THE
                    <i>HUBBLE SPACE TELESCOPE</i>
                    WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2-2 μm WAVELENGTH

Windhorst, Rogier A.; Cohen, Seth H.; Hathi, N. P.; McCarthy, Patrick J.; Ryan, Russell E.; Yan, Haojing; Baldry, I. K.; Driver, Simon P.; Frogel, J. A.; Hill, D. T.; Kelvin, Lee S.; Koekemoer, Anton M.; Mechtley, Matthew; O’Connell, R. W.; Robotham, Aaron S. G.; Rutkowski, Michael J.; Seibert, Mark; Straughn, Amber N.; Tuffs, R.; Balick, Bruce; Bond, Howard E.; Bushouse, H.; Calzetti, Daniela; Crockett, M.; Disney, M. J.; Dopita, Michael A.; Hall, Donald N. B.; Holtzman, Jon A.; Kaviraj, Sugata; Kimble, Randy A.; MacKenty, John; Mutchler, Max; Paresce, Francesco; Saha, A.; Silk, Joseph; Trauger, John T.; Walker, A. R.; Whitmore, Bradley C.; Young, Erick T.

doi:10.1088/0067-0049/193/2/27

Cited by 274 publications

(308 citation statements)

References 112 publications

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“…The field was observed in the F435W, F606W, F775W, F814W and F850LP bands. Near-infrared WFC3/IR data combines data from Grogin et al (2011), Koekemoer et al (2011) and Windhorst et al (2011) with observations made in the F098M, F125W, and F160W bands. The VLT/HAWK-I K s -band imaging are taken from the HUGS survey (Fontana et al 2014).…”

Section: Photometrymentioning

confidence: 99%

An extreme [O III] emitter atz= 3.2: a low metallicity Lyman continuum source

Barros

Vanzella

Amorín

et al. 2015

A&A

191

158

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Aims. Cosmic reionization is an important process occurring in the early epochs of the Universe. However, because of observational limitations due to the opacity of the intergalactic medium to Lyman continuum photons, the nature of ionizing sources is still not well constrained. While high-redshift star-forming galaxies are thought to be the main contributors to the ionizing background at z > 6, it is impossible to directly detect their ionizing emission. Therefore, looking at intermediate redshift analogues (z ∼ 2−4) can provide useful hints about cosmic reionization. Methods. We investigate the physical properties of one of the best Lyman continuum emitter candidate at z = 3.212 found in the GOODS-S/CANDELS field with photometric coverage from the U to the MIPS 24 μm band and VIMOS/VLT and MOSFIRE/Keck spectroscopy. These observations allow us to derive physical properties such as stellar mass, star formation rate, age of the stellar population, dust attenuation, metallicity, and ionization parameter, and to determine how these parameters are related to the Lyman continuum emission. Results. Investigation of the UV spectrum confirms a direct spectroscopic detection of the Lyman continuum emission with S /N > 5.Non-zero Lyα flux at the systemic redshift and high Lyman-α escape fraction ( f esc (Lyα) ≥ 0.78) suggest a low H i column density.The weak C and Si low-ionization absorption lines are also consistent with a low covering fraction along the line of sight. The subsolar abundances are consistent with a young and extreme starburst. The [O iii]λλ4959, 5007+Hβ equivalent width (EW) is one of the largest reported for a galaxy at z > 3 (EW([O iii]λλ4959, 5007 + Hβ) 1600 Å, rest-frame; 6700 Å observed-frame) and the near-infrared spectrum shows that this is mainly due to an extremely strong [O (>10) and high ionization parameter are consistent with prediction from photoionization models in the case of a density-bounded nebula scenario. Furthermore, the EW([O iii]λλ4959, 5007+Hβ) is comparable to recent measurements reported at z ∼ 7−9, in the reionization epoch. We also investigate the possibility of an AGN contribution to explain the ionizing emission but most of the AGN identification diagnostics suggest that stellar emission dominates instead. Conclusions. This source is currently the first high-z example of a Lyman continuum emitter exhibiting indirect and direct evidences of a Lyman continuum leakage and having physical properties consistent with theoretical expectation from Lyman continuum emission from a density-bounded nebula. A low H i column density, low covering fraction, compact star formation activity, and a possible interaction/merging of two systems may contribute to the Lyman continuum photon leakage.

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Section: Photometrymentioning

confidence: 99%

An extreme [O III] emitter atz= 3.2: a low metallicity Lyman continuum source

Barros

Vanzella

Amorín

et al. 2015

A&A

191

158

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“…Cassata et al (2013) derive the number density of compact (i.e. 1σ below the local SMR) and ultracompact (more than 0.4 dex smaller than local counterparts of the same mass) passive (sSFR < 10 −11 yr −1 ) galaxies with elliptical morphology and M > 10 10 M in the ∼120 arcmin 2 of the GOODS-South field covered by the first four CANDELS observations (Grogin et al 2011;Koekemoer et al 2011) and by the Early Release Science Program 2 (Windhorst et al 2011). Using their published sample of 107 galaxies, we selected the only two galaxies with M > 10 11 M and Σ > 2500 M pc −2 at 1.2 z 1.6, which account for a number density of 1.47(±1.04)10 −5 gal/Mpc 3 .…”

Section: Intermediate Redshift Rangementioning

confidence: 99%

Ultramassive dense early-type galaxies: Velocity dispersions and number density evolution sincez= 1.6

Gargiulo

Saracco

Tamburri

et al. 2016

A&A

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Aims. We investigate the stellar mass assembly history of ultramassive (M 10 11 M ) dense (Σ = M /2πR 2 e > 2500 M pc −2 ) early-type galaxies (ETGs, elliptical and spheroidal galaxies) selected on basis of visual classification over the last 9 Gyr. Methods. We traced the evolution of the comoving number density ρ of ultramassive dense ETGs and compared their structural (effective radius R e and stellar mass M ) and dynamical (velocity dispersion σ e ) parameters over the redshift range 0 < z < 1.6. We derived the number density ρ at 1.6 < z < 1 from the MUNICS and GOODS-South surveys, while we took advantage of the COSMOS spectroscopic survey to probe the intermediate redshift range [0.2−1.0]. We derived the number density of ultramassive dense local ETGs from the SDSS sample taking all of the selection bias affecting the spectroscopic sample into account. To compare the dynamical and structural parameters, we collected a sample of 11 ultramassive dense ETGs at 1.2 < z < 1.6 for which velocity dispersion measurements are available. For four of these ETGs (plus one at z = 1.91), we present previously unpublished estimates of velocity dispersion, based on optical VLT-FORS2 spectra. We probe the intermediate redshift range (0.2 < ∼ z < ∼ 0.9) and the local Universe with different ETGs samples. Results. We find that the comoving number density of ultramassive dense ETGs evolves with z as ρ(z) ∝ (1 + z) 0.3 ± 0.8 implying a decrease of ∼25% of the population of ultramassive dense ETGs since z = 1.6. By comparing the structural and dynamical properties of high-z ultramassive dense ETGs over the range 0 < ∼ z < 1.6 in the [R e , M , σ e ] plane, we find that all of the ETGs of the high-z sample have counterparts with similar properties in the local Universe. This implies either that the majority (∼70%) of ultramassive dense ETGs already completed the assembly and shaping at z = 1.4, or that, if a significant portion of dense ETGs evolves in size, new ultramassive dense ETGs must form at z < 1.5 to maintain their number density at almost constant. The difficulty in identify good progenitors for these new dense ETGs at z < ∼ 1.5 and the stellar populations properties of local ultramassive dense ETGs point towards the first hypothesis. In this case, the ultramassive dense galaxies missing in the local Universe could have joined, in the last 9 Gyr, the so colled non-dense ETGs population through minor mergers, thus contributing to mean size growth. In any case, the comparison between their number density and the number density of the whole population of ultramassive ETGs relegates their contribution to the mean size evolution to a secondary process.

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“…arcmin to J = 26.7) and the extended groth strip (EGS, 110 sq. arcmin to J = 26.7) from the CANDELS-Wide survey (Grogin et al 2011;Koekemoer et al 2011), the Early Release Science (Windhorst et al 2011) on the GOODS-S field (GOODS-ERS, 40 sq. arcmin.…”

Section: The Photometric Samplementioning

confidence: 99%

“…The advent of the WFC3 instrument onboard Hubble Space Telescope (HST) has opened a new window for the study of galaxy shape, size, and morphology up to very high redshifts (Windhorst et al 2011). The combination of large area, fine resolution, and near-infrared (NIR) wavelengths achieved with this powerful instrument allows us to study galaxies in the ultraviolet (UV) rest frame at z ∼ 7-8 with impressive accuracy.…”

Section: Introductionmentioning

confidence: 99%

The size-luminosity relation atz = 7 in CANDELS and its implication on reionization

Grazian

Castellano

Fontana

et al. 2012

A&A

102

157

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Context. The exploration of the relation between galaxy sizes and other physical parameters (luminosity, mass, star formation rate) has provided important clues for understanding galaxy formation, but such exploration has until recently been limited to intermediate redshift objects. Aims. We use the currently available CANDELS Deep+Wide surveys in the GOODS-South, UDS and EGS fields, complemented by data from the HUDF09 program, to address the relation between size and luminosity at z ∼ 7. Methods. The six different fields used for this study are characterized by a wide combination of depth and areal coverage, well suited for reducing the biases on the observed size-magnitude plane. From these fields, we select 153 z-band dropout galaxies. Detailed simulations have been carried out for each of these six fields, inserting simulated galaxies at different magnitudes and half light radius in the two dimensional images for all the Hubble Space Telescope (HST) bands available and recovering them as carried out for the real galaxies. These simulations allow us to derive precisely the completeness as a function of size and magnitude and to quantify measurements errors/biases, under the assumption that the 2D profile of z = 7 galaxies is well represented by an exponential disk function. Results. We find in a rather robust way that the half light radius distribution function of z ∼ 7 galaxies fainter than J = 26.6 is peaked at ≤0.1 arcsec (or equivalently 0.5 kpc proper), while at brighter magnitudes high-z galaxies are typically larger than ∼0.15 arcsec. We also find a well defined size-luminosity relation, Rh ∝ L 1/2 . We compute the luminosity function (LF) in the HUDF and P12HUDF fields, finding large spatial variation on the number density of faint galaxies. Adopting the size distribution and the size-luminosity relation found for faint galaxies at z = 7, we derive a mean slope of −1.7 ± 0.1 for the LF of LBGs at this redshift. Conclusions. Using this LF, we find that the number of ionizing photons emitted from galaxies at z ∼ 7 cannot keep the Universe re-ionized if the IGM is clumpy (C HII ≥ 3) and the Lyman continuum escape fraction of high-z LBGs is relatively low ( f esc ≤ 0.3). If these results are confirmed and strengthened by future CANDELS data, in particular by the forthcoming deep observations in GOODS-South and North and the wide field COSMOS, we can put severe limits to the role of galaxies in the reionization of the Universe.

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THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2-2 μm WAVELENGTH

Cited by 274 publications

References 112 publications

An extreme [O III] emitter atz= 3.2: a low metallicity Lyman continuum source

An extreme [O III] emitter atz= 3.2: a low metallicity Lyman continuum source

Ultramassive dense early-type galaxies: Velocity dispersions and number density evolution sincez= 1.6

The size-luminosity relation atz = 7 in CANDELS and its implication on reionization

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