Date and Time of the Query: 2019-05-24 T00:54:17 PDT
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Notes for object NGC 0660

14 note(s) found in NED.

1. 2005MNRAS.357..361S
Re:NGC 0660
NGC 660. This inclined galaxy (i= 66^deg^) is core-dominated in both
submillimetre and optical maps. The submillimetre peak is offset from the
optical peak by ~7 arcsec to the north-west, corresponding to a projected linear
offset of ~670 pc. However, the intrinsic centre of the distribution of stars
(and therefore starlight) in the galaxy is likely to be given by the
submillimetre peak. The apparent optical peak may simply be the brightest part
of the galactic core that is not obscured by dust.

2. 2004A&A...418..429F
Re:NGC 0660
NGC 660 The soft X-ray region is about 0.5' in extent in the
Northeast-Southwest direction, about the size and orientation of the
radio emitting region (see Filho et al. 2002). The hard X-ray nuclear
region, spatially coincident with the radio core (Filho et al. 2002),
comprises only about 10 counts, such that no spectral fit was possible.

3. 2002ApJS..142..223F
Re:NGC 0660
NGC 660. NVSS detected a 373 mJy source, consistent with the 54"
resolution observations of Condon (1987) at the same frequency. 184 mJy
were detected in the Green Bank survey; 5", 1.5", and 0.5" resolution
maps at 1.4 and 4.85 GHz (Condon 1980, 1987; Condon et al. 1982, 1990)
show a double structure in the northeast-southwest direction.
High-resolution, 15 GHz observations (Carral, Turner, & Ho 1990) show
an edge-on ring or linear jet structure composed of several aligned
components at a position angle of 71deg. The optical nucleus is located
about 3" south of the strongest 15 GHz peak.
The overall radio morphology of NGC 660 measures about 6" and
appears cospatial with the small optical galaxy. From the tapered (25"
resolution) image, we compute the total flux density to be about 60 mJy.
The full resolution 8.4 GHz map shows a beautiful symmetric ring
of radio emission and what looks to be a radio source in its center. We
shall designate this radio component as the "core," and we estimate it
comprises less than 3 mJy. Although individual points of emission can
be identified, we call attention to two strong northeastern components,
about 2"-2.5" from the core; these have also been observed by Carral et
al. (1990). For consistency with the Carral et al. (1990) maps we have
designated them components C1 and C2. Comparison of our and the Carral
et al. (1990) measurements of these components shows that they are
steep spectrum and/or variable, hence possible supernova remnants.

4. 2001A&A...378...51B
Re:NGC 0660
NGC 660: Combes et al. (1992) detected CO in the polar ring near the
HI maxima. Given the size of the ring, the CO is likely to have been
formed from the HI. Nonetheless, the result of a major fusion, producing
a polar ring, is a rather confused object so we chose not to include it
in our sample.

5. 1998A&A...335..807A
Re:NGC 0660
This is an almost edge-on (i = 70^deg^), barred spiral with quite a high
FIR-to-blue luminosity ratio (L_FIR_/L_B_~4; Alton 1996, Alton et al.
(1998a)). It is distinguished by a massive 'polar' ring containing young
stars and also copious amounts of dust and molecular gas (van Driel et
al. 1996). These features, along with emission-line broadening
associated with starburst- driven outflow (Armus et al. 1990), testify
to a recent violent past in which NGC 660 probably collided with another
galaxy. High resolution IRAS data show a bright, point-like (< 3 kpc)
source associated with the nuclear starburst. In Fig. 1,the 200 micron
image also seems fairly 'point-like' but faint structure, possible
emanating from the outer disk and polar ring, is also apparent. The
compact emission at 200 micron emphasizes the fact that warm dust tends
to 'out-shine' cold grains unless the latter are present in sufficiently
large quantities. This assertion is particularly apt for starburst
galaxies which emit the majority of their bolometric luminosity from
sites of recent star formation (Alton et al. 1998a).

6. 1997MNRAS.284..773G
Re:NGC 0660
3.4 NGC 660 (C-13)
This edge-on galaxy has multiple, inclined rings making an `integral' sign on
the sky. Its systemic velocity is 852 km s^-1^. It has been studied at 21 cm by
Gottesman & Mahon (1990), who produced a detailed rotational picture of the
central body and the major axis of the outermost ring. A kinematical model of
the complex H I velocity field has been produced by Arnaboldi & Galletta(1993).
The field around it contains three objects of similar redshift (within 80
km s^-1^); two of them, UGC 1195 and 1200, are aligned with the outer ring
direction and lie at distances of 22 and 29 arcmin (~89 and ~117 kpc)
CO emission from the rings was detected by Combes et al. (1992). H I emission
is strongest at velocities between 780 and 840 km ^-1^, while the CO is
brighter between 700 and 760 km ^-1^ (Combes et al. 1992). This asymmetry is
similar to that found in the SB0 galaxy NGC 4546 by Sage & Galletta (1994). On
the basis of a detailed investigation, van Driel et al. (1995) concluded that
NGC 660 is a spiral galaxy whose ring is sustained by self-gravity.
NGC 660 is so big in the sky that we observed only a few points on the rings.
We detected CO at three positions: (30 arcsec, -50 arcsec), (-30 arcsec, 50
arcsec) and (25 arcsec, 100 arcsec). The velocities of the CO lines agree with
those of the H I at the last position only; the wide peak between 900 and 1100
km s^-1^ at the (30 arcsec, -50 arcsec) position is ~130 km s^-1^ higher than
the 21-cm emission. Of course, the atomic and molecular gas may be in very
different spatial locations, yet still along the same line of sight. We suggest
that the H I and CO data indicate a complex of rings with different velocities,
with the north side of the galaxy approaching.
Based on the observations of CO emission from the rings (Combes et al. 1992;
this work), and comparison with larger scale studies of the entire galaxy
(Solomon & Sage 1988), we estimate that ~10 per cent of the total molecular
mass associated with the galaxy lies within the rings.

7. 1997ApJS..112..391H
Re:NGC 0660
NGC 660.--This transition object (LINER+H II nucleus) may contain extremely
weak broad H{alpha} emission, but its reality is suspect because of a possible
template mismatch. As the narrow lines have unusually small widths (FWHM~200
km s^-1^), very faint emission between H{alpha} and [N II] is discernible. When
fitted with a single Gaussian, the broad component appears to contain about 8%
of the total flux of the blend (Fig. 4c).

8. 1996AJ....111..712H
Re:NGC 0660
0140+134 (NGC 660). This is a spectacular example of an interaction with two
dust lanes that dominate the optical appearance. The main gaiaxy looks like a
warped disk seen near to edge-on, and it is intersected by a strong dust lane
associated with a much less luminous disk. There are several bright knots
associated with the outer parts of the second dust lane, as well as others
lying around the main galaxy. The mairi galaxy has a knotty appearance along
its bright ridge.
The reddest knots all lie outside the main galaxy, associated with the strong
dust lane, and also on the side opposite from the dust lane. These are also
the brightest of the knots. The population of outside knots defines the upper
layer of knot brightness at all colors. The faintest objects measured trace
the main galaxy. The bluest objects trace both dust lanes.
This is the lowest redshift gaiaxy in the group, and knots are measured to
faint magnitudes (but no fainter than in the highest redshift object). The
faintest objects have the luminosity of individuai stars of mass as low as
10 M_sun_, but are redder. Dereddening them corresponds to main sequence 40
M_sun_ stars. The brightest knots are brighter than 100 M_sun_ stars, and
dereddening would bring them up to M_BOL_ = -17 if they are hot.

9. 1996A&AS..115..439E
Re:NGC 0660
NGC 660 is discussed by Braine et a]. (1993). It is a peculiar galaxy with a
prominent central bar-like structure and a strongly warped outer disk
structure. H I and OH has been observed in absorption towards the nucleus by
Baan et a]. (1992) using the VLA. van Driel et al. (1995) have recently
presented a thorough study of this galaxy in the optical and radio spectral

10. 1994AJ....107...99R
Re:NGC 0660
C-13 = NGC 660 = UGC 1201. This nearby starburst galaxy contains
optically-emitting gas mixed with dust in a warped ring that is highly
inclined to the central body. The strong double-horned profile seen with
the GB 140' contains 8.5 x 10^9^ M_sun_ of HI. The nearby UGC 1211 is
16' away with a radial velocity ~2404 km/s that is 1600 km s^-1^ higher
than that of NGC 660; it is not a source of confusion for our
observations. Previous Arecibo observations (cf Huchtmeier & Richter
1989) give a flux integral of 54 Jy km s^-1^, about one-third of our
flux, but since the optical diameter of this galaxy is about 8', the GB
140' beam is well-matched to the size of the system, whereas the 3'
Arecibo beam would be expected to miss emission. New high-resolution VLA
observations (Mahon 1992) show about 80% of the GB 140' flux and a
slightly larger linewidth. It is likely that all the HI that we detect
is in fact associated with NGC 660, which makes it quite gas-rich, with
an M_HI_/L_B_ = 1.6. In the far-infrared, NGC 660 is one of the more
luminous galaxies in our sample.

11. 1993A&AS...97..887B
Re:NGC 0660
NGC 660 is probably a nearly completed merger, and it has a polar ring.
Tidal tails are seen to the North and South extending over several
arcminutes. It is one of the few galaxies where the CO emission is
significantly wider than the HI. The CO appears quite localized as is the
FIR emission (Rice et al. 1988). The dust temperature is quite high for a
LINER (cf. SM sample). NGC 660 and its polar ring will be discussed
further in a future article (Combes et al. 1992).

12. 1976RC2...C...0000d
Re:NGC 0660
HII Regions:
"Atlas and Catalogue", Univ. Washington, Seattle, 1966.

13. 1973UGC...C...0000N
Re:UGC 01201
SB(s)a pec (de Vaucouleurs)
Bar 2.8 x 0.9 in position angle 217, thin absorption lane, complex absorption
regions in north-preceding part of bar
2 diffuse very broad arms, extremely faint outskirts to 11.8 x 5.2

14. 1964RC1...C...0000d
Re:NGC 0660
Bright bar with a complex dark lane: 2.85 arcmin x 0.7 arcmin
Very faint smooth arms.
Heid. 9 dimensions (2.2 arcmin x 0.7 arcmin) rejected, bar only.

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