Photometric parameters of edge-on galaxies from 2MASS observations

Bizyaev, Dmitry; Митронова, С. Н.

doi:10.1051/0004-6361:20020633

Cited by 66 publications

(99 citation statements)

References 15 publications

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“…While the dust lane is evident for this nearly edge-on object in the V-band, only a weak asymmetry can be seen in the K -band for the bulge above and below the galactic plane. The K s -band value for h s derived by Bizyaev & Mitronova (2002) is consistent with the result of the present fit.…”

Section: Comments On Individual Galaxiessupporting

confidence: 90%

“…As with NGC 5746, the fit to the extinction lane in the V-band is poor, even though the global fit quality is not very different from the other objects. An estimate for h s is available for the K s -band, which is about 20% smaller than the present value (Bizyaev & Mitronova 2002). The fitted θ is consistent with the aspect of the K ring, which suggests θ = 83.5…”

Section: Comments On Individual Galaxiessupporting

confidence: 48%

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The dust distribution in edge-on galaxies

Bianchi¹,

Fermi²

2007

A&A

103

188

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Aims. I have analyzed a sample of seven nearby edge-on galaxies observed in the V and K -bands, in order to infer the properties of the dust distribution. Methods. A radiative transfer model, including scattering, was used to decompose each image into a stellar disk, a bulge, and a dust disk. The parameters describing the distributions were obtained through standard χ 2 minimization techniques. Results. The dust disks fitted to the V-band images are consistent with previous work in the literature: the radial scalelength of dust is larger than for stars (h d /h s ∼ 1.5); the dust disk has a smaller vertical scalelength than the stellar (z d /z s ∼ 1/3); the dust disk is almost transparent when seen face-on (central, face-on, optical depth τ 0 = 0.5−1.5). Equivalent fits can be produced using faster radiative transfer models that neglect scattering. In the K -band, no trace is found of a second, massive, dust disk, which has been invoked to explain observations of dust emission in the submillimeter. I discuss the model degeneracies and the effect of complex structures on the fitted distributions. In particular, most bulges in the sample show a box/peanuts morphology with large residuals; two lower-inclination galaxies show a dust ring distribution, which could be the cause of the large, fitted, dust scalelengths.

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Section: Comments On Individual Galaxiessupporting

confidence: 90%

Section: Comments On Individual Galaxiessupporting

confidence: 48%

The dust distribution in edge-on galaxies

Bianchi¹,

Fermi²

2007

A&A

103

188

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“…In agreement with its identification as a superthin galaxy by Goad & Roberts (1981), the global scale height of IC 2233 is on the small end for Sd galaxies (cf. Bizyaev & Mitronova 2002;Seth et al 2005), although it is notably thicker than the more massive superthin galaxy UGC 7321 (h z ≈ 150d 10 pc; Matthews 2000). In addition, we see evidence that the stellar disk of IC 2233 flares at larger galactocentric radii (see below).…”

Section: Properties Of the Ic 2233 Stellar Diskmentioning

confidence: 69%

H I Imaging Observations of Superthin Galaxies. Ii. Ic 2233 and the Blue Compact Dwarf NGC 2537

Matthews

Uson

2007

The Astronomical Journal

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We have used the Very Large Array to image the H i 21 cm line emission in the edge-on Sd galaxy IC 2233 and the blue compact dwarf NGC 2537. We also present new optical B, R, and Hα imaging of IC 2233 obtained with the WIYN telescope. Despite evidence of localized massive star formation in the form of prominent H ii regions and shells, supergiant stars, and a blue integrated color, IC 2233 is a low surface brightness system with a very low global star formation rate ( 0.05 M yr −1 ), and we detect no significant 21 cm radio continuum emission from the galaxy. The H i and ionized gas disks of IC 2233 are clumpy and vertically distended, with scale heights comparable to that of the young stellar disk. Both the stellar and H i disks of IC 2233 appear flared, and we also find a vertically extended, rotationally anomalous component of H i extending to ∼ 2.4d 10 kpc from the midplane. The H i disk exhibits a mild lopsidedness as well as a global corrugation pattern with a period of ∼7d 10 kpc and an amplitude of ∼150d 10 pc. To our knowledge, this is the first time corrugations of the gas disk have been reported in an external galaxy; these undulations may be linked to bending instabilities or to underlying spiral structure and suggest that the disk is largely self-gravitating. Lying at a projected distance of 16 .7 from IC 2233, NGC 2537 has an H i disk with a bright, tilted inner ring and a flocculent, dynamically cold outer region that extends to ∼3.5 times the extent of the stellar light (D 25 ). Although NGC 2537 is rotationally-dominated, we measure H i velocity dispersions as high as σ V ,H i ∼ 25 km s −1 near its center, indicative of significant turbulent motions. The inner rotation curve rises steeply, implying a strong central mass concentration. Our data indicate that IC 2233 and NGC 2537 do not constitute a bound pair and most likely lie at different distances. We also find no compelling evidence of a recent minor merger in either IC 2233 or NGC 2537, suggesting that both are examples of small disk galaxies evolving in relative isolation.

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“…The black solid curve corresponds to the γ = 1 interpolating function and the black dashed curve to γ = 2. The green curve is the probability density of the sample of 153 galaxies from Bizyaev & Mitronova (2002). The vertical solid red line represents the value of h R /z 0 at which the sample of Mosenkov et al (2010) begins to decline from a previously flat value.…”

Section: Sech 2 Vertical Distributionsmentioning

confidence: 99%

“…26, the posterior probability densities are plotted for the ratios of the fitted h R to z 0 for the γ = 1 and 2 interpolating functions. These are compared with data from Mosenkov, Sotnikova & Reshetnikov (2010) and Bizyaev & Mitronova (2002). From fig.…”

Section: Sech 2 Vertical Distributionsmentioning

confidence: 99%

Mass models of disc galaxies from the DiskMass Survey in modified Newtonian dynamics

Angus¹,

Gentile²,

Swaters³

et al. 2015

Mon. Not. R. Astron. Soc.

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This article explores the agreement between the predictions of modified Newtonian dynamics (MOND) and the rotation curves and stellar velocity dispersion profiles measured by the DiskMass Survey (DMS). A bulge-disk decomposition was made for each of the thirty published galaxies, and a MOND Poisson solver was used to simultaneously compute, from the baryonic mass distributions, model rotation curves and vertical velocity dispersion profiles, which were compared to the measured values. The two main free parameters, the stellar disk's mass-to-light ratio (M/L) and its exponential scaleheight (h z ), were estimated by Markov Chain Monte Carlo modelling. The average best-fitting K-band stellar mass-to-light ratio was M/L ≃ 0.55 ± 0.15. However, to match the DMS data, the vertical scaleheights would have to be in the range h z = 200-400 pc which is a factor of 2 lower than those derived from observations of edge-on galaxies with a similar scalelength. The reason is that modified gravity versions of MOND characteristically require a larger M/L to fit the rotation curve in the absence of dark matter and therefore predict a stronger vertical gravitational field than Newtonian models. It was found that changing the MOND acceleration parameter, the shape of the velocity dispersion ellipsoid, the adopted vertical distribution of stars, as well as the galaxy inclination, within any realistic range, all had little impact on these results.

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Photometric parameters of edge-on galaxies from 2MASS observations

Cited by 66 publications

References 15 publications

The dust distribution in edge-on galaxies

The dust distribution in edge-on galaxies

H I Imaging Observations of Superthin Galaxies. Ii. Ic 2233 and the Blue Compact Dwarf NGC 2537

Mass models of disc galaxies from the DiskMass Survey in modified Newtonian dynamics

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