The VIMOS Ultra-Deep Survey: ~10 000 galaxies with spectroscopic redshifts to study galaxy assembly at early epochs 2 &lt;<i>z</i>≃ 6

Fèvre, O. Le; Tasca, L.; Cassata, P.; Garilli, B.; Brun, V. Le; Maccagni, D.; Pentericci, L.; Thomas, Romain; Vanzella, E.; Zamorani, G.; Zucca, E.; Amorín, R.; Bardelli, S.; Capak, P.; Cassarà, L. P.; Castellano, M.; Cimatti, A.; Cuby, J. G.; Cucciati, O.; Torre, S. de la; Durkalec, A.; Fontana, A.; Giavalisco, Mauro; Grazian, A.; Hathi, N. P.; Ilbert, O.; Lemaux, B. C.; Moreau, C.; Paltani, S.; Ribeiro, B.; Salvato, M.; Schaerer, D.; Scodeggio, M.; Sommariva, V.; Talia, M.; Taniguchi, Yoshiaki; Tresse, L.; Vergani, D.; Wang, P.W.; Charlot, S.; Contini, T.; Fotopoulou, S.; López-Sanjuán, C.; Mellier, Y.; Scoville, N. Z.

doi:10.1051/0004-6361/201423829

Cited by 309 publications

(234 citation statements)

References 109 publications

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“…Photometric redshifts from HyperZ based on the original, multi-band, position-matched catalogs and our new forced photometry are compared to high-quality spectroscopic redshifts 21 from the VIMOS VLT Deep Survey (VVDS; Le Fèvre et al 2013) and the VIMOS Ultra-Deep Survey (VUDS; Le Fèvre et al 2015) in Figure 12. The top left and right panels of this figure show photometric redshifts from the original VIDEO-selected input catalog and our new forced photometry, respectively.…”

Section: Spectroscopic Redshift Comparisonmentioning

confidence: 99%

An Application of Multi-band Forced Photometry to One Square Degree of SERVS: Accurate Photometric Redshifts and Implications for Future Science

Nyland

Lacy

Sajina

et al. 2017

ApJS

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We apply The Tractor image modeling code to improve upon existing multi-band photometry for the Spitzer Extragalactic Representative Volume Survey (SERVS). SERVS consists of post-cryogenic Spitzer observations at 3.6 and 4.5 μm over five well-studied deep fields spanning 18 deg 2 . In concert with data from ground-based near-infrared (NIR) and optical surveys, SERVS aims to provide a census of the properties of massive galaxies out to z≈5. To accomplish this, we are using The Tractor to perform "forced photometry." This technique employs prior measurements of source positions and surface brightness profiles from a high-resolution fiducial band from the VISTA Deep Extragalactic Observations survey to model and fit the fluxes at lower-resolution bands. We discuss our implementation of The Tractor over a square-degree test region within the XMM Large Scale Structure field with deep imaging in 12 NIR/optical bands. Our new multi-band source catalogs offer a number of advantages over traditional position-matched catalogs, including (1) consistent source cross-identification between bands, (2) deblending of sources that are clearly resolved in the fiducial band but blended in the lowerresolution SERVS data, (3) a higher source detection fraction in each band, (4) a larger number of candidate galaxies in the redshift range 5<z<6, and (5) a statistically significant improvement in the photometric redshift accuracy as evidenced by the significant decrease in the fraction of outliers compared to spectroscopic redshifts. Thus, forced photometry using The Tractor offers a means of improving the accuracy of multi-band extragalactic surveys designed for galaxy evolution studies. We will extend our application of this technique to the full SERVS footprint in the future.

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Section: Spectroscopic Redshift Comparisonmentioning

confidence: 99%

An Application of Multi-band Forced Photometry to One Square Degree of SERVS: Accurate Photometric Redshifts and Implications for Future Science

Nyland

Lacy

Sajina

et al. 2017

ApJS

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“…Its main aim is to study early phases of galaxy formation and evolution at 2 < z < 6. Details about the survey strategy, target selection, and data processing and redshift measurements are presented in Le Fèvre et al (2015).…”

Section: Vuds Datamentioning

confidence: 99%

“…The sample used here contains 3022 galaxies with reliable spectroscopic redshifts (spectroscopy reliability flags 2, 3, 4 and 9, see Le Fèvre et al 2015) and with a stellar mass in the range 9 < log (M * ) < 11 M as presented in Fig. 1.…”

Section: Vuds Datamentioning

confidence: 99%

Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency atz≃ 3

Durkalec

Fèvre

Torre

et al. 2015

A&A

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The relation between the galaxy stellar mass M and the dark matter halo mass M h gives important information on the efficiency in forming stars and assembling stellar mass in galaxies. We present measurements of the ratio of stellar mass to halo mass (SMHR) at redshifts 2 < z < 5, obtained from the VIMOS Ultra Deep Survey. We use halo occupation distribution (HOD) modelling of clustering measurements on ∼3000 galaxies with spectroscopic redshifts to derive the dark matter halo mass M h , and spectral energy density fitting over a large set of multi-wavelength data to derive the stellar mass M and compute the SMHR = M /M h . We find that the SMHR ranges from 1% to 2.5% for galaxies with M = 1.3 × 10 9 M to M = 7.4 × 10 9 M in DM halos with M h = 1.3 × 10 11 M to M h = 3 × 10 11 M . We derive the integrated star formation efficiency (ISFE) of these galaxies and find that the star formation efficiency is a moderate 6−9% for lower mass galaxies, while it is relatively high at 16% for galaxies with the median stellar mass of the sample ∼7 × 10 9 M . The lower ISFE at lower masses may indicate that some efficient means of suppressing star formation is at work (like SNe feedback), while the high ISFE for the average galaxy at z ∼ 3 indicates that these galaxies efficiently build up their stellar mass at a key epoch in the mass assembly process. Based on our results, we propose a possible scenario in which the average massive galaxy at z ∼ 3 begins to experience truncation of its star formation within a few million years.

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“…To date, the number of z ∼ 6, z ∼ 7, and z ≥ 8 galaxies selected in deep surveys count in the thousands (e.g., Le Fevre et al 2015;Bouwens et al 2014b;Monna et al 2014;Willott et al 2013), several hundreds (e.g., Bouwens et al 2011;Ouchi et al 2009;Ouchi et al 2013;Tilvi et al 2013) and about one hundred (e.g., Labbé et al 2013;Oesch et al 2014b;Schmidt et al 2014;Zheng et al 2012;Trenti et al 2012), respectively. Thanks to A&A 575, A92 (2015) the ever-increasing numbers of objects, the evolution and properties of galaxies is relatively well constrained up to z ∼ 6, with many secure spectroscopic confirmations (e.g., Jiang et al 2013;Willott et al 2013;Stark et al 2014;Curtis-Lake et al 2013;Schenker et al 2012;Le Fevre et al 2015). Beyond z ∼ 6, however, spectroscopic follow-up remains extremely challenging as a result of the decreasing mean brightness of these objects (Finkelstein et al 2013) and the nature of extreme mid-z interlopers that may contaminate the high-z sample (Hayes et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Frontier Fields: Combining HST, VLT, andSpitzerdata to explore thez~ 8 Universe behind the lensing cluster MACSJ0416.1−2403

Laporte

Streblyanska

Kim

et al. 2015

A&A

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Context. The Hubble Space Telescope (HST) Frontier Fields (HFFs) project started at the end of 2013 with the aim of providing extremely deep images of six massive galaxy clusters. One of the main goals of this program is to push several telescopes to their limits to provide the best current view of the earliest stages of the Universe. The analysis of the initial data has already demonstrated the huge capabilities of the program. Aims. We present a detailed analysis of z ∼ 8 objects behind the HFFs lensing cluster, MACSJ0416.1-2403, combining 0.3−1.6 µm imaging from HST, ground-based K s imaging from VLT HAWK-I, and 3.6 µm and 4.5 µm Spitzer Space Telescope. The images probe to 5σ depths of ≈29 AB for HST, 25.6 AB for HAWK-I, and ≈0.310 and 0.391 µJy at 3.6 and 4.5 µm, respectively. With these datasets, we assess the photometric properties of z ∼ 8 galaxies in this field, as well as their distribution in luminosity, to unprecedented sensitivity. Methods. We applied the classical Lyman break (LB) technique, which combines non detection criteria in bands blueward of the Lyman break at z ∼ 8 and color-selection in bands redward of the break. To avoid contamination by mid-z interlopers, we required a strong break between optical and near-infrared data. We determined the photometric properties of z ∼ 8 selected candidates using spectral energy distribution (SED)-fitting with standard library templates. The luminosity function at z ∼ 8 is computed using a Monte-Carlo method taking advantage of the SED-fitting results. A piece of cautionary information is gleaned from new deep optical photometry of a previously identified z ∼ 8 galaxy in this cluster, which is now firmly detected as a mid-z interloper with a strong ≈1.5 mag Balmer break (between F606W and F125W). Using the SED of this interloper, we estimated the contamination rate of our MACSJ0416.1−2403 sample, and that of previous samples in Abell 2744 that were based on HFF data, we highlight the dangers of pushing the LB technique too close to the photometry limits. Results. Our selection reliably recovers four objects with m F160W ranging from 26.0 to 27.9 AB that are located in modestamplification regions (µ < 2.4). Two of the objects display a secondary break between the IRAC 3.6 µm and 4.5 µm bands, which could be associated to the Balmer break or emission lines at z ∼ 8. The SED-fitting analysis suggests that all of these objects favor high-z solutions with no reliable secondary solutions. The candidates generally have star formation rates around ∼10 M /yr and sizes ranging from 0.2 to 0.5 kpc, which agrees well with previous observations and expectations for objects in the early Universe. The sample size and luminosity distribution are consistent with previous findings.

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The VIMOS Ultra-Deep Survey: ~10 000 galaxies with spectroscopic redshifts to study galaxy assembly at early epochs 2 <z≃ 6

Cited by 309 publications

References 109 publications

An Application of Multi-band Forced Photometry to One Square Degree of SERVS: Accurate Photometric Redshifts and Implications for Future Science

An Application of Multi-band Forced Photometry to One Square Degree of SERVS: Accurate Photometric Redshifts and Implications for Future Science

Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency atz≃ 3

Frontier Fields: Combining HST, VLT, andSpitzerdata to explore thez~ 8 Universe behind the lensing cluster MACSJ0416.1−2403

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