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Notes for object NGC 0383

23 note(s) found in NED.

1. 2009ApJ...693.1142S
Re:NGC 0383
NGC 383 hosts a bright FRI radio source 3C31. There is a background cluster
centered on 2MASX J01065891+3209285 at z = 0.1116. We derived the surface
brightness profile centered on the background cluster and also analyzed a short
exposure (ObsID 3555, 5.1 ks) centered on the background cluster. The cluster
emission is detected to ~4' radius. In the analysis for NGC 383, we excluded the
region within 6.5' of 2MASX J01065891+3209285, which is a bit larger than its
r_500_ (5.9' for kT = 2.3 keV).

2. 2006ApJS..164..307M
Re:3C 031
This galaxy covers most of the area of the detector. A face on dust ring around
the galaxy's nucleus can be seen on the infrared image. The WFPC2 image shows
that this dust ring is composed of several dust strands with a larger absorption
on the southwestern side (Martel et al. 1999 and de Koff et al. 2000).

3. 2006ApJ...642...96E
Re:3C 031
We initially attempted to model the source spectrum with a single unabsorbed
power law. However, the fit was poor ({chi}^2^ = 49.3 for 27 dof [degrees of
freedom]), with strong residuals at ~1 keV, suggesting that a contribution from
thermal emission is necessary. The fit was substantially improved
({DELTA}{chi}^2^ = 39.7 for two additional parameters) by adding a thermal
(Apec) model of temperature kT = 0.68^+0.08^_-0.07_ keV, abundance 0.3 of solar,
and normalization 3.39^+0.80^_-0.85_ x 10^-5^. No further significant
improvement was obtained by including intrinsic absorption in the model fit. The
1 keV flux density and spectral index are consistent with previously published
Chandra results (Hardcastle et al. 2002; Donato et al. 2004). The 0.5-5 keV
radial surface brightness shows a deficit of counts approaching a factor of 2
compared with those measured spectrally. As discussed by Hardcastle et al.
(2002), the discrepancy may be resolved by postulating that there exists an
additional, unresolved dense component of thermal emission that lies clo se to
the core.

4. 2006A&A...453..447E
Re:3C 031
3C 31
The cool X-ray environment of the extended radio source 3C 31 is associated with
a group of galaxies. X-ray measurements suggest that this group shows properties
similar to a cool core of a galaxy cluster. Therefore, it seems to be a good
case to test our model in a different situation. The parameters for the gas were
taken from Hardcastle et al. (2002). However we use the total luminosity from
Komossa & Bohringer (1999).
Detailed RM measurements have been carried out by Laing et al. (in prep.).
They determine the RM dispersion to be 25 rad m^-2^(Laing, private

5. 2003ApJS..148..419N
Re:NGC 0383
NGC 383 (UGC 689).-This S0 galaxy has a nuclear dust disk (b/a =
0.77). It has a core-jet radio morphology on VLBA scales and a twin-jet
morphology on VLA scales. The STIS slits were aligned parallel to the
galaxy major axis. The central kinematic and flux properties are listed
in Table 8; the gas exhibits a regular rotation profile. In the negative
offset side slit there is a dip in the velocity dispersion profile at a
position close to the nucleus. The fit to the central spectrum is
improved by the addition of a broad component. Data for this galaxy are
shown in Figure 4 (see key in Fig. 1 for an explanation of these plots).

6. 2003A&A...403..889T
Re:3C 031
3C 31. In Paper I we derived, from Rosat/PSPC data, a nuclear flux of
{approx}2.0 x 10^-13^ erg cm^-2^ s^-1^, uncertain within a factor
{approx}2 (1{sigma}) and without any estimate of the spectral index.
From the Chandra observation of November 2000 (Hardcastle et al. 2002)
the inner region has been resolved in the pointlike nucleus and a jet,
with comparable luminosities in the Rosat X-ray band. The spectrum is
quite flat ({alpha}_x_ = 0.5 ^+0.3^_-0.2_), with no evidence of a local
absorption (N_H_ = 1.5^+2.2^_-1.4_ x 10^21^ cm^-2^). The shape of the
SED is very similar to that of 3C 189 (see Fig. 1). The flux is
{approx}5 x 10^-14^ erg cm^-2^ s^-1^, i.e. {approx}4 times less than
detected in Rosat but still consistent considering the statistical
fluctuations and the jet contribution.

7. 2002AJ....124..675C
Re:UGC 00689
3C 31. This radio source is very extended (Andernach et al. 1992), so
the NVSS flux density is probably too low.

8. 2001ApJ...552..508G
Re:3C 031
0104+32 (3C 31). - Observations at 6 cm were published in Lara et al.

9. 2001AJ....121..808C
Re:NGC 0383
NGC 383. - A linear dust feature is seen in the color map. IRAS detected
this galaxy at 60 and 100 microns (Knapp et al. 1989).

10. 2000ApJS..129...33D
Re:3C 031
3C 31 (NGC 383), z = 0.0167. - This galaxy is the brightest in a
chain of eight galaxies and appears to be interacting with a close
(~ 30") companion NGC 382 (Arp 331). Low surface brightness emission
connects the two galaxies. Figure 2 shows a spectacular face-on disk in
which as many as eight dust strands are visible, with a typical
projected separation of about 70 pc (see also Verdoes Kleijn et al.
1999). The disk shows more absorption on the southwestern side than the
other, presumably indicating the orientation of the disk with respect to
the observer; from the axial ratio (b/a) of the dust disk, the
southwestern region can then be taken as pointing toward the observer
with an inclination of arccos(b/a) ~ 41^deg^ with respect to the plane
of the sky. This agrees with the result of Fraix-Burnet, Golombek, &
Macchetto (1991), who derived the inclination using the same method.
The large-scale radio map shows well-defined radio jets with
several sharp bends within a projected distance of 100 kpc from the
galaxy. Figure 2 shows the innermost part of the radio jet superposed on
the HST image; the radio map shows a bright radio core and a gap between
the core and the jet corresponding to about the projected size of the
dust disk. No direct evidence is found for a relation between the
morphology of the radio source and the dust.

11. 2000AJ....120.2950X
Re:UGC 00689
UGC 00689 (NGC 383=3C 31)-On the arcsecond scale, this source
displays an S-type symmetry and a sidedness ratio of >=20. The
sidedness ratio of our VLBA image is >=6. Lara et al. (1997) measured
sidedness ratios at 30", 15", and 8 mas to be 1.5, 6, and greater than
16, respectively, with VLA and VLBI data at 5 GHz. The spectral index of
the VLBI core between 1.65 and 4.95 GHz is found to be -0.44, indicating
an inverted spectrum and assuming no flux density variations between our
observations on 1997 April 9 and those of Lara et al. (1997) on 1993
February 25.

12. 2000A&A...362..871C
Re:NGC 0383
0104+32 (NGC 383, 3C 31): An extended circum-nuclear dusty disk is seen
at low inclination, with an unresolved nuclear component at its center.
The disk diameter is ~ 7" (2.5 kpc) along the major axis
(P.A. ~ 40^deg^). The galaxy belongs to a chain of which it is the
brightest member. See also Martel et al. (1999) and Verdoes Klein et al.

13. 1999MNRAS.309..969H
Re:3C 031
3.2 3C 31
Our results for this FRI radio galaxy (NGC 383) are consistent with
Trussoni et al. (1997). PSPC images show extended emission, but the HRI
detects only point-like emission, with a component coincident with
3C 31's nucleus. Emission coincident with NGC 380 and 379, other members
of 3C 31's group, is also detected.

14. 1999MNRAS.306..857C
Re:1RXS J010721.2+322254
RXJ0107.4+3227 This cluster is also known as the group IV Zw 038, and
the galaxy observed (NGC 383) is associated with the radio source 3C31.
Colina & Perez-Fournon (1990) note a central dust lane in this galaxy.

15. 1999ApJS..122...81M
Re:3C 031
3C 31 (NGC 383). - Our HST image reveals a beautiful, nearly face-on
dust disk surrounding the galaxy's nucleus (Fig. 8). Its diameter is
approximately 7" (2.5 kpc) along the major axis, and its inclination is
i ~ 45^deg^. Surprisingly, the core of the southwest companion, NGC 382,
also shows a very similar disk, though slightly smaller, 5" (1.8 kpc),
and at a smaller inclination, i ~ 35^deg^ (Fig. 9). The two disks are
not completely opaque there are enhancements in the light distribution
across their surfaces. These ridges of emission are thin, partially
broken, and generally follow the circular shape of the disks. The origin
of this emission is speculative. It could come from stellar radiation
originating behind the disks and punching through gaps in the disks, or
from nuclear light scattered off the uneven surface of the disks, or
even from within the disks themselves, perhaps from star-forming
regions. The nucleus of NGC 383 is unresolved. The presence of such
morphological peculiarities in the cores of these two fascinating
galaxies suggests that they are interacting.

16. 1999AJ....118.2592V
Re:NGC 0383
NGC 383 is the brightest galaxy in the Zwicky cluster 0107.5+3212
(Sakai, Giovanelli, & Wegner 1994). NGC 383 is inside a chain of
galaxies and forms a dumbbell pair with Arp 331 (NGC 382), which is at
34" (11 kpc). NGC 383 has a nearly face-on central dust disk (diameter
2.3 kpc/7.4"), which shows a spiral structure with a counterclockwise
orientation. The spiral structure becomes flocculent at the outer edges.
Martel et al. (1999) detected a dust disk in the companion NGC 382 as
well. NGC 383 has a central unresolved bright H{alpha} + [N II]
emission peak with low surface brightness emission extending out to
~1" (300 pc) around it. Owen, O'Dea, & Keel (1990) detected a rotating
extended emission disk from a spectroscopic study. NGC 383 has a nuclear
point source that is clearly bluer than its surroundings. Komossa &
Bohringer (1999) performed an X-ray study of the NGC 383 group and found
indications for a hard X-ray component that might be associated with the
central AGN. Our isophotal analysis is in very good agreement with
previous ground-based studies by Fraix-Burnet, Golombek, & Macchetto
(1991) and De Juan et al. (1994). The latter found an increase in
ellipticity from 0.1 to 0.3 outward of r ~ 10". The radio jet has been
extensively studied (e.g., Lara et al. 1997 and references therein). The
radio jet shows a distorted morphology, suggesting gravitational
interaction between NGC 383 and its companion NGC 382 (Blandford & Icke
1978; Parma, Cameron, & de Ruiter 1991). However, the optical isophotes
out to scales larger than our HST imaging show no indication of
interaction (Fraix-Burnet et al. 1991). Evidence for an optical jet was
claimed by Butcher, van Breugel, & Miley (1980), but not confirmed by
later studies (Keel 1988; Owen et al. 1990; Fraix-Burnet et al. 1991).

17. 1997A&A...327...27T
Re:3C 031
2.1. 3C 31 (B2 0104+32, NGC 383)
The radio source 3C 31 is associated with the galaxy NGC 383, the brightest
member of the group (chain) Arp 331, in the Perseus-Pisces super-cluster,
comprising NGC 379, NGC 380, and NGC 382-386 (NGC 382 is at ~35" from NGC 383
in the SW direction). The galaxy shows a dust lane at ~3.7" from the central
region (Fraix-Burnet et al. 1991) and is also an infrared source with a total
luminosity in the range 10-100 microns of L_IR_~8x10^43^ erg s^-1^ (Impey,
Wynn-Williams & Becklin 1990).
At radio wavelengths, 3C 31 is an intermediate luminosity source (P_1.4 GHz_
~10^24^ W Hz^-1^) that shows two prominent radio jets emerging from a central
unresolved core, for a total extent of ~25' (~750 kpc, see Strom et al. 1983).
Observations with the IPC detector of the Einstein satellite provided quite
detailed data on the hot gas surrounding the galaxy (Morganti et al. 1988). In
the HRI, an unresolved source was detected coincident with the galactic nucleus
and the radio core.

18. 1976RC2...C...0000d
Re:NGC 0383
= 3C 031

19. 1973UGC...C...0000N
Re:UGC 00689
VV 193 (with UGC 00688)
Brightest in a chain of 8 galaxies, this chain is Arp 331
S0 (de Vaucouleurs), Pisces cloud
Paired with U688 at 0.55, 2.3
01 04.8 {+32 07} = {NGC 387} at 2.1, 127, 0.15 x 0.12, E3 (de Vaucouleurs),
m={16.:}, v = 5555, v(0) = 5753
At least 3 fainter group members
See UGC 00682, UGC 00683, UGC 00686, UGC 00687, UGC 00688
{UGC incorrectly notes "+32 05", "NGC 386", and "15.4". H. Corwin}

20. 1971CGPG..C...0000Z
Re:CGPG 0104.7+3209
NGC 0383
One of the brighter members of the Group C2
which is a prominent part of the Pisces Cloud
= +4,888 km/sec
m(pg) = 13.6

21. 1964RC1...C...0000d
Re:NGC 0383
In a group of ellipticals and lenticulars including:
NGC 0375, NGC 0379, NGC 0380, NGC 0382, NGC 0383, NGC 0384,
NGC 0385, NGC 0386, and NGC0388
Brightest galaxy is NGC 0383.
P.A.S.P., 71, 191, 1961.
P.A.S.P., 73, 191, 1961.
A.J., 66, 545, 554, 1961.

22. 1961AJ.....66..541B
Re:NGC 0383
5. NGC 383 Group
NGC 375, 379, 380, 382, 383, 384, 385, 386, and 388 are a group of nine galaxies
for which velocities are given by Humason et al. (1956). They form part of what
Hubble and Humason (1931) called the Pisces group, which, they suggested,
consisted of about 25 elliptical galaxies. They are the brightest members.
Zwicky (1937) has suggested that the group is contained in a large and elongated
cluster extending over 15 square degrees or more. The nine galaxies listed above
have rather a large velocity dispersion, and application of the virial theorem
gives galactic masses in the range 10^11^-10^13^ M_sun_ and mass-to-light ratios
of about 260 (Burbidge and Burbidge 1961c). Thus if these nine galaxies,
together with the other 16, form a separate physical group, as was suggested by
Hubble and Humason, then the group is probably unstable unless there is much
dark material present.

23. 1959VV....C...0000V
Re:VV 193a
= NGC 0383
V= +5,086 km/sec

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