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Z>~7 galaxies with red Spitzer/IRAC [3.6]-[4.5] colors in the full CANDELS data set: the brightest-known galaxies at Z~7-9 and a probable spectroscopic confirmation at Z=7.48 | | G. W. Roberts-Borsani
; R. J. Bouwens
; P. A. Oesch
; I. Labbe
; R. Smit
; G. D. Illingworth
; P. van Dokkum
; B. Holden
; V. Gonzalez
; M. Stefanon
; B. Holwerda
; S. Wilkins
; | | Date: |
2 Jun 2015 | | Abstract: | We identify 4 unusually bright (H<~25.5) galaxies from HST and Spitzer
CANDELS data with probable redshifts z~7-9. These identifications constitute
the brightest-known galaxies to date at z>~7.5. As Y-band observations are not
available over the full CANDELS program to perform a standard Lyman-break
selection of z>7 galaxies, here we employ an alternate strategy using the deep
Spitzer/IRAC data. We identify z~7.1-9.1 galaxies by selecting z>~6 galaxies
from the HST CANDELS data that show quite red IRAC [3.6]-[4.5] colors,
indicating a strong [OIII] line in the 4.5mu band. This selection strategy was
validated using a modest sample for which we have deep Y-band coverage. Here we
focus on using this criterion to select the brightest z>~7 sources. Applying
the IRAC criteria to all HST-selected optical-dropout galaxies over the full
~900 arcmin**2 of the 5 CANDELS fields revealed four unusually bright z~7.1,
7.6, 7.9 and 8.6 candidates. The median [3.6]-[4.5] color of our selected
z~7.1-9.1 sample is consistent with rest-frame [OIII]+Hbeta EWs of ~1600A in
the [4.5] band. Keck/MOSFIRE spectroscopy has already been reported for one of
our selected sources EGS-zs8-1, showing Lyalpha at a redshift of
7.7302$pm$0.0006. We present similar Keck/MOSFIRE spectroscopy for a second
selected galaxy with a probable 4.7sigma Lyalpha-line at a redshift of
7.4770+/-0.0008. Both have H-band magnitudes of ~25 mag and are ~0.5 mag more
luminous (M(UV)~-22.0) than any previously discovered z~8 galaxy, with
important implications for the UV LF. Our 3 brightest, highest redshift z>~7
galaxies all lie within the CANDELS EGS field, providing a dramatic
illustration of the potential impact of field-to-field variance. | | Source: | arXiv, 1506.0854 | | Services: | Forum | Review | PDF | Favorites | |
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