The bright end of the<i>z</i> ~ 7<i>UV</i>luminosity function from a wide and deep HAWK-I survey

Castellano, M.; Fontana, A.; Paris, D.; Grazian, A.; Pentericci, L.; Boutsia, K.; Santini, P.; Testa, V.; Dickinson, Mark; Giavalisco, Mauro; Bouwens, Rychard; Cuby, Jean-Gabriel; Mannucci, F.; Clément, Benjamin; Cristiani, S.; Fiore, F.; Gallozzi, S.; Giallongo, E.; Maiolino, R.; Menci, Nicola; Moorwood, A. F. M.; Nonino, M.; Renzini, A.; Rosati, P.; Salimbeni, S.; Vanzella, E.

doi:10.1051/0004-6361/201015195

Cited by 80 publications

(63 citation statements)

References 78 publications

(115 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We first produce a set of UV absolute magnitudes and redshifts (M 1500 , z) according to an evolving LF by Castellano et al (2010b), and then convert it into a set of predicted magnitudes using the BC03 models with a range of ages, metallicities, dust content and Lyα emission as in Grazian et al (2011). We have also added the IGM absorption using the average evolution as in Fan et al (2006).…”

Section: Completenessmentioning

confidence: 99%

“…The observed lack of extended galaxies at faint magnitude limits (Rh ∼ 0.2 arcsec at J > 27) implies that the typical half light radius is less than ∼0.1 arcsec (Rh mode ). Ouchi et al 2009; red squares by Castellano et al 2010b, and cyan dots by Bouwens et al 2010b), while the open points are the number densities for the HUDF (triangles) and P12HUDF (circles). The cosmic variance between the two fields is greater than the statistical uncertainties.…”

Section: The Impact On the Reionization Processmentioning

confidence: 99%

See 1 more Smart Citation

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

Grazian

Castellano

Fontana

et al. 2012

A&A

Self Cite

101

157

View full text Add to dashboard Cite

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.

show abstract

Section: Completenessmentioning

confidence: 99%

Section: The Impact On the Reionization Processmentioning

confidence: 99%

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

Grazian

Castellano

Fontana

et al. 2012

A&A

Self Cite

101

157

View full text Add to dashboard Cite

show abstract

“…To make the scenario even more complex, for a significant number of galaxies at z∼6-7 the [Cii] emission appears to be significantly offset both in spatial position and in velocity. A key result in this context has been our ALMA detection of [Cii] emission associated with the normal star forming galaxy (SFR≈6 M yr −1 ) BDF − 3299 at z=7.1 (Castellano et al 2010;Vanzella et al 2011). This galaxy shows [Cii] emission fully consistent with the Lyα redshift, but spatially offset by 4 kpc relative to the optical emission .…”

Section: Introductionmentioning

confidence: 99%

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Carniani

Maiolino

Pallottini

et al. 2017

A&A

Self Cite

187

237

View full text Add to dashboard Cite

We present new ALMA observations of the [Oiii]88µm line and high angular resolution observations of the [Cii]158µm line in a normal star forming galaxy at z=7.1. Previous [Cii] observations of this galaxy had detected [Cii] emission consistent with the Lyα redshift but spatially slightly offset relative to the optical (UV-rest frame) emission. The new [Cii] observations reveal that the [Cii] emission is partly clumpy and partly diffuse on scales larger than about 1kpc.[Oiii] emission is also detected at high significance, offset relative to the optical counterpart in the same direction as the [Cii] clumps, but mostly not overlapping with the bulk of the [Cii] emission. The offset between different emission components (optical/UV and different far-IR tracers) is similar to that which is observed in much more powerful starbursts at high redshift. We show that the [Oiii] emitting clump cannot be explained in terms of diffuse gas excited by the UV radiation emitted by the optical galaxy, but it requires excitation by in-situ (slightly dust obscured) star formation, at a rate of about 7 M yr −1 . Within 20 kpc from the optical galaxy the ALMA data reveal two additional [Oiii] emitting systems, which must be star forming companions. We discuss that the complex properties revealed by ALMA in the z∼7.1 galaxy are consistent with expectations by recent models and cosmological simulations, in which differential dust extinction, differential excitation and different metal enrichment levels, associated with different subsystems assembling a galaxy, are responsible for the various appearance of the system when observed with distinct tracers.

show abstract

“…Over the past few years, ground-and space-based observations have allowed a statistically significant data set to be collected for z;6-10 Lyman Break galaxies (LBGs; Bouwens et al 2010Bouwens et al , 2011Bouwens et al , 2015bCastellano et al 2010;McLure et al 2010McLure et al , 2013Oesch et al 2010Oesch et al , 2013Oesch et al , 2016Bradley et al 2012;Bowler et al 2014Bowler et al , 2015Atek et al 2015;Livermore et al 2016). In this work, our aim is to revisit the constraints allowed on the WDM particle mass by combining these "galaxy" data sets with the latest limits on the cosmological electron scattering optical depth inferred by Planck.…”

Section: Introductionmentioning

confidence: 99%

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

Dayal

Choudhury

Bromm

et al. 2017

ApJ

View full text Add to dashboard Cite

We compare model results from a semi-analytic (merger-tree based) framework for high-redshift (z;5-20) galaxy formation against reionization indicators, including the Planck electron scattering optical depth (τ es ) and the ionizing photon emissivity (ṅ ion ), to shed light on the reionization history and sources in Cold (CDM) and Warm Dark Matter (WDM; particle masses of m x =1.5, 3, and 5 keV) cosmologies. This model includes all ofthe key processes of star formation, supernova feedback, the merger/accretion/ejectiondriven evolution of gas and stellar mass and the effect of the ultra-violet background (UVB), created during reionization, in photo-evaporating the gas content of galaxies in halos with M h 10 9  M . We find that the delay in the start of reionization in light (1.5 keV) WDM models can be compensated by a steeper redshift evolution of the ionizing photon escape fraction and a faster mass assembly, resulting in reionization ending at comparable redshifts (z;5.5) in all the dark matter models considered. We find thatthe bulk of the reionization photons come from galaxies with a halo mass of M h 10 9  M and a UV magnitude of −15M UV −10 in CDM. The progressive suppression of low-mass halos with decreasing m x leads to a shift in the "reionization" population to larger halo masses of M h 10 9  M and −17M UV −13 for 1.5 keV WDM. We find that current observations of τ es and the ultra violet luminosity function are equally compatible with all the (cold and warm) dark matter models considered in this work. Quantifying the impact of the UVB on galaxy observables (luminosity functions, stellar mass densities, andstellar to halo mass ratios) for different DM models, we propose that global indicators including the redshift evolution of the stellar mass density and the stellar mass-halo mass relation, observable with the James Webb Space Telescope, can be used to distinguish between CDM and WDM (1.5 keV) cosmologies.

show abstract

The bright end of thez ~ 7UVluminosity function from a wide and deep HAWK-I survey

Cited by 80 publications

References 78 publications

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

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

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Reionization and Galaxy Formation in Warm Dark Matter Cosmologies

Contact Info

Product

Resources

About