A low mass cluster of extremely red galaxies at<i>z</i>= 1.10 in the GOODS Southern Field

Díaz‐Sánchez, A.; Villó-Pérez, Isidro; Pérez‐Garrido, A.; Rebolo, R.

doi:10.1111/j.1365-2966.2007.11643.x

Cited by 14 publications

(18 citation statements)

References 43 publications

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“…1994;Scodeggio & Silva. 2000;Brown et al 2005;Kong et al 2006;Díaz-Sánchez et al 2007;Wilson et al 2007). Since the UDF field has not I−band or R−band observation data, we cannot use R − K or I − K color criteria for EROs selection.…”

Section: Ero Sample Selectionmentioning

confidence: 99%

Classification of extremely red objects in the Hubble Ultra Deep Field

Fang

Kong

Wang

2009

Res. Astron. Astrophys.

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In this paper we present a quantitative study of the classification of Extremely Red Objects (EROs). The analysis is based on the multi-band spatial-and ground-based observations (HST/ACS-BV iz, HST/NICMOS-JH, VLT-JHK) in the Hubble Ultra Deep Field (UDF). Over a total sky area of 5.50 arcmin 2 in the UDF, we select 24 EROs with the color criterion (i − K) Vega > 3.9, corresponding to (I − K) Vega > ∼ 4.0, down to K Vega = 22. We develop four methods to classify EROs into Old passively evolving Galaxies (OGs) and Dusty star-forming Galaxies (DGs), including (i − K) vs. (J − K) color diagram, spectral energy distribution fitting method, Spitzer MIPS 24 µm image matching, and nonparametric measure of galaxy morphology, and found that the classification results from these methods agree well. Using these four classification methods, we classify our EROs sample into 6 OGs and 8 DGs to K Vega < 20.5, and 8 OGs and 16 DGs to K Vega < 22, respectively. The fraction of DGs increases from 8/14 at K Vega < 20.5 to 16/24 at K Vega < 22. To study the morphology of galaxies with its wavelength, we measure the central concentration and the Gini coefficient for the 24 EROs in our sample in HST/ACS-i, z and HST/NICMOS-J, H bands. We find that the morphological parameters of galaxies in our sample depend on the wavelength of observation, which suggests that caution is necessary when comparing single wavelength band images of galaxies at a variety of redshifts.

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Section: Ero Sample Selectionmentioning

confidence: 99%

Classification of extremely red objects in the Hubble Ultra Deep Field

Fang

Kong

Wang

2009

Res. Astron. Astrophys.

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“…Some of these have already been partially described (Gilli et al 2003;Adami et al 2005;Vanzella et al 2005;Trevese et al 2007;Díaz-Sánchez et al 2007;Castellano et al 2007). Figure 1 shows the position of these overdensities over the photometric redshift distributions of our sample.These overdensities are also traced by the distribution of the spectroscopically confirmed AGNs in our catalogue, as shown in the lower panel of Fig.…”

Section: A Catalogue Of the Detected Overdensities In The Goods-southmentioning

confidence: 99%

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Salimbeni

Castellano

Pentericci

et al. 2009

A&A

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Aims. The aim of the present paper is to identify and study the properties and galactic content of groups and clusters in the GOODSSouth field up to z ∼ 2.5, and to analyse the physical properties of galaxies as a continuous function of environmental density up to high redshift. Methods. We used the deep (z 850 ∼ 26), multi-wavelength GOODS-MUSIC catalogue, which has a 15% of spectroscopic redshifts and accurate photometric redshifts for the remaining fraction. On these data, we applied a (2+1)D algorithm, previously developed by our group, that provides an adaptive estimate of the 3D density field. We supported our analysis with simulations to evaluate the purity and the completeness of the cluster catalogue produced by our algorithm. Results. We find several high-density peaks embedded in larger structures in the redshift range 0.4-2.5. From the analysis of their physical properties (mass profile, M 200 , σ v , L X , U − B vs. B diagram), we find that most of them are groups of galaxies, while two are poor clusters with masses a few times 10 14 M . For these two clusters we find from the Chandra 2Ms data an X-ray emission significantly lower than expected from their optical properties, suggesting that the two clusters are either not virialised or are gas poor. We find that the slope of the colour magnitude relation, for these groups and clusters, is constant at least up to z ∼ 1. We also analyse the dependence on environment of galaxy colours, luminosities, stellar masses, ages, and star formations. We find that galaxies in high-density regions are, on average, more luminous and massive than field galaxies up to z ∼ 2. The fraction of red galaxies increases with luminosity and with density up to z ∼ 1.2. At higher z this dependence on density disappears. The variation of galaxy properties as a function of redshift and density suggests that a significant change occurs at z ∼ 1.5-2.

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“…We have estimated the velocity dispersion of the cluster along the line-of-sight from the 11 galaxy members of the cluster with available spectroscopic redshifts (Table 1), which is σ 1D = 684 km s −1 . In order to estimate the size of the cluster we calculate the radius R 200 , which approximates the virial radius, from σ 1D (Díaz-Sánchez et al 2007) and we obtain R 200 = 1.39 Mpc. We use the relation given in reference Saro et al (2013) between the mass M cl and σ 1D to calculate the cluster mass, which gives M cl = (3.3 ± 0.5) × 10 14 M .…”

Section: Galaxy Clustermentioning

confidence: 99%

The Einstein ring GAL-CLUS-022058s: a Lensed Ultrabright Submillimeter Galaxy at z=1.4796

Díaz-Sánchez,

Dannerbauer,

Sulzenauer

et al. 2021

Preprint

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We report an ultra-bright lensed submillimeter galaxy at z spec = 1.4796, identified as a result of a full-sky cross-correlation of the AllWISE and Planck compact source catalogs aimed to search for bright submillimeter galaxies at z ∼ 1.5 − 2.8. APEX/LABOCA observations of the candidate galaxy reveal a source with flux (S 870µm = 54 ± 8 mJy). The position of the APEX source coincides with the position of the AllWISE mid-IR source, and with the Einstein ring GAL-CLUS-022058s, observed with the HST. Archival VLT/FORS observations reveal the redshift of this Einstein ring, z spec = 1.4796, and detection of the CO(5-4) line at z spec = 1.4802 with APEX/nFLASH230 confirms the redshift of the submillimeter emission. The lensed source appears to be gravitationally magnified by a massive foreground galaxy cluster lens at z = 0.36. We use Lenstool to model the gravitational lensing, which is near to a "fold arc" configuration for an elliptical mass distribution of the central halo, where four images of the lensed galaxy are seen; the mean magnification is µ L = 18 ± 4. We have determined an intrinsic rest-frame infrared luminosity of L IR ≈ 10 12 L and a likely star formation rate of ∼ 70 − 170 M yr −1 . The molecular gas mass is M mol ∼ 2.6 × 10 10 M and the gas fraction is f = 0.34 ± 0.07. We also obtain a stellar mass log(M * /M ) = 10.7 ± 0.1 and a specific star formation rate log(sSF R/Gyr −1 ) = 0.15 ± 0.03. This galaxy lies on the so-called main sequence of star-forming galaxies at this redshift.

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A low mass cluster of extremely red galaxies atz= 1.10 in the GOODS Southern Field

Cited by 14 publications

References 43 publications

Classification of extremely red objects in the Hubble Ultra Deep Field

Classification of extremely red objects in the Hubble Ultra Deep Field

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

The Einstein ring GAL-CLUS-022058s: a Lensed Ultrabright Submillimeter Galaxy at z=1.4796

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