NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-20 T02:12:22 PDT
Help | Comment | NED Home

Notes for object NGC 7130

23 note(s) found in NED.


1. 2009ApJ...696.1218Z
Re:IC 5135
IC 5135 (NGC 7130). The optical spectrum for IC 5135 has strong [O III] and [N
II] narrow lines. The log([O III]/H{beta}) and log([N II]/H{alpha}) line ratios,
0.6990 and -0.0231 respectively (Vaceli et al. 1997), place it in the Seyfert 2
region of the BPT diagram. Shu et al. (2007) report an [O III] luminosity,
log(L[O III]) = 42.55 erg s^-1^.

2. 2007AJ....134..648M
Re:NGC 7130
NGC 7130 (Figs. 7.65, 8.9, 9.65, 20.65): This shows an interesting morphology,
with a ring and an inner bar. It is very rich in star-forming knots and stellar
clusters, with a very bright region that is off-center from the ring. We have
chosen as the galaxy center the centroid of the brightest of these blobs. The
morphology of the center in F330W coincides with that of F210M presented in
Gonzalez Delgado et al. (1998).

3. 2006A&A...460...45G
Re:NGC 7130
NGC 7130 (IC 5135). This galaxy shows a well-defined nuclear source at high
X-ray energies (Fig. 5). Since most of the UV emission is spectrally
characteristic of star formation (Thuan 1984; Gonzalez-Delgado et al. 1998),
Levenson et al. (2005) tried to decompose the AGN and Starburst contributions
and find that the AGN contribution manifested mainly at higher energies, higher
than 3 keV. They find that the obscuration of the nucleus is Compton-thick,
which prevents the detection of the intrinsic emission in the Chandra bandpass
below 8 keV. We recall that our spectral fitting is not statistically acceptable
for this source.

4. 2003ApJS..146..353M
Re:NGC 7130
NGC 7130 (GD)
This is a good example of a galaxy whose large-scale bar is clearly
transporting material to within several hundred kiloparsecs of the
nucleus. The dust lanes from the large-scale bar have some star
formation on their leading edges, indicative of a weak bar, and there
appear to be several knots of star formation in the very center.

5. 2002ApJS..143...47D
Re:IRAS 21453-3511
IRAS 21453-3511 (NGC 7130).---This is a peculiar/ disturbed spiral
galaxy (Lauberts 1982). Our H{alpha} image shows strong emission in
the nucleus, a prominent asymmetric barred ring of emission, faint
spiral arms to the south and some diffuse H{alpha} emission to the
north. Two small faint H{alpha} knots are observed to the southeast of
the galaxy. The unusual, asymmetric H{alpha} distribution may indicate
that this galaxy is undergoing or has undergone a collision, as
suggested previously by de Vaucouleurs et al. (1976). It has a
companion (IC 5131) 12 0 to the east, although it is unclear whether
this is causing the unusual H{alpha} emission. This galaxy contains an
AGN as well as circumnuclear star formation (e.g., Phillips,
Charles, & Baldwin 1983; Shields & Filippenko 1990).

6. 2002ApJ...564..650C
Re:NGC 7130
9. IRAS 21453-3511 (NGC 7130, IC 5135) is a known AGN, identified by
Phillips, Charles, & Baldwin (1983) as a Seyfert 2 active nucleus
surrounded by a starburst ring. Observations by Thuan (1984) further
showed that the starburst dominates the galaxy emission contributing
75% of the emission in the UV. Its optical emission line ratios have
confirmed its AGN classification, but it falls on the borderline
between the Seyfert 2 and LINER classes, with Veilleux et al. (1997)
classifying it as a LINER while Heisler et al. (1997) and Vaceli et al.
(1997) classify it as a Seyfert 2. We also classify it as a Seyfert 2,
and it is possible that the differences between the classifications
reflect differing contributions from the starburst emission in the slit.
We detect a 4.7 mJy (10^4.1^ L_sun_) core in IRAS 21453-3511 and a
radio excess at 4.8 GHz of 92% (i.e., the 4.8 GHz luminosity is nearly
twice that predicted from the FIR luminosity). The compact radio core
contributes 3.8% of the total radio luminosity at 2.3 GHz, but after
subtraction of the core the source still exhibits an excess radio flux
above the radio-FIR correlation of greater than 80% of the total radio
luminosity. Heisler et al. (1997) measured a compact core flux at 2.3 GHz
of 14 mJy using the PTI baseline with a resolution of 01, twice that of
ours, which implies that the source has compact radio structures between
25 and 50 pc in size that we have resolved out. These structures could
be associated with a radio jet. Alternatively, the difference between
the PTI flux and our measurements could be due to intrinsic variability
of the compact core.

7. 2001MNRAS.327..459L
Re:NGC 7130
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.

8. 2001ApJS..133..269L
Re:NGC 7130
5.12. NGC 7130
NGC 7130 is peculiar and contains a bar, detected at near-infrared
wavelengths (Mulchaey et al. 1997). The X-ray spectrum is best fitted with
a single power law and thermal emission. The latter dominates, accounting
for 57% of the soft X-ray flux. In this model, the absorption on the power
law is low, consistent with the Galactic value alone, which implies that
we do not observe the buried AGN directly. The quality of these ASCA data
is not extremely high, however. Although the complex model does not
significantly improve the fit, it yields reasonable results. We find
N_H_ = 10^24^ cm^-2^ and a scattered fraction f_scatt_ = 0.01 in this case,
while the thermal contribution does not change. We detect extended emission
in the extremely short (5 ks) HRI exposure, with R_kpc_ = 16.

9. 2000ApJ...544..747S
Re:NGC 7130
Figure 17d shows the clear HOBL in this spectrum, another case of
nuclear starburst well studied by GD98 and GD01. The latter authors have
suggested the same population as that derived for NGC 5135. Although the
W values support the same population, the bluer continuum of NGC 7130
suggests a somewhat younger population, or a mixture including a larger
proportion of the younger components. The model we show in the figure is
the same composite model as the one adopted for NGC 5135, with a somewhat
larger contribution in flux at 4020 A of the bulge combined with the 10 Myr
stellar population: 75%, while the bulge combined with the 100 Myr
population contributes with 25% of the flux.
In summary, for the four Sc and Sd Seyfert galaxies, three present
recent episodes of star formation in the nuclear region, with the HOBL
clearly visible in the spectra, while one presents ~10% mass contribution
of an intermediate-aged population.

10. 1998MNRAS.297..579C
Re:NGC 7130
NGC 7130. Like NGC 5135, this galaxy has a Seyfert 2 nucleus surrounded by a
starburst (Phillips et al. 1983). Thuan (1984) presented IUE spectra which show
both high-excitation emission lines typical of Seyfert 2s and absorption lines
typical of starbursts. The starburst component dominates the UV emission, with
~75 per cent of the flux. Shields & Filippenko (1990) showed that the
narrow-line region has two kinematical components and emission-line ratios which
vary from those of AGN in the nucleus to those typical of HII regions farther
out.
Both Ws and continuum ratios show a marked gradient (Fig. 28). The Ws change
from values similar to S7 at the nucleus to S6 farther out, while the continuum
ratios change from S6-S7 at the nucleus to S5-S6 farther out. This gradient is
due to the presence of a circumnuclear star-forming region.

11. 1998ApJ...505..174G
Re:NGC 7130
The NGC 7130 K band shows an inner bar oriented at P.A. = 0^deg^
not visible at optical wavelengths (Mulchaey, Regan, & Kundu 1997). In
the digital sky survey it can be seen that NGC 7130 has two dwarf
companion galaxies located to the northwest at 50" (15.5 kpc) and to the
southwest at 30" (9 kpc). An H{alpha} image shows two bright arms and
circumnuclear extended emission, but the [O III] image only shows
emission concentrated in the nucleus (Shields & Filippenko 1990). There
is an extremely luminous infrared source, with a very compact radio
source (Norris et al. 1990). It was classified as a Seyfert nucleus by
Phillips, Charles, & Baldwin (1983). It shows high-excitation lines,
such as [Ne V] {lambda}3426 and He II {lambda}4686, with line ratios
typical of Seyfert 2 nuclei ([Ne V]/H{beta} = 0.78,
He II{lambda}4686/H{beta} = 0.16, [O III]/H{beta} = 6.0,
[N II]{lambda}6584/H{alpha} = 0.96 taken from Shields & Filippenko 1990).
The IUE spectrum (through a large 10 " x 20" aperture, equivalent to
3.1 x 6.2 kpc) shows starburst characteristics mixed with emission lines
(Thuan 1984; Kinney et al. 1993). This dual nature has also been shown
at optical (Shields & Filippenko 1990) and near-IR wavelengths (Goldader
et al. 1997). At optical wavelengths stellar absorption underlies the
Balmer emission lines, and at 2{microns} the CO stellar absorption band
is clearly detected.

12. 1997ApJS..110..299M
Re:NGC 7130
Bar is visible in both the ellipse fits and the K_S_image. Unbarred in the
RSA.

13. 1997ApJ...477..631V
Re:IC 5135
IC 5135 = NGC 7130
IC 5135 was originally identified as a Seyfert 2 galaxy by Phillips,
Charles, & Baldwin (1983). More recently, Shields & Filippenko (1990)
studied its optical emission-line spectrum in detail and concluded that a
circumnuclear starburst is also present in this object. No spectrum was
obtained in the J band. The line emission from Br{gamma} and H_2_ 2.121
microns dominates the K-band spectrum (Fig. 2c). Both lines have similar
widths, and neither shows any obvious broad wings at low intensity
levels. Any broad (FWHM ~ 2600 km s^-1^) emission at Br{gamma} must be
weaker than about 3 x 10^-15^ ergs s^-1^ cm^-2^. A number of other
features may be identified in the spectrum. The line at 2.094 microns is
redshifted He I{lambda}2.058, while the weaker features at 2.26 microns
and 2.110 microns probably correspond to H_2_{lambda}2.223 and H_2_
{lambda}2.073, respectively.

14. 1997A&A...319...52V
Re:IC 5135
In the case of IC 5135, although the optical emission line ratios in the
nucleus are characteristic of Seyfert galaxies (Phillips et al., 1983;
Storchi-Bergmann et al., 1995), the lines have profiles with two kinematic
components, apparently resulting from a combination of relatively broad
emission (FWHM ~1000 km s^-1^) from the Seyfert nucleus and narrow emission
(FWHM ~250 km s^-1^) from low excitation, circumstellar HII regions (Shields
and Filippenko, 1990).

15. 1996ApJS..103...81C
Re:NGC 7130
NGC 7130.--IC 5135. Seyfert 2. The 4.86 GHz flux density is S = 70.1 mJy
(van Driel et al. 1991). The 1.1 mJy radio source at {alpha} = 21h45m17.1s,
{delta} = -35^deg^10'32" (Fig. 2) coincides with the faint galaxy 58NW at
optical position {alpha} = 21h45m17.2s, {delta} = -35^deg^10'30"
(van den Broek et al. 1991).

16. 1996A&AS..115..439E
Re:NGC 7130
NGC 7130 is a peculiar spiral galaxy.

17. 1994CAG1..B...0000S
Re:IC 5135
Pair
Sa pec
(E/I,L,1/2)
CD-1553-S/Br
Aug 8/9, 1980
103aO + GG385
45 min
IC 5135 has no close companions; no
current interaction is evident. However, IC 5131 is
12' distant to the west, and the peculiar (S0_1_
pec) galaxy NGC 7135 (panel 51) with its
unusual plume (presumably tidal) is 18' distant to
the east. The redshifts of v_o(5135) = 4808 km/s
and v_o(7135) = 4889 km/s are similar
enough to assure a common distance. The mean
redshift of = 4848 km/s gives a redshift
distance of 97 Mpc (H = 50). The projected
linear separation of IC 5135 and NGC 7135 is
508 kpc, similar to the distance between our
Galaxy and M31, at 690 kpc (m - M = 24.2).
Because IC 5135 and NGC 7135 are both
peculiar and form a wide pair, a circumstantial
case exists that a tidal interaction has occurred
in the past and the interacting galaxies have
moved apart. However, the time scale belies this
possibility. At a separation of 500 kpc and a
velocity difference even as high as 200 km/s
(larger than is observed), the time of the
encounter would have been 2 x 10^9^ years ago. This
is so long a time that any tidal plumes would have
disappeared. Hence, the present peculiarities of
NGC 7135 and IC 5135 would seem to be
generic to the galaxies and are not a result of a
previous encounter.
The arms in IC 5135 are smooth. There is
no large central bulge nor normal bright underlying
disk. There is no coherent central region.
The smoothness of the evident spiral arms
requires a type classification of Sa if the galaxy is
to be put into the classification sequence at all.

18. 1993ApJS...86....5K
Re:NGC 7130
NGC 7130; Sa pec, Seyfert 2 + starburst.
NGC 7130 is an extremely luminous far-infrared source with a compact
radio core (Norris et al. 1990). Both characteristics are related to the
Seyfert activity. Thuan (1984) discusses the dual nature of the nucleus
of this galaxy as seen in the IUE UV spectrum, with both broad absorption
lines and blue continuum showing the presence of massive stars and star
formation, and the Ly{alpha} emission line. Shields & Filippenko (1990)
have confirmed the dual nature of the nucleus in optical and IR studies.
NGC 7130 is similar to NGC 5135 in having both Seyfert 2 activity and a
vigorous star-forming H II region.

19. 1993ApJ...412..535W
Re:IC 5135
IC 5135.-Our position at 10 microns agrees with the radio position of
van Driel, van den Broek, & de Jong (1991) to within 1".

20. 1985SGC...C...0000C
Re:NGC 7130
= IC 5135
Plate 683
Overexposed center, very faint smooth outer arms, loops. Possible
S0?sp with dark lane + bright nucleus. Note 30' correction to NGC dec.
Faint companion 0.8 north-preceding.

21. 1982ESOU..C...0000L
Re:ESO 214520-3511.1
=ESO 403- G 32
peculiar
disturbed
in cluster
NGC Dec off 30'

22. 1976RC2...C...0000d
Re:IC 5135
= NGC 7130 with NGC coordinates corrected.
Collision?
Non-interacting pair with IC 5131 at 12 arcmin and faint anonymous spindle,
SBm?, at 6.5 arcmin following.
NGC 7135 at 18 arcmin north-following.
Spectrum:
Velocity from source G1 (A.J., 72, 730, 1967) was incorrectly attributed
to NGC 7135. Source L2 (Freeman 1975, private comm.) confirms correct
identification.

23. 1964RC1...C...0000d
Re:IC 5135
= NGC 7130 with 30 arcmin correction to NGC Dec.
Extremely bright center. Incomplete pseudo (r): 0.4 arcmin x 0.3 arcmin.
2 main curved streamers form a pseudo (R): 1.0 arcmin x 1.0 arcmin. Colliding
system?
Non-interacting pair with IC 5131 at 12 arcmin.
Non-interacting pair a faint anonymous spindle, possibly an SBm galaxy, at
6.5 arcmin following.
Distantly paired with NGC 7135 at 18 arcmin.


Back to NED Home