Abstract

We combine Hubble Space Telescope (HST)/Wide Field Camera3 (WFC3) imaging and G141 grism observations from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) and 3D-HST surveys to produce a catalog of grism spectroscopic redshifts for galaxies in the CANDELS/GOODS-South field. The WFC3/G141 grism spectra cover a wavelength range of 1.1 ≼ λ ≼ 1.7 μm with a resolving power of R ~ 130 for point sources, thus providing rest-frame optical spectra for galaxies out to z ~ 3.5. The catalog is selected in the H-band (F160W) and includes both galaxies with and without previously published spectroscopic redshifts. Grism spectra are extracted for all H-band detected galaxies with H ≼ 24 and a CANDELS photometric redshift zphot ≽ 0.6. The resulting spectra are visually inspected to identify emission lines, and redshifts are determined using cross-correlation with empirical spectral templates. To establish the accuracy of our redshifts, we compare our results against high-quality spectroscopic redshifts from the literature. Using a sample of 411 control galaxies, this analysis yields a precision of σNMAD = 0.0028 for the grism-derived redshifts, which is consistent with the accuracy reported by the 3D-HST team. Our final catalog covers an area of 153 arcmin2 and contains 1019 redshifts for galaxies in GOODS-S. Roughly 60% (608/1019) of these redshifts are for galaxies with no previously published spectroscopic redshift. These new redshifts span a range of 0.677 ≼ z ≼ 3.456 and have a median redshift of z = 1.282. The catalog contains a total of 234 new redshifts for galaxies at z > 1.5. In addition, we present 20 galaxy pair candidates identified for the first time using the grism redshifts in our catalog, including four new galaxy pairs at z ~ 2, nearly doubling the number of such pairs previously identified.

Document Type

Article

Publication Date

5-8-2015

Notes/Citation Information

Published in The Astronomical Journal, v. 149, no. 6, article 178, p. 1-10.

© 2015. The American Astronomical Society. All rights reserved.

Reproduced by permission of the AAS.

Digital Object Identifier (DOI)

http://dx.doi.org/10.1088/0004-6256/149/6/178

Funding Information

This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program (GO 12177) and the 3D-HST Treasury Program (GO 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555 and by Spitzer, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We also acknowledge partial support from NSF 0808133 and HST-AR 12822.03A.

Related Content

This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program (GO 12177) and the 3D-HST Treasury Program (GO 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555 and by Spitzer, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.

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