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Notes for object NGC 1265

14 note(s) found in NED.


1. 2006ApJS..164..307M
Re:3C 083.1
The near-infrared image shows an elliptical elongated north to south and
covering most of the detector area. The image reveals a thin dust lane wrapping
around the nucleus. A bright nearby star generates diffraction spikes crossing
the detector. Some faint globular clusters are also visible.

2. 2006ApJ...642...96E
Re:NGC 1265
We attempted to fit several models to the nuclear spectrum of 3C 83.1B but found
that the only one that gave an acceptable fit ({chi}^2^ = 9.45 for 12 dof)
consisted of the sum of an absorbed power law and thermal emission of abundance
0.3 of solar. The best-fitting spectral parameters for this model are N_H_ =
3.2^+0.08^_-0.7_ x 10^22^ atoms cm^-2^, {GAMMA} = 2.00^+0.27^_-0.20_. The
temperature of the thermal component is 0.58^+0.15^_-0.14_ keV, with
normalization 9.69^+2.95^_-2.74_ x 10^-6^. These parameters are consistent with
those measured by Sun et al. (2005), who performed the original observation.

3. 2002AJ....124..675C
Re:UGC 02651
Very extended head-tail radio source; the 1.4 GHz
flux density is from Condon & Broderick (1988).

4. 2000ApJS..131...95F
Re:VSOP J0318+4151
J0318+4151 (NGC 1265, 3C 83.1). - No detection: according to global VLBI
observations at 5 GHz by Xu, O'Dea, & Biretta (1999), the core of this
double-tail radio galaxy has a brightness of 13 mJy beam^-1^, too weak for
us to be detected.

5. 2000ApJS..129...33D
Re:3C 083.1
3C 83.1 (NGC 1265), z = 0.0255. - This galaxy is a member of the
Perseus cluster. It shows a sharp, well defined edge-on disk (Fig. 5),
although a nearby star at 3" distance from the galaxy core makes
modeling of the galaxy impossible.
The radio map shows a "narrow angle tail" radio structure, with
several wiggles in the radio jet before the large-scale radio tail bends
toward the northwest. Figure 5 shows that the inner jet and dust disk
are oriented almost perpendicular to each other.

6. 1999ApJS..122...81M
Re:3C 083.1
3C 83.1 (NGC 1265). - NGC 1265 (the host of 3C 83.1) shows a narrow dust
lane in our HST image. A diffraction spike from a bright nearby star to
the east crosses the center of the galaxy. The dust lane is oriented
along a P.A. of ~ 171^deg^, nearly orthogonal to the radio jet, and is
approximately 1.5 kpc in length. Its existence is consistent with the
suggestion of O'Dea & Owen (1987) that there is an external foreground
screen located in the interstellar medium that explains the observed
variations of the differential rotation measure. A nearby elliptical
lies 44" (24 kpc) east of NGC 1265.

7. 1998ApJS..114..177Z
Re:3C 083.1
3C 83.1.--This galaxy is an archetypical narrow angle tail source (O'Dea & Owen
1986). Hardcastle et al. (1996) claim that the jet of 3C 83.1 is similar in
symmetry and polarization to that of 3C 66B. The F702W image shows an
elliptical galaxy that is elongated slightly toward the north and south (the
object close to the nucleus of the galaxy is a saturated, bright star). This
ellipticity seems to go all the way into the center (Poulain, Nieto, & Davoust
1992), but the inner regions of the F702W image show two peaks separated by
0.5. No jet is visible in this image. It is likely that a nuclear disk (~1.9"
in length, spanning north to south) causes this structure. At UV wavelengths,
the galaxy appears to have some extended and some nuclear UV flux (the PSF
contribution is 39+/-6, and the q-parameter is only 0.58); however, the S/N
ratio is rather poor.

8. 1998A&A...331..475F
Re:NGC 1265
3.2. NGC 1265 - 0314+416
NGC 1265 is located in a peripheral region of the Perseus Cluster, at about 27'
north-west of the active galaxy NGC 1275 (3C 84). Previous studies of this
source are listed in Mack et al. (1993), who obtained the first image at 10.6
GHz. The 10.6-GHz map presented here (Fig. 2) has a much higher sensitivity
than that of Mack et al. (1993), owing to a longer observing time. We also
obtained observations at 4750 MHz and extracted WSRT maps at 327 and 610 MHz
from the Perseus Cluster image obtained by Sijbring (1993). We note that the
very-low-brightness feature first reported by Gisler & Miley (1979) and
observed with higher sensitivity and dynamic range by Burns et al. (1992) and
by Sijbring (1993) is just indicated in our 10.6-GHz map if smoothed to a 1.5'
beam, especially in the (more sensitive) map of linear polarization. At the
other frequencies the feature, if present, is concealed by the sidelobe
structure which we could not yet clean at this wavelength.
All maps were smoothed to the common resolution of 147" for a multifrequency
comparison. The trend of the spectral index along the ridge of maximum
brightness for the 3 frequency pairs is presented in Fig. 5. Between 0.3 and
4.8 GHz it is in the range 0.5-0.8, while beyond 4.8 GHz a strong steepening is
evident, which increases with distance from the core, reaching a value
{alpha}>2 at the tail's end.
Strong linear polarization is found in the external tail region (see Fig. 6).
The polarization percentage at 10.6 GHz increases along the tail up to ~40%. At
4.8 GHz, the degree of polarization is comparable to that at 10.6 GHz up to 5'
from the core, and is lower beyond that distance. The electric vector at both
frequencies is perpendicular to the tail orientation.

9. 1996ApJS..107..541L
Re:NGC 1265
0314+416.--The slit was positioned to avoid a foreground star projected close
to the center of the galaxy.

10. 1992A&AS...95..129P
Re:NGC 1265
NGC 1265: The bright star at ~2 arcsec from the nucleus prevents any
reliable isophotal analysis. Probably E from profile (?)

11. 1988ApJ...328..114P
Re:NGC 1265
0314 +416 (3C 83.1B, NGC 1265).-NGC 1265 is a famous "twin tail" source
of Fanaroff-Riley class I. A recent VLA study is that of O'Dea and Owen
(1986), which indicates that the nuclear component has a flux density of
25 mJy at 5 GHz. This component has been detected in a VLBI observation
at 5 GHz (37 +- 6 mJy on the Westerbork-Effelsberg baseline: van Breugel
et al. 1981), but it is too weak for detection in our finding survey,
and it was not included in the mapping observations.
Where necessary, we have assumed H_0_ = 100h km s^-1^ Mpc^-1^
and q_0_ = 0.5 to convert angles to projected distances.

12. 1976RC2...C...0000d
Re:NGC 1265
= 3C 083.1
In the Perseus Cluster.
There is a star superposed.
Radio galaxy with a tail.
Description and Classification:
Ap. J., 140, 35, 1964.
P.A.S.P., 80, 129, 1968.
Photograph:
Ap. J., 168, 321, 1971.
Astrophys. Lett., 14, 7, 1973.
Photometry:
Astrophys. Lett., 14, 7, 1973.
Photometry:(VBR)
Ap. J., 183, 731, 1973.
Dynamics:
Bull. A.A.S., 3, 238, 1971.
Ap. J., 168, 321, 1971.
For the velocities of many anonymous objects and the dynamics
of clusters, see also A.J., 77, 4, 1972.
Radio Observations:
Nature, 205, 488, 1965.
Nature, 237, 269, 1972.
Nature, 244, 502, 1973.
M.N.R.A.S., 138, 1, 1968.
M.N.R.A.S., 161, 167, 1973.
Sov. A.J., 13, 881, 1970.
Astr. Ap., 26, 413, 1973.
IAU Symp. No.58, p.113, 1974.

13. 1973UGC...C...0000N
Re:UGC 02651
Perseus cluster
Companions 2.7, 246, 0.7 x 0.4, diffuse; and 4.2, 308, (0.5 x 0.4)

14. 1964ApJ...140...35M
Re:3C 083.1
No. ll.-In cluster A426, richness 2. Redshift from Humason et al. (1956).


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