Date and Time of the Query: 2019-06-18 T15:57:12 PDT
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Notes for object NGC 5953

15 note(s) found in NED.

1. 2008ApJS..174..337M
Re:NGC 5953
NGC 5953 (Fig. 5n).-The nonbarred galaxy has a nuclear ring that appears
complete with 23 H II regions. Although we know of no bar to directly fuel the
ring, it is well formed and resolved both azimuthally and radially.

2. 2006A&A...457...61R
Re:NGC 5953
NGC 5953. This Arp-Madore galaxy is interacting with NGC 5954 (Arp
1966). It has a Seyfert 2 nucleus (Rafanelli et al. 1990), surrounded
by a ring of star formation with a radius of ~4". Long-slit
spectroscopy shows that in the circumnuclear region a starburst
coexists with moderate-excitation gas ionized by the active nucleus
(Gonzalez Delgado & Perez 1996b). The J-band spectroscopy of
Alonso-Herrero et al. (2000) shows a spectrum dominated by [Fe II]
1.257 microns and weak Pa{beta} emission. Our spectrum displays low-
and moderate-ionization emission lines, on top of a steep continuum
with numerous stellar absorption features. The Ca II triplet in
absorption dominates the blue end of the spectrum, while strong 2.3
microns CO bandheads are observed at the red edge. The CO absorption
bands are also strong in H. The highest (and most intense) forbidden
line detected is [S III]. In addition, [Fe II] emission is prominent in
the J and H. In K, the most conspicuous emission features are from H2 .
Br{gamma} is rather weak, and Pa{alpha} is severely affected by
telluric absorption. A comparison of the NGC 5953 spectrum with the
ones discussed in this section allows us to conclude that NGC 5953 is
the edge of a Seyfert 2/LINER classification.

3. 2005MNRAS.364.1253V
Re:NGC 5953
NGC 5953/4 is also in the IRS SLUGS sample. While D00 used colour-corrected IRAS
fluxes as listed in the IRAS Bright Galaxy Sample (from Soifer et al. 1989) we
present here, as for all the OS sample, fluxes from the IRAS FSC.

4. 2004AJ....127.3235S
Re:NGC 5953
NGC 5953. Given as CPG 468 by Domingue et al. (2003). The HIRES data
agree with the higher resolution ISOPHOT data indicating the dominance
of the southwestern component.

5. 2003ApJS..146..353M
Re:NGC 5953
NGC 5953 (TW)
There are a large number of fragmented spiral dust arms with low pitch
angle, and unlike the other tightly wound nuclear dust spirals in the
sample, these arms appear to have associated star formation.

6. 2001A&A...368..797P
Re:NGC 5953
NGC 5953: This interacting system (Rafanelli et al. 1990) is detected in
the survey and pointed observations. The X-ray emission of this system in
the pointed observation is mainly caused by the Seyfert 2 galaxy NGC 5953.
In the survey observation the emission is centered on the companion of
NGC 5953 and no emission from the Seyfert 2 galaxy is detected. Due to the
PSPC pointing accuracy we are not able to decide whether NGC 5953 is a
transient source in the soft X-ray band.

7. 2000ApJ...530..688A
Re:NGC 5953
NGC 5953.-This is an Sa pec galaxy interacting with the
LINER/starburst galaxy NGC 5954. The determination of the activity class
of the nucleus of this galaxy has been somehow problematic. It has been
classified as a LINER by Veilleux et al. (1995), and as a Seyfert 2 by
Gonzalez-Delgado & Perez (1996a). Note that some of optical line ratios
reported for this galaxy in these two works differ by a factor of 2.
Using the reddening-corrected optical line ratios given in Keel et al.
(1985) and Veilleux et al. (1995), and the diagnostic diagrams, we find
that NGC 5953 is located in the region occupied by both LINERs and
transition objects. It shows strong circumnuclear star formation
activity as inferred from both two-dimensional optical spectroscopic
data (Gonzalez-Delgado & Perez 1996a; Veron, Goncalves, & Veron-Cetty
1997) and HST/UV images (Colina et al. 1997). Our J-band spectrum shows
strong [Fe II] and Pa{beta} emission lines. The ratio
[Fe II] 1.2567 micron/Pa{beta} decreases for the large aperture
(Table 5), which is an indication for an increased star formation
activity in the circumnuclear regions as seen in the optical.
H- and K-band spectroscopy of the companion NGC 5954 is presented in
Vanzi et al. (1998).

8. 1999A&AS..135..437G
Re:NGC 5953
NGC 5953 is a peculiar S0 (Rampazzo et al. 1995) or Sa (Gonzalez Delgado
& Perez 1996) galaxy interacting with NGC 5954 (Arp 1966). It has a
Seyfert 2 nucleus (Rafanelli et al. 1990; Gonzalez Delgado & Perez)
surrounded by a ring of star formation with a radius of ~ 4" (Gonzalez
Delgado & Perez). Rafanelli et al. and Gonzalez Delgado & Perez studied
this object using a slit width of 2."0 and 1.5" respectively. The
seeing was ~1" during Gonzalez Delgado & Perez' observations, while it
was not specified by Rafanelli et al. who, however, easily separated the
galaxy nucleus from a star located 3" away. We may reasonably assume
that, in both cases, the nuclear spectrum corresponds to a 2.0" x 2.0",
or smaller, aperture. The line ratios given by these authors (see Table
2) are typical of a Seyfert 2 region, although [O I]{lambda}6300 may be
somewhat weak for this type of objects; but as stressed before, we
cannot exclude some contamination by the circumstellar emission region.
Both Keel et al. (1985) and Kim et al. (1995) have observed the NGC 5953
nuclear region with a relatively large aperture: Keel et al. used a
{phi} = 4.7" circular aperture, while Kim et al. used a long 2" x 14"
slit. It is clear that these two large aperture spectra must contain a
significant contribution from the circumstellar emission region and,
indeed, the published line intensity ratios are those of "transition"
spectra. We used a 2 ."1 slit and the seeing was 2.6"; we extracted 7
columns, i.e., 7.6", so some contamination from the circumstellar
emission region was expected. Effectively, by doing the line profile
fitting analysis, we were able to identify two components of different
line widths and strengths, one of which can be associated with a H II
region ({lambda}5007/H{beta} = 0.55, {lambda}6583/H{alpha} = 0.60,
{lambda}6300/H{alpha} = 0.03 and FWHM ~ 200 km s^-1^); the other
component, broader ( FWHM ~ 400 km s^-1^), reveals the presence of a
Seyfert 2 nebulosity, the measured line intensities being:
{lambda}6583/H{alpha} = 1.96 and {lambda}6300/H{alpha} = 0.18, with
{lambda}5007/H{beta} fixed to 10. Lines of [Fe III] {lambda}4659 and
[Fe VII]{lambda}5158 are clearly visible in the blue spectrum. A very
weak broad H{alpha} line is possibly detected, which would qualify
NGC 5953 as a Seyfert 1.9 galaxy.

9. 1997ApJS..108..155G
Re:NGC 5953
NGC 5953 - NGC 5954. NGC 5953 is an S2 nucleus in an Sa galaxy in
interaction with NGC 5954 that has a LINER nucleus in an Scd galaxy. Both
galaxies are experiencing a burst of star formation in the circumnuclear
region. In NGC 5953, all the emission is within the central 10" (1.3
kpc). The nucleus is also extended to the north. The [O III] image is
also extended to the northeast, aligned with the companion. Long-slit
spectroscopy shows that in the circumnuclear region a starburst coexists
with high-excitation gas ionized by the active nucleus (see Gonzalez
Delgado & Perez 1996c).

10. 1997A&A...319...52V
Re:NGC 5953
The spectrum of the nucleus of NGC 5953 cannot be easily classified from the
emission-line ratios; however, out of the nucleus, the spectrum is similar to
that of a HII region, suggesting that the emission line region is a composite
of a HII and a Seyfert like cloud (Jenkins, 1984).

11. 1995A&AS..110..131R
Re:NGC 5953
NGC 5953: There has been considerable confusion about the morphological
type of this galaxy. It shows emission knots, a rotationally supported
disk and blue color. The lack of obvious spiral structure suggests that
it is unusual.
Jenkins (1984) studied NGC 5953 suggesting that the "spectrum and the
color of this galaxy are largely the result of rapid star formation
involving ~10^65^ M_sun_". and possibly related to interaction with the
companion. He classifies this galaxy as an early-type "of fairly smooth
and amorphous appearance without any obvious spiral arms with center
distorted into a pear-shape".
The images of Reshetnikov (1993) suggest that the bright core of NGC
5953 is embedded in a large halo that merges with a component that
envelops the pair. In integrated light it is almost twice as bright as
its spiral neighbor.
Our B photometry of this galaxy (Fig. 16) shows that we are dealing
with an (underlying) S0 galaxy with some obvious peculiarities. The model
subtraction shows the presence of four luminous knots concentrated near
the center of the galaxy and forming a sort of "Greek cross". This is not
to be confused with the prototypical X-structure (see for instance
IC 1452) observed in some galaxies. No spiral structure is revealed after
model subtraction. Comparison of our photometry with the V measures of
Reshetnikov (1993) supports, with the presence of a broad band color
gradient, the existence of considerable star formation near the center.
In fact, inside 5 arcsec, where the knots are located, (B - V) is ~0.3 -
0.35 rising rapidly to values 0.8 - 1.0 towards the outskirts. The
ellipticity outside 5 arcsec variates between 0.1 and 0.25 showing a
tendency to increase in the outer part indicating the presence of a disk
which we see in the luminosity profile. The twisting is ~30^deg^. The
knots dominate the isophotal shape and we measure an a4/a that
corresponds to a boxiness that reaches 2% in that area. The fact that the
presence of such a "cross structure" correlates with the measured
boxiness of a galaxy was already noticed by Forbes & Thomson (1992). The
knots mask the bulge of this galaxy and force us to fit only a disk
component in the profile interpolation (Fig. 20). In this sense the model
is quite unsatisfactory. Reshetnikov (1993) notes that his derived bulge
to disk ratio B/D~2 is more consistent with type S0 or S0/a than
Previous spectroscopic data exist from Jenkins (1984), Keel et al.
(1985) and Rafanelli et al. (1990). NGC 5953 = Markarian 1512 is
classified as a Seyfert 2 galaxy.
Our data about the stellar component of NGC 5953 (Fig. 5) shows a
maximum velocity gradient of ~200 km s^-1^ near the pair axis. The
rotational structure is concentrated within +/-10 arcsec of the center.
Similar rotation is observed in the gas and starlight components but the
two show a striking spatial displacement of about 0.5 kpc. The rotation
velocity deduced from the gas is ~100 km s^-1^ higher. The emission line
measurements obtained in this work are fully consistent with those of
Reshetnikov (1993). The data of Reshetnikov (1993) also show evidence for
a turnover on both ends of the rotation curve. This interpretation is
complicated by evidence for noncircular motions beyond r = 10 arcsec. Gas
is measured quasi continuously in projected space and velocity into the
spiral neighbor.

12. 1976RC2...C...0000d
Re:NGC 5953
= Holm 714b
in Arp 091
in VV 244
in Kara[72] 468
Colliding or strongly interacting pair at 0.8 arcmin
Radio Observations:
M.N.R.A.S., 167, 251, 1974.

13. 1973UGC...C...0000N
Re:UGC 09903
VV 244a, Arp 91
E (de Vaucouleurs)
Paired with UGC 09904 at 0.75 north-following, total m=12.7
In Arp's class "spiral galaxies with large high surface brightness companions
on arms"; "broad peculiar arm to companion, then absorption; faint extension
from companion" (Arp)

14. 1964RC1...C...0000d
Re:NGC 5953
= Holm 714b
Pair with NGC 5954 at 0.8 arcmin.
Ap. J., 116, 66, 1962.
P.A.S.P., 168, 386, 1957.

15. 1959VV....C...0000V
Re:VV 244a
= NGC 5953
V = +2,210 km/sec from H{alpha}, [NII], {lambda}3727
(Page, T., Ap. J., 116, 63, 1952)

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