Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample

Aniano, G.; Draine, B. T.; Hunt, L. K.; Sandström, Karin; Calzetti, Daniela; Kennicutt, Robert C.; Dale, Daniel A.; Galametz, M.; Gordon, K. D.; Leroy, Adam K.; Smith, J. D.; Roussel, H.; Sauvage, M.; Walter, Fabian; Armus, L.; Bolatto, Alberto D.; Boquien, M.; Crocker, Alison F.; Looze, I. De; Meyer, Jennifer Donovan; Hélou, G.; Hinz, J. L.; Johnson, Benjamin D.; Koda, Jin; Miller, Amy E. Stevens; Montiel, Edward; Murphy, E. J.; Relaño, M.; Rix, Hans─Walter; Schinnerer, E.; Skibba, Ramin; Wolfire, M. G.; Engelbracht, C. W.

doi:10.3847/1538-4357/ab5fdb

Cited by 83 publications

(71 citation statements)

References 100 publications

(85 reference statements)

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“…(1) Far-IR line fluxes may be suppressed by optically thick continuum absorption (e.g., Scoville et al 2017a (Okada et al 2013;Salgado et al 2016), the Large Magellanic Cloud (Lebouteiller et al 2012;Chevance et al 2016), and local galaxies (Croxall et al 2012;Abdullah et al 2017;Bigiel et al 2020). (4) Metallicity may influence the strength of cooling lines and the PAHs (Cormier et al 2015;Smith et al 2017;Croxall et al 2017;Cormier et al 2019;Aniano et al 2020). However, direct effects on the PAH grains appear most pronounced at metallicities well below those seen in GOALS galaxies, which typically have Z/Z e ∼ 1-2 (Inami et al 2013;Díaz-Santos et al 2017).…”

Section: Alternative Explanations For Decreasing ò Pe With σ Irmentioning

confidence: 99%

Regulating Star Formation in Nearby Dusty Galaxies: Low Photoelectric Efficiencies in the Most Compact Systems

McKinney

Armus

Pope

et al. 2021

ApJ

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Star formation in galaxies is regulated by heating and cooling in the interstellar medium (ISM). In particular, the processing of molecular gas into stars will depend strongly on the ratio of gas heating to gas cooling in the neutral gas around sites of recent star formation. In this work, we combine mid-infrared (mid-IR) observations of polycyclic aromatic hydrocarbons (PAHs), the dominant heating mechanism of gas in the ISM, with [C II], [O I], and [Si II] fine-structure emission, the strongest cooling channels in dense, neutral gas. The ratio of IR cooling line emission to PAH emission measures the photoelectric efficiency, a property of the ISM which dictates how much energy carried by ultraviolet photons gets transferred into the gas. We find that star-forming, IR-luminous galaxies in the Great Observatories All-Sky LIRG Survey with high IR surface densities have low photoelectric efficiencies. These systems also have, on average, higher ratios of radiation field strength to gas densities, and larger average dust grain size distributions. The data support a scenario in which the most compact galaxies have more young starforming regions per unit area that exhibit less efficient gas heating. These conditions may be more common at high z, and may help explain the higher star formation rates at cosmic noon. We make predictions on how this can be investigated with the James Webb Space Telescope.

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Section: Alternative Explanations For Decreasing ò Pe With σ Irmentioning

confidence: 99%

Regulating Star Formation in Nearby Dusty Galaxies: Low Photoelectric Efficiencies in the Most Compact Systems

McKinney

Armus

Pope

et al. 2021

ApJ

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“…18 The suffixes of model labels represent the total C abundance (per H nucleus) in ppm, e.g., MW3.1_60 means 60 ppm C/H in PAHs in this model (Weingartner & Draine 2001). Since the publication of the Draine & Li (2007) model, observations have suggested that the dust/gas ratio used in this model is systematically overestimated (Aniano et al 2020). Aniano et al (2020) found that a typical correction of ∼0.62 should be applied to dust mass derived from the Draine & Li (2007) model for their sample.…”

Section: Variations In Ssp Modelsmentioning

confidence: 99%

“…Since the publication of the Draine & Li (2007) model, observations have suggested that the dust/gas ratio used in this model is systematically overestimated (Aniano et al 2020). Aniano et al (2020) found that a typical correction of ∼0.62 should be applied to dust mass derived from the Draine & Li (2007) model for their sample. Thus, the conversion from carbon abundance (in ppm) to q PAH should be updated.…”

Section: Variations In Ssp Modelsmentioning

confidence: 99%

The Age Dependence of Mid-infrared Emission around Young Star Clusters

Lin

Calzetti

Kong

et al. 2020

ApJ

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Using the star cluster catalogs from the Hubble Space Telescope program Legacy Extragalactic UV survey (LEGUS) and 8 μm images from the IRAC camera on the Spitzer Space Telescope for five galaxies within 5 Mpc, we investigate how the 8 μm dust luminosity correlates with the stellar age on the 30-50 pc scale of star-forming regions. We construct a sample of 97 regions centered at local peaks of 8 μm emission, each containing one or more young star cluster candidates from the LEGUS catalogs. We find a tight anticorrelation with a Pearson correlation coefficient of r=−0.84±0.05 between the mass-normalized dust-only 8 μm luminosity and the age of stellar clusters younger than 1 Gyr; the 8 μm luminosity decreases with increasing age of the stellar population. Simple assumptions on a combination of stellar and dust emission models reproduce the observed trend. We also explore how the scatter of the observed trend depends on assumptions of stellar metallicity, polycyclic aromatic hydrocarbon (PAH) abundance, fraction of stellar light absorbed by dust, and instantaneous versus continuous star formation models. We find that variations in stellar metallicity have little effect on the scatter, while PAH abundance and the fraction of dust-absorbed light bracket the full range of the data. We also find that the trend is better explained by continuous star formation, rather than instantaneous burst models. We ascribe this result to the presence of multiple star clusters with different ages in many of the regions. Upper limits of the dust-only 8 μm emission as a function of age are provided.

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“…Although observational studies sometimes approximate galaxies' dust SEDs by one or two components in modifiedblackbody fitting, physical models based on assuming PDFs for the ISRF have been proposed and calculated by Dale et al (2001), Dale & Helou (2002), Li & Draine (2002), and (Draine & Li 2007, hereafter DL07). See also subsequent applications in Draine et al ( , 2014, Aniano et al (2012Aniano et al ( , 2020, Magdis et al (2012), Daddi et al (2015), Dale et al (2017), and Schreiber et al (2018).…”

Section: Introductionmentioning

confidence: 99%

CO Excitation, Molecular Gas Density, and Interstellar Radiation Field in Local and High-redshift Galaxies

Liu

Daddi

Schinnerer

et al. 2021

ApJ

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We study the carbon monoxide (CO) excitation, mean molecular gas density, and interstellar radiation field (ISRF) intensity in a comprehensive sample of 76 galaxies from local to high redshift (z ∼ 0–6), selected based on detections of their CO transitions J = 2 → 1 and 5 → 4 and their optical/infrared/(sub)millimeter spectral energy distributions (SEDs). We confirm the existence of a tight correlation between CO excitation as traced by the CO (5–4)/(2–1) line ratio R 52 and the mean ISRF intensity U as derived from infrared SED fitting using dust SED templates. By modeling the molecular gas density probability distribution function (PDF) in galaxies and predicting CO line ratios with large velocity gradient radiative transfer calculations, we present a framework linking global CO line ratios to the mean molecular hydrogen gas density n H 2 and kinetic temperature T kin. Mapping in this way observed R 52 ratios to n H 2 and T kin probability distributions, we obtain positive U – n H 2 and U –T kin correlations, which imply a scenario in which the ISRF in galaxies is mainly regulated by T kin and (nonlinearly) by n H 2 . A small fraction of starburst galaxies showing enhanced n H 2 could be due to merger-driven compaction. Our work demonstrates that ISRF and CO excitation are tightly coupled and that density–PDF modeling is a promising tool for probing detailed ISM properties inside galaxies.

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Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample

Cited by 83 publications

References 100 publications

Regulating Star Formation in Nearby Dusty Galaxies: Low Photoelectric Efficiencies in the Most Compact Systems

Regulating Star Formation in Nearby Dusty Galaxies: Low Photoelectric Efficiencies in the Most Compact Systems

The Age Dependence of Mid-infrared Emission around Young Star Clusters

CO Excitation, Molecular Gas Density, and Interstellar Radiation Field in Local and High-redshift Galaxies

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