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HISTORY OF GALAXY INTERACTIONS AND THEIR IMPACT ON STAR FORMATION OVER THE LAST 7 Gyr FROM GEMS
Jogee, Shardha1; Miller, Sarah H.1,2; Penner, Kyle1,3; Skelton, Rosalind E.4; Conselice, Christopher J.5; Somerville, Rachel S.4; Bell, Eric F.4; Zheng, Xian Zhong6; Rix, Hans-Walter4; Robaina, Aday R.4; Barazza, Fabio D.7; Barden, Marco8; Borch, Andrea4; Beckwith, Steven V. W.9; Caldwell, John A. R.10; Peng, Chien Y.11; Heymans, Catherine12; McIntosh, Daniel H.13; Haeussler, Boris4; Jahnke, Knud4; Meisenheimer, Klaus4; Sanchez, Sebastian F.14; Wisotzki, Lutz15; Wolf, Christian2; Papovich, Casey16,17
2009-06-01
Source PublicationASTROPHYSICAL JOURNAL
ISSN0004-637X
Volume697Issue:2Pages:1971-1992
AbstractWe perform a comprehensive estimate of the frequency of galaxy mergers and their impact on star formation over z similar to 0.24-0.80 (lookback time T(b) similar to 3-7 Gyr) using similar to 3600 (M >= 1 x 10(9) M(circle dot)) galaxies with GEMS Hubble Space Telescope, COMBO-17, and Spitzer data. Our results are as follows. (1) Among similar to 790 high-mass (M >= 2.5 x 10(10) M(circle dot)) galaxies, the visually based merger fraction over z similar to 0.24-0.80, ranges from 9% +/- 5% to 8% +/- 2%. Lower limits on the major merger and minor merger fraction over this interval range from 1.1% to 3.5%, and 3.6% to 7.5%, respectively. This is the first, albeit approximate, empirical estimate of the frequency of minor mergers over the last 7 Gyr. Assuming a visibility timescale of similar to 0.5 Gyr, it follows that over T(b) similar to 3-7 Gyr, similar to 68% of high-mass systems have undergone a merger of mass ratio > 1/10, with similar to 16%, 45%, and 7% of these corresponding respectively to major, minor, and ambiguous "major or minor" mergers. The average merger rate is similar to a few x 10(-4) galaxies Gyr(-1) Mpc(-3). Among similar to 2840 blue-cloud galaxies of mass M >= 1.0 x 10(9) M(circle dot), similar results hold. (2) We compare the empirical merger fraction and merger rate for high-mass galaxies to three. cold dark matter-based models: halo occupation distribution models, semi-analytic models, and hydrodynamic SPH simulations. We find qualitative agreement between observations and models such that the (major+minor) merger fraction or rate from different models bracket the observations, and show a factor of 5 dispersion. Near-future improvements can now start to rule out certain merger scenarios. (3) Among similar to 3698 M >= 1.0 x 10(9) M(circle dot) galaxies, we find that the mean star formation rate (SFR) of visibly merging systems is only modestly enhanced compared to non-interacting galaxies over z similar to 0.24-0.80. Visibly merging systems only account for a small fraction (< 30%) of the cosmic SFR density over T(b) similar to 3-7 Gyr. This complements the results of Wolf et al. over a shorter time interval of T(b) similar to 6.2-6.8 Gyr, and suggests that the behavior of the cosmic SFR density over the last 7 Gyr is predominantly shaped by non-interacting galaxies.
KeywordGalaxies: Evolution Galaxies: Fundamental Parameters Galaxies: Kinematics And Dynamics Galaxies: Structure
Subject AreaAstronomy & Astrophysics
WOS HeadingsScience & Technology ; Physical Sciences
DOI10.1088/0004-637X/697/2/1971
WOS KeywordDEEP-FIELD-SOUTH ; DARK-MATTER HALOES ; MULTIBAND IMAGING PHOTOMETER ; ACTIVE GALACTIC NUCLEI ; FRANCE REDSHIFT SURVEY ; POINT-SOURCE CATALOGS ; INITIAL MASS FUNCTION ; ELLIPTIC GALAXIES ; FORMATION RATES ; STELLAR MASS
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000266159500080
Citation statistics
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/1587
Collection星系中的恒星形成研究团组
Affiliation1.Univ Texas Austin, Dept Astron, Austin, TX 78712 USA
2.Univ Oxford, Oxford OX1 3RH, England
3.Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA
4.Max Planck Inst Astron, D-69117 Heidelberg, Germany
5.Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England
6.Acad Sinica, Purple Mt Observ, Nanjing 210008, Peoples R China
7.Ecole Polytech Fed Lausanne, Astrophys Lab, CH-1290 Sauverny, Switzerland
8.Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria
9.Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
10.Univ Texas McDonald Observ, Ft Davis, TX 79734 USA
11.Herzberg Inst Astrophys, NRC, Victoria, BC, Canada
12.Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland
13.Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA
14.CSIC MPG, Calar Alto, Ctr Astron Hispano Aleman, E-04004 Almeria, Spain
15.Astrophys Inst Potsdam, D-14482 Potsdam, Germany
16.Texas A&M Univ, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA
17.Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA
Recommended Citation
GB/T 7714
Jogee, Shardha,Miller, Sarah H.,Penner, Kyle,et al. HISTORY OF GALAXY INTERACTIONS AND THEIR IMPACT ON STAR FORMATION OVER THE LAST 7 Gyr FROM GEMS[J]. ASTROPHYSICAL JOURNAL,2009,697(2):1971-1992.
APA Jogee, Shardha.,Miller, Sarah H..,Penner, Kyle.,Skelton, Rosalind E..,Conselice, Christopher J..,...&Papovich, Casey.(2009).HISTORY OF GALAXY INTERACTIONS AND THEIR IMPACT ON STAR FORMATION OVER THE LAST 7 Gyr FROM GEMS.ASTROPHYSICAL JOURNAL,697(2),1971-1992.
MLA Jogee, Shardha,et al."HISTORY OF GALAXY INTERACTIONS AND THEIR IMPACT ON STAR FORMATION OVER THE LAST 7 Gyr FROM GEMS".ASTROPHYSICAL JOURNAL 697.2(2009):1971-1992.
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