THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY

By R. Skibba, C. Engelbracht, D. Dale, J. Hinz, S. Zibetti, A. Crocker, B. Groves, L. Hunt, Benjamin D. Johnson, S. Meidt and 22 more. 2011

132 citations recorded by the source corpus.

Using new far-infrared imaging from the Herschel Space Observatory with ancillary data from ultraviolet (UV) to submillimeter wavelengths, we estimate the total emission from dust and stars of 62 nearby galaxies in the KINGFISH survey in a way that is as empirical and model independent as possible. We collect and exploit these data in order to measure from the spectral energy distributions (SEDs) precisely how much stellar radiation is intercepted and re-radiated by dust, and how this quantity varies with galaxy properties. By including SPIRE data, we are more sensitive to emission from cold dust grains than previous analyses at shorter wavelengths, allowing for more accurate estimates of dust temperatures and masses. The dust/stellar flux ratio, which we measure by integrating the SEDs, has a range of nearly three decades (from 10−2.2 to 100.5). The inclusion of SPIRE data shows that estimates based on data not reaching these far-IR wavelengths are biased low by 17% on average. We find that the dust/stellar flux ratio varies with morphology and total infrared (IR) luminosity, with dwarf galaxies having faint luminosities, spirals having relatively high dust/stellar ratios and IR luminosities, and some early types having low dust/stellar ratios. We also find that dust/stellar flux ratios are related to gas-phase metallicity ( and −0.22 ± 0.12 for metal-poor and intermediate-metallicity galaxies, respectively), while the dust/stellar mass ratios are less so (differing by ≈0.2 dex); the more metal-rich galaxies span a much wider range of the flux ratios. In addition, the substantial scatter between dust/stellar flux and dust/stellar mass indicates that the former is a poor proxy of the latter. Comparing the dust/stellar flux ratios and dust temperatures, we also show that early types tend to have slightly warmer temperatures (by up to 5 K) than spiral galaxies, which may be due to more intense interstellar radiation fields, or possibly to different dust grain compositions. Finally, we show that early types and early-type spirals have a strong correlation between the dust/stellar flux ratio and specific star formation rate, which suggests that the relatively bright far-IR emission of some of these galaxies is due to ongoing (if limited) star formation as well as to the radiation field from older stars, which is heating the dust grains.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/70320314fa7e164e52b61a10265cb1c30bde93d7

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Citations in the corpus

THE HERSCHEL REFERENCE SURVEY: DUST IN EARLY-TYPE GALAXIES AND ACROSS THE HUBBLE SEQUENCE (2011, background): “(Kennicutt et al. 2011) results based on 10 nearby early types (Skibba et al. 2011).”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, methodology): “…Nearby Galaxies Survey (SINGS; Draine et al. 2007), with stellar masses from da Cunha et al. (2008)14 and from the Herschel KINGFISH survey (Skibba et al. 2011).15 These samples were selected to be representative of normal galaxies at z ∼ 0 (Kennicutt et al. 2003); therefore, their dust…”
The dust scaling relations of the Herschel Reference Survey (2012, background): “5, theMdust/M∗ ratio rapidly decreases when moving from late- to early-type galaxies (see also Skibba et al. 2011).”
Gas-to-dust mass ratios in local galaxies over a 2 dex metallicity range (2013, methodology): “We perform the test for 67 galaxies of the sample, with MHII derived from Hα measurements of Gil de Paz et al. (2003); Kennicutt et al. (2009); Skibba et al. (2011) and found MHII/MHI ∼ 0.2%.”
REGULARITY UNDERLYING COMPLEXITY: A REDSHIFT-INDEPENDENT DESCRIPTION OF THE CONTINUOUS VARIATION OF GALAXY-SCALE MOLECULAR GAS PROPERTIES IN THE MASS-STAR FORMATION RATE PLANE (2013, unknown): “Stellar masses (converted to the Chabrier (2003) scale) and morphological information are taken from the compilations of Skibba et al. (2011) or Leroy et al. (2008, 2009), or from the NASA/IPAC Extragalactic Database (NED)9 if not listed in either of the former.”
HERSCHEL FAR-INFRARED AND SUBMILLIMETER PHOTOMETRY FOR THE KINGFISH SAMPLE OF NEARBY GALAXIES (2011, background): “Dunne & Eales (2001) likewise find a factor of two deficiency for single blackbody-based dust masses, in their case compared to the dust mass derived from two (modified) blackbodies (see also Skibba et al. 2011).”
ALMA IMAGING OF GAS AND DUST IN A GALAXY PROTOCLUSTER AT REDSHIFT 5.3: [C ii] EMISSION IN “TYPICAL” GALAXIES AND DUSTY STARBURSTS ≈1 BILLION YEARS AFTER THE BIG BANG (2014, methodology): “The dust temperatures of the dwarf galaxies used as templates are Tdust≃26–37 K (e.g., Israel et al. 1996b; Skibba et al. 2011), which would require corrections at the few per cent level at most. opacity power law index of β=1.5 yields Mdust<3.1– 9.4×107M⊙,22 where the range indicates the…”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “Herschel surveys will be providing higher resolution [25′′ at 350 µm (Griffin et al. 2010) and 6′′ at 70 µm (Poglitsch et al. 2010)] images of the nearby clouds (André et al. 2010), the Galactic Plane (Molinari et al. 2010), and many other galaxies (e.g., Skibba et al. 2011; Wuyts et al. 2011).”
Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift (2017, background): “The warm components were 51 - 59 K and the cold components had fitted T = 17 - 24 K and the fraction of the total far infrared luminosity in the warm component was 21 - 81%, with a mean value ∼ 50% (see also Skibba et al. 2011; Dale et al. 2012).”