A Decade of WHIM search:
|
|
- Amber Bond
- 5 years ago
- Views:
Transcription
1 A Decade of WHIM search: Where do We Stand Where do We Go F. Nicastro (OAR-INAF) Y. Krongold, M. Elvis, S. Mathur 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 1
2 The Missing Baryons Problems McGaugh+1 Ω b WMAP h - =.6 h - =.456 ~ 5% Shull+1 ~ 3-4% (or more) of Baryons Still Missing at z~ Cosmological Baryon Fraction f b =.17 5/18/16 XMM-Newton: the Next Decade (F. Nicastro)
3 The WHIM in Hydro-dynamical simula6ons Britton+1 Cool-Phase: ~% Branchini+1 Warm-Phase: ~6% Hot-Phase: ~% 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 3
4 First Claimed WHIM Detections: Exceptional Outburst State (Nicastro+5, Nature, ApJ) However: - z(mkn 41) only.3 - Mkn 41 outbursts are unique + OII Kβ Controversial: - Not confirmed by XMM (though consistent with; Rassmussen+7) - Close to instrument systematics (Kaastra+6) Ω b (N OVII > ) = [O / H ] 1 % ~ Ω Miss 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 4
5 A Serendipitous hot X-Ray/BLA PKS (z=.137) Filament at z=.118? From X-rays è logt < 6.75; logn H =1.5±.3 (Z/Z.1 ) -1 From lack of OVI è logt > 6.5 From HI and T è Z = (1-4)% Z From Z and T è δ 3 and Theory From δ and N H è D=4-7 Mpc Combined Statistical Significance = 5.σ (5σ if FUSE systematics are included) [Nicastro+1] 5/18/16 (Nicastro+1) XMM-Newton: the Next Decade (F. Nicastro) 5
6 Galaxy concentrations as WHIM tracers But: N Right Ascension OVII ~ 8 x 1 16 cm -!!! Buote+9, Fang+1 H Mkn 51 5/18/16 Ren, Fang & XMM-Newton: Buote, 14 the Next Decade (F. Nicastro) 6
7 OII z= Not z=.3 <EW(OII Kβ)> = 14 ± 4 må.6 Nicastro+16, MNRAS, 457, 676 <EW(OII Kβ)> = 18 ± 5 må /18/16 XMM-Newton: the Next Decade (F. Nicastro) 7
8 The Case of H & the z=-limm / z=.3-whim conspiracy z= OII Kβ or z.3 OVII Kα.15.1 z= OII Kα z= OIV Kα or z.3 OVI Kα.5 z= OI Kα or z.3 OIV Kα.15.1 EW(OII Kβ) = 18 ± 5 må vs <EW(OII Kβ)> AGN = 18 ± 5 må Nicastro+16, MNRAS, 485, L13.5 z.3 WHIM not statistically required. If present must have: T 3x1 5 K b 1 km s-1 NOVII 4x1 15 cm - (<< 8x1 16 cm - of Fang+1) 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 8
9 Best WHIM Target in the Universe: 1ES z>.3 logt = CV CIII CVI.1 CIV CII OIII OIV OV OVII.1 OII OVI OVIII HI z >.4 - F X ~ 1- mcrab - High S/N COS spectrum with 5 priors (HI Lyα with 4<b<8 km s -1 : BLAs - è 5. < logt < 5.5 è Mostly CV) 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 9
10 Tentative IGM IDs Nicastro+13 Redshift CV CVI OIV OV OVII BLA OVI (ma) CIV (ma).41±. NA NA NA NA.3σ 9.6σ <65 <13.133±. 3.8σ.7σ NA NA NA 5.4σ <14 <5.184±.1 3.6σ NA NA NA NA NA <11 NA.19±.1.σ NA NA 1.7σ NA 9.3σ 7.6σ NA.37±.1 3.9σ NA NA? NA 5,.σ <13 NA.31±.1 4.1σ 4.1σ NA? NA 8.1σ 3.6σ NA 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 1
11 Cool WHIM at z=.31: (6.3σ X-ray only) Nicastro HI BLA From COS BLA and OVI b: è b th = 5 ± 7 km s -1 (b turb = 3 ± 14 km s -1 ) è logt = 5. ±.1 Fully Consistent with presence of CV, CVI, OV OVIa OVIb /18/16 XMM-Newton: the Next Decade (F. Nicastro) 11
12 Best-Fitting WHIM Parameters Redshift logt N H (1 19 cm - ) n b (1-6 cm -3 ) Z/Z [= N H (X)/N H (FUV)].41± ± ± , +.7, -.1 *.133±. 5.4, +., -.6 **. 15 NA.19± ± ± , +.4, ± ±.1.3, +., , +1.8, -..31± ±.5 3.1, +1.6, , +.19, -. * No consistent X-Ray-FUV solution: BLA is too narrow and shallow to be imprinted by the X-ray absorber and OVI should be visible if logt<5. ** From N H (X) divided by the average <Z/Z > =.8 ±.4 determined for the z=.41,.19,.31 systems 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 1
13 Cool WHIM contains 15% of MBs 1 1 Ω b = 1 µm p ρ cr, i i N H Δl comoving σ Ωb = 1 1 [1 1/ K] 1/ ρ cr, K i i µm p [N H < N H i=1 Δl comoving >] dl comoving = c H(z) dz logt>5.5 WHIM? Missing.1 logt<5.5 WHIM.1 Ω b (5. < logt < 5.5;EW CV,OVII >1 m A o ) =.69 ±.18 = (15± 4)% Ω b 5% of Baryons are still Missing 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 13
14 XMM VLP: 1.6 Ms on 1ES logt = CV CIII CVI.1 CIV CII OV OIII OVII OIV.3.1 OII OVI OVIII h at GTC SDSS u,g r,i,z 4.5 in S/N=5 (.L* at z=.5) Allows Δz= HI With the sensitivity of the current 5 ks Chandra bound to detect only the cool WHIM in CV. ~1.6 Ms XMM è ~4x S/N in OVII è N OVII > 1 15 cm - è ~5-1 systems sampling the hot WHIM 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 14
15 4σ Detection of logt>5.5 WHIM in Multiple Lines OIV Kα z= Redshift z z=.54 logt = K è b HI > 9 km s -1 + Tentatively confirms z=.43 OVII detects z=.37 OVII In the short-term, only ultra-deep XMM and Chandra observations can detect the missing 5% of baryons and solve the puzzle 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 15
16 The Long-term Future: Athena 6 AGNs Exposures: < T (ks) < 3 each -1 OVII-Forest - Total Exposure (in Msec) Redshift 5 ks for F.5- =.1 mcrab along a random WHIM LOS from Cen+6: detects 5 Systems with logt = K, lognh = (Z/Z )-1 cm- at z<.5 All in OVII-OVIII; in CV + OIV-OVI (Cool-Phase): excellent Density Diagnostics 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 16
17 Summary and Future - After proper ionization and metallicity correction, CV-OVI-BLA dominated cool WHIM contains ~ 15% of Baryons è 4-5 % of Baryons still Missing and likely to reside in logt>5.5 WHIM: detectable only with ultra-deep XMM and Chandra pointings - In the future Athena will enable: (a) accurate (few %) measure of the Cosmological Mass Density of Baryons in the Universe (b) study of the interplay between galaxy and AGN outflows and the IGM (feedback) (c) understanding of the role of shocks in the formation of structures in the Universe (d) mapping of the Universe s Dark-Matter concentrations 5/18/16 XMM-Newton: the Next Decade (F. Nicastro) 17
The Cool Portion of the WHIM & The Cold/Warm Milky Way CGM
The Cool Portion of the WHIM & The Cold/Warm Milky Way CGM F. Nicastro (OAR-INAF) F. Senatore, Y. Krongold, M. Elvis, S. Mathur 8/25/15 Chandra Workshop 215 (F. Nicastro) 1 Outline Chandra Detection of
More informationPicturing Feedback in Action in the Milky Way
Picturing Feedback in Action in the Milky Way ADistantEchoofMilkyWayCentralActivityclosesthe Galaxy s Baryon Census F. Nicastro 1,2,F.Senatore [1,3], Y. Krongold 4,S.Mathur [5,6], M. Elvis 2 Nicastro (OAR-INAF)
More informationThe Circumgalactic Medium, the Intergalactic Medium, and Prospects with TMT
The Circumgalactic Medium, the Intergalactic Medium, and Prospects with TMT Taotao Fang 方陶陶 Xiamen University 厦 门 大学 2014.11 Beijing 1 The circumgalactic medium (CGM) and the intergalactic medium (IGM)
More informationX-Ray observability of WHIM and our new mission concept DIOS Intergalactic. Oxygen. Surveyor ) Noriko Yamasaki ISAS/JAXA
X-Ray observability of WHIM and our new mission concept DIOS (Diffuse Intergalactic Oxygen Surveyor ) Noriko Yamasaki ISAS/JAXA 1 Cosmic Baryon Budget requires missing baryon The observed baryons are only
More informationarxiv: v2 [astro-ph.co] 13 Mar 2013
Chandra View of the Warm-Hot IGM toward 1ES 1553+113: Absorption Line Detections and Identifications (Paper I) arxiv:11.7177v [astro-ph.co] 13 Mar 13 F. Nicastro 1,, M. Elvis, Y. Krongold 3, S. Mathur,
More informationarxiv: v1 [astro-ph.co] 22 Nov 2018
Astronomy& Astrophysics manuscript no. pks_whim_nov21_print c ESO 2018 November 26, 2018 To be or not to be: hot WHIM absorption in the blazar PKS 2155-304 sight line? J. Nevalainen 1,, E. Tempel 1, 2,
More informationThe Physical Properties of Low-z OVI Absorbers in the OverWhelmingly Large Simulations
The Physical Properties of Low-z OVI Absorbers in the OverWhelmingly Large Simulations Thorsten Tepper García in collaboration with: Philipp Richter (Universität Potsdam) Joop Schaye (Sterrewacht Leiden)
More informationThe Cosmic Web of Baryons
The Cosmic Web of Baryons A White Paper submitted to Galaxies across Cosmic Time (GCT) and The Cosmology and Fundamental Physics (CFP) Science Frontiers Panels Joel N. Bregman Department of Astronomy University
More informationDetection of the Missing Baryons in a Warm-Hot Intergalactic Medium
Detection of the Missing Baryons in a Warm-Hot Intergalactic Medium F. Nicastro 1,2, J. Kaastra 3, Y. Krongold 4, S. Borgani 5,6,7, E. Branchini 8, R. Cen 9, M. Dadina 10, C.W. Danforth 11, M. Elvis 2,
More informationThe Warm Hot Environment of the Milky Way
The Warm Hot Environment of the Milky Way DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Rik
More informationTracing the bright and dark sides of the universe with X-ray observations. Yasushi Suto. Department of Physics University of Tokyo
Tracing the bright and dark sides of the universe with X-ray observations Yasushi Suto Department of Physics University of Tokyo 1 WMAP summary of cosmic energy budget baryons ordinary matter makes up
More informationAtomic Spectra in Astrophysics
Atomic Spectra in Astrophysics Potsdam University : Wi 2016-17 : Dr. Lidia Oskinova lida@astro.physik.uni-potsdam.de Helium Spectra 01 He is the second-most abundant element: 25% by mass of the Universe
More informationHow Big. Are IGM Absorbers? What? Charles Danforth U. Colorado. John Stocke Mike Shull Brian Keeney Devin Silvia etc.
How Big What? Are IGM Absorbers? Charles Danforth U. Colorado John Stocke Mike Shull Brian Keeney Devin Silvia etc. The Leiden Summer CGM-Galaxy Interface Workshop 20/6/13 The cartoon picture of the Lyα
More informationQuasar Winds: the 4 th element
Quasar Winds: the 4 th element Martin Elvis Harvard-Smithsonian Center for Astrophysics* * (way) previous address: Univ. Leicester X-ray astronomy group 42 Years of X-ray Astronomy: Problem Posed & Solved
More informationarxiv:astro-ph/ v2 8 Mar 2005
Astronomy & Astrophysics manuscript no. 2479 2nd February 2008 (DOI: will be inserted by hand later) A search for Warm-Hot Intergalactic Medium features in the X-ray spectra of Mkn 421 with the XMM-Newton
More informationX-ray Surveyor and the Spectroscopy of Supermassive Black Hole Outflows
X-ray Surveyor and the Spectroscopy of Supermassive Black Hole Outflows Martin Elvis Harvard-Smithsonian Center for Astrophysics I X-ray Surveyor The need has long been obvious Because: Diagnostics! hereisfree.com
More informationGalaxies 626. Lecture 9 Metals (2) and the history of star formation from optical/uv observations
Galaxies 626 Lecture 9 Metals (2) and the history of star formation from optical/uv observations Measuring metals at high redshift Metals at 6 How can we measure the ultra high z star formation? One robust
More informationQSO ABSORPTION LINE STUDIES with the HUBBLE SPACE TELESCOPE
QSO ABSORPTION LINE STUDIES with the HUBBLE SPACE TELESCOPE COLORADO GROUP: JOHN STOCKE, MIKE SHULL, JAMES GREEN, STEVE PENTON, CHARLES DANFORTH, BRIAN KEENEY Results thus far based on: > 300 QSO ABSORBERS
More informationWhere are the missing baryons?
Interview of BSc dissertation Where are the missing baryons? Brandon Qiang Wang 6 th February 2018 Image from Millennium Simulation Content I. Introduction II. Simulations III. Results IV. Conclusion 2
More informationFuture X-rayX Spectroscopy Missions. Jan-Willem den Herder
Future X-rayX Spectroscopy Missions Jan-Willem den Herder contents Plasma diagnostics in the 0.1 to 10 kev band with resolution > 100 X-ray spectrometers: instrumental promises Future missions (a dream)
More informationProspects for the direct WHIM detection by Athena
Exploring the Hot and Energetic Universe: 2mm The rst scientic conference dedicated to the Athena X-ray observatory Prospects for the direct WHIM detection by Athena The soft X-ray WHIM emission with WFI
More informationTHE GALACTIC CORONA. In honor of. Jerry Ostriker. on his 80 th birthday. Chris McKee Princeton 5/13/2017. with Yakov Faerman Amiel Sternberg
THE GALACTIC CORONA In honor of Jerry Ostriker on his 80 th birthday Chris McKee Princeton 5/13/2017 with Yakov Faerman Amiel Sternberg A collaboration that began over 40 years ago and resulted in a lifelong
More informationX-raying galactic feedback in nearby disk galaxies. Q. Daniel Wang University of Massachusetts
X-raying galactic feedback in nearby disk galaxies Q. Daniel Wang University of Massachusetts Chandra survey of diffuse X-ray emission from 53 edge-on galaxies i > 60 o, D < 30 Mpc (Li, J.-T. & Wang, Q.D.
More informationWeighing the dark side of the universe
Weighing the dark side of the universe Department of Physics The University of Tokyo Yasushi Suto June 18, 2004 Particle Physics Group Seminar Tsukuba University Hierarchical structure in the universe
More informationGALAXIES. Edmund Hodges-Kluck Andrew Ptak
GALAXIES Edmund Hodges-Kluck Andrew Ptak Galaxy Science with AXIS How does gas get into and out of galaxies? How important is hot accretion for L* or larger galaxies? How does star formation/black hole
More informationKilling Dwarfs with Hot Pancakes. Frank C. van den Bosch (MPIA) with Houjun Mo, Xiaohu Yang & Neal Katz
Killing Dwarfs with Hot Pancakes Frank C. van den Bosch (MPIA) with Houjun Mo, Xiaohu Yang & Neal Katz The Paradigm... SN feedback AGN feedback The halo mass function is much steeper than luminosity function
More informationAC Fabian, M. Cappi, J Sanders. Cosmic Feedback from AGN
AC Fabian, M. Cappi, J Sanders Cosmic Feedback from AGN AC Fabian, M Cappi, J Sanders, S Heinz, E Churazov, B McNamara, J Croston, D Worrall, F Humphrey, F Tombesi, J Reeves, M Giustini, P O Brien, T Reiprich
More informationWhere are the missing baryons? Craig Hogan SLAC Summer Institute 2007
Where are the missing baryons? Craig Hogan SLAC Summer Institute 2007 Reasons to care Concordance of many measures of baryon number (BBN, CMB,.) Evolution of our personal baryons (galaxies, stars, planets,
More informationarxiv: v1 [astro-ph] 7 Jan 2008
SSRv manuscript No. (will be inserted by the editor) FUV and X-ray absorption in the Warm-Hot Intergalactic Medium P. Richter F.B.S. Paerels J.S. Kaastra arxiv:0801.0975v1 [astro-ph] 7 Jan 2008 Received:
More informationFUV and X-Ray Absorption in the Warm-Hot Intergalactic Medium
Space Sci Rev (2008) 134: 25 49 DOI 10.1007/s11214-008-9325-4 FUV and X-Ray Absorption in the Warm-Hot Intergalactic Medium P. Richter F.B.S. Paerels J.S. Kaastra Received: 20 September 2007 / Accepted:
More informationPrecision Cosmology with X-ray and SZE Galaxy Cluster Surveys?
Precision Cosmology with X-ray and SZE Galaxy Cluster Surveys? Joe Mohr University of Illinois Outline SZE and X-ray Observations of Clusters Cluster survey yields and cosmology Precision cosmology and
More informationConstraining Dark Energy with BOSS. Nicolas Busca - APC Rencontres de Moriond 19/10/2010
Constraining Dark Energy with BOSS Nicolas Busca - APC Rencontres de Moriond 19/10/2010 Outline BOSS: What? How? Current Status of BOSS Constraints on Cosmology Conclusions What: Baryon Acoustic Oscilations
More informationSoft X-ray Emission Lines in Active Galactic Nuclei. Mat Page
Soft X-ray Emission Lines in Active Galactic Nuclei Mat Page MSSL-UCL Observations of soft X-ray line emission allow us to investigate highly ionized plasmas in galaxies and AGN. I ll start with the most
More informationX-raying Galaxy Ecosystems of Disk Galaxies. Q. Daniel Wang IoA/Cambridge University University of Massachusetts
X-raying Galaxy Ecosystems of Disk Galaxies Q. Daniel Wang IoA/Cambridge University University of Massachusetts Hot Gaseous Corona Wang et al. (2001) Key questions to be addressed: 1. How do diffuse X-ray
More informationClusters: Observations
Clusters: Observations Last time we talked about some of the context of clusters, and why observations of them have importance to cosmological issues. Some of the reasons why clusters are useful probes
More informationX-ray spectroscopy of nearby galactic nuclear regions
X-ray spectroscopy of nearby galactic nuclear regions 1. How intermittent are AGNs? 2. What about the silent majority of the SMBHs? 3. How do SMBHs interplay with their environments? Q. Daniel Wang University
More informationarxiv: v1 [astro-ph] 18 Dec 2007
Mem. S.A.It. Vol. 75, 282 c SAIt 2004 Memorie della ÇÙØ ÓÛ Ò Û Ò Ò Æ ÓÖ Ë Ñ Óй M. Cappi 1, F. Tombesi 1,2, and M. Giustini 1,2 arxiv:0712.2977v1 [astro-ph] 18 Dec 2007 1 INAF-IASF, Bologna, Via Gobetti
More informationarxiv:astro-ph/ v1 4 Jan 2005
Draft version September 23, 2017 Preprint typeset using L A TEX style emulateapj v. 6/22/04 AN O VI BARYON CENSUS OF THE LOW-z WARM-HOT INTERGALACTIC MEDIUM Charles W. Danforth & J. Michael Shull 1 CASA,
More informationarxiv: v1 [astro-ph.ga] 8 Nov 2017
The O VI mystery: mismatch between X-ray and UV column densities S. Mathur 1,2, F. Nicastro 3,4, A. Gupta 5, Y. Krongold 6, B.M. McLaughlin 7,8, N. Brickhouse 4, A. Pradhan 1 arxiv:1711.03055v1 [astro-ph.ga]
More informationWhere are the missing baryons?
Where are the missing baryons? Qiang Wang (Brandon) B.Sc. Supervisor: Dr Scott Kay School of Physics and Astronomy, University of Manchester 27/29 June 2018 Image from Millennium Simulation 1 Content I.
More informationNon Baryonic Nature of Dark Matter
Non Baryonic Nature of Dark Matter 4 arguments MACHOs Where are the dark baryons? Phys 250-13 Non Baryonic 1 Map of the territory dark matter and energy clumped H 2? gas baryonic dust VMO? MACHOs Primordial
More informationLarge-Scale Structure
Large-Scale Structure Evidence for Dark Matter Dark Halos in Ellipticals Hot Gas in Ellipticals Clusters Hot Gas in Clusters Cluster Galaxy Velocities and Masses Large-Scale Distribution of Galaxies 1
More informationThe Galaxy Environment of O VI Absorption Systems
The Galaxy Environment of O VI Absorption Systems John T. Stocke, Steven V. Penton, Charles W. Danforth, J. Michael Shull, Jason Tumlinson 1,andKevinM.McLin 2 Center for Astrophysics and Space Astronomy,
More informationThe gas-galaxy-halo connection
The gas-galaxy-halo connection Jean Coupon (University of Geneva) Collaborators: Miriam Ramos, Dominique Eckert, Stefano Ettori, Mauro Sereno, Keiichi Umetsu, Sotiria Fotopoulou, Stéphane Paltani, and
More informationTori & Winds, Leicester 14 September Disk Winds - tests? Martin Elvis. Harvard-Smithsonian Center for Astrophysics
Disk Winds - tests? Martin Elvis Harvard-Smithsonian Center for Astrophysics Air Wind/ Quasar Atmosphere www.chemsoc.org/timeline/graphic/0400_eawf.jpg Water Fluid = jet? Earth Fire Radiation = disk? Gravity
More informationWhere are oxygen synthesized in stars?
The oxygen abundance from X-rays : methods and prospects K. Matsushita Where are oxygen synthesized in stars? Hot intracluster medium (ICM) Warm-hot intergalactic medium? Hot interstellar medium in early-type
More informationIntergalactic HI and OVI: A Survey of 259 low-z COS Absorbers with Reference to Ionization Mechanics
University of Colorado, Boulder CU Scholar Undergraduate Honors Theses Honors Program Spring 2017 Intergalactic HI and OVI: A Survey of 259 low-z COS Absorbers with Reference to Ionization Mechanics Shannon
More informationDIFFUSE BARYONIC MATTER BEYOND 2020
DIFFUSE BARYONIC MATTER BEYOND 2020 M. MARKEVITCH, F. NICASTRO, P. NULSEN, E. RASIA, A. VIKHLININ, A. KRAVTSOV, W. FORMAN, G. BRUNETTI, C. SARAZIN, M. ELVIS, G. FABBIANO, A. HORNSCHEMEIER, R. BRISSENDEN,
More informationSupernova Remnant Science with AXIS. Brian Williams & Hiroya Yamaguchi
Supernova Remnant Science with AXIS Brian Williams & Hiroya Yamaguchi Big Picture Questions - How do supernovae dictate the life cycle of elements in the ISM? - What are the progenitors of the various
More informationGalaxies 626. Lecture 5
Galaxies 626 Lecture 5 Galaxies 626 The epoch of reionization After Reionization After reionization, star formation was never the same: the first massive stars produce dust, which catalyzes H2 formation
More informationDan Evans (Harvard), Julia Lee (Harvard), Jane Turner (UMBC/GSFC), Kim Weaver (GSFC), Herman Marshall (MIT) NGC 2110 Spectroscopy
Dan Evans (Harvard), Julia Lee (Harvard), Jane Turner (UMBC/GSFC), Kim Weaver (GSFC), Herman Marshall (MIT) Fe Kα Lines and Reflection: AGN Geometry The Fe Kα line complex in general consists of a narrow
More informationBAO and Lyman-α with BOSS
BAO and Lyman-α with BOSS Nathalie Palanque-Delabrouille (CEA-Saclay) BAO and Ly-α The SDSS-III/BOSS experiment Current results with BOSS - 3D BAO analysis with QSOs - 1D Ly-α power spectra and ν mass
More informationBaryon Census in Hydrodynamical Simulations of Galaxy Clusters
Baryon Census in Hydrodynamical Simulations of Galaxy Clusters Susana Planelles (Univ.Trieste-INAF) Collaborators: S.Borgani (Univ. Trieste-INAF), G.Murante (INAF Torino), L.Tornatore (Univ. Trieste),
More informationLocating missing baryons from oxygen emission lines with DIOS
Locating missing baryons from oxygen emission lines with DIOS (Diffuse Intergalactic Oxygen Surveyor) Yasushi Suto Department of Physics University of Tokyo July 19, 2004 University College London WHIM
More informationThe Hot Gaseous Halos of Spiral Galaxies. Joel Bregman, Matthew Miller, Edmund Hodges Kluck, Michael Anderson, XinyuDai
The Hot Gaseous Halos of Spiral Galaxies Joel Bregman, Matthew Miller, Edmund Hodges Kluck, Michael Anderson, XinyuDai Hot Galaxy Halos and Missing Baryons Dai et al. (2010) Rich clusters have nearly all
More informationObservational signatures of the warm-hot intergalactic medium and X-ray absorption lines by the halo of our Galaxy
Chin. J. Astron. Astrophys. Vol. 3 (2003) Suppl. 169 180 (http: /www.chjaa.org) Chinese Journal of Astronomy and Astrophysics Observational signatures of the warm-hot intergalactic medium and X-ray absorption
More informationTHE SCIENCE ENABLED BY UV EMISSION LINE MAPPING OF THE INTERGALACTIC MEDIUM AND THE CIRCUM-GALACTIC MEDIUM
THE SCIENCE ENABLED BY UV EMISSION LINE MAPPING OF THE INTERGALACTIC MEDIUM AND THE CIRCUM-GALACTIC MEDIUM A Science White Paper submitted to the Astro2010 Survey Submitted to Science Frontiers Panels:
More informationIlluminating the Dark Ages: Luminous Quasars in the Epoch of Reionisation. Bram Venemans MPIA Heidelberg
Illuminating the Dark Ages: Luminous Quasars in the Epoch of Reionisation Bram Venemans MPIA Heidelberg Workshop The Reionization History of the Universe Bielefeld University, March 8-9 2018 History of
More informationDetection of hot gas in the filament connecting the clusters of galaxies Abell 222 and Abell 223
Astronomy & Astrophysics manuscript no. 09599 c ESO 2008 March 19, 2008 Detection of hot gas in the filament connecting the clusters of galaxies Abell 222 and Abell 223 N. Werner 1, A. Finoguenov 2, J.
More informationCosmology The Road Map
Cosmology The Road Map Peter Schneider Institut für Astrophysik, Bonn University on behalf of the Astronomy Working Group Cosmology s Themes Fundamental Cosmology Probing inflation Investigating Dark Energy
More informationChandra: the Next Decade
Chandra The Next Decade Cyg A Tycho Crab 2016: Excellent Senior Review Results! Belinda Wilkes Director Chandra X-ray Center Cen A Chandra:17 years and counting! Detailed engineering review showed no show-stoppers
More informationX-raying the interstellar medium at high latitudes
X-raying the interstellar medium at high latitudes Ciro Pinto J. S. Kaastra(1,2), J. Kriss(3,4), E. Costantini(1), and the Mrk 509 consortium (1) SRON Netherlands Institute for Space Research (2) Astronomical
More informationMissing Baryons. Michael E. Anderson. 1. Outline
Missing Baryons Michael E. Anderson 1. Outline - Motivation - CMB census - Lyman-α forest census - low-z census - the WHIM, the CGM, and two formulations of the missing baryons problem - How to detect
More informationMeasuring star formation in galaxies and its evolution. Andrew Hopkins Australian Astronomical Observatory
Measuring star formation in galaxies and its evolution Andrew Hopkins Australian Astronomical Observatory Evolution of Star Formation Evolution of Star Formation Evolution of Star Formation Evolution of
More informationThe effect of large scale environment on galaxy properties
The effect of large scale environment on galaxy properties Toulouse, June 2017 Iris Santiago-Bautista The LSS baryonic component is composed by substructures of gas and galaxies embedded in dark matter
More informationRadiative Transfer in a Clumpy Universe: the UVB. Piero Madau UC Santa Cruz
Radiative Transfer in a Clumpy Universe: the UVB Piero Madau UC Santa Cruz The cosmic UVB originates from the integrated emission of starforming galaxies and QSOs. It determines the thermal and ionization
More informationThe quest for Type 2 quasars: What are the X-ray observations of optically selected QSOs2 telling us?
The quest for Type 2 quasars: What are the X-ray observations of optically selected QSOs2 telling us? Cristian Vignali Dipartimento di Astronomia, Universita`degli Studi di Bologna In collaboration with
More informationThis week at Astro 3303
This week at Astro 3303 First, we have the in-class presentations Then I will return the test I will collect HW#5 HW#6 is posted and due next Wednesday Includes elements from the test Soon, we will get
More informationHigh-Redshift Galaxies: A brief summary
High-Redshift Galaxies: A brief summary Brant Robertson (Caltech) on behalf of David Law (UCLA), Bahram Mobasher (UCR), and Brian Siana (Caltech/Incoming CGE) Observable Cosmological History t~3.7x10 5
More informationMultiwavelength observation campaign of Mrk 509: UV spectra of the X-ray Outflow!!!!Gerard Kriss!! STScI!!! (with N. Arav, J. Kaastra & the Mrk 509
Multiwavelength observation campaign of Mrk 509: UV spectra of the X-ray Outflow!!!!Gerard Kriss!! STScI!!! (with N. Arav, J. Kaastra & the Mrk 509 Team)!! The Influence of AGN Outflows! «They may affect
More informationHigh Energy Astrophysics: A View on Chemical Enrichment, Outflows & Particle Acceleration. (Feedback at work)
High Energy Astrophysics: A View on Chemical Enrichment, Outflows & Particle Acceleration (Feedback at work) Jacco Vink Utrecht University High Energy Astrophysics HEA aims at understanding the extreme
More informationJunfeng Wang, G. Fabbiano, G. Risaliti, M. Elvis, M. Karovska, A. Zezas (Harvard CfA/SAO), C. G. Mundell (Liverpool John Moores University, UK), G.
Junfeng Wang, G. Fabbiano, G. Risaliti, M. Elvis, M. Karovska, A. Zezas (Harvard CfA/SAO), C. G. Mundell (Liverpool John Moores University, UK), G. Dumas, E. Schinnerer (MPIA), J. M. Mazzarella, J. H.
More informationThe Probes and Sources of Cosmic Reionization Francesco Haardt University of Como INFN, Milano-Bicocca
1 The Probes and Sources of Cosmic Reionization Francesco Haardt University of Insubria@Lake Como INFN, Milano-Bicocca 2 TALK OUTLINE 1. Dark Ages and Reionization 2. Observations: QSO Absorption Lines
More informationThe Intergalactic Medium: Overview and Selected Aspects
The Intergalactic Medium: Overview and Selected Aspects Draft Version Tristan Dederichs June 18, 2018 Contents 1 Introduction 2 2 The IGM at high redshifts (z > 5) 2 2.1 Early Universe and Reionization......................................
More informationThe O VII X-ray forest toward Markarian 421: Consistency between XMM-Newton and Chandra
SLAC-PUB-11844 astro-ph/0604519 April 2006 The O VII X-ray forest toward Markarian 421: Consistency between XMM-Newton and Chandra J.S. Kaastra, N. Werner and J.W.A. den Herder SRON Netherlands Institute
More informationIs the high-redshift inter-galactic medium metal enriched? Valentina D Odorico INAF Osservatorio Astronomico di Trieste
Is the high-redshift inter-galactic medium metal enriched? Valentina D Odorico INAF Osservatorio Astronomico di Trieste 1 Collaborators DEEP SPECTRUM PROJECT Paramita Barai, George Becker, Francesco Calura,
More informationThe Sunyaev-Zeldovich Effect as a Probe of Black Hole Feedback
The Sunyaev-Zeldovich Effect as a Probe of Black Hole Feedback Suchetana Chatterjee University of Pittsburgh 08/03/2009 Collaborators: Prof. Tiziana Di Matteo (CMU), Dr. Shirley Ho (LBNL), Prof. Arthur
More informationCosmology with Galaxy Clusters. V. The Cluster Mass Function
Cosmology with Galaxy Clusters V. The Cluster Mass Function Baryon Fraction Summary Assuming clusters large enough to be representative, mass composition should match Universe observe fb and constrain
More informationThe Athena X-ray Integral Field Unit
The Athena X-ray Integral Field Unit 1000 X-IFU - Perseus core Didier Barret X-IFU Principal Investigator (IRAP, FR) Thien Lam-Trong X-IFU Project Manager (CNES, FR) Jan-Willem den Herder (SRON, NL) &
More informationHow to cheat with maps. perfectly sensible, honest version
How to cheat with maps watch out for weasel maps : logarithmic (favors solar system) conformal (blows up BB singularity into something significant, popular with CMB types) comoving (makes the local universe
More informationThe Hard X-Ray Luminosity Function of High-Redshift (z > 3) AGN
The Hard X-Ray Luminosity Function of High-Redshift (z > 3) AGN Fabio Vito Dipartimento di Fisica e Astronomia - Università di Bologna INAF-OABo F Vito, RGilli, C Vignali, A Comastri, M Brusa, N Cappelluti,
More informationPlanck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher accuracy
12-14 April 2006, Rome, Italy Francesco Melchiorri Memorial Conference Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher
More informationShedding light on hyperluminous quasars at the golden epoch of AGN/galaxy coevolu<on
Shedding light on hyperluminous quasars at the golden epoch of AGN/galaxy coevolu
More informationRadio emission from galaxies in the Bootes Voids
Radio emission from galaxies in the Bootes Voids Mousumi Das, Indian Institute of Astrophysics, Bangalore Large Scale Structure and galaxy flows, Quy Nhon, July 3-9, 2016 Collaborators K.S. Dwarkanath
More informationeboss Lyman-α Forest Cosmology
Moriond Cosmology Conference, La Thuile, 18th March 2018 eboss Lyman-α Forest Cosmology Matthew Pieri and BOSS & eboss Lyα Working Groups Quasar Spectra and Lyman α Forest Quasar Intergalactic medium Line-of-sight
More informationRotation of the Hot Gas around the Milky Way. Edmund Hodges-Kluck Matthew Miller and Joel Bregman University of Michigan
Rotation of the Hot Gas around the Milky Way Edmund Hodges-Kluck Matthew Miller and Joel Bregman University of Michigan Agenda Galaxy Halos OVII Absorption Lines in the RGS Archive Halo Model Halo Rotation?
More informationarxiv:astro-ph/ v2 11 Oct 2006
Mon. Not. R. Astron. Soc. 000, 000 000 (2006) Printed 25 August 2017 (MN LATEX style file v2.2) The Enrichment History of Baryons in the Universe Romeel Davé & Benjamin D. Oppenheimer Astronomy Department,
More informationRupert Croft. QuickTime and a decompressor are needed to see this picture.
Rupert Croft QuickTime and a decompressor are needed to see this picture. yesterday: Plan for lecture 1: History : -the first quasar spectra -first theoretical models (all wrong) -CDM cosmology meets the
More informationMagnetic Fields (and Turbulence) in Galaxy Clusters
Magnetic Fields (and Turbulence) in Galaxy Clusters Dongsu Ryu (UNIST, Ulsan National Institute of Science and Technology, Korea) with Hyesung Kang (Pusan Nat. U, Korea), Jungyeon Cho (Chungnam Nat. U.),
More informationSolving. Andrey Kravtsov The University of Chicago Department of Astronomy & Astrophysics Kavli Institute for Cosmological Physics
Solving Constraining galaxy formation with gaseous halos Andrey Kravtsov The University of Chicago Department of Astronomy & Astrophysics Kavli Institute for Cosmological Physics X-ray Vision workshop:
More informationHigh Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
More informationObservational Cosmology
(C. Porciani / K. Basu) Lecture 7 Cosmology with galaxy clusters (Mass function, clusters surveys) Course website: http://www.astro.uni-bonn.de/~kbasu/astro845.html Outline of the two lecture Galaxy clusters
More informationarxiv:astro-ph/ v1 16 Jun 2002
Chandra Detection of O VIII Lyα Absorption from an Overdense Region in the Intergalactic Medium Taotao Fang, Herman L. Marshall, Julia C. Lee, David S. Davis AND Claude R. Canizares arxiv:astro-ph/0206264v1
More informationAGN-driven turbulence revealed by extreme [CII]158µm line cooling in radio-galaxies
AGN-driven turbulence revealed by extreme [CII]158µm line cooling in radio-galaxies Pierre Guillard CNES Fellow Intitut d Astrophysique Spatiale, Orsay, France The Universe Explored by Herschel, ESTEC,
More informationGlobal Hot Gas in and around the Galaxy
University of Massachusetts Amherst ScholarWorks@UMass Amherst Astronomy Department Faculty Publication Series Astronomy 2009 Global Hot Gas in and around the Galaxy QD Wang University of Massachusetts
More informationFrancesco Tombesi. University of Rome, Tor Vergata NASA - Goddard Space Flight Center University of Maryland, College Park
Francesco Tombesi University of Rome, Tor Vergata NASA - Goddard Space Flight Center University of Maryland, College Park (credit JAXA s press release) Warm Absorbers (WAs) (Photo) ionized Mrk 509 v~300-800
More informationCosmic Web, IGM tomography and Clamato
The mystery figure Cosmic Web, IGM tomography and Clamato Martin White with K-G Lee, J. Hennawi, E. Kitanidis, P. Nugent, J. Prochaska, D. Schlegel, M.Schmittfull, C. Stark, et al. http://clamato.lbl.gov
More informationProbing dark matter and the physical state of the IGM with the Lyα forest
Probing dark matter and the physical state of the IGM with the Lyα forest Martin Haehnelt in collaboration with: George Becker, James Bolton, Jonathan Chardin, Laura Keating, Ewald Puchwein, Debora Sijacki,
More informationThe perspective of X-ray galaxy clusters with the XIFU/Athena instrument
The perspective of X-ray galaxy clusters with the XIFU/Athena instrument Nicolas Clerc IRAP Toulouse, France AtomDB workshop 17, Athens, GA November 3rd 17 Clusters of galaxies ; large-scale structure
More informationThe Epoch of Reionization: Observational & Theoretical Topics
The Epoch of Reionization: Observational & Theoretical Topics Lecture 1 Lecture 2 Lecture 3 Lecture 4 Current constraints on Reionization Physics of the 21cm probe EoR radio experiments Expected Scientific
More information