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1. The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters

Author

Mathew S. Madhavacheril, Frank J. Qu, Blake D. Sherwin, Niall MacCrann, Yaqiong Li, Irene Abril-Cabezas, Peter A. R. Ade, Simone Aiola, Tommy Alford, Mandana Amiri, Stefania Amodeo, Rui An, Zachary Atkins, Jason E. Austermann, Nicholas Battaglia, Elia Stefano Battistelli, James A. Beall, Rachel Bean, Benjamin Beringue, Tanay Bhandarkar, Emily Biermann, Boris Bolliet, J Richard Bond, Hongbo Cai, Erminia Calabrese, Victoria Calafut, Valentina Capalbo, Felipe Carrero, Anthony Challinor, Grace E. Chesmore, Hsiao-mei Cho, Steve K. Choi, Susan E. Clark, Rodrigo Córdova Rosado, Nicholas F. Cothard, Kevin Coughlin, William Coulton, Kevin T. Crowley, Roohi Dalal, Omar Darwish, Mark J. Devlin, Simon Dicker, Peter Doze, Cody J. Duell, Shannon M. Duff, Adriaan J. Duivenvoorden, Jo Dunkley, Rolando Dünner, Valentina Fanfani, Max Fankhanel, Gerrit Farren, Simone Ferraro, Rodrigo Freundt, Brittany Fuzia, Patricio A. Gallardo, Xavier Garrido, Jahmour Givans, Vera Gluscevic, Joseph E. Golec, Yilun Guan, Kirsten R. Hall, Mark Halpern, Dongwon Han, Ian Harrison, Matthew Hasselfield, Erin Healy, Shawn Henderson, Brandon Hensley, Carlos Hervías-Caimapo, J. Colin Hill, Gene C. Hilton, Matt Hilton, Adam D. Hincks, Renée Hložek, Shuay-Pwu Patty Ho, Zachary B. Huber, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Kent Irwin, Giovanni Isopi, Hidde T. Jense, Ben Keller, Joshua Kim, Kenda Knowles, Brian J. Koopman, Arthur Kosowsky, Darby Kramer, Aleksandra Kusiak, Adrien La Posta, Alex Lague, Victoria Lakey, Eunseong Lee, Zack Li, Michele Limon, Martine Lokken, Thibaut Louis, Marius Lungu, Amanda MacInnis, Diego Maldonado, Felipe Maldonado, Maya Mallaby-Kay, Gabriela A. Marques, Jeff McMahon, Yogesh Mehta, Felipe Menanteau, Kavilan Moodley, Thomas W. Morris, Tony Mroczkowski, Sigurd Naess, Toshiya Namikawa, Federico Nati, Laura Newburgh, Andrina Nicola, Michael D. Niemack, Michael R. Nolta, John Orlowski-Scherer, Lyman A. Page, Shivam Pandey, Bruce Partridge, Heather Prince, Roberto Puddu, Federico Radiconi, Naomi Robertson, Felipe Rojas, Tai Sakuma, Maria Salatino, Emmanuel Schaan, Benjamin L. Schmitt, Neelima Sehgal, Shabbir Shaikh, Carlos Sierra, Jon Sievers, Cristóbal Sifón, Sara Simon, Rita Sonka, David N. Spergel, Suzanne T. Staggs, Emilie Storer, Eric R. Switzer, Niklas Tampier, Robert Thornton, Hy Trac, Jesse Treu, Carole Tucker, Joel Ullom, Leila R. Vale, Alexander Van Engelen, Jeff Van Lanen, Joshiwa van Marrewijk, Cristian Vargas, Eve M. Vavagiakis, Kasey Wagoner, Yuhan Wang, Lukas Wenzl, Edward J. Wollack, Zhilei Xu, Fernando Zago, and Kaiwen Zheng

Subjects
Cosmology, Observational cosmology, Cosmic microwave background radiation, Large-scale structure of the universe, Cosmological neutrinos, Particle astrophysics, Astrophysics, QB460-466
Abstract

We present cosmological constraints from a gravitational lensing mass map covering 9400 deg ^2 reconstructed from measurements of the cosmic microwave background (CMB) made by the Atacama Cosmology Telescope (ACT) from 2017 to 2021. In combination with measurements of baryon acoustic oscillations and big bang nucleosynthesis, we obtain the clustering amplitude σ _8 = 0.819 ± 0.015 at 1.8% precision, ${S}_{8}\equiv {\sigma }_{8}{({{\rm{\Omega }}}_{{\rm{m}}}/0.3)}^{0.5}=0.840\pm 0.028$ , and the Hubble constant H _0 = (68.3 ± 1.1) km s ^−1 Mpc ^−1 at 1.6% precision. A joint constraint with Planck CMB lensing yields σ _8 = 0.812 ± 0.013, ${S}_{8}\equiv {\sigma }_{8}{({{\rm{\Omega }}}_{{\rm{m}}}/0.3)}^{0.5}=0.831\pm 0.023$ , and H _0 = (68.1 ± 1.0) km s ^−1 Mpc ^−1 . These measurements agree with ΛCDM extrapolations from the CMB anisotropies measured by Planck. We revisit constraints from the KiDS, DES, and HSC galaxy surveys with a uniform set of assumptions and find that S _8 from all three are lower than that from ACT+Planck lensing by levels ranging from 1.7 σ to 2.1 σ . This motivates further measurements and comparison, not just between the CMB anisotropies and galaxy lensing but also between CMB lensing probing z ∼ 0.5–5 on mostly linear scales and galaxy lensing at z ∼ 0.5 on smaller scales. We combine with CMB anisotropies to constrain extensions of ΛCDM, limiting neutrino masses to ∑ m _ν < 0.13 eV (95% c.l.), for example. We describe the mass map and related data products that will enable a wide array of cross-correlation science. Our results provide independent confirmation that the universe is spatially flat, conforms with general relativity, and is described remarkably well by the ΛCDM model, while paving a promising path for neutrino physics with lensing from upcoming ground-based CMB surveys.

Published
2024
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2. The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and Its Implications for Structure Growth

Author

Frank J. Qu, Blake D. Sherwin, Mathew S. Madhavacheril, Dongwon Han, Kevin T. Crowley, Irene Abril-Cabezas, Peter A. R. Ade, Simone Aiola, Tommy Alford, Mandana Amiri, Stefania Amodeo, Rui An, Zachary Atkins, Jason E. Austermann, Nicholas Battaglia, Elia Stefano Battistelli, James A. Beall, Rachel Bean, Benjamin Beringue, Tanay Bhandarkar, Emily Biermann, Boris Bolliet, J Richard Bond, Hongbo Cai, Erminia Calabrese, Victoria Calafut, Valentina Capalbo, Felipe Carrero, Julien Carron, Anthony Challinor, Grace E. Chesmore, Hsiao-mei Cho, Steve K. Choi, Susan E. Clark, Rodrigo Córdova Rosado, Nicholas F. Cothard, Kevin Coughlin, William Coulton, Roohi Dalal, Omar Darwish, Mark J. Devlin, Simon Dicker, Peter Doze, Cody J. Duell, Shannon M. Duff, Adriaan J. Duivenvoorden, Jo Dunkley, Rolando Dünner, Valentina Fanfani, Max Fankhanel, Gerrit Farren, Simone Ferraro, Rodrigo Freundt, Brittany Fuzia, Patricio A. Gallardo, Xavier Garrido, Vera Gluscevic, Joseph E. Golec, Yilun Guan, Mark Halpern, Ian Harrison, Matthew Hasselfield, Erin Healy, Shawn Henderson, Brandon Hensley, Carlos Hervías-Caimapo, J. Colin Hill, Gene C. Hilton, Matt Hilton, Adam D. Hincks, Renée Hložek, Shuay-Pwu Patty Ho, Zachary B. Huber, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Kent Irwin, Giovanni Isopi, Hidde T. Jense, Ben Keller, Joshua Kim, Kenda Knowles, Brian J. Koopman, Arthur Kosowsky, Darby Kramer, Aleksandra Kusiak, Adrien La Posta, Alex Lague, Victoria Lakey, Eunseong Lee, Zack Li, Yaqiong Li, Michele Limon, Martine Lokken, Thibaut Louis, Marius Lungu, Niall MacCrann, Amanda MacInnis, Diego Maldonado, Felipe Maldonado, Maya Mallaby-Kay, Gabriela A. Marques, Jeff McMahon, Yogesh Mehta, Felipe Menanteau, Kavilan Moodley, Thomas W. Morris, Tony Mroczkowski, Sigurd Naess, Toshiya Namikawa, Federico Nati, Laura Newburgh, Andrina Nicola, Michael D. Niemack, Michael R. Nolta, John Orlowski-Scherer, Lyman A. Page, Shivam Pandey, Bruce Partridge, Heather Prince, Roberto Puddu, Federico Radiconi, Naomi Robertson, Felipe Rojas, Tai Sakuma, Maria Salatino, Emmanuel Schaan, Benjamin L. Schmitt, Neelima Sehgal, Shabbir Shaikh, Carlos Sierra, Jon Sievers, Cristóbal Sifón, Sara Simon, Rita Sonka, David N. Spergel, Suzanne T. Staggs, Emilie Storer, Eric R. Switzer, Niklas Tampier, Robert Thornton, Hy Trac, Jesse Treu, Carole Tucker, Joel Ullom, Leila R. Vale, Alexander Van Engelen, Jeff Van Lanen, Joshiwa van Marrewijk, Cristian Vargas, Eve M. Vavagiakis, Kasey Wagoner, Yuhan Wang, Lukas Wenzl, Edward J. Wollack, Zhilei Xu, Fernando Zago, and Kaiwen Zheng

Subjects
Cosmological parameters, Cosmological parameters from large-scale structure, Astrophysics, QB460-466
Abstract

We present new measurements of cosmic microwave background (CMB) lensing over 9400 deg ^2 of the sky. These lensing measurements are derived from the Atacama Cosmology Telescope (ACT) Data Release 6 (DR6) CMB data set, which consists of five seasons of ACT CMB temperature and polarization observations. We determine the amplitude of the CMB lensing power spectrum at 2.3% precision (43 σ significance) using a novel pipeline that minimizes sensitivity to foregrounds and to noise properties. To ensure that our results are robust, we analyze an extensive set of null tests, consistency tests, and systematic error estimates and employ a blinded analysis framework. Our CMB lensing power spectrum measurement provides constraints on the amplitude of cosmic structure that do not depend on Planck or galaxy survey data, thus giving independent information about large-scale structure growth and potential tensions in structure measurements. The baseline spectrum is well fit by a lensing amplitude of A _lens = 1.013 ± 0.023 relative to the Planck 2018 CMB power spectra best-fit ΛCDM model and A _lens = 1.005 ± 0.023 relative to the ACT DR4 + WMAP best-fit model. From our lensing power spectrum measurement, we derive constraints on the parameter combination ${S}_{8}^{\mathrm{CMBL}}\equiv {\sigma }_{8}{\left({{\rm{\Omega }}}_{m}/0.3\right)}^{0.25}$ of ${S}_{8}^{\mathrm{CMBL}}=0.818\pm 0.022$ from ACT DR6 CMB lensing alone and ${S}_{8}^{\mathrm{CMBL}}=0.813\pm 0.018$ when combining ACT DR6 and Planck NPIPE CMB lensing power spectra. These results are in excellent agreement with ΛCDM model constraints from Planck or ACT DR4 + WMAP CMB power spectrum measurements. Our lensing measurements from redshifts z ∼ 0.5–5 are thus fully consistent with ΛCDM structure growth predictions based on CMB anisotropies probing primarily z ∼ 1100. We find no evidence for a suppression of the amplitude of cosmic structure at low redshifts.

Published
2024
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4. Atacama Cosmology Telescope: Combined kinematic and thermal Sunyaev-Zel’dovich measurements from BOSS CMASS and LOWZ halos

Author

Emmanuel Schaan, Simone Ferraro, Stefania Amodeo, Nicholas Battaglia, Simone Aiola, Jason E. Austermann, James A. Beall, Rachel Bean, Daniel T. Becker, Richard J. Bond, Erminia Calabrese, Victoria Calafut, Steve K. Choi, Edward V. Denison, Mark J. Devlin, Shannon M. Duff, Adriaan J. Duivenvoorden, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Dongwon Han, J. Colin Hill, Gene C. Hilton, Matt Hilton, Renée Hložek, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Brian J. Koopman, Amanda MacInnis, Jeff McMahon, Mathew S. Madhavacheril, Kavilan Moodley, Tony Mroczkowski, Sigurd Naess, Federico Nati, Laura B. Newburgh, Michael D. Niemack, Lyman A. Page, Bruce Partridge, Maria Salatino, Neelima Sehgal, Alessandro Schillaci, Cristóbal Sifón, Kendrick M. Smith, David N. Spergel, Suzanne Staggs, Emilie R. Storer, Hy Trac, Joel N. Ullom, Jeff Van Lanen, Leila R. Vale, Alexander van Engelen, Mariana Vargas Magaña, Eve M. Vavagiakis, Edward J. Wollack, and Zhilei Xu

Published
2021
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5. The Atacama Cosmology Telescope: DR4 maps and cosmological parameters

Author

Simone Aiola, Erminia Calabrese, Loic Maurin, Sigurd Naess, Benjamin L. Schmitt, Maximilian H. Abitbol, Graeme E. Addison, Peter A. R. Ade, David Alonso, Mandana Amiri, Stefania Amodeo, Elio Angile, Jason E. Austermann, Taylor Baildon, Nick Battaglia, James A. Beall, Rachel Bean, Daniel T. Becker, J Richard Bond, Sarah Marie Bruno, Victoria Calafut, Luis E. Campusano, Felipe Carrero, Grace E. Chesmore, Hsiao-mei Cho, Steve K. Choi, Susan E. Clark, Nicholas F. Cothard, Devin Crichton, Kevin T. Crowley, Omar Darwish, Rahul Datta, Edward V. Denison, Mark J. Devlin, Cody J. Duell, Shannon M. Duff, Adriaan J. Duivenvoorden, Jo Dunkley, Rolando Dunner, Thomas Essinger-Hileman, Max Fankhanel, Simone Ferraro, Anna E. Fox, Brittany Fuzia, Patricio A. Gallardo, Vera Gluscevic, Joseph E. Golec, Emily Grace, Megan Gralla, Yilun Guan, 8 Mark Halpern, Dongwon Han, Peter Hargrave, Matthew Hasselfield, Jakob M. Helton, Shawn Henderson, Brandon Hensley, J. Colin Hill, Gene C. Hilton, Matt Hilton, Adam D. Hincks, Renee Hlozek, Shuay-Pwu Patty Ho, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Leopoldo Infante, Kent Irwin, Rebecca Jackson, Jeff Klein, Kenda Knowles, Brian Koopman, Arthur Kosowsky, Vincent Lakey, Dale Li, Yaqiong Li, Zack Li, Martine Lokken, Thibaut Louis, Marius Lungu, Amanda MacInnis, Mathew Madhavacheril, Felipe Maldonado, Maya Mallaby-Kay, Danica Marsden, Jeff McMahon, Felipe Menanteau, Kavilan Moodley, Tim Morton, Toshiya Namikawa, Federico Nati, Laura Newburgh, John P. Nibarger, Andrina Nicola, Michael D. Niemack, Michael R. Nolta, John Orlowski-Sherer, Lyman A. Page, Christine G. Pappas, Bruce Partridge, Phumlani Phakathi, Giampaolo Pisano, Heather Prince, Roberto Puddu, Frank J. Qu, Jesus Rivera, Naomi Robertson, Felipe Rojas, Maria Salatino, Emmanuel Schaan, Alessandro Schillaci, Neelima Sehgal, Blake D. Sherwin, Carlos Sierra, Jon Sievers, Cristobal Sifon, Precious Sikhosana, Sara Simon, David N. Spergel, Suzanne T. Staggs, Jason Stevens, Emilie Storer, Dhaneshwar D. Sunder, Eric R. Switzer, Ben Thorne, Robert Thornton, Hy Trac, Jesse Treu, Carole Tucker, Leila R. Vale, Alexander Van Engelen, Jeff Van Lanen, Eve M. Vavagiakis, Kasey Wagoner, Yuhan Wang, Jonathan T. Ward, Edward J Wollack, Zhilei Xu, Fernando Zago, and Ningfeng Zhu

Subjects
Astrophysics, Physics Of Elementary Particles And Fields
Abstract

We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013{2016 at 98 and 150 GHz. The maps cover more than 17,000 deg(^2), the deepest 600 deg(^2) with noise levels below 10µK-arcmin. We use the power spectrum derived from almost 6,000 deg(^2) of these maps to constrain cosmology. The ACT data enable a measurement of the angular scale of features in both the divergence-like polarization and the temperature anisotropy, tracing both the velocity and density at last-scattering. From these one can derive the distance to the last-scattering surface and thus infer the local expansion rate, H0. By combining ACT data with large-scale information from WMAP we measure H0 = 67:6±1:1 km/s/Mpc, at 68% confidence, in excellent agreement with the independently measured Planck satellite estimate (from ACT alone we find H0 = 67:9± 1:5 km/s/Mpc). The ΛCDM model provides a good fit to the ACT data, and we find no evidence for deviations: both the spatial curvature, and the departure from the standard lensing signal in the spectrum, are zero to within 1σ; the number of relativistic species, the primordial Helium fraction, and the running of the spectral index are consistent with ΛCDM predictions to within 1.5{2.2σ. We compare ACT, WMAP, and Planck at the parameter level and find good consistency; we investigate how the constraints on the correlated spectral index and baryon density parameters readjust when adding CMB large-scale information that ACT does not measure. The DR4 products presented here will be publicly released on the NASA Legacy Archive for Microwave Background Data Analysis.

Published
2020
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6. The Atacama Cosmology Telescope: Weighing Distant Clusters with the Most Ancient Light

Author

Mathew S. Madhavacheril, Cristobal Sifon, Nicholas Battaglia, Simone Aiola, Stefania Amodeo, Jason E. Austermann, James A. Beall, Daniel T. Becker, J. Richard Bond, Erminia Calabrese, Steve K. Choi, Edward V. Denison, Mark J Devlin, Simon R. Dicker, Shannon M. Duff, Adriaan J. Duivenvoorden, Jo Dunkley, Rolando Dunner, Simone Ferraro, Patricio A. Gallardo, Yilun Guan, Dongwon Han, J. Colin Hill, Gene C Hilton, Matt Hilton, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Brian J. Koopman, Arthur Kosowsky, Jeff Van Lanen, Eunseong Lee, Thibaut Louis, Amanda MacInnis, Jeffrey McMahon, Kavilan Moodley, Sigurd Naess, Toshiya Namikawa, Federico Nati, Laura Newburgh, Michael D. Niemack, Lyman A. Page, Bruce Partridge, Frank J. Qu, Naomi C. Robertson, Maria Salatino, Emmanuel Schaan, Alessandro Schillaci, Benjamin L. Schmitt, Neelima Sehgal, Blake D. Sherwin, Sara M. Simon, David N. Spergel, Suzanne Staggs, Emilie R. Storer, Joel N. Ullom, Leila R. Vale, Alexander van Engelen, Eve M. Vavagiakis, Edward J Wollack, and Zhilei Xu

Subjects
Earth Resources And Remote Sensing, Space Sciences (General)
Abstract

We use gravitational lensing of the cosmic microwave background (CMB) to measure the mass of the most distant blindly selected sample of galaxy clusters on which a lensing measurement has been performed to date. In CMB data from the the Atacama Cosmology Telescope and the Planck satellite, we detect the stacked lensing effect from 677 near-infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS), which have a mean redshift of (z)=1.08. There are currently no representative optical weak lensing measurements of clusters that match the distance and average mass of this sample. We detect the lensing signal with a significance of . We model the signal with a halo model framework to find the mean mass of the population from which these clusters are drawn. Assuming that the clusters follow Navarro–Frenk–White (NFW) density profiles, we infer a mean mass of (M(500c))=(1.7 ± 0.4) x 10^14M(ʘ). We consider systematic uncertainties from cluster redshift errors, centering errors, and the shape of the NFW profile. These are all smaller than 30% of our reported uncertainty. This work highlights the potential of CMB lensing to enable cosmological constraints from the abundance of distant clusters populating ever larger volumes of the observable universe, beyond the capabilities of optical weak lensing measurements.

Published
2020
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8. SciLake Deliverable 6.1: Communication, engagement, and exploitation Plan

Author

Stefania Amodeo, Zacharoula Xenou, and Natalia Manola

Abstract

Initial planning and preparation for SciLake communication, engagement, and exploitation activities., The deliverable awaits official approval by the Project Officer. This project has received funding from the European Union's Horizon Europe framework programme under grant agreement No.101058573. Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Executive Agency. Neither the European Union nor the European Research Executive Agency can be held responsible for them.

Published
2023
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9. Constraining Cosmic Microwave Background Temperature Evolution With Sunyaev–Zel’Dovich Galaxy Clusters from the Atacama Cosmology Telescope

Author

Yunyang 云炀 Li 李, Adam D. Hincks, Stefania Amodeo, Elia S. Battistelli, J. Richard Bond, Erminia Calabrese, Steve K. Choi, Mark J. Devlin, Jo Dunkley, Simone Ferraro, Vera Gluscevic, Yilun Guan, Mark Halpern, Matt Hilton, Renee Hlozek, Tobias A. Marriage, Jeff McMahon, Kavilan Moodley, Sigurd Naess, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Bruce Partridge, Maria Salatino, Emmanuel Schaan, Alessandro Schillaci, Neelima Sehgal, Cristóbal Sifón, Suzanne T. Staggs, Alexander van Engelen, Edward J. Wollack, and Zhilei Xu

Published
2021
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10. Erratum: Atacama Cosmology Telescope: Modeling the gas thermodynamics in BOSS CMASS galaxies from kinematic and thermal Sunyaev-Zel’dovich measurements [Phys. Rev. D 103 , 063514 (2021)]

Author

Stefania Amodeo, Nicholas Battaglia, Emmanuel Schaan, Simone Ferraro, Emily Moser, Simone Aiola, Jason E. Austermann, James A. Beall, Rachel Bean, Daniel T. Becker, Richard J. Bond, Erminia Calabrese, Victoria Calafut, Steve K. Choi, Edward V. Denison, Mark Devlin, Shannon M. Duff, Adriaan J. Duivenvoorden, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Kirsten R. Hall, Dongwon Han, J. Colin Hill, Gene C. Hilton, Matt Hilton, Renée Hložek, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Brian J. Koopman, Amanda MacInnis, Jeff McMahon, Mathew S. Madhavacheril, Kavilan Moodley, Tony Mroczkowski, Sigurd Naess, Federico Nati, Laura B. Newburgh, Michael D. Niemack, Lyman A. Page, Bruce Partridge, Alessandro Schillaci, Neelima Sehgal, Cristóbal Sifón, David N. Spergel, Suzanne Staggs, Emilie R. Storer, Joel N. Ullom, Leila R. Vale, Alexander van Engelen, Jeff Van Lanen, Eve M. Vavagiakis, Edward J. Wollack, and Zhilei Xu

Published
2023

11. Morphology-density Relation, Quenching, and Mergers in CARLA Clusters and Proto-Clusters at $1.4<z<2.8$

Author

Simona Mei, Nina A. Hatch, Stefania Amodeo, Anton V. Afanasiev, Carlos De Breuck, Daniel Stern, Elizabeth A. Cooke, Anthony H. Gonzalez, Gaël Noirot, Alessandro Rettura, Nick Seymour, Spencer A. Stanford, Joël Vernet, Dominika Wylezalek, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Space and Planetary Science, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies
Abstract

(Abridged) To understand if the morphology-density and passive-density relations are already established at z>1.5, we study galaxies in 16 confirmed clusters at $1.3, Comment: 31 pages, 22 figures, A&A, in press

Published
2022

12. The galaxy mass-size relation in CARLA clusters and proto-clusters at 1.4 < z < 2.8: Larger cluster galaxy sizes

Author

Anton V. Afanasiev, Simona Mei, Hao Fu, Francesco Shankar, Stefania Amodeo, Daniel Stern, Elizabeth A. Cooke, Anthony H. Gonzalez, Gaël Noirot, Alessandro Rettura, Dominika Wylezalek, Carlos De Breuck, Nina A. Hatch, Spencer A. Stanford, Joël Vernet, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies
Abstract

(Abridged) We study the galaxy mass-size relation in CARLA spectroscopically confirmed clusters at $1.410.5$ are systematically $\gtrsim 0.2-0.3~{\rm dex}$ larger than field ETGs. The passive ETG average size evolution is slower at $1, Comment: 15 pages, 10 figures, accepted for publication in Astronomy & Astrophysics

Published
2023

13. Probing Hot Gas Components of Circumgalactic Medium in Cosmological Simulations with the Thermal Sunyaev-Zel'dovich Effect

Author

Junhan Kim, Sunil Golwala, James G. Bartlett, Stefania Amodeo, Nicholas Battaglia, Andrew J. Benson, J. Colin Hill, Philip F. Hopkins, Cameron B. Hummels, Emily Moser, Matthew E. Orr, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The thermal Sunyaev-Zel'dovich (tSZ) effect is a powerful tool with the potential for constraining directly the properties of the hot gas that dominates dark matter halos because it measures pressure and thus thermal energy density. Studying this hot component of the circumgalactic medium (CGM) is important because it is strongly impacted by star-formation and active galactic nuclei (AGN) activity in galaxies, participating in the feedback loop that regulates star and black hole mass growth in galaxies. We study the tSZ effect across a wide halo mass range using three cosmological hydrodynamical simulations: Illustris-TNG, EAGLE, and FIRE-2. Specifically, we present the scaling relation between tSZ signal and halo mass and radial profiles of gas density, temperature, and pressure for all three simulations. The analysis includes comparisons to Planck tSZ observations and to the thermal pressure profile inferred from the Atacama Cosmology Telescope (ACT) measurements. We compare these tSZ data to the simulations to interpret the measurements in terms of feedback and accretion processes in the CGM. We also identify as-yet unobserved potential signatures of these processes that may be visible in future measurements, which will have the capability of measuring tSZ signals to even lower masses. We also perform internal comparisons between runs with different physical assumptions. We conclude: (1) there is strong evidence for the impact of feedback at $R_{500}$ but that this impact decreases by $5R_{500}$, and (2) the thermodynamic profiles of the CGM are highly dependent on the implemented model, such as cosmic-ray or AGN feedback prescriptions., 21 pages, 10 figures, submitted to ApJ, comments welcome

Published
2021

14. Constraining baryonic feedback and cosmology with weak-lensing, X-ray, and kinematic Sunyaev-Zeldovich observations

Author

Aurel Schneider, Sambit K Giri, Stefania Amodeo, Alexandre Refregier, University of Zurich, and Schneider, Aurel

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 1912 Space and Planetary Science, 530 Physics, Space and Planetary Science, 10231 Institute for Computational Science, FOS: Physical sciences, 3103 Astronomy and Astrophysics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Modern weak-lensing observations are becoming increasingly sensitive to baryonic feedback processes which are still poorly understood. So far, this challenge has been faced either by imposing scale-cuts in the data or by modelling baryonic effects with simple, one-parameter models. In this paper, we rely on a more general, seven-parameter prescription of baryonic feedback effects, which is primarily motivated by observations and has been shown to agree with a plethora of hydrodynamical simulations. By combining weak-lensing data from the Kilo-Degree Survey (KiDS-1000) with observations of gas around galaxy clusters, we are able to constrain baryonic parameters and learn more about feedback and cosmology. In particular, we use cluster gas fractions from X-ray data and gas profiles from kinematic Sunyaev-Zeldovich (kSZ) observations to provide evidence for baryonic feedback that is stronger than predicted by most hydrodynamical simulations. In terms of the matter power spectrum, we report a beyond-percent effect at wave-modes above $k\sim 0.1-0.45$ h/Mpc and a maximum suppression of $12-33$ percent at $k\sim7$ h/Mpc (68 percent confidence level). Regarding the combined parameter $\Sigma_8=\sigma_8(\Omega_m/0.3)^{0.58}$, we find the known tension with the Planck satellite data to be reduced from 3.8 to 2.9 $\sigma$ once baryonic effects are fully included in the analysis pipeline. The tension is further decreased to 2.6 $\sigma$ when the weak-lensing data is combined with X-ray and kSZ observations. We conclude that, while baryonic feedback effects become more important in modern weak-lensing surveys, they are unlikely to act as the main culprit for the observed $\Sigma_8$-tension., Comment: 14 pages, 9 figures, published in MNRAS

Published
2021

15. The Impacts of Modeling Choices on the Inference of Circumgalactic Medium Properties from Sunyaev–Zeldovich Observations

Author

Emily Moser, Nicholas Battaglia, Marcelo A. Alvarez, Emmanuel Schaan, Simone Ferraro, and Stefania Amodeo

Subjects
Matching (statistics), astro-ph.GA, FOS: Physical sciences, Sample (statistics), Bioengineering, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Atomic, Particle and Plasma Physics, 0103 physical sciences, Nuclear, Statistical physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Mass distribution, 010308 nuclear & particles physics, Molecular, Astronomy and Astrophysics, Observable, Astrophysics - Astrophysics of Galaxies, Galaxy, Term (time), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, Astronomical and Space Sciences, Free parameter, Physical Chemistry (incl. Structural)
Abstract

As the signal-to-noise of Sunyaev-Zeldovich (SZ) cross-correlation measurements of galaxies improves our ability to infer properties about the circumgalactic medium (CGM), we will transition from being limited by statistical uncertainties to systematic uncertainties. Using thermodynamic profiles of the CGM created from the IllustrisTNG (The Next Generation) simulations we investigate the importance of specific choices in modeling the galaxy sample. These choices include different sample selections in the simulation (stellar versus halo mass, color selections) and different fitting models (matching by the shape of the mass distribution, inclusion of a two-halo term). We forward model a mock galaxy sample into projected SZ observable profiles and fit these profiles to a generalized Navarro-Frenk-White profile using forecasted errors of the upcoming Simons Observatory experiment. We test the number of free parameters in the fits and show that this is another modeling choice that yields different results. Finally, we show how different fitting models can reproduce parameters of a fiducial profile, and show that the addition of a two-halo term and matching by the mass distribution of the sample are extremely important modeling choices to consider., 23 pages, 9 figures, published in the Astrophysical Journal

Published
2021

16. Atacama Cosmology Telescope measurements of a large sample of candidates from the Massive and Distant Clusters of WISE Survey: Sunyaev-Zeldovich effect confirmation of MaDCoWS candidates using ACT

Author

Suzanne T. Staggs, Dongwon Han, Alessandro Schillaci, Kavilan Moodley, Charles Romero, Anthony H. Gonzalez, Simon Dicker, Maria Salatino, Zhilei Xu, Tanay Bhandarkar, Mark Brodwin, Neelima Sehgal, Alex Manduca, Federico Nati, Spencer A. Stanford, Eve M. Vavagiakis, Robert Thornton, Luca Di Mascolo, Jo Dunkley, Brian J. Koopman, Matt Hilton, Bruce Partridge, Mark J. Devlin, Steve K. Choi, Edward J. Wollack, Tony Mroczkowski, Michael D. Niemack, Kenda Knowles, Lyman A. Page, Stefania Amodeo, Nick Battaglia, Cristóbal Sifón, Amanda MacInnis, Kevin M. Huffenberger, Ningfeng Zhu, John P. Hughes, Ian Lowe, John Orlowski-Scherer, Orlowski-Scherer, J, Di Mascolo, L, Bhandarkar, T, Manduca, A, Mroczkowski, T, Amodeo, S, Battaglia, N, Brodwin, M, Choi, S, Devlin, M, Dicker, S, Dunkley, J, Gonzalez, A, Han, D, Hilton, M, Huffenberger, K, Hughes, J, Macinnis, A, Knowles, K, Koopman, B, Lowe, I, Moodley, K, Nati, F, Niemack, M, Page, L, Partridge, B, Romero, C, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, Staggs, S, Stanford, S, Thornton, R, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Orlowski-Scherer, J., Di Mascolo, L., Bhandarkar, T., Manduca, A., Mroczkowski, T., Amodeo, S., Battaglia, N., Brodwin, M., Choi, S. K., Devlin, M., Dicker, S., Dunkley, J., Gonzalez, A. H., Han, D., Hilton, M., Huffenberger, K., Hughes, J. P., Macinnis, A., Knowles, K., Koopman, B. J., Lowe, I., Moodley, K., Nati, F., Niemack, M. D., Page, L. A., Partridge, B., Romero, C., Salatino, M., Schillaci, A., Sehgal, N., Sifon, C., Staggs, S., Stanford, S. A., Thornton, R., Vavagiakis, E. M., Wollack, E. J., Xu, Z., and Zhu, N.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, Context (language use), clusters: intracluster medium [Galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cosmic background radiation, Radio continuum: galaxie, 01 natural sciences, Radio continuum: galaxies, galaxies [Submillimeter], Submillimeter: galaxie, Spitzer Space Telescope, Galaxies: clusters: general, Galaxies: clusters: intracluster medium, Submillimeter: galaxies, 0103 physical sciences, Galaxy formation and evolution, Cluster (physics), galaxie [Radio continuum], 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Atacama Cosmology Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Galaxy clusters are an important tool for cosmology, and their detection and characterization are key goals for current and future surveys. Using data from the Wide-field Infrared Survey Explorer (WISE), the Massive and Distant Clusters of WISE Survey (MaDCoWS) located 2,839 significant galaxy overdensities at redshifts $0.7\lesssim z\lesssim 1.5$, which included extensive follow-up imaging from the Spitzer Space Telescope to determine cluster richnesses. Concurrently, the Atacama Cosmology Telescope (ACT) has produced large area mm-wave maps in three frequency bands along with a large catalog of Sunyaev-Zeldovich (SZ) selected clusters, as part of its Data Release 5 (DR5). Using the maps and cluster catalog from DR5, we explore the scaling between SZ mass and cluster richness. We use complementary radio survey data from the Very Large Array, submillimeter data from Herschel, and ACT 224~GHz data to assess the impact of contaminating sources on the SZ signals. We then use a hierarchical Bayesian model to fit the mass-richness scaling relation. We find that MaDCoWS clusters have submillimeter contamination which is consistent with a gray-body spectrum, while the ACT clusters are consistent with no submillimeter emission on average. We find the best fit ACT SZ mass vs. MaDCoWS richness scaling relation has a slope of $\kappa = 1.84^{+0.15}_{-0.14}$, where the slope is defined as $M\propto \lambda_{15}^{\kappa}$ where $\lambda_{15}$ is the richness. Additionally, we find that the approximate level of in-fill of the ACT and MaDCoWS cluster SZ signals to be at the percent level, Comment: 25 pages, 17 Figures; accepted for publication in A&A

Published
2021

17. The Atacama Cosmology Telescope: A Measurement of the Cosmic Microwave Background Power Spectra at 98 and 150 GHz

Author

Kavilan Moodley, Emilie R. Storer, Simone Aiola, Phumlani Phakathi, Jeff Van Lanen, E. Grace, Stefania Amodeo, Felipe Rojas, Yaqiong Li, Nick Battaglia, Precious Sikhosana, Suzanne T. Staggs, Vera Gluscevic, Robert Thornton, Benjamin L. Schmitt, Christine G. Pappas, Rolando Dünner, Danica Marsden, Yilun Guan, Felipe Carrero, Blake D. Sherwin, Sigurd Naess, Leopoldo Infante, Adam D. Hincks, Toshiya Namikawa, Zhilei Xu, Brittany Fuzia, Graeme E. Addison, Kasey Wagoner, Daniel T. Becker, J. Richard Bond, Jason E. Austermann, Sarah Marie Bruno, Matthew Hasselfield, Naomi Robertson, Jesse Treu, Vincent Lakey, John P. Nibarger, Timothy D. Morton, Sara M. Simon, David N. Spergel, Jesus Rivera, Michael R. Nolta, Zack Li, Shawn W. Henderson, Max Fankhanel, Martine Lokken, B. Thorne, Mark J. Devlin, Thomas Essinger-Hileman, James A. Beall, Yuhan Wang, Kevin T. Crowley, John Orlowski-Sherer, Bruce Partridge, Adriaan J. Duivenvoorden, Laura Newburgh, Grace E. Chesmore, Alessandro Schillaci, Jon Sievers, Dhaneshwar D. Sunder, Federico Nati, Rahul Datta, Dale Li, Shuay-Pwu Patty Ho, Shannon M. Duff, Edward V. Denison, Peter A. R. Ade, Mathew S. Madhavacheril, Maya Mallaby-Kay, Erminia Calabrese, Roberto Puddu, J. Colin Hill, Elio Angile, Jo Dunkley, Omar Darwish, Kenda Knowles, Marius Lungu, Megan Gralla, Susan E. Clark, Jeff Klein, Fernando Zago, Dongwon Han, Brandon S. Hensley, Devin Crichton, Renée Hložek, Peter Charles Hargrave, Frank J. Qu, Neelima Sehgal, Leila R. Vale, Matt Hilton, Gene C. Hilton, Joseph E. Golec, Heather Prince, Mandana Amiri, Alexander van Engelen, Maria Salatino, Loïc Maurin, Andrina Nicola, Lyman A. Page, Thibaut Louis, Steve K. Choi, Michael D. Niemack, Eve M. Vavagiakis, Nicholas F. Cothard, Victoria Calafut, Jonathan T. Ward, Carole Tucker, Arthur Kosowsky, Kevin M. Huffenberger, Kent D. Irwin, Hsiao-Mei Cho, Edward J. Wollack, Anna E. Fox, Ningfeng Zhu, Amanda MacInnis, Felipe Maldonado, Brian J. Koopman, Jeff McMahon, Cristóbal Sifón, Emmanuel Schaan, Johannes Hubmayr, Mark Halpern, Simone Ferraro, Hy Trac, Patricio A. Gallardo, Maximilian H. Abitbol, Taylor Baildon, Luis E. Campusano, Rebecca Jackson, Carlos Sierra, Felipe Menanteau, Jason R. Stevens, John P. Hughes, Cody J. Duell, Eric R. Switzer, Kirsten Hall, Rachel Bean, David Alonso, Choi, S, Hasselfield, M, Ho, S, Koopman, B, Lungu, M, Abitbol, M, Addison, G, Ade, P, Aiola, S, Alonso, D, Amiri, M, Amodeo, S, Angile, E, Austermann, J, Baildon, T, Battaglia, N, Beall, J, Bean, R, Becker, D, Richard Bond, J, Bruno, S, Calabrese, E, Calafut, V, Campusano, L, Carrero, F, Chesmore, G, Cho, H, Clark, S, Cothard, N, Crichton, D, Crowley, K, Darwish, O, Datta, R, Denison, E, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Essinger-Hileman, T, Fankhanel, M, Ferraro, S, Fox, A, Fuzia, B, Gallardo, P, Gluscevic, V, Golec, J, Grace, E, Gralla, M, Guan, Y, Hall, K, Halpern, M, Han, D, Hargrave, P, Henderson, S, Hensley, B, Colin Hill, J, Hilton, G, Hilton, M, Hincks, A, Hlozek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Infante, L, Irwin, K, Jackson, R, Klein, J, Knowles, K, Kosowsky, A, Lakey, V, Li, D, Li, Y, Li, Z, Lokken, M, Louis, T, Macinnis, A, Madhavacheril, M, Maldonado, F, Mallaby-Kay, M, Marsden, D, Maurin, L, Mcmahon, J, Menanteau, F, Moodley, K, Morton, T, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nibarger, J, Nicola, A, Niemack, M, Nolta, M, Orlowski-Sherer, J, Page, L, Pappas, C, Partridge, B, Phakathi, P, Prince, H, Puddu, R, Qu, F, Rivera, J, Robertson, N, Rojas, F, Salatino, M, Schaan, E, Schillaci, A, Schmitt, B, Sehgal, N, Sherwin, B, Sierra, C, Sievers, J, Sifon, C, Sikhosana, P, Simon, S, Spergel, D, Staggs, S, Stevens, J, Storer, E, Sunder, D, Switzer, E, Thorne, B, Thornton, R, Trac, H, Treu, J, Tucker, C, Vale, L, van Engelen, A, van Lanen, J, Vavagiakis, E, Wagoner, K, Wang, Y, Ward, J, Wollack, E, Xu, Z, Zago, F, Zhu, N, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and ACT

Subjects
Physics, CMBR polarisation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Library science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmological parameters from CMBR, 0103 physical sciences, Atacama Cosmology Telescope, CMBR experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the temperature and polarization angular power spectra of the CMB measured by the Atacama Cosmology Telescope (ACT) from 5400 deg$^2$ of the 2013-2016 survey, which covers $>$15000 deg$^2$ at 98 and 150 GHz. For this analysis we adopt a blinding strategy to help avoid confirmation bias and, related to this, show numerous checks for systematic error done before unblinding. Using the likelihood for the cosmological analysis we constrain secondary sources of anisotropy and foreground emission, and derive a "CMB-only" spectrum that extends to $\ell=4000$. At large angular scales, foreground emission at 150 GHz is $\sim$1% of TT and EE within our selected regions and consistent with that found by Planck. Using the same likelihood, we obtain the cosmological parameters for $\Lambda$CDM for the ACT data alone with a prior on the optical depth of $\tau=0.065\pm0.015$. $\Lambda$CDM is a good fit. The best-fit model has a reduced $\chi^2$ of 1.07 (PTE=0.07) with $H_0=67.9\pm1.5$ km/s/Mpc. We show that the lensing BB signal is consistent with $\Lambda$CDM and limit the celestial EB polarization angle to $\psi_P =-0.07^{\circ}\pm0.09^{\circ}$. We directly cross correlate ACT with Planck and observe generally good agreement but with some discrepancies in TE. All data on which this analysis is based will be publicly released., Comment: 44 pages, 27 figures, products available on the NASA LAMBDA website, version accepted for publication in JCAP

Published
2020
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18. Massive molecular gas reservoir around the central AGN in the CARLA J1103+3449 cluster at z=1.44

Author

Gaël Noirot, Carlos De Breuck, Dominika Wylezalek, Francoise Combes, Vladan Markov, Nick Seymour, Daniel Stern, Simona Mei, Anthony H. Gonzalez, Audrey Galametz, Philippe Salomé, Nina A. Hatch, Alessandro Rettura, E. A. Cooke, Stefania Amodeo, Spencer A. Stanford, Joel Vernet, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: clusters: individual: CARLA J1103 + 3449, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, radio continuum: galaxies, Spectral index, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, galaxies: jets, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Synchrotron emission, 13. Climate action, Space and Planetary Science, galaxies: star formation, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Passive early-type galaxies dominate cluster cores at z $\lesssim$1.5. At higher redshift, cluster core galaxies are observed to have still on-going star-formation, fuelled by cold molecular gas. We measure the molecular gas reservoir of the central region around the radio-loud AGN in the cluster CARLA J1103+3449 at z=1.44 with NOEMA. The AGN synchrotron emission dominates the continuum emission at 94.48 GHz, and we measure its flux at the AGN position and at the position of two radio jets. Combining our measurements with published results over the range 4.71 GHz-94.5 GHz, we obtain a flat spectral index $\alpha = 0.14 \pm 0.03$ for the AGN core emission, and a steeper index $\alpha = 1.43 \pm 0.04$ and $\alpha = 1.15 \pm 0.04$ at positions close to the western and eastern lobe, respectively. The total spectral index is $\alpha = 0.92 \pm 0.02$ over the range 73.8 MHz-94.5 GHz. We detect two CO(2-1) emission lines, both blue-shifted with respect to the AGN. Their emission corresponds to two regions, ~17 kpc south-east and ~14 kpc south-west of the AGN, not associated with galaxies. In these two regions, we find a total massive molecular gas reservoir of $M_{gas}$ = 3.9 $\pm$ 0.4 $10^{10} M_{\odot}$, which dominates (~ 60%) the central total molecular gas reservoir. These results can be explained by massive cool gas flows in the center of the cluster. The AGN early-type host is not yet quenched; its star formation rate is consistent with being on the main sequence of star-forming galaxies in the field (SFR~30-140 $M_{\odot}$/yr), and the cluster core molecular gas reservoir is expected to feed the AGN and the host star-formation before quiescence. The other cluster confirmed members show star formation rates at ~2 $\sigma$ below the field main sequence at similar redshifts and do not have molecular gas masses larger than galaxies of similar stellar mass in the field., Comment: 18 pages, 14 figures, A&A, accepted for publication

Published
2020
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19. I sette nodi del destino

Author

Stefania Amodeo and Stefania Amodeo

Abstract

Il destino unisce le vite di Alexandra Marshall, giovane ricercatrice universitaria appassionata di fotografia a quello di Robert James Sander, affascinante opinion leader del Sud degli Stati Uniti, scrittore di fama. Alexandra conosce l'uomo soltanto attraverso i suoi libri, ma la profezia della saggia nonna di lui, nativa americana chiamata Sposa del Mare, annuncia grandi cambiamenti che infine avverranno. Si ritroveranno in Sudafrica a preparare un reportage per il giornale «Wild Life» e a concorrere al più ambito premio del settore. Soprattutto, apprenderanno il significato dei “sette nodi del destino”, i cui passaggi segnerebbero l'esistenza di ogni essere umano. Alexandra imparerà ad avere il coraggio di seguire i propri sogni, uscire da credenze limitanti, avere fiducia in se stessa. In qualche modo tutti i personaggi troveranno la chiave per cambiare nodo del destino e vivere l'amore incondizionato. Perché il miracolo è sempre in agguato per chi non smette di sognare.

Published
2017

20. Calibrating the Planck Cluster Mass Scale with Cluster Velocity Dispersions

Author

Daniel Stern, Stefania Amodeo, Hyunjin Shim, Jean-Baptiste Melin, Charles R. Lawrence, Francine R. Marleau, Ranga-Ram Chary, James G. Bartlett, Spencer A. Stanford, Simona Mei, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS ), Université Paris Diderot - Paris 7 ( UPD7 ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Planck mass, Cosmic background radiation, FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Electromagnetic radiation, symbols.namesake, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, Galaxy cluster, Physics, 010308 nuclear & particles physics, Velocity dispersion, Astronomy and Astrophysics, Redshift, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, symbols, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We measure the Planck cluster mass bias using dynamical mass measurements based on velocity dispersions of a subsample of 17 Planck-detected clusters. The velocity dispersions were calculated using redshifts determined from spectra obtained at Gemini observatory with the GMOS multi-object spectrograph. We correct our estimates for effects due to finite aperture, Eddington bias and correlated scatter between velocity dispersion and the Planck mass proxy. The result for the mass bias parameter, $(1-b)$, depends on the value of the galaxy velocity bias $b_v$ adopted from simulations: $(1-b)=(0.51\pm0.09) b_v^3$. Using a velocity bias of $b_v=1.08$ from Munari et al., we obtain $(1-b)=0.64\pm 0.11$, i.e, an error of 17% on the mass bias measurement with 17 clusters. This mass bias value is consistent with most previous weak lensing determinations. It lies within $1\sigma$ of the value needed to reconcile the Planck cluster counts with the Planck primary CMB constraints. We emphasize that uncertainty in the velocity bias severely hampers precision measurements of the mass bias using velocity dispersions. On the other hand, when we fix the Planck mass bias using the constraints from Penna-Lima et al., based on weak lensing measurements, we obtain a positive velocity bias $b_v \gtrsim 0.9$ at $3\sigma$., Comment: 13 pages, 1 figure, ApJ, in press

Published
2017

21. On the evolution of the entropy and pressure profiles in X-ray luminous galaxy clusters at z > 0.4

Author

Stefano Ettori, R. Capasso, Stefania Amodeo, Vittorio Ghirardini, Mauro Sereno, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS ), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Ghirardini, V., Ettori, S., Amodeo, S., Capasso, R., and Sereno, M.

Subjects
galaxies: clusters: intracluster medium, 010504 meteorology & atmospheric sciences, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, COSMIC cancer database, X-ray, X-rays: Galaxies: Cluster, Astronomy and Astrophysics, Polytropic process, Astronomy and Astrophysic, Redshift, 13. Climate action, Space and Planetary Science, galaxies: clusters: general, X-rays: galaxies: clusters, Halo, intergalactic medium, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Galaxy clusters are the most recent products of hierarchical accretion over cosmological scales. The gas accreted from the cosmic field is thermalized inside the cluster halo. Gas entropy and pressure are expected to have a self-similar behaviour with their radial distribution following a power law and a generalized Navarro-Frenk-White profile, respectively. This has been shown also in many different hydrodynamical simulations. We derive the spatially-resolved thermodynamical properties of 47 X-ray galaxy clusters observed with Chandra in the redshift range 0.4 < z < 1.2, the largest sample investigated so far in this redshift range with X-rays spectroscopy, with a particular care in reconstructing the gas entropy and pressure radial profiles. We search for deviation from the self-similar behaviour and look for possible evolution with redshift. The entropy and pressure profiles lie very close to the baseline prediction from gravitational structure formation. We show that these profiles deviate from the baseline prediction as function of redshift, in particular at z > 0.75, where, in the central regions, we observe higher values of the entropy (by a factor of 2.2) and systematically lower estimates (by a factor of 2.5) of the pressure. The effective polytropic index, which retains informations about the thermal distribution of the gas, shows a slight linear positive evolution with the redshift and the concentration of the dark matter distribution. A prevalence of non-cool-core, disturbed systems, as we observe at higher redshifts, can explain such behaviours., Comment: 14 pages, 18 figures, accepted for publication by A&A

Published
2017

22. The relation between mass and concentration in X-ray galaxy clusters at high redshift

Author

Stefano Ettori, Mauro Sereno, Stefania Amodeo, R. Capasso, Amodeo, Serafino, Ettori, S., Capasso, Raffaella, and Sereno, Mauro

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology: observation, law.invention, Gravitational potential, law, 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Intergalactic medium, Physics, Mass distribution, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, Accretion (astrophysics), Redshift, Space and Planetary Science, Halo, Galaxies: clusters: general, Hydrostatic equilibrium, X-rays: galaxie, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Galaxy clusters are the most recent, gravitationally-bound products of the hierarchical mass accretion over cosmological scales. How the mass is concentrated is predicted to correlate with the total mass in the cluster's halo, with systems at higher mass being less concentrated at given redshift and for any given mass, systems with lower concentration are found at higher redshifts. Through a spatial and spectral X-ray analysis, we reconstruct the total mass profile of 47 galaxy clusters observed with Chandra in the redshift range $0.40.4$, and is well suited to provide the first constraint on the concentration--mass relation at $z>0.7$ from X-ray analysis. Under the assumptions that the distribution of the X-ray emitting gas is spherically symmetric and in hydrostatic equilibrium, we combine the deprojected gas density and spectral temperature profiles through the hydrostatic equilibrium equation to recover the parameters that describe a NFW total mass distribution. The comparison with results from weak lensing analysis reveals a very good agreement both for masses and concentrations. Uncertainties are however too large to make any robust conclusion on the hydrostatic bias of these systems. The relation is well described by the form $c \propto M^B (1+z)^C$, with $B=-0.50 \pm 0.20$, $C=0.12 \pm 0.61$ (at 68.3\% confidence), it is slightly steeper than the one predicted by numerical simulations ($B\sim-0.1$) and does not show any evident redshift evolution. We obtain the first constraints on the properties of the concentration--mass relation at $z > 0.7$ from X-ray data, showing a reasonable good agreement with recent numerical predictions., Comment: A&A accepted, 18 pages, 13 figures, 1 Appendix

Published
2016

23. Probing Cosmology with Dark Matter Halo Sparsity Using X-ray Cluster Mass Measurements

Author

Dominique Eckert, Pier Stefano Corasaniti, M.-A. Breton, Yann Rasera, Stefano Ettori, Mauro Sereno, V. Ghirardini, Stefania Amodeo, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, methods: numerical, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], cosmology: theory, 0103 physical sciences, Cluster (physics), cosmological parameters, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Halo mass function, Astronomy and Astrophysics, Redshift, Baryon, Dark matter halo, Space and Planetary Science, X-rays: galaxies: clusters, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a new cosmological probe for galaxy clusters, the halo sparsity. This characterises halos in terms of the ratio of halo masses measured at two different radii and carries cosmological information encoded in the halo mass profile. Building upon the work of Balmes et al. (2014) we test the properties of the sparsity using halo catalogs from a numerical N-body simulation of ($2.6$ Gpc/h)$^3$ volume with $4096^3$ particles. We show that at a given redshift the average sparsity can be predicted from prior knowledge of the halo mass function. This provides a quantitative framework to infer cosmological parameter constraints using measurements of the sparsity of galaxy clusters. We show this point by performing a likelihood analysis of synthetic datasets with no systematics, from which we recover the input fiducial cosmology. We also perform a preliminary analysis of potential systematic errors and provide an estimate of the impact of baryonic effects on sparsity measurements. We evaluate the sparsity for a sample of 104 clusters with hydrostatic masses from X-ray observations and derive constraints on the cosmic matter density $\Omega_m$ and the normalisation amplitude of density fluctuations at the $8$ Mpc h$^{-1}$ scale, $\sigma_8$. Assuming no systematics, we find $\Omega_m=0.42\pm 0.17$ and $\sigma_8=0.80\pm 0.31$ at $1\sigma$, corresponding to $S_8\equiv \sigma_8\sqrt{\Omega_m}=0.48\pm 0.11$. Future cluster surveys may provide opportunities for precise measurements of the sparsity. A sample of a few hundreds clusters with mass estimate errors at a few percent level can provide competitive cosmological parameter constraints complementary to those inferred from other cosmic probes., Comment: 20 pages, 15 figures; working example extended to other overdensities, detailed analysis of systematic error from hydrostatic mass bias, overall results unchanged. ApJ accepted version. Halo sparsity code available at https://github.com/pierste75/Halo_Sparsity

24. Spectroscopic Confirmation and Velocity Dispersions for 20 Planck Galaxy Clusters at 0.16 < z < 0.78.

Author

Stefania Amodeo, Simona Mei, Spencer A. Stanford, Charles R. Lawrence, James G. Bartlett, Daniel Stern, Ranga-Ram Chary, Hyunjin Shim, Francine R. Marleau, Jean-Baptiste Melin, and Carmen Rodríguez-Gonzálvez

Subjects
*DISPERSION (Chemistry), *STELLAR mass, *GALAXY clusters, *REDSHIFT, *DISTRIBUTION (Probability theory)
Abstract

We present Gemini and Keck spectroscopic redshifts and velocity dispersions for 20 clusters detected via the Sunyaev–Zel’dovich (SZ) effect by the Planck space mission, with estimated masses in the range . Cluster members were selected for spectroscopic follow-up with Palomar, Gemini, and Keck optical and (in some cases) infrared imaging. Seven cluster redshifts were measured for the first time with this observing campaign, including one of the most distant Planck clusters confirmed to date, at , PSZ2 G085.95+25.23. The spectroscopic redshift catalogs of members of each confirmed cluster are included as online tables. We show the galaxy redshift distributions and measure the cluster velocity dispersions. The cluster velocity dispersions obtained in this paper were used in a companion paper to measure the Planck mass bias and to constrain the cluster velocity bias. [ABSTRACT FROM AUTHOR]

Published
2018
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25. The Atacama Cosmology Telescope: Weighing Distant Clusters with the Most Ancient Light

Author

Nicholas Battaglia, Johannes Hubmayr, Laura Newburgh, Kavilan Moodley, Rolando Dünner, Suzanne T. Staggs, Adriaan J. Duivenvoorden, Amanda MacInnis, Sigurd Naess, Shannon M. Duff, Edward V. Denison, J. Colin Hill, Steve K. Choi, David N. Spergel, Dongwon Han, Kevin M. Huffenberger, J. Richard Bond, Frank J. Qu, Eve M. Vavagiakis, Gene C. Hilton, Jason E. Austermann, Emilie Storer, Benjamin L. Schmitt, Federico Nati, Blake D. Sherwin, Mark J. Devlin, Sara M. Simon, Arthur Kosowsky, Brian J. Koopman, Jeff McMahon, Maria Salatino, Toshiya Namikawa, Zhilei Xu, Matt Hilton, Jeff Van Lanen, Alexander van Engelen, Joel N. Ullom, Neelima Sehgal, Stefania Amodeo, Mathew S. Madhavacheril, Cristóbal Sifón, John P. Hughes, Eunseong Lee, Emmanuel Schaan, Simone Ferraro, Bruce Partridge, Simon Dicker, N. C. Robertson, James A. Beall, Patricio A. Gallardo, Yilun Guan, Alessandro Schillaci, Erminia Calabrese, Lyman A. Page, Jo Dunkley, Daniel T. Becker, Leila R. Vale, Thibaut Louis, Edward J. Wollack, Simone Aiola, Michael D. Niemack, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), ACT, Namikawa, Toshiya [0000-0003-3070-9240], Apollo - University of Cambridge Repository, Madhavacheril, M, Sifon, C, Battaglia, N, Aiola, S, Amodeo, S, Austermann, J, Beall, J, Becker, D, Richard Bond, J, Calabrese, E, Choi, S, Denison, E, Devlin, M, Dicker, S, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Gallardo, P, Guan, Y, Han, D, Colin Hill, J, Hilton, G, Hilton, M, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, van Lanen, J, Lee, E, Louis, T, Macinnis, A, Mcmahon, J, Moodley, K, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Qu, F, Robertson, N, Salatino, M, Schaan, E, Schillaci, A, Schmitt, B, Sehgal, N, Sherwin, B, Simon, S, Spergel, D, Staggs, S, Storer, E, Ullom, J, Vale, L, van Engelen, A, Vavagiakis, E, Wollack, E, and Xu, Z

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, astro-ph.GA, Cosmic microwave background, Population, Gravitational lensing, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, High-redshift galaxy clusters, 01 natural sciences, Cosmology, Cosmic microwave background radiation, 0103 physical sciences, education, 010303 astronomy & astrophysics, Galaxy cluster, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, gravitational lensing, cosmic microwave background, Gravitational lens, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Atacama Cosmology Telescope, astro-ph.CO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use gravitational lensing of the cosmic microwave background (CMB) to measure the mass of the most distant blindly-selected sample of galaxy clusters on which a lensing measurement has been performed to date. In CMB data from the the Atacama Cosmology Telescope (ACT) and the Planck satellite, we detect the stacked lensing effect from 677 near-infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS), which have a mean redshift of $ \langle z \rangle = 1.08$. There are no current optical weak lensing measurements of clusters that match the distance and average mass of this sample. We detect the lensing signal with a significance of $4.2 \sigma$. We model the signal with a halo model framework to find the mean mass of the population from which these clusters are drawn. Assuming that the clusters follow Navarro-Frenk-White density profiles, we infer a mean mass of $\langle M_{500c}\rangle = \left(1.7 \pm 0.4 \right)\times10^{14}\,\mathrm{M}_\odot$. We consider systematic uncertainties from cluster redshift errors, centering errors, and the shape of the NFW profile. These are all smaller than 30% of our reported uncertainty. This work highlights the potential of CMB lensing to enable cosmological constraints from the abundance of distant clusters populating ever larger volumes of the observable Universe, beyond the capabilities of optical weak lensing measurements., Comment: 14 pages, 3 figures, matches version accepted in ApJL, code available at https://github.com/ACTCollaboration/madcows_lensing/

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26. Calibrating the Planck Cluster Mass Scale with Cluster Velocity Dispersions.

Author

Stefania Amodeo, Simona Mei, Spencer A. Stanford, James G. Bartlett, Jean-Baptiste Melin, Charles R. Lawrence, Ranga-Ram Chary, Hyunjin Shim, Francine Marleau, and Daniel Stern

Subjects
*VELOCITY, *STAR clusters, *SPECTROGRAPHS, *REDSHIFT, *SIMULATION methods & models, *COSMIC background radiation
Abstract

We measure the Planck cluster mass bias using dynamical mass measurements based on velocity dispersions of a subsample of 17 Planck-detected clusters. The velocity dispersions were calculated using redshifts determined from spectra that were obtained at the Gemini observatory with the GMOS multi-object spectrograph. We correct our estimates for effects due to finite aperture, Eddington bias, and correlated scatter between velocity dispersion and the Planck mass proxy. The result for the mass bias parameter, , depends on the value of the galaxy velocity bias, , adopted from simulations: . Using a velocity bias of from Munari et al., we obtain , i.e., an error of 17% on the mass bias measurement with 17 clusters. This mass bias value is consistent with most previous weak-lensing determinations. It lies within of the value that is needed to reconcile the Planck cluster counts with the Planck primary cosmic microwave background constraints. We emphasize that uncertainty in the velocity bias severely hampers the precision of the measurements of the mass bias using velocity dispersions. On the other hand, when we fix the Planck mass bias using the constraints from Penna–Lima et al., based on weak-lensing measurements, we obtain a positive velocity bias of at . [ABSTRACT FROM AUTHOR]

Published
2017
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