CaltechAUTHORS
  A Caltech Library Service

The Bursty Star Formation Histories of Low-mass Galaxies at 0.4 < z < 1 Revealed by Star Formation Rates Measured From Hβ and FUV

Guo, Yicheng and Rafelski, Marc and Faber, S. M. and Koo, David C. and Krumholz, Mark R. and Trump, Jonathan R. and Willner, S. P. and Amorín, Ricardo and Barro, Guillermo and Bell, Eric F. and Gardner, Jonathan P. and Gawiser, Eric and Hathi, Nimish P. and Koekemoer, Anton M. and Pacifici, Camilla and Pérez-González, Pablo G. and Ravindranath, Swara and Reddy, Naveen A. and Teplitz, Harry I. and Yesuf, Hassen (2016) The Bursty Star Formation Histories of Low-mass Galaxies at 0.4 < z < 1 Revealed by Star Formation Rates Measured From Hβ and FUV. Astrophysical Journal, 833 (1). Art. No. 37. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20161212-153959377

[img] PDF - Published Version
See Usage Policy.

1265Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20161212-153959377

Abstract

We investigate the burstiness of star formation histories (SFHs) of galaxies at 0.4 < z < 1 by using the ratio of star formation rates (SFRs) measured from Hβ and FUV (1500 Å) (Hβ-to-FUV ratio). Our sample contains 164 galaxies down to stellar mass (M_*) of 10^(8.5) M_⊙ in the CANDELS GOODS-N region, where Team Keck Redshift Survey Keck/DEIMOS spectroscopy and Hubble Space Telescope/WFC3 F275W images from CANDELS and Hubble Deep UV Legacy Survey are available. When the ratio of Hβ- and FUV-derived SFRs is measured, dust extinction correction is negligible (except for very dusty galaxies) with the Calzetti attenuation curve. The Hβ-to-FUV ratio of our sample increases with M_* and SFR. The median ratio is ~0.7 at M_* ~ 10^(8.5) M_⊙ (or SFR ~ 0.5 M_⊙ yr^(−1)) and increases to ~1 at M_* ~ 10^(10) M_⊙ (or SFR ~ 10 M_⊙ yr^(−1)). At M_* < 10^(9.5) M_⊙, our median Hβ-to-FUV ratio is lower than that of local galaxies at the same M_*, implying a redshift evolution. Bursty SFH on a timescale of a few tens of megayears on galactic scales provides a plausible explanation for our results, and the importance of the burstiness increases as M_* decreases. Due to sample selection effects, our Hβ-to-FUV ratio may be an upper limit of the true value of a complete sample, which strengthens our conclusions. Other models, e.g., non-universal initial mass function or stochastic star formation on star cluster scales, are unable to plausibly explain our results.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/1538-4357/833/1/37DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/833/1/37PublisherArticle
https://arxiv.org/abs/1604.05314arXivDiscussion Paper
ORCID:
AuthorORCID
Guo, Yicheng0000-0003-2775-2002
Rafelski, Marc0000-0002-9946-4731
Faber, S. M.0000-0003-4996-214X
Koo, David C.0000-0003-3385-6799
Krumholz, Mark R.0000-0003-3893-854X
Willner, S. P.0000-0002-9895-5758
Barro, Guillermo0000-0001-6813-875X
Hathi, Nimish P.0000-0001-6145-5090
Koekemoer, Anton M.0000-0002-6610-2048
Pacifici, Camilla0000-0003-4196-0617
Pérez-González, Pablo G.0000-0003-4528-5639
Reddy, Naveen A.0000-0001-9687-4973
Teplitz, Harry I.0000-0002-7064-5424
Additional Information:© 2016. The American Astronomical Society. Received 2016 April 15; revised 2016 September 26; accepted 2016 October 2; published 2016 December 6. We thank the anonymous referee for the valuable and constructive comments, which improve this article. Y.G., S.M.F., D.C.K., G.B., and H.Y. acknowledge support from NSF Grant AST-0808133. Support for Program HST-GO-12060 and HST-AR-13891 were provided by NASA through a grant from the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. MR acknowledges support from an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center. Facilities: HST (WFC3) - , Keck (DEIMOS) - .
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NSFAST-0808133
NASANAS5-26555
NASA Postdoctoral ProgramUNSPECIFIED
NASA Hubble FellowshipUNSPECIFIED
Subject Keywords:galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: starburst; galaxies: star formation
Issue or Number:1
Record Number:CaltechAUTHORS:20161212-153959377
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20161212-153959377
Official Citation:Yicheng Guo et al 2016 ApJ 833 37
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72735
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:12 Dec 2016 23:55
Last Modified:09 Mar 2020 13:19

Repository Staff Only: item control page