Date and Time of the Query: 2019-04-24 T06:28:58 PDT
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Notes for object NGC 7465

14 note(s) found in NED.

1. 2005MNRAS.364.1253V
Re:NGC 7465
NGC 7463. This galaxy is part of a triple system with NGC 7464 (to the S of NGC
7463) and NGC 7465 (not shown in Fig. 1). At 850 {mu}m we clearly detect
emission from both NGC 7463 and 7464, which seem to be joined by a bridge of
submm emission. The flux listed in Table 1 is for NGC 7463 alone, measured in an
aperture corresponding to its main optical extent. Unfortunately, a very noisy
bolometer to the SE prevents us measuring the flux from the eastern half of NGC
7464, but excluding this region we measure a flux for the pair of 0.051+/-0.012
Jy, though obviously a lower limit.
An IRAS source is associated with NGC 7465, which is resolved from the other
members of the system at 60 {mu}m (HIRES; Aumann, Fowler & Melnyk 1990). Dust
properties of this system (using SCUBA data observed as part of SLUGS) are
studied in detail by Thomas et al. (2002).

2. 2002AJ....124..675C
Re:UGC 12317
See the UGC 12316 notes.

3. 2000ApJS..128..139F
Re:NGC 7465
5.12. NGC 7465 (Markarian 313) - Seyfert 2
NGC 7465 is an SB0 galaxy hosting a Seyfert 2 nucleus. It has been
studied mostly as a part of the NGC 7448 group of galaxies (Li &
Seaquist 1994; van Driel et al. 1992). It forms an interacting pair with
NGC 7464 and displays an H I ring that could be polar (Li & Seaquist
1994). The continuum images and color maps of this galaxy in Figure 24
reveal a complex structure. The brightest continuum regions are found
within 5" (0.7 kpc) of the nucleus. They display an inverted S-shaped
morphology with a photometric major axis P.A. of ~ 120^deg^ in the inner
4" (560 pc), increasing progressively toward ~ 160^deg^-165^deg^ beyond
10" (1.4 kpc). This change in P.A. is consistent with previous
ground-based continuum images (Figs. 2h and 2m in van Driel et al. 1992;
M96). The morphology of the central regions southeast of the nucleus is
strongly affected by a set of dust lanes running perpendicular to the
photometric major axis of the galaxy (Fig. 24, right-hand panels). This
suggests that the southeast side of the galaxy is its near side. The
nucleus itself corresponds to a deep, compact, minimum in the
log (F547M/F791W) ratio (~ -0.15), suggestive of strong reddening. It is
straddled by two regions of blue continuum (log [F547M/F791W] ~ 0.1-0.15)
located roughly 2" (280 pc) east and west. Several other regions of blue
continuum can be seen farther away from the nucleus (see Fig. 24, bottom
left-hand panel). These relatively high values of log (F547M/F791W),
which can be reproduced with only templates E8 or S7 (see Table 3),
suggest a strong contribution of young (less than a few 10^8^ years old)
stars or scattered nuclear light to the continuum in these two regions.
The emission-line images and line ratio maps of NGC 7465 are
displayed in Figure 25. The [O III] emission is concentrated in the
inner 1" (140 pc), with the exception of a region of emission located
5" (700 pc) south of the nucleus. The [N II] + H{alpha} emission is much
more extended and displays a chaotic structure of H II regions. The
[O III] emitting region south of the nucleus (see above) is very bright
in [N II] + H{alpha} and is associated with a blue continuum region,
suggesting that it is a site of intense star formation. The regions of
high [O III]/([N II] + H{alpha}) are elongated in a southeast-northwest
directions (see also M96) and restricted to the inner 2" (280 pc). The
integrated spectral properties of the nuclear regions of NGC 7465
correspond to a mixture of Seyfert/Liner and H II region components
(see Goncalves, Veron-Cetty, & Veron 1999 and references therein). This
is presumably the result of smearing in the integration box
(5" x 2.1" [700 x 290 pc] in the case of Goncalves et al. 1999) the
contributions of off-nuclear H II regions with the nuclear regions,
which have a high [O III]/([N II] + H{alpha}) ratio (i.e., a
Seyfert-type spectrum).

4. 1999ApJS..120..209N
Re:NGC 7465
NGC 7465 (type 2; Fig. 15) - In the 20cm map, the source sits on a
large, low-level plateau, so the flux value is uncertain. Gaussian
deconvolution of the 3.6cm source suggests a P.A. of 32^deg^, but the
source size is less than half the beam size. There is a significant
displacement (3") between the apparent positions of the 3.6 and 20cm
sources. The VLA calibrator manual lists a position code of "Terrible"
("positional error" >0.15" and frequently much greater) for 2247+140,
the calibrator used at 20cm. Since the 3.6cm calibrator, 2251+158, has
a position code of "A" (positional error <0.002") and the 3.6cm
resolution is higher than the 20cm resolution, the position of the
3.6cm source is more reliable and is listed in Table 1. The position
angle of the major axis of the host galaxy is not listed in the RC3 or
UGC catalogs. UGC lists an external diameter of 1.2' x 0.7' in B. A
second-generation DSS image reveals a diameter of ~1.7' but shows clear
signs of interaction between NGC 7465 and two nearby galaxies.

5. 1999A&AS..135..437G
Re:MRK 0313
Mark 313 is a Seyfert 2 galaxy according to Osterbrock & Pogge (1987)
(with {lambda}5007/H{beta} = 3.52, {lambda}6583/H{alpha} = 0.52 and
{lambda}6300/H{alpha} = 0.10), and Moran et al. (1996); the [O III]
lines are relatively weak for a Seyfert 2. Images in [O III] and
H{alpha}+[N II] show a very complex structure, with high excitation gas
restricted to a symmetric, linear feature (Mulchaey et al. 1996). From a
two-component Gaussian fitting of high-dispersion spectra of the nucleus
of this object, Maehara & Noguchi (1988) concluded that it is a
"composite object" with a H II region and a Liner nebulosity. Line
profile analysis of our spectra reveals the contribution of two
different line-emitting regions: one, with {lambda}5007/H{beta} = 2.29,
{lambda}6583/H{alpha} = 0.44, {lambda}6300/H{alpha} = 0.10 and narrow
width (135 km s^-1^ FWHM), is typical of a H II region; the other, much
weaker, is not detected in the blue and its line ratios are
{lambda}6583/H{alpha} = 0.71 and {lambda}6300/H{alpha} = 0.28; it could
be either a Seyfert 2 or a Liner, depending on the {lambda}5007/H{beta}

6. 1998AJ....116.2682C
Re:IRAS 22595+1541
NGC 7465, Mrk 313. Seyfert 2. VLA B- and C-configuration maps at
1.49 GHz in Condon et al. (1990). Optical position from Takase &
Miyauchi-Isobe (1985).

7. 1996ApJS..102..309M
Re:NGC 7465
NGC 7465 shows very complex structure in both emission lines. Near the
nucleus, the [O III] emission is elongated in the east-west direction. Farther
out, the isophotes twist forming a slight inverted S-shaped morphology. In the
near-nuclear region, H{alpha} looks similar to [O III]. On larger scales,
there is some correspondence between features in the two lines, but the
H{alpha} image is more complex with many peaks and knots. The excitation map
is considerably simpler. The high excitation gas is restricted to a symmetric,
linear feature with peak ~ 1.5" (345 pc) north of the nucleus and major axis
running southeast-northwest.

8. 1985AnTok..202.237T
Re:KUG 2259+156
This forms a triple system with KUG 2259+157A and KUG 2259+157B.

9. 1976RC2...C...0000d
Re:NGC 7465
= MRK 0313
= Holm 802b
In a triple syatem with NGC 7463 and NGC 7464.
SN1950 was not confirmed.

10. 1973UGC...C...0000N
Re:UGC 12317
E? (de Vaucouleurs)
SN? 1950 (photographic effect?)
Brightest in subgroup of 3
See UGC 12315, UGC 12316

11. 1971Afz.....7..299M
Re:MRK 0313
= Holm 802
= NGC 7465
In the NGC 7448 Group [UGC].
Evidently a spiral galaxy
with a large condensation at the center.
It is observed edge-on.
It possibly forms a group with NGC 7463-NGC 7464.
H{alpha} is quite noticeable in the spectrum

12. 1971Afz.....7..299M
Re:MRK 0313
= II Zw 187, Sargent [4].
Compact appearance.

13. 1964RC1...C...0000d
Re:NGC 7465
= Holm 802b
SN 1950
IAU Circ., 1348.

14. 1918PLicO..13....9C
Re:NGC 7465
Oval 0.8' long, with very bright, round center.

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