<i>HERSCHEL</i>FAR-INFRARED AND SUBMILLIMETER PHOTOMETRY FOR THE KINGFISH SAMPLE OF NEARBY GALAXIES

Dale, Daniel A.; Aniano, G.; Engelbracht, C. W.; Hinz, J. L.; Krause, O.; Montiel, Edward; Roussel, H.; Appleton, P. N.; Armus, L.; Beirão, P.; Bolatto, Alberto D.; Brandl, Bernhard R.; Calzetti, Daniela; Crocker, Alison F.; Croxall, K. V.; Draine, B. T.; Galametz, M.; Gordon, K. D.; Groves, Brent; Hao, Cai-Na; Hélou, G.; Hunt, L. K.; Johnson, Benjamin D.; Kennicutt, Robert C.; Koda, Jin; Leroy, Adam K.; Li, Y.; Meidt, Sharon E.; Miller, Amy E. Stevens; Murphy, E. J.; Rahman, Nurur; Rix, Hans─Walter; Sandström, Karin; Sauvage, M.; Schinnerer, E.; Skibba, Ramin; Smith, J. D.; Tabatabaei, F. S.; Walter, Fabian; Wilson, C. D.; Wolfire, M. G.; Zibetti, S.

doi:10.1088/0004-637x/745/1/95

Cited by 224 publications

(312 citation statements)

References 55 publications

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“…In this paper, we will also make use of dust mass estimates derived using these more complex models, such as in Sandstrom et al (2013), Rémy-Ruyer et al (2014b), Ciesla et al (2014) and Santini et al (2014). Dale et al (2012) showed that dust masses derived from single temperature MBB fits on far-IR fluxes are about a factor of two lower than those derived using a more complex formalism on the full IR SED. These dust mass discrepancies could be larger for galaxies with colder dust.…”

Section: Measuring Dust Massesmentioning

confidence: 91%

The dust content of galaxies from z = 0 to z = 9

Popping

Somerville

Galametz

2017

Monthly Notices of the Royal Astronomical Society

237

326

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We study the dust content of galaxies from z = 0 to z = 9 in semi-analytic models of galaxy formation that include new recipes to track the production and destruction of dust. We include condensation of dust in stellar ejecta, the growth of dust in the interstellar medium (ISM), the destruction of dust by supernovae and in the hot halo, and dusty winds and inflows. The rate of dust growth in the ISM depends on the metallicity and density of molecular clouds. Our fiducial model reproduces the relation between dust mass and stellar mass from z = 0 to z = 7, the number density of galaxies with dust masses less than 10 8.3 M , and the cosmic density of dust at z = 0. The model accounts for the double power-law trend between dust-togas (DTG) ratio and gas-phase metallicity of local galaxies and the relation between DTG ratio and stellar mass. The dominant mode of dust formation is dust growth in the ISM, except for galaxies with M * < 10 7 M , where condensation of dust in supernova ejecta dominates. The dust-to-metal ratio of galaxies depends on the gasphase metallicity, unlike what is typically assumed in cosmological simulations. Model variants including higher condensation efficiencies, a fixed timescale for dust growth in the ISM, or no growth at all reproduce some of the observed constraints, but fail to simultaneously reproduce the shape of dust scaling relations and the dust mass of high-redshift galaxies.

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Section: Measuring Dust Massesmentioning

confidence: 91%

The dust content of galaxies from z = 0 to z = 9

Popping

Somerville

Galametz

2017

Monthly Notices of the Royal Astronomical Society

237

326

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“…For the spiral galaxies we fitted their IR SEDs using the models of Draine & Li (2007) to the photometry provided by the Kingfish project (Dale et al 2012), in analogy to the procedures used for the BzK galaxies (see Magdis et al 2011Magdis et al , 2012. We use here and in the following only objects for which U could be measured, which limits the sample to six objects in total.…”

Section: What Is the Main Driver Of Co Excitation?mentioning

confidence: 99%

CO excitation of normal star-forming galaxies out toz= 1.5 as regulated by the properties of their interstellar medium

Daddi

Dannerbauer

Liu

et al. 2015

A&A

Self Cite

288

101

484

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We investigate the CO excitation of normal (near-IR selected BzK) star-forming (SF) disk galaxies at z = 1.5 using IRAM Plateau de Bure observations of the CO[2-1], CO , and CO[5-4] transitions for four galaxies, including VLA observations of CO[1-0] for three of them, with the aim of constraining the average state of H 2 gas. By exploiting previous knowledge of the velocity range, spatial extent, and size of the CO emission, we measure reliable line fluxes with a signal-to-noise ratio >4-7 for individual transitions. While the average CO spectral line energy distribution (SLED) has a subthermal excitation similar to the Milky Way (MW) up to CO[3-2], we show that the average CO emission is four times stronger than assuming MW excitation. This demonstrates that there is an additional component of more excited, denser, and possibly warmer molecular gas. The ratio of CO[5-4] to lower-J CO emission is lower than in local (ultra-)luminous infrared galaxies (ULIRGs) and high-redshift starbursting submillimeter galaxies, however, and appears to be closely correlated with the average intensity of the radiation field U and with the star formation surface density, but not with the star formation efficiency. The luminosity of the CO transition is found to be linearly correlated with the bolometric infrared luminosity over four orders of magnitudes. For this transition, z = 1.5 BzK galaxies follow the same linear trend as local spirals and (U)LIRGs and high-redshift star-bursting submillimeter galaxies. The CO[5-4] luminosity is thus empirically related to the dense gas and might be a more convenient way to probe it than standard high-density tracers that are much fainter than CO. We see excitation variations among our sample galaxies that can be linked to their evolutionary state and clumpiness in optical rest-frame images. In one galaxy we see spatially resolved excitation variations, where the more highly excited part of the galaxy corresponds to the location of massive SF clumps. This provides support to models that suggest that giant clumps are the main source of the high-excitation CO emission in high-redshift disk-like galaxies.

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“…It has already been shown that AKARI fluxes are in good agreement with analogous measurements by Spitzer and Herschel (Suzuki et al 2010;Hattori et al 2016), but we nevertheless check the quality of our measurement here by comparing our AKARI 90 and 140 µm flux densities with Spitzer and Herschel measurements. Among our sample, 89 galaxies have published Spitzer 70 µm measurements (Amblard et al 2014), and 22 galaxies have both Herschel 100 and 160 µm measurements (Dale et al 2012;di Serego Alighieri et al 2013;Baes et al 2014). In all cases (AKARI 90 µm vs. Spitzer 70 µm, AKARI 90 µm vs. Herschel 100 µm and AKARI 140 µm vs. Herschel 160 µm), we find that most measurements are consistent within the uncertainties, and that they are proportional with a slope of approximately unity and a small intrinsic scatter of 0.2 dex, thus confirming the reliability of our measurements.…”

Section: Akari All-sky Surveymentioning

confidence: 99%

A star formation study of the ATLAS^3Dearly-type galaxies with the AKARI all-sky survey

Kokusho

Kaneda

Bureau

et al. 2017

A&A

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Context. The star formation properties of early-type galaxies (ETGs) are currently the subject of considerable interest, particularly whether they differ from those of gas-rich spirals. Aims. We perform a systematic study of star formation in a large sample of local ETGs using polycyclic aromatic hydrocarbon (PAH) and dust emission, focusing on the galaxies' star formation rates (SFRs) and star formation efficiencies (SFEs). Methods. Our sample is composed of the 260 ETGs from the ATLAS 3D survey, from which we use the cold gas measurements (H i and CO). The SFRs are estimated from stellar, PAH and dust fits to spectral energy distributions created from new AKARI measurements and literature data from WISE and 2MASS. Results. The mid-infrared luminosities of non-CO-detected galaxies are well correlated with their stellar luminosities, showing that they trace (circum)stellar dust emission. CO-detected galaxies show an excess above these correlations, uncorrelated with their stellar luminosities, indicating that they likely contain PAHs and dust of interstellar origin. PAH and dust luminosities of CO-detected galaxies show tight correlations with their molecular gas masses, and the derived current SFRs are typically 0.01 -1 M ⊙ yr −1 . These SFRs systematically decrease with stellar age at fixed stellar mass, while they correlate nearly linearly with stellar mass at fixed age. The majority of local ETGs follow the same star-formation law as local star-forming galaxies, and their current SFEs do not depend on either stellar mass or age. Conclusions. Our results clearly indicate that molecular gas is fueling current star formation in local ETGs, that appear to acquire this gas via mechanisms regulated primarily by stellar mass. The current SFEs of local ETGs are similar to those of local star-forming galaxies, indicating that their low SFRs are likely due to smaller cold gas fractions rather than a suppression of star formation.

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HERSCHELFAR-INFRARED AND SUBMILLIMETER PHOTOMETRY FOR THE KINGFISH SAMPLE OF NEARBY GALAXIES

Cited by 224 publications

References 55 publications

The dust content of galaxies from z = 0 to z = 9

The dust content of galaxies from z = 0 to z = 9

CO excitation of normal star-forming galaxies out toz= 1.5 as regulated by the properties of their interstellar medium

A star formation study of the ATLAS^3Dearly-type galaxies with the AKARI all-sky survey

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HERSCHELFAR-INFRARED AND SUBMILLIMETER PHOTOMETRY FOR THE KINGFISH SAMPLE OF NEARBY GALAXIES

Cited by 224 publications

References 55 publications

The dust content of galaxies from z = 0 to z = 9

The dust content of galaxies from z = 0 to z = 9

CO excitation of normal star-forming galaxies out toz= 1.5 as regulated by the properties of their interstellar medium

A star formation study of the ATLAS3Dearly-type galaxies with the AKARI all-sky survey

Contact Info

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A star formation study of the ATLAS^3Dearly-type galaxies with the AKARI all-sky survey