The Constant Average Relationship between Dust-obscured Star Formation and Stellar Mass from z = 0 to z = 2.5

Whitaker, Katherine E.; Pope, Alexandra; Cybulski, Ryan; Casey, Caitlin M.; Popping, Gergö; Yun, Min S.

doi:10.3847/1538-4357/aa94ce

Cited by 183 publications

(245 citation statements)

References 98 publications

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“…The total SFR can be accounted for by adding both IR and UV estimates (SFR IR+UV ). Not surprisingly, the star formation is dominated by SFR IR , with SFR UV only contributing at the level of 2%-20% to the total SFR (SFR IR+UV ), in agreement with other previous works comparing obscured and unobscured star formation in starburst galaxies (e.g., Puglisi et al 2017) and galaxies with similar stellar mass (e.g., Whitaker et al 2017).…”

Section: Spatially Resolved Uv Slopessupporting

confidence: 78%

Starburst to Quiescent from HST/ALMA: Stars and Dust Unveil Minor Mergers in Submillimeter Galaxies at z ∼ 4.5

Gómez-Guijarro

Toft

Karim

et al. 2018

ApJ

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Dust-enshrouded, starbursting, submillimeter galaxies (SMGs) at z3 have been proposed as progenitors of z2 compact quiescent galaxies (cQGs). To test this connection, we present a detailed spatially resolved study of the stars, dust, and stellar mass in a sample of six submillimeter-bright starburst galaxies at z∼4.5. The stellar UV emission probed by HST is extended and irregular and shows evidence of multiple components. Informed by HST, we deblend Spitzer/ IRAC data at rest-frame optical, finding that the systems are undergoing minor mergers with a typical stellar mass ratio of 1:6.5. The FIR dust continuum emission traced by ALMA locates the bulk of star formation in extremely compact regions (median r e =0.70±0.29 kpc), and it is in all cases associated with the most massive component of the mergers (median M M log 10.49 0.32We compare spatially resolved UV slope (β) maps with the FIR dust continuum to study the infrared excess (IRX=L IR /L UV )-β relation. The SMGs display systematically higher IRX values than expected from the nominal trend, demonstrating that the FIR and UV emissions are spatially disconnected. Finally, we show that the SMGs fall on the mass-size plane at smaller stellar masses and sizes than the cQGs at z=2. Taking into account the expected evolution in stellar mass and size between z=4.5 and z=2 due to the ongoing starburst and mergers with minor companions, this is in agreement with a direct evolutionary connection between the two populations.

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Section: Spatially Resolved Uv Slopessupporting

confidence: 78%

Starburst to Quiescent from HST/ALMA: Stars and Dust Unveil Minor Mergers in Submillimeter Galaxies at z ∼ 4.5

Gómez-Guijarro

Toft

Karim

et al. 2018

ApJ

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“…where f obscured corresponds to the obscured fraction of star formation and SFR total corresponds to the total SFR of galaxies (the sum of the obscured and unobscured fraction). To calculate f obscured we use the empirical relation derived by Whitaker et al (2017) between the obscured fraction of star formation and the stellar mass for main-sequence galaxies in the redshift range from z = 0.5 to z = 2.5. We assume that this empirical fit extends towards higher redshift and also applies for galaxies above the main-sequence.…”

Section: Generating Mock Lightconesmentioning

confidence: 99%

“…All star-formation is obscured -We adopted the fit presented in Whitaker et al (2017) to estimate the obscured fraction of SF. An extreme alternative is to assume that all SF happens in dust environments and f obscured = 1.…”

Section: A Is the Flattening In The Number Counts Robust Against Thementioning

confidence: 99%

The ALMA Spectroscopic Survey in the HUDF: A Model to Explain Observed 1.1 and 0.85 mm Dust Continuum Number Counts

Popping

Walter

Behroozi

et al. 2020

ApJ

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We present a new semi-empirical model for the dust continuum number counts of galaxies at 1.1 millimeter and 850 µm. Our approach couples an observationally motivated model for the stellar mass and SFR distribution of galaxies with empirical scaling relations to predict the dust continuum flux density of these galaxies. Without a need to tweak the IMF, the model reproduces the currently available observations of the 1.1 millimeter and 850 µm number counts, including the observed flattening in the 1.1 millimeter number counts below 0.3 mJy (González-López et al. 2020) and the number counts in discrete bins of different galaxy properties. Predictions of our work include : (1) the galaxies that dominate the number counts at flux densities below 1 mJy (3 mJy) at 1.1 millimeter (850 µm) have redshifts between z = 1 and z = 2, stellar masses of ∼ 5 × 10 10

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“…They also found that the relation does not undergo any redshift evolution. Since our sample lies at z 3, we decided to investigate how it compares with the lower-redshift sources of Whitaker et al (2017).…”

Section: Fraction Of Obscured Star Formationmentioning

confidence: 99%

An ALMA survey of the SCUBA-2 cosmology legacy survey UKIDSS/UDS field: Dust attenuation in high-redshift Lyman-break galaxies

Koprowski

Coppin

Dudzevičiūtė

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We analyse 870µm Atacama Large Millimetre Array (ALMA) dust continuum detections of 41 canonically-selected z 3 Lyman-break galaxies (LBGs), as well as 209 ALMA-undetected LBGs, in follow-up of SCUBA-2 mapping of the UKIDSS Ultra Deep Survey (UDS) field. We find that our ALMA-bright LBGs lie significantly off the locally calibrated IRX-beta relation and tend to have relatively bluer rest-frame UV slopes (as parametrised by β), given their high values of the 'infrared excess' (IRX ≡ L IR /L UV ), relative to the average 'local' IRX-β relation. We attribute this finding in part to the young ages of the underlying stellar populations but we find that the main reason behind the unusually blue UV slopes are the relatively shallow slopes of the corresponding dust attenuation curves. We show that, when stellar masses, M * , are being established via SED fitting, it is absolutely crucial to allow the attenuation curves to vary (rather than fixing it on Calzetti-like law), where we find that the inappropriate curves may underestimate the resulting stellar masses by a factor of 2-3× on average. In addition, we find these LBGs to have relatively high specific star-formation rates (sSFRs), dominated by the dust component, as quantified via the fraction of obscured star formation ( f obs ≡ SFR IR /SFR UV+IR ). We conclude that the ALMA-bright LBGs are, by selection, massive galaxies undergoing a burst of a star formation (large sSFRs, driven, for example, by secular or merger processes), with a likely geometrical disconnection of the dust and stars, responsible for producing shallow dust attenuation curves.

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The Constant Average Relationship between Dust-obscured Star Formation and Stellar Mass from z = 0 to z = 2.5

Cited by 183 publications

References 98 publications

Starburst to Quiescent from HST/ALMA: Stars and Dust Unveil Minor Mergers in Submillimeter Galaxies at z ∼ 4.5

Starburst to Quiescent from HST/ALMA: Stars and Dust Unveil Minor Mergers in Submillimeter Galaxies at z ∼ 4.5

The ALMA Spectroscopic Survey in the HUDF: A Model to Explain Observed 1.1 and 0.85 mm Dust Continuum Number Counts

An ALMA survey of the SCUBA-2 cosmology legacy survey UKIDSS/UDS field: Dust attenuation in high-redshift Lyman-break galaxies

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