The faint and extremely red K-band-selected galaxy population in the DEEP2/Palomar fields
Identifieur interne : 000148 ( Main/Exploration ); précédent : 000147; suivant : 000149The faint and extremely red K-band-selected galaxy population in the DEEP2/Palomar fields
Auteurs : C. J. Conselice [Royaume-Uni] ; K. Bundy [Canada] ; U. Vivian [États-Unis] ; 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.
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* > 1011M⊙ 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* > 1011M⊙ 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>Royaume-Uni</li><li>États-Unis</li></country><region><li>Hawaï</li><li>Ontario</li></region><settlement><li>Toronto</li></settlement><orgName><li>Université de Toronto</li></orgName></list><tree><country name="Royaume-Uni"><noRegion><name sortKey="Conselice, C J" sort="Conselice, C J" uniqKey="Conselice C" first="C. J." last="Conselice">C. J. Conselice</name></noRegion></country><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"><region name="Hawaï"><name sortKey="Vivian, U" sort="Vivian, U" uniqKey="Vivian U" first="U" last="Vivian">U. Vivian</name></region><name sortKey="Eisenhardt, P" sort="Eisenhardt, P" uniqKey="Eisenhardt P" first="P." last="Eisenhardt">P. Eisenhardt</name><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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