Date and Time of the Query: 2019-06-25 T19:20:48 PDT
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Notes for object NGC 0507

13 note(s) found in NED.

1. 2006ApJ...639..136H
Re:NGC 0507
NGC 507. We extracted spectra in seven contiguous, concentric annuli, with
outer radii 0.6',1.0', 1.3', 1.9', 2.7', 4.0', and 5.6' (14, 23, 31, 44,
63, 93, and 130 kpc), respectively. To improve the abundance constraints,
we tied Z_Fe_ between the first and second annuli, the third and fourth
annuli, and the fifth and sixth annuli. The temperatures were allowed to
vary in each annulus. The best-fitting temperature profile rose from ~1
keV in the center to ~1.3 keV in the outermost radii. The abundance
profile is essentially flat, except for the outermost bin. The measured
abundances generally agreed with Kraft et al. (2004), who used the Chandra
data. We did not find any statistically significant improvement in chi^2^
if a second hot gas component was added (delta chi^2^ ~ 2). Nevertheless,
to compare with the XMM results of Kim & Fabbiano (2004b), we experimented
with the addition of such a component to the innermost bin. We found that
this increased the central Z_Fe_ to 0.87^+0.64^_+0.28_, which is
marginally inconsistent with Z_Fe_ ~ 2 found by these authors. The reason
for this discrepancy is unclear since the temperatures of these components
(kT ~ 0.8 and 1.4 keV) and the total flux of unresolved point sources
within D_25_ (~4 x 10^-13^ ergs s^-1^ cm^-2^), which might systematically
affect Z_Fe_, were very similar to those found by Kim & Fabbiano (2004b).
Nonetheless, our abundance ratios were broadly consistent with those
reported for XMM.

2. 2002AJ....124..675C
Re:UGC 00938
The NVSS identification is a double radio source straddling the

3. 2001MNRAS.326.1563J
Re:6C* 0120+329
6C*0120+329 This source has an angular size {theta} ~ 95 arcsec
(Parma et al. 1986), so is excluded from the sample. The redshift of this
source is z = 0.0164 (de Ruiter et al. 1986).

4. 2000A&A...362..871C
Re:NGC 0507
0120+33 (NGC 507): Brightest galaxy of the Zw cluster 0107+3212. The
galaxy appears very regular and smooth.

5. 1999MNRAS.310...30C
Re:B2 0120+33
B2 0120+33
Identified with the galaxy NGC 507, the source lies in Zwicky cluster
0107+3212 and is one of the brightest galaxies in a very dense region.
Extended X-ray emission is seen out to a radius of at least 16 arcmin,
and there is evidence for the presence of a cooling flow and possible
undetected cooling clumps distributed at large radii (Kim & Fabbiano
1995). B2 0120+33 has a steep radio spectrum and weak core. It may be
a source with particularly weak jets, or possibly a remnant of a radio
galaxy whose nuclear engine is almost inactive and whose luminosity has
decreased due to synchrotron or adiabatic losses (Fanti et al. 1987).
The HRI map shows the central region of this source to be
asymmetrical, with a large extended emission region to the south-west.
Radial-profile fitting of the innermost parts of this galaxy with point,
{beta}, and point + {beta} models, show that a good fit to the data is
achieved by using a single {beta} model with {beta} = 0.67, which gives
a core radius of 4 arcsec. The {beta} + point model gives a marginally
better fit, but the additional component is not significant on an F-test
at the 90 per cent confidence level. Therefore, we have taken the total
counts from the inner regions of this source as an upper limit on any
unresolved emission present, keeping in mind that this may also include
a cooling-flow contribution (this also holds for other sources with
possible unresolved cooling flows such as B2 0149+35, 1346+26 and

6. 1999MNRAS.306..857C
Re:RX J0123.6+3315
NGC 499 and NGC 507 form a double system.

7. 1999MNRAS.306..857C
Re:1RXS J012337.2+331508
RXJ0123.2+3327 (NGC 499) and RXJ0123.6+3315 (NGC 507) form a double

8. 1986A&AS...64..135P
Re:B2 0120+33
The radio galaxy (NGC 507) is located in the Zwicky Cluster 0107+3212,
and is the brightest (or second brightest) galaxy in a very dense region:
there are 80 galaxies with magnitude m_pg_ < 15.7 within a projected
distance of 1.5 Mpc from NGC 507. This is the so-called Pisces Group.
The radio emission is very faint and diffuse: the surface
brightness is of the order of 0.05 mJy per square arcsec. The radio
spectrum of the source is very steep (Ekers et al 1981). Although
the radio structure is clearly very distorted, a more detailed study
of the source morphology is difficult, due to its faintness.

9. 1977A&AS...29..279F
Re:B2 0120+33
0120+33 The radio source, detected at 1415 MHz, is displaced west of the
center of the galaxy by 15", but it is still well within the main body
of it. At 610 MHz a second component may have been detected, at a level
of 40 mJy (~6{sigma}) east of the galaxy. The WSRT 1415 MHz flux density
is significantly lower than the total power flux density from the Nancay
telescope (reported in paper II), suggesting a low brightness large
scale structure. The galaxy belongs to the Zwicky cluster (0lh07.5m +

10. 1976RC2...C...0000d
Re:NGC 0507
= Arp 229
= VV 207
= B2 radio source
Extensive halo.
Brightest in cluster with NGC 0495, NGC 0499, and NGC 0508.
NGC 0508 is 1.5 arcmin north.
NGC 0504 is 4.0 arcmin south-preceding.
Ap. J., 173, 485, 1972.
Photometry: (UBVR)
Ap. J., 178, 1, 1972.
Ap. J., 183, 731, 1973.
A.J., 75, 695, 1970.

11. 1973UGC...C...0000N
Re:UGC 00938
VV 207, Arp 229
E3 (de Vaucouleurs)
`Circular or near circular rings of small density difference' (Arp)
Paired with UGC 00939 at 1.5, 6 (inside envelope)

12. 1964RC1...C...0000d
Re:NGC 0507
In a group consisting of NGC 0495, NGC 0499 and NGC 0507.
NGC 0507 is the brightest.

13. 1959VV....C...0000V
Re:VV 207a
= NGC 0507
V = +5,121 km/sec.

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