The Infrared Spectral Energy Distribution of Normal Star-forming Galaxies: Calibration at Far-Infrared and Submillimeter Wavelengths

By D. Dale, G. Helou. 2000

931 citations recorded by the source corpus.

New far-infrared and submillimeter data are used to solidify and to extend to long wavelengths the empirical calibration of the infrared spectral energy distribution (SED) of normal star-forming galaxies. As was found by Dale and coworkers in 2001, a single parameter family, characterized by fν(60 μm)/fν(100 μm), is adequate to describe the range of normal galaxy SEDs observed by the Infrared Astronomical Satellite and Infrared Space Observatory from 3 to 100 μm. However, predictions based on the first-generation models at longer wavelengths (122-850 μm) are increasingly overluminous compared to the data for smaller fν(60 μm)/fν(100 μm), or alternatively, for weaker global interstellar radiation fields. After slightly modifying the far-infrared/submillimeter dust emissivity in those models as a function of the radiation field intensity to better match the long-wavelength data, a suite of SEDs from 3 μm to 20 cm in wavelength is presented. Results from relevant applications are also discussed, including submillimeter-based photometric redshift indicators, the infrared energy budget and simple formulae for recovering the bolometric infrared luminosity, and dust mass estimates in galaxies. Regarding the latter, since galaxy infrared SEDs are not well described by single blackbody curves, the usual methods of estimating dust masses can be grossly inadequate. The improved model presented herein is used to provide a more accurate relation between infrared luminosity and dust mass.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/5a5843e2100ecabddc02e87bea6a224d3dbfed0b

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Citations in the corpus

COMPARISON OF Hα AND UV STAR FORMATION RATES IN THE LOCAL VOLUME: SYSTEMATIC DISCREPANCIES FOR DWARF GALAXIES (2009, methodology): “…are available for the majority of galaxies used in this analysis (Dale et al. 2009), and we compute TIR fluxes for those galaxies that have robust detections in all three bands (50% of our sample) using the calibration of Dale & Helou (2002): TIR = 1.559νfν(24) + 0.7686νfν(70) + 1.347νfν(24).”
ISM properties in low-metallicity environments I. mid-infrared spectra of dwarf galaxies (2005, background): “The MIR spectrum toward the central 24” of M 82 is clearly dominated by material originating from the disk, which shows dominant PAH emission (e.g. Laurent et al. 2000; Roussel et al. 2001b; Dale & Helou 2002; Förster Schreiber et al. 2003; Vogler et al. 2005).”
Far-Infrared Spectroscopy of Normal Galaxies: Physical Conditions in the Interstellar Medium (2001, background): “The distant galaxies were selected to span a range of galaxy properties (Dale et al. 2001) : 1.”
A PUBLIC Ks-SELECTED CATALOG IN THE COSMOS/UltraVISTA FIELD: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR POPULATION PARAMETERS, (2013, methodology): “We use the log-average of the Dale & Helou (2002) templates for this computation (see, Wuyts et al. 2008), but note that using the log-average of the Chary & Elbaz (2001) templates would provide very similar results (Muzzin et al. 2010).”
GRAVITATIONAL LENS MODELS BASED ON SUBMILLIMETER ARRAY IMAGING OF HERSCHEL-SELECTED STRONGLY LENSED SUB-MILLIMETER GALAXIES AT z > 1.5 (2013, methodology): “The top axis in Figure 7 shows the SFRs that are inferred based on the Kennicutt (1998) prescription for converting LIR (computed from LFIR assuming a bolometric correction factor of 1.91; Dale et al. 2001) to SFR assuming a Salpeter IMF.”
Spitzer View on the Evolution of Star-forming Galaxies from z = 0 to z ~ 3 (2005, methodology): “However, the models are only distinct for wavelengths redder than 3 m in the case of Chary & Elbaz (2001) and 10 m in the case of Dale & Helou (2002), although the observed SEDs in real galaxies actually present very different shapes at bluer wavelengths (see Figs.”
Planckintermediate results (2016, background): “…studies of star-forming galaxies have demonstrated the inadequacy of a single temperature model for detailed, high signal-to-noise SED shapes (e.g. Dale & Helou 2002; Wiklind 2003), the cold dust component (λ >∼ 100 µm) tends to be well represented using a single effective temperature modified…”
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).”
Star Formation in AEGIS Field Galaxies since z = 1.1: The Dominance of Gradually Declining Star Formation, and the Main Sequence of Star-forming Galaxies (2007, methodology): “For galaxies with robust 24mm detections ( mJy), SFRs were derived following Le Floc’h et al.f 1 60 (2005), using Chary & Elbaz (2001) SED templates; using templates from Dale & Helou (2002) yields no significant differences.”
TOWARD A UNIFICATION OF STAR FORMATION RATE DETERMINATIONS IN THE MILKY WAY AND OTHER GALAXIES (2011, methodology): “…(LHα + 0.0024 LTIR) (A1) where LHα and LTIR are both in units of erg s −1, LHα is corrected for foreground Galactic extinction, and LTIR is a linear combination of luminosity measurements in the Infrared Astronomical Satellite (IRAS) 25, 60, and 100 µm bands as suggested by Dale & Helou (2002).”
THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 ⩽ z ⩽ 2.2 (2011, methodology): “The MIPS 24µm fluxes are converted to total IR luminosities (LIR = L8−1000µm) using the Dale & Helou (2002) templates, where we adopt the log average conversion for templates with 1 < α < 2.5 (see Wuyts et al. 2008).”
Deriving Physical Properties from Broadband Photometry with Prospector: Description of the Model and a Demonstration of its Accuracy Using 129 Galaxies in the Local Universe (2016, background): “The inclusion of this delta function at the minimum starlight intensity is the major difference between the Draine & Li (2007) and Dale & Helou (2002) models for dM dUdust .”
Hubble Space Telescope and Spitzer Imaging of Red and Blue Galaxies at z ~ 2.5: A Correlation between Size and Star Formation Activity from Compact Quiescent Galaxies to Extended Star-forming Galaxies (2007, methodology): “Adopting an M82-like template instead of the Arp 220 template leads to a factor of 2 lower SFR (Webb et al. 2006), while adopting the model templates of Dale & Helou (2002) can result in factors of 2Y6 lower SFRs (Papovich et al. 2007).”
The evolution of the dust and gas content in galaxies (2013, methodology): “The same results are found if the MS template of Elbaz et al. (2011) is used instead of the Dale & Helou (2002) library.”
Non-standard grain properties, dark gas reservoir, and extended submillimeter excess, probed by Herschel in the Large Magellanic Cloud (2011, background): “The distribution of starlight intensities per unit dust mass, throughout the region, can be approximated by a power-law (Dale et al., 2001): dMdust dU ∝ U−α with Umin ≤ U ≤ Umin + ∆U. (4) This is an empirical prescription.”
The Hubble Deep Field-North SCUBA Super-map - IV. Characterizing submillimetre galaxies using deep Spitzer imaging (2006, methodology): “Templates used include Chary & Elbaz (2001, hereafter CEO1) and Dale & Helou (2002) star forming galaxy templates, covering a wide range of luminosities, as well as an AGN template, Mrk231 (mid-IR spectrum from Rigopoulou et al. 1999, spliced with a fit to theInfrared Astronomical Satellite, IRAS,…”