Photometric Redshifts and Selection of High-Redshift Galaxies in the NTT and Hubble Deep Fields

Fontana, A.; D’Odorico, S.; Poli, F.; Giallongo, E.; Arnouts, S.; Cristiani, S.; Moorwood, A. F. M.; Saracco, P.

doi:10.1086/316803

Cited by 154 publications

(177 citation statements)

References 42 publications

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“…Fontana et al (2000) find that photometric redshifts including IR colours select nearly a factor of 2 more high redshift galaxy candidates in the Hubble Deep Fields (HDFs) than pure LBG photometric selection does, to the same flux limits. However, this discrepancy cannot be resolved spectroscopically.…”

Section: Introductionmentioning

confidence: 94%

Probing the faint end of the Galaxy luminosity function at $\vec{z}=$ 3 with Lyαemission

Fynbo

Møller

Thomsen³

2001

A&A

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Abstract. We present spectroscopic observations obtained with the ESO Very Large Telecope (VLT) of seven candidate Lyα emitting galaxies in the field of the radio quiet Q1205-30 at z = 3.04 previously detected with deep narrow band imaging. Based on equivalent widths and limits on line ratios we confirm that all seven objects are Lyα emitting galaxies. Deep images also obtained with the VLT in the B and I bands show that five of the seven galaxies have very faint continuum fluxes (I(AB) ≈ 26.8 and B(AB) ≈ 27.3). The star formation rates of these seven galaxies estimated from the rest-frame UV continuum around 2000Å, as probed by the I-band detections, as well as from the Lyα luminosities, are 1-4 M yr −1 assuming a Hubble constant of 65 km s −1 Mpc −1 , Ωm = 0.3, and ΩΛ = 0.7. This is 1-3 orders of magnitude lower than for other known populations of star-forming galaxies at similar redshifts (the Lyman-Break galaxies and the sub-mm selected sources). The inferred density of the objects is high, 16 ± 4 per arcmin 2 per unit redshift. This is consistent with the integrated luminosity function for Lyman-Break galaxies down to R = 27 if the fraction of Lyα emitting galaxies is ≈70% at the faint end of the luminosity function. However, if this fraction is 20% as reported for the bright end of the luminosity function then the space density in this field is significantly larger (by a factor of 3.5) than expected from the luminosity function for Lyman-Break galaxies in the HDF-North. This would be an indication that at least some radio quiet QSOs at high redshift reside in overdense environments or that the faint end slope of the high redshift luminosity function has been underestimated. We find evidence that the faint Lyα galaxies are essentially dust-free. These observations show that Lyα emission is an efficient method by which to probe the faint end of the luminosity function at high redshifts.

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Section: Introductionmentioning

confidence: 94%

Probing the faint end of the Galaxy luminosity function at $\vec{z}=$ 3 with Lyαemission

Fynbo

Møller

Thomsen³

2001

A&A

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“…Finally we also release de-magnified M star and SFRs as a function of redshift for galaxies in our catalogues obtained through SED fitting. Galaxy properties are computed by fitting Bruzual & Charlot (2003) templates with our custom zphot.exe code (Giallongo et al 1998;Fontana et al 2000;Grazian et al 2006) at the previously determined median photometric redshift. In the BC03 fit we assume exponentially declining star formation histories with e-folding time 0.1 ≤ τ ≤ 15, a Salpeter (1955) initial mass function, and we allow both Calzetti et al (2000) and Small Magellanic Cloud (Prevot et al 1984) extinction laws.…”

Section: Demagnified Number Counts and Rest-frame Physical Propertiesmentioning

confidence: 99%

The ASTRODEEP Frontier Fields catalogues

Criscienzo

Merlin

Castellano

et al. 2017

A&A

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Aims. We present the multiwavelength photometry of two Frontier Fields massive galaxy clusters, MACS-J0717 and MACS-J1149, and their parallel fields, ranging from Hubble Space Telescope (HST) to ground-based K and Spitzer IRAC bands, and the public release of photometric redshifts and rest-frame properties of galaxies found in cluster and parallel pointings. This work was carried out within the ASTRODEEP project and aims to provide a reference for future investigations of extragalactic populations. Methods. To fully exploit the depth of the images and detect faint sources, we used an accurate procedure, which carefully removes the foreground light of bright cluster sources and the intra-cluster light thus enabling detection and measurement of accurate fluxes in crowded cluster regions. This same procedure has been successfully used to derive the photometric catalogue of MACS-J0416 and Abell-2744. Results. The obtained multiband photometry was used to derive photometric redshifts, magnification, and physical properties of sources. In line with the first two FF catalogues released by ASTRODEEP, the photometric redshifts reach ∼4% accuracy. Moreover we extend the presently available samples to galaxies intrinsically as faint as H160 ∼ 32-34 mag thanks to the magnification factors induced by strong gravitational lensing. Our analysis allows us to probe galaxy masses larger than 10 7 M and/or SFR = 0.1-1 M /yr out to redshift z > 6.

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“…Next, the mode of the distribution is calculated, and all the objects beyond ±3σ from the FWHM mode can be rejected. Based on the NTT deep field catalogue (Fontana et al 2000) we estimate that ∼45% of compact galaxies have colours consistent with GRBs (see the lower right panel of Fig. 2).…”

Section: Rejection Of Non-transient Sources With Similar Colours As Oasmentioning

confidence: 99%

“…Most of the galaxies can however be eliminated because of their non-stellar profile. Lower right panel: we have over-plotted the colours of the galaxies from the NTT deep field (Fontana et al 2000) to illustrate the problem of the contamination by galaxies (see Sect. 3.4).…”

Section: Candidate Selection Using Colour-colour Diagramsmentioning

confidence: 99%

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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Abstract.We report the discovery of the optical and near-infrared counterparts to GRB 001011. The GRB 001011 error box determined by Beppo-SAX was simultaneously imaged in the near-infrared by the 3.58-m New Technology Telescope and in the optical by the 1.54-m Danish Telescope ∼8 hr after the gamma-ray event. Here we implement the colour-colour discrimination technique proposed by Rhoads (2001) and extend it using near-IR data as well. We present the results provided by an automatic colour-colour discrimination pipe-line developed to discern the different populations of objects present in the GRB 001011 error box. Our software revealed three candidates based on single-epoch images. Second-epoch observations carried out ∼3.2 days after the burst revealed that the most likely candidate had faded, thus identifying it with the counterpart to the GRB. In deep R-band images obtained 7 months after the burst a faint (R = 25.38 ± 0.25) elongated object, presumably the host galaxy of GRB 001011, was detected at the position of the afterglow. The GRB 001011 afterglow is the first discovered with the assistance of colour-colour diagram techniques. We discuss the advantages of using this method and its application to error boxes determined by future missions.

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Photometric Redshifts and Selection of High-Redshift Galaxies in the NTT and Hubble Deep Fields

Cited by 154 publications

References 42 publications

Probing the faint end of the Galaxy luminosity function at $\vec{z}=$ 3 with Lyαemission

Probing the faint end of the Galaxy luminosity function at $\vec{z}=$ 3 with Lyαemission

The ASTRODEEP Frontier Fields catalogues

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

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