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Notes for object UGC 10205

6 note(s) found in NED.


1. 2005MNRAS.364.1253V
Re:UGC 10205
UGC 10205. The 850-{mu}m map in Fig. 1 is a co-add of two observations. Since
emission at the optical galaxy position is very clear in one observation (both
at 850 and 450 {mu}m) and not in the other observation, and since we find no
explanation for this, we simply co-add the two observations (Section 2.2). The
submm emission coincident with the main optical galaxy extent, and also the peak
to the S, are not associated with any noisy bolometers. Peaks to the N and W of
the galaxy lie in a region of the map which is slightly noisy. We note that this
observation was carried out in less than ideal weather.

2. 2004A&A...417..527L
Re:UGC 10205
UGC 10205 (VV 624) (Fig. 11) is already studied in detail by Reshetnikov
& Evstigneeva (1999) and Vega et al. (1997). Both note that the bright
spots in this galaxy (first mentioned by Vorontsov-Velyaminov 1977)
belong to an outer equatorial (edge-on) ring. Other interpretations of
this structure as a merger remnant (Vorontsov-Velyaminov 1977) or polar
ring (Whitmore et al. 1990; van Driel et al. 2000), seem to be very
unlikely. Reshetnikov & Evstigneeva (1999) point also to the asymmetric
weak envelope surrounding the galaxy. However, they do not mention its
boxy structure at certain contour levels. The asymmetry of the boxy
envelope is especially remarkable in the outer parts of the
galaxy. Additionally, Reshetnikov & Evstigneeva (1999) explain an
"extended, diffuse structure" at one side of the galaxy, only detectable
in deep exposures (not visible in our DSS image, but in Fig. 2 in
Reshetnikov & Evstigneeva 1999), as result of an accretion event.

3. 2000A&AS..141..385V
Re:UGC 10205
C-50 = UGC 10205. (E,G,N) Looks like a normal SO/a-Sa type galaxy in
many respects, but its edge-on absorption "disc" (Gavazzi & Randone
1994) shows evidence for a brightness bump in the light profile and a
warp (PRC), and deep exposures indicate diffuse debris and shell
structure in the outer regions (Rubin 1987, PRC). Long-slit H{alpha}
spectra show 3 gas kinematic components structures along the major axis,
one of which is in counterrotation (Rubin et al. 1985; Vega et al.
1997). Low-resolution near-infrared mapping: see Giovanardi & Hunt
(1996). Its main peculiarities were modeled by Reshetnikov & Evstigneeva
(1999) as the early stage in the capture and tidal disruption of a small
type E/S0 companion by the massive central galaxy. Compared to the
Nancay and Effelsberg results, the Green Bank central velocity is
213 km s^-1^ higher and its 163 km s^-1^ FWHM is much narrower than the
560 km s^-1^ measured elsewehere, though the line fluxes are similar. The
only possible companion, at the edge of the Nancay search area (12.7'
distance), might be IRAS F16036+3019, of unknown redshift.

4. 1998A&AS..130..333T
Re:PGC 057173
Atypical profile for a single object. Also VV624: "3 members or
an ellipse or a ring edge-on?". Nilson catalogue: "very large nucleus
bulge with a faint halo similar to M104?"

5. 1994AJ....107...99R
Re:UGC 10205
C-50 = UGC 10205. In many respects, this galaxy looks like a normal Sa
galaxy, but its edge-on absorption 'disk' shows evidence for a brightness
bump in the light profile (PRC); deep exposures also indicate diffuse
debris and shell structure in the outer regions (Rubin, 1987). The GB
140' sees 3.9 x 10^9^ M_sun_ of HI, which gives it a gas-to-light
M_HI_/L_B_ = 0.16. NED lists no optical companions within the GB 140'
beam.

6. 1973UGC...C...0000N
Re:UGC 10205
Similar to NGC 4594
Very large nuclear bulge, faint halo


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