The Distribution of Active Galactic Nuclei in a Large Sample of Galaxy Clusters
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Arxiv:1903.02002V1 [Astro-Ph.GA] 5 Mar 2019
Draft version March 7, 2019 Typeset using LATEX twocolumn style in AASTeX62 RELICS: Reionization Lensing Cluster Survey Dan Coe,1 Brett Salmon,1 Maruˇsa Bradacˇ,2 Larry D. Bradley,1 Keren Sharon,3 Adi Zitrin,4 Ana Acebron,4 Catherine Cerny,5 Nathalia´ Cibirka,4 Victoria Strait,2 Rachel Paterno-Mahler,3 Guillaume Mahler,3 Roberto J. Avila,1 Sara Ogaz,1 Kuang-Han Huang,2 Debora Pelliccia,2, 6 Daniel P. Stark,7 Ramesh Mainali,7 Pascal A. Oesch,8 Michele Trenti,9, 10 Daniela Carrasco,9 William A. Dawson,11 Steven A. Rodney,12 Louis-Gregory Strolger,1 Adam G. Riess,1 Christine Jones,13 Brenda L. Frye,7 Nicole G. Czakon,14 Keiichi Umetsu,14 Benedetta Vulcani,15 Or Graur,13, 16, 17 Saurabh W. Jha,18 Melissa L. Graham,19 Alberto Molino,20, 21 Mario Nonino,22 Jens Hjorth,23 Jonatan Selsing,24, 25 Lise Christensen,23 Shotaro Kikuchihara,26, 27 Masami Ouchi,26, 28 Masamune Oguri,29, 30, 28 Brian Welch,31 Brian C. Lemaux,2 Felipe Andrade-Santos,13 Austin T. Hoag,2 Traci L. Johnson,32 Avery Peterson,32 Matthew Past,32 Carter Fox,3 Irene Agulli,4 Rachael Livermore,9, 10 Russell E. Ryan,1 Daniel Lam,33 Irene Sendra-Server,34 Sune Toft,24, 25 Lorenzo Lovisari,13 and Yuanyuan Su13 1Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 2Department of Physics, University of California, Davis, CA 95616, USA 3Department of Astronomy, University of Michigan, 1085 South University Ave, Ann Arbor, MI 48109, USA 4Physics Department, Ben-Gurion University of the Negev, P.O. -
PUBLICATIONS Publications (As of Dec 2020): 335 on Refereed Journals, 90 Selected from Non-Refereed Journals. Citations From
PUBLICATIONS Publications (as of Sep 2021): 350 on refereed journals, 92 selected from non-refereed journals. Citations from ADS: 32263, H-index= 97. Refereed 350. Caminha, G.B.; Suyu, S.H.; Grillo, C.; Rosati, P.; et al. 2021 Galaxy cluster strong lensing cosmography: cosmological constraints from a sample of regular galaxy clusters, submitted to A&A 349. Mercurio, A..; Rosati, P., Biviano, A. et al. 2021 CLASH-VLT: Abell S1063. Cluster assembly history and spectroscopic catalogue, submitted to A&A, (arXiv:2109.03305) 348. G. Granata et al. (9 coauthors including P. Rosati) 2021 Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: the case of Abell S1063, submitted to A&A, (arXiv:2107.09079) 347. E. Vanzella et al. (19 coauthors including P. Rosati) 2021 High star cluster formation efficiency in the strongly lensed Sunburst Lyman-continuum galaxy at z = 2:37, submitted to A&A, (arXiv:2106.10280) 346. M.G. Paillalef et al. (9 coauthors including P. Rosati) 2021 Ionized gas kinematics of cluster AGN at z ∼ 0:8 with KMOS, MNRAS, 506, 385 6 crediti 345. M. Scalco et al. (12 coauthors including P. Rosati) 2021 The HST large programme on Centauri - IV. Catalogue of two external fields, MNRAS, 505, 3549 344. P. Rosati et al. 2021 Synergies of THESEUS with the large facilities of the 2030s and guest observer opportunities, Experimental Astronomy, 2021ExA...tmp...79R (arXiv:2104.09535) 343. N.R. Tanvir et al. (33 coauthors including P. Rosati) 2021 Exploration of the high-redshift universe enabled by THESEUS, Experimental Astronomy, 2021ExA...tmp...97T (arXiv:2104.09532) 342. -
Source-Plane Reconstruction of the Giant Gravitational Arc in A2667: a Candidate Wolf–Rayet Galaxy At
SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1 Shuo Cao, Giovanni Covone, Eric Jullo, Johan Richard, Luca Izzo, Zong-Hong Zhu To cite this version: Shuo Cao, Giovanni Covone, Eric Jullo, Johan Richard, Luca Izzo, et al.. SOURCE-PLANE RE- CONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF– RAYET GALAXY AT z ∼ 1. Astronomical Journal, American Astronomical Society, 2015, 149, pp.8. 10.1088/0004-6256/149/1/3. hal-01109685 HAL Id: hal-01109685 https://hal.archives-ouvertes.fr/hal-01109685 Submitted on 26 Jan 2015 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. The Astronomical Journal, 149:3 (8pp), 2015 January doi:10.1088/0004-6256/149/1/3 C 2015. The American Astronomical Society. All rights reserved. SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1 Shuo Cao1,2, Giovanni Covone2,3, Eric Jullo4, Johan Richard5, Luca Izzo6,7, and Zong-Hong Zhu1 1 Department of Astronomy, Beijing Normal University, 100875 Beijing, China; [email protected] 2 Dipartimento di Scienze Fisiche, Universita` di Napoli “Federico II,” Via Cinthia, I-80126 Napoli, Italy 3 INFN Sez. -
THE DISTRIBUTION of ACTIVE GALACTIC NUCLEI in CLUSTERS of GALAXIES ABSTRACT We Present a Study of the Distribution of AGN In
APJ ACCEPTED [18 APRIL 2007] Preprint typeset using LATEX style emulateapj v. 12/14/05 THE DISTRIBUTION OF ACTIVE GALACTIC NUCLEI IN CLUSTERS OF GALAXIES PAUL MARTINI Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, [email protected] JOHN S. MULCHAEY, DANIEL D. KELSON Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101-1292 ApJ accepted [18 April 2007] ABSTRACT We present a study of the distribution of AGN in clusters of galaxies with a uniformly selected, spectroscop- ically complete sample of 35 AGN in eight clusters of galaxies at z = 0:06 ! 0:31. We find that the 12 AGN 42 −1 with LX > 10 erg s in cluster members more luminous than a rest-frame MR < −20 mag are more centrally concentrated than typical cluster galaxies of this luminosity, although these AGN have comparable velocity and substructure distributions to other cluster members. In contrast, a larger sample of 30 cluster AGN with 41 −1 LX > 10 erg s do not show evidence for greater central concentration than inactive cluster members, nor evidence for a different kinematic or substructure distribution. As we do see clear differences in the spatial and kinematic distributions of the blue Butcher-Oemler and red cluster galaxy populations, any difference in the AGN and inactive galaxy population must be less distinct than that between these two pairs of popula- tions. Comparison of the AGN fraction selected via X-ray emission in this study to similarly-selected AGN in the field indicates that the AGN fraction is not significantly lower in clusters, contrary to AGN identified via visible-wavelength emission lines, but similar to the approximately constant radio-selected AGN fraction in clusters and the field. -
Imaging Non-Thermal X-Ray Emission from Galaxy Clusters: Results and Implications
Journal of The Korean Astronomical Society 37: 299 » 305, 2004 IMAGING NON-THERMAL X-RAY EMISSION FROM GALAXY CLUSTERS: RESULTS AND IMPLICATIONS Mark Henriksen and Danny Hudson Joint Center for Astrophysics, Physics Department, University of Maryland, Baltimore, MD 21250, USA E-mail: [email protected] ABSTRACT We ¯nd evidence of a hard X-ray excess above the thermal emission in two cool clusters (Abell 1750 and IC 1262) and a soft excess in two hot clusters (Abell 754 and Abell 2163). Our modeling shows that the excess components in Abell 1750, IC 1262, and Abell 2163 are best ¯t by a steep powerlaw indicative of a signi¯cant non-thermal component. In the case of Abell 754, the excess emission is thermal, 1 keV emission. We analyze the dynamical state of each cluster and ¯nd evidence of an ongoing or recent merger in all four clusters. In the case of Abell 2163, the detected, steep spectrum, non-thermal X-ray emission is shown to be associated with the weak merger shock seen in the temperature map. However, this shock is not able to produce the flatter spectrum radio halo which we attribute to post- shock turbulence. In Abell 1750 and IC 1262, the shocked gas appears to be spatially correlated with non-thermal emission suggesting cosmic-ray acceleration at the shock front. Key words : clusters of galaxies { inverse-Compton emission { mergers I. INTRODUCTION with energy. For example, the e®ective area of the Bep- poSax PDS (15 - 300 keV) is 10 times lower than the Inverse-Compton measurements for galaxy clusters RXTE PCA (2 - 60 Kev). -
INVESTIGATING ACTIVE GALACTIC NUCLEI with LOW FREQUENCY RADIO OBSERVATIONS By
INVESTIGATING ACTIVE GALACTIC NUCLEI WITH LOW FREQUENCY RADIO OBSERVATIONS by MATTHEW LAZELL A thesis submitted to The University of Birmingham for the degree of DOCTOR OF PHILOSOPHY School of Physics & Astronomy College of Engineering and Physical Sciences The University of Birmingham March 2015 University of Birmingham Research Archive e-theses repository This unpublished thesis/dissertation is copyright of the author and/or third parties. The intellectual property rights of the author or third parties in respect of this work are as defined by The Copyright Designs and Patents Act 1988 or as modified by any successor legislation. Any use made of information contained in this thesis/dissertation must be in accordance with that legislation and must be properly acknowledged. Further distribution or reproduction in any format is prohibited without the permission of the copyright holder. Abstract Low frequency radio astronomy allows us to look at some of the fainter and older synchrotron emission from the relativistic plasma associated with active galactic nuclei in galaxies and clusters. In this thesis, we use the Giant Metrewave Radio Telescope to explore the impact that active galactic nuclei have on their surroundings. We present deep, high quality, 150–610 MHz radio observations for a sample of fifteen predominantly cool-core galaxy clusters. We in- vestigate a selection of these in detail, uncovering interesting radio features and using our multi-frequency data to derive various radio properties. For well-known clusters such as MS0735, our low noise images enable us to see in improved detail the radio lobes working against the intracluster medium, whilst deriving the energies and timescales of this event. -
Revisiting the Cooling Flow Problem in Galaxies, Groups, and Clusters of Galaxies
Revisiting the Cooling Flow Problem in Galaxies, Groups, and Clusters of Galaxies The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation McDonald, Michael et. al., "Revisiting the Cooling Flow Problem in Galaxies, Groups, and Clusters of Galaxies." Astrophysical Journal 858, 1 (May 2018): no. 45 doi. 10.3847/1538-4357/AABACE ©2018 Authors As Published 10.3847/1538-4357/AABACE Publisher American Astronomical Society Version Final published version Citable link https://hdl.handle.net/1721.1/125311 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal, 858:45 (15pp), 2018 May 1 https://doi.org/10.3847/1538-4357/aabace © 2018. The American Astronomical Society. All rights reserved. Revisiting the Cooling Flow Problem in Galaxies, Groups, and Clusters of Galaxies M. McDonald1 , M. Gaspari2,5 , B. R. McNamara3 , and G. R. Tremblay4 1 Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA; [email protected] 2 Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544-1001, USA 3 Department of Physics & Astronomy, University of Waterloo, Canada 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA Received 2018 January 6; revised 2018 March 13; accepted 2018 March 27; published 2018 May 3 Abstract We present a study of 107 galaxies, groups, and clusters spanning ∼3 orders of magnitude in mass, ∼5 orders of magnitude in central galaxy star formation rate (SFR), ∼4 orders of magnitude in the classical cooling rate (MMrrt˙ coolº< gas() cool cool) of the intracluster medium (ICM), and ∼5 orders of magnitude in the central black hole accretion rate. -
Small-Scale Structure Is It a Valid Motivation?
Small-scale Structure Is it a valid motivation? Jakub Scholtz IPPP (Durham) Small Scale Structure Problems <—> All the reasons why “CDM is not it” How did we get here? We are gravitationally sensitive to something sourcing T • <latexit sha1_base64="055AcnSYYRkGsBe2aYAe7vH1peg=">AAAB8XicbVDLSgNBEOz1GeMr6tHLYBA8hV0R9Bj04jFCXphdwuxkNhkyM7vMQwhL/sKLB0W8+jfe/BsnyR40saChqOqmuyvOONPG97+9tfWNza3t0k55d2//4LBydNzWqVWEtkjKU9WNsaacSdoyzHDazRTFIua0E4/vZn7niSrNUtk0k4xGAg8lSxjBxkmPzX4eChtKO+1Xqn7NnwOtkqAgVSjQ6Fe+wkFKrKDSEI617gV+ZqIcK8MIp9NyaDXNMBnjIe05KrGgOsrnF0/RuVMGKEmVK2nQXP09kWOh9UTErlNgM9LL3kz8z+tZk9xEOZOZNVSSxaLEcmRSNHsfDZiixPCJI5go5m5FZIQVJsaFVHYhBMsvr5L2ZS3wa8HDVbV+W8RRglM4gwsI4BrqcA8NaAEBCc/wCm+e9l68d+9j0brmFTMn8Afe5w/beZEG</latexit> µ⌫ —> we are fairly certain that DM exists. • An exception is MOND, which has issues of its own. However, the MOND community has been instrumental in pointing out some of the discrepancies with CDM. • But how do we verify the picture? —> NBODY simulations (disclaimer: I have never run a serious body simulation) 2WalterDehnen,JustinI.Read:N-body SimulationsN-body simulations of gravitational dynamics have reached over 106 particles [6], while collisionless calculations can now reach more than 109 particles [7–10]. This disparity reflects the difference in complexity of these rather dissimilar N-body problems. The significant increase in N in the last decade was driven by the usage of parallel computers. In this review, we discuss the state-of-the art software algo- Takerithms N and dark hardware matter improvements -
The Luminosity Function of the Milky Way Satellites
Draft version June 3, 2018 A Preprint typeset using LTEX style emulateapj v. 02/07/07 THE LUMINOSITY FUNCTION OF THE MILKY WAY SATELLITES S. Koposov1,2, V. Belokurov2, N.W. Evans2, P.C. Hewett2, M.J. Irwin2, G. Gilmore2, D.B. Zucker2, H.-W. Rix1, M. Fellhauer2, E.F. Bell1, E.V. Glushkova3 Draft version June 3, 2018 ABSTRACT We quantify the detectability of stellar Milky Way satellites in the Sloan Digital Sky Survey (SDSS) Data Release 5. We show that the effective search volumes for the recently discovered SDSS–satellites depend strongly on their luminosity, with their maximum distance, Dmax, substantially smaller than the Milky Way halo’s virial radius. Calculating the maximum accessible volume, Vmax, for all faint detected satellites, allows the calculation of the luminosity function for Milky Way satellite galaxies, accounting quantitatively for their detectability. We find that the number density of satellite galaxies continues to rise towards low luminosities, but may flatten at MV 5; within the uncertainties, the ∼− 0.1(MV +5) luminosity function can be described by a single power law dN/dMV = 10 10 , spanning × luminosities from MV = 2 all the way to the luminosity of the Large Magellanic Cloud. Comparing these results to several semi-analytic− galaxy formation models, we find that their predictions differ significantly from the data: either the shape of the luminosity function, or the surface brightness distributions of the models, do not match. Subject headings: Galaxy: halo – Galaxy: structure – Galaxy: formation – Local Group 1. INTRODUCTION ing satellite” problem. First identified by Klypin et al. In Cold Dark Matter (CDM) models, large spiral (1999) and Moore et al. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
Radial Temperature Profiles for a Large Sample of Galaxy Clusters Observed with XMM-Newton
A&A 486, 359–373 (2008) Astronomy DOI: 10.1051/0004-6361:200809538 & c ESO 2008 Astrophysics Radial temperature profiles for a large sample of galaxy clusters observed with XMM-Newton A. Leccardi1,2 and S. Molendi2 1 Università degli Studi di Milano, Dip. di Fisica, via Celoria 16, 20133 Milano, Italy 2 INAF-IASF Milano, via Bassini 15, 20133 Milano, Italy e-mail: [email protected] Received 8 February 2008 / Accepted 8 April 2008 ABSTRACT Aims. We measure radial temperature profiles as far out as possible for a sample of ≈50 hot, intermediate redshift galaxy clusters, selected from the XMM-Newton archive, keeping systematic errors under control. Methods. Our work is characterized by two major improvements. First, we used background modeling, rather than background subtraction, and the Cash statistic rather than the χ2. This method requires a careful characterization of all background components. Second, we assessed systematic effects in detail. We performed two groups of tests. Prior to the analysis, we made use of extensive simulations to quantify the impact of different spectral components on simulated spectra. After the analysis, we investigated how the measured temperature profile changes, when choosing different key parameters. Results. The mean temperature profile declines beyond 0.2 R180. For the first time, we provide an assessment of the source and the magnitude of systematic uncertainties. When comparing our profile with those obtained from hydrodynamic simulations, we find the slopes beyond ≈0.2 R180 to be similar. Our mean profile is similar but somewhat flatter with respect to those obtained by previous observational works, possibly as a consequence of a different level of characterizing systematic effects. -
Hst Frontier Fields Preliminary Map Modeling
HST FRONTIER FIELDS PRELIMINARY MAP MODELING CATs Team (Clusters As Telescopes) Johan Richard (CRAL Lyon), Benjamin Clement (University of Arizona), Mathilde Jauzac (University of KwaZulu-Natal), Eric Jullo (LAM Marseille), Marceau Limousin (LAM, Marseille), Harald Ebeling (IfA, Hawaii), Priyamvada Natarajan (Yale University), Jean-Paul Kneib (EPFL Lausanne) & Eiichi Egami (University of Arizona). RECONSTRUCTION METHODOLOGY Producing a magnification map involves solving the lens equation for light rays originating from distant sources and deflected by the massive foreground cluster. This is ultimately an inversion problem for which several sets of codes and approaches have been developed independently (see recent review by Kneib & Natarajan 2010). Our collaboration uses LENSTOOL1, an algorithm developed collectively by us over the years. LENSTOOL is a hybrid code that combines observational strong- and weak-lensing data to constrain the cluster mass model. The total mass distribution of clusters is assumed to consist of several smooth, large-scale potentials that are modeled either in a parametric form or non-parametrically, along with contributions from many (typically N > 50) individual cluster galaxies that are modeled using physically motivated parametric forms. For lensing clusters a multi-scale approach is optimal, in as much as the constraints resulting from this inversion exercise are derived from a range of scales. Further details of the methodology are outlined in Jullo & Kneib (2009) and have been extended to the weak-lensing regime (Jauzac et al. 2012). At present, the prevailing modeling approach is to assign a small-scale dark-matter clump to each major cluster galaxy and a large-scale dark-matter clump to prominent concentrations of cluster galaxies (Natarajan & Kneib 1997).