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ALFALFA Hα Reveals How Galaxies Use Their Hi Fuel

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

Anne Jaskot ,
Sally Oey ,
John Salzer ,
Angie Van Sistine ,
Eric Bell  and
Martha Haynes
Anne Jaskot
Affiliation:
Dept. of Astronomy, Smith College, Northampton, MA 01063, USA email: ajaskot@smith.edu
Sally Oey
Affiliation:
Dept. of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA
John Salzer
Affiliation:
Dept. of Astronomy, Indiana University, Bloomington, IN 47405, USA
Angie Van Sistine
Affiliation:
Dept. of Astronomy, Indiana University, Bloomington, IN 47405, USA
Eric Bell
Affiliation:
Dept. of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA
Martha Haynes
Affiliation:
Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14853, USA
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Abstract

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Atomic hydrogen traces the raw material from which molecular clouds and stars form. With 565 galaxies from the ALFALFA Hα survey, a statistically complete subset of the ALFALFA survey, we examine the processes that affect galaxies' abilities to access and consume their Hi gas. On galaxy-wide scales, Hi gas fractions correlate only weakly with instantaneous specific star formation rates (sSFRs) but tightly with galaxy color. We show that a connection between dust and Hi content, arising from the fundamental mass-metallicity-Hi relation, leads to this tight color correlation. We find that disk galaxies follow a relation between stellar surface density and Hi depletion time, consistent with a scenario in which higher mid-plane pressure leads to more efficient molecular cloud formation from Hi. In contrast, spheroids show no such trend. Starbursts, identified by Hα equivalent width, do not show enhanced Hi gas fractions relative to similar mass non-starburst galaxies. The starbursts' shorter Hi depletion times indicate more efficient consumption of Hi, and galaxy interactions drive this enhanced star formation efficiency in several starbursts. Interestingly, the most disturbed starbursts show greater enhancements in Hi gas fraction, which may indicate an excess of Hi at early merger stages. At low galaxy stellar masses, the triggering mechanism for starbursts is less clear; the high scatter in efficiency and sSFR among low-mass galaxies may result from periodic bursts. We find no evidence for depleted Hi reservoirs in starbursts, which suggests that galaxies may maintain sufficient Hi to fuel multiple starburst episodes.

Keywords

galaxies: evolutiongalaxies: generalgalaxies: interactionsgalaxies: ISMgalaxies: starburstradio lines: galaxiessurveys
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , E37
Copyright
Copyright © International Astronomical Union 2016 

References

Blitz, L., & Rosolowsky, E. 2006, ApJ, 650, 933 Google Scholar
Bothwell, M.S., Maiolino, R., Kennicutt, R., et al. 2013, MNRAS, 433, 1425 Google Scholar
Calzetti, D., Armus, L., Bohlin, R.C., et al. 2000, ApJ, 533, 682 CrossRefGoogle Scholar
Cardelli, J.A., Clayton, G.C., & Mathis, J. S. 1989, ApJ, 345, 245 CrossRefGoogle Scholar
Catinella, B., Schiminovich, D., Kauffmann, G., et al. 2010, MNRAS, 403, 683 Google Scholar
Giovanelli, R., Haynes, M.P., Kent, B.R., et al. 2005, AJ, 130, 2598 Google Scholar
Huang, S., Haynes, M.P., Giovanelli, R., & Brinchmann, J. 2012, ApJ, 756, 113 Google Scholar
Jaskot, A.E., Oey, M.S., Salzer, J.J., et al. 2015, ApJ, 808, 66 Google Scholar
Simard, L., Mendel, J.T., Patton, D.R., et al. 2011, ApJS, 196, 11 Google Scholar
Van Sistine, A., Salzer, J.J., Sugden, A., et al. 2015, ApJ, SubmittedGoogle Scholar
Wen, X.-Q., Wu, H., Zhu, Y.-N., et al. 2014, MNRAS, 438, 97 Google Scholar