Galaxy Cluster Mergers & Star Formation
|
|
|
- Lewis Holland
- 6 years ago
- Views:
Transcription
1 Galaxy Cluster Mergers & Star Formation Chiara Ferrari In collaboration with: C.Benoist, J.Brinchmann, A.Cappi, A.Diaferio, L.Feretti, R.Hunstead, W.Kapferer, T.Kronberger, J.C.Mauduit, S.Maurogordato, J.L.Sauvageot, S.Schindler, E.Slezak
2 Outline of the talk Introduction: merging clusters & star formation Observational analysis of the galaxy cluster Abell 3921 Dynamical state (Optical & X-rays: Ferrari+ 05; Belsole+ 05) Star formation (SF) properties (Optical & Radio: Ferrari+ 05; 06; in prep.) Comparison with numerical simulations Ram-pressure on spiral galaxies (Kronberger+ 08; Kapferer+ 09) Ram-pressure on interacting galaxies (Kapferer+ 08)
3 Star formation in (merging) clusters Observed evolution in the star formation properties of cluster galaxies with redshift Increasing fraction of blue galaxies with z (e.g. Butcher & Oemler 78) Metevier+ 00 Increasing fraction of star forming/post-star forming galaxies with z (e.g. Dressler+ 87,99) Evolution of cluster members hierarchical growth of large scale structures? Blue fraction Debated observational evidence that cluster mergers may trigger star formation (e.g. Caldwell+ 93; Bardelli+ 98; Miller+ 05; Owen+ 05) redshift
4 Multi-λ analysis of merging clusters Optical: WFI, X-rays: XMM, Chandra Radio: VLA, ATCA Dynamical state of clusters Pre-merger A2933 Merger (Belsole+ 05,04; Ferrari+ 03,06a; Maurogordato+ 08; Sauvageot+ 05) A1413 A3921 Correlation with star formation properties (Ferrari+ 05,06b; Maurogordato+ in prep.) Presence of diffuse intra-cluster radio emission (Ferrari+ 06a) Relaxed Galaxy iso-density maps + X-ray surface brightness cts. (DSS + ROSAT)
5 A detailed multi-λ analysis of A3921 Why this cluster? Precise knowledge of the dynamical state of the cluster Quite simple and well determined merging scenario Analysis of the correlation between star formation & cluster-cluster collision
6 A3921: an off-axis pre-merger event Observations Galaxy iso-density map + ICM temperature map & surface brightness contours (ESO: Ferrari+ 05 ; XMM: Belsole+ 05) ICM metallicity distribution (XMM: Belsole+ 05) Simulations ICM temperature map + X-ray surface brightness (Ricker & Sarazin 01) ICM metallicity distribution + galaxy isodensity contours (Kapferer+ 06)
7 SF in the collision region Optical (EFOSC2+WFI) + Radio (ATCA) - Ferrari+ 05, 06 N E A3921 galaxies k (old population of stars) - 71% k+a (recent star formation) - 16% SFR < 3-4 MSun/yr SFR = 8 MSun/yr SFR = 50 MSun/yr e (ongoing star formation) - 13% Galaxy iso-density map + SF galaxies Star formation enhanced by cluster collision?
8 SF enhanced by cluster collision? Completeness in the central cluster field Precise determination of cluster members Discrimination between star forming galaxies and AGNs Physical mechanisms driving the observational properties
9 SF enhanced by cluster collision? 2dF spectroscopy from [OII] to [NII] Completeness in the central cluster field Precise determination of cluster members Discrimination between star forming galaxies and AGNs Physical mechanisms driving the observational properties Numerical simulations
10 2dF spectroscopy from [OII] to [NII] Ferrari+ in prep. 968 very good z determinations Spatial and velocity distribution of objects with high quality z determination
![2dF spectroscopy from [OII] to [NII] Ferrari+ in prep.](/docs-images/72/66948875/images/11-1.jpg "+ Katgert+ 98; Ferrari+ 05; Pimbblet+ 06 Completeness in the central cluster field R<19 ( R*+3) Precise determination of cluster")
11 2dF spectroscopy from [OII] to [NII] Ferrari+ in prep. + Katgert+ 98; Ferrari+ 05; Pimbblet+ 06 Completeness in the central cluster field R<19 ( R*+3) Precise determination of cluster members Discrimination between star forming galaxies and AGNs 40 arcmin 80% 20% 40% 60%
12 2dF spectroscopy from [OII] to [NII] Ferrari+ in prep. Completeness in the central cluster field Precise determination of cluster members Discrimination between star forming galaxies and AGNs 968 very good z determinations 311 cluster members Caustic method: Diaferio 99
![2dF spectroscopy from [OII] to [NII] Ferrari+ in prep.](/docs-images/72/66948875/images/13-3.jpg "Lamareille+ 04 Completeness in the central cluster field Precise determination of cluster members Discrimination")
13 2dF spectroscopy from [OII] to [NII] Ferrari+ in prep. Lamareille+ 04 Completeness in the central cluster field Precise determination of cluster members Discrimination between star forming galaxies and AGNs Kewley+ 01 Kauffmann+ 03
14 15% of emission line galaxies SF vs. non-sf galaxies: spatial distribution different at 5% sig. level Star formation & merging event Clear correlation between SF galaxies & collision region
15 >80 % 15% of emission line galaxies SF vs. non-sf galaxies: spatial distribution different at 5% sig. level Star formation & merging event Clear correlation between SF galaxies & collision region
16 Star forming galaxies vs. AGNs Ferrari+ in prep. Kauffmann+ 03 Kewley+ 01 Lamareille+ 04 Kewley+ 01
17 SF enhanced in the collision region: why? Comparison with numerical simulations by Hydro-Ski team S. Schindler & Innsbruck University
18 SF enhanced in the collision region: why? 500 Myr after the galaxy starts to feel the ram-pressure Kapferer+ 09 Ram-pressure can enhance star formation in a galaxy
19 Where do stars form? Kapferer+ 09 Kronberger+ 08
20 Where do stars form? ρ ICM = g/cm 3 ρ ICM = g/cm 3 ρ ICM = g/cm 3 v rel = 1000 km/s ρ ICM = g/cm 3 Surface density of stellar component 500 Myr after ram-pressure has started Kapferer+ 09
21 SF enhanced in the collision region: why? Galaxy-galaxy interactions and mergers (e.g. Duc+ 97) Galaxy mergers + ram-pressure (e.g. Kapferer+ 08) Galaxy mergers + cluster tidal field (e.g. Martig & Bournaud 08) HST observations of dusty star forming galaxies at the center of the merging cluster A851 (Oemler+ 09)
22 SF enhanced in the collision region: why? Galaxy-galaxy interactions and mergers (e.g. Duc+ 97) Galaxy mergers + ram-pressure (e.g. Kapferer+ 08) Galaxy mergers + cluster tidal field (e.g. Martig & Bournaud 08) No emission lines log (L 22cm (W/Hz)) = (SFR=19.6) Not in the collision region Ferrari + 06 e(b) spectral type (SFR=1.74) log (L 22cm (W/Hz)) < (SFR<3.05) In the collision region
23 Simulations vs. other observations ρicm = g/cm3 vrel = 1000 km/s Late type galaxy Ttail 107 K A3627 Kapferer+ 09 Sun+ 06,07 See also e.g. Randall+ 08; Kim+ 08
24 Simulations vs. other observations ρ ICM = g/cm 3 v rel = 1000 km/s Late type galaxy infalling in A2667 Star forming knots Cortese+ 07 Kenney+ 04 Kapferer+ 09 See also, e.g.: Crowl+ 05; Oosterloo+ 05; Cortese+ 06; Yoshida+ 02,04,08
25 Simulations vs. other observations Kapferer+ 09 Fast (<< 1 Gyr) gas depletion of the disk by ram-pressure In agreement with observational evidence that the physical mechanism(s) switching off star formation in dense environments must act on short timescales (e.g. Balogh+ 04; Cassata+ 07; Poggianti+ 09)
26 Cluster Mergers & Star Formation Star formation enhanced in the collision region of A3921 Possible physical origin: ram-pressure enhancement and subsequent quenching of star formation in cluster galaxies Closest core encounter A168 (Tomita+ 96) -0.2 Gyrs +0.2 Gyrs +0.6 Gyrs A3921, A2125, A2255 (Ferrari+ 05; Miller+ 05; Sakelliou & Ponman 06) Need of detailed multi-wavelength analyses of significant samples of merging clusters at different redshifts
27 Increasing fraction of red galaxies with density and / or difference in the fraction of star forming galaxies difference in the SFR of star forming galaxies Balogh et al. 2004
28 Distribution of EW(Hα) for galaxies in: Low density environment (dotted line) High density environment (solid line) Balogh et al The physical mechanism(s) switching off SF in dense environments must act on short timescales (< 1 Gyr)
The star formation history of Virgo spiral galaxies
The star formation history of Virgo spiral galaxies Combined spectral and photometric inversion Ciro Pappalardo INAF Osservatorio Astrofisico di Arcetri Cluster galaxies Abell 1689 Physical effects acting
Upcoming class schedule
Upcoming class schedule Thursday March 15 2pm AGN evolution (Amy Barger) th Monday March 19 Project Presentation (Brad) nd Thursday March 22 postponed to make up after spring break.. Spring break March
How environment shapes galaxy evolution: the satellite galaxies' perspective
How environment shapes galaxy evolution: the satellite galaxies' perspective Anna Pasquali Astronomisches Rechen Institut, Zentrum für Astronomie der Universität Heidelberg NGC 4651 Why do we care? At
Observing Galaxy Evolution in the Stormy Environment of Shapley Supercluster
Observing Galaxy Evolution in the Stormy Environment of Shapley Supercluster Paola Merluzzi INAF - Osservatorio Astronomico di Capodimonte Napoli - Italy & G. Busarello, C.P. Haines, A. Mercurio, M.A.
Morphological Composition of z~0.4 Groups: The site of S0 Formation?
Morphological Composition of z~0.4 Groups: The site of S0 Formation? Dave Wilman Max Planck Institute for Extraterrestrial Physics, Munich Wilman, Oemler, Mulchaey, McGee, Balogh & Bower 2009, ApJ, 692,
Morphological Composition of z~0.4 Groups: The site of S0 Formation?
Morphological Composition of z~0.4 Groups: The site of S0 Formation? Dave Wilman Wilman, Oemler, Mulchaey, McGee, Balogh & Bower 2009, ApJ, 692, 298 * *Also described as a Research Highlight in Nature,
The effect of ram pressure on the star formation, mass distribution and morphology of galaxies
Astronomy & Astrophysics manuscript no. kapferer rps galaxies c ESO 2009 March 12, 2009 The effect of ram pressure on the star formation, mass distribution and morphology of galaxies W. Kapferer 1, C.
The Radio/X-ray Interaction in Abell 2029
The Radio/X-ray Interaction in Abell 2029 Tracy Clarke (Univ. of Virginia) Collaborators: Craig Sarazin (UVa), Elizabeth Blanton (UVa) Abell 2029: Background z = 0.0767, D=320 Mpc, scale = 1.44 kpc/ typically
arxiv:astro-ph/ v1 6 Jul 2006
Astronomy & Astrophysics manuscript no. A3921 ATCA February 5, 2008 (DOI: will be inserted by hand later) ATCA observations of the galaxy cluster Abell 3921 I. Radio emission from the central merging sub-clusters
Aeree Chung Yonsei University
Evolutionary Paths in Galaxy Morphology, 2013 Sep 23-26, Sydney Australia Environmentally Galaxy Evolution: From a Gas Perspective Aeree Chung Yonsei University S + Irr dominant in the field Morphology-density
The Evolution of Spiral Galaxies in a Cluster Environment
The Evolution of Spiral Galaxies in a Cluster Environment ESA/ESAC, XMM-Newton Science Operations Centre In collaboration with: M. Weżgowiec 1,2, R.-J. Dettmar 1, B. Vollmer 3, M. Soida 2, K.T. Chyży 2,
Publ. Astron. Obs. Belgrade No. 86 (2009), TURKISH NATIONAL OBSERVATORY (TUG) VIEW OF CLUSTERS OF GALAXIES
Publ. Astron. Obs. Belgrade No. 86 (2009), 125-130 Contributed paper TURKISH NATIONAL OBSERVATORY (TUG) VIEW OF CLUSTERS OF GALAXIES M. HUDAVERDI 1,2, E. N. ERCAN 2, M. BOZKURT 2, F. GÖK3 and E. AKTEKIN
Snowballs in hell! X-ray galactic coronae in galaxy! clusters and the need for sub-arcsecond resolution! Simona Giacintucci (NRL)!
Snowballs in hell X-ray galactic coronae in galaxy clusters and the need for sub-arcsecond resolution Simona Giacintucci (NRL) M. Markevitch (GSFC), T. Clarke (NRL), E. Richards (NRC-NRL) X-ray Skies with
Galaxy evolution in clusters from the CLASH-VLT survey
Galaxy evolution in clusters from the CLASH-VLT survey Andrea Biviano INAF-Osservatorio Astronomico di Trieste (on behalf of the CLASH-VLT team) (part of) The CLASH-VLT team M. Nonino, co-i I. Balestra
Dissecting jellyfish galaxies with MUSE
Dissecting jellyfish galaxies with MUSE Yara L. Jaffé (ESO Chile) & the GASP collaboration reviewby byboselli Boselli &&Gavazzi (2006) SeeSee review Gavazzi (2006) Gas stripping of cluster galaxies cold
Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics
Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics with: Tim Heckman (JHU) GALEX Science Team (PI: Chris Martin), Lee Armus,
A mid and far-ir view of the star formation activity in galaxy systems and their surroundings
A mid and far-ir view of the star formation activity in galaxy systems and their surroundings Andrea Biviano Andrea Biviano INAF/Osservatorio Astronomico di Trieste Outline: mid-ir & multiwavelength observations
arxiv:astro-ph/ v2 14 Oct 2002
Star Formation through Time ASP Conference Series, Vol. **VOLUME**, 2003 Pérez, González Delgado, Tenorio-Tagle The Environmental Dependence of Star Formation in the Nearby Universe arxiv:astro-ph/0210242v2
Moore et al Kenney et al. 2004
Moore et al. 1996 Kenney et al. 2004 (i) Interaction with other cluster members and/or with the cluster potential (ii) Interactions with the hot gas that permeates massive galaxy systems. The influence
arxiv:astro-ph/ v1 8 Apr 2004
Outskirts of Galaxy Clusters: intense life in the suburbs Proceedings IAU Colloquium No. 195, 2004 A. Diaferio, ed. c 2004 International Astronomical Union DOI: 00.0000/X000000000000000X Luminous Infrared
Stellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
Hot Gas Halos in Early-Type Galaxies
Hot Gas Halos in Early-Type Galaxies Tesla Jeltema University of California, Santa Cruz Collaborators: John Mulchaey, Breanna Binder, Jesper Rasmussen, Xue-Ning Bai, Jacqueline van Gorkom, Ann Zabludoff
arxiv:astro-ph/ v1 4 Dec 2002
Gas in Groups and Clusters of Galaxies Sabine Schindler Institut für Astrophysik, Universität Innsbruck arxiv:astro-ph/0212104 v1 4 Dec 2002 Abstract. Groups and clusters contain a large fraction of hot
AGN feedback and its influence on massive galaxy evolution
AGN feedback and its influence on massive galaxy evolution Darren Croton (University of California Berkeley) Simon White, Volker Springel, et al. (MPA) DEEP2 & AEGIS collaborations (Berkeley & everywhere
Embedded Spiral Patterns in the massive galaxy cluster Abell 1835
2017/06/08 X-ray Universe @ Rome Embedded Spiral Patterns in the massive galaxy cluster Abell 1835 Shutaro Ueda (ISAS/JAXA), Tetsu Kitayama (Toho University), Tadayasu Dotani (ISAS/JAXA, SOKENDAI) This
arxiv:astro-ph/ v1 26 Jul 2005
A High Resolution HI Study of Selected Virgo Galaxies - Preliminary Results on Gas Morphology & Extra-Planar Gas arxiv:astro-ph/0507592v1 26 Jul 2005 Aeree Chung and J. H. van Gorkom Department of Astronomy,
Density. Red. Low high. Blue. Cluster galaxy population: passive and red Hogg et al. 2004
Red Density Blue Low high Cluster galaxy population: passive and red Hogg et al. 2004 Normal spiral galaxy Red S0 galaxy Cluster spiral Field spiral Chung et al. 2009 Walter et al. 2008 Yellow contours:
Galaxy Systems in the Optical and Infrared. Andrea Biviano INAF/Oss.Astr.Trieste
Galaxy Systems in the Optical and Infrared Andrea Biviano INAF/Oss.Astr.Trieste Plan of the lectures: I. Identification, global properties, and scaling relations II. Structure and dynamics III. Properties
The Evolution of Galaxy Morphologies in Clusters
The Evolution of Galaxy Morphologies in Clusters New Views of the Universe KICP, U. Chicago, December 2005 Marc Postman & collaborators: Frank Bartko Txitxo Benitez John Blakeslee Nick Cross Ricardo Demarco
Probing the Outskirts of Strongly Merging Double Clusters
Probing the Outskirts of Strongly Merging Double Clusters S. W. Randall - CfA E. Bulbul, R. Paterno-Mahler, C. Jones, W. Forman, E. Miller, S. Murray, C. Sarazin, E. Blanton Probing the Outskirts of Strongly
Galaxy clusters. Dept. of Physics of Complex Systems April 6, 2018
Galaxy clusters László Dobos Dept. of Physics of Complex Systems dobos@complex.elte.hu É 5.60 April 6, 2018 Satellite galaxies Large galaxies are surrounded by orbiting dwarfs approx. 14-16 satellites
arxiv:astro-ph/ v1 4 Mar 2004
Recycling intergalactic and interstellar matter IAU Symposium Series, Vol. 217, 2004 Pierre-Alain Duc, Jonathan Braine and Elias Brinks, eds. Spiral Galaxy - ICM Interactions in the Virgo Cluster Jeffrey
Molecular Gas and the Host Galaxies of Infrared-Excess Quasi-Stellar Objects
Molecular Gas and the Host Galaxies of Infrared-Excess Quasi-Stellar Objects A. S. Evans (Stony Brook) J. A. Surace & D. T. Frayer (Caltech) D. B. Sanders (Hawaii) Luminous Infrared Galaxies Properties
Lessons from the Virgo Cluster
The Role of Hydrogen in the Evolution of Galaxies 15-19 Sep 2014 Kuching, Malaysia Environments and the Evolution of Cool Gas in Galaxies Lessons from the Virgo Cluster Aeree Chung Yonsei University Seoul,
Optical studies of an ultraluminous X-ray source: NGC1313 X-2
Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu Harvard-Smithsonian Center for Astrophysics in collaboration with Joel Bregman, Jon Miller, Philip Kaaret outline background: ultraluminous
Demographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers?
Elaine M. Sadler Black holes in massive galaxies Demographics of radio galaxies nearby and at z~0.55 Are radio galaxies signposts to black-hole mergers? Work done with Russell Cannon, Scott Croom, Helen
The Different Physical Mechanisms that Drive the Star-formation Histories of Giant and Dwarf Galaxies
The Different Physical Mechanisms that Drive the Star-formation Histories of Giant and Dwarf Galaxies Chris Haines (University of Birmingham) Adriana Gargiulo, Gianni Busarello, Francesco La Barbera, Amata
Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies. Amy Reines Einstein Fellow NRAO Charlottesville
Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies Amy Reines Einstein Fellow NRAO Charlottesville Motivation: The origin of supermassive BH seeds Motivation: The origin of
Dual and Binary MBHs and AGN: Connecting Dynamics and Accretion
Dual and Binary MBHs and AGN: Connecting Dynamics and Accretion Sandor Van Wassenhove Marta Volonteri Lucio Mayer Jillian Bellovary Massimo Dotti Simone Callegari BH-Galaxy Coevolution Black holes found
Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines!
Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines Idealized 21cm spectra Example observed 21cm spectra HI densities
High 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
Clusters of Galaxies Ch 7 S&G! Coma Cluster-the nearest massive cluster! The apparent nature of clusters depends on the wavelength one looks at!
Clusters of Galaxies Ch 7 S&G Clusters of galaxies are the largest gravitationally bound systems in the Universe. At optical wavelengths they appear as over-densities of galaxies with respect to the field
Anatomy of an X-ray detected cluster at z = 2: low metallicities and enhanced specific star formation rates in star-forming galaxies.
Anatomy of an X-ray detected cluster at z = 2: low metallicities and enhanced specific star formation rates in star-forming galaxies. F. Valentino 1, E. Daddi 1, V. Strazzullo 1,2, R. Gobat 1,3, F. Bournaud
Galaxy Ecology. an Environmental Impact Assessment. Frank van den Bosch (MPIA)
Galaxy an Environmental Impact Assessment Frank van den Bosch (MPIA) in collaboration with Xiaohu Yang (SHAO), Houjun Mo (UMass), Simone Weinmann (Zürich) Anna Pasquali (MPIA), Daniel Aquino (MPIA) Aspen,
Part 2. Hot gas halos and SMBHs in optically faint ellipticals. Part 3. After Chandra?
Hot gas and AGN Feedback in Nearby Groups and Galaxies Part 1. Cool cores and outbursts from supermassive black holes in clusters, groups and normal galaxies Part 2. Hot gas halos and SMBHs in optically
New Results on the AGN Content of Galaxy Clusters
Carnegie Observatories Astrophysics Series, Vol. 3: Clusters of Galaxies: Probes of Cosmological Structure and Galaxy Evolution ed. J. S. Mulchaey, A. Dressler, and A. Oemler (Pasadena; Carnegie Observatories:
Radio 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
Role of the Environment in the Evolution of Galaxies Richard Ellis
Role of the Environment in the Evolution of Galaxies Richard Ellis http://www.astro.caltech.edu/~rse/ay211_env.ppt Hubble s Tuning Fork (1922-1926, 1936)..describes a true order among the galaxies, not
Galaxies undergoing ram-pressure stripping: the influence of the bulge on morphology and star formation rate
DOI: 10.1051/0004-6361/201118311 c ESO 2012 Astronomy & Astrophysics Galaxies undergoing ram-pressure stripping: the influence of the bulge on morphology and D. Steinhauser, M. Haider, W. Kapferer, and
Large-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
COSMOS-CLASH:The existence and universality of the FMR at z<2.5 and environmental effects
COSMOS-CLASH:The existence and universality of the FMR at z
Clusters of galaxies and the large scale structure of the universe. Gastão B. Lima Neto IAG/USP
Clusters of galaxies and the large scale structure of the universe Gastão B. Lima Neto IAG/USP IWARA, Maresias 10/2009 Our story begins... William Herschel recognizes the clustering of nebulae and their
Contents. List of Participants
Table of Introduction List of Participants page xi xiii 1 Galaxy clusters as probes of cosmology and astrophysics August E. Evrard 1 1.1 Introduction 1 1.2 Clusters as Dark Matter Potential Wells 4 1.3
A Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA
M87 A Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA interactions galore; stripping at work, M87 outburst Low Eddington ratio accretion (like other normal
arxiv: v1 [astro-ph.ga] 7 Apr 2016
![arxiv: v1 [astro-ph.ga] 7 Apr 2016](/thumbs/72/66711727.jpg "arxiv: v1 [astro-ph.ga] 7 Apr 2016")
Draft version April 8, 2016 Preprint typeset using L A TEX style emulateapj v. 5/2/11 HST IMAGING OF DUST STRUCTURES AND STARS IN THE RAM PRESSURE STRIPPED VIRGO SPIRALS NGC 4402 AND NGC 4522: STRIPPED
Neutral Hydrogen Gas in Star Forming Galaxies at z=0.24 Philip Lah. HI Survival Through Cosmic Times Conference
Neutral Hydrogen Gas in Star Forming Galaxies at z=0.24 Philip Lah HI Survival Through Cosmic Times Conference Collaborators: Frank Briggs (ANU) Jayaram Chengalur (NCRA) Matthew Colless (AAO) Roberto De
Star formation history in high redshift radio galaxies
Cygnus A Star formation history in high redshift radio galaxies Collaborators: B. Rocca-Volmerange (IAP), C. De Breuck (ESO), J. Vernet (ESO), N. Seymour (CASS), D. Stern (JPL), M. Lehnert (IAP), P. Barthel
arxiv:astro-ph/ v1 24 Apr 2004
Outskirts of Galaxy Clusters: intense life in the suburbs Proceedings IAU Colloquium No. 195, 2004 A. Diaferio, ed. c 2004 International Astronomical Union DOI: 00.0000/X000000000000000X Newcomers Meet
13.1 Galaxy Evolution: Introduction
13.1 Galaxy Evolution: Introduction Galaxies Must Evolve Stars evolve: they are born from ISM, evolve, shed envelopes or explode, enriching the ISM, more stars are born Structure evolves: density fluctuations
On the influence of environment on star-forming galaxies
On the influence of environment on star-forming galaxies Lizhi Xie 谢利智 Tianjin Normal University; INAF-OATS Collaborators: G. De Lucia; F. Fontanot; D. Wilman; M. Fossati Galaxy properties correlate with
Giant cosmic tsunamis: the impact of shocks and turbulence on galaxy evolution
Giant cosmic tsunamis: the impact of shocks and turbulence on galaxy evolution Andra Stroe ESO Fellow astroe@eso.org Twitter: @Andra_Stroe www.eso.org/~astroe D. Sobral, M. J. Jee, W. Dawson, H. Hoekstra,
Multi-wavelength Surveys for AGN & AGN Variability. Vicki Sarajedini University of Florida
Multi-wavelength Surveys for AGN & AGN Variability Vicki Sarajedini University of Florida What are Active Galactic Nuclei (AGN)? Galaxies with a source of non-stellar emission arising in the nucleus (excessive
Clusters of Galaxies " High Energy Objects - most of the baryons are in a hot (kt~ k) gas." The x-ray luminosity is ergs/sec"
Clusters of Galaxies! Ch 4 Longair Clusters of galaxies are the largest gravitationally bound systems in the Universe. At optical wavelengths they appear as over-densities of galaxies with respect to the
Lecture 11: SDSS Sources at Other Wavelengths: From X rays to radio. Astr 598: Astronomy with SDSS
Astr 598: Astronomy with SDSS Spring Quarter 4, University of Washington, Željko Ivezić Lecture : SDSS Sources at Other Wavelengths: From X rays to radio Large Surveys at Many Wavelengths SDSS: UV-IR five-band
A new mechanism for the formation of PRGs
A new mechanism for the formation of PRGs Spavone Marilena (INAF-OAC) Iodice Enrica (INAF-OAC), Arnaboldi Magda (ESO-Garching), Longo Giuseppe (Università Federico II ), Gerhard Ortwin (MPE-Garching).
Fossil G roups Groups Fossil? Groups? Renato Dupke
Fossil Groups Fossil? Groups? Renato Dupke Collaborators: Eric Miller (MIT) Claudia Mendes de Oliveira, Rob Proctor, Raimundo Lopes de Oliveira, (IAG-USP), Pieter Westera (National Observatory Brazil,
Radio emission in clusters of galaxies. An observational perspective
Radio emission in clusters of galaxies An observational perspective Tiziana Venturi INAF, IRA, Bologna IV ESTRELA Workshop, Bologna, 19 January 2009 Overview - What are galaxy clusters - Radio emission
Tidal disruption events from the first XMM-Newton Slew Survey
Tidal disruption events from the first XMM-Newton Slew Survey Pilar Esquej Centro de Astrobiologia (INTA-CSIC) Richard Saxton, Stefanie Komossa, Andy Read, M. Sanchez-Portal et al. Tidal disruption events
Deep Impact :! Molecular Gas Properties under Strong ICM Pressure
Deep Impact : Molecular Gas Properties under Strong ICM Pressure Bumhyun Lee & Aeree Chung Department of Astronomy, Yonsei University (Korea) The 3rd workshop on Large Aperture Mm/Submm Telescopes in the
Astronomy. Astrophysics. Chandra observation of the multiple merger cluster Abell 521
A&A 446, 417 428 (2006) DOI: 10.1051/0004-6361:20053946 c ESO 2006 Astronomy & Astrophysics Chandra observation of the multiple merger cluster Abell 521 C. Ferrari 1,M.Arnaud 2, S. Ettori 3, S. Maurogordato
Star-formation Across Cosmic Time: Initial Results from the e-merge Study of the μjy Radio Source Population. SPARCs VII The Precursors Awaken
Star-formation Across Cosmic Time: Initial Results from the e-merge Study of the μjy Radio Source Population SPARCs VII The Precursors Awaken Tom Muxlow & Nick Wrigley JBCA Manchester for the e-merge Consortium
The The largest assembly ESO high-redshift. Lidia Tasca & VUDS collaboration
The The largest assembly ESO high-redshift of massive Large galaxies Programme at 2
Clustering of Star-forming Galaxies and connections with AGN activity
Clustering of Star-forming Galaxies and connections with AGN activity MANUELA MAGLIOCCHETTI IAPS-INAF Collaborators: Herschel PEP team (D.Lutz, P.Popesso, D.Rosario et al.) & A.Lapi, M.Negrello, G.De Zotti.,
Spatially-Resolved Molecular Gas, Dust and Star Formation in Early-Types
Spatially-Resolved Molecular Gas, Dust and Star Formation in Early-Types CO (Katey Alatalo, Leo Blitz, Francoise Combes, Alison Crocker, Timothy Davis, Lisa Young) Optical (SAURON + Atlas 3D teams) Plans:
Environmental effects on galaxy evolution in the distant Universe
Environmental effects on galaxy evolution in the distant Universe Francesco Valentino Advisor: Dr. Emanuele Daddi Journées des thésards, Saclay, July 1 st 2015 All you want to know about me First name,
An analogy. "Galaxies" can be compared to "cities" What would you like to know about cities? What would you need to be able to answer these questions?
An analogy "Galaxies" can be compared to "cities" What would you like to know about cities? how does your own city look like? how big is it? what is its population? history? how did it develop? how does
The evolution of satellite galaxy quenching. Sean McGee University of Birmingham
The evolution of satellite galaxy quenching Sean McGee University of Birmingham Traditional environmental gas picture This ball of gas and stars falls into a group/cluster and is stripped. Hot Gas If the
Galaxy Collisions & the Origin of Starburst Galaxies & Quasars. February 24, 2003 Hayden Planetarium
Galaxy Collisions & the Origin of Starburst Galaxies & Quasars February 24, 2003 Hayden Planetarium Normal massive galaxy types elliptical & spiral galaxies Spiral Bulge of old stars Large black hole Very
The Combined effects of ram pressure stripping, and tidal influences on Virgo cluster dwarf galaxies, using N body/ SPH simulation
The Combined effects of ram pressure stripping, and tidal influences on Virgo cluster dwarf galaxies, using N body/ SPH simulation Author: Rory Smith, Cardiff University Collaborators: Jonathon Davies,
Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau
Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau Bachelor of Physics, Master of Astrophysics Université de Strasbourg PhD, Université Paris-Diderot Observatoire de Strasbourg Les
1. Overview. Theory lags behind and there are many unsolved problems, including the nature of dark matter and dark energy.
PC2491: Galaxies 1. Overview The aim of this course is to understand the observed properties of galaxies in the hierarchical structure formation model. This is a particular exciting time to study galaxies
Galaxy Ecology. an Environmental Impact Assessment. Frank van den Bosch (MPIA)
Galaxy an Environmental Impact Assessment Frank van den Bosch (MPIA) in collaboration with Xiaohu Yang (SHAO), Houjun Mo (UMass), Simone Weinmann (Zürich) Anna Pasquali (MPIA), Daniel Aquino (MPIA) Heidelberg,
Molecular Gas and Star Formation in Early-Type Galaxies
Molecular Gas and Star Formation in Early-Type Galaxies CO (Katey Alatalo, Estelle Bayet, Leo Blitz, Francoise Combes, Alison Crocker, Timothy Davis, Melanie Krips, Lisa Young) Optical (SAURON + Atlas
X-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.
Other Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies
Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at
Course of Galaxies course organizer: Goeran Ostlin ESSAY. X-ray physics of Galaxy Clusters
Course of Galaxies course organizer: Goeran Ostlin ESSAY X-ray physics of Galaxy Clusters Student: Angela Adamo angela@astro.su.se fall 2006 Front:-The double cluster A1750. The contours of the XMM-Newton
Radio Quiet AGN: Black Hole & Host Galaxy Proper;es
Radio Quiet AGN: Black Hole & Host Galaxy Proper;es (ESO) Collaborators: V. Mainieri, P. Padovani, P. Rosa6, N. Miller, K. I. Kellermann, P. Tozzi, S. Va>akunnel, A. Bongiorno, + PEP Collaboration Credit:
Deep Keck Spectroscopy of High-Redshift Quiescent Galaxies
Sirio Belli Max-Planck Institute for Extraterrestrial Physics Deep Keck Spectroscopy of High-Redshift Quiescent Galaxies with Andrew Newman and Richard Ellis Introduction Schawinski et al. 2014 red sequence
Satellite Galaxy Evolution in Groups & Clusters
Satellite Galaxy Evolution in Groups & Clusters Andrew Wetzel Yale University Jeremy Tinker (NYU) & Charlie Conroy (Harvard/CfA) Tinker, Wetzel & Conroy 2011, ArXiv 1107.5046 Wetzel, Tinker & Conroy 2011,
HW#6 is due; please pass it in. HW#7 is posted; it requires you to write out answers clearly and completely explaining your logic.
Oct 21, 2015 Basic properties of groups and clusters of galaxies Number density, structure X-ray emission from hot ICM Estimating cluster masses Cluster scaling relations Impact of environment on galaxies
Chapter 17. Active Galaxies and Supermassive Black Holes
Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study
Gas and stars in compact (young) radio sources
Gas and stars in compact (young) radio sources ASTRON, Dwingeloo Kapteyn Inst. Groningen B. Emonts, J. Holt, C. Tadhunter, T. Oosterloo C. Struve Motivations Learn more about the formation and evolution
STAR FORMATION ALONG A CLUSTER-FEEDING FILAMENT
STAR FORMATION ALONG A CLUSTER-FEEDING FILAMENT DARIO FADDA IPAC / Caltech Outline * Discovery of the filament * The obscured star formation in different environments * Radio observation and the density
HI as a probe for dwarf galaxy evolution in different environments: Voids to clusters
HI as a probe for dwarf galaxy evolution in different environments: Voids to clusters Sushma Kurapati Collaborators: Jayaram N Chengalur, NCRA, India Simon Pustilnik, SAO RAS, Russia 2017 PHISCC Workshop
Galaxy groups: X-ray scaling relations, cool cores and radio AGN
Galaxy groups: X-ray scaling relations, cool cores and radio AGN Ming Sun (UVA) (M. Voit, W. Forman, P. Nulsen, M. Donahue, C. Jones, A. Vikhlinin, C. Sarazin ) Outline: 1) Scaling relations and baryon
Formation of z~6 Quasars from Hierarchical Galaxy Mergers
Formation of z~6 Quasars from Hierarchical Galaxy Mergers Yuexing Li et al Presentation by: William Gray Definitions and Jargon QUASAR stands for QUASI-stellAR radio source Extremely bright and active
Star Formation in Brightest Cluster Galaxies in Cool Cores:
Star Formation in Brightest Cluster Galaxies in Cool Cores: Christopher O Dea Rochester Institute of Technology SPITZER: Chris O Dea, Stefi Baum, George Privon, Jake Noel-Storr (RIT) Alice Quillen, Nick
Halo Gas Velocities Using Multi-slit Spectroscopy
Halo Gas Velocities Using Multi-slit Spectroscopy Cat Wu Thesis Proposal, Fall 2009 Astronomy Department New Mexico State University Outline Diffuse ionized gas; galaxy halos Origin of halo galactic fountain
Chapter 25: Galaxy Clusters and the Structure of the Universe
Chapter 25: Galaxy Clusters and the Structure of the Universe Distribution of galaxies Evolution of galaxies Study of distant galaxies Distance derived from redshift Hubble s constant age of the Universe:
Star Formation Indicators
Star Formation Indicators Calzetti 2007 astro-ph/0707.0467 Brinchmann et al. 2004 MNRAS 351, 1151 SFR indicators in general! SFR indicators are defined from the X ray to the radio! All probe the MASSIVE