Date and Time of the Query: 2019-06-18 T14:51:42 PDT
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Notes for object NGC 5135

18 note(s) found in NED.

1. 2007AJ....134..648M
Re:NGC 5135
NGC 5135 (Figs. 7.56, 8.7, 9.56, 20.56): This is a nice example of a very strong
nuclear starburst, with many bright star clusters individually resolved and two
wide-open spiral arms, traced by star-forming regions.

2. 2003ApJS..146..353M
Re:NGC 5135
NGC 5135 (GD)
There is a clear, grand-design spiral at larger radii with some
associated star formation along the leading edges of the dust arms.
This star formation suggests that the bar is relatively weak
(Athanassoula 1992). Within the central kiloparsec the spiral becomes
much less ordered and the classification is consequently more
uncertain. There also appears to be a great deal of circumnuclear star

3. 2001MNRAS.327..459L
Re:NGC 5135
NGC 5135 and NGC 7130: Detailed optical and ultraviolet studies of
these galaxies were carried out by Gonzalez Delgado et al. (1998) and
Gonzalez Delgado et al. (2001). They found evidence that the optical
continuum was dominated by a young starburst. As with IC 3639, the
starburst has a similar bolometric luminosity to the AGN.

4. 2001ApJS..133..269L
Re:NGC 5135
5.6. NGC 5135
NGC 5135 contains a bar, which has also been observed in the
near-infrared (Mulchaey et al. 1997), and it is in a group
(Kollatschny & Fricke 1989). NGC 5135 is best fitted with the
three-component model of a scattered power law and thermal emission. The
soft X-ray flux from the thermal component is slightly stronger than that
of the scattered power law; 54% of the soft X-ray emission is thermal.
The residuals of the fit suggest that an additional low-energy
(E < 0.5 keV) source is present. Analogous to nearby starbursts, this is
likely an additional thermal component, but we cannot measure it
significantly in the present data. The X-ray emission from NGC 5135 is
extended, both in HRI and in PSPC observations, on scales of 5.3 and
13 kpc, respectively, and the soft and the hard emission within the
PSPC bandpass are spatially distinct.

5. 2000MNRAS.314..573T
Re:NGC 5135
NGC 5135: Despite the bright radio flux of the nucleus at lower
resolutions and frequencies (Ulvestad & Wilson 1989), no radio emission
is observed at the nucleus in the current observations. Wynn-Williams &
Becklin (1993) have suggested that 'most of the radio emission of this
Seyfert galaxy emanates from structures on either side of the nucleus
rather than from the nucleus itself'. We detect a weak component with a
flux density of 2.33 mJy at {alpha} = 13^h^ 25^m^ 44.9^s^,
{delta} = -29^deg^ 50' 16.17", but it is unlikely to be related to the
active nucleus (see Section 4.3).

6. 2000ApJ...544..747S
Re:NGC 5135
The HOBL are clear in the spectrum. The W values, CR, and other features
of the spectrum can be approximately reproduced by the combination of 50%
each in flux at 4020 A of two of our models: the first is the bulge
template combined with 1% in mass of a 10 Myr stellar population, and the
second is the bulge template combined with 1% in mass of a 100 Myr stellar
population (Fig. 17a). There is some line emission of
H{epsilon}+ Ne III {lambda}3968, H8, and possibly H9.
The starburst in this galaxy has been studied extensively by Gonzalez
Delgado et al. (1998) and Gonzalez Delgado, Heckman, & Leitherer (2001),
hereafter GD98 and GD01. GD98 have shown that the UV spectrum presents
clear signatures of O and B stars, estimating an age between 3 and 5 Myr
for the burst, while GD01 concludes that there is also a similar
contribution in flux from an intermediate-aged population and a small
contribution of an old component. Our model is consistent with the latter

7. 1999ApJ...516...97N
Re:NGC 5135
NGC 5135 (ESO 444-G32, MCG-5-32-13): RC3 lists log R_25_ = 0.15 but
does not list a major axis P.A. ESO lists a diameter of 3.5'x 3.3'.
Corwin, de Vaucouleurs, & de Vaucouleurs (1985) find the galaxy diameter
to be 5.5' x 5.37'. A first generation DSS image confirms that the
galaxy is nearly circular.

8. 1998MNRAS.297..579C
Re:NGC 5135
NGC 5135. NGC 5135 was descrihed by Phillips et al. (1983) as having a composite
nucleus with characteristics of both Seyfert 2 and starburst. Thuan (1984)
obtained IUE spectra of this galaxy, confirming the dual nature of the nucleus,
which presents both emission lines typical of Seyfert 2s and absorption lines
typical of starbursts, the latter component contributing 25 per cent of the
total UV emission.
The Ws (Fig. 24) show a gradient from values typical of an S7 template at the
nucleus to S6-S5 at 7 arcsec. The continuum ratios also show a gradient from S6
at the nucleus to S5 at 7 arcsec. This gradient is due to the presence of young
stars in the nuclear region, as revealed by strong He I absorption features.

9. 1998ApJ...505..174G
Re:NGC 5135
NGC 5135 belongs to a group of seven galaxies (Kollatschny & Fricke
1989). It has a near-IR bar aligned at P.A. = 123^deg^ (Mulchaey et al.
1997). The nucleus has also been classified as a Seyfert nucleus
(Phillips et al. 1983). The nucleus shows high-excitation lines with
line ratios typical of a Seyfert 2 nucleus ([Ne V] is present,
He II/H{beta} = 0.18, [O III]/H {beta} = 4.8, [N II]/H{beta} = 5.5,
taken from Phillips et al. 1983). The spectrum through the IUE aperture
(projected size 2.7 x 5.4 kpc) shows mixed Seyfert and starburst
characteristics (Thuan 1984; Kinney et al. 1993). The radio continuum
map at 6 and 20 cm shows an asymmetric structure with faint emission
extended to the northeast (P.A. = 30^deg^) of the bright core source.
The overall linear extent is about 9". The H{alpha} narrowband image
shows extended emission aligned with the radio emission (Haniff, Wilson,
& Ward 1988; Garcia Barreto 1996). The high-excitation gas, mapped
through the [O III] {lambda}5007 emission line, is aligned north-south
on a 2" scale.

10. 1997ApJS..113...23T
Re:NGC 5135
A14. NGC 5135
The ultraviolet spectrum of NGC 5135 shows evidence for the presence of very
massive and hot O stars in the host galaxy. The relatively high level of
starburst activity compared to Seyfert type characteristics has led Thuan
(1984) to suggest that this source may be in a transition from starburst to
Seyfert galaxy. The soft X-ray lines present in the spectrum of this source
make the Raymond-Smith plus power-law model the nominal best fit. Our analysis
of the ROSAT PSPC image shows NGC 5135 to be consistent with a point source.

11. 1997ApJS..110..299M
Re:NGC 5135
Bar is visible in the K_S_image. The ellipticity and P.A. also suggest the
presence of a bar, although the fits do not trace the full length of the

12. 1996ApJS..103...81C
Re:NGC 5135
NGC 5135.--Seyfert 2. High-resolution VLA maps at 1.49 and 4.86 GHz in
Ulvestad & Wilson (1989). An unpublished VLA D-configuration map from the
Condon et al. (1995) identifications gives a flux density S = 69 mJy at
4.86 GHz.

13. 1994CAG1..B...0000S
Re:NGC 5135
SBb pec
March 28/29, 1982
103aO + GG385
45 min
The dust lanes in the bar of NGC 5135 are
themselves curved into a spiral pattern similar
to, but not as extreme as, the famous case of
NGC 4314 (SBa; Hubble Atlas, p. 44; panels 95, 106
here). The faint spiral arms begin in an (s)-type
NGC 1300 pattern from the ends of the bar. The
brightest HII region candidates occur in one of
the arms close to its beginning near the end of the
bar. The largest of these resolves into a disk at
about the 1" level. The redshift of NGC 5135 is
v_o = 3906 km/s.
The absolute magnitude of the galaxy is
bright, at M_B_ = -22.5 (H = 50).

14. 1993ApJS...86....5K
Re:NGC 5135
NGC 5135; SABb, Seyfert 2.
NGC 5135 is a high-excitation emission-line galaxy belonging to a group
of seven galaxies which are gravitationally bound and lie within 1 Mpc of
one another. Tidal interactions may be causally related to the Seyfert 2
activity (Kollatschny & Fricke 1989). From X-ray and radio observations
and from the luminosities of the optical emission lines, the nucleus of
NGC 5135 has been called a mini- Seyfert 2 (Phillips et al. 1983; Thuan
1984). The UV spectrum shows a dual nature; several narrow emission lines
are present, including Ly{alpha}, C IV {lambda}1550, and He II
{lambda}1640, while absorption features of Si IV {lambda}{lambda}1397,
1402 and He II {lambda}1640 are also present. The luminosity of the
Seyfert nucleus is sufficiently low that the underlying absorption
features of the H II regions (contributing ~25% of the emission; Thuan
1984) are still detectable.
This galaxy has an anomalous ratio of Ly{alpha}/H{beta} (~5),
suggesting the presence of dust or an extinction law for NGC 5135
different from that of our Galaxy (Thuan 1984).

15. 1993ApJ...412..535W
Re:NGC 5135
NGC 5135.-The position of the galaxy at 10 microns was determined to be
13h 22m 56.45s +/- 0.1s, -29d 34'24.4" +/- 1.0". It therefore coincides
with one of the fainter maxima in Ulvestad & Wilson's (1989) map at 6 cm
rather than with the brightest radio peak, which is 3" to the south. We
determined that the 10 micron peak coincides to within 1" with the
visible peak. On this basis we would suggest that most of the radio
emission of this Seyfert galaxy emanates from structures on either side
of the nucleus rather than from the nucleus itself.

16. 1985SGC...C...0000C
Re:NGC 5135
Plate 1484
Very bright bulge, faint patchy arms. Cluster in background.

17. 1976RC2...C...0000d
Re:NGC 5135
Non-interacting pair with IC 4248 at 13.5 arcmin

18. 1964RC1...C...0000d
Re:NGC 5135
Very bright nucleus in a bright bar: 1.3 arcmin x 0.3 arcmin.
Non-interacting pair with IC 4248 at 13.5 arcmin.

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