|
| | | | |
| | | |
| Stat |
Members: 3645
Articles: 2'504'928
Articles rated: 2609
26 April 2024 |
|
| | | | |
|
Article overview
| |
|
|
Galaxy inclination and the IRX-beta relation: Effects on UV star-formation rate measurements at intermediate to high redshifts | | Weichen Wang
; Susan A. Kassin
; Camilla Pacifici
; Guillermo Barro
; Alexander de la Vega
; Raymond C. Simons
; S. M. Faber
; Brett Salmon
; Henry C. Ferguson
; Pablo G. Perez-Gonzalez
; Gregory F. Snyder
; Karl D. Gordon
; Zhu Chen
; Dritan Kodra
; | | Date: |
8 Nov 2018 | | Abstract: | At intermediate and high redshifts, measurements of galaxy star-formation
rates are usually based on rest-frame ultraviolet (UV) data. A correction for
dust attenuation, A_UV, is needed for these measurements. This correction is
typically inferred from UV spectral slopes (beta) using an equation known as
"Meurer’s Relation." In this paper, we study this relation at a redshift of 1.5
using images and photometric measurements in the rest-frame UV (HST) through
mid-infrared (Spitzer). It is shown that massive star-forming galaxies (above
10^10 Msun) have dust corrections that are dependent on their inclination to
the line-of-sight. Edge-on galaxies have higher A_UV and infrared excess
(IRX=L(IR)/L(UV)) than face-on galaxies at a given beta. Interestingly, dust
corrections for low-mass star-forming galaxies do not depend on inclination.
This is likely because more massive galaxies have more disk-like
shapes/kinematics, while low-mass galaxies are more prolate and have more
disturbed kinematics. To account for an inclination-dependent dust correction,
a modified Meurer’s Relation is derived: A_UV=4.43+1.99 beta - 1.73 (b/a-0.67),
where b/a is the galaxy axis ratio. This inclination-dependence of A_UV can be
explained by a two-component model of the dust distribution inside galaxies. In
such a model, the dust attenuation of edge-on galaxies has a higher
contribution from a "mixture" component (dust uniformly mixed with stars in the
diffuse interstellar medium), and a lower contribution from a "birth cloud"
component (near-spherical dust shells surrounding young stars in H II regions)
than that of face-on galaxies. The difference is caused by the larger
path-lengths through disks at higher inclinations. | | Source: | arXiv, 1811.3671 | | 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