked void-galaxy cross-correlation function in every bin. Fitting a linear-theory model to the data, we obtained constraints on f/b and DMH, where f is the linear growth rate of density fluctuations, b the galaxy bias, DM the comoving angular diameter distance, and H the Hubble rate. In addition, we marginalized over two nuisance parameters included in our model to account for unknown systematic effects in the analysis. With this approach, Euclid will be able to reach a relative precision of about 4% on measurements of f/b and 0.5% on DMH in each redshift bin. Better modeling or calibration of the nuisance parameters may further increase this precision to 1% and 0.4%, respectively. Our results show that the exploitation of cosmic voids in Euclid will provide competitive constraints on cosmology even as a stand-alone probe. For example, the equation-of-state parameter, w, for dark energy will be measured with a precision of about 10%, consistent with previous more approximate forecasts.

This paper is published on behalf of the Euclid Consortium.


RU-D
(545)Galaxy velocity bias in cosmological simulations: towards per cent-level calibration
  • Dhayaa Anbajagane,
  • Han Aung,
  • August E. Evrard,
  • Arya Farahi,
  • Daisuke Nagai
  • +6
  • David J. Barnes,
  • Weiguang Cui,
  • Klaus Dolag,
  • Ian G. McCarthy,
  • Elena Rasia,
  • Gustavo Yepes
  • (less)
Monthly Notices of the Royal Astronomical Society (02/2022) doi:10.1093/mnras/stab3587
abstract + abstract -

Galaxy cluster masses, rich with cosmological information, can be estimated from internal dark matter (DM) velocity dispersions, which in turn can be observationally inferred from satellite galaxy velocities. However, galaxies are biased tracers of the DM, and the bias can vary over host halo and galaxy properties as well as time. We precisely calibrate the velocity bias, bv - defined as the ratio of galaxy and DM velocity dispersions - as a function of redshift, host halo mass, and galaxy stellar mass threshold ($M_{\rm \star , sat}$), for massive haloes ($M_{\rm 200c}\gt 10^{13.5} \, {\rm M}_\odot$) from five cosmological simulations: IllustrisTNG, Magneticum, Bahamas + Macsis, The Three Hundred Project, and MultiDark Planck-2. We first compare scaling relations for galaxy and DM velocity dispersion across simulations; the former is estimated using a new ensemble velocity likelihood method that is unbiased for low galaxy counts per halo, while the latter uses a local linear regression. The simulations show consistent trends of bv increasing with M200c and decreasing with redshift and $M_{\rm \star , sat}$. The ensemble-estimated theoretical uncertainty in bv is 2-3 per cent, but becomes percent-level when considering only the three highest resolution simulations. We update the mass-richness normalization for an SDSS redMaPPer cluster sample, and find our improved bv estimates reduce the normalization uncertainty from 22 to 8 per cent, demonstrating that dynamical mass estimation is competitive with weak lensing mass estimation. We discuss necessary steps for further improving this precision. Our estimates for $b_v(M_{\rm 200c}, M_{\rm \star , sat}, z)$ are made publicly available.


CN-7
(544)Muonic boson limits: Supernova redux
  • Andrea Caputo,
  • Georg Raffelt,
  • Edoardo Vitagliano
abstract + abstract -

We derive supernova (SN) bounds on muon-philic bosons, taking advantage of the recent emergence of muonic SN models. Our main innovations are to consider scalars ϕ in addition to pseudoscalars a and to include systematically the generic two-photon coupling Gγ γ implied by a muon triangle loop. This interaction allows for Primakoff scattering and radiative boson decays. The globular-cluster bound Gγ γ<0.67 ×10-10 GeV-1 carries over to the muonic Yukawa couplings as ga<3.1 ×10-9 and gϕ<4.6 ×10-9 for ma ,ϕ≲100 keV , so SN arguments become interesting mainly for larger masses. If bosons escape freely from the SN core the main constraints originate from SN 1987A γ rays and the diffuse cosmic γ -ray background. The latter allows at most 10-4 of a typical total SN energy of ESN≃3 ×1053 erg to show up as γ rays, for ma ,ϕ≳100 keV implying ga≲0.9 ×10-10 and gϕ≲0.4 ×10-10. In the trapping regime the bosons emerge as quasi-thermal radiation from a region near the neutrino sphere and match Lν for ga ,ϕ≃10-4. However, the 2 γ decay is so fast that all the energy is dumped into the surrounding progenitor-star matter, whereas at most 10-2ESN may show up in the explosion. To suppress boson emission below this level we need yet larger couplings, ga≳2 ×10-3 and gϕ≳4 ×10-3. Muonic scalars can explain the muon magnetic-moment anomaly for gϕ≃0.4 ×10-3, a value hard to reconcile with SN physics despite the uncertainty of the explosion-energy bound. For generic axionlike particles, this argument covers the "cosmological triangle" in the Ga γ γ- ma parameter space.


RU-D
(543)On the tidal formation of dark matter-deficient galaxies
  • Go Ogiya,
  • Frank C. van den Bosch,
  • Andreas Burkert
Monthly Notices of the Royal Astronomical Society (02/2022) doi:10.1093/mnras/stab3658
abstract + abstract -

Previous studies have shown that dark matter-deficient galaxies (DMDG) such as NGC 1052-DF2 (hereafter DF2) can result from tidal stripping. An important question, though, is whether such a stripping scenario can explain DF2's large specific frequency of globular clusters (GCs). After all, tidal stripping and shocking preferentially remove matter from the outskirts. We examine this using idealized, high-resolution simulations of a regular dark matter-dominated galaxy that is accreted on to a massive halo. As long as the initial (pre-infall) dark matter halo of the satellite is cored, which is consistent with predictions of cosmological, hydrodynamical simulations, the tidal remnant can be made to resemble DF2 in all its properties, including its GC population. The required orbit has a pericentre at the 8.3 percentile of the distribution for subhaloes at infall, and thus is not particularly extreme. On this orbit the satellite loses 98.5 (30) per cent of its original dark matter (stellar) mass, and thus evolves into a DMDG. The fraction of GCs that is stripped off depends on the initial radial distribution. If, at infall, the median projected radius of the GC population is roughly two times that of the stars, consistent with observations of isolated galaxies, only ~20 per cent of the GCs are stripped off. This is less than for the stars, which is due to dynamical friction counteracting the tidal stirring. We predict that, if indeed DF2 was crafted by strong tides, its stellar outskirts should have a very shallow metallicity gradient.


(542)A novel black hole mass scaling relation based on coronal gas, and its dependence with the accretion disc
  • Almudena Prieto,
  • Alberto Rodríguez-Ardila,
  • Swayamtrupta Panda,
  • Murilo Marinello
Monthly Notices of the Royal Astronomical Society (02/2022) doi:10.1093/mnras/stab3414
abstract + abstract -

Using bona-fide black hole (BH) mass estimates from reverberation mapping and the line ratio [Si VI] 1.963$\rm{\mu m}$/Brγbroad as tracer of the AGN ionizing continuum, a novel BH-mass scaling relation of the form log(MBH) = (6.40 ± 0.17) - (1.99 ± 0.37) × log ([Si VI]/Brγbroad), dispersion 0.47 dex, over the BH mass interval, 106-108 M is found. Following on the geometrically thin accretion disc approximation and after surveying a basic parameter space for coronal lines production, we believe one of main drivers of the relation is the effective temperature of the disc, which is effectively sampled by the [Si VI] 1.963$\rm{\mu m}$ coronal line for the range of BH masses considered. By means of CLOUDY photoionization models, the observed anticorrelation appears to be formally in line with the thin disc prediction Tdisc ∝ MBH-1/4.


(541)Subdiffusive Activity Spreading in the Diffusive Epidemic Process
  • Borislav Polovnikov,
  • Patrick Wilke,
  • Erwin Frey
Physical Review Letters (02/2022) doi:10.1103/PhysRevLett.128.078302
abstract + abstract -

The diffusive epidemic process is a paradigmatic example of an absorbing state phase transition in which healthy and infected individuals spread with different diffusion constants. Using stochastic activity spreading simulations in combination with finite-size scaling analyses we reveal two qualitatively different processes that characterize the critical dynamics: subdiffusive propagation of infection clusters and diffusive fluctuations in the healthy population. This suggests the presence of a strong-coupling regime and sheds new light on a long-standing debate about the theoretical classification of the system.


(540)The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium
  • Jessica M. Hislop,
  • Thorsten Naab,
  • Ulrich P. Steinwandel,
  • Natalia Lahén,
  • Dimitrios Irodotou
  • +2
  • Peter H. Johansson,
  • Stefanie Walch
  • (less)
Monthly Notices of the Royal Astronomical Society (02/2022) doi:10.1093/mnras/stab3347
abstract + abstract -

We present results on the star cluster properties from a series of high resolution smoothed particles hydrodynamics (SPH) simulations of isolated dwarf galaxies as part of the GRIFFIN project. The simulations at sub-parsec spatial resolution and a minimum particle mass of 4 M incorporate non-equilibrium heating, cooling, and chemistry processes, and realize individual massive stars. The simulations follow feedback channels of massive stars that include the interstellar-radiation field variable in space and time, the radiation input by photo-ionization and supernova explosions. Varying the star formation efficiency per free-fall time in the range ϵff = 0.2-50${{\ \rm per\ cent}}$ neither changes the star formation rates nor the outflow rates. While the environmental densities at star formation change significantly with ϵff, the ambient densities of supernovae are independent of ϵff indicating a decoupling of the two processes. At low ϵff, gas is allowed to collapse more before star formation, resulting in more massive, and increasingly more bound star clusters are formed, which are typically not destroyed. With increasing ϵff, there is a trend for shallower cluster mass functions and the cluster formation efficiency Γ for young bound clusters decreases from $50 {{\ \rm per\ cent}}$ to $\sim 1 {{\ \rm per\ cent}}$ showing evidence for cluster disruption. However, none of our simulations form low mass (<103 M) clusters with structural properties in perfect agreement with observations. Traditional star formation models used in galaxy formation simulations based on local free-fall times might therefore be unable to capture star cluster properties without significant fine tuning.


(539)HOLISMOKES. VII. Time-delay measurement of strongly lensed Type Ia supernovae using machine learning
  • S. Huber,
  • S. H. Suyu,
  • D. Ghoshdastidar,
  • S. Taubenberger,
  • V. Bonvin
  • +5
  • J. H. H. Chan,
  • M. Kromer,
  • U. M. Noebauer,
  • S. A. Sim,
  • L. Leal-Taixé
  • (less)
Astronomy and Astrophysics (02/2022) doi:10.1051/0004-6361/202141956
abstract + abstract -

The Hubble constant (H0) is one of the fundamental parameters in cosmology, but there is a heated debate around the > 4σ tension between the local Cepheid distance ladder and the early Universe measurements. Strongly lensed Type Ia supernovae (LSNe Ia) are an independent and direct way to measure H0, where a time-delay measurement between the multiple supernova (SN) images is required. In this work, we present two machine learning approaches for measuring time delays in LSNe Ia, namely, a fully connected neural network (FCNN) and a random forest (RF). For the training of the FCNN and the RF, we simulate mock LSNe Ia from theoretical SN Ia models that include observational noise and microlensing. We test the generalizability of the machine learning models by using a final test set based on empirical LSN Ia light curves not used in the training process, and we find that only the RF provides a low enough bias to achieve precision cosmology; as such, RF is therefore preferred over our FCNN approach for applications to real systems. For the RF with single-band photometry in the i band, we obtain an accuracy better than 1% in all investigated cases for time delays longer than 15 days, assuming follow-up observations with a 5σ point-source depth of 24.7, a two day cadence with a few random gaps, and a detection of the LSNe Ia 8 to 10 days before peak in the observer frame. In terms of precision, we can achieve an approximately 1.5-day uncertainty for a typical source redshift of ∼0.8 on the i band under the same assumptions. To improve the measurement, we find that using three bands, where we train a RF for each band separately and combine them afterward, helps to reduce the uncertainty to ∼1.0 day. The dominant source of uncertainty is the observational noise, and therefore the depth is an especially important factor when follow-up observations are triggered. We have publicly released the microlensed spectra and light curves used in this work.

https://github.com/shsuyu/HOLISMOKES-public/tree/main/HOLISMOKES_VII


(538)Exploring the relation between turbulent velocity and density fluctuations in the stratified intracluster medium
  • M. Simonte,
  • F. Vazza,
  • F. Brighenti,
  • M. Brüggen,
  • T. W. Jones
  • +1
Astronomy and Astrophysics (02/2022) doi:10.1051/0004-6361/202141703
abstract + abstract -

Context. The dynamics of the intracluster medium (ICM) is affected by turbulence driven by several processes, such as mergers, accretion and feedback from active galactic nuclei.
Aims: X-ray surface brightness fluctuations have been used to constrain turbulence in galaxy clusters. Here, we use simulations to further investigate the relation between gas density and turbulent velocity fluctuations, with a focus on the effect of the stratification of the ICM.
Methods: In this work, we studied the turbulence driven by hierarchical accretion by analysing a sample of galaxy clusters simulated with the cosmological code ENZO. We used a fixed scale filtering approach to disentangle laminar from turbulent flows.
Results: In dynamically perturbed galaxy clusters, we found a relation between the root mean square of density and velocity fluctuations, albeit with a different slope than previously reported. The Richardson number is a parameter that represents the ratio between turbulence and buoyancy, and we found that this variable has a strong dependence on the filtering scale. However, we could not detect any strong relation between the Richardson number and the logarithmic density fluctuations, in contrast to results by recent and more idealised simulations. In particular, we find a strong effect from radial accretion, which appears to be the main driver for the gas fluctuations. The ubiquitous radial bias in the dynamics of the ICM suggests that homogeneity and isotropy are not always valid assumptions, even if the turbulent spectra follow Kolmogorov's scaling. Finally, we find that the slope of the velocity and density spectra are independent of cluster-centric radii.


(537)Hidden in the haystack: low-luminosity globular clusters towards the Milky Way bulge
  • F. Gran,
  • M. Zoccali,
  • I. Saviane,
  • E. Valenti,
  • A. Rojas-Arriagada
  • +6
  • R. Contreras Ramos,
  • J. Hartke,
  • J. A. Carballo-Bello,
  • C. Navarrete,
  • M. Rejkuba,
  • J. Olivares Carvajal
  • (less)
Monthly Notices of the Royal Astronomical Society (02/2022) doi:10.1093/mnras/stab2463
abstract + abstract -

Recent wide-area surveys have enabled us to study the Milky Way with unprecedented detail. Its inner regions, hidden behind dust and gas, have been partially unveiled with the arrival of near-infrared (IR) photometric and spectroscopic data sets. Among recent discoveries, there is a population of low-mass globular clusters, known to be missing, especially towards the Galactic bulge. In this work, five new low-luminosity globular clusters located towards the bulge area are presented. They were discovered by searching for groups in the multidimensional space of coordinates, colours, and proper motions from the Gaia EDR3 catalogue and later confirmed with deeper VVV survey near-IR photometry. The clusters show well-defined red giant branches and, in some cases, horizontal branches with their members forming a dynamically coherent structure in proper motion space. Four of them were confirmed by spectroscopic follow-up with the MUSE instrument on the ESO VLT. Photometric parameters were derived, and when available, metallicities, radial velocities, and orbits were determined. The new clusters Gran 1 and 5 are bulge globular clusters, while Gran 2, 3 and 4 present halo-like properties. Preliminary orbits indicate that Gran 1 might be related to the Main Progenitor, or the so-called 'low-energy' group, while Gran 2, 3 and 5 appears to follow the Gaia-Enceladus/Sausage structure. This study demonstrates that the Gaia proper motions, combined with the spectroscopic follow-up and colour-magnitude diagrams, are required to confirm the nature of cluster candidates towards the inner Galaxy. High stellar crowding and differential extinction may hide other low-luminosity clusters.


(536)Robust sampling for weak lensing and clustering analyses with the Dark Energy Survey
  • P. Lemos,
  • N. Weaverdyck,
  • R.P. Rollins,
  • J. Muir,
  • A. Ferté
  • +66
  • A.R. Liddle,
  • A. Campos,
  • D. Huterer,
  • M. Raveri,
  • J. Zuntz,
  • E. Di Valentino,
  • X. Fang,
  • W.G. Hartley,
  • M. Aguena,
  • S. Allam,
  • J. Annis,
  • E. Bertin,
  • S. Bocquet,
  • D. Brooks,
  • D.L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • F.J. Castander,
  • A. Choi,
  • M. Costanzi,
  • M. Crocce,
  • L.N. da Costa,
  • M.E.S. Pereira,
  • J.P. Dietrich,
  • S. Everett,
  • I. Ferrero,
  • J. Frieman,
  • J. García-Bellido,
  • M. Gatti,
  • E. Gaztanaga,
  • D.W. Gerdes,
  • D. Gruen,
  • R.A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • S.R. Hinton,
  • D.L. Hollowood,
  • K. Honscheid,
  • D.J. James,
  • K. Kuehn,
  • N. Kuropatkin,
  • M. Lima,
  • M. March,
  • P. Melchior,
  • F. Menanteau,
  • R. Miquel,
  • R. Morgan,
  • A. Palmese,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A.A. Plazas Malagón,
  • A. Porredon,
  • E. Sanchez,
  • V. Scarpine,
  • M. Schubnell,
  • S. Serrano,
  • I. Sevilla-Noarbe,
  • M. Smith,
  • E. Suchyta,
  • M.E.C. Swanson,
  • G. Tarle,
  • D. Thomas,
  • C. To,
  • T.N. Varga,
  • J. Weller
  • (less)
(02/2022) e-Print:2202.08233
abstract + abstract -

Recent cosmological analyses rely on the ability to accurately sample from high-dimensional posterior distributions. A variety of algorithms have been applied in the field, but justification of the particular sampler choice and settings is often lacking. Here we investigate three such samplers to motivate and validate the algorithm and settings used for the Dark Energy Survey (DES) analyses of the first 3 years (Y3) of data from combined measurements of weak lensing and galaxy clustering. We employ the full DES Year 1 likelihood alongside a much faster approximate likelihood, which enables us to assess the outcomes from each sampler choice and demonstrate the robustness of our full results. We find that the ellipsoidal nested sampling algorithm $\texttt{MultiNest}$ reports inconsistent estimates of the Bayesian evidence and somewhat narrower parameter credible intervals than the sliced nested sampling implemented in $\texttt{PolyChord}$. We compare the findings from $\texttt{MultiNest}$ and $\texttt{PolyChord}$ with parameter inference from the Metropolis-Hastings algorithm, finding good agreement. We determine that $\texttt{PolyChord}$ provides a good balance of speed and robustness, and recommend different settings for testing purposes and final chains for analyses with DES Y3 data. Our methodology can readily be reproduced to obtain suitable sampler settings for future surveys.


MIAPbP
(535)Harvesting quantum coherence from axion dark matter
  • Sugumi Kanno,
  • Akira Matsumura,
  • Jiro Soda
Modern Physics Letters A (02/2022) doi:10.1142/S0217732322500286
abstract + abstract -

Quantum coherence is one of the most striking features of quantum mechanics rooted in the superposition principle. Recently, it has been demonstrated that it is possible to harvest the quantum coherence from a coherent scalar field. In order to explore a new method of detecting axion dark matter, we consider a point-like Unruh-DeWitt detector coupled to the axion field and quantify a coherent measure of the detector. We show that the detector can harvest the quantum coherence from the axion dark matter. To be more precise, we consider a two-level electron system in an atom as the detector. In this case, we obtain the coherence measure C = 2.2 × 10−6γ(T/1s) where T and γ are an observation time and the Lorentz factor. At the same time, the axion mass ma we can probe is determined by the energy gap of the detector.


RU-C
(534)In-flight polarization angle calibration for LiteBIRD: blind challenge and cosmological implications
  • N. Krachmalnicoff,
  • T. Matsumura,
  • E. de la Hoz,
  • S. Basak,
  • A. Gruppuso
  • +66
  • Y. Minami,
  • C. Baccigalupi,
  • E. Komatsu,
  • E. Martínez-González,
  • P. Vielva,
  • J. Aumont,
  • R. Aurlien,
  • S. Azzoni,
  • A. J. Banday,
  • R. B. Barreiro,
  • N. Bartolo,
  • M. Bersanelli,
  • E. Calabrese,
  • A. Carones,
  • F. J. Casas,
  • K. Cheung,
  • Y. Chinone,
  • F. Columbro,
  • P. de Bernardis,
  • P. Diego-Palazuelos,
  • J. Errard,
  • F. Finelli,
  • U. Fuskeland,
  • M. Galloway,
  • R. T. Genova-Santos,
  • M. Gerbino,
  • T. Ghigna,
  • S. Giardiello,
  • E. Gjerløw,
  • M. Hazumi,
  • S. Henrot-Versillé,
  • T. Kisner,
  • L. Lamagna,
  • M. Lattanzi,
  • F. Levrier,
  • G. Luzzi,
  • D. Maino,
  • S. Masi,
  • M. Migliaccio,
  • L. Montier,
  • G. Morgante,
  • B. Mot,
  • R. Nagata,
  • F. Nati,
  • P. Natoli,
  • L. Pagano,
  • A. Paiella,
  • D. Paoletti,
  • G. Patanchon,
  • F. Piacentini,
  • G. Polenta,
  • D. Poletti,
  • G. Puglisi,
  • M. Remazeilles,
  • J. Rubino-Martin,
  • M. Sasaki,
  • M. Shiraishi,
  • G. Signorelli,
  • S. Stever,
  • A. Tartari,
  • M. Tristram,
  • M. Tsuji,
  • L. Vacher,
  • I. K. Wehus,
  • M. Zannoni,
  • LiteBIRD Collaboration
  • (less)
Journal of Cosmology and Astroparticle Physics (01/2022) doi:10.1088/1475-7516/2022/01/039
abstract + abstract -

We present a demonstration of the in-flight polarization angle calibration for the JAXA/ISAS second strategic large class mission, LiteBIRD, and estimate its impact on the measurement of the tensor-to-scalar ratio parameter, r, using simulated data. We generate a set of simulated sky maps with CMB and polarized foreground emission, and inject instrumental noise and polarization angle offsets to the 22 (partially overlapping) LiteBIRD frequency channels. Our in-flight angle calibration relies on nulling the EB cross correlation of the polarized signal in each channel. This calibration step has been carried out by two independent groups with a blind analysis, allowing an accuracy of the order of a few arc-minutes to be reached on the estimate of the angle offsets. Both the corrected and uncorrected multi-frequency maps are propagated through the foreground cleaning step, with the goal of computing clean CMB maps. We employ two component separation algorithms, the Bayesian-Separation of Components and Residuals Estimate Tool (B-SeCRET), and the Needlet Internal Linear Combination (NILC). We find that the recovered CMB maps obtained with algorithms that do not make any assumptions about the foreground properties, such as NILC, are only mildly affected by the angle miscalibration. However, polarization angle offsets strongly bias results obtained with the parametric fitting method. Once the miscalibration angles are corrected by EB nulling prior to the component separation, both component separation algorithms result in an unbiased estimation of the r parameter. While this work is motivated by the conceptual design study for LiteBIRD, its framework can be broadly applied to any CMB polarization experiment. In particular, the combination of simulation plus blind analysis provides a robust forecast by taking into account not only detector sensitivity but also systematic effects.


CN-2
RU-E
(533)Dynamic Exchange of Substituents in a Prebiotic Organocatalyst: Initial Steps towards an Evolutionary System
  • A. C. Closs,
  • M. Bechtel,
  • O. Trapp
Angew. Chem. Int. Ed. (01/2022) doi:10.1002/anie.202112563
abstract + abstract -

All evolutionary biological processes lead to a change in heritable traits over successive generations. The responsible genetic information encoded in DNA is altered, selected, and inherited by mutation of the base sequence. While this is well known at the biological level, an evolutionary change at the molecular level of small organic molecules is unknown but represents an important prerequisite for the emergence of life. Here, we present a class of prebiotic imidazolidine-4-thione organocatalysts able to dynamically change their constitution and potentially capable to form an evolutionary system. These catalysts functionalize their building blocks and dynamically adapt to their (self-modified) environment by mutation of their own structure. Depending on the surrounding conditions, they show pronounced and opposing selectivity in their formation. Remarkably, the preferentially formed species can be associated with different catalytic properties, which enable multiple pathways for the transition from abiotic matter to functional biomolecules.


RU-C
(532)Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies
  • S. Mau,
  • E.O. Nadler,
  • R.H. Wechsler,
  • A. Drlica-Wagner,
  • K. Bechtol
  • +64
  • G. Green,
  • D. Huterer,
  • T.S. Li,
  • Y.-Y. Mao,
  • C.E. Martínez-Vázquez,
  • M. McNanna,
  • B. Mutlu-Pakdil,
  • A.B. Pace,
  • A. Peter,
  • A.H. Riley,
  • L. Strigari,
  • M.-Y. Wang,
  • M. Aguena,
  • S. Allam,
  • J. Annis,
  • D. Bacon,
  • E. Bertin,
  • S. Bocquet,
  • D. Brooks,
  • D.L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • M. Costanzi,
  • M. Crocce,
  • M.E.S. Pereira,
  • T.M. Davis,
  • J. De Vicente,
  • S. Desai,
  • P. Doel,
  • I. Ferrero,
  • B. Flaugher,
  • J. Frieman,
  • J. García-Bellido,
  • M. Gatti,
  • G. Giannini,
  • D. Gruen,
  • R.A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • S.R. Hinton,
  • D.L. Hollowood,
  • K. Honscheid,
  • D.J. James,
  • K. Kuehn,
  • O. Lahav,
  • M.A.G. Maia,
  • J.L. Marshall,
  • R. Miquel,
  • J.J. Mohr,
  • R. Morgan,
  • R.L.C. Ogando,
  • F. Paz-Chinchón,
  • A. Pieres,
  • M. Rodriguez-Monroy,
  • E. Sanchez,
  • V. Scarpine,
  • S. Serrano,
  • I. Sevilla-Noarbe,
  • E. Suchyta,
  • G. Tarle,
  • C. To,
  • D.L. Tucker,
  • J. Weller
  • (less)
(01/2022) e-Print:2201.11740
abstract + abstract -

We use a recent census of the Milky Way (MW) satellite galaxy population to constrain the lifetime of particle dark matter (DM). We consider two-body decaying dark matter (DDM) in which a heavy DM particle decays with lifetime $\tau$ comparable to the age of the Universe to a lighter DM particle (with mass splitting $\epsilon$) and to a dark radiation species. These decays impart a characteristic "kick velocity," $V_{\mathrm{kick}}=\epsilon c$, on the DM daughter particles, significantly depleting the DM content of low-mass subhalos and making them more susceptible to tidal disruption. We fit the suppression of the present-day DDM subhalo mass function (SHMF) as a function of $\tau$ and $V_{\mathrm{kick}}$ using a suite of high-resolution zoom-in simulations of MW-mass halos, and we validate this model on new DDM simulations of systems specifically chosen to resemble the MW. We implement our DDM SHMF predictions in a forward model that incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk using an empirical model for the galaxy--halo connection. By comparing to the observed MW satellite population, we conservatively exclude DDM models with $\tau < 18\ \mathrm{Gyr}$ ($29\ \mathrm{Gyr}$) for $V_{\mathrm{kick}}=20\ \mathrm{km}\, \mathrm{s}^{-1}$ ($40\ \mathrm{km}\, \mathrm{s}^{-1}$) at $95\%$ confidence. These constraints are among the most stringent and robust small-scale structure limits on the DM particle lifetime and strongly disfavor DDM models that have been proposed to alleviate the Hubble and $S_8$ tensions.


CN-3
RU-B
(531)Probing spin-dependent dark matter interactions with $^6$Li: CRESST Collaboration
  • G. Angloher,
  • G. Benato,
  • A. Bento,
  • E. Bertoldo,
  • A. Bertolini
  • +53
  • R. Breier,
  • C. Bucci,
  • L. Canonica,
  • A. D'Addabbo,
  • S. Di Lorenzo,
  • L. Einfalt,
  • A. Erb,
  • F. v. Feilitzsch,
  • N. Ferreiro Iachellini,
  • S. Fichtinger,
  • D. Fuchs,
  • A. Fuss,
  • A. Garai,
  • V.M. Ghete,
  • P. Gorla,
  • S. Gupta,
  • D. Hauff,
  • M. Ješkovský,
  • J. Jochum,
  • M. Kaznacheeva,
  • A. Kinast,
  • H. Kluck,
  • H. Kraus,
  • A. Langenkämper,
  • M. Mancuso,
  • L. Marini,
  • V. Mokina,
  • A. Nilima,
  • M. Olmi,
  • T. Ortmann,
  • C. Pagliarone,
  • V. Palušová,
  • L. Pattavina,
  • F. Petricca,
  • W. Potzel,
  • P. Povinec,
  • F. Pröbst,
  • F. Pucci,
  • F. Reindl,
  • J. Rothe,
  • K. Schäffner,
  • J. Schieck,
  • D. Schmiedmayer,
  • S. Schönert,
  • C. Schwertner,
  • M. Stahlberg,
  • L. Stodolsky,
  • C. Strandhagen,
  • R. Strauss,
  • I. Usherov,
  • F. Wagner,
  • M. Willers,
  • V. Zema
  • (less)
abstract + abstract -

CRESST is one of the most prominent direct detection experiments for dark matter particles with sub-GeV/c$^2$ mass. One of the advantages of the CRESST experiment is the possibility to include a large variety of nuclides in the target material used to probe dark matter interactions. In this work, we discuss in particular the interactions of dark matter particles with protons and neutrons of $^{6}$Li. This is now possible thanks to new calculations on nuclear matrix elements of this specific isotope of Li. To show the potential of using this particular nuclide for probing dark matter interactions, we used the data collected previously by a CRESST prototype based on LiAlO$_2$ and operated in an above ground test-facility at Max-Planck-Institut für Physik in Munich, Germany. In particular, the inclusion of $^{6}$Li in the limit calculation drastically improves the result obtained for spin-dependent interactions with neutrons in the whole mass range. The improvement is significant, greater than two order of magnitude for dark matter masses below 1 GeV/c$^2$, compared to the limit previously published with the same data.


(530)The dark energy survey 5-yr photometrically identified type Ia supernovae
  • A. Möller,
  • M. Smith,
  • M. Sako,
  • M. Sullivan,
  • M. Vincenzi
  • +78
  • P. Wiseman,
  • P. Armstrong,
  • J. Asorey,
  • D. Brout,
  • D. Carollo,
  • T.M. Davis,
  • C. Frohmaier,
  • L. Galbany,
  • K. Glazebrook,
  • L. Kelsey,
  • R. Kessler,
  • G.F. Lewis,
  • C. Lidman,
  • U. Malik,
  • R.C. Nichol,
  • D. Scolnic,
  • B.E. Tucker,
  • T.M.C. Abbott,
  • M. Aguena,
  • S. Allam,
  • J. Annis,
  • E. Bertin,
  • S. Bocquet,
  • D. Brooks,
  • D.L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • F.J. Castander,
  • C. Conselice,
  • M. Costanzi,
  • M. Crocce,
  • L.N. da Costa,
  • J. De Vicente,
  • S. Desai,
  • H.T. Diehl,
  • P. Doel,
  • S. Everett,
  • I. Ferrero,
  • D.A. Finley,
  • B. Flaugher,
  • D. Friedel,
  • J. Frieman,
  • J. García-Bellido,
  • D.W. Gerdes,
  • D. Gruen,
  • R.A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • K. Herner,
  • S.R. Hinton,
  • D.L. Hollowood,
  • K. Honscheid,
  • D.J. James,
  • K. Kuehn,
  • N. Kuropatkin,
  • O. Lahav,
  • M. March,
  • J.L. Marshall,
  • F. Menanteau,
  • R. Miquel,
  • R. Morgan,
  • A. Palmese,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A.A. Plazas Malagón,
  • A.K. Romer,
  • A. Roodman,
  • E. Sanchez,
  • V. Scarpine,
  • M. Schubnell,
  • S. Serrano,
  • I. Sevilla-Noarbe,
  • E. Suchyta,
  • G. Tarle,
  • D. Thomas,
  • C. To,
  • T.N. Varga
  • (less)
Mon.Not.Roy.Astron.Soc. (01/2022) e-Print:2201.11142 doi:10.1093/mnras/stac1691
abstract + abstract -

As part of the cosmology analysis using Type Ia Supernovae (SN Ia) in the Dark Energy Survey (DES), we present photometrically identified SN Ia samples using multiband light curves and host galaxy redshifts. For this analysis, we use the photometric classification framework SuperNNovatrained on realistic DES-like simulations. For reliable classification, we process the DES SN programme (DES-SN) data and introduce improvements to the classifier architecture, obtaining classification accuracies of more than 98 per cent on simulations. This is the first SN classification to make use of ensemble methods, resulting in more robust samples. Using photometry, host galaxy redshifts, and a classification probability requirement, we identify 1863 SNe Ia from which we select 1484 cosmology-grade SNe Ia spanning the redshift range of 0.07 < z < 1.14. We find good agreement between the light-curve properties of the photometrically selected sample and simulations. Additionally, we create similar SN Ia samples using two types of Bayesian Neural Network classifiers that provide uncertainties on the classification probabilities. We test the feasibility of using these uncertainties as indicators for out-of-distribution candidates and model confidence. Finally, we discuss the implications of photometric samples and classification methods for future surveys such as Vera C. Rubin Observatory Legacy Survey of Space and Time.


RU-C
RU-D
(529)Response approach to the integrated shear 3-point correlation function: the impact of baryonic effects on small scales
  • Anik Halder,
  • Alexandre Barreira
Mon.Not.Roy.Astron.Soc. (01/2022) e-Print:2201.05607 doi:10.1093/mnras/stac2046
abstract + abstract -

The integrated shear 3-point correlation function ζ_± is a higher-order statistic of the cosmic shear field that describes the modulation of the 2-point correlation function ξ_± by long-wavelength features in the field. Here, we introduce a new theoretical model to calculate ζ_± that is accurate on small angular scales, and that allows to take baryonic feedback effects into account. Our model builds on the realization that the small-scale ζ_± is dominated by the non-linear matter bispectrum in the squeezed limit, which can be evaluated accurately using the non-linear matter power spectrum and its first-order response functions to density and tidal field perturbations. We demonstrate the accuracy of our model by showing that it reproduces the small-scale ζ_± measured in simulated cosmic shear maps. The impact of baryonic feedback enters effectively only through the corresponding impact on the non-linear matter power spectrum, thereby permitting to account for these astrophysical effects on ζ_± similarly to how they are currently accounted for on ξ_±. Using a simple idealized Fisher matrix forecast for a DES-like survey we find that, compared to ξ_±, a combined |$\xi _{\pm }\ \&\ \zeta _{\pm }$| analysis can lead to improvements of order |$20\!-\!40{{\ \rm per\ cent}}$| on the constraints of cosmological parameters such as σ_8 or the dark energy equation of state parameter w_0. We find similar levels of improvement on the constraints of the baryonic feedback parameters, which strengthens the prospects for cosmic shear data to obtain tight constraints not only on cosmology but also on astrophysical feedback models. These encouraging results motivate future works on the integrated shear 3-point correlation function towards applications to real survey data.


MIAPbP
(528)Redshift-space effects in voids and their impact on cosmological tests - II. The void-galaxy cross-correlation function
  • Carlos M. Correa,
  • Dante J. Paz,
  • Nelson D. Padilla,
  • Ariel G. Sánchez,
  • Andrés N. Ruiz
  • +1
Monthly Notices of the Royal Astronomical Society (01/2022) doi:10.1093/mnras/stab3070
abstract + abstract -

This is the second part of a thorough investigation of the redshift-space effects that affect void properties and the impact they have on cosmological tests. Here, we focus on the void-galaxy cross-correlation function, specifically, on the projected versions that we developed in a previous work. The pillar of the analysis is the one-to-one relationship between real and redshift-space voids above the shot-noise level identified with a spherical void finder. Under this mapping, void properties are affected by three effects: (i) a systematic expansion as a consequence of the distortions induced by galaxy dynamics, (ii) the Alcock-Paczynski volume effect, which manifests as an overall expansion or contraction depending on the fiducial cosmology, and (iii) a systematic off-centring along the line of sight as a consequence of the distortions induced by void dynamics. We found that correlations are also affected by an additional source of distortions: the ellipticity of voids. This is the first time that distortions due to the off-centring and ellipticity effects are detected and quantified. With a simplified test, we verified that the Gaussian streaming model is still robust provided all these effects are taken into account, laying the foundations for improvements in current models in order to obtain unbiased cosmological constraints from spectroscopic surveys. Besides this practical importance, this analysis also encodes key information about the structure and dynamics of the Universe at the largest scales. Furthermore, some of the effects constitute cosmological probes by themselves, as is the case of the void ellipticity.


CN-2
MIAPbP
RU-D
(527)Dust entrainment in photoevaporative winds: Densities and imaging
  • R. Franz,
  • B. Ercolano,
  • S. Casassus,
  • G. Picogna,
  • T. Birnstiel
  • +3
Astronomy and Astrophysics (01/2022) doi:10.1051/0004-6361/202140812
abstract + abstract -

Context. X-ray- and extreme-ultraviolet- (together: XEUV-) driven photoevaporative winds acting on protoplanetary disks around young T-Tauri stars may crucially impact disk evolution, affecting both gas and dust distributions.
Aims: We constrain the dust densities in a typical XEUV-driven outflow, and determine whether these winds can be observed at μm-wavelengths.
Methods: We used dust trajectories modelled atop a 2D hydrodynamical gas model of a protoplanetary disk irradiated by a central T-Tauri star. With these and two different prescriptions for the dust distribution in the underlying disk, we constructed wind density maps for individual grain sizes. We used the dust density distributions obtained to synthesise observations in scattered and polarised light.
Results: For an XEUV-driven outflow around a M* = 0.7 M T-Tauri star with LX = 2 × 1030 erg s−1, we find a dust mass-loss rate Ṁdust ≲ 4.1 × 10−11 M yr−1 for an optimistic estimate of dust densities in the wind (compared to Ṁgas ≈ 3.7 × 10−8 M yr−1). The synthesised scattered-light images suggest a distinct chimney structure emerging at intensities I∕Imax < 10−4.5 (10−3.5) at λobs = 1.6 (0.4) μm, while the features in the polarised-light images are even fainter. Observations synthesised from our model do not exhibit clear features for SPHERE IRDIS, but show a faint wind signature for JWST NIRCam under optimal conditions.
Conclusions: Unambiguous detections of photoevaporative XEUV winds launched from primordial disks are at least challenging with current instrumentation; this provides a possible explanation as to why disk winds are not routinely detected in scattered or polarised light. Our calculations show that disk scale heights retrieved from scattered-light observations should be only marginally affected by the presence of an XEUV wind.


(526)Precision tests of fundamental physics with η and η<SUP>′</SUP> mesons
  • Liping Gan,
  • Bastian Kubis,
  • Emilie Passemar,
  • Sean Tulin
Physics Reports (01/2022) doi:10.1016/j.physrep.2021.11.001
abstract + abstract -

Decays of the neutral and long-lived η and η mesons provide a unique, flavor-conserving laboratory to test low-energy Quantum Chromodynamics and search for new physics beyond the Standard Model. They have drawn world-wide attention in recent years and have inspired broad experimental programs in different high-intensity-frontier centers. New experimental data will offer critical inputs to precisely determine the light quark mass ratios, η-η mixing parameters, and hadronic contributions to the anomalous magnetic moment of the muon. At the same time, it will provide a sensitive probe to test potential new physics. This includes searches for hidden photons, light Higgs scalars, and axion-like particles that are complementary to worldwide efforts to detect new light particles below the GeV mass scale, as well as tests of discrete symmetry violation. In this review, we give an update on theoretical developments, discuss the experimental opportunities, and identify future research needed in this field.


CN-5
RU-D
(525)Driving Galactic Outflows with Magnetic Fields at Low and High Redshift
  • Ulrich P. Steinwandel,
  • Klaus Dolag,
  • Harald Lesch,
  • Andreas Burkert
The Astrophysical Journal (01/2022) doi:10.3847/1538-4357/ac2ffd
abstract + abstract -

Although galactic outflows play a key role in our understanding of the evolution of galaxies, the exact mechanism by which galactic outflows are driven is still far from being understood and, therefore, our understanding of associated feedback mechanisms that control the evolution of galaxies is still plagued by many enigmas. In this work, we present a simple toy model that can provide insight on how non-axisymmetric instabilities in galaxies (bars, spiral arms, warps) can lead to local exponential magnetic field growth by radial flows beyond the equipartition value by at least two orders of magnitude on a timescale of a few 100 Myr. Our predictions show that the process can lead to galactic outflows in barred spiral galaxies with a mass-loading factor η ≍ 0.1, in agreement with our numerical simulations. Moreover, our outflow mechanism could contribute to an understanding of the large fraction of barred spiral galaxies that show signs of galactic outflows in the CHANG-ES survey. Extending our model shows the importance of such processes in high-redshift galaxies by assuming equipartition between magnetic energy and turbulent energy. Simple estimates for the star formation rate in our model together with cross correlated masses from the star-forming main sequence at redshifts z ~ 2 allow us to estimate the outflow rate and mass-loading factors by non-axisymmetric instabilities and a subsequent radial inflow dynamo, giving mass-loading factors of η ≍ 0.1 for galaxies in the range of M = 109-1012 M , in good agreement with recent results of SINFONI and KMOS 3D.


CN-2
(524)Silicon in the dayside atmospheres of two ultra-hot Jupiters
  • D. Cont,
  • F. Yan,
  • A. Reiners,
  • L. Nortmann,
  • K. Molaverdikhani
  • +20
  • E. Pallé,
  • M. Stangret,
  • Th. Henning,
  • I. Ribas,
  • A. Quirrenbach,
  • J. A. Caballero,
  • M. R. Zapatero Osorio,
  • P. J. Amado,
  • J. Aceituno,
  • N. Casasayas-Barris,
  • S. Czesla,
  • A. Kaminski,
  • M. López-Puertas,
  • D. Montes,
  • J. C. Morales,
  • G. Morello,
  • E. Nagel,
  • A. Sánchez-López,
  • E. Sedaghati,
  • M. Zechmeister
  • (less)
Astronomy and Astrophysics (01/2022) doi:10.1051/0004-6361/202142776
abstract + abstract -

Atmospheres of highly irradiated gas giant planets host a large variety of atomic and ionic species. Here we observe the thermal emission spectra of the two ultra-hot Jupiters WASP-33b and KELT-20b/MASCARA-2b in the near-infrared wavelength range with CARMENES. Via high-resolution Doppler spectroscopy, we searched for neutral silicon (Si) in their dayside atmospheres. We detect the Si spectral signature of both planets via cross-correlation with model spectra. Detection levels of 4.8σ and 5.4σ, respectively, are observed when assuming a solar atmospheric composition. This is the first detection of Si in exoplanet atmospheres. The presence of Si is an important finding due to its fundamental role in cloud formation and, hence, for the planetary energy balance. Since the spectral lines are detected in emission, our results also confirm the presence of an inverted temperature profile in the dayside atmospheres of both planets.


CN-2
(523)Final Report for SAG 21: The Effect of Stellar Contamination on Space-based Transmission Spectroscopy
  • Benjamin V. Rackham,
  • Néstor Espinoza,
  • Svetlana V. Berdyugina,
  • Heidi Korhonen,
  • Ryan J. MacDonald
  • +56
  • Benjamin T. Montet,
  • Brett M. Morris,
  • Mahmoudreza Oshagh,
  • Alexander I. Shapiro,
  • Yvonne C. Unruh,
  • Elisa V. Quintana,
  • Robert T. Zellem,
  • Dániel Apai,
  • Thomas Barclay,
  • Joanna K. Barstow,
  • Giovanni Bruno,
  • Ludmila Carone,
  • Sarah L. Casewell,
  • Heather M. Cegla,
  • Serena Criscuoli,
  • Catherine Fischer,
  • Damien Fournier,
  • Mark S. Giampapa,
  • Helen Giles,
  • Aishwarya Iyer,
  • Greg Kopp,
  • Nadiia M. Kostogryz,
  • Natalie Krivova,
  • Matthias Mallonn,
  • Chima McGruder,
  • Karan Molaverdikhani,
  • Elisabeth R. Newton,
  • Mayukh Panja,
  • Sarah Peacock,
  • Kevin Reardon,
  • Rachael M. Roettenbacher,
  • Gaetano Scandariato,
  • Sami Solanki,
  • Keivan G. Stassun,
  • Oskar Steiner,
  • Kevin B. Stevenson,
  • Jeremy Tregloan-Reed,
  • Adriana Valio,
  • Sven Wedemeyer,
  • Luis Welbanks,
  • Jie Yu,
  • Munazza K. Alam,
  • James R. A. Davenport,
  • Drake Deming,
  • Chuanfei Dong,
  • Elsa Ducrot,
  • Chloe Fisher,
  • Emily Gilbert,
  • Veselin Kostov,
  • Mercedes López-Morales,
  • Mike Line,
  • Teo Močnik,
  • Susan Mullally,
  • Rishi R. Paudel,
  • Ignasi Ribas,
  • Jeff A. Valenti
  • (less)
arXiv e-prints (01/2022) e-Print:2201.09905
abstract + abstract -

Study Analysis Group 21 (SAG21) of the Exoplanet Exploration Program Analysis Group (ExoPAG) was organized to study the effect of stellar contamination on space-based transmission spectroscopy, a method for studying exoplanetary atmospheres by measuring the wavelength-dependent radius of a planet as it transits its star. Transmission spectroscopy relies on a precise understanding of the spectrum of the star being occulted. However, stars are not homogeneous, constant light sources but have temporally evolving photospheres and chromospheres with inhomogeneities like spots, faculae, and plages. This SAG has brought together an interdisciplinary team of more than 100 scientists, with observers and theorists from the heliophysics, stellar astrophysics, planetary science, and exoplanetary atmosphere research communities, to study the current needs that can be addressed in this context to make the most of transit studies from current NASA facilities like HST and JWST. The analysis produced 14 findings, which fall into three Science Themes encompassing (1) how the Sun is used as our best laboratory to calibrate our understanding of stellar heterogeneities ("The Sun as the Stellar Benchmark"), (2) how stars other than the Sun extend our knowledge of heterogeneities ("Surface Heterogeneities of Other Stars") and (3) how to incorporate information gathered for the Sun and other stars into transit studies ("Mapping Stellar Knowledge to Transit Studies").


CN-7
RU-A
(522)Neutrino absorption and other physics dependencies in neutrino-cooled black hole accretion discs
  • O. Just,
  • S. Goriely,
  • H. -Th Janka,
  • S. Nagataki,
  • A. Bauswein
Monthly Notices of the Royal Astronomical Society (01/2022) doi:10.1093/mnras/stab2861
abstract + abstract -

Black hole (BH) accretion discs formed in compact-object mergers or collapsars may be major sites of the rapid-neutron-capture (r-)process, but the conditions determining the electron fraction (Ye) remain uncertain given the complexity of neutrino transfer and angular-momentum transport. After discussing relevant weak-interaction regimes, we study the role of neutrino absorption for shaping Ye using an extensive set of simulations performed with two-moment neutrino transport and again without neutrino absorption. We vary the torus mass, BH mass and spin, and examine the impact of rest-mass and weak-magnetism corrections in the neutrino rates. We also test the dependence on the angular-momentum transport treatment by comparing axisymmetric models using the standard α-viscosity with viscous models assuming constant viscous length-scales (lt) and 3D magnetohydrodynamic (MHD) simulations. Finally, we discuss the nucleosynthesis yields and basic kilonova properties. We find that absorption pushes Ye towards ~0.5 outside the torus, while inside increasing the equilibrium value $Y_\mathrm{ e}^{\mathrm{eq}}$ by ~0.05-0.2. Correspondingly, a substantial ejecta fraction is pushed above Ye = 0.25, leading to a reduced lanthanide fraction and a brighter, earlier, and bluer kilonova than without absorption. More compact tori with higher neutrino optical depth, τ, tend to have lower $Y_\mathrm{ e}^{\mathrm{eq}}$ up to τ ~ 1-10, above which absorption becomes strong enough to reverse this trend. Disc ejecta are less (more) neutron rich when employing an lt = const. viscosity (MHD treatment). The solar-like abundance pattern found for our MHD model marginally supports collapsar discs as major r-process sites, although a strong r-process may be limited to phases of high mass-infall rates, $\dot{M}\, \, \raise0.14em\rm{\gt }\lower0.28em\rm{\sim }\, \, 2\times 10^{-2}$ M s-1.


RU-D
(521)Mass determination of protoplanetary disks from dust evolution
  • Riccardo Franceschi,
  • Tilman Birnstiel,
  • Thomas Henning,
  • Paola Pinilla,
  • Dmitry Semenov
  • +1
Astronomy and Astrophysics (01/2022) doi:10.1051/0004-6361/202141705
abstract + abstract -

Context. The mass of protoplanetary disks is arguably one of their most important quantities shaping their evolution toward planetary systems, but it remains a challenge to determine this quantity. Using the high spatial resolution now available on telescopes such as the Atacama Large Millimeter/submillimeter Array (ALMA), recent studies derived a relation between the disk surface density and the location of the "dust lines". This is a new concept in the field, linking the disk size at different continuum wavelengths with the radial distribution of grain populations of different sizes.
Aims: We aim to use a dust evolution model to test the dependence of the dust line location on disk gas mass. In particular, we are interested in the reliability of the method for disks showing radial substructures, as recent high-resolution observations revealed.
Methods: We performed dust evolution calculations, which included perturbations to the gas surface density with different amplitudes at different radii, to investigate their effect on the global drift timescale of dust grains. These models were then used to calibrate the relation between the dust grain drift timescale and the disk gas mass. We investigated under which condition the dust line location is a good mass estimator and tested how different stellar and disk properties (disk mass, stellar mass, disk age, and dust-to-gas ratio) affect the dust line properties. Finally, we show the applicability of this method to disks such as TW Hya and AS 209 that have been observed at high angular resolution with ALMA and show pronounced disk structures.
Results: Our models without pressure bumps confirm a strong dependence of the dust line location on the disk gas mass and its applicability as a reliable mass estimator. The other disk properties do not significantly affect the dust line location, except for the age of the system, which is the major source of uncertainty for this mass estimator. A population of synthetic disks was used to calibrate an analytic relation between the dust line location and the disk mass for smooth disks, finding that previous mass estimates based on dust lines overestimate disk masses by about one order of magnitude. Radial pressure bumps can alter the location of the dust line by up to ~10 au, while its location is mainly determined by the disk mass. Therefore, an accurate mass estimation requires a proper evaluation of the effect of bumps. However, when radial substructures act as traps for dust grains, the relation between the dust line location and disk mass becomes weaker, and other mass estimators need to be adopted.
Conclusions: Our models show that the determination of the dust line location is a promising approach to the mass estimate of protoplanetay disks, but the exact relation between the dust line location and disk mass depends on the structure of the particular disk. We calibrated the relation for disks without evidence of radial structures, while for more complex structures we ran a simple dust evolution model. However, this method fails when there is evidence of strong dust traps. It is possible to reveal when dust evolution is dominated by traps, providing the necessary information for when the method should be applied with caution.


(520)QCD static force in gradient flow
  • Nora Brambilla,
  • Hee Sok Chung,
  • Antonio Vairo,
  • Xiang-Peng Wang
Journal of High Energy Physics (01/2022) doi:10.1007/JHEP01(2022)184
abstract + abstract -

We compute the QCD static force and potential using gradient flow at next-to-leading order in the strong coupling. The static force is the spatial derivative of the static potential: it encodes the QCD interaction at both short and long distances. While on the one side the static force has the advantage of being free of the O(ΛQCD) renormalon affecting the static potential when computed in perturbation theory, on the other side its direct lattice QCD computation suffers from poor convergence. The convergence can be improved by using gradient flow, where the gauge fields in the operator definition of a given quantity are replaced by flowed fields at flow time t, which effectively smear the gauge fields over a distance of order √{t }, while they reduce to the QCD fields in the limit t → 0. Based on our next-to-leading order calculation, we explore the properties of the static force for arbitrary values of t, as well as in the t → 0 limit, which may be useful for lattice QCD studies.


(519)Proca theory from the spinning worldline
  • Matthias Carosi,
  • Ivo Sachs
Journal of High Energy Physics (01/2022) doi:10.1007/JHEP01(2022)135
abstract + abstract -

We obtain Proca field theory from the quantisation of the N = 2 supersymmetric worldline upon supplementing the graded BRST-algebra with an extra multiplet of oscillators. The linearised theory describes the BV-extended spectrum of Proca theory, together with a Stückelberg field. When coupling the theory to background fields we derive the Proca equations, arising as consistency conditions in the BRST procedure. We also explore non-abelian modifications, complexified vector fields as well as coupling to a dilaton field. We propose a cubic action on the space of BRST-operators which reproduces the known Proca action.


RU-A
(518)Publishing statistical models: Getting the most out of particle physics experiments
  • Kyle Cranmer,
  • Sabine Kraml,
  • Harrison Prosper,
  • Philip Bechtle,
  • Florian Bernlochner
  • +28
  • Itay M. Bloch,
  • Enzo Canonero,
  • Marcin Chrzaszcz,
  • Andrea Coccaro,
  • Jan Conrad,
  • Glen Cowan,
  • Matthew Feickert,
  • Nahuel Ferreiro,
  • Andrew Fowlie,
  • Lukas A. Heinrich,
  • Alexander Held,
  • Thomas Kuhr,
  • Anders Kvellestad,
  • Maeve Madigan,
  • Farvah Nazila Mahmoudi,
  • Knut Dundas Morå,
  • Mark S. Neubauer,
  • Maurizio Pierini,
  • Juan Rojo,
  • Sezen Sekmen,
  • Luca Silvestrini,
  • Veronica Sanz,
  • Giordon H. Stark,
  • Riccardo Torre,
  • Robert Thorne,
  • Wolfgang Waltenberger,
  • Nicholas Wardle,
  • Jonas Wittbrodt
  • (less)
SciPost Physics (01/2022) doi:10.21468/SciPostPhys.12.1.037
abstract + abstract -

The statistical models used to derive the results of experimental analyses are of incredible scientific value and are essential information for analysis preservation and reuse. In this paper, we make the scientific case for systematically publishing the full statistical models and discuss the technical developments that make this practical. By means of a variety of physics cases -- including parton distribution functions, Higgs boson measurements, effective field theory interpretations, direct searches for new physics, heavy flavor physics, direct dark matter detection, world averages, and beyond the Standard Model global fits -- we illustrate how detailed information on the statistical modelling can enhance the short- and long-term impact of experimental results.


CN-4
RU-C
(517)Production of Very Light Elements and Strontium in the Early Ejecta of Neutron Star Mergers
  • Albino Perego,
  • Diego Vescovi,
  • Achille Fiore,
  • Leonardo Chiesa,
  • Christian Vogl
  • +8
  • Stefano Benetti,
  • Sebastiano Bernuzzi,
  • Marica Branchesi,
  • Enrico Cappellaro,
  • Sergio Cristallo,
  • Andreas Flörs,
  • Wolfgang E. Kerzendorf,
  • David Radice
  • (less)
The Astrophysical Journal (01/2022) doi:10.3847/1538-4357/ac3751
abstract + abstract -

We study the production of very light elements (Z < 20) in the dynamical and spiral-wave wind ejecta of binary neutron star mergers by combining detailed nucleosynthesis calculations with the outcome of numerical relativity merger simulations. All our models are targeted to GW170817 and include neutrino radiation. We explore different finite-temperature, composition-dependent nuclear equations of state, and binary mass ratios, and find that hydrogen and helium are the most abundant light elements. For both elements, the decay of free neutrons is the driving nuclear reaction. In particular, ~0.5-2 × 10-6 M of hydrogen are produced in the fast expanding tail of the dynamical ejecta, while ~1.5-11 × 10-6 M of helium are synthesized in the bulk of the dynamical ejecta, usually in association with heavy r-process elements. By computing synthetic spectra, we find that the possibility of detecting hydrogen and helium features in kilonova spectra is very unlikely for fiducial masses and luminosities, even when including nonlocal thermodynamic equilibrium effects. The latter could be crucial to observe helium lines a few days after merger for faint kilonovae or for luminous kilonovae ejecting large masses of helium. Finally, we compute the amount of strontium synthesized in the dynamical and spiral-wave wind ejecta, and find that it is consistent with (or even larger than, in the case of a long-lived remnant) the one required to explain early spectral features in the kilonova of GW170817.


(516)Variable structures in M87* from space, time and frequency resolved interferometry
  • Philipp Arras,
  • Philipp Frank,
  • Philipp Haim,
  • Jakob Knollmüller,
  • Reimar Leike
  • +2
  • Martin Reinecke,
  • Torsten Enßlin
  • (less)
Nature Astronomy (01/2022) doi:10.1038/s41550-021-01548-0
abstract + abstract -

The immediate vicinity of an active supermassive black hole—with its event horizon, photon ring, accretion disk and relativistic jets—is an appropriate place to study physics under extreme conditions, particularly general relativity and magnetohydrodynamics. Observing the dynamics of such compact astrophysical objects provides insights into their inner workings, and the recent observations of M87* by the Event Horizon Telescope1-6 using very-long-baseline interferometry techniques allows us to investigate the dynamical processes of M87* on timescales of days. Compared with most radio interferometers, very-long-baseline interferometry networks typically have fewer antennas and low signal-to-noise ratios. Furthermore, the source is variable, prohibiting integration over time to improve signal-to-noise ratio. Here, we present an imaging algorithm7,8 that copes with the data scarcity and temporal evolution, while providing an uncertainty quantification. Our algorithm views the imaging task as a Bayesian inference problem of a time-varying brightness, exploits the correlation structure in time and reconstructs (2 + 1 + 1)-dimensional time-variable and spectrally resolved images. We apply this method to the Event Horizon Telescope observations of M87*9 and validate our approach on synthetic data. The time- and frequency-resolved reconstruction of M87* confirms variable structures on the emission ring and indicates extended and time-variable emission structures outside the ring itself.


RU-D
(515)Star formation near the Sun is driven by expansion of the Local Bubble
  • Catherine Zucker,
  • Alyssa A. Goodman,
  • João Alves,
  • Shmuel Bialy,
  • Michael Foley
  • +6
  • Joshua S. Speagle,
  • Josefa Groβschedl,
  • Douglas P. Finkbeiner,
  • Andreas Burkert,
  • Diana Khimey,
  • Cameren Swiggum
  • (less)
abstract + abstract -

For decades we have known that the Sun lies within the Local Bubble, a cavity of low-density, high-temperature plasma surrounded by a shell of cold, neutral gas and dust1-3. However, the precise shape and extent of this shell4,5, the impetus and timescale for its formation6,7, and its relationship to nearby star formation8 have remained uncertain, largely due to low-resolution models of the local interstellar medium. Here we report an analysis of the three-dimensional positions, shapes and motions of dense gas and young stars within 200 pc of the Sun, using new spatial9-11 and dynamical constraints12. We find that nearly all of the star-forming complexes in the solar vicinity lie on the surface of the Local Bubble and that their young stars show outward expansion mainly perpendicular to the bubble's surface. Tracebacks of these young stars' motions support a picture in which the origin of the Local Bubble was a burst of stellar birth and then death (supernovae) taking place near the bubble's centre beginning approximately 14 Myr ago. The expansion of the Local Bubble created by the supernovae swept up the ambient interstellar medium into an extended shell that has now fragmented and collapsed into the most prominent nearby molecular clouds, in turn providing robust observational support for the theory of supernova-driven star formation.


CN-4
RU-C
(514)Intrinsic alignments of galaxies around cosmic voids
  • William d'Assignies D.,
  • Nora Elisa Chisari,
  • Nico Hamaus,
  • Sukhdeep Singh
Monthly Notices of the Royal Astronomical Society (01/2022) doi:10.1093/mnras/stab2986
abstract + abstract -

The intrinsic alignments of galaxies, i.e. the correlation between galaxy shapes and their environment, are a major source of contamination for weak gravitational lensing surveys. Most studies of intrinsic alignments have so far focused on measuring and modelling the correlations of luminous red galaxies with galaxy positions or the filaments of the cosmic web. In this work, we investigate alignments around cosmic voids. We measure the intrinsic alignments of luminous red galaxies detected by the Sloan Digital Sky Survey around a sample of voids constructed from those same tracers and with radii in the ranges: [20-30; 30-40; 40-50] h-1 Mpc and in the redshift range z = 0.4-0.8. We present fits to the measurements based on a linear model at large scales, and on a new model based on the void density profile inside the void and in its neighbourhood. We constrain the free scaling amplitude of our model at small scales, finding no significant alignment at 1σ for either sample. We observe a deviation from the null hypothesis, at large scales, of 2σ for voids with radii between 20 and 30 h-1 Mpc, and 1.5σ for voids with radii between 30 and 40 h-1 Mpc and constrain the amplitude of the model on these scales. We find no significant deviation at 1σ for larger voids. Our work is a first attempt at detecting intrinsic alignments of galaxy shapes around voids and provides a useful framework for their mitigation in future void lensing studies.


CN-2
RU-D
(513)Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region
  • J. Szulágyi,
  • F. Binkert,
  • C. Surville
The Astrophysical Journal (01/2022) doi:10.3847/1538-4357/ac32d1
abstract + abstract -

We carried out 3D dust + gas radiative hydrodynamic simulations of forming planets. We investigated a parameter grid of a Neptune-mass, a Saturn-mass, a Jupiter-mass, and a five-Jupiter-mass planet at 5.2, 30, and 50 au distance from their star. We found that the meridional circulation (Szulágyi et al. 2014; Fung & Chiang 2016) drives a strong vertical flow for the dust as well, hence the dust is not settled in the midplane, even for millimeter-sized grains. The meridional circulation will deliver dust and gas vertically onto the circumplanetary region, efficiently bridging over the gap. The Hill-sphere accretion rates for the dust are ~10-8-10-10 M Jup yr-1, increasing with planet mass. For the gas component, the gain is 10-6-10-8 M Jup yr-1. The difference between the dust and gas-accretion rates is smaller with decreasing planetary mass. In the vicinity of the planet, the millimeter-sized grains can get trapped easier than the gas, which means the circumplanetary disk might be enriched with solids in comparison to the circumstellar disk. We calculated the local dust-to-gas ratio (DTG) everywhere in the circumstellar disk and identified the altitude above the midplane where the DTG is 1, 0.1, 0.01, and 0.001. The larger the planetary mass, the more the millimeter-sized dust is delivered and a larger fraction of the dust disk is lifted by the planet. The stirring of millimeter-sized dust is negligible for Neptune-mass planets or below, but significant above Saturn-mass planets.


CN-2
RU-E
(512)Thermally induced habitat for the emergence of life - enrichment of phosphorus, divalent salts and compact oligomer folds.
  • Christof Mast,
  • Dieter Braun,
  • Thomas Matruex,
  • Paula Aikkila,
  • Bettina Scheu
  • +3
  • Don Dingwell,
  • Kris Le Vay,
  • Hannes Mutschler
  • (less)
APS March Meeting Abstracts (2022)
abstract + abstract -

The early Earth 4 billion years ago was a scarce place for the emergence of life. After the formation of the oceans, it was most likely difficult to extract the essential ionic building blocks of life, such as phosphate or salts, from the existing geomaterial in sufficiently high concentrations and suitable mixing ratios. We show how ubiquitous heat fluxes through rock fractures implement a physical solution to this problem: Thermal convection and thermophoresis together are able to separate calcium from phosphorus and thus use ubiquitous but otherwise inert apatite as a phosphate source. Furthermore, the mixing ratio of different salts is modified according to their thermophoretic properties, providing a suitable non-equilibrium environment for the first prebiotic reactions.

Funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) - Project-ID 364653263 - TRR 235 (CRC235). Funding by the Volkswagen Initiative 'Life? - A Fresh Scientific Approach to the Basic Principles of Life', from the Simons Foundation and from Germany's Excellence Strategy EXC-2094-390783311 is gratefully acknowledged. We are grateful for funding by the European Research Council (ERC starting Grant, RiboLife) under 802000 and the MaxSynBio consortium, which is jointly funded by the Federal Ministry of Education and Research of Germany and the Max Planck Society. We wish to acknowledge the support of ERC ADV 2018 Grant 834225 (EAVESDROP). We thank for financial support from ERC-2017-ADG from the European Research Council. The work is supported by the Center for Nanoscience Munich (CeNS).


MIAPbP
RU-A
(511)Searching for New Physics in Rare (K) and (B) Decays without (|V_{cb}|) and (|V_{ub}|) Uncertainties
  • A. J. Buras,
  • E. Venturini
Acta Physica Polonica B (2022) doi:10.5506/APhysPolB.53.6-A1
abstract + abstract -

We reemphasize the strong dependence of the branching ratios $B(K^+\to\pi^+\nu\bar\nu)$ and $B(K_L\to\pi^0\nu\bar\nu)$ on $|V_{cb}|$ that is stronger than in rare $B$ decays, in particular for $K_L\to\pi^0\nu\bar\nu$. Thereby the persistent tension between inclusive and exclusive determinations of $|V_{cb}|$ weakens the power of these theoretically clean decays in the search for new physics (NP). We demonstrate how this uncertainty can be practically removed by considering within the SM suitable ratios of the two branching ratios between each other and with other observables like the branching ratios for $K_S\to\mu^+\mu^-$, $B_{s,d}\to\mu^+\mu^-$ and $B\to K(K^*)\nu\bar\nu$. We use as basic CKM parameters $V_{us}$, $|V_{cb}|$ and the angles $\beta$ and $\gamma$ in the unitarity triangle (UT). This avoids the use of the problematic $|V_{ub}|$. A ratio involving $B(K^+\to\pi^+\nu\bar\nu)$ and $B(B_s\to\mu^+\mu^-)$ while being $|V_{cb}|$-independent exhibits sizable dependence on the angle $\gamma$. It should be of interest for several experimental groups in the coming years. We point out that the $|V_{cb}|$-independent ratio of $B(B^+\to K^+\nu\bar\nu)$ and $B(B_s\to\mu^+\mu^-)$ from Belle II and LHCb signals a $1.8\sigma$ tension with its SM value. As a complementary test of the Standard Model, we propose to extract $|V_{cb}|$ from different observables as a function of $\beta$ and $\gamma$. We illustrate this with $\epsilon_K$, $\Delta M_d$ and $\Delta M_s$ finding tensions between these three determinations of $|V_{cb}|$ within the SM. From $\Delta M_s$ and $S_{\psi K_S}$ alone we find $|V_{cb}|=41.8(6)\times 10^{-3}$ and $|V_{ub}|=3.65(12)\times 10^{-3}$. We stress the importance of a precise measurement of $\gamma$. We obtain most precise SM predictions for considered branching ratios of rare K and B decays to date.


(510)Radioactive Decay
  • Roland Diehl
Handbook of X-ray and Gamma-ray Astrophysics. Edited by Cosimo Bambi and Andrea Santangelo (2022) doi:10.1007/978-981-16-4544-0_86-1
abstract + abstract -

Radioactive decay of unstable atomic nuclei leads to liberation of nuclear binding energy in the forms of gamma-ray photons and secondary particles (electrons, positrons); their energy then energises surrounding matter. Unstable nuclei are formed in nuclear reactions, which can occur either in hot and dense extremes of stellar interiors or explosions, or from cosmic-ray collisions. In high-energy astronomy, direct observations of characteristic gamma-ray lines from the decay of radioactive isotopes are important tools to study the process of cosmic nucleosynthesis and its sources, as well as tracing the flows of ejecta from such sources of nucleosynthesis. These observations provide a valuable complement to indirect observations of radioactive energy deposits, such as the measurement of supernova light in the optical. Here we present basics of radioactive decay in astrophysical context, and how gamma-ray lines reveal details about stellar interiors, about explosions on stellar surfaces or of entire stars, and about the interstellar-medium processes that direct the flow and cooling of nucleosynthesis ashes once having left their sources. We address radioisotopes such as $^{56}$Ni, $^{44}$Ti, $^{26}$Al, $^{60}$Fe, $^{22}$Na, $^{7}$Be, and also how characteristic gamma-ray emission from the annihilation of positrons is connected to these.


(509)Calculational Techniques in Particle Theory
  • L. Tancredi
The European Physical Society Conference on High Energy Physics. 26-30 July 2021. Online conference (2022)
abstract + abstract -

In this contribution, I review some of the latest advances in calculational techniques in theoretical particle physics. I focus, in particular, on their application to the calculation of highly non-trivial scattering processes, which are relevant for precision phenomenology studies at the Large Hadron Collider at CERN.


(508)Inclusive Hadroproduction of P-wave Heavy Quarkonia in pNRQCD
  • Hee Sok Chung
EPJ Web Conf. (2022) doi:10.1051/epjconf/202225804005
abstract + abstract -

We compute NRQCD long-distance matrix elements that appear in the inclusive production cross sections of P-wave heavy quarkonia in the framework of potential NRQCD. The formalism developed in this work applies to strongly coupled charmonia and bottomonia. This makes possible the determination of color-octet NRQCD long-distance matrix elements without relying on measured cross section data, which has not been possible so far. We obtain results for inclusive production cross sections of χcJ and χbJ at the LHC, which are in good agreement with measurements.


CN-7
RU-D
(507)Gamma-ray observations of cosmic nuclei
  • Roland Diehl
EPJ Web Conf. (2022) doi:10.1051/epjconf/202226010001
abstract + abstract -

Gamma rays from nuclear processes such as radioactive decay and de-excitations are among the most-direct tools to witness the production and existence of specific nuclei and isotopes in and near cosmic nucleosynthesis sites. With space-borne instrumentation such as NuSTAR and SPI/INTEGRAL, and experimental techniques to handle a substantial instrumental background from cosmic-ray activations of the spacecraft and instrument, unique results have been obtained, from diffuse emissions of nuclei and positrons in interstellar surroundings of sources, as well as from observations of cosmic explosions and their radioactive afterglows. These witness non-sphericity in supernova explosions and a flow of nucleosynthesis ejecta through superbubbles as common source environments. Next-generation experiments that are awaiting space missions promise a next level of observational nuclear astrophysics.


CN-3
RU-B
(506)Improving the Quality of CaWO$_{4}$ Target Crystals for CRESST
  • A. Kinast,
  • G. Angloher,
  • G. Benato,
  • A. Bento,
  • A. Bertolini
  • +53
  • R. Breier,
  • C. Bucci,
  • L. Canonica,
  • A. D’Addabbo,
  • S.Di Lorenzo,
  • L. Einfalt,
  • A. Erb,
  • F.V. Feilitzsch,
  • N.Ferreiro Iachellini,
  • S. Fichtinger,
  • D. Fuchs,
  • A. Fuss,
  • A. Garai,
  • V.M. Ghete,
  • P. Gorla,
  • S. Gupta,
  • F. Hamilton,
  • D. Hauff,
  • M. Ješkovský,
  • J. Jochum,
  • M. Kaznacheeva,
  • H. Kluck,
  • H. Kraus,
  • A. Langenkämper,
  • M. Mancuso,
  • L. Marini,
  • V. Mokina,
  • A. Nilima,
  • M. Olmi,
  • T. Ortmann,
  • C. Pagliarone,
  • V. Palušová,
  • L. Pattavina,
  • F. Petricca,
  • W. Potzel,
  • P. Povinec,
  • F. Pröbst,
  • F. Pucci,
  • F. Reindl,
  • J. Rothe,
  • K. Schäffner,
  • J. Schieck,
  • D. Schmiedmayer,
  • S. Schönert,
  • C. Schwertner,
  • M. Stahlberg,
  • L. Stodolsky,
  • C. Strandhagen,
  • R. Strauss,
  • I. Usherov,
  • F. Wagner,
  • M. Willers,
  • V. Zema
  • (less)
J.Low Temp.Phys. (2022) doi:10.1007/s10909-022-02743-7
abstract + abstract -

The Cryogenic Rare Event Search with Superconducting Thermometers (CRESST) experiment aims at the direct detection of dark matter particles via their elastic scattering off nuclei in a scintillating CaWO$_4$ target crystal. The CaWO$_4$ crystal is operated together with a light detector at mK temperature and read out by a Transition Edge Sensor. For many years, CaWO$_4$ crystals have successfully been produced in-house at Technical University of Munich (TUM) with a focus on high radiopurity which is crucial to reduce background originating from radioactive contamination. In order to further improve the CaWO$_4$ crystals, an extensive chemical purification of the raw materials and the synthesised CaWO$_4$ powder has been performed. In addition, a temperature gradient simulation of the growth process and subsequently an optimisation of the growth furnace with the goal to reduce the intrinsic stress was carried out. We present results on the intrinsic stress in the CaWO$_4$ crystals and on the CaWO$_4$ powder radiopurity. A crystal grown from the purified material was installed in the current CRESST set-up. The detector is equipped with an instrumented holder which is used to measure the alpha decay rate of the crystal. We present a preliminary analysis showing a significantly reduced intrinsic background from natural decay chains.


(505)First Sagittarius A* Event Horizon Telescope Results. IV. Variability, Morphology, and Black Hole Mass
  • Kazunori Akiyama,
  • Antxon Alberdi,
  • Walter Alef,
  • Juan Carlos Algaba,
  • Richard Anantua
  • +264
  • Keiichi Asada,
  • Rebecca Azulay,
  • Uwe Bach,
  • Anne-Kathrin Baczko,
  • David Ball,
  • Mislav Baloković,
  • John Barrett,
  • Michi Bauböck,
  • Bradford A. Benson,
  • Dan Bintley,
  • Lindy Blackburn,
  • Raymond Blundell,
  • Katherine L. Bouman,
  • Geoffrey C. Bower,
  • Hope Boyce,
  • Michael Bremer,
  • Christiaan D. Brinkerink,
  • Roger Brissenden,
  • Silke Britzen,
  • Avery E. Broderick,
  • Dominique Broguiere,
  • Thomas Bronzwaer,
  • Sandra Bustamante,
  • Do-Young Byun,
  • John E. Carlstrom,
  • Chiara Ceccobello,
  • Andrew Chael,
  • Chi-kwan Chan,
  • Koushik Chatterjee,
  • Shami Chatterjee,
  • Ming-Tang Chen,
  • Yongjun Chen,
  • Xiaopeng Cheng,
  • Ilje Cho,
  • Pierre Christian,
  • Nicholas S. Conroy,
  • John E. Conway,
  • James M. Cordes,
  • Thomas M. Crawford,
  • Geoffrey B. Crew,
  • Alejandro Cruz-Osorio,
  • Yuzhu Cui,
  • Jordy Davelaar,
  • Mariafelicia De Laurentis,
  • Roger Deane,
  • Jessica Dempsey,
  • Gregory Desvignes,
  • Jason Dexter,
  • Vedant Dhruv,
  • Sheperd S. Doeleman,
  • Sean Dougal,
  • Sergio A. Dzib,
  • Ralph P. Eatough,
  • Razieh Emami,
  • Heino Falcke,
  • Joseph Farah,
  • Vincent L. Fish,
  • Ed Fomalont,
  • H.Alyson Ford,
  • Raquel Fraga-Encinas,
  • William T. Freeman,
  • Per Friberg,
  • Christian M. Fromm,
  • Antonio Fuentes,
  • Peter Galison,
  • Charles F. Gammie,
  • Roberto García,
  • Olivier Gentaz,
  • Boris Georgiev,
  • Ciriaco Goddi,
  • Roman Gold,
  • I. Arturo Gómez-Ruiz,
  • José L. Gómez,
  • Minfeng Gu,
  • Mark Gurwell,
  • Kazuhiro Hada,
  • Daryl Haggard,
  • Kari Haworth,
  • Michael H. Hecht,
  • Ronald Hesper,
  • Dirk Heumann,
  • Luis C. Ho,
  • Paul Ho,
  • Mareki Honma,
  • Chih-Wei L. Huang,
  • Lei Huang,
  • David H. Hughes,
  • Shiro Ikeda,
  • C.M.Violette Impellizzeri,
  • Makoto Inoue,
  • Sara Issaoun,
  • J. David James,
  • Buell T. Jannuzi,
  • Michael Janssen,
  • Britton Jeter,
  • Wu Jiang,
  • Alejandra Jiménez-Rosales,
  • Michael D. Johnson,
  • Svetlana Jorstad,
  • V. Abhishek Joshi,
  • Taehyun Jung,
  • Mansour Karami,
  • Ramesh Karuppusamy,
  • Tomohisa Kawashima,
  • Garrett K. Keating,
  • Mark Kettenis,
  • Dong-Jin Kim,
  • Jae-Young Kim,
  • Jongsoo Kim,
  • Junhan Kim,
  • Motoki Kino,
  • Jun Yi Koay,
  • Prashant Kocherlakota,
  • Yutaro Kofuji,
  • Patrick M. Koch,
  • Shoko Koyama,
  • Carsten Kramer,
  • Michael Kramer,
  • Thomas P. Krichbaum,
  • Cheng-Yu Kuo,
  • Noemi La Bella,
  • Tod R. Lauer,
  • Daeyoung Lee,
  • Sang-Sung Lee,
  • Po Kin Leung,
  • Aviad Levis,
  • Zhiyuan Li,
  • Rocco Lico,
  • Greg Lindahl,
  • Michael Lindqvist,
  • Mikhail Lisakov,
  • Jun Liu,
  • Kuo Liu,
  • Elisabetta Liuzzo,
  • Wen-Ping Lo,
  • Andrei P. Lobanov,
  • Laurent Loinard,
  • J. Colin Lonsdale,
  • Ru-Sen Lu,
  • Jirong Mao,
  • Nicola Marchili,
  • Sera Markoff,
  • Daniel P. Marrone,
  • Alan P. Marscher,
  • Iván Martí-Vidal,
  • Satoki Matsushita,
  • Lynn D. Matthews,
  • Lia Medeiros,
  • Karl M. Menten,
  • Daniel Michalik,
  • Izumi Mizuno,
  • Yosuke Mizuno,
  • James M. Moran,
  • Kotaro Moriyama,
  • Monika Moscibrodzka,
  • Cornelia Müller,
  • Alejandro Mus,
  • Gibwa Musoke,
  • Ioannis Myserlis,
  • Andrew Nadolski,
  • Hiroshi Nagai,
  • Neil M. Nagar,
  • Masanori Nakamura,
  • Ramesh Narayan,
  • Gopal Narayanan,
  • Iniyan Natarajan,
  • Antonios Nathanail,
  • Santiago Navarro Fuentes,
  • Joey Neilsen,
  • Roberto Neri,
  • Chunchong Ni,
  • Aristeidis Noutsos,
  • Michael A. Nowak,
  • Junghwan Oh,
  • Hiroki Okino,
  • Héctor Olivares,
  • Gisela N. Ortiz-León,
  • Tomoaki Oyama,
  • Daniel C.M. Palumbo,
  • Georgios Filippos Paraschos,
  • Jongho Park,
  • Harriet Parsons,
  • Nimesh Patel,
  • Ue-Li Pen,
  • Dominic W. Pesce,
  • Vincent Piétu,
  • Richard Plambeck,
  • Aleksandar PopStefanija,
  • Oliver Porth,
  • Felix M. Pötzl,
  • Ben Prather,
  • Jorge A. Preciado-López,
  • Hung-Yi Pu,
  • Venkatessh Ramakrishnan,
  • Ramprasad Rao,
  • Mark G. Rawlings,
  • Alexander W. Raymond,
  • Luciano Rezzolla,
  • Angelo Ricarte,
  • Bart Ripperda,
  • Freek Roelofs,
  • Alan Rogers,
  • Eduardo Ros,
  • Cristina Romero-Cañizales,
  • Arash Roshanineshat,
  • Helge Rottmann,
  • Alan L. Roy,
  • Ignacio Ruiz,
  • Chet Ruszczyk,
  • Kazi L.J. Rygl,
  • Salvador Sánchez,
  • David Sánchez-Argüelles,
  • Miguel Sánchez-Portal,
  • Mahito Sasada,
  • Kaushik Satapathy,
  • Tuomas Savolainen,
  • F.Peter Schloerb,
  • Jonathan Schonfeld,
  • Karl-Friedrich Schuster,
  • Lijing Shao,
  • Zhiqiang Shen,
  • Des Small,
  • Bong Won Sohn,
  • Jason SooHoo,
  • Kamal Souccar,
  • He Sun,
  • Fumie Tazaki,
  • J. Alexandra Tetarenko,
  • Paul Tiede,
  • Remo P.J. Tilanus,
  • Michael Titus,
  • Pablo Torne,
  • Efthalia Traianou,
  • Tyler Trent,
  • Sascha Trippe,
  • Matthew Turk,
  • Ilse van Bemmel,
  • Huib Jan van Langevelde,
  • Daniel R. van Rossum,
  • Jesse Vos,
  • Jan Wagner,
  • Derek Ward-Thompson,
  • John Wardle,
  • Jonathan Weintroub,
  • Norbert Wex,
  • Robert Wharton,
  • Maciek Wielgus,
  • Kaj Wiik,
  • Gunther Witzel,
  • Michael F. Wondrak,
  • George N. Wong,
  • Qingwen Wu,
  • Paul Yamaguchi,
  • Doosoo Yoon,
  • André Young,
  • Ken Young,
  • Ziri Younsi,
  • Feng Yuan,
  • Ye-Fei Yuan,
  • J.Anton Zensus,
  • Shuo Zhang,
  • Guang-Yao Zhao,
  • Shan-Shan Zhao,
  • Dominic O. Chang
  • (less)
Astrophys.J.Lett. (2022) doi:10.3847/2041-8213/ac6736
abstract + abstract -

In this paper we quantify the temporal variability and image morphology of the horizon-scale emission from Sgr A*, as observed by the EHT in 2017 April at a wavelength of 1.3 mm. We find that the Sgr A* data exhibit variability that exceeds what can be explained by the uncertainties in the data or by the effects of interstellar scattering. The magnitude of this variability can be a substantial fraction of the correlated flux density, reaching ∼100% on some baselines. Through an exploration of simple geometric source models, we demonstrate that ring-like morphologies provide better fits to the Sgr A* data than do other morphologies with comparable complexity. We develop two strategies for fitting static geometric ring models to the time-variable Sgr A* data; one strategy fits models to short segments of data over which the source is static and averages these independent fits, while the other fits models to the full data set using a parametric model for the structural variability power spectrum around the average source structure. Both geometric modeling and image-domain feature extraction techniques determine the ring diameter to be 51.8 ± 2.3 μas (68% credible intervals), with the ring thickness constrained to have an FWHM between ∼30% and 50% of the ring diameter. To bring the diameter measurements to a common physical scale, we calibrate them using synthetic data generated from GRMHD simulations. This calibration constrains the angular size of the gravitational radius to be

μas, which we combine with an independent distance measurement from maser parallaxes to determine the mass of Sgr A* to be

M

$_{⊙}$.


CN-6
RU-B
(504)The EUSO@TurLab project in the framework of the JEM-EUSO program
  • P. Barrillon,
  • M. Battisti,
  • A. Belov,
  • M. Bertaina,
  • F. Bisconti
  • +31
  • S. Blin-Bondil,
  • R. Bonino,
  • F. Capel,
  • R. Caruso,
  • M. Casolino,
  • G. Contino,
  • G. Cotto,
  • S. Dagoret‑Campagne,
  • F. Fenu,
  • C. Fornaro,
  • R. Forza,
  • P. Gorodetzky,
  • N. Guardone,
  • A. Jung,
  • P. Klimov,
  • M. Manfrin,
  • L. Marcelli,
  • M. Mignone,
  • H. Miyamoto,
  • R. Mulas,
  • M. Onorato,
  • E. Parizot,
  • L. Piotrowski,
  • Z. Plebaniak,
  • G. Prevot,
  • J. Szabelski,
  • G. Suino,
  • Y. Takizawa,
  • P. Tibaldi,
  • C. Vigorito,
  • A. Youssef
  • (less)
Exper.Astron. (2022) doi:10.1007/s10686-022-09871-8
abstract + abstract -

<jats:title>Abstract</jats:title><jats:p>The EUSO@TurLab project aims at performing experiments to reproduce Earth UV emissions as seen from a low Earth orbit by the planned missions of the JEM-EUSO program. It makes use of the TurLab facility, which is a laboratory, equipped with a 5 m diameter and 1 m depth rotating tank, located at the Physics Department of the University of Turin. All the experiments are designed and performed based on simulations of the expected response of the detectors to be flown in space. In April 2016 the TUS detector and more recently in October 2019 the Mini-EUSO experiment, both part of the JEM-EUSO program, have been placed in orbit to map the UV Earth emissions. It is, therefore, now possible to compare the replicas performed at TurLab with the actual images detected in space to understand the level of fidelity in terms of reproduction of the expected signals. We show that the laboratory tests reproduce at the order of magnitude level the measurements from space in terms of spatial extension and time duration of the emitted UV light, as well as the intensity in terms of expected counts per pixel per unit time when atmospheric transient events, diffuse nightlow background light, and artificial light sources are considered. Therefore, TurLab is found to be a very useful facility for testing the acquisition logic of the detectors of the present and future missions of the JEM-EUSO program and beyond in order to reproduce atmospheric signals in the laboratory.</jats:p>


LRSM
(503)SDD Analog Readout System for the ComPol CubeSat Compton Polarimeter
  • L. G. Toscano,
  • G. Deda,
  • G. Di Giovanni,
  • M. Arrigucci,
  • P. King
  • +7
  • P. Lechner,
  • M. J. Losekamm,
  • M. Meier,
  • S. Mertens,
  • M. Willers,
  • M. Carminati,
  • C. Fiorini
  • (less)
2022 IEEE Nuclear Science Symposium and Medical Imaging Conference (2022) doi:10.1109/NSS/MIC44845.2022.10398890
abstract + abstract -

Astronomical X-ray polarimetry is a powerful tool to extract information from hard X-rays spectrum of celestial bodies. In this context, the ComPol project aims to fly a Compton polarimeter in a CubeSat to investigate the emissions of the binary black hole (BBH) system Cygnus X-1. Based on Compton events detection, the CubeSat is featured by two detection systems: 1) a Silicon Drift Detector (SDD) matrix employed as scatterer and 2) a scintillator read by Silicon Photon Multiplier (SiPM) array to absorb the scattered photons. This paper focuses on the development of the first detection system for the reconstruction of Compton events. The readout electronic chain is composed of two 7-pixel SDD matrices, CUBE preamplifiers and SFERA ASIC Analog Pulse Processor (APP) handled by FPGA technology for its control and data flow management. This paper presents this readout system, composed by two boards: one housing SFERA ASIC, which includes an on-chip ADC, the other which includes the SDD matrix and the preamplifiers. In this manuscript, the test results performed with the pre-prototype system devised in the first phase of the project to characterize the SDD module and to evaluate the SFERA internal ADC performances are reported together with the ones performed with the prototype system.


CN-7
RU-A
(502)Symmetry restoration in mean-field approaches
  • J.A. Sheikh,
  • J. Dobaczewski,
  • P. Ring,
  • L. M. Robledo,
  • C. Yannouleas
Journal of Physics G: Nuclear and Particle Physics (November/2021) e-Print:1901.06992 doi:10.1088/1361-6471/ac288a
abstract + abstract -

The mean-field approximation based on effective interactions or density functionals plays a pivotal role in the description of finite quantum many-body systems that are too large to be treated by ab initio methods. Some examples are strongly interacting medium and heavy mass atomic nuclei and mesoscopic condensed matter systems. In this approach, the linear Schrödinger equation for the exact many-body wave function is mapped onto a non-linear one-body potential problem. This approximation, not only provides computationally very simple solutions even for systems with many particles, but due to the non-linearity, it also allows for obtaining solutions that break essential symmetries of the system, often connected with phase transitions. In this way, additional correlations are subsumed in the system. However, the mean-field approach suffers from the drawback that the corresponding wave functions do not have sharp quantum numbers and, therefore, many results cannot be compared directly with experimental data. In this article, we discuss general group-theory techniques to restore the broken symmetries, and provide detailed expressions on the restoration of translational, rotational, spin, isospin, parity and gauge symmetries, where the latter corresponds to the restoration of the particle number. In order to avoid the numerical complexity of exact projection techniques, various approximation methods available in the literature are examined. Applications of the projection methods are presented for simple nuclear models, realistic calculations in relatively small configuration spaces, nuclear energy density functional (EDF) theory, as well as in other mesoscopic systems. We also discuss applications of projection techniques to quantum statistics in order to treat the averaging over restricted ensembles with fixed quantum numbers. Further, unresolved problems in the application of the symmetry restoration methods to the EDF theories are highlighted in the present work.


CN-7
RU-A
(501)Nuclear matter in relativistic Brueckner-Hartree-Fock theory with Bonn potential in the full Dirac space
  • Sibo Wang,
  • Qiang Zhao,
  • Peter Ring,
  • Jie Meng
abstract + abstract -

Starting from the Bonn potential, the relativistic Brueckner-Hartree-Fock (RBHF) equations are solved for nuclear matter in the full Dirac space, which provides a unique way to determine the single-particle potentials and avoids the approximations applied in the RBHF calculations in the Dirac space with positive-energy states (PESs) only. The uncertainties of the RBHF calculations in the Dirac space with PESs only are investigated, and the importance of RBHF calculations in the full Dirac space is demonstrated. In the RBHF calculations in the full Dirac space, the empirical saturation properties of symmetric nuclear matter are reproduced, and the obtained equation of state agrees with the results based on the relativistic Green's function approach up to the saturation density.


CN-7
RU-A
(500)Finite-temperature linear response theory based on relativistic Hartree Bogoliubov model with point-coupling interaction
  • A. Ravlić,
  • Y. F. Niu,
  • T. Nikšić,
  • N. Paar,
  • P. Ring
Physical Review C (December/2021) e-Print:2108.08702 doi:10.1103/PhysRevC.104.064302
abstract + abstract -

The finite-temperature linear response theory based on the finite-temperature relativistic Hartree-Bogoliubov (FT-RHB) model is developed in the charge-exchange channel to study the temperature evolution of spin-isospin excitations. Calculations are performed self-consistently with relativistic point-coupling interactions DD-PC1 and DD-PCX. In the charge-exchange channel, the pairing interaction can be split into isovector (T=1) and isoscalar (T=0) parts. For the isovector component, the same separable form of the Gogny D1S pairing interaction is used both for the ground-state calculation as well as for the residual interaction, while the strength of the isoscalar pairing in the residual interaction is determined by comparison with experimental data on Gamow-Teller resonance (GTR) and isobaric analog resonance (IAR) centroid energy differences in even-even tin isotopes. The temperature effects are introduced by treating Bogoliubov quasiparticles within a grand-canonical ensemble. Thus, unlike the conventional formulation of the quasiparticle random-phase approximation (QRPA) based on the Bardeen-Cooper-Schrieffer (BCS) basis, our model is formulated within the Hartree-Fock-Bogoliubov (HFB) quasiparticle basis. Implementing a relativistic point-coupling interaction and a separable pairing force allows for the reduction of complicated two-body residual interaction matrix elements, which considerably decreases the dimension of the problem in the coordinate space. The main advantage of this method is to avoid the diagonalization of a large QRPA matrix, especially at finite temperature where the size of configuration space is significantly increased. The implementation of the linear response code is used to study the temperature evolution of IAR, GTR, and spin-dipole resonance (SDR) in even-even tin isotopes in the temperature range T=0–1.5 MeV.


CN-7
RU-A
(499)Study of the Strong Interaction Among Hadrons with Correlations at the LHC
  • L. Fabbietti,
  • V. Mantovani Sarti,
  • O. Vázquez Doce
Annual Review of Nuclear and Particle Science (9/2021) doi:10.1146/annurev-nucl-102419-034438
abstract + abstract -

The strong interaction among hadrons has been measured in the past by scattering experiments. Although this technique has been extremely successful in providing information about the nucleon-nucleon and pion-nucleon interactions, when unstable hadrons are considered the experiments become more challenging. In the last few years, the analysis of correlations in the momentum space for pairs of stable and unstable hadrons measured in pp and p+Pb collisions by the ALICE Collaboration at the LHC has provided a new method to investigate the strong interaction among hadrons. In this article, we review the numerous results recently achieved for hyperon-nucleon, hyperon-hyperon, and kaon-nucleon pairs, which show that this new method opens the possibility of measuring the residual strong interaction of any hadron pair.


CN-7
PhD Thesis
RU-A
(498)Analysis techniques for femtoscopy and correlation studies in small collision systems and their applications to the investigation of proton-Lambda and Lambda-Lambda interactions with ALICE
  • Dimitar Lubomirov Mihaylov - Advisor: Laura Fabbietti
Thesis (8/2021) link
abstract + abstract -

The topic of this work is the non-traditional baryon–baryon femtoscopy, the goal of which is to study the interaction potential between different baryon pairs, assuming that their emission source is known. A new analysis framework (CATS) has been developed to model the correlation function. Further, a new model to describe the emission source was created, which accounts for the modulation related to particle production through the decays of short-lived resonances. Finally, these new analysis methods were applied to study the strong interaction acting between proton-Lambda and Lambda-Lambda pairs.


CN-6
PhD Thesis
(497)The Origin of High-Energy Cosmic Particles: IceCube Neutrinos and the Blazar Case
  • Theo Glauch - Advisor: Elisa Resconi
Thesis (2/2021) link
abstract + abstract -

This thesis presents several multi-messenger analyses, searching for the long-sough sources of high-energy cosmic radiation. By combining data from the IceCube Neutrino Detector and other multi-frequency observatories, the first two significant neutrino point sources - the blazar TXS 0506+056 and the Seyfert 2 galaxy NGC 1068 - are identified. Furthermore, a correlation study of high-energy neutrinos with gamma-ray blazars finds 3.2σ evidence for an astrophysical neutrino flux contribution from IBL/HBL blazars. Finally, we present a deep neural network that helps to optimize IceCube’s event selection pipeline.


RU-C
(496)The local PNG bias of neutral Hydrogen, H$_{I}$
  • Alexandre Barreira
abstract + abstract -

We use separate universe simulations with the IllustrisTNG galaxy formation model to predict the local PNG bias parameters bΦ and bΦδ of atomic neutral hydrogen, H$_{I}$. These parameters and their relation to the linear density bias parameter b

$_{1}$ play a key role in observational constraints of the local PNG parameter f

$_{NL}$ using the H$_{I}$ power spectrum and bispectrum. Our results show that the popular calculation based on the universality of the halo mass function overpredicts the bΦ(b

$_{1}$) and bΦδ(b

$_{1}$) relations measured in the simulations. In particular, our results show that at z ≲ 1 the H$_{I}$ power spectrum is more sensitive to f

$_{NL}$ compared to previously thought (bΦ is more negative), but is less sensitive at other epochs (bΦ is less positive). We discuss how this can be explained by the competition of physical effects such as that large-scale gravitational potentials with local PNG (i) accelerate the conversion of hydrogen to heavy elements by star formation, (ii) enhance the effects of baryonic feedback that eject the gas to regions more exposed to ionizing radiation, and (iii) promote the formation of denser structures that shield the H$_{I}$ more efficiently. Our numerical results can be used to revise existing forecast studies on f

$_{NL}$ using 21 cm line-intensity mapping data. Despite this first step towards predictions for the local PNG bias parameters of H$_{I}$, we emphasize that more work is needed to assess their sensitivity on the assumed galaxy formation physics and H$_{I}$ modeling strategy.


CN-4
RU-D
(495)CLASH-VLT: Abell~S1063. Cluster assembly history and spectroscopic catalogue
  • A. Mercurio,
  • P. Rosati,
  • A. Biviano,
  • M. Annunziatella,
  • M. Girardi
  • +29
  • B. Sartoris,
  • M. Nonino,
  • M. Brescia,
  • G. Riccio,
  • C. Grillo,
  • I. Balestra,
  • G. B. Caminha,
  • G. De Lucia,
  • R. Gobat,
  • S. Seitz,
  • P. Tozzi,
  • M. Scodeggio,
  • E. Vanzella,
  • G. Angora,
  • P. Bergamini,
  • S. Borgani,
  • R. Demarco,
  • M. Meneghetti,
  • V. Strazzullo,
  • L. Tortorelli,
  • K. Umetsu,
  • A. Fritz,
  • D. Gruen,
  • D. Kelson,
  • M. Lombardi,
  • C. Maier,
  • M. Postman,
  • G. Rodighiero,
  • B. Ziegler
  • (less)
abstract + abstract -

Using the CLASH-VLT survey, we assembled an unprecedented sample of 1234 spectroscopically confirmed members in Abell~S1063, finding a dynamically complex structure at z_cl=0.3457 with a velocity dispersion \sigma_v=1380 -32 +26 km s^-1. We investigate cluster environmental and dynamical effects by analysing the projected phase-space diagram and the orbits as a function of galaxy spectral properties. We classify cluster galaxies according to the presence and strength of the [OII] emission line, the strength of the Hδ absorption line, and colours. We investigate the relationship between the spectral classes of galaxies and their position in the projected phase-space diagram. We analyse separately red and blue galaxy orbits. By correlating the observed positions and velocities with the projected phase-space constructed from simulations, we constrain the accretion redshift of galaxies with different spectral types. Passive galaxies are mainly located in the virialised region, while emission-line galaxies are outside r_200, and are accreted later into the cluster. Emission-lines and post-starbursts show an asymmetric distribution in projected phase-space within r_200, with the first being prominent at Delta_v/sigma <~-1.5$, and the second at Delta_v/ sigma >~ 1.5, suggesting that backsplash galaxies lie at large positive velocities. We find that low-mass passive galaxies are accreted in the cluster before the high-mass ones. This suggests that we observe as passives only the low-mass galaxies accreted early in the cluster as blue galaxies, that had the time to quench their star formation. We also find that red galaxies move on more radial orbits than blue galaxies. This can be explained if infalling galaxies can remain blue moving on tangential orbits.


CN-4
RU-D
(494)The PAU Survey: Measurement of Narrow-band galaxy properties with Approximate Bayesian Computation
  • Luca Tortorelli,
  • Malgorzata Siudek,
  • Beatrice Moser,
  • Tomasz Kacprzak,
  • Pascale Berner
  • +20
  • Alexandre Refregier,
  • Adam Amara,
  • Juan García-Bellido,
  • Laura Cabayol,
  • Jorge Carretero,
  • Francisco J. Castander,
  • Juan De Vicente,
  • Martin Eriksen,
  • Enrique Fernandez,
  • Enrique Gaztanaga,
  • Hendrik Hildebrandt,
  • Benjamin Joachimi,
  • Ramon Miquel,
  • Ignacio Sevilla-Noarbe,
  • Cristóbal Padilla,
  • Pablo Renard,
  • Eusebio Sanchez,
  • Santiago Serrano,
  • Pau Tallada-Crespí,
  • Angus H. Wright
  • (less)
abstract + abstract -

Narrow-band imaging surveys allow the study of the spectral characteristics of galaxies without the need of performing their spectroscopic follow-up. In this work, we forward-model the Physics of the Accelerating Universe Survey (PAUS) narrow-band data. The aim is to improve the constraints on the spectral coefficients used to create the galaxy spectral energy distributions (SED) of the galaxy population model in Tortorelli et al. 2020. In that work, the model parameters were inferred from the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) data using Approximate Bayesian Computation (ABC). This led to stringent constraints on the B-band galaxy luminosity function parameters, but left the spectral coefficients only broadly constrained. To address that, we perform an ABC inference using CFHTLS and PAUS data. This is the first time our approach combining forward-modelling and ABC is applied simultaneously to multiple datasets. We test the results of the ABC inference by comparing the narrow-band magnitudes of the observed and simulated galaxies using Principal Component Analysis, finding a very good agreement. Furthermore, we prove the scientific potential of the constrained galaxy population model to provide realistic stellar population properties by measuring them with the SED fitting code \textsc{CIGALE}. We use CFHTLS broad-band and PAUS narrow-band photometry for a flux-limited (i<22.5) sample of galaxies up to redshift z∼0.8. We find that properties like stellar masses, star-formation rates, mass-weighted stellar ages and metallicities are in agreement within errors between observations and simulations. Overall, this work shows the ability of our galaxy population model to correctly forward-model a complex dataset such as PAUS and the ability to reproduce the diversity of galaxy properties at the redshift range spanned by CFHTLS and PAUS.


RU-C
(493)Lattice simulations of inflation
  • Angelo Caravano,
  • Eiichiro Komatsu,
  • Kaloian D. Lozanov,
  • Jochen Weller
Journal of Cosmology and Astroparticle Physics (12/2021) doi:10.1088/1475-7516/2021/12/010
abstract + abstract -

The scalar field theory of cosmological inflation constitutes nowadays one of the preferred scenarios for the physics of the early universe. In this paper we aim at studying the inflationary universe making use of a numerical lattice simulation. Various lattice codes have been written in the last decades and have been extensively used for understating the reheating phase of the universe, but they have never been used to study the inflationary phase itself far from the end of inflation (i.e. about 50 e-folds before the end of inflation). In this paper we use a lattice simulation to reproduce the well-known results of some simple models of single-field inflation, particularly for the scalar field perturbation. The main model that we consider is the standard slow-roll inflation with an harmonic potential for the inflaton field. We explore the technical aspects that need to be accounted for in order to reproduce with precision the nearly scale invariant power spectrum of inflaton perturbations. We also consider the case of a step potential, and show that the simulation is able to correctly reproduce the oscillatory features in the power spectrum of this model. Even if a lattice simulation is not needed in these cases, that are well within the regime of validity of linear perturbation theory, this sets the basis to future work on using lattice simulations to study more complicated models of inflation.


(492)The DESI N-body simulation project – I. Testing the robustness of simulations for the DESI dark time survey
  • Cameron Grove,
  • Chia-Hsun Chuang,
  • Ningombam Chandrachani Devi,
  • Lehman Garrison,
  • Benjamin L'Huillier
  • +17
  • Yu Feng,
  • John Helly,
  • César Hernández-Aguayo,
  • Shadab Alam,
  • Hanyu Zhang,
  • Yu Yu ,
  • Shaun Cole,
  • Daniel Eisenstein,
  • Peder Norberg,
  • Risa Wechsler,
  • David Brooks,
  • Kyle Dawson,
  • Martin Landriau,
  • Aaron Meisner,
  • Claire Poppett,
  • Gregory Tarlé,
  • Octavio Valenzuela
  • (less)
Mon.Not.Roy.Astron.Soc. (12/2021) e-Print:2112.09138 doi:10.1093/mnras/stac1947
abstract + abstract -

Analysis of large galaxy surveys requires confidence in the robustness of numerical simulation methods. The simulations are used to construct mock galaxy catalogues to validate data analysis pipelines and identify potential systematics. We compare three N-body simulation codes, abacus, gadget-2, and swift, to investigate the regimes in which their results agree. We run N-body simulations at three different mass resolutions, 6.25 × 10^8, 2.11 × 10^9, and 5.00 × 10^9 h^−1 M_⊙, matching phases to reduce the noise within the comparisons. We find systematic errors in the halo clustering between different codes are smaller than the Dark Energy Spectroscopic Instrument (DESI) statistical error for s > 20 h−1 Mpc in the correlation function in redshift space. Through the resolution comparison we find that simulations run with a mass resolution of 2.1 × 10^9 h^−1 M_⊙ are sufficiently converged for systematic effects in the halo clustering to be smaller than the DESI statistical error at scales larger than 20 h−1 Mpc. These findings show that the simulations are robust for extracting cosmological information from large scales which is the key goal of the DESI survey. Comparing matter power spectra, we find the codes agree to within 1 per cent for k ≤ 10 h Mpc^−1. We also run a comparison of three initial condition generation codes and find good agreement. In addition, we include a quasi-N-body code, FastPM, since we plan use it for certain DESI analyses. The impact of the halo definition and galaxy–halo relation will be presented in a follow-up study.


(491)Combining Planck and SPT cluster catalogs: cosmological analysis and impact on Planck scaling relation calibration
  • L. Salvati,
  • A. Saro,
  • S. Bocquet,
  • M. Costanzi,
  • B. Ansarinejad
  • +39
  • B.A. Benson,
  • L.E. Bleem,
  • M.S. Calzadilla,
  • J.E. Carlstrom,
  • C.L. Chang,
  • R. Chown,
  • A.T. Crites,
  • T. de Haan,
  • M.A. Dobbs,
  • W.B. Everett,
  • B. Floyd,
  • S. Grandis,
  • E.M. George,
  • N.W. Halverson,
  • G.P. Holder,
  • W.L. Holzapfel,
  • J.D. Hrubes,
  • A.T. Lee,
  • D. Luong-Van,
  • M. McDonald,
  • J.J. McMahon,
  • S.S. Meyer,
  • M. Millea,
  • L.M. Mocanu,
  • J.J. Mohr,
  • T. Natoli,
  • Y. Omori,
  • S. Padin,
  • C. Pryke,
  • C.L. Reichardt,
  • J.E. Ruhl,
  • F. Ruppin,
  • K.K. Schaffer,
  • T. Schrabback,
  • E. Shirokoff,
  • Z. Staniszewski,
  • A.A. Stark,
  • J.D. Vieira,
  • R. Williamson
  • (less)
(12/2021) e-Print:2112.03606
abstract + abstract -

We provide the first combined cosmological analysis of South Pole Telescope (SPT) and Planck cluster catalogs. The aim is to provide an independent calibration for Planck scaling relations, exploiting the cosmological constraining power of the SPT-SZ cluster catalog and its dedicated weak lensing (WL) and X-ray follow-up observations. We build a new version of the Planck cluster likelihood. In the $\nu \Lambda$CDM scenario, focusing on the mass slope and mass bias of Planck scaling relations, we find $\alpha_{\text{SZ}} = 1.49 _{-0.10}^{+0.07}$ and $(1-b)_{\text{SZ}} = 0.69 _{-0.14}^{+0.07}$ respectively. The results for the mass slope show a $\sim 4 \, \sigma$ departure from the self-similar evolution, $\alpha_{\text{SZ}} \sim 1.8$. This shift is mainly driven by the matter density value preferred by SPT data, $\Omega_m = 0.30 \pm 0.03$, lower than the one obtained by Planck data alone, $\Omega_m = 0.37 _{-0.06}^{+0.02}$. The mass bias constraints are consistent both with outcomes of hydrodynamical simulations and external WL calibrations, $(1-b) \sim 0.8$, and with results required by the Planck cosmic microwave background cosmology, $(1-b) \sim 0.6$. From this analysis, we obtain a new catalog of Planck cluster masses $M_{500}$. We estimate the relation between the published Planck derived $M_{\text{SZ}}$ masses and our derived masses, as a measured mass bias. We analyse the mass, redshift and detection noise dependence of this quantity, finding an increasing trend towards high redshift and low mass. These results mimic the effect of departure from self-similarity in cluster evolution, showing different dependencies for the low-mass high-mass, low-z high-z regimes.


CN-6
(490)Observation of $\Lambda_b^0\rightarrow D^+ p \pi^-\pi^-$ and $\Lambda_b^0\rightarrow D^{*+} p \pi^-\pi^-$ decays
  • Roel Aaij,
  • Ahmed Sameh Wagih Abdelmotteleb,
  • Carlos Abellán Beteta,
  • Fernando Jesus Abudinén,
  • Thomas Ackernley
  • +1008
  • Bernardo Adeva,
  • Marco Adinolfi,
  • Hossein Afsharnia,
  • Christina Agapopoulou,
  • Christine Angela Aidala,
  • Salvatore Aiola,
  • Ziad Ajaltouni,
  • Simon Akar,
  • Johannes Albrecht,
  • Federico Alessio,
  • Michael Alexander,
  • Alejandro Alfonso Albero,
  • Zakariya Aliouche,
  • Georgy Alkhazov,
  • Paula Alvarez Cartelle,
  • Sandra Amato,
  • Jake Lewis Amey,
  • Yasmine Amhis,
  • Liupan An,
  • Lucio Anderlini,
  • Martin Andersson,
  • Aleksei Andreianov,
  • Mirco Andreotti,
  • Flavio Archilli,
  • Alexander Artamonov,
  • Marina Artuso,
  • Kenenbek Arzymatov,
  • Elie Aslanides,
  • Michele Atzeni,
  • Benjamin Audurier,
  • Sebastian Bachmann,
  • Marie Bachmayer,
  • John Back,
  • Pablo Baladron Rodriguez,
  • Vladislav Balagura,
  • Wander Baldini,
  • Juan Baptista de Souza Leite,
  • Matteo Barbetti,
  • Roger Barlow,
  • Sergey Barsuk,
  • William Barter,
  • Matteo Bartolini,
  • Fedor Baryshnikov,
  • Jan-Marc Basels,
  • Saliha Bashir,
  • Giovanni Bassi,
  • Baasansuren Batsukh,
  • Alexander Battig,
  • Aurelio Bay,
  • Anja Beck,
  • Maik Becker,
  • Franco Bedeschi,
  • Ignacio Bediaga,
  • Andrew Beiter,
  • Vladislav Belavin,
  • Samuel Belin,
  • Violaine Bellee,
  • Konstantin Belous,
  • Ilia Belov,
  • Ivan Belyaev,
  • Giovanni Bencivenni,
  • Eli Ben-Haim,
  • Alexander Berezhnoy,
  • Roland Bernet,
  • Daniel Berninghoff,
  • Harris Conan Bernstein,
  • Claudia Bertella,
  • Alessandro Bertolin,
  • Christopher Betancourt,
  • Federico Betti,
  • Ia. Bezshyiko,
  • Iaroslava Bezshyiko,
  • Srishti Bhasin,
  • Jihyun Bhom,
  • Lingzhu Bian,
  • Martin Stefan Bieker,
  • Nicolo Vladi Biesuz,
  • Simone Bifani,
  • Pierre Billoir,
  • Alice Biolchini,
  • Matthew Birch,
  • Fionn Caitlin Ros Bishop,
  • Alexander Bitadze,
  • Andrea Bizzeti,
  • Mikkel Bjørn,
  • Michele Piero Blago,
  • Thomas Blake,
  • Frederic Blanc,
  • Steven Blusk,
  • Dana Bobulska,
  • Julian Alexander Boelhauve,
  • Oscar Boente Garcia,
  • Thomas Boettcher,
  • Alexey Boldyrev,
  • Alexander Bondar,
  • Nikolay Bondar,
  • Silvia Borghi,
  • Maxim Borisyak,
  • Martino Borsato,
  • Jozef Tomasz Borsuk,
  • Sonia Amina Bouchiba,
  • Themistocles Bowcock,
  • Alexandre Boyer,
  • Concezio Bozzi,
  • Matthew John Bradley,
  • Svende Braun,
  • Alexandre Brea Rodriguez,
  • Jolanta Brodzicka,
  • Arnau Brossa Gonzalo,
  • Davide Brundu,
  • Annarita Buonaura,
  • Laura Buonincontri,
  • Aodhan Tomas Burke,
  • Christopher Burr,
  • Albert Bursche,
  • Anatoly Butkevich,
  • Jordy Sebastiaan Butter,
  • Jan Buytaert,
  • Wiktor Byczynski,
  • Sandro Cadeddu,
  • Hao Cai,
  • Roberto Calabrese,
  • Lukas Calefice,
  • Stefano Cali,
  • Ryan Calladine,
  • Marta Calvi,
  • Miriam Calvo Gomez,
  • Patricia Camargo Magalhaes,
  • Pierluigi Campana,
  • Angel Fernando Campoverde Quezada,
  • Simone Capelli,
  • Lorenzo Capriotti,
  • Angelo Carbone,
  • Giovanni Carboni,
  • Roberta Cardinale,
  • Alessandro Cardini,
  • Ina Carli,
  • Paolo Carniti,
  • Leon David Carus,
  • Kazuyoshi Carvalho Akiba,
  • Adrian Casais Vidal,
  • Rowina Caspary,
  • Gianluigi Casse,
  • Marco Cattaneo,
  • Giovanni Cavallero,
  • Sara Celani,
  • Jacopo Cerasoli,
  • Daniel Cervenkov,
  • Abbie Jane Chadwick,
  • Matthew George Chapman,
  • Matthew Charles,
  • Philippe Charpentier,
  • Ph. Charpentier,
  • Carlos Alberto Chavez Barajas,
  • Maximilien Chefdeville,
  • Chen Chen,
  • Shanzhen Chen,
  • Aleksei Chernov,
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  • Zhiyu Xiang,
  • Dong Xiao,
  • Yuehong Xie,
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  • Jingyi Xu,
  • Li Xu,
  • Menglin Xu,
  • Qingnian Xu,
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  • Zhihao Xu,
  • Di Yang,
  • Shuangli Yang,
  • Youhua Yang,
  • Zhenwei Yang,
  • Zishuo Yang,
  • Yuezhe Yao,
  • Lauren Emma Yeomans,
  • Hang Yin,
  • Jiesheng Yu,
  • Xuhao Yuan,
  • Oleg Yushchenko,
  • Ettore Zaffaroni,
  • Mikhail Zavertyaev,
  • Milosz Zdybal,
  • Oleksandr Zenaiev,
  • Ming Zeng,
  • Dongliang Zhang,
  • Liming Zhang,
  • Shulei Zhang,
  • Shunan Zhang,
  • Yanxi Zhang,
  • Yu Zhang,
  • Alina Zharkova,
  • Alexey Zhelezov,
  • Yangheng Zheng,
  • Tianwen Zhou,
  • Xiaokang Zhou,
  • Yixiong Zhou,
  • Valeriia Zhovkovska,
  • Xianglei Zhu,
  • Xiaoyu Zhu,
  • Zhanwen Zhu,
  • Valery Zhukov,
  • Jennifer Brigitta Zonneveld,
  • Quan Zou,
  • Stefano Zucchelli,
  • Davide Zuliani,
  • Gianluca Zunica
  • (less)
abstract + abstract -

The multihadron decays $ {\Lambda}_b^0 $ → D+pπ−π− and $ {\Lambda}_b^0 $ → D$^{*}$+pπ−π− are observed in data corresponding to an integrated luminosity of 3 fb$^{−1}$, collected in proton-proton collisions at centre-of-mass energies of 7 and 8 TeV by the LHCb detector. Using the decay $ {\Lambda}_b^0 $ → $ {\Lambda}_c^{+} $π$^{+}$π$^{−}$π$^{−}$ as a normalisation channel, the ratio of branching fractions is measured to be$ \frac{\mathcal{B}\left({\Lambda}_b^0\to {D}^{+}p{\pi}^{-}{\pi}^{-}\right)}{\mathcal{B}\left({\Lambda}_b^0\to {\Lambda}_c^0{\pi}^{+}{\pi}^{-}{\pi}^{-}\right)}\times \frac{\mathcal{B}\left({D}^{+}\to {K}^{-}{\pi}^{+}{\pi}^{+}\right)}{\mathcal{B}\left({\Lambda}_c^0\to {pK}^{-}{\pi}^{-}\right)}=\left(5.35\pm 0.21\pm 0.16\right)\%, $where the first uncertainty is statistical and the second systematic. The ratio of branching fractions for the $ {\Lambda}_b^0 $ → D$^{*+}$pπ$^{−}$π$^{−}$ and $ {\Lambda}_b^0 $ → D$^{+}$pπ$^{−}$π$^{−}$ decays is found to be$ \frac{\mathcal{B}\left({\Lambda}_b^0\to {D}^{\ast +}p{\pi}^{-}{\pi}^{-}\right)}{\mathcal{B}\left({\Lambda}_b^0\to {D}^{+}p{\pi}^{-}{\pi}^{-}\right)}\times \left(\mathcal{B}\left({D}^{\ast +}\to {D}^{+}{\pi}^0\right)+\mathcal{B}\left({D}^{\ast +}\to {D}^{+}\gamma \right)\right)=\left(61.3\pm 4.3\pm 4.0\right)\%. $[graphic not available: see fulltext]


RU-C
(489)The SHiP experiment at the proposed CERN SPS Beam Dump Facility
  • C. Ahdida,
  • A. Akmete,
  • R. Albanese,
  • J. Alt,
  • A. Alexandrov
  • +340
  • A. Anokhina,
  • S. Aoki,
  • G. Arduini,
  • E. Atkin,
  • N. Azorskiy,
  • J.J. Back,
  • A. Bagulya,
  • F. Baaltasar Dos Santos,
  • A. Baranov,
  • F. Bardou,
  • G.J. Barker,
  • M. Battistin,
  • J. Bauche,
  • A. Bay,
  • V. Bayliss,
  • G. Bencivenni,
  • A.Y. Berdnikov,
  • Y.A. Berdnikov,
  • M. Bertani,
  • C. Betancourt,
  • I. Bezshyiko,
  • O. Bezshyyko,
  • D. Bick,
  • S. Bieschke,
  • A. Blanco,
  • J. Boehm,
  • M. Bogomilov,
  • I. Boiarska,
  • K. Bondarenko,
  • W.M. Bonivento,
  • J. Borburgh,
  • A. Boyarsky,
  • R. Brenner,
  • D. Breton,
  • A. Brignoli,
  • V. Büscher,
  • A. Buonaura,
  • S. Buontempo,
  • S. Cadeddu,
  • A. Calcaterra,
  • M. Calviani,
  • M. Campanelli,
  • M. Casolino,
  • N. Charitonidis,
  • P. Chau,
  • J. Chauveau,
  • A. Chepurnov,
  • M. Chernyavskiy,
  • K.-Y. Choi,
  • A. Chumakov,
  • P. Ciambrone,
  • V. Cicero,
  • M. Climescu,
  • A. Conaboy,
  • L. Congedo,
  • K. Cornelis,
  • M. Cristinziani,
  • A. Crupano,
  • G.M. Dallavalle,
  • A. Datwyler,
  • N. D'Ambrosio,
  • G. D'Appollonio,
  • R. de Asmundis,
  • J. De Carvalho Saraiva,
  • G. De Lellis,
  • M. de Magistris,
  • A. De Roeck,
  • M. De Serio,
  • D. De Simone,
  • L. Dedenko,
  • P. Dergachev,
  • A. Di Crescenzo,
  • L. Di Giulio,
  • N. Di Marco,
  • C. Dib,
  • H. Dijkstra,
  • V. Dmitrenko,
  • L.A. Dougherty,
  • A. Dolmatov,
  • D. Domenici,
  • S. Donskov,
  • V. Drohan,
  • A. Dubreuil,
  • O. Durhan,
  • M. Ehlert,
  • E. Elikkaya,
  • T. Enik,
  • A. Etenko,
  • F. Fabbri,
  • O. Fedin,
  • F. Fedotovs,
  • G. Felici,
  • M. Ferrillo,
  • M. Ferro-Luzzi,
  • K. Filippov,
  • R.A. Fini,
  • H. Fischer,
  • P. Fonte,
  • C. Franco,
  • M. Fraser,
  • R. Fresa,
  • R. Froeschl,
  • T. Fukuda,
  • G. Galati,
  • J. Gall,
  • L. Gatignon,
  • G. Gavrilov,
  • V. Gentile,
  • B. Goddard,
  • L. Golinka-Bezshyyko,
  • A. Golovatiuk,
  • V. Golovtsov,
  • D. Golubkov,
  • A. Golutvin,
  • P. Gorbounov,
  • D. Gorbunov,
  • S. Gorbunov,
  • V. Gorkavenko,
  • M. Gorshenkov,
  • V. Grachev,
  • A.L. Grandchamp,
  • E. Graverini,
  • J.-L. Grenard,
  • D. Grenier,
  • V. Grichine,
  • N. Gruzinskii,
  • A.M. Guler,
  • Yu. Guz,
  • G.J. Haefeli,
  • C. Hagner,
  • H. Hakobyan,
  • I.W. Harris,
  • E. van Herwijnen,
  • C. Hessler,
  • A. Hollnagel,
  • B. Hosseini,
  • M. Hushchyn,
  • G. Iaselli,
  • A. Iuliano,
  • R. Jacobsson,
  • D. Jokovic,
  • M. Jonker,
  • I. Kadenko,
  • V. Kain,
  • B. Kaiser,
  • C. Kamiscioglu,
  • D. Karpenkov,
  • K. Kershaw,
  • M. Khabibullin,
  • E. Khalikov,
  • G. Khaustov,
  • G. Khoriauli,
  • A. Khotyantsev,
  • Y.G. Kim,
  • V. Kim,
  • N. Kitagawa,
  • J.-W. Ko,
  • K. Kodama,
  • A. Kolesnikov,
  • D.I. Kolev,
  • V. Kolosov,
  • M. Komatsu,
  • A. Kono,
  • N. Konovalova,
  • S. Kormannshaus,
  • I. Korol,
  • I. Korol'ko,
  • A. Korzenev,
  • V. Kostyukhin,
  • E. Koukovini Platia,
  • S. Kovalenko,
  • I. Krasilnikova,
  • Y. Kudenko,
  • E. Kurbatov,
  • P. Kurbatov,
  • V. Kurochka,
  • E. Kuznetsova,
  • H.M. Lacker,
  • M. Lamont,
  • G. Lanfranchi,
  • O. Lantwin,
  • A. Lauria,
  • K.S. Lee,
  • K.Y. Lee,
  • N. Leonardo,
  • J.-M. Lévy,
  • V.P. Loschiavo,
  • L. Lopes,
  • E. Lopez Sola,
  • F. Lyons,
  • V. Lyubovitskij,
  • J. Maalmi,
  • A.-M. Magnan,
  • V. Maleev,
  • A. Malinin,
  • Y. Manabe,
  • A.K. Managadze,
  • M. Manfredi,
  • S. Marsh,
  • A.M. Marshall,
  • A. Mefodev,
  • P. Mermod,
  • A. Miano,
  • S. Mikado,
  • Yu. Mikhaylov,
  • A. Mikulenko,
  • D.A. Milstead,
  • O. Mineev,
  • A. Montanari,
  • M.C. Montesi,
  • K. Morishima,
  • S. Movchan,
  • Y. Muttoni,
  • N. Naganawa,
  • M. Nakamura,
  • T. Nakano,
  • S. Nasybulin,
  • P. Ninin,
  • A. Nishio,
  • B. Obinyakov,
  • S. Ogawa,
  • N. Okateva,
  • J. Osborne,
  • M. Ovchynnikov,
  • N. Owtscharenko,
  • P.H. Owen,
  • P. Pacholek,
  • A. Paoloni,
  • B.D. Park,
  • A. Pastore,
  • M. Patel,
  • D. Pereyma,
  • A. Perillo-Marcone,
  • G.L. Petkov,
  • K. Petridis,
  • A. Petrov,
  • D. Podgrudkov,
  • V. Poliakov,
  • N. Polukhina,
  • J. Prieto Prieto,
  • M. Prokudin,
  • A. Prota,
  • A. Quercia,
  • A. Rademakers,
  • A. Rakai,
  • F. Ratnikov,
  • T. Rawlings,
  • F. Redi,
  • A. Reghunath,
  • S. Ricciardi,
  • M. Rinaldesi,
  • Volodymyr Rodin,
  • Viktor Rodin,
  • P. Robbe,
  • A.B. Rodrigues Cavalcante,
  • T. Roganova,
  • H. Rokujo,
  • G. Rosa,
  • T. Rovelli,
  • O. Ruchayskiy,
  • T. Ruf,
  • V. Samoylenko,
  • V. Samsonov,
  • F. Sanchez Galan,
  • P. Santos Diaz,
  • A. Sanz Ull,
  • A. Saputi,
  • O. Sato,
  • E.S. Savchenko,
  • J.S. Schliwinski,
  • W. Schmidt-Parzefall,
  • M. Schumann,
  • N. Serra,
  • S. Sgobba,
  • O. Shadura,
  • A. Shakin,
  • M. Shaposhnikov,
  • P. Shatalov,
  • T. Shchedrina,
  • L. Shchutska,
  • V. Shevchenko,
  • H. Shibuya,
  • L. Shihora,
  • S. Shirobokov,
  • A. Shustov,
  • S.B. Silverstein,
  • S. Simone,
  • R. Simoniello,
  • M. Skorokhvatov,
  • S. Smirnov,
  • G. Soares,
  • J.Y. Sohn,
  • A. Sokolenko,
  • E. Solodko,
  • N. Starkov,
  • L. Stoel,
  • M.E. Stramaglia,
  • D. Sukhonos,
  • Y. Suzuki,
  • S. Takahashi,
  • J.L. Tastet,
  • P. Teterin,
  • S. Than Naing,
  • I. Timiryasov,
  • V. Tioukov,
  • D. Tommasini,
  • M. Torii,
  • N. Tosi,
  • D. Treille,
  • R. Tsenov,
  • S. Ulin,
  • E. Ursov,
  • A. Ustyuzhanin,
  • Z. Uteshev,
  • L. Uvarov,
  • G. Vankova-Kirilova,
  • F. Vannucci,
  • P. Venkova,
  • V. Venturi,
  • I. Vidulin,
  • S. Vilchinski,
  • Heinz Vincke,
  • Helmut Vincke,
  • C. Visone,
  • K. Vlasik,
  • A. Volkov,
  • R. Voronkov,
  • S. van Waasen,
  • R. Wanke,
  • P. Wertelaers,
  • O. Williams,
  • J.-K. Woo,
  • M. Wurm,
  • S. Xella,
  • D. Yilmaz,
  • A.U. Yilmazer,
  • C.S. Yoon,
  • Yu. Zaytsev,
  • A. Zelenov,
  • J. Zimmerman
  • (less)
abstract + abstract -

The Search for Hidden Particles (SHiP) Collaboration has proposed a general-purpose experimental facility operating in beam-dump mode at the CERN SPS accelerator to search for light, feebly interacting particles. In the baseline configuration, the SHiP experiment incorporates two complementary detectors. The upstream detector is designed for recoil signatures of light dark matter (LDM) scattering and for neutrino physics, in particular with tau neutrinos. It consists of a spectrometer magnet housing a layered detector system with high-density LDM/neutrino target plates, emulsion-film technology and electronic high-precision tracking. The total detector target mass amounts to about eight tonnes. The downstream detector system aims at measuring visible decays of feebly interacting particles to both fully reconstructed final states and to partially reconstructed final states with neutrinos, in a nearly background-free environment. The detector consists of a 50$\mathrm { \,m}$ long decay volume under vacuum followed by a spectrometer and particle identification system with a rectangular acceptance of 5 m in width and 10 m in height. Using the high-intensity beam of 400$\,\mathrm {GeV}$ protons, the experiment aims at profiting from the $4\times 10^{19}$ protons per year that are currently unexploited at the SPS, over a period of 5–10 years. This allows probing dark photons, dark scalars and pseudo-scalars, and heavy neutral leptons with GeV-scale masses in the direct searches at sensitivities that largely exceed those of existing and projected experiments. The sensitivity to light dark matter through scattering reaches well below the dark matter relic density limits in the range from a few ${\mathrm {\,MeV\!/}c^2}$ up to 100 MeV-scale masses, and it will be possible to study tau neutrino interactions with unprecedented statistics. This paper describes the SHiP experiment baseline setup and the detector systems, together with performance results from prototypes in test beams, as it was prepared for the 2020 Update of the European Strategy for Particle Physics. The expected detector performance from simulation is summarised at the end.


CN-1
PhD Thesis
RU-D
(488)Accretion onto black holes across the mass scale.
  • Riccardo Arcodia - Advisor: Kirpal Nandra
Thesis (12/2021) doi:10.5282/edoc.28675
abstract + abstract -

Black holes are amongst the most fascinating concepts both for (astro-) physicists and the public. However, they are not only intriguing objects lurking in the cosmic shadows. Many of the most luminous phenomena, both persistent and transient, that we know in the Universe are somehow related to accretion of matter onto them. Black holes are predicted and inferred to exist in different mass ranges, with two main populations consisting of stellar-mass and supermassive

black holes (SMBHs). [...]


CN-7
RU-A
(487)Symmetry restoration in mean-field approaches
  • J. A. Sheikh,
  • J. Dobaczewski,
  • P. Ring,
  • L. M. Robledo,
  • C. Yannouleas
Journal of Physics G Nuclear Physics (12/2021) doi:10.1088/1361-6471/ac288a
abstract + abstract -

The mean-field approximation based on effective interactions or density functionals plays a pivotal role in the description of finite quantum many-body systems that are too large to be treated by ab initio methods. Some examples are strongly interacting medium and heavy mass atomic nuclei and mesoscopic condensed matter systems. In this approach, the linear Schrödinger equation for the exact many-body wave function is mapped onto a non-linear one-body potential problem. This approximation, not only provides computationally very simple solutions even for systems with many particles, but due to the non-linearity, it also allows for obtaining solutions that break essential symmetries of the system, often connected with phase transitions. In this way, additional correlations are subsumed in the system. However, the mean-field approach suffers from the drawback that the corresponding wave functions do not have sharp quantum numbers and, therefore, many results cannot be compared directly with experimental data. In this article, we discuss general group-theory techniques to restore the broken symmetries, and provide detailed expressions on the restoration of translational, rotational, spin, isospin, parity and gauge symmetries, where the latter corresponds to the restoration of the particle number. In order to avoid the numerical complexity of exact projection techniques, various approximation methods available in the literature are examined. Applications of the projection methods are presented for simple nuclear models, realistic calculations in relatively small configuration spaces, nuclear energy density functional (EDF) theory, as well as in other mesoscopic systems. We also discuss applications of projection techniques to quantum statistics in order to treat the averaging over restricted ensembles with fixed quantum numbers. Further, unresolved problems in the application of the symmetry restoration methods to the EDF theories are highlighted in the present work.


CN-6
(486)Constraints on the CKM angle $\gamma$ from $B^\pm\rightarrow Dh^\pm$ decays using $D\rightarrow h^\pm h^{\prime\mp}\pi^0$ final states
  • Roel Aaij,
  • Ahmed Sameh Wagih Abdelmotteleb,
  • Carlos Abellán Beteta,
  • Fernando Jesus Abudinén,
  • Thomas Ackernley
  • +1010
  • Bernardo Adeva,
  • Marco Adinolfi,
  • Hossein Afsharnia,
  • Christina Agapopoulou,
  • Christine Angela Aidala,
  • Salvatore Aiola,
  • Ziad Ajaltouni,
  • Simon Akar,
  • Johannes Albrecht,
  • Federico Alessio,
  • Michael Alexander,
  • Alejandro Alfonso Albero,
  • Zakariya Aliouche,
  • Georgy Alkhazov,
  • Paula Alvarez Cartelle,
  • Sandra Amato,
  • Jake Lewis Amey,
  • Yasmine Amhis,
  • Liupan An,
  • Lucio Anderlini,
  • N. Andersson,
  • Martin Andersson,
  • Aleksei Andreianov,
  • Mirco Andreotti,
  • Flavio Archilli,
  • Alexander Artamonov,
  • Marina Artuso,
  • Kenenbek Arzymatov,
  • Elie Aslanides,
  • Michele Atzeni,
  • Benjamin Audurier,
  • Sebastian Bachmann,
  • Marie Bachmayer,
  • John Back,
  • Pablo Baladron Rodriguez,
  • Vladislav Balagura,
  • Wander Baldini,
  • Juan Baptista de Souza Leite,
  • Matteo Barbetti,
  • Roger Barlow,
  • Sergey Barsuk,
  • William Barter,
  • Matteo Bartolini,
  • Fedor Baryshnikov,
  • Jan-Marc Basels,
  • S. Bashir,
  • Giovanni Bassi,
  • Baasansuren Batsukh,
  • Alexander Battig,
  • Aurelio Bay,
  • Anja Beck,
  • Maik Becker,
  • Franco Bedeschi,
  • Ignacio Bediaga,
  • Andrew Beiter,
  • Vladislav Belavin,
  • Samuel Belin,
  • Violaine Bellee,
  • Konstantin Belous,
  • Ilia Belov,
  • Ivan Belyaev,
  • Giovanni Bencivenni,
  • Eli Ben-Haim,
  • Alexander Berezhnoy,
  • Roland Bernet,
  • Daniel Berninghoff,
  • Harris Conan Bernstein,
  • Claudia Bertella,
  • Alessandro Bertolin,
  • Christopher Betancourt,
  • Federico Betti,
  • Iaroslava Bezshyiko,
  • Ia. Bezshyiko,
  • Srishti Bhasin,
  • Jihyun Bhom,
  • Lingzhu Bian,
  • Martin Stefan Bieker,
  • Nicolo Vladi Biesuz,
  • Simone Bifani,
  • Pierre Billoir,
  • Alice Biolchini,
  • Matthew Birch,
  • Fionn Caitlin Ros Bishop,
  • Alexander Bitadze,
  • Andrea Bizzeti,
  • Mikkel Bjørn,
  • Michele Piero Blago,
  • Thomas Blake,
  • Frederic Blanc,
  • Steven Blusk,
  • Dana Bobulska,
  • Julian Alexander Boelhauve,
  • Oscar Boente Garcia,
  • Thomas Boettcher,
  • Alexey Boldyrev,
  • Alexander Bondar,
  • Nikolay Bondar,
  • Silvia Borghi,
  • Maxim Borisyak,
  • Martino Borsato,
  • Jozef Tomasz Borsuk,
  • Sonia Amina Bouchiba,
  • Themistocles Bowcock,
  • Alexandre Boyer,
  • Concezio Bozzi,
  • Matthew John Bradley,
  • Svende Braun,
  • Alexandre Brea Rodriguez,
  • Jolanta Brodzicka,
  • Arnau Brossa Gonzalo,
  • Davide Brundu,
  • Annarita Buonaura,
  • Laura Buonincontri,
  • Aodhan Tomas Burke,
  • Christopher Burr,
  • Albert Bursche,
  • Anatoly Butkevich,
  • Jordy Sebastiaan Butter,
  • Jan Buytaert,
  • Wiktor Byczynski,
  • Sandro Cadeddu,
  • Hao Cai,
  • Roberto Calabrese,
  • Lukas Calefice,
  • Stefano Cali,
  • Ryan Calladine,
  • Marta Calvi,
  • Miriam Calvo Gomez,
  • Patricia Camargo Magalhaes,
  • Pierluigi Campana,
  • Angel Fernando Campoverde Quezada,
  • Simone Capelli,
  • Lorenzo Capriotti,
  • Angelo Carbone,
  • Giovanni Carboni,
  • Roberta Cardinale,
  • Alessandro Cardini,
  • Ina Carli,
  • Paolo Carniti,
  • Leon David Carus,
  • Kazuyoshi Carvalho Akiba,
  • Adrian Casais Vidal,
  • Rowina Caspary,
  • Gianluigi Casse,
  • Marco Cattaneo,
  • Giovanni Cavallero,
  • Sara Celani,
  • Jacopo Cerasoli,
  • Daniel Cervenkov,
  • Abbie Jane Chadwick,
  • Matthew George Chapman,
  • Matthew Charles,
  • Philippe Charpentier,
  • Ph. Charpentier,
  • Georgios Chatzikonstantinidis,
  • Carlos Alberto Chavez Barajas,
  • Maximilien Chefdeville,
  • Chen Chen,
  • Shanzhen Chen,
  • Aleksei Chernov,
  • Veronika Chobanova,
  • Serhii Cholak,
  • Marcin Chrzaszcz,
  • Alexsei Chubykin,
  • Vladimir Chulikov,
  • Paolo Ciambrone,
  • Maria Flavia Cicala,
  • Xabier Cid Vidal,
  • Gregory Ciezarek,
  • P.E. L. Clarke,
  • Marco Clemencic,
  • Harry Cliff,
  • Joel Closier,
  • John Leslie Cobbledick,
  • Victor Coco,
  • Joao A.B. Coelho,
  • Julien Cogan,
  • Eric Cogneras,
  • Lucian Cojocariu,
  • Paula Collins,
  • Tommaso Colombo,
  • Liliana Congedo,
  • Andrea Contu,
  • Naomi Cooke,
  • George Coombs,
  • Imanol Corredoira,
  • Gloria Corti,
  • Cayo Mar Costa Sobral,
  • Benjamin Couturier,
  • Daniel Charles Craik,
  • Jana Crkovská,
  • Melissa Maria Cruz Torres,
  • Robert Currie,
  • Cesar Luiz Da Silva,
  • Shakhzod Dadabaev,
  • Lingyun Dai,
  • Elena Dall'Occo,
  • Jeremy Dalseno,
  • Carmelo D'Ambrosio,
  • Anna Danilina,
  • Philippe d'Argent,
  • Aigerim Dashkina,
  • Jonathan Edward Davies,
  • Adam Davis,
  • Oscar De Aguiar Francisco,
  • Kristof De Bruyn,
  • Stefano De Capua,
  • Michel De Cian,
  • Erika De Lucia,
  • Jussara De Miranda,
  • Leandro De Paula,
  • Marilisa De Serio,
  • Dario De Simone,
  • Patrizia De Simone,
  • Fabio De Vellis,
  • Jacco de Vries,
  • Cameron Thomas Dean,
  • Francesco Debernardis,
  • Daniel Decamp,
  • Vlad-George Dedu,
  • Luigi Del Buono,
  • Blaise Delaney,
  • Hans Peter Dembinski,
  • Adam Dendek,
  • Vadym Denysenko,
  • Denis Derkach,
  • Olivier Deschamps,
  • Fabrice Desse,
  • Francesco Dettori,
  • Biplab Dey,
  • Alessandro Di Cicco,
  • Pasquale Di Nezza,
  • Sergey Didenko,
  • Lorena Dieste Maronas,
  • Hans Dijkstra,
  • Vasyl Dobishuk,
  • Chenzhi Dong,
  • Amanda May Donohoe,
  • Francesca Dordei,
  • Alberto dos Reis,
  • Lauren Douglas,
  • Anatoliy Dovbnya,
  • Anthony Gavin Downes,
  • Maciej Wojciech Dudek,
  • Laurent Dufour,
  • Viacheslav Duk,
  • Paolo Durante,
  • John Matthew Durham,
  • Deepanwita Dutta,
  • Agnieszka Dziurda,
  • Alexey Dzyuba,
  • Sajan Easo,
  • Ulrik Egede,
  • Victor Egorychev,
  • Semen Eidelman,
  • Stephan Eisenhardt,
  • Surapat Ek-In,
  • Lars Eklund,
  • Scott Ely,
  • Alexandru Ene,
  • Eliane Epple,
  • Stephan Escher,
  • Jonas Nathanael Eschle,
  • Sevda Esen,
  • Timothy Evans,
  • Lucas Falcao,
  • Yanting Fan,
  • Bo Fang,
  • Stephen Farry,
  • Davide Fazzini,
  • Mauricio Féo,
  • Antonio Fernandez Prieto,
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  • Piera Muzzetto,
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  • Niklas Stefan Nolte,
  • Camille Normand,
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  • Rudolf Oldeman,
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  • C.J. G. Onderwater,
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  • Klaas Ole Padeken,
  • Bhagyashree Pagare,
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  • Joan Ruiz Vidal,
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  • Biagio Saitta,
  • Matteo Salomoni,
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  • Alessandro Scarabotto,
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  • Marian Stahl,
  • Sascha Stahl,
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  • Sheldon Stone,
  • Daria Strekalina,
  • Fidan Suljik,
  • Jiayin Sun,
  • Liang Sun,
  • Yipeng Sun,
  • Peter Svihra,
  • Paul Nathaniel Swallow,
  • Krzysztof Swientek,
  • Adam Szabelski,
  • Tomasz Szumlak,
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  • Kayleigh Anne Thomson,
  • Hanae Tilquin,
  • Vincent Tisserand,
  • Stephane T'Jampens,
  • Mark Tobin,
  • Luca Tomassetti,
  • Xingyu Tong,
  • Diego Torres Machado,
  • Da Yu Tou,
  • Ekaterina Trifonova,
  • Stoyan Miroslavov Trilov,
  • Carina Trippl,
  • Giulia Tuci,
  • Alison Tully,
  • Niels Tuning,
  • Artur Ukleja,
  • Daniel Joachim Unverzagt,
  • Eduard Ursov,
  • Andrii Usachov,
  • Andrey Ustyuzhanin,
  • Ulrich Uwer,
  • Alexander Vagner,
  • Vincenzo Vagnoni,
  • Andrea Valassi,
  • Giovanni Valenti,
  • Nuria Valls Canudas,
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  • Eric van Herwijnen,
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  • Ricardo Vazquez Gomez,
  • Pablo Vazquez Regueiro,
  • Carlos Vázquez Sierra,
  • Stefania Vecchi,
  • Jaap Velthuis,
  • Michele Veltri,
  • Aravindhan Venkateswaran,
  • Michele Veronesi,
  • Mika Vesterinen,
  • Daniel Vieira,
  • Maria Vieites Diaz,
  • Harald Viemann,
  • Xavier Vilasis-Cardona,
  • Eva Vilella Figueras,
  • Andrea Villa,
  • Pascal Vincent,
  • Felicia Carolin Volle,
  • Dorothea Vom Bruch,
  • Alexey Vorobyev,
  • Vitaly Vorobyev,
  • Nikolai Voropaev,
  • Kimberley Vos,
  • Roland Waldi,
  • John Walsh,
  • Chishuai Wang,
  • Jialu Wang,
  • Jianchun Wang,
  • Jianqiao Wang,
  • Jike Wang,
  • Mengzhen Wang,
  • Rui Wang,
  • Yilong Wang,
  • Zhenzi Wang,
  • Zirui Wang,
  • Ziyi Wang,
  • Jake Alexander Ward,
  • Nigel Watson,
  • Steffen Georg Weber,
  • David Websdale,
  • Constantin Weisser,
  • Benedict Donald C. Westhenry,
  • Dylan Jaide White,
  • Mark Whitehead,
  • Aidan Richard Wiederhold,
  • Dirk Wiedner,
  • Guy Wilkinson,
  • Michael Kent Wilkinson,
  • Ifan Williams,
  • Mike Williams,
  • Mark Richard James Williams,
  • Fergus Wilson,
  • Wojciech Wislicki,
  • Mariusz Witek,
  • Lukas Witola,
  • Guy Wormser,
  • Stephen Wotton,
  • Hangyi Wu,
  • Kenneth Wyllie,
  • Zhiyu Xiang,
  • Dong Xiao,
  • Yuehong Xie,
  • Ao Xu,
  • Jingyi Xu,
  • Li Xu,
  • Menglin Xu,
  • Qingnian Xu,
  • Zehua Xu,
  • Zhihao Xu,
  • Di Yang,
  • Shuangli Yang,
  • Youhua Yang,
  • Zhenwei Yang,
  • Zishuo Yang,
  • Yuezhe Yao,
  • Lauren Emma Yeomans,
  • Hang Yin,
  • Jiesheng Yu,
  • Xuhao Yuan,
  • Oleg Yushchenko,
  • Ettore Zaffaroni,
  • Mikhail Zavertyaev,
  • Milosz Zdybal,
  • Oleksandr Zenaiev,
  • Ming Zeng,
  • Dongliang Zhang,
  • Liming Zhang,
  • Shulei Zhang,
  • Shunan Zhang,
  • Yanxi Zhang,
  • Yu Zhang,
  • Alina Zharkova,
  • Alexey Zhelezov,
  • Yangheng Zheng,
  • Tianwen Zhou,
  • Xiaokang Zhou,
  • Yixiong Zhou,
  • Valeriia Zhovkovska,
  • Xianglei Zhu,
  • Xiaoyu Zhu,
  • Zhanwen Zhu,
  • Valery Zhukov,
  • Jennifer Brigitta Zonneveld,
  • Quan Zou,
  • Stefano Zucchelli,
  • Davide Zuliani,
  • Gianluca Zunica
  • (less)
abstract + abstract -

A data sample collected with the LHCb detector corresponding to an integrated luminosity of 9 fb$^{-1}$ is used to measure eleven $CP$ violation observables in $B^\pm\to Dh^\pm$ decays, where $h$ is either a kaon or a pion. The neutral $D$ meson decay is reconstructed in the three-body final states: $K^\pm\pi^\mp\pi^0$; $\pi^+\pi^-\pi^0$; $K^+K^-\pi^0$ and the suppressed $\pi^\pm K^\mp\pi^0$ combination. The mode where a large $CP$ asymmetry is expected, $B^\pm\to [\pi^\pm K^\mp\pi^0]_DK^\pm$, is observed with a significance greater than seven standard deviations. The ratio of the partial width of this mode relative to that of the favoured mode, $B^\pm\to [K^\pm\pi^\mp\pi^0]_D K^\pm$, is $R_{{\rm ADS}(K)} = (1.27\pm0.16\pm0.02)\times 10^{-2}$. Evidence for a large $CP$ asymmetry is also seen: $A_{{\rm ADS}(K)} = -0.38\pm0.12\pm0.02$. Constraints on the CKM angle $\gamma$ are calculated from the eleven reported observables.


(485)Three-Loop Gluon Scattering in QCD and the Gluon Regge Trajectory
  • Fabrizio Caola,
  • Amlan Chakraborty,
  • Giulio Gambuti,
  • Andreas von Manteuffel,
  • Lorenzo Tancredi
abstract + abstract -

We compute the three-loop helicity amplitudes for the scattering of four gluons in QCD. We employ projectors in the ’t Hooft-Veltman scheme and construct the amplitudes from a minimal set of physical building blocks, which allows us to keep the computational complexity under control. We obtain relatively compact results that can be expressed in terms of harmonic polylogarithms. In addition, we consider the Regge limit of our amplitude and extract the gluon Regge trajectory in full three-loop QCD. This is the last missing ingredient required for studying single-Reggeon exchanges at next-to-next-to-leading logarithmic accuracy.


(484)CLMM: a LSST-DESC cluster weak lensing mass modeling library for cosmology
  • M. Aguena,
  • C. Avestruz,
  • C. Combet,
  • S. Fu,
  • R. Herbonnet
  • +20
  • A. I. Malz,
  • M. Penna-Lima,
  • M. Ricci,
  • S. D. P. Vitenti,
  • L. Baumont,
  • H. Fan,
  • M. Fong,
  • M. Ho,
  • M. Kirby,
  • C. Payerne,
  • D. Boutigny,
  • B. Lee,
  • B. Liu,
  • T. McClintock,
  • H. Miyatake,
  • C. Sifón,
  • A. von der Linden,
  • H. Wu,
  • M. Yoon,
  • LSST Dark Energy Science Collaboration
  • (less)
Monthly Notices of the Royal Astronomical Society (12/2021) doi:10.1093/mnras/stab2764
abstract + abstract -

We present the v1.0 release of CLMM, an open source PYTHON library for the estimation of the weak lensing masses of clusters of galaxies. CLMM is designed as a stand-alone toolkit of building blocks to enable end-to-end analysis pipeline validation for upcoming cluster cosmology analyses such as the ones that will be performed by the Vera C. Rubin Legacy Survey of Space and Time-Dark Energy Science Collaboration (LSST-DESC). Its purpose is to serve as a flexible, easy-to-install, and easy-to-use interface for both weak lensing simulators and observers and can be applied to real and mock data to study the systematics affecting weak lensing mass reconstruction. At the core of CLMM are routines to model the weak lensing shear signal given the underlying mass distribution of galaxy clusters and a set of data operations to prepare the corresponding data vectors. The theoretical predictions rely on existing software, used as backends in the code, that have been thoroughly tested and cross-checked. Combined theoretical predictions and data can be used to constrain the mass distribution of galaxy clusters as demonstrated in a suite of example Jupyter Notebooks shipped with the software and also available in the extensive online documentation.


(483)Quantum probing of null singularities
  • Ivo Sachs,
  • Marc Schneider,
  • Maximilian Urban
Physical Review D (12/2021) doi:10.1103/PhysRevD.104.125020
abstract + abstract -

We adapt the dual-null foliation to the functional Schrödinger representation of quantum field theory and study the behavior of quantum probes in plane-wave space-times near the null singularity. A comparison between the Einstein-Rosen and the Brinkmann patch, where the latter extends beyond the first, shows a seeming tension that can be resolved by comparing the configuration spaces. Our analysis concludes that Einstein-Rosen space-times support exclusively configurations with nonempty gravitational memory that are focused to a set of measure zero in the focal plane with respect to a Brinkmann observer. To conclude, we provide a rough framework to estimate the qualitative influence of backreactions on these results.


CN-7
RU-A
(482)Charge radii in covariant density functional theory: A global view
  • U. C. Perera,
  • A. V. Afanasjev,
  • P. Ring
Physical Review C (12/2021) doi:10.1103/PhysRevC.104.064313
abstract + abstract -

A systematic global investigation of differential charge radii has been performed within the CDFT framework for the first time. Theoretical results obtained with conventional covariant energy density functionals and the separable pairing interaction of Tian et al. [Phys. Lett. B 676, 44 (2009), 10.1016/j.physletb.2009.04.067] are compared with experimental differential charge radii in the regions of the nuclear chart in which available experimental data crosses the neutron shell closures at N =28 ,50 ,82 , and 126. The analysis of absolute differential radii of different isotopic chains and their relative properties indicate clearly that such properties are reasonably well described in model calculations in the cases when the mean-field approximation is justified. However, while the observed clusterization of differential charge radii of different isotopic chains is well described above the N =50 and N =126 shell closures, it is more difficult to reproduce it above the N =28 and N =82 shell closures because of possible deficiencies in the underlying single-particle structure. The impact of the latter has been evaluated for spherical shapes and it was shown that the relative energies of the single-particle states and the patterns of their occupation with increasing neutron number have an appreciable impact on the evolution of the δ «r2»N ,N' values. These factors also limit the predictive power of model calculations in the regions of high densities of the single-particle states of different origin. It is shown that the kinks in the charge radii at neutron shell closures are due to the underlying single-particle structure and due to weakening or collapse of pairing at these closures. The regions of the nuclear chart in which the correlations beyond mean field are expected to have an impact on charge radii are indicated; the analysis shows that the assignment of a calculated excited prolate minimum to the experimental ground state allows us to understand the trends of the evolution of differential charge radii with neutron number in many cases of shape coexistence even at the mean-field level. It is usually assumed that pairing is a dominant contributor to odd-even staggering (OES) in charge radii. Our analysis paints a more complicated picture. It suggests a new mechanism in which the fragmentation of the single-particle content of the ground state in odd-mass nuclei due to particle-vibration coupling provides a significant contribution to OES in charge radii.


CN-5
(481)The angular momentum structure of CR-driven galactic outflows triggered by stream accretion
  • N. Peschken,
  • M. Hanasz,
  • T. Naab,
  • D. Wóltański,
  • A. Gawryszczak
Monthly Notices of the Royal Astronomical Society (12/2021) doi:10.1093/mnras/stab2784
abstract + abstract -

We investigate the impact of gas accretion in streams on the evolution of disc galaxies, using magnetohydrodynamic simulations including advection and anisotropic diffusion of cosmic rays (CRs) generated by supernovae as the only source of feedback. Stream accretion has been suggested as an important galaxy growth mechanism in cosmological simulations and we vary their orientation and angular momentum in idealized setups. We find that accretion streams trigger the formation of galactic rings and enhanced star formation. The star formation rates and consequently the CR-driven outflow rates are higher for low angular momentum accretion streams, which also result in more compact, lower angular momentum discs. The CR generated outflows show a characteristic structure. At low outflow velocities (<50 km s-1), the angular momentum distribution is similar to the disc and the gas is in a fountain flow. Gas at high outflow velocities (>200 km s-1), penetrating deep into the halo, has close to zero angular momentum, and originates from the centre of the galaxies. As the mass loading factors of the CR-driven outflows are of the order of unity and higher, we conclude that this process is important for the removal of low angular momentum gas from evolving disc galaxies and the transport of, potentially metal enriched, material from galactic centres far into the galactic haloes.


(480)Interplanetary Dust as a Foreground for the LiteBIRD CMB Satellite Mission
  • Ken Ganga,
  • Michele Maris,
  • Mathieu Remazeilles,
  • LiteBIRD Collaboration
The Open Journal of Astrophysics (12/2021) doi:10.21105/astro.2110.13856
abstract + abstract -

As ever-more sensitive experiments are made in the quest for primordial CMB B Modes, the number of potentially significant astrophysical contaminants becomes larger as well. Thermal emission from interplanetary dust, for example, has been detected by the Planck satellite. While the polarization fraction of this Zodiacal, or interplanetary dust emission (IPDE) is expected to be low, it is bright enough to be detected in total power. Here, estimates of the magnitude of the effect as it might be seen by the LiteBIRD satellite are made. The COBE IPDE model from Kelsall et al. (1998) is combined with a model of the LiteBIRD experiment's scanning strategy to estimate potential contamination of the CMB in both total power and in polarization power spectra. LiteBIRD should detect IPDE in temperature across all of its bands, from 40 through 402 GHz, and should improve limits on the polarization fraction of IPDE at the higher end of this frequency range. If the polarization fraction of IPDE is of order 1%, the current limit from ISO/CAM measurements in the mid-infrared, it may induce large-scale polarization B Modes comparable to cosmological models with an r of order 0.001. In this case, the polarized IPDE would also need to be modeled and removed. As a CMB foreground, IPDE will always be subdominant to Galactic emissions, though because it caused by emission from grains closer to us, it appears variable as the Earth travels around the Sun, and may thereby complicate the data analysis somewhat. But with an understanding of some of the symmetries of the emission and some flexibility in the data processing, it should not be the primary impediment to the CMB polarization measurement.


CN-2
RU-D
(479)The dispersal of protoplanetary discs - III. Influence of stellar mass on disc photoevaporation
  • Giovanni Picogna,
  • Barbara Ercolano,
  • Catherine C. Espaillat
Monthly Notices of the Royal Astronomical Society (12/2021) doi:10.1093/mnras/stab2883
abstract + abstract -

The strong X-ray irradiation from young solar-type stars may play a crucial role in the thermodynamics and chemistry of circumstellar discs, driving their evolution in the last stages of disc dispersal as well as shaping the atmospheres of newborn planets. In this paper, we study the influence of stellar mass on circumstellar disc mass-loss rates due to X-ray irradiation, extending our previous study of the mass-loss rate's dependence on the X-ray luminosity and spectrum hardness. We focus on stars with masses between 0.1 and 1 M, which are the main target of current and future missions to find potentially habitable planets. We find a linear relationship between the mass-loss rates and the stellar masses when changing the X-ray luminosity accordingly with the stellar mass. This linear increase is observed also when the X-ray luminosity is kept fixed because of the lower disc aspect ratio which allows the X-ray irradiation to reach larger radii. We provide new analytical relations for the mass-loss rates and profiles of photoevaporative winds as a function of the stellar mass that can be used in disc and planet population synthesis models. Our photoevaporative models correctly predict the observed trend of inner-disc lifetime as a function of stellar mass with an increased steepness for stars smaller than 0.3 M, indicating that X-ray photoevaporation is a good candidate to explain the observed disc dispersal process.


CN-2
RU-D
(478)The dispersal of protoplanetary discs - II: photoevaporation models with observationally derived irradiating spectra
  • Barbara Ercolano,
  • Giovanni Picogna,
  • Kristina Monsch,
  • Jeremy J. Drake,
  • Thomas Preibisch
Monthly Notices of the Royal Astronomical Society (12/2021) doi:10.1093/mnras/stab2590
abstract + abstract -

Young solar-type stars are known to be strong X-ray emitters and their X-ray spectra have been widely studied. X-rays from the central star may play a crucial role in the thermodynamics and chemistry of the circumstellar material as well as in the atmospheric evolution of young planets. In this paper, we present model spectra based on spectral parameters derived from the observations of young stars in the Orion nebula cluster from the Chandra Orion Ultradeep Project (COUP). The spectra are then used to calculate new photoevaporation prescriptions that can be used in disc and planet population synthesis models. Our models clearly show that disc wind mass loss rates are controlled by the stellar luminosity in the soft ($100\, \mathrm{eV}$ to $1\, \mathrm{keV}$) X-ray band. New analytical relations are provided for the mass loss rates and profiles of photoevaporative winds as a function of the luminosity in the soft X-ray band. The agreement between observed and predicted transition disc statistics moderately improved using the new spectra, but the observed population of strongly accreting large cavity discs can still not be reproduced by these models. Furthermore, our models predict a population of non-accreting transition discs that are not observed. This highlights the importance of considering the depletion of millimetre-sized dust grains from the outer disc, which is a likely reason why such discs have not been detected yet.


CN-2
RU-E
(477)From amino acid mixtures to peptides in liquid sulphur dioxide on early Earth
  • Fabian Sauer,
  • Maren Haas,
  • Constanze Sydow,
  • Alexander F. Siegle,
  • Christoph A. Lauer
  • +1
Nature Communications (12/2021) doi:10.1038/s41467-021-27527-7
abstract + abstract -

The formation of peptide bonds is one of the most important biochemical reaction steps. Without the development of structurally and catalytically active polymers, there would be no life on our planet. However, the formation of large, complex oligomer systems is prevented by the high thermodynamic barrier of peptide condensation in aqueous solution. Liquid sulphur dioxide proves to be a superior alternative for copper-catalyzed peptide condensations. Compared to water, amino acids are activated in sulphur dioxide, leading to the incorporation of all 20 proteinogenic amino acids into proteins. Strikingly, even extremely low initial reactant concentrations of only 50 mM are sufficient for extensive peptide formation, yielding up to 2.9% of dialanine in 7 days. The reactions carried out at room temperature and the successful use of the Hadean mineral covellite (CuS) as a catalyst, suggest a volcanic environment for the formation of the peptide world on early Earth.


RU-A
(476)BSM master formula for ε'/ε in the WET basis at NLO in QCD
  • Jason Aebischer,
  • Christoph Bobeth,
  • Andrzej J. Buras,
  • Jacky Kumar
Journal of High Energy Physics (12/2021) doi:10.1007/JHEP12(2021)043
abstract + abstract -

As an important step towards a complete next-to-leading (NLO) QCD analysis of the ratio ε'/ε within the Standard Model Effective Field Theory (SMEFT), we present for the first time the NLO master formula for the BSM part of this ratio expressed in terms of the Wilson coefficients of all contributing operators evaluated at the electroweak scale. To this end we use the common Weak Effective Theory (WET) basis (the so-called JMS basis) for which tree-level and one-loop matching to the SMEFT are already known. The relevant hadronic matrix elements of BSM operators at the electroweak scale are taken from Dual QCD approach and the SM ones from lattice QCD. It includes the renormalization group evolution and quark-flavour threshold effects at NLO in QCD from hadronic scales, at which these matrix elements have been calculated, to the electroweak scale.


CN-3
RU-D
(475)Rotation Curves in z 1-2 Star-forming Disks: Comparison of Dark Matter Fractions and Disk Properties for Different Fitting Methods
  • S. H. Price,
  • T. T. Shimizu,
  • R. Genzel,
  • H. Übler,
  • N. M. Förster Schreiber
  • +20
  • L. J. Tacconi,
  • R. I. Davies,
  • R. T. Coogan,
  • D. Lutz,
  • S. Wuyts,
  • E. Wisnioski,
  • A. Nestor,
  • A. Sternberg,
  • A. Burkert,
  • R. Bender,
  • A. Contursi,
  • R. L. Davies,
  • R. Herrera-Camus,
  • M. -J. Lee,
  • T. Naab,
  • R. Neri,
  • A. Renzini,
  • R. Saglia,
  • A. Schruba,
  • K. Schuster
  • (less)
The Astrophysical Journal (12/2021) doi:10.3847/1538-4357/ac22ad
abstract + abstract -

We present a follow-up analysis examining the dynamics and structures of 41 massive, large star-forming galaxies at z ~ 0.67 - 2.45 using both ionized and molecular gas kinematics. We fit the galaxy dynamics with models consisting of a bulge, a thick, turbulent disk, and an NFW dark matter halo, using code that fully forward-models the kinematics, including all observational and instrumental effects. We explore the parameter space using Markov Chain Monte Carlo (MCMC) sampling, including priors based on stellar and gas masses and disk sizes. We fit the full sample using extracted 1D kinematic profiles. For a subset of 14 well-resolved galaxies, we also fit the 2D kinematics. The MCMC approach robustly confirms the results from least-squares fitting presented in Paper I: the sample galaxies tend to be baryon-rich on galactic scales (within one effective radius). The 1D and 2D MCMC results are also in good agreement for the subset, demonstrating that much of the galaxy dynamical information is captured along the major axis. The 2D kinematics are more affected by the presence of noncircular motions, which we illustrate by constructing a toy model with constant inflow for one galaxy that exhibits residual signatures consistent with radial motions. This analysis, together with results from Paper I and other studies, strengthens the finding that massive, star-forming galaxies at z ~ 1 - 2 are baryon-dominated on galactic scales, with lower dark matter fractions toward higher baryonic surface densities. Finally, we present details of the kinematic fitting code used in this analysis.


MIAPbP
(474)Mass-ratio and Magnetic Flux Dependence of Modulated Accretion from Circumbinary Disks
  • Scott C. Noble,
  • Julian H. Krolik,
  • Manuela Campanelli,
  • Yosef Zlochower,
  • Bruno C. Mundim
  • +2
  • Hiroyuki Nakano,
  • Miguel Zilhão
  • (less)
The Astrophysical Journal (12/2021) doi:10.3847/1538-4357/ac2229
abstract + abstract -

Accreting supermassive binary black holes (SMBBHs) are potential multimessenger sources because they emit both gravitational-wave and electromagnetic (EM) radiation. Past work has shown that their EM output may be periodically modulated by an asymmetric density distribution in the circumbinary disk, often called an "overdensity" or "lump;" this modulation could possibly be used to identify a source as a binary. We explore the sensitivity of the overdensity to SMBBH mass ratio and magnetic flux through the accretion disk. We find that the relative amplitude of the overdensity and its associated EM periodic signal both degrade with diminishing mass ratio, vanishing altogether somewhere between 1:2 and 1:5. Greater magnetization also weakens the lump and any modulation of the light output. We develop a model to describe how lump formation results from internal stress degrading faster in the lump region than it can be rejuvenated through accretion inflow, and predicts a threshold value in specific internal stress below which lump formation should occur and which all our lump-forming simulations satisfy. Thus, detection of such a modulation would provide a constraint on both mass ratio and magnetic flux piercing the accretion flow.


RU-D
(473)The formation of wide exoKuiper belts from migrating dust traps
  • E. Miller,
  • S. Marino,
  • S. M. Stammler,
  • P. Pinilla,
  • C. Lenz
  • +2
Monthly Notices of the Royal Astronomical Society (12/2021) doi:10.1093/mnras/stab2935
abstract + abstract -

The question of what determines the width of Kuiper belt analogues (exoKuiper belts) is an open one. If solved, this understanding would provide valuable insights into the architecture, dynamics, and formation of exoplanetary systems. Recent observations by ALMA have revealed an apparent paradox in this field, the presence of radially narrow belts in protoplanetary discs that are likely the birthplaces of planetesimals, and exoKuiper belts nearly four times as wide in mature systems. If the parent planetesimals of this type of debris disc indeed form in these narrow protoplanetary rings via streaming instability where dust is trapped, we propose that this width dichotomy could naturally arise if these dust traps form planetesimals whilst migrating radially, e.g. as caused by a migrating planet. Using the dust evolution software DUSTPY, we find that if the initial protoplanetary disc and trap conditions favour planetesimal formation, dust can still effectively accumulate and form planetesimals as the trap moves. This leads to a positive correlation between the inward radial speed and final planetesimal belt width, forming belts up to ~100AU over 10 Myr of evolution. We show that although planetesimal formation is most efficient in low-viscosity (α = 10-4) discs with steep dust traps to trigger the streaming instability, the large widths of most observed planetesimal belts constrain α to values ≥4 × 10-4 at tens of AU, otherwise the traps cannot migrate far enough. Additionally, the large spread in the widths and radii of exoKuiper belts could be due to different trap migration speeds (or protoplanetary disc lifetimes) and different starting locations, respectively. Our work serves as a first step to link exoKuiper belts and rings in protoplanetary discs.


CN-3
RU-C
(472)Two-loop bispectrum of large-scale structure
  • Tobias Baldauf,
  • Mathias Garny,
  • Petter Taule,
  • Theo Steele
Physical Review D (12/2021) doi:10.1103/PhysRevD.104.123551
abstract + abstract -

The bispectrum is the leading non-Gaussian statistic in large-scale structure, carrying valuable information on cosmology that is complementary to the power spectrum. To access this information, we need to model the bispectrum in the weakly nonlinear regime. In this work we present the first two-loop, i.e. next-to-next-to-leading order perturbative description of the bispectrum within an effective field theory (EFT) framework. Using an analytic expansion of the perturbative kernels up to F6 we derive a renormalized bispectrum that is demonstrated to be independent of the UV cutoff. We show that the EFT parameters associated with the four independent second-order EFT operators known from the one-loop bispectrum are sufficient to absorb the UV sensitivity of the two-loop contributions in the double-hard region. In addition, we employ a simplified treatment of the single-hard region, introducing one extra EFT parameter at two-loop order. We compare our results to N -body simulations using the realization-based grid perturbation theory method and find good agreement within the expected range, as well as consistent values for the EFT parameters. The two-loop terms start to become relevant at k ≈0.07 h Mpc-1. The range of wave numbers with percent-level agreement, independently of the shape, extends from 0.08 to 0.15 h Mpc-1 when going from one to two loops at z =0 . In addition, we quantify the impact of using exact instead of Einstein-de-Sitter kernels for the one-loop bispectrum, and discuss in how far their impact can be absorbed into a shift of the EFT parameters.