A Survey of Star-Forming Galaxies in the z=1.4-2.5 `Redshift Desert': Overview

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dc.creatorSteidel, C. C.
dc.creatorShapley, A. E.
dc.creatorPettini, M.
dc.creatorAdelberger, K. L.
dc.creatorErb, D. K.
dc.creatorReddy, N. A.
dc.creatorHunt, M. P.
dc.date2004-01-21
dc.date.accessioned2026-07-07T10:27:09Z
dc.date.available2026-07-07T10:27:09Z
dc.descriptionWe present the first results of a large-scale survey, using the UV/blue sensitive LRIS-B spectrograph on the Keck I telescope, of galaxies in the redshift interval 1.4<z<2.5, often called the `redshift desert' because of historical difficulties in spectroscopically identifying galaxies in that range. We introduce two samples of star forming galaxies, `BX' galaxies at <z>=2.20+/-0.32 and `BM' galaxies at <z>=1.70+/-0.34; currently we have spectroscopically confirmed 749 of the former and 114 of the latter. We also present initial results of deep near-IR photometry and spectroscopy, from which we show that z~2 galaxies are significantly redder in their optical/IR colors compared to similarly UV-selected galaxies at z~3, but that the characteristics of their galaxy-scale outflows are quite similar. We illustrate by example the information which can be deduced on the stellar populations, metallicities, and kinematics of `redshift desert' galaxies from easily accessible rest-frame far-UV and rest-frame optical spectra. Far from being hostile to observations, the universe at z~2 is uniquely suited to providing information on the astrophysics of star-forming galaxies and the intergalactic medium, and the relationship between the two [abridged].
dc.descriptionTo appear in ApJ, April 2004. 16 pages, uses emulateapj
dc.identifierhttps://arxiv.org/abs/astro-ph/0401439
dc.identifierhttp://arxiv.org/abs/astro-ph/0401439
dc.identifierAstrophys.J.604:534-550,2004
dc.identifierdoi:10.1086/381960
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/177072
dc.subjectAstrophysics
dc.titleA Survey of Star-Forming Galaxies in the z=1.4-2.5 `Redshift Desert': Overview
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