An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies
Durham University1, University of Nottingham2, Dalhousie University3, Academia Sinica Institute of Astronomy and Astrophysics4, University of Hertfordshire5, Chalmers University of Technology6, Leiden University7, European Southern Observatory8, University of British Columbia9, University of Manchester10, Max Planck Society11, Lancaster University12
02 Mar 2021-Monthly Notices of the Royal Astronomical Society (Oxford Academic)-Vol. 502, Iss: 3, pp 3426-3435
TL;DR: In this article, a robust sample of 30 near-infrared-faint (KAB > 25.3, 5σ) submillimetre galaxies (SMGs) selected from a 0.96 deg2 field was analyzed to investigate their properties and the cause of their faintness in optical/nearinfrared wavebands.
Abstract: We analyse a robust sample of 30 near-infrared-faint (KAB > 25.3, 5σ) submillimetre galaxies (SMGs) selected from a 0.96 deg2
field to investigate their properties and the cause of their faintness in optical/near-infrared wavebands. Our analysis exploits
precise identifications based on Atacama Large Millimeter Array (ALMA) 870-μm continuum imaging, combined with very
deep near-infrared imaging from the UKIDSS Ultra Deep Survey. We estimate that SMGs with KAB > 25.3 mag represent 15
± 2 per cent of the total population brighter than S870 = 3.6 mJy, with a potential surface density of ∼450 deg−2 above S870
≥ 1 mJy. As such, they pose a source of contamination in surveys for both high-redshift ‘quiescent’ galaxies and very high
redshift Lyman-break galaxies. We show that these K-faint SMGs represent the tail of the broader submillimetre population,
with comparable dust and stellar masses to KAB ≤ 25.3 mag SMGs, but lying at significantly higher redshifts (z = 3.44 ± 0.06
versus z = 2.36 ± 0.11) and having higher dust attenuation (AV = 5.2 ± 0.3 versus AV = 2.9 ± 0.1). We investigate the origin
of the strong dust attenuation and find indications that these K-faint galaxies have smaller dust continuum sizes than the KAB ≤
25.3 mag galaxies, as measured by ALMA, which suggests their high attenuation is related to their compact sizes. We identify
a correlation of dust attenuation with star formation rate surface density (SFR), with the K-faint SMGs representing the higher
SFR and highest AV galaxies. The concentrated, intense star formation activity in these systems is likely to be associated with
the formation of spheroids in compact galaxies at high redshifts, but as a result of their high obscuration these galaxies are
completely missed in ultraviolet, optical, and even near-infrared surveys.
Citations
More filters
TL;DR: In this paper, the authors used ALMA Band 9 continuum observations of the normal, dusty star-forming galaxy A1689-zD1 at z = 7.13, resulting in a ∼4.6 σ detection at 702 GHz.
Abstract: We report ALMA Band 9 continuum observations of the normal, dusty star-forming galaxy A1689-zD1 at z = 7.13, resulting in a ∼4.6 σ detection at 702 GHz. For the first time, these observations probe the far-infrared spectrum shortward of the emission peak of a galaxy in the Epoch of Reionization (EoR). Together with ancillary data from earlier works, we derive the dust temperature, Td, and mass, Md, of A1689-zD1 using both traditional modified blackbody spectral energy density fitting, and a new method that relies only on the [C ii] 158 μm line and underlying continuum data. The two methods give Td = (42+13-7, 40+13-) K, and Md} = (1.7+1.3-0.7, 2.0+1.8-1.0), ×, 107, M⊙. Band 9 observations improve the accuracy of the dust temperature (mass) estimate by ∼50 per cent (6 times). The derived temperatures confirm the reported increasing Td-redshift trend between z = 0 and 8; the dust mass is consistent with a supernova origin. Although A1689-zD1 is a normal UV-selected galaxy, our results, implying that ∼85 per cent of its star-formation rate is obscured, underline the non-negligible effects of dust in EoR galaxies.
31 citations
TL;DR: In this paper, the authors studied the impact of different galaxy statistics and empirical metallicity scaling relations on the merging rates and on the properties of compact objects binaries and found that the bulk of the star formation occurs at relatively high metallicities even at high redshift.
Abstract: We study the impact of different galaxy statistics and empirical metallicity scaling relations on the merging rates and on the properties of compact objects binaries. First, we analyze the similarities and differences of using the star formation rate functions or the stellar mass functions as galaxy statistics for the computation of the cosmic star formation rate density. Then we investigate the effects of adopting the Fundamental Metallicity Relation or a classic Mass Metallicity Relation to assign metallicity to galaxies with given properties. We find that when the Fundamental Metallicity Relation is exploited, the bulk of the star formation occurs at relatively high metallicities even at high redshift; the opposite holds when the Mass Metallicity Relation is employed, since in this case the metallicity at which most of the star formation takes place strongly decreases with redshift. We discuss the various reasons and possible biases originating this discrepancy. Finally, we show the impact that these different astrophysical prescriptions have on the merging rates and on the properties of compact objects binaries; specifically, we present results for the redshift dependent merging rates and for the chirp mass and time delay distributions of the merging binaries.
22 citations
Durham University1, National Taiwan University2, Academia Sinica Institute of Astronomy and Astrophysics3, Chinese Academy of Sciences4, University of British Columbia5, National Research Council6, Dalhousie University7, European Southern Observatory8, Imperial College London9, Spanish National Research Council10, University of La Laguna11, Peking University12, Korea Astronomy and Space Science Institute13, Nicolaus Copernicus University in Toruń14, Kyungpook National University15, Kyoto University16, Ehime University17
TL;DR: In this paper, the physical properties of 121 SNR and 5 sub-millimetre galaxies were analyzed using MAGPHYS+photo-z and compared to similar modelling of 850μm-selected SMG sample from AS2UDS to understand the fundamental physical differences between the two populations at the observed depths.
Abstract: We analyse the physical properties of 121 SNR ≥ 5 sub-millimetre galaxies (SMGs) from the STUDIES 450 μm survey. We model their UV-to-radio spectral energy distributions using MAGPHYS+photo-z and compare the results to similar modelling of 850 μm-selected SMG sample from AS2UDS, to understand the fundamental physical differences between the two populations at the observed depths. The redshift distribution of the 450-μm sample has a median of z = 1.85 ± 0.12 and can be described by strong evolution of the far-infrared luminosity function. The fainter 450-μm sample has ∼14 times higher space density than the brighter 850-μm sample at z ≲ 2, and a comparable space density at z = 2–3, before rapidly declining, suggesting LIRGs are the main obscured population at z ∼ 1–2, while ULIRGs dominate at higher redshifts. We construct rest-frame ∼180-μm-selected and dust-mass-matched samples at z = 1–2 and z = 3–4 from the 450 and 850-μm samples, respectively, to probe the evolution of a uniform sample of galaxies spanning the cosmic noon era. Using far-infrared luminosity, dust masses, and an optically thick dust model, we suggest that higher redshift sources have higher dust densities due to inferred dust continuum sizes which are roughly half of those for the lower redshift population at a given dust mass, leading to higher dust attenuation. We track the evolution in the cosmic dust mass density and suggest that the dust content of galaxies is governed by a combination of both the variation of gas content and dust destruction time-scale.
19 citations
TL;DR: In this paper , the spectral energy distributions of two likely high-redshift sources, identified in the 2 mm Mapping Obscuration to Reionization with ALMA (MORA) survey, were analyzed to fit spectral energy distribution and estimate redshifts before deriving physical properties.
Abstract: Abstract The 2 mm Mapping Obscuration to Reionization with ALMA (MORA) Survey was designed to detect high-redshift ( z ≳ 4), massive, dusty star-forming galaxies (DSFGs). Here we present two likely high-redshift sources, identified in the survey, whose physical characteristics are consistent with a class of optical/near-infrared (OIR)-invisible DSFGs found elsewhere in the literature. We first perform a rigorous analysis of all available photometric data to fit spectral energy distributions and estimate redshifts before deriving physical properties based on our findings. Our results suggest the two galaxies, called MORA-5 and MORA-9, represent two extremes of the “OIR-dark” class of DSFGs. MORA-5 ( z phot = 4.3 − 1.3 + 1.5 ) is a significantly more active starburst with a star formation rate (SFR) of 830 − 190 + 340 M ⊙ yr −1 compared to MORA-9 ( z phot = 4.3 − 1.0 + 1.3 ), whose SFR is a modest 200 − 60 + 250 M ⊙ yr −1 . Based on the stellar masses ( M ⋆ ≈ 10 10−11 M ⊙ ), space density ( n ∼ (5 ± 2) × 10 −6 Mpc −3 , which incorporates two other spectroscopically confirmed OIR-dark DSFGs in the MORA sample at z = 4.6 and z = 5.9), and gas depletion timescales (<1 Gyr) of these sources, we find evidence supporting the theory that OIR-dark DSFGs are the progenitors of recently discovered 3 < z < 4 massive quiescent galaxies.
14 citations
TL;DR: In this article , the ALMA-Herschel joint analysis of sources detected by ALMA Lensing Cluster Survey (ALCS) at 1.15 mm was presented, where the authors performed far-infrared spectral energy distribution modeling and derived the physical properties of dusty star formation for 125 sources (109 independently) that are detected at 2σ in at least one Herschel band.
Abstract: We present an ALMA-Herschel joint analysis of sources detected by the ALMA Lensing Cluster Survey (ALCS) at 1.15 mm. Herschel/PACS and SPIRE data at 100–500 μm are deblended for 180 ALMA sources in 33 lensing cluster fields that are detected either securely (141 sources; in our main sample) or tentatively at S/N ≥ 4 with cross-matched HST/Spitzer counterparts, down to a delensed 1.15 mm flux density of ∼0.02 mJy. We performed far-infrared spectral energy distribution modeling and derived the physical properties of dusty star formation for 125 sources (109 independently) that are detected at >2σ in at least one Herschel band. A total of 27 secure ALCS sources are not detected in any Herschel bands, including 17 optical/near-IR-dark sources that likely reside at z = 4.2 ± 1.2. The 16th, 50th, and 84th percentiles of the redshift distribution are 1.15, 2.08, and 3.59, respectively, for ALCS sources in the main sample, suggesting an increasing fraction of z ≃ 1 − 2 galaxies among fainter millimeter sources (f 1150 ∼ 0.1 mJy). With a median lensing magnification factor of μ=2.6−0.8+2.6 , ALCS sources in the main sample exhibit a median intrinsic star formation rate of 94−54+84 M ⊙ yr−1, lower than that of conventional submillimeter galaxies at similar redshifts by a factor of ∼3. Our study suggests weak or no redshift evolution of dust temperature with L IR < 1012 L ⊙ galaxies within our sample at z ≃ 0 − 2. At L IR > 1012 L ⊙, the dust temperatures show no evolution across z ≃ 1–4 while being lower than those in the local universe. For the highest-redshift source in our sample (z = 6.07), we can rule out an extreme dust temperature (>80 K) that was reported for MACS0416 Y1 at z = 8.31.
12 citations
References
More filters
University of Edinburgh1, Imperial College London2, University of Nottingham3, Durham University4, University of Leicester5, University of Hertfordshire6, UK Astronomy Technology Centre7, Cardiff University8, Queen Mary University of London9, University of Cambridge10, Liverpool John Moores University11
TL;DR: The final version published in MNRAS August 2007 included significant revisions including significant revisions to the original version April 2006.
Abstract: Final published version including significant revisions. Twenty four pages, fourteen figures. Original version April 2006; final version published in MNRAS August 2007
2,562 citations
TL;DR: A measure of dependence for two-variable relationships: the maximal information coefficient (MIC), which captures a wide range of associations both functional and not, and for functional relationships provides a score that roughly equals the coefficient of determination of the data relative to the regression function.
Abstract: Identifying interesting relationships between pairs of variables in large data sets is increasingly important. Here, we present a measure of dependence for two-variable relationships: the maximal information coefficient (MIC). MIC captures a wide range of associations both functional and not, and for functional relationships provides a score that roughly equals the coefficient of determination (R2) of the data relative to the regression function. MIC belongs to a larger class of maximal information-based nonparametric exploration (MINE) statistics for identifying and classifying relationships. We apply MIC and MINE to data sets in global health, gene expression, major-league baseball, and the human gut microbiota and identify known and novel relationships.
2,414 citations
TL;DR: In this article, the spectral energy distribution of the power reradiated by dust in stellar birth clouds and in the ambient interstellar medium (ISM) in galaxies is computed using an angle-averaged prescription.
Abstract: We present a simple, largely empirical but physically motivated model to interpret the mid- and far-infrared spectral energy distributions of galaxies consistently with the emission at ultraviolet, optical and near-infrared wavelengths. Our model relies on an existing angle-averaged prescription to compute the absorption of starlight by dust in stellar birth clouds and in the ambient interstellar medium (ISM) in galaxies. We compute the spectral energy distribution of the power reradiated by dust in stellar birth clouds as the sum of three components: a component of polycyclic aromatic hydrocarbons (PAHs); a mid-infrared continuum characterising the emission from hot grains at temperatures in the range 130–250 K; and a component of grains in thermal equilibrium with adjustable temperature in the range 30–60 K. In the ambient ISM, we fix for simplicity the relative proportions of these three components to reproduce the spectral shape of diffuse cirrus emission in the Milky Way, and we include a component of cold grains in thermal equilibrium with adjustable temperature in the range 15–25 K. Our model is both simple and versatile enough that it can be used to derive statistical constraints on the star formation histories and dust contents of large samples of galaxies using a wide range of ultraviolet, optical and infrared observations. We illustrate this by deriving median-likelihood estimates of the star formation rates, stellar masses, effective dust optical depths, dust masses, and relative strengths of different dust components of 66 well-studied nearby star-forming galaxies from the Spitzer Infrared Nearby Galaxy Survey (SINGS). We explore how the constraints derived in this way depend on the available spectral information. From our analysis of the SINGS sample, we conclude that the mid- and far-infrared colours of galaxies correlate strongly with the specific star formation rate, as well as with other galaxywide quantities connected to this parameter, such as the ratio of infrared luminosity between stellar birth clouds and the ambient ISM, the contributions by PAHs and grains in thermal equilibrium to the total infrared emission, and the ratio of dust mass to stellar mass. Our model can be straightforwardly applied to interpret ultraviolet, optical and infrared spectral energy distributions from any galaxy sample.
1,156 citations
Max Planck Society1, Leiden University2, Yale University3, Goddard Space Flight Center4, Space Telescope Science Institute5, University of Michigan6, University of California, Santa Cruz7, Colby College8, University of Hertfordshire9, University of Oxford10, Hebrew University of Jerusalem11, University of Wisconsin-Madison12, Open University13, Carnegie Institution for Science14, University of Kentucky15
TL;DR: In this paper, the galaxy size-mass distribution over the redshift range 0 3 × 10{sup 9} M {sub ☉}, and steep, R{sub eff}∝M{sub ∗}{sup 0.75}, for early-type galaxies with stellar mass > 2 × 10,sup 10} M{sub ǫ, and the intrinsic scattermore is ≲0.2 dex for all galaxy types and redshifts.
Abstract: Spectroscopic+photometric redshifts, stellar mass estimates, and rest-frame colors from the 3D-HST survey are combined with structural parameter measurements from CANDELS imaging to determine the galaxy size-mass distribution over the redshift range 0 3 × 10{sup 9} M {sub ☉}, and steep, R{sub eff}∝M{sub ∗}{sup 0.75}, for early-type galaxies with stellar mass >2 × 10{sup 10} M {sub ☉}. The intrinsic scattermore » is ≲0.2 dex for all galaxy types and redshifts. For late-type galaxies, the logarithmic size distribution is not symmetric but is skewed toward small sizes: at all redshifts and masses, a tail of small late-type galaxies exists that overlaps in size with the early-type galaxy population. The number density of massive (∼10{sup 11} M {sub ☉}), compact (R {sub eff} < 2 kpc) early-type galaxies increases from z = 3 to z = 1.5-2 and then strongly decreases at later cosmic times.« less
1,004 citations
Open University1, University of California, Irvine2, University of Oxford3, California Institute of Technology4, Jet Propulsion Laboratory5, National Radio Astronomy Observatory6, Harvard University7, Institut d'Astrophysique de Paris8, French Alternative Energies and Atomic Energy Commission9, University of Johannesburg10, Search for extraterrestrial intelligence11, University of Crete12, University of Padua13, University of Hertfordshire14, University of Edinburgh15, Cardiff University16, National Institute of Astrophysics, Optics and Electronics17, University of Bonn18, European Space Agency19, University of Nottingham20, University of St Andrews21, Spanish National Research Council22, University of La Laguna23, Goddard Space Flight Center24, Imperial College London25, Ghent University26, University of Louisville27, University of Paris-Sud28, Liverpool John Moores University29, Ames Research Center30, University of Chicago31, University of Pennsylvania32, Rutgers University33, University of Bristol34, Aix-Marseille University35, Queen Mary University of London36, University of Colorado Boulder37, University of Maryland, College Park38, Carnegie Institution for Science39, Japan Aerospace Exploration Agency40, University of Central Lancashire41, Rutherford Appleton Laboratory42, University of British Columbia43, Durham University44, Max Planck Society45, Leiden University46
TL;DR: Early data from the Herschel Astrophysical Terahertz Large Area Survey are used to demonstrate that wide-area submillimeter surveys can simply and easily detect strong gravitational lensing events, with close to 100% efficiency.
Abstract: Gravitational lensing is a powerful astrophysical and cosmological probe and is particularly valuable at submillimeter wavelengths for the study of the statistical and individual properties of dusty star-forming galaxies. However, the identification of gravitational lenses is often time-intensive, involving the sifting of large volumes of imaging or spectroscopic data to find few candidates. We used early data from the Herschel Astrophysical Terahertz Large Area Survey to demonstrate that wide-area submillimeter surveys can simply and easily detect strong gravitational lensing events, with close to 100% efficiency.
436 citations