The K20 survey

Cimatti, A.; Daddi, E.; Mignoli, M.; Pozzetti, L.; Renzini, A.; Zamorani, G.; Broadhurst, Tom; Fontana, A.; Saracco, P.; Poli, F.; Cristiani, S.; D’Odorico, S.; Giallongo, E.; Gilmozzi, R.; Menci, Nicola

doi:10.1051/0004-6361:20011696

Cited by 267 publications

(444 citation statements)

References 25 publications

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“…Without similar spectroscopic or morphological information, earlier ERO surveys divided the ERO population into two components: old, evolved systems or dusty, massive starbursts. But the true nature of K-selected EROs is likely to be much more complex, as suggested by recent work (McCarthy et al 2001;Cimatti et al 2002). McCarthy et al (2001) find a large scatter in the (VÀI ) colors of their ERO sample, best fitted by passive evolution models with extended star formation ( ¼ 1 Gyr).…”

Section: Introductionmentioning

confidence: 93%

“…Second, we adopt the generic colors of ðRÀIÞ ¼ 1:3 mag and ðHÀKÞ ¼ 1:0 mag to convert the surveys based on R-or H-band data to our IÀK colors. Third, we plot without additional correction the Cimatti et al (2002) results, even though they select EROs at a bluer limit: ðRÀK s Þ ! 5:0 mag.…”

Section: No 2 2003mentioning

confidence: 99%

“…This implies that the star formation history of EROs is more complex than a binary division into evolved elliptical galaxies or dusty, massive starbursts implies. From their K20 survey, Cimatti et al (2002) found that about half of their spectroscopic sample of $30 EROs are dusty star-forming galaxies with emission lines, while the remaining half are old stellar populations with absorption line spectra. However, the simple presence of line emission could span a wide range of galaxy types, from bulge-dominated, late-type spiral galaxies with a small amount of star formation through the more massive starbursts like HR 10.…”

Section: Introductionmentioning

confidence: 99%

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Hubble Space TelescopeWFPC2 Morphologies ofK‐selected Extremely Red Galaxies

Yan

Thompson

2003

ApJ

110

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We selected 115 extremely red objects (EROs) from deep Hubble Space Telescope (HST) WFPC2 archive data combined with ground-based K-band images, with (F814WÀK s ) ! 4, K-band signal-to-noise ratio !5, and a median limiting K s magnitude of $18.7, over a corresponding area of 228 arcmin 2 , for a morphological study of the ERO galaxy population. The survey covered a total of $409 arcmin 2 over 77 separate WFPC2 fields. This is the first complete sample of bright EROs with high-resolution HST morphologies. From a visual morphological classification, we find that 30% AE 5% of our (F814WÀK s ) ! 4 selected sample have morphologies consistent with a pure bulge or bulge-dominated galaxy (equivalent to E/S0), while disks comprise 64% AE 7% of the sample. Only 6% of the EROs remained unclassifiable. Mergers or strongly interacting systems, which includes sources from both classes, make up 17% AE 4% of the full sample. The quantitative Medium Deep Survey profile fitting is consistent with these results. These results highlight the complex nature of optical/near-IR color selected EROs. The dominant component of our sample is composed of disks, not spheroids or strongly interacting systems like HR 10. Using Bruzual & Charlot spectral energy distribution models, we investigated population differences in EROs selected by their (IÀK) versus (RÀK) colors and found that I-band based surveys preferentially select systems with prolonged star formation. Real differences in the surface densities of EROs in R-band and I-band based survey may reflect this color selection effect, complicating the comparisons between and interpretations on the nature of the ERO population. We conclude that only a small fraction of EROs at z $ 1 2 could be passively evolving elliptical galaxies formed at high redshift through a '' monolithic collapse '' mechanism. For the majority of EROs, even if most of their stellar mass is already in place at z $ 1, interaction with the environment and accretion of gas still play important roles in their continuing evolution.

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Section: Introductionmentioning

confidence: 93%

Section: No 2 2003mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Hubble Space TelescopeWFPC2 Morphologies ofK‐selected Extremely Red Galaxies

Yan

Thompson

2003

ApJ

110

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“…This color cut criterion alone may also select elliptical galaxies at z ' 2 (e.g., Cimatti et al 2002) and cool low-mass M/L/T stars (e.g., Kirkpatrick et al 1999;Hawley et al 2002). We can guard against such contaminants by utilizing near-infrared photometry.…”

Section: Near-infrared Imagingmentioning

confidence: 99%

Hubble Space TelescopeImaging and Keck Spectroscopy ofz≈ 6i‐Band Dropout Galaxies in the Advanced Camera for Surveys GOODS Fields

Stanway

Bunker

McMahon

et al. 2004

ApJ

140

169

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We measure the surface density of i 0 -band dropout galaxies at z $ 6 through wide-field Hubble Space Telescope (HST ) Advanced Camera for Surveys (ACS) imaging and ultradeep Keck DEIMOS spectroscopy. Using deep HST ACS SDSS i 0 (F775W) and SDSS z 0 (F850LP) imaging from the Great Observatories Origins Deep Survey-North (GOODS-N; 200 arcmin 2 ), we identify nine i 0 -drops satisfying (i 0 Àz 0 ) AB > 1:5 to a depth of z 0 AB ¼ 25:6 (corresponding to L Ã UV at z $ 3). We use HK 0 imaging data to improve the fidelity of our sample, discriminating against lower redshift red galaxies and cool Galactic stars. Three i 0 -drops are consistent with M/L/T dwarf stars. We present ultradeep Keck DEIMOS spectroscopy of 10 objects from our combined GOODS-N and GOODS-S i 0 -drop sample. We detect Ly emission at z ¼ 5:83 from one object in the GOODS-S field, which lies only 8 0 (i.e., 3 h À1 70 Mpc) away from a previously confirmed z ¼ 5:78 object. One possible Ly emitter at z ¼ 6:24 is found in the GOODS-N field (although identification of this spatially offset emission line is ambiguous). Using the rest-frame UV continuum from our six candidate z $ 6 galaxies from the GOODS-N field, we determine a lower limit to the unobscured volume-averaged global star formation rate at z $ 6 of (5:4 AE 2:2) ; 10 À4 h 70 M yr À1 Mpc À3 . We find that the cosmic star formation density in Lyman break galaxies (LBGs) with unobscured star formation rates greater than 15 M yr À1 falls by a factor of 8 between z $ 3 and z $ 6. Hence, the luminosity function of LBGs must evolve in this redshift interval: a constant integrated star formation density at z > 3 requires a much steeper faint-end slope, or a brighter characteristic luminosity. This result is in agreement with our previous measurement from the GOODS-S field, indicating that cosmic variance is not a dominant source of uncertainty.

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“…Our algorithm evaluates the 3D galaxy density using angular positions and photometric redshifts with the purpose of: i) detecting galaxy overdensities in three dimensions; and ii) assigning to each galaxy a measure of the environmental density, to extend the analysis of the environmental effects on galaxy evolution to the limits of photometric surveys. The method is applied to a deep photometric survey of the Chandra Deep Field South (Cimatti et al 2002a), where we re-discover some previously known overdensities and we find a clear relation between the fraction of blue and red galactic types and the local density. The paper is organised as follows.…”

Section: Introductionmentioning

confidence: 99%

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

Trèvese

Castellano

Fontana

et al. 2006

A&A

Self Cite

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Aims. We study galaxy clustering and explore the dependence of galaxy properties on the the environment up to a redshift z ∼ 1, on the basis of a deep multi-band survey in the Chandra Deep Field South. Methods. We have developed a new method which combines galaxy angular positions and photometric redshifts to estimate the local galaxy number-density. This allows both the detection of overdensities in the galaxy distribution and the study of the properties of the galaxy population as a function of the environmental density. Results. We detect two moderate overdensities at z ∼ 0.7 and z ∼ 1 previously identified spectroscopically. We find that the fraction of red galaxies within each structure increases with volume density, extending to z ∼ 1 previous results. We measure "red sequence" slopes consistent with the values found in X-ray selected clusters, supporting the notion that the mass-metallicity relation hold constant up to z ∼ 1. Conclusions. Our method based on photometric redshifts allows to extend structure detection and density estimates up to the limits of photometric surveys, i.e. considerably deeper than spectroscopic surveys. Since X-ray cluster detection at high redshift is presently limited to massive relaxed structures, galaxy volume density based on photometric redshift appears as a valuable tool in the study of galaxy evolution.

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The K20 survey

Cited by 267 publications

References 25 publications

Hubble Space TelescopeWFPC2 Morphologies ofK‐selected Extremely Red Galaxies

Hubble Space TelescopeWFPC2 Morphologies ofK‐selected Extremely Red Galaxies

Hubble Space TelescopeImaging and Keck Spectroscopy ofz≈ 6i‐Band Dropout Galaxies in the Advanced Camera for Surveys GOODS Fields

A new (2+1)D cluster finding algorithm based on photometric redshifts: large scale structure in the Chandra deep field south

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