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(920)Calorimeter calibration of the ComPol CubeSat gamma-ray polarimeter
  • Ion Cojocari,
  • Matthias Meier,
  • Philippe Laurent,
  • Adrien Laviron,
  • Marco Arrigucci
  • +16
  • Marco Carminati,
  • Griseld Deda,
  • Carlo Fiorini,
  • Katrin Geigenberger,
  • Cynthia Glas,
  • Jochen Greiner,
  • Peter Hindenberger,
  • Pietro King,
  • Peter Lechner,
  • Martin Losekamm,
  • Susanne Mertens,
  • David Meßmann,
  • Sebastian Rückerl,
  • Lorenzo Toscano,
  • Ulrich Walter,
  • Michael Willers
  • (less)
Nucl.Instrum.Meth.A (2023) doi:10.1016/j.nima.2022.167662
abstract + abstract -

ComPol is a proposed CubeSat mission dedicated to long-term study of gamma-ray polarisation of astrophysical objects. Besides spectral and timing measurements, polarisation analysis can be a powerful tool in constraining current models of the geometry, magnetic field structure and acceleration mechanisms of different astrophysical sources. The ComPol payload is a Compton telescope optimised for polarimetry and consists of a 2 layer stacked detector configuration. The top layer, the scatterer, is a Silicon Drift Detector matrix developed by the Max Planck Institute for Physics and Politecnico di Milano. The second layer is a calorimeter consisting of a CeBr<math display="inline" id="d1e778" altimg="si10.svg"><msub><mrow/><mrow><mn>3</mn></mrow></msub></math> scintillator read-out by silicon photo-multipliers developed at CEA Saclay. This paper presents the results of the prototype calorimeter calibration campaign, executed in March 2022 at IJCLab Orsay and simulations of the expected performance of the polarimeter using updated performance figures of the detectors.


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(919)Low Energy Event Reconstruction in IceCube DeepCore
  • R. Abbasi,
  • M. Ackermann,
  • J. Adams,
  • J. A. Aguilar,
  • M. Ahlers
  • +380
  • M. Ahrens,
  • J.M. Alameddine,
  • A. A. Alves Jr.,
  • N. M. Amin,
  • K. Andeen,
  • T. Anderson,
  • G. Anton,
  • C. Argüelles,
  • Y. Ashida,
  • S. Axani,
  • X. Bai,
  • A. Balagopal V.,
  • S. W. Barwick,
  • B. Bastian,
  • V. Basu,
  • S. Baur,
  • R. Bay,
  • J. J. Beatty,
  • K.-H. Becker,
  • J. Becker Tjus,
  • J. Beise,
  • C. Bellenghi,
  • S. Benda,
  • S. BenZvi,
  • D. Berley,
  • E. Bernardini,
  • D. Z. Besson,
  • G. Binder,
  • D. Bindig,
  • E. Blaufuss,
  • S. Blot,
  • M. Boddenberg,
  • F. Bontempo,
  • J. Y. Book,
  • J. Borowka,
  • S. Böser,
  • O. Botner,
  • J. Böttcher,
  • E. Bourbeau,
  • F. Bradascio,
  • J. Braun,
  • B. Brinson,
  • S. Bron,
  • J. Brostean-Kaiser,
  • R. T. Burley,
  • R. S. Busse,
  • M. A. Campana,
  • E. G. Carnie-Bronca,
  • C. Chen,
  • Z. Chen,
  • D. Chirkin,
  • K. Choi,
  • B. A. Clark,
  • K. Clark,
  • L. Classen,
  • A. Coleman,
  • G. H. Collin,
  • J. M. Conrad,
  • P. Coppin,
  • P. Correa,
  • D. F. Cowen,
  • R. Cross,
  • C. Dappen,
  • P. Dave,
  • C. De Clercq,
  • J. J. DeLaunay,
  • D. Delgado López,
  • H. Dembinski,
  • K. Deoskar,
  • A. Desai,
  • P. Desiati,
  • K. D. de Vries,
  • G. de Wasseige,
  • M. de With,
  • T. DeYoung,
  • A. Diaz,
  • J. C. Díaz-Vélez,
  • M. Dittmer,
  • H. Dujmovic,
  • M. Dunkman,
  • M. A. DuVernois,
  • T. Ehrhardt,
  • P. Eller,
  • R. Engel,
  • H. Erpenbeck,
  • J. Evans,
  • P. A. Evenson,
  • K. L. Fan,
  • A. R. Fazely,
  • A. Fedynitch,
  • N. Feigl,
  • S. Fiedlschuster,
  • A. T. Fienberg,
  • C. Finley,
  • L. Fischer,
  • D. Fox,
  • A. Franckowiak,
  • E. Friedman,
  • A. Fritz,
  • P. Fürst,
  • T. K. Gaisser,
  • J. Gallagher,
  • E. Ganster,
  • A. Garcia,
  • S. Garrappa,
  • L. Gerhardt,
  • A. Ghadimi,
  • C. Glaser,
  • T. Glauch,
  • T. Glüsenkamp,
  • N. Goehlke,
  • J. G. Gonzalez,
  • S. Goswami,
  • D. Grant,
  • T. Grégoire,
  • S. Griswold,
  • C. Günther,
  • P. Gutjahr,
  • C. Haack,
  • A. Hallgren,
  • R. Halliday,
  • L. Halve,
  • F. Halzen,
  • M. Ha Minh,
  • K. Hanson,
  • J. Hardin,
  • A. A. Harnisch,
  • A. Haungs,
  • D. Hebecker,
  • K. Helbing,
  • F. Henningsen,
  • E. C. Hettinger,
  • S. Hickford,
  • J. Hignight,
  • C. Hill,
  • G. C. Hill,
  • K. D. Hoffman,
  • R. Hoffmann,
  • K. Hoshina,
  • W. Hou,
  • F. Huang,
  • M. Huber,
  • T. Huber,
  • K. Hultqvist,
  • M. Hünnefeld,
  • R. Hussain,
  • K. Hymon,
  • S. In,
  • N. Iovine,
  • A. Ishihara,
  • M. Jansson,
  • G. S. Japaridze,
  • M. Jeong,
  • M. Jin,
  • B. J. P. Jones,
  • D. Kang,
  • W. Kang,
  • X. Kang,
  • A. Kappes,
  • D. Kappesser,
  • L. Kardum,
  • T. Karg,
  • M. Karl,
  • A. Karle,
  • U. Katz,
  • M. Kauer,
  • M. Kellermann,
  • J. L. Kelley,
  • A. Kheirandish,
  • K. Kin,
  • T. Kintscher,
  • J. Kiryluk,
  • S. R. Klein,
  • A. Kochocki,
  • R. Koirala,
  • H. Kolanoski,
  • T. Kontrimas,
  • L. Köpke,
  • C. Kopper,
  • S. Kopper,
  • D. J. Koskinen,
  • P. Koundal,
  • M. Kovacevich,
  • M. Kowalski,
  • T. Kozynets,
  • E. Krupczak,
  • E. Kun,
  • N. Kurahashi,
  • N. Lad,
  • C. Lagunas Gualda,
  • J. L. Lanfranchi,
  • M. J. Larson,
  • F. Lauber,
  • J. P. Lazar,
  • J. W. Lee,
  • K. Leonard,
  • A. Leszczyńska,
  • Y. Li,
  • M. Lincetto,
  • Q. R. Liu,
  • M. Liubarska,
  • E. Lohfink,
  • C. J. Lozano Mariscal,
  • L. Lu,
  • F. Lucarelli,
  • A. Ludwig,
  • W. Luszczak,
  • Y. Lyu,
  • W. Y. Ma,
  • J. Madsen,
  • K. B. M. Mahn,
  • Y. Makino,
  • S. Mancina,
  • I. C. Mari{ş},
  • I. Martinez-Soler,
  • R. Maruyama,
  • S. McCarthy,
  • T. McElroy,
  • F. McNally,
  • J. V. Mead,
  • K. Meagher,
  • S. Mechbal,
  • A. Medina,
  • M. Meier,
  • S. Meighen-Berger,
  • J. Micallef,
  • D. Mockler,
  • T. Montaruli,
  • R. W. Moore,
  • R. Morse,
  • M. Moulai,
  • T. Mukherjee,
  • R. Naab,
  • R. Nagai,
  • U. Naumann,
  • J. Necker,
  • L. V. Nguy{\~{ê}}n,
  • H. Niederhausen,
  • M. U. Nisa,
  • S. C. Nowicki,
  • A. Obertacke Pollmann,
  • M. Oehler,
  • B. Oeyen,
  • A. Olivas,
  • E. O'Sullivan,
  • H. Pandya,
  • D. V. Pankova,
  • N. Park,
  • G. K. Parker,
  • E. N. Paudel,
  • L. Paul,
  • C. Pérez de los Heros,
  • L. Peters,
  • J. Peterson,
  • S. Philippen,
  • S. Pieper,
  • A. Pizzuto,
  • M. Plum,
  • Y. Popovych,
  • A. Porcelli,
  • M. Prado Rodriguez,
  • B. Pries,
  • G. T. Przybylski,
  • C. Raab,
  • J. Rack-Helleis,
  • A. Raissi,
  • M. Rameez,
  • K. Rawlins,
  • I. C. Rea,
  • Z. Rechav,
  • A. Rehman,
  • P. Reichherzer,
  • R. Reimann,
  • G. Renzi,
  • E. Resconi,
  • S. Reusch,
  • W. Rhode,
  • M. Richman,
  • B. Riedel,
  • E. J. Roberts,
  • S. Robertson,
  • G. Roellinghoff,
  • M. Rongen,
  • C. Rott,
  • T. Ruhe,
  • D. Ryckbosch,
  • D. Rysewyk Cantu,
  • I. Safa,
  • J. Saffer,
  • P. Sampathkumar,
  • S. E. Sanchez Herrera,
  • A. Sandrock,
  • M. Santander,
  • S. Sarkar,
  • S. Sarkar,
  • K. Satalecka,
  • M. Schaufel,
  • H. Schieler,
  • S. Schindler,
  • T. Schmidt,
  • A. Schneider,
  • J. Schneider,
  • F. G. Schröder,
  • L. Schumacher,
  • G. Schwefer,
  • S. Sclafani,
  • D. Seckel,
  • S. Seunarine,
  • A. Sharma,
  • S. Shefali,
  • N. Shimizu,
  • M. Silva,
  • B. Skrzypek,
  • B. Smithers,
  • R. Snihur,
  • J. Soedingrekso,
  • D. Soldin,
  • C. Spannfellner,
  • G. M. Spiczak,
  • C. Spiering,
  • J. Stachurska,
  • M. Stamatikos,
  • T. Stanev,
  • R. Stein,
  • J. Stettner,
  • T. Stezelberger,
  • T. Stürwald,
  • T. Stuttard,
  • G. W. Sullivan,
  • I. Taboada,
  • S. Ter-Antonyan,
  • J. Thwaites,
  • S. Tilav,
  • F. Tischbein,
  • K. Tollefson,
  • C. Tönnis,
  • S. Toscano,
  • D. Tosi,
  • A. Trettin,
  • M. Tselengidou,
  • C. F. Tung,
  • A. Turcati,
  • R. Turcotte,
  • C. F. Turley,
  • J. P. Twagirayezu,
  • B. Ty,
  • M. A. Unland Elorrieta,
  • N. Valtonen-Mattila,
  • J. Vandenbroucke,
  • N. van Eijndhoven,
  • D. Vannerom,
  • J. van Santen,
  • J. Veitch-Michaelis,
  • S. Verpoest,
  • C. Walck,
  • W. Wang,
  • T. B. Watson,
  • C. Weaver,
  • P. Weigel,
  • A. Weindl,
  • M. J. Weiss,
  • J. Weldert,
  • C. Wendt,
  • J. Werthebach,
  • M. Weyrauch,
  • N. Whitehorn,
  • C. H. Wiebusch,
  • N. Willey,
  • D. R. Williams,
  • M. Wolf,
  • G. Wrede,
  • J. Wulff,
  • X. W. Xu,
  • J. P. Yanez,
  • E. Yildizci,
  • S. Yoshida,
  • S. Yu,
  • T. Yuan,
  • Z. Zhang,
  • P. Zhelnin
  • (less)
The European Physical Journal C (September/2022) e-Print:2203.02303 doi:10.1140/epjc/s10052-022-10721-2
abstract + abstract -

The reconstruction of event-level information, such as the direction or energy of a neutrino interacting in IceCube DeepCore, is a crucial ingredient to many physics analyses. Algorithms to extract this high level information from the detector's raw data have been successfully developed and used for high energy events. In this work, we address unique challenges associated with the reconstruction of lower energy events in the range of a few to hundreds of GeV and present two separate, state-of-the-art algorithms. One algorithm focuses on the fast directional reconstruction of events based on unscattered light. The second algorithm is a likelihood-based multipurpose reconstruction offering superior resolutions, at the expense of larger computational cost.


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(918)Online triggers for supernova and pre-supernova neutrino detection with cryogenic detectors
  • Philipp Eller,
  • Nahuel Ferreiro Iachellini,
  • Luca Pattavina,
  • Lolian Shtembari
Journal of Cosmology and Astroparticle Physics (October/2022) e-Print:2205.03350 doi:10.1088/1475-7516/2022/10/024

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(917)Discovering neutrinoless double-beta decay in the era of precision neutrino cosmology
  • Manuel Ettengruber,
  • Matteo Agostini,
  • Allen Caldwell,
  • Philipp Eller,
  • Oliver Schulz
Physical Review (October/2022) e-Print:2208.09954 doi:10.1103/PhysRevD.106.073004
abstract + abstract -

We evaluate the discovery probability of a combined analysis of proposed neutrinoless double-beta decay experiments in a scenario with normal ordered neutrino masses. The discovery probability strongly depends on the value of the lightest neutrino mass, ranging from zero in case of vanishing masses and up to 80-90\% for values just below the current constraints. We study the discovery probability in different scenarios, focusing on the exciting prospect in which cosmological surveys will measure the sum of neutrino masses. Uncertainties in nuclear matrix element calculations partially compensate each other when data from different isotopes are available. Although a discovery is not granted, the theoretical motivations for these searches and the presence of scenarios with high discovery probability strongly motivates the proposed international, multi-isotope experimental program.


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(916)Graph Neural Networks for Low-Energy Event Classification & Reconstruction in IceCube
  • R. Abbasi,
  • M. Ackermann,
  • J. Adams,
  • N. Aggarwal,
  • J. A. Aguilar
  • +379
  • M. Ahlers,
  • M. Ahrens,
  • J.M. Alameddine,
  • A. A. Alves Jr.,
  • N. M. Amin,
  • K. Andeen,
  • T. Anderson,
  • G. Anton,
  • C. Argüelles,
  • Y. Ashida,
  • S. Athanasiadou,
  • S. Axani,
  • X. Bai,
  • A. Balagopal V.,
  • M. Baricevic,
  • S. W. Barwick,
  • V. Basu,
  • R. Bay,
  • J. J. Beatty,
  • K.-H. Becker,
  • J. Becker Tjus,
  • J. Beise,
  • C. Bellenghi,
  • S. Benda,
  • S. BenZvi,
  • D. Berley,
  • E. Bernardini,
  • D. Z. Besson,
  • G. Binder,
  • D. Bindig,
  • E. Blaufuss,
  • S. Blot,
  • F. Bontempo,
  • J. Y. Book,
  • J. Borowka,
  • C. Boscolo Meneguolo,
  • S. Böser,
  • O. Botner,
  • J. Böttcher,
  • E. Bourbeau,
  • J. Braun,
  • B. Brinson,
  • J. Brostean-Kaiser,
  • R. T. Burley,
  • R. S. Busse,
  • M. A. Campana,
  • E. G. Carnie-Bronca,
  • C. Chen,
  • Z. Chen,
  • D. Chirkin,
  • K. Choi,
  • B. A. Clark,
  • L. Classen,
  • A. Coleman,
  • G. H. Collin,
  • A. Connolly,
  • J. M. Conrad,
  • P. Coppin,
  • P. Correa,
  • S. Countryman,
  • D. F. Cowen,
  • R. Cross,
  • C. Dappen,
  • P. Dave,
  • C. De Clercq,
  • J. J. DeLaunay,
  • D. Delgado López,
  • H. Dembinski,
  • K. Deoskar,
  • A. Desai,
  • P. Desiati,
  • K. D. de Vries,
  • G. de Wasseige,
  • T. DeYoung,
  • A. Diaz,
  • J. C. Díaz-Vélez,
  • M. Dittmer,
  • H. Dujmovic,
  • M. A. DuVernois,
  • T. Ehrhardt,
  • P. Eller,
  • R. Engel,
  • H. Erpenbeck,
  • J. Evans,
  • P. A. Evenson,
  • K. L. Fan,
  • A. R. Fazely,
  • A. Fedynitch,
  • N. Feigl,
  • S. Fiedlschuster,
  • A. T. Fienberg,
  • C. Finley,
  • L. Fischer,
  • D. Fox,
  • A. Franckowiak ,
  • E. Friedman,
  • A. Fritz,
  • P. Fürst,
  • T. K. Gaisser,
  • J. Gallagher,
  • E. Ganster,
  • A. Garcia,
  • S. Garrappa,
  • L. Gerhardt,
  • A. Ghadimi,
  • C. Glaser,
  • T. Glauch,
  • T. Glüsenkamp,
  • N. Goehlke,
  • J. G. Gonzalez,
  • S. Goswami,
  • D. Grant,
  • S. J. Gray,
  • T. Grégoire,
  • S. Griswold,
  • C. Günther,
  • P. Gutjahr,
  • C. Haack,
  • A. Hallgren,
  • R. Halliday,
  • L. Halve,
  • F. Halzen,
  • H. Hamdaoui,
  • M. Ha Minh,
  • K. Hanson,
  • J. Hardin,
  • A. A. Harnisch,
  • P. Hatch,
  • A. Haungs,
  • K. Helbing,
  • J. Hellrung,
  • F. Henningsen,
  • L. Heuermann,
  • S. Hickford,
  • C. Hill,
  • G. C. Hill,
  • K. D. Hoffman,
  • K. Hoshina,
  • W. Hou,
  • T. Huber,
  • K. Hultqvist,
  • M. Hünnefeld,
  • R. Hussain,
  • K. Hymon,
  • S. In,
  • N. Iovine,
  • A. Ishihara,
  • M. Jansson,
  • G. S. Japaridze,
  • M. Jeong,
  • M. Jin,
  • B. J. P. Jones,
  • D. Kang,
  • W. Kang,
  • X. Kang,
  • A. Kappes,
  • D. Kappesser,
  • L. Kardum,
  • T. Karg,
  • M. Karl,
  • A. Karle,
  • U. Katz,
  • M. Kauer,
  • J. L. Kelley,
  • A. Kheirandish,
  • K. Kin,
  • J. Kiryluk,
  • S. R. Klein,
  • A. Kochocki,
  • R. Koirala,
  • H. Kolanoski,
  • T. Kontrimas,
  • L. Köpke,
  • C. Kopper,
  • D. J. Koskinen,
  • P. Koundal,
  • M. Kovacevich,
  • M. Kowalski,
  • T. Kozynets,
  • E. Krupczak,
  • E. Kun,
  • N. Kurahashi,
  • N. Lad,
  • C. Lagunas Gualda,
  • M. J. Larson,
  • F. Lauber,
  • J. P. Lazar,
  • J. W. Lee,
  • K. Leonard,
  • A. Leszczyńska,
  • M. Lincetto,
  • Q. R. Liu,
  • M. Liubarska,
  • E. Lohfink,
  • C. Love,
  • C. J. Lozano Mariscal,
  • L. Lu,
  • F. Lucarelli,
  • A. Ludwig,
  • W. Luszczak,
  • Y. Lyu,
  • W. Y. Ma,
  • J. Madsen,
  • K. B. M. Mahn,
  • Y. Makino,
  • S. Mancina,
  • W. Marie Sainte,
  • I. C. Mariş,
  • S. Marka,
  • Z. Marka,
  • M. Marsee,
  • I. Martinez-Soler,
  • R. Maruyama,
  • T. McElroy,
  • F. McNally,
  • J. V. Mead,
  • K. Meagher,
  • S. Mechbal,
  • A. Medina,
  • M. Meier,
  • S. Meighen-Berger,
  • Y. Merckx,
  • J. Micallef,
  • D. Mockler,
  • T. Montaruli,
  • R. W. Moore,
  • R. Morse,
  • M. Moulai,
  • T. Mukherjee,
  • R. Naab,
  • R. Nagai,
  • U. Naumann,
  • A. Nayerhoda,
  • J. Necker,
  • M. Neumann,
  • H. Niederhausen,
  • M. U. Nisa,
  • S. C. Nowicki,
  • A. Obertacke Pollmann,
  • M. Oehler,
  • B. Oeyen,
  • A. Olivas,
  • R. Orsoe,
  • J. Osborn,
  • E. O'Sullivan,
  • H. Pandya,
  • D. V. Pankova,
  • N. Park,
  • G. K. Parker,
  • E. N. Paudel,
  • L. Paul,
  • C. Pérez de los Heros,
  • L. Peters,
  • T. C. Petersen,
  • J. Peterson,
  • S. Philippen,
  • S. Pieper,
  • A. Pizzuto,
  • M. Plum,
  • Y. Popovych,
  • A. Porcelli,
  • M. Prado Rodriguez,
  • B. Pries,
  • R. Procter-Murphy,
  • G. T. Przybylski,
  • C. Raab,
  • J. Rack-Helleis,
  • M. Rameez,
  • K. Rawlins,
  • Z. Rechav,
  • A. Rehman,
  • P. Reichherzer,
  • G. Renzi,
  • E. Resconi,
  • S. Reusch,
  • W. Rhode,
  • M. Richman,
  • B. Riedel,
  • E. J. Roberts,
  • S. Robertson,
  • S. Rodan,
  • G. Roellinghoff,
  • M. Rongen,
  • C. Rott,
  • T. Ruhe,
  • L. Ruohan,
  • D. Ryckbosch,
  • D. Rysewyk Cantu,
  • I. Safa,
  • J. Saffer,
  • D. Salazar-Gallegos,
  • P. Sampathkumar,
  • S. E. Sanchez Herrera,
  • A. Sandrock,
  • M. Santander,
  • S. Sarkar,
  • S. Sarkar,
  • M. Schaufel,
  • H. Schieler,
  • S. Schindler,
  • B. Schlueter,
  • T. Schmidt,
  • J. Schneider,
  • F. G. Schröder,
  • L. Schumacher,
  • G. Schwefer,
  • S. Sclafani,
  • D. Seckel,
  • S. Seunarine,
  • A. Sharma,
  • S. Shefali,
  • N. Shimizu,
  • M. Silva,
  • B. Skrzypek,
  • B. Smithers,
  • R. Snihur,
  • J. Soedingrekso,
  • A. Søgaard,
  • D. Soldin,
  • C. Spannfellner,
  • G. M. Spiczak,
  • C. Spiering,
  • M. Stamatikos,
  • T. Stanev,
  • R. Stein,
  • T. Stezelberger,
  • T. Stürwald,
  • T. Stuttard,
  • G. W. Sullivan,
  • I. Taboada,
  • S. Ter-Antonyan,
  • W. G. Thompson,
  • J. Thwaites,
  • S. Tilav,
  • K. Tollefson,
  • C. Tönnis,
  • S. Toscano,
  • D. Tosi,
  • A. Trettin,
  • C. F. Tung,
  • R. Turcotte,
  • J. P. Twagirayezu,
  • B. Ty,
  • M. A. Unland Elorrieta,
  • K. Upshaw,
  • N. Valtonen-Mattila,
  • J. Vandenbroucke,
  • N. van Eijndhoven,
  • D. Vannerom,
  • J. van Santen,
  • J. Vara,
  • J. Veitch-Michaelis,
  • S. Verpoest,
  • D. Veske,
  • C. Walck,
  • W. Wang,
  • T. B. Watson,
  • C. Weaver,
  • P. Weigel,
  • A. Weindl,
  • J. Weldert,
  • C. Wendt,
  • J. Werthebach,
  • M. Weyrauch,
  • N. Whitehorn,
  • C. H. Wiebusch,
  • N. Willey,
  • D. R. Williams,
  • M. Wolf,
  • G. Wrede,
  • J. Wulff,
  • X. W. Xu,
  • J. P. Yanez,
  • E. Yildizci,
  • S. Yoshida,
  • S. Yu,
  • T. Yuan,
  • Z. Zhang,
  • P. Zhelnin
  • (less)
Journal of Instrumentation (November/2022) e-Print:2209.03042 doi:10.1088/1748-0221/17/11/P11003
abstract + abstract -

IceCube, a cubic-kilometer array of optical sensors built to detect atmospheric and astrophysical neutrinos between 1 GeV and 1 PeV, is deployed 1.45 km to 2.45 km below the surface of the ice sheet at the South Pole. The classification and reconstruction of events from the in-ice detectors play a central role in the analysis of data from IceCube. Reconstructing and classifying events is a challenge due to the irregular detector geometry, inhomogeneous scattering and absorption of light in the ice and, below 100 GeV, the relatively low number of signal photons produced per event. To address this challenge, it is possible to represent IceCube events as point cloud graphs and use a Graph Neural Network (GNN) as the classification and reconstruction method. The GNN is capable of distinguishing neutrino events from cosmic-ray backgrounds, classifying different neutrino event types, and reconstructing the deposited energy, direction and interaction vertex. Based on simulation, we provide a comparison in the 1-100 GeV energy range to the current state-of-the-art maximum likelihood techniques used in current IceCube analyses, including the effects of known systematic uncertainties. For neutrino event classification, the GNN increases the signal efficiency by 18% at a fixed false positive rate (FPR), compared to current IceCube methods. Alternatively, the GNN offers a reduction of the FPR by over a factor 8 (to below half a percent) at a fixed signal efficiency. For the reconstruction of energy, direction, and interaction vertex, the resolution improves by an average of 13%-20% compared to current maximum likelihood techniques in the energy range of 1-30 GeV. The GNN, when run on a GPU, is capable of processing IceCube events at a rate nearly double of the median IceCube trigger rate of 2.7 kHz, which opens the possibility of using low energy neutrinos in online searches for transient events.


ODSL
RU-B
(915)Fast and precise model calculation for KATRIN using a neural network
  • Christian Karl,
  • Philipp Eller,
  • Susanne Mertens
The European Physical Journal C (May/2022) e-Print:2201.04523 doi:10.1140/epjc/s10052-022-10384-z
abstract + abstract -

We present a fast and precise method to approximate the physics model of the Karlsruhe Tritium Neutrino (KATRIN) experiment using a neural network. KATRIN is designed to measure the effective electron anti-neutrino mass using the kinematics of beta-decay with a sensitivity of 200 meV at 90% confidence level. To achieve this goal, a highly accurate model prediction with relative errors below the 1e-4-level is required. Using the regular numerical model for the analysis of the final KATRIN dataset is computationally extremely costly or requires approximations to decrease the computation time. Our solution to reduce the computational requirements is to train a neural network to learn the predicted beta-spectrum and its dependence on all relevant input parameters. This results in a speed-up of the calculation by about three orders of magnitude, while meeting the stringent accuracy requirements of KATRIN.


ODSL
RU-B
(914)Parallelizing MCMC Sampling via Space Partitioning
  • Vasyl Hafych,
  • Philipp Eller,
  • Oliver Schulz,
  • Allen Caldwell
Statistics and Computing (June/2022) e-Print:2008.03098 doi:10.1007/s11222-022-10116-z
abstract + abstract -

Efficient sampling of many-dimensional and multimodal density functions is a task of great interest in many research fields. We describe an algorithm that allows parallelizing inherently serial Markov chain Monte Carlo (MCMC) sampling by partitioning the space of the function parameters into multiple subspaces and sampling each of them independently. The samples of the different subspaces are then reweighted by their integral values and stitched back together. This approach allows reducing sampling wall-clock time by parallel operation. It also improves sampling of multimodal target densities and results in less correlated samples. Finally, the approach yields an estimate of the integral of the target density function.


RU-D
(913)The signature of large-scale turbulence driving on the structure of the interstellar medium
  • Colman,
  • T.,
  • Robitaille,
  • J.-F.,
  • Hennebelle
  • +19
  • P.,
  • Miville-Deschênes,
  • M.-A.,
  • Brucy,
  • N.,
  • Klessen,
  • R. S.,
  • Glover,
  • S. C. O.,
  • Soler,
  • J. D.,
  • Elia,
  • D.,
  • Traficante,
  • A.,
  • Molinari,
  • S.,
  • & Testi,
  • L
  • (less)
abstract + abstract -

The mechanisms that maintain turbulence in the interstellar medium (ISM) are still not identified. This work investigates how we can distinguish between two fundamental driving mechanisms: the accumulated effect of stellar feedback versus the energy injection from galactic scales. We perform a series of numerical simulations describing a stratified star-forming ISM subject to self-consistent stellar feedback. Large-scale external turbulent driving, of various intensities, is added to mimic galactic driving mechanisms. We analyse the resulting column density maps with a technique called Multi-scale non-Gaussian segmentation, which separates the coherent structures and the Gaussian background. This effectively discriminates between the various simulations and is a promising method to understand the ISM structure. In particular, the power spectrum of the coherent structures flattens above 60 pc when turbulence is driven only by stellar feedback. When large-scale driving is applied, the turn-over shifts to larger scales. A systematic comparison with the Large Magellanic Cloud (LMC) is then performed. Only 1 out of 25 regions has a coherent power spectrum that is consistent with the feedback-only simulation. A detailed study of the turn-over scale leads us to conclude that regular stellar feedback is not enough to explain the observed ISM structure on scales larger than 60 pc. Extreme feedback in the form of supergiant shells likely plays an important role but cannot explain all the regions of the LMC. If we assume ISM structure is generated by turbulence, another large-scale driving mechanism is needed to explain the entirety of the observations.

 


CN-3
CN-6
PhD Thesis
RU-A
(912)Modeling of the Galactic Cosmic-Ray Antiproton Flux and Development of a Multi-Purpose Active-Target Particle Telescope for Cosmic Rays
  • Thomas Pöschl - Advisor: Stephan Paul
Thesis (7/2022) link
abstract + abstract -

Cosmic rays are an excellent probe to study energetic processes in our galaxy. The measurement of antinuclei is particularly informative. In this thesis, the production and propagation of cosmic antiprotons in our galaxy is investigated. In addition, a novel detector concept based on scintillating plastic fibers coupled to silicon photomultipliers is presented. The detector shall be used for cosmic-ray studies in future.


CN-7
RU-A
(911)First measurement of massive virtual photon emission from N* baryon resonances
  • R. Abou Yassine,
  • J. Adamczewski-Musch,
  • O. Arnold,
  • E.T. Atomssa,
  • M. Becker
  • +116
  • C. Behnke,
  • J.C. Berger-Chen,
  • A. Blanco,
  • C. Blume,
  • M. Böhmer,
  • L. Chlad,
  • P. Chudoba,
  • I. Ciepal,
  • C. Deveaux,
  • D. Dittert,
  • J. Dreyer,
  • E. Epple,
  • L. Fabbietti,
  • P. Fonte,
  • C. Franco,
  • J. Friese,
  • I. Fröhlich,
  • J. Förtsch,
  • T. Galatyuk,
  • J.A. Garzon,
  • R. Gernhäuser,
  • R. Greifenhagen,
  • M. Grunwald,
  • M. Gumberidze,
  • S. Harabasz,
  • T. Heinz,
  • T. Hennino,
  • C. Höhne,
  • F. Hojeij,
  • R. Holzmann,
  • M. Idzik,
  • B. Kämpfer,
  • K-H. Kampert,
  • B. Kardan,
  • V. Kedych,
  • I. Koenig,
  • W. Koenig,
  • M. Kohls,
  • B.W. Kolb,
  • G. Korcyl,
  • G. Kornakov,
  • F. Kornas,
  • R. Kotte,
  • W. Krueger,
  • A. Kugler,
  • T. Kunz,
  • R. Lalik,
  • K. Lapidus,
  • S. Linev,
  • L. Lopes,
  • M. Lorenz,
  • T. Mahmoud,
  • L. Maier,
  • A. Malige,
  • J. Markert,
  • S. Maurus,
  • V. Metag,
  • J. Michel,
  • D.M. Mihaylov,
  • V. Mikhaylov,
  • A. Molenda,
  • C. Müntz,
  • R. Münzer,
  • L. Naumann,
  • K. Nowakowski,
  • J.-H. Otto,
  • Y. Parpottas,
  • M. Parschau,
  • C. Pauly,
  • V. Pechenov,
  • O. Pechenova,
  • J. Pietraszko,
  • T. Povar,
  • A. Prozorov,
  • W. Przygoda,
  • K. Pysz,
  • B. Ramstein,
  • N. Rathod,
  • P. Rodriguez-Ramos,
  • A. Rost,
  • P. Salabura,
  • T. Scheib,
  • N. Schild,
  • K. Schmidt-Sommerfeld,
  • H. Schuldes,
  • E. Schwab,
  • F. Scozzi,
  • F. Seck,
  • P. Sellheim,
  • J. Siebenson,
  • L. Silva,
  • U. Singh,
  • J. Smyrski,
  • S. Spataro,
  • S. Spies,
  • M.S. Stefaniak,
  • H. Ströbele,
  • J. Stroth,
  • P. Strzempek,
  • C. Sturm,
  • K. Sumara,
  • O. Svoboda,
  • M. Szala,
  • P. Tlusty,
  • M. Traxler,
  • H. Tsertos,
  • O. Vazquez-Doce,
  • V. Wagner,
  • A.A. Weber,
  • C. Wendisch,
  • M.G. Wiebusch,
  • J. Wirth,
  • H.P. Zbroszczyk,
  • E. Zherebtsova,
  • P. Zumbruch,
  • M. Zetenyi
  • (less)
abstract + abstract -

First information on the timelike electromagnetic structure of baryons in the second resonance region has been obtained from measurements of invariant mass and angular distributions in the quasi-free reaction $\pi^- p \to nee$ at $\sqrt{s_{\pi^- p}}$ = 1.49 GeV with the High Acceptance Di-Electron Spectrometer (HADES) detector at GSI using the pion beam impinging on a CH$_2$ target. We find a total cross section $\sigma (\pi^- p \to nee) = 2.97 \pm 0.07^{data} \pm 0.21^{acc} \pm 0.31^{\rm{Z}_{\rm{eff}}} \mu$b. Combined with the Partial Wave Analysis of the concurrently measured two-pion channel, these data sets provide a crucial test of Vector Meson Dominance (VMD) inspired models. The commonly used "strict VMD" approach strongly overestimates the $e^+e^-$ yield. Instead, approaches based on a VMD amplitude vanishing at small $e^+e^-$ invariant masses supplemented coherently by a direct photon amplitude provide a better agreement. A good description of the data is also obtained using a calculation of electromagnetic timelike baryon transition form factors in a covariant spectator-quark model, demonstrating the dominance of meson cloud effects. The angular distributions of $e^+e^-$ pairs demonstrate the contributions of virtual photons with longitudinal polarization, in contrast to real photons. The virtual photon angular dependence supports the dominance of J=3/2, I=1/2 contributions observed in both the $\gamma^{\star} n$ and the $\pi \pi n$ channels.


CN-2
CN-8
PhD Thesis
RU-D
RU-E
(910)Hadean water-dew cycles drive the evolution of DNA and protocells.
  • Alan Ianeselli - Advisor: Dieter Braun
Thesis (4/2022) doi:10.5282/edoc.29754
abstract + abstract -

Liquid water is a fundamental requirement for any form of life. On Earth, it can ubiquitously be found in the form of bulk, fog or dew, and cycling between them requires a continuous influx of energy. These water evaporation-condensation cycles can be provided globally by the sun, or locally by differences in temperatures. Differentially heated rock pores on the Hadean Earth present the non-equilibrium conditions to evaporate bulk water and re-condense it as fog and dew. The resulting microscale bulk-dew cycles are driven by the surface tension of water and lead to periodic oscillations in the concentration of salts and molecules, pH and wet-dry states. [...]


CN-3
CN-4
PhD Thesis
RU-B
RU-C
RU-D
(909)Machine learning strong lensing
  • Stefan Schuldt - Advisor: Sherry Suyu
Thesis (4/2022) link
abstract + abstract -

The main focus of the dissertation is the development of a neural network to model fast and autonomusly strong gravitational lenses. For generating realistic training data, we developed a simulation pipeline that accepts real observed images, simulating only the gravitational lensing effect. We have further carried out a dedicated comparison on real lenses to traditionally obtained models. Besides this, we present NetZ, a photo-z network using a novel approach.


CN-7
RU-A
(908)Reevaluation of the cosmic antideuteron flux from cosmic-ray interactions and from exotic sources
  • Laura ŠerkšnytÄ--,
  • Stephan Königstorfer,
  • Philip von Doetinchem,
  • Laura Fabbietti,
  • Diego Mauricio Gomez-Coral
  • +6
  • Johannes Herms,
  • Alejandro Ibarra,
  • Thomas Pöschl,
  • Anirvan Shukla,
  • Andrew Strong,
  • Ivan Vorobyev
  • (less)
Physical Review D (4/2022) doi:10.1103/PhysRevD.105.083021
abstract + abstract -

Cosmic-ray antideuterons could be a key for the discovery of exotic phenomena in our Galaxy, such as dark-matter annihilations or primordial black hole evaporation. Unfortunately the theoretical predictions of the antideuteron flux at Earth are plagued with uncertainties from the mechanism of antideuteron production and propagation in the Galaxy. We present the most up-to-date calculation of the antideuteron fluxes from cosmic-ray collisions with the interstellar medium and from exotic processes. We include for the first time the antideuteron inelastic interaction cross section recently measured by the ALICE collaboration to account for the loss of antideuterons during propagation. In order to bracket the uncertainty in the expected fluxes, we consider several state-of-the-art models of antideuteron production and of cosmic-ray propagation.


CN-7
RU-A
(907)Impact of the Coulomb field on charged-pion spectra in few-GeV heavy-ion collisions
  • J. Adamczewski-Musch,
  • O. Arnold,
  • C. Behnke,
  • A. Belounnas,
  • A. Belyaev
  • +122
  • J.C. Berger-Chen,
  • A. Blanco,
  • C. Blume,
  • M. Böhmer,
  • P. Bordalo,
  • S. Chernenko,
  • L. Chlad,
  • I. Ciepał,
  • C. Deveaux,
  • J. Dreyer,
  • E. Epple,
  • L. Fabbietti,
  • O. Fateev,
  • P. Filip,
  • P. Fonte,
  • C. Franco,
  • J. Friese,
  • I. Fröhlich,
  • T. Galatyuk,
  • J.A. Garzon,
  • R. Gernhäuser,
  • S. Gläßel,
  • R. Greifenhagen,
  • F. Guber,
  • M. Gumberidze,
  • S. Harabasz,
  • T. Heinz,
  • T. Hennino,
  • S. Hlavac,
  • C. Höhne,
  • R. Holzmann,
  • A. Ierusalimov,
  • A. Ivashkin,
  • B. Kämpfer,
  • T. Karavicheva,
  • B. Kardan,
  • I. Koenig,
  • W. Koenig,
  • M. Kohls,
  • B.W. Kolb,
  • G. Korcyl,
  • G. Kornakov,
  • F. Kornas,
  • R. Kotte,
  • A. Kugler,
  • T. Kunz,
  • A. Kurepin,
  • A. Kurilkin,
  • P. Kurilkin,
  • V. Ladygin,
  • R. Lalik,
  • K. Lapidus,
  • A. Lebedev,
  • S. Linev,
  • L. Lopes,
  • M. Lorenz,
  • T. Mahmoud,
  • L. Maier,
  • A. Malige,
  • A. Mangiarotti,
  • J. Markert,
  • T. Matulewicz,
  • S. Maurus,
  • V. Metag,
  • J. Michel,
  • D.M. Mihaylov,
  • S. Morozov,
  • C. Müntz,
  • R. Münzer,
  • M. Nabroth,
  • L. Naumann,
  • K. Nowakowski,
  • Y. Parpottas,
  • M. Parschau,
  • V. Pechenov,
  • O. Pechenova,
  • O. Petukhov,
  • K. Piasecki,
  • J. Pietraszko,
  • W. Przygoda,
  • K. Pysz,
  • S. Ramos,
  • B. Ramstein,
  • N. Rathod,
  • A. Reshetin,
  • P. Rodriguez-Ramos,
  • P. Rosier,
  • A. Rost,
  • A. Rustamov,
  • A. Sadovsky,
  • P. Salabura,
  • T. Scheib,
  • H. Schuldes,
  • N. Schild,
  • E. Schwab,
  • F. Scozzi,
  • F. Seck,
  • P. Sellheim,
  • I. Selyuzhenkov,
  • J. Siebenson,
  • L. Silva,
  • U. Singh,
  • J. Smyrski,
  • Yu.G. Sobolev,
  • S. Spataro,
  • S. Spies,
  • H. Ströbele,
  • J. Stroth,
  • C. Sturm,
  • K. Sumara,
  • O. Svoboda,
  • M. Szala,
  • P. Tlusty,
  • M. Traxler,
  • H. Tsertos,
  • E. Usenko,
  • V. Wagner,
  • C. Wendisch,
  • M.G. Wiebusch,
  • J. Wirth,
  • Y. Zanevsky,
  • P. Zumbruch
  • (less)
abstract + abstract -

In nuclear collisions the incident protons generate a Coulomb field which acts on produced charged particles. The impact of these interactions on charged pion transverse-mass and rapidity spectra, as well as on pion-pion momentum correlations is investigated in Au+Au collisions at $\sqrt{s_{NN}}$ = 2.4 GeV. We show that the low-mt part of the data ($m_t < 0.2$ GeV/c$^2$) can be well described with a Coulomb-modified Boltzmann distribution that also takes changes of the Coulomb field during the expansion of the fireball into account. The observed centrality dependence of the fitted mean Coulomb potential deviates strongly from a $A_{part}^{2/3}$ scaling, indicating that, next to the fireball, the non-interacting charged spectators have to be taken into account. For the most central collisions, the Coulomb modifications of the HBT source radii are found to be consistent with the potential extracted from the single-pion transverse-mass distributions. This finding suggests that the region of homogeneity obtained from two-pion correlations coincides with the region in which the pions freeze-out. Using the inferred mean-square radius of the charge distribution at freeze-out, we have deduced a baryon density, in fair agreement with values obtained from statistical hadronization model fits to the particle yields.


RU-A
(906)Charm mass effects in the static energy computed in 2+1+1 flavor lattice QCD
  • Johannes Heinrich Weber,
  • Nora Brambilla,
  • Rafael L. Delgado,
  • Andreas Kronfeld,
  • Viljami Leino
  • +3
  • Peter Petreczky,
  • Sebastian Steinbeißer,
  • Antonio Vairo
  • (less)
abstract + abstract -

We report our analysis for the static energy in (2+1+1)-flavor QCD over a wide range of lattice spacings and several quark masses. We obtain results for the static energy out to distances of nearly 1 fm, allowing us to perform a simultaneous determination of the lattice scales $r_2$, $r_1$ and $r_0$ as well as the string tension, $\sigma$. While our results for ${r_0}/{r_1}$ and $r_0$ $\sqrt{\sigma}$ agree with published (2+1)-flavor results, our result for ${r_1}/{r_2}$ differs significantly from the value obtained in the (2+1)-flavor case, likely due to the effect of the charm quark. We study in detail the effect of the charm quark on the static energy by comparing our results on the finest lattices with the previously published (2+1)-flavor QCD results at similar lattice spacing. The lattice results agree well with the two-loop perturbative expression of the static energy incorporating finite charm mass effects.


CN-6
(905)Mildly Relativistic Perpendicular Multiple-ion GRB Shocks
  • Jonas M. Graw,
  • Martin S. Weidl,
  • Frank Jenko
The Astrophysical Journal (12/2022) doi:10.3847/1538-4357/ac9bf1
abstract + abstract -

Mildly relativistic perpendicular, collisionless multiple-ion gamma-ray burst shocks are analyzed using 2D3V particle-in-cell simulations. A characteristic feature of multiple-ion shocks is alternating maxima of the α particle and the proton densities, at least in the early downstream. Turbulence, shock-drift acceleration, and evidence of stochastic acceleration are observed. We performed simulations with both in-plane (B y ) and out-of-plane (B z ) magnetic fields, as well as in a perpendicular shock setup with φ = 45°, and saw multiple differences: while with B z , the highest-energetic particles mostly gain energy at the beginning of the shock, with B y , particles continue gaining energy and it does not appear that they have reached their final energy level. A larger magnetization σ leads to more high-energetic particles in our simulations. One important quantity for astronomers is the electron acceleration efficiency ϵ e , which is measurable due to synchrotron radiation. This quantity hardly changes when changing the amount of α particles while keeping σ constant. It is, however, noteworthy that ϵ e strongly differs for in-plane and out-of-plane magnetic fields. When looking at the proton and α acceleration efficiency, ϵ p and ϵ α , the energy of α particles always decreases when passing the shock into the downstream, whereas the energy of protons can increase if α particles account for the majority of the ions.


RU-D
(904)The impact of dynamic pressure bumps on the observational properties of protoplanetary disks
  • Jochen Stadler,
  • Matías Gárate,
  • Paola Pinilla,
  • Christian Lenz,
  • Cornelis P. Dullemond
  • +2
  • Til Birnstiel,
  • Sebastian M. Stammler
  • (less)
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202243338
abstract + abstract -

Context. Over the last years, large (sub-)millimetre surveys of protoplanetary disks in different star forming regions have well constrained the demographics of disks, such as their millimetre luminosities, spectral indices, and disk radii. Additionally, several high-resolution observations have revealed an abundance of substructures in the disk's dust continuum. The most prominent are ring like structures, which are likely caused by pressure bumps trapping dust particles. The origins and characteristics of these pressure bumps, nevertheless, need to be further investigated.
Aims: The purpose of this work is to study how dynamic pressure bumps affect observational properties of protoplanetary disks. We further aim to differentiate between the planetary- versus zonal flow-origin of pressure bumps.
Methods: We perform one-dimensional gas and dust evolution simulations, setting up models with varying pressure bump features, including their amplitude and location, growth time, and number of bumps. We subsequently run radiative transfer calculations to obtain synthetic images, from which we obtain the different quantities of observations.
Results: We find that the outermost pressure bump determines the disk's dust size across different millimetre wavelengths and confirm that the observed dust masses of disks with optically thick inner bumps (<40 au) are underestimated by up to an order of magnitude. Our modelled dust traps need to form early (<0.1 Myr), fast (on viscous timescales), and must be long lived (>Myr) to obtain the observed high millimetre luminosities and low spectral indices of disks. While the planetary bump models can reproduce these observables irrespectively of the opacity prescription, the highest opacities are needed for the dynamic bump model, which mimics zonal flows in disks, to be in line with observations.
Conclusions: Our findings favour the planetary- over the zonal flow-origin of pressure bumps and support the idea that planet formation already occurs in early class 0-1 stages of circumstellar disks. The determination of the disk's effective size through its outermost pressure bump also delivers a possible answer to why disks in recent low-resolution surveys appear to have the same sizes across different millimetre wavelengths.


CN-2
RU-D
(903)Modelling photoevaporation in planet forming discs
  • Barbara Ercolano,
  • Giovanni Picogna
European Physical Journal Plus (12/2022) doi:10.1140/epjp/s13360-022-03515-8
abstract + abstract -

Planets are born from the gas and dust discs surrounding young stars. Energetic radiation from the central star can drive thermal outflows from the discs atmospheres, strongly affecting the evolution of the discs and the nascent planetary system. In this context, several numerical models of varying complexity have been developed to study the process of disc photoevaporation from their central stars. We describe the numerical techniques, the results and the predictivity of current models and identify observational tests to constrain them.


(902)Constraining the multi-scale dark-matter distribution in CASSOWARY 31 with strong gravitational lensing and stellar dynamics
  • H. Wang,
  • R. Cañameras,
  • G. B. Caminha,
  • S. H. Suyu,
  • A. Yıldırım
  • +4
  • G. Chirivì,
  • L. Christensen,
  • C. Grillo,
  • S. Schuldt
  • (less)
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202243600
abstract + abstract -

We study the inner structure of the group-scale lens CASSOWARY 31 (CSWA 31) by adopting both strong lensing and dynamical modeling. CSWA 31 is a peculiar lens system. The brightest group galaxy (BGG) is an ultra-massive elliptical galaxy at z = 0.683 with a weighted mean velocity dispersion of σ = 432 ± 31 km s−1. It is surrounded by group members and several lensed arcs probing up to ≃150 kpc in projection. Our results significantly improve on previous analyses of CSWA 31 thanks to the new HST imaging and MUSE integral-field spectroscopy. From the secure identification of five sets of multiple images and measurements of the spatially resolved stellar kinematics of the BGG, we conduct a detailed analysis of the multi-scale mass distribution using various modeling approaches, in both the single and multiple lens-plane scenarios. Our best-fit mass models reproduce the positions of multiple images and provide robust reconstructions for two background galaxies at z = 1.4869 and z = 2.763. Despite small variations related to the different sets of input constraints, the relative contributions from the BGG and group-scale halo are remarkably consistent in our three reference models, demonstrating the self-consistency between strong lensing analyses based on image position and extended image modeling. We find that the ultra-massive BGG dominates the projected total mass profiles within 20 kpc, while the group-scale halo dominates at larger radii. The total projected mass enclosed within Reff = 27.2 kpc is 1.10−0.04+0.02 × 1013 M. We find that CSWA 31 is a peculiar fossil group, strongly dark-matter dominated toward the central region, and with a projected total mass profile similar to higher-mass cluster-scale halos. The total mass-density slope within the effective radius is shallower than isothermal, consistent with previous analyses of early-type galaxies in overdense environments.

Full Table B.1 is only available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/668/A162


(901)Length Regulation Drives Self-Organization in Filament-Motor Mixtures
  • Moritz Striebel,
  • Fridtjof Brauns,
  • Erwin Frey
Physical Review Letters (12/2022) doi:10.1103/PhysRevLett.129.238102
abstract + abstract -

Cytoskeletal networks form complex intracellular structures. Here we investigate a minimal model for filament-motor mixtures in which motors act as depolymerases and thereby regulate filament length. Combining agent-based simulations and hydrodynamic equations, we show that resource-limited length regulation drives the formation of filament clusters despite the absence of mechanical interactions between filaments. Even though the orientation of individual remains fixed, collective filament orientation emerges in the clusters, aligned orthogonal to their interfaces.


(900)Three-loop helicity amplitudes for quark-gluon scattering in QCD
  • Fabrizio Caola,
  • Amlan Chakraborty,
  • Giulio Gambuti,
  • Andreas von Manteuffel,
  • Lorenzo Tancredi
Journal of High Energy Physics (12/2022) doi:10.1007/JHEP12(2022)082
abstract + abstract -

We compute the three-loop helicity amplitudes for q q ¯ → gg and its crossed partonic channels, in massless QCD. Our analytical results provide a non-trivial check of the color quadrupole contribution to the infrared poles for external states in different color representations. At high energies, the qg → qg amplitude shows the predicted factorized form from Regge theory and confirms previous results for the gluon Regge trajectory extracted from qq' → qq' and gg → gg scattering.


RU-D
(899)Rapid formation of massive planetary cores in a pressure bump
  • Tommy Chi Ho Lau,
  • Joanna Drążkowska,
  • Sebastian M. Stammler,
  • Tilman Birnstiel,
  • Cornelis P. Dullemond
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202244864
abstract + abstract -

Context. Models of planetary core growth by either planetesimal or pebble accretion are traditionally disconnected from the models of dust evolution and formation of the first gravitationally bound planetesimals. State-of-the-art models typically start with massive planetary cores already present.
Aims: We aim to study the formation and growth of planetary cores in a pressure bump, motivated by the annular structures observed in protoplanetary disks, starting with submicron-sized dust grains.
Methods: We connect the models of dust coagulation and drift, planetesimal formation in the streaming instability, gravitational interactions between planetesimals, pebble accretion, and planet migration into one uniform framework.
Results: We find that planetesimals forming early at the massive end of the size distribution grow quickly, predominantly by pebble accretion. These few massive bodies grow on timescales of ~100 000 yr and stir the planetesimals that form later, preventing the emergence of further planetary cores. Additionally, a migration trap occurs, allowing for retention of the growing cores.
Conclusions: Pressure bumps are favourable locations for the emergence and rapid growth of planetary cores by pebble accretion as the dust density and grain size are increased and the pebble accretion onset mass is reduced compared to a smooth-disc model.


(898)Strong lensing time-delay cosmography in the 2020s
  • Tommaso Treu,
  • Sherry H. Suyu,
  • Philip J. Marshall
Astronomy and Astrophysics Review (12/2022) doi:10.1007/s00159-022-00145-y
abstract + abstract -

Multiply imaged time-variable sources can be used to measure absolute distances as a function of redshifts and thus determine cosmological parameters, chiefly the Hubble Constant H0. In the two decades up to 2020, through a number of observational and conceptual breakthroughs, this so-called time-delay cosmography has reached a precision sufficient to be an important independent voice in the current "Hubble tension" debate between early- and late-universe determinations of H0. The 2020s promise to deliver major advances in time-delay cosmography, owing to the large number of lenses to be discovered by new and upcoming surveys and the vastly improved capabilities for follow-up and analysis. In this review, after a brief summary of the foundations of the method and recent advances, we outline the opportunities for the decade and the challenges that will need to be overcome in order to meet the goal of the determination of H0 from time-delay cosmography with 1% precision and accuracy.


RU-A
(897)Implications of gradient flow on the static force
  • Nora Brambilla,
  • Viljami Leino,
  • Julian Mayer-Steudte,
  • Antonio Vairo
abstract + abstract -

We use gradient flow to compute the static force based on a Wilson loop with a chromoelectric field insertion. The result can be compared on one hand to the static force from the numerical derivative of the lattice static energy, and on the other hand to the perturbative calculation, allowing a precise extraction of the $\Lambda_0$ parameter. This study may open the way to gradient flow calculations of correlators of chromoelectric and chromomagnetic fields, which typically arise in the nonrelativistic effective field theory factorization.


CN-4
RU-C
(896)Voids fill us in on rising cosmology tensions
  • Sofia Contarini,
  • Alice Pisani,
  • Nico Hamaus,
  • Federico Marulli,
  • Lauro Moscardini
  • +1
abstract + abstract -

We investigate the main tensions within the current standard model of cosmology from the perspective of the void size function in BOSS DR12 data. For this purpose, we present the first cosmological constraints on the parameters $S_8\equiv \sigma_8\sqrt{\Omega_{\rm m}/0.3}$ and $H_0$ obtained from voids as a stand-alone probe. We rely on an extension of the popular volume-conserving model for the void size function, tailored to the application on data, including geometric and dynamic distortions. We calibrate the two nuisance parameters of this model with the official BOSS collaboration mock catalogs and propagate their uncertainty through the statistical analysis of the BOSS void number counts. We focus our analysis on the $\Omega_{\rm m}$--$\sigma_8$ and $\Omega_{\rm m}$--$H_0$ parameter planes and derive the marginalized constraints $S_8 = 0.78^{+0.16}_{-0.14}$ and $H_0=65.2^{+4.5}_{-3.6}$ $\mathrm{km} \ \mathrm{s}^{-1} \ \mathrm{Mpc}^{-1}$. Our estimate of $S_8$ is fully compatible with constraints from the literature, while our $H_0$ value slightly disagrees by more than $1\sigma$ with recent local distance ladder measurements of type Ia supernovae. Our results open up a new viewing angle on the rising cosmological tensions and are expected to improve notably in precision when jointly analyzed with independent probes.


(895)Razor-thin dust layers in protoplanetary disks: Limits on the vertical shear instability
  • C. P. Dullemond,
  • A. Ziampras,
  • D. Ostertag,
  • C. Dominik
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202244218
abstract + abstract -

Context. Recent observations with the Atacama Large Millimeter Array (ALMA) have shown that the large dust aggregates observed at millimeter wavelengths settle to the midplane into a remarkably thin layer. This sets strong limits on the strength of the turbulence and other gas motions in these disks.
Aims: We intend to find out if the geometric thinness of these layers is evidence against the vertical shear instability (VSI) operating in these disks. We aim to verify if a dust layer consisting of large enough dust aggregates could remain geometrically thin enough to be consistent with the latest observations of these dust layers, even if the disk is unstable to the VSI. If this is falsified, then the observed flatness of these dust layers proves that these disks are stable against the VSI, even out to the large radii at which these dust layers are observed.
Methods: We performed hydrodynamic simulations of a protoplanetary disk with a locally isothermal equation of state, and let the VSI fully develop. We sprinkled dust particles with a given grain size at random positions near the midplane and followed their motion as they got stirred up by the VSI, assuming no feedback onto the gas. We repeated the experiment for different grain sizes and determined for which grain size the layer becomes thin enough to be consistent with ALMA observations. We then verified if, with these grain sizes, it is still possible (given the constraints of dust opacity and gravitational stability) to generate a moderately optically thick layer at millimeter wavelengths, as observations appear to indicate.
Results: We found that even very large dust aggregates with Stokes numbers close to unity get stirred up to relatively large heights above the midplane by the VSI, which is in conflict with the observed geometric thinness. For grains so large that the Stokes number exceeds unity, the layer can be made to remain thin, but we show that it is hard to make dust layers optically thick at ALMA wavelengths (e.g., τ1.3mm ≳ 1) with such large dust aggregates.
Conclusions: We conclude that protoplanetary disks with geometrically thin midplane dust layers cannot be VSI unstable, at least not down to the disk midplane. Explanations for the inhibition of the VSI out to several hundreds of au include a high dust-to-gas ratio of the midplane layer, a modest background turbulence, and/or a reduced dust-to-gas ratio of the small dust grains that are responsible for the radiative cooling of the disk. A reduction of small grains by a factor of between 10 and 100 is sufficient to quench the VSI. Such a reduction is plausible in dust growth models, and still consistent with observations at optical and infrared wavelengths.


(894)Comparing accretion flow morphology in numerical simulations of black holes from the ngEHT Model Library: the impact of radiation physics
  • Koushik Chatterjee,
  • Andrew Chael,
  • Paul Tiede,
  • Yosuke Mizuno,
  • Razieh Emami
  • +16
  • Christian Fromm,
  • Angelo Ricarte,
  • Lindy Blackburn,
  • Freek Roelofs,
  • Michael D. Johnson,
  • Sheperd S. Doeleman,
  • Philipp Arras,
  • Antonio Fuentes,
  • Jakob Knollmüller,
  • Nikita Kosogorov,
  • Greg Lindahl,
  • Hendrik Müller,
  • Nimesh Patel,
  • Alexander Raymond,
  • Thalia Traiano,
  • Justin Vega
  • (less)
abstract + abstract -

In the past few years, the Event Horizon Telescope (EHT) has provided the first-ever event horizon-scale images of the supermassive black holes (BHs) M87* and Sagittarius A* (Sgr A*). The next-generation EHT project is an extension of the EHT array that promises larger angular resolution and higher sensitivity to the dim, extended flux around the central ring-like structure, possibly connecting the accretion flow and the jet. The ngEHT Analysis Challenges aim to understand the science extractability from synthetic images and movies so as to inform the ngEHT array design and analysis algorithm development. In this work, we take a look at the numerical fluid simulations used to construct the source models in the challenge set, which currently target M87* and Sgr A*. We have a rich set of models encompassing steady-state radiatively-inefficient accretion flows with time-dependent shearing hotspots, radiative and non-radiative general relativistic magneto-hydrodynamic simulations that incorporate electron heating and cooling. We find that the models exhibit remarkably similar temporal and spatial properties, except for the electron temperature since radiative losses substantially cool down electrons near the BH and the jet sheath. We restrict ourselves to standard torus accretion flows, and leave larger explorations of alternate accretion models to future work.


(893)The probability of galaxy-galaxy strong lensing events in hydrodynamical simulations of galaxy clusters
  • Massimo Meneghetti,
  • Antonio Ragagnin,
  • Stefano Borgani,
  • Francesco Calura,
  • Giulia Despali
  • +25
  • Carlo Giocoli,
  • Gian Luigi Granato,
  • Claudio Grillo,
  • Lauro Moscardini,
  • Elena Rasia,
  • Piero Rosati,
  • Giuseppe Angora,
  • Luigi Bassini,
  • Pietro Bergamini,
  • Gabriel B. Caminha,
  • Giovanni Granata,
  • Amata Mercurio,
  • Robert Benton Metcalf,
  • Priyamvada Natarajan,
  • Mario Nonino,
  • Giada Venusta Pignataro,
  • Cinthia Ragone-Figueroa,
  • Eros Vanzella,
  • Ana Acebron,
  • Klaus Dolag,
  • Giuseppe Murante,
  • Giuliano Taffoni,
  • Luca Tornatore,
  • Luca Tortorelli,
  • Milena Valentini
  • (less)
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202243779
abstract + abstract -

Context. An excess of galaxy-galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the Λ cold-dark-matter (CDM) cosmological model has recently been reported. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in ΛCDM cosmology.
Aims: We quantify the impact of the numerical resolution and active galactic nucleus (AGN) feedback scheme adopted in cosmological simulations on the predicted GGSL probability, and determine if varying these simulation properties can alleviate the gap with observations.
Methods: We analyze cluster-size halos (M200 > 5 × 1014 M) simulated with different mass and force resolutions and implementing several independent AGN feedback schemes. Our analysis focuses on galaxies with Einstein radii in the range 0.5 ≤ θE ≤ 3″.
Results: We find that improving the mass resolution by factors of 10 and 25, while using the same galaxy formation model that includes AGN feedback, does not affect the GGSL probability. We find similar results regarding the choice of gravitational softening. On the contrary, adopting an AGN feedback scheme that is less efficient at suppressing gas cooling and star formation leads to an increase in the GGSL probability by a factor of between 3 and 6. However, we notice that such simulations form overly massive galaxies whose contribution to the lensing cross section would be significant but that their Einstein radii are too large to be consistent with the observations. The primary contributors to the observed GGSL cross sections are galaxies with smaller masses that are compact enough to become critical for lensing. The population with these required characteristics appears to be absent from simulations. Conclusion. Based on these results, we reaffirm the tension between observations of GGSL and theoretical expectations in the framework of the ΛCDM cosmological model. The GGSL probability is sensitive to the galaxy formation model implemented in the simulations. Still, all the tested models have difficulty simultaneously reproducing the stellar mass function and the internal structure of galaxies.


CN-7
RU-A
(892)Evidence of a p-$\phi$ bound state
  • Emma Chizzali,
  • Yuki Kamiya,
  • Raffaele Del Grande,
  • Takumi Doi,
  • Laura Fabbietti
  • +2
abstract + abstract -

The existence of a nucleon-$\phi$ (N-$\phi$) bound state has been subject of theoretical and experimental investigations for decades. In this letter a re-analysis of the p-$\phi$ correlation measured at the LHC is presented, using as input recent lattice calculations of the N-$\phi$ interaction in the spin 3/2 channel obtained by the HAL QCD collaboration. A constrained fit of the experimental data allows to determine the spin 1/2 channel of the p-$\phi$ interaction with evidence of the formation of a p-$\phi$ bound state. The scattering length and effective range extracted from the spin 1/2 channel are $f_0^{(1/2)}=(-1.47^{+0.44}_{-0.37}(\mathrm{stat.})^{+0.14}_{-0.17}(\mathrm{syst.})+i\cdot0.00^{+0.26}_{-0.00}(\mathrm{stat.})^{+0.15}_{-0.00}(\mathrm{syst.}))$ fm and $d_0^{(1/2)}=(0.37^{+0.07}_{-0.08}(\mathrm{stat.})^{+0.03}_{-0.03}(\mathrm{syst.})+i\cdot~0.00^{+0.00}_{-0.02}(\mathrm{stat.})^{+0.00}_{-0.01}(\mathrm{syst.}))$ fm, respectively. The corresponding binding energy is estimated to be in the range $14.7-56.6$ MeV. This is the first experimental evidence of a p-$\phi$ bound state.


CN-3
RU-B
(891)Results on sub-GeV Dark Matter from a 10 eV Threshold CRESST-III Silicon Detector
  • CRESST Collaboration,
  • G. Angloher,
  • S. Banik,
  • G. Benato,
  • A. Bento
  • +57
  • A. Bertolini,
  • R. Breier,
  • C. Bucci,
  • J. Burkhart,
  • 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,
  • S. Gerster,
  • P. Gorla,
  • P. V. Guillaumon,
  • S. Gupta,
  • D. Hauff,
  • M. Ješkovský,
  • J. Jochum,
  • M. Kaznacheeva,
  • A. Kinast,
  • H. Kluck,
  • H. Kraus,
  • A. Langenkämper,
  • M. Mancuso,
  • L. Marini,
  • L. Meyer,
  • V. Mokina,
  • A. Nilima,
  • M. Olmi,
  • T. Ortmann,
  • C. Pagliarone,
  • 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 -

We present limits on the spin-independent interaction cross section of dark matter particles with silicon nuclei, derived from data taken with a cryogenic calorimeter with 0.35 g target mass operated in the CRESST-III experiment. A baseline nuclear recoil energy resolution of $(1.36\pm 0.05)$ eV$_{\text{nr}}$, currently the lowest reported for macroscopic particle detectors, and a corresponding energy threshold of $(10.0\pm 0.2)$ eV$_{\text{nr}}$ have been achieved, improving the sensitivity to light dark matter particles with masses below 160 MeV/c$^2$ by a factor of up to 20 compared to previous results. We characterize the observed low energy excess, and we exclude noise triggers and radioactive contaminations on the crystal surfaces as dominant contributions.


CN-2
(890)Reducing the complexity of chemical networks via interpretable autoencoders
  • T. Grassi,
  • F. Nauman,
  • J. P. Ramsey,
  • S. Bovino,
  • G. Picogna
  • +1
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202039956
abstract + abstract -

In many astrophysical applications, the cost of solving a chemical network represented by a system of ordinary differential equations (ODEs) grows significantly with the size of the network and can often represent a significant computational bottleneck, particularly in coupled chemo-dynamical models. Although standard numerical techniques and complex solutions tailored to thermochemistry can somewhat reduce the cost, more recently, machine learning algorithms have begun to attack this challenge via data-driven dimensional reduction techniques. In this work, we present a new class of methods that take advantage of machine learning techniques to reduce complex data sets (autoencoders), the optimization of multiparameter systems (standard backpropagation), and the robustness of well-established ODE solvers to to explicitly incorporate time dependence. This new method allows us to find a compressed and simplified version of a large chemical network in a semiautomated fashion that can be solved with a standard ODE solver, while also enabling interpretability of the compressed, latent network. As a proof of concept, we tested the method on an astrophysically relevant chemical network with 29 species and 224 reactions, obtaining a reduced but representative network with only 5 species and 12 reactions, and an increase in speed by a factor 65.


RU-D
(889)Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): Scattered light detection of a possible disk wind in RY Tau
  • P. -G. Valegård,
  • C. Ginski,
  • C. Dominik,
  • J. Bae,
  • M. Benisty
  • +12
  • T. Birnstiel,
  • S. Facchini,
  • A. Garufi,
  • M. Hogerheijde,
  • R. G. van Holstein,
  • M. Langlois,
  • C. F. Manara,
  • P. Pinilla,
  • Ch. Rab,
  • Á. Ribas,
  • L. B. F. M. Waters,
  • J. Williams
  • (less)
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202244001
abstract + abstract -

Context. Disk winds are an important mechanism for accretion and disk evolution around young stars. The accreting intermediate-mass T-Tauri star RY Tau has an active jet and a previously known disk wind. Archival optical and new near-infrared observations of the RY Tau system show two horn-like components stretching out as a cone from RY Tau. Scattered light from the disk around RY Tau is visible in the near-infrared, but not seen at optical wavelengths. In the near-infrared, dark wedges separate the horns from the disk, indicating that we may see the scattered light from a disk wind.
Aims: We aim to test the hypothesis that a dusty disk wind could be responsible for the optical effect in which the disk around RY Tau is hidden in the I band, but visible in the H band. This could be the first detection of a dusty disk wind in scattered light. We also want to constrain the grain size and dust mass in the wind and the wind-launching region.
Methods: We used archived Atacama-Large-Millimetre-Array (ALMA) and Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) I band observations combined with newly acquired SPHERE H band observations and available literature to build a simple geometric model of the RY Tau disk and disk wind. We used Monte Carlo radiative transfer modelling MCMax3D to create comparable synthetic observations that test the effect of a dusty wind on the optical effect in the observations. We constrained the grain size and dust mass needed in the disk wind to reproduce the effect from the observations.
Results: A model geometrically reminiscent of a dusty disk wind with small micron to sub-micron-sized grains elevated above the disk can reproduce the optical effect seen in the observations. The mass in the obscuring component of the wind has been constrained to 1 × 10−9 M ≤ M ≤ 5 × 10−8 M, which corresponds to a mass-loss rate in the wind of about ~1 × 10−8 M yr−1.
Conclusions: A simple model of a disk wind with micron to sub-micron-sized grains elevated above the disk is able to prevent stellar radiation to scatter in the disk at optical wavelengths while allowing photons to reach the disk in the near-infrared. Estimates of mass-loss rate correspond to previously presented theoretical models and points towards the idea that a magneto-hydrodynamic-type wind is the more likely scenario.


(888)On the Proof of Chiral Symmetry Breaking from Anomaly Matching in QCD-like Theories
  • Luca Ciambriello,
  • Roberto Contino,
  • Ling-Xiao Xu
abstract + abstract -

We critically reconsider the argument based on 't Hooft anomaly matching that aims at proving chiral symmetry breaking in QCD-like theories with $N_c>2$ colors and $N_f$ flavors of vectorlike quarks in the fundamental representation. The main line of reasoning relies on a property of the solutions of the anomaly matching and persistent mass equations called $N_f$-independence. The validity of $N_f$-independence was assumed based on qualitative arguments, but it was never proven rigorously. We provide a detailed proof and clarify under which (dynamical) conditions it holds. Our result is valid for a generic spectrum of massless composite fermions including baryons and exotics. We then present a novel argument that does not require any dynamical assumption and is based on downlifting solutions to smaller values of $N_f$. When applied to QCD ($N_c=3)$, our theorem implies that chiral symmetry must be spontaneously broken for $3\leq N_f<N_f^{CFT}$, where $N_f^{CFT}$ is the lower edge of the conformal window. A second argument is also presented based on continuity, which assumes the absence of phase transitions when the quark masses are sent to infinity. When applied to QCD, this result explains why chiral symmetry is broken for $N_f=2$, despite integer solutions of the equations exist in this case. Explicit examples and a numerical analysis are presented in a companion paper.


CN-5
RU-D
(887)A new scenario for magnetar formation: Tayler-Spruit dynamo in a proto-neutron star spun up by fallback
  • P. Barrère,
  • J. Guilet,
  • A. Reboul-Salze,
  • R. Raynaud,
  • H. -T. Janka
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202244172
abstract + abstract -

Magnetars are isolated young neutron stars characterised by the most intense magnetic fields known in the Universe, which power a wide variety of high-energy emissions from giant flares to fast radio bursts. The origin of their magnetic field is still a challenging question. In situ magnetic field amplification by dynamo action could potentially generate ultra-strong magnetic fields in fast-rotating progenitors. However, it is unclear whether the fraction of progenitors harbouring fast core rotation is sufficient to explain the entire magnetar population. To address this point, we propose a new scenario for magnetar formation involving a slowly rotating progenitor, in which a slow-rotating proto-neutron star is spun up by the supernova fallback. We argue that this can trigger the development of the Tayler-Spruit dynamo while other dynamo processes are disfavoured. Using the findings of previous studies of this dynamo and simulation results characterising the supernova fallback, we derive equations modelling the coupled evolution of the proto-neutron star rotation and magnetic field. Their time integration for different accreted masses is successfully compared with analytical estimates of the amplification timescales and saturation value of the magnetic field. We find that the magnetic field is amplified within 20 − 40 s after the core bounce, and that the radial magnetic field saturates at intensities between ∼1013 and 1015 G, therefore spanning the full range of a magnetar's dipolar magnetic fields. The toroidal magnetic field is predicted to be a factor of 10-100 times stronger, lying between ∼1015 and 3 × 1016 G. We also compare the saturation mechanisms proposed respectively by H.C. Spruit and J. Fuller, showing that magnetar-like magnetic fields can be generated for a neutron star spun up to rotation periods of ≲8 ms and ≲28 ms, corresponding to accreted masses of ≳ 4 × 10−2 M and ≳ 1.1 × 10−2 M, respectively. Therefore, our results suggest that magnetars can be formed from slow-rotating progenitors for accreted masses compatible with recent supernova simulations and leading to plausible initial rotation periods of the proto-neutron star.


MIAPbP
(886)Tidal Love numbers of novel and admixed celestial objects
  • Michael Collier,
  • Djuna Croon,
  • Rebecca K. Leane
Physical Review D (12/2022) doi:10.1103/PhysRevD.106.123027
abstract + abstract -

A subfraction of dark matter or new particles trapped inside celestial objects can significantly alter their macroscopic properties. We investigate the new physics imprint on celestial objects by using a generic framework to solve the Tolman-Oppenheimer-Volkoff (TOV) equations for up to two fluids. We test the impact of populations of new particles on celestial objects, including the sensitivity to self-interaction sizes, new particle mass, and net population mass. Applying our setup to neutron stars and boson stars, we find rich phenomenology for a range of these parameters, including the creation of extended atmospheres. These atmospheres are detectable by their impact on the tidal Love number, which can be measured at upcoming gravitational wave experiments such as Advanced LIGO, the Einstein Telescope, and LISA. We release our calculation framework as a publicly available code, allowing the TOV equations to be generically solved for arbitrary new physics models in novel and admixed celestial objects.


RU-A
(885)Shared Data and Algorithms for Deep Learning in Fundamental Physics
  • Lisa Benato,
  • Erik Buhmann,
  • Martin Erdmann,
  • Peter Fackeldey,
  • Jonas Glombitza
  • +8
  • Nikolai Hartmann,
  • Gregor Kasieczka,
  • William Korcari,
  • Thomas Kuhr,
  • Jan Steinheimer,
  • Horst Stöcker,
  • Tilman Plehn,
  • Kai Zhou
  • (less)
Computing and Software for Big Science (12/2022) doi:10.1007/s41781-022-00082-6
abstract + abstract -

We introduce a PYTHON package that provides simple and unified access to a collection of datasets from fundamental physics research—including particle physics, astroparticle physics, and hadron- and nuclear physics—for supervised machine learning studies. The datasets contain hadronic top quarks, cosmic-ray-induced air showers, phase transitions in hadronic matter, and generator-level histories. While public datasets from multiple fundamental physics disciplines already exist, the common interface and provided reference models simplify future work on cross-disciplinary machine learning and transfer learning in fundamental physics. We discuss the design and structure and line out how additional datasets can be submitted for inclusion. As showcase application, we present a simple yet flexible graph-based neural network architecture that can easily be applied to a wide range of supervised learning tasks. We show that our approach reaches performance close to dedicated methods on all datasets. To simplify adaptation for various problems, we provide easy-to-follow instructions on how graph-based representations of data structures, relevant for fundamental physics, can be constructed and provide code implementations for several of them. Implementations are also provided for our proposed method and all reference algorithms.


CN-5
RU-D
(884)Taking off the edge - simultaneous filament and end core formation
  • S. Heigl,
  • E. Hoemann,
  • A. Burkert
Monthly Notices of the Royal Astronomical Society (12/2022) doi:10.1093/mnras/stac3110
abstract + abstract -

Simulations of idealized star-forming filaments of finite length typically show core growth that is dominated by two cores forming at its respective end. The end cores form due to a strong increasing acceleration at the filament ends that leads to a sweep-up of material during the filament collapse along its axis. As this growth mode is typically faster than any other core formation mode in a filament, the end cores usually dominate in mass and density compared to other cores forming inside a filament. However, observations of star-forming filaments do not show this prevalence of cores at the filament ends. We explore a possible mechanism to slow the growth of the end cores using numerical simulations of simultaneous filament and embedded core formation, in our case a radially accreting filament forming in a finite converging flow. While such a set-up still leads to end cores, they soon begin to move inwards and a density gradient is formed outside of the cores by the continued accumulation of material. As a result, the outermost cores are no longer located at the exact ends of the filament and the density gradient softens the inward gravitational acceleration of the cores. Therefore, the two end cores do not grow as fast as expected and thus do not dominate over other core formation modes in the filament.


(883)Fragmentation with discontinuous Galerkin schemes: non-linear fragmentation
  • Maxime Lombart,
  • Mark Hutchison,
  • Yueh-Ning Lee
Monthly Notices of the Royal Astronomical Society (12/2022) doi:10.1093/mnras/stac2232
abstract + abstract -

Small grains play an essential role in astrophysical processes such as chemistry, radiative transfer, and gas/dust dynamics. The population of small grains is mainly maintained by the fragmentation process due to colliding grains. An accurate treatment of dust fragmentation is required in numerical modelling. However, current algorithms for solving fragmentation equation suffer from an overdiffusion in the conditions of 3D simulations. To tackle this challenge, we developed a discontinuous Galerkin scheme to solve efficiently the non-linear fragmentation equation with a limited number of dust bins.


RU-D
(882)A multisimulation study of relativistic SZ temperature scalings in galaxy clusters and groups
  • Elizabeth Lee,
  • Dhayaa Anbajagane,
  • Priyanka Singh,
  • Jens Chluba,
  • Daisuke Nagai
  • +4
  • Scott T. Kay,
  • Weiguang Cui,
  • Klaus Dolag,
  • Gustavo Yepes
  • (less)
Monthly Notices of the Royal Astronomical Society (12/2022) doi:10.1093/mnras/stac2781
abstract + abstract -

The Sunyaev-Zeldovich (SZ) effect is a powerful tool in modern cosmology. With future observations promising ever improving SZ measurements, the relativistic corrections to the SZ signals from galaxy groups and clusters are increasingly relevant. As such, it is important to understand the differences between three temperature measures: (a) the average relativistic SZ (rSZ) temperature, (b) the mass-weighted temperature relevant for the thermal SZ (tSZ) effect, and (c) the X-ray spectroscopic temperature. In this work, we compare these cluster temperatures, as predicted by the BAHAMAS & MACSIS, ILLUSTRISTNG, MAGNETICUM, and THE THREE HUNDRED PROJECT simulations. Despite the wide range of simulation parameters, we find the SZ temperatures are consistent across the simulations. We estimate a $\simeq 10{{\ \rm per\ cent}}$ level correction from rSZ to clusters with Y ≃ 10-4 Mpc-2. Our analysis confirms a systematic offset between the three temperature measures; with the rSZ temperature $\simeq 20{{\ \rm per\ cent}}$ larger than the other measures, and diverging further at higher redshifts. We demonstrate that these measures depart from simple self-similar evolution and explore how they vary with the defined radius of haloes. We investigate how different feedback prescriptions and resolutions affect the observed temperatures, and discover the SZ temperatures are rather insensitive to these details. The agreement between simulations indicates an exciting avenue for observational and theoretical exploration, determining the extent of relativistic SZ corrections. We provide multiple simulation-based fits to the scaling relations for use in future SZ modelling.


CN-2
RU-D
(881)The interplay between forming planets and photoevaporating discs I: forbidden line diagnostics
  • Michael L. Weber,
  • Barbara Ercolano,
  • Giovanni Picogna,
  • Christian Rab
Monthly Notices of the Royal Astronomical Society (12/2022) doi:10.1093/mnras/stac2954
abstract + abstract -

Disc winds and planet formation are considered to be two of the most important mechanisms that drive the evolution and dispersal of protoplanetary discs and in turn define the environment in which planets form and evolve. While both have been studied extensively in the past, we combine them into one model by performing three-dimensional radiation-hydrodynamic simulations of giant planet hosting discs that are undergoing X-ray photoevaporation, with the goal to analyse the interactions between both mechanisms. In order to study the effect on observational diagnostics, we produce synthetic observations of commonly used wind-tracing forbidden emission lines with detailed radiative transfer and photoionization calculations. We find that a sufficiently massive giant planet carves a gap in the gas disc that is deep enough to affect the structure and kinematics of the pressure-driven photoevaporative wind significantly. This effect can be strong enough to be visible in the synthetic high-resolution observations of some of our wind diagnostic lines, such as the [O I] 6300 Å or [S II] 6730 Å lines. When the disc is observed at inclinations around 40° and higher, the spectral line profiles may exhibit a peak in the redshifted part of the spectrum, which cannot easily be explained by simple wind models alone. Moreover, massive planets can induce asymmetric substructures within the disc and the photoevaporative wind, giving rise to temporal variations of the line profiles that can be strong enough to be observable on time-scales of less than a quarter of the planet's orbital period.


CN-1
CN-3
RU-D
(880)Accuracy and precision of triaxial orbit models - II. Viewing angles, shape, and orbital structure
  • Stefano de Nicola,
  • Bianca Neureiter,
  • Jens Thomas,
  • Roberto P. Saglia,
  • Ralf Bender
Monthly Notices of the Royal Astronomical Society (12/2022) doi:10.1093/mnras/stac2852
abstract + abstract -

We explore the potential of our novel triaxial modelling machinery in recovering the viewing angles, the shape, and the orbit distribution of galaxies by using a high-resolution N-body merger simulation. Our modelling technique includes several recent advancements. (i) Our new triaxial deprojection algorithm shape3d is able to significantly shrink the range of possible orientations of a triaxial galaxy and therefore to constrain its shape relying only on photometric information. It also allows to probe degeneracies, i.e. to recover different deprojections at the same assumed orientation. With this method we can constrain the intrinsic shape of the N-body simulation, i.e. the axis ratios p = b/a and q = c/a, with Δp and Δq ≲ 0.1 using only photometric information. The typical accuracy of the viewing angles reconstruction is 15°-20°. (ii) Our new triaxial Schwarzschild code smart exploits the full kinematic information contained in the entire non-parametric line-of-sight velocity distributions along with a 5D orbital sampling in phase space. (iii) We use a new generalized Akaike information criterion AICp to optimize the smoothing and to select the best-fitting model, avoiding potential biases in purely χ2-based approaches. With our deprojected densities, we recover the correct orbital structure and anisotropy parameter β with Δβ ≲ 0.1. These results are valid regardless of the tested orientation of the simulation and suggest that even despite the known intrinsic photometric and kinematic degeneracies the above described advanced methods make it possible to recover the shape and the orbital structure of triaxial bodies with unprecedented accuracy.


RU-C
(879)New Constraint on the Tensor-to-scalar Ratio from the Planck and BICEP/Keck Array Data Using the Profile Likelihood
  • Paolo Campeti,
  • Eiichiro Komatsu
The Astrophysical Journal (12/2022) doi:10.3847/1538-4357/ac9ea3
abstract + abstract -

Motivated by the discrepancy between Bayesian and frequentist upper limits on the tensor-to-scalar ratio parameter r found by the SPIDER collaboration, we investigate whether a similar trend is also present in the latest Planck and BICEP/Keck Array data. We derive a new upper bound on r using the frequentist profile likelihood method. We vary all the relevant cosmological parameters of the ΛCDM model, as well as the nuisance parameters. Unlike the Bayesian analysis using Markov Chain Monte Carlo (MCMC), our analysis is independent of the choice of priors. Using Planck Public Release 4, BICEP/Keck Array 2018, Planck cosmic microwave background lensing, and baryon acoustic oscillation data, we find an upper limit of r < 0.037 at 95% Confidence Level (C.L.), similar to the Bayesian MCMC result of r < 0.038 for a flat prior on r and a conditioned Planck lowlEB covariance matrix.


RU-D
(878)Simultaneous radio and optical polarimetry of GRB 191221B afterglow
  • Yuji Urata,
  • Kenji Toma,
  • Stefano Covino,
  • Klaas Wiersema,
  • Kuiyun Huang
  • +14
  • Jiro Shimoda,
  • Asuka Kuwata,
  • Sota Nagao,
  • Keiichi Asada,
  • Hiroshi Nagai,
  • Satoko Takahashi,
  • Chao En Chung,
  • Glen Petitpas,
  • Kazutaka Yamaoka,
  • Luca Izzo,
  • Johan Fynbo,
  • Antonio de Ugarte Postigo,
  • Maryam Arabsalmani,
  • Makoto Tashiro
  • (less)
abstract + abstract -

Gamma-ray bursts (GRBs) are the most luminous transients in the universe and are utilized as probes of early stars, gravitational wave counterparts and collisionless shock physics. In spite of studies on polarimetry of GRBs in individual wavelengths that characterized intriguing properties of prompt emission and afterglow, no coordinated multi-wavelength measurements have yet been performed. Here we report the first coordinated simultaneous polarimetry in the optical and radio bands for the afterglow associated with the typical long GRB 191221B. Our observations successfully caught the radio emission, which is not affected by synchrotron self-absorption, and show that the emission is depolarized in the radio band compared with the optical one. Our simultaneous polarization angle measurement and temporal polarization monitoring indicate the existence of cool electrons that increase the estimate of jet kinetic energy by a factor of more than 4 for this GRB afterglow. Further coordinated multi-wavelength polarimetric campaigns would improve our understanding of the total jet energies and magnetic field configurations in the emission regions of various types of GRBs, which are required to comprehend the mass scales of their progenitor systems and the physics of collisionless shocks.


RU-C
(877)Non-local contribution from small scales in galaxy-galaxy lensing: Comparison of mitigation schemes
  • J. Prat,
  • G. Zacharegkas,
  • Y. Park,
  • N. MacCrann,
  • E.R. Switzer
  • +110
  • S. Pandey,
  • C. Chang,
  • J. Blazek,
  • R. Miquel,
  • A. Alarcon,
  • O. Alves,
  • A. Amon,
  • F. Andrade-Oliveira,
  • K. Bechtol,
  • M.R. Becker,
  • G.M. Bernstein,
  • R. Chen,
  • A. Choi,
  • H. Camacho,
  • A. Campos,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • R. Cawthon,
  • J. Cordero,
  • M. Crocce,
  • C. Davis,
  • J. DeRose,
  • H.T. Diehl,
  • S. Dodelson,
  • C. Doux,
  • A. Drlica-Wagner,
  • K. Eckert,
  • T.F. Eifler,
  • J. Elvin-Poole,
  • S. Everett,
  • X. Fang,
  • A. Ferté,
  • P. Fosalba,
  • O. Friedrich,
  • M. Gatti,
  • G. Giannini,
  • D. Gruen,
  • R.A. Gruendl,
  • I. Harrison,
  • W.G. Hartley,
  • K. Herner,
  • H. Huang,
  • E.M. Huff,
  • M. Jarvis,
  • E. Krause,
  • N. Kuropatkin,
  • P.-F. Leget,
  • J. McCullough,
  • J. Myles,
  • A. Navarro-Alsina,
  • A. Porredon,
  • M. Raveri,
  • R.P. Rollins,
  • A. Roodman,
  • R. Rosenfeld,
  • A.J. Ross,
  • E.S. Rykoff,
  • C. Sánchez,
  • J. Sanchez,
  • L.F. Secco,
  • I. Sevilla-Noarbe,
  • E. Sheldon,
  • T. Shin,
  • M.A. Troxel,
  • I. Tutusaus,
  • T.N. Varga,
  • B. Yanny,
  • B. Yin,
  • Y. Zhang,
  • J. Zuntz,
  • M. Aguena,
  • S. Allam,
  • J. Annis,
  • D. Bacon,
  • E. Bertin,
  • S. Bocquet,
  • D. Brooks,
  • D.L. Burke,
  • J. Carretero,
  • M. Costanzi,
  • M.E.S. Pereira,
  • J. De Vicente,
  • S. Desai,
  • I. Ferrero,
  • B. Flaugher,
  • D.W. Gerdes,
  • G. Gutierrez,
  • S.R. Hinton,
  • D.L. Hollowood,
  • K. Honscheid,
  • D.J. James,
  • M. Lima,
  • F. Menanteau,
  • J. Mena-Fernández,
  • A. Palmese,
  • M. Paterno,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A.A. Plazas Malagón,
  • M. Rodriguez-Monroy,
  • E. Sanchez,
  • M. Schubnell,
  • M. Smith,
  • M. Soares-Santos,
  • E. Suchyta,
  • M.E.C. Swanson,
  • G. Tarle,
  • C. To,
  • N. Weaverdyck,
  • J. Weller
  • (less)
(12/2022) e-Print:2212.03734
abstract + abstract -

Recent cosmological analyses with large-scale structure and weak lensing measurements, usually referred to as 3$\times$2pt, had to discard a lot of signal-to-noise from small scales due to our inability to precisely model non-linearities and baryonic effects. Galaxy-galaxy lensing, or the position-shear correlation between lens and source galaxies, is one of the three two-point correlation functions that are included in such analyses, usually estimated with the mean tangential shear. However, tangential shear measurements at a given angular scale $\theta$ or physical scale $R$ carry information from all scales below that, forcing the scale cuts applied in real data to be significantly larger than the scale at which theoretical uncertainties become problematic. Recently there have been a few independent efforts that aim to mitigate the non-locality of the galaxy-galaxy lensing signal. Here we perform a comparison of the different methods, including the Y transformation described in Park et al. (2021), the point-mass marginalization methodology presented in MacCrann et al. (2020) and the Annular Differential Surface Density statistic described in Baldauf et al. (2010). We do the comparison at the cosmological constraints level in a noiseless simulated combined galaxy clustering and galaxy-galaxy lensing analysis. We find that all the estimators perform equivalently using a Rubin Observatory Legacy Survey of Space and Time (LSST) Year 1 like setup. This is because all the estimators project out the mode responsible for the non-local nature of the galaxy-galaxy lensing measurements, which we have identified as $1/R^2$. We finally apply all the estimators to DES Y3 data and confirm that they all give consistent results.


RU-A
(876)(Extended) Proca-Nuevo under the two-dimensional loupe
  • Verónica Errasti Díez
arXiv e-prints (12/2022) e-Print:2212.02549
abstract + abstract -

Recently, two new families of non-linear massive electrodynamics have been proposed: Proca-Nuevo and Extended Proca-Nuevo. We explicitly show that both families are irremediably ghostful in two dimensions. Our calculations indicate the need to revisit the classical consistency of (Extended) Proca-Nuevo in higher dimensions before these settings can be regarded as ghostfree.


C2PAP
CN-5
(875)The role of physical and numerical viscosity in hydrodynamical instabilities
  • Tirso Marin-Gilabert,
  • Milena Valentini,
  • Ulrich P. Steinwandel,
  • Klaus Dolag
Monthly Notices of the Royal Astronomical Society (12/2022) doi:10.1093/mnras/stac3042
abstract + abstract -

The evolution of the Kelvin-Helmholtz Instability (KHI) is widely used to assess the performance of numerical methods. We employ this instability to test both the smoothed particle hydrodynamics (SPH) and the meshless finite mass (MFM) implementation in OPENGADGET3. We quantify the accuracy of SPH and MFM in reproducing the linear growth of the KHI with different numerical and physical set-ups. Among them, we consider: (i) numerical induced viscosity, and (ii) physically motivated, Braginskii viscosity, and compare their effect on the growth of the KHI. We find that the changes of the inferred numerical viscosity when varying nuisance parameters such as the set-up or the number of neighbours in our SPH code are comparable to the differences obtained when using different hydrodynamical solvers, i.e. MFM. SPH reproduces the expected reduction of the growth rate in the presence of physical viscosity and recovers well the threshold level of physical viscosity needed to fully suppress the instability. In the case of galaxy clusters with a virial temperature of 3 × 107 K, this level corresponds to a suppression factor of ≍10-3 of the classical Braginskii value. The intrinsic, numerical viscosity of our SPH implementation in such an environment is inferred to be at least an order of magnitude smaller (i.e. ≍10-4), re-ensuring that modern SPH methods are suitable to study the effect of physical viscosity in galaxy clusters.


CN-4
RU-C
(874)StaNdaRT: a repository of standardised test models and outputs for supernova radiative transfer
  • Stéphane Blondin,
  • Sergei Blinnikov,
  • Fionntan P. Callan,
  • Christine E. Collins,
  • Luc Dessart
  • +24
  • Wesley Even,
  • Andreas Flörs,
  • Andrew G. Fullard,
  • D. John Hillier,
  • Anders Jerkstrand,
  • Daniel Kasen,
  • Boaz Katz,
  • Wolfgang Kerzendorf,
  • Alexandra Kozyreva,
  • Jack O'Brien,
  • Ezequiel A. Pássaro,
  • Nathaniel Roth,
  • Ken J. Shen,
  • Luke Shingles,
  • Stuart A. Sim,
  • Jaladh Singhal,
  • Isaac G. Smith,
  • Elena Sorokina,
  • Victor P. Utrobin,
  • Christian Vogl,
  • Marc Williamson,
  • Ryan Wollaeger,
  • Stan E. Woosley,
  • Nahliel Wygoda
  • (less)
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202244134
abstract + abstract -

We present the first results of a comprehensive supernova (SN) radiative-transfer (RT) code-comparison initiative (StaNdaRT), where the emission from the same set of standardised test models is simulated by currently used RT codes. We ran a total of ten codes on a set of four benchmark ejecta models of Type Ia SNe. We consider two sub-Chandrasekhar-mass (Mtot = 1.0 M) toy models with analytic density and composition profiles and two Chandrasekhar-mass delayed-detonation models that are outcomes of hydrodynamical simulations. We adopt spherical symmetry for all four models. The results of the different codes, including the light curves, spectra, and the evolution of several physical properties as a function of radius and time are provided in electronic form in a standard format via a public repository. We also include the detailed test model profiles and several Python scripts for accessing and presenting the input and output files. We also provide the code used to generate the toy models studied here. In this paper, we describe the test models, radiative-transfer codes, and output formats in detail, and provide access to the repository. We present example results of several key diagnostic features.


CN-4
RU-C
(873)Unveiling the Universe with emerging cosmological probes
  • Michele Moresco,
  • Lorenzo Amati,
  • Luca Amendola,
  • Simon Birrer,
  • John P. Blakeslee
  • +20
  • Michele Cantiello,
  • Andrea Cimatti,
  • Jeremy Darling,
  • Massimo Della Valle,
  • Maya Fishbach,
  • Claudio Grillo,
  • Nico Hamaus,
  • Daniel Holz,
  • Luca Izzo,
  • Raul Jimenez,
  • Elisabeta Lusso,
  • Massimo Meneghetti,
  • Ester Piedipalumbo,
  • Alice Pisani,
  • Alkistis Pourtsidou,
  • Lucia Pozzetti,
  • Miguel Quartin,
  • Guido Risaliti,
  • Piero Rosati,
  • Licia Verde
  • (less)
Living Reviews in Relativity (12/2022) doi:10.1007/s41114-022-00040-z
abstract + abstract -

The detection of the accelerated expansion of the Universe has been one of the major breakthroughs in modern cosmology. Several cosmological probes (Cosmic Microwave Background, Supernovae Type Ia, Baryon Acoustic Oscillations) have been studied in depth to better understand the nature of the mechanism driving this acceleration, and they are being currently pushed to their limits, obtaining remarkable constraints that allowed us to shape the standard cosmological model. In parallel to that, however, the percent precision achieved has recently revealed apparent tensions between measurements obtained from different methods. These are either indicating some unaccounted systematic effects, or are pointing toward new physics. Following the development of CMB, SNe, and BAO cosmology, it is critical to extend our selection of cosmological probes. Novel probes can be exploited to validate results, control or mitigate systematic effects, and, most importantly, to increase the accuracy and robustness of our results. This review is meant to provide a state-of-art benchmark of the latest advances in emerging "beyond-standard" cosmological probes. We present how several different methods can become a key resource for observational cosmology. In particular, we review cosmic chronometers, quasars, gamma-ray bursts, standard sirens, lensing time-delay with galaxies and clusters, cosmic voids, neutral hydrogen intensity mapping, surface brightness fluctuations, stellar ages of the oldest objects, secular redshift drift, and clustering of standard candles. The review describes the method, systematics, and results of each probe in a homogeneous way, giving the reader a clear picture of the available innovative methods that have been introduced in recent years and how to apply them. The review also discusses the potential synergies and complementarities between the various probes, exploring how they will contribute to the future of modern cosmology.


CN-6
(872)Assessing coincident neutrino detections using population models
  • F. Capel,
  • J. M. Burgess,
  • D. J. Mortlock,
  • P. Padovani
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202243116
abstract + abstract -

Several tentative associations between high-energy neutrinos and astrophysical sources have been recently reported, but a conclusive identification of these potential neutrino emitters remains challenging. We explore the use of Monte Carlo simulations of source populations to gain deeper insight into the physical implications of proposed individual source-neutrino associations. In particular, we focus on the IC170922A-TXS 0506+056 observation. Assuming a null model, we find a 7.6% chance of mistakenly identifying coincidences between γ-ray flares from blazars and neutrino alerts in 10-year surveys. We confirm that a blazar-neutrino connection based on the γ-ray flux is required to find a low chance coincidence probability and, therefore, a significant IC170922A-TXS 0506+056 association. We then assume this blazar-neutrino connection for the whole population and find that the ratio of neutrino to γ-ray fluxes must be ≲10−2 in order not to overproduce the total number of neutrino alerts seen by IceCube. For the IC170922A-TXS 0506+056 association to make sense, we must either accept this low flux ratio or suppose that only some rare sub-population of blazars is capable of high-energy neutrino production. For example, if we consider neutrino production only in blazar flares, we expect the flux ratio of between 10−3 and 10−1 to be consistent with a single coincident observation of a neutrino alert and flaring γ-ray blazar. These constraints should be interpreted in the context of the likelihood models used to find the IC170922A-TXS 0506+056 association, which assumes a fixed power-law neutrino spectrum of E−2.13 for all blazars.


CN-2
(871)Lower-than-expected flare temperatures for TRAPPIST-1
  • A. J. Maas,
  • E. Ilin,
  • M. Oshagh,
  • E. Pallé,
  • H. Parviainen
  • +10
  • K. Molaverdikhani,
  • A. Quirrenbach,
  • E. Esparza-Borges,
  • F. Murgas,
  • V. J. S. Béjar,
  • N. Narita,
  • A. Fukui,
  • C. -L. Lin,
  • M. Mori,
  • P. Klagyivik
  • (less)
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202243869
abstract + abstract -


Aims: Stellar flares emit thermal and nonthermal radiation in the X-ray and ultraviolet (UV) regime. Although high energetic radiation from flares is a potential threat to exoplanet atmospheres and may lead to surface sterilization, it might also provide the extra energy for low-mass stars needed to trigger and sustain prebiotic chemistry. Despite the UV continuum emission being constrained partly by the flare temperature, few efforts have been made to determine the flare temperature for ultra-cool M-dwarfs. We investigate two flares on TRAPPIST-1, an ultra-cool dwarf star that hosts seven exoplanets of which three lie within its habitable zone. The flares are detected in all four passbands of the MuSCAT2 instrument allowing a determination of their temperatures and bolometric energies.
Methods: We analyzed the light curves of the MuSCATl (multicolor simultaneous camera for studying atmospheres of transiting exoplanets) and MuSCAT2 instruments obtained between 2016 and 2021 in g, r, i, zs-filters. We conducted an automated flare search and visually confirmed possible flare events. The black body temperatures were inferred directly from the spectral energy distribution (SED) by extrapolating the filter-specific flux. We studied the temperature evolution, the global temperature, and the peak temperature of both flares.
Results: White-light M-dwarf flares are frequently described in the literature by a black body with a temperature of 9000-10 000 K. For the first time we infer effective black body temperatures of flares that occurred on TRAPPIST-1. The black body temperatures for the two TRAPPIST-1 flares derived from the SED are consistent with TSED = 7940−390+430 K and TSED = 6030−270+300 K. The flare black body temperatures at the peak are also calculated from the peak SED yielding TSEDp = 13 620−1220+1520 K and TSEDp = 8290−550+660 K. We update the flare frequency distribution of TRAPPIST-1 and discuss the impacts of lower black body temperatures on exoplanet habitability.
Conclusions: We show that for the ultra-cool M-dwarf TRAPPIST-1 the flare black body temperatures associated with the total continuum emission are lower and not consistent with the usually adopted assumption of 9000-10 000 K in the context of exoplanet research. For the peak emission, both flares seem to be consistent with the typical range from 9000 to 14 000 K, respectively. This could imply different and faster cooling mechanisms. Further multi-color observations are needed to investigate whether or not our observations are a general characteristic of ultra-cool M-dwarfs. This would have significant implications for the habitability of exoplanets around these stars because the UV surface flux is likely to be overestimated by the models with higher flare temperatures.

The photometry of the two flares in g, r, i, and zs filters is only available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/668/A111


RU-D
(870)Comets and Planetesimal Formation
  • Jacob B. Simon,
  • Jürgen Blum,
  • Til Birnstiel,
  • David Nesvorný
abstract + abstract -

In this chapter, we review the processes involved in the formation of planetesimals and comets. We will start with a description of the physics of dust grain growth and how this is mediated by gas-dust interactions in planet-forming disks. We will then delve into the various models of planetesimal formation, describing how these planetesimals form as well as their resulting structure. In doing so, we focus on and compare two paradigms for planetesimal formation: the gravitational collapse of particle over-densities (which can be produced by a variety of mechanisms) and the growth of particles into planetesimals via collisional and gravitational coagulation. Finally, we compare the predictions from these models with data collected by the Rosetta and New Horizons missions and that obtained via observations of distant Kuiper Belt Objects.


(869)Condensed dark matter with a Yukawa interaction
  • Raghuveer Garani,
  • Michel H. G. Tytgat,
  • Jérôme Vandecasteele
Physical Review D (12/2022) doi:10.1103/PhysRevD.106.116003
abstract + abstract -

We explore the possible phases of a condensed dark matter (DM) candidate taken to be in the form of a fermion with a Yukawa coupling to a scalar particle, at zero temperature but at finite density. This theory essentially depends on only four parameters, the Yukawa coupling, the fermion mass, the scalar mediator mass, and the DM density. At low-fermion densities we delimit the Bardeen-Cooper-Schrieffer (BCS), Bose-Einstein condensate (BEC), and crossover phases as a function of model parameters using the notion of scattering length. We further study the BCS phase by consistently including emergent effects such as the scalar-density condensate and superfluid gaps. Within the mean-field approximation, we derive the consistent set of gap equations, retaining their momentum dependence, and valid in both the nonrelativistic and relativistic regimes. We present numerical solutions to the set of gap equations, in particular when the mediator mass is smaller and larger than the DM mass. Finally, we discuss the equation of state and possible astrophysical implications for asymmetric DM.


CN-2
RU-D
(868)Interpreting molecular hydrogen and atomic oxygen line emission of T Tauri disks with photoevaporative disk-wind models
  • Ch. Rab,
  • M. Weber,
  • T. Grassi,
  • B. Ercolano,
  • G. Picogna
  • +4
  • P. Caselli,
  • W. -F. Thi,
  • I. Kamp,
  • P. Woitke
  • (less)
Astronomy and Astrophysics (12/2022) doi:10.1051/0004-6361/202244362
abstract + abstract -

Context. Winds in protoplanetary disks play an important role in their evolution and dispersal. However, the physical process that is actually driving the winds is still unclear (i.e. magnetically versus thermally driven), and can only be understood by directly confronting theoretical models with observational data.
Aims: We aim to interpret observational data for molecular hydrogen and atomic oxygen lines that show kinematic disk-wind signatures in order to investigate whether or not purely thermally driven winds are consistent with the data.
Methods: We use hydrodynamic photoevaporative disk-wind models and post-process them with a thermochemical model to produce synthetic observables for the spectral lines o-H2 1-0 S(1) at 2.12 µm and [OI] 1D2-3P2 at 0.63 µm and directly compare the results to a sample of observations.
Results: We find that our photoevaporative disk-wind model is consistent with the observed signatures of the blueshifted narrow low-velocity component (NLVC) - which is usually associated with slow disk winds - for both tracers. Only for one out of seven targets that show blueshifted NLVCs does the photoevaporative model fail to explain the observed line kinematics. Our results also indicate that interpreting spectral line profiles using simple methods, such as the thin-disk approximation, to determine the line emitting region is not appropriate for the majority of cases and can yield misleading conclusions. This is due to the complexity of the line excitation, wind dynamics, and the impact of the actual physical location of the line-emitting regions on the line profiles.
Conclusions: The photoevaporative disk-wind models are largely consistent with the studied observational data set, but it is not possible to clearly discriminate between different wind-driving mechanisms. Further improvements to the models are necessary, such as consistent modelling of the dynamics and chemistry, and detailed modelling of individual targets (i.e. disk structure) would be beneficial. Furthermore, a direct comparison of magnetically driven disk-wind models to the observational data set is necessary in order to determine whether or not spatially unresolved observations of multiple wind tracers are sufficient to discriminate between theoretical models.


(867)Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers
  • H. -Thomas Janka,
  • Andreas Bauswein
abstract + abstract -

Neutron stars (NSs) and black holes (BHs) are born when the final collapse of the stellar core terminates the lives of stars more massive than about 9 Msun. This can trigger the powerful ejection of a large fraction of the star's material in a core-collapse supernova (CCSN), whose extreme luminosity is energized by the decay of radioactive isotopes such as 56Ni and 56Co. When evolving in close binary systems, the compact relics of such infernal catastrophes spiral towards each other on orbits gradually decaying by gravitational-wave emission. Ultimately, the violent collision of the two components forms a more massive, rapidly spinning remnant, again accompanied by the ejection of considerable amounts of matter. These merger events can be observed by high-energy bursts of gamma rays with afterglows and electromagnetic transients called kilonovae, which radiate the energy released in radioactive decays of freshly assembled rapid neutron-capture elements. By means of their mass ejection and the nuclear and neutrino reactions taking place in the ejecta, both CCSNe and compact object mergers (COMs) are prominent sites of heavy-element nucleosynthesis and play a central role in the cosmic cycle of matter and the chemical enrichment history of galaxies. The nuclear equation of state (EoS) of NS matter, from neutron-rich to proton-dominated conditions and with temperatures ranging from about zero to ~100 MeV, is a crucial ingredient in these astrophysical phenomena. It determines their dynamical processes, their remnant properties even at the level of deciding between NS or BH, and the properties of the associated emission of neutrinos, whose interactions govern the thermodynamic conditions and the neutron-to-proton ratio for nucleosynthesis reactions in the innermost ejecta. This chapter discusses corresponding EoS dependent effects of relevance in CCSNe as well as COMs. (slightly abridged)


(866)The ESO-VLT MIKiS survey reloaded: exploring the internal kinematics of NGC 6440
  • Silvia Leanza,
  • Cristina Pallanca,
  • Francesco R. Ferraro,
  • Barbara Lanzoni,
  • Emanuele Dalessandro
  • +5
  • Mario Cadelano,
  • Enrico Vesperini,
  • Livia Origlia,
  • Alessio Mucciarelli,
  • Elena Valenti
  • (less)
abstract + abstract -

In the context of the ESO-VLT Multi-Instrument Kinematic Survey (MIKiS) of Galactic globular clusters, here we present the line-of-sight velocity dispersion profile of NGC 6440, a massive globular cluster located in the Galactic bulge. By combining the data acquired with four different spectrographs, we obtained the radial velocity of a sample of $\sim 1800$ individual stars distributed over the entire cluster extension, from $\sim$0.1$"$ to 778$"$ from the center. Using a properly selected sample of member stars with the most reliable radial velocity measures, we derived the velocity dispersion profile up to 250$"$ from the center. The profile is well described by the same King model that best fits the projected star density distribution, with a constant inner plateau (at ${\sigma}_0 \sim $ 12 km s$^{-1}$) and no evidence of a central cusp or other significant deviations. Our data allowed to study the presence of rotation only in the innermost regions of the cluster (r < 5$"$), revealing a well-defined pattern of ordered rotation with a position angle of the rotation axis of $\sim$132 $\pm$ 2° and an amplitude of $\sim$3 km s$^{-1}$ (corresponding to Vrot/${\sigma}_0 \sim$ 0.3). Also, a flattening of the system qualitatively consistent with the rotation signal has been detected in the central region.


RU-D
(865)Testing the Galaxy-collision-induced Formation Scenario for the Trail of Dark-matter-deficient Galaxies with the Susceptibility of Globular Clusters to the Tidal Force
  • Go Ogiya,
  • Frank C. van den Bosch,
  • Andreas Burkert,
  • Xi Kang
The Astrophysical Journal (12/2022) doi:10.3847/2041-8213/aca2a7
abstract + abstract -

It has been suggested that a trail of diffuse galaxies, including two dark-matter-deficient galaxies (DMDGs), in the vicinity of NGC 1052 formed because of a high-speed collision between two gas-rich dwarf galaxies, one bound to NGC 1052 and the other one on an unbound orbit. The collision compresses the gas reservoirs of the colliding galaxies, which in turn triggers a burst of star formation. In contrast, the dark matter and preexisting stars in the progenitor galaxies pass through it. Since the high pressures in the compressed gas are conducive to the formation of massive globular clusters (GCs), this scenario can explain the formation of DMDGs with large populations of massive GCs, consistent with the observations of NGC 1052-DF2 (DF2) and NGC 1052-DF4. A potential difficulty with this "mini bullet cluster" scenario is that the observed spatial distributions of GCs in DMDGs are extended. GCs experience dynamical friction causing their orbits to decay with time. Consequently, their distribution at formation should have been even more extended than that observed at present. Using a semianalytic model, we show that the observed positions and velocities of the GCs in DF2 imply that they must have formed at a radial distance of 5-10 kpc from the center of DF2. However, as we demonstrate, the scenario is difficult to reconcile with the fact that the strong tidal forces from NGC 1052 strip the extendedly distributed GCs from DF2, requiring 33-59 massive GCs to form at the collision to explain observations.


CN-4
RU-C
RU-D
(864)Rapid Simulations of Halo and Subhalo Clustering
  • Pascale Berner,
  • Alexandre Refregier,
  • Raphael Sgier,
  • Tomasz Kacprzak,
  • Luca Tortorelli
  • +1
abstract + abstract -

The analysis of cosmological galaxy surveys requires realistic simulations for their interpretation. Forward modelling is a powerful method to simulate galaxy clustering without the need for an underlying complex model. This approach requires fast cosmological simulations with a high resolution and large volume, to resolve small dark matter halos associated to single galaxies. In this work, we present fast halo and subhalo clustering simulations based on the Lagrangian perturbation theory code PINOCCHIO, which generates halos and merger trees. The subhalo progenitors are extracted from the merger history and the survival of subhalos is modelled. We introduce a new fitting function for the subhalo merger time, which includes a redshift dependence of the fitting parameters. The spatial distribution of subhalos within their hosts is modelled using a number density profile. We compare our simulations with the halo finder ROCKSTAR applied to the full N-body code GADGET-2. The subhalo velocity function and the correlation function of halos and subhalos are in good agreement. We investigate the effect of the chosen number density profile on the resulting subhalo clustering. Our simulation is approximate yet realistic and significantly faster compared to a full N-body simulation combined with a halo finder. The fast halo and subhalo clustering simulations offer good prospects for galaxy forward models using subhalo abundance matching.


MIAPbP
(863)B-meson decay into a proton and dark antibaryon from QCD light-cone sum rules
  • Alexander Khodjamirian,
  • Marcel Wald
Physics Letters B (11/2022) doi:10.1016/j.physletb.2022.137434
abstract + abstract -

The recently developed B-Mesogenesis scenario predicts decays of B mesons into a baryon and hypothetical dark antibaryon Ψ. We suggest a method to calculate the amplitude of the simplest exclusive decay mode B+ → pΨ. Considering two models of B-Mesogenesis, we obtain the B → p hadronic matrix elements by applying QCD light-cone sum rules with the proton light-cone distribution amplitudes. We estimate the B+ → pΨ decay width as a function of the mass and effective coupling of the dark antibaryon.


MIAPbP
(862)Primordial dusty rings and episodic outbursts in protoplanetary discs
  • Kundan Kadam,
  • Eduard Vorobyov,
  • Shantanu Basu
Monthly Notices of the Royal Astronomical Society (11/2022) doi:10.1093/mnras/stac2455
abstract + abstract -

We investigate the formation and evolution of 'primordial' dusty rings occurring in the inner regions of protoplanetary discs, with the help of long-term, coupled dust-gas, magnetohydrodynamic simulations. The simulations are global and start from the collapse phase of the parent cloud core, while the dead zone is calculated via an adaptive α formulation by taking into account the local ionization balance. The evolution of the dusty component includes its growth and back reaction on to the gas. Previously, using simulations with only a gas component, we showed that dynamical rings form at the inner edge of the dead zone. We find that when dust evolution, as well as magnetic field evolution in the flux-freezing limit are included, the dusty rings formed are more numerous and span a larger radial extent in the inner disc, while the dead zone is more robust and persists for a much longer time. We show that these dynamical rings concentrate enough dust mass to become streaming unstable, which should result in a rapid planetesimal formation even in the embedded phases of the system. The episodic outbursts caused by the magnetorotational instability have a significant impact on the evolution of the rings. The outbursts drain the inner disc of grown dust, however, the period between bursts is sufficiently long for the planetesimal growth via streaming instability. The dust mass contained within the rings is large enough to ultimately produce planetary systems with the core accretion scenario. The low-mass systems rarely undergo outbursts, and, thus, the conditions around such stars can be especially conducive for planet formation.


CN-4
(861)Toolkit for Scalar Fields in Universes with finite-dimensional Hilbert Space
  • Oliver Friedrich,
  • Ashmeet Singh,
  • Olivier Doré
Class. Quantum Grav. (11/2022) e-Print:2201.08405 doi:10.1088/1361-6382/ac95f0
abstract + abstract -

The holographic principle suggests that the Hilbert space of quantum gravity is locally finite-dimensional. Motivated by this point-of-view, and its application to the observable Universe, we introduce a set of numerical and conceptual tools to describe scalar fields with finite-dimensional Hilbert spaces, and to study their behaviour in expanding cosmological backgrounds. These tools include accurate approximations to compute the vacuum energy of a field mode k as a function of the dimension dk of the mode Hilbert space, as well as a parametric model for how that dimension varies with |k|. We show that the maximum entropy of our construction momentarily scales like the boundary area of the observable Universe for some values of the parameters of that model. And we find that the maximum entropy generally follows a sub-volume scaling as long as dk decreases with |k|. We also demonstrate that the vacuum energy density of the finite-dimensional field is dynamical and decays between two constant epochs in our fiducial construction. These results rely on a number of non-trivial modelling choices, but our general framework may serve as a starting point for future investigations of the impact of finite-dimensionality of Hilbert space on cosmological physics.


(860)Production of loosely bound hadron molecules from bottomonium decays
  • Davide Marietti,
  • Alessandro Pilloni,
  • Umberto Tamponi
Physical Review D (11/2022) doi:10.1103/PhysRevD.106.094040
abstract + abstract -

We present multiple results on the production of loosely bound molecules in bottomonium annihilations and e+e- collisions at √{s }=10.58 GeV . We perform the first comprehensive test of several models for deuteron production against all the existing data in this energy region. We fit the free parameters of the models to reproduce the observed cross sections, and we predict the deuteron spectrum and production and the cross section for the e+e-→d d ¯+X process both at the ϒ (1 ,2 ,3 S ) resonances and at √{s }=10.58 GeV . The predicted spectra show differences but are all compatible with the uncertainties of the existing data. These differences could be addressed if larger datasets are collected by the Belle II experiment. Fixing the source size parameter to reproduce the deuteron data, we then predict the production rates for H dibaryon and hypertriton in this energy region using a simple coalescence model. Our prediction on the H dibaryon production rate is below the limits set by the direct search at the Belle experiment, but in the range accessible to the Belle II experiment. The systematic effect due to the MC modeling of quarks and gluon fragmentation into baryons is reduced, deriving a new tuning of the PYTHIA 8 Monte Carlo generator using the available measurement of single- and double-particle spectra in ϒ decays.


CN-3
CN-4
RU-C
RU-D
(859)Euclid: Cosmological forecasts from the void size function
  • S. Contarini,
  • G. Verza,
  • A. Pisani,
  • N. Hamaus,
  • M. Sahlén
  • +121
  • C. Carbone,
  • S. Dusini,
  • F. Marulli,
  • L. Moscardini,
  • A. Renzi,
  • C. Sirignano,
  • L. Stanco,
  • M. Aubert,
  • M. Bonici,
  • G. Castignani,
  • H. M. Courtois,
  • S. Escoffier,
  • D. Guinet,
  • A. Kovacs,
  • G. Lavaux,
  • E. Massara,
  • S. Nadathur,
  • G. Pollina,
  • T. Ronconi,
  • F. Ruppin,
  • Z. Sakr,
  • A. Veropalumbo,
  • B. D. Wandelt,
  • A. Amara,
  • N. Auricchio,
  • M. Baldi,
  • D. Bonino,
  • E. Branchini,
  • M. Brescia,
  • J. Brinchmann,
  • S. Camera,
  • V. Capobianco,
  • J. Carretero,
  • M. Castellano,
  • S. Cavuoti,
  • R. Cledassou,
  • G. Congedo,
  • C. J. Conselice,
  • L. Conversi,
  • Y. Copin,
  • L. Corcione,
  • F. Courbin,
  • M. Cropper,
  • A. Da Silva,
  • H. Degaudenzi,
  • F. Dubath,
  • C. A. J. Duncan,
  • X. Dupac,
  • A. Ealet,
  • S. Farrens,
  • S. Ferriol,
  • P. Fosalba,
  • M. Frailis,
  • E. Franceschi,
  • B. Garilli,
  • W. Gillard,
  • B. Gillis,
  • C. Giocoli,
  • A. Grazian,
  • F. Grupp,
  • L. Guzzo,
  • S. Haugan,
  • W. Holmes,
  • F. Hormuth,
  • K. Jahnke,
  • M. Kümmel,
  • S. Kermiche,
  • A. Kiessling,
  • M. Kilbinger,
  • M. Kunz,
  • H. Kurki-Suonio,
  • R. Laureijs,
  • S. Ligori,
  • P. B. Lilje,
  • I. Lloro,
  • E. Maiorano,
  • O. Mansutti,
  • O. Marggraf,
  • K. Markovic,
  • R. Massey,
  • M. Melchior,
  • M. Meneghetti,
  • G. Meylan,
  • M. Moresco,
  • E. Munari,
  • S. M. Niemi,
  • C. Padilla,
  • S. Paltani,
  • F. Pasian,
  • K. Pedersen,
  • W. J. Percival,
  • V. Pettorino,
  • S. Pires,
  • G. Polenta,
  • M. Poncet,
  • L. Popa,
  • L. Pozzetti,
  • F. Raison,
  • J. Rhodes,
  • E. Rossetti,
  • R. Saglia,
  • B. Sartoris,
  • P. Schneider,
  • A. Secroun,
  • G. Seidel,
  • G. Sirri,
  • C. Surace,
  • P. Tallada-Crespí,
  • A. N. Taylor,
  • I. Tereno,
  • R. Toledo-Moreo,
  • F. Torradeflot,
  • E. A. Valentijn,
  • L. Valenziano,
  • Y. Wang,
  • J. Weller,
  • G. Zamorani,
  • J. Zoubian,
  • S. Andreon,
  • D. Maino,
  • S. Mei
  • (less)
Astronomy and Astrophysics (11/2022) doi:10.1051/0004-6361/202244095
abstract + abstract -

The Euclid mission - with its spectroscopic galaxy survey covering a sky area over 15 000 deg2 in the redshift range 0.9 < z < 1.8 - will provide a sample of tens of thousands of cosmic voids. This paper thoroughly explores for the first time the constraining power of the void size function on the properties of dark energy (DE) from a survey mock catalogue, the official Euclid Flagship simulation. We identified voids in the Flagship light-cone, which closely matches the features of the upcoming Euclid spectroscopic data set. We modelled the void size function considering a state-of-the art methodology: we relied on the volume-conserving (Vdn) model, a modification of the popular Sheth & van de Weygaert model for void number counts, extended by means of a linear function of the large-scale galaxy bias. We found an excellent agreement between model predictions and measured mock void number counts. We computed updated forecasts for the Euclid mission on DE from the void size function and provided reliable void number estimates to serve as a basis for further forecasts of cosmological applications using voids. We analysed two different cosmological models for DE: the first described by a constant DE equation of state parameter, w, and the second by a dynamic equation of state with coefficients w0 and wa. We forecast 1σ errors on w lower than 10% and we estimated an expected figure of merit (FoM) for the dynamical DE scenario FoMw0, wa = 17 when considering only the neutrino mass as additional free parameter of the model. The analysis is based on conservative assumptions to ensure full robustness, and is a pathfinder for future enhancements of the technique. Our results showcase the impressive constraining power of the void size function from the Euclid spectroscopic sample, both as a stand-alone probe, and to be combined with other Euclid cosmological probes.

This paper is published on behalf of the Euclid Consortium.


(858)Structure of axion miniclusters
  • David Ellis,
  • David J. E. Marsh,
  • Benedikt Eggemeier,
  • Jens Niemeyer,
  • Javier Redondo
  • +1
Physical Review D (11/2022) doi:10.1103/PhysRevD.106.103514
abstract + abstract -

The peak-patch algorithm is used to identify the densest minicluster seeds in the initial axion density field simulated from string decay. The fate of these dense seeds is found by tracking the subsequent gravitational collapse in cosmological N -body simulations. We find that miniclusters at late times are well described by Navarro-Frenk-White profiles, although for around 80% of simulated miniclusters a single power-law density profile of r-2.9 is an equally good fit due to the unresolved scale radius. Under the assumption that all miniclusters with an unresolved scale radius are described by a power-law plus axion star density profile, we identify a significant number of miniclusters that might be dense enough to give rise to gravitational microlensing if the axion mass is 0.2 meV ≲ma≲3 meV . Higher resolution simulations resolving the inner structure and axion star formation are necessary to explore this possibility further.


(857)Polarization Modulator Unit Harness Thermal Design for the Mid- and High-Frequency Telescopes of the LiteBIRD Space Mission
  • F. Columbro,
  • P. de Bernardis,
  • S. Masi
Journal of Low Temperature Physics (11/2022) doi:10.1007/s10909-022-02919-1
abstract + abstract -

Polarization modulator units (PMUs) represent a critical and powerful component in CMB polarization experiments to suppress the 1/f noise component and mitigate systematic uncertainties induced by detector gain drifts and beam asymmetries. The LiteBIRD mission (expected launch in the late 2020 s) will be equipped with 3 PMUs, one for each of the 3 telescopes, and aims at detecting the primordial gravitational waves with a sensitivity of δ r <0.001 . Each PMU is based on a continuously rotating transmissive half-wave plate held by a superconducting magnetic bearing in the 5 K environment. To achieve and monitor the rotation a number of subsystems is needed: clamp and release system and motor coils for the rotation; optical encoder, capacitive, Hall and temperature sensors to monitor its dynamic stability. In this contribution, we present a preliminary thermal design of the harness configuration for the PMUs of the mid- and high- frequency telescopes. The design is based on both the stringent system constraint for the total thermal budget available for the PMUs (≲ 4 mW at 5 K) and on the requirements for different subsystem: coils currents (up to 10 mA), optical fibers for encoder readout, 25 MHz bias signal for temperature and levitation monitors.


(856)Toy models for hierarchy studies
  • Clara Álvarez-Luna,
  • José A. R. Cembranos,
  • Juan José Sanz-Cillero
European Physical Journal C (11/2022) doi:10.1140/epjc/s10052-022-11014-4
abstract + abstract -

We provide a simple computation in order to estimate the probability of a given hierarchy between two scales. In particular, we work in a model provided with a gauge symmetry, with two scalar doublets. We start from a scale-invariant classical Lagrangian, but by taking into account the Coleman-Weinberg mechanism, we obtain masses for the gauge bosons and the scalars. This approach typically provides a light (L) and a heavy (H) sector related to the two different vacuum expectation values of the two scalars. We compute the size of the hypervolume of the parameter space of the model associated with an interval of mass ratios between these two sectors. We define the probability as proportional to this size and conclude that probabilities of very large hierarchies are not negligible in the type of models studied in this work.


CN-7
(855)Neutrino fast flavor pendulum. II. Collisional damping
  • Ian Padilla-Gay,
  • Irene Tamborra,
  • Georg G. Raffelt
abstract + abstract -

In compact astrophysical objects, the neutrino density can be so high that neutrino-neutrino refraction can lead to fast flavor conversion of the kind νeν¯e↔νxν¯x with x =μ , τ , depending on the neutrino angle distribution. Previously, we have shown that in a homogeneous, axisymmetric two-flavor system, these collective solutions evolve in analogy to a gyroscopic pendulum. In flavor space, its deviation from the weak-interaction direction is quantified by a variable cos ϑ that moves between +1 and cos ϑmin, the latter following from a linear mode analysis. As a next step, we include collisional damping of flavor coherence, assuming a common damping rate Γ for all modes. Empirically we find that the damped pendular motion reaches an asymptotic level of pair conversion f =A +(1 -A )cos ϑmin (numerically A ≃0.370 ) that does not depend on details of the angular distribution (except for fixing cos ϑmin), the initial seed, nor Γ . On the other hand, even a small asymmetry between the neutrino and antineutrino damping rates strongly changes this picture and can even enable flavor instabilities in otherwise stable systems.


CN-3
RU-B
(854)Testing spin-dependent dark matter interactions with lithium aluminate targets in CRESST-III
  • G. Angloher,
  • S. Banik,
  • G. Benato,
  • A. Bento,
  • A. Bertolini
  • +57
  • R. Breier,
  • C. Bucci,
  • J. Burkhart,
  • 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,
  • S. Gerster,
  • P. Gorla,
  • P. V. Guillaumon,
  • S. Gupta,
  • D. Hauff,
  • M. Ješkovský,
  • J. Jochum,
  • M. Kaznacheeva,
  • A. Kinast,
  • H. Kluck,
  • H. Kraus,
  • A. Langenkämper,
  • M. Mancuso,
  • L. Marini,
  • L. Meyer,
  • V. Mokina,
  • A. Nilima,
  • M. Olmi,
  • T. Ortmann,
  • C. Pagliarone,
  • 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,
  • CRESST Collaboration
  • (less)
Physical Review D (11/2022) doi:10.1103/PhysRevD.106.092008
abstract + abstract -

In the past decades, numerous experiments have emerged to unveil the nature of dark matter, one of the most discussed open questions in modern particle physics. Among them, the Cryogenic Rare Event Search with Superconducting Thermometers (CRESST) experiment, located at the Laboratori Nazionali del Gran Sasso, operates scintillating crystals as cryogenic phonon detectors. In this work, we present first results from the operation of two detector modules which both have 10.46 g LiAlO2 targets in CRESST-III. The lithium contents in the crystal are Li 6 , with an odd number of protons and neutrons, and Li 7 , with an odd number of protons. By considering both isotopes of lithium and Al 27 , we set the currently strongest cross section upper limits on spin-dependent interaction of dark matter with protons and neutrons for the mass region between 0.25 and 1.5 GeV /c2 .


(853)Ammonia in the interstellar medium of a starbursting disc at z = 2.6
  • M. J. Doherty,
  • J. E. Geach,
  • R. J. Ivison,
  • K. M. Menten,
  • A. M. Jacob
  • +2
Monthly Notices of the Royal Astronomical Society (11/2022) doi:10.1093/mnrasl/slac111
abstract + abstract -

We report the detection of the ground state rotational emission of ammonia, ortho-NH3 (JK = 10 → 00) in a gravitationally lensed intrinsically hyperluminous star-bursting galaxy at z = 2.6. The integrated line profile is consistent with other molecular and atomic emission lines which have resolved kinematics well modelled by a 5 kpc-diameter rotating disc. This implies that the gas responsible for NH3 emission is broadly tracing the global molecular reservoir, but likely distributed in pockets of high density (n ≳ 5 × 104 cm-3). With a luminosity of 2.8 × 106 L, the NH3 emission represents 2.5 × 10-7 of the total infrared luminosity of the galaxy, comparable to the ratio observed in the Kleinmann-Low nebula in Orion and consistent with sites of massive star formation in the Milky Way. If $L_{\rm NH_3}/L_{\rm IR}$ serves as a proxy for the 'mode' of star formation, this hints that the nature of star formation in extreme starbursts in the early Universe is similar to that of Galactic star-forming regions, with a large fraction of the cold interstellar medium in this state, plausibly driven by a storm of violent disc instabilities in the gas-dominated disc. This supports the 'full of Orions' picture of star formation in the most extreme galaxies seen close to the peak epoch of stellar mass assembly.


CN-6
(852)Evidence for neutrino emission from the nearby active galaxy NGC 1068
  • IceCube Collaboration: R. Abbasi,
  • M. Ackermann,
  • J. Adams,
  • J. A. Aguilar,
  • M. Ahlers
  • +380
  • M. Ahrens,
  • J.M. Alameddine,
  • C. Alispach,
  • A. A. Alves Jr.,
  • N. M. Amin,
  • K. Andeen,
  • T. Anderson,
  • G. Anton,
  • C. Argüelles,
  • Y. Ashida,
  • S. Axani,
  • X. Bai,
  • A. Balagopal V.,
  • A. Barbano,
  • S. W. Barwick,
  • B. Bastian,
  • V. Basu,
  • S. Baur,
  • R. Bay,
  • J. J. Beatty,
  • K.-H. Becker,
  • J. Becker Tjus,
  • C. Bellenghi,
  • S. BenZvi,
  • D. Berley,
  • E. Bernardini,
  • D. Z. Besson,
  • G. Binder,
  • D. Bindig,
  • E. Blaufuss,
  • S. Blot,
  • M. Boddenberg,
  • F. Bontempo,
  • J. Borowka,
  • S. Böser,
  • O. Botner,
  • J. Böttcher,
  • E. Bourbeau,
  • F. Bradascio,
  • J. Braun,
  • B. Brinson,
  • S. Bron,
  • J. Brostean-Kaiser,
  • S. Browne,
  • A. Burgman,
  • R. T. Burley,
  • R. S. Busse,
  • M. A. Campana,
  • E. G. Carnie-Bronca,
  • C. Chen,
  • Z. Chen,
  • D. Chirkin,
  • K. Choi,
  • B. A. Clark,
  • K. Clark,
  • L. Classen,
  • A. Coleman,
  • G. H. Collin,
  • J. M. Conrad,
  • P. Coppin,
  • P. Correa,
  • D. F. Cowen,
  • R. Cross,
  • C. Dappen,
  • P. Dave,
  • C. De Clercq,
  • J. J. DeLaunay,
  • D. Delgado López,
  • H. Dembinski,
  • K. Deoskar,
  • A. Desai,
  • P. Desiati,
  • K. D. de Vries,
  • G. de Wasseige,
  • M. de With,
  • T. DeYoung,
  • A. Diaz,
  • J. C. Díaz-Vélez,
  • M. Dittmer,
  • H. Dujmovic,
  • M. Dunkman,
  • M. A. DuVernois,
  • E. Dvorak,
  • T. Ehrhardt,
  • P. Eller,
  • R. Engel,
  • H. Erpenbeck,
  • J. Evans,
  • P. A. Evenson,
  • K. L. Fan,
  • A. R. Fazely,
  • A. Fedynitch,
  • N. Feigl,
  • S. Fiedlschuster ,
  • A. T. Fienberg,
  • K. Filimonov,
  • C. Finley,
  • L. Fischer,
  • D. Fox,
  • A. Franckowiak,
  • E. Friedman,
  • A. Fritz,
  • P. Fürst,
  • T. K. Gaisser,
  • J. Gallagher,
  • E. Ganster,
  • A. Garcia,
  • S. Garrappa,
  • L. Gerhardt,
  • A. Ghadimi,
  • C. Glaser,
  • T. Glauch,
  • T. Glüsenkamp,
  • A. Goldschmidt,
  • J. G. Gonzalez,
  • S. Goswami,
  • D. Grant,
  • T. Grégoire,
  • S. Griswold,
  • C. Günther,
  • P. Gutjahr,
  • C. Haack,
  • A. Hallgren,
  • R. Halliday,
  • L. Halve,
  • F. Halzen,
  • M. Ha Minh,
  • K. Hanson,
  • J. Hardin,
  • A. A. Harnisch,
  • A. Haungs,
  • D. Hebecker,
  • K. Helbing,
  • F. Henningsen,
  • E. C. Hettinger,
  • S. Hickford,
  • J. Hignight,
  • C. Hill,
  • G. C. Hill,
  • K. D. Hoffman,
  • R. Hoffmann,
  • B. Hokanson-Fasig,
  • K. Hoshina,
  • F. Huang,
  • M. Huber,
  • T. Huber,
  • K. Hultqvist,
  • M. Hünnefeld,
  • R. Hussain,
  • K. Hymon,
  • S. In,
  • N. Iovine,
  • A. Ishihara,
  • M. Jansson,
  • G. S. Japaridze,
  • M. Jeong,
  • M. Jin,
  • B. J. P. Jones,
  • D. Kang,
  • W. Kang,
  • X. Kang,
  • A. Kappes,
  • D. Kappesser,
  • L. Kardum,
  • T. Karg,
  • M. Karl,
  • A. Karle,
  • U. Katz,
  • M. Kauer,
  • M. Kellermann,
  • J. L. Kelley,
  • A. Kheirandish,
  • K. Kin,
  • T. Kintscher,
  • J. Kiryluk,
  • S. R. Klein,
  • R. Koirala,
  • H. Kolanoski,
  • T. Kontrimas,
  • L. Köpke,
  • C. Kopper,
  • S. Kopper,
  • D. J. Koskinen,
  • P. Koundal,
  • M. Kovacevich,
  • M. Kowalski,
  • T. Kozynets,
  • E. Kun,
  • N. Kurahashi,
  • N. Lad,
  • C. Lagunas Gualda,
  • J. L. Lanfranchi,
  • M. J. Larson,
  • F. Lauber,
  • J. P. Lazar,
  • J. W. Lee,
  • K. Leonard,
  • A. Leszczyńska,
  • Y. Li,
  • M. Lincetto,
  • Q. R. Liu,
  • M. Liubarska,
  • E. Lohfink,
  • C. J. Lozano Mariscal,
  • L. Lu,
  • F. Lucarelli,
  • A. Ludwig,
  • W. Luszczak,
  • Y. Lyu,
  • W. Y. Ma,
  • J. Madsen,
  • K. B. M. Mahn,
  • Y. Makino,
  • S. Mancina,
  • I. C. Mariş,
  • I. Martinez-Soler,
  • R. Maruyama,
  • K. Mase,
  • T. McElroy,
  • F. McNally,
  • J. V. Mead,
  • K. Meagher,
  • S. Mechbal,
  • A. Medina,
  • M. Meier,
  • S. Meighen-Berger,
  • J. Micallef,
  • D. Mockler,
  • T. Montaruli,
  • R. W. Moore,
  • R. Morse,
  • M. Moulai,
  • R. Naab,
  • R. Nagai,
  • R. Nahnhauer,
  • U. Naumann,
  • J. Necker,
  • L. V. Nguyên,
  • H. Niederhausen,
  • M. U. Nisa,
  • S. C. Nowicki,
  • D. Nygren,
  • A. Obertacke Pollmann,
  • M. Oehler,
  • B. Oeyen,
  • A. Olivas,
  • E. O'Sullivan,
  • H. Pandya,
  • D. V. Pankova,
  • N. Park,
  • G. K. Parker,
  • E. N. Paudel,
  • L. Paul,
  • C. Pérez de los Heros,
  • L. Peters,
  • J. Peterson,
  • S. Philippen,
  • S. Pieper,
  • M. Pittermann,
  • A. Pizzuto,
  • M. Plum,
  • Y. Popovych,
  • A. Porcelli,
  • M. Prado Rodriguez,
  • P. B. Price,
  • B. Pries,
  • G. T. Przybylski,
  • C. Raab,
  • J. Rack-Helleis,
  • A. Raissi,
  • M. Rameez,
  • K. Rawlins,
  • I. C. Rea,
  • A. Rehman,
  • P. Reichherzer,
  • R. Reimann,
  • G. Renzi,
  • E. Resconi,
  • S. Reusch,
  • W. Rhode,
  • M. Richman,
  • B. Riedel,
  • E. J. Roberts,
  • S. Robertson,
  • G. Roellinghoff,
  • M. Rongen,
  • C. Rott,
  • T. Ruhe,
  • D. Ryckbosch,
  • D. Rysewyk Cantu,
  • I. Safa,
  • J. Saffer,
  • S. E. Sanchez Herrera,
  • A. Sandrock,
  • J. Sandroos,
  • M. Santander,
  • S. Sarkar,
  • S. Sarkar,
  • K. Satalecka,
  • M. Schaufel,
  • H. Schieler,
  • S. Schindler,
  • T. Schmidt,
  • A. Schneider,
  • J. Schneider,
  • F. G. Schröder,
  • L. Schumacher,
  • G. Schwefer,
  • S. Sclafani,
  • D. Seckel,
  • S. Seunarine,
  • A. Sharma,
  • S. Shefali,
  • M. Silva,
  • B. Skrzypek,
  • B. Smithers,
  • R. Snihur,
  • J. Soedingrekso,
  • D. Soldin,
  • C. Spannfellner,
  • G. M. Spiczak,
  • C. Spiering,
  • J. Stachurska,
  • M. Stamatikos,
  • T. Stanev,
  • R. Stein,
  • J. Stettner,
  • A. Steuer,
  • T. Stezelberger,
  • R. Stokstad,
  • T. Stürwald,
  • T. Stuttard,
  • G. W. Sullivan,
  • I. Taboada,
  • S. Ter-Antonyan,
  • S. Tilav,
  • F. Tischbein,
  • K. Tollefson,
  • C. Tönnis,
  • S. Toscano,
  • D. Tosi,
  • A. Trettin,
  • M. Tselengidou,
  • C. F. Tung,
  • A. Turcati,
  • R. Turcotte,
  • C. F. Turley,
  • J. P. Twagirayezu,
  • B. Ty,
  • M. A. Unland Elorrieta,
  • N. Valtonen-Mattila,
  • J. Vandenbroucke,
  • N. van Eijndhoven,
  • D. Vannerom,
  • J. van Santen,
  • S. Verpoest,
  • C. Walck,
  • T. B. Watson,
  • C. Weaver,
  • P. Weigel,
  • A. Weindl,
  • M. J. Weiss,
  • J. Weldert,
  • C. Wendt,
  • J. Werthebach,
  • M. Weyrauch,
  • N. Whitehorn,
  • C. H. Wiebusch,
  • D. R. Williams,
  • M. Wolf,
  • K. Woschnagg,
  • G. Wrede,
  • J. Wulff,
  • X. W. Xu,
  • J. P. Yanez,
  • S. Yoshida,
  • S. Yu,
  • T. Yuan,
  • Z. Zhang,
  • P. Zhelnin
  • (less)
abstract + abstract -

We report three searches for high energy neutrino emission from astrophysical objects using data recorded with IceCube between 2011 and 2020. Improvements over previous work include new neutrino reconstruction and data calibration methods. In one search, the positions of 110 a priori selected gamma-ray sources were analyzed individually for a possible surplus of neutrinos over atmospheric and cosmic background expectations. We found an excess of 79+22−20 neutrinos associated with the nearby active galaxy NGC 1068 at a significance of 4.2σ. The excess, which is spatially consistent with the direction of the strongest clustering of neutrinos in the Northern Sky, is interpreted as direct evidence of TeV neutrino emission from a nearby active galaxy. The inferred flux exceeds the potential TeV gamma-ray flux by at least one order of magnitude.


CN-2
RU-E
(851)Selective Phosphorylation of RNA- and DNA-Nucleosides under Prebiotically Plausible Conditions
  • M. Bechtel,
  • E. Hümmer,
  • O. Trapp
ChemSystemsChem (11/2022) doi:10.1002/syst.202200020
abstract + abstract -

Nucleotides play a fundamental role in organisms, from adenosine triphosphate (ATP), the body‘s main source of energy, to cofactors of enzymatic reactions (e. g. coenzyme A), to nucleoside monophosphates as essential building blocks of deoxyribonucleic acid (DNA) and ribonucleic acid (RNA). Although nucleotides play such an elemental role, there is no pathway to date for the selective formation of nucleoside 5′-monophosphates. Here, we demonstrate a selective reaction pathway for 5’ mono-phosphorylation for all canonical purine and pyrimidine bases under exceptionally mild prebiotic relevant conditions in water and without using a condensing agent. The pivotal reaction step involves activated imidazolidine-4-thione phosphates. The selective formation of non-cyclic mono-phosphorylated nucleosides represents a novel and unique route to nucleotides and opens exciting perspectives in the study of the origins of life.


CN-2
RU-E
(850)Phosphorylation in liquid sulfur dioxide under prebiotically plausible conditions
  • C. Sydow,
  • C. Seiband,
  • A. F. Siegle,
  • O. Trapp
Communications Chemistry (11/2022) doi:10.1038/s42004-022-00761-w
abstract + abstract -

In nature, organophosphates provide key functions such as information storage and transport, structural tasks, and energy transfer. Since condensations are unfavourable in water and nucleophilic attack at phosphate is kinetically inhibited, various abiogenesis hypotheses for the formation of organophosphate are discussed. Recently, the application of phosphites as phosphorylation agent showed promising results. However, elevated temperatures and additional reaction steps are required to obtain organophosphates. Here we show that in liquid sulfur dioxide, which acts as solvent and oxidant, efficient organophosphate formation is enabled. Phosphorous acid yields up to 32.6% 5′ nucleoside monophosphate, 3.6% 5′ nucleoside diphosphate, and the formation of nucleoside triphosphates and dinucleotides in a single reaction step at room temperature. In addition to the phosphorylation of organic compounds, we observed diserine formation. Thus, we suggest volcanic environments as reaction sites for biopolymer formation on Early Earth. Because of the simple recyclability of sulfur dioxide, the reaction is also interesting for synthesis chemistry.


RU-D
(849)A Neural Network Subgrid Model of the Early Stages of Planet Formation
  • Thomas Pfeil,
  • Miles Cranmer,
  • Shirley Ho,
  • Philip J. Armitage,
  • Tilman Birnstiel
  • +1
arXiv e-prints (11/2022) e-Print:2211.04160
abstract + abstract -

Planet formation is a multi-scale process in which the coagulation of $\mathrm{\mu m}$-sized dust grains in protoplanetary disks is strongly influenced by the hydrodynamic processes on scales of astronomical units ($\approx 1.5\times 10^8 \,\mathrm{km}$). Studies are therefore dependent on subgrid models to emulate the micro physics of dust coagulation on top of a large scale hydrodynamic simulation. Numerical simulations which include the relevant physical effects are complex and computationally expensive. Here, we present a fast and accurate learned effective model for dust coagulation, trained on data from high resolution numerical coagulation simulations. Our model captures details of the dust coagulation process that were so far not tractable with other dust coagulation prescriptions with similar computational efficiency.


(848)QuantumFDTD -- A computational framework for the relativistic Schrödinger equation
  • Rafael L. Delgado,
  • Sebastian Steinbeißer,
  • Michael Strickland,
  • Johannes H. Weber
arXiv e-prints (11/2022) e-Print:2211.10185
abstract + abstract -

We extend the publicly available quantumfdtd code. It was originally intended for solving the time-independent three-dimensional Schrödinger equation via the finite-difference time-domain (FDTD) method and for extracting the ground, first, and second excited states. We (a) include the case of the relativistic Schrödinger equation and (b) add two optimized FFT-based kinetic energy terms for the non-relativistic case. All the three new kinetic terms are computed using Fast Fourier Transform (FFT). We release the resulting code as version 3 of quantumfdtd. Finally, the code now supports arbitrary external file-based potentials and the option to project out distinct parity eigenstates from the solutions. Our goal is quark models used for phenomenological descriptions of QCD bound states, described by the three-dimensional Schrödinger equation. However, we target any field where solving either the non-relativistic or the relativistic three-dimensional Schrödinger equation is required.


CN-3
RU-B
(847)Proton Capture in Compact Dark Stars and Observable Implications
  • Boris Betancourt Kamenetskaia,
  • Anja Brenner,
  • Alejandro Ibarra,
  • Chris Kouvaris
Journal of Cosmology and Astroparticle Physics (11/2022) e-Print:2211.05845 doi:10.48550/arXiv.2211.05845
abstract + abstract -

Asymmetric dark matter under certain conditions could form compact star-like objects, which can be searched either through gravitational lensing or by observation of gravitational waves from binaries involving such compact objects. In this paper we analyze possible signatures of such dark stars made of asymmetric dark matter with a portal to the Standard Model. We argue that compact dark stars could capture protons and electrons from the interstellar medium, which then accumulate in the core of the dark star, forming a very hot gas that emits X-rays or $\gamma$-rays. For dark matter parameters compatible with current laboratory constraints, compact dark stars could be sufficiently luminous to be detected at the Earth as point sources in the X-ray or $\gamma$-ray sky.


(846)White dwarfs as a probe of light QCD axions
  • Reuven Balkin,
  • Javi Serra,
  • Konstantin Springmann,
  • Stefan Stelzl,
  • Andreas Weiler
arXiv e-prints (11/2022) e-Print:2211.02661
abstract + abstract -

We study the effects of light QCD axions on the stellar configuration of white dwarfs. At finite baryon density, the non-derivative coupling of the axion to nucleons displaces the axion from its in-vacuum minimum which implies a reduction of the nucleon mass. This dramatically alters the composition of stellar remnants. In particular, the modifications of the mass-radius relationship of white dwarfs allow us to probe large regions of unexplored axion parameter space without requiring it to be a significant fraction of dark matter.


(845)Novel approaches in hadron spectroscopy
  • Miguel Albaladejo,
  • Łukasz Bibrzycki,
  • Sebastian M. Dawid,
  • César Fernández-Ramírez,
  • Sergi Gonzàlez-Solís
  • +13
  • Astrid N. Hiller Blin,
  • Andrew W. Jackura,
  • Vincent Mathieu,
  • Mikhail Mikhasenko,
  • Victor I. Mokeev,
  • Emilie Passemar,
  • Alessandro Pilloni,
  • Arkaitz Rodas,
  • Jorge A. Silva-Castro,
  • Wyatt A. Smith,
  • Adam P. Szczepaniak,
  • Daniel Winney,
  • (Joint Physics Analysis Center)
  • (less)
Progress in Particle and Nuclear Physics (11/2022) doi:10.1016/j.ppnp.2022.103981
abstract + abstract -

The last two decades have witnessed the discovery of a myriad of new and unexpected hadrons. The future holds more surprises for us, thanks to new-generation experiments. Understanding the signals and determining the properties of the states requires a parallel theoretical effort. To make full use of available and forthcoming data, a careful amplitude modeling is required, together with a sound treatment of the statistical uncertainties, and a systematic survey of the model dependencies. We review the contributions made by the Joint Physics Analysis Center to the field of hadron spectroscopy.


CN-7
RU-D
(844)Cosmic nucleosynthesis: A multi-messenger challenge
  • Roland Diehl,
  • Andreas J. Korn,
  • Bruno Leibundgut,
  • Maria Lugaro,
  • Anton Wallner
Progress in Particle and Nuclear Physics (11/2022) doi:10.1016/j.ppnp.2022.103983
abstract + abstract -

The origins of the elements and isotopes of cosmic material is a critical aspect of understanding the evolution of the universe. Nucleosynthesis typically requires physical conditions of high temperatures and densities. These are found in the Big Bang, in the interiors of stars, and in explosions with their compressional shocks and high neutrino and neutron fluxes. Many different tools are available to disentangle the composition of cosmic matter, in material of extraterrestrial origins such as cosmic rays, meteorites, stardust grains, lunar and terrestrial sediments, and through astronomical observations across the electromagnetic spectrum. Understanding cosmic abundances and their evolution requires combining such measurements with approaches of astrophysical, nuclear theories and laboratory experiments, and exploiting additional cosmic messengers, such as neutrinos and gravitational waves. Recent years have seen significant progress in almost all these fields; they are presented in this review.

The Sun and the solar system are our reference system for abundances of elements and isotopes. Many direct and indirect methods are employed to establish a refined abundance record from the time when the Sun and the Earth were formed. Indications for nucleosynthesis in the local environment when the Sun was formed are derived from meteoritic material and inclusion of radioactive atoms in deep-sea sediments. Spectroscopy at many wavelengths and the neutrino flux from the hydrogen fusion processes in the Sun have established a refined model of how the nuclear energy production shapes stars. Models are required to explore nuclear fusion of heavier elements. These stellar evolution calculations have been confirmed by observations of nucleosynthesis products in the ejecta of stars and supernovae, as captured by stardust grains and by characteristic lines in spectra seen from these objects. One of the successes has been to directly observe γ rays from radioactive material synthesised in stellar explosions, which fully support the astrophysical models. Another has been the observation of radioactive afterglow and characteristic heavy-element spectrum from a neutron-star merger, confirming the neutron rich environments encountered in such rare explosions. The ejecta material captured by Earth over millions of years in sediments and identified through characteristic radio-isotopes suggests that nearby nucleosynthesis occurred in recent history, with further indications for sites of specific nucleosynthesis. Together with stardust and diffuse γ rays from radioactive ejecta, these help to piece together how cosmic materials are transported in interstellar space and re-cycled into and between generations of stars. Our description of cosmic compositional evolution needs such observational support, as it rests on several assumptions that appear challenged by recent recognition of violent events being common during evolution of a galaxy. This overview presents the flow of cosmic matter and the various sites of nucleosynthesis, as understood from combining many techniques and observations, towards the current knowledge of how the universe is enriched with elements.


(843)Multi-scale organization in communicating active matter
  • Alexander Ziepke,
  • Ivan Maryshev,
  • Igor S. Aranson,
  • Erwin Frey
Nature Communications (11/2022) doi:10.1038/s41467-022-34484-2
abstract + abstract -

The emergence of collective motion among interacting, self-propelled agents is a central paradigm in non-equilibrium physics. Examples of such active matter range from swimming bacteria and cytoskeletal motility assays to synthetic self-propelled colloids and swarming microrobots. Remarkably, the aggregation capabilities of many of these systems rely on a theme as fundamental as it is ubiquitous in nature: communication. Despite its eminent importance, the role of communication in the collective organization of active systems is not yet fully understood. Here we report on the multi-scale self-organization of interacting self-propelled agents that locally process information transmitted by chemical signals. We show that this communication capacity dramatically expands their ability to form complex structures, allowing them to self-organize through a series of collective dynamical states at multiple hierarchical levels. Our findings provide insights into the role of self-sustained signal processing for self-organization in biological systems and open routes to applications using chemically driven colloids or microrobots.


CN-4
RU-D
(842)The Metallicity and Distance of NGC 2403 from Blue Supergiants
  • Fabio Bresolin,
  • Rolf-Peter Kudritzki,
  • Miguel A. Urbaneja
The Astrophysical Journal (11/2022) doi:10.3847/1538-4357/ac9584
abstract + abstract -

We present the first quantitative spectral analysis of blue supergiant stars in the nearby galaxy NGC 2403. Out of a sample of 47 targets observed with the LRIS spectrograph at the Keck I telescope we have extracted 16 B- and A-type supergiants for which we have data of sufficient quality to carry out a comparison with model spectra of evolved massive stars and infer the stellar parameters. The radial metallicity gradient of NGC 2403 that we derive has a slope of -0.14(±0.05) dex ${r}_{e}^{-1}$ , and is in accordance with the analysis of H II region oxygen abundances. We present evidence that the stellar metallicities that we obtain in extragalactic systems in general agree with the nebular abundances based on the analysis of the auroral lines, over more than 1 order of magnitude in metallicity. Adopting the known relation between stellar parameters and intrinsic luminosity we find a distance modulus μ = 27.38 ± 0.08 mag. While this can be brought into agreement with Cepheid-based determinations, it is 0.14 mag short of the value measured from the tip of the red giant branch. We update the mass-metallicity relation secured from chemical abundance studies of stars in resolved star-forming galaxies.


(841)TDCOSMO. IX. Systematic comparison between lens modelling software programs: Time-delay prediction for WGD 2038−4008
  • A. J. Shajib,
  • K. C. Wong,
  • S. Birrer,
  • S. H. Suyu,
  • T. Treu
  • +13
  • E. J. Buckley-Geer,
  • H. Lin,
  • C. E. Rusu,
  • J. Poh,
  • A. Palmese,
  • A. Agnello,
  • M. W. Auger-Williams,
  • A. Galan,
  • S. Schuldt,
  • D. Sluse,
  • F. Courbin,
  • J. Frieman,
  • M. Millon
  • (less)
Astronomy and Astrophysics (11/2022) doi:10.1051/0004-6361/202243401
abstract + abstract -

The importance of alternative methods for measuring the Hubble constant, such as time-delay cosmography, is highlighted by the recent Hubble tension. It is paramount to thoroughly investigate and rule out systematic biases in all measurement methods before we can accept new physics as the source of this tension. In this study, we perform a check for systematic biases in the lens modelling procedure of time-delay cosmography by comparing independent and blind time-delay predictions of the system WGD 2038−4008 from two teams using two different software programs: GLEE and LENSTRONOMY. The predicted time delays from the two teams incorporate the stellar kinematics of the deflector and the external convergence from line-of-sight structures. The un-blinded time-delay predictions from the two teams agree within 1.2σ, implying that once the time delay is measured the inferred Hubble constant will also be mutually consistent. However, there is a ∼4σ discrepancy between the power-law model slope and external shear, which is a significant discrepancy at the level of lens models before the stellar kinematics and the external convergence are incorporated. We identify the difference in the reconstructed point spread function (PSF) to be the source of this discrepancy. When the same reconstructed PSF was used by both teams, we achieved excellent agreement, within ∼0.6σ, indicating that potential systematics stemming from source reconstruction algorithms and investigator choices are well under control. We recommend that future studies supersample the PSF as needed and marginalize over multiple algorithms or realizations for the PSF reconstruction to mitigate the systematics associated with the PSF. A future study will measure the time delays of the system WGD 2038−4008 and infer the Hubble constant based on our mass models.


CN-3
RU-D
(840)Euclid: Modelling massive neutrinos in cosmology -- a code comparison
  • J. Adamek,
  • R. E. Angulo,
  • C. Arnold,
  • M. Baldi,
  • M. Biagetti
  • +131
  • B. Bose,
  • C. Carbone,
  • T. Castro,
  • J. Dakin,
  • K. Dolag,
  • W. Elbers,
  • C. Fidler,
  • C. Giocoli,
  • S. Hannestad,
  • F. Hassani,
  • C. Hernández-Aguayo,
  • K. Koyama,
  • B. Li,
  • R. Mauland,
  • P. Monaco,
  • C. Moretti,
  • D. F. Mota,
  • C. Partmann,
  • G. Parimbelli,
  • D. Potter,
  • A. Schneider,
  • S. Schulz,
  • R. E. Smith,
  • V. Springel,
  • J. Stadel,
  • T. Tram,
  • M. Viel,
  • F. Villaescusa-Navarro,
  • H. A. Winther,
  • B. S. Wright,
  • M. Zennaro,
  • N. Aghanim,
  • L. Amendola,
  • N. Auricchio,
  • D. Bonino,
  • E. Branchini,
  • M. Brescia,
  • S. Camera,
  • V. Capobianco,
  • V. F. Cardone,
  • J. Carretero,
  • F. J. Castander,
  • M. Castellano,
  • S. Cavuoti,
  • A. Cimatti,
  • R. Cledassou,
  • G. Congedo,
  • L. Conversi,
  • Y. Copin,
  • A. Da Silva,
  • H. Degaudenzi,
  • M. Douspis,
  • F. Dubath,
  • C. A. J. Duncan,
  • X. Dupac,
  • S. Dusini,
  • S. Farrens,
  • S. Ferriol,
  • P. Fosalba,
  • M. Frailis,
  • E. Franceschi,
  • S. Galeotta,
  • B. Garilli,
  • W. Gillard,
  • B. Gillis,
  • A. Grazian,
  • S. V. Haugan,
  • W. Holmes,
  • A. Hornstrup,
  • K. Jahnke,
  • S. Kermiche,
  • A. Kiessling,
  • M. Kilbinger,
  • T. Kitching,
  • M. Kunz,
  • H. Kurki-Suonio,
  • P. B. Lilje,
  • I. Lloro,
  • O. Mansutti,
  • O. Marggraf,
  • F. Marulli,
  • R. Massey,
  • E. Medinaceli,
  • M. Meneghetti,
  • G. Meylan,
  • M. Moresco,
  • L. Moscardini,
  • E. Munari,
  • S. -M. Niemi,
  • C. Padilla,
  • S. Paltani,
  • F. Pasian,
  • K. Pedersen,
  • W. J. Percival,
  • V. Pettorino,
  • G. Polenta,
  • M. Poncet,
  • L. A. Popa,
  • F. Raison,
  • R. Rebolo,
  • A. Renzi,
  • J. Rhodes,
  • G. Riccio,
  • E. Romelli,
  • M. Roncarelli,
  • R. Saglia,
  • D. Sapone,
  • B. Sartoris,
  • P. Schneider,
  • T. Schrabback,
  • A. Secroun,
  • G. Seidel,
  • C. Sirignano,
  • G. Sirri,
  • L. Stanco,
  • J. -L. Starck,
  • P. Tallada-Crespí,
  • A. N. Taylor,
  • I. Tereno,
  • R. Toledo-Moreo,
  • F. Torradeflot,
  • I. Tutusaus,
  • L. Valenziano,
  • T. Vassallo,
  • Y. Wang,
  • J. Weller,
  • A. Zacchei,
  • G. Zamorani,
  • J. Zoubian,
  • G. Fabbian,
  • V. Scottez
  • (less)
arXiv e-prints (11/2022) e-Print:2211.12457
abstract + abstract -

The measurement of the absolute neutrino mass scale from cosmological large-scale clustering data is one of the key science goals of the Euclid mission. Such a measurement relies on precise modelling of the impact of neutrinos on structure formation, which can be studied with $N$-body simulations. Here we present the results from a major code comparison effort to establish the maturity and reliability of numerical methods for treating massive neutrinos. The comparison includes eleven full $N$-body implementations (not all of them independent), two $N$-body schemes with approximate time integration, and four additional codes that directly predict or emulate the matter power spectrum. Using a common set of initial data we quantify the relative agreement on the nonlinear power spectrum of cold dark matter and baryons and, for the $N$-body codes, also the relative agreement on the bispectrum, halo mass function, and halo bias. We find that the different numerical implementations produce fully consistent results. We can therefore be confident that we can model the impact of massive neutrinos at the sub-percent level in the most common summary statistics. We also provide a code validation pipeline for future reference.


(839)Persistent homology in cosmic shear. II. A tomographic analysis of DES-Y1
  • Sven Heydenreich,
  • Benjamin Brück,
  • Pierre Burger,
  • Joachim Harnois-Déraps,
  • Sandra Unruh
  • +3
  • Tiago Castro,
  • Klaus Dolag,
  • Nicolas Martinet
  • (less)
Astronomy and Astrophysics (11/2022) doi:10.1051/0004-6361/202243868
abstract + abstract -

We demonstrate how to use persistent homology for cosmological parameter inference in a tomographic cosmic shear survey. We obtain the first cosmological parameter constraints from persistent homology by applying our method to the first-year data of the Dark Energy Survey. To obtain these constraints, we analyse the topological structure of the matter distribution by extracting persistence diagrams from signal-to-noise maps of aperture masses. This presents a natural extension to the widely used peak count statistics. Extracting the persistence diagrams from the cosmo-SLICS, a suite of N-body simulations with variable cosmological parameters, we interpolate the signal using Gaussian processes and marginalise over the most relevant systematic effects, including intrinsic alignments and baryonic effects. For the structure growth parameter, we find S8 = 0.747−0.031+0.025, which is in full agreement with other late-time probes. We also constrain the intrinsic alignment parameter to A = 1.54 ± 0.52, which constitutes a detection of the intrinsic alignment effect at almost 3σ.


CN-7
(838)Parameterisations of thermal bomb explosions for core-collapse supernovae and 56Ni production
  • Liliya Imasheva,
  • Hans-Thomas Janka,
  • Achim Weiss
Monthly Notices of the Royal Astronomical Society (11/2022) doi:10.1093/mnras/stac3239
abstract + abstract -

Thermal bombs are a widely used method to artificially trigger explosions of core-collapse supernovae (CCSNe) to determine their nucleosynthesis or ejecta and remnant properties. Recently, their use in spherically symmetric (1D) hydrodynamic simulations led to the result that 56, 57Ni and 44Ti are massively underproduced compared to observational estimates for Supernova 1987A, if the explosions are slow, i.e., if the explosion mechanism of CCSNe releases the explosion energy on long timescales. It was concluded that rapid explosions are required to match observed abundances, i.e., the explosion mechanism must provide the CCSN energy nearly instantaneously on timescales of some ten to order 100 ms. This result, if valid, would disfavor the neutrino-heating mechanism, which releases the CCSN energy on timescales of seconds. Here, we demonstrate by 1D hydrodynamic simulations and nucleosynthetic post-processing that these conclusions are a consequence of disregarding the initial collapse of the stellar core in the thermal-bomb modelling before the bomb releases the explosion energy. We demonstrate that the anti-correlation of 56Ni yield and energy-injection timescale vanishes when the initial collapse is included and that it can even be reversed, i.e., more 56Ni is made by slower explosions, when the collapse proceeds to small radii similar to those where neutrino heating takes place in CCSNe. We also show that the 56Ni production in thermal-bomb explosions is sensitive to the chosen mass cut and that a fixed mass layer or fixed volume for the energy deposition cause only secondary differences. Moreover, we propose a most appropriate setup for thermal bombs.


RU-C
(837)Impact of half-wave plate systematics on the measurement of cosmic birefringence from CMB polarization
  • Marta Monelli,
  • Eiichiro Komatsu,
  • Alexandre E. Adler,
  • Matteo Billi,
  • Paolo Campeti
  • +4
  • Nadia Dachlythra,
  • Adriaan J. Duivenvoorden,
  • Jon E. Gudmundsson,
  • Martin Reinecke
  • (less)
(11/2022) e-Print:2211.05685
abstract + abstract -

Polarization of the cosmic microwave background (CMB) can probe new parity-violating physics such as cosmic birefringence (CB), which requires exquisite control over instrumental systematics. The non-idealities of the half-wave plate (HWP) represent a source of systematics when used as a polarization modulator. We study their impact on the CMB angular power spectra, which is partially degenerate with CB and miscalibration of the polarization angle. We use full-sky beam convolution simulations including HWP to generate mock noiseless time-ordered data, process them through a bin averaging map-maker, and calculate the power spectra including $TB$ and $EB$ correlations. We also derive analytical formulae which accurately model the observed spectra. For our choice of HWP parameters, the HWP-induced angle amounts to a few degrees, which could be misinterpreted as CB. Accurate knowledge of the HWP is required to mitigate this. Our simulation and analytical formulae will be useful for deriving requirements for the accuracy of HWP calibration.


(836)Set-Conditional Set Generation for Particle Physics
  • Francesco Armando Di Bello,
  • Etienne Dreyer,
  • Sanmay Ganguly,
  • Eilam Gross,
  • Lukas Heinrich
  • +4
  • Marumi Kado,
  • Nilotpal Kakati,
  • Jonathan Shlomi,
  • Nathalie Soybelman
  • (less)
abstract + abstract -

The simulation of particle physics data is a fundamental but computationally intensive ingredient for physics analysis at the Large Hadron Collider, where observational set-valued data is generated conditional on a set of incoming particles. To accelerate this task, we present a novel generative model based on a graph neural network and slot-attention components, which exceeds the performance of pre-existing baselines.


CN-3
CN-4
PhD Thesis
RU-C
(835)Simulating the inflationary Universe: from single-field to the axion-U(1) model.
  • Angelo Caravano - Advisor: Jochen Weller
Thesis (11/2022) doi:10.5282/edoc.30905
abstract + abstract -

The observed homogeneity and spatial flatness of the Universe suggest that there was a period of accelerated expansion just after the Big Bang, called inflation. In the standard picture, this expansion is driven by the inflaton, a scalar field beyond the standard model of particle physics. If other fields are present during this epoch, they can leave sizable traces on inflationary ob- servables that might be revealed using upcoming experiments. Studying the phenomenological consequences of such fields often requires going beyond perturbation theory due to the nonlinear physics involved in several non-minimal inflationary scenarios.[...]


PhD Thesis
RU-A
(834)Soft-collinear Gravity and Soft Theorems
  • Patrick Hager - Advisor: Martin Beneke
Thesis (11/2022) link
abstract + abstract -

In this thesis, we construct the soft-collinear Lagrangian for gravity systematically beyond leading power in the power-counting parameter and provide a set of minimal building blocks for the N-jet operators. We find that the effective theory is covariant with respect to an emergent soft background field that is obscured in the full theory. The emission of a soft gluon and graviton from a non-radiative process is investigated and an operatorial version of the soft theorem is obtained.


CN-8
PhD Thesis
(833)A statistical view on the origin of homochirality
  • Gabin Laurent - Advisor: Ulrich Gerland
Thesis (11/2022) link
abstract + abstract -

Living systems on earth are homochiral. This means that for every chiral species they contain, one of the two possible enantiomers is present in much higher fraction than its mirrored counterpart. Homochirality has continuously puzzled scientists ever since the discovery of chirality by Pasteur, because a mechanism for its emergence is not yet solved, nor is the question of whether homochirality is a prerequisite or a consequence of life. In this thesis, we propose two physical scenarios in which homochirality could have emerged prior to or alongside life. We first show that large and complex chiral chemical networks are subject to a symmetry breaking transition from a racemic state to a homochiral one as the number of chiral compounds they contain becomes large. This robust mechanism relies on properties of large random matrices and requires only a few constraints on the chemical network. It is illustrated with a generalization of the famous Frank model which contains a large number of chemical species. We also quantify how abundant chiral molecules are in nature through an analysis of molecular databanks which shows a threshold above which chiral compounds dominate achiral ones. In a second part, we present a scenario based on template-directed ligation of biopolymers such as RNA, which involves the extension of RNA polymers by ligation with other oligomers or monomer compatible with base paring. This process presents autocatalysis and chiral inhibition which are two key ingredients for a symmetry breaking transition leading to a homochiral state. Using detailed stochastic simulations of template-directed ligation of chiral polymeric systems, we thus investigate the propensity of systems inocculated initially with a racemic mixture of RNA monomers to evolve towards a homochiral polymer system in the presence of racemization reactions. Two kinds of reactors and their different conditions are studied in this work: closed out-of-equilibrium reactors with a conserved number of RNA monomers and open reactors in which species are being degraded over time and some are chemostated. In addition, temperature cycles or dry-wet cycles are assumed to be present in both cases. We find that full homochirality is reached for closed systems in presence of racemization reactions due to chiral stalling, which slows ligation when opposite chiralities are paired closed to the ligation site. Remarkably, the homochirality transition helps the system to reach longer average polymer length, which is typically difficult in non-enzymatic polymerization. Open reactor simulations can only reach partial and transient enantiomeric excesses but without the need of racemization reactions. The work presented in this thesis focuses on the amplification process of a small initial enantiomeric excess imbalance generated by a particular physical or chemical phenomenon or simply by statistical fluctuations.


IDSL
RU-E
(832)Prebiotic foam environments to oligomerize and accumulate RNA
  • Emre Tekin; Annalena Salditt; Philipp Schwintek; Sree Wunnava; Juliette Langlais; James Saenz; Dora Tang; Petra Schwille; Christof Mast; Dieter Braun
ChemBioChem (11/2022) doi:10.1002/cbic.202200423
abstract + abstract -

When water interacts with porous rocks, its wetting and surface tension properties create air bubbles in large number. To probe their relevance as a setting for the emergence of life, we microfluidically created foams that were stabilized with lipids. A persistent non-equilibrium setting was provided by a thermal gradient. The foam's large surface area triggers capillary flows and wet-dry reactions that accumulate, aggregate and oligomerize RNA, offering a compelling habitat for RNA-based early life as it offers both wet and dry conditions in direct neighborhood. Lipids were screened to stabilize the foams. The prebiotically more probable myristic acid stabilized foams over many hours. The capillary flow created by the evaporation at the water-air interface provided an attractive force for molecule localization and selection for molecule size. For example, self-binding oligonucleotide sequences accumulated and formed micrometer-sized aggregates which were shuttled between gas bubbles. The wet-dry cycles at the foam bubble interfaces triggered a non-enzymatic RNA oligomerization from 2’,3’-cyclic CMP and GMP which despite the small dry reaction volume was superior to the corresponding dry reaction. The found characteristics make heated foams an interesting, localized setting for early molecular evolution.


(831)The MADPSZ catalogue of Planck clusters over the DES region: extending to lower mass and higher redshift
  • D. Hernández-Lang,
  • J. J. Mohr,
  • M. Klein,
  • S. Grandis,
  • J. -B. Melin
  • +56
  • P. Tarrío,
  • M. Arnaud,
  • G. W. Pratt,
  • T. M. C. Abbott,
  • M. Aguena,
  • O. Alves,
  • F. Andrade-Oliveira,
  • D. Bacon,
  • E. Bertin,
  • D. Brooks,
  • D. L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • F. J. Castander,
  • M. Costanzi,
  • L. N. da Costa,
  • M. E. S. Pereira,
  • S. Desai,
  • H. T. Diehl,
  • P. Doel,
  • S. Everett,
  • I. Ferrero,
  • B. Flaugher,
  • J. Frieman,
  • J. García-Bellido,
  • D. Gruen,
  • R. A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • S. R. Hinton,
  • D. L. Hollowood,
  • K. Honscheid,
  • D. J. James,
  • K. Kuehn,
  • N. Kuropatkin,
  • O. Lahav,
  • C. Lidman,
  • P. Melchior,
  • J. Mena-Fernández,
  • F. Menanteau,
  • R. Miquel,
  • A. Palmese,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A. A. Plazas Malagón,
  • M. Raveri,
  • M. Rodriguez-Monroy,
  • A. K. Romer,
  • V. Scarpine,
  • I. Sevilla-Noarbe,
  • M. Smith,
  • E. Suchyta,
  • G. Tarle,
  • D. Thomas,
  • N. Weaverdyck
  • (less)
arXiv e-prints (10/2022) e-Print:2210.04666
abstract + abstract -

We present the first systematic follow-up of Planck Sunyaev-Zeldovich effect (SZE) selected candidates down to signal-to-noise (S/N) of 3 over the 5000 deg$^2$ covered by the Dark Energy Survey. Using the MCMF cluster confirmation algorithm, we identify optical counterparts, determine photometric redshifts and richnesses and assign a parameter, $f_{\rm cont}$, that reflects the probability that each SZE-optical pairing represents a real cluster rather than a random superposition of physically unassociated systems. The new MADPSZ cluster catalogue consists of 1092 MCMF confirmed clusters and has a purity of 85%. We present the properties of subsamples of the MADPSZ catalogue that have purities ranging from 90% to 97.5%, depending on the adopted $f_{\rm cont}$ threshold. $M_{500}$ halo mass estimates, redshifts, richnesses, and optical centers are presented for all MADPSZ clusters. The MADPSZ catalogue adds 828 previously unknown Planck identified clusters over the DES footprint and provides redshifts for an additional 50 previously published Planck selected clusters with S/N>4.5. Using the subsample with spectroscopic redshifts, we demonstrate excellent cluster photo-$z$ performance with an RMS scatter in $\Delta z/(1+z)$ of 0.47%. Our MCMF based analysis allows us to infer the contamination fraction of the initial S/N>3 Planck selected candidate list, which is 50%. We present a method of estimating the completeness of the MADPSZ cluster sample and $f_{\rm cont}$ selected subsamples. In comparison to the previously published Planck cluster catalogues. this new S/N $>$ 3 MCMF confirmed cluster catalogue populates the lower mass regime at all redshifts and includes clusters up to z$\sim$1.3.


CN-2
RU-D
(830)Monitoring accretion rate variability in the Orion Nebula Cluster with the Wendelstein Wide Field Imager
  • S. Flaischlen,
  • T. Preibisch,
  • M. Kluge,
  • C. F. Manara,
  • B. Ercolano
Astronomy and Astrophysics (10/2022) doi:10.1051/0004-6361/202142630
abstract + abstract -

Context. The understanding of the accretion process has a central role in the understanding of star and planet formation.
Aims: We aim to test how accretion variability influences previous correlation analyses of the relation between X-ray activity and accretion rates, which is important for understanding the evolution of circumstellar disks and disk photoevaporation.
Methods: We monitored accreting stars in the Orion Nebula Cluster from November 24, 2014, until February 17, 2019, for 42 epochs with the Wendelstein Wide Field Imager in the Sloan Digital Sky Survey u'g'r' filters on the 2 m Fraunhofer Telescope on Mount Wendelstein. Mass accretion rates were determined from the measured ultraviolet excess. The influence of the mass accretion rate variability on the relation between X-ray luminosities and mass accretion rates was analyzed statistically.
Results: We find a typical interquartile range of ∼0.3 dex for the mass accretion rate variability on timescales from weeks to ∼2 yr. The variability has likely no significant influence on a correlation analysis of the X-ray luminosity and the mass accretion rate observed at different times when the sample size is large enough.
Conclusions: The observed anticorrelation between the X-ray luminosity and the mass accretion rate predicted by models of photoevaporation-starved accretion is likely not due to a bias introduced by different observing times.

Full Tables 1-3 and reduced data 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/666/A55


MIAPbP
(829)Enhancing Searches for Heavy QCD Axions via Dimuon Final States
  • Raymond T. Co,
  • Soubhik Kumar,
  • Zhen Liu
arXiv e-prints (10/2022) e-Print:2210.02462
abstract + abstract -

Heavy QCD axions are well-motivated extensions of the QCD axion that address the quality problem while still solving the strong CP problem. Owing to the gluon coupling, critical for solving the strong CP problem, these axions can be produced in significant numbers in beam dump and collider environments for axion decay constants as large as PeV, relevant for addressing the axion quality problem. In addition, if these axions have leptonic couplings, they can give rise to long-lived decay into lepton pairs, in particular, dominantly into muons above the dimuon threshold and below the GeV scale in a broad class of axion models. Considering existing constraints, primarily from rare meson decays, we demonstrate that current and future neutrino facilities and long-lived particle searches have the potential to probe significant parts of the heavy QCD axion parameter space via dimuon final states.


(828)Evidence for past interaction with an asymmetric circumstellar shell in the young SNR Cassiopeia A
  • 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)
Astronomy and Astrophysics (10/2022) doi:10.1051/0004-6361/202243258
abstract + abstract -

Context. Observations of the supernova remnant (SNR) Cassiopeia A (Cas A) show significant asymmetries in the reverse shock that cannot be explained by models describing a remnant expanding through a spherically symmetric wind of the progenitor star.
Aims: We investigate whether a past interaction of Cas A with a massive asymmetric shell of the circumstellar medium can account for the observed asymmetries of the reverse shock.
Methods: We performed three-dimensional (3D) (magneto)-hydrodynamic simulations that describe the remnant evolution from the SN explosion to its interaction with a massive circumstellar shell. The initial conditions (soon after the shock breakout at the stellar surface) are provided by a 3D neutrino-driven SN model whose morphology closely resembles Cas A and the SNR simulations cover ≈2000 yr of evolution. We explored the parameter space of the shell, searching for a set of parameters able to produce an inward-moving reverse shock in the western hemisphere of the remnant at the age of ≈350 yr, analogous to that observed in Cas A.
Results: The interaction of the remnant with the shell can produce asymmetries resembling those observed in the reverse shock if the shell was asymmetric with the densest portion in the (blueshifted) nearside to the northwest (NW). According to our favorite model, the shell was thin (thickness σ ≈ 0.02 pc) with a radius rsh ≈ 1.5 pc from the center of the explosion. 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 most 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; and (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−1) than in other regions (below 2000 km s−1).
Conclusions: The large-scale asymmetries observed in the reverse shock of Cas A can be interpreted as signatures of the interaction of the remnant with an asymmetric dense circumstellar shell that occurred between ≈180 and ≈240 yr after the SN event. We suggest that the shell was, most likely, the result of a massive eruption from the progenitor star that occurred between 104 and 105 yr prior to core-collapse. We estimate a total mass of the shell of the order of 2 M.


(827)Exploring the cosmological synergy between galaxy cluster and cosmic void number counts
  • Davide Pelliciari,
  • Sofia Contarini,
  • Federico Marulli,
  • Lauro Moscardini,
  • Carlo Giocoli
  • +2
  • Giorgio Francesco Lesci,
  • Klaus Dolag
  • (less)
arXiv e-prints (10/2022) e-Print:2210.07248
abstract + abstract -

Galaxy clusters and cosmic voids are the most extreme objects of our Universe in terms of mass and size, tracing two opposite sides of the large-scale matter density field. By studying their abundance as a function of their mass and radius, respectively, i.e. the halo mass function (HMF) and void size function (VSF), it is possible to achieve fundamental constraints on the cosmological model. While the HMF has already been extensively exploited providing robust constraints on the main cosmological model parameters (e.g. $\Omega_{\rm m}$, $\sigma_8$ and $S_8$), the VSF is still emerging as a viable and effective cosmological probe. Given the expected complementarity of these statistics, in this work we aim at estimating the costraining power deriving from their combination. To achieve this goal, we exploit realistic mock samples of galaxy clusters and voids extracted from state-of-the-art large hydrodynamical simulations, in the redshift range $0.2 \leq z \leq 1$. We perform an accurate calibration of the free parameters of the HMF and VSF models, needed to take into account the differences between the types of mass tracers used in this work and those considered in previous literature analyses. Then, we obtain constraints on $\Omega_{\rm m}$ and $\sigma_8$ by performing a Bayesian Markov Chain Monte Carlo analysis. We find that cluster and void counts represent powerful independent and complementary probes to test the cosmological framework. In particular, we found that the constraining power of the HMF on $\Omega_{\rm m}$ and $\sigma_8$ improves drastically with the VSF contribution, increasing the $S_8$ constraint precision by a factor of about $60\%$.


CN-3
CN-4
RU-C
(826)Why Cosmic Voids Matter: Nonlinear Structure & Linear Dynamics
  • Nico Schuster,
  • Nico Hamaus,
  • Klaus Dolag,
  • Jochen Weller
arXiv e-prints (10/2022) e-Print:2210.02457
abstract + abstract -

We use the Magneticum suite of state-of-the-art hydrodynamical simulations to identify cosmic voids based on the watershed technique and investigate their most fundamental properties across different resolutions in mass and scale. This encompasses the distributions of void sizes, shapes, and content, as well as their radial density and velocity profiles traced by the distribution of cold dark matter particles and halos. We also study the impact of various tracer properties, such as their sparsity and mass, and the influence of void merging on these summary statistics. Our results reveal that all of the analyzed void properties are physically related to each other and describe universal characteristics that are largely independent of tracer type and resolution. Most notably, we find that the motion of tracers around void centers is perfectly consistent with linear dynamics, both for individual, as well as stacked voids. Despite the large range of scales accessible in our simulations, we are unable to identify the occurrence of nonlinear dynamics even inside voids of only a few Mpc in size. This suggests voids to be among the most pristine probes of cosmology down to scales that are commonly referred to as highly nonlinear in the field of large-scale structure.


(825)Landau and leading singularities in arbitrary space-time dimensions
  • Wojciech Flieger,
  • William J. Torres Bobadilla
arXiv e-prints (10/2022) e-Print:2210.09872
abstract + abstract -

Using the decomposition of the $D$-dimensional space-time into parallel and perpendicular subspaces, we study and prove a connection between Landau and leading singularities for $N$-point one-loop Feynman integrals by applying multi-dimensional theory of residues. We show that if $D=N$ and $D=N+1$, the leading singularity corresponds to the inverse of the square root of the leading Landau singularity of the first and second type, respectively. We make use of this outcome to systematically provide differential equations of Feynman integrals in canonical forms and the extension of the connection of these singularities at multi-loop level by exploiting the loop-by-loop approach. Illustrative examples with the calculation of Landau and leading singularities are provided to supplement our results.


RU-C
(824)Robustness of cosmic birefringence measurement against Galactic foreground emission and instrumental systematics
  • P. Diego-Palazuelos,
  • E. Martínez-González,
  • P. Vielva,
  • R. B. Barreiro,
  • M. Tristram
  • +9
  • E. de la Hoz,
  • J. R. Eskilt,
  • Y. Minami,
  • R. M. Sullivan,
  • A. J. Banday,
  • K. M. Górski,
  • R. Keskitalo,
  • E. Komatsu,
  • D. Scott
  • (less)
arXiv e-prints (10/2022) e-Print:2210.07655
abstract + abstract -

The polarization of the cosmic microwave background (CMB) can be used to search for parity-violating processes like that predicted by a Chern-Simons coupling to a light pseudoscalar field. Such an interaction rotates $E$ modes into $B$ modes in the observed CMB signal by an effect known as cosmic birefringence. Even though isotropic birefringence can be confused with the rotation produced by a miscalibration of the detectors' polarization angles the degeneracy between both effects is broken when Galactic foreground emission is used as a calibrator. In this work, we use realistic simulations of the High-Frequency Instrument of the Planck mission to test the impact that Galactic foreground emission and instrumental systematics have on the recent birefringence measurements obtained through this technique. Our results demonstrate the robustness of the methodology against the miscalibration of polarization angles and other systematic effects, like intensity-to-polarization leakage, beam leakage, or cross-polarization effects. However, our estimator is sensitive to the $EB$ correlation of polarized foreground emission. Here we propose to correct the bias induced by dust $EB$ by modeling the foreground signal with templates produced in Bayesian component-separation analyses that fit parametric models to CMB data. Acknowledging the limitations of currently available dust templates like that of the Commander sky model, high-precision CMB data and a characterization of dust beyond the modified blackbody paradigm are needed to obtain a definitive measurement of cosmic birefringence in the future.


CN-6
(823)Multi-messenger characterization of Mrk 501 during historically low X-ray and $\gamma$-ray activity
  • MAGIC collaboration,
  • H. Abe,
  • S. Abe,
  • V. A. Acciari,
  • I. Agudo
  • +320
  • T. Aniello,
  • S. Ansoldi,
  • L. A. Antonelli,
  • A. Arbet Engels,
  • C. Arcaro,
  • M. Artero,
  • K. Asano,
  • D. Baack,
  • A. Babić,
  • A. Baquero,
  • U. Barres de Almeida,
  • J. A. Barrio,
  • I. Batković,
  • J. Baxter,
  • J. Becerra González,
  • W. Bednarek,
  • E. Bernardini,
  • M. Bernardos,
  • A. Berti,
  • J. Besenrieder,
  • W. Bhattacharyya,
  • C. Bigongiari,
  • A. Biland,
  • O. Blanch,
  • G. Bonnoli,
  • Ž. Bošnjak,
  • I. Burelli,
  • G. Busetto,
  • R. Carosi,
  • M. Carretero-Castrillo,
  • A. J. Castro-Tirado,
  • G. Ceribella,
  • Y. Chai,
  • A. Chilingarian,
  • S. Cikota,
  • E. Colombo,
  • J. L. Contreras,
  • J. Cortina,
  • S. Covino,
  • G. D'Amico,
  • V. D'Elia,
  • P. Da Vela,
  • F. Dazzi,
  • A. De Angelis,
  • B. De Lotto,
  • A. Del Popolo,
  • M. Delfino,
  • J. Delgado,
  • C. Delgado Mendez,
  • D. Depaoli,
  • F. Di Pierro,
  • L. Di Venere,
  • E. Do Souto Espiñeira,
  • D. Dominis Prester,
  • A. Donini,
  • D. Dorner,
  • M. Doro,
  • D. Elsaesser,
  • G. Emery,
  • J. Escudero,
  • V. Fallah Ramazani,
  • L. Fariña,
  • A. Fattorini,
  • L. Foffano,
  • L. Font,
  • C. Fruck,
  • S. Fukami,
  • Y. Fukazawa,
  • R. J. García López,
  • M. Garczarczyk,
  • S. Gasparyan,
  • M. Gaug,
  • J. G. Giesbrecht Paiva,
  • N. Giglietto,
  • F. Giordano,
  • P. Gliwny,
  • N. Godinović,
  • R. Grau,
  • D. Green,
  • J. G. Green,
  • D. Hadasch,
  • A. Hahn,
  • T. Hassan,
  • L. Heckmann,
  • J. Herrera,
  • D. Hrupec,
  • M. Hütten,
  • R. Imazawa,
  • T. Inada,
  • R. Iotov,
  • K. Ishio,
  • I. Jiménez Martínez,
  • J. Jormanainen,
  • D. Kerszberg,
  • Y. Kobayashi,
  • H. Kubo,
  • J. Kushida,
  • A. Lamastra,
  • D. Lelas,
  • F. Leone,
  • E. Lindfors,
  • L. Linhoff,
  • S. Lombardi,
  • F. Longo,
  • R. López-Coto,
  • M. López-Moya,
  • A. López-Oramas,
  • S. Loporchio,
  • A. Lorini,
  • E. Lyard,
  • B. Machado de Oliveira Fraga,
  • P. Majumdar,
  • M. Makariev,
  • G. Maneva,
  • N. Mang,
  • M. Manganaro,
  • S. Mangano,
  • K. Mannheim,
  • M. Mariotti,
  • M. Martínez,
  • A. Mas-Aguilar,
  • D. Mazin,
  • S. Menchiari,
  • S. Mender,
  • S. Mićanović,
  • D. Miceli,
  • T. Miener,
  • J. M. Miranda,
  • R. Mirzoyan,
  • E. Molina,
  • H. A. Mondal,
  • A. Moralejo,
  • D. Morcuende,
  • V. Moreno,
  • T. Nakamori,
  • C. Nanci,
  • L. Nava,
  • V. Neustroev,
  • M. Nievas Rosillo,
  • C. Nigro,
  • K. Nilsson,
  • K. Nishijima,
  • T. Njoh Ekoume,
  • K. Noda,
  • S. Nozaki,
  • Y. Ohtani,
  • T. Oka,
  • A. Okumura,
  • J. Otero-Santos,
  • S. Paiano,
  • M. Palatiello,
  • D. Paneque,
  • R. Paoletti,
  • J. M. Paredes,
  • L. Pavletić,
  • M. Persic,
  • M. Pihet,
  • G. Pirola,
  • F. Podobnik,
  • P. G. Prada Moroni,
  • E. Prandini,
  • G. Principe,
  • C. Priyadarshi,
  • W. Rhode,
  • M. Ribó,
  • J. Rico,
  • C. Righi,
  • A. Rugliancich,
  • N. Sahakyan,
  • T. Saito,
  • S. Sakurai,
  • K. Satalecka,
  • F. G. Saturni,
  • B. Schleicher,
  • K. Schmidt,
  • F. Schmuckermaier,
  • J. L. Schubert,
  • T. Schweizer,
  • J. Sitarek,
  • V. Sliusar,
  • D. Sobczynska,
  • A. Spolon,
  • A. Stamerra,
  • J. Strišković,
  • D. Strom,
  • M. Strzys,
  • Y. Suda,
  • T. Surić,
  • H. Tajima,
  • M. Takahashi,
  • R. Takeishi,
  • F. Tavecchio,
  • P. Temnikov,
  • K. Terauchi,
  • T. Terzić,
  • M. Teshima,
  • L. Tosti,
  • S. Truzzi,
  • A. Tutone,
  • S. Ubach,
  • J. van Scherpenberg,
  • M. Vazquez Acosta,
  • S. Ventura,
  • V. Verguilov,
  • I. Viale,
  • C. F. Vigorito,
  • V. Vitale,
  • I. Vovk,
  • R. Walter,
  • M. Will,
  • C. Wunderlich,
  • T. Yamamoto,
  • D. Zarić,
  • Other groups,
  • collaborations,
  • :,
  • M. Cerruti,
  • J. A. Acosta-Pulido,
  • G. Apolonio,
  • R. Bachev,
  • M. Baloković,
  • E. Benítez,
  • I. Björklund,
  • V. Bozhilov,
  • L. F. Brown,
  • A. Bugg,
  • W. Carbonell,
  • M. I. Carnerero,
  • D. Carosati,
  • C. Casadio,
  • W. Chamani,
  • W. P. Chen,
  • R. A. Chigladze,
  • G. Damljanovic,
  • K. Epps,
  • A. Erkenov,
  • M. Feige,
  • J. Finke,
  • A. Fuentes,
  • K. Gazeas,
  • M. Giroletti,
  • T. S. Grishina,
  • A. C. Gupta,
  • M. A. Gurwell,
  • E. Heidemann,
  • D. Hiriart,
  • W. J. Hou,
  • T. Hovatta,
  • S. Ibryamov,
  • M. D. Joner,
  • S. G. Jorstad,
  • J. Kania,
  • S. Kiehlmann,
  • G. N. Kimeridze,
  • E. N. Kopatskaya,
  • M. Kopp,
  • M. Korte,
  • B. Kotas,
  • S. Koyama,
  • J. A. Kramer,
  • L. Kunkel,
  • S. O. Kurtanidze,
  • O. M. Kurtanidze,
  • A. Lähteenmäki,
  • J. M. López,
  • V. M. Larionov,
  • E. G. Larionova,
  • L. V. Larionova,
  • C. Leto,
  • C. Lorey,
  • R. Mújica,
  • G. M. Madejski,
  • N. Marchili,
  • A. P. Marscher,
  • M. Minev,
  • A. Modaressi,
  • D. A. Morozova,
  • T. Mufakharov,
  • I. Myserlis,
  • A. A. Nikiforova,
  • M. G. Nikolashvili,
  • E. Ovcharov,
  • M. Perri,
  • C. M. Raiteri,
  • A. C. S. Readhead,
  • A. Reimer,
  • D. Reinhart,
  • S. Righini,
  • K. Rosenlehner,
  • A. C. Sadun,
  • S. S. Savchenko,
  • A. Scherbantin,
  • L. Schneider,
  • K. Schoch,
  • D. Seifert,
  • E. Semkov,
  • L. A. Sigua,
  • C. Singh,
  • P. Sola,
  • Y. Sotnikova,
  • M. Spencer,
  • R. Steineke,
  • M. Stojanovic,
  • A. Strigachev,
  • M. Tornikoski,
  • E. Traianou,
  • A. Tramacere,
  • Yu. V. Troitskaya,
  • I. S. Troitskiy,
  • J. B. Trump,
  • A. Tsai,
  • A. Valcheva,
  • A. A. Vasilyev,
  • F. Verrecchia,
  • M. Villata,
  • O. Vince,
  • K. Vrontaki,
  • Z. R. Weaver,
  • E. Zaharieva,
  • N. Zottmann
  • (less)
abstract + abstract -

We study the broadband emission of Mrk 501 using multi-wavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi-LAT, NuSTAR, Swift, GASP-WEBT, and OVRO. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wavebands, with the highest occurring at X-rays and very-high-energy (VHE) $\gamma$-rays. A significant correlation ($>$3$\sigma$) between X-rays and VHE $\gamma$-rays is measured, supporting leptonic scenarios to explain the variable parts of the emission, also during low activity. This is further supported when we extend our data from 2008 to 2020, and identify, for the first time, significant correlations between Swift-XRT and Fermi-LAT. We additionally find correlations between high-energy $\gamma$-rays and radio, with the radio lagging by more than 100 days, placing the $\gamma$-ray emission zone upstream of the radio-bright regions in the jet. Furthermore, Mrk 501 showed a historically low activity in X-rays and VHE $\gamma$-rays from mid-2017 to mid-2019 with a stable VHE flux ($>$0.2 TeV) of 5% the emission of the Crab Nebula. The broadband spectral energy distribution (SED) of this 2-year-long low-state, the potential baseline emission of Mrk 501, can be characterized with one-zone leptonic models, and with (lepto)-hadronic models fulfilling neutrino flux constraints from IceCube. We explore the time evolution of the SED towards the low-state, revealing that the stable baseline emission may be ascribed to a standing shock, and the variable emission to an additional expanding or traveling shock.


(822)Forecasting cosmological parameter constraints using multiple sparsity measurements as tracers of the mass profiles of dark matter haloes
  • P. S. Corasaniti,
  • A. M. C. Le Brun,
  • T. R. G. Richardson,
  • Y. Rasera,
  • S. Ettori
  • +2
Monthly Notices of the Royal Astronomical Society (10/2022) doi:10.1093/mnras/stac2196
abstract + abstract -

The dark matter halo sparsity, i.e. the ratio between spherical halo masses enclosing two different overdensities, provides a non-parametric proxy of the halo mass distribution that has been shown to be a sensitive probe of the cosmological imprint encoded in the mass profile of haloes hosting galaxy clusters. Mass estimations at several overdensities would allow for multiple sparsity measurements, which can potentially retrieve the entirety of the cosmological information imprinted on the halo profile. Here, we investigate the impact of multiple sparsity measurements on the cosmological model parameter inference. For this purpose, we analyse N-body halo catalogues from the Raygal and M2Csims simulations and evaluate the correlations among six different sparsities from spherical overdensity halo masses at Δ = 200, 500, 1000, and 2500 (in units of the critical density). Remarkably, sparsities associated to distinct halo mass shells are not highly correlated. This is not the case for sparsities obtained using halo masses estimated from the Navarro-Frenk-White (NFW) best-fitting profile, which artificially correlates different sparsities to order one. This implies that there is additional information in the mass profile beyond the NFW parametrization and that it can be exploited with multiple sparsities. In particular, from a likelihood analysis of synthetic average sparsity data, we show that cosmological parameter constraints significantly improve when increasing the number of sparsity combinations, though the constraints saturate beyond four sparsity estimates. We forecast constraints for the CHEX-MATE cluster sample and find that systematic mass bias errors mildly impact the parameter inference, though more studies are needed in this direction.


MIAPbP
RU-A
RU-B
(821)Electric dipole moments at one-loop in the dimension-6 SMEFT
  • Jonathan Kley,
  • Tobias Theil,
  • Elena Venturini,
  • Andreas Weiler
European Physical Journal C (10/2022) doi:10.1140/epjc/s10052-022-10861-5
abstract + abstract -

In this paper we present the complete expressions of the lepton and neutron electric dipole moments (EDMs) in the Standard Model Effective Field Theory (SMEFT), up to 1-loop and dimension-6 level and including both renormalization group running contributions and finite corrections. The latter play a fundamental role in the cases of operators that do not renormalize the dipoles, but there are also classes of operators for which they provide an important fraction, 10-20%, of the total 1-loop contribution, if the new physics scale is around Λ =5 TeV. We present the full set of bounds on each individual Wilson coefficient contributing to the EDMs using both the current experimental constraints, as well as those from future experiments, which are expected to improve by at least an order of magnitude.