Descriptor: "Astrophysics - Cosmology and Nongalactic Astrophysics" / Database: OpenAIRE / Publisher: hal ccsd / Topic: 010303 astronomy & astrophysics - Searchworks@Jio Institute Digital Library Search Results

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1,290 results on '"Astrophysics - Cosmology and Nongalactic Astrophysics"'

1. The effects of lensing by local structures on the dipole of radio source counts

Author: Murray, Calum, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), and Université Grenoble Alpes (UGA)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 01 natural sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Our peculiar motion in a homogeneous and isotropic universe imprints a dipole in the cosmic microwave background (CMB) temperature field and similarly imprints a dipole in the distribution of extragalactic radio sources on the sky. Each of these effects have been measured; however, each of these measurements give different results for the velocity of our motion through the Universe: the radio dipole measurements finds the speed of our motion to be around three times larger than that of the CMB. Here we show the effects of the previously unconstrained lensing dipole, whereby necessarily local structures (required for large angular lensing scales) will distort the distribution of radio sources on the sky. We find that the inclusion of these effects does not reduce the tension between the CMB and radio source dipole measurements; however, without their inclusion future extragalactic number counts could lead to incorrect inferences of our peculiar motion. In addition we can constrain the size of the lensing dipole to be κ < 3 · 10−2 at the 2σ level.
Published: 2022

2. The eROSITA Final Equatorial-Depth Survey (eFEDS) - Characterization of morphological properties of galaxy groups and clusters

Author: Vittorio Ghirardini, Y. Emre Bahar, Esra Bulbul, Ang Liu, Nicolas Clerc, Florian Pacaud, Johan Comparat, Teng Liu, Miriam E. Ramos-Ceja, Duy Hoang, Jacob Ider-Chitham, Matthias Klein, Andrea Merloni, Kirpal Nandra, Naomi Ota, Peter Predehl, Thomas H. Reiprich, Jeremy Sanders, Tim Schrabback, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Space and Planetary Science, galaxies: clusters: general, X-rays: galaxies: clusters, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Understanding the cluster population of clusters of galaxies is of the utmost importance for using cluster samples in both astrophysical and cosmological studies. We present an in-depth analysis of the X-ray morphological parameters of the galaxy clusters and groups detected in the eROSITA Final Equatorial-Depth Survey (eFEDS). We study the eROSITA X-ray imaging data for a sample of 325 clusters and groups that are significantly detected in the eFEDS field. We characterize their dynamical properties by measuring a number of dynamical estimators: concentration, central density, cuspiness, ellipticity, power-ratios, photon asymmetry, and Gini coefficient. The galaxy clusters and groups detected in eFEDS, covering a luminosity range of more than three orders of magnitude and large redshift range out to 1.2 provide an ideal sample for studying the redshift and luminosity evolution of the morphological parameters and characterization of the underlying dynamical state of the sample. Based on these measurements we construct a new dynamical indicator, relaxation score, for all the clusters in the sample. We find no evidence for bimodality in the distribution of morphological parameters of our clusters, rather we observe a smooth transition from the cool-core to non-cool-core and from relaxed to disturbed states. A significant evolution in redshift and luminosity is also observed in the morphological parameters examined in this study after carefully taking into account the selection effects. We determine that our eFEDS-selected cluster sample, differently than ROSAT-based cluster samples, is not biased toward relaxed clusters, but contains a similar fraction of disturbed as SZ surveys., 21 pages, 10 figures, 2 tables, Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission
Published: 2022

3. Cosmic shear beyond 2-point statistics: Accounting for galaxy intrinsic alignment with projected tidal fields

Author: Joachim Harnois-Déraps, Robert Reischke, Nicolas Martinet, 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), and 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)
Subjects: Current (mathematics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Omega, Cosmology, dark matter, methods: numerical, gravitational lensing: weak, 0103 physical sciences, Statistics, dark energy, 010303 astronomy & astrophysics, Weak gravitational lensing, media_common, Physics, 010308 nuclear & particles physics, Sigma, Astronomy and Astrophysics, Galaxy, Universe, Space and Planetary Science, Coupling parameter, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Developing analysis pipelines based on statistics beyond two-point functions is critical for extracting a maximal amount of cosmological information from current and upcoming weak lensing surveys. In this paper, we study the impact of the intrinsic alignment of galaxies (IA) on three promising probes measured from aperture mass maps -- the lensing peaks, minima and full PDF, in comparison and in combination with the shear two-point correlation functions ($\gamma$-2PCFs). Our two-dimensional IA infusion method converts the light-cone-projected mass sheets into projected tidal tensors, which are then linearly coupled to an intrinsic ellipticity component with a strength controlled by the coupling parameter $A_{\rm IA}$. We validate our method with the $\gamma$-2PCFs statistics, recovering well the analytical calculations from the linear alignment model of Bridle \& King in a full tomographic setting, and for different $A_{\rm IA}$ values. We next use our method to infuse at the galaxy catalogue level a non-linear IA model that includes the density-weighting term introduced in \citet{Blazek2015}, and compute the impact on the three aperture mass map statistics. We find that large \snr peaks are maximally affected, with deviations reaching 30\% (10\%) for a {\it Euclid}-like (KiDS-like) survey. Modelling the signal in a $w$CDM cosmology universe with $N$-body simulations, we forecast the cosmological bias caused by unmodelled IA for 100 deg$^2$ of {\it Euclid}-like data, finding very large offsets in $w_0$ (5-10$\sigma_{\rm stat}$), $\Omega_{\rm m}$ (4-6$\sigma_{\rm stat}$), and $S_8 \equiv \sigma_8\sqrt{\Omega_{\rm m}/0.3}$ ($\sim$3$\sigma_{\rm stat}$). The method presented in this paper offers a compelling avenue to account for IA in beyond-two-point weak lensing statistics, with a flexibility comparable to that of current $\gamma$-2PCFs IA analytical models., Comment: 21 pages, 12 figures, accepted version
Published: 2022

4. The XXL survey - XLVI. Forward cosmological analysis of the C1 cluster sample

Author: C. Adami, C. Garrel, Marguerite Pierre, Keiichi Umetsu, Lauro Moscardini, Elias Koulouridis, L. Chiappetti, Dominique Eckert, Sunayana Bhargava, Fabio Gastaldello, Jean-Paul Le Fevre, N. Clerc, Alfonso Veropalumbo, Mauro Sereno, Florian Pacaud, Patrick Valageas, Manolis Plionis, Federico Marulli, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and 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)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Population, FOS: Physical sciences, Astrophysics, Correlation function (astronomy), 01 natural sciences, Omega, Cosmology, symbols.namesake, surveys, 0103 physical sciences, Planck, cosmological parameters, education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Space and Planetary Science, X-rays: galaxies: clusters, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the forward cosmological analysis of an $XMM$ selected sample of galaxy clusters out to a redshift of unity. Following our previous 2018 study based on the dn/dz quantity alone, we perform an upgraded cosmological analysis of the same XXL C1 cluster catalogue (178 objects), with a detailed account of the systematic errors. We follow the ASpiX methodology: the distribution of the observed X-ray properties of the cluster population is analysed in a 3D observable space (count rate, hardness ratio, redshift) and modelled as a function of cosmology. Compared to more traditional methods, ASpiX allows the inclusion of clusters down to a few tens of photons. We obtain an improvement by a factor of 2 compared to the previous analysis by letting the normalisation of the M-T relation and the evolution of the L-T relation free. Adding constraints from the XXL cluster 2-point correlation function and the BAO from various surveys decreases the uncertainties by 23 and 53 % respectively, and 62% when adding both. Switching to the scaling relations from the Subaru analysis, and letting free more parameters, our final constraints are $\sigma_8$ = $0.99^{+0.14}_{-0.23}$, $\Omega_m$ = 0.296 $\pm$ 0.034 ($S_8 = 0.98^{+0.11}_{-0.21}$) for the XXL sample alone. Finally, we combine XXL ASpiX, the XXL cluster 2-point correlation function and the BAO, with 11 free parameters, allowing for the cosmological dependence of the scaling relations in the fit. We find $\sigma_8$ = $0.793^{+0.063}_{-0.12}$, $\Omega_m$ = 0.364 $\pm$ 0.015 ($S_8 = 0.872^{+0.068}_{-0.12}$), but still compatible with Planck CMB at 2.2$\sigma$. The results obtained by the ASpiX method are promising; further improvement is expected from the final XXL cosmological analysis involving a cluster sample twice as large. Such a study paves the way for the analysis of the eROSITA and future Athena surveys., Comment: 20 pages, 10 figures, accepted for publication in A&A, A&A version has the unabridged abstract
Published: 2022

5. Deep transfer learning for blended source identification in galaxy survey data

Author: A. Guinot, S. Farrens, A. Lacan, A. Z. Vitorelli, Université Paris-Saclay, Université Paris Cité (UPCité), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Kedge Business School (Kedge BS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), The authors wish to acknowledge the COSMIC project funded by the CEA DRF-Impulsion call in 2016, the CrossDisciplinary Program on Numerical Simulation (SILICOSMIC project in 2018) of CEA, the French Alternative Energies and Atomic Energy Commission., The Euclid Collaboration, the European Space Agency and the support of the Centre National d’Etudes Spatiales., ANR-19-CE23-0024,AstroDeep,Analyse de données astronomiques massives avec de l'apprentissage machine(2019), HEP, INSPIRE, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, techniques: image processing, Astrophysics, 01 natural sciences, Standard deviation, methods: numerical, gravitational lensing: weak, 0103 physical sciences, Code (cryptography), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, computer.programming_language, Physics, Pixel, 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, Pattern recognition, Python (programming language), methods: data analysis, Noise, Identification (information), Space and Planetary Science, [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Parametric model, Artificial intelligence, Transfer of learning, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], computer, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present BlendHunter, a proof-of-concept for a deep transfer learning based approach for the automated and robust identification of blended sources in galaxy survey data. We take the VGG-16 network with pre-trained convolutional layers and train the fully connected layers on parametric models of COSMOS images. We test the efficacy of the transfer learning by taking the weights learned on the parametric models and using them to identify blends in more realistic CFIS-like images. We compare the performance of this method to SEP (a Python implementation of SExtractor) as function of noise level and the separation between sources. We find that BlendHunter outperforms SEP by $\sim 15\%$ in terms of classification accuracy for close blends ($, 9 pages, 6 figures, accepted for publication in A&A
Published: 2022

6. The BINGO project - V. Further steps in component separation and bispectrum analysis

Author: Fornazier, Karin S.F., Abdalla, Filipe B., Remazeilles, Mathieu, Vieira, Jordany, Marins, Alessandro, Abdalla, Elcio, Santos, Larissa, Delabrouille, Jacques, Mericia, Eduardo, Landim, Ricardo G., Ferreira, Elisa G.M., Barosi, Luciano, Brito, Francisco A., Queiroz, Amilcar R., Villela, Thyrso, Wang, Bin, Wuensche, Carlos A., Costa, Andre A., Liccardo, Vincenzo, Novaes, Camila Paiva, Peel, Michael W., dos Santos, Marcelo V., Zhang, Jiajun, 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, telescopes, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Space and Planetary Science, cosmology: observations, 0103 physical sciences, RADIOTELESCÓPIOS, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, radio lines: general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Observing the neutral hydrogen distribution across the Universe via redshifted 21cm line intensity mapping constitutes a powerful probe for cosmology. However, the redshifted 21cm signal is obscured by the foreground emission from our Galaxy and other extragalactic foregrounds. This paper addresses the capabilities of the BINGO survey to separate such signals. Specifically, this paper looks in detail at the different residuals left over by foreground components, shows that a noise-corrected spectrum is unbiased, and shows that we understand the remaining systematic residuals by analyzing nonzero contributions to the three-point function. We use the generalized needlet internal linear combination, which we apply to sky simulations of the BINGO experiment for each redshift bin of the survey. We present our recovery of the redshifted 21cm signal from sky simulations of the BINGO experiment, including foreground components. We test the recovery of the 21cm signal through the angular power spectrum at different redshifts, as well as the recovery of its non-Gaussian distribution through a bispectrum analysis. We find that non-Gaussianities from the original foreground maps can be removed down to, at least, the noise limit of the BINGO survey with such techniques. Our component separation methodology allows us to subtract the foreground contamination in the BINGO channels down to levels below the cosmological signal and the noise, and to reconstruct the 21cm power spectrum for different redshift bins without significant loss at multipoles $20 \lesssim \ell \lesssim 500$. Our bispectrum analysis yields strong tests of the level of the residual foreground contamination in the recovered 21cm signal, thereby allowing us to both optimize and validate our component separation analysis. (Abridged), 20 pages. Version accepted in A&A
Published: 2022

7. Dark matter dilution scenarios in the early universe

Author: Arnab Chaudhuri, Maxim Yu. Khlopov, 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: black hole: decay, Cosmology and Nongalactic Astrophysics (astro-ph.CO), nucleosynthesis: big bang, FOS: Physical sciences, 01 natural sciences, dark matter, High Energy Physics - Phenomenology (hep-ph), cosmological model: parameter space, 0103 physical sciences, electroweak interaction: critical phenomena, 010303 astronomy & astrophysics, Mathematical Physics, plasma, space-time: expansion, 010308 nuclear & particles physics, dark matter: mass, dark matter: relic density, primordial black holes, Elementary particles, Astronomy and Astrophysics, black hole: mass, High Energy Physics - Phenomenology, Space and Planetary Science, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], electroweak phase transition, entropy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], potential: Higgs, black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: When the vacuum like energy of the Higgs potential within the standard model undergoes electroweak phase transition, an influx of entropy into the primordial plasma can lead to a significant dilution of frozen out dark matter density that was already present before the onset of the phase transition. The same effect can take place, if the early Universe was dominated by primordial black holes of small mass, evaporating before the period of Big Bang Nucleosynthesis. In this paper we calculate the dilution factor for the above mentioned scenarios., 12 pages, 2 figures. arXiv admin note: text overlap with arXiv:1711.01801, arXiv:2001.11219
Published: 2021

8. Theoretical and numerical perspectives on cosmic distance averages

Author: Pierre Fleury, Michel-Andrès Breton, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Length scale, large-scale structure of Universe, distance scale, cosmology: theory, methods: numerical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Structure formation, media_common.quotation_subject, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, 01 natural sciences, Cosmology, Distance measures, General Relativity and Quantum Cosmology, methods: numerical, symbols.namesake, Friedmann–Lemaître–Robertson–Walker metric, cosmology: theory, 0103 physical sciences, Statistical physics, 010303 astronomy & astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Universe, Gravitational lens, Space and Planetary Science, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], symbols, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The interpretation of cosmological observations relies on a notion of an average Universe, which is usually considered as the homogeneous and isotropic Friedmann-Lema\^itre-Robertson-Walker (FLRW) model. However, inhomogeneities may statistically bias the observational averages with respect to FLRW, notably for distance measurements, due to a number of effects such as gravitational lensing and redshift perturbations. In this article, we review the main known theoretical results on average distance measures in cosmology, based on second-order perturbation theory, and we fill in some of their gaps. We then comprehensively test these theoretical predictions against ray tracing in a high-resolution dark-matter $N$-body simulation. This method allows us to describe the effect of small-scale inhomogeneities deep into the non-linear regime of structure formation on light propagation up to $z=10$. We find that numerical results are in remarkably good agreement with theoretical predictions in the limit of super-sample variance. No unexpectedly large bias originates from very small scales, whose effect is fully encoded in the non-linear power spectrum. Specifically, the directional average of the inverse amplification and the source-averaged amplification are compatible with unity; the change in area of surfaces of constant cosmic time is compatible with zero; the biases on other distance measures, which can reach slightly less than $1\%$ at high redshift, are well understood. As a side product, we also confront the predictions of the recent finite-beam formalism with numerical data and find excellent agreement., Comment: 21+8 pages, 23 figures. Accepted version
Published: 2021

9. Fossil group origins: XI. The dependence of galaxy orbits on the magnitude gap

Author: S. Zarattini, Marisa Girardi, Elena D'Onghia, Andrea Biviano, J. A. L. Aguerri, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofisica de Canarias (IAC), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), Università degli studi di Trieste, University of Wisconsin-Madison, European Project: 340519,EC:FP7:ERC,ERC-2013-ADG,M2C(2014), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Zarattini, S., Biviano, A., Aguerri, J. A. L., Girardi, M., D'Onghia, E., Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli studi di Trieste = University of Trieste, Harvard University [Cambridge]-Smithsonian Institution, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and HEP, INSPIRE
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Magnitude (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, Inversion (discrete mathematics), galaxies: groups: general, 0103 physical sciences, Order (group theory), 10. No inequality, Anisotropy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Group (mathematics), Isotropy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, groups: general [Galaxies], Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: clusters: general, Galaxies: groups: general, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We aim to study how the orbits of galaxies in clusters depend on the prominence of the corresponding central galaxies. We divided our data set of $\sim$ 100 clusters and groups into four samples based on their magnitude gap between the two brightest members, $\Delta m_{12}$. We then stacked all the systems in each sample, in order to create four stacked clusters, and derive the mass and velocity anisotropy profiles for the four groups of clusters using the MAMPOSSt procedure. Once the mass profile is known, we also obtain the (non parametric) velocity anisotropy profile via the inversion of the Jeans equation. In systems with the largest $\Delta m_{12}$, galaxy orbits are prevalently radial, except near the centre, where orbits are isotropic (or tangential when also the central galaxies are considered in the analysis). In the other three samples with smaller $\Delta m_{12}$, galaxy orbits are isotropic or only mildly radial. Our study supports the results of numerical simulations that identify radial orbits of galaxies as the cause of an increasing $\Delta m_{12}$ in groups., Comment: 12 pages, 5 figures, and 6 tables. Accepted for publication in Astronomy and Astrophysics
Published: 2021

10. On the relative effect of nodes and filaments of the cosmic web on the quenching of galaxies and the orientation of their spin

Author: Daniela Galárraga-Espinosa, Mathieu Langer, Nabila Aghanim, C. Gouin, Nicola Malavasi, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Quenching, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Orientation (graph theory), 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Cosmic web, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Spin-½, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Filaments and clusters of the cosmic web have an impact on the properties of galaxies, switching off their star-formation, contributing to the build-up of their stellar mass, and influencing the acquisition of their angular momentum. In this work we make use of the IllustrisTNG simulation, coupled with the DisPerSE cosmic web extraction algorithm, to test which is the galaxy property most affected by the cosmic web and, conversely, to assess the differential impact of the various cosmic web features on a given galaxy property. Our aim is to use this information to better understand galaxy evolution and to identify on which galaxy property future efforts should focus to detect the cosmic web from the galaxy distribution. We provide a comprehensive analysis of the relation between galaxy properties and cosmic web features. We also perform extensive tests in which we try to disentangle the effect of local overdensities of galaxies on their properties from the effect of the large scale structure environment. Our results show that star-formation is the quantity that shows the strongest variation with the distances from the cosmic web features, but it is also the one that shows the strongest relation to the local environment of galaxies. On the other hand, the direction of the angular momentum of galaxies is the property that shows the weakest trends with distance from cosmic web features, while also being more independent from the local environment of galaxies. We conclude that the direction of the angular momentum of galaxies and its use to improve our detection of the cosmic web features could be the focus of futures studies benefiting from larger statistical samples., Updated version to match the one accepted for publication in A&A
Published: 2021

11. Fitting spectral energy distributions of FMOS-COSMOS emission-line galaxies at z$\sim$1.6: Star formation rates, dust attenuation, and [OIII]$\lambda$5007 emission-line luminosities

Author: V. Buat, Médéric Boquien, Patrice Theulé, J. A. Villa-Vélez, Denis Burgarella, 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), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Centro de Astronomia [Antofagasta] (CITEVA), Universidad de Antofagasta, and 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)
Subjects: 010504 meteorology & atmospheric sciences, catalogs -galaxies, Metallicity, Extinction (astronomy), Continuum (design consultancy), Astrophysics, 01 natural sciences, 0103 physical sciences, Emission spectrum, dust -extinction, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation), Luminous infrared galaxy, Physics, high-redshift -galaxies, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, galaxies -ISM, 13. Climate action, Space and Planetary Science, ISM -infrared, Spectral energy distribution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform SED fitting analysis on a COSMOS sample covering UV-to-FIR wavelengths with emission lines from the FMOS survey. The sample of 182 objects with H$\alpha$ and [OIII]$\lambda5007$ emission spans over a range of $1.40, Comment: Accepted for publication in A&A, 17 pages, 19 figures
Published: 2021

12. A geometric distance to the supermassive black Hole of NGC 3783

Author: N. M. Förster Schreiber, M. L. Bolzer, Pierre-Olivier Petrucci, E. Sturm, Jason Dexter, Thibaut Paumard, Florentin Millour, Christopher A. Onken, Christian Straubmeier, Sebastian F. Hönig, Daniel Rouan, Makoto Kishimoto, Reinhard Genzel, Yann Clénet, P. T. de Zeeuw, Julien Woillez, Ric Davies, D. Kaltenbrunner, António Amorim, A. Drescher, Jinyi Shangguan, S. von Fellenberg, D. Gratadour, Misty C. Bentz, Linda J. Tacconi, J. Stadler, Karine Perraut, Felix Widmann, P. Vermot, Amiel Sternberg, Thomas Ott, Paulo J. V. Garcia, Rachel Street, Wolfgang Brandner, Odele Straub, Dieter Lutz, Hagai Netzer, Mercedes Prieto, Taro Shimizu, Stefan Gillessen, Konrad R. W. Tristram, Oliver Pfuhl, M. Bauböck, Frank Eisenhauer, Andreas Eckart, Guy Perrin, Sylvestre Lacour, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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 Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and GRAVITY
Subjects: Length scale, Gravity (chemistry), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Galaxies: Seyfert, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Angular diameter, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxies: nuclei, Physics, Supermassive black hole, Distance scale, Quasars: individual: NGC 3783, Astronomy and Astrophysics, Galaxies: active, Light curve, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), symbols, Reverberation mapping, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The angular size of the broad line region (BLR) of the nearby active galactic nucleus (AGN) NGC 3783 has been spatially resolved by recent observations with VLTI/GRAVITY. A reverberation mapping (RM) campaign has also recently obtained high quality light curves and measured the linear size of the BLR in a way that is complementary to the GRAVITY measurement. The size and kinematics of the BLR can be better constrained by a joint analysis that combines both GRAVITY and RM data. This, in turn, allows us to obtain the mass of the supermassive black hole in NGC3783 with an accuracy that is about a factor of two better than that inferred from GRAVITY data alone. We derive $M_\mathrm{BH}=2.54_{-0.72}^{+0.90}\times 10^7\,M_\odot$. Finally, and perhaps most notably, we are able to measure a geometric distance to NGC 3783 of $39.9^{+14.5}_{-11.9}$ Mpc. We are able to test the robustness of the BLR-based geometric distance with measurements based on the Tully-Fisher relation and other indirect methods. We find the geometric distance is consistent with other methods within their scatter. We explore the potential of BLR-based geometric distances to directly constrain the Hubble constant, $H_0$, and identify differential phase uncertainties as the current dominant limitation to the $H_0$ measurement precision for individual sources., 9 pages and 5 figures in main text, Accepted for publication in A&A
Published: 2021

13. The MUSE Extremely Deep Field: Evidence for SFR-induced cores in dark-matter dominated galaxies at z=1

Author: Bouché, Nicolas, Bera, Samuel, Krajnovic, Davor, Emsellem, Eric, Mercier, Wilfried, Schaye, Joop, Épinat, Benoît, Richard, Johan, Zoutendijk, Sebastiaan L., Abril-Melgarejo, Valentina, Brichman, Jarle, Bacon, Roland, Contini, Thierry, Boogaard, Leindert, Wisotzki, Lutz, Maseda, Michael, Steinmetz, Matthias, Zoutendijk, Sebastiaan, Brinchmann, Jarle, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Leibniz Institute for Astrophysics Potsdam (AIP), European Southern Observatory (ESO), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, 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), Universidade do Porto = University of Porto, Max Planck Institute for Astronomy (MPIA), ANR-17-CE31-0017,3DGASFLOWS,Comprendre le rôle des écoulements de gaz autour des galaxies grâce à une confrontation entre observations 3D et simulations numériques(2017), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Leiden University, and Sciences, EDP
Subjects: Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Hubble Deep Field, Star (game theory), Dark matter, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, 01 natural sciences, rotation, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], dark matter: halo, star, Methods: data analysis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, formation, Galaxies: high-redshift, Galaxies: kinematics and dynamics, Galaxies: evolution, Astronomy and Astrophysics, Navarro-Frenk-White profile, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, surface: density, Astrophysics of Galaxies (astro-ph.GA), stacking, MUSE, Content (measure theory), spectral, Halo, galaxy, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Disc-halo decomposition on rotationally supported star-forming galaxies (SFGs) at $z>1$ are often limited to massive galaxies ($M_\star>10^{10}~M_\odot$) and rely on either deep Integral Field Spectroscopy data or stacking analyses. We present a study of the dark matter (DM) content of nine $z\approx1$ SFGs selected Using the brightest [OII] emitters in the deepest Multi-Unit Spectrograph Explorer (MUSE) field to date, namely the 140hr MUSE Extremely Deep Field, we perform disk-halo decompositions on 9 low-mass SFGs (with $10^{8.5}10^{10}~M_\odot$. The DM halos show constant surface densities of $\sim100~M_\odot$ pc$^{-2}$. Half of the sample shows a strong preference for cored over cuspy DM profiles. The presence of DM cores appears to be related to galaxies with stellar-to-halo mass $\log M_\star/M_{\rm vir}\approx-2.5$. In addition, the cuspiness of the DM profiles is found to be a strong function of the recent star-formation activity. Both of these results are interpreted as evidence for feedback-induced core formation in the Cold Dark Matter context., Comment: 19 pages, 11 figures, accepted for publication in MNRAS
Published: 2021

14. Impact of survey geometry and super-sample covariance on future photometric galaxy surveys

Author: Beauchamps, S. Gouyou, Lacasa, F., Tutusaus, I., Aubert, M., Baratta, P., Gorce, A., Sakr, Z., Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Centre National D'Etudes Spatiales (France), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Canadian Institute for Advanced Research, Agence Nationale de la Recherche (France), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Space and Planetary Science, 0201 Astronomical and Space Sciences, 0103 physical sciences, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Photometric galaxy surveys probe the late-time Universe where the density field is highly non-Gaussian. A consequence is the emergence of the super-sample covariance (SSC), a non-Gaussian covariance term that is sensitive to fluctuations on scales larger than the survey window. In this work, we study the impact of the survey geometry on the SSC and, subsequently, on cosmological parameter inference. We devise a fast SSC approximation that accounts for the survey geometry and compare its performance to the common approximation of rescaling the results by the fraction of the sky covered by the survey, fSKY, dubbed ‘full-sky approximation’. To gauge the impact of our new SSC recipe, that we call ‘partial-sky’, we perform Fisher forecasts on the parameters of the (w0, wa)-CDM model in a 3 × 2 point analysis, varying the survey area, the geometry of the mask, and the galaxy distribution inside our redshift bins. The differences in the marginalised forecast errors –with the full-sky approximation performing poorly for small survey areas but excellently for stage-IV-like areas– are found to be absorbed by the marginalisation on galaxy bias nuisance parameters. For large survey areas, the unmarginalised errors are underestimated by about 10% for all probes considered. This is a hint that, even for stage-IV-like surveys, the partial-sky method introduced in this work will be necessary if tight priors are applied on these nuisance parameters. We make the partial-sky method public with a new release of the public code PySSC., S. G. B., F. L., I. T., M. A., P. B. and A. G. thank the organisers of the Euclid France 2019 summer school (https://ecole-euclid.cnrs.fr), where this project was initiated. F.L. was partially supported by a postdoctoral grant from Centre National d’Études Spatiales (CNES). I. T. acknowledges support from the Spanish Ministry of Science, Innovation and Universities through grant ESP2017-89838, and the H2020 programme of the European Commission through grant 776247. A. G. acknowledges financial support from the European Research Council under ERC grant number StG-638743 (“FIRSTDAWN”) and from the Trottier Chair in Astrophysics, through the McGill Astrophysics Fellowship, as well as from the Canadian Institute for Advanced Research (CIFAR) Azrieli Global Scholars program and the Canada 150 Programme. This work also acknowledges support from the OCEVU LABEX (Grant No. ANR-11-LABX-0060) and the A*MIDEX project (Grant No. ANR-11-IDEX-0001-02) funded by the Investissements d’Avenir french government program managed by the ANR. This research made use of astropy, a community-developed core Python package for astronomy (Astropy Collaboration 2013, 2018); of matplotlib, a Python library for publication quality graphics (Hunter 2007); of scipy, a Python-based ecosystem of open-source software for mathematics, science, and engineering (Jones et al. 2001) – including numpy (Oliphant 2006); of class, a Boltzmann solver code for cosmology (Blas et al. 2011) and of the Healpix package (Górski et al. 2005).
Published: 2021

15. Detectability of the gravitational redshift effect from the asymmetric galaxy clustering

Author: Shohei Saga, Atsushi Taruya, Yann Rasera, Michel-Andrès Breton, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), Laboratoire d'Astrophysique de Marseille (LAM), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and 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)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Space and Planetary Science, gravitation, cosmology: theory, 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: It has been recently recognized that the observational relativistic effects, mainly arising from the light propagation in an inhomogeneous universe, induce the dipole asymmetry in the cross-correlation function of galaxies. In particular, the dipole asymmetry at small scales is shown to be dominated by the gravitational redshift effects. In this paper, we exploit a simple analytical description for the dipole asymmetry in the cross-correlation function valid at quasi-linear regime. In contrast to the previous model, a new prescription involves only one dimensional integrals, providing a faster way to reproduce the results obtained by Saga et al. (2020). Using the analytical model, we discuss the detectability of the dipole signal induced by the gravitational redshift effect from upcoming galaxy surveys. The gravitational redshift effect at small scales enhances the signal-to-noise ratio (S/N) of the dipole, and in most of the cases considered, the S/N is found to reach a maximum at $z\approx0.5$. We show that current and future surveys such as DESI and SKA provide an idealistic data set, giving a large S/N of $10\sim 20$. Two potential systematics arising from off-centered galaxies are also discussed (transverse Doppler effect and diminution of the gravitational redshift effect), and their impacts are found to be mitigated by a partial cancellation between two competitive effects. Thus, the detection of the dipole signal at small scales is directly linked to the gravitational redshift effect, and should provide an alternative route to test gravity., Comment: 24 pages, 15 figures
Published: 2021

16. The BIG X-ray tail

Author: Rongxin Luo, P. Jáchym, Ming Sun, Alessandro Boselli, William R. Forman, Christine Jones, Masafumi Yagi, Irina Zhuravleva, Matteo Fossati, Eugene Churazov, Chong Ge, Li Ji, University of Alabama in Huntsville (UAH), Ge, C, Sun, M, Yagi, M, Fossati, M, Forman, W, Jachym, P, Churazov, E, Zhuravleva, I, Boselli, A, Jones, C, Ji, L, and Luo, R
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, galaxies: clusters: individual: Abell 1367, Metallicity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, galaxies: groups: general, Intracluster medium, 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, X-rays: galaxies: cluster, Galaxy, Accretion (astrophysics), Interstellar medium, Compact group, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Galaxy clusters grow primarily through the continuous accretion of group-scale haloes. Group galaxies experience preprocessing during their journey into clusters. A star-bursting compact group, the Blue Infalling Group (BIG), is plunging into the nearby cluster A1367. Previous optical observations reveal rich tidal features in the BIG members, and a long H$\alpha$ trail behind. Here we report the discovery of a projected $\sim 250$ kpc X-ray tail behind the BIG using Chandra and XMM-Newton observations. The total hot gas mass in the tail is $\sim 7\times 10^{10}\ {\rm M}_\odot$ with an X-ray bolometric luminosity of $\sim 3.8\times 10^{41}$ erg s$^{-1}$. The temperature along the tail is $\sim 1$ keV, but the apparent metallicity is very low, an indication of the multi-$T$ nature of the gas. The X-ray and H$\alpha$ surface brightnesses in the front part of the BIG tail follow the tight correlation established from a sample of stripped tails in nearby clusters, which suggests the multiphase gas originates from the mixing of the stripped interstellar medium (ISM) with the hot intracluster medium (ICM). Because thermal conduction and hydrodynamic instabilities are significantly suppressed, the stripped ISM can be long lived and produce ICM clumps. The BIG provides us a rare laboratory to study galaxy transformation and preprocessing., Comment: 5 pages, 2 figures, MNRAS Letter accepted
Published: 2021

17. The viewing angle in AGN SED models, a data-driven analysis

Author: Andrés F Ramos Padilla, Lingyu Wang, Katarzyna Małek, Andreas Efstathiou, Guang Yang (杨光), 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), and Astronomy
Subjects: methods: statistical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, methods: data analysis, 01 natural sciences, galaxies: Seyfert, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, astronomical data bases: miscellaneous, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, 010303 astronomy & astrophysics, Techniques: photometric, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The validity of the unified active galactic nuclei (AGN) model has been challenged in the last decade, especially when different types of AGNs are considered to only differ in the viewing angle to the torus. We aim to assess the importance of the viewing angle in classifying different types of Seyfert galaxies in spectral energy distribution (SED) modelling. We retrieve photometric data from publicly available astronomical databases: CDS and NED, to model SEDs with X-CIGALE in a sample of 13 173 Seyfert galaxies located at redshift range from $z=0$ to $z=3.5$, with a median redshift of $z\approx0.2$. We assess whether the estimated viewing angle from the SED models reflects different Seyfert classifications. Two AGN models with either a smooth or clumpy torus structure are adopted in this paper. We find that the viewing angle in Type-1 AGNs is better constrained than in Type-2 AGNs. Limiting the viewing angles representing these two types of AGNs do not affect the physical parameter estimates such as star-formation rate (SFR) or AGN fractional contribution ($f_{\rm{AGN}}$). In addition, the viewing angle is not the most discriminating physical parameter to differentiate Seyfert types. We suggest that the observed and intrinsic AGN disc luminosity can: i) be used in $z, 19 pages, 10 figures, 6 tables (plus appendix). Accepted for publication in MNRAS
Published: 2021

18. Baryogenesis from ultra-slow-roll inflation

Author: Yi-Peng Wu, Elena Pinetti, Kalliopi Petraki, Joseph Silk, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, and Sorbonne Université (SU)
Subjects: High Energy Physics - Theory, Nuclear and High Energy Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Affleck-Dine model, FOS: Physical sciences, QC770-798, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, power spectrum, baryogenesis, 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), Nuclear and particle physics. Atomic energy. Radioactivity, 0103 physical sciences, lepton number, inflation, 010303 astronomy & astrophysics, 010308 nuclear & particles physics, background, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], effective potential, condensation: scalar, formation, Effective Field Theories, deceleration, trigger, Cosmology of Theories beyond the SM, boundary condition, inflaton, coherence, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], baryon: asymmetry, cosmic coincidence, curvature: perturbation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The ultra-slow-roll (USR) inflation represents a class of single-field models with sharp deceleration of the rolling dynamics on small scales, leading to a significantly enhanced power spectrum of the curvature perturbations and primordial black hole (PBH) formation. Such a sharp transition of the inflationary background can trigger the coherent motion of scalar condensates with effective potentials governed by the rolling rate of the inflaton field. We show that a scalar condensate carrying (a combination of) baryon or lepton number can achieve successful baryogenesis through the Affleck-Dine mechanism from unconventional initial conditions excited by the USR transition. Viable parameter space for creating the correct baryon asymmetry of the Universe naturally incorporates the specific limit for PBHs to contribute significantly to dark matter, shedding light on the cosmic coincidence problem between the baryon and dark matter densities today., Comment: 32 + 2 pages, 9 figures, addressed the correlation length of local baryon asymmetry, version matched with publication; v3, added a missing grant information
Published: 2021

19. X-ray analysis of the Planck-detected triplet-cluster system PLCK G334.8-38

Author: Edouard Lecoq, Etienne Pointecouteau, Marian Douspis, Nabila Aghanim, Alexander Kolodzig, 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Joint analysis, Equilateral triangle, 01 natural sciences, symbols.namesake, galaxies: groups: general, 0103 physical sciences, Cluster (physics), Planck, X ray analysis, Spectroscopy, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Projection (relational algebra), Space and Planetary Science, galaxies: clusters: general, X-rays: galaxies: clusters, symbols, large-scale structure of Universe, Astrophysics - High Energy Astrophysical Phenomena, X-rays: diffuse background, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We conducted an X-ray analysis of one of the two Planck-detected triplet-cluster systems, PLCK G334.8-38.0, with a $\sim100$~ks deep XMM-Newton data. We find that the system has a redshift of $z=0.37\pm{0.01}$ but the precision of the X-ray spectroscopy for two members is too low to rule out a projected triplet system, demanding optical spectroscopy for further investigation. In projection, the system looks almost like an equilateral triangle with an edge length of $\sim2.0\,\mathrm{Mpc}$, but masses are very unevenly distributed ($M_{500} \sim [2.5,0.7,0.3] \times 10^{14}\,\mathrm{M_{\odot}}$ from bright to faint). The brightest member appears to be a relaxed cool-core cluster and is more than twice as massive as both other members combined. The second brightest member appears to be a disturbed non-cool-core cluster and the third member was too faint to make any classification. None of the clusters have an overlapping $R_{500}$ region and no signs of cluster interaction were found; however, the XMM-Newton data alone are probably not sensitive enough to detect such signs, and a joint analysis of X-ray and the thermal Sunyaev-Zeldovich effect (tSZ) is needed for further investigation, which may also reveal the presence of the warm-hot intergalactic medium (WHIM) within the system. The comparison with the other Planck-detected triplet-cluster-system (PLCK G214.6+36.9) shows that they have rather different configurations, suggesting rather different merger scenarios, under the assumption that they are both not simply projected triplet systems., Comment: Accepted for publication by A&A. Comments welcome! (22 pages, 13 figures)
Published: 2021

20. Using the sample variance of 21 cm maps as a tracer of the ionisation topology

Author: Jonathan R. Pritchard, A. Hutter, Adélie Gorce, Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), and Astronomy
Subjects: Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), first stars, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radio telescope, 0103 physical sciences, Sample variance, dark ages, 010303 astronomy & astrophysics, Reionization, Physics, methods: statistical, 010308 nuclear & particles physics, Intensity mapping, Astrophysics::Instrumentation and Methods for Astrophysics, Estimator, Astronomy and Astrophysics, Galaxy, Space and Planetary Science, reionization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Intensity mapping of the 21cm signal of neutral hydrogen will yield exciting insights into the Epoch of Reionisation and the nature of the first galaxies. However, the large amount of data that will be generated by the next generation of radio telescopes, such as the Square Kilometre Array (SKA), as well as the numerous observational obstacles to overcome, require analysis techniques tuned to extract the reionisation history and morphology. In this context, we introduce a one-point statistic, to which we refer as the local variance, $\sigma_\mathrm{loc}$, that describes the distribution of the mean differential 21cm brightness temperatures measured in two-dimensional maps along the frequency direction of a light-cone. The local variance takes advantage of what is usually considered an observational bias, the sample variance. We find the redshift-evolution of the local variance to not only probe the reionisation history of the observed patches of the sky, but also trace the ionisation morphology. This estimator provides a promising tool to constrain the midpoint of reionisation as well as gaining insight into the ionising properties of early galaxies., Comment: 14 pages, 14 figures, published in A&A
Published: 2021

21. Euclid Preparation. XIV. The Complete Calibration of the Color–Redshift Relation (C3R2) Survey: Data Release 3

Author: P. Tallada Crespí, Alina Kiessling, L. Stanco, Y. Copin, E. Zucca, Edwin A. Valentijn, L. Moscardini, C. A. J. Duncan, F. Torradeflot, G. Sirri, Bahram Mobasher, F. J. Castander, Harry I. Teplitz, F. Pasian, H. Degaudenzi, Marian Douspis, Santiago Serrano, E. Munari, Henk Hoekstra, Stefano Cavuoti, C. Sirignano, Jean Coupon, G. Mainetti, Massimo Brescia, S. Bardelli, Ariel G. Sánchez, Stefano Camera, Matteo Viel, Pablo Fosalba, V. Scottez, A. Balaguera-Antolínez, D. Di Ferdinando, G. Polenta, R. B. Metcalf, J. Nightingale, Andrea Zacchei, G. A. Verdoes Kleijn, Jason Rhodes, V. Capobianco, Enrico Bozzo, Gianluca Castignani, Florent Sureau, Natalia Auricchio, L. Patrizii, Ivan Lloro, L. Whittaker, Doug Potter, C. S. Carvalho, B. Kubik, S. Casas, M. Fabricius, R. Cledassou, Andrea Biviano, J. Valiviita, Nabila Aghanim, E. Borsato, Peter Schneider, K. Pedersen, M. Frailis, Carlo Baccigalupi, Lucia Pozzetti, I. Davidzon, Sandrine Pires, Andrea Cimatti, Domenico Sapone, Eugenio Maiorano, Massimo Meneghetti, C. C. Kirkpatrick, S. de la Torre, J. Carretero, S. Dusini, Roberto Scaramella, M. Farina, R. Nakajima, G. Congedo, Ralf Bender, Pedro G. Ferreira, David B. Sanders, B. Morin, Ole Marggraf, Peter Capak, Martin Kunz, P. Flose-Reimberg, Luca Conversi, Giuseppe Riccio, A. Balestra, Stéphane Paltani, M. Tenti, W. Gillard, Luca Valenziano, M. Schultheis, Carlo Giocoli, Martin Kilbinger, Carlo Burigana, P. B. Lilje, P. Hudelot, Ken Ganga, Marco Baldi, A. Da Silva, P. Franzetti, D. Masters, S. Kermiche, N. Hernitschek, F. Raison, Anne Costille, S. A. Stanford, C. Bodendorf, Leonardo Corcione, Daniel Stern, Frank Grupp, Romain Teyssier, Stefano Andreon, Herve Aussel, Mischa Schirmer, Cristobal Padilla, Adam Amara, E. Romelli, Ghassem Gozaliasl, Yu Wang, Marco Castellano, Enzo Branchini, N. Martinet, Mark Cropper, M. Poncet, Sami-Matias Niemi, G. Seidel, Ismael Tereno, F. Dubath, Hélène M. Courtois, C. J. Conselice, Katarina Markovic, Davide Maino, Felix Hormuth, A. Cappi, S. Maurogordato, D. Bonino, Roberto P. Saglia, Simona Mei, V. Lindholm, E. Keihänen, Richard Massey, Knud Jahnke, Georges Meylan, Mauro Roncarelli, S. Farrens, Sotiria Fotopoulou, A. N. Taylor, Matteo Maturi, W. Holmes, A. Renzi, Federico Marulli, M. Fumana, Ricard Casas, C. Colodro-Conde, Bianca Garilli, Michele Moresco, Jarle Brinchmann, G. Zamorani, M. Kümmel, R. Kohley, Sebastiano Ligori, E. Franceschi, Rafael Toledo-Moreo, Achille A. Nucita, X. Dupac, Stein Vidar Hagfors Haugan, L. Popa, Javier Graciá-Carpio, C. Neissner, Remi A. Cabanac, Hannu Kurki-Suonio, S. Galeotta, Jean-Gabriel Cuby, Thomas D. Kitching, Behnam Darvish, Emanuel Rossetti, Julien Zoubian, T. Vassallo, A. Secroun, E. Medinaceli, J. G. Cohen, Valeria Pettorino, Carmelita Carbone, René J. Laureijs, Fabio Finelli, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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 Cité (UPCité), 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), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Stanford, S. A., Masters, D., Darvish, B., Stern, D., Cohen, J. G., Capak, P., Hernitschek, N., Davidzon, I., Rhodes, J., Sanders, D. B., Mobasher, B., Castander, F. J., Paltani, S., Aghanim, N., Amara, A., Auricchio, N., Balestra, A., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Casas, R., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Conselice, C. J., Corcione, L., Costille, A., Cropper, M., Degaudenzi, H., Douspis, M., Dubath, F., Dusini, S., Fosalba, P., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Garilli, B., Giocoli, C., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kiessling, A., Kilbinger, M., Kitching, T., Kubik, B., Kummel, M., Kunz, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Marggraf, O., Markovic, K., Massey, R., Meneghetti, M., Meylan, G., Moscardini, L., Niemi, S. M., Padilla, C., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Roncarelli, M., Rossetti, E., Saglia, R., Scaramella, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Taylor, A. N., Teplitz, H. I., Tereno, I., Toledo-Moreo, R., Valentijn, E. A., Valenziano, L., Verdoes Kleijn, G. A., Wang, Y., Zamorani, G., Zoubian, J., Brescia, M., Congedo, G., Conversi, L., Copin, Y., Kermiche, S., Kohley, R., Medinaceli, E., Mei, S., Moresco, M., Morin, B., Munari, E., Polenta, G., Sureau, F., Tallada Crespi, P., Vassallo, T., Zacchei, A., Andreon, S., Aussel, H., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Bardelli, S., Biviano, A., Borsato, E., Bozzo, E., Burigana, C., Cabanac, R., Camera, S., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J. -G., Da Silva, A., De La Torre, S., Di Ferdinando, D., Duncan, C. A. J., Dupac, X., Fabricius, M., Farina, M., Farrens, S., Ferreira, P. G., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Gillard, W., Gozaliasl, G., Gracia-Carpio, J., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Martinet, N., Marulli, F., Maturi, M., Maurogordato, S., Metcalf, R. B., Nakajima, R., Neissner, C., Nightingale, J. W., Nucita, A. A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., Romelli, E., Sanchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Stanco, L., Tenti, M., Teyssier, R., Torradeflot, F., Valiviita, J., Viel, M., Whittaker, L., Zucca, E., Astronomy, Stanford S.A., Masters D., Darvish B., Stern D., Cohen J.G., Capak P., Hernitschek N., Davidzon I., Rhodes J., Sanders D.B., Mobasher B., Castander F.J., Paltani S., Aghanim N., Amara A., Auricchio N., Balestra A., Bender R., Bodendorf C., Bonino D., Branchini E., Brinchmann J., Capobianco V., Carbone C., Carretero J., Casas R., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Conselice C.J., Corcione L., Costille A., Cropper M., Degaudenzi H., Douspis M., Dubath F., Dusini S., Fosalba P., Frailis M., Franceschi E., Franzetti P., Fumana M., Garilli B., Giocoli C., Grupp F., Haugan S.V.H., Hoekstra H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kiessling A., Kilbinger M., Kitching T., Kubik B., Kummel M., Kunz M., Kurki-Suonio H., Laureijs R., Ligori S., Lilje P.B., Lloro I., Maiorano E., Marggraf O., Markovic K., Massey R., Meneghetti M., Meylan G., Moscardini L., Niemi S.M., Padilla C., Pasian F., Pedersen K., Pettorino V., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Roncarelli M., Rossetti E., Saglia R., Scaramella R., Schneider P., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Taylor A.N., Teplitz H.I., Tereno I., Toledo-Moreo R., Valentijn E.A., Valenziano L., Verdoes Kleijn G.A., Wang Y., Zamorani G., Zoubian J., Brescia M., Congedo G., Conversi L., Copin Y., Kermiche S., Kohley R., Medinaceli E., Mei S., Moresco M., Morin B., Munari E., Polenta G., Sureau F., Tallada Crespi P., Vassallo T., Zacchei A., Andreon S., Aussel H., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Bardelli S., Biviano A., Borsato E., Bozzo E., Burigana C., Cabanac R., Camera S., Cappi A., Carvalho C.S., Casas S., Castignani G., Colodro-Conde C., Coupon J., Courtois H.M., Cuby J.-G., Da Silva A., De La Torre S., Di Ferdinando D., Duncan C.A.J., Dupac X., Fabricius M., Farina M., Farrens S., Ferreira P.G., Finelli F., Flose-Reimberg P., Fotopoulou S., Galeotta S., Ganga K., Gillard W., Gozaliasl G., Gracia-Carpio J., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Martinet N., Marulli F., Maturi M., Maurogordato S., Metcalf R.B., Nakajima R., Neissner C., Nightingale J.W., Nucita A.A., Patrizii L., Potter D., Renzi A., Riccio G., Romelli E., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Stanco L., Tenti M., Teyssier R., Torradeflot F., Valiviita J., Viel M., Whittaker L., and Zucca E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Calibration (statistics), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Color space, 01 natural sciences, Cosmology, Large-scale structure, 010309 optics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxy, spectroscopy, Settore FIS/05 - Astronomia e Astrofisica, Spitzer Space Telescope, 0103 physical sciences, DISTRIBUTIONS, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, Hardware_MEMORYSTRUCTURES, Astrophysics::Instrumentation and Methods for Astrophysics, Euclid, Astronomy and Astrophysics, Redshift, Galaxy, Space and Planetary Science, Galaxy spectroscopy, Dark energy, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Stanford, S. A., et al., The Complete Calibration of the Color–Redshift Relation (C3R2) survey is obtaining spectroscopic redshifts in order to map the relation between galaxy color and redshift to a depth of i ∼ 24.5 (AB). The primary goal is to enable sufficiently accurate photometric redshifts for Stage iv dark energy projects, particularly Euclid and the Nancy Grace Roman Space Telescope (Roman), which are designed to constrain cosmological parameters through weak lensing. We present 676 new high-confidence spectroscopic redshifts obtained by the C3R2 survey in the 2017B–2019B semesters using the DEIMOS, LRIS, and MOSFIRE multiobject spectrographs on the Keck telescopes. Combined with the 4454 redshifts previously published by this project, the C3R2 survey has now obtained and published 5130 high-quality galaxy spectra and redshifts. If we restrict consideration to only the 0.2 < zp < 2.6 range of interest for the Euclid cosmological goals, then with the current data release, C3R2 has increased the spectroscopic redshift coverage of the Euclid color space from 51% (as reported by Masters et al.) to the current 91%. Once completed and combined with extensive data collected by other spectroscopic surveys, C3R2 should provide the spectroscopic calibration set needed to enable photometric redshifts to meet the cosmology requirements for Euclid, and make significant headway toward solving the problem for Roman.
Published: 2021

22. Lifting weak lensing degeneracies with a field-based likelihood

Author: Guilhem Lavaux, Natalia Porqueres, Alan Heavens, Daniel J. Mortlock, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Science and Technology Facilities Council (STFC)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), Primordial fluctuations, COSMIC SHEAR, POWER SPECTRUM, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 2-POINT, 01 natural sciences, Omega, gravitational lensing: weak, 0103 physical sciences, 0201 Astronomical and Space Sciences, DARK-MATTER, Statistical physics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Weak gravitational lensing, KIDS-450 COSMOLOGICAL CONSTRAINTS, Physics, COUNTS, Science & Technology, 010308 nuclear & particles physics, Matter power spectrum, Spectral density, Astronomy and Astrophysics, methods: data analysis, PEAK STATISTICS, PRECISION, Amplitude, Space and Planetary Science, Physical Sciences, SKEWNESS, INFERENCE, large-scale structure of Universe, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a field-based approach to the analysis of cosmic shear data to infer jointly cosmological parameters and the dark matter distribution. This forward modelling approach samples the cosmological parameters and the initial matter fluctuations, using a physical gravity model to link the primordial fluctuations to the non-linear matter distribution. Cosmological parameters are sampled and updated consistently through the forward model, varying (1) the initial matter power spectrum, (2) the geometry through the distance-redshift relationship, and (3) the growth of structure and light-cone effects. Our approach extracts more information from the data than methods based on two-point statistics. We find that this field-based approach lifts the strong degeneracy between the cosmological matter density, $\Omega_\mathrm{m}$, and the fluctuation amplitude, $\sigma_8$, providing tight constraints on these parameters from weak lensing data alone. In the simulated four-bin tomographic experiment we consider, the field-based likelihood yields marginal uncertainties on $\sigma_8$ and $\Omega_\mathrm{m}$ that are, respectively, a factor of 3 and 5 smaller than those from a two-point power spectrum analysis applied to the same underlying data., Comment: Accepted in MNRAS
Published: 2021

23. Intrinsic alignments of galaxies around cosmic voids

Author: William, d'Assignies D., Chisari, Nora Elisa, Hamaus, Nico, Singh, Sukhdeep, Sub String Theory Cosmology and ElemPart, Theoretical Physics, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sub String Theory Cosmology and ElemPart, and Theoretical Physics
Subjects: Void (astronomy), Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, data analysis, gravitational lensing, weak, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, methods, 0103 physical sciences, galaxies, 010303 astronomy & astrophysics, Scaling, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, media_common, Physics, COSMIC cancer database, 010308 nuclear & particles physics, (cosmology) large-scale structure of Universe, Astronomy and Astrophysics, Galaxy, Redshift, Amplitude, 13. Climate action, Sky, statistics, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The intrinsic alignments of galaxies, i.e., the correlation between galaxy shapes and their environment, are a major source of contamination for weak gravitational lensing surveys. Most studies of intrinsic alignments have so far focused on measuring and modelling the correlations of luminous red galaxies with galaxy positions or the filaments of the cosmic web. In this work, we investigate alignments around cosmic voids. We measure the intrinsic alignments of luminous red galaxies detected by the Sloan Digital Sky Survey around a sample of voids constructed from those same tracers and with radii in the ranges: $[20-30; 30-40; 40-50]$ $h^{-1}$ Mpc and in the redshift range $z=0.4-0.8$. We present fits to the measurements based on a linear model at large scales, and on a new model based on the void density profile inside the void and in its neighbourhood. We constrain the free scaling amplitude of our model at small scales, finding no significant alignment at $1\sigma$ for either sample. We observe a deviation from the null hypothesis, at large scales, of 2$\sigma$ for voids with radii between 20 and 30 $h^{-1}$ Mpc, and 1.5 $\sigma$ for voids with radii between 30 and 40 $h^{-1}$ Mpc and constrain the amplitude of the model on these scales. We find no significant deviation at 1$\sigma$ for larger voids. Our work is a first attempt at detecting intrinsic alignments of galaxy shapes around voids and provides a useful framework for their mitigation in future void lensing studies., Comment: 11 pages, 8 figures, matches accepted version
Published: 2021

24. The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray Observable-to-Mass-and-Redshift Relations of Galaxy Clusters and Groups with Weak-Lensing Mass Calibration from the Hyper Suprime-Cam Subaru Strategic Program Survey

Author: I-Non Chiu, Vittorio Ghirardini, Ang Liu, Sebastian Grandis, Esra Bulbul, Y. Emre Bahar, Johan Comparat, Sebastian Bocquet, Nicolas Clerc, Matthias Klein, Teng Liu, Xiangchong Li, Hironao Miyatake, Joseph Mohr, Surhud More, Masamune Oguri, Nobuhiro Okabe, Florian Pacaud, Miriam E. Ramos-Ceja, Thomas H. Reiprich, Tim Schrabback, Keiichi Umetsu, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: clusters: intracluster medium, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, gravitational lensing: weak, 0103 physical sciences, dark energy, education, 010303 astronomy & astrophysics, Scaling, Galaxy cluster, Weak gravitational lensing, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Observable, Redshift, galaxies: clusters: general, Space and Planetary Science, cosmology: observations, Product (mathematics), large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first weak-lensing mass calibration and X-ray scaling relations of galaxy clusters and groups selected in the $eROSITA$ Final Equatorial Depth Survey (eFEDS) observed by Spectrum Roentgen Gamma/$eROSITA$ over a contiguous footprint with an area of $\approx140$ deg$^2$, using the three-year (S19A) weak-lensing data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. In this work, a sample of $434$ optically confirmed galaxy clusters (and groups) at redshift $0.01\lesssim z \lesssim1.3$ with a median of $0.35$ is studied, of which $313$ systems are uniformly covered by the HSC survey to enable the extraction of the weak-lensing shear observable. In a Bayesian population modelling, we perform a blind analysis for the weak-lensing mass calibration by simultaneously modelling the observed count rate $\eta$ and the shear profile $g$ of individual clusters through the count rate-to-mass-and-redshift ($\eta$--$M_{500}$--$z$) and weak-lensing mass-to-mass-and-redshift ($M_{\mathrm{WL}}$--$M_{500}$--$z$) relations, respectively, while accounting for the bias in these observables using simulation-based calibrations. As a result, the count rate-inferred and lensing-calibrated cluster mass is obtained from the joint modelling of the scaling relations, as the ensemble mass spanning a range of $10^{13}h^{-1}M_{\odot}\lesssim M_{500}\lesssim10^{15} h^{-1}M_{\odot}$ with a median of $\approx10^{14} h^{-1}M_{\odot}$ for the eFEDS sample. With the mass calibration, we further model the X-ray observable-to-mass-and-redshift relations, including the rest-frame soft-band and bolometric luminosity ($L_{\mathrm{X}}$ and $L_{\mathrm{b}}$), the emission-weighted temperature $T_{\mathrm{X}}$, the mass of intra-cluster medium $M_{\mathrm{g}}$, and the mass proxy $Y_{\mathrm{X}}$, which is the product of $T_{\mathrm{X}}$ and $M_{\mathrm{g}}$. (abridged), Comment: Accepted for publication in A&A. Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission
Published: 2021

25. The potential role of binary neutron star merger afterglows in multimessenger cosmology

Author: E. Chassande-Mottin, Robert Mochkovitch, Raphaël Duque, S. Mastrogiovanni, Frédéric Daigne, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-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 Cité (UPCité), and ANR-18-IDEX-0001,Université de Paris,Université de Paris(2018)
Subjects: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, Orbital inclination, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, stars: neutron, 0103 physical sciences, cosmological parameters, 010303 astronomy & astrophysics, Luminosity distance, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, Computer Science::Information Retrieval, Astronomy and Astrophysics, Redshift, Afterglow, Neutron star, gravitational waves, Space and Planetary Science, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Kuiper belt: general, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: Binary neutron star mergers offer a new and independent means of measuring the Hubble constant H0 by combining the gravitational-wave inferred source luminosity distance with its redshift obtained from electromagnetic follow-up. This method is limited by the intrinsic degeneracy between the system distance and orbital inclination in the gravitational-wave signal. Observing the afterglow counterpart to a merger can further constrain the inclination angle, allowing this degeneracy to be partially lifted and improving the measurement of H0. In the case of the binary neutron star merger GW170817, afterglow light-curve and imaging modeling thus allowed the H0 measurement to be improved by a factor of three. However, systematic access to afterglow data is far from guaranteed. In fact, though each one allows a leap in H0 precision, these afterglow counterparts should prove rare in forthcoming multimessenger campaigns. We combine models for emission and detection of gravitational-wave and electromagnetic radiation from binary neutron star mergers with realistic population models and estimates for afterglow inclination angle constraints. Using these models, we quantify how fast H0 will be narrowed down by successive multimessenger events with and without the afterglow. We find that because of its rareness and though it greatly refines angle estimates, the afterglow counterpart should not significantly contribute to the measurement of H0 in the long run.
Published: 2021

26. The X-CLASS survey: A catalogue of 1646 X-ray-selected galaxy clusters up to z$\sim$1.5

Author: Koulouridis, E., Clerc, N., Sadibekova, T., Chira, M., Drigga, E., Faccioli, L., Fèvre, J.P. Le, Garrel, C., Gaynullina, E., Gkini, A., Kosiba, M., Pacaud, F., Pierre, M., Ridl, J., Tazhenova, K., Adami, C., Altieri, B., Baguley, J.-C., Cabanac, R., Cucchetti, E., Khalikova, A., Lieu, M., Melin, J.-B., Molham, M., Ramos-Ceja, M.E., Soucail, G., Takey, A., Valtchanov, I., Le Fèvre, J., Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing [Penteli] (IAASARS), National Observatory of Athens (NOA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Aristotle University of Thessaloniki, Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Department of Astrophysics, Astronomy and Mechanics [Kapodistrian Univ], National and Kapodistrian University of Athens (NKUA), Masaryk University [Brno] (MUNI), Dipartimento di Fisica [Torino], Università degli studi di Torino (UNITO), Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, European Space Astronomy Centre (ESAC), European Space Agency (ESA), H. H. Wills Physics Laboratory [Bristol], University of Bristol [Bristol], School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), National Research Institute of Astronomy and Geophysics [Helwan] (NRIAG), Telespazio, Services par satellites, Operations Department (ESAC), European Space Agency (ESA)-European Space Agency (ESA), The Saclay team, 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), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli studi di Torino = University of Turin (UNITO), Agence Spatiale Européenne = European Space Agency (ESA), and Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Galaxy cluster, media_common, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Universe, Determining the number of clusters in a data set, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Cluster sampling, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Cosmological probes based on galaxy clusters rely on cluster number counts and large-scale structure information. X-ray cluster surveys are well suited for this purpose, since they are far less affected than optical surveys by projection effects, and cluster properties can be predicted with good accuracy. The XMM Cluster Archive Super Survey, X-CLASS, is a serendipitous search of X-ray-detected galaxy clusters in 4176 XMM-Newton archival observations until August 2015. All observations are clipped to exposure times of 10 and 20 ks to obtain uniformity and they span ~269 deg$^2$ across the high-Galactic latitude sky ($|b|> 20^o$). The main goal of the survey is the compilation of a well-selected cluster sample suitable for cosmological analyses. We describe the detection algorithm, the visual inspection, the verification process and the redshift validation of the cluster sample, as well as the cluster selection function computed by simulations. We also present the various metadata that are released with the catalogue, along with the redshifts of 124 clusters obtained with a dedicated multi-object spectroscopic follow-up programme. With this publication we release the new X-CLASS catalogue of 1646 well-selected X-ray-detected clusters over a wide sky area, along with their selection function. The sample spans a wide redshift range, from the local Universe up to z~1.5, with 982 spectroscopically confirmed clusters, and over 70 clusters above z=0.8. Because of its homogeneous selection and thorough verification, the cluster sample can be used for cosmological analyses, but also as a test-bed for the upcoming eROSITA observations and other current and future large-area cluster surveys. It is the first time that such a catalogue is made available to the community via an interactive database which gives access to a wealth of supplementary information, images, and data., Accepted for publication in A&A
Published: 2021

27. Forecasting the $Y_{500}-M_{500}$ scaling relation from the NIKA2 SZ Large Program

Author: Kéruzoré, Florian, Artis, Emmanuel, Macías-Pérez, Juan-Francisco, Mayet, Frédéric, Muñoz-Echeverría, Miren, Perotto, Laurence, Ruppin, Florian, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), and Université Grenoble Alpes (UGA)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Physics, QC1-999, 0103 physical sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 01 natural sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: One of the key elements needed to perform the cosmological exploitation of a cluster survey is the relation between the survey observable and the cluster masses. Among these observables, the integrated Compton parameter $Y$ is a measurable quantity in Sunyaev-Zeldovich (SZ) surveys, which tightly correlates with cluster mass. The calibration of the relation between the Compton parameter $Y_{500}$ and the mass $M_{500}$ enclosed within radius $R_{500}$ is one of the scientific goals of the NIKA2 SZ Large Program (LPSZ). We present an ongoing study to forecast the constraining power of this program, using mock simulated datasets that mimic the large program sample, selection function, and typical uncertainties on $Y_{500}$ and $M_{500}$. We use a Bayesian hierarchical modeling that enables taking into account a large panel of systematic effects. Our results show that the LPSZ can yield unbiased estimates of the scaling relation parameters for realistic input parameter values. The relative uncertainties on these parameters is $\sim 10\%$ for the intercept and slope of the scaling relation, and $\sim 34\%$ for its intrinsic scatter, foreshadowing precise estimates to be delivered by the LPSZ., Comment: To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences
Published: 2021

28. Constraining AGN feedback model with SZ profile

Author: Hideki Tanimura, Gary Hinshaw, Ian G. McCarthy, Ludovic Van Waerbeke, Nabila Aghanim, Yin-Zhe Ma, Alexander Mead, Tilman Tröster, Alireza Hojjati, Bruno Moraes, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Physics, QC1-999, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, 13. Climate action, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Relativistic jets from AGN have a wide range of impacts on galaxy groups and clusters and are key for understanding their formation and physical properties. However, this non-gravitational process is not well understood. Galaxy groups with shallow gravitational potentials are ideal laboratories to study and constrain the AGN feedback model. We studied hot gas in ~66,000 SDSS LRG halos with an average halo mass of 3 x 10^13 Msun using the Planck tSZ map. We have detected their average tSZ radial profile at ~17 sigma and compared it with the cosmo-OWLS cosmological hydrodynamical simulations with different AGN feedback models. The best agreement has been obtained for the AGN 8.0 model in the simulations. We have also compared our measured tSZ profile with the prediction from the universal pressure profile assuming the self-similar relation and found them consistent if the model accounts for the clustering of neighboring haloes via a two-halo term., Comment: To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences
Published: 2021

29. Characterizing the bulk and turbulent gas motions in galaxy clusters

Author: Simon Dupourqué, Etienne Pointecouteau, Nicolas Clerc, Dominique Eckert, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, 13. Climate action, Physics, QC1-999, 0103 physical sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 01 natural sciences, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The most massive halos of matter in the Universe grow via accretion and merger events throughout cosmic times. These violent processes generate shocks at many scales and induce large-scale bulk and turbulent motions. These processes inject kinetic energy at large scales, which is transported to the viscous dissipation scales, contributing to the overall heating and virialisation of the halo, and acting as a source of non-thermal pressure in the intra-cluster medium. Characterizing the physical properties of these gas motions will help us to better understand the assembly of massive halos, hence the formation and the evolution of these large-scale structures. We base this characterization on the study of the X-ray and Sunyaev-Zel'dovich effect brightness fluctuations. Our work relies on three complementary samples covering a wide range of redshifts, masses and dynamical states of clusters. We present the results of our X-ray analysis for the low redshift sample, X-COP, and a subsample of higher redshift clusters. We investigate the derived properties according to the dynamical state of our clusters, and the possibility of a self-similar behaviour based on the reconstructed gas motions power-spectra and the correlation with various morphological indicators., To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences
Published: 2021

30. Ultra-luminous high-redshift quasars from SkyMapper -- II. New quasars and the bright end of the luminosity function

Author: Christopher A Onken, Christian Wolf, Fuyan Bian, Xiaohui Fan, Wei Jeat Hon, David Raithel, Patrick Tisserand, Samuel Lai, Université Pierre et Marie Curie - Paris 6 (UPMC), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 01 natural sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We search for ultra-luminous Quasi-Stellar Objects (QSOs) at high redshift using photometry from the SkyMapper Southern Survey Data Release 3 (DR3), in combination with 2MASS, VHS DR6, VIKING DR5, AllWISE, and CatWISE2020, as well as parallaxes and proper motions from Gaia DR2 and eDR3. We report 142 newly discovered Southern QSOs at $3.880$ per cent complete for $M_{145}, Comment: 25 pages. Resubmitted to MNRAS after significant revisions. 23 new QSOs added; overhaul of methodology; important changes to results
Published: 2021

31. Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Data Calibration

Author: Amon, A., Gruen, D., Troxel, M. A., MacCrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., DeRose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferté, A., Raveri, M., Lemos, P., Campos, A., Prat, J., Sánchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P. -F., Liddle, A. R., McCullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kron, R., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Weller, J., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Generalitat de Catalunya, Department of Energy (US), National Science Foundation (US), National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Amon, A., Gruen, D., Troxel, M. A., Maccrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., Derose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferte, A., Lemos, P., Raveri, M., Campos, A., Prat, J., Sanchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Gaztanaga, E., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P., Liddle, A. R., Mccullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kron, R., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Petravick, D., Pieres, A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Tarle, G., Thomas, D., To, C., Weller, J., Stanford University, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, Duke University, University of Cambridge, Carnegie Mellon University, The Ohio State University, University of Pennsylvania, University of Chicago, University of Arizona, University of Manchester, Lawrence Berkeley National Laboratory, Universidade Estadual de Campinas (UNICAMP), Laboratório Interinstitucional de E-Astronomia, Observatoire de Sauverny, Argonne National Laboratory, California Institute of Technology, University College London, University of Sussex, University of Michigan, Universidade Estadual Paulista (UNESP), University of Wisconsin-Madison, Instituto de Astrofisica de Canarias, Universidad de la Laguna, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Fermi National Accelerator Laboratory, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Santa Cruz Institute for Particle Physics, The Barcelona Institute of Science and Technology, Denys Wilkinson Building, University of Geneva, University of Edinburgh, Universidade de Lisboa, Perimeter Institute for Theoretical Physics, The University of Tokyo, ETH Zurich, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, University of Portsmouth, Institut d'Astrophysique de Paris, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics|Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, and UAM. Departamento de Física Teórica
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), microwave background anisotropies, systematic-errors, FOS: Physical sciences, parameter constraints, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, large-scale structure, Astrophysic, weak-lensing surveys, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, internal consistency, Weak, redshift distributions, 010303 astronomy & astrophysics, Gravitational Lensing, 010308 nuclear & particles physics, Física, Dark Energy, intrinsic correlation, matter power spectrum, 2-point correlation-functions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: A. Amon et al., This work, together with its companion paper, Secco, Samuroff et al. [Phys. Rev. D 105, 023515 (2022)], present the Dark Energy Survey Year 3 cosmic-shear measurements and cosmological constraints based on an analysis of over 100 million source galaxies. With the data spanning 4143 deg2 on the sky, divided into four redshift bins, we produce a measurement with a signal-to-noise of 40. We conduct a blind analysis in the context of the Lambda-Cold Dark Matter (ΛCDM) model and find a 3% constraint of the clustering amplitude, S8≡σ8(Ωm/0.3)0.5=0.759+0.025−0.023. A ΛCDM-Optimized analysis, which safely includes smaller scale information, yields a 2% precision measurement of S8=0.772+0.018−0.017 that is consistent with the fiducial case. The two low-redshift measurements are statistically consistent with the Planck Cosmic Microwave Background result, however, both recovered S8 values are lower than the high-redshift prediction by 2.3σ and 2.1σ (p-values of 0.02 and 0.05), respectively. The measurements are shown to be internally consistent across redshift bins, angular scales and correlation functions. The analysis is demonstrated to be robust to calibration systematics, with the S8 posterior consistent when varying the choice of redshift calibration sample, the modeling of redshift uncertainty and methodology. Similarly, we find that the corrections included to account for the blending of galaxies shifts our best-fit S8 by 0.5σ without incurring a substantial increase in uncertainty. We examine the limiting factors for the precision of the cosmological constraints and find observational systematics to be subdominant to the modeling of astrophysics. Specifically, we identify the uncertainties in modeling baryonic effects and intrinsic alignments as the limiting systematics., This research manuscript made use of Astropy [204,205], GetDist [206], ChainConsumer10 [207] and Matplotlib [208], and has been prepared using NASA’s Astrophysics Data System Bibliographic Services. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana- Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, and Office of High Energy Physics.
Published: 2021

32. Three Lyman-α-emitting filaments converging to a massive galaxy group at z = 2.91: discussing the case for cold gas infall

Author: Shuowen Jin, Alexis Finoguenov, David Elbaz, James D. Neill, Max Gronke, I. Delvecchio, Emanuele Daddi, Raphael Gobat, Tao Wang, B.S. Kalita, Daizhong Liu, C. D'Eugenio, Annagrazia Puglisi, D. C. Martin, A. Calabrò, Donal O'Sullivan, Francesco Valentino, Frederic Bournaud, Antoine Marchal, V. Strazzullo, R. M. Rich, Peter Laursen, Eva Schinnerer, R. Coogan, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Department of Physics, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), SIMILAR-TO 2, galaxies: clusters: intracluster medium, CIRCUMGALACTIC MEDIUM, FOS: Physical sciences, galaxies: groups: individual: RO-1001, Astrophysics, groups: individual: RO-1001 [galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, LY-ALPHA, COOL GAS, Galaxy group, 0103 physical sciences, Galaxy formation and evolution, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, CLUSTER CL J1449+0856, MAIN-SEQUENCE, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, MULTIPHASE GAS, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, formation [Galaxy], 13. Climate action, Space and Planetary Science, clusters: intracluster medium [galaxies], Galaxy: formation, Astrophysics of Galaxies (astro-ph.GA), BLACK-HOLE ACCRETION, Astrophysics::Earth and Planetary Astrophysics, large-scale structure of Universe, STELLAR MASS, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have discovered a 300kpc-wide giant Lya nebula centered on the massive galaxy group RO-1001 at z=2.91 in the COSMOS field. Keck Cosmic Web Imager observations reveal three cold gas filaments converging into the center of the potential well of its ~4x10^13Msun dark matter halo, hosting 1200Msun/yr of star formation as probed by ALMA and NOEMA observations. The nebula morphological and kinematics properties and the prevalence of blueshifted components in the Lya spectra are consistent with a scenario of gas accretion. The upper limits on AGN activity and overall energetics favor gravity as the primary Lya powering source and infall as the main source of gas flows to the system. Although interpretational difficulties remain, with outflows and likely also photoionization with ensuing recombination still playing a role, this finding provides arguably an ideal environment to quantitatively test models of cold gas accretion and galaxy feeding inside an actively star-forming massive halo at high redshift., Comment: 20 pages, 12 figures, 3 tables. Accepted for publication in A&A
Published: 2021

33. Closing up the cluster tension?

Author: Stéphane Ilić, Alain Blanchard, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), LERMA Cergy (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics beyond the Standard Model, Dark matter, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, 0103 physical sciences, Planck, cosmological parameters, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Sigma, Astronomy and Astrophysics, Redshift, Amplitude, Space and Planetary Science, galaxies: clusters: general, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Free parameter, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The excellent measurements of the cosmic microwave background (CMB) fluctuations by Planck allow us to tightly constrain the amplitude of matter fluctuations at redshift $\sim 1100$ in the $\Lambda$-cold dark matter ($\Lambda$CDM) model. This amplitude can be extrapolated to the present epoch, yielding constraints on the value of the $\sigma_8$ parameter. On the other hand, the abundance of Sunyaev-Zeldovich (SZ) clusters detected by Planck, with masses inferred using a hydrostatic equilibrium assumption, leads to a significantly lower value of the same parameter. This discrepancy is often dubbed the $\sigma_8$ tension in the literature and is sometimes regarded as a possible sign of new physics. Here, we examine a direct determination of $\sigma_8$ at the present epoch in $\Lambda$CDM, and thereby the cluster mass calibrations using cosmological data at low redshift, namely the measurements of $f\sigma_8$ from the analysis of the completed Sloan Digital Sky Survey (SDSS). We combined redshift-space distortion measurements with Planck CMB constraints, X-ray, and SZ cluster counts within the $\Lambda$CDM framework, but leaving the present-day amplitude of matter fluctuations as an independent parameter (i.e. no extrapolation is made from high-redshift CMB constraints). The calibration of X-ray and SZ masses are left as free parameters throughout the whole analysis. Our study yields tight constraints on the aforementioned calibrations, with values entirely consistent with results obtained from the full combination of CMB and cluster data only. Such an agreement suggests an absence of tension in the $\Lambda$CDM model between CMB-based estimates of $\sigma_8$ and constraints from low-redshift on $f\sigma_8$; however, it also indicates tension with the standard calibration of clusters masses., Comment: 4 pages, 1 figure, accepted in A&A, v2: replaced to match the accepted version
Published: 2021

34. Galaxy Clustering in Harmonic Space from the Dark Energy Survey Year 1 Data: Compatibility with Real-Space Results

Author: R. Cawthon, M. Smith, D. H. Brooks, Josh Frieman, Bhuvnesh Jain, Ofer Lahav, Robert Morgan, Xiao Fang, R. L. C. Ogando, F. Andrade-Oliveira, A. Troja, O. Alves, Santiago Avila, Chihway Chang, Felipe Menanteau, Samuel Hinton, V. Scarpine, Martin Crocce, Shantanu Desai, M. Carrasco Kind, Antonella Palmese, Rogerio Rosenfeld, J. Carretero, L. Faga, D. L. Burke, Enrique Gaztanaga, M. Rodriguez-Monroy, I. Sevilla-Noarbe, Gregory Tarle, M. Soares-Santos, N. Kuropatkin, E. Suchyta, S. Everett, J. Myles, L. N. da Costa, C. Doux, Chun-Hao To, August E. Evrard, E. J. Sanchez, D. Gruen, Alex Drlica-Wagner, N. Kokron, Javier Sanchez, Santiago Serrano, S. Allam, Robert A. Gruendl, S. Pandey, Ramon Miquel, Jack Elvin-Poole, J. Annis, M. Costanzi, D. L. Hollowood, David James, A. Choi, R. Gomes, Peter Melchior, M. A. G. Maia, Michel Aguena, Marcos Lima, D. W. Gerdes, F. Paz-Chinchón, I. Ferrero, Maria E. S. Pereira, Juan Garcia-Bellido, E. Bertin, Oliver Friedrich, H. Camacho, Vivian Miranda, M. March, A. A. Plazas Malagón, Peter Doel, H. T. Diehl, Niall MacCrann, A. Porredon, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Andrade-Oliveira, F., Camacho, H., Faga, L., Gomes, R., Rosenfeld, R., Troja, A., Alves, O., Doux, C., Elvin-Poole, J., Fang, X., Friedrich, O., Kokron, N., Lima, M., Miranda, V., Pandey, S., Porredon, A., Sanchez, J., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Cawthon, R., Chang, C., Choi, A., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Jain, B., James, D. J., Kuropatkin, N., Lahav, O., Maccrann, N., Maia, M. A. G., March, M., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Des, Collaboration, National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de e-Astronomia - LIneA, Universidade de São Paulo (USP), University of Michigan, University of Pennsylvania, The Ohio State University, University of Arizona, University of Cambridge, Stanford University, Institut d’Estudis Espacials de Catalunya (IEEC), CSIC), Fermi National Accelerator Laboratory, Universidad Autonoma de Madrid, Institut d’Astrophysique de Paris, University College London, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, University of Wisconsin-Madison, University of Chicago, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Santa Cruz Institute for Particle Physics, University of Oslo, University of Queensland, Harvard & Smithsonian, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Medioambientales y Tecnológicas (CIEMAT), University of Southampton, and Oak Ridge National Laboratory
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, cosmology: observations, large-scale structure of Universe, Pipeline (computing), FOS: Physical sciences, Scale (descriptive set theory), observations, large-scale structure of Universe [cosmology], Space (mathematics), 7. Clean energy, 01 natural sciences, 0103 physical sciences, observations [Cosmology], Cluster analysis, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Covariance matrix, Cosmology: observations, Astronomy and Astrophysics, cosmology: observations, large-scale structure of Universe, Galaxy, Space and Planetary Science, Log-normal distribution, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Andrade-Oliveira, F., et al. (DES Collaboration), We perform an analysis in harmonic space of the Dark Energy Survey Year 1 Data (DES-Y1) galaxy clustering photometric data using products obtained for the real-space analysis. We test our pipeline with a suite of lognormal simulations, which are used to validate scale cuts in harmonic space as well as to provide a covariance matrix that takes into account the DES-Y1 mask. We then apply this pipeline to DES-Y1 data taking into account survey property maps derived for the real-space analysis. We compare with real-space DES-Y1 results obtained from a similar pipeline. We show that the harmonic space analysis we develop yields results that are compatible with the real-space analysis for the bias parameters. This verification paves the way to performing a harmonic space analysis for the upcoming DES-Y3 data., The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021

35. SatGen: a semi-analytical satellite galaxy generator – I. The model and its application to Local-Group satellite statistics

Author: Frank C. van den Bosch, Fangzhou Jiang, Philip F. Hopkins, Jonathan Freundlich, Avishai Dekel, Sheridan B. Green, Xiaolong Du, Andrew J. Benson, 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: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, 010308 nuclear & particles physics, Star formation, Milky Way, Local Group, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Statistics, Satellite galaxy, Satellite, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a semi-analytic model of satellite galaxies, SatGen, which can generate large samples of satellite populations for a host halo of desired mass, redshift, and assembly history. The model combines dark-matter halo merger trees, empirical relations for the galaxy-halo connection, and analytic prescriptions for tidal effects, dynamical friction, and ram pressure stripping. SatGen emulates cosmological zoom-in hydro-simulations in certain aspects. Satellites can reside in cored or cuspy DM subhaloes, depending on the halo response to baryonic physics that can be formulated from hydro-simulations and physical modeling. The subhalo profile and the stellar mass and size of a satellite evolves depending on its tidal mass loss and initial structure. The host galaxy can include a baryonic disc and a stellar bulge, each described by a density profile that allows analytic orbit integration. SatGen complements simulations by propagating the effect of halo response found in simulated field galaxies to satellites (not properly resolved in simulations) and outperforms simulations by sampling the halo-to-halo variance of satellite statistics and overcoming artificial disruption due to insufficient resolution. As a first application, we use the model to study satellites of Milky Way sized hosts, making it emulate simulations of bursty star formation and of smooth star formation, respectively, and to experiment with a disc potential in the host halo. Our model reproduces the observed satellite statistics reasonably well. Different physical recipes make a difference in satellite abundance and spatial distribution at the 25% level, not large enough to be distinguished by current observations given the halo-to-halo variance. The MW disc depletes satellites by 20% and has a subtle effect of diversifying the internal structure of satellites, important for alleviating certain small-scale problems., Comment: 18 pages, 9 figures, submitted to MNRAS
Published: 2021

36. Information content in mean pairwise velocity and mean relative velocity between pairs in a triplet

Author: Joseph Kuruvilla, Nabila Aghanim, Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)
Subjects: Particle physics, velocity, Cosmology and Nongalactic Astrophysics (astro-ph.CO), statistical analysis: confidence limit, higher-order, triplet, halo, kinetic, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, triangulation, cosmic background radiation, Sunyaev–Zel'dovich effect, 01 natural sciences, Omega, cosmology: theory, cosmological model: parameter space, 0103 physical sciences, Peculiar velocity, neutrino: mass, structure, 010303 astronomy & astrophysics, perturbation theory, information theory, Physics, 010308 nuclear & particles physics, Relative velocity, Order (ring theory), Astronomy and Astrophysics, Space and Planetary Science, statistics, Content (measure theory), Sunyaev-Zel'dovich effect, many-body problem, n-point function: 3, large-scale structure of Universe, Halo, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Velocity field provides a complementary avenue to constrain cosmological information, either through the peculiar velocity surveys or the kinetic Sunyaev Zel'dovich effect. One of the commonly used statistics is the mean radial pairwise velocity. Here, we consider the three-point mean relative velocity, i.e. the mean relative velocities between pairs in a triplet. Using halo catalogs from the Quijote suite of N-body simulations, we first showcase how the analytical prediction for the mean relative velocities between pairs in a triplet achieve better than 4-5% accuracy using standard perturbation theory at leading order for triangular configurations with a minimum separation of $r \geq 50\ h^{-1}$Mpc. Furthermore, we present the three-point relative velocity as a novel probe of neutrino mass estimation. We explore the full cosmological information content of the halo mean pairwise velocities, and the mean relative velocities between halo pairs in a triplet. We undertake this through the Fisher-matrix formalism using 22,000 simulations from the Quijote suite, and considering all triangular configurations with a minimum and a maximum separation of $20\ h^{-1}$Mpc and $120\ h^{-1}$Mpc, respectively. We find that the mean relative velocities in a triplet allows a 1$\sigma$ neutrino mass ($M_\nu$) constraint of 0.065 eV, that is roughly 13 times better than the mean pairwise velocity constraint (0.877 eV). This information gain is not limited only to neutrino mass, but extends to other cosmological parameters: $\Omega_{\mathrm{m}}$, $\Omega_{\mathrm{b}}$, $h$, $n_{\mathrm{s}}$ and $\sigma_{8}$ achieving a gain of 8.9, 11.8, 15.5, 20.9 and 10.9 times respectively. These results illustrate the possibility of exploiting the mean three-point relative velocities for constraining the cosmological parameters accurately from future cosmic microwave background experiments and peculiar velocity surveys., Comment: 13 pages, 10 figures, accepted for publication in A&A
Published: 2021

37. Gamma-ray detection toward the Coma cluster with Fermi-LAT: Implications for the cosmic ray content in the hadronic scenario

Author: Steve D.M. Brown, H. Goksu, Chiara Ferrari, R. Adam, Lawrence Rudnick, Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Proton, Point source, electron: acceleration, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, electron: relativistic, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, energy: thermal, 01 natural sciences, programming, energy spectrum: slope, Secondary electrons, GLAST, galaxies: clusters: individual: Coma, cosmic rays, gas, cluster: formation, 0103 physical sciences, synchrotron, Coma Cluster, energy: ratio, model: cluster, 010303 astronomy & astrophysics, Galaxy cluster, gamma rays: galaxies: clusters, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, radio wave, cosmic radiation: energy spectrum, 010308 nuclear & particles physics, electron: cosmic radiation, Astronomy and Astrophysics, electron: secondary, cosmic radiation: primary, gamma ray: emission, 13. Climate action, Space and Planetary Science, p: cosmic radiation, Content (measure theory), galaxy: cluster, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The presence of relativistic electrons within the diffuse gas phase of galaxy clusters is now well established, but their detailed origin remains unclear. Cosmic ray protons are also expected to accumulate during the formation of clusters and would lead to gamma-ray emission through hadronic interactions within the thermal gas. Recently, the detection of gamma-ray emission has been reported toward the Coma cluster with Fermi-LAT. Assuming that this gamma-ray emission arises from hadronic interactions in the ICM, we aim at exploring the implication of this signal on the cosmic ray content of the Coma cluster. We use the MINOT software to build a physical model of the cluster and apply it to the Fermi-LAT data. We also consider contamination from compact sources and the impact of various systematic effects. We confirm that a significant gamma-ray signal is observed within the characteristic radius $\theta_{500}$ of the Coma cluster, with a test statistic TS~27 for our baseline model. The presence of a possible point source may account for most of the observed signal. However, this source could also correspond to the peak of the diffuse emission of the cluster itself and extended models match the data better. We constrain the cosmic ray to thermal energy ratio within $R_{500}$ to $X_{\rm CRp}=1.79^{+1.11}_{-0.30}$\% and the slope of the energy spectrum of cosmic rays to $\alpha=2.80^{+0.67}_{-0.13}$. Finally, we compute the synchrotron emission associated with the secondary electrons produced in hadronic interactions assuming steady state. This emission is about four times lower than the overall observed radio signal, so that primary cosmic ray electrons or reacceleration of secondary electrons is necessary to explain the total emission. Assuming an hadronic origin of the signal, our results provide the first quantitative measurement of the cosmic ray proton content in a cluster.[Abridged], Comment: 27 pages, accepted in A&A
Published: 2021

38. Shape and connectivity of groups and clusters: Impact of dynamical state and accretion history

Author: Tony Bonnaire, Nabila Aghanim, C. Gouin, Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Recherche en Informatique (LRI), Université Paris-Sud - Paris 11 (UP11)-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Dynamique des Fluides (DynFluid), Conservatoire National des Arts et Métiers [CNAM] (CNAM)-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, methods: statistical, Strongly connected component, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Accretion (astrophysics), methods: numerical, galaxies: clusters: general, Space and Planetary Science, Phase (matter), 0103 physical sciences, large-scale structure of Universe, Halo, Anisotropy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Distribution (differential geometry), Sign (mathematics), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Matter distribution around clusters is highly anisotropic from their being the nodes of the cosmic web. Clusters' shape and the number of filaments they are connected to, i.e., their connectivity, should reflect their level of anisotropic matter distribution and must be, in principle, related to their physical properties. We investigate the influence of the dynamical state and the formation history on both the morphology and local connectivity of about 2400 groups and clusters of galaxies from the large hydrodynamical simulation IllustrisTNG at z=0. We find that the mass of groups and clusters mainly influences the geometry of the matter distribution: massive halos are significantly more elliptical, and more connected to the cosmic web than low-mass ones. Beyond the mass-driven effect, ellipticity and connectivity are correlated and are imprints of the growth rate of groups and clusters. Both anisotropy measures appear to trace different dynamical states, such that unrelaxed groups and clusters are more elliptical and more connected than relaxed ones. This relation between matter anisotropies and dynamical state is the sign of different accretion histories. Relaxed groups and clusters are mostly formed long time ago, and slowly accreting matter at the present time. They are rather spherical and weakly connected to their environment, mostly because they had enough time to relax and, hence, lost the connection with their preferential directions of accretion and merging. In contrast, late-formed unrelaxed objects are highly anisotropic with large connectivities and ellipticities. These groups and clusters are in formation phase and must be strongly affected by the infalling of materials from filaments., Accepted to A&A, 13 pages, 11 figures, comments are welcome
Published: 2021

39. Close-up view of a luminous star-forming galaxy at z = 2.95

Author: A. Carnero Rosell, I. Perez-Fournon, C. N. Herrera, Steve Serjeant, Andrew I. Harris, R. Neri, C. Yang, Axel Weiß, Lucia Marchetti, A. J. Young, Catherine Vlahakis, Hugo Messias, M. Krips, T. Bakx, Mattia Negrello, David H. Hughes, Asantha Cooray, Guilaine Lagache, Alexandre Beelen, Rob Ivison, Helmut Dannerbauer, Matthew D. Lehnert, Pierre Cox, S. Urquhart, Andrew J. Baker, P. van der Werf, Simon Dye, B. M. Jones, Alain Omont, V. Buat, Dominik Riechers, Shuowen Jin, Isabella Cortzen, Raphael Gavazzi, Loretta Dunne, F. Stanley, S. Berta, Steve Eales, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Astronomia [Padova], Università degli Studi di Padova = University of Padua (Unipd), Tongji University, Department of Astronomy [Ithaca], Cornell University [New York], Institut für Astronomie [Wien], Universität Wien, Instituto de Astrofisica de Canarias (IAC), 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)-Centre National d’Études Spatiales [Paris] (CNES), 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), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), School of Physics and Astronomy [Cardiff], Cardiff University, Max-Planck-Institut für Extraterrestrische Physik (MPE), Max-Planck-Institut für Radioastronomie (MPIFR), AUTRES, CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universita degli Studi di Padova, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Irvine] (UCI), University of California-University of California, and BUAT, Veronique
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Absorption spectroscopy, Einstein ring, Infrared, Astrophysics - cosmology and nongalactic astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Spectral line, [SDU] Sciences of the Universe [physics], symbols.namesake, galaxies: high-redshift, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, [PHYS]Physics [physics], radio lines: ISM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Galaxy, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], galaxies: star formation, symbols, Millimeter, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract: (Abridged) Exploiting the sensitivity and broad band width of NOEMA, we have studied the molecular gas and dust in the galaxy HerBS-89a, at z=2.95. High angular resolution images reveal a partial 1.0" diameter Einstein ring in the dust continuum emission and the molecular emission lines of 12CO(9-8) and H2O(2_02-1_11). We report the detection of the three fundamental transitions of the molecular ion OH+, seen in absorption; the molecular ion CH+(1-0) seen in absorption (and tentatively in emission); two transitions of amidogen (NH2), seen in emission; and HCN(11-10) and/or NH(1_2-0_1) seen in absorption. The NOEMA data are complemented with VLA data tracing the 12CO(1-0) emission line, which provides a measurement of the total mass of molecular gas and an anchor for a CO excitation analysis. In addition, we present HST imaging that reveals the foreground lensing galaxy in the near-infrared. Together with data from the GTC, we derive a photometric redshift of z(phot)~0.9 for the foreground lensing galaxy. Modelling the lensing of HerBS-89a, we reconstruct the dust continuum and molecular emission lines (magnified by a factor ~4-5) in the source plane. The 12CO(9-8) and H2O emission lines have comparable spatial and kinematic distributions; the source-plane reconstructions do not clearly distinguish between a one-component and a two-component scenario, but the latter accounts for the observed broad line widths. HerBS-89a is a powerful star forming galaxy with a dust-to-gas ratio delta(GDR)~80, a SFR = 614 +/- 59 Msun/yr and a depletion timescale tau(depl) = (3.4 +/- 1.0) 1e8 years. The OH+ and CH+ absorption lines, all have their main velocity component red-shifted by \Delta(V)~100 km/s relative to the global CO reservoir. We argue that these absorption lines trace a rare example of gas inflow towards the center of the galaxy., Comment: 33 pages, Accepted for publication on A&A
Published: 2021

40. Negative cosmological constant in the dark sector?

Author: Benjamin L'Huillier, David Polarski, Rodrigo Calderón, Radouane Gannouji, Laboratoire Charles Coulomb (L2C), and Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Large class, Physics, Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, media_common.quotation_subject, Big Rip, FOS: Physical sciences, Cosmological constant, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Redshift, Universe, General Relativity and Quantum Cosmology, Theoretical physics, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], 010303 astronomy & astrophysics, Value (mathematics), Scale factor (cosmology), media_common, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We consider the possibility that the dark sector of our Universe contains a negative cosmological constant dubbed $\lambda$. For such models to be viable, the dark sector should contain an additional component responsible for the late-time accelerated expansion rate ($X$). We explore the departure of the expansion history of these models from the concordance $\Lambda$ Cold Dark Matter model. For a large class of our models the accelerated expansion is transient with a nontrivial dependence on the model parameters. All models with $w_X>-1$ will eventually contract and we derive an analytical expression for the scale factor $a(t)$ in the neighborhood of its maximal value. We find also the scale factor for models ending in a Big Rip in the regime where dustlike matter density is negligible compared to $\lambda$. We address further the viability of such models, in particular when a high $H_0$ is taken into account. While we find no decisive evidence for a nonzero $\lambda$, the best models are obtained with a phantom behavior on redshifts $z\gtrsim 1$ with a higher evidence for nonzero $\lambda$. An observed value for $h$ substantially higher than $0.70$ would be a decisive test of their viability., Comment: 12 pages, 5 figures, 4 tables. v3: Matches published version
Published: 2021

41. Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog

Author: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, R. D. Wilkinson, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Department of Energy (US), National Science Foundation (US), Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, Ministerio de Economía y Competitividad (España), UAM. Departamento de Física Teórica, Everett, S., Yanny, B., Kuropatkin, N., Huff, E. M., Zhang, Y., Myles, J., Masegian, A., Elvin-Poole, J., Allam, S., Bernstein, G. M., Sevilla-Noarbe, I., Splettstoesser, M., Sheldon, E., Jarvis, M., Amon, A., Harrison, I., Choi, A., Hartley, W. G., Alarcon, A., Sanchez, C., Gruen, D., Eckert, K., Prat, J., Tabbutt, M., Busti, V., Becker, M. R., Maccrann, N., Diehl, H. T., Tucker, D. L., Bertin, E., Jeltema, T., Drlica-Wagner, A., Gruendl, R. A., Bechtol, K., Rosell, A. C., Abbott, T. M. C., Aguena, M., Annis, J., Bacon, D., Bhargava, S., Brooks, D., Burke, D. L., Kind, M. C., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Derose, J., Desai, S., Eifler, T. F., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kent, S., Krause, E., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Troxel, M. A., Varga, T. N., Weller, J., Wilkinson, R. D., Everett, S [0000-0002-3745-2882], Yanny, B [0000-0002-9541-2678], Kuropatkin, N [0000-0003-2511-0946], Huff, EM [0000-0002-9378-3424], Myles, J [0000-0001-6145-5859], Elvin-Poole, J [0000-0001-5148-9203], Bernstein, GM [0000-0002-8613-8259], Sevilla-Noarbe, I [0000-0002-1831-1953], Sheldon, E [0000-0001-9194-0441], Gruen, D [0000-0003-3270-7644], Eckert, K [0000-0002-1407-4700], Becker, MR [0000-0001-7774-2246], Diehl, HT [0000-0002-8357-7467], Tucker, DL [0000-0001-7211-5729], Bertin, E [0000-0002-3602-3664], Jeltema, T [0000-0001-6089-0365], Drlica-Wagner, A [0000-0001-8251-933X], Gruendl, RA [0000-0002-4588-6517], Abbott, TMC [0000-0003-1587-3931], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Carretero, J [0000-0002-3130-0204], Castander, FJ [0000-0001-7316-4573], Conselice, C [0000-0003-1949-7638], Costanzi, M [0000-0001-8158-1449], Derose, J [0000-0002-0728-0960], Fosalba, P [0000-0002-1510-5214], García-Bellido, J [0000-0002-9370-8360], Gaztanaga, E [0000-0001-9632-0815], Gerdes, DW [0000-0001-6942-2736], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Huterer, D [0000-0001-6558-0112], Kent, S [0000-0003-4207-7420], Kuehn, K [0000-0003-0120-0808], Marshall, JL [0000-0003-0710-9474], Melchior, P [0000-0002-8873-5065], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Palmese, A [0000-0002-6011-0530], Paz-Chinchón, F [0000-0003-1339-2683], Romer, AK [0000-0002-9328-879X], Roodman, A [0000-0001-5326-3486], Serrano, S [0000-0002-0211-2861], Soares-Santos, M [0000-0001-6082-8529], Tarle, G [0000-0003-1704-0781], Weller, J [0000-0002-8282-2010], and Apollo - University of Cambridge Repository
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysic, Weak, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 1464, 351, 1857, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Gravitational Lensing, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, Dark Energy, Space and Planetary Science, astro-ph.CO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: DES Collaboration: Everett et al., We describe an updated calibration and diagnostic framework, Balrog, used to directly sample the selection and photometric biases of the Dark Energy Survey (DES) Year 3 (Y3) data set. We systematically inject onto the single-epoch images of a random 20% subset of the DES footprint an ensemble of nearly 30 million realistic galaxy models derived from DES Deep Field observations. These augmented images are analyzed in parallel with the original data to automatically inherit measurement systematics that are often too difficult to capture with generative models. The resulting object catalog is a Monte Carlo sampling of the DES transfer function and is used as a powerful diagnostic and calibration tool for a variety of DES Y3 science, particularly for the calibration of the photometric redshifts of distant "source" galaxies and magnification biases of nearer "lens" galaxies. The recovered Balrog injections are shown to closely match the photometric property distributions of the Y3 GOLD catalog, particularly in color, and capture the number density fluctuations from observing conditions of the real data within 1% for a typical galaxy sample. We find that Y3 colors are extremely well calibrated, typically within ∼1–8 mmag, but for a small subset of objects, we detect significant magnitude biases correlated with large overestimates of the injected object size due to proximity effects and blending. We discuss approaches to extend the current methodology to capture more aspects of the transfer function and reach full coverage of the survey footprint for future analyses., S.E. and T.J. acknowledge support from the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under award numbers DESC0010107 and A00-1465-001. Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021

42. Higher-order statistics of shear field via a machine learning approach

Author: Roberto Maoli, Vincenzo F. Cardone, Edouard Tollet, Carolina Parroni, Roberto Scaramella, Galaxies, Etoiles, Physique, Instrumentation (GEPI), 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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Higher-order statistics, Astrophysics::Cosmology and Extragalactic Astrophysics, Machine learning, computer.software_genre, 01 natural sciences, Measure (mathematics), gravitational lensing: weak, cosmology: theory, 0103 physical sciences, 010303 astronomy & astrophysics, Weak gravitational lensing, media_common, Physics, methods: statistical, 010308 nuclear & particles physics, business.industry, Estimator, Astronomy and Astrophysics, Graph theory, Universe, Space and Planetary Science, Artificial intelligence, Degeneracy (mathematics), business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], computer, Smoothing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Context.The unprecedented amount and the excellent quality of lensing data expected from upcoming ground and space-based surveys present a great opportunity for shedding light on questions that remain unanswered with regard to our universe and the validity of the standard ΛCDM cosmological model. The development of new techniques that are capable of exploiting the vast quantity of data provided by future observations, in the most effective way possible, is of great importance.Aims.This is the reason we chose to investigate the development of a new method for treating weak-lensing higher-order statistics, which are known to break the degeneracy among cosmological parameters thanks to their capacity to probe non-Gaussian properties of the shear field. In particular, the proposed method applies directly to the observed quantity, namely, the noisy galaxy ellipticity.Methods.We produced simulated lensing maps with different sets of cosmological parameters and used them to measure higher-order moments, Minkowski functionals, Betti numbers, and other statistics related to graph theory. This allowed us to construct datasets with a range of sizes, levels of precision, and smoothing. We then applied several machine learning algorithms to determine which method best predicts the actual cosmological parameters associated with each simulation.Results.The most optimal model turned out to be a simple multidimensional linear regression. We use this model to compare the results coming from the different datasets and find that we can measure, with a good level of accuracy, the majority of the parameters considered in this study. We also investigated the relation between each higher-order estimator and the different cosmological parameters for several signal-to-noise thresholds and redshifts bins.Conclusions.Given the promising results we obtained, we consider this approach a valuable resource that is worthy of further development.
Published: 2021

43. CODEX Weak Lensing Mass Catalogue and implications on the mass-richness relation

Author: Lance Miller, N Cibirka, J. Valiviita, L. van Waerbeke, P. Spinelli, Eduardo Rozo, Nicolas Clerc, J. Patrick Henry, R. A. Dupke, M. Costanzi, K. Kiiveri, Alexis Finoguenov, C. C. Kirkpatrick, Eduardo Serra Cypriano, Eli S. Rykoff, Jochen Weller, Ghassem Gozaliasl, Steffen Hagstotz, J. P. Kneib, Thomas Erben, Huanyuan Shan, Daniel Gruen, Laboratoire d'Astrophysique de Marseille (LAM), 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), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Helsinki Institute of Physics, Department of Physics, 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), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of Helsinki, Helsinki Institute of Physics, University of Helsinki, Department of Physics, Kiiveri, K., Gruen, D., Finoguenov, A., Erben, T., van Waerbeke, L., Rykoff, E., Miller, L., Hagstotz, S., Dupke, R., Henry, J. Patrick, Kneib, J. -P., Gozaliasl, G., Kirkpatrick, C. C., Cibirka, N., Clerc, N., Costanzi, M., Cypriano, E. S., Rozo, E., Shan, H., Spinelli, P., Valiviita, J., and Weller, J.
Subjects: COSMOLOGICAL CONSTRAINTS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, PROFILE, 01 natural sciences, 114 Physical sciences, gravitational lensing: weak, MAXBCG, weak [gravitational lensing], 0103 physical sciences, LARGE-SCALE STRUCTURE, clusters: general [galaxies], PROBE, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, LOCUSS, Physics, TEMPERATURE RELATION, 010308 nuclear & particles physics, Astronomy and Astrophysics, observations [cosmology], Redshift, REDUCTION, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, GIANTS, GALAXY CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The COnstrain Dark Energy with X-ray clusters (CODEX) sample contains the largest flux limited sample of X-ray clusters at $0.35 < z < 0.65$. It was selected from ROSAT data in the 10,000 square degrees of overlap with BOSS, mapping a total number of 2770 high-z galaxy clusters. We present here the full results of the CFHT CODEX program on cluster mass measurement, including a reanalysis of CFHTLS Wide data, with 25 individual lensing-constrained cluster masses. We employ $lensfit$ shape measurement and perform a conservative colour-space selection and weighting of background galaxies. Using the combination of shape noise and an analytic covariance for intrinsic variations of cluster profiles at fixed mass due to large scale structure, miscentring, and variations in concentration and ellipticity, we determine the likelihood of the observed shear signal as a function of true mass for each cluster. We combine 25 individual cluster mass likelihoods in a Bayesian hierarchical scheme with the inclusion of optical and X-ray selection functions to derive constraints on the slope $\alpha$, normalization $\beta$, and scatter $\sigma_{\ln \lambda | \mu}$ of our richness-mass scaling relation model in log-space: $\left = \alpha \mu + \beta$, with $\mu = \ln (M_{200c}/M_{\mathrm{piv}})$, and $M_{\mathrm{piv}} = 10^{14.81} M_{\odot}$. We find a slope $\alpha = 0.49^{+0.20}_{-0.15}$, normalization $ \exp(\beta) = 84.0^{+9.2}_{-14.8}$ and $\sigma_{\ln \lambda | \mu} = 0.17^{+0.13}_{-0.09}$ using CFHT richness estimates. In comparison to other weak lensing richness-mass relations, we find the normalization of the richness statistically agreeing with the normalization of other scaling relations from a broad redshift range ($0.0, Comment: 37 pages, 12 figures
Published: 2021

44. Small-scale primordial fluctuations in the 21 cm Dark Ages signal

Author: Joseph Silk, Philippa S. Cole, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and IoP (FNWI)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Primordial fluctuations, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, first stars, FOS: Physical sciences, Primordial black hole, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, General Relativity and Quantum Cosmology, Binary black hole, cosmology: theory, 0103 physical sciences, dark ages, inflation, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Physics, Supermassive black hole, 010308 nuclear & particles physics, Matter power spectrum, Spectral density, Astronomy and Astrophysics, early Universe, Space and Planetary Science, cosmology: observations, reionization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Primordial black hole production in the mass range $10-10^4 \,{\rm M_\odot}$ is motivated respectively by interpretations of the LIGO/Virgo observations of binary black hole mergers and by their ability to seed intermediate black holes which would account for the presence of supermassive black holes at very high redshift. Their existence would imply a boost in the primordial power spectrum if they were produced by overdensities reentering the horizon and collapsing after single-field inflation. This, together with their associated Poisson fluctuations would cause a boost in the matter power spectrum on small scales. In fact, any evidence of extra power above that of an almost scale-invariant primordial power spectrum on small scales would suggest a non-single-field slow-roll model of inflation, whether or not primordial black holes were produced. The extra power could become potentially observable in the 21cm power spectrum on scales around $k\sim0.1 - 50\,{\rm Mpc^{-1}}$ either with the new generation of filled low frequency interferometers. We explicitly include the contribution from primordial fluctuations in our prediction of the 21cm signal which has been previously neglected, by constructing primordial power spectra motivated by single-field models of inflation that would produce extra power on small scales. We find that depending on the mass and abundance of primordial black holes, it is important to include this contribution from the primordial fluctuations, so as not to underestimate the 21cm signal. Evidently our predictions of detectability, which lack any modelling of foregrounds, are unrealistic, but we hope that they will motivate improved cleaning algorithms that can enable us to access this intriguing corner of PBH-motivated parameter space., Comment: 14 pages, 9 figures
Published: 2021

45. Active gas features in three HSC-SSP CAMIRA clusters revealed by high angular resolution analysis of MUSTANG-2 SZE and XXL X-ray observations

Author: Vernesa Smolčić, Keiichi Umetsu, Fabio Gastaldello, Keigo Tanaka, Dominique Eckert, Elinor Medezinski, Cathy Horellou, Craig L. Sarazin, Atsushi Yoshida, Sara Stanchfield, Kotaro Kohno, John ZuHone, Tony Mroczkowski, Chong Yang, Brian Mason, Marguerite Pierre, Satoshi Miyazaki, Mark Birkinshaw, Hiroki Akamatsu, Masamune Oguri, Mauro Sereno, Tetsu Kitayama, Jonathan Sievers, Charles Romero, Ayaka Honda, I-Non Chiu, Atsushi J. Nishizawa, Ikuyuki Mitsuishi, Yen-Ting Lin, Florian Pacaud, Kai-Yang Lin, Nobuhiro Okabe, Mark J. Devlin, Simon Dicker, Naomi Ota, Ryoichi Yamamoto, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, gravitational lensing: weak, Supercluster, weak [gravitational lensing], 0103 physical sciences, Cluster (physics), clusters: general [galaxies], Angular resolution, Surface brightness, 010306 general physics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, galaxies: clusters: general, radio continuum: galaxies, X-rays: galaxies: clusters, Astrophysics - Cosmology and Nongalactic Astrophysics, Physics, Astronomy and Astrophysics, Galaxy, Redshift, Core (optical fiber), Space and Planetary Science, clusters: intracluster medium [galaxies], galaxies [dio continuum], galaxies: clusters [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present results from simultaneous modeling of high angular resolution GBT/MUSTANG-2 90 GHz Sunyaev-Zel'dovich effect (SZE) measurements and XMM-XXL X-ray images of three rich galaxy clusters selected from the HSC-SSP Survey. The combination of high angular resolution SZE and X-ray imaging enables a spatially resolved multi-component analysis, which is crucial to understand complex distributions of cluster gas properties. The targeted clusters have similar optical richnesses and redshifts, but exhibit different dynamical states in their member galaxy distributions: a single-peaked cluster, a double-peaked cluster, and a cluster belonging to a supercluster. A large-scale residual pattern in both regular Compton-parameter $y$ and X-ray surface brightness distributions is found in the single-peaked cluster, indicating a sloshing mode. The double-peaked cluster shows an X-ray remnant cool core between two SZE peaks associated with galaxy concentrations. The temperatures of the two peaks reach $\sim20-30$ keV in contrast to the cool core component of $\sim2$ keV, indicating a violent merger. The main SZE signal for the supercluster is elongated along a direction perpendicular to the major axis of the X-ray core, suggesting a minor merger before core passage. The $S_X$ and $y$ distributions are thus perturbed at some level, regardless of the optical properties. We find that the integrated Compton $y$ parameter and the temperature for the major merger are boosted from those expected by the weak-lensing mass and those for the other two clusters show no significant deviations, which is consistent with predictions of numerical simulations., Comment: 36 pages, 25 figures, 5 tables; accepted for the publication in MNRAS
Published: 2021

46. Multi-tasking the growth of cosmological structures

Author: Louis Perenon, Michelle Lochner, Matteo Martinelli, Chris Clarkson, Stéphane Ilić, Roy Maartens, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, and 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)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Structure (category theory), FOS: Physical sciences, Gaussian processes, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Root mean square, symbols.namesake, 0103 physical sciences, Growth of structures, Sensitivity (control systems), 010303 astronomy & astrophysics, Gaussian process, Physics, 010308 nuclear & particles physics, Contrast (statistics), Astronomy and Astrophysics, Galaxy, Space and Planetary Science, symbols, Focus (optics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Next-generation large-scale structure surveys will deliver a significant increase in the precision of growth data, allowing us to use `agnostic' methods to study the evolution of perturbations without the assumption of a cosmological model. We focus on a particular machine learning tool, Gaussian processes, to reconstruct the growth rate $f$, the root mean square of matter fluctuations $\sigma_8$, and their product $f\sigma_8$. We apply this method to simulated data, representing the precision of upcoming Stage IV galaxy surveys. We extend the standard single-task approach to a multi-task approach that reconstructs the three functions simultaneously, thereby taking into account their inter-dependence. We find that this multi-task approach outperforms the single-task approach for future surveys and will allow us to detect departures from the standard model with higher significance. By contrast, the limited sensitivity of current data severely hinders the use of agnostic methods, since the Gaussian processes parameters need to be fine tuned in order to obtain robust reconstructions., Comment: 14 pages; 7 figures; Significant improvements. Version accepted by Phys. Dark Universe
Published: 2021

47. The Cluster HEritage project with XMM-Newton: Mass Assembly and Thermodynamics at the Endpoint of structure formation. I. Programme overview

Author: Alina Streblyanska, Raphael Gavazzi, I. Bartalucci, Mathilde Jauzac, P. S. Corasaniti, Paolo Tozzi, R. F. J. van der Burg, Jack Sayers, Mario Nonino, Dominique Eckert, Franco Vazza, M. Rossetti, S. Molendi, Christine Jones, A. Saro, Stefano Ettori, E. Rasia, A. Ferragamo, Nicolas Clerc, Jean-Baptiste Melin, Jose Alberto Rubino-Martin, Barbara Sartoris, Nobuhiro Okabe, R. T. Duffy, A. Iqbal, Sandrine Pires, F. Andrade-Santos, S. De Grandi, Rossella Cassano, F. Gastaldello, G. Schellenberger, Gustavo Yepes, Annalisa Bonafede, R. Barrena, Mauro Sereno, M. De Petris, Keiichi Umetsu, Etienne Pointecouteau, Paula Tarrío, Hervé Bourdin, Jean-Charles Cuillandre, Klaus Dolag, Chris P. Haines, Pasquale Mazzotta, S. Zarattini, Mario Radovich, Stefano Borgani, L. Salvati, Tiziana Venturi, M. Arnaud, Florian Kéruzoré, Simona Ghizzardi, David J. Barnes, Megan Donahue, Massimo Gaspari, S. Paltani, G. W. Pratt, Myriam Gitti, A. M. C. LeBrun, L. Perotto, S. Burkutean, F. Mayet, Scott T. Kay, Melanie Johnston-Hollitt, Lorenzo Lovisari, Herve Aussel, S. Maurogordato, Ben J Maughan, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), 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), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), University of Geneva [Switzerland], INAF-IASF Milano, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), 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), Université de Genève = University of Geneva (UNIGE), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Arnaud, M., Ettori, S., Pratt, G. W., Rossetti, M., Eckert, D., Gastaldello, F., Gavazzi, R., Kay, S. T., Lovisari, L., Maughan, B. J., Pointecouteau, E., Sereno, M., Bartalucci, I., Bonafede, A., Bourdin, H., Cassano, R., Duffy, R. T., Iqbal, A., Maurogordato, S., Rasia, E., Sayers, J., Andrade-Santos, F., Aussel, H., Barnes, D. J., Barrena, R., Borgani, S., Burkutean, S., Clerc, N., Corasaniti, P. -S., Cuillandre, J. -C., De Grandi, S., De Petris, M., Dolag, K., Donahue, M., Ferragamo, A., Gaspari, M., Ghizzardi, S., Gitti, M., Haines, C. P., Jauzac, M., Johnston-Hollitt, M., Jones, C., Keruzore, F., Lebrun, A. M. C., Mayet, F., Mazzotta, P., Melin, J. -B., Molendi, S., Nonino, M., Okabe, N., Paltani, S., Perotto, L., Pires, S., Radovich, M., Rubino-Martin, J. -A., Salvati, L., Saro, A., Sartoris, B., Schellenberger, G., Streblyanska, A., Tarrio, P., Tozzi, P., Umetsu, K., Van Der Burg, R. F. J., Vazza, F., Venturi, T., Yepes, G., Zarattini, S., Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), UAM.Departamento de Física Teórica, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Arnaud M., Ettori S., Pratt G.W., Rossetti M., Eckert D., Gastaldello F., Gavazzi R., Kay S.T., Lovisari L., Maughan B.J., Pointecouteau E., Sereno M., Bartalucci I., Bonafede A., Bourdin H., Cassano R., Duffy R.T., Iqbal A., Maurogordato S., Rasia E., Sayers J., Andrade-Santos F., Aussel H., Barnes D.J., Barrena R., Borgani S., Burkutean S., Clerc N., Corasaniti P.-S., Cuillandre J.-C., De Grandi S., De Petris M., Dolag K., Donahue M., Ferragamo A., Gaspari M., Ghizzardi S., Gitti M., Haines C.P., Jauzac M., Johnston-Hollitt M., Jones C., Keruzore F., Lebrun A.M.C., Mayet F., Mazzotta P., Melin J.-B., Molendi S., Nonino M., Okabe N., Paltani S., Perotto L., Pires S., Radovich M., Rubino-Martin J.-A., Salvati L., Saro A., Sartoris B., Schellenberger G., Streblyanska A., Tarrio P., Tozzi P., Umetsu K., Van Der Burg R.F.J., Vazza F., Venturi T., Yepes G., and Zarattini S.
Subjects: Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Dark matter, Population, Thermodynamics, FOS: Physical sciences, observation [Cosmology], Astrophysics, clusters: intracluster medium [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cosmology: observation, 01 natural sciences, Observations [Cosmology], law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, law, 0103 physical sciences, Cluster (physics), Planck, education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Settore FIS/05, 010308 nuclear & particles physics, Cosmology: observations, Física, Galaxies: clusters: general, Galaxies: clusters: intracluster medium, Astronomy and Astrophysics, Astronomía, Dark matter halo, [SDU]Sciences of the Universe [physics], Space and Planetary Science, symbols, Hydrostatic equilibrium, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Cluster HEritage project with XMM-Newton - Mass Assembly and Thermodynamics at the Endpoint of structure formation (CHEX-MATE) is a three mega-second Multi-Year Heritage Programme to obtain X-ray observations of a minimally-biased, signal-to-noise limited sample of 118 galaxy clusters detected by Planck through the Sunyaev-Zeldovich effect. The programme, described in detail in this paper, aims to study the ultimate products of structure formation in time and mass. It is composed of a census of the most recent objects to have formed (Tier-1: 0.05 < z < 0.2; 2 x 10e14 M_sun < M_500 < 9 x 10e14 M_sun), together with a sample of the highest-mass objects in the Universe (Tier-2: z < 0.6; M_500 > 7.25 x 10e14 M_sun). The programme will yield an accurate vision of the statistical properties of the underlying population, measure how the gas properties are shaped by collapse into the dark matter halo, uncover the provenance of non-gravitational heating, and resolve the major uncertainties in mass determination that limit the use of clusters for cosmological parameter estimation. We will acquire X-ray exposures of uniform depth, designed to obtain individual mass measurements accurate to 15-20% under the hydrostatic assumption. We present the project motivations, describe the programme definition, and detail the ongoing multi-wavelength observational (lensing, SZ, radio) and theoretical effort that is being deployed in support of the project., 27 pages, 11 figures; A&A, in press
Published: 2021

48. Constraining cosmology with a new all-sky Compton parameter map from the Planck PR4 data

Author: Nabila Aghanim, Hideki Tanimura, L. Salvati, Marian Douspis, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, 01 natural sciences, Cosmology, law.invention, symbols.namesake, law, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, media_common, Physics, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, 16. Peace & justice, 13. Climate action, Space and Planetary Science, Sky, cosmology: observations, symbols, large-scale structure of Universe, Hydrostatic equilibrium, Multipole expansion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We constructed a new all-sky Compton parameter map (y-map) of the thermal Sunyaev-Zel'dovich (tSZ) effect from the 100 to 857 GHz frequency channel maps delivered within the Planck data release 4. The improvements in terms of noise and systematic effects translated into a y-map with a noise level smaller by ~7% compared to the maps released in 2015, and with significantly reduced survey stripes. The produced 2020 y-map is also characterized by residual foreground contamination, mainly due to thermal dust emission at large angular scales and to CIB and extragalactic point sources at small angular scales. Using the new Planck data, we computed the tSZ angular power spectrum and found that the tSZ signal dominates the y-map in the multipole range, 60 < l < 600. We performed the cosmological analysis with the tSZ angular power spectrum and found S8=0.764+0.015-0.018(stat)+0.031-0.016(sys), including systematic uncertainties from a hydrostatic mass bias and pressure profile model. The S8 value may differ by +-0.016 depending on the hydrostatic mass bias model and by +0.021 depending on the pressure profile model used for the analysis. The obtained value is fully consistent with recent KiDS and DES weak-lensing observations. While our result is slightly lower than the Planck CMB one, it is consistent with the latter within 2 sigma., 14 pages, 17 figures, Accepted for publication in MNRAS
Published: 2021

49. Power spectrum of halo intrinsic alignments in simulations

Author: Ken Osato, Takahiro Nishimichi, Toshiki Kurita, Masahiro Takada, Ryuichi Takahashi, Yosuke Kobayashi, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Matter power spectrum, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Spectral line, methods: numerical, Amplitude, gravitational lensing: weak, Space and Planetary Science, cosmology: theory, 0103 physical sciences, Halo, Baryon acoustic oscillations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use a suite of $N$-body simulations to study intrinsic alignments (IA) of halo shapes with the surrounding large-scale structure in the $\Lambda$CDM model. For this purpose, we develop a novel method to measure multipole moments of the three-dimensional power spectrum of the $E$-mode field of halo shapes with the matter/halo distribution, $P_{\delta E}^{(\ell)}(k)$ (or $P^{(\ell)}_{{\rm h}E}$), and those of the auto-power spectrum of the $E$ mode, $P^{(\ell)}_{EE}(k)$, based on the $E$/$B$-mode decomposition. The IA power spectra have non-vanishing amplitudes over the linear to nonlinear scales, and the large-scale amplitudes at $k\lesssim 0.1~h~{\rm Mpc}^{-1}$ are related to the matter power spectrum via a constant coefficient ($A_{\rm IA}$), similar to the linear bias parameter of galaxy or halo density field. We find that the cross- and auto-power spectra $P_{\delta E}$ and $P_{EE}$ at nonlinear scales, $k\gtrsim 0.1~h~{\rm Mpc}^{-1}$, show different $k$-dependences relative to the matter power spectrum, suggesting a violation of the nonlinear alignment model commonly used to model contaminations of cosmic shear signals. The IA power spectra exhibit baryon acoustic oscillations, and vary with halo samples of different masses, redshifts and cosmological parameters ($\Omega_{\rm m}, S_8$). The cumulative signal-to-noise ratio for the IA power spectra is about 60% of that for the halo density power spectrum, where the super-sample covariance is found to give a significant contribution to the total covariance. Thus our results demonstrate that the IA power spectra of galaxy shapes, measured from imaging and spectroscopic surveys for an overlapping area of the sky, can be used to probe the underlying matter power spectrum, the primordial curvature perturbations, and cosmological parameters, in addition to the standard galaxy density power spectrum., Comment: 20 pages, 21 figures; updated to reflect accepted version
Published: 2021

50. Illuminating the dark side of cosmic star formation two billion years after the Big Bang

Author: Andreas L. Faisst, Andrea Cimatti, Marika Giulietti, Vernesa Smolčić, Margherita Talia, Olivier Le Fevre, G. Zamorani, Matthieu Béthermin, 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), Talia M., Cimatti A., Giulietti M., Zamorani G., Bethermin M., Faisst A., Le F vre O., and Smol ic V.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Galaxy evolution, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysic, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Galaxy formation, High-redshift galaxies, Star formation, 594, 595, 734, 1569, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Physics, Astronomy, Astronomy and Astrophysics, Billion years, Redshift, Universe, Galaxy, High-redshift galaxie, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: How and when did galaxies form and assemble their stars and stellar mass? The answer to these questions, so crucial to astrophysics and cosmology, requires the full reconstruction of the so called cosmic star formation rate density (SFRD), i.e. the evolution of the average star formation rate per unit volume of the universe. While the SFRD has been reliably traced back to 10-11 billion years ago, its evolution is still poorly constrained at earlier cosmic epochs, and its estimate is mainly based on galaxies luminous in the ultraviolet and with low obscuration by dust. This limited knowledge is largely due to the lack of an unbiased census of all types of star-forming galaxies in the early universe. We present a new approach to find dust-obscured star-forming galaxies based on their emission at radio wavelengths coupled with the lack of optical counterparts. Here, we present a sample of 197 galaxies selected with this method. These systems were missed by previous surveys at optical and near-infrared wavelengths, and 22 of them are at very high redshift (i.e. z > 4.5). The contribution of these elusive systems to the SFRD is substantial and can be as high as 40% of the previously known SFRD based on UV-luminous galaxies. The mere existence of such heavily obscured galaxies in the first two billion years after the Big Bang opens new avenues to investigate the early phases of galaxy formation and evolution, and to understand the links between these systems and the massive galaxies which ceased their star formation at later cosmic times., 15 pages, 6 figures. Accepted for publication in ApJ. Corrected a typo in Table 3. Minor changes to match the accepted version
Published: 2021

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