Analysis of seven face-on spiral galaxies

Pompei, E.; Natali, G.

doi:10.1051/aas:1997183

Cited by 15 publications

(16 citation statements)

References 7 publications

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“…Secondly, for systems with small bulges MacArthur et al (2003) showed that results from one-dimensional photometry are equivalent to those derived from two-dimensional fits (as required by this work). The resulting sample is comprised of 61 galaxies taken from Möllenhoff (2004), MacArthur et al (2003), Prieto et al (2001) and Pompei & Natali (1997). Since MacArthur et al had measurements in B V R H, their R band scalelengths were converted to I band scalelengths by multiplying them by a factor of 0.981.…”

Section: Application To Local Universe Disk Galaxiesmentioning

confidence: 99%

Modelling the spectral energy distribution of galaxies

Möllenhoff¹,

Popescu

Tuffs

2006

A&A

123

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We present corrections for the change in the apparent scalelengths, central surface brightnesses and axis ratios due to the presence of dust in pure disk galaxies, as a function of inclination, central face-on opacity in the B-band (τ f B ) and wavelength. The correction factors were derived from simulated images of disk galaxies created using geometries for stars and dust which can reproduce the entire spectral energy distribution from the ultraviolet (UV) to the Far-infrared (FIR)/submillimeter (submm) and can also account for the observed surface-brightness distributions in both the optical/Near-infrared and FIR/submm. We found that dust can significantly affect both the scalelength and central surface brightness, inducing variations in the apparent to intrinsic quantities of up to 50% in scalelength and up to 1.5 mag in central surface brightness. We also identified some astrophysical effects for which, although the absolute effect of dust is non-negligible, the predicted variation over a likely range in opacity is relatively small, such that an exact knowledge of opacity is not needed. Thus, for a galaxy at a typical inclination of 37• and having any τ f B > 2, the effect of dust is to increase the scalelength in B relative to that in I by a factor of 1.12 ± 0.02 and to change the B − I central colour by 0.36 ± 0.05 mag. Finally we use the model to analyse the observed scalelength ratios between B and I for a sample of disk-dominated spiral galaxies, finding that the tendency for apparent scalelength to increase with decreasing wavelength is primarily due to the effects of dust.

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Section: Application To Local Universe Disk Galaxiesmentioning

confidence: 99%

Modelling the spectral energy distribution of galaxies

Möllenhoff¹,

Popescu

Tuffs

2006

A&A

123

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“…However, we oftenly face again the problem of disjunct samples (e.g. Kent 1985;Prieto et al 1992;Courteau 1996;Pompei & Natali 1997;Lu 1998). Héraudau & Simien (1996) presented CCD photometry in V and I of 234 spiral galaxies.…”

Section: Comparison With Previous Papersmentioning

confidence: 99%

Surface photometry of spiral galaxies in NIR: Structural parameters of disks and bulges

Möllenhoff¹,

Heidt²

2001

A&A

148

169

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Abstract.A sample of 40 bright spiral galaxies (BT < 12) with low inclination and without bar was observed with JHK filters. For this purpose the MAGIC NICMOS3 camera at the 2.2 m telescope of the Calar Alto observatory, Spain was used. With a newly developed 2-dimensional algorithm the distribution of the surface brightness was fitted simultaneously by corresponding functions for the disk-and bulge-structure. While the disk was fitted with an exponential function, the bulge profile was fitted with a generalized de Vaucouleurs R β law, with the concentration parameter β = 1/n as a further fit variable. The correlation of the resulting structural parameters of disks and bulges lead to some interesting relations: 1. The use of a variable exponent β is necessary for a realistic description of the bulge structure; 2. Disks and bulges show similar correlations between effective radius, effective surface brightness and luminosity; 3. They populate a common strip in the fundamental plane; 4. From the correlations between β and Hubble type some conclusions about the formation and evolution of spiral galaxies can be drawn.

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“…This effect was later also observed in many galaxies by a number of observational groups, both in edge-on galaxies (Jensen & Thuan 1982;Sasaki 1987;Fry et al 1999;Barteldrees & Dettmar 1994;Pohlen et al 2000a;de Grijs et al 2001;Kregel et al 2002), and also in face-on galaxies (Pompei & Natali 1997;Pohlen et al 2002). For a recent summary of this topic, see van der Kruit (2001).…”

Section: Introductionmentioning

confidence: 65%

The puzzle about the radial cut-off in galactic disks

Narayan¹,

Jog²

2003

A&A

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Abstract. The stellar disk in a spiral galaxy is believed to be truncated physically because the disk surface brightness is observed to fall faster than that for an exponential in the outer, faint regions. We review the literature associated with this phenomenon and find that a number of recent observations contradict the truncation picture. Hence we question the very existence of a physical outer cut-off in stellar disks. We show, in this paper, that the observed drop in the surface brightness profiles in fact corresponds to a negligible decrease in intensity, and that this minor change at the faint end appears to be exaggerated on a log-normal plot. Since minor deviations from a perfect exponential are common throughout the disk, we suggest that such a deviation at the faint end could easily give rise to the observed sharp drop.

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Analysis of seven face-on spiral galaxies

Cited by 15 publications

References 7 publications

Modelling the spectral energy distribution of galaxies

Modelling the spectral energy distribution of galaxies

Surface photometry of spiral galaxies in NIR: Structural parameters of disks and bulges

The puzzle about the radial cut-off in galactic disks

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