NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-05-20 T15:48:38 PDT
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Notes for object NGC 0266

6 note(s) found in NED.


1. 2008MNRAS.390..466E
Re:UGC 00508
UGC 508. H I inclination (25^deg^, Noordermeer et al. 2005) as well as
photometric inclination (14^deg^, from an axis ratio of 0.97) lead to a very
high maximum rotation velocity (~550 km s^-1^). From Tully-Fisher relationship,
its absolute magnitude M_B_ suggests a maximum velocity around 270 km s^-1^,
leading to an axis ratio of 0.5 (hence an inclination of 60^deg^). This strongly
barred galaxy shows moreover clear evidence for interaction, resulting in a
perturbed morphology and velocity field. This biases the determination of the
inclination by morphological as well as kinematical methods, leading to an
unrealistically high-maximum rotation velocity.

2. 2005A&A...442..137N
Re:UGC 00508
UGC 508 (NGC 266) lies about 23' to the northeast of UGC 499; the peculiar
structure of the gas in UGC 499 might be a result of a past interaction with its
neighbour. The H I properties of UGC 499 were discussed in detail by Heckman et
al. (1982) and Simkin et al. (1987).

3. 2000ApJ...542..186N
Re:NGC 0266
NGC 266.-Our simultaneous 3.6 and 2 cm observations on 1996 October
11, with resolutions 0.29" x 0.24" and 0.15" x 0.13", detected an
unresolved nuclear source with flux densities 3.1 and 4.1 mJy,
respectively. The nucleus therefore has an inverted radio spectrum,
{alpha}_2_^3.6^ >= 0.5. This source was, however, not detected at a
10 {sigma} upper limit of 10 mJy in our simultaneous 0.7 cm
observation. NGC 266 has been identified with source NVSS J004947+321637
by the NASA Extragalactic Database (NED; Helou et al. 1991); i.e., it
has been detected in the 20 cm NRAO VLA sky survey (NVSS), with a peak
flux density of 8.9 mJy beam^-1^ at a resolution of 45", though the
20 cm position is offset 44" from our 2 cm position. In any case,
8.9 mJy may be taken as an upper limit to the 20 cm flux density.

4. 1997ApJS..112..391H
Re:NGC 0266
NGC 266.--A broad H{alpha} component is obvious even before profile
decomposition, as evidenced by the extra bump between narrow H{alpha} and
[N II] {lambda}6583 (Fig. 4a). Since the rather noisy [S II] region could not
be fitted to give a reliable model for the narrow lines, we resorted to fitting
the H{alpha}+[N II] complex independently. Each of the narrow lines required
two components, as they are each slightly asymmetric to the blue, but we forced
all three lines to have identical profiles. The resulting narrow-line profile,
when applied to the [S II] lines, provided a reasonable fit. The broad H{alpha}
line, with FWHM~1350 km s^-1^ and f_blend_~30%, appears to be redshifted by
~350 km s^-1^ with respect to the narrow component of H{alpha}. The latter
effect may be an artifact of the uncertain continuum level, as the negative
dip shortward of [N II] {lambda}6548 probably influences the derived central
wavelength of the broad H{alpha} feature.

5. 1976RC2...C...0000d
Re:NGC 0266
m{_pg} = 12.6 in CGCG, Vol. VI, 1968.

6. 1973UGC...C...0000N
Re:UGC 00508
Companion 3.6, 219, 0.4 x 0.1:


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