Vindicating single-<i>T</i>modified blackbody fits to<i>Herschel</i>SEDs

Bianchi, S.

doi:10.1051/0004-6361/201220866

Cited by 119 publications

(155 citation statements)

References 27 publications

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“…Dale et al 2012;Aniano et al 2012, respectively) show that only a minor fraction of the dust mass (smaller than a few percent) is exposed to the more intense fields. Thus, fits to λ ≥ 100 µm Herschel SEDs assuming that dust is heated by a single radiation field with U = U min can retrieve the bulk of the dust mass (see also Magrini et al 2011;Bianchi 2013 Initially, we derived the dust mass surface density Σ dust and radiation field intensity U for all the pixels where the Herschel surface brightness was larger than 2σ in all bands with λ ≥ 160µm. We thus produced Σ dust and U maps, in a way analogous to Magrini et al (2011).…”

Section: Dust Massmentioning

confidence: 99%

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Casasola

Cassarà

Bianchi

et al. 2017

A&A

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127

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Aims. The purpose of this work is the characterization of the radial distribution of dust, stars, gas, and star-formation rate (SFR) in a sub-sample of 18 face-on spiral galaxies extracted from the DustPedia sample. Methods. This study is performed by exploiting the multi-wavelength, from ultraviolet (UV) to sub-millimeter bands, DustPedia database, in addition to molecular ( 12 CO) and atomic (Hi) gas maps and metallicity abundance information available in the literature. We fitted the surface brightness profiles of the tracers of dust and stars, the mass surface density profiles of dust, stars, molecular gas, and total gas, and the SFR surface density profiles with an exponential curve and derived their scale-lengths. We also developed a method to solve for the CO-to-H 2 conversion factor (α CO ) per galaxy by using dust and gas mass profiles. Results. Although each galaxy has its own peculiar behaviour, we identified a common trend of the exponential scale-lengths vs. wavelength. On average, the scale-lengths normalized to the B-band 25 mag/arcsec 2 radius decrease from UV to 70 µm, from 0.4 to 0.2, and then increase back up to ∼0.3 at 500 microns. The main result is that, on average, the dust mass surface density scale-length is about 1.8 times the stellar one derived from IRAC data and the 3.6 µm surface brightness, and close to that in the UV. We found a mild dependence of the scale-lengths on the Hubble stage T: the scale-lengths of the Herschel bands and the 3.6 µm scale-length tend to increase from earlier to later types, the scale-length at 70 µm tends to be smaller than that at longer sub-mm wavelength with ratios between longer sub-mm wavelengths and 70 µm that decrease with increasing T. The scale-length ratio of SFR and stars shows a weak increasing trend towards later types. Our α CO determinations are in the range (0.3 − 9) M pc −2 (K km s −1 ) −1 , almost invariant by using a fixed dust-to-gas ratio mass (DGR) or a DGR depending on metallicity gradient.

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Section: Dust Massmentioning

confidence: 99%

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Casasola

Cassarà

Bianchi

et al. 2017

A&A

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“…The FIR emission can be used to derive an average effective temperature and a total mass for large dust particles, although for certain sources it is possible that even the 70 m m emission comes from hotter dust associated with the AGN. Bianchi (2013) compares different methods to derive dust masses and temperatures by fitting the FIR SEDs with (1) a single temperature modified blackbody, (2) a dust emission model, i.e., assuming a combination of different grains populations, the details of these grain models being beyond the scope of this paper. Bianchi (2013) used two dust models: that of Draine & Li (2007) and that of Compiègne et al (2011).…”

Section: Dust Mass and Temperature Estimatesmentioning

confidence: 99%

“…Bianchi (2013) compares different methods to derive dust masses and temperatures by fitting the FIR SEDs with (1) a single temperature modified blackbody, (2) a dust emission model, i.e., assuming a combination of different grains populations, the details of these grain models being beyond the scope of this paper. Bianchi (2013) used two dust models: that of Draine & Li (2007) and that of Compiègne et al (2011). Both of these models have been used intensively in the analysis of Spitzer and Herschel data, from nearby to high Notes.…”

Section: Dust Mass and Temperature Estimatesmentioning

confidence: 99%

HERSCHEL SURVEY OF THE PALOMAR-GREEN QSOs AT LOW REDSHIFT

Petric

Flagey

et al. 2015

ApJS

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We investigate the global cold dust properties of 85 nearby (z 0.5 ⩽ ) QSOs, chosen from the Palomar-Green sample of optically luminous quasars. We determine their infrared spectral energy distributions and estimate their rest-frame luminosities by combining Herschel data from 70 to 500 μm with near-infrared and mid-infrared measurements from the 2MASS and the Wide-Field Infrared Survey Explorer. In most sources the far-infrared (FIR) emission can be attributed to thermally heated dust. Single temperature modified blackbody fits to the FIR photometry give an average dust temperature for the sample of 33 K, with a standard deviation of 8 K, and an average dust mass of M 7 10 6  with a standard deviation of M 9 10 6  . Estimates of star formation rates that are based on the FIR continuum emission correlate with those based on the 11.3 μm polycyclic aromatic hydrocarbon (PAH) feature, however, the star formation rates estimated from the FIR continuum are higher than those estimated from the 11.3 μm PAH emission. We attribute this result to a variety of factors including the possible destruction of the PAHs and that, in some sources, a fraction of the FIR originates from dust heated by the active galactic nucleus and by old stars.

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“…Since such lower coefficient was applied to the local galaxies observed with Herschel, used in Sect. 5.1 as a comparison sample, we recomputed the dust mass of the GRB 980425 host applying a comparable method outlined in Bianchi (2013), obtaining log(M d /M ) = 6.57 ± 0.05, indeed a factor of two higher than the Magphys estimate.…”

Section: Basic Physical Propertiesmentioning

confidence: 99%

“…3. Dust masses for the KINGFISH galaxies are taken from Bianchi (2013), and stellar masses from Skibba et al (2011) are corrected to the Kennicutt et al (2011) distance scale. Finally, we mark the Large Magellanic Cloud (LMC) using the compilation in Israel et al (2010) and Meixner et al (2013).…”

Section: Flux Ratiosmentioning

confidence: 99%

Spatially-resolved dust properties of the GRB 980425 host galaxy

Michałowski

Hunt

Palazzi

et al. 2014

A&A

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Gamma-ray bursts (GRBs) have been proposed as a tool for studying star formation in the Universe, so it is crucial to investigate whether their host galaxies and immediate environments are in any way special compared with other star-forming galaxies. Here we present spatially resolved maps of dust emission of the host galaxy of the closest known GRB 980425 at z = 0.0085 using our new high-resolution observations from Herschel, Atacama Pathfinder Experiment (APEX), Atacama Large Millimeter Array (ALMA) and Australia Telescope Compact Array (ATCA). We modelled the spectral energy distributions of the host and of the star-forming region displaying the Wolf-Rayet signatures in the spectrum (WR region), located 800 pc from the GRB position. The host is characterised by low dust content and a high fraction of UV-visible star formation, similar to other dwarf galaxies. These galaxies are abundant in the local universe, so it is not surprising to find a GRB in one of them, assuming the correspondence between the GRB rate and star formation. The WR region contributes substantially to the host emission at the far-infrared, millimetre, and radio wavelengths and we propose that this is a consequence of its high gas density. If dense environments are also found close to the positions of other GRBs, then the ISM density should also be considered, along with metallicity, an important factor influencing whether a given stellar population can produce a GRB.

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Vindicating single-Tmodified blackbody fits toHerschelSEDs

Cited by 119 publications

References 27 publications

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

HERSCHEL SURVEY OF THE PALOMAR-GREEN QSOs AT LOW REDSHIFT

Spatially-resolved dust properties of the GRB 980425 host galaxy

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