1998
DOI: 10.1086/306166
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The Intrinsic Shapes of Low Surface Brightness Dwarf Irregular Galaxies and Comparison to Other Types of Dwarf Galaxies

Abstract: In this paper, we measure the ellipticities of 30 LSB dI galaxies and compare the ellipticity distribution with that of 80 dEs (Ryden & Terndrup 1994;Ryden et al. 1998) and 62 BCDs (Sung et al. 1998). We find that the ellipticity distribution of LSB dIs is very similar to that of BCDs, and marginally different from that of dEs. We then determine the distribution of intrinsic shapes of dI galaxies and compare to those of other type dwarf galaxies under various assumptions. First, we assume that LSB dIs are eith… Show more

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Cited by 46 publications
(32 citation statements)
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“…The predicted rotation curve for an exponential mass distribution corresponding to the observed exponential surface brightness profile has been analytically given for a thin, self-gravitating exponential disk (Freeman 1970). Providing a characteristic inner disk radius this description may serve here as a simple model for the luminous matter distribution and the related Keplerian kinematics despite dwarf irregular and low-surface brightness galaxies being known to be better characterized by expanded disks (Sung et al 1998). The velocity profile exhibits a peak at radius R peak = 2.14 α −1 where it has a value of v d = 0.62(2πGΥ I 0 α −1 ) 0.5 ; here G is the gravitational constant, Υ the disk mass-to-light ratio, I 0 the face-on central mass surface density, and α −1 the scale length (e.g., Chiba & Yoshi 1995).…”
Section: Linkage Of Photometric and Kinematic Parametersmentioning
confidence: 99%
“…The predicted rotation curve for an exponential mass distribution corresponding to the observed exponential surface brightness profile has been analytically given for a thin, self-gravitating exponential disk (Freeman 1970). Providing a characteristic inner disk radius this description may serve here as a simple model for the luminous matter distribution and the related Keplerian kinematics despite dwarf irregular and low-surface brightness galaxies being known to be better characterized by expanded disks (Sung et al 1998). The velocity profile exhibits a peak at radius R peak = 2.14 α −1 where it has a value of v d = 0.62(2πGΥ I 0 α −1 ) 0.5 ; here G is the gravitational constant, Υ the disk mass-to-light ratio, I 0 the face-on central mass surface density, and α −1 the scale length (e.g., Chiba & Yoshi 1995).…”
Section: Linkage Of Photometric and Kinematic Parametersmentioning
confidence: 99%
“…To date (O'Neil, Bothun, & Schombert 1998 and references therein), three main classes of LSB galaxies have been identified: (1) dwarfs, defined by objects with scale lengths 1 kpc; (2) disk galaxies with scale lengths 1 5 kpc and circular velocities in the range 80-200 km s À1 ; and (3) giant disk galaxies with scale lengths !5 kpc. Dwarf LSBs include both irregular (dI) and more regular spiral (dS) galaxies (Sung et al 1998;Schombert et al 2001). Dwarf LSB galaxies have much in common with blue compact dwarfs (BCDs): a large amount of H i, often with small OB associations, and blue colors (BÀV $ 0.5 mag).…”
Section: Introductionmentioning
confidence: 99%
“…But dwarf irregulars are distinguished from BCDs by having amorphous shapes, as well as by having star-forming regions that are not centrally concentrated. Also, dwarf LSBs are known to have higher total masses (within a given surface brightness) and larger linear diameters than BCDs (Sung et al 1998). Meanwhile, normal-size or giant LSBs are more similar to late-type spiral galaxies in their general properties, except in overall low stellar density.…”
Section: Introductionmentioning
confidence: 99%
“…More recently, Sung et al (1998) have argued that BCDGs and dEs have similar intrinsic shapes, i.e. their axis ratios show a similar distribution.…”
Section: Introductionmentioning
confidence: 99%