ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS

By Rychard J. Bouwens, M. Aravena, R. Decarli, F. Walter, E. da Cunha, I. Labbé, Franz E. Bauer, F. Bertoldi, C. Carilli, S. Chapman and 18 more. 2016

231 citations recorded by the source corpus.

We make use of deep 1.2 mm continuum observations (12.7 μJy beam−1 rms) of a 1 arcmin2 region in the Hubble Ultra Deep Field to probe dust-enshrouded star formation from 330 Lyman-break galaxies spanning the redshift range z = 2–10 (to ∼2–3 M⊙ yr−1 at 1σ over the entire range). Given the depth and area of ASPECS, we would expect to tentatively detect 35 galaxies, extrapolating the Meurer z ∼ 0 IRX–β relation to z ≥ 2 (assuming dust temperature Td ∼ 35 K). However, only six tentative detections are found at z ≳ 2 in ASPECS, with just three at >3σ. Subdividing our z = 2–10 galaxy samples according to stellar mass, UV luminosity, and UV-continuum slope and stacking the results, we find a significant detection only in the most massive (>109.75 M⊙) subsample, with an infrared excess (IRX = LIR/LUV) consistent with previous z ∼ 2 results. However, the infrared excess we measure from our large selection of sub-L∗ (<109.75 M⊙) galaxies is ± 0.34 (bootstrap and formal uncertainties) and ± 0.18 at z = 2–3 and z = 4–10, respectively, lying below even an IRX–β relation for the Small Magellanic Cloud (95% confidence). These results demonstrate the relevance of stellar mass for predicting the IR luminosity of z ≳ 2 galaxies. We find that the evolution of the IRX–stellar mass relationship depends on the evolution of the dust temperature. If the dust temperature increases monotonically with redshift ( ) such that Td ∼ 44–50 K at z ≥ 4, current results are suggestive of little evolution in this relationship to z ∼ 6. We use these results to revisit recent estimates of the z ≥ 3 star formation rate density.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5a5ffed981c74d4405bc0f950c5d0496cceff1d6

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. P. V. van Dokkum
4. C. Conroy
5. R. Somerville
6. M. Franx
7. Richard S. Ellis
8. R. Dav'e

In Instrumentation

1. C. Conroy
2. P. V. van Dokkum
3. M. Franx
4. Richard S. Ellis
5. J. Dunlop
6. R. Bouwens
7. I. Labbé
8. P. Oesch

Citations in the corpus

• The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, methodology): “…curve steeper than that of the SMC. Figure 9 summarizes a few recent measurements of IRX-β for young and low-mass galaxies at z ∼ 2 (Baker et al. 2001; Siana et al. 2009; Reddy et al. 2010, 2012a), low-mass galaxies and LBGs in general at z ∼ 4 − 10 (Bouwens et al. 2016b), and our own measurements.”
• The Dearth of z ∼ 10 Galaxies in All HST Legacy Fields—The Rapid Evolution of the Galaxy Population in the First 500 Myr (2017, methodology): “In particular, we plot the values assuming an evolving dust temperature from Table 10 in Bouwens et al. (2016a), which were integrated to the same UV luminosity limit.”
• The MUSE Hubble Ultra Deep Field Survey: I. Survey description, data reduction and source detection (2017, background): “…2015; Parsa et al. 2016), the evolution of star formation rate with redshift (e.g., Ellis et al. 2013; Madau & Dickinson 2014; Rafelski et al. 2016; Bouwens et al. 2016; Dunlop et al. 2017), measurements of stellar mass (e.g., González et al. 2011; Grazian et al. 2015; Song et al. 2016), galaxy…”
• Rapid Reionization by the Oligarchs: The Case for Massive, UV-bright, Star-forming Galaxies with High Escape Fractions (2019, methodology): “…constraints on ξion can be placed using Hα measurements and some assumptions about fesc, and now exist from direct spectroscopy (Nakajima et al. 2016; Matthee et al. 2017; Shivaei et al. 2018; Tang et al. 2019) and IRAC-excess inferences of Hα out to z∼5 (Bouwens et al. 2016b; Lam et al. 2019).”
• UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, methodology): “Including dust priors from ALMA measurements (Bouwens et al. 2016b) made little difference for bright galaxies, because they were consistent with SED-derived dust estimates (Fig.”
• The dust content of galaxies from z = 0 to z = 9 (2016, background): “Our results have significant consequences for studies of the redshift distribution of sub-mm continuum selected galaxies (Aravena et al. 2016; Bouwens et al. 2016; Dunlop et al. 2016).”
• The Star Formation Main Sequence in the Hubble Space Telescope Frontier Fields (2017, result): “We note that recent ALMA results have found consistency with the Meurer et al. (1999) law at z ∼ 3, while suggesting a possible evolution towards lower attenuations at z larger than 4 or 5 (Capak et al. 2015; Bouwens et al. 2016; Fudamoto et al. 2017).”
• Big Three Dragons: A z = 7.15 Lyman-break galaxy detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum with ALMA (2018, methodology): “The authors have compared the whole system of B14-65666 with the z≈3−5 results (Fudamoto et al. 2017; Koprowski et al. 2018), a stacking result of z≈4−10 (Bouwens et al. 2016), and with another z > 7 galaxy that has a dust continuum detection, A1689 zD1 (Watson et al. 2015; Knudsen et al. 2017).”
• The Universe Is Reionizing at z ∼ 7: Bayesian Inference of the IGM Neutral Fraction Using Lyα Emission from Galaxies (2017, background): “…contain less dust (as ALMA and Plateau de Bure Interferometer (PdBI) re- sults are suggesting, Walter et al. 2012; Ouchi et al. 2013; Ota et al. 2014; Schaerer et al. 2015; Maiolino et al. 2015; Capak et al. 2015; Bouwens et al. 2016b; Pentericci et al. 2016) and neutral gas than at low redshifts.”
• ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: SURVEY DESCRIPTION (2016, background): “• In Paper VI (Bouwens et al. 2016) we investigate where high–redshift galaxies from ASPECS lie in relation to known IRX–β and IRX–stellar mass relationships, concluding that less dust continuum emission is detected in z>2.5 than expected (unless high dust temperatures, T∼50 K, are assumed).”