The faint and extremely red K‐band‐selected galaxy population in the DEEP2/Palomar fields
Identifieur interne : 000176 ( Main/Exploration ); précédent : 000175; suivant : 000177The faint and extremely red K‐band‐selected galaxy population in the DEEP2/Palomar fields
Auteurs : C. J. Conselice ; K. Bundy [Canada] ; P. Eisenhardt [États-Unis] ; J. Lotz [États-Unis] ; J. Newman [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008-02-01.
English descriptors
Abstract
We present in this paper an analysis of the faint and red near‐infrared (NIR) selected galaxy population found in NIR imaging from the Palomar Observatory Wide‐Field Infrared Survey. This survey covers 1.53 deg2 to 5σ detection limits of Kvega= 20.5–21 and Jvega= 22.5, and overlaps with the DEEP2 spectroscopic redshift survey. We discuss the details of this NIR survey, including our J‐ and K‐band counts. We show that the K‐band galaxy population has a redshift distribution that varies with K magnitude, with most K < 17 galaxies at z < 1.5 and a significant fraction (38.3 ± 0.3 per cent) of K > 19 systems at z > 1.5. We further investigate the stellar masses and morphological properties of K‐selected galaxies, particularly extremely red objects (EROs), as defined by (R−K) > 5.3 and (I−K) > 4. One of our conclusions is that the ERO selection is a good method for picking out galaxies at z > 1.2, and within our magnitude limits, the most massive galaxies at these redshifts. The ERO limit finds 75 per cent of all M* > 1011 M⊙ galaxies at z∼ 1.5 down to Kvega= 19.7. We further find that the morphological breakdown of K < 19.7 EROs is dominated by early‐types (57 ± 3 per cent) and peculiars (34 ± 3 per cent). However, about a fourth of the early‐types are distorted ellipticals, and within CAS (concentration, asymmetry, clumpiness) parameter space these bridge the early‐type and peculiar population, suggesting a morphological evolutionary sequence. We also investigate the use of a (I−K) > 4 selection to locate EROs, finding that it selects galaxies at slightly higher average redshifts (〈z〉= 1.43 ± 0.32) than the (R−K) > 5.3 limit with 〈z〉= 1.28 ± 0.23. Finally, by using the redshift distribution of K < 20 selected galaxies, and the properties of our EROs, we are able to rule out all monolithic collapse models for the formation of massive galaxies.
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DOI: 10.1111/j.1365-2966.2007.12686.x
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This survey covers 1.53 deg2 to 5σ detection limits of Kvega= 20.5–21 and Jvega= 22.5, and overlaps with the DEEP2 spectroscopic redshift survey. We discuss the details of this NIR survey, including our J‐ and K‐band counts. We show that the K‐band galaxy population has a redshift distribution that varies with K magnitude, with most K < 17 galaxies at z < 1.5 and a significant fraction (38.3 ± 0.3 per cent) of K > 19 systems at z > 1.5. We further investigate the stellar masses and morphological properties of K‐selected galaxies, particularly extremely red objects (EROs), as defined by (R−K) > 5.3 and (I−K) > 4. One of our conclusions is that the ERO selection is a good method for picking out galaxies at z > 1.2, and within our magnitude limits, the most massive galaxies at these redshifts. The ERO limit finds 75 per cent of all M* > 1011 M⊙ galaxies at z∼ 1.5 down to Kvega= 19.7. We further find that the morphological breakdown of K < 19.7 EROs is dominated by early‐types (57 ± 3 per cent) and peculiars (34 ± 3 per cent). However, about a fourth of the early‐types are distorted ellipticals, and within CAS (concentration, asymmetry, clumpiness) parameter space these bridge the early‐type and peculiar population, suggesting a morphological evolutionary sequence. We also investigate the use of a (I−K) > 4 selection to locate EROs, finding that it selects galaxies at slightly higher average redshifts (〈z〉= 1.43 ± 0.32) than the (R−K) > 5.3 limit with 〈z〉= 1.28 ± 0.23. Finally, by using the redshift distribution of K < 20 selected galaxies, and the properties of our EROs, we are able to rule out all monolithic collapse models for the formation of massive galaxies.</div></front></TEI><affiliations><list><country><li>Canada</li><li>États-Unis</li></country><region><li>Ontario</li></region><settlement><li>Toronto</li></settlement><orgName><li>Université de Toronto</li></orgName></list><tree><noCountry><name sortKey="Conselice, C J" sort="Conselice, C J" uniqKey="Conselice C" first="C. J." last="Conselice">C. J. Conselice</name></noCountry><country name="Canada"><region name="Ontario"><name sortKey="Bundy, K" sort="Bundy, K" uniqKey="Bundy K" first="K." last="Bundy">K. Bundy</name></region></country><country name="États-Unis"><noRegion><name sortKey="Eisenhardt, P" sort="Eisenhardt, P" uniqKey="Eisenhardt P" first="P." last="Eisenhardt">P. Eisenhardt</name></noRegion><name sortKey="Lotz, J" sort="Lotz, J" uniqKey="Lotz J" first="J." last="Lotz">J. Lotz</name><name sortKey="Newman, J" sort="Newman, J" uniqKey="Newman J" first="J." last="Newman">J. Newman</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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