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26 April 2024 |
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The MOSDEF Survey: Dissecting the star-formation rate vs. stellar mass relation using H$alpha$ and H$eta$ emission lines at z ~ 2 | | Irene Shivaei
; Naveen A. Reddy
; Alice E. Shapley
; Mariska Kriek
; Brian Siana
; Bahram Mobasher
; Alison L. Coil
; William R. Freeman
; Ryan Sanders
; Sedona H. Price
; Laura de Groot
; Mojegan Azadi
; | | Date: |
10 Jul 2015 | | Abstract: | We present results on the SFR-$M_*$ relation (i.e., the "main sequence")
among star-forming galaxies at $1.37leq z leq2.61$ using the MOSFIRE Deep
Evolution Field (MOSDEF) survey. Based on a sample of 261 star-forming galaxies
with observations of H$alpha$ and H$eta$ emission lines, we have estimated
robust dust-corrected instantaneous star-formation rates (SFRs) over a large
dynamic range in stellar mass ($sim 10^{9.0}-10^{11.5}M_odot$). We find a
tight correlation between SFR(H$alpha$) and $M_*$ with an intrinsic scatter of
0.36 dex, 0.05 dex larger than that of UV-based SFRs. This increased scatter is
consistent with predictions from numerical simulations of 0.03 - 0.1 dex, and
is attributed to H$alpha$ more accurately tracing SFR variations. The slope of
the $log( ext{SFR})-log(M_*)$ relation, using SFR(H$alpha$), at $1.4<
z<2.6$ and over the stellar mass range of $10^{9.5}$ to $10^{11.5}M_odot$ is
$0.65pm 0.09$. We find that different assumptions for the dust correction,
such as using the stellar $E(B-V)$ with a Calzetti et al. (2000) attenuation
curve, as well as the sample biases against red and dusty star-forming galaxies
at large masses, could yield steeper slopes. Moreover, not correcting the
Balmer emission line fluxes for the underlying Balmer absorption results in
overestimating the dust extinction of H$alpha$ and SFR(H$alpha$) at the
high-mass end by 2.1 (2.5) at $10^{10.6} M_odot$ ($10^{11.1} M_odot$) and
artificially increases the slope of the main-sequence. The shallower
main-sequence slope found here compared to that of galaxy evolution simulations
may be indicative of different feedback processes governing the low- and/or
high-mass end of the main sequence. | | Source: | arXiv, 1507.3017 | | Services: | Forum | Review | PDF | Favorites | |
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