Beecroft Institute for Particle Astrophysics and Cosmology

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The role of AGN on the structure, kinematics and evolution of ETGs in the Horizon simulations

(2020)

Authors:

MS Rosito, SE Pedrosa, PB Tissera, NE Chisari, R Dominguez-Tenreiro, Y Dubois, S Peirani, J Devriendt, C Pichon, A Slyz
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A fast semi-discrete optimal transport algorithm for a unique reconstruction of the early Universe

(2020)

Authors:

Bruno Lévy, Roya Mohayaee, Sebastian VON HAUSEGGER
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MIGHTEE: are giant radio galaxies more common than we thought?

Monthly Notices of the Royal Astronomical Society Oxford University Press 501:3 (2020) 3833-3845

Authors:

J Delhaize, Ian Heywood, M Prescott, Matthew Jarvis, I Delvecchio, Ih Whittam, Sv White, Mj Hardcastle, Cl Hale, J Afonso, Y Ao, M Brienza, M Brüggen, Jd Collier, E Daddi, M Glowacki, N Maddox, Lk Morabito, I Prandoni, Z Randriamanakoto, S Sekhar, F An, Nj Adams, S Blyth, Rebecca Bowler, L Leeuw, L Marchetti, Sm Randriamampandry, K Thorat, N Seymour, O Smirnov, Ar Taylor, C Tasse, M Vaccari

Abstract:

We report the discovery of two new giant radio galaxies (GRGs) using the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) survey. Both GRGs were found within a ∼1 deg2 region inside the COSMOS field. They have redshifts of z = 0.1656 and z = 0.3363 and physical sizes of 2.4 and 2.0 Mpc, respectively. Only the cores of these GRGs were clearly visible in previous high-resolution Very Large Array observations, since the diffuse emission of the lobes was resolved out. However, the excellent sensitivity and uv coverage of the new MeerKAT telescope allowed this diffuse emission to be detected. The GRGs occupy an unpopulated region of radio power – size parameter space. Based on a recent estimate of the GRG number density, the probability of finding two or more GRGs with such large sizes at z < 0.4 in a ∼1 deg2 field is only 2.7 × 10−6, assuming Poisson statistics. This supports the hypothesis that the prevalence of GRGs has been significantly underestimated in the past due to limited sensitivity to low surface brightness emission. The two GRGs presented here may be the first of a new population to be revealed through surveys like MIGHTEE that provide exquisite sensitivity to diffuse, extended emission.
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Calibration of QUBIC: The Q and U bolometric interferometer for cosmology

SPIE, the international society for optics and photonics (2020) 174

Authors:

James Murphy, D Burke, MM Gamboa Lerena, Jean-Christophe Hamilton, L Mousset, M De Petris, C O'Sullivan, S Torchinsky, Peter AR Ade, JG Alberro, A Almela, G Amico, LH Arnaldi, D Auguste, J Aumont, S Azzoni, S Banfi, B Bélier, ES Battistelli, A Baù, D Bennett, L Bergé, P de Bernardis, JP Bernard, M Bersanelli, MA Bigot-Sazy, J Bonaparte, J Bonis, E Bunn, D Buzi, F Cavaliere, P Chanial, C Chapron, R Charlassier, AC Cobos Cerutti, F Columbro, A Coppolecchia, G D'Alessandro, G De Gasperis, M De Leo, Stéphane Dheilly, C Duca, L Dumoulin, A Etchegoyen, A Fasciszewski, LP Ferreyro, D Fracchia, Cristian Franceschet, Kenneth Ganga, B García, ME García Redondo, M Gaspard, D Gayer, M Gervasi, M Giard, V Gilles, Y Giraud-Heraud, Laurent Grandsire, M Gómez Berisso, M González, Marcin Gradziel, MR Hampel, D Harari, S Henrot-Versillé, F Incardona, E Jules, J Kaplan, C Kristukat, L Lamagna, S Loucatos, T Louis, B Maffei, S Marnieros, W Marty, A Mattei, A May, M McCulloch, L Mele, S Masi, D Melo, A Mennella, L Montier, LM Mundo, JA Murphy, F Nati, E Olivieri, Christine Oriol, A Paiella, F Pajot, A Passerini, H Pastoriza, A Pelosi, C Perbost, M Perciballi, F Pezzotta, F Piacentini, M Piat, L Piccirillo, G Pisano, M Platino, G Polenta, D Prêle, R Puddu, D Rambaud, E Rasztocky, P Ringegni, GE Romero, JM Salum, C Scóccola, A Schillaci, S Scully, S Spinelli, Guillaume Stankowiak, M Stolpovskiy, AD Supanitsky, A Tartari, JP Thermeau, P Timbie, M Tomasi, G Tucker, Carole Tucker, D Viganò, N Vittorio, F Voisin, F Wicek, M Wright, M Zannoni, A Zullo
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Detection chain and electronic readout of the QUBIC instrument

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X Society of Photo-Optical Instrumentation Engineers 11453 (2020)

Authors:

G Stankowiak, M Piat, Es Battistelli, Susanna Azzoni

Abstract:

The Q and U Bolometric Interferometer for Cosmology (QUBIC) Technical Demonstrator (TD) aiming to shows the feasibility of the combination of interferometry and bolometric detection. The electronic readout system is based on an array of 128 NbSi Transition Edge Sensors cooled at 350mK readout with 128 SQUIDs at 1K controlled and amplified by an Application Specific Integrated Circuit at 40K. This readout design allows a 128:1 Time Domain Multiplexing. We report the design and the performance of the detection chain in this paper. The technological demonstrator unwent a campaign of test in the lab. Evaluation of the QUBIC bolometers and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. Currently the mean Noise Equivalent Power is ~ 2 x 10-16W= p √Hz
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