skip to main content

SciTech ConnectSciTech Connect

Title: Predicting future space near-IR grism surveys using the WFC3 infrared spectroscopic parallels survey

We present near-infrared emission line counts and luminosity functions from the Hubble Space Telescope Wide Field Camera 3 Infrared Spectroscopic Parallels (WISP) program for 29 fields (0.037 deg{sup 2}) observed using both the G102 and G141 grism. Altogether we identify 1048 emission line galaxies with observed equivalent widths greater than 40 Å, 467 of which have multiple detected emission lines. We use simulations to correct for significant (>20%) incompleteness introduced in part by the non-dithered, non-rotated nature of the grism parallels. The WISP survey is sensitive to fainter flux levels ((3-5) × 10{sup –17} erg s{sup –1} cm{sup –2}) than the future space near-infrared grism missions aimed at baryonic acoustic oscillation cosmology ((1-4) × 10{sup –16} erg s{sup –1} cm{sup –2}), allowing us to probe the fainter emission line galaxies that the shallower future surveys may miss. Cumulative number counts of 0.7 < z < 1.5 galaxies reach 10,000 deg{sup –2} above an Hα flux of 2 × 10{sup –16} erg s{sup –1} cm{sup –2}. Hα-emitting galaxies with comparable [O III] flux are roughly five times less common than galaxies with just Hα emission at those flux levels. Galaxies with low Hα/[O III] ratios are very rare at the brightermore » fluxes that future near-infrared grism surveys will probe; our survey finds no galaxies with Hα/[O III] < 0.95 that have Hα flux greater than 3 × 10{sup –16} erg s{sup –1} cm{sup –2}. Our Hα luminosity function contains a comparable number density of faint line emitters to that found by the Near IR Camera and Multi-Object Spectrometer near-infrared grism surveys, but significantly fewer (factors of 3-4 less) high-luminosity emitters. We also find that our high-redshift (z = 0.9-1.5) counts are in agreement with the high-redshift (z = 1.47) narrowband Hα survey of HiZELS (Sobral et al.), while our lower redshift luminosity function (z = 0.3-0.9) falls slightly below their z = 0.84 result. The evolution in both the Hα luminosity function from z = 0.3-1.5 and the [O III] luminosity function from z = 0.7-2.3 is almost entirely in the L {sub *} parameter, which steadily increases with redshift over those ranges.« less
Authors:
;  [1] ; ;  [2] ;  [3] ; ;  [4] ; ;  [5] ; ; ;  [6] ; ;  [7] ;  [8] ;  [9]
  1. Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125 (United States)
  2. Infrared Processing and Analysis Center, Caltech, Pasadena, CA 91125 (United States)
  3. Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH (United Kingdom)
  4. Department of Physics and Astronomy, University of California, Los Angeles, CA (United States)
  5. Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, MN 55455 (United States)
  6. Department of Physics and Astronomy, University of California Riverside, Riverside, CA 92521 (United States)
  7. Observatories of the Carnegie Institution for Science, Pasadena, CA 91101 (United States)
  8. Astrophysics Science Division, Goddard Space Flight Center, Code 665, Greenbelt, MD 20771 (United States)
  9. Department of Physics, University of California, Santa Barbara, CA 93106 (United States)
Publication Date:
OSTI Identifier:
22348547
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 779; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BARYONS; COMPARATIVE EVALUATIONS; COSMOLOGY; DENSITY; EMISSION; EVOLUTION; GALAXIES; LUMINOSITY; MASS; OSCILLATIONS; RED SHIFT; SIMULATION; SPACE; SPECTROMETERS; TELESCOPES