DOCSLIB.ORG

Galaxy Clusters

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Galaxy Clusters Dark Energy: Galaxy Clusters Adam Mantz (KIPAC/Stanford) SLAC Summer Institute August 22, 2017 Zwicky measured the velocities of galaxies in the Coma cluster, and concluded that its mass was much greater than the galaxies themselves could account for. Chapter I: background Clusters have provided key insights since the early days of cosmology 1915 General Relativity The Universe could be dynamic! 1929 Hubble Law The Universe is dynamic! 1933 Dark matter Clusters contain dark matter?! Chapter I: background Clusters have provided key insights since the early days of cosmology 1915 General Relativity The Universe could be dynamic! 1929 Hubble Law The Universe is dynamic! 1933 Dark matter Clusters contain dark matter?! Zwicky measured the velocities of galaxies in the Coma cluster, and concluded that its mass was much greater than the galaxies themselves could account for. I A very massive, bound collection of dark matter, gas, and galaxies I The real-universe analog of the most massive \halos" to form > 14 > M ∼ 10 M , kT ∼ 1 keV Galaxy clusters: an introduction Galaxy cluster (n): I A bunch of galaxies physically near to one another I The real-universe analog of the most massive \halos" to form > 14 > M ∼ 10 M , kT ∼ 1 keV Galaxy clusters: a delicious introduction Galaxy cluster (n): I A bunch of galaxies physically near to one another I A very massive, bound collection of dark matter, gas, and galaxies > 14 > M ∼ 10 M , kT ∼ 1 keV Galaxy clusters: a delicious introduction Galaxy cluster (n): I A bunch of galaxies physically near to one another I A very massive, bound collection of dark matter, gas, and galaxies I The real-universe analog of the most massive \halos" to form Galaxy clusters: a delicious introduction Galaxy cluster (n): I A bunch of galaxies physically near to one another I A very massive, bound collection of dark matter, gas, and galaxies I The real-universe analog of the most massive \halos" to form > 14 > M ∼ 10 M , kT ∼ 1 keV Galaxy clusters at X-ray wavelengths I (Mostly) thermal emission from the dominant baryonic component (intra-cluster medium). I Primary observables (density, temperature) carry information about the ICM thermodynamic state and the overall gravitational potential. Galaxy clusters at mm wavelengths I Sunyaev-Zel'dovich (SZ) effect: distortion of the CMB blackbody spectrum due to the ICM. I Primary observable (∆T ) is related to the ICM pressure. I Signal is less radius- and redshift-dependent that X-rays. Galaxy clusters at optical/IR wavelengths I Cluster galaxies: approximately collisionless test particles orbiting in the gravitational potential. I Background galaxies: gravitationally lensed by the cluster. Clusters mass estimation It's useful to distinguish between absolute (average) and relative mass estimation: I Absolute masses are best probed by weak lensing, which is not sensitive to gas astrophysics. However, individual cluster masses from lensing are inherently noisy. I Relative masses can be obtained from various other observables that have a smaller per-cluster scatter with true mass, but may have an overall bias. Galaxy cluster surveys Surveys using each observational window probe complementary parts of the population I X-ray and SZ: high purity for the most massive clusters I Optical/IR: high completeness ROSAT All-Sky Survey (RASS) { X-ray down to lower mass, but more complex selection 25 30 0.30 35 ] 0.25 2 n 40 i m c r DEC 0.20 45 a [ g n 50 0.15 0.10 120 100 320 300 RA South Pole Telescope (SPT)-SZ { 3mm Dark Energy Survey red galaxy density Galaxy cluster surveys Surveys using each observational ● ● ● window probe complementary parts ● ● ● 20 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ●●● ● ● ● ● ● ●● ● of the population ● ●● ●● ●● ● ● ● ) ● ● ● ● ●●● ● ● ●● ● ● ● ● ● ● ● ● ● ● ● ●●●●●●●●● ● ● ● ● ● ● ● ● ● ●●● ●● ● ●● ● ●●● ●● ● ● 10 ●●●●●●● ● ● ● ●● ● ●●●● ● ● ● ● ● ● ● ● ● ●● ●● ●●● ● ● ●● M ● ●●● ●●● ●● ● ●●●●● ● ●● ●● ● ● ●● ●●● ● ●●●● ●●●● ● ●●● ● ●●●● ●●●●●●● ●● ● ●● ●●●● ●●●●● ●●● X-ray and SZ: high purity for ● ● ● ● I ● ● ● ● ●● ● 14 ● ●●●●● ●●●● ● ●● ●●● ●●● ●●●● ●●● ●●●● ● ●●●● ●●●●●●●●●● ●●●● ●● ●●●● ●●●● ●●● ●● 5 ●●●●● ● ● ●● ●●●● 10 ● ● ● ● ●●●●●●●●●●●● ● ● ●●● ( ● ●●● ●●●●●●●●●●●● ●● the most massive clusters ●●● ● ●● ●●●●●●●●●●● ●●● ●●●●●●● ●●●●●●●●●● ●●●●●● ●●●●●●●●● 500 ● ● ●● ●●●●●●●●●●● ●●●●●● ●●●●●●● ●●●●●●● M ● ●●●● ● ●●●●●●●● 2 ●●●●●●● Optical/IR: high completeness ●●● I ●●●●●●● ●●●● ●●●●●● ● ● ●●●●●●●● ●●●●● RASS ●●●● ●● ●● ●●●●● SPT−SZ down to lower mass, but more ●●●●● 1 ●●● ● ●●● ●●●●● DES ●●● ●●●● ●●● ●●● complex selection ●● ●●●● ● ●●●● ●●● 0.5 ● ●●● ●● ●●● ●● ● 0.0● 0.5 1.0 1.5 2.0 3.0 ●● ●● ● redshift But we can do better that this: for massive clusters, excluding their cores, we can reliably predict the depletion of hot gas M =M Υ = gas tot : Ωb=Ωm For massive and dynamically relaxed clusters, we can reliably measure Mgas fgas = : Mtot Chapter II: Cosmology from cluster composition To zeroth order, the ratio of baryon to total mass in clusters should be identical to Ωb=Ωm. For massive and dynamically relaxed clusters, we can reliably measure Mgas fgas = : Mtot Chapter II: Cosmology from cluster composition To zeroth order, the ratio of baryon to total mass in clusters should be identical to Ωb=Ωm. But we can do better that this: for massive clusters, excluding their cores, we can reliably predict the depletion of hot gas M =M Υ = gas tot : Ωb=Ωm Chapter II: Cosmology from cluster composition To zeroth order, the ratio of baryon to total mass in clusters should be identical to Ωb=Ωm. But we can do better that this: for massive clusters, excluding their cores, we can reliably predict the depletion of hot gas M =M Υ = gas tot : Ωb=Ωm For massive and dynamically relaxed clusters, we can reliably measure Mgas fgas = : Mtot Cluster composition as a cosmic standard These properties make fgas a useful standard, an intrinsic property 0.90 Battaglia et al. 2013 14 15 3.1 × 10 M < M200 < 1 × 10 M 1. that can be predicted 2. that has a small scatter ) 0.80 500 r ● < ● ● ● 3. whose measurement depends on ( ● s a g ϒ distance 0.70 Observations of fgas depend on both 0.60 dL(z) and dA(z) { a combined 0.0 0.2 0.4 0.6 0.8 1.0 redshift candle and ruler. ! 5% precision in d(z) to a cluster Ingredients for cosmology from cluster composition 1. A sample of massive, relaxed clusters (surveys + X-ray follow-up) 2. Measurements of fgas (X-ray) 3. Calibration of total mass measurements (weak lensing) Ingredients for cosmology from cluster composition 1. A sample of massive, relaxed clusters (surveys + X-ray follow-up) 2. Measurements of fgas (X-ray) 3. Calibration of total mass measurements (weak lensing) A1835 A2163 ● ● ● ● ● ● ● ● 1 ● A1835 ● ● ● ● ● ●● ● ● ● ) ● ● ●● S 1 A2163 ● ●● f ● − ● ● ● ● ( ● ● ● ● ● ● ● ●● ● ● ● ● ● ● ● ● ● ● ● ●●●●● ● ● ●●●●● ● ● ● ●●●●●● ● 10 ● ●●● ● ●●●●●● ● s ● ●●●● ●● ●●●●●● ●● ●●●●●● ●●● s ●●● ●● ●● ●●●●● ●●●● ●●● ● ●●● e ●● ●●● ●●● ●● ●●●● ●●● ●●●●● ●●● n ●●● ●●● ● ●●● t ● ●●● 2 ●● ●●● ●●● ● ●● ●● ●●●●● − ●●●● ●●●● h ●●● ●● ●●●●●●● ●●● ●●● ●●● ●●●●●● ● ● ●● ● g ●● ●● ●● ● ● ● ● i ●● ●●●● ● ●●●● 10 ●● ● r ● ●●● ●● ●● ●●● ●●● ●●●●● ●● ●●●● b ● ● ●● ● ●●●●● ●●● ●●●● ● ● ●● ●●●● ●●● ●●● ● ●●● e ● ●●● ●●● ●●●● ● ●● c ●● ● ● 3 ● ●● ● ● a − ● ● f ● ● r ● ● 10 u ● ● s ● ● ● 4 ● − 10 1 3 10 30 100 300 radius (arcsec) Ingredients for cosmology from cluster composition Abell 20291. A sampleAbell 478 ofRX J1524.2−3154 massive,PKS relaxed 0745−191 clustersAbell 2204 (surveysRX J0439.0+0520 + X-rayZwicky 2701 RX J1504.1−0248 follow-up) 2. Measurements of fgas (X-ray) Zwicky 2089 RX J2129.6+0005 RX J1459.4−1811 Abell 1835 Abell 3444 MS 2137.3−2353 MACS J0242.5−2132 MACS J1427.6−2521 3. Calibration of total mass measurements (weak lensing) MACS J2229.7−2755 MACS J0947.2+7623 MACS J1931.8−2634 MACS J1115.8+0129 MACS J1532.8+3021 MACS J0150.3−1005 MACS J0011.7−1523 MACS J1720.2+3536 MACS J0429.6−0253 MACS J0159.8−0849 MACS J2046.0−3430 IRAS 09104+4109 MACS J1359.1−1929 RX J1347.5−1145 3C 295 MACS J1621.3+3810 MACS J1427.2+4407 MACS J1423.8+2404 SPT−CL J2331−5051 SPT−CL J2344−4242 SPT−CL J0000−5748 SPT−CL J2043−5035 CL J1415+3612 3C 186 Ingredients for cosmology from cluster composition 1. A sample of massive, relaxed clusters (surveys + X-ray follow-up) 2. Measurements of fgas (X-ray) 3. Calibration of total mass measurements (weak lensing) 0.5 0.5 0.2 0.2 ) ) ∆ ∆ r r ( ( s s a a g g f f 0.1 0.1 0.05 0.05 500 500 2500 2500 105 104 103 102 105 104 103 102 ∆ ∆ Ingredients for cosmology from cluster composition 1. A sample of massive, relaxed clusters (surveys + X-ray follow-up) 2. Measurements of fgas (X-ray) 3. Calibration of total mass measurements (weak lensing) Constraints from cluster fgas With priors on ΛCDM 2 OCDM 1. Ωbh (important) 0.18 w = − 3 ● ) 2. h (less important), ● ● 1.2 ● < ● ● ● ● ● ● ● the low-z data constrain Ωm: ● 0.14 ● ● ● ● 2500 ● ● r ● ● ● ● ● ● r ● ● ● ●● ● < Ω ● b ● 3=2 ● ● < ● fgas(z ∼ 0:15) / h 0.8 ● ● ● ( Ω 0.10 ● m s a g f 0.06 Apparent evolution constrains dark energy: 0.0 0.2 0.4 0.6 0.8 1.0 redshift −3=2 fgas(z) / d(z) Constraints from cluster fgas non-flat ΛCDM flat, constant-w 1.5 0.0 ●● fgas 1.0 ●● CMB −1.0 ●● SNIa ● Λ ● BAO w Ω ●● Combined 0.5 ●● fgas ●● CMB −2.0 ●● SNIa ●● BAO 0.0 ●● Combined −3.0 0.0 0.2 0.4 0.6 0.8 0.0 0.2 0.4 0.6 0.8 Ω m Ωm • Cluster fgas • Union 2.1 SNIa • WMAP CMB • 6df/SDSS/BOSS BAO Chapter III: Cosmology from cluster counts The number of clusters as a function of mass and redshift (columns) is a sensitive probe of cosmological models (rows). (Millenium Simulation/Virgo Consortium) Chapter III: Cosmology
Load more

Recommended publications
  • Clusters of Galaxies…
    Budapest University, MTA-Eötvös François Mernier …and the surprisesoftheir spectacularhotatmospheres Clusters ofgalaxies… K complex ) ⇤ Fe ) α [email protected] - Wallon Super - Wallon [email protected] Fe XXVI (Ly (/ Fe XXIV) L complex ) ) (incl. Ne) α α ) Fe ) ) α ) α α ) ) ) ) α ⇥ ) ) ) α α α α α α Si XIV (Ly Mg XII (Ly Ni XXVII / XXVIII Fe XXV (He S XVI (Ly O VIII (Ly Si XIII (He S XV (He Ca XIX (He Ca XX (Ly Fe XXV (He Cr XXIII (He Ar XVII (He Ar XVIII (Ly Mn XXIV (He Ca XIX / XX Yo u are h ere ! 1 km = 103 m Yo u are h ere ! (somewhere behind…) 107 m Yo u are h ere ! (and this is the Moon) 109 m ≃3.3 light seconds Yo u are h ere ! 1012 m ≃55.5 light minutes 1013 m 1014 m Yo u are h ere ! ≃4 light days 1013 m Yo u are h ere ! 1014 m 1017 m ≃10.6 light years 1021 m Yo u are h ere ! ≃106 000 light years 1 million ly Yo u are h ere ! The Local Group Andromeda (M31) 1 million ly Yo u are h ere ! The Local Group Triangulum (M33) 1 million ly Yo u are h ere ! The Local Group 10 millions ly The Virgo Supercluster Virgo cluster 10 millions ly The Virgo Supercluster M87 Virgo cluster 10 millions ly The Virgo Supercluster 2dFGRS Survey The large scale structure of the universe Abell 2199 (429 000 000 light years) Abell 2029 (1.1 billion light years) Abell 2029 (1.1 billion light years) Abell 1689 Abell 1689 (2.2 billion light years) Les amas de galaxies 53 Light emits at optical “colors”… …but also in infrared, radio, …and X-ray! Light emits at optical “colors”… …but also in infrared, radio, …and X-ray! Light emits at optical “colors”…
    [Show full text]
  • THE MASSIVELY ACCRETING CLUSTER A2029 Group Matches the Peak of the Photometric Galaxy Den- Sity Map
    Last updated:August 3, 2018 A Preprint typeset using LTEX style emulateapj v. 12/16/11 THE MASSIVELY ACCRETING CLUSTER A2029 Jubee Sohn1, Margaret J. Geller1, Stephen A. Walker2, Ian Dell’Antonio3, Antonaldo Diaferio4,5, Kenneth J. Rines6 1 Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA 2 Astrophysics Science Division, X-ray Astrophysics Laboratory, Code 662, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 3 Department of Physics, Brown University, Box 1843, Providence, RI 02912, USA 4 Universit`adi Torino, Dipartimento di Fisica, Torino, Italy 5 Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Torino, Torino, Italy and 6 Department of Physics and Astronomy, Western Washington University, Bellingham, WA 98225, USA Last updated:August 3, 2018 ABSTRACT We explore the structure of galaxy cluster Abell 2029 and its surroundings based on intensive spec- troscopy along with X-ray and weak lensing observations. The redshift survey includes 4376 galaxies (1215 spectroscopic cluster members) within 40′of the cluster center; the redshifts are included here. Two subsystems, A2033 and a Southern Infalling Group (SIG) appear in the infall region based on the spectroscopy as well as on the weak lensing and X-ray maps. The complete redshift survey of A2029 also identifies at least 12 foreground and background systems (10 are extended X-ray sources) in the A2029 field; we include a census of their properties. The X-ray luminosities (LX ) – velocity dispersions (σcl) scaling relations for A2029, A2033, SIG, and the foreground/background systems are consistent with the known cluster scaling relations. The combined spectroscopy, weak lensing, and X-ray observations provide a robust measure of the masses of A2029, A2033, and SIG.
    [Show full text]
  • Physical Properties of the X-Ray Gas As a Dynamical Diagnosis for Galaxy
    MNRAS 000, 1–24 (2019) Preprint 7 February 2019 Compiled using MNRAS LATEX style file v3.0 Physical properties of the X-ray gas as a dynamical diagnosis for galaxy clusters T. F. Lagan´a,1⋆ F. Durret2 and P. A. A. Lopes3 1NAT, Universidade Cruzeiro do Sul, Rua Galv˜ao Bueno, 868, CEP:01506-000, S˜ao Paulo-SP, Brazil 2 Sorbonne Universit´e, CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis Bd Arago, F-75014 Paris, France. 3 Observat´orio do Valongo, Universidade Federal do Rio de Janeiro, Ladeira do Pedro Antˆonio 43, Rio de Janeiro, RJ, 20080-090, Brazil Accepted 2018 December 19. Received 2018 December 17; in original form 2018 November 29. ABSTRACT We analysed XMM-Newton EPIC data for 53 galaxy clusters. Through 2D spec- tral maps, we provide the most detailed and extended view of the spatial distribution of temperature (kT), pressure (P), entropy (S) and metallicity (Z) of galaxy clusters to date with the aim of correlating the dynamical state of the system to six cool-core diagnoses from the literature. With the objective of building 2D maps and resolving structures in kT, P, S and Z, we divide the data in small regions from which spectra can be extracted. Our analysis shows that when clusters are spherically symmetric the cool-cores (CC) are preserved, the systems are relaxed with little signs of perturbation, and most of the CC criteria agree. The disturbed clusters are elongated, show clear signs of interaction in the 2D maps, and most do not have a cool-core.
    [Show full text]
  • Observational Cosmology - 30H Course 218.163.109.230 Et Al
    Observational cosmology - 30h course 218.163.109.230 et al. (2004–2014) PDF generated using the open source mwlib toolkit. See http://code.pediapress.com/ for more information. PDF generated at: Thu, 31 Oct 2013 03:42:03 UTC Contents Articles Observational cosmology 1 Observations: expansion, nucleosynthesis, CMB 5 Redshift 5 Hubble's law 19 Metric expansion of space 29 Big Bang nucleosynthesis 41 Cosmic microwave background 47 Hot big bang model 58 Friedmann equations 58 Friedmann–Lemaître–Robertson–Walker metric 62 Distance measures (cosmology) 68 Observations: up to 10 Gpc/h 71 Observable universe 71 Structure formation 82 Galaxy formation and evolution 88 Quasar 93 Active galactic nucleus 99 Galaxy filament 106 Phenomenological model: LambdaCDM + MOND 111 Lambda-CDM model 111 Inflation (cosmology) 116 Modified Newtonian dynamics 129 Towards a physical model 137 Shape of the universe 137 Inhomogeneous cosmology 143 Back-reaction 144 References Article Sources and Contributors 145 Image Sources, Licenses and Contributors 148 Article Licenses License 150 Observational cosmology 1 Observational cosmology Observational cosmology is the study of the structure, the evolution and the origin of the universe through observation, using instruments such as telescopes and cosmic ray detectors. Early observations The science of physical cosmology as it is practiced today had its subject material defined in the years following the Shapley-Curtis debate when it was determined that the universe had a larger scale than the Milky Way galaxy. This was precipitated by observations that established the size and the dynamics of the cosmos that could be explained by Einstein's General Theory of Relativity.
    [Show full text]
  • A Catalogue of Radio Sources at 151.5 Mhz
    Appendix B A catalogue of radio sources at 151.5 MHz 547 Appendix B. A catalogue of radio sources at 151.5 MHz 548 In this Appendix, we present a source list extracted from the deconvolved images pre- sented in this thesis. The source extraction and catalogue construction was carried out by the algorithm discussed in Sec. 7.3 for sources having peak detection threshold higher than 5σ. The reliability of all sources presented here has been confirmed by visual inspection. Details of sky coverage, accuracy of flux densities and positions are discussed in Sec. 7.3.2. Catalogue Format : The catalogue is organized in order of increasing RA and declination. The various columns of the catalogue are : Column 1 : This follows the IAU convention of naming sources. Jhhmm-ddmm(J2000). As a prefix to the name we use MRT for the name of the survey. Column 2 : RA position of the source (J2000). Column 3 : Declination position of the source (J2000). 1 Column 4 : Flux density of the source in Jy beam− . In case the source is extended, inte- grated flux density is given. Column 5 : The ratio of flux density estimate to the χ value obtained during fitting. This is a confidence level estimate of the least square fit. It is different from the signal to noise ratio in the sense that the value of χ depends not only on the local noise but also on the presence of other sources, sidelobes, large scale structures in the neighbourhood. Column 6 : Sources which are well extended are marked as E.
    [Show full text]
  • SRG/ART-XC All-Sky X-Ray Survey: Catalog of Sources Detected During the first Year M
    Astronomy & Astrophysics manuscript no. art_allsky ©ESO 2021 July 14, 2021 SRG/ART-XC all-sky X-ray survey: catalog of sources detected during the first year M. Pavlinsky1, S. Sazonov1?, R. Burenin1, E. Filippova1, R. Krivonos1, V. Arefiev1, M. Buntov1, C.-T. Chen2, S. Ehlert3, I. Lapshov1, V. Levin1, A. Lutovinov1, A. Lyapin1, I. Mereminskiy1, S. Molkov1, B. D. Ramsey3, A. Semena1, N. Semena1, A. Shtykovsky1, R. Sunyaev1, A. Tkachenko1, D. A. Swartz2, and A. Vikhlinin1, 4 1 Space Research Institute, 84/32 Profsouznaya str., Moscow 117997, Russian Federation 2 Universities Space Research Association, Huntsville, AL 35805, USA 3 NASA/Marshall Space Flight Center, Huntsville, AL 35812 USA 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA July 14, 2021 ABSTRACT We present a first catalog of sources detected by the Mikhail Pavlinsky ART-XC telescope aboard the SRG observatory in the 4–12 keV energy band during its on-going all-sky survey. The catalog comprises 867 sources detected on the combined map of the first two 6-month scans of the sky (Dec. 2019 – Dec. 2020) – ART-XC sky surveys 1 and 2, or ARTSS12. The achieved sensitivity to point sources varies between ∼ 5 × 10−12 erg s−1 cm−2 near the Ecliptic plane and better than 10−12 erg s−1 cm−2 (4–12 keV) near the Ecliptic poles, and the typical localization accuracy is ∼ 1500. Among the 750 sources of known or suspected origin in the catalog, 56% are extragalactic (mostly active galactic nuclei (AGN) and clusters of galaxies) and the rest are Galactic (mostly cataclysmic variables (CVs) and low- and high-mass X-ray binaries).
    [Show full text]
  • 2018 CFHT Annual Report
    2018 CFHT Annual Report Table of Contents Director’s Message……………………………………………………………………………………………... 3 Science Report ………………………………………………........................................................ 5 A PRISTINE Star..........................................................…………………..…………………… 5 Is ‘Oumuamua Really a Comet?........................................…………………………………. 6 Revealing the Complexity of the Nebula in NGC 1275 with SITELLE.............……. 8 Widespread Galactic Cannibalism in Stephan's Quintet Revealed by CFHT........ 9 Finding Extragalactic Supermassive Black Holes .........……………………………….……. 10 Astronomers Find a Famous Exoplanet's Doppelgänger .........................………... 13 Engineering Report ………..………………………………….……………………………………….……… 15 SITELLE Debugging and Performance..…………………………………..…......................... 15 SPIRou Technical Commissioning…………………………………………………………….......... 16 SITELLE Status………………………………………………………………………………………………….. 13 MegaCam Performance Improvements….…………………………….……………………….… 18 Other Technical Activities............….…………………………………………………………….… 20 MSE Report ……………………………………………………………………………………………………..…. 26 Partnership and Governance……………………………………………………………………………. 26 Science…………………………………………………………………………………………………………….. 27 Project Office Activity.........................………………………………………………………………. 29 Strategy Going Forward...............................……………………………………………………… 30 Administration Report............................……………………….………………………………..…. 31 Overview ………..……………………………….………………………………………………………….…… 31 Summary of
    [Show full text]
  • X-Ray Properties of the Northern Galactic Cap Agns in the 58-Month
    Accepted for publication in ApJ Preprint typeset using LATEX style emulateapj v. 08/22/09 X-RAY PROPERTIES OF THE NORTHERN GALACTIC CAP SOURCES IN THE 58-MONTH SWIFT-BAT CATALOG Ranjan V. Vasudevan1,*, William N. Brandt2,3, Richard F. Mushotzky1, Lisa M. Winter4, Wayne H. Baumgartner5, Thomas T. Shimizu1, Donald. P. Schneider2,3, John Nousek2 Accepted for publication in ApJ ABSTRACT We present a detailed X-ray spectral analysis of a complete sample of hard X-ray selected AGN in the Northern Galactic Cap of the 58-month Swift Burst Alert Telescope (Swift/BAT) catalog, consisting of 100 AGN with b > 50◦. This sky area has excellent potential for further dedicated study due to a wide range of multi-wavelength data that are already available, and we propose it as a low-redshift analog to the ‘deep field’ observations of AGN at higher redshifts (e.g. CDFN/S, COSMOS, Lockman Hole). We present distributions of luminosity, absorbing column density, and other key quantities for the catalog. We use a consistent approach to fit new and archival X-ray data gathered from XMM-Newton, Swift/XRT, ASCA and Swift/BAT. We probe to deeper redshifts than the 9-month BAT catalog (hzi =0.043 compared to hzi =0.03 for the 9-month catalog), and uncover a broader absorbing column density distribution. The fraction of obscured (logNH ≥ 22) objects in the sample is ∼ 60%, and 43–56% of the sample exhibits ‘complex’ 0.4–10 keV spectra. We present the properties of iron lines, soft excesses and ionized absorbers for the subset of ob- jects with sufficient signal-to-noise ratio.
    [Show full text]
  • The 22 Month Swift-Bat All-Sky Hard X-Ray Survey
    The Astrophysical Journal Supplement Series, 186:378–405, 2010 February doi:10.1088/0067-0049/186/2/378 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE 22 MONTH SWIFT-BAT ALL-SKY HARD X-RAY SURVEY J. Tueller1, W. H. Baumgartner1,2,3, C. B. Markwardt1,3,4,G.K.Skinner1,3,4, R. F. Mushotzky1, M. Ajello5, S. Barthelmy1, A. Beardmore6, W. N. Brandt7, D. Burrows7, G. Chincarini8, S. Campana8, J. Cummings1, G. Cusumano9, P. Evans6, E. Fenimore10, N. Gehrels1, O. Godet6,D.Grupe7, S. Holland1,3,J.Kennea7,H.A.Krimm1,3,M.Koss1,3,4, A. Moretti8, K. Mukai1,2,3, J. P. Osborne6, T. Okajima1,11, C. Pagani7, K. Page6, D. Palmer10, A. Parsons1, D. P. Schneider7, T. Sakamoto1,12, R. Sambruna1, G. Sato13, M. Stamatikos1,12, M. Stroh7, T. Ukwata1,14, and L. Winter15 1 NASA/Goddard Space Flight Center, Astrophysics Science Division, Greenbelt, MD 20771, USA; [email protected] 2 Joint Center for Astrophysics, University of Maryland-Baltimore County, Baltimore, MD 21250, USA 3 CRESST/ Center for Research and Exploration in Space Science and Technology, 10211 Wincopin Circle, Suite 500, Columbia, MD 21044, USA 4 Department of Astronomy, University of Maryland College Park, College Park, MD 20742, USA 5 SLAC National Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, 2575 Sand Hill Road, Menlo Park, CA 94025, USA 6 X-ray and Observational Astronomy Group/Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK 7 Department of Astronomy & Astrophysics, Pennsylvania
    [Show full text]
  • Feedback in Galaxy Clusters and Brightest Cluster Galaxy Star
    Feedback in Galaxy Clusters and Brightest Cluster Galaxy Star Formation by Kevin Fogarty A dissertation submitted to The Johns Hopkins University in conformity with the requirements for the degree of Doctor of Philosophy. Baltimore, Maryland August, 2017 c Kevin Fogarty 2017 All rights reserved Abstract My main thesis work is to understand the relationship between star forma- tion in the brightest cluster galaxy (BCG) and the thermodynamical state of the intracluster medium (ICM) of cool core galaxy clusters. Detailed photometry of BCGs in galaxy clusters observed in the Cluster Lensing and Supernova survey with Hubble (CLASH) reveal ultraviolet and Hα emitting knot and filamentary structures extending several tens of kpc. I initially focus on these structures, −1 which harbor starbursts forming stars at rates between < 1 M yr and ∼ −1 250 M yr . I perform ultraviolet through far-infrared Spectral Energy Dis- tribution (SED) fitting on combined Hubble, Spitzer, and Herschel photometry of CLASH BCGs, and measure star formation rates (SFRs), dust contents, and constrain the duration of starburst activity. Using X-ray data from Chandra, I find a tight relationship between CLASH BCG SFRs and the cooling-to-freefall time ratio in the ICM. I propose treating the cooling-to-freefall time ratio as a proxy for the mass condensation efficiency of the ICM in the core of cool-core clusters, an interpretation which is motivated by recent theoretical work de- ii ABSTRACT scribing feedback regulated condensation and precipitation of the ICM in cool core clusters. I follow up this work by performing similar SED fitting on a larger sample of clusters observed in the Cosmic Evolution Survey (COSMOS).
    [Show full text]
  • The Onset of Thermally Unstable Cooling from the Hot Atmospheres of Giant Galaxies in Clusters: Constraints on Feedback Models
    The Onset of Thermally Unstable Cooling from the Hot Atmospheres of Giant Galaxies in Clusters: Constraints on Feedback Models The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Hogan, M. T., B. R. McNamara, F. A. Pulido, P. E. J. Nulsen, A. N. Vantyghem, H. R. Russell, A. C. Edge, Iu. Babyk, R. A. Main, and M. McDonald. “The Onset of Thermally Unstable Cooling from the Hot Atmospheres of Giant Galaxies in Clusters: Constraints on Feedback Models.” The Astrophysical Journal 851, no. 1 (December 13, 2017): 66. As Published http://dx.doi.org/10.3847/1538-4357/AA9AF3 Publisher American Astronomical Society Version Final published version Citable link http://hdl.handle.net/1721.1/117575 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, 851:66 (20pp), 2017 December 10 https://doi.org/10.3847/1538-4357/aa9af3 © 2017. The American Astronomical Society. All rights reserved. The Onset of Thermally Unstable Cooling from the Hot Atmospheres of Giant Galaxies in Clusters: Constraints on Feedback Models M. T. Hogan1,2, B. R. McNamara1,2 , F. A. Pulido1 , P. E. J. Nulsen3,4 , A. N. Vantyghem1 , H. R. Russell5, A. C. Edge6 , Iu. Babyk1,7 , R. A. Main8, and M. McDonald9 1 Department of Physics and Astronomy, University of Waterloo, Waterloo, ON, N2L 3G1, Canada; [email protected] 2 Perimeter Institute for Theoretical Physics,
    [Show full text]
  • K Gas in the Rich Clusters of Galaxies Abell 2029 and Abell 3112
    A&A 421, 503–507 (2004) Astronomy DOI: 10.1051/0004-6361:20035938 & c ESO 2004 Astrophysics FUSE search for 105–106 K gas in the rich clusters of galaxies Abell 2029 and Abell 3112 A. Lecavelier des Etangs1, Gopal-Krishna2,, and F. Durret1 1 Institut d’Astrophysique de Paris, CNRS, 98 bis Bld Arago, 75014 Paris, France 2 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Germany Received 23 December 2003 / Accepted 18 March 2004 Abstract. Recent Chandra and XMM X-ray observations of rich clusters of galaxies have shown that the amount of hot gas which is cooling below ∼1 keV is generally more modest than previous estimates. Yet, the real level of the cooling flows, if any, remains to be clarified by making observations sensitive to different temperature ranges. As a follow-up of the FUSE observations reporting a positive detection of the O doublet at 1032, 1038 Å in the cluster of galaxies Abell 2597, which provided the first direct evidence for ∼3 × 105 K gas in a cluster of galaxies, we have carried out sensitive spectroscopy of two rich clusters, Abell 2029 and Abell 3112 (z ∼ 0.07) located behind low HI columns. In neither of these clusters could we detect −1 −1 the O doublet, yielding fairly stringent limits of ∼27 M yr (Abell 2029) and ∼25 M yr (Abell 3112) to the cooling flow rates using the 105−106 K gas as a tracer. The non-detections support the emerging picture that the cooling-flow rates are much more modest than deduced from earlier X-ray observations.
    [Show full text]