Emission-line-selected galaxies at<i>z</i>= 0.6–2 in GOODS South: Stellar masses, SFRs, and large-scale structure

Kochiashvili, I.; Møller, P.; Milvang-Jensen, B.; Christensen, L.; Fynbo, J. P. U.; Freudling, W.; Clément, Benjamin; Cuby, Jean-Gabriel; Zabl, Johannes; Zibetti, S.

doi:10.1051/0004-6361/201425535

Cited by 13 publications

(13 citation statements)

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“…For example, most existing approaches rely on the adoption of a rigid physical model (e.g., analytic, two-parameter star formation histories combined with a standard dust attenuation curve and the assumption that all stars in a galaxy have the same metallicity) to describe galaxy SEDs (e.g. Bolzonella et al 2010;Wuyts et al 2011;Ilbert et al 2013;Muzzin et al 2013;Hernán-Caballero et al 2013;Bauer et al 2013;Lundgren et al 2014;Mortlock et al 2015;Kawinwanichakij et al 2016;Kochiashvili et al 2015). Even with the inclusion of superimposed bursts of star formation (e.g.…”

Section: Introductionmentioning

confidence: 99%

Modelling and interpreting spectral energy distributions of galaxies with beagle

Chevallard

Charlot

2016

Mon. Not. R. Astron. Soc.

356

298

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We present a new-generation tool to model and interpret spectral energy distributions (SEDs) of galaxies, which incorporates in a consistent way the production of radiation and its transfer through the interstellar and intergalactic media. This flexible tool, named beagle (for BayEsian Analysis of GaLaxy sEds), allows one to build mock galaxy catalogues as well as to interpret any combination of photometric and spectroscopic galaxy observations in terms of physical parameters. The current version of the tool includes versatile modeling of the emission from stars and photoionized gas, attenuation by dust and accounting for different instrumental effects, such as spectroscopic flux calibration and line spread function.We show a first application of the beagle tool to the interpretation of broadband SEDs of a published sample of ∼10 4 galaxies at redshifts 0.1 z 8. We find that the constraints derived on photometric redshifts using this multi-purpose tool are comparable to those obtained using public, dedicated photometric-redshift codes and quantify this result in a rigorous statistical way. We also show how the post-processing of beagle output data with the Python extension pyp-beagle allows the characterization of systematic deviations between models and observations, in particular through posterior predictive checks. The modular design of the beagle tool allows easy extensions to incorporate, for example, the absorption by neutral galactic and circumgalactic gas, and the emission from an active galactic nucleus, dust and shock-ionized gas. Information about public releases of the beagle tool will be maintained on http://www.jacopochevallard.org/beagle.

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Section: Introductionmentioning

confidence: 99%

Modelling and interpreting spectral energy distributions of galaxies with beagle

Chevallard

Charlot

2016

Mon. Not. R. Astron. Soc.

356

298

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“…For GOODS-S, the survey took a total integration time in the NB of 31.9 h and 3.3 h in the J-band. Kochiashvili et al (2015) has recently published a study focused on the main sequence of starformation using ELGs at z = 0.6−2 within this large programme data. In our work, we make use of these deep GOODS-S images to extract a sample of Hα emitters at z ∼ 0.62.…”

Section: Data and Sample Selectionmentioning

confidence: 99%

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Gómez-Guijarro

Gallego

Villar

et al. 2016

A&A

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Context. Studies measuring the star formation rate density, luminosity function, and properties of star-forming galaxies are numerous. However, it exists a gap at 0.5 < z < 0.8 in Hα-based studies. Aims. Our main goal is to study the properties of a sample of faint Hα emitters at z ∼ 0.62. We focus on their contribution to the faint end of the luminosity function and derived star formation rate density, characterising their morphologies and basic photometric and spectroscopic properties. Methods. We use a narrow-band technique in the near-infrared, with a filter centred at 1.06 µm. The data come from ultra-deep VLT/HAWK-I observations in the GOODS-S field with a total of 31.9 h in the narrow-band filter. In addition to our survey, we mainly make use of ancillary data coming from the CANDELS and Rainbow Cosmological Surveys Database, from the 3D-HST for comparison, and also spectra from the literature. We perform a visual classification of the sample and study their morphologies from structural parameters available in CANDELS. In order to obtain the luminosity function, we apply a traditional V/V max method and perform individual extinction corrections for each object to accurately trace the shape of the function. Results. Our 28 Hα-selected sample of faint star-forming galaxies reveals a robust faint-end slope of the luminosity function α = −1.46 +0.16 −0.08 . The derived star formation rate density at z ∼ 0.62 is ρ SFR = 0.036 +0.012 −0.008 M yr −1 Mpc −3 . The sample is mainly composed of disks, but an important contribution of compact galaxies with Sérsic indexes n ∼ 2 display the highest specific star formation rates. Conclusions. The luminosity function at z ∼ 0.62 from our ultra-deep data points towards a steeper α when an individual extinction correction for each object is applied. Compact galaxies are low-mass, low-luminosity, and starburst-dominated objects with a light profile in an intermediate stage from early to late types.

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“…There is still some debate over whether submm galaxies lie above the main sequence, or simply form its high-mass end. This debate is not primarily concerned with the form of the main sequence, as most studies agree that, at high redshifts, the main sequence continues to extend to high stellar masses with SFR ∝ M x * , where x is in the range 0.75-1.0 (Karim et al 2011;Speagle et al 2014;Renzini & Peng 2015;Schreiber et al 2015;Koprowski et al 2016;Dunlop et al 2017) with no evidence of any break as has been suggested at lower redshifts (Oliver et al 2010;Whitaker et al 2014;Ilbert et al 2015;Lee et al 2015;Tomczak et al 2016), or from galaxy surveys based purely on optical data (Kochiashvili et al 2015;Tasca et al 2015). Based on morphological decomposition at low redshifts this break was shown to disappear when only disc (not bulge) stellar mass was used (Abramson et al 2014).…”

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confidence: 99%

The SCUBA-2 Cosmology Legacy Survey: the nature of bright submm galaxies from 2 deg2 of 850-μm imaging

Michałowski

Dunlop

Koprowski

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present physical properties [redshifts (z), star formation rates (SFRs) and stellar masses (M star )] of bright (S 850 4 mJy) submm galaxies in the ≃ 2 deg 2 COSMOS and UDS fields selected with SCUBA-2/JCMT. We complete the galaxy identification process for all (≃ 2 000) S/N 3.5 850-µm sources, but focus our scientific analysis on a high-quality subsample of 651 S/N 4 sources with complete multiwavelength coverage including 1.1-mm imaging. We check the reliability of our identifications, and the robustness of the SCUBA-2 fluxes by revisiting the recent ALMA follow-up of 29 sources in our sample. Considering > 4 mJy ALMA sources, our identification method has a completeness of ≃ 86 per cent with a reliability of ≃ 92 per cent, and only ≃ 15-20 per cent of sources are significantly affected by multiplicity (when a secondary component contributes > 1/3 of the primary source flux). The impact of source blending on the 850-µm source counts as determined with SCUBA-2 is modest; scaling the single-dish fluxes by ≃ 0.9 reproduces the ALMA source counts. For our final SCUBA-2 sample, we find median z = 2.40 +0.10 −0.04 , SFR = 287 ± 6 M ⊙ yr −1 and log(M star /M ⊙ ) = 11.12 ± 0.02 (the latter for 349/651 sources with optical identifications). These properties clearly locate bright submm galaxies on the high-mass end of the 'main sequence' of star-forming galaxies out to z ≃ 6, suggesting that major mergers are not a dominant driver of the high-redshift submm-selected population. Their number densities are also consistent with the evolving galaxy stellar mass function. Hence, the submm galaxy population is as expected, albeit reproducing the evolution of the main sequence of star-forming galaxies remains a challenge for theoretical models/simulations.

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Emission-line-selected galaxies atz= 0.6–2 in GOODS South: Stellar masses, SFRs, and large-scale structure

Cited by 13 publications

References 85 publications

Modelling and interpreting spectral energy distributions of galaxies with beagle

Modelling and interpreting spectral energy distributions of galaxies with beagle

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

The SCUBA-2 Cosmology Legacy Survey: the nature of bright submm galaxies from 2 deg2 of 850-μm imaging

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