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26 April 2024 |
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HST Grism-derived Forecasts for Future Galaxy Redshift Surveys | | Micaela B. Bagley
; Claudia Scarlata
; Vihang Mehta
; Harry Teplitz
; Ivano Baronchelli
; Daniel J. Eisenstein
; Lucia Pozzetti
; Andrea Cimatti
; Michael Rutkowski
; Yun Wang
; Alexander Merson
; | | Date: |
5 Jun 2020 | | Abstract: | The mutually complementary Euclid and Roman galaxy redshift surveys will use
Halpha- and [OIII]-selected emission line galaxies as tracers of the large
scale structure at $0.9 lesssim z lesssim 1.9$ (Halpha) and $1.5 lesssim z
lesssim 2.7$ ([OIII]). It is essential to have a reliable and sufficiently
precise knowledge of the expected numbers of Halpha-emitting galaxies in the
survey volume in order to optimize these redshift surveys for the study of dark
energy. Additionally, these future samples of emission-line galaxies will, like
all slitless spectroscopy surveys, be affected by a complex selection function
that depends on galaxy size and luminosity, line equivalent width, and redshift
errors arising from the misidentification of single emission-line galaxies.
Focusing on the specifics of the Euclid survey, we combine two slitless
spectroscopic WFC3-IR datasets -- 3D-HST+AGHAST and the WISP survey -- to
construct a Euclid-like sample that covers an area of 0.56 deg$^2$ and includes
1277 emission line galaxies. We detect 1091 ($sim$3270 deg$^{-2}$)
Halpha+[NII]-emitting galaxies in the range $0.9leq z leq 1.6$ and 162
($sim$440 deg$^{-2}$) [OIII]$lambda$5007-emitters over $1.5leq z leq 2.3$
with line fluxes $geq 2 imes 10^{-16}$ erg s$^{-1}$ cm$^{-2}$. The median of
the Halpha+[NII] equivalent width distribution is $sim$250
{A}, and the
effective radii of the continuum and Halpha+[NII] emission are correlated with
a median of $sim$0.38" and significant scatter ($sigma sim $0.2"$-$0.35").
Finally, we explore the prevalence of redshift misidentification in future
Euclid samples, finding potential contamination rates of $sim$14-20% and
$sim$6% down to $2 imes 10^{-16}$ and $6 imes 10^{-17}$ erg s$^{-1}$
cm$^{-2}$, respectively, though with increased wavelength coverage these
percentages drop to nearly zero. | | Source: | arXiv, 2006.3602 | | Services: | Forum | Review | PDF | Favorites | |
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