paper

The 3D-HST Survey: Hubble Space Telescope WFC3/G141 grism spectra, redshifts, and emission line measurements for galaxies

arXiv:1510.02106 · doi:10.3847/0067-0049/225/2/27

Abstract

We present reduced data and data products from the 3D-HST survey, a 248-orbit HST Treasury program. The survey obtained WFC3 G141 grism spectroscopy in four of the five CANDELS fields: AEGIS, COSMOS, GOODS-S, and UDS, along with WFC3 imaging, parallel ACS G800L spectroscopy, and parallel imaging. In a previous paper (Skelton et al. 2014) we presented photometric catalogs in these four fields and in GOODS-N, the fifth CANDELS field. Here we describe and present the WFC3 G141 spectroscopic data, again augmented with data from GO-1600 in GOODS-N. The data analysis is complicated by the fact that no slits are used: all objects in the WFC3 field are dispersed, and many spectra overlap. We developed software to automatically and optimally extract interlaced 2D and 1D spectra for all objects in the Skelton et al. (2014) photometric catalogs. The 2D spectra and the multi-band photometry were fit simultaneously to determine redshifts and emission line strengths, taking the morphology of the galaxies explicitly into account. The resulting catalog has 98,663 measured redshifts and line strengths down to and 22,548 with , where we comfortably detect continuum emission. Of this sample 5,459 galaxies are at and 9,621 are at , where H falls in the G141 wavelength coverage. Based on comparisons with ground-based spectroscopic redshifts, and on analyses of paired galaxies and repeat observations, the typical redshift error for galaxies in our catalog is , i.e., one native WFC3 pixel. The limit for emission line fluxes of point sources is ergs s cm. We show various representations of the full dataset, as well as individual examples that highlight the range of spectra that we find in the survey.

v2 updates Figure 22. Submitted to ApJS. All 2D and 1D spectra, as well as redshifts, line fluxes, and other derived parameters, are publicly available at available at http://3dhst.research.yale.edu

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