A star-forming galaxy at<b>z</b>= 5.78 in the<b>Chandra</b>Deep Field South

Bunker, Andrew J.; Stanway, Elizabeth R.; Ellis, Richard S.; McMahon, R. G.; McCarthy, Patrick J.

doi:10.1046/j.1365-8711.2003.06664.x

Cited by 103 publications

(130 citation statements)

References 33 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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“…A substantial amount of spectroscopic confirmation is available for LBGs at z ∼ 5−6 (Bunker et al 2003;Stanway et al 2004;Dickinson et al 2004;Eyles et al 2007;Stark et al 2007;Vanzella et al 2008). This allowed early estimates of the stellar mass density at those redshifts.…”

Section: Introductionmentioning

confidence: 99%

Searching for massive galaxies at z ≥ 3.5 in GOODS-North

Mancini

Matute

Cimatti

et al. 2009

A&A

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Aims. We constrain the space density and properties of massive galaxy candidates at redshifts of z ≥ 3.5 in the Great Observatories Origin Deep Survey North (GOODS-N) field. By selecting sources in the Spitzer + IRAC bands, a sample highly complete in stellarmass is assembled, including massive galaxies that are very faint in the optical/near-IR bands and would be missed by samples selected at shorter wavelengths. Methods. The z ≥ 3.5 sample was selected to m AB = 23 mag at 4.5 μm using photometric redshifts obtained by fitting the galaxies spectral energy distribution at optical, near-IR bands, and IRAC bands. We also require that the brightest band (in AB scale) in which candidates are detected is the IRAC 8.0 μm band to ensure that the near-IR 1.6 μm (rest-frame) peak is falling in or beyond this band. Results. We found 53 z ≥ 3.5 candidates, of masses in the range M ∼ 10 10 −10 11 M . At least ∼81% of these galaxies are missed by traditional Lyman Break selection methods based on ultraviolet light. Spitzer + MIPS emission is detected for 60% of the sample of z ≥ 3.5 galaxy candidates. Although in some cases this might suggest a residual contamination from lower redshift starforming galaxies or Active Galactic Nuclei, 37% of these objects are also detected in the sub-mm/mm bands in SCUBA, AzTEC, and MAMBO surveys, and have properties fully consistent with vigorous starburst galaxies at z ≥ 3.5. The comoving number density of galaxies with stellar masses of above 5 × 10 10 M (a reasonable stellar-mass completeness limit for our sample) is 2.6 × 10 −5 Mpc −3 (using the volume within 3.5 < z < 5), and the corresponding stellar mass density is ∼(2.9 ± 1.5) × 10 6 M Mpc −3 , or about 3% of the local density above the same stellar mass limit. For the subsample of MIPS-undetected galaxies, we measure a number density of ∼0.97 × 10 −5 Mpc −3 and a stellar mass density of ∼(1.15 ± 0.7) × 10 6 M Mpc −3 . Even in the unlikely case that these are all truly quiescent galaxies, this would imply an increase in the space density of passive galaxies by a factor of ∼15 between z ∼ 4 and z = 2, and by ∼100 to z = 0.

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“…Motivated by the discovery of high-redshift, z % 6 quasars with what appeared to be Gunn-Peterson troughs (Becker et al 2001;Djorgovski et al 2001), many research groups began to search for the sources responsible for reionization (see, e.g., Lehnert & Bremer 2003;Bremer et al 2004b;Stanway et al 2004aStanway et al , 2004bBunker et al 2003;Ajiki et al 2003;Rhoads et al 2003;Bouwens et al 2004;Hu et al 2004). The Wilkinson Microwave Anisotropy Probe (WMAP) result of the surprising detection of a large Thompson electron optical depth of ¼ 0:17 AE 0:04 (Kogut et al 2003) and questions about whether the intergalactic opacity at z % 6 is due to the neutral intergalactic medium (IGM) or to discrete absorbers (e.g., Songaila & Cowie 2002) have led observers to try and push discovery techniques into the near-infrared (NIR) and beyond the redshift of the most distant Sloan quasars (Pelló et al 2004;Kneib et al 2004).…”

Section: Introductionmentioning

confidence: 99%

“…To reconcile the possible Gunn-Peterson troughs observed in high-redshift quasar spectra and the WMAP results, the fact that the ionizing photon density at high redshift appears to be declining (e.g., Lehnert & Bremer 2003;Bunker et al 2003) and the rapidly increasing density necessary to ionize the IGM at successively higher redshifts (e.g., Madau et al 1999) suggest that the universe may have had a complex reionization history. Indeed, these arguments led some researchers to propose complex models such as extended partial reionization (e.g., Madau et al 2004;Ricotti & Ostriker 2004) or twice reionization (e.g., Cen 2003;Ciardi et al 2003;Wyithe & Loeb 2003).…”

Section: Introductionmentioning

confidence: 99%

Deep Very Large TelescopeV‐Band Imaging of the Field of az= 10 Candidate Galaxy: Below the Lyman Limit?

Lehnert¹,

Schreiber²,

Bremer³

2005

ApJ

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We present a deep 16.8 ks V-band image of the field of a candidate z ¼ 10 galaxy magnified by the foreground (z ¼ 0:25) cluster A1835. The image was obtained with FORS1 on VLT-Kueyen to test whether the V band lies below the Lyman limit for this very high redshift candidate. A detection would unambiguously rule out that the source is at z ¼ 10. The 3 detection limit of the image in the area of the z ¼ 10 candidate is V AB ¼ 28:0 mag in a 2 00 diameter aperture (about 3 times the seeing FWHM of 0B7). No source at the position of the candidate galaxy is detected down to this limit. Formally, this is consistent with the V-band probing below the Lyman limit in the rest frame of a z ¼ 10 source. However, given the recent nondetection of the object in a deep H-band exposure with NIRI on Gemini North down to H AB ¼ 26:0 mag (3 in a 1B4 aperture) and concerns about the detection of the reported associated emission line, it may be possible that this source is spurious. We discuss several astrophysical possibilities to explain the puzzling nature of this source and find none of them compelling.

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A star-forming galaxy atz= 5.78 in theChandraDeep Field South

Cited by 103 publications

References 33 publications

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

Searching for massive galaxies at z ≥ 3.5 in GOODS-North

Deep Very Large TelescopeV‐Band Imaging of the Field of az= 10 Candidate Galaxy: Below the Lyman Limit?

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