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Start Over Author "Amorin, R." Topic galaxies: high-redshift
70 results on '"Amorin, R."'

1. The KMOS Lens-Amplified Spectroscopic Survey (KLASS): kinematics and clumpiness of low-mass galaxies at cosmic noon

Author

Girard, M, Mason, CA, Fontana, A, Dessauges-Zavadsky, M, Morishita, T, Amorin, R, Fisher, DB, Jones, T, Schaerer, D, Schmidt, KB, Treu, T, and Vulcani, B

Subjects
galaxies: evolution, galaxies: high-redshift, galaxies: kinematics and dynamics, astro-ph.GA, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

ABSTRACT We present results from the KMOS Lens-Amplified Spectroscopic Survey (KLASS), an ESO Very Large Telescope (VLT) large program using gravitational lensing to study the spatially resolved kinematics of 44 star-forming galaxies at 0.6 < z < 2.3 with a stellar mass of 8.1 < log(M⋆/M⊙) < 11.0. These galaxies are located behind six galaxy clusters selected from the Hubble Space Telescope Grism Lens-Amplified Survey from Space (GLASS). We find that the majority of the galaxies show a rotating disc, but most of the rotation-dominated galaxies only have a low υ rot/σ0 ratio (median of υrot/σ0 ∼ 2.5). We explore the Tully–Fisher relation by adopting the circular velocity, $V_{\mathrm{ circ}}=(\upsilon _{\mathrm{ rot}}^2+3.4\sigma _0^2)^{1/2}$, to account for pressure support. We find that our sample follows a Tully–Fisher relation with a positive zero-point offset of +0.18 dex compared to the local relation, consistent with more gas-rich galaxies that still have to convert most of their gas into stars. We find a strong correlation between the velocity dispersion and stellar mass in the KLASS sample. When combining our data to other surveys from the literature, we see an increase of the velocity dispersion with stellar mass at all redshift. We obtain an increase of υrot/σ0 with stellar mass at 0.5 < z < 1.0. This could indicate that massive galaxies settle into regular rotating discs before the low-mass galaxies. For higher redshift (z > 1), we find a weak increase or flat trend. We find no clear trend between the rest-frame UV clumpiness and the velocity dispersion and υrot/σ0. This could suggest that the kinematic properties of galaxies evolve after the clumps formed in the galaxy disc or that the clumps can form in different physical conditions.

Published
2020

2. Constraining Lyman-alpha spatial offsets at 3 < z < 5.5 from VANDELS slit spectroscopy

Author

Hoag, A, Treu, T, Pentericci, L, Amorin, R, Bolzonella, M, Bradač, M, Castellano, M, Cullen, F, Fynbo, JPU, Garilli, B, Guaita, L, Hathi, N, Henry, A, Jones, T, Mason, C, McLeod, D, McLure, R, Morishita, T, Pozzetti, L, Schaerer, D, Schmidt, KB, Talia, M, and Thomas, R

Subjects
Astronomical Sciences, Physical Sciences, galaxies: high-redshift, astro-ph.GA, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We constrain the distribution of spatially offset Lyman-alpha emission (Ly α) relative to rest-frame ultraviolet emission in ∼300 high redshift (3 < z < 5.5) Lyman-break galaxies (LBGs) exhibiting Ly α emission from VANDELS, a VLT/VIMOS slit-spectroscopic survey of the CANDELS Ultra Deep Survey and Chandra Deep Field South fields (≈0.2 deg2 total). Because slit spectroscopy only provides one spatial dimension, we use Bayesian inference to recover the underlying two-dimensional Ly α spatial offset distribution. We model the distribution using a two-dimensional circular Gaussian, defined by a single parameter σr,Ly α, the standard deviation expressed in polar coordinates. Over the entire redshift range of our sample (3 < z < 5.5), we find σr,Ly α = 1.70+0.09-0.08 kpc (68 per cent conf.), corresponding to ∼0′.25 at 〈z〉 = 4.5. We also find that σr,Ly α decreases significantly with redshift. Because Ly α spatial offsets can cause slit losses, the decrease in σr,Ly α with redshift can partially explain the increase in the fraction of Ly α emitters observed in the literature over this same interval, although uncertainties are still too large to reach a strong conclusion. If σr,Ly α continues to decrease into the reionization epoch, then the decrease in Ly α transmission from galaxies observed during this epoch might require an even higher neutral hydrogen fraction than what is currently inferred. Conversely, if spatial offsets increase with the increasing opacity of the intergalactic medium, slit losses may explain some of the drop in Ly α transmission observed at z > 6. Spatially resolved observations of Ly α and UV continuum at 6 < z

Published
2019

3. Inferences on the timeline of reionization at z ∼ 8 from the KMOS Lens-Amplified Spectroscopic Survey

Author

Mason, CA, Fontana, A, Treu, T, Schmidt, KB, Hoag, A, Abramson, L, Amorin, R, Bradač, M, Guaita, L, Jones, T, Henry, A, Malkan, MA, Pentericci, L, Trenti, M, and Vanzella, E

Subjects
galaxies: evolution, galaxies: high-redshift, intergalactic medium, dark ages, reionization, first stars, astro-ph.CO, astro-ph.GA, dark ages, reionization, first stars, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

Detections and non-detections of Lyman alpha (Lyα) emission from z > 6 galaxies ( 7, where Lyα redshifts to near infra-red wavelengths. Here we present a search for z > 7.2 Lyα emission in 53 intrinsically faint Lyman Break Galaxy candidates, gravitationally lensed by massive galaxy clusters, in the KMOS Lens-Amplified Spectroscopic Survey (KLASS). With integration times of ∼7-10 h, we detect no Lyα emission with signal-to-noise ratio (S/N) > 5 in our sample. We determine our observations to be 80 per cent complete for 5σ spatially and spectrally unresolved emission lines with integrated line flux >5.7 × 10−18 erg s−1 cm−2. We define a photometrically selected sub-sample of 29 targets at z = 7.9 ± 0.6, with a median 5σ Lyα EW limit of 58 Å. We perform a Bayesian inference of the average intergalactic medium (IGM) neutral hydrogen fraction using their spectra. Our inference accounts for the wavelength sensitivity and incomplete redshift coverage of our observations, and the photometric redshift probability distribution of each target. These observations, combined with samples from the literature, enable us to place a lower limit on the average IGM neutral hydrogen fraction of > 0.76 (68 per cent), > 0.46 (95 per cent) at z ∼ 8, providing further evidence of rapid reionization at z ∼ 6-8. We show that this is consistent with reionization history models extending the galaxy luminosity function to MUV −12, with low ionizing photon escape fractions, fesc 15 per cent.

Published
2019

4. First Results from the KMOS Lens-Amplified Spectroscopic Survey (KLASS): Kinematics of Lensed Galaxies at Cosmic Noon

Author

Mason, CA, Treu, T, Fontana, A, Jones, T, Morishita, T, Amorin, R, Bradač, M, Finney, EQ, Grillo, C, Henry, A, Hoag, A, Huang, KH, Schmidt, KB, Trenti, M, and Vulcani, B

Subjects
galaxies: evolution, galaxies: high-redshift, galaxies: kinematics and dynamics, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences, Organic Chemistry, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present the first results of the K-band Multi-Object Spectrometer (KMOS) Lens-Amplified Spectroscopic Survey, a new ESO Very Large Telescope large program, doing multi-object integral field spectroscopy of galaxies gravitationally lensed behind seven galaxy clusters selected from the Hubble Space Telescope (HST) Grism Lens-Amplified Survey from Space. Using the power of the cluster magnification, we are able to reveal the kinematic structure of 25 galaxies at 0.7 z 2.3, in four cluster fields, with stellar masses 7.8log;(M∗/Mo) 10.5. This sample includes five sources at Z > 1 with lower stellar masses than in any previous kinematic integral field unit (IFU) surveys. Our sample displays a diversity in kinematic structure over this mass and redshift range. The majority of our kinematically resolved sample is rotationally supported, but with a lower ratio of rotational velocity to velocity dispersion than in the local universe, indicating the fraction of dynamically hot disks changes with cosmic time. We find that no galaxies with stellar mass

Published
2017

5. THE GRISM LENS-AMPLIFIED SURVEY from SPACE (GLASS). IV. MASS RECONSTRUCTION of the LENSING CLUSTER ABELL 2744 from FRONTIER FIELD IMAGING and GLASS SPECTROSCOPY

Author

Wang, X, Hoag, A, Huang, KH, Treu, T, Bradac, M, Schmidt, KB, Brammer, GB, Vulcani, B, Jones, TA, Ryan, RE, Amorin, R, Castellano, M, Fontana, A, Merlin, E, and Trenti, M

Subjects
galaxies: clusters: individual, galaxies: evolution, galaxies: high-redshift, astro-ph.GA, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present a strong and weak lensing reconstruction of the massive cluster Abell 2744, the first cluster for which deep Hubble Frontier Fields (HFF) images and spectroscopy from the Grism Lens-Amplified Survey from Space (GLASS) are available. By performing a targeted search for emission lines in multiply imaged sources using the GLASS spectra, we obtain five high-confidence spectroscopic redshifts and two tentative ones. We confirm one strongly lensed system by detecting the same emission lines in all three multiple images. We also search for additional line emitters blindly and use the full GLASS spectroscopic catalog to test reliability of photometric redshifts for faint line emitters. We see a reasonable agreement between our photometric and spectroscopic redshift measurements, when including nebular emission in photometric redshift estimations. We introduce a stringent procedure to identify only secure multiple image sets based on colors, morphology, and spectroscopy. By combining 7 multiple image systems with secure spectroscopic redshifts (at 5 distinct redshift planes) with 18 multiple image systems with secure photometric redshifts, we reconstruct the gravitational potential of the cluster pixellated on an adaptive grid, using a total of 72 images. The resulting mass map is compared with a stellar mass map obtained from the deep Spitzer Frontier Fields data to study the relative distribution of stars and dark matter in the cluster. We find that the stellar to total mass ratio varies substantially across the cluster field, suggesting that stars do not trace exactly the total mass in this interacting system. The maps of convergence, shear, and magnification are made available in the standard HFF format.

Published
2015

6. STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS

Author

Santini, P, Ferguson, HC, Fontana, A, Mobasher, B, Barro, G, Castellano, M, Finkelstein, SL, Grazian, A, Hsu, LT, Lee, B, Lee, S-K, Pforr, J, Salvato, M, Wiklind, T, Wuyts, S, Almaini, O, Cooper, MC, Galametz, A, Weiner, B, Amorin, R, Boutsia, K, Conselice, CJ, Dahlen, T, Dickinson, ME, Giavalisco, M, Grogin, NA, Guo, Y, Hathi, NP, Kocevski, D, Koekemoer, AM, Kurczynski, P, Merlin, E, Mortlock, A, Newman, JA, Paris, D, Pentericci, L, Simons, R, and Willner, SP

Subjects
Space Sciences, Physical Sciences, catalogs, galaxies: fundamental parameters, galaxies: high-redshift, galaxies: stellar content, surveys, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present the public release of the stellar mass catalogs for the GOODS-S and UDS fields obtained using some of the deepest near-IR images available, achieved as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey project. We combine the effort from 10 different teams, who computed the stellar masses using the same photometry and the same redshifts. Each team adopted their preferred fitting code, assumptions, priors, and parameter grid. The combination of results using the same underlying stellar isochrones reduces the systematics associated with the fitting code and other choices. Thanks to the availability of different estimates, we can test the effect of some specific parameters and assumptions on the stellar mass estimate. The choice of the stellar isochrone library turns out to have the largest effect on the galaxy stellar mass estimates, resulting in the largest distributions around the median value (with a semi interquartile range larger than 0.1 dex). On the other hand, for most galaxies, the stellar mass estimates are relatively insensitive to the different parameterizations of the star formation history. The inclusion of nebular emission in the model spectra does not have a significant impact for the majority of galaxies (less than a factor of 2 for 80% of the sample). Nevertheless, the stellar mass for the subsample of young galaxies (age

Published
2015

7. The VANDELS ESO public spectroscopic survey

Author

McLure, R.J., Pentericci, L., Cimatti, A., Dunlop, J.S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A.C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S.L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W.G., Iovino, A., Jarvis, M.J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, Omar, Balestra, I., Bardelli, S., Bell, E.F., Bourne, N., Bowler, R.A.A., Brusa, M., Buitrago, F., Caputi, K.I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G.G., Ferguson, H.C., Fiore, F., Franco, M., Fynbo, J P U, Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N.P., Jung, I., Kim, S., Koekemoer, A.M., Khusanova, Y., Lotz, J.M., Mannucci, F., Maltby, David T., Matsuoka, K., McLeod, D.J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D.P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D.P., Tasca, L.A.M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C.C., Zamorani, G., and Zucca, E.

Subjects
surveys, galaxies: high-redshift, galaxies: star formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

VANDELS is a uniquely deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO’s Very Large Telescope (VLT). The survey has obtained ultradeep optical (0.48 < λ < 1.0 μm) spectroscopy of ≃2100 galaxies within the redshift interval 1.0 ≤ z ≤ 7.0, over a total area of ≃0.2 deg2 centred on the CANDELS Ultra Deep Survey and Chandra Deep Field South fields. Based on accurate photometric redshift pre-selection, 85 per cent of the galaxies targeted by VANDELS were selected to be at z ≥ 3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high-signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities, and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < tint< 80 h), the VANDELS survey targeted: (a) bright star-forming galaxies at 2.4 ≤ z ≤ 5.5, (b) massive quiescent galaxies at 1.0 ≤ z ≤ 2.5, (c) fainter star-forming galaxies at 3.0 ≤ z ≤ 7.0, and (d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multiwavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper, we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design, and target selection.

Published
2018

8. The VIMOS Ultra Deep Survey: The role of HI kinematics and HI column density on the escape of Lyα photons in star-forming galaxies at 2 < z < 4

Author

Guaita, L, Talia, M, Pentericci, L, Verhamme, A, Cassata, P, Lemaux, BC, Orlitova, I, Ribeiro, B, Schaerer, D, Zamorani, G, Garilli, B, Le Brun, V, Le Fèvre, O, MacCagni, D, Tasca, LAM, Thomas, R, Vanzella, E, Zucca, E, Amorin, R, Bardelli, S, Castellano, M, Grazian, A, Hathi, NP, Koekemoer, A, and Marchi, F

Subjects
ISM: kinematics and dynamics, techniques: imaging spectroscopy, galaxies: high-redshift, galaxies: star formation, scattering
Abstract

© 2017 ESO. Aims. We wish to assess the role of kinematics and neutral hydrogen column density in the escape and distribution of Lya photons. Methods. We selected a sample of 76 Lya emitting galaxies from the VIMOS Ultra Deep Survey (VUDS) at 2 = z = 4. We estimated the velocity of the neutral gas flowing out of the interstellar medium as the velocity offset, δv, between the systemic redshift (zsys) and the center of low-ionization absorption line systems (LIS). To increase the S/N of VUDS spectra, we stacked subsamples defined based on median values of their photometric and spectroscopic properties. We measured the systemic redshift from the rest-frame UV spectroscopic data using the CIII]1908 nebular emission line, and we considered SiII1526 as the highest signal-to-noise LIS line. We calculated the Lya peak shift with respect to the zsys, the EW(Lya), and the Lya spatial extension, Ext(Lya-C), from the in the 2D stacked spectra. Results. The galaxies that are faint in the rest-frame UV continuum, strong in Lya and CIII] , with compact UV morphology, and localized in an underdense environment are characterized by outflow velocities of the order of a few hundreds of km s -1 . The subsamples with smaller δv are characterized by larger Lya peak shifts, larger Ext(Lya-C), and smaller EW(Lya). In general we find that EW(Lya) anti-correlates with Ext(Lya-C) and Lya peak shift. Conclusions. We interpret these trends using a radiative-transfer shell model. The model predicts that an HI gas with a column density larger than 1020 cm -2 is able to produce Lya peak shifts larger than > 300 km s -1 . An ISM with this value of NHI would favour a large amount of scattering events, especially when the medium is static, so it can explain large values of Ext(Lya-C) and small EW(Lya). On the contrary, an ISM with a lower NHI, but large velocity outflows would lead to a Lya spatial profile peaked at the galaxy center (i.e. low values of Ext(Lya-C)) and to a large EW(Lya), as we see in our data. Our results and their interpretation via radiative-transfer models tell us that it is possible to use Lya to study the properties of the HI gas. Also, the fact that Lya emitters are characterized by large δv could give hints about their stage of evolution in the sense that they could be experiencing short bursts of star formation that push strong outflows., This work is supported by funding from the European Research Council Advanced Grant ERC–2010–AdG–268107–EARLY and by INAF Grants PRIN 2010, PRIN 2012, and PICS 2013. This work is based on data products made available at the CESAM data center, Laboratoire d’Astrophysique de Marseille, France. R.A. acknowledges support from the ERC Advanced Grant 695671 “QUENCH” and I.O. from the Czech Science Foundation grant 17-06217Y.

Published
2017
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9. AGN-enhanced outflows of low-ionization gas in star-forming galaxies at 1.7 < z < 4.6

Author

Talia, M, Brusa, M, Cimatti, A, Lemaux, BC, Amorin, R, Bardelli, S, Cassarà, LP, Cucciati, O, Garilli, B, Grazian, A, Guaita, L, Hathi, NP, Koekemoer, A, Fèvre, OL, Maccagni, D, Nakajima, K, Pentericci, L, Pforr, J, Schaerer, D, Vanzella, E, Vergani, D, Zamorani, G, and Zucca, E

Subjects
ISM: jets and outflows, galaxies: high-redshift, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, ultraviolet: ISM, Astrophysics::Galaxy Astrophysics, galaxies: ISM
Abstract

Fast and energetic winds are invoked by galaxy formation models as essential processes in the evolution of galaxies. These outflows can be powered either by star formation (SF) and/or active galactic nucleus (AGN) activity, but the relative dominance of the two mechanisms is still under debate. We use spectroscopic stacking analysis to study the properties of the low-ionization phase of the outflow in a sample of 1330 star-forming galaxies (SFGs) and 79 X-ray-detected (1042 < LX < 1045 erg s−1) Type 2 AGN at 1.7 < z < 4.6 selected from a compilation of deep optical spectroscopic surveys, mostly zCOSMOS-Deep and VIMOS Ultra Deep Survey (VUDS). We measure mean velocity offsets of ∼− 150 km s−1 in the SFGs, while in the AGN sample the velocity is much higher (∼− 950 km s−1), suggesting that the AGN is boosting the outflow up to velocities that could not be reached only with the SF contribution. The sample of X-ray AGN has on average a lower SF rate than non-AGN SFGs of similar mass: this, combined with the enhanced outflow velocity in AGN hosts, is consistent with AGN feedback in action. We further divide our sample of AGN into two X-ray luminosity bins: we measure the same velocity offsets in both stacked spectra, at odds with results reported for the highly ionized phase in local AGN, suggesting that the two phases of the outflow may be mixed only up to relatively low velocities, while the highest velocities can be reached only by the highly ionized phase., This work is supported by funding from the European Research Council Advanced Grant ERC–2010–AdG–268107–EARLY and by INAF Grants PRIN 2010, PRIN 2012 and PICS 2013. AC, OC, and MT acknowledge the grant MIUR PRIN 2010–2011. MB acknowledges support from the FP7 grant ‘eEASy’: (CIG 321913). RA acknowledges support from the ERC Advanced Grant 695671 ‘QUENCH’. We acknowledge the grants ASI n.I/023/12/0 ‘Attività relative alla fase B2/C per la missione Euclid’ and MIUR PRIN 2010-2011 ‘The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid’ and PRIN MIUR 2015 ‘Cosmology and Fundamental Physics: illuminating the Dark Universe with Euclid’.

Published
2017
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10. Optical Line Emission from $z$ ∼ 6.8 Sources with Deep Constraints on Ly$\alpha$ Visibility

Author

Castellano, M, Pentericci, L, Fontana, A, Vanzella, E, Merlin, E, Barros, SD, Amorin, R, Caputi, KI, Cristiani, S, Finkelstein, SL, Giallongo, E, Grazian, A, Koekemoer, A, Maiolino, R, Paris, D, Pilo, S, Santini, P, Yan, H, Amorin Barbieri, Ricardo [0000-0001-5758-1000], Maiolino, Roberto [0000-0002-4985-3819], and Apollo - University of Cambridge Repository

Subjects
galaxies: high-redshift, dark ages, reionization, first stars
Abstract

We analyze a sample of $z$-dropout galaxies in the CANDELS GOODS South and UDS fields that have been targeted by a dedicated spectroscopic campaign aimed at detecting their Ly$\alpha$ line. Deep IRAC observations at 3.6 and 4.5 μm are used to determine the strength of optical emission lines affecting these bands at $z$ ~ 6.5-6.9 in order to (1) investigate possible physical differences between Ly$\alpha$ emitting and non-emitting sources; (2) constrain the escape fraction of ionizing photons; and (3) provide an estimate of the specific star formation rate at high redshifts. We find evidence of strong [O III]+Hβ emission in the average (stacked) SEDs of galaxies both with and without Ly$\alpha$ emission. The blue IRAC [3.6]-[4.5] color of the stack with detected Ly$\alpha$ line can be converted into a rest-frame equivalent width EW([O III]+Hβ) = 1500$^{+530}_{-440}$Å assuming a flat intrinsic stellar continuum. This strong optical line emission enables a first estimate of $f_{esc} \lesssim$ 20% on the escape fraction of ionizing photons from Ly$\alpha$ detected objects. The objects with no Ly$\alpha$ line show less extreme EW([O III]+Hβ) = Å, suggesting different physical conditions of the H II regions with respect to Ly$\alpha$-emitting ones, or a larger $f_{esc}$. The latter case is consistent with a combined evolution of $f_{esc}$ and the neutral hydrogen fraction as an explanation of the lack of bright Ly$\alpha$ emission at $z$ > 6. A lower limit on the specific star formation rate, SSFR > 9.1 Gyr$^{-1}$ for $M_{star}$ = 2 $\times$ 10$^9$ $M_\odot$ galaxies at these redshifts can be derived from the spectroscopically confirmed sample., K.C. acknowledges funding from the European Research Council through the award of the Consolidator Grant ID 681627-BUILDUP. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007–2013) under grant agreement n 312725. This work is based on data obtained with ESO Programmes 084.A-0951, 085.A-0844, 086.A-0968, 088.A-1013, 088.A-0192, and 190.A-0685.

Published
2017
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11. Optical Line Emission from z similar to 6.8 Sources with Deep Constraints on Ly alpha Visibility

Author

Castellano, M., Pentericci, L., Fontana, A., Vanzella, E., Merlin, E., De Barros, S., Amorin, R., Caputi, K. I., Cristiani, S., Finkelstein, S. L., Giallongo, E., Grazian, A., Koekemoer, A., Maiolino, R., Paris, D., Pilo, S., Santini, P., Yan, H., and Astronomy

Subjects
BROAD-BAND PHOTOMETRY, GOODS-SOUTH FIELD, IONIZING PHOTON ESCAPE, galaxies: high-redshift, SURVEY. SURVEY DESIGN, dark ages, reionization, first stars, HUBBLE-SPACE-TELESCOPE, IRAC SOURCE COUNTS, EXTRAGALACTIC LEGACY SURVEY, STAR-FORMATION RATE, LYMAN BREAK GALAXIES, HIGH-REDSHIFT GALAXIES
Abstract

We analyze a sample of z-dropout galaxies in the CANDELS GOODS South and UDS fields that have been targeted by a dedicated spectroscopic campaign aimed at detecting their Ly alpha line. Deep IRAC observations at 3.6 and 4.5 mu m are used to determine the strength of optical emission lines affecting these bands at z similar to 6.5-6.9 in order to (1) investigate possible physical differences between Ly alpha emitting and non-emitting sources; (2) constrain the escape fraction of ionizing photons; and. (3) provide an estimate of the specific star formation rate at high redshifts. We find evidence of strong [O III]+H beta emission in the average (stacked) SEDs of galaxies both with and without Lya emission. The blue IRAC [3.6]-[4.5] color of the stack with detected Ly alpha line can be converted into a rest-frame equivalent width EW([O III]+ H beta) = 1500(-440) (+530) angstrom assuming a flat intrinsic stellar continuum. This strong optical line emission enables a first estimate of f(esc) less than or similar to 20% on the escape fraction of ionizing photons from Ly alpha detected objects. The objects with no Ly alpha line show less extreme EW([O III]+ H beta) = 520(-150)(+170) angstrom suggesting different physical conditions of the H II regions with respect to Ly alpha-emitting ones, or a larger f(esc). The latter case is consistent with a combined evolution of f(esc) and the. neutral hydrogen fraction as an. explanation of the lack of bright Lya emission at z > 6. A lower limit on the specific star formation rate, SSFR > 9.1 Gyr(-1) for M-star = 2 x 10(9) M-circle dot galaxies at these redshifts can be derived from the spectroscopically confirmed sample.

Published
2017

12. The ALPINE-ALMA [C II] survey: Molecular gas budget in the early Universe as traced by [C II].

Author

Dessauges-Zavadsky, M., Ginolfi, M., Pozzi, F., Béthermin, M., Le Fèvre, O., Fujimoto, S., Silverman, J. D., Jones, G. C., Vallini, L., Schaerer, D., Faisst, A. L., Khusanova, Y., Fudamoto, Y., Cassata, P., Loiacono, F., Capak, P. L., Yan, L., Amorin, R., Bardelli, S., and Boquien, M.

Subjects
STELLAR mass, STAR formation, UNIVERSE, GASES, MOLECULAR weights, SUBMILLIMETER astronomy, GALACTIC redshift
Abstract

The molecular gas content of normal galaxies at z >  4 is poorly constrained because the commonly used molecular gas tracers become hard to detect at these high redshifts. We use the [C II] 158 μm luminosity, which was recently proposed as a molecular gas tracer, to estimate the molecular gas content in a large sample of main sequence star-forming galaxies at z = 4.4 − 5.9, with a median stellar mass of 109.7 M⊙, drawn from the ALMA Large Program to INvestigate [C II] at Early times survey. The agreement between the molecular gas masses derived from [C II] luminosities, dynamical masses, and rest-frame 850 μm luminosities extrapolated from the rest-frame 158 μm continuum supports [C II] as a reliable tracer of molecular gas in our sample. We find a continuous decline of the molecular gas depletion timescale from z = 0 to z = 5.9, which reaches a mean value of (4.6 ± 0.8) × 108 yr at z ∼ 5.5, only a factor of between two and three shorter than in present-day galaxies. This suggests a mild enhancement of the star formation efficiency toward high redshifts. Our estimates also show that the previously reported rise in the molecular gas fraction flattens off above z ∼ 3.7 to achieve a mean value of 63%±3% over z = 4.4 − 5.9. This redshift evolution of the gas fraction is in line with that of the specific star formation rate. We use multi-epoch abundance-matching to follow the gas fraction evolution across cosmic time of progenitors of z = 0 Milky Way-like galaxies in ∼1013 M⊙ halos and of more massive z = 0 galaxies in ∼1014 M⊙ halos. Interestingly, the former progenitors show a monotonic increase of the gas fraction with redshift, while the latter show a steep rise from z = 0 to z ∼ 2 followed by a constant gas fraction from z ∼ 2 to z = 5.9. We discuss three possible effects, namely outflows, a pause in gas supply, and over-efficient star formation, which may jointly contribute to the gas fraction plateau of the latter massive galaxies. [ABSTRACT FROM AUTHOR]

Published
2020
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13. The ALPINE-ALMA [CII] survey: Dust attenuation properties and obscured star formation at z ∼ 4.4–5.8.

Author

Fudamoto, Y., Oesch, P. A., Faisst, A., Béthermin, M., Ginolfi, M., Khusanova, Y., Loiacono, F., Le Fèvre, O., Capak, P., Schaerer, D., Silverman, J. D., Cassata, P., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Fujimoto, S., and Gruppioni, C.

Subjects
STELLAR mass, GALAXY formation, STAR formation, SMALL magellanic cloud, DUST, GALACTIC redshift, STELLAR luminosity function
Abstract

We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ∼4.4 − 5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 μm obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (β), stellar mass (M⋆), and infrared excess (IRX = LIR/LUV). Twenty-three galaxies are individually detected in the continuum at > 3.5σ significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z ∼ 4.4 − 5.8. The individual detections and stacks show that the IRX–β relation at z ∼ 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z <  4). The attenuation curve is similar to or even steeper than that of the extinction curve of the Small Magellanic Cloud. This systematic change of the IRX–β relation as a function of redshift suggests an evolution of dust attenuation properties at z >  4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX–M⋆ relations at z ≲ 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z ≳ 4 are characterised by (i) a steeper attenuation curve than at z ≲ 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (log M⋆/M⊙ >  10) at z ∼ 5 − 6 already exhibit an obscured fraction of star formation of ∼45%, indicating a rapid build-up of dust during the epoch of reionization. [ABSTRACT FROM AUTHOR]

Published
2020
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14. The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties.

Author

Béthermin, M., Fudamoto, Y., Ginolfi, M., Loiacono, F., Khusanova, Y., Capak, P. L., Cassata, P., Faisst, A., Le Fèvre, O., Schaerer, D., Silverman, J. D., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Davidzon, I., Dessauges-Zavadsky, M., Fujimoto, S., and Gruppioni, C.

Subjects
ELECTRONIC data processing, SPECTRAL energy distribution, SUBMILLIMETER astronomy, STAR formation, ACTINIC flux, CATALOGS, COSMIC background radiation, GALACTIC redshift
Abstract

The Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE) targets the [CII] 158 μm line and the far-infrared continuum in 118 spectroscopically confirmed star-forming galaxies between z = 4.4 and z = 5.9. It represents the first large [CII] statistical sample built in this redshift range. We present details regarding the data processing and the construction of the catalogs. We detected 23 of our targets in the continuum. To derive accurate infrared luminosities and obscured star formation rates (SFRs), we measured the conversion factor from the ALMA 158 μm rest-frame dust continuum luminosity to the total infrared luminosity (LIR) after constraining the dust spectral energy distribution by stacking a photometric sample similar to ALPINE in ancillary single-dish far-infrared data. We found that our continuum detections have a median LIR of 4.4 × 1011L⊙. We also detected 57 additional continuum sources in our ALMA pointings. They are at a lower redshift than the ALPINE targets, with a mean photometric redshift of 2.5 ± 0.2. We measured the 850 μm number counts between 0.35 and 3.5 mJy, thus improving the current interferometric constraints in this flux density range. We found a slope break in the number counts around 3 mJy with a shallower slope below this value. More than 40% of the cosmic infrared background is emitted by sources brighter than 0.35 mJy. Finally, we detected the [CII] line in 75 of our targets. Their median [CII] luminosity is 4.8 × 108L⊙ and their median full width at half maximum is 252 km s−1. After measuring the mean obscured SFR in various [CII] luminosity bins by stacking ALPINE continuum data, we find a good agreement between our data and the local and predicted SFR–L[CII] relations. [ABSTRACT FROM AUTHOR]

Published
2020
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15. The ALPINE-ALMA [C II] survey: Little to no evolution in the [C II]–SFR relation over the last 13 Gyr.

Author

Schaerer, D., Ginolfi, M., Béthermin, M., Fudamoto, Y., Oesch, P. A., Le Fèvre, O., Faisst, A., Capak, P., Cassata, P., Silverman, J. D., Yan, Lin, Jones, G. C., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Giavalisco, M., Hathi, N. P., and Fujimoto, S.

Subjects
STAR formation, GALACTIC redshift, STELLAR mass, GALAXY formation, GALAXIES, DETECTION limit
Abstract

The [C II] 158 μm line is one of the strongest IR emission lines, which has been shown to trace the star formation rate (SFR) of galaxies in the nearby Universe, and up to z ∼ 2. Whether this is also the case at higher redshift and in the early Universe remains debated. The ALPINE survey, which targeted 118 star-forming galaxies at 4.4 <  z <  5.9, provides a new opportunity to examine this question with the first statistical dataset. Using the ALPINE data and earlier measurements from the literature, we examine the relation between the [C II] luminosity and the SFR over the entire redshift range from z ∼ 4 − 8. ALPINE galaxies, which are both detected in [C II] and in dust continuum, show good agreement with the local L([CII])–SFR relation. Galaxies undetected in the continuum by ALMA are found to be over-luminous in [C II] when the UV SFR is used. After accounting for dust-obscured star formation, by an amount of SFR(IR) ≈ SFR(UV) on average, which results from two different stacking methods and SED fitting, the ALPINE galaxies show an L([CII])–SFR relation comparable to the local one. When [C II] non-detections are taken into account, the slope may be marginally steeper at high-z, although this is still somewhat uncertain. When compared homogeneously, the z >  6 [C II] measurements (detections and upper limits) do not behave very differently to the z ∼ 4 − 6 data. We find a weak dependence of L([CII])/SFR on the Lyα equivalent width. Finally, we find that the ratio L([CII])/LIR ∼ (1 − 3) × 10−3 for the ALPINE sources, comparable to that of "normal" galaxies at lower redshift. Our analysis, which includes the largest sample (∼150 galaxies) of [C II] measurements at z > 4 available so far, suggests no or little evolution of the [C II]–SFR relation over the last 13 Gyr of cosmic time. [ABSTRACT FROM AUTHOR]

Published
2020
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16. X-ray properties of He ii λ 1640 emitting galaxies in VANDELS.

Author

Saxena, A, Pentericci, L, Schaerer, D, Schneider, R, Amorin, R, Bongiorno, A, Calabrò, A, Castellano, M, Cimatti, A, Cullen, F, Fontana, A, Fynbo, J P U, Hathi, N, McLeod, D J, Talia, M, and Zamorani, G

Subjects
GALAXIES, X-rays, ACTIVE galactic nuclei, STELLAR populations, X-ray binaries, STAR formation
Abstract

We explore X-ray emission from a sample of 18 He  ii  λ1640 emitting star-forming galaxies at z  ∼ 2.3–3.6 from the VANDELS survey in the Chandra Deep Field South, to set constraints on the role of X-ray sources in powering the He  ii  emission. We find that 4 He  ii  emitters have tentative detections with S/N ∼ 2 and have X-ray luminosities, LX  = 1.5−4.9 × 1041 erg s−1. The stacked luminosity of all 18 He  ii  emitters is 2.6 × 1041 erg s−1, and that of a subset of 13 narrow He  ii  emitters (FHWM(He  ii) < 1000 km s−1) is 3.1 × 1041 erg s−1. We also measure stacked LX for non-He  ii  emitters through bootstrapping of matched samples, and find LX  = 2.5 × 1041 erg s−1, which is not significantly different from LX measured for He  ii  emitters. The LX per star formation rate for He  ii  emitters (log (LX /SFR) ∼ 40.0) and non-emitters (log (LX /SFR) ∼ 39.9) are also comparable and in line with the redshift evolution and metallicity dependence predicted by models. Due to the non-significant difference between the X-ray emission from galaxies with and without He  ii , we conclude that X-ray binaries or weak or obscured active galactic nuclei are unlikely to be the dominant producers of He  ii  ionizing photons in VANDELS star-forming galaxies at z  ∼ 3. Given the comparable physical properties of both He  ii  emitters and non-emitters reported previously, alternative He  ii  ionizing mechanisms such as localized low-metallicity stellar populations, Pop-III stars, etc. may need to be explored. [ABSTRACT FROM AUTHOR]

Published
2020
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17. Characterizing elusive, faint dusty star-forming galaxies: a lensed, optically undetected ALMA galaxy at z similar to 3.3

Author

Santini, P., Castellano, M., Fontana, A., Merlin, E., Maiolino, R., Mason, C., Mignano, A., Pilo, S., Amorin, R., Berta, S., Bourne, N., Calura, F., Daddi, E., Elbaz, D., Grazian, A., Magliocchetti, M., Michalowski, M.J., Pentericci, L., Pozzi, F., Rodighiero, G., Schreiber, C., and Valiante, R.

Subjects
submillimeter: galaxies, galaxies: photometry, galaxies: high-redshift, cosmology: observations, galaxies: fundamental parameters, galaxies: evolution
Published
2016

18. The VANDELS survey: the role of ISM and galaxy physical properties in the escape of Lyα emission in z ∼ 3.5 star-forming galaxies.

Author

Marchi, F., Pentericci, L., Guaita, L., Talia, M., Castellano, M., Hathi, N., Schaerer, D., Amorin, R., Bolzonella, M., Carnall, A. C., Charlot, S., Chevallard, J., Cullen, F., Finkelstein, S. L., Fontana, A., Fontanot, F., Garilli, B., Hibon, P., Koekemoer, A. M., and Maccagni, D.

Subjects
GALAXIES, SPECTRAL energy distribution, AGE of stars, STELLAR mass, STAR formation, INTERSTELLAR medium
Abstract

Aims. We wish to investigate the physical properties of a sample of Lyα emitting galaxies in the VANDELS survey, with particular focus on the role of kinematics and neutral hydrogen column density in the escape and spatial distribution of Lyα photons. Methods. From all the Lyα emitting galaxies in the VANDELS Data Release 2 at 3.5 ≲ z ≲ 4.5, we selected a sample of 52 galaxies that also have a precise systemic redshift determination from at least one nebular emission line (HeII or CIII]). For these galaxies, we derived different physical properties (stellar mass, age, dust extinction, and star formation rate) from spectral energy distribution (SED) fitting of the exquisite multiwavelength photometry available in the VANDELS fields, using the dedicated spectral modeling tool BEAGLE and the UV β slope from the observed photometry. We characterized the Lyα emission in terms of kinematics, equivalent width (EW), full width at half-maximum, and spatial extension and then estimated the velocity of the neutral outflowing gas. The ultra-deep VANDELS spectra (up to 80 h on-source integration) enable this for individual galaxies without the need to rely on stacks. We then investigated the correlations between the Lyα properties and the other measured properties to study how they affect the shape and intensity of Lyα emission. Results. We reproduce some of the well-known correlations between Lyα EW and stellar mass, dust extinction, and UV β slope, in the sense that the emission line appears brighter in galaxies with lower mass that are less dusty and bluer. We do not find any correlation with the SED-derived star formation rate, while we find that galaxies with brighter Lyα tend to be more compact in both UV and in Lyα. Our data reveal an interesting correlation between the Lyα velocity offset and the shift of the interstellar absorption lines with respect to the systemic redshift, observed for the first time at high redshifts: galaxies with higher interstellar medium (ISM) outflow velocities show smaller Lyα velocity shifts. We interpret this relation in the context of the shell-model scenario, where the velocity of the ISM and the HI column density contribute together in determining the Lyα kinematics. In support to our interpretation, we observe that galaxies with high HI column densities have much more extended Lyα spatial profiles; this is a sign of increased scattering. However, we do not find any evidence that the HI column density is related to any other physical properties of the galaxies, although this might be due in part to the limited range of parameters that our sample spans. [ABSTRACT FROM AUTHOR]

Published
2019
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19. The evolving star formation rate: MBlack star relation and sSFR since z ≃ 5 from the VUDS spectroscopic survey

Author

Tasca, L. A. M., Le Fèvre, O., Hathi, N. P., Schaerer, D., Ilbert, O., Zamorani, G., Lemaux, B. C., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Amorin, R., Bardelli, S., Cassarà, L. P., Castellano, M., Cimatti, A., Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Paltani, S., Ribeiro, B., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., De La Torre, S., Dunlop, J., Fotopoulou, S., Koekemoer, A., López-Sanjuan, C., Mellier, Y., Pforr, J., Salvato, M., Scoville, N., Taniguchi, Y., and Wang, P. W.

Subjects
galaxies: high-redshift, Space and Planetary Science, galaxies: star formation, galaxies: formation, Astronomy and Astrophysics, galaxies: evolution
Published
2015

20. The progeny of a cosmic titan: a massive multi-component proto-supercluster in formation at z = 2.45 in VUDS.

Author

Cucciati, O., Lemaux, B. C., Zamorani, G., Le Fèvre, O., Tasca, L. A. M., Hathi, N. P., Lee, K.-G., Bardelli, S., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Lubin, L. M., Amorin, R., Cassarà, L. P., and Cimatti, A.

Subjects
SUPERCLUSTERS, STAR formation, ASTRONOMICAL photometry, REDSHIFT, OPTICAL polarimetry
Abstract

We unveil the complex shape of a proto-supercluster at z ∼ 2.45 in the COSMOS field exploiting the synergy of both spectroscopic and photometric redshifts. Thanks to the spectroscopic redshifts of the VIMOS Ultra-Deep Survey (VUDS), complemented by the zCOSMOS-Deep spectroscopic sample and high-quality photometric redshifts, we compute the three-dimensional (3D) overdensity field in a volume of ∼100 × 100 × 250 comoving Mpc3 in the central region of the COSMOS field, centred at z ∼ 2.45 along the line of sight. The method relies on a two-dimensional (2D) Voronoi tessellation in overlapping redshift slices that is converted into a 3D density field, where the galaxy distribution in each slice is constructed using a statistical treatment of both spectroscopic and photometric redshifts. In this volume, we identify a proto-supercluster, dubbed "Hyperion" for its immense size and mass, which extends over a volume of ∼60 × 60 × 150 comoving Mpc3 and has an estimated total mass of ∼4.8 × 1015M⊙. This immensely complex structure contains at least seven density peaks within 2.4 ≲ z ≲ 2.5 connected by filaments that exceed the average density of the volume. We estimate the total mass of the individual peaks, Mtot, based on their inferred average matter density, and find a range of masses from ∼0.1 × 1014M⊙ to ∼2.7 × 1014M⊙. By using spectroscopic members of each peak, we obtain the velocity dispersion of the galaxies in the peaks, and then their virial mass Mvir (under the strong assumption that they are virialised). The agreement between Mvir and Mtot is surprisingly good, at less than 1−2σ, considering that (almost all) the peaks are probably not yet virialised. According to the spherical collapse model, these peaks have already started or are about to start collapsing, and they are all predicted to be virialised by redshift z ∼ 0.8−1.6. We finally perform a careful comparison with the literature, given that smaller components of this proto-supercluster had previously been identified using either heterogeneous galaxy samples (Lyα emitters, sub-mm starbursting galaxies, CO emitting galaxies) or 3D Lyα forest tomography on a smaller area. With VUDS, we obtain, for the first time across the central ∼1 deg2 of the COSMOS field, a panoramic view of this large structure, that encompasses, connects, and considerably expands in a homogeneous way on all previous detections of the various sub-components. The characteristics of this exceptional proto-supercluster, its redshift, its richness over a large volume, the clear detection of its sub-components, together with the extensive multi-wavelength imaging and spectroscopy granted by the COSMOS field, provide us the unique possibility to study a rich supercluster in formation. [ABSTRACT FROM AUTHOR]

Published
2018
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21. Lyα-Lyman continuum connection in 3.5 ≤ z ≤ 4.3 star-forming galaxies from the VUDS survey.

Author

Marchi, F., Pentericci, L., Guaita, L., Schaerer, D., Verhamme, A., Castellano, M., Ribeiro, B., Garilli, B., Fèvre, O. Le, Amorin, R., Bardelli, S., Cassata, P., Durkalec, A., Grazian, A., Hathi, N. P., Lemaux, B. C., Maccagni, D., Vanzella, E., and Zucca, E.

Subjects
STAR formation, GALACTIC evolution, ASTRONOMICAL observations, STATISTICAL correlation, UNIVERSE
Abstract

Context. To identify the galaxies responsible for the reionization of the Universe, we must rely on the investigation of the Lyman continuum (LyC) properties of z ≲ 5 star-forming galaxies, where we can still directly observe their ionizing radiation. Aims. The aim of this work is to explore the correlation between the LyC emission and some of the proposed indirect indicators of LyC radiation at z ~ 4 such as a bright Lyα emission and a compact UV continuum size. Methods. We selected a sample of 201 star-forming galaxies from the Vimos Ultra Deep Survey (VUDS) at 3.5 ≤ z ≤ 4.3 in the COSMOS, ECDFS, and VVDS-2h fields, including only those with reliable spectroscopic redshifts, a clean spectrum in the LyC range and clearly not contaminated by bright nearby sources in the same slit. For all galaxies we measured the Lyα EW, the Lyα velocity shift with respect to the systemic redshift, the Lyα spatial extension and the UV continuum effective radius. We then selected different sub-samples according to the properties predicted to be good LyC emission indicators: in particular we created sub-samples of galaxies with EW(Lyα) ≥ 70 Å, Lyαext ≤ 5.7 kpc, rUV ≤ 0.30 kpc and |ΔvLyα|≤ 200 km s−1. We stacked all the galaxies in each sub-sample and measured the flux density ratio (fλ(895)∕fλ(1470)), that we considered to be a proxy for LyC emission. We then compared these ratios to those obtained for the complementary samples. Finally, to estimate the statistical contamination from lower redshift inter-lopers in our samples, we performed dedicated Monte Carlo simulations using an ultradeep U-band image of the ECDFS field. Results. We find that the stacks of galaxies which are UV compact (rUV ≤ 0.30 kpc) and have bright Lyα emission (EW(Lyα) ≥ 70 Å), have much higher LyC fluxes compared to the rest of the galaxy population. These parameters appear to be good indicators of LyC radiation in agreement with theoretical studies and previous observational works. In addition we find that galaxies with a low Lyα spatial extent (Lyαext ≤ 5.7 kpc) have higher LyC flux compared to the rest of the population. Such a correlation had never been analysed before and seems even stronger than the correlation with high EW(Lyα) and small rUV. These results assume that the stacks from all sub-samples present the same statistical contamination from lower redshift interlopers. If we subtract a statistical contamination from low redshift interlopers obtained with the simulations from the flux density ratios (fλ(895)∕fλ(1470)) of the significant sub-samples we find that these samples contain real LyC leaking flux with a very high probability, although the true average escape fractions are very uncertain. Conclusions. Our work indicates that galaxies with very high EW(Lyα), small Ly αext and small rUV are very likely the best candidates to show Lyman continuum radiation at z ~ 4 and could therefore be the galaxies that have contributed most to reionisation. [ABSTRACT FROM AUTHOR]

Published
2018
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22. AGN-enhanced outflows of low-ionization gas in star-forming galaxies at 1.7 < z < 4.6.

Author

Talia, M., Brusa, M., Cimatti, A., Lemaux, B. C., Amorin, R., Bardelli, S., Cassarà, L. P., Cucciati, O., Garilli, B., Grazian, A., Guaita, L., Hathi, N. P., Koekemoer, A., Le Fèvre, O., Maccagni, D., Nakajima, K., Pentericci, L., Pforr, J., Schaerer, D., and Vanzella, E.

Subjects
ACTIVE galactic nuclei, GALAXY formation, STAR formation
Abstract

Fast and energetic winds are invoked by galaxy formation models as essential processes in the evolution of galaxies. These outflows can be powered either by star formation (SF) and/or active galactic nucleus (AGN) activity, but the relative dominance of the two mechanisms is still under debate. We use spectroscopic stacking analysis to study the properties of the low-ionization phase of the outflow in a sample of 1330 star-forming galaxies (SFGs) and 79 X-ray-detected (1042 < LX < 1045 erg s-1) Type 2 AGN at 1.7 < z < 4.6 selected from a compilation of deep optical spectroscopic surveys, mostly zCOSMOS-Deep and VIMOS Ultra Deep Survey (VUDS). We measure mean velocity offsets of ~- 150 km s-1 in the SFGs, while in the AGN sample the velocity is much higher (~- 950 km s-1), suggesting that the AGN is boosting the outflow up to velocities that could not be reached only with the SF contribution. The sample of X-ray AGN has on average a lower SF rate than non-AGN SFGs of similar mass: this, combined with the enhanced outflow velocity in AGN hosts, is consistent with AGN feedback in action. We further divide our sample of AGN into two X-ray luminosity bins: we measure the same velocity offsets in both stacked spectra, at odds with results reported for the highly ionized phase in local AGN, suggesting that the two phases of the outflow may be mixed only up to relatively low velocities, while the highest velocities can be reached only by the highly ionized phase. [ABSTRACT FROM AUTHOR]

Published
2017
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23. The ASTRODEEP Frontier Fields catalogues: III. Multiwavelength photometry and rest-frame properties of MACS-J0717 and MACS-J1149.

Author

Criscienzo, M. Di, Merlin, E., Castellano, M., Santini, P., Fontana, A., Amorin, R., Boutsia, K., Derriere, S., Dunlop, J. S., Elbaz, D., Grazian, A., McLure, R. J., Mármol-Queraltó, E., Michalowski, M. J., Mortlock, S., Parsa, S., and Pentericci, L.

Abstract

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 107 M⊙ and/or SFR = 0.1–1 M⊙/yr out to redshift z> 6. [ABSTRACT FROM AUTHOR]

Published
2017
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24. New constraints on the average escape fraction of Lyman continuum radiation in z ~ 4 galaxies from the VIMOS Ultra Deep Survey (VUDS).

Author

Marchi, F., Pentericci, L., Guaita, L., Ribeiro, B., Castellano, M., Schaerer, D., Hathi, N. P., Lemaux, B. C., Grazian, A., Le Fèvre, O., Garilli, B., Maccagni, D., Amorin, R., Bardelli, S., Cassata, P., Fontana, A., Koekemoer, A. M., Le Brun, V., Tasca, L. A. M., and Thomas, R.

Subjects
CONTINUUM hypothesis, PHOTON emission, REDSHIFT, IONIZING radiation, STAR formation
Abstract

Context: Determining the average fraction of Lyman continuum (LyC) photons escaping high redshift galaxies is essential for understanding how reionization proceeded in the z> 6 Universe. Aims: We want to measure the LyC signal from a sample of sources in the Chandra Deep Field South (CDFS) and COSMOS fields for which ultra-deep VIMOS spectroscopy as well as multi-wavelength Hubble Space Telescope (HST) imaging are available. Methods: We select a sample of 46 galaxies at z ~ 4 from the VIMOS Ultra Deep Survey (VUDS) database, such that the VUDS spectra contain the LyC part, that is, the rest-frame range 880-910 Å. Taking advantage of the HST imaging, we apply a careful cleaning procedure and reject all the sources showing nearby clumps with different colours, that could potentially be lower-redshift interlopers. After this procedure, the sample is reduced to 33 galaxies. We measure the ratio between ionizing flux (LyC at 895 Å) and non-ionizing emission (at ~ 1500 Å) for all individual sources. We also produce a normalized stacked spectrum of all sources. Results: Assuming an intrinsic average L(1470)/L(895) of 3, we estimate the individual and average relative escape fraction. We do not detect ionizing radiation from any individual source, although we identify a possible LyC emitter with very high Lya equivalent width (EW). From the stacked spectrum and assuming a mean transmissivity for the sample, we measure a relative escape fraction f escrel = 0.09 ± 0.04. We also look for correlations between the limits in the LyC flux and source properties and find a tentative correlation between LyC flux and the EW of the Lya emission line. Conclusions: Our results imply that the LyC flux emitted by V = 25-26 star-forming galaxies at z ~ 4 is at most very modest, in agreement with previous upper limits from studies based on broad and narrow band imaging. [ABSTRACT FROM AUTHOR]

Published
2017
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25. The VIMOS Ultra Deep Survey first data release: Spectra and spectroscopic redshifts of 698 objects up to zspec ~ 6 in CANDELS.

Author

Tasca, L. A. M., Le Fèvre, O., Ribeiro, B., Thomas, R., Moreau, C., Cassata, P., Garilli, B., Le Brun, V., Lemaux, B. C., Maccagni, D., Pentericci, L., Schaerer, D., Vanzella, E., Zamorani, G., Zucca, E., Amorin, R., Bardelli, S., Cassarà, L. P., Castellano, M., and Cimatti, A.

Subjects
GALACTIC redshift, ASTRONOMICAL photometry, STELLAR mass, SPECTRAL energy distribution, ABSORPTION
Abstract

This paper describes the first data release (DR1) of the VIMOS Ultra Deep Survey (VUDS). The VUDS-DR1 is the release of all low-resolution spectroscopic data obtained in 276.9 arcmin² of the CANDELS-COSMOS and CANDELS-ECDFS survey areas, including accurate spectroscopic redshifts zspec and individual spectra obtained with VIMOS on the ESO-VLT. A total of 698 objects have a measured redshift, with 677 galaxies, two type-I AGN, and a small number of 19 contaminating stars. The targets of the spectroscopic survey are selected primarily on the basis of their photometric redshifts to ensure a broad population coverage. About 500 galaxies have zspec > 2, 48 of which have zspec > 4; the highest reliable redshifts reach beyond zspec = 6. This data set approximately doubles the number of galaxies with spectroscopic redshifts at z > 3 in these fields. We discuss the general properties of the VUDS-DR1 sample in terms of the spectroscopic redshift distribution, the distribution of Lyman-α equivalent widths, and physical properties including stellar masses M* and star formation rates derived from spectral energy distribution fitting with the knowledge of zspec. We highlight the properties of the most massive star-forming galaxies, noting the wide range in spectral properties, with Lyman-α in emission or in absorption, and in imaging properties with compact, multi-component, or pair morphologies. We present the catalogue database and data products. All VUDS-DR1 data are publicly available and can be retrieved from a dedicated query-based database. Future VUDS data releases will follow this VUDS-DR1 to give access to the spectra and associated measurement of 8000 objects in the full ~1 square degree of the VUDS survey. [ABSTRACT FROM AUTHOR]

Published
2017
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26. Constraints on the star-formation rate of z ~ 3 LBGs with measured metallicity in the CANDELS GOODS-South field.

Author

Castellano, M., Sommariva, V., Fontana, A., Pentericci, L., Santini, P., Grazian, A., Amorin, R., Donley, J. L., Dunlop, J. S., Ferguson, H. C., Fiore, F., Galametz, A., Giallongo, E., Guo, Y., Huang, K.-H., Koekemoer, A., Maiolino, R., McLure, R. J., Paris, D., and Schaerer, D.

Subjects
STAR formation, GALACTIC redshift, ULTRAVIOLET radiation, NEBULAR hypothesis, STELLAR populations
Abstract

Aims. We aim to constrain the assembly history of high-redshift galaxies and the reliability of UV-based estimates of their physical parameters from an accurate analysis of a unique sample of z ~ 3 Lyman-break galaxies (LBGs). Methods. We analyse 14 LBGs at z ~ 2.8–3.8 constituting the only sample where both a spectroscopic measurement of their metallicity and deep IR observations (CANDELS+HUGS survey) are available. Fixing the metallicity of population synthesis models to the observed values, we determine best-fit physical parameters under different assumptions about the star-formation history (SFH) and also consider the effect of nebular emission. For comparison, we determine the UV slope of the objects, and use it to estimate their SFRUV99 by correcting the UV luminosity. Results. A comparison between star-formation rate (SFR) obtained through SED-fitting (SFRfit) and the SFRUV99 shows that the latter are underestimated by a factor of 2–10, regardless of the assumed SFH. Other SFR indicators (radio, far-IR, X-ray, recombination lines) coherently indicate SFRs a factor of 2–4 larger than SFRUV99 and in closer agreement with SFRfit. This discrepancy is due to the solar metallicity implied by the usual ß - A1600 conversion factor. We propose a refined relation, appropriate for subsolar metallicity LBGs: A1600 = 5.32 + 1.99 * ß. This relation reconciles the dust-corrected UV with the SED-fitting and the other SFR indicators. We show that the fact that z ~ 3 galaxies have subsolar metallicity implies an upward revision by a factor of ~1.5–2 of the global SFRD, depending on the assumptions about the age of the stellar populations. We find very young best-fit ages (10–500 Myr) for all our objects. From a careful examination of the uncertainties in the fit and the amplitude of the Balmer break we conclude that there is little evidence of the presence of old stellar population in at least half of the LBGs in our sample, suggesting that these objects are probably caught during a huge star-formation burst, rather than being the result of a smooth evolution. [ABSTRACT FROM AUTHOR]

Published
2014
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27. Characterizing elusive, faint dusty star-forming galaxies: A lensed, optically undetected ALMA galaxy at z ∼ 3.3

Author

Santini, P, Castellano, M, Fontana, A, Merlin, E, Maiolino, R, Mason, C, Mignano, A, Pilo, S, Amorin, R, Berta, S, Bourne, N, Calura, F, Daddi, E, Elbaz, D, Grazian, A, Magliocchetti, M, Michałowski, MJ, Pentericci, L, Pozzi, F, Rodighiero, G, Schreiber, C, and Valiante, R

Subjects
submillimeter: galaxies, galaxies: photometry, galaxies: high-redshift, cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, galaxies: fundamental parameters, Astrophysics::Cosmology and Extragalactic Astrophysics, 10. No inequality, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

We present the serendipitous ALMA detection of a faint submillimeter galaxy (SMG) lensed by a foreground $\textit{z}$ ∼ 1 galaxy. By optimizing the source detection to deblend the system, we accurately build the full spectral energy distribution of the distant galaxy from the I814 band to radio wavelengths. It is extremely red, with a $\textit{I-K}$ colour larger than 2.5. We estimate a photometric redshift of 3.28 and determine the physical parameters. The distant galaxy turns out to be magnified by the foreground lens by a factor of ∼1.5, which implies an intrinsic $\textit{K}$$_{s}$-band magnitude of ∼24.5, a submillimeter flux at 870 $\textit{μ}$m of ∼2.5 mJy and a SFR of ∼150-300 $\textit{M}$$_{⊙}$/yr, depending on the adopted tracer. These values place our source towards the faint end of the distribution of observed SMGs, and in particular among the still few faint SMGs with a fully characterized spectral energy distribution, which allows us not only to accurately estimate its redshift, but also to measure its stellar mass and other physical properties. The galaxy studied in this work is a representative of the population of faint SMGs, of which only few objects are known to date, that are undetected in optical and therefore are not typically accounted for when measuring the cosmic star formation history (SFH). This faint galaxy population thus likely represents an important and missing piece in our understanding of the cosmic SFH. Its observation and characterization is of major importance to achieve a solid picture of galaxy evolution., The research leading to these results has received funding from the European Union Seventh Framework Programme ASTRODEEP (FP7/2007-2013) under grant agreement No. 312725. R.M. and R.A. acknowledge support from the ERC Advanced Grant 695671 QUENCH.

28. The ALPINE-ALMA [CII] survey:Molecular gas budget in the early Universe as traced by [CII]

Author

Andrea Cimatti, S. Bardelli, Andreas L. Faisst, E. Zucca, G. Rodighiero, Y. Khusanova, Daniel Schaerer, Pascal Oesch, Sune Toft, Paolo Cassata, Livia Vallini, Nimish P. Hathi, Carlotta Gruppioni, M. Romano, Francesca Pozzi, F. Loiacono, G. Zamorani, Michele Ginolfi, Lin Yan, John D. Silverman, Miroslava Dessauges-Zavadsky, Anton M. Koekemoer, Y. Fudamoto, G. C. Jones, Desika Narayanan, Margherita Talia, Brian C. Lemaux, Daniela Vergani, Seiji Fujimoto, Peter Capak, Edo Ibar, Médéric Boquien, Matthieu Béthermin, O. Le Fevre, Ricardo Amorín, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Dessauges-Zavadsky M., Ginolfi M., Pozzi F., Bethermin M., Le Fevre O., Fujimoto S., Silverman J.D., Jones G.C., Vallini L., Schaerer D., Faisst A.L., Khusanova Y., Fudamoto Y., Cassata P., Loiacono F., Capak P.L., Yan L., Amorin R., Bardelli S., Boquien M., Cimatti A., Gruppioni C., Hathi N.P., Ibar E., Koekemoer A.M., Lemaux B.C., Narayanan D., Oesch P.A., Rodighiero G., Romano M., Talia M., Toft S., Vergani D., Zamorani G., Zucca E., Dessauges-Zavadsky, M., Ginolfi, M., Pozzi, F., Bethermin, M., Le Fevre, O., Fujimoto, S., Silverman, J. D., Jones, G. C., Vallini, L., Schaerer, D., Faisst, A. L., Khusanova, Y., Fudamoto, Y., Cassata, P., Loiacono, F., Capak, P. L., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Gruppioni, C., Hathi, N. P., Ibar, E., Koekemoer, A. M., Lemaux, B. C., Narayanan, D., Oesch, P. A., Rodighiero, G., Romano, M., Talia, M., Toft, S., Vergani, D., Zamorani, G., and Zucca, E.

Subjects
C-II, Stellar mass, MASS-METALLICITY RELATION, FOS: Physical sciences, DUST, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, CONVERSION FACTOR, SCALING RELATIONS, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, MAIN-SEQUENCE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], molecules [ISM], Physics, LEGACY SURVEY, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM [galaxies], 010308 nuclear & particles physics, Star formation, Gas depletion, Gas supply, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, ISM: molecules, EVOLUTION, MODEL, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Halo, galaxies: evolution, Cosmic time, galaxies: ISM, high-redshift [galaxies]
Abstract

The molecular gas content of normal galaxies at z>4 is poorly constrained, because the commonly used molecular gas tracers become hard to detect. We use the [CII]158um luminosity, recently proposed as a molecular gas tracer, to estimate the molecular gas content in a large sample of main-sequence star-forming galaxies at z=4.4-5.9, with a median stellar mass of 10^9.7 Msun, drawn from the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey. The agreement between molecular gas masses derived from [CII] luminosity, dynamical mass, and rest-frame 850um luminosity, extrapolated from the rest-frame 158um continuum, supports [CII] as a reliable tracer of molecular gas in our sample. We find a continuous decline of the molecular gas depletion timescale from z=0 to z=5.9, which reaches a mean value of (4.6+/-0.8)x10^8 yr at z~5.5, only a factor of 2-3 shorter than in present-day galaxies. This suggests a mild enhancement of star formation efficiency toward high redshifts, unless the molecular gas fraction significantly increases. Our estimates show that the rise in molecular gas fraction as reported previously, flattens off above z~3.7 to achieve a mean value of 63%+/-3 over z=4.4-5.9. This redshift evolution of the gas fraction is in line with the one of the specific star formation rate. We use multi-epoch abundance matching to follow the gas fraction evolution over cosmic time of progenitors of z=0 Milky Way-like galaxies in 10^13 Msun halos and of more massive z=0 galaxies in 10^14 Msun halos. Interestingly, the former progenitors show a monotonic decrease of the gas fraction with cosmic time, while the latter show a constant gas fraction from z=5.9 to z~2 and a decrease at z, 16 pages, 9 figures, 2 tables. Submitted to Astronomy & Astrophysics

Published
2020
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29. The ALPINE-ALMA [CII] survey: Dust attenuation properties and obscured star formation at z~4.4-5.8

Author

Anton M. Koekemoer, Margherita Talia, Guilaine Lagache, Ricardo Amorín, Desika Narayanan, G. Rodighiero, Sune Toft, Brian C. Lemaux, G. Zamorani, Miroslava Dessauges-Zavadsky, Livia Vallini, Y. Khusanova, Matthieu Béthermin, Roberto Maiolino, Andrea Cimatti, Lin Yan, Daniela Vergani, Y. Fudamoto, Francesca Pozzi, Nimish P. Hathi, F. Loiacono, Michele Ginolfi, Edo Ibar, Seiji Fujimoto, S. Bardelli, Médéric Boquien, G. C. Jones, Carlotta Gruppioni, Daniel Schaerer, Andreas L. Faisst, O. Le Fèvre, E. Zucca, Dominik A. Riechers, John D. Silverman, Pascal Oesch, Peter Capak, Paolo Cassata, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Fudamoto Y., Oesch P.A., Faisst A., Bethermin M., Ginolfi M., Khusanova Y., Loiacono F., Le Fevre O., Capak P., Schaerer D., Silverman J.D., Cassata P., Yan L., Amorin R., Bardelli S., Boquien M., Cimatti A., Dessauges-Zavadsky M., Fujimoto S., Gruppioni C., Hathi N.P., Ibar E., Jones G.C., Koekemoer A.M., Lagache G., Lemaux B.C., Maiolino R., Narayanan D., Pozzi F., Riechers D.A., Rodighiero G., Talia M., Toft S., Vallini L., Vergani D., Zamorani G., Zucca E., Fudamoto, Y., Oesch, P. A., Faisst, A., Bethermin, M., Ginolfi, M., Khusanova, Y., Loiacono, F., Le Fevre, O., Capak, P., Schaerer, D., Silverman, J. D., Cassata, P., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Fujimoto, S., Gruppioni, C., Hathi, N. P., Ibar, E., Jones, G. C., Koekemoer, A. M., Lagache, G., Lemaux, B. C., Maiolino, R., Narayanan, D., Pozzi, F., Riechers, D. A., Rodighiero, G., Talia, M., Toft, S., Vallini, L., Vergani, D., Zamorani, G., Zucca, E., Jones, Gareth [0000-0002-0267-9024], Maiolino, Roberto [0000-0002-4985-3819], and Apollo - University of Cambridge Repository

Subjects
Stellar mass, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, high-redshift [Galaxies], Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, ISM [Galaxies], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Physics, Infrared excess, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, extinction, Astronomy and Astrophysics, Dust, Extinction, Atacama Large Millimeter Array, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), dust, Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM
Abstract

We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ~4.4-5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158��m obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope ($��$), stellar mass (M_*), and infrared excess (IRX=L_IR/L_UV). Twenty-three galaxies are individually detected in the continuum at >3.5 sigma significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z~4.4-5.8. The individual detections and stacks show that the IRX-$��$ relation at z~5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z4. Similarly, we find that our galaxies have lower IRX values, up to 1dex on average, at a fixed mass compared to previously studied IRX-M_* relations at z4 are characterised by (i) a steeper attenuation curve than at z10) at z~5-6 already exhibit an obscured fraction of star formation of ~45%, indicating a rapid build-up of dust during the epoch of reionization., 12 pages, 6 figures. accepted for publication in Astronomy & Astrophysics. Minor revisions

Published
2020
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30. The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties

Author

Dominik A. Riechers, Brian C. Lemaux, Sune Toft, Livia Vallini, Daniela Vergani, Nimish P. Hathi, E. Zucca, S. Bardelli, Y. Khusanova, Ricardo Amorín, Paolo Cassata, Lin Yan, Seiji Fujimoto, Andreas L. Faisst, Iary Davidzon, Y. Fudamoto, Michele Ginolfi, O. Le Fèvre, Daniel Schaerer, G. C. Jones, Carlotta Gruppioni, Pascal Oesch, G. Zamorani, Matthieu Béthermin, Edo Ibar, Margherita Talia, C. Moreau, Francesca Pozzi, Médéric Boquien, F. Loiacono, John D. Silverman, Anton M. Koekemoer, Guilaine Lagache, Peter Capak, Andrea Cimatti, Miroslava Dessauges-Zavadsky, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Bethermin M., Fudamoto Y., Ginolfi M., Loiacono F., Khusanova Y., Capak P.L., Cassata P., Faisst A., Le Fevre O., Schaerer D., Silverman J.D., Yan L., Amorin R., Bardelli S., Boquien M., Cimatti A., Davidzon I., Dessauges-Zavadsky M., Fujimoto S., Gruppioni C., Hathi N.P., Ibar E., Jones G.C., Koekemoer A.M., Lagache G., Lemaux B.C., Moreau C., Oesch P.A., Pozzi F., Riechers D.A., Talia M., Toft S., Vallini L., Vergani D., Zamorani G., Zucca E., Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Bethermin, M., Fudamoto, Y., Ginolfi, M., Loiacono, F., Khusanova, Y., Capak, P. L., Cassata, P., Faisst, A., Le Fevre, O., Schaerer, D., Silverman, J. D., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Davidzon, I., Dessauges-Zavadsky, M., Fujimoto, S., Gruppioni, C., Hathi, N. P., Ibar, E., Jones, G. C., Koekemoer, A. M., Lagache, G., Lemaux, B. C., Moreau, C., Oesch, P. A., Pozzi, F., Riechers, D. A., Talia, M., Toft, S., Vallini, L., Vergani, D., Zamorani, G., and Zucca, E.

Subjects
submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Continuum (design consultancy), FOS: Physical sciences, Astrophysics, star formation [Galaxies], 01 natural sciences, Luminosity, high-redshift [Galaxies], galaxies [Submillimeter], Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, Cosmic infrared background, ISM [Galaxies], 0103 physical sciences, 010303 astronomy & astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Atacama Large Millimeter Array, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Spectral energy distribution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The ALPINE-ALMA large program targets the [CII] 158 $\mu$m line and the far-infrared continuum in 118 spectroscopically confirmed star-forming galaxies between z=4.4 and z=5.9. It represents the first large [CII] statistical sample built in this redshift range. We present details of the data processing and the construction of the catalogs. We detected 23 of our targets in the continuum. To derive accurate infrared luminosities and obscured star formation rates, we measured the conversion factor from the ALMA 158 $\mu$m rest-frame dust continuum luminosity to the total infrared luminosity (L$_{\rm IR}$) after constraining the dust spectral energy distribution by stacking a photometric sample similar to ALPINE in ancillary single-dish far-infrared data. We found that our continuum detections have a median L$_{\rm IR}$ of 4.4$\times 10^{11}$ L$_\odot$. We also detected 57 additional continuum sources in our ALMA pointings. They are at lower redshift than the ALPINE targets, with a mean photometric redshift of 2.5$\pm$0.2. We measured the 850 $\mu$m number counts between 0.35 and 3.5 mJy, improving the current interferometric constraints in this flux density range. We found a slope break in the number counts around 3 mJy with a shallower slope below this value. More than 40 % of the cosmic infrared background is emitted by sources brighter than 0.35 mJy. Finally, we detected the [CII] line in 75 of our targets. Their median [CII] luminosity is 4.8$\times$10$^8$ L$_\odot$ and their median full width at half maximum is 252 km/s. After measuring the mean obscured SFR in various [CII] luminosity bins by stacking ALPINE continuum data, we find a good agreement between our data and the local and predicted SFR-L$_{\rm [CII]}$ relations of De Looze et al. (2014) and Lagache et al. (2018)., Comment: 44 pages, 29 figures, 14 tables, accepted by A&A, ALPINE products released at https://cesam.lam.fr/a2c2s/, luminosities in table B2 corrected

Published
2020
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31. X-ray properties of He ii λ 1640 emitting galaxies in VANDELS

Author

Angela Bongiorno, G. Zamorani, Raffaella Schneider, Fergus Cullen, Marco Castellano, Margherita Talia, Johan P. U. Fynbo, Andrea Cimatti, Nimish P. Hathi, A. Saxena, A. Calabrò, Adriano Fontana, Laura Pentericci, Ricardo Amorín, D. J. McLeod, Daniel Schaerer, Saxena, A, Pentericci, L, Zamorani, G, Talia, M, McLeod, D J, Hathi, N, Fynbo, J P U, Fontana, A, Cullen, F, Cimatti, A, Castellano, M, Calabrò, A, Bongiorno, A, Amorin, R, Schneider, R, and Schaerer, D

Subjects
Physics, Photon, galaxies: high-redshift – X-rays: binaries – galaxies: evolution, 010308 nuclear & particles physics, Metallicity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Redshift, Galaxy, Luminosity, X-rays: binaries, Stars, galaxies: high-redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Chandra Deep Field South, galaxies: evolution, 010303 astronomy & astrophysics, Line (formation)
Abstract

We explore X-ray emission from a sample of 18 He II 1640 emitting star-forming galaxies at z ~ 2.3-3.6 from the VANDELS survey in the Chandra Deep Field South, to set constraints on the role of X-ray sources in powering the He II emission. We find that 4 He II emitters have tentative detections with S/N ~ 2 and have X-ray luminosities, L_X = 1.5-4.9 x 10^41 erg/s. The stacked luminosity of all 18 He II emitters is 2.6 x 10^41 erg/s, and that of a subset of 13 narrow He II emitters (FHWM(He II) < 1000 km/s) is 3.1 x 10^41 erg/s. We also measure stacked L_X for non-He II emitters through bootstrapping of matched samples, and find L_X = 2.5 x 10^41 erg/s, which is not significantly different from L_X measured for He II emitters. The L_X per star-formation rate for He II emitters (log (L_X/SFR) ~ 40.0) and non-emitters (log (L_X/SFR) ~ 39.9) are also comparable and in line with the redshift evolution and metallicity dependence predicted by models. Due to the non-significant difference between the X-ray emission from galaxies with and without He II, we conclude that X-ray binaries or weak or obscured AGNs are unlikely to be the dominant producers of He II ionising photons in VANDELS star-forming galaxies at z ~ 3. Given the comparable physical properties of both He II emitters and non-emitters reported previously, alternative He II ionising mechanisms such as localised low-metallicity stellar populations, Pop-III stars, etc. may need to be explored., 12 pages, 5 figures, accepted for publication in MNRAS

Published
2020
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32. The VANDELS survey: a strong correlation between Ly α equivalent width and stellar metallicity at 3 ≤ z ≤ 5

Author

A. Calabrò, O. Cucciati, G. Zamorani, D. J. McLeod, Ross J. McLure, Nimish P. Hathi, Lucia Guaita, B. Garilli, James Dunlop, Johan P. U. Fynbo, Laura Pentericci, Mauro Giavalisco, Marco Castellano, Margherita Talia, Andrea Cimatti, Fergus Cullen, Adriano Fontana, M. Bolzonella, A. Saxena, Ricardo Amorín, Giovanni Cresci, A. C. Carnall, F. Mannucci, Michele Cirasuolo, Fabio Fontanot, Matt J. Jarvis, Lucia Pozzetti, Anton M. Koekemoer, Alice E. Shapley, ITA, USA, GBR, FRA, DEU, Cullen, F, McLure, RJ, Dunlop, JS, Carnall, AC, McLeod, DJ, Shapley, AE, Amorin, R, Bolzonella, M, Castellano, M, Cimatti, A, Cirasuolo, M, Cucciati, O, Fontana, A, Fontanot, F, Garilli, B, Guaita, L, Jarvis, MJ, Pentericci, L, Pozzetti, L, Talia, M, Zamorani, G, Calabro, A, Cresci, G, Fynbo, JPU, Hathi, NP, Giavalisco, M, Koekemoer, A, Mannucci, F, and Saxena, A

Subjects
Physics, education.field_of_study, Stellar population, 010308 nuclear & particles physics, astro-ph.GA, Metallicity, Population, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Spectral line, galaxies: high-redshift, Space and Planetary Science, 0103 physical sciences, Spectral fitting, galaxies: evolution, education, 010303 astronomy & astrophysics, Equivalent width, evolution [galaxies], high-redshift [galaxies]
Abstract

We present the results of a new study investigating the relationship between observed Ly α equivalent width (Wλ(Ly α)) and the metallicity of the ionizing stellar population ( Z⋆) for a sample of 768 star-forming galaxies at 3 ≤ z ≤ 5 drawn from the VANDELS survey. Dividing our sample into quartiles of rest-frame Wλ(Ly α) across the range $-58 \,\rm {\mathring{\rm A}} \lesssim$ Wλ(Ly α) $\lesssim 110 \,\rm {\mathring{\rm A}}$ , we determine Z⋆ from full spectral fitting of composite far-ultraviolet spectra and find a clear anticorrelation between Wλ(Ly α) and Z⋆. Our results indicate that Z⋆ decreases by a factor ≳ 3 between the lowest Wλ(Ly α) quartile (λ(Ly α) $\rangle =-18\,\rm {\mathring{\rm A}}$ ) and the highest Wλ(Ly α) quartile (λ(Ly α) $\rangle =24\,\rm {\mathring{\rm A}}$ ). Similarly, galaxies typically defined as Lyman alpha emitters (LAEs; Wλ(Ly α) $\gt 20\,\rm {\mathring{\rm A}}$ ) are, on average, metal poor with respect to the non-LAE galaxy population (Wλ(Ly α) $\le 20\,\rm {\mathring{\rm A}}$ ) with Z⋆non-LAE ≳ 2 × Z⋆LAE. Finally, based on the best-fitting stellar models, we estimate that the increasing strength of the stellar ionizing spectrum towards lower Z⋆ is responsible for ${\simeq}15{-}25{{\ \rm per\ cent}}$ of the observed variation in Wλ(Ly α) across our sample, with the remaining contribution ( ${\simeq}75{-}85{{\ \rm per\ cent}}$ ) being due to a decrease in the H I/dust covering fractions in low- Z⋆ galaxies.

Published
2020
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33. The ALPINE-ALMA [CII] survey: Obscured star formation rate density and main sequence of star-forming galaxies at z > 4

Author

Miroslava Dessauges-Zavadsky, Francesca Pozzi, F. Loiacono, Daniela Vergani, Dominik A. Riechers, Michele Ginolfi, Pascal Oesch, M. Romano, G. C. Jones, Carlotta Gruppioni, Peter Capak, O. Le Fèvre, G. Zamorani, Daniel Schaerer, Paolo Cassata, Andreas L. Faisst, Ricardo Amorín, Sune Toft, Médéric Boquien, E. Zucca, Nimish P. Hathi, Brian C. Lemaux, Andrea Cimatti, John D. Silverman, Anton M. Koekemoer, Margherita Talia, Roberto Maiolino, Y. Khusanova, Lin Yan, Y. Fudamoto, Matthieu Béthermin, S. Bardelli, Guilaine Lagache, Khusanova Y., Bethermin M., Le Fevre O., Capak P., Faisst A.L., Schaerer D., Silverman J.D., Cassata P., Yan L., Ginolfi M., Fudamoto Y., Loiacono F., Amorin R., Bardelli S., Boquien M., Cimatti A., Dessauges-Zavadsky M., Gruppioni C., Hathi N.P., Jones G.C., Koekemoer A.M., Lagache G., Maiolino R., Lemaux B.C., Oesch P., Pozzi F., Riechers D.A., Romano M., Talia M., Toft S., Vergani D., Zamorani G., and Zucca E.

Subjects
EMISSION-LINES, SPECTROSCOPIC SURVEY, Stellar mass, ULTRA DEEP FIELD, Continuum (design consultancy), BILLION YEARS, galaxies [submillimeter], Astrophysics, Star (graph theory), 01 natural sciences, Luminosity, 0103 physical sciences, NUMBER COUNTS, Proxy (statistics), PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, evolution [galaxies], Physics, DUST ATTENUATION, Galaxies: star formation, UV LUMINOSITY FUNCTIONS, 010308 nuclear & particles physics, Star formation, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, LYMAN-BREAK GALAXIES, Submillimeter: galaxies, Space and Planetary Science, STELLAR MASS FUNCTION, star formation [galaxies], high-redshift [galaxies]
Abstract

Star formation rate (SFR) measurements at z>4 have relied mostly on rest-frame far-ultraviolet (FUV) observations. The corrections for dust attenuation based on IRX-$\beta$ relation are highly uncertain and are still debated in the literature. Hence, rest-frame far-infrared (FIR) observations are necessary to constrain the dust-obscured component of the SFR. In this paper, we exploit the rest-frame FIR continuum observations collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) to directly constrain the obscured SFR in galaxies at 4.4, Comment: submitted to A&A, 19 pages

Published
2021
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34. Less and more IGM-transmitted galaxies from z ∼ 2.7 to z ∼ 6 from VANDELS and VUDS

Author

E. Zucca, J. P. U. Fynbo, Margherita Talia, Ricardo Amorín, Anton M. Koekemoer, Y. Khusanova, Stefano Cristiani, Pascale Hibon, Laura Pentericci, Marco Castellano, F. Mannucci, Daniel Schaerer, S. Bardelli, V. Le Brun, Andrea Cimatti, R. Thomas, B. Garilli, M. Franco, O. Le Fevre, Adriana Gargiulo, Giovanni Cresci, Fabio Fontanot, Nimish P. Hathi, Brian C. Lemaux, G. Zamorani, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Thomas R., Pentericci L., Le Fevre O., Koekemoer A.M., Castellano M., Cimatti A., Fontanot F., Gargiulo A., Garilli B., Talia M., Amorin R., Bardelli S., Cristiani S., Cresci G., Franco M., Fynbo J.P.U., Hathi N.P., Hibon P., Khusanova Y., Le Brun V., Lemaux B.C., Mannucci F., Schaerer D., Zamorani G., and Zucca E.

Subjects
Physics, 0303 health sciences, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: miscellaneou, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, 03 medical and health sciences, Space and Planetary Science, galaxies: high-redshift, Intergalactic medium, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, intergalactic medium, cosmology: miscellaneous, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 030304 developmental biology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Aim. Our aim is to analyse the variance of the Inter-Galactic Medium transmission (IGM) by studying this parameter in the rest-frame UV spectra of a large sample of high redshift galaxies. Method. We make use of the VIMOS Ultra Deep Survey and the VANDELS public survey to have an insight into the far UV spectrum of $2.7, Comment: Accepted for publication on A&A

Published
2021
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35. The properties of He IIλ1640 emitters at z ∼ 2.5-5 from the VANDELS survey

Author

Nimish P. Hathi, Casey Papovich, M. Mirabelli, Johan P. U. Fynbo, Daniel Schaerer, Marco Castellano, Lucia Pozzetti, Adriano Fontana, G. Zamorani, O. Cucciati, B. Garilli, M. Bolzonella, Lucia Guaita, Ross J. McLure, Angela Bongiorno, Margherita Talia, F. Marchi, Adriana Gargiulo, T. Hutchison, Laura Pentericci, D. J. McLeod, Raffaella Schneider, A. Saxena, Ricardo Amorín, A. C. Carnall, Fergus Cullen, Anton M. Koekemoer, Saxena A., Pentericci L., Mirabelli M., Schaerer D., Schneider R., Cullen F., Amorin R., Bolzonella M., Bongiorno A., Carnall A.C., Castellano M., Cucciati O., Fontana A., Fynbo J.P.U., Garilli B., Gargiulo A., Guaita L., Hathi N.P., Hutchison T.A., Koekemoer A.M., Marchi F., Mcleod D.J., Mclure R.J., Papovich C., Pozzetti L., Talia M., and Zamorani G.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, Stellar population, Metallicity, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Computer Science::Computational Geometry, 01 natural sciences, galaxies: high-redshift, Ionization, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, galaxies: evolution, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Strong He II emission is produced by low-metallicity stellar populations. Here, we aim to identify and study a sample of He II $��1640$-emitting galaxies at redshifts of $z \sim 2.5-5$ in the deep VANDELS spectroscopic survey.. We identified a total of 33 Bright He II emitters (S/N > 2.5) and 17 Faint emitters (S/N < 2.5) in the VANDELS survey and used the available deep multi-wavelength data to study their physical properties. After identifying seven potential AGNs in our sample and discarding them from further analysis, we divided the sample of \emph{Bright} emitters into 20 \emph{Narrow} (FWHM < 1000 km s$^{-1}$) and 6 \emph{Broad} (FWHM > 1000 km s$^{-1}$) He II emitters. We created stacks of Faint, Narrow, and Broad emitters and measured other rest-frame UV lines such as O III] and C III] in both individual galaxies and stacks. We then compared the UV line ratios with the output of stellar population-synthesis models to study the ionising properties of He II emitters. We do not see a significant difference between the stellar masses, star-formation rates, and rest-frame UV magnitudes of galaxies with He II and no He II emission. The stellar population models reproduce the observed UV line ratios from metals in a consistent manner, however they under-predict the total number of \heii ionising photons, confirming earlier studies and suggesting that additional mechanisms capable of producing He II are needed, such as X-ray binaries or stripped stars. The models favour subsolar metallicities ($\sim0.1Z_\odot$) and young stellar ages ($10^6 - 10^7$ years) for the He II emitters. However, the metallicity measured for He II emitters is comparable to that of non-He II emitters at similar redshifts. We argue that galaxies with He II emission may have undergone a recent star-formation event, or may be powered by additional sources of He II ionisation., 21 pages, 11 figures (including appendix), Accepted for publication in A&A

Published
2020
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36. UV and Ly$\alpha$ luminosity functions of galaxies and star formation rate density at the end of HI reionization from the VIMOS UltraDeep Survey (VUDS)

Author

Paolo Cassata, F. Marchi, Marco Castellano, Laurence Tresse, Nimish P. Hathi, O. Cucciati, Janine Pforr, O. Le Fevre, Daniel Schaerer, Anton M. Koekemoer, Mauro Giavalisco, L. A. M. Tasca, Y. Khusanova, Ricardo Amorín, S. Bardelli, Laura Pentericci, R. Thomas, B. Ribeiro, D. Maccagni, Brian C. Lemaux, Daniela Vergani, Letizia P. Cassarà, E. Zucca, G. Zamorani, Andrea Cimatti, V. Le Brun, O. Ilbert, B. Garilli, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Khusanova Y., Le Fevre O., Cassata P., Cucciati O., Lemaux B.C., Tasca L.A.M., Thomas R., Garilli B., Le Brun V., MacCagni D., Pentericci L., Zamorani G., Amorin R., Bardelli S., Castellano M., Cassara L.P., Cimatti A., Giavalisco M., Hathi N.P., Ilbert O., Koekemoer A.M., Marchi F., Pforr J., Ribeiro B., Schaerer D., Tresse L., Vergani D., and Zucca E.

Subjects
galaxies: high-redshift, galaxies: evolution, galaxies: formation, galaxies: star formation, dark ages, reionization, first stars, galaxies: luminosity function, mass function, Population, first stars, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, dark ages, education, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, education.field_of_study, 010308 nuclear & particles physics, Galaxies: luminosity function, mass function, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Dark ages, reionization, first star, galaxies: luminosity function, Space and Planetary Science, mass function, reionization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We establish a robust statistical description of the star-forming galaxy population at the end of cosmic HI reionization ($5.0\le{}z\le6.6$) from a large sample of 52 galaxies with spectroscopically confirmed redshifts from the VIMOS UltraDeep Survey. We identify galaxies with Ly$\alpha$ either in absorption or in emission, at variance with most spectroscopic samples in the literature where Ly$\alpha$ emitters dominate. We find that star-forming galaxies at these redshifts are distributed along a main sequence in the stellar mass vs. SFR plane. We report a flat evolution of the sSFR(z) in 32. The bright end of the Ly$\alpha$ luminosity function has a high number density, indicating a significant star formation activity concentrated in the brightest Ly$\alpha$ emitters (LAE) at these redshifts. LAE with EW>25\AA ~contribute to about 75\% of the total UV-derived SFRD. While our analysis favors a low dust content in 5.0, Comment: 27 pages, submitted to A&A

Published
2020
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37. The VANDELS survey: the role of ISM and galaxy physical properties in the escape of Lyα emission in z ∼ 3.5 star-forming galaxies⋆

Author

A. Saxena, F. Marchi, Stéphane Charlot, Daniel Schaerer, Adriano Fontana, Steve Finkelstein, Nimish P. Hathi, Lucia Pozzetti, Margherita Talia, D. Maccagni, Fergus Cullen, Fabio Fontanot, Ross J. McLure, B. Garilli, Ricardo Amorín, Jacopo Chevallard, Pascale Hibon, Laura Pentericci, Lucia Guaita, Marco Castellano, M. Bolzonella, Anton M. Koekemoer, A. C. Carnall, Casey Papovich, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Universidad Diego Portales [Santiago] (UDP), University of Bologna, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Dipartimento di Fisica [Povo], Università degli Studi di Trento (UNITN), European Southern Observatory (ESO), Space Telescope Science Institute (STSci), Steward Observatory, University of Arizona, INAF - Osservatorio Astronomico di Capodimonte (OAC), Center for Pervasive Communications and Computing, University of California [Irvine] (UCI), University of California-University of California, University of Bologna/Università di Bologna, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), Marchi, F., Pentericci, L., Guaita, L., Talia, M., Castellano, M., Hathi, N., Schaerer, D., Amorin, R., Bolzonella, M., Carnall, A. C., Charlot, S., Chevallard, J., Cullen, F., Finkelstein, S. L., Fontana, A., Fontanot, F., Garilli, B., Hibon, P., Koekemoer, A. M., Maccagni, D., McLure, R. J., Papovich, C., Pozzetti, L., Saxena, A., Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Charlot, Stephane

Subjects
Stellar mass, astro-ph.GA, Extinction (astronomy), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS] Physics [physics], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, 0103 physical sciences, galaxies: formation, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Interstellar medium, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, galaxies: star formation, Spectral energy distribution, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: evolution, Equivalent width, galaxies: ISM
Abstract

We investigate the physical properties of a sample of 52 Ly{\alpha} emitting galaxies in the VANDELS survey, with particular focus on the role of kinematics and neutral hydrogen column density in the escape and spatial distribution of Ly{\alpha} photons. For these galaxies, we derive different physical properties and characterize the Ly{\alpha} emission in terms of kinematics, EW, FWHM and spatial extension and then estimate the velocity of the neutral outflowing gas. We reproduce some of the well known correlations between Ly{\alpha} EW and stellar mass, dust extinction and UV \b{eta} slope, in the sense that the emission line appears brighter in lower mass, less dusty and bluer galaxies. We do not find any correlation with the SED-derived star formation rate, while we find that galaxies with brighter Ly{\alpha} tend to be more compact both in UV and in Ly{\alpha}. Our data reveal a new interesting correlation between the Ly{\alpha} velocity and the offset of the inter-stellar absorption lines with respect to the systemic redshift, in the sense that galaxies with larger inter-stellar medium (ISM) out-flow velocities show smaller Ly{\alpha} velocity shifts. We interpret this relation in the context of the shell-model scenario, where the velocity of the ISM and the HI column density contribute together in determining the Ly{\alpha} kinematics. In support to our interpretation, we observe that galaxies with high HI column densities have much more extended Ly{\alpha} spatial profiles, a sign of increased scattering. However, we do not find any evidence that the HI column density is related to any other physical properties of the galaxies, although this might be due in part to the limited range of parameters that our sample spans., Comment: submitted to A&A

Published
2019
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38. Constraining Lyman-alpha spatial offsets at 3 < z < 5.5 from VANDELS slit spectroscopy

Author

T. Morishita, Lucia Pozzetti, Lucia Guaita, Daniel Schaerer, Ricardo Amorín, Austin Hoag, D. J. McLeod, B. Garilli, Ross J. McLure, Margherita Talia, Johan P. U. Fynbo, Tommaso Treu, Tucker Jones, Laura Pentericci, Marusa Bradac, Nimish P. Hathi, Fergus Cullen, Marco Castellano, M. Bolzonella, Kasper B. Schmidt, R. Thomas, Alaina Henry, Charlotte Mason, Hoag, A, Treu, T, Pentericci, L, Amorin, R, Bolzonella, M, Bradač, M, Castellano, M, Cullen, F, Fynbo, J P U, Garilli, B, Guaita, L, Hathi, N, Henry, A, Jones, T, Mason, C, McLeod, D, McLure, R, Morishita, T, Pozzetti, L, Schaerer, D, Schmidt, K B, Talia, M, and Thomas, R

Subjects
Physics, Opacity, 010308 nuclear & particles physics, Spatially resolved, astro-ph.GA, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, galaxies: high-redshift, Intergalactic medium, 0103 physical sciences, Chandra Deep Field South, Spectroscopy, 010303 astronomy & astrophysics, Reionization, Astronomical and Space Sciences, high-redshift [galaxies]
Abstract

We constrain the distribution of spatially offset Lyman-alpha emission (Ly$\alpha$) relative to rest-frame ultraviolet emission in $\sim300$ high redshift ($36$. Spatially resolved observations of Ly$\alpha$ and UV continuum at $6, Comment: Submitted to MNRAS

Published
2019
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39. The VANDELS survey: The relation between the UV continuum slope and stellar metallicity in star-forming galaxies at z ∼ 3

Author

M. Bolzonella, Fabio Fontanot, Nimish P. Hathi, Andrea Cimatti, P. Santini, Adriano Fontana, F. Mannucci, Laura Pentericci, G. Zamorani, Giovanni Cresci, Marco Castellano, A. Calabrò, A. Saxena, F. Marchi, M. Franco, Daniel Schaerer, Nicola Menci, Ricardo Amorín, Lizhi Xie, G. De Lucia, Johan P. U. Fynbo, Pascale Hibon, Margherita Talia, Ross J. McLure, Michaela Hirschmann, Fergus Cullen, Calabro A., Castellano M., Pentericci L., Fontanot F., Menci N., Cullen F., Mclure R., Bolzonella M., Cimatti A., Marchi F., Talia M., Amorin R., Cresci G., De Lucia G., Fynbo J., Fontana A., Franco M., Hathi N.P., Hibon P., Hirschmann M., Mannucci F., Santini P., Saxena A., Schaerer D., Xie L., and Zamorani G.

Subjects
Metallicity, Continuum (design consultancy), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), 01 natural sciences, abundances [galaxies], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, SPECTRAL-SYNTHESIS, FIELD, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, HIERARCHICAL FORMATION, 010308 nuclear & particles physics, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, GALACTIC STELLAR, stellar content [galaxies], Galaxies: stellar content, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Galaxy, TO 2, CHEMICAL ENRICHMENT, LYMAN-BREAK GALAXIES, ULTRAVIOLET LUMINOSITY DENSITY, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), DUST OBSCURATION, Astrophysics::Earth and Planetary Astrophysics, high-redshift [galaxies], Galaxies: abundance
Abstract

The estimate of stellar metallicities (Z*) of high-z galaxies are of paramount importance in order to understand the complexity of dust effects and the reciprocal interrelations among stellar mass, dust attenuation, stellar age, and metallicity. Benefiting from uniquely deep FUV spectra of >500 star-forming galaxies at redshifts 2, Comment: 25 pages, 4 tables, 16 figures, and 5 Appendix subsections; accepted for publication in A&A

Published
2021
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40. The VANDELS survey: Discovery of massive overdensities of galaxies at z > 2

Author

L. Guaita, M. Bolzonella, Anton M. Koekemoer, Lizhi Xie, O. Cucciati, P. Hibon, Laura Pentericci, Nimish P. Hathi, Ricardo Amorín, Emanuela Pompei, Lucia Pozzetti, R. C. Thomas, G. De Lucia, Adriana Gargiulo, G. Zamorani, F. Fontanot, M. Hirschmann, Anna Zoldan, M. Castellano, Margherita Talia, Franz E. Bauer, Ross J. McLure, Guaita L., Pompei E., Castellano M., Pentericci L., Cucciati O., Zamorani G., Zoldan A., Fontanot F., Bauer F.E., Amorin R., Bolzonella M., De Lucia G., Gargiulo A., Hathi N.P., Hibon P., Hirschmann M., Koekemoer A.M., McLure R., Pozzetti L., Talia M., Thomas R., and Xie L.

Subjects
Physics, Field (physics), 010308 nuclear & particles physics, Galaxies: high-redshift, Galaxies: kinematics and dynamics, Astronomy and Astrophysics, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, Stars, Gravitational potential, Galaxies: interaction, Space and Planetary Science, 0103 physical sciences, Cluster (physics), Outflow, Galaxies: clusters: general, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Context. The advent of deep, multi-wavelength surveys, together with the availability of extensive numerical simulations, now allow us for the systematic search and study of (proto)clusters and their surrounding environment as a function of redshift. Aims. We aim to define the environment and to identify overdensities in the VANDELS Chandra Deep Field-South (CDFS) and UKIDSS Ultra Deep Survey (UDS) fields. We want to investigate whether we can use Lyα emission to obtain additional information of the environment properties and whether Lyα emitters show different characteristics as a function of their environment. Methods. We estimated local densities using a three-dimensional algorithm which works in the RA-dec-redshift space. We took advantage of the physical parameters of all the sources in the VANDELS fields to study their properties as a function of environment. In particular, we focused on the rest-frame U − V color to evaluate the stage of evolution of the galaxies located in the overdensities and in the field. Then we selected a sample of 131 Lyα-emitting galaxies (EW(Lyα) > 0 Å), unbiased with respect to environmental density, from the first two seasons of the VANDELS survey to study their location with respect to the over- or under-dense environment and infer whether they are useful tracers of overdense regions. Results. We identify 13 (proto)cluster candidates in the CDFS and nine in the UDS at 2 < z < 4, based on photometric and spectroscopic redshifts from VANDELS and from all the available literature. No significant difference is observed in the rest-frame U − V color between field and galaxies located within the identified overdensities, but the star-forming galaxies in overdense regions tend to be more massive and to have low specific SFRs than in the field. We study the distribution of the VANDELS Lyα emitters (LAEVs) and we find that Lyα emitters lie preferentially outside of overdense regions as the majority of the galaxies with spectroscopic redshifts from VANDELS. The LAEVs in overdense regions tend to have low Lyα equivalent widths and low specific SFRs, and they also tend to be more massive than the LAEVs in the field. Their stacked Lyα profile shows a dominant red peak and a hint of a blue peak. There is evidence that their Lyα emission is more extended and offset with respect to the UV continuum. Conclusions. LAEVs are likely to be influenced by the environment. In fact, our results favour a scenario that implies outflows of low expansion velocities and high HI column densities for galaxies in overdense regions. An outflow with low expansion velocity could be related to the way galaxies are forming stars in overdense regions; the high HI column density can be a consequence of the gravitational potential of the overdensity. Therefore, Lyα-emitting galaxies can provide useful insights on the environment in which they reside.

Published
2020
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41. The Intergalactic medium transmission towards z>4 galaxies with VANDELS and the impact of dust attenuation

Author

Nimish P. Hathi, D. J. McLeod, Steve Finkelstein, G. Zamorani, M. Bolzonella, Johan P. U. Fynbo, Y. Khusanova, Lucia Guaita, A. Saxena, R. Thomas, Margherita Talia, A. C. Carnall, Pascale Hibon, F. Marchi, O. Le Fèvre, Stefano Cristiani, Marco Castellano, Fabio Fontanot, L. Pentericci, Ricardo Amorín, Lucia Pozzetti, Anton M. Koekemoer, Fergus Cullen, Ross J. McLure, Daniel Schaerer, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Thomas, R, Pentericci, L, Le Fevre, O, Zamorani, G, Schaerer, D, Amorin, R, Castellano, M, Carnall, AC, Cristiani, S, Cullen, F, Finkelstein, SL, Fontanot, F, Guaita, L, Hibon, P, Hathi, N, Fynbo, JPU, Khusanova, Y, Koekemoer, AM, McLeod, D, McLure, RJ, Marchi, F, Pozzetti, L, Saxena, A, Talia, M, and Bolzonella, M

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Extinction (astronomy), Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, high-redshift, Photometry (optics), galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Line-of-sight, 010308 nuclear & particles physics, galaxie, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, galaxies: general, Redshift, Galaxy, general, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Spectral energy distribution, intergalactic medium, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Aims. Our aim is to estimate the intergalactic medium transmission towards UV-selected star-forming galaxies at redshift 4 and above and study the effect of the dust attenuation on these measurements. Methods. The ultra-violet spectrum of high redshift galaxies is a combination of their intrinsic emission and the effect of the Inter-Galactic medium (IGM) absorption along their line of sight. Using data coming from the unprecedented deep spectroscopy from the VANDELS ESO public survey carried out with the VIMOS instrument we compute both the dust extinction and the mean transmission of the IGM as well as its scatter from a set of 281 galaxies at z>3.87. Because of a degeneracy between the dust content of the galaxy and the IGM, we first estimate the stellar dust extinction parameter E(B-V) and study the result as a function of the dust prescription. Using these measurements as constraint for the spectral fit we estimate the IGM transmission Tr(Lyalpha). Both photometric and spectroscopic SED fitting are done using the SPectroscopy And photometRy fiTting tool for Astronomical aNalysis (SPARTAN) that is able to fit the spectral continuum of the galaxies as well as photometric data. Results. Using the classical Calzetti's attenuation law we find that E(B-V) goes from 0.11 at z=3.99 to 0.08 at z=5.15. These results are in very good agreement with previous measurements from the literature. We estimate the IGM transmission and find that the transmission is decreasing with increasing redshift from Tr(Lyalpha)=0.53 at z=3.99 to 0.28 at z=5.15. We also find a large standard deviation around the average transmission that is more than 0.1 at every redshift. Our results are in very good agreement with both previous measurements from AGN studies and with theoretical models., Accepted for publication in A&A

Published
2019
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42. The VANDELS ESO public spectroscopic survey

Author

H. Mendez-Hernandez, Matt J. Jarvis, Mark Dickinson, D. Maccagni, Lucia Pozzetti, Ricardo Amorín, Christina C. Williams, B. Garilli, Eros Vanzella, David T. Maltby, A. Iovino, Omar Almaini, Marco Castellano, Antonis Georgakakis, Italo Balestra, Daniel Schaerer, M. Mignoli, Y. Khusanova, D. P. Rosario, Steve Finkelstein, P. Popesso, Andrea Grazian, Marcella Brusa, Anton M. Koekemoer, Maurilio Pannella, S. Juneau, Ross J. McLure, Michele Cirasuolo, Vivienne Wild, P. Santini, Nimish P. Hathi, K. Matsuoka, Seock-Sam Kim, Giovanni Cresci, Kirpal Nandra, Jairo Méndez-Abreu, Fabio Fontanot, F. Mannucci, A. C. Carnall, Laura Pentericci, Eric F. Bell, P. Franzetti, Fernando Buitrago, Michele Moresco, D. J. McLeod, Andrea Cimatti, Adriana Gargiulo, James Dunlop, E. Curtis-Lake, Rebecca A. A. Bowler, S. de Barros, Fabrizio Fiore, M. Bolzonella, D. Elbaz, Johan P. U. Fynbo, Giovanni G. Fazio, Margherita Talia, V. Sommariva, Marco Scodeggio, Stefano Cristiani, Jennifer M. Lotz, S. Bardelli, Mario Nonino, M. Giavalisco, Corentin Schreiber, Mara Salvato, Henry C. Ferguson, Audrey Galametz, E. Zucca, O. Le Fevre, Angela Bongiorno, M. Fumana, L. A. M. Tasca, Daniel P. Stark, Nathan Bourne, F. Marchi, M. Franco, W. G. Hartley, Stéphane Charlot, Adriano Fontana, Paolo Cassata, E. Mármol-Queraltó, W. Karman, Karina Caputi, Tommaso Treu, R. Thomas, Casey Papovich, Emanuela Pompei, O. Cucciati, Alice Mortlock, Annalisa Citro, Fergus Cullen, Intae Jung, G. Zamorani, Lucia Guaita, Astronomy, McLure, R. J., Pentericci, L., Cimatti, A., Dunlop, J. S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S. L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W. G., Iovino, A., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Mármol-Queraltó, E., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astronomico di Bologna (OABO), Department of Surgery, Santi Giovanni e Paolo Hospital, Association de Coordination Technique Agricole (ACTA), Space Telescope Science Institute (STSci), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Department of Agronomy, Food, Natural Resources, Animals and the Environment (DAFNAE), Universita degli Studi di Padova, Institute for General Botany, Johannes Gutenberg - Universität Mainz (JGU), Les instituts techniques agricoles (Acta), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository

Subjects
Active galactic nucleus, Stellar population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Survey, 010303 astronomy & astrophysics, Galaxies: high, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Galaxies: evolution, Galaxies: star formation, Surveys, Chandra Deep Field South, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract

VANDELS is a uniquely-deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO's Very Large Telescope (VLT). The survey has obtained ultra-deep optical (0.48 < lambda < 1.0 micron) spectroscopy of ~2100 galaxies within the redshift interval 1.0 < z < 7.0, over a total area of ~0.2 sq. degrees centred on the CANDELS UDS and CDFS fields. Based on accurate photometric redshift pre-selection, 85% of the galaxies targeted by VANDELS were selected to be at z>=3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < t_int < 80 hours), the VANDELS survey targeted: a) bright star-forming galaxies at 2.4 < z < 5.5, b) massive quiescent galaxies at 1.0 < z < 2.5, c) fainter star-forming galaxies at 3.0 < z < 7.0 and d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multi-wavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design and target selection., 19 pages, 9 figures, accepted for publication in MNRAS

Published
2018
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43. The VANDELS ESO public spectroscopic survey: observations and first data release

Author

O. Cucciati, Andrea Grazian, E. Zucca, Y. Khusanova, Emma Curtis-Lake, A. Iovino, Stéphane Charlot, R. J. McLure B. Garilli, James Dunlop, Adriana Gargiulo, Johan P. U. Fynbo, Alice Mortlock, Mara Salvato, E. Mármol-Queraltó, Nimish P. Hathi, Seock-Sam Kim, L. A. M. Tasca, Fabrizio Fiore, Italo Balestra, Kirpal Nandra, A. Georgakakis, Emanuela Pompei, D. Elbaz, Anton M. Koekemoer, S. L. Finkelstein, F. Marchi, M. Franco, Maurilio Pannella, Tommaso Treu, Audrey Galametz, Corentin Schreiber, H. Mendez-Hernandez, Andrea Cimatti, P. Popesso, M. Fumana, Giovanni G. Fazio, S. Cristiani, Angela Bongiorno, David J. Rosario, Laura Pentericci, Marco Castellano, Piero Rosati, Vivienne Wild, Giovanni Cresci, A. C. Carnall, C. Caputi, M. Giavalisco, Paolo Cassata, Lucia Pozzetti, Marcella Brusa, M. Bolzonella, R. C. Thomas, Margherita Talia, D. Maccagni, S. Bardelli, W. Karman, S. DeBarros, K. Matsuoka, H. C. Ferguson, Jennifer M. Lotz, F. Fontanot, Adriano Fontana, C. Papovich, W. G. Hartley, Michele Moresco, Eros Vanzella, David T. Maltby, Omar Almaini, S. Juneau, Rebecca A. A. Bowler, Daniel Schaerer, Daniel P. Stark, Nathan Bourne, S. M. Faber, D. J. McLeod, Ricardo Amorín, Michele Cirasuolo, P. Franzetti, Fernando Buitrago, O. Le Fevre, Annalisa Citro, Mario Nonino, Fergus Cullen, Intae Jung, G. Zamorani, Eric F. Bell, Lucia Guaita, Christina C. Williams, V. Sommariva, Marco Scodeggio, M. Mignoli, Matt J. Jarvis, Mark Dickinson, P. Santini, Jairo Méndez-Abreu, F. Mannucci, ITA, USA, GBR, FRA, DEU, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Milano (OAM), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Brera (OAB), Università di Bologna, Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), INAF - Osservatorio Astronomico di Bologna (OAB), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), CNR-INFM CRS-Soft, c/o Dipartimento di Fisica, CNR-INFM CRS-Soft, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), INAF-IASF Milano, European Southern Observatory (ESO), University of Bologna, INAF - Osservatorio Astronomico di Trieste (OAT), Dipartimento di Fisica e Astronomia [Bologna], University of Groningen [Groningen], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Osservatorio Astronomico (INAF), NOAO, Max-Planck-Institut für Extraterrestrische Physik (MPE), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Space Telescope Science Institute (STSci), Department of computer science, Kyushu Institute of Technology, University of Texas-Pan American (UTPA), University of Texas-Pan, Excellence Cluster Universe, Technische Universität München [München] (TUM), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), National Optical Astronomy Observatory (NOAO), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Bologna/Università di Bologna, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Kyushu Institute of Technology (Kyutech), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Pentericci, L., McLure, R. J., Garilli, B., Cucciati, O., Franzetti, P., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., De Barros, S., Dunlop, J. S., Elbaz, D., Finkelstein, S. L., Fontana, A., Fontanot, F., Fumana, M., Gargiulo, A., Guaita, L., Hartley, W. G., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Marmol-Queralto, E., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository

Subjects
media_common.quotation_subject, REDSHIFT, Galaxies: fundamental parameter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, fundamental parameters [galaxies], QB Astronomy, Survey, Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: general, Galaxies: high-redshift, Surveys, Astronomy and Astrophysics, Space and Planetary Science, 010303 astronomy & astrophysics, Spectrograph, evolution [galaxies], QC, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, media_common, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, galaxies: fundamental parameters, 3rd-DAS, Astronomy and Astrophysic, galaxies: general, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Universe, Data set, GALAXIES, QC Physics, Sky, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), VIMOS, galaxies: evolution, high-redshift [galaxies], Data reduction, general [galaxies]
Abstract

This paper describes the observations and the first data release (DR1) of the ESO public spectroscopic survey "VANDELS, a deep VIMOS survey of the CANDELS CDFS and UDS fields". VANDELS' main targets are star-forming galaxies at 2.4, Comment: Submitted to A&A

Published
2018
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44. The progeny of a Cosmic Titan: a massive multi-component proto-supercluster in formation at $z=2.45$ in VUDS

Author

Letizia P. Cassarà, V. Le Brun, Paolo Cassata, Eros Vanzella, Mara Salvato, Daniela Vergani, O. Le Fèvre, Nimish P. Hathi, L. Pentericci, E. Zucca, Anton M. Koekemoer, L. M. Lubin, D. Maccagni, Janine Pforr, Ricardo Amorín, Lidia Tasca, Bianca Garilli, Andrea Cimatti, Olga Cucciati, K. G. Lee, Brian C. Lemaux, S. Bardelli, Margherita Talia, G. Zamorani, R. C. Thomas, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Cucciati, O., Lemaux, B.C., Zamorani, G., Le Fèvre, O., Tasca, L.A.M., Hathi, N.P., Lee, K.-G., Bardelli, S., Cassata, P., Garilli, B., Le Brun, V., Maccagni, D., Pentericci, L., Thomas, R., Vanzella, E., Zucca, E., Lubin, L.M., Amorin, R., Cassarà, L.P., Cimatti, A., Talia, M., Vergani, D., Koekemoer, A., Pforr, J., Salvato, M., and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cosmology: observation, 01 natural sciences, Supercluster, galaxies: high-redshift, 0103 physical sciences, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Line-of-sight, 010308 nuclear & particles physics, Velocity dispersion, Astronomy and Astrophysics, Virial mass, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmology: observations, Galaxies: clusters: general, Galaxies: high-redshift, Large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Abridged] We unveil the complex shape of a proto-supercluster at z~2.45 in the COSMOS field using the spectroscopic redshifts of the VIMOS Ultra-Deep Survey (VUDS), complemented by the zCOSMOS-Deep sample and high-quality photometric redshifts. The method relies on a 2D Voronoi tessellation in overlapping redshift slices that is converted into a 3D density field. The galaxy distribution is constructed using a statistical treatment of spectroscopic and photometric redshifts. We identify a proto-supercluster, dubbed "Hyperion" for its immense size and mass, which extends over a volume of ~60x60x150 comoving Mpc^3 and has an estimated total mass of ~4.8x 10^15 M_sun. This immensely complex structure contains at least 7 density peaks within 2.4 < z < 2.5, connected by filaments. Based on the peaks average matter density, we estimate their total mass, M_tot, and find a range of masses from ~0.1x10^14 M_sun to ~2.7x10^14 M_sun. By using spectroscopic members of each peak, we obtain the velocity dispersion of the galaxies in the peaks, and then their virial mass M_vir (under the strong assumption that they are virialised). The agreement between M_vir and M_tot is surprisingly good, considering that almost all the peaks are probably not yet virialised. According to the spherical collapse model, the peaks have already started or are about to start collapsing, and they are all predicted to be virialised by redshift z~0.8-1.6. We finally perform a careful comparison with the literature, given that smaller components of this proto-supercluster had previously been identified using heterogeneous galaxy samples. With VUDS, we obtain a panoramic view of this large structure, that encompasses, connects, and considerably expands in a homogeneous way on all previous detections of the various sub-components. This provides us the unique possibility to study a rich supercluster in formation., 22 pages, 13 figures, accepted to be published in A&A, very minor corrections after language editing

Published
2018
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45. The VIMOS Ultra Deep Survey: Nature, ISM properties, and ionizing spectra of CIII]λ1909 emitters at z = 2-4

Author

Laura Pentericci, G. Zamorani, Eros Vanzella, Lucia Guaita, Brian C. Lemaux, S. Bardelli, L. A. M. Tasca, O. Le Fevre, Andrea Grazian, E. Zucca, Kimihiko Nakajima, Margherita Talia, Nimish P. Hathi, Ricardo Amorín, Daniel Schaerer, Nakajima K., Schaerer D., Le Fevre O., Amorin R., Talia M., Lemaux B.C., Tasca L.A.M., Vanzella E., Zamorani G., Bardelli S., Grazian A., Guaita L., Hathi N.P., Pentericci L., Zucca E., European Southern Observatory (ESO), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), University of California [Davis] (UC Davis), University of California, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), INAF - Osservatorio Astronomico di Brera (OAB), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and University of California (UC)

Subjects
Active galactic nucleus, Stellar population, Metallicity, FOS: Physical sciences, Photoionization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Interstellar medium, Galaxies: ISM, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies: abundance
Abstract

Context: Ultraviolet (UV) emission-line spectra are used to spectroscopically confirm high-z galaxies and increasingly also to determine their physical properties. Aims: To interpret the observed UV spectra of distant galaxies in terms of the dominant radiation field and the physical condition of the interstellar medium. Methods: We construct a large grid of photoionization models and derive new spectral UV line diagnostics using equivalent widths (EWs) of CIII]1909, CIV1549 and the line ratios of CIII], CIV, and HeII1640 recombination lines. We apply these diagnostics to a sample of 450 CIII]-emitting galaxies at z=2-4 previously identified in the VIMOS Ultra Deep Survey. Results: We show that the average star-forming galaxy (EW(CIII])~2A) is well described by stellar photoionization from single and binary stars. The inferred metallicity and ionization parameter is typically Z=0.3-0.5Zsun and logU=-2.7 to -3, in agreement with earlier works at similar redshifts. The models also indicate an average age of 50-200Myr since the beginning of the current star-formation, and an ionizing photon production rate, xi_ion, of log(xi_ion/[Hz/erg])~25.3-25.4. Among the sources with EW(CIII])=10-20A, ~30% are likely dominated by AGNs. Their derived metallicity is low, Z=0.02-0.2Zsun, and the ionization parameter higher (logU=-1.7). To explain the average UV observations of the strongest but rarest CIII] emitters (EW(CIII])>20A), we find that stellar photoionization is clearly insufficient. A radiation field consisting of a mix of a young stellar population (log(xi_ion/[Hz/erg])~25.7) plus an AGN component is required. Furthermore an enhanced C/O abundance ratio is needed for metallicities Z=0.1-0.2Zsun and logU=-1.7 to -1.5. Conclusions: The UV diagnostics we propose should serve as an important basis for the interpretation of observations of high-redshift galaxies. [abridged], 27 pages, 18 figures. Accepted for publication in A&A

Published
2018
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46. The VIMOS Ultra-Deep Survey: evidence for AGN feedback in galaxies with CIII]-λ1908 Å emission 10.8 to 12.5 Gyr ago

Author

Nimish P. Hathi, G. Zamorani, Lucia Guaita, E. Zucca, O. Le Fevre, Kimihiko Nakajima, P. Cassata, B. Garilli, James Dunlop, L. A. M. Tasca, S. Bardelli, Daniel Schaerer, Eros Vanzella, F. Marchi, Andrea Cimatti, Margherita Talia, Laura Pentericci, D. Maccagni, Ricardo Amorín, Brian C. Lemaux, Mauro Giavalisco, Daniela Vergani, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Institut de recherche et d'enseignement sur la négociation (IRENE), ESSEC Business School, INAF - Osservatorio Astronomico di Bologna (OABO), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Essec Business School, Le Fevre O., Lemaux B.C., Nakajima K., Schaerer D., Talia M., Zamorani G., Cassata P., Garilli B., MacCagni D., Pentericci L., Tasca L.A.M., Zucca E., Amorin R., Bardelli S., Cimatti A., Giavalisco M., Guaita L., Hathi N.P., Marchi F., Vanzella E., Vergani D., and Dunlop J.

Subjects
Galaxy: evolution, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Population, Galaxies: Formation, Galaxies: High-redshift, Galaxies: Star formation, Galaxy: Evolution, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Redshift, Spectral line, galaxies: high-redshift, Space and Planetary Science, galaxies: star formation, 0103 physical sciences, Galaxy formation and evolution, galaxies: formation, Emission spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], education, 010303 astronomy & astrophysics, Line (formation)
Abstract

We analyze the CIII]-1908\AA emission properties in a sample of 3899 star-forming galaxies (SFGs) at 23\AA, including 20% with 310\AA. A significant fraction of 1.2% of SFGs presents strong CIII] emission 2010^10 MSun at z~3 into the population of quiescent galaxies observed at redshift z~1-2., Comment: 19 pages, 14 figures, submitted to A&A

Published
2019
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47. The VIMOS Ultra Deep Survey First Data Release: spectra and spectroscopic redshifts of 698 objects up to z~6 in CANDELS

Author

C. Moreau, A. Durkalec, S. Paltani, Mara Salvato, M. Castellano, Nimish P. Hathi, E. Vanzella, Adriano Fontana, B. Garilli, S. Bardelli, G. Zamorani, James Dunlop, B. Ribeiro, Yoshiaki Taniguchi, Peter Capak, O. Cucciati, A. Grazian, Marco Scodeggio, Paolo Cassata, P. W. Wang, Ricardo Amorín, V. Sommariva, S. de la Torre, L. Guaita, Yannick Mellier, Laura Pentericci, Anton M. Koekemoer, Margherita Talia, Letizia P. Cassarà, L. Tresse, Rajat M. Thomas, C. Lopez-Sanjuan, Stéphane Charlot, V. Le Brun, O. Ilbert, Nick Scoville, D. Maccagni, M. Giavalisco, E. Zucca, Daniel Schaerer, Janine Pforr, Sotiria Fotopoulou, L. A. M. Tasca, O. Le Fevre, T. Contini, Brian Lemaux, D. Vergani, A. Cimatti, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Tasca, L.A.M., Le Fèvre, O., Ribeiro, B., Thomas, R., Moreau, C., Cassata, P., Garilli, B., Le Brun, V., Lemaux, B.C., Maccagni, D., Pentericci, L., Schaerer, D., Vanzella, E., Zamorani, G., Zucca, E., Amorin, R., Bardelli, S., Cassarà, L.P., Castellano, M., Cimatti, A., Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Paltani, S., Pforr, J., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vergani, D., Capak, P., Charlot, S., Contini, T., De La Torre, S., Dunlop, J., Fotopoulou, S., Guaita, L., Koekemoer, A., López-Sanjuan, C., Mellier, Y., Salvato, M., Scoville, N., Taniguchi, Y., and Wang, P.W.

Subjects
Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Surveys, 01 natural sciences, Cosmology: observation, Spectral line, Galaxies: distances and redshifts, 0103 physical sciences, Galaxies: distances and redshift, [INFO]Computer Science [cs], education, Survey, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Cosmology: observations, Galaxies: high-redshift, Catalogs, Astronomy and Astrophysics, Space and Planetary Science, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Stars, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Catalog, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

This paper describes the first data release (DR1) of the VIMOS Ultra Deep Survey (VUDS). The DR1 includes all low-resolution spectroscopic data obtained in 276.9 arcmin2 of the CANDELS-COSMOS and CANDELS-ECFDS survey areas, including accurate spectroscopic redshifts z_spec and individual spectra obtained with VIMOS on the ESO-VLT. A total of 698 objects have a measured redshift, with 677 galaxies, two type-I AGN and a small number of 19 contaminating stars. The targets of the spectroscopic survey are selected primarily on the basis of their photometric redshifts to ensure a broad population coverage. About 500 galaxies have z_spec>2, 48 with z_spec>4, and the highest reliable redshifts reach beyond z_spec=6. This dataset approximately doubles the number of galaxies with spectroscopic redshifts at z>3 in these fields. We discuss the general properties of the sample in terms of the spectroscopic redshift distribution, the distribution of Lyman-alpha equivalent widths, and physical properties including stellar masses M_star and star formation rates (SFR) derived from spectral energy distribution fitting with the knowledge of z_spec. We highlight the properties of the most massive star-forming galaxies, noting the large range in spectral properties, with Lyman-alpha in emission or in absorption, and in imaging properties with compact, multi-component or pair morphologies. We present the catalogue database and data products. All data are publicly available and can be retrieved from a dedicated query-based database available at http://cesam.lam.fr/vuds., 11 pages, 6 figures, submitted to A&A

Published
2017
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48. The VIMOS Ultra Deep Survey: The role of HI kinematics and HI column density on the escape of Lya photons in star-forming galaxies at 2 < z < 4

Author

Anton M. Koekemoer, Ricardo Amorín, Ivana Orlitova, Marco Castellano, R. Thomas, Andrea Grazian, S. Bardelli, Daniel Schaerer, L. A. M. Tasca, E. Zucca, B. Ribeiro, Brian C. Lemaux, F. Marchi, Nimish P. Hathi, Anne Verhamme, Paolo Cassata, Margherita Talia, D. Maccagni, O. Le Fevre, Laura Pentericci, Le Brun, B. Garilli, Eros Vanzella, G. Zamorani, Lucia Guaita, Guaita, L., Talia, M., Pentericci, L., Verhamme, A., Cassata, P., Lemaux, B.C., Orlitova, I., Ribeiro, B., Schaerer, D., Zamorani, G., Garilli, B., Le Brun, V., Le Fèvre, O., MacCagni, D., Tasca, L.A.M., Thomas, R., Vanzella, E., Zucca, E., Amorin, R., Bardelli, S., Castellano, M., Grazian, A., Hathi, N.P., Koekemoer, A., Marchi, F., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository

Subjects
Physics, ISM: kinematics and dynamics, Data products, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: star formation, 010308 nuclear & particles physics, European research, Galaxies: high-redshift, Astronomy and Astrophysics, Astrophysics, Astronomy and Astrophysic, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Scattering, Space and Planetary Science, ISM: kinematics and dynamic, 0103 physical sciences, Techniques: imaging spectroscopy, 010303 astronomy & astrophysics
Abstract

We selected a sample of 76 Lya emitting galaxies from the VIMOS Ultra Deep Survey (VUDS) at 2300km/sec. An ISM with this value of NHI would favour a large amount of scattering events, especially when the medium is static, so it can explain large values of Ext(Lya-C) and small EW(Lya). On the contrary, an ISM with a lower NHI, but large velocity outflows would lead to a Lya spatial profile peaked at the galaxy center (i.e. low values of Ext(Lya-C)) and to a large EW(Lya), as we see in our data. Our results and their interpretation via radiative-transfer models tell us that it is possible to use Lya to study the properties of the HI gas., Comment: Accepted on May 2017

Published
2017
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49. VIMOS Ultra-Deep Survey (VUDS): IGM transmission towards galaxies with $2.5 < z < 5.5$ and the colour selection of high-redshift galaxies

Author

Daniela Vergani, Yannick Mellier, C. Lopez-Sanjuan, Nick Scoville, Paolo Cassata, Rajat M. Thomas, Laurence Tresse, S. Paltani, B. Ribeiro, Ricardo Amorín, Letizia P. Cassarà, Andrea Cimatti, Brian C. Lemaux, Bianca Garilli, Andrea Grazian, Stéphane Charlot, Margherita Talia, Laura Pentericci, D. Maccagni, Adriano Fontana, Nimish P. Hathi, G. Zamorani, V. Le Brun, Lidia Tasca, O. Ilbert, Peter Capak, A. Durkalec, Thierry Contini, E. Zucca, S. Bardelli, Daniel Schaerer, Anton M. Koekemoer, Marco Castellano, James Dunlop, Mauro Giavalisco, V. Sommariva, Marco Scodeggio, P. W. Wang, Jean-Gabriel Cuby, Mara Salvato, Yoshiaki Taniguchi, Eros Vanzella, O. Cucciati, S. de la Torre, Sotiria Fotopoulou, Janine Pforr, O. Le Fevre, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Thomas, R., Le Fèvre, O., Le Brun, V., Cassata, P., Garilli, B., Lemaux, B.C., Maccagni, D., Pentericci, L., Tasca, L.A.M., Zamorani, G., Zucca, E., Amorin, R., Bardelli, S., Cassarà, L., Castellano, M., Cimatti, A., Cucciati, O., Durkalec, A., Fontana, A., Giavalisco, M., Grazian, A., Hathi, N.P., Ilbert, O., Paltani, S., Pforr, J., Ribeiro, B., Schaerer, D., Scodeggio, M., Sommariva, V., Talia, M., Tresse, L., Vanzella, E., Vergani, D., Capak, P., Charlot, S., Contini, T., Cuby, J.G., De La Torre, S., Dunlop, J., Fotopoulou, S., Koekemoer, A., López-Sanjuan, C., Mellier, Y., Salvato, M., Scoville, N., Taniguchi, Y., Wang, P.W., Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
QSOS, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Extinction (astronomy), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Cosmology: observation, Spectral line, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Galaxy: evolution, Line-of-sight, 010308 nuclear & particles physics, Astronomy and Astrophysics, Cosmic variance, Astronomy and Astrophysic, Redshift, Galaxy, Cosmology: observations, Galaxies: high-redshift, Galaxy: formation, Large-scale structure of Universe, Space and Planetary Science, cosmology: observations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(arXiv abridged abstract) The observed UV rest-frame spectra of distant galaxies are the result of their intrinsic emission combined with absorption along the line of sight produced by the inter-galactic medium (IGM). Here we analyse the evolution of the mean IGM transmission Tr(Ly_alpha) and its dispersion along the line of sight for 2127 galaxies with 2.5= 4 compared to results from QSOs, but a degeneracy between dust extinction and IGM prevents to draw firm conclusions if the internal dust extinction for star-forming galaxies at z>4 takes a mean value significantly in excess of E(B-V)>0.15. Most importantly, we find a large dispersion of IGM transmission along the lines of sight towards distant galaxies with 68% of the distribution within 10 to 17% of the median value in delta z=0.5 bins, similar to what is found on the LOS towards QSOs. We demonstrate the importance of taking into account this large range of IGM transmission when selecting high redshift galaxies based on their colour properties (e.g. LBG or photometric redshift selection) or otherwise face a significant incompleteness in selecting high redshift galaxy populations., Comment: 15 pages, 11 figures, submitted to A&A

Published
2017
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50. Characterizing elusive, faint dusty star-forming galaxies: a lensed, optically undetected ALMA galaxy at z ~ 3.3

Author

S. Berta, Emanuele Daddi, Roberto Maiolino, Manuela Magliocchetti, Ricardo Amorín, Michał J. Michałowski, Andrea Grazian, Giulia Rodighiero, Rosa Valiante, Paola Santini, David Elbaz, S. Pilo, Charlotte Mason, Nathan Bourne, L. Pentericci, Marco Castellano, Francesco Calura, E. Merlin, Francesca Pozzi, Adriano Fontana, A. Mignano, Corentin Schreiber, ITA, USA, GBR, FRA, NLD, Santini, P., Castellano, M., Fontana, A., Merlin, E., Maiolino, R., Mason, C., Mignano, A., Pilo, S., Amorin, R., Berta, S., Bourne, N., Calura, F., Daddi, E., Elbaz, D., Grazian, A., Magliocchetti, M., Michałowski, M.J., Pentericci, L., Pozzi, F., Rodighiero, G., Schreiber, C., Valiante, R., Maiolino, Roberto [0000-0002-4985-3819], Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository

Subjects
Galaxies: fundamental parameters, Stellar mass, Population, Galaxies: fundamental parameter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cosmology: observation, 01 natural sciences, Submillimeter: galaxie, 0103 physical sciences, Galaxy formation and evolution, 10. No inequality, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Cosmology: observations, Galaxies: high-redshift, Astrophysics::Instrumentation and Methods for Astrophysics, Galaxies: evolution, Astronomy and Astrophysics, Galaxies: photometry, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Submillimeter: galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution
Abstract

We present the serendipitous ALMA detection of a faint submillimeter galaxy (SMG) lensed by a foreground z~1 galaxy. By optimizing the source detection to deblend the system, we accurately build the full spectral energy distribution of the distant galaxy from the I814 band to radio wavelengths. It is extremely red, with a I-K colour larger than 2.5. We estimate a photometric redshift of 3.28 and determine the physical parameters. The distant galaxy turns out to be magnified by the foreground lens by a factor of ~1.5, which implies an intrinsic Ks-band magnitude of ~24.5, a submillimeter flux at 870um of ~2.5 mJy and a SFR of ~150-300Msun/yr, depending on the adopted tracer. These values place our source towards the faint end of the distribution of observed SMGs, and in particular among the still few faint SMGs with a fully characterized spectral energy distribution, which allows us not only to accurately estimate its redshift but also to measure its stellar mass and other physical properties. The galaxy studied in this work is a representative of the population of faint SMGs, of which only few objects are known to date, that are undetected in optical and therefore are not typically accounted for when measuring the cosmic star formation history (SFH). This faint galaxy population thus likely represents an important and missing piece in our understanding of the cosmic SFH. Its observation and characterization is of major importance to achieve a solid picture of galaxy evolution., A&A, in press. Very minor changes to match the printed version

Published
2016
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