|
| | | | |
| | | |
| Stat |
Members: 3645
Articles: 2'504'928
Articles rated: 2609
25 April 2024 |
|
| | | | |
|
Article overview
| |
|
|
The Bursty Star Formation Histories of Low-mass Galaxies at $0.4<z<1$ Revealed by Star Formation Rates Measured from FUV and H$eta$ | | Yicheng Guo
; Marc Rafelski
; S. M. Faber
; David C. Koo
; Mark R. Krumholz
; Jonathan R. Trump
; S. P. Willner
; Ricardo Amorín
; Guillermo Barro
; Eric F. Bell
; Jonathan P. Gardner
; Eric Gawiser
; Nimish P. Hathi
; Anton M. Koekemoer
; Camilla Pacifici
; Pablo G. Pérez-González
; Swara Ravindranath
; Naveen Reddy
; Harry I. Teplitz
; Hassen Yesuf
; | | Date: |
18 Apr 2016 | | 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
FUV (1500 AA) and H$eta$ (FUV--to--H$eta$ ratio). Our sample contains 164
galaxies down to stellar mass (M*) of $10^{8.5} M_odot$ in the CANDELS GOODS-N
region, where TKRS Keck/DEIMOS spectroscopy and HST/WFC3 F275W images from
CANDELS and HDUV are available. When the ratio of FUV- and H$eta$-derived
SFRs is measured, dust extinction correction is negligible (except for very
dusty galaxies) with the Calzetti attenuation curve. The FUV--to--H$eta$
ratio of our sample increases with the decrease of M* and SFR. The median ratio
is $sim$1 at M* $sim 10^{10} M_odot$ (or SFR = 20 $M_odot$/yr) and
increases to $sim$1.6 at M* $sim 10^{8.5} M_odot$ (or SFR $sim 0.5
M_odot$/yr). At M* $< 10^{9.5} M_odot$, our median FUV--to--H$eta$ ratio is
higher than that of local galaxies at the same M*, implying a redshift
evolution. Bursty SFH on a timescale of $sim$10 Myr on galactic scales
provides a plausible explanation of our results, and the importance of the
burstiness increases as M* decreases. Due to sample selection effects, our
FUV--to--H$eta$ ratio may be a lower 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. | | Source: | arXiv, 1604.5314 | | Services: | Forum | Review | PDF | Favorites | |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
browser Mozilla/5.0 AppleWebKit/537.36 (KHTML, like Gecko; compatible; ClaudeBot/1.0; +claudebot@anthropic.com)
|
| |
|
|
|
|
News, job offers and information for researchers and scientists:
| |
REGISTER