Early Science with the Large Millimeter Telescope: Detection of Dust Emission in Multiple Images of a Normal Galaxy at z &gt; 4 Lensed by a Frontier Fields Cluster

Pope, Alexandra; Montaña, Alfredo; Battisti, Andrew; Limousin, M.; Marchesini, Danilo; Wilson, Grant; Alberts, Stacey; Aretxaga, I.; Avila-Reese, Vladimir; Bermejo-Climent, J. R.; Brammer, Gabriel; Bravo-Alfaro, H.; Calzetti, Daniela; Chary, R.-R.; Cybulski, Ryan; Giavalisco, Mauro; Hughes, D. H.; Kado-Fong, Erin; Keller, Erica; Kirkpatrick, Allison; Labbé, Ivo; Lange-Vagle, Daniel; Lowenthal, James D.; Murphy, E. J.; Oesch, Pascal; Rosa-González, D.; Sánchez-Argüelles, David; Shipley, Heath; Stefanon, Mauro; Vega, O.; Whitaker, Katherine E.; Williams, Christina C.; Yun, Min S.; Zavala, Jorge A.; Zeballos, M.

doi:10.3847/1538-4357/aa6573

Cited by 24 publications

(30 citation statements)

References 69 publications

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“…We found that deviations towards red UV-slopes with respect to the canonical IRX -β relations are driven by either an ageing stellar population or by varying dust types. Similar values for β and IRX as observed by Capak et al (2015), Bouwens et al (2016), Pope et al (2017), and Smit et al (2017), can be obtained when the stellar emission from a 50-100 Myr old stellar population passes through a screen of dust with a MW attenuation curve. The effect of ageing has been discussed before by many authors (e.g., Kong et al 2004;Grasha et al 2013).…”

Section: Smc Dust In Early Galaxiessupporting

confidence: 68%

“…Capak et al (2015), Bouwens et al (2016), Pope et al (2017), and Smit et al (2017) observed a number of highredshift (z > 4) galaxies with a UV-slope β ∼ −1 and IRX∼ 1 or less. These works concluded that these values are consistent with an SMC attenuation curve, suggesting that dust in early Universe galaxies is similar to SMC dust.…”

Section: Smc Dust In Early Galaxiesmentioning

confidence: 99%

“…High-redshift observations have demonstrated that dusty star-forming galaxies (DSFGs) have bluer UV continuum slopes for a given IRX (increasingly deviating from the Meurer et al relation as a function of IR luminosity, e.g., Oteo et al 2013;Casey et al 2014;Bourne et al 2017). High-redshift Lyman Break Galaxies are observed to have redder UV continuum slopes β for a given IRX value, more consistent with a Small Magellanic Cloud (SMC) or Large Magellanic Cloud (LMC) attenuation curve than the canonical Meurer, Heckman & Calzetti (1999) relation (e.g., Capak et al 2015;Bouwens et al 2016;Koprowski et al 2016;Pope et al 2017;Smit et al 2017). A similar conclusion was reached for normal star-forming galaxies at z ∼ 2 (Reddy et al 2012(Reddy et al , 2017 and for lensed Lyman Break Galaxies at z ∼ 3 (Siana et al 2008(Siana et al , 2009).…”

Section: Introductionmentioning

confidence: 99%

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Dissecting the IRX–β dust attenuation relation: exploring the physical origin of observed variations in galaxies

Popping

Puglisi

Norman

2017

Monthly Notices of the Royal Astronomical Society

121

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The use of ultraviolet (UV) emission as a tracer of galaxy star-formation rate (SFR) is hampered by dust obscuration. The empirical relationship between UV slope, β, and the ratio between far-infrared and UV luminosity, IRX, is commonly employed to account for obscured UV emission. We present a simple model that explores the physical origin of variations in the IRX -β dust attenuation relation. A relative increase in FUV compared to NUV attenuation and an increasing stellar population age cause variations towards red UV slopes for a fixed IRX. Dust geometry effects (turbulence, dust screen with holes, mixing of stars within the dust screen, two-component dust model) cause variations towards blue UV slopes. Poor photometric sampling of the UV spectrum causes additional observational variations. We provide an analytic approximation for the IRX -β relation invoking a subset of the explored physical processes (dust type, stellar population age, turbulence). We discuss observed variations in the IRX -β relation for local (sub-galactic scales) and high-redshift (normal and dusty star-forming galaxies, galaxies during the epoch of reionization) galaxies in the context of the physical processes explored in our model. High spatial resolution imaging of the UV and sub-mm emission of galaxies can constrain the IRX -β dust attenuation relation for different galaxy types at different epochs, where different processes causing variations may dominate. These constraints will allow the use of the IRX -β relation to estimate intrinsic SFRs of galaxies, despite the lack of a universal relation.

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Section: Smc Dust In Early Galaxiessupporting

confidence: 68%

Section: Smc Dust In Early Galaxiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Dissecting the IRX–β dust attenuation relation: exploring the physical origin of observed variations in galaxies

Popping

Puglisi

Norman

2017

Monthly Notices of the Royal Astronomical Society

121

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“…Second, conversely, interstellar dust may provide protection from the UV background of the intergalactic medium (IGM), which by photoionization heating, could have evaporated dwarf galaxies during the epoch of reionization (Barkana & Loeb 1999). Furthermore, dust obscures as much as half of the light in star-forming galaxies (Lagache et al 2005), and at high redshifts (z3), our understanding of dust-obscured star formation activity in typical star-forming galaxies is very incomplete (e.g., Pope et al 2017).…”

Section: Introductionmentioning

confidence: 99%

A Model Connecting Galaxy Masses, Star Formation Rates, and Dust Temperatures across Cosmic Time

Imara

Loeb

Johnson

et al. 2018

ApJ

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We investigate the evolution of dust content in galaxies from redshifts z=0 to z=9.5. Using empirically motivated prescriptions, we model galactic-scale properties-including halo mass, stellar mass, star formation rate, gas mass, and metallicity-to make predictions for the galactic evolution of dust mass and dust temperature in main-sequence galaxies. Our simple analytic model, which predicts that galaxies in the early universe had greater quantities of dust than their low-redshift counterparts, does a good job of reproducing observed trends between galaxy dust and stellar mass out to z≈6. We find that for fixed galaxy stellar mass, the dust temperature increases from z=0 to z=6. Our model forecasts a population of low-mass, high-redshift galaxies with interstellar dust as hot as, or hotter than, their more massive counterparts; but this prediction needs to be constrained by observations. Finally, we make predictions for observing 1.1 mm flux density arising from interstellar dust emission with the Atacama Large Millimeter Array.

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“…Such achievement has become feasible only recently thanks to wide-area far-IR/sub-mm surveys conducted by Herschel, ASTE/AzTEC, APEX/LABOCA, JCMT/SCUBA2, and ALMA-SPT (e.g., Gruppioni et al 2013Gruppioni et al , 2015Lapi et al 2011;Weiss et al 2013;Strandet et al 2016;Koprowski et al 2014Koprowski et al , 2016, in many instances eased by gravitational lensing from foreground objects (e.g., Negrello et al 2014Negrello et al , 2017Nayyeri et al 2016). In fact, galaxies endowed with star formation ratesṀ ⋆ a few tens M ⊙ yr −1 at redshift z 2 were largely missed by rest-frame optical/UV surveys because of heavy dust obscuration, difficult to correct for with standard techniques based only on UV spectral data (e.g., Bouwens et al 2016Bouwens et al , 2017Mancuso et al 2016a;Pope et al 2017;Ikarashi et al 2017;Simpson et al 2017). High-resolution, follow-up observations of these galaxies in the far-IR/sub-mm/radio band via ground-based interferometers, such as SMA, VLA, PdBI, and recently ALMA, have revealed star formation to occur in a few collapsing clumps distributed over spatial scales smaller than a few kpcs (see Simpson et al 2015;Ikarashi et al 2015;Straatman et al 2015;Spilker et al 2016;Barro et al 2016;Tadaki et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Stellar Mass Function of Active and Quiescent Galaxies via the Continuity Equation

Lapi

Mancuso

Bressan

et al. 2017

ApJ

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The continuity equation is developed for the stellar mass content of galaxies, and exploited to derive the stellar mass function of active and quiescent galaxies over the redshift range z ∼ 0 − 8. The continuity equation requires two specific inputs gauged on observations: (i) the star formation rate functions determined on the basis of the latest UV+far-IR/sub-mm/radio measurements; (ii) average star-formation histories for individual galaxies, with different prescriptions for discs and spheroids. The continuity equation also includes a source term taking into account (dry) mergers, based on recent numerical simulations and consistent with observations. The stellar mass function derived from the continuity equation is coupled with the halo mass function and with the SFR functions to derive the star formation efficiency and the main sequence of star-forming galaxies via the abundance matching technique. A remarkable agreement of the resulting stellar mass function for active and quiescent galaxies, of the galaxy main sequence and of the star-formation efficiency with current observations is found; the comparison with data also allows to robustly constrain the characteristic timescales for star formation and quiescence of massive galaxies, the star formation history of their progenitors, and the amount of stellar mass added by in-situ star formation vs. that contributed by external merger events. The continuity equation is shown to yield quantitative outcomes that must be complied by detailed physical models, that can provide a basis to improve the (sub-grid) physical recipes implemented in theoretical approaches and numerical simulations, and that can offer a benchmark for forecasts on future observations with multi-band coverage, as it will become routinely achievable in the era of JWST.

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Early Science with the Large Millimeter Telescope: Detection of Dust Emission in Multiple Images of a Normal Galaxy at z > 4 Lensed by a Frontier Fields Cluster

Cited by 24 publications

References 69 publications

Dissecting the IRX–β dust attenuation relation: exploring the physical origin of observed variations in galaxies

Dissecting the IRX–β dust attenuation relation: exploring the physical origin of observed variations in galaxies

A Model Connecting Galaxy Masses, Star Formation Rates, and Dust Temperatures across Cosmic Time

Stellar Mass Function of Active and Quiescent Galaxies via the Continuity Equation

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