Distant Red Galaxies in the Hubble Ultra Deep Field

Toft, Sune; Dokkum, Pieter van; Franx, Marijn; Thompson, Rodger I.; Illingworth, G. D.; Kriek, Mariska

doi:10.1086/430346

Cited by 111 publications

(156 citation statements)

References 25 publications

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“…The cSFGs are formed by gas-rich processes such as major mergers at high redshifts, and rapidly quenched (probably by AGN) into cQGs, most of which are classified as spheroidal quiescent DRGs. These compact QGs at z ∼ 2 may be the cores of today's massive elliptical galaxies, as described by van de Sande et al 2013 andPatel et al 2013, these quiescent galaxies at z ∼ 2 grow inside-out, consistent with the expectations from minor mergers.…”

Section: Nonparametric Morphologysupporting

confidence: 78%

“…The morphologies of DRGs are diverse. Toft et al 2005 analyzed the morphologies of DRGs in the Hubble Ultra Deep Field based on HST Advanced Camera for Surveys (ACS) images and Near Infrared Camera and Multi-Object Spectrometer (NICMOS) images, and found that the rest-frame optical morphology of DRG is quite different from the rest-frame UV morphology. In the near-infrared images, some DRGs are extended and others are compact.…”

Section: Introductionmentioning

confidence: 99%

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Physical properties of distant red galaxies in the COSMOS/UltraVISTA field

Ma¹,

Fang²,

Kong³

et al. 2015

Publications of the Astronomical Society of Japan

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We present a study on physical properties for a large distant red galaxy (DRG) sample, using the K-selected multi-band photometry catalog of the COSMOS/UltraVISTA field and the CANDELS NIR data. Our sample includes 4485 DRGs with (J − K) AB > 1.16 and K AB <23.4 mag, and 132 DRGs have HST/WFC3 morphological measurements. The results of nonparametric measurements of DRG morphology are consistent with our rest-frame UVJ color classification: quiescent DRGs are generally compact while star-forming DRGs tend to have extended structures. We find the star formation rate (SFR) and the stellar mass of star-forming DRGs present tight "main sequence" relations in all redshift bins. Moreover, the specific SFR (sSFR) of DRGs increase with redshift in all stellar mass bins and DRGs with higher stellar masses generally have lower sSFRs, which indicates that galaxies were much more active on average in the past, and star formation contributes more to the mass growth of low-mass galaxies than to high-mass galaxies. The infrared (IR) derived SFR dominate the total SFR of DRGs which occupy the high-mass 1 range, implying that the J − K color criterion effectively selects massive and dusty galaxies. DRGs with higher M * generally have redder (U − V ) rest colors, and the (U − V ) rest colors of DRGs become bluer at higher redshifts, suggesting high-mass galaxies have higher internal dust extinctions or older stellar ages and they evolve with time. Finally, we find that DRGs have different overlaps with EROs, BzKs, IEROs and high-z ULIRGs indicating DRGs is not a special population and they can also be selected by other color criteria.

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Section: Nonparametric Morphologysupporting

confidence: 78%

Section: Introductionmentioning

confidence: 99%

Physical properties of distant red galaxies in the COSMOS/UltraVISTA field

Ma¹,

Fang²,

Kong³

et al. 2015

Publications of the Astronomical Society of Japan

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“…A number of DRGs have been spectroscopically confirmed (van Dokkum et al 2003;Kriek et al 2006aKriek et al , 2006b Quadri et al 2006).…”

Section: Color Selection Of Red Galaxiesmentioning

confidence: 96%

The Density and Spectral Energy Distributions of Red Galaxies at z ~ 3.7

Brammer

Dokkum

2007

ApJ

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We use the deep NIR imaging of the FIRES survey to investigate trends with redshift of the properties of galaxies selected to have strong Balmer/4000 breaks at . Analogous to the (AB) color A 2! z ! 4.5 J Ϫ K 1 1.3 criterion designed to select red galaxies at , we propose two color criteria, and , z 1 2 J Ϫ H 1 0.9 H Ϫ K 1 0.9 to select red galaxies in two redshift bins at and , respectively. From the FIRES catalogs of 2 ! z ! 3 3! z ! 4.5 the HDF-S (4.7 arcmin 2 ) and MS 1054Ϫ03 (26.3 arcmin 2 ) fields, we find 18 galaxies with that Az S p 2.4 phot satisfy, and 23 galaxies with that satisfy , , where thes phot s s flux limits are chosen to match the limiting rest-frame luminosities at the different median redshifts of the two samples. The space densities of the and samples are and Ϫ4 J Ϫ H HϪ K (1.5 ‫ע‬ 0.5) # 10 (1.2 ‫ע‬ 0.4) # s sMpc Ϫ3 , respectively. The rest-frame colors of galaxies in both samples are similarly red (as expected Ϫ4 10 U Ϫ B from the definition of the color criteria), but the rest-frame UV properties are different: galaxies in the higher redshift selected sample have blue NUV-optical colors and UV slopes similar to those of Lyman break H Ϫ K s galaxies, while the galaxies are generally red over the entire wavelength range observed. Synthetic template J Ϫ H s fits indicate that the distinct rest-NUV properties of the two samples are primarily a result of dust: we find mag and mag. The median stellar mass determined from the template fits decreases by AA S p 1 AA S p 0.2 V JH V HKa factor of ∼5 from to 3.7, which, coupled with the fact that the space density of such galaxies remains z p 2.4 roughly constant, may imply that the stellar mass density in red galaxies decreases by a similar factor over this redshift range.

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“…These colors may arise due to the presence of a redshifted Balmer (3646 Å) or 4000 Å break in the spectral energy distribution (SED) of the source. However, the degeneracy between stellar age, redshift, and dust extinction means that proposed "passive" samples, selected on apparent colors, suffer high (80%) contamination from dusty interlopers at low and high redshift (Smail et al 2002b;Toft et al 2005;Boone et al 2011;Caputi et al 2012). Indeed, an early attempt to identify a z > 3 passive galaxy was presented by Mobasher et al (2005), who claimed the detection of a bright post-starburst galaxy at z ∼ 6.5.…”

Section: Introductionmentioning

confidence: 99%

An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z = 3.717 “Passive” System, ZF 20115

Simpson

Smail

Wang

et al. 2017

ApJL

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The identification of high-redshift, massive galaxies with old stellar populations may pose challenges to some models of galaxy formation. However, to securely classify a galaxy as quiescent, it is necessary to exclude significant ongoing star formation, something that can be challenging to achieve at high redshifts. In this letter, we analyse deep ALMA / 870 µm and SCUBA-2 / 450 µm imaging of the claimed "post-starburst" galaxy ZF-20115 at z = 3.717 that exhibits a strong Balmer break and absorption lines. The far-infrared imaging reveals a luminous starburst located 0.4 ± 0.1 (∼ 3 kpc in projection) from the position of the rest-frame ultra-violet / optical emission, with an obscured star-formation rate of 100 +15 −70 M yr −1 . This star-forming component is undetected in the restframe ultraviolet but contributes significantly to the lower angular resolution photometry at restframe wavelengths > ∼ 3500 Å, significantly complicating the determination of a reliable stellar mass. Importantly, in the presence of dust obscuration, strong Balmer features are not a unique signature of a post-starburst galaxy and are indeed frequently observed in infrared-luminous galaxies. We conclude that the ZF 20015 system does not pose a challenge to current models of galaxy formation and that deep sub-/millimeter observations are a pre-requisite for any claims of quiescence. The multiwavelength observations of ZF 20115 unveil a complex system with an intricate and spatially-varying star-formation history. ZF 20115 demonstrates that understanding high-redshift obscured starbursts will only be possible with multi-wavelength studies that include high-resolution observations, available with the JWST, at mid-infrared wavelengths.

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Distant Red Galaxies in the Hubble Ultra Deep Field

Cited by 111 publications

References 25 publications

Physical properties of distant red galaxies in the COSMOS/UltraVISTA field

Physical properties of distant red galaxies in the COSMOS/UltraVISTA field

The Density and Spectral Energy Distributions of Red Galaxies at z ~ 3.7

An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z = 3.717 “Passive” System, ZF 20115

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