Infrared Spectral Energy Distributions of Nearby Galaxies

By D. Dale, G. Bendo, C. Engelbracht, K. Gordon, M. Regan, Lee Armus, J. Cannon, D. Calzetti, B. Draine, G. Helou and 18 more. 2005

214 citations recorded by the source corpus.

The Spitzer Infrared Nearby Galaxies Survey (SINGS) is carrying out a comprehensive multiwavelength survey on a sample of 75 nearby galaxies. The 1-850 μm spectral energy distributions (SEDs) are presented using broadband imaging data from Spitzer, 2MASS, ISO, IRAS, and SCUBA. The infrared colors derived from the globally integrated Spitzer data are generally consistent with the previous generation of models that were developed using global data for normal star-forming galaxies, although significant deviations are observed. Spitzer's excellent sensitivity and resolution also allow a detailed investigation of the infrared SEDs for various locations within the three large, nearby galaxies NGC 3031 (M81), NGC 5194 (M51), and NGC 7331. A wide variety of spectral shapes is found within each galaxy, especially for NGC 3031, the closest of the three targets and thus the galaxy for which the smallest spatial scales can be explored. Strong correlations exist between the local star formation rate and the infrared colors fν(70 μm)/fν(160 μm) and fν(24 μm)/fν(160 μm), suggesting that the 24 and 70 μm emission are useful tracers of the local star formation activity level. Preliminary evidence indicates that variations in the 24 μm emission, and not variations in the emission from polycyclic aromatic hydrocarbons at 8 μm, drive the variations in the fν(8.0 μm)/fν(24 μm) colors within NGC 3031, NGC 5194, and NGC 7331. If the galaxy-to-galaxy variations in SEDs seen in our sample are representative of the range present at high redshift, then extrapolations of total infrared luminosities and star formation rates from the observed 24 μm flux will be uncertain at the factor of 5 level (total range). The corresponding uncertainties using the redshifted 8.0 μm flux (e.g., observed 24 μm flux for a z = 2 source) are factors of 10-20. Considerable caution should be used when interpreting such extrapolated infrared luminosities.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy’s Evolution (SAGE). I. Overview and Initial Results (2006, unknown): “…IRAC mapping of the lowermetallicity LMCwill yield high-resolution insight into recent work on the paucity of PAH emission in low-metallicity galaxies (Madden 2000, 2006; Houck et al. 2004; Engelbracht et al. 2005; Galliano et al. 2005; Dale et al. 2005; Wu et al. 2006; O’Halloran et al. 2006).”
THE CALIBRATION OF MONOCHROMATIC FAR-INFRARED STAR FORMATION RATE INDICATORS (2010, background): “Previous works (Roussel et al. 2001; Boselli, Lequeux & Gavazzi 2004; Förster Schreiber et al. 2004; Calzetti et al. 2005; Dale et al. 2005; Wu et al. 2005; Alonso–Herrero et al. 2006; Perez–Gonzalez et al. 2006; Calzetti et al. 2007; Dale et al. 2007; Relaño et al. 2007; Zhu et al. 2008; Rieke…”
The fundamental properties of galaxies and a new galaxy classification system (2006, background): “For example, we now know that the bulk emission from an average galaxy c© 2002 RAS, MNRAS 000, 1–22 is in the mid infrared (e.g., Dale et al. 2005), and if any wavelength should be used to classify galaxies it would naturally be where most of the light is emitted.”
A simple model to interpret the ultraviolet, optical and infrared emission from galaxies (2008, background): “Also, the infrared Spitzer IRAC and MIPS fluxes include extendedsource aperture corrections (amounting typically to 10 per cent; see Dale et al. 2005, 2007).”
On Extending the Mass-Metallicity Relation of Galaxies by 2.5 Decades in Stellar Mass (2006, background): “As shown in Figure 3, our measured flux densities for the selected SINGS galaxies are consistent with those reported by Dale et al. (2005).”
Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample (2009, methodology): “The listed data comprises theFUV (∼ 1500 Å) andNUV (∼ 2300 Å) filters ofGALEX (Gil de Paz et al. 2007), 2MASS data forJ, H, and Ks (Jarrett et al. 2003), and IRAC and MIPS data for the filters centred on 3.6, 4.5, 5.8, 8.0, 24, 70, and 160µm (Dale et al. 2005).”
The Mid-Infrared Properties of Starburst Galaxies from Spitzer-IRS Spectroscopy (2006, methodology): “These uncertainties are similar to the luminosities derived from theMIPS 24 m flux alone for a large sample of Spitzer Infrared Nearby Galaxies Survey (SINGS) galaxies (Dale et al. 2005).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “…the different dust emission components translate into considerable variations in the dust SEDs within and between galaxies (e.g., Dale & Helou 2002; Dale et al. 2005; Smith et al. 2007), and as a consequence the conversion of infrared luminosities into SFRs must change for different IR wavelengths.”
The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields (2007, methodology): “Furthermore, to extrapolate their conclusions to high redshifts, Dale et al. (2005) make use of the complete set of Dale & Helou (2002) models.”
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, background): “They also show a diversity in PAH emission relative to hot dust, as measured by the ratio 8/24 µm (Table 1), typical for normal star-forming galaxies (Dale et al. 2005).”
THE DISKMASS SURVEY. I. OVERVIEW (2010, unknown): “Based on Dale et al. (2005), we estimate average flux levels to be 0.025±0.005 MJy sr−1, 0.14±0.04 MJy sr−1, 0.15±0.03 MJy sr−1 and 1.4±0.4 MJy sr−1 at 4.5, 8, 24. and 70 µm, respectively.”
COLOR–MASS-TO-LIGHT-RATIO RELATIONS FOR DISK GALAXIES (2014, methodology): “This follows from the mean color Ks − [3.6] = 0.31 ± 0.11 that we obtain for the 74 galaxies of Dale et al. (2005).”
Multiwavelength Study of Massive Galaxies at z~2. I. Star Formation and Galaxy Growth (2007, background): “Spitzer observations show a substantial scatter in the local correlation of mid-IR luminosity versus the total infrared luminosity LIR (Dale et al. 2005; Smith et al. 2007; Armus et al. 2007).”
Planck2013 results. XXVIII. ThePlanckCatalogue of Compact Sources (2013, background): “Figure 13 shows a comparison between Planck flux densities at 353 GHz and those from two SCUBA catalogues (Dale et al. 2005; Dunne et al. 2000 [SLUGS]) at 850 µm.”
The Hubble Deep Field-North SCUBA Super-map - IV. Characterizing submillimetre galaxies using deep Spitzer imaging (2006, methodology): “Both of these approaches areindirect and require assumptions about the shape of the SED whichis known to differ for different galaxy types (e.g. Dale et al. 2005).”
The Mid-Infrared Spectrum of Star-forming Galaxies: Global Properties of Polycyclic Aromatic Hydrocarbon Emission (2006, methodology): “To estimate the magnitude of this effect, we considered the nuclear and inner disk MIPS photometry of Dale et al. (2005), from nearby SINGS galaxies M81 and M51.”
Dust in starburst nuclei and ULIRGs - SED models for observers (2006, background): “The dust is assumed to be heated in a given radiation field which is usually a scaled–up version of the interstellar field (Devriendt et al. 1999, Dale et al. 2001, 2005, Lagache et al. 2003).”