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Notes for object NGC 3628

27 note(s) found in NED.


1. 2006ApJ...647..140F
Re:NGC 3628
This galaxy (T2, Sb) has five point sources in its central kiloparsec, including
a bright point source 1 kpc away from the center. There is no point source at
the center of the galaxy, but a central patch of diffuse emission. The spectrum
of the diffuse emission is well fitted by a variety of models with a
two-temperature plasma or a power law giving the best fits. The resulting
luminosity is L_0.5-10 keV_ = 4.6 x 10^38^ ergs s^-1^. An extended radio source
was detected at the center of NGC 3628 (Condon 1987), which could indicate a
supernova-driven superbubble. This galaxy is believed to be a starburst galaxy
due to the presence of numerous XRBs (Strickland et al. 2001). There is no study
of the stellar population that gives an estimate of the age. The absence of an
LLAGN, the point sources, and the diffuse emission suggest that the X-ray
emission of this LINER is powered by stellar processes (perhaps a young
starburst).

2. 2006A&A...460...45G
Re:NGC 3628
NGC 3628 (UGC 6350, Arp 317C). The hard X-ray morphology shows an unresolved
nuclear component that also appears in the Fe image (Fig. 5). Chandra X-ray and
ground-based optical H{alpha}, arc-second resolution imaging is studied by
Strickland et al. (2004), with the main aim of determining both spectral and
spatial properties of the diffuse X-ray emission. They also show the total
counts for the nuclear region (an extraction of 1 kpc radius around the
dynamical center that, for this galaxy, corresponds to the central 20"), but no
spectral fitting was attempted. Our morphological classification does not agree
with that of Dudik et al. (2005), who have classified this galaxy as an object
displaying no nuclear source according to its morphology in Chandra ACIS data;
this galaxy is taken as a LINER/transition object and an upper limit of 2.7 x
10^37^ erg s^-1^ (corrected to our adopted distance) is given for its (2-10 keV)
nuclear luminosity, about 6 times fainter than our estimated luminosity. Note
that high absorption is derived from the position of this galaxy in the
color-color diagrams.

3. 2005MNRAS.357..361S
Re:NGC 3628
NGC 3628. The optical image of this edge-on galaxy is heavily obscured by a
prominent dust lane. The submillimetre emission follows the dust lane extremely
well; however, it is seen slightly to the north. This effect is caused by the
slight inclination of the galaxy on the sky; as the observed submillimetre
emission samples both the southern near side associated with the dust lane, and
the unseen northern far side.

4. 2005ApJS..157...59L
Re:NGC 3628
NGC 3628 is an edge-on Sb spiral galaxy at the distance of 10.6 Mpc with a
starburst nucleus, and distorted dust lanes due to its interaction with
other Leo Triplet galaxies NGC 3627 and NGC 3623. ULX1 is located on the
tip of the dust lane where distortions occur due to tidal interactions.
Note that the aspect solution of the HRI observation for this galaxy was
offset by up to 15".

5. 2004MNRAS.349.1193R
Re:NGC 3628
4.2.2 CXOU J112037.3+133429 (NGC 3628 X-2) This ULX had faded to a
luminosity of only ~7 x 10^38^ erg s^-1^ in our Chandra observations,
hence the spectra are of low quality, and the spectral models were not
strongly constrained. A power-law continuum was again the preferred
model in both epochs, though the MCDBB, also, gave a statistically
acceptable fit in the second epoch. The source flux appeared to change
little between the epochs, perhaps fading slightly in the three months
between observations. However, despite the low quality, the intrinsic
X-ray spectrum showed changes between the epochs, with the first
observation showing an intrinsically hard ({GAMMA}~ 1.57) but unobscured
power-law continuum, whereas the second observation showed a softer
intrinsic slope ({GAMMA}~ 2.2) with a low-energy turnover as a result of
absorption.

6. 2004MNRAS.349.1193R
Re:NGC 3628
A2 NGC 3628 X-2 (CXOU J112037.3+133429) This source was first detected
as point source two in a 1979 December Einstein IPC image of NGC 3628,
as reported by Bregman & Glassgold (1982), where it was observed to lie
at the eastern end of the edge-on galaxy disc. They derived a 0.3-2.9
keV luminosity of 2.1 x 10^39^ erg s^-1^ for NGC 3628 X-2, corrected to
our assumed a distance of 7.7 Mpc (this correction is assumed for all
the following luminosities). However, the reprocessed IPC data contour
map presented by Fabbiano, Kim & Trinchieri (1992) suggests, in
retrospect, that this flux may be an upper limit as a result of
confusion with two X-ray sources since resolved to the north of X-2.6 It
was also detected in three separate ROSAT observations, once with the
PSPC and twice with the HRI, as reported in Dahlem, Heckman & Fabbiano
(1995) and Dahlem et al. (1996). In particular, the 1991 November PSPC
observation provides a measurement of its X-ray luminosity in the 0.1-2
keV band of 0.6 x 10^39^ erg s^-1^, several times lower than the
Einstein value. This apparent variability is supported by the ROSAT HRI
images, which demonstrate that the count rate of NGC 3628 X-2 drops
substantially between 1991 December and 1994 May. NGC 3628 X-2 was also
detected in a 1993 December ASCA observation (Yaqoob et al. 1995). Its
ASCA SIS spectrum is well fitted with a simple power-law continuum
model, with {GAMMA}~ 2.4 and an absorption column of N_H_~ 7 x 10^21^
atom cm^-2^, well in excess of the foreground Galactic column. This
model implies luminosities of 0.7 and 1.7 x 10^39^ erg s^-1^ in the
0.5-2 and 2-10 keV bands, respectively, consistent with the ROSAT PSPC
measurement in the soft X-ray regime, though this must again be regarded
as an upper limit as a result of the likelihood of confusion with other
sources in the wide ASCA beam. Yaqoob et al. (1995) comment that the
X-ray spectrum of NGC 3628 X-2 is consistent with either a low-mass
X-ray binary or a very young supernova remnant, noting that if it is an
accreting source then it is substantially super-Eddington for a 1 M_sun_
object. Finally, NGC 3628 X-2 was not covered in the previous Chandra
ACIS-S observation of NGC 3628 discussed by Strickland et al. (2001), as
their observation was aligned along the minor axis of the galaxy.

7. 2004ApJS..151..193S
Re:NGC 3628
4.2.4. NGC 3628 NGC 3628, a member of the Leo triplet, hosts a compact
nuclear star-forming disk, approximately 300 pc in diameter based on the
nonthermal radio emission from young supernovae (Carral et al. 1990;
Irwin & Sofue 1996; Zhao et al. 1997; Cole, Mundell, & Pedlar 1998),
although the star formation rate is high within the entire central
kiloparsec (e.g., Irwin & Sofue 1996). An optical and H I tidal arm
extends ~100 kpc to the east of NGC 3628 (Kormendy & Bahcall 1974; Rots
1978; Haynes, Giovanelli, & Chincarini 1984), evidence of a close
interaction between NGC 3628 and NGC 3627 approximately 800 Myr ago,
based on the modeling of Rots (1978). A very distinct boxy/peanut-shaped
bulge suggests a bar may be present.
The Chandra X-ray observations (Fig. 7) reveal a wealth of detail,
generally in agreement with the Einstein and ROSAT observations of
Fabbiano et al. (1990), Read et al. (1997), and Dahlem et al. (1996).
We find extended hard X-ray emission associated with the optically
obscured nuclear starburst region (Figs. 7d and 7e). The major-axis
spatial extent of this emission (~8") is similar to the
6"-diameter ridge of 1.4 GHz (Cole et al. 1998) and 15 GHz radio
emission (Carral et al. 1990). The nuclear hard X-ray emission is most
likely predominantly a blend of spatially unresolved high-mass X-ray
binaries, rather than genuinely diffuse emission. The relative faintness
of the nuclear emission, as compared to other binaries seen in
projection within the central 2 kpc, is no doubt related to the high
absorbing column density toward the nucleus.
Relatively bright, but patchy, H{alpha}emission extends ~10" (~450 pc)
to both the north and south of the location of this nuclear disk
(Fig. 7c). We speculate that this is emission from a well-collimated
nuclear outflow, seen along sight lines of lower than normal
obscuration. The Chandra data support this hypothesis, as we also see
diffuse soft X-ray emission in the same region (Fig. 7b), again
preferentially extended along the minor axis. The adaptive smoothing
applied to Figure 7b tends to destroy details of the structure of the
diffuse emission. In the unsmoothed pixel maps the diffuse soft X-ray
emission clearly separates into two approximately rectangular regions,
separated from each other by a ~3" thick soft-X-ray-dark region,
corresponding spatially to the starburst region. The region to the north
the nucleus is ~8" wide (~390 pc) and extends ~12" (~580 pc) to the NNE
along the minor axis. The southern region has a similar major-axis
extent but only extends ~5" (~250 pc) to the SSW. The northern rectangle
or cylinder is the brighter of the two, consistent with the commonly
assumed geometry of NGC 3628, which is that the disk of NGC 3628 is
inclined so we see its northern face. These structures are likely to be
analogous to the nuclear outflow cones seen in NGC 253 and NGC 4945.
On the larger scale (Figs. 7g-7l), diffuse soft X-ray emission is again
found in association with H{alpha} emission, within the limited field of
view of the H{alpha} image. To both the north and south of the disk, the
westernmost edge of the diffuse emission is the brightest. There is
suggestive evidence for a eastern limb to the X-ray emission in both the
north and south, i.e., a bipolar, limb-brightened, cavity somewhat
similar to an open-ended hourglass in morphology (dashed and dotted
lines have been added to Figure 7 to guide the reader these faint
features, and the others we describe below).

8. 2004ApJS..151..193S
Re:NGC 3628
The X-ray emission to the south of the optical disk of the galaxy is
brightest in the region bounded by the ~4 kpc-long H{alpha} filament
discovered by Fabbiano et al. (1990; for a clearer presentation of this,
see Fig. 3 in Strickland 2002). This X-ray-plus-H{alpha} filament is very
similar to the ~650 pc long filament 6 in the dwarf starburst NGC 1569
(Martin, Heckman, & Kobulnicky 2002). This filament appears to join the
disk of the galaxy 20" (1.0 kpc) to the west of the nucleus, although
the inclination of the galaxy makes the location of the filament at
heights z <~ 1 kpc of the plane uncertain. To the east of the nucleus,
extraplanar H{alpha} filamentation is less pronounced and can only be
traced with confidence to ~2 kpc south of the plane. Diffuse soft X-ray
emission is present within this region but lacks any clearly developed
limb/filament of the sort found on the western limb.
On the northern side of the galaxy the H{alpha} emission appears in the
form of a series of faint <= 2 kpc-long filaments, primarily above the
nucleus and to the west of the nucleus. The westernmost extent of the
H{alpha} emission coincides with a bright H II complex {approx}40"
({approx}2 kpc) to the west of the nucleus. Extraplanar diffuse X-ray
emission is relatively bright above this region. East of the nucleus,
the lack of significant extraplanar H{alpha}emission is matched by a
similar lack in diffuse X-ray emission.
It is interesting to note that the base of the eastern and western edges
of the extraplanar H{alpha}and X-ray emission is similar to the maximum
extent of the box-shaped bulge seen in optical continuum images, which
may be related to a bar (see e.g., Irwin & Sofue 1996; Cole et
al. 1998).
What is the cause of the pronounced east/west emission asymmetry?
J. Bland-Hawthorn (2000, private communication) has suggested that some
of the asymmetry in the M82 wind, in particular the apparent ~10deg
bending of the flow away from the minor axis, might be due to ram
pressure acting on the wind as M82 moves through the intergroup
medium. If NGC 3628 is moving primarily to the west, then ram pressure
confinement or compression would lead to higher gas densities on the
western side of the wind and hence produce the higher H{alpha}and X-ray
surface brightness that is seen. Unfortunately, NGC 3628's motion within
the Leo triplet is unknown, as only the kinematic model of the Leo
triplet (Rots 1978) deals with the relative motion of NGC 3627 with
respect to NGC 3628.
With the higher sensitivity, and better point-source rejection afforded
by the use of Chandra, we robustly trace the diffuse emission out to
~2.4' (~7.0 kpc) to the north and ~3.7' (~10.8 kpc) to the south of the
disk. The maximum major-axis width of the emission is ~3.7' in the north
and slightly less to the south.
The diffuse X-ray emission to the north of the disk may extend even
further from galaxy (beyond the outermost contour in Fig. 7h), out to
~5.0' (~14.6 kpc), at low surface brightness, but the signal-to-noise
ratio is low, given that this region lies on the lower sensitivity
front-illuminated S2 chip.
The ability to robustly remove unrelated X-ray point sources makes much
more of a difference to determining the morphology and extent of the
diffuse X-ray emission in NGC 3628 than it does in nearer objects such
as M82 and NGC 253. Our large-scale diffuse emission image is closest in
resemblance to the smoothed point-source-subtracted ROSAT PSPC image of
Read et al. (1997). Many of the features in the images of Fabbiano et
al. (1990), and the ostensibly point-source-subtracted images of Dahlem
et al. (1996), are due to background point sources. Consequently, the
spatial extent of the diffuse emission we report is somewhat smaller
than previously reported values.

9. 2004A&A...418..877A
Re:NGC 3628
NGC 3628: this starburst/low level AGN exhibits extensive outgassed
plumes of neutral hydrogen and is apparently ejecting X-ray material
along its minor axis. Point X-ray sources might be associated with this
ejected material and a number have already turned out to be quasars
(Arp et al. 2002). We lists 7 of these quasars which have log L_X_
between 38.8 and 39.6 erg s^-1^. Column 10 shows that six of these
quasars fall within the same radial distances as most of the ULXs in
this table. The seventh, which has the strongest, log L_X_ =
39.6 erg s^-1^, falls at a greater distance, very similar to the radial
distance of the bright BL Lac from NGC 1365.

10. 2003ApJ...592...79M
Re:NGC 3628
A5. NGC 3628
NGC 3628 is a starbursting Sb galaxy that is a member of the Leo
Triplet. Located at a distance of 6.7 Mpc, it has an inclination angle
of 87^deg^ (Tully 1988). Imaged by Fabbiano, Heckman, & Keel (1990),
they detected a large plume extending about 9 kpc from the west side
of the galaxy (see also Dahlem et al. 1996). It is not exactly
perpendicular to the disk of the galaxy but lies at a position angle
of 210^deg^ (while the disk of the galaxy lies at a position angle of
104^deg^). In order to cover as much of this plume as possible, we
positioned the slit to extend only to vertical heights to the south
side of the disk, following the extent of the plume, rather than
centered on the disk of the galaxy (see Fig. 1). Fabbiano et al. also
obtained spectroscopic information along the minor axis of NGC 3628,
although not through the detected plume. They detected a midplane
[N II]/H{alpha} ratio of 0.4 that increased to greater than 1.0 at
higher |z|. [S II]/H{alpha} was also detected and observed to increase
with |z|, having a midplane value of 0.3 and rising to ~0.8 at large
heights. Shock ionization was proposed by Fabbiano et al. (1990) to
explain these line ratios. Figure 6 shows that pure shock or
photoionization/shock hybrid models are unable to reproduce the small
[O III]/H{alpha} line ratios in the extraplanar plume; this is
different from the conclusion of Fabbiano et al. (1990) who did not
have constraints on the [O III] emission. The photoionization/TML
hybrid models with a mixing gas temperature of log T = 5.0 are more
successful at explaining the observations. On the basis of this model,
the TML region would contribute roughly 50% to the observed line
ratios, although the exact amount differs between the [O III]/H{alpha}
and [S II]/H{alpha} data points. The plume may represent the interface
where hot wind gas mixes with entrained disk material (Dahlem et al.
1996).

11. 2003A&A...406..505R
Re:NGC 3628
NGC 3628 NGC 3628 is a member of the Leo triplet, which also includes
NGC 3623 and NGC 3627. It is a starburst galaxy with a very prominent
dust lane, which obscures most parts of the emission in the galactic
midplane. It has been studied extensively in almost all wavelength
regimes, and has also been the target for a multi-wavelength study in
the context of the disk-halo connection. Radio continuum observations
(Schlickeiser et al. 1984) reveal extended emission, and in the X-ray
regime a T~2x10^6^ K, extended halo has been detected by
sensitive PSPC observations with ROSAT (Dahlem et al. 1996). Prominent
X-ray emission, tracing the collimated outflow from the nuclear
starburst, was found to be spatially correlated with the H{alpha} plume
(Fabbiano et al. 1990). Extraplanar dust has already been detected
(Howk & Savage 1999; Rossa 2001). We also observed extended emission
from the nuclear outflow, localized extended emission (filamentary),
and several extraplanar H II regions.

12. 2002AJ....124..675C
Re:UGC 06350
F11176+1351 is the correct identification despite the large
FSC/optical offset. Large galaxy; flux density from Condon (1987).

13. 2001MNRAS.324..737R
Re:NGC 3628
A2 NGC 3628
NGC 3628 is an edge-on galaxy, also in the Leo Triplet, that shows clear
morphological distortions (e.g. in H I; Haynes, Giovanelli & Roberts 1979)
because of its interaction with the other Leo Triplet galaxies. Although
the nucleus is obscured by a prominent dust lane, there is evidence for a
nuclear starburst, though it may be intrinsically less active than in the
prototypical starburst galaxies NGC 253 and M82 (see Dahlem et al. 1996
and references therein).
The presence of the nuclear starburst has made NGC 3628 a popular target
for X-ray observations. Einstein observations of the galaxy detected two
point X-ray sources, one of which was coincident with the nucleus (Bregman
& Glassgold 1982), together with an X-ray bright outflow aligned along the
minor axis of the galaxy (Fabbiano, Heckman & Keel 1990). The presence of
the latter was confirmed by ROSAT PSPC observations (Dahlem et al. 1996).
The nuclear source has shown a remarkable level of variability, with its
flux changing by factors of up to ~20 between observations. This
establishes the domination of a single source which may be either a LLAGN
or luminous X-ray binary (Dahlem et al. 1995). If it is a luminous binary,
then its luminosity is such that it is probably an example of the so-called
ultraluminous X-ray source phenomena (ULX; Makishima et al. 2000) situated
close to the dynamical centre of the galaxy, as seen in many nearby
galaxies (Colbert & Mushotzky 1999). Spectral studies of NGC 3628 using
ASCA have shown the nuclear source to have a very flat spectral shape, with
simple power-law fits giving a spectral index {GAMMA} ~ 1.2 (Yaqoob et al.
1995). More complicated models (including one or more thermal plasma
components and a heavily absorbed power-law continuum) have also been
successfully fitted to the ASCA and ROSAT PSPC data (Dahlem, Weaver &
Heckman 1998; Ptak et al. 1999).

14. 2001ApJS..137..139S
Re:NGC 3628
NGC 3628. - There are no direct distance estimates. NGC 3628 is a member
of the NGC 3627 Group (Garcia 1993). Theureau et al. (1997) quote a
Cepheid-based distance to NGC 3627, and we adopt this distance for
NGC 3628.

15. 2000ApJS..129...93F
Re:NGC 3628
NGC 3628. - Like NGC 3627, this galaxy also belongs to the Leo
triplet. Our 8.4 GHz full-resolution map shows some extended emission to
the north and an eastern extension that is roughly aligned with the
projected disk of the galaxy. The nuclear region is clearly resolved.
The total flux density on our low-resolution map is about 70 mJy, 70% of
which is in ~ 15" diffuse emission. The NVSS measured 292 mJy, whereas
WB92, at lower resolution, detected 402 mJy, indicating resolved
large-scale emission. At 1.4 GHz Condon et al. (1990) measured 203 mJy
and 205 mJy at 5" and 1.5" resolution, respectively. These and our data
imply a steep-spectrum radio source, in agreement with the results from
the Effelsberg 100 m telescope (Schlickeiser, Werner, & Wielebinski
1984). Carral, Turner, & Ho (1990) observed this object at 15 GHz using
the VLA in A configuration and measured a total flux of 23 mJy. These
authors sampled the innermost part of the source and obtained a ~ 4"
string of a dozen components aligned with the major axis of the galaxy
that they suggest could be star-forming regions in the disk.

16. 1998ApJS..118..401D
Re:NGC 3628
For a full description of the NGC 3628 data, we refer to D96 and Dahlem,
Heckman, & Fabbiano (1995a). We found an indication of an X-shaped
emission cone near the center, which is resolved only in the HRI data
because of its small angular extent.

17. 1998ApJS..118..401D
Re:NGC 3628
Raw images
A few prominent point sources were detected in the disk of NGC 3628 in
both the 0.75 and 1.5 keV bands. No extended disk emission can be seen.
However, close to the nuclear area, extended 0.75 keV emission is
visible in the halo regime, extending perpendicular to the disk plane.
At 0.25 keV the galaxy is practically invisible at a resolution of
48.5" (Figs. 1-3 in D96).
Final images
This analysis was described in detail by D96. An extended soft X-ray
halo was detected after removal of point sources and smoothing the
residual emission to 3' (FWHM). The temperature of the halo gas is about
3 x 10^6^ K, and the extent of the halo is ~28 x 40 kpc, i.e., the
largest soft X-ray halo found so far in a spiral galaxy (Figs. 4-6 in
D96). These results were confirmed by Read et al. (1997).

18. 1998ApJS..118..401D
Re:NGC 3628
The PSPC resolves NGC 3628 into several discrete point sources along
with diffuse emission. For spatially resolved PSPC spectroscopy, we
followed D96 and have extracted diffuse halo emission from a large
elliptical region, being careful to exclude all of the point sources as
defined in the 1.5 keV map. The spatially resolved spectra of the core,
the integrated halo emission, and the integrated emission from the point
sources are all shown in SECTION 3.4.3 and Appendix C.
One group of companion point sources is resolved with ASCA and has
been designated as the "off-nuclear" source by Y95. This source is
clearly visible in the GIS image but falls in the gaps between the SIS
chips so that there are too few SIS counts to be useful. We have
extracted the GIS spectrum of this emission separately from the rest of
NGC 3628.
NGC 3628 is the only object in our sample for which the total
(joint) spectrum does not include all of the emission from the galaxy.
Owing to possible contamination of the ASCA spectrum by the off-nuclear
source, we have chosen small extraction regions for the integral galaxy
spectrum. For ASCA these regions are circular, with radii of 3', and for
the PSPC elliptical, with half axes of a = 3.25' and b = 4.25'. The
regions include the galaxy disk and about 25% of the diffuse halo
emission.

19. 1995ApJS...98..477H
Re:NGC 3628
The location of the nucleus was very difficult to identify in the 2-D
spectrum; a large dust lane obscures much of the light in this edge-on
spiral.

20. 1995A&A...302..691D
Re:NGC 3628
Reuter et al. (1991) mapped this galaxy with the VLA at {lambda}20 cm.
They found a similar morphology as we did in our {lambda}2.8 cm
measurements. A strong central source (the well-known starburst) can be
seen in our map. The decrease of surface brightness along the major axis
is not smooth; there are a few maxima along the major axis on either side
of the nucleus. They may be associated with (tangentially seen) spiral
arms.
The polarized intensity shows two clear maxima on either side of the
nuclear region above and below the plane. About 25% of these maxima may
be caused by spurious polarization. Linear polarization is also detected
at a 2-{sigma} level (first contour) east and west of the nucleus. These
features are certainly real because at their distance from the central
source instrumental polarization is already distinctly reduced. In the
outer regions the linearly polarized emission is not bright enough to be
detected. The orientation of the observed magnetic field lines is in
general parallel to the galactic plane, as in NGC 891.

21. 1993A&AS...97..887B
Re:NGC 3628
NGC 3623, NGC 3627 and NGC 3628 make up the Leo Triplet. NGC 3623 is an
Sa galaxy that has defied several detection attempts, placing it below
the FIR-CO relationship. NGC 3627 is a LINER (SM) where we detect CO(2-1)
out to 2' (5.4 kpc) to the North and South (as far out as observed) and
distinguish the arm/interarm regions. NGC 3628 has a higher dust
temperature and stronger CO emission. NGC 3628 is discussed further in
Boissey et al. (1987) and Reuter et al. (1991) and NGC 3627 in our Paper
IV on radial distributions and rotation curves of the better observed
sample galaxies.

22. 1976RC2...C...0000d
Re:NGC 3628
= Arp 317
= VV 308
= Holm 246c
In M66 Group.
Very faint extensions.
Photograph:
Mem. S.A. Ital., 44, 359, 1973.
A.J., 79, 671, 1974.
Photometry:
Mem. S.A. Ital., 44, 359, 1973.
Isodensitometry:
A.J., 79, 671, 1974.
Rotation Curve:
Systemic Velocity Astr. Ap., 8, 364, 1970.
HII Regions:
"Atlas and Catalogue", Univ. Washington, Seattle, 1966.
Radio Observations:
Australian J. Phys., 19, 565, 1966.
Ap. J., 150, 413, 1967.
M.N.R.A.S., 167, 251, 1974.

23. 1973UGC...C...0000N
Re:UGC 06350
VV 308b, Arp 317
Sb pec (de Vaucouleurs), Sb+ (Holmberg)
Square-shaped absorption lane slightly inclined to the symmetry plane
VV picture shows only this object
See UGC 06346

24. 1964RC1...C...0000d
Re:NGC 3628
= Holm 246c
Edge-on. It has two equatorial planes, marked by dark matter tilted a few
degrees to each other.
In the M65/M66 Group.
Heidelberg Veroff. Vol. 9, 1926 major axis dimension (17.0 arcmin) is excessive.
Drawing:
Erg. d. Exakt. Naturwiss., XXIX, 376, 1956.
Photometry:
Izv. Pulkovo, 20, No.156, 87, 1956.
Sov. A.J., 32, 16, 1955.

25. 1959VV....C...0000V
Re:VV 308b
= NGC 3628
V = +728 km/sec
Yerkes Type: S:S7:

26. 1956AJ.....61...97H
Re:NGC 3628
HMS Note No. 110
Slit on brighter nuclear region north of dark lane.

27. 1918PLicO..13....9C
Re:NGC 3628
Moderately bright; 12' x 1.5' in p.a. 100^deg^. There are no well marked
condonsations. A wide dark lane runs down its entire length; the southern
portion is the narrower and fainter. An edgewise spiral. See Abs. Eff. 19 s.n.


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