Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample

By B. Draine, D. Dale, G. Bendo, K. Gordon, John-David T. Smith, Lee Armus, C. Engelbracht, G. Helou, Robert C. Kennicutt Jr., Aigen Li and 10 more. 2007

815 citations recorded by the source corpus.

Physical dust models are presented for 65 galaxies in SINGS that are strongly detected in the four IRAC bands and three MIPS bands. For each galaxy we estimate (1) the total dust mass, (2) the fraction of the dust mass contributed by PAHs, and (3) the intensity of the starlight heating the dust grains. We find that spiral galaxies have dust properties resembling the dust in the local region of the Milky Way, with similar dust-to-gas ratio and similar PAH abundance. The observed SEDs, including galaxies with SCUBA photometry, can be reproduced by dust models that do not require "cold" (T ≲ 10 K) dust. The dust-to-gas ratio is observed to be dependent on metallicity. In the interstellar media of galaxies with AO ≡ 12 +(O/H) > 8.1, grains contain a substantial fraction of interstellar Mg, Si, and Fe. Galaxies with AO < 8.1 and extended H I envelopes in some cases appear to have global dust-to-gas ratios that are low for their measured oxygen abundance, but the dust-to-gas ratio in the regions where infrared emission is detected generally appears to be consistent with a substantial fraction of interstellar Mg, Si, and Fe being contained in dust. The PAH index qPAH, the fraction of the dust mass in the form of PAHs, correlates with metallicity. The nine galaxies in our sample with AO < 8.1 have a median qPAH = 1.0%, whereas galaxies with AO > 8.1 have a median qPAH = 3.55%. The derived dust masses favor a value XCO ≈ 4 × 1020 cm-2 (K km s-1)-1 for the CO-to-H2 conversion factor. Except for some starbursting systems (Mrk 33, Tol 89, NGC 3049), dust in the diffuse ISM dominates the IR power.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a2fba342a2464f6f281a2e570a03e70d29abaf3f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Somerville
4. R. Dav'e
5. C. Conroy
6. A. Dekel
7. T. Naab
8. D. Narayanan

Citations in the corpus

• The Resolved Properties of Extragalactic Giant Molecular Clouds (2008, neutral): “The metallicity for this galaxy is uncertain, but the polycyclic aromatic hydrocarbon abundance and dust-to-gas ratios derived by Draine et al. (2007) suggests it is similar to Galactic.”
• The Horizon-AGN simulation: evolution of galaxy properties over cosmic time (2016, methodology): “The gas density and metallicity are extracted, under the assumption that the dust mass scales with the gas metal mass, with a dust-to-metal ratio of 0.4 (e.g. Dwek 1998; Draine et al. 2007).”
• Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample (2009, methodology): “For 13 sample galaxies Ldust determinations are also available by Draine et al. (2007) who derived them from the SINGS IR SEDs using the Draine & Li (2007) dust models.”
• ISM MASSES AND THE STAR FORMATION LAW AT Z = 1 TO 6: ALMA OBSERVATIONS OF DUST CONTINUUM IN 145 GALAXIES IN THE COSMOS SURVEY FIELD (2015, methodology): “Often, the far infrared SEDs are analyzed by fitting either modified black body curves or libraries of dust SEDs to the observed SEDs (e.g. Draine et al. 2007; da Cunha & Charlot 2011; Magdis et al. 2012a,b).”
• COLD GASS, an IRAM legacy survey of molecular gas in massive galaxies – I. Relations between H2, H i, stellar content and structural properties (2011, methodology): “Our choice of αCO is roughly the mean of values estimated in the Milky Way and in nearby galaxies (e.g. Strong & Mattox 1996; Dame, Hartmann & Thaddeus 2001; Blitz et al. 2007; Draine et al. 2007; Heyer et al. 2009; Abdo et al. 2010).”
• Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey (2014, methodology): “A good correlation is found between the Umin parameter, which is the intensity of the diffuse ISRF (Draine et al. 2007; Aniano et al. 2012), and the Hα surface brightness (ρ =0.70), and a moderate anti-correlation between Umin and the H-band Ciesla et al.: SED fitting of the Herschel Reference Surve”
• STRUCTURE AND FORMATION OF ELLIPTICAL AND SPHEROIDAL GALAXIES (2008, background): “A not-yet-relaxed merger in progress (Schweizer & Seitzer 1992), the observation of nuclear dust (Rest et al. 2001; Lauer et al. 2005; Draine et al. 2007) – which prevents us from classifying the central profile – suggests that the merger involved some cold gas.”
• Investigations of dust heating in M81, M83 and NGC 2403 with the Herschel Space Observatory (2011, background): “…findings fromradiative transfer models (e.g. da Cunha et al. 2008; Bianchi 2008; Popsecu et al. 2011) as well as other dust emission models (e.g. Draine et al. 2007) that had suggested that dust absoprtion and emission can only be accurately modelled if it contains a dust component heated by…”
• DISCOVERY OF AN ACTIVE GALACTIC NUCLEUS DRIVEN MOLECULAR OUTFLOW IN THE LOCAL EARLY-TYPE GALAXY NGC 1266 (2011, methodology): “Draine et al. (2007) derive a total dust mass of 1.02 × 107 M⊙ in NGC 1266 (rescaled to our distance of 29.9 Mpc), using Spitzer Infrared Nearby Galaxy Survey (SINGS) data.”
• Three-Dimensional Dust Radiative Transfer ∗ (2013, background): “The emission from small grains is necessary to explain the observed MIR emission of many objects (see, e.g., Boulanger & Perault 1988, Draine et al. 2007, Helou et al. 2000, Sellgren 1984, Smith et al. 2007).”
• The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types (2014, background): “2006; Madden et al. 2006; Draine et al. 2007; Engelbracht et al. 2008; Galliano et al. 2008), while the abundance of very small grains grows drastically relative to the large grain population due to the fragmentation of those large grains through shocks experienced in the turbulent ISM (Jones et…”
• ANDROMEDA'S DUST (2013, background): “However, as noted by Draine et al. (2007), this dust mass/ H is in mild conflict with elemental abundances in the solarneighborhood ISM: the total mass of elements “depleted” from the gas in the diffuse ISM is estimated to be less than what would be calculated for the WD01 dust model with the above…”
• THE EVOLUTION OF INTERSTELLAR MEDIUM MASS PROBED BY DUST EMISSION: ALMA OBSERVATIONS AT z = 0.3–2 (2014, background): “However, we note that Draine et al. (2007) see no variation in the dust abundance down to ∼ 20% of solar metallicity and it is reassuring that the low z sample and the high z SMGs yield similar α850µm.”
• Molecular line emission in NGC 1068 imaged with ALMA: I. An AGN-driven outflow in the dense molecular gas (2014, methodology): “Applying the linear dust/gas scaling ratio of Draine et al. (2007) (see also Sandstrom et al. 2013) to the gas-phase oxygen abundances measured in the central 2 kpc of NGC 1068 (∼ 12+log (O/H)∼ 8.8; Pilyugin et al. 2004, 2007), which yields a gas–to–dust mass ratio of ∼ 60+30−30, we estimate that…”
• Gas-to-dust mass ratios in local galaxies over a 2 dex metallicity range (2013, background): “…studied over the past decades (e.g., Issa et al. 1990; Lisenfeld & Ferrara 1998; Hirashita et al. 2002; James et al. 2002; Hunt et al. 2005; Draine et al. 2007; Engelbracht et al. 2008; Galliano et al. 2008; Muñoz-Mateos et al. 2009; Bendo et al. 2010; Galametz et al. 2011; Magrini et al.…”
• Fitting the integrated spectral energy distributions of galaxies (2010, background): “Simpler IR emission models assume a functional form of dust mass over heating intensity; dMd = f (U)dU , with f (U) most often assumed to be a power law (see e.g. Dale et al. 2001; Dale and Helou 2002; Draine et al. 2007).”
• MOLECULAR GAS AND STAR FORMATION IN NEARBY DISK GALAXIES (2013, background): “…using only Spitzer do scatter by ≈ 0.3 dex (a factor of two) compared to Herschelbased dust masses and show weak systematic trends with the sense that Spitzer underestimates the mass of cooler (∼ 15 K) dust in the outskirts of galaxies (both consistent with the analysis of Draine et al. 2007).”