EROs and the Large-Scale Structure of High-z Ellipticals

Daddi, E.; Zamorani, G.; Cimatti, A.; Röttgering, H. J. A.; Renzini, A.

doi:10.1007/10854354_70

Cited by 76 publications

(139 citation statements)

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“…The photo-z derived redshift distributions lead to inferred comoving correlation lengths, r 0 , of 9 ∼ 11h −1 Mpc (h = H o /100 km s −1 Mpc −1 ) in and 6h −1 Mpc in Firth et al (2001). Daddi et al (2001) used a pure luminosity evolution model to derive a redshift distribution for their R − K > 5, K < 19.5 sample. The PLE models have a tail to higher redshifts than the N(z) derived from the photometric redshifts and thus Daddi et al (2001) derive a larger clustering scale, finding r 0 ∼ 12h −1 Mpc.…”

Section: Clustering Of Red Galaxiesmentioning

confidence: 99%

“…Daddi et al (2001) used a pure luminosity evolution model to derive a redshift distribution for their R − K > 5, K < 19.5 sample. The PLE models have a tail to higher redshifts than the N(z) derived from the photometric redshifts and thus Daddi et al (2001) derive a larger clustering scale, finding r 0 ∼ 12h −1 Mpc. The difference between the two approaches is not all that large given the substantial uncertainties in each measurement and both approaches imply large correlation lengths.…”

Section: Clustering Of Red Galaxiesmentioning

confidence: 99%

“…As seen clearly from the submillimeter and X-ray studies there is more than one class of red galaxy, and there are reasons to believe that their redshift distributions are not the same and that the starburst population extends to higher redshifts and should have a smaller correlation angle. Indeed, Daddi et al (2001) found that the angular clustering strength of red galaxies with spectral features indicative of ongoing star formation is much weaker than that of passively evolving populations, and they infer r 0 < 2.5h −1 Mpc for the starburst ERO population.…”

Section: Clustering Of Red Galaxiesmentioning

confidence: 99%

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Eros and Faint Red Galaxies

McCarthy

2004

Annu. Rev. Astron. Astrophys.

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■ Abstract This chapter reviews the properties of faint IR-selected field galaxies and the extremely red color-selected populations in particular. These populations are a mix of passively evolving stellar systems and heavily obscured star-forming galaxies. The star-forming component appears to constitute 20-50% of the population depending on the magnitude and color cuts employed. The remaining objects are a mix of passively evolving ellipticals and early-type disk galaxies. The passively evolving red galaxies are strongly clustered in space and are likely the high-mass high-luminosity end of the elliptical galaxy progenitor population at redshifts between one and two. These galaxies have masses and space densities that appear to be in conflict with late-forming hierarchical galaxy-formation models. The red galaxies appear to be a population that is distinct from the moderately star-forming Lyman-Break galaxies but may be related to the starburst population at z > 2 seen in deep submillimeter surveys.

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Section: Clustering Of Red Galaxiesmentioning

confidence: 99%

Section: Clustering Of Red Galaxiesmentioning

confidence: 99%

Section: Clustering Of Red Galaxiesmentioning

confidence: 99%

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Eros and Faint Red Galaxies

McCarthy

2004

Annu. Rev. Astron. Astrophys.

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“…In contrast, in semi‐analytic models of galaxy formation, very few ellipticals this red and this luminous would be expected in the field at redshifts z ∼ 1.6 (cf. Daddi, Cimatti & Renzini 2000b).…”

Section: Galaxy Counts and Coloursmentioning

confidence: 99%

Red galaxy overdensities and the varied cluster environments of powerful radio sources with z 1.6

Best

Lehnert

Miley

et al. 2003

Monthly Notices of the Royal Astronomical Society

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The environments of a complete subsample of six of the most powerful radio-loud active galactic nuclei (AGN) at redshifts z ∼ 1.6 are investigated, using deep RJK imaging to depths of R ∼ 26, J ∼ 22.4 and K ∼ 20.6. An excess of galaxy counts in the K band is seen across these fields; these surplus galaxy counts are predominantly associated with red galaxies (R − K 4) of magnitudes 17.5 K 20.5 found within radial distances of ∼1 Mpc of the AGN host. These are exactly (though not uniquely) the magnitudes, colours and locations that would be expected of old passive elliptical galaxies in cluster environments at the redshifts of these AGN. Using both an Abell-style classification scheme and investigations of the angular and spatial cross-correlation functions of the galaxies, the average environment of the fields around these AGN is found to be consistent with Abell cluster richness classes 0 and 1. The amplitude of the angular cross-correlation function around the AGN is shown to be a strong function of galaxy colour and is highest when only those galaxies with the colours expected of old elliptical galaxies at these redshifts are considered.The images cover a relatively wide field, 5 × 5 arcmin 2 , allowing the distribution of the surplus galaxy counts to be investigated. The galaxy overdensities are found on two scales around the AGN: (i) pronounced central concentrations on radial scales within ∼150 kpc; where present, these are composed almost entirely of red (R − K 4) galaxies, suggesting that the morphology-density relation is imprinted into the centres of clusters at a high redshift;(ii) weaker large-scale excesses extending out to between 1 and 1.5-Mpc radius. The presence or absence of galaxy excesses on these two scales, however, differs greatly between the six different fields: the fields of two AGN do show red galaxy excesses on both scales, another two fields show only a large-scale red galaxy overdensity with no pronounced central concentration, and one field shows only a sharp central peak of red galaxies with no large-scale overdensity. The final field shows little evidence for an excess on any scale; this field is associated with an unresolved radio source, perhaps indicating that only extended radio sources probe cluster environments.Clearly, there is a large range in both the richness and the degree of concentration of any clustering environments around these distant AGN. The implications of this for both cluster formation and the nature of high-redshift AGN are discussed.

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“…The authors suggested that these objects may be high-redshift galaxies (z > 6) undergoing a luminous star-forming phase, or weakly evolved ETGs at z ∼ 1-1.5. Since the late 1980s a great deal of effort has been devoted to surveying the infrared sky and many more EROs have been found (McCarthy et al 1992;Thompson et al 1999;Daddi et al 2000).…”

Section: Extremely Red Objectsmentioning

confidence: 99%

VEXAS: VISTA EXtension to Auxiliary Surveys

Spiniello

Agnello²

2019

A&A

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Context. We present the first public data release of the VISTA EXtension to Auxiliary Surveys (VEXAS), comprising nine cross-matched multi-wavelength photometric catalogues where each object has a match in at least two surveys. Aims. Our aim is to provide spatial coverage that is as uniform as possible in the multi-wavelength sky and to provide the astronomical community with reference magnitudes and colours for various scientific uses: object classification (e.g. quasars, galaxies, and stars; high-z galaxies, white dwarfs); photometric redshifts of large galaxy samples; searches of exotic objects (e.g. extremely red objects and lensed quasars). Methods. We cross-matched the wide-field VISTA catalogues (the VISTA Hemisphere Survey and the VISTA Kilo Degree Infrared Galaxy Survey) with the AllWISE mid-infrared Survey, requiring a match within 10″. We have further matched this table with X-ray and radio data (ROSAT, XMM, SUMSS). We also performed a second cross-match between VISTA and AllWISE, with a smaller matching radius (3″), including WISE magnitudes. We then cross-matched this resulting table (≈138 × 106 objects) with three photometric wide-sky optical deep surveys (DES, SkyMapper, PanSTARRS). We finally included matches to objects with spectroscopic follow-up by the SDSS and 6dFGS. Results. To demonstrate the power of all-sky multi-wavelength cross-match tables, we show two examples of scientific applications of VEXAS, in particular using the publicly released tables to discover strong gravitational lenses (beyond the reach of previous searches) and to build a statistically large sample of extremely red objects. Conclusions. The VEXAS catalogue is currently the widest and deepest public optical-to-IR photometric and spectroscopic database in the southern hemisphere.

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EROs and the Large-Scale Structure of High-z Ellipticals

Cited by 76 publications

References 0 publications

Eros and Faint Red Galaxies

Eros and Faint Red Galaxies

Red galaxy overdensities and the varied cluster environments of powerful radio sources with z 1.6

VEXAS: VISTA EXtension to Auxiliary Surveys

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