A Significant Population of Red, Near-Infrared-selected High-Redshift Galaxies

Franx, Marijn; Labbé, Ivo; Rudnick, Gregory; Dokkum, Pieter van; Daddi, E.; Schreiber, N. M. Foerster; Moorwood, A. F. M.; Rix, H. W.; Röttgering, H. J. A.; Wel, Arjen Van de; Werf, P. van der; Starkenburg, Lottie van

doi:10.1086/375155

Cited by 448 publications

(591 citation statements)

References 23 publications

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“…from filaments, as proposed by Bournaud et al (2005) -on the other, it is not clear how much happens at which redshift. Recent detections of unexpectedly massive, evolved, and numerous galaxies at high redshift (Chapman et al 2004;Cimatti et al 2004;Franx et al 2003;Le Floc'h et al 2004) have challenged at least the semi-analytic version of the otherwise widely accepted Λ-CDM models.…”

Section: Importance Of Starbursts At High Redshiftsmentioning

confidence: 99%

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

Alvensleben¹,

Bicker

2006

A&A

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We present evolutionary synthesis models for galaxies of spectral types Sa through Sd with starbursts of various strengths triggered at various redshifts and study their photometric evolution before, during, and after their bursts in a cosmological context. We find that bursts at high redshift, even very strong ones, only cause a small blueing of their intrinsically blue young parent galaxies. At lower redshift, in contrast, even small bursts cause a significant blueing of their intrinsically redder galaxies. While the burst phase is generally short, typically a few hundred Myr in normal-mass galaxies, the postburst stage with its red colors and, in particular the very red ones for early bursts at high redshift, lasts much longer, on the order of several Gyr. We find that, even without any dust, which in the postburst stage is not expected to play an important role anyway, models easily reach the colors of EROs in the redshift range z ∼ 2 through z ∼ 0.5 after starbursts at redshifts between 2 and 4. We therefore propose a third alternative for the ERO galaxies beyond the two established ones of passive galaxies vs. dusty starbursts: the dust-free post-(strong-)starbursts. A very first comparison of our models to HDF data with photometric redshifts shows that almost all of the outliers that could not be described with our chemically consistent models for undisturbed normal galaxy types E through Sd can now be explained very well. Galaxies in the redshift range from z ∼ 2.5 to z ∼ 0.5 that are redder, and in some cases much redder, than our reddest undisturbed model for a high-metallicity classical elliptical are well described by post-starburst models after starbursts at redshifts between 2 and 4. Galaxies bluer than our bluest low metallicity Sd model, most of which have redshifts lower than 1, are well explained by ongoing starbursts.

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Section: Importance Of Starbursts At High Redshiftsmentioning

confidence: 99%

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

Alvensleben¹,

Bicker

2006

A&A

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“…Robust and accurate photo-zs can now be obtained for a large number of objects efficiently and to a depth which is inaccessible to spectroscopy at even the largest telescopes (e.g. Sawicki et al 1997;Hogg et al 1998;Csabai et al 2003;Franx et al 2003;Mobasher et al 2004;Capak et al 2007;Ilbert et al 2006Ilbert et al , 2009Salvato et al 2009;Bouwens et al 2010;McLure et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Photometric redshifts for gamma-ray burst afterglows from GROND andSwift/UVOT

Krühler

Schady

Greiner

et al. 2011

A&A

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Aims. We present a framework to obtain photometric redshifts (photo-zs) for gamma-ray burst afterglows. Using multi-band photometry from GROND and Swift/UVOT, photo-zs are derived for five GRBs for which spectroscopic redshifts are not available. Methods. We use UV/optical/NIR data and synthetic photometry based on afterglow observations and theory to derive the photometric redshifts of GRBs and their accuracy. Taking into account the afterglow synchrotron emission properties, we investigate the application of photometry to derive redshifts in a theoretical range between z ∼ 1 to z ∼ 12.Results. The measurement of photo-zs for GRB afterglows provides a quick, robust and reliable determination of the distance scale to the burst, particularly in those cases where spectroscopic observations in the optical/NIR range cannot be obtained. Given a sufficiently bright and mildly reddened afterglow, the relative photo-z accuracy η = Δz/(1 + z) is better than 10% between z = 1.5 and z ∼ 7 and better than 5% between z = 2 and z = 6. We detail the approach on 5 sources without spectroscopic redshifts observed with UVOT on-board Swift and/or GROND. The distance scale to those same afterglows is measured to be z = 4.31 +0.14 −0.15 for GRB 080825B, z = 2.13 +0.14 −0.20 for GRB 080906, z = 3.44 +0.15 −0.32 for GRB 081228, z = 2.03 +0.16 −0.14 for GRB 081230 and z = 1.28 +0.16 −0.15 for GRB 090530. Conclusions. Due to the exceptional luminosity and simple continuum spectrum of GRB afterglows, photometric redshifts can be obtained to an accuracy as good as η ∼ 0.03 over a large redshift range including robust (η ∼ 0.1) measurements in the ultra-high redshift regime (z 7). Combining the response from UVOT with ground-based observatories and in particular GROND operating in the optical/NIR wavelength regime, reliable photo-zs can be obtained from z ∼ 1.0 out to z ∼ 10, and possibly even at higher redshifts in some favorable cases, provided that these GRBs exist, are localized quickly, have sufficiently bright afterglows and are not heavily obscured.

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“…Since the Balmer break enters the J filter at z ∼ 1.9, J − K > 2.3 mag (in the Vega system) is a very effective criterion (Saracco et al 2001;Franx et al 2003) for selecting z > ∼ 2 galaxies. The spectroscopic study by Reddy et al (2005), by 1 Cluster names are acronyms indicating the filter pair used for the detection (gr, Rz, JK) followed by the string CS, for colour selected, followed by the order number in the catalogue.…”

Section: Introductionmentioning

confidence: 99%

JKCS 041: a colour-detected galaxy cluster at $z_{\mathrm{phot}}$ ~ 1.9 with deep potential well as confirmed by X-ray data

Andreon¹,

Maughan

Trinchieri³

et al. 2009

A&A

121

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We report the discovery of JKCS 041, a massive near-infrared selected cluster of galaxies at z phot ∼ 1.9. The cluster was originally discovered using a modified red-sequence method and also detected in follow-up Chandra data as an extended X-ray source. Optical and near-infrared imaging data alone allow us to show that the detection of JKCS 041 is secure, even in the absence of the X-ray data. We investigate the possibility that JKCS 041 is not a galaxy cluster at z ∼ 1.9, and find other explanations unlikely. The X-ray detection and statistical arguments rule out the hypothesis that JKCS 041 is actually a blend of groups along the line of sight, and we find that the X-ray emitting gas is too hot and dense to be a filament projected along the line of sight. The absence of a central radio source and the extent and morphology of the X-ray emission argue against the possibility that the X-ray emission comes from inverse Compton scattering of CMB photons by a radio plasma. The cluster has an X-ray core radius of 36.6 +8.3 −7.6 arcsec (about 300 kpc), an X-ray temperature of 7.4 +5.3 −3.3 keV, a bolometric X-ray luminosity within R 500 of (7.6 ± 0.5) × 10 44 erg s −1 , and an estimated mass of M 500 = 2.9 +3.8 −2.4 × 10 14 M , the last derived under the usual (and strong) assumptions. The cluster is composed of 16.4 ± 6.3 galaxies within 1.5 arcmin (750 kpc) brighter than K ∼ 20.7 mag. The high redshift of JKCS 041 is determined from the detection colour, from the detection of the cluster in a galaxy sample formed by z phot > 1.6 galaxies and from a photometric redshift based on 11-band spectral energy distribution fitting. By means of the latter we find the cluster redshift to be 1.84 < z < 2.12 at 68% confidence. Therefore, JKCS 041 is a cluster of galaxies at z phot ∼ 1.9 with a deep potential well, making it the most distant cluster with extended X-ray emission known.

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A Significant Population of Red, Near-Infrared-selected High-Redshift Galaxies

Cited by 448 publications

References 23 publications

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

Photometric redshifts for gamma-ray burst afterglows from GROND andSwift/UVOT

JKCS 041: a colour-detected galaxy cluster at $z_{\mathrm{phot}}$ ~ 1.9 with deep potential well as confirmed by X-ray data

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