RADIAL DISTRIBUTION OF STARS, GAS, AND DUST IN SINGS GALAXIES. II. DERIVED DUST PROPERTIES

By J. Muńoz-Mateos, A. Paz, S. Boissier, J. Zamorano, D. Dale, P. Pérez-González, J. Gallego, B. Madore, G. Bendo, M. Thornley and 28 more. 2009

178 citations recorded by the source corpus.

We present a detailed analysis of the radial distribution of dust properties in the SINGS sample, performed on a set of ultraviolet (UV), infrared (IR), and H i surface brightness profiles, combined with published molecular gas profiles and metallicity gradients. The internal extinction, derived from the total-IR (TIR)-to-far-UV (FUV) luminosity ratio, decreases with radius, and is larger in Sb–Sbc galaxies. The TIR-to-FUV ratio correlates with the UV spectral slope β, following a sequence shifted to redder UV colors with respect to that of starbursts. The star formation history (SFH) is identified as the main driver of this departure. Both LTIR/LFUV and β correlate well with metallicity, especially in moderately face-on galaxies. The relation shifts to redder colors with increased scatter in more edge-on objects. By applying physical dust models to our radial spectral energy distributions, we have derived radial profiles of the total dust mass surface density, the fraction of the total dust mass contributed by polycyclic aromatic hydrocarbons (PAHs), and the intensity of the radiation field heating the grains. The dust profiles are exponential, their radial scale length being constant from Sb to Sd galaxies (only ∼10% larger than the stellar scale length). Many S0/a–Sab galaxies have central depressions in their dust radial distributions. The PAH abundance increases with metallicity for 12 + log(O/H) < 9, and at larger metallicities the trend flattens and even reverses, with the SFH being a plausible underlying driver for this behavior. The dust-to-gas ratio is also well correlated with metallicity and therefore decreases with galactocentric radius. Although most of the total emitted IR power (especially in the outer regions of disks) is contributed by dust grains heated by diffuse starlight with a similar intensity as the local Milky Way radiation field, a small amount of the dust mass (∼1%) is required to be exposed to very intense starlight in order to reproduce the observed fluxes at 24 μm, accounting for ∼10% of the total integrated IR power.

Subfields: Astronomy and Astrophysics, Instrumentation

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In Astronomy and Astrophysics

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Citations in the corpus

• MOLECULAR GAS AND STAR FORMATION IN NEARBY DISK GALAXIES (2013, methodology): “The dust-to-gas ratio derived from Spitzer observations of low metallicity regions appears somewhat lower than one would predict from a linear scaling of their metallicity (Muñoz-Mateos et al. 2009).”
• 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. 2011).”
• The CO-to-H2 Conversion Factor (2013, background): “Very importantly for CO emission, the low metal abundance in these systems implies lower C and O abundances and low dust-to-gas ratios (e.g., Draine et al. 2007; Muñoz-Mateos et al. 2009).”
• The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, background): “…UV slope is sensitive to metallicity and star-formation history (e.g., Kong et al. 2004; Seibert et al. 2005; Johnson et al. 2007; Dale et al. 2009; Muñoz-Mateos et al. 2009; Reddy et al. 2010; Wilkins et al. 2011; Boquien et al. 2012; Reddy et al. 2012b; Schaerer et al. 2013; Wilkins et al.…”
• RECONSTRUCTING THE STELLAR MASS DISTRIBUTIONS OF GALAXIES USING S4G IRAC 3.6 AND 4.5 μm IMAGES. I. CORRECTING FOR CONTAMINATION BY POLYCYCLIC AROMATIC HYDROCARBONS, HOT DUST, AND INTERMEDIATE-AGE STARS (2011, methodology): “…NGC 4321 and NGC 5194 (M51) (see Table 1), were chosen for their range of morphological properties, dust contents, and star formation histories from SINGS (Kennicutt et al. 2003 and see, e.g., Draine et al. 2007, Calzetti 2007, Bendo et al. 2008, Muñoz-Mateos et al. 2009b, Moustakas et al. 2010).”
• Probing the dust properties of galaxies up to submillimetre wavelengths. II. Dust-to-gas mass ratio trends with metallicity and the submm excess in dwarf galaxies (2011, background): “…knowledge of the dust properties of the ISM such as the distribution of the different dust components (polycyclic aromatic hydrocarbons (PAHs), silicate, graphite) and how they are affected by metallicity (Galliano et al. 2008; Engelbracht et al. 2008; Bendo et al. 2008; Muñoz-Mateos et al. 2009).”
• Modelling the spectral energy distribution of galaxies - V. The dust and PAH emission SEDs of disk galaxies (2010, background): “From resolved studies of galaxies it was also found that there is a large scale distributionof diffuse dust having a face-on opacity that decreases with radius (Boissier et al. 2004, Popescu et al. 2005, Pérez-González et al. 2006, Boissier et al. 2007, Muñoz-Mateos et al. 2009).”
• THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCE z = 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS (2012, background): “Finally, while the Leroy et al. (2011) sample yields a slope of −1.0 in the δGDR−Z relation, Muñoz-Mateos et al (2009), find a rather steeper slope of -2.45.”
• THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS). I. A CLOUD-SCALE/MULTI-WAVELENGTH VIEW OF THE INTERSTELLAR MEDIUM IN A GRAND-DESIGN SPIRAL GALAXY (2013, background): “Muñoz-Mateos et al. (2009) studied the radial profile of the dust emission in the SINGS sample, including M 51.”
• THE CO-TO-H2 CONVERSION FACTOR FROM INFRARED DUST EMISSION ACROSS THE LOCAL GROUP (2011, methodology): “Our focus on star-forming regions likely biases us towards high δGDR; studies of all material find a steeper relation (Lisenfeld & Ferrara 1998; Muñoz-Mateos et al. 2009).”
• ESTIMATING THE STAR FORMATION RATE AT 1 kpc SCALES IN NEARBY GALAXIES (2012, methodology): “See Muñoz-Mateos et al. (2009a) for more details.”
• The dust scaling relations of the Herschel Reference Survey (2012, methodology): “…if the dust disk is significantly less extended than the gas disk (Thomas et al. 2004) or, in other words, if the dust-to-gas ratio decreases monotonically with increasing distance from the center of galaxies (Bendo et al. 2010; Muñoz-Mateos et al. 2009; Pohlen et al. 2010; Magrini et al. 2011).”
• THE HERSCHEL REFERENCE SURVEY: DUST IN EARLY-TYPE GALAXIES AND ACROSS THE HUBBLE SEQUENCE (2011, background): “…as the 70µm fluxes are treated as upper limits in our SED fitting; we estimate that including a warm temperature component to fit the MIR–70µm emission would contribute (on average) 3% to the FIR luminosity, though for some sources this can be up to 17%— see also Muñoz-Mateos et al. 2009.)”
• Evolution of the dust emission of massive galaxies up to z=4 and constraints on their dominant mode of star formation (2014, methodology): “The second method is based on the estimate of the dust mass, which is then converted into gas mass using the locally-calibrated relation between the gas-to-dust ratio and the gas metallicity (e.g., Muñoz-Mateos et al. 2009; Leroy et al. 2011; Rémy-Ruyer et al. 2014).”
• THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, methodology): “Motivated by this, we attempt to estimate the stellar contribution beyond 5 µm, as some authors have done (e.g., Draine et al. 2007; Muñoz-Mateos et al. 2009a).”
• THE GREAT OBSERVATORIES ALL-SKY LIRG SURVEY: COMPARISON OF ULTRAVIOLET AND FAR-INFRARED PROPERTIES (2010, background): “Muñoz-Mateos et al. (2009) examined radial profiles of all available SINGS galaxies and found that star formation history is the primary driver determining the position on the IRX-β diagram of a radial annulus within a galaxy.”
• OPTICAL SPECTROSCOPY AND NEBULAR OXYGEN ABUNDANCES OF THE SPITZER/SINGS GALAXIES (2010, methodology): “The photometry in Muñoz-Mateos et al. (2009a) for 54/75 galaxies is based on a careful curve-of-growth analysis and recalibration of imaging available in the literature (Prugniel & Heraudeau 1998; Dale et al. 2007).”
• Empirical determination of the shape of dust attenuation curves in star-forming galaxies (2011, background): “…stars, there is a diffuse component exhibitingstrong radial gradients (e.g. Persson & Helou 1987; Peletier et al.1995; Boissier et al. 2004; Muñoz-Mateos et al. 2009), and there is some evidence that diffuse interstellar dust is distributed throughout the disk with a smaller scaleheight…”
• LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, background): “In typical spirals, the dust-to-gas ratio and internal extinction (AFUV) decline steadily with radius (Muñoz-Mateos et al. 2009), meaning that for ram pressure stripping events where gas is removed from the outside in, the more extended unobscured star formation component should be preferentially…”