Date and Time of the Query: 2019-02-18 T10:36:54 PST
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Notes for object NGC 0278

17 note(s) found in NED.

1. 2008ApJS..174..337M
Re:NGC 0278
NGC 278 (Fig. 5a).-The entire ring as seen in H{alpha} is very small in size
(0.2 kpc in radius) with 20 individual H II regions detected that comprise the
ring. This ring is the smallest one recognized in the galaxy; a second "outer"
nuclear ring appears at ~1 kpc and is discussed in detail in Knapen et al.
(2004). This outer ring is considered "nonstandard" as it is very wide and more
a region of star formation with rather abrupt delimitations on the inner and
outer radial range. In addition to this, we were in practice unable to derive a
recognizable ring pattern of H II regions using SExtractor and have thus opted
for concentrating on the inner nuclear ring. The host galaxy does not contain a
bar in the optical nor near-IR wavelengths (Knapen et al. 2004). There is a
decrease in the log (EW) (i.e., an increase in age) over approximately one-third
of the inner ring ranging from the positions of the H II regions centered at
azimuth 124^deg^-236^deg^. This indicates a counterclockwise rotation with in
the ring. A radial gradient spans the same range, with the younger H II regions
lying on the inner side of the ring. A similar pattern, although not as clearly
defined, appears over the range of 12^deg^-100^deg^.

2. 2007A&A...468..129T
Re:NGC 0278
4.2.9 NGC 278 As in the case of NGC 4217, there are two candidate X-ray
counterparts, U and L, roughly equidistant from the optical position, with 60
and 29 counts, respectively. The X-ray colours for both sources are quite soft,
suggesting no intrinsic absorption, steep photon indices (2.3-2.7), and are
consistent with LMXBs.

3. 2005MNRAS.364..283E
Re:NGC 0278
NGC 278. Both optical and near-IR images indicate that this SAB galaxy is not
actually barred (e.g. Eskridge et al. 2000).

4. 2003A&A...399...51G
Re:UGC 00528
UGC 528 This SAB(rs)b galaxy has a very compact spiral structure. There
is H{alpha} emission all over the optical disk which shows a barred
spiral structure. The isovelocity map confirms the presence of a bar and
suggests a warp (independently of the bar) in the outer parts of the
optical disk. As a result, the major axis is not quite perpendicular to
the minor axis (100deg between the two), but the rotation curve remains
symmetric and regular until 30 arcsec (3 kpc) with a maximum of
75 km s^-1^ at 16 arcsec.

5. 2002ApJS..143...73E
Re:NGC 0278
NGC 278.---Sb: Face-on. Centrally condensed, resolved circular
nucleus, embedded in a slightly elliptical bulge. Fairly high B/D
ratio. Two-armed spiral pattern, with tightly wrapped spiral arms.
Arms have obvious dust lanes and numerous bright star-forming knots.

6. 2001A&A...368...16M
Re:NGC 0278
1. NGC 278 is a face-on multiple-armed Sbc galaxy (T = 4). On HST images
Phillips et al. (1996) could follow the spiral structure to 2-3 arcsec from
the centre. The fits of the surface-brightness (SB) distributions in JHK
lead to similar results for the structural parameters (Tables 3 and 4). The
residuum shows remnants of the spiral arms and of dust filaments, but looks
good concerning the fit quality (Fig. 3). The exact distance determination
for NGC 278 is a problem, since the small radial velocity is not meaningful
for that. We use the mean value of the discordant distance values from
Tully (14.74 Mpc) and Bottinelli et al. (32.65 Mpc).

7. 1996ApJS..103...81C
Re:NGC 0278
NGC 0278.--VLA D-configuration map at 4.86 GHz in Condon, Frayer, & Broderick

8. 1996AJ....111.1566P
Re:NGC 0278
NGC 278--Spiral structure is apparent to within 2"-3" of the nucleus; there is
evidence for a narrow dust lane approaching within 0.5" of the very center.
There appears to be a "shelf" in the central light distribution about 2" in
radius. The actual nucleus looks to be an unresolved point source: the
deconvolved nucleus has a triangular appearance similar to the core of the
PSF, and faint rings and filaments also resemble those of the PSF.

9. 1996A&AS..115..439E
Re:NGC 0278
NGC 278 has a flocculent appearance with obvious large H II regions. It has an
emission line spectrum that indicates active star formation processes (Schmidt
et al. 1990). It has also a continuum radio source (Condon 1987). The CO is
distributed in an unsymmetric fashion with some concentration towards the
southeastern region.

10. 1995ApJS...98..477H
Re:NGC 0278
Intense H II regions fill the slit. The nucleus shows very strong Balmer
absorption lines with narrow emission cores, a blue continuum, and H II
region nebular lines, indicative of a young stellar population and
ongoing star formation.

11. 1994CAG1..B...0000S
Re:NGC 0278
Sep 25/26, 1951
5 min
The surface brightness of the multiple-armed
spiral pattern in NGC 278 is exceedingly
high, although not as high as those of the two
principal inner arms of the Seyfert galaxy
NGC 1068 (Sb; panel 138), which are among the
brightest arms in the RSA. Multiple exposures at
short-exposure times also show a very bright
nucleus in NGC 278, which, however, is still
diffuse at the 2" level rather than unresolved
(starlike) as in many Seyfert galaxies. The print
here is from a short-exposure, early 200-inch
Palomar plate, underexposed to show the
multiple-armed pattern that begins at the center.
The redshift of NGC 278 is v_o = 932 km/s.
The two diffuse knots may be HII complexes; the
largest has an angular diameter of about 5",
corresponding to a linear diameter of 450 psc.
Faint luminosity exists outside the edge of
the bright disk. A spiral pattern exists in dust
that is silhouetted against the envelope

12. 1993A&AS...97..887B
Re:NGC 0278
NGC 278
Dickel & Rood (1978) estimate the inclination to be 25^deg^ from their HI
observations but from the photograph in Pease (1917) it appears more
face-on. Prominent dust lanes are visible which are probably responsible
for the large correction to the blue magnitude found in the RSA and RC2.
The CO emission shows two distinct parts. In each line there are two
components, each having about the same width in both transitions. P89
lists NGC 278 as having a nuclear ring. Given the small inclination and
the 6" radius of the ring, however, we would not expect to find a dip at
the systemic velocity. Perhaps the ring is broken or the beginning of
spiral arms.

13. 1976RC2...C...0000d
Re:NGC 0278
Photometry: (5 Color)
A.J., 73, 313, 1968.

14. 1973UGC...C...0000N
Re:UGC 00528
SAB(rs)b (de Vaucouleurs)
`Large bright nucleus, several knotty massive arms. Bright part has sharp
edge' (de Vaucouleurs)

15. 1964RC1...C...0000d
Re:NGC 0278
Large, bright nucleus.
Several knotty, massive arms.
Bright part has a sharp edge.
M.N.R.A.S., 72, 408, 1912.
Lick Obs. Bull., 497, 1939.

16. 1956AJ.....61...97H
Re:NGC 0278
HMS Note No. 009
Strong hydrogen absorption lines.

17. 1918PLicO..13....9C
Re:NGC 0278
A very bright, compact, nearly round spiral, 1.2' in diameter. The nucleus is
well defined and shows in a 5m exposure. The matter in the inner whorls is
quite bright. 6 s.n.

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