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Title: THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z {approx} 1.4 AND {approx}1

Abstract

We present an analysis of the Mg II {lambda}{lambda}2796, 2803 and Fe II {lambda}{lambda}2586, 2600 absorption line profiles in co-added spectra of 468 galaxies at 0.7 < z < 1.5. The galaxy sample, drawn from the Team Keck Treasury Redshift Survey of the GOODS-N field, has a range in stellar mass (M{sub *}) comparable to that of the sample at z {approx} 1.4 analyzed in a similar manner by Weiner et al. (W09), but extends to lower redshifts and has specific star formation rates which are lower by {approx}0.6 dex. We identify outflows of cool gas from the Doppler shift of the Mg II absorption lines and find that the equivalent width (EW) of absorption due to outflowing gas increases on average with M{sub *} and star formation rate (SFR). We attribute the large EWs measured in spectra of the more massive, higher-SFR galaxies to optically thick absorbing clouds having large velocity widths. The outflows have hydrogen column densities N(H) {approx}> 10{sup 19.4} cm{sup -2} and extend to velocities of {approx}500 km s{sup -1}. While galaxies with SFR>10 M{sub sun} yr{sup -1} host strong outflows in both this and the W09 sample, we do not detect outflows in lower-SFR (i.e.,more » log M{sub *}/M{sub sun} {approx}< 10.5) galaxies at lower redshifts. Using a simple galaxy evolution model that assumes exponentially declining SFRs, we infer that strong outflows persist in galaxies with log M{sub *}/M{sub sun} > 10.5 as they age between z = 1.4 and z {approx} 1, presumably because of their high absolute SFRs. Finally, our spectral analysis, combined with high-resolution Hubble Space Telescope/Advanced Camera for Surveys imaging, weakly suggests that outflow absorption strength increases with galaxy SFR surface density.« less

Authors:
; ;  [1];  [2];  [3];  [4]
  1. University of California Observatories, University of California, Santa Cruz, CA 95064 (United States)
  2. Steward Observatory, 933 North Cherry Street, University of Arizona, Tucson, AZ 85721 (United States)
  3. Department of Physics, University of California, Santa Barbara, CA 93106 (United States)
  4. Department of Physics, University of California, San Diego, CA 92093 (United States)
Publication Date:
OSTI Identifier:
21457076
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 719; Journal Issue: 2; Other Information: DOI: 10.1088/0004-637X/719/2/1503; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; DOPPLER EFFECT; GALACTIC EVOLUTION; GALAXIES; HYDROGEN; RED SHIFT; SPECTRA; STARS; SURFACES; ELEMENTS; EVOLUTION; NONMETALS; SORPTION

Citation Formats

Rubin, Kate H. R., Koo, David C, Prochaska, J Xavier, Weiner, Benjamin J, Martin, Crystal L, Coil, Alison L, and Newman, Jeffrey A., E-mail: rubin@ucolick.or. THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z {approx} 1.4 AND {approx}1. United States: N. p., 2010. Web. doi:10.1088/0004-637X/719/2/1503.
Rubin, Kate H. R., Koo, David C, Prochaska, J Xavier, Weiner, Benjamin J, Martin, Crystal L, Coil, Alison L, & Newman, Jeffrey A., E-mail: rubin@ucolick.or. THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z {approx} 1.4 AND {approx}1. United States. https://doi.org/10.1088/0004-637X/719/2/1503
Rubin, Kate H. R., Koo, David C, Prochaska, J Xavier, Weiner, Benjamin J, Martin, Crystal L, Coil, Alison L, and Newman, Jeffrey A., E-mail: rubin@ucolick.or. 2010. "THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z {approx} 1.4 AND {approx}1". United States. https://doi.org/10.1088/0004-637X/719/2/1503.
@article{osti_21457076,
title = {THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z {approx} 1.4 AND {approx}1},
author = {Rubin, Kate H. R. and Koo, David C and Prochaska, J Xavier and Weiner, Benjamin J and Martin, Crystal L and Coil, Alison L and Newman, Jeffrey A., E-mail: rubin@ucolick.or},
abstractNote = {We present an analysis of the Mg II {lambda}{lambda}2796, 2803 and Fe II {lambda}{lambda}2586, 2600 absorption line profiles in co-added spectra of 468 galaxies at 0.7 < z < 1.5. The galaxy sample, drawn from the Team Keck Treasury Redshift Survey of the GOODS-N field, has a range in stellar mass (M{sub *}) comparable to that of the sample at z {approx} 1.4 analyzed in a similar manner by Weiner et al. (W09), but extends to lower redshifts and has specific star formation rates which are lower by {approx}0.6 dex. We identify outflows of cool gas from the Doppler shift of the Mg II absorption lines and find that the equivalent width (EW) of absorption due to outflowing gas increases on average with M{sub *} and star formation rate (SFR). We attribute the large EWs measured in spectra of the more massive, higher-SFR galaxies to optically thick absorbing clouds having large velocity widths. The outflows have hydrogen column densities N(H) {approx}> 10{sup 19.4} cm{sup -2} and extend to velocities of {approx}500 km s{sup -1}. While galaxies with SFR>10 M{sub sun} yr{sup -1} host strong outflows in both this and the W09 sample, we do not detect outflows in lower-SFR (i.e., log M{sub *}/M{sub sun} {approx}< 10.5) galaxies at lower redshifts. Using a simple galaxy evolution model that assumes exponentially declining SFRs, we infer that strong outflows persist in galaxies with log M{sub *}/M{sub sun} > 10.5 as they age between z = 1.4 and z {approx} 1, presumably because of their high absolute SFRs. Finally, our spectral analysis, combined with high-resolution Hubble Space Telescope/Advanced Camera for Surveys imaging, weakly suggests that outflow absorption strength increases with galaxy SFR surface density.},
doi = {10.1088/0004-637X/719/2/1503},
url = {https://www.osti.gov/biblio/21457076}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 719,
place = {United States},
year = {Fri Aug 20 00:00:00 EDT 2010},
month = {Fri Aug 20 00:00:00 EDT 2010}
}