Panchromatic Study of the First Galaxies with Large ALMA Programs

Abstract

Thanks to deep optical to near-IR imaging and spectroscopy, significant progress is made in characterizing the rest-frame UV to optical properties of galaxies in the early universe (z > 4). Surveys with Hubble, Spitzer, and ground-based facilities (Keck, Subaru, and VLT) provide spectroscopic and photometric redshifts, measurements of the spatial structure, stellar masses, and optical emission lines for large samples of galaxies. Recently, the Atacama Large (Sub) Millimeter Array (ALMA) has become a major player in pushing studies of high redshift galaxies to far-infrared wavelengths, hence making panchromatic surveys over many orders of frequencies possible. While past studies focused mostly on bright sub-millimeter galaxies, the sensitivity of ALMA now enables surveys like ALPINE, which focuses on measuring the gas and dust properties of a large sample of normal main-sequence galaxies at z > 4. Combining observations across different wavelengths into a single, panchromatic picture of galaxy formation and evolution is currently and in the future an important focus of the astronomical community.

4 pages, 2 figures. Submitted to Proceedings IAU Symposium No. 341, 2018

References in corpus (6)

• Cosmic Star Formation History
• The Cosmic Evolution Survey (COSMOS) -- Overview
• UV Luminosity Functions at redshifts z~4 to z~10: 10000 Galaxies from HST Legacy Fields
• The DEIMOS 10k spectroscopic survey catalog of the COSMOS field
• ALMA Imaging of Gas and Dust in a Galaxy Protocluster at Redshift 5.3: [CII] Emission in "Typical" Galaxies and Dusty Starbursts ~1 Billion Years after the Big Bang
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Cited by in corpus (5)

• The ALPINE-ALMA [CII] survey: Star-formation-driven outflows and circumgalactic enrichment in the early Universe
• ALMA Characterises the Dust Temperature of z ~ 5.5 Star-Forming Galaxies
• The ALPINE-ALMA [CII] Survey: A Triple Merger at z~4.56
• The ALPINE-ALMA [C II] Survey: [C II]158micron Emission Line Luminosity Functions at $z\sim 4-6$
• Merging history of massive galaxies at 3<z<6