The great observatories origins deep survey

Popesso, P.; Dickinson, Mark; Nonino, M.; Vanzella, E.; Daddi, E.; Fosbury, R. A. E.; Küntschner, H.; Mainieri, V.; Cristiani, S.; Césarsky, C. J.; Giavalisco, Mauro; Renzini, A.

doi:10.1051/0004-6361:200809617

Cited by 249 publications

(303 citation statements)

References 25 publications

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“…Our first galaxy sample contains 2422 galaxies with secure spectroscopic redshifts (z spec ) from the ESO public compilation in the Chandra Deep Field South (CDFS; Cristiani et al 2000;Croom et al 2001;Bunker et al 2003;Dickinson et al 2004;Stanway et al 2004aStanway et al , 2004bStrolger et al 2004;Szokoly et al 2004;van der Wel et al 2004;Doherty et al 2005;Le Fèvre et al 2005;Mignoli et al 2005;Ravikumar et al 2007;Popesso et al 2009;Balestra et al 2010;Silverman et al 2010;Kurk et al 2013;Vanzella et al 2014) and from Morris et al (2015). In order to obtain multiwavelength photometry for these galaxies, we cross-matched this sample with the public Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS; Grogin et al 2011;Koekemoer et al 2011) catalog for the Great Observatory Origins Deep Survey South field (GOODS-S) obtained by Guo et al (2013).…”

Section: Samplementioning

confidence: 99%

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

Bisigello

Caputi

Colina

et al. 2016

ApJS

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The determination of galaxy redshifts in the James Webb Space Telescope's (JWST) blank-field surveys will mostly rely on photometric estimates, based on the data provided by JWST's Near-Infrared Camera (NIRCam) at 0.6-5.0 μm and Mid Infrared Instrument (MIRI) at l m > 5.0 m. In this work we analyze the impact of choosing different combinations of NIRCam and MIRI broadband filters (F070W to F770W), as well as having ancillary data at l m < 0.6 m, on the derived photometric redshifts (z phot ) of a total of 5921 real and simulated galaxies, with known input redshifts z=0-10. We found that observations at l m < 0.6 m are necessary to control the contamination of high-z samples by low-z interlopers. Adding MIRI (F560W and F770W) photometry to the NIRCam data mitigates the absence of ancillary observations at l m < 0.6 m and improves the redshift estimation. At z=7-10, accurate z phot can be obtained with the NIRCam broadbands alone when  S N 10, but the z phot quality significantly degrades at  S N 5. Adding MIRI photometry with 1 mag brighter depth than the NIRCam depth allows for a redshift recovery of 83%-99%, depending on spectral energy distribution type, and its effect is particularly noteworthy for galaxies with nebular emission. The vast majority of NIRCam galaxies with [F150W]=29AB mag at z=7-10 will be detected with MIRI at [F560W, F770W] < 28 mag if these sources are at least mildly evolved or have spectra with emission lines boosting the mid-infrared fluxes.

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Section: Samplementioning

confidence: 99%

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

Bisigello

Caputi

Colina

et al. 2016

ApJS

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“…During this work, when the identification and SED analysis of GOODS-S sources had already been completed, a number of additional spectroscopic redshifts were made available (Ravikumar et al 2007;Vanzella et al 2008;Popesso et al 2009), which Wuyts et al 2008 compiled into their FIREWORKS catalog. We then adopted the FIREWORKS spectroscopic redshifts for the optical/NIR/IRAC sources that we had previously identified as robust counterparts to 24 μm sources.…”

Section: Goods-s Fieldmentioning

confidence: 99%

Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelengthSpitzerobservations up toz ~ 2.5

Rodighiero¹,

Vaccari²,

Franceschini³

et al. 2010

A&A

155

145

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Context. Studies of the infrared (IR) emission of cosmic sources have proven essential to constraining the evolutionary history of cosmic star formation and the gravitational accretion of nuclear black holes, because many of these events occur inside heavily dustextinguished environments. Aims. The Spitzer Space Telescope has provided a large amount of data to constrain the nature and cosmological evolution of infrared source populations. In the present paper we exploit a large homogeneous dataset to derive a self-consistent picture of IR emission based on the time-dependent λ eff = 24, 15, 12, and 8 μm monochromatic and bolometric IR luminosity functions (LF) over the full 0 < z < 2.5 redshift range. Methods. Our present analysis is based on a combination of data from deep Spitzer surveys of the VIMOS VLT Deep Survey (VVDS-SWIRE) and GOODS fields. To our limiting flux of S 24 = 400 μJy, our sample derived from VVDS-SWIRE includes 1494 sources, and 666 and 904 sources brighter than S 24 = 80 μJy are catalogued in GOODS-S and GOODS-N, respectively, for a total area of ∼0.9 square degrees. Apart from a few galaxies, we obtain reliable optical identifications and redshifts for all these sources, providing a rich and robust dataset for our luminosity function determination. The final combined reliable sample includes 3029 sources, the fraction with photometric redshifts being 72% over all redshifts and almost all galaxies at z > 1.5. Based on the multiwavelength information available in these areas, we constrain the LFs at 8, 12, 15, and 24 μm. We also infer the total IR luminosities from our best-fit model of the observed SEDs of each source, and use this to derive the bolometric (8−1000 μm) LF and comoving volume emissivity to z ∼ 2.5. Results. In the redshift interval 0 < z < 1, the bolometric IR luminosity density evolves as (1 + z) 3.8±0.4 . Although it is more uncertain at higher-z, our results show a flattening in the IR luminosity density at z > 1. The mean redshift of the peak in the source number density shifts with luminosity: the brightest IR galaxies appear to form stars at earlier cosmic times (z > 1.5), while star formation in the less luminous galaxies continues until more recent epochs (z ∼ 1 for L IR < 10 11 L ), in overall agreement with similar analyses in the literature. Conclusions. Our results are indicative of a rapid increase in the galaxy IR comoving volume emissivity up to z ∼ 1 and a constant average emissivity at z > 1. We also appear to measure a difference in the evolutionary rate of the source number densities as a function of luminosity, which is consistent with the downsizing evolutionary patterns reported for other samples of cosmic sources.

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“…) and GOODS-S (Szokoly et al 2004;Le Fèvre et al 2004;Mignoli et al 2005;Vanzella et al 2005Vanzella et al , 2006Vanzella et al , 2008Ravikumar et al 2007;Popesso et al 2009;Kurk et al 2009;Balestra et al 2010;…”

Section: Goods Sampleunclassified

GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

Hwang¹,

Elbaz²,

Dickinson³

et al. 2011

A&A

Self Cite

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Aims. We study the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies and its evolution at 0 < z < 1.2. Methods. Using the high-z galaxies in the fields of Great Observatories Origins Deep Survey (GOODS) observed by the Herschel Space Observatory in the framework of the GOODS-Herschel key program and the local IRAS or AKARI-selected galaxies in the field of Sloan Digital Sky Survey Data Release 7, we investigate the dependence of galaxy properties on the morphology of and the distance to the nearest neighbor galaxy. Results. We find that the star-formation rates (SFRs) and the specific SFRs (SSFRs) of galaxies on average depend on the morphology of and the distance to the nearest neighbor galaxy in this redshift range. When a late-type galaxy has a close neighbor galaxy, the SFR and the SSFR increase as it approaches a late-type neighbor, which is supported by Kolmogorov-Smirnov (K-S) and Monte Carlo (MC) tests with a significance level of >99%. However, the SFR and the SSFR decrease or do not change much as the galaxy approaches an early-type neighbor. The bifurcations of SFRs and SSFRs depending on the neighbor's morphology seem to occur at R n ≈ 0.5r vir,nei (virial radius of the neighbor), which is supported by K-S and MC tests with a significance level of >98%. For all redshift bins, the SSFRs of late-type galaxies interacting with late-type neighbors are increased by factors of about 1.8 ± 0.7 and 4.0 ± 1.2 compared to those of non-interacting galaxies when the pair separation is smaller than 0.5r vir,nei and 0.1r vir,nei , respectively. The dust temperature of both local and high-z late-type galaxies that strongly interact with late-type neighbors (i.e. R n ≤ 0.1r vir,nei ) appears to be higher than that of non-interacting galaxies with a significance level of 96−99%. However, the dust temperature of local late-type galaxies that strongly interact with early-type neighbors seems to be lower than or similar to that of non-interacting galaxies. Conclusions. Our results suggest that galaxy-galaxy interactions and mergers have been strongly affecting the SFR and the dust properties of star-forming galaxies over at least 8 billion years.

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The great observatories origins deep survey

Cited by 249 publications

References 25 publications

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelengthSpitzerobservations up toz ~ 2.5

GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

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