Kavli Affiliate: Luis C. Ho
| First 5 Authors: Taehyun Kim, Minjin Kim, Luis C. Ho, Yang A. Li, Woong-Seob Jeong
| Summary:
Future satellite missions are expected to perform all-sky surveys, thus
providing the entire sky near-infrared spectral data and consequently opening a
new window to investigate the evolution of galaxies. Specifically, the infrared
spectral data facilitate the precise estimation of stellar masses of numerous
low-redshift galaxies. We utilize the synthetic spectral energy distribution
(SED) of 2853 nearby galaxies drawn from the DustPedia (435) and Stripe 82
regions (2418). The stellar mass-to-light ratio ($M_*/L$) estimation accuracy
over a wavelength range of $0.75-5.0$ $mu$m is computed through the SED
fitting of the multi-wavelength photometric dataset, which has not yet been
intensively explored in previous studies. We find that the scatter in $M_*/L$
is significantly larger in the shorter and longer wavelength regimes due to the
effect of the young stellar population and the dust contribution, respectively.
While the scatter in $M_*/L$ approaches its minimum ($sim0.10$ dex) at
$sim1.6$ $mu$m, it remains sensitive to the adopted star formation history
model. Furthermore, $M_*/L$ demonstrates weak and strong correlations with the
stellar mass and the specific star formation rate (SFR), respectively. Upon
adequately correcting the dependence of $M_*/L$ on the specific SFR, the
scatter in the $M_*/L$ further reduces to $0.02$ dex at $sim1.6$ $mu$m. This
indicates that the stellar mass can be estimated with an accuracy of $sim0.02$
dex with a prior knowledge of SFR, which can be estimated using the infrared
spectra obtained with future survey missions.
| Search Query: ArXiv Query: search_query=au:”Luis C. Ho”&id_list=&start=0&max_results=3