Date and Time of the Query: 2019-06-25 T15:02:03 PDT
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Notes for object NGC 5273

23 note(s) found in NED.

1. 2007AJ....134..648M
Re:NGC 5273
NGC 5273 (Figs. 7.25, 9.25, 20.25): This is a lenticular galaxy with the typical
morphology of an early-type galaxy. It shows a pointlike nucleus with extended
light emission within the central 100 pc. There are some bright areas and dark
lanes. The morphology seen with F606W is very similar, suggesting that the dark
lanes are caused by thick dust clouds.

2. 2006A&A...453...27C
Re:UGC 08675
UGC 8675: we grouped the data to have at least 10 counts per channel and we
applied the Poissonian statistic. The spectrum is fitted using an absorbed
powerlaw (N_H_ = 4.4 x 10^22^ cm^-2^ and photon index {GAMMA} fixed to 1.9) plus
a thermal model.

3. 2005AJ....129..630B
Re:UGC 08675
This is a little-studied S0 galaxy hosting a Seyfert 1.5 nucleus and
has been classified as an SA0 galaxy in the RC3. The isophotes of the
galaxy are nearly circular, and at 5" the ellipticity becomes 0.15,
which is consistent with the values obtained by De Robertis et al.
(1998) and Ferruit et al. (2000). A dust absorption pattern is seen
near the nucleus in the B-R and B-K' color and extinction maps.
Ferruit et al. (2000) have found from Hubble Space Telescope
observations a U-shaped dust lane circling around the nucleus.

4. 2003ApJS..146..353M
Re:NGC 5273
NGC 5273 (CS)
The small nuclear spiral in this galaxy almost takes the form of a
nuclear dust ring, although the arms do not quite form a circle. There
are also some low-contrast dust features at larger radii.

5. 2002AJ....124..675C
Re:UGC 08675
F13400+3553 is a blend of UGC 08675 and UGC 08680. CfA Seyfert 1
(Huchra & Burg 1992).

6. 2001ApJS..133...77H
Re:NGC 5273
NGC 5273 (S1.5). - We detect a compact, unresolved core at both
frequencies. The source is slightly resolved along P.A. = 0^deg^ in the
6 cm data of Ulvestad & Wilson (1984b). Both Kukula et al. (1995) and
Nagar et al. (1999) have observed NGC 5273 at 3.6 cm with
{DELTA}{theta} = 0.3"; the former did not detect the nucleus
(S_3.6_ < 0.23 mJy), but the latter did (S_3.6_ = 0.6 mJy), which suggests
that the source is variable.

7. 2001ApJ...562..139M
Re:NGC 5273
NGC 5273. - There is a "spike" in the ellipticity distribution at
r_J_ ~ 0.5" or r_H_ ~ 0.6" (corresponding to a projected semimajor axis
length of ~40 pc). While this spike is of sufficient amplitude to meet our
nuclear bar selection criteria, the fact that the variation in ellipticity
occurs at a larger semimajor axis in the longer wavelength filter suggests
that this is probably an artifact of the strong nuclear point source. Dust
may also be a factor as the ellipticity variation is greater at J than at
H. For these reasons we do not classify this spike as a nuclear bar

8. 2001AJ....122..653R
Re:NGC 5273
NGC 5273: The galaxy hosts a bright Seyfert nucleus. The dust absorption
pattern seen in the archival optical image corresponds closely to the
structures in the NIR residual map.

9. 2000ApJS..128..139F
Re:NGC 5273
5.9. NGC 5273 - Seyfert 1.5
NGC 5273 is a little studied S0 galaxy hosting a Seyfert 1.5
nucleus. The continuum images and color maps for this galaxy are shown
in Figure 18. The isophotes of the galaxy are nearly circular (see
Fig. 18, top and middle left-hand panels). Beyond 5" (375 pc) from the
nucleus, we derive an ellipticity of ~ 0.15 (i.e., an inclination of
~ 30^deg^ for the galaxy), which is consistent with the values obtained
by De Robertis, Hayhoe, & Yee (1998). However, we find a photometric
major axis P.A. of 170^deg^-180^deg^ between 5" (375 pc) and 20"
(1.5 kpc), which is very different from the P.A. of 100^deg^-110^deg^
measured by De Robertis et al. (1998) between 10" (750 pc) and 60"
(4.5 kpc) from the nucleus. The origin of this discrepancy is unclear,
but as the ground-based, continuum images of De Robertis et al. (1998)
are much deeper than our continuum images, we think our estimates of
the PA should not be interpreted as the disk major axis. The main
feature in the images of the nuclear regions is a U-shaped dust lane
circling around the nucleus (see Fig. 18, top, middle, and bottom
right-hand panels).
The emission-line region of NGC 5273 is spatially resolved in our
images (see Fig. 19). Both the [O III] and [N II] + H{alpha} images
display a small (< 1", 75 pc) arc of emission south of the nucleus. In
the [O III]/([N II] + H{alpha}) map, the nucleus corresponds to a
minimum of the [O III]/([N II] + H{alpha}) ratio. This is probably
caused by the contribution of the broad H{alpha} line to the emission of
the Seyfert 1.5 nucleus in the [N II] + H{alpha} image.

10. 2000ApJ...542..186N
Re:NGC 5273
NGC 5273.-FIRST lists a peak flux density of 2.6 mJy beam^-1^ at
20 cm; the extended radio emission (P.A. 180^deg^) is along the major
axis of the host galaxy disk. We did not detect this galaxy at 2 cm.

11. 1999ApJS..120..209N
Re:NGC 5273
NGC 5273 (type 1.5; Fig. 13) - A Gaussian deconvolution suggests
that the 20cm source is extended in P.A. 179^deg^, but the deconvolved
source size is less than half the beam size. The southern extension to
the source at 3.6cm (in P.A.~175^deg^) does not appear in a uniformly
weighted (robust=-4) map but does appear in the uniformly weighted
(robust=0) map and in naturally weighted maps. A Gaussian deconvolution
of the 3.6cm source suggests a P.A. of 170^deg^; again, the deconvolved
source size is less than half the beam size. Ulvestad & Wilson (Paper
VI) have observed this source at 6 and 20cm and list the source as "S."
Their unpublished map shows an extension in P.A. 5^deg^. We therefore
adopt a radio source classification of "S" and a radio P.A. of 5^deg^.
Paper VII gives a 20cm flux of 2.5 mJy, in agreement with our measured
value, and a 6cm flux of 0.9 mJy. There is a confusing source 9.5'
away. H{alpha}+[N II] and [O III] images have been published by Pogge
(1989). Whittle (1992a) classifies this object as a Seyfert 1.9. Ho et
al. (1997) have detected broad lines in both H{alpha} and H{beta}. They
have used the criteria of Whittle (1992a) to classify this object as a
Seyfert 1.5.

12. 1998ApJ...500..685P
Re:NGC 5273
10. NGC 5273.--NGC 5273 has a Seyfert 1 type nucleus. Morphologically it has
been classified as a SA0 galaxy. The optical broadband images show a prominent
nucleus, but neither conspicuous star-forming regions nor dust are apparent in
the disk. Again three thermal components fit the mid- and far-IR SED of this
galaxy. The components have temperatures of 30, 68, and 217 K, and widths of 8,
14, and 100 K, respectively. These three central temperatures are higher than
found in the rest of the objects studied. As of now, we do not have an
explanation for these high temperatures. The lowest temperature component is the
more intense one in this object.

13. 1997ApJS..112..391H
Re:NGC 5273
NGC 5273.--The broad and variable (Stauffer 1982; Paper I) H{alpha} emission of
the low-luminosity Seyfert 1 nucleus in NGC 5273 (Fig. 6g) closely resembles
that of NGC 4639 (Fig. 6f) in relative strength (f_blend_~84%) and profile
(FWHM~3350 km s^-1^; FWZI~10,000 km s^-1^). As in NGC 4639, soft X-ray emission
has been detected from the compact nucleus (Koratkar et al. 1995). The [N II]
lines and the narrow component of H{alpha} are not well fitted by the model
profile derived from [S II], although in this instance the mismatch has an
insignificant effect on the measured broad H{alpha} flux. Both H{beta} and
H{gamma} also have a broad component.

14. 1997ApJS..108..155G
Re:NGC 5273
The host galaxy is an S0/a. We find no evidence of extended emission or
H II regions in the disk. The nuclear emission is compact.

15. 1997A&A...319...33A
Re:NGC 5273
NGC 5273 This Seyfert has one conspicuous pair across itself (C=7.8and 12.6).
Originally it was thought that the pairs C=39.2 and 18.2 were, in addition, a
less well aligned pair across the Seyfert. However, there are better aligned
possibilities as shown in Fig. 19.
Fig. 19 shows that there is exact alignment through the C=4.1 source. But the
optical identification of that source is not impressive. As Table 11 indicates,
there is only a faintish. very red object within the X-ray error circle.
Comparing the Palomar E and O plates to B and R plates taken with the same
instrument about 40 years later suggests this object is variable. It may well
be the correct X-ray identification albeit a very unusual one.
Actually, there is another, optically brighter, origin for this alignment as
shown by the cross in Fig. 19. The cross represents the position of NGC 5276, a
B=14.6 mag., cz=5,548km s^-1^ SBa galaxy. It is a typical, high redshift,
active companion of the kind associated with large low redshift galaxies (Arp
1981; 1987). The alignment of the C=39.2 and 18.2 sources across it is rather
good ({DELTA}{theta}=6^deg^) and the alignment is roughly in the minor axis
direction. Moreover there are two BSO's (not registered as X-ray sources in the
reduced PSPC exposure) between 1' and 2' of NGC 5276 and another further out
along the direction to the C=4.1 source. Although either is possible, it is
felt that NGC 5276 is the most likely origin for these later objects.

16. 1995MNRAS.276.1262K
Re:NGC 5273
NGC 5273: Type 1(1.9). Host galaxy: lenticular (CPG), S0 (UGC). Radio: C-
array shows a faint unresolved component coincident with the optical
nucleus, but there is no detection with A-array. The object is known to
be extended in PA 0^deg^ at 6 cm (Ulvestad & Wilson 1984b).

17. 1995ApJS...98..477H
Re:NGC 5273
The red spectrum of this Seyfert galaxy resembles that of NGC 4639,
showing very prominent broad H{alpha} emission. In the blue, broad
H{beta} (and possibly H{gamma}) are visible, as well as a feature near
4560 A which is due to Fe II. Unresolved X-ray emission was detected by
Koratkar et al. (1995).

18. 1994CAG1..B...0000S
Re:NGC 5273
Hubble Atlas, p. 8
Feb 5/6, 1954
103aO + WG2
30 min
A definite spiral pattern in NGC 5273
threads through a classical S0 disk, well seen
when this print is viewed from a distance. The
reproduction is from the same 200-inch plate
used in the Hubble Atlas. It is not clear if the
spiral pattern is due to dust or to a luminous

19. 1976RC2...C...0000d
Re:NGC 5273
= Holm 535a
= Kara[72] 391a
Non-interacting pair with NGC 5276 at 3.3 arcmin
Photometry (11 Color):
Astr. Ap., 29, 77, 1973.

20. 1973UGC...C...0000N
Re:UGC 08675
SA(s)0/a (de Vaucouleurs)
Paired with UGC 08680 at 3.4, 124

21. 1964RC1...C...0000d
Re:NGC 5273
= Holm 535a
Small, bright diffuse nucleus with 2 weak dark patches. Very faint spiral
whorls in lens: 1.4 arcmin x 1.2 arcmin. Smooth nebulosity.
HA 88, 2 dimensions (1.0 arcmin x 1.0: arcmin: serie mc) are for the nucleus
or lens only.
Lund 9 dimensions are for the lens only.
Non-interacting pair with NGC 5276 at 3.3 arcmin.

22. 1961Hubbl.B...0000S
Re:NGC 5273
Feb. 5/6, 1954
103aO + WG2
30 min
Enlarged 6.0X
NGC 5273 is a transition between an S01 and an Sa galaxy.
A very faint spiral pattern is visible. It is probably
due to a thin dust lane that winds outward through the
envelope. The lane is not opaque, so that the arms are
difficult to trace.

23. 1957HPh....53..275d
Re:NGC 5273
(Plate 2)
Traces of spiral structure in the smooth lens and envelope
surrounding the large nucleus; little or no dark matter.
With lower resolution, lens and envelope would simulate a
late elliptical.
Compare with NGC 7144 (Plate 1) and NGC 7457 (Plate 5).

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