The Physical Drivers of the Luminosity-weighted Dust Temperatures in High-redshift Galaxies

Burnham, Anne D.; Casey, Caitlin M.; Zavala, Jorge A.; Manning, Sinclaire M.; Spilker, Justin; Chapman, Scott; Chen, Chian-Chou; Cooray, Asantha; Sanders, D. B.; Scoville, N. Z.

doi:10.3847/1538-4357/abe401

Cited by 13 publications

(17 citation statements)

References 74 publications

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“…The right panel of Figure 9 shows the variation of peak with the sSFR (SFR calculated using stars born in the last 10 Myr) for different redshifts. We have also over-plotted two galaxies at ∼ 4.5 from Burnham et al (2021) which are in agreement with our = 5 relation within the scatter. We see a very tight relation for the F galaxies at the high-sSFR (sSFR/Gyr −1 0) end.…”

Section: T Peaksupporting

confidence: 86%

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First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

Vijayan

Lovell

Wilkins

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the photometric properties of galaxies in the First Light and Reionisation Epoch Simulations (Flares). The simulations trace the evolution of galaxies in a range of overdensities through the Epoch of Reionistion (EoR). With a novel weighting scheme we combine these overdensities, extending significantly the dynamic range of observed composite distribution functions compared to periodic simulation boxes. Flares predicts a significantly larger number of intrinsically bright galaxies, which can be explained through a simple model linking dust-attenuation to the metal content of the interstellar medium, using a line-of-sight (LOS) extinction model. With this model we present the photometric properties of the Flares galaxies for z ∈ [5, 10]. We show that the ultraviolet (UV) luminosity function (LF) matches the observations at all redshifts. The function is fit by Schechter and double power-law forms, with the latter being favoured at these redshifts by the Flares composite UV LF. We also present predictions for the UV continuum slope as well as the attenuation in the UV. The impact of environment on the UV LF is also explored, with the brightest galaxies forming in the densest environments. We then present the line luminosity and equivalent widths of some prominent nebular emission lines arising from the galaxies, finding rough agreement with available observations. We also look at the relative contribution of obscured and unobscured star formation, finding comparable contributions at these redshifts.

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Section: T Peaksupporting

confidence: 86%

“…This measure has been used in many observational studies to understand the evolution of luminosity weighted dust temperature across redshifts and galaxy properties (e.g. Casey et al 2018;Schreiber et al 2018;Burnham et al 2021). It suffers less from model dependent biases compared to other dust temperature values.…”

Section: T Peakmentioning

confidence: 99%

First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

Vijayan

Lovell

Wilkins

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Conversely, f gas does not seem to correlate with Σ SFR . These type of relations have been reported by several studies in the literature, both in the case of τ dep (e.g., Elbaz et al 2018;Franco et al 2020b) and T dust (Burnham et al 2021), establishing a physical connection between the increase in Σ SFR and the origin of such relations. However, in order to better establish such physical connections, it is necessary to account for the stellar mass and redshift evolution of the studied properties.…”

Section: Compact Star Formation As a Physical Driver Of Depletion Tim...supporting

confidence: 71%

GOODS-ALMA 2.0: Starbursts in the main sequence reveal compact star formation regulating galaxy evolution prequenching

Gómez-Guijarro,

Elbaz,

Xiao

et al. 2022

Preprint

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Compact star formation appears to be generally common in dusty star-forming galaxies (SFGs). However, its role in the framework set by the scaling relations in galaxy evolution remains to be understood. In this work we follow up on the galaxy sample from the GOODS-ALMA 2.0 survey, an ALMA blind survey at 1.1 mm covering a continuous area of 72.42 arcmin 2 using two array configurations. We derived physical properties, such as star formation rates, gas fractions, depletion timescales, and dust temperatures for the galaxy sample built from the survey. There exists a subset of galaxies that exhibit starburst-like short depletion timescales, but they are located within the scatter of the so-called main sequence of SFGs. These are dubbed starbursts in the main sequence and display the most compact star formation and they are characterized by the shortest depletion timescales, lowest gas fractions, and highest dust temperatures of the galaxy sample, compared to typical SFGs at the same stellar mass and redshift. They are also very massive, accounting for ∼ 60% of the most massive galaxies in the sample (log(M * /M ) > 11.0). We find trends between the areas of the ongoing star formation regions and the derived physical properties for the sample, unveiling the role of compact star formation as a physical driver of these properties. Starbursts in the main sequence appear to be the extreme cases of these trends. We discuss possible scenarios of galaxy evolution to explain the results drawn from our galaxy sample. Our findings suggest that the star formation rate is sustained in SFGs by gas and star formation compression, keeping them within the main sequence even when their gas fractions are low and they are presumably on the way to quiescence.

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“…A proxy for radiation field intensity is the SFR surface density, Σ SFR , indicating the compactness of the star forming region. The effect of Σ SFR on dust temperature is shown in previous observational studies (Lehnert & Heckman 1996;Chanial et al 2007;Burnham et al 2021), as well as the theoretical models of De Rossi et al (2018). In the latter study, a "bluer" SED is produced by increasing star formation efficiency, which is accompanied by a decrease in the virial radius, and hence an increase in luminosity density.…”

Section: Possible Physical Causes For the Elevated Warmmentioning

confidence: 65%

IR SED and Dust Masses of Sub-solar Metallicity Galaxies at z~2.3

Shivaei,

Popping,

Rieke

et al. 2022

Preprint

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We present results from ALMA 1.2 mm continuum observations of a sample of 27 star-forming galaxies at z = 2.1 − 2.5 from the MOSFIRE Deep Evolution Field (MOSDEF) survey. These galaxies have gas-phase metallicity and star-formation rate measurements from Hβ, [Oiii], Hα, and [Nii]. Using stacks of Spitzer, Herschel, and ALMA photometry (rest-frame ∼ 8 − 400 µm), we examine the IR SED of high-redshift subsolar metallicity (∼ 0.5 Z ) LIRGs. We find that the data agree well with an average SED template of higher luminosity local low-metallicity dwarf galaxies (reduced χ 2 of 1.8). When compared with the commonly used templates for solar-metallicity local galaxies or highredshift LIRGs and ULIRGs, even in the most favorable case (with reduced χ 2 of 2.8), the templates are rejected at > 98% confidence level. The broader and hotter IR SED of both the local dwarfs and high-redshift subsolar metallicity galaxies may result from different grain properties, a clumpy dust geometry, or a harder/more intense ionizing radiation field that heats the dust to higher temperatures. The obscured SFR indicated by the FIR emission of the subsolar metallicity galaxies is only ∼ 60% of the total SFR, which is considerably lower than that of the local LIRGs with ∼ 96 − 97% obscured fractions. Due to the evolving IR SED shape, the local LIRG templates fit to mid-IR data can overestimate the Rayleigh-Jeans tail measurements at z ∼ 2 by a factor of 2 − 20, and these templates underestimate IR luminosities if fit to the observed ALMA fluxes by > 0.4 dex. At a given stellar mass or metallicity, dust masses at z ∼ 2.3 are an order of magnitude higher than those at z ∼ 0. Given the predicted molecular gas mass fractions, the observed z ∼ 2.3 dust-to-stellar mass ratios suggest lower dust-to-molecular gas masses than in local galaxies at the same metallicity. CO observations are necessary to better constrain the molecular gas content of sub-solar metallicity galaxies at z > 1.

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The Physical Drivers of the Luminosity-weighted Dust Temperatures in High-redshift Galaxies

Cited by 13 publications

References 74 publications

First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

First Light And Reionisation Epoch Simulations (FLARES) II: The Photometric Properties of High-Redshift Galaxies

GOODS-ALMA 2.0: Starbursts in the main sequence reveal compact star formation regulating galaxy evolution prequenching

IR SED and Dust Masses of Sub-solar Metallicity Galaxies at z~2.3

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