@gpkulkarni

Luminous Lyman-alpha Emitters with Very Blue UV-continuum Slopes at Redshift 5.7 <= z <= 6.6

, , , , , , and . (2020)cite arxiv:2002.02028Comment: Published in ApJ on 2020 Feb 1; Authors' version (9 pages); See published version at https://iopscience.iop.org/article/10.3847/1538-4357/ab64ea.

Abstract

We study six luminous Lyman-alpha emitters (LAEs) with very blue rest-frame UV continua at $5.7z 6.6$. These LAEs have previous HST and Spitzer IRAC observations. Combining our newly acquired HST images, we find that their UV-continuum slopes $\beta$ are in a range of $-3.4-2.6$. Unlike previous, tentative detections of $-3$ in photometrically selected, low-luminosity galaxies, our LAEs are spectroscopically confirmed and luminous ($M_UV<-20$ mag). We model their broadband spectral energy distributions (SEDs), and find that two $\beta\simeq-2.6\pm0.2$ galaxies can be well fitted with young and dust-free stellar populations. However, it becomes increasingly difficult to fit bluer galaxies. We explore further interpretations by including non-zero LyC escape fraction $f_esc$, very low metallicities, and/or AGN contributions. Assuming $f_esc\simeq0.2$, we achieve the bluest slopes $\beta\simeq-2.7$ when nebular emission is considered. This can nearly explain the SEDs of two galaxies with $\beta\simeq-2.8$ and --2.9 ($\sigma_\beta=0.15$). Larger $f_esc$ values and very low metallicities are not favored by the strong nebular line emission (evidenced by the IRAC flux) or the observed (IRAC 1 - IRAC 2) color. Finally, we find that the $\beta\simeq-2.9$ galaxy can potentially be well explained by the combination of a very young population with a high $f_\rm esc$ ($\ge0.5$) and an old, dusty population. We are not able to produce two $-3.4 \pm0.4$ galaxies. Future deep spectroscopic observations are needed to fully understand these galaxies.

Description

Luminous Lyman-alpha Emitters with Very Blue UV-continuum Slopes at Redshift 5.7 <= z <= 6.6

Links and resources

URL:
BibTeX key:
jiang2020luminous
search on:

Comments and Reviews  
(0)

There is no review or comment yet. You can write one!

Tags


Cite this publication