Extinction in SC galaxies

Giovanelli, Riccardo; Haynes, Martha P.; Salzer, John J.; Wegner, Gary A.; Costa, L. N. da; Freudling, W.

doi:10.1086/117014

Cited by 259 publications

(343 citation statements)

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“…The mean stellar scale-lengths we find in this work (e.g., h 3.6 µm /r 25 ∼ 0.24) are consistent within the scatter to those found from detailed two-dimensional bulge-disk decompositions of spiral galaxy images (0.25-0.30, e.g., Giovanelli et al 1994;Moriondo et al 1998;Hunt et al 2004). Also, the decrease in the surface brightness scale-lengths from the UV to the NIR is in line with several previous works in the literature (Peletier et al 1994;de Jong 1996;Pompei & Natali 1997;Moriondo et al 1998;MacArthur et al 2003;Möllenhoff 2004;Taylor et al 2005;Fathi et al 2010).…”

Section: Discussion and Comparison With The Literaturesupporting

confidence: 89%

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

Casasola

Cassarà

Bianchi

et al. 2017

A&A

131

140

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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: Discussion and Comparison With The Literaturesupporting

confidence: 89%

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

Casasola

Cassarà

Bianchi

et al. 2017

A&A

131

140

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“…However, the measured r d of a given galaxy varies by about 50% purely as the disk inclination varies from intermediate to high values (see, e.g., Fig. 12 of Giovanelli et al 1994), and the conversion r d ! r d is quite uncertain.…”

Section: Which Reference Radius For Rc Width Measurement?mentioning

confidence: 99%

Rotational Widths for Use in the Tully-Fisher Relation. II. The Impact of Surface Brightness

2007

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Using a large sample of spiral galaxies for which 21 cm single-dish and/or long-slit optical spectra are available, we make a detailed comparison between various estimates of rotational widths. Different optical width estimators are considered and their limitations discussed, with emphasis on biases associated with rotation curve properties (shape and extent) and disk central surface brightness. The best match with H i rotational velocities is obtained with Polyex widths, which are measured at the optical radius (encompassing a fixed fraction of the total light of the galaxy) from a model fit to the rotation curve. In contrast with Polyex widths, optical rotational velocities measured at 2.15 disk scale lengths r d deviate from H i widths by an amount that correlates with the central surface brightness of the disk. This bias occurs because the rotation curves of galaxies are in general still rising at 2:15r d , and the fraction of total mass contained within this radius decreases with increasing disk surface brightness. Statistical corrections, parameterized by the radial extent of the observed rotation curve, are provided to reduce Polyex and H i width measurements into a homogeneous system. This yields a single robust estimate of rotational velocity to be used for applications of disk scaling relations.

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“…The optical thickness of disk galaxies remains a hotly debated issue locally (Valentijn 1990(Valentijn , 1994Giovanelli et al 1994;Disney et al 1992), and this issue obviously has important consequences for the interpretation of local and high-redshift photodisk data. The photodisk optical thickness is not one of the fitting parameters, but photodisks can be fitted with surface brightness profiles of different optical thicknesses given by the parameter C abs in the equation…”

Section: No 1 2002 Hst Structural Parameters Of Gss Galaxiesmentioning

confidence: 99%

The DEEP Groth Strip Survey. II. Hubble Space Telescope Structural Parameters of Galaxies in the Groth Strip

Simard

Willmer

Vogt

et al. 2002

ASTROPHYS J SUPPL S

410

176

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The quantitative morphological classification of distant galaxies is essential to the understanding of the evolution of galaxies over the history of the universe. This paper presents Hubble Space Telescope WFPC2 F606W and F814W photometric structural parameters for 7450 galaxies in the '' Groth Strip.'' These parameters are based on a two-dimensional bulge + disk surface brightness model and were obtained using an automated reduction and analysis pipeline described in detail here. A first set of fits was performed separately in each bandpass, and a second set of fits was performed simultaneously on both bandpasses. The information produced by these two types of fits can be used to explore different science goals. Systematic and random fitting errors in all structural parameters as well as bulge and disk colors are carefully characterized through extensive sets of simulations. The results of these simulations are given in catalogs similar to the real science catalogs so that both real and simulated measurements can be sampled according to the same selection criteria to show biases and errors in the science data subset of interest. The effects of asymmetric structures on the recovered bulge+disk fitting parameters are also explored through simulations. The full multidimensional photometric survey selection function of the Groth Strip is also computed. This selection function, coupled to bias maps from simulations, provides a complete and objective reproduction of the observational limits, and these limits can be applied to theoretical predictions from galaxy evolution models for direct comparisons with the data.

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Extinction in SC galaxies

Cited by 259 publications

References 0 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

Rotational Widths for Use in the Tully-Fisher Relation. II. The Impact of Surface Brightness

The DEEP Groth Strip Survey. II. Hubble Space Telescope Structural Parameters of Galaxies in the Groth Strip

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