We utilize a two-color Lyman-break selection criterion to search for z ~ 9-10 galaxies over the first 19 clusters in the CLASH program. A systematic search yields three z ~ 9-10 candidates. While we have already reported the most robust of these candidates, MACS1149-JD, two additional z ~ 9 candidates are also found and have H 160-band magnitudes of ~26.2-26.9. A careful assessment of various sources of contamination suggests lsim1 contaminants for our z ~ 9-10 selection. To determine the implications of these search results for the luminosity function (LF) and star formation rate density at z ~ 9, we introduce a new differential approach to deriving these quantities in lensing fields. Our procedure is to derive the evolution by comparing the number of z ~ 9-10 galaxy candidates found in CLASH with the number of galaxies in a slightly lower-redshift sample (after correcting for the differences in selection volumes), here taken to be z ~ 8. This procedure takes advantage of the fact that the relative volumes available for the z ~ 8 and z ~ 9-10 selections behind lensing clusters are not greatly dependent on the details of the lensing models. We find that the normalization of the UV LF at z ~ 9 is just 0.28-0.20+0.39× that at z ~ 8, which is ~1.4-0.8+3.0× lower than extrapolating z ~ 4-8 LF results. While consistent with the evolution in the UV LF seen at z ~ 4-8, these results marginally favor a more rapid evolution at z > 8. Compared to similar evolutionary findings from the HUDF, our result is less insensitive to large-scale structure uncertainties, given our many independent sightlines on the high-redshift universe.

A census of star-forming galaxies in the z ∼ 9-10 universe based on hst+spitzer observations over 19 clash clusters: Three candidate z ∼ 9-10 galaxies and improved constraints on the star formation rate density at z

ROSATI, Piero;
2014

Abstract

We utilize a two-color Lyman-break selection criterion to search for z ~ 9-10 galaxies over the first 19 clusters in the CLASH program. A systematic search yields three z ~ 9-10 candidates. While we have already reported the most robust of these candidates, MACS1149-JD, two additional z ~ 9 candidates are also found and have H 160-band magnitudes of ~26.2-26.9. A careful assessment of various sources of contamination suggests lsim1 contaminants for our z ~ 9-10 selection. To determine the implications of these search results for the luminosity function (LF) and star formation rate density at z ~ 9, we introduce a new differential approach to deriving these quantities in lensing fields. Our procedure is to derive the evolution by comparing the number of z ~ 9-10 galaxy candidates found in CLASH with the number of galaxies in a slightly lower-redshift sample (after correcting for the differences in selection volumes), here taken to be z ~ 8. This procedure takes advantage of the fact that the relative volumes available for the z ~ 8 and z ~ 9-10 selections behind lensing clusters are not greatly dependent on the details of the lensing models. We find that the normalization of the UV LF at z ~ 9 is just 0.28-0.20+0.39× that at z ~ 8, which is ~1.4-0.8+3.0× lower than extrapolating z ~ 4-8 LF results. While consistent with the evolution in the UV LF seen at z ~ 4-8, these results marginally favor a more rapid evolution at z > 8. Compared to similar evolutionary findings from the HUDF, our result is less insensitive to large-scale structure uncertainties, given our many independent sightlines on the high-redshift universe.
2014
Bouwens, R. J.; Bradley, L.; Zitrin, A.; Coe, D.; Franx, M.; Zheng, W.; Smit, R.; Host, O.; Postman, M.; Moustakas, L.; Labbé, I.; Carrasco, M.; Molino, A.; Donahue, M.; Kelson, D. D.; Meneghetti, M.; Benítez, N.; Lemze, D.; Umetsu, K.; Broadhurst, T.; Moustakas, J.; Rosati, Piero; Jouvel, S.; Bartelmann, M.; Ford, H.; Graves, G.; Grillo, C.; Infante, L.; Jimenez Teja, Y.; Lahav, O.; Maoz, D.; Medezinski, E.; Melchior, P.; Merten, J.; Nonino, M.; Ogaz, S.; Seitz, S.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11392/2333708
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