Global Extinction in Spiral Galaxies

Tully, R. Brent; Pierce, Michael; Huang, Jia-Sheng; Saunders, Will; Verheijen, Marc; Witchalls, Peter L.

doi:10.1086/300379

Cited by 284 publications

(495 citation statements)

References 32 publications

(55 reference statements)

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“…These vectors were derived from Tully et al (1998) Bell & de Jong (2001), is just consistent with the reddening-corrected data. The bar streaming motions modeling therefore provides some of the (Fioc & Rocca-Volmerange 1997).…”

Section: Disk Velocity Dispersionssupporting

confidence: 55%

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Comparing Dynamical and Stellar Population Mass-to-Light Ratio Estimates

Jong¹,

Bell²

Island Universes

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We investigate the mass-to-light ratios of stellar populations as predicted by stellar population synthesis codes and compare those to dynamical/gravitational measurements. In Bell & de Jong (2001) we showed that population synthesis models predict a tight relation between the color and mass-to-light ratio of a stellar population. The normalization of this relation depends critically on the shape of the stellar IMF at the low-mass end. These faint stars contribute significantly to the mass, but insignificantly to the luminosity and color of a stellar system. In Bell & de Jong (2001) we used rotation curves to normalize the relation, but rotation curves provide only an upper limit to the stellar masses in a system. Here we compare stellar and dynamical masses for a range of stellar systems in order to constrain the mass normalization of stellar population models. We find that the normalization of Bell & de Jong (2001)

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Section: Disk Velocity Dispersionssupporting

confidence: 55%

“…The two data points for NGC 4123 and NGC 3095 are indicated with formal errorbars. The arrows on the data points indicate the reddening for these galaxies according to Tully et al (1998). On the left we show the Bell & de Jong (2001) normalization, at the right a 0.1 dex lower normalization.…”

Section: Disk Velocity Dispersionsmentioning

confidence: 99%

Comparing Dynamical and Stellar Population Mass-to-Light Ratio Estimates

Jong¹,

Bell²

Island Universes

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“…The luminosities of their galaxies have been corrected for absorption as if observed face-on. Unfortunately this correction does not take into account the demonstrated dependence of such a correction on total luminosity of a galaxy (Giovanelli et al 1997;Tully et al 1998). In practice Palunas & Williams make a correction more or less as if all their galaxies belong to the most luminous category.…”

Section: The Mass-to-light Ratiomentioning

confidence: 99%

Dark and luminous matter in the NGC 3992 group of galaxies

Bottema¹,

Verheijen²

2002

A&A

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Abstract. Detailed neutral hydrogen observations have been obtained of the large barred spiral galaxy NGC 3992 and its three small companion galaxies, UGC 6923, UGC 6940, and UGC 6969. For the main galaxy, the H i distribution is regular with a low level radial extension outside the stellar disc. However, at exactly the region of the bar, there is a pronounced central H i hole in the gas distribution. Likely gas has been transported inwards by the bar and because of the emptyness of the hole no large accretion events can have happened in recent galactic times. The gas kinematics is very regular and it is demonstrated that the influence of the bar potential on the velocity field is negligible. A precise and extended rotation curve has been derived showing some distinct features which can be explained by the non-exponential radial light distribution of NGC 3992. The decomposition of the rotation curve gives a slight preference for a sub maximal disc, though a range of disc contributions, up to a maximum disc situation fits nearly equally well. For such a maximum disc contribution, which might be expected in order to generate and maintain the bar, the required mass-to-light ratio is large but not exceptional.

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“…Although the bulk of LSB galaxies are known to be rich in neutral hydrogen gas (H I), they are generally presumed to be dust and molecule-poor systems. Numerous observations directly and indirectly support this picture, including : low metal abundances (e.g., McGaugh 1994 ;, low statistically inferred Ronnback internal extinctions (e.g., Tully et al 1998 ;Matthews, van Driel, & Gallagher 1998), strong similarities between optical and near-infrared (NIR) morphologies (Bergvall et al 1999) ; undetectable CO Ñuxes (Schombert et al 1990 ;Knezek 1993 ;de Blok & van der Hulst 1998 ; but see Matthews & Gao 2001), and the high transparency of their stellar disks (e.g., OÏNeil et al 1998 ;Matthews et al 1999a ;Matthews, Gallagher, & van Driel 1999b, hereafter MGvD99). Theoretical and numerical models also suggest that the low surface densities and low metallicities of LSB galaxies cannot support signiÐcant molecular gas fractions (e.g., Mihos, Spaans, & McGaugh 1999 ;Gerritsen & de Blok 1999).…”

mentioning

confidence: 94%

Modeling the Interstellar Medium of Low Surface Brightness Galaxies: Constraining Internal Extinction, Disk Color Gradients, and Intrinsic Rotation Curve Shapes

Matthews

Wood

2001

Astrophysical Journal

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We use a combination of three-dimensional Monte Carlo radiative transfer techniques and multiwavelength (BRHK, Ha) imaging data to investigate the nature of the interstellar medium (ISM) in the edge-on, low surface brightness (LSB) galaxy UGC 7321. Using realistic models that incorporate multiple scattering e †ects and clumping of the stars and the interstellar material, we explore the distribution and opacity of the interstellar material (gas]dust) and its e †ects on the observed stellar disk luminosity proÐles, color gradients, and rotation curve shape. We Ðnd that UGC 7321 contains a small but nonnegligible dusty component to its ISM, yielding a B-band optical depth from disk edge to q6 e,B D 4.0 center. A signiÐcant fraction (D50%^10%) of the interstellar material in the innermost regions of UGC 7321 appears to be contained in a clumpy medium, indicating that LSB galaxies can support a modest, multiphase ISM structure. In spite of the clear presence of dust, we conclude that the large radial optical color gradients observed in UGC 7321 and other similar LSB spiral galaxies cannot be accounted for by dust and must result primarily from signiÐcant stellar population and/or metallicity gradients. We show that realistic optical depth e †ects will have little impact on the observed rotation curves of edge-on disk galaxies and cannot explain the linear, slowly rising rotation curves seen in some edge-on LSB spirals. Projection e †ects create a far larger uncertainty in recovering the true underlying rotation curve shape of galaxies viewed at inclinations i Z 85¡.

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Global Extinction in Spiral Galaxies

Cited by 284 publications

References 32 publications

Comparing Dynamical and Stellar Population Mass-to-Light Ratio Estimates

Comparing Dynamical and Stellar Population Mass-to-Light Ratio Estimates

Dark and luminous matter in the NGC 3992 group of galaxies

Modeling the Interstellar Medium of Low Surface Brightness Galaxies: Constraining Internal Extinction, Disk Color Gradients, and Intrinsic Rotation Curve Shapes

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