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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 731743.0, MPI für Astronomie / Publikationen_mpia
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
Authors:Bouwens, R. J.; Aravena, M.; Decarli, R.; Walter, F.; da Cunha, E.; Labbé, I.; Bauer, F. E.; Bertoldi, F.; Carilli, C.; Chapman, S.; Daddi, E.; Hodge, J.; Ivison, R. J.; Karim, A.; Le Fevre, O.; Magnelli, B.; Ota, K.; Riechers, D.; Smail, I. R.; van der Werf, P.; Weiss, A.; Cox, P.; Elbaz, D.; Gonzalez-Lopez, J.; Infante, L.; Oesch, P.; Wagg, J.; Wilkins, S.
Date of Publication (YYYY-MM-DD):2016
Title of Journal:The Astrophysical Journal
Issue / Number:1
Start Page:id. 72 (32 pp)
Audience:Not Specified
Abstract / Description: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 T d ∼ 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 = L IR/L UV) consistent with previous z ∼ 2 results. However, the infrared excess we measure from our large selection of sub-L (<109.75 M ) galaxies is {0.11}-0.42+0.32 ± 0.34 (bootstrap and formal uncertainties) and {0.14}-0.14+0.15 ± 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 (\propto {(1+z)}0.32) such that T d ∼ 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.
Free Keywords:galaxies: evolution; galaxies: ISM; galaxies: star formation; galaxies: statistics; instrumentation: interferometers; submillimeter: galaxies
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X %R 10.3847/1538-4357/833/1/72
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