The Evolving Interstellar Medium of Star-forming Galaxies, as Traced by Stardust*

Kokorev, Vasily; Magdis, G.; Davidzon, I.; Brammer, Gabriel; Valentino, F.; Daddi, E.; Ciesla, L.; Liu, Daizhong; Jin, S.; Cortzen, Isabella; Delvecchio, I.; Giménez-Arteaga, Clara; Gómez-Guijarro, Carlos; Sargent, M.; Toft, Sune; Weaver, John R.

doi:10.3847/1538-4357/ac18ce

Cited by 39 publications

(33 citation statements)

References 212 publications

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“…the COSMOS sample has higher fitted τ f B , indicating a higher average M dust , compared to SDSS and GAMA at similar M * , our results imply a correlation between the M dust -M * ratio and redshift, which is consistent with the literature (e.g., Liu et al 2019;Magnelli et al 2020;Kokorev et al 2021).…”

Section: Evolution Of Dust Propertiessupporting

confidence: 91%

“…We compare the fitted values for r bulge to the average and 32-68th percentile of the bulge-to-total distribution of the selected samples, labeled as data. galaxies with higher M * have higher M dust (e.g., Liu et al 2019;Magnelli et al 2020;Kokorev et al 2021) hinting at the paired production of stars and dust (e.g., De Vis et al 2017;Pastrav 2020). The correlation with µ * is similar to the Grootes et al (2013) relation for low-z galaxies but deviates for high-µ * galaxies and high-z because the T04 model is unable to cover the high τ B estimated by the Grootes et al (2013) relation for these bins.…”

Section: Dependence Of Model Parameters On Galaxy Propertiesmentioning

confidence: 99%

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Probing star formation and ISM properties using galaxy disk inclination

Giessen

Leslie

Groves

et al. 2022

A&A

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Attenuation by dust severely impacts our ability to obtain unbiased observations of galaxies, especially as the amount and wavelength dependence of the attenuation varies with the stellar mass M*, inclination i, and other galaxy properties. In this study, we used the attenuation – inclination models in ultraviolet, optical, and near-infrared bands designed by Tuffs and collaborators to investigate the average global dust properties in galaxies as a function of M*, the stellar mass surface density μ*, the star-formation rate SFR, the specific star-formation rate sSFR, the star-formation main-sequence offset dMS, and the star-formation rate surface density ΣSFR at redshifts z ∼ 0 and z ∼ 0.7. We used star-forming galaxies from the Sloan Digital Sky Survey (∼20 000) and Galaxy And Mass Assembly (∼2000) to form our low-z sample at 0.04 < z < 0.1 and star-forming galaxies from Cosmological Evolution Survey (∼2000) for the sample at 0.6 < z < 0.8. We found that galaxies at z ∼ 0.7 have a higher optical depth τBf and clumpiness F than galaxies at z ∼ 0. The increase in F hints that the stars of z ∼ 0.7 galaxies are less likely to escape their birth cloud, which might indicate that the birth clouds are larger. We also found that τBf increases with M* and μ*, independent of the sample and therefore redshift. We found no clear trends in τBf or F with the SFR, which could imply that the dust mass distribution is independent of the SFR. In turn, this would imply that the balance of dust formation and destruction is independent of the SFR. Based on an analysis of the inclination dependence of the Balmer decrement, we found that reproducing the Balmer line emission requires not only a completely optically thick dust component associated with star-forming regions, as in the standard model, but an extra component of an optically thin dust within the birth clouds. This new component implies the existence of dust inside H II regions that attenuates the Balmer emission before it escapes through gaps in the birth cloud and we found it is more important in high-mass galaxies. These results will inform our understanding of dust formation and dust geometry in star-forming galaxies across redshift.

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Section: Evolution Of Dust Propertiessupporting

confidence: 91%

Section: Dependence Of Model Parameters On Galaxy Propertiesmentioning

confidence: 99%

Probing star formation and ISM properties using galaxy disk inclination

Giessen

Leslie

Groves

et al. 2022

A&A

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“…For the galaxies with a Herschel counterpart (69/88) we employed the panchromatic SED fitting tool Stardust 2 developed by Kokorev et al (2021). In summary, this code performs a multi-component fit that combines linearly stellar libraries, AGN torus templates, and IR models of dust emission from star formation.…”

Section: Infrared Sed Fittingmentioning

confidence: 99%

“…Investigation of the evolution of the cold gas density has uncovered that it closely follows the evolution of the SFR density (e.g., Riechers et al 2019;Decarli et al 2019;Magnelli et al 2020). In the last decade, numerous studies have progressively revealed the increase in the gas content and decrease in the depletion timescales with increasing redshift (e.g., Daddi et al 2008Daddi et al , 2010Tacconi et al 2010;Genzel et al 2010;Magdis et al 2012;Béthermin et al 2015;Dessauges-Zavadsky et al 2020;Donevski et al 2020;Kokorev et al 2021). More recently, large statistical galaxy samples have established the gas scaling relations for the gas fractions ( f gas = M gas /(M gas + M * )) and depletion timescales (τ dep = M gas /SFR), with their dependencies on a specific star formation rate (sSFR = SFR/M * ), stellar mass, as well as lookback time (e.g., Scoville et al 2017;Tacconi et al 2018;Liu et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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

Gómez-Guijarro

Elbaz

Xiao

et al. 2022

A&A

Self Cite

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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 arcmin2 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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“…We fit the available photometry from UV to mm wavelengths with the SED-fitting code STARDUST 108 , which models the emission from stars, active galactic nucleus (AGN), and infrared emission arising from dust heated by star formation. The method does not rely on energy balance assumptions, and rather fits an independent linear combination of templates.…”

Section: Uv-millimeter Sed Fittingmentioning

confidence: 99%

A dusty compact object bridging galaxies and quasars at cosmic dawn

Fujimoto,

Brammer,

Watson

et al. 2022

Preprint

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The Evolving Interstellar Medium of Star-forming Galaxies, as Traced by Stardust*

Cited by 39 publications

References 212 publications

Probing star formation and ISM properties using galaxy disk inclination

Probing star formation and ISM properties using galaxy disk inclination

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

A dusty compact object bridging galaxies and quasars at cosmic dawn

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