Evolution of Luminous Galaxy Pairs out to z=1.2 in the HST/ACS COSMOS Field Jeyhan Kartaltepe, IfA, Hawaii Dave Sanders, IfA, Hawaii Nick Scoville, Caltech.

Slides:



Advertisements
Similar presentations
Evolution of clustering in COSMOS: a progress report Luigi Guzzo (INAF, Milano) N. Scoville, O. Le Fevre, A. Pollo, B. Meneux, & COSMOS Team.
Advertisements

207th AAS Meeting Washington D.C., 8-13 January The Spitzer SWIRE Legacy Program Spitzer Wide-Area Infrared Extragalactic Survey Mari Polletta (UCSD)
15 years of science with Chandra– Boston 20141/16 Faint z>4 AGNs in GOODS-S looking for contributors to reionization Giallongo, Grazian, Fiore et al. (Candels.
Hierarchical Clustering Leopoldo Infante Pontificia Universidad Católica de Chile Reunión Latinoamericana de Astronomía Córdoba, septiembre 2001.
Clusters, Galaxies and the COSMOS J Berian James (IfA Edinburgh), John Peacock, Alexis Finoguenov, Henry Joy McCracken & Gigi Guzzo for the COSMOS collaboration.
COSMOS Kyoto meeting May 2005 Obscured AGN in the COSMOS field Andrea Comastri (INAF – Bologna) on behalf of the XMM-COSMOS team.
The multiwavelength surveys of the ELAIS-S1 and GOODS fields Fabrizio Fiore & M. Brusa, A. Comastri, C. Feruglio, A. Fontana, A. Grazian, F. La Franca,
Clustering in the Cosmic Evolution Survey (COSMOS) Luigi Guzzo (INAF, Milano) N. Scoville, A. El Zant, O. Le Fevre, B. Meneux, A. Pollo & COSMOS Team (Fundamental.
Luminosity Density of Star- Forming Galaxies Giavalisco et al Presented by Brandon Patel.
July 7, 2008SLAC Annual Program ReviewPage 1 Weak Lensing of The Faint Source Correlation Function Eric Morganson KIPAC.
Redshift Evolution of the Correlation Function Peter Capak J. Blazek, D. Sanders, I. Szapudi, N. Scoville Kyoto, May 23, 2005.
Evolution of Luminous Galaxy Pairs out to z=1.2 in the HST/ACS COSMOS Field Jeyhan Kartaltepe, IfA, Hawaii Dave Sanders, IfA, Hawaii Nick Scoville, Caltech.
Weak-Lensing selected, X-ray confirmed Clusters and the AGN closest to them Dara Norman NOAO/CTIO 2006 November 6-8 Boston Collaborators: Deep Lens Survey.
Growth of Structure Measurement from a Large Cluster Survey using Chandra and XMM-Newton John R. Peterson (Purdue), J. Garrett Jernigan (SSL, Berkeley),
AGN and Quasar Clustering at z= : Results from the DEEP2 + AEGIS Surveys Alison Coil Hubble Fellow University of Arizona Chandra Science Workshop.
Exploring the Stellar Populations of Early-Type Galaxies in the 6dF Galaxy Survey Philip Lah Honours Student h Supervisors: Matthew Colless Heath Jones.
Measuring the clustering of galaxies in COSMOS Measuring the clustering of galaxies in COSMOS Olivier Le Fèvre, LAM Why ? Why ? How ? correlation function.
The STAGES Supercluster: A challenge for semi-analytical models? Rhys Rhodes The University of Nottingham 25 th June 2008 Meghan Gray and Frazer Pearce.
Statistical Properties of Radio Galaxies in the local Universe Yen-Ting Lin Princeton University Pontificia Universidad Católica de Chile Yue Shen, Michael.
Relating Mass and Light in the COSMOS Field J.E. Taylor, R.J. Massey ( California Institute of Technology), J. Rhodes ( Jet Propulsion Laboratory) & the.
Angular clustering and halo occupation properties of COSMOS galaxies Cristiano Porciani.
Photometric Catalog I-band selected photometric catalog containing ~800,000 galaxies (I (AB) < 26 mag) in 8 bands (UBVgRizK) Star-Galaxy separation using.
March, Galaxies and structure through cosmic time Venice 2006 The AGN content of the COSMOS: the XMM-Newton view Marcella Brusa (MPE) on behalf.
Masami Ouchi (Space Telescope Science Institute) for the SXDS Collaboration Cosmic Web Made of 515 Galaxies at z=5.7 Kona 2005 Ouchi et al ApJ, 620,
NAOKI YASUDA, MAMORU DOI (UTOKYO), AND TOMOKI MOROKUMA (NAOJ) SN Survey with HSC.
How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray.
Luminosity and Mass functions in spectroscopically-selected groups at z~0.5 George Hau, Durham University Dave Wilman (MPE) Mike Balogh (Waterloo) Richard.
The Evolution of Quasars and Massive Black Holes “Quasar Hosts and the Black Hole-Spheroid Connection”: Dunlop 2004 “The Evolution of Quasars”: Osmer 2004.
Cosmic scaffolding and the growth of structure Richard Massey (CalTech ) with Jason Rhodes (JPL), David Bacon (Edinburgh), Joel Berg é (Saclay), Richard.
Culling K-band Luminous, Massive Star Forming Galaxies at z>2 X.Kong, M.Onodera, C.Ikuta (NAOJ),K.Ohta (Kyoto), N.Tamura (Durham),A.Renzini, E.Daddi (ESO),
Jeyhan S. Kartaltepe Hubble Fellow - NOAO Hubble Fellows Symposium 2012 March 7.
RADIO OBSERVATIONS IN VVDS FIELD : PAST - PRESENT - FUTURE P.Ciliegi(OABo), Marco Bondi (IRA) G. Zamorani(OABo), S. Bardelli (OABo) + VVDS-VLA collaboration.
ASTRONOMY BROWN BAG SEMINAR SWIRE Spitzer Wide – area Infra Red Extragalactic survey MARCH 17, 2009 DAVID CORLISS.
The Extremely Red Objects in the CLASH Fields The Extremely Red Galaxies in CLASH Fields Xinwen Shu (CEA, Saclay and USTC) CLASH 2013 Team meeting – September.
Testing the Shear Ratio Test: (More) Cosmology from Lensing in the COSMOS Field James Taylor University of Waterloo (Waterloo, Ontario, Canada) DUEL Edinburgh,
High redshift cluster search (SA22 field) KIAS SSG workshop Jae-Woo Kim (SNU) M. Im, S.-K. Lee & M. Hyun (SNU)
The Environmental Effect on the UV Color-Magnitude Relation of Early-type Galaxies Hwihyun Kim Journal Club 10/24/2008 Schawinski et al. 2007, ApJS 173,
D. B. Sanders Institute for Astronomy, University of Hawaii Gas-Rich Mergers and the origin of nuclear starbursts and AGN The Dusty and Molecular Universe:
Counting individual galaxies from deep mid-IR Spitzer surveys Giulia Rodighiero University of Padova Carlo Lari IRA Bologna Francesca Pozzi University.
MMT Science Symposium1 “false-color” keV X-ray image of the Bootes field Thousands of AGNs in the 9.3 square degree Bootes field * X-ray and infrared.
June 7, 2010COSMOS Team Meeting, IfA, Hawaii 1 The COSMOS Archive: Eight Years of Data Patrick L. Shopbell (Caltech), Nick Scoville (Caltech), The COSMOS.
FRI RADIO GALAXIES AT z > 1 STUDYING THE BUILDING BLOCKS OF TODAY'S MOST MASSIVE GALAXIES AND CLUSTERS Marco Chiaberge Space Telescope Science Institute.
Revealing X-ray obscured Quasars in SWIRE sources with extreme MIR/O Giorgio Lanzuisi Fabrizio Fiore Enrico Piconcelli Chiara Feruglio Cristian Vignali.
Naoyuki Tamura (University of Durham) The Universe at Redshifts from 1 to 2 for Early-Type Galaxies ~ Unveiling “Build-up Era” with FMOS ~
Major dry-merger rate and extremely massive major dry-mergers of BCGs Deng Zugan June 31st Taiwan.
Z-FOURGE - the FourStar Galaxy Evolution Survey Status Report at the 1.3-year mark.
Field O Stars: A Mode of Sparse Star Formation Joel Lamb Sally Oey University of Michigan.
USING LOW POWER RADIO GALAXIES AS BEACONS FOR CLUSTERS AT 1
Emission Line Galaxy Targeting for BigBOSS Nick Mostek Lawrence Berkeley National Lab BigBOSS Science Meeting Novemenber 19, 2009.
Cosmos Survey PI Scoville HST 590 orbits I-band 2 deg. 2 !
A multi-band view on the evolution of starburst merging galaxies A multi-band view on the evolution of starburst merging galaxies Yiping Wang (王益萍) Purple.
LAMOST 补充星系样本和LAMOST-SDSS星系对样本
Luminous Red Galaxies in the SDSS Daniel Eisenstein ( University of Arizona) with Blanton, Hogg, Nichol, Tegmark, Wake, Zehavi, Zheng, and the rest of.
Clustering of BzK-selected galaxies in the COSMOS field Xu KONG collaborators : A. Renzini, E. Daddi, N. Arimoto, A. Cimatti , COSMOS.
The First Galaxies in the Hubble Frontier Fields Rachana Bhatawdekar, Christopher Conselice The University of Nottingham.
The First Galaxies in the Hubble Frontier Fields Rachana Bhatawdekar, Christopher Conselice The University of Nottingham.
The Black Hole-Galaxy Evolution Connection Ezequiel Treister Einstein Fellow IfA, Hawaii IfA, Hawaii Credit: ESO/NASA, the AVO project and Paolo Padovani.
The HerMES SPIRE Submillimeter Luminosity Function Mattia Vaccari & Lucia Marchetti & Alberto Franceschini (University of Padova) Isaac Roseboom (University.
Mahdi Khadem Ferdowsi University of Mashhad Supervisors: Dr S. Arbabi (INO) Dr J. Ghanbari (FUM)
KASI Galaxy Evolution Journal Club A Massive Protocluster of Galaxies at a Redshift of z ~ P. L. Capak et al. 2011, Nature, in press (arXive: )
Speaker: Dave Wilman (MPE) Collaborators: Mike Balogh (Waterloo), George Hau, Richard Bower (Durham); John Mulchaey, Gus Oemler (Carnegie); Ray Carlberg.
Evolution of Absorption in AGN Günther Hasinger NGC 3079 Sy2 + SB Gal HST & Chandra Ringberg HE Meeting February,
The GOOD NICMOS Survey (GNS): Observing Massive Galaxies at z > 2 Christopher J. Conselice (University of Nottingham) with Asa Bluck, Ruth Gruethbacher,
9 Gyr of massive galaxy evolution Bell (MPIA), Wolf (Oxford), Papovich (Arizona), McIntosh (UMass), and the COMBO-17, GEMS and MIPS teams Baltimore 27.
The optical morphologies of the 2Jy sample of southern radio galaxies Cristina Ramos Almeida & Clive N. Tadhunter University of Sheffield.
The Mass-Dependent Role of Galaxy Mergers Kevin Bundy (UC Berkeley) Hubble Symposium March, 2009 Masataka Fukugita, Richard Ellis, Tom Targett Sirio Belli,
A Survey of Starburst Galaxies An effort to help understand the starburst phenomenon and its importance to galaxy evolution Megan Sosey & Duilia deMello.
The Evolving Luminosity Function of Red Galaxies
Jessica L. Rosenberg George Mason University
Authod: Ryan L. Sanders et al.(2018)
Presentation transcript:

Evolution of Luminous Galaxy Pairs out to z=1.2 in the HST/ACS COSMOS Field Jeyhan Kartaltepe, IfA, Hawaii Dave Sanders, IfA, Hawaii Nick Scoville, Caltech Venice, Italy 2006 March 28 Galaxies and Structures Through Cosmic Times

Background Role of mergers in galaxy formation and evolution Methods: –Morphological approach Look for irregular or peculiar galaxies Select galaxies in the process of merging Morphology difficult to classify at high z Morphological K-correction –Pair statistics Look for number of close pairs Probes galaxies that will eventually merge Linked to merger rate by timescale of process

Background Merger rates & pair evolution Parameterized as: (1+z) m & (1+z) n, respectively Previous work finds wide range of results: m, n = 0-6 Nearby Examples: The Mice & NGC 520

The COSMOS Field Previous studies –Very small samples –Small range in z The COSMOS field has –High resolution ACS images and catalog –Contiguous 2-deg 2 field – over 1 million galaxies! –Multiwavelength ground and space-based follow-up Ground based photometry catalog Photometric redshifts Ideal survey for this study!

Method: Selection of Sample Galaxies brighter than M v = (~L * ) –Allows for a complete sample out to z limit –Probes most massive galaxies Reliable photometric redshifts –Detected in 4 bands (including Ks) –I < 26 –Small errors in z (~ 0.05 out to z=1.2)  97, 066 galaxies in sample

Method: Searching for Pairs Ground based catalog –Use ground based catalog for photometric redshifts –Find pairs with a projected separation < 50 kpc in 11 redshift bins (0.1 < z < 1.2) –Misses some pairs < 3” apart due to blending ACS Catalog –Find pairs missed in ground based catalog (0.1” < sep < 0.3”) –Match to ground based catalog to get one photoz for pair –Visual inspection to remove artifacts

Method: Searching for Pairs Local Sample –Catalog of pairs from SDSS (Allam et al. 2004) –Applied same search criteria –In 0 < z < 0.1  22 pairs over 462 square degrees Random line of sight galaxy pairs –Calculate number of random pairs expected at various separations and redshifts

Results At higher separations, numbers match random Low number statistics at low redshift

12 Galaxy Pairs Selected from all z-bins, various separations Selected based on presence of obvious signs of interaction

12 Galaxy Pairs Selected from all z-bins, various separations Selected based on lack of obvious signs of interaction

Results Power law is not a good fit Evidence of LSS? What is happening at z > 0.8 Value of n can range from 4-8! Evidence for strong evolution! Total of 3,990 pairs found! Evolution ~ (1+z) n  Slope, n = 4.2 ± 0.69

Conclusion Slope, n = 4.2 ± 0.69 Power law not best fit – range n ~ 4-8 In contrast with results that show zero/weak evolution but consistent with results that show strong evolution –Differences in selection criteria? Also consistent with strong evolution of –ULIGs (n=7.2 ± 3.6: Kim & Sanders 1998) –QSOs (n~6-8: Schmidt & Green 1983)  Evidence suggests that these are formed by the merger of equal mass, ~L * galaxy pairs (e.g. Ishida 2004 & Guyon, Sanders & Stockton 2005)

Future Work Remove L * criterion for comparison Push out to higher redshifts Morphological criterion Spectroscopic redshifts  kinematic pairs Explore effects of LSS IR properties (morphologies, luminosities) –Spitzer observations –Ongoing ground based nIR observations

Acknowledgments For all of their help and support with this project, thanks go to: Peter Capak Lisa Kewley The COSMOS team