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Notes for object NGC 3516

35 note(s) found in NED.

1. 2009ApJ...705..962C
Re:NGC 3516
The NGC 3516 sight line passes near Complex C, but not through a detectable (21
cm) column of H I. A Si III feature is detected centered at V_LSR_ ~ -150
km s^-1^, a velocity similar to that of Complex C in that vicinity. The feature
is also clearly detected in C II {lambda}1334.53, and possibly in weak features
of O i {lambda}1302.17 and Si iii {lambda}1193.29. This sight line likely probes
a low column density portion of Complex C.

2. 2009ApJ...690.1322W
Re:NGC 3516
NGC 3516. NGC 3516 has a very complex spectrum. A very significant
({DELTA}{chi}^2^ {approx} 600) blackbody component was also added with
kT = 52.2^+1.4^ _-2.0_ eV and a normalization of 0.086. This source is
extensively studied, particularly because of the complex absorption

3. 2007AJ....134.1061D
Re:NGC 3516
We present in this paper two new observations of NGC 3516 taken by FUSE. There
have been a total of six observations taken with FUSE. In the first observation
Kriss (2002) identified the same components seen in FOS, STIS, and GHRS data by
Crenshaw et al. (1999) and Kraemer et al. (2001). Kraemer et al. showed that NGC
3516 shows variability in the absorption features, allowing them to find a lower
limit on the transverse velocity of ~1800 km s^-1^.

4. 2007AJ....134..648M
Re:NGC 3516
NGC 3516 (Figs. 7.8, 9.8, 20.8): There is diffuse light surrounding the bright
nucleus of this galaxy up to several hundred parsecs away. There is also
evidence of obscuration by dust to the south and to the north of the nucleus.
The northern dusty patches trace a spiral pattern.

5. 2007A&A...461.1209D
Re:NGC 3516
NGC 3516: The source is known to be variable and to display a complex
X-ray spectrum. A recent paper (Turner et al. 2005) reconciles the
behavior of the source recorded during 2001 simultaneous BeppoSAX,
Chandra, and XMM-Newton observations in a single scenario. In the
proposed framework, the primary emission is absorbed by at least 3
components. For two of these, the ionization state is coupled with the
variations of intrinsic emission, and the changes of their ionization
state could explain much of the spectral variations observed in
NGC 3516. BeppoSAX observed the source 6 times during its lifetime,
recording a flux variation of a factor of ~2.9 both in the 2-10 keV and
20-100 keV bands. For this source the adoption of a single baseline
model was hampered. For observations a, d, and f the best fit was
obtained including a relativistically broadened FeK{alpha} line that was
unnecessary (although not excluded) in observations b and e. In the same
manner, observations c, d, and e require a ionized absorber (modeled
here with absorption in XSPEC). Observations d and e also require a
partial absorber (modeled with pcfabs in XSPEC). Moreover, all the best
fits adopted here also consider a total absorber that displays strong
variations from ~0 to ~2 x 10^22^ cm^-2^. The overall picture coming
from the present data are in agreement with the scenario painted by
Turner et al. (2005), where the absorption is most probably due to
different components, some of which are ionized and variable. Thus, the
results reported here can be considered only as indicators of a possible
scenario, since i) the exclusion of the data below ~2 keV have hampered
any possibility of detailed modelizations of the complex absorber and
ii) the huge sensitivity of XMM-Newton permitted us to disentangle the
various components of the absorbers.

6. 2006A&A...453...27C
Re:UGC 06153
UGC 6153: Netzer et al. (2002) fitted the spectrum obtained with the Chandra Low
Energy Transmission Grating using a photon index {GAMMA} = 1.7 plus a reflection
spectrum of gas with a column density of N_H_ = 10^24^cm^-2^ and a covering
factor of 0.4-0.7.

7. 2005A&A...440...73C
Re:UGC 06153
UGC 6153: dust patches cover a large fraction of the nuclear regions of this
galaxy and a bright point source is present. Nonetheless, the profile is
relatively well behaved and suggests a classification as power-law. The
residuals larger than average for the other sources makes it tentative.

8. 2004MNRAS.350.1087S
Re:NGC 3516
NGC 3516: we have fitted to this SB0^0^ galaxy a Freeman type II disc
with r_cut_= 5.7 kpc (25 arcsec).

9. 2004ApJ...613..682P
Re:NGC 3516
NGC 3516. This is another object observed by the LAG consortium (Wanders
et al. 1993). We note that the light curves for this object may be less
reliable than those of other objects as the extended narrow-line region
in this object makes narrow line-based flux calibration vulnerable to
seeing effects, which then have to be modeled (Wanders et al. 1992). We
used the scaled and corrected spectra to determine the rms spectrum,
following Onken et al. (2003).

10. 2004A&A...422...65B
Re:NGC 3516
3.3.7 NGC 3516 The BMS for NGC 3516 includes also the soft X-ray data,
because the source is probably seen through a complex absorber (see
e.g. Guainazzi et al. 2001; Costantini et al. 2000) and excluding the
spectrum below 2.5 keV gives erroneous results on the continuum
parameters. The need to model the low energy part of the spectrum
required the inclusion of a large number of components to the BMS,
mainly absorption edges and emission lines. The resulting {chi}^2^ is
acceptable (296/256 d.o.f.): a detailed discussion on the parameters of
this fit is beyond the scopes of this work. It is worth noting, however,
that the source appears absorbed by a considerable column density of
ionized gas (about 1.5 x 10^22^ cm-2), while that from neutral gas
is almost negligible (around 4 x 10^20^ cm^-2^).
In addition to a 6.4 keV narrow emission line (required at the 99.99%
confidence level according to F-test), an interesting feature in the
spectrum is found at 6.08+-0.03 keV, whose detection is also at the
99.99% confidence level. Similar lines were found by Turner et
al. (2002) in another XMM-Newton observation of NGC 3516 and a Chandra
one performed simultaneously. On the other hand, our analysis of the
partly overlapping 73 ks Chandra observation does not show any evidence
for features other than the 6.4 keV line. However, the upper limit to
the flux of a narrow line around 6.1 keV is consistent with the flux
measured in the XMM-Newton observation. This emission line belongs to
the peculiar features possibly arising in an orbiting spot in the
accretion disk, as proposed for ESO198-G024 and IC 4329A. Again, we
refer the reader to Dovciak et al. (2004) for details.

11. 2003ApJS..148..327S
Re:NGC 3516
5.32. NGC 3516
The [O III] image of this Seyfert 1 galaxy is presented in the top
right panel of Figure 10. The emission is S-shaped, extended by 13.6"
(2330 pc) along P.A. = 20^deg^. The extension of the emission along
the E-W direction at the bottom and top of the S-shaped structure is
6.9" (1180 pc). A detailed study of the NLR of this source is
presented by Ferruit, Wilson, & Mulchaey (1998). Nagar et al. (1999)
detected extended radio emission along P.A. = 10^deg^.

12. 2003ApJS..146..353M
Re:NGC 3516
NGC 3516 (LW)
This bright AGN has a number of spiral dust arms to the north of the
nucleus, along with several large, diffuse emission-line regions at
larger radii. To the south there is relatively little dust structure
in the circumnuclear region, although this may be due to inclination.

13. 2002MNRAS.337..808K
Re:NGC 3516
A6 NGC 3516
This galaxy hosts a Seyfert 1.5 nucleus, but shows little structure in the
optical. The images displayed in Fig. 1(f) have a field of view roughly
half as big as the rest of the galaxies, owing to the larger distance and
smaller angular size of this galaxy. The H{alpha} image shows enhanced
emission from the nuclear region, not necessarily from SF but quite
possibly from the AGN. We do not detect any sign of SF in the bar or disc
of this galaxy. The B-I colour index image shows no convincing structure in
the disc, except possibly two redder regions near the ends of the (main)
bar. The nucleus is red, as seen in the B-I image and profile, but the
white patch es seen in the image (Fig. 1f) may be artificial and induced by
the near by presence of the strong nuclear peak. The B-I profile decreases
from the nucleus, and becomes stable at 2.5 mag. The H{alpha} emission in
the CNR of NGC 3516 (Fig. 2f) is featureless apart from a slight extension
in the east-west direction.

14. 2002AJ....124..675C
Re:UGC 06153
CfA Seyfert 1 (Huchra & Burg 1992).

15. 2001ApJS..133...77H
Re:NGC 3516
NGC 3516 (S1.2). - The shape of the synthesized beam is highly
elongated, and our maps do not sample well the extended emission in this
object. A strong (122 mJy at 6 cm, 326 mJy at 20 cm) background source
4.3' to the southeast also contributes sidelobe confusion. The central
core component in NGC 3516 has been well documented in previous
observations at 20, 6, 3.6, and 2 cm (Ulvestad & Wilson 1984b, 1989;
Kukula et al. 1995; Nagar et al. 1999). The deeper 20 cm map
({DELTA}{theta} = 1) presented by Miyaji, Wilson, & Perez-Fournon (1992)
shows elongated, one-sided emission extending 20 northeast of the nucleus.
The apparent spatial coincidence of the radio continuum with optical
emission-line nebulosity suggested to these authors that the two components
are related to a bipolar gaseous outflow from the nucleus. Our 20 cm map
clearly detected the same northeast extension, but we also see a weaker
counterpart, of approximately the same length, toward the southwest. Both
have roughly equal strength, each ~4 mJy. The double-sidedness of the
linear feature is even more evident in the tapered 6 cm map. The total
angular extent of the source is ~51", which corresponds to a projected
length of 9.6 kpc, along P.A. = 38^deg^. The southwestern extension can
also be seen in the {DELTA}{theta} = 6" 6 cm WSRT image of Baum et al.
(1993). It is of interest to note that the [O III] {lambda}5007 image of
Miyaji et al. (1992) shows significant line emission to the southwest of
the nucleus, roughly coincident with the southwestern jet component.

16. 2001ApJ...550..261W
Re:NGC 3516
3.3.4. NGC 3516
NGC 3516 has been observed by ASCA on four occasions. The source flux
varies by ~50%, decreasing most between the first and second observations,
separated by less than a year (Fig. 8d). The line energy changes somewhat
on long timescales. Nandra et al. (1999) also find short-timescale
variability in the line profile.
Changes in line flux and EW are significant. The line flux follows the
continuum drop-off between observations 1 and 2 ({DELTA}t ~ 1 yr) but then
increases again as the source becomes fainter ({DELTA}t ~ 3 yr). The latter
change is accompanied by an increase in EW. The fact that the line first
follows the continuum change and then becomes stronger as the continuum
weakens is difficult to understand in terms of simple disk models of the
iron line.

17. 2000MNRAS.317..234P
Re:NGC 3516
3.6 NGC 3516
The only obvious feature in our images is the very red nucleus. Neither
the broad-band HST H image nor our ground-based NIR colour maps reveal
any other structure (Figs 1 and 2f). Regan & Mulchaey (1999) used an
HST WFPC2-NICMOS colour index map to show that a single spiral dust
pattern dominates the circumnuclear morphology of this galaxy. They
described a strong red dust lane that emerges from a blue feature north
of the nucleus at a radius of 3 arcsec. The spatial resolution of our
images is not high enough to reveal such fine details. The differences
between our images and HST images are probably due to the longer
spectral baseline that Regan & Mulchaey used (0.55 to 1.6 microns) and
the different spatial resolution.
Quillen et al. (1999) noticed that the inner J-band isophotes are
slightly elongated in a direction roughly perpendicular to the outer
bar, so the galaxy may be doubly barred. Our H-band profile indeed
shows an isophote twist of about 50^deg^ (Fig. 2f). Quillen et al.
(1999) saw a curved dust feature at about 4 arcsec south of the nucleus
in their HST WFPC2-NICMOS colour index map.

18. 1999ApJS..120..209N
Re:NGC 3516
NGC 3516 (type 1.2; Fig. 10) - The 20cm map shows an extension to
the north in P.A. ~8^deg^, but the 3.6cm map shows only the unresolved
nucleus. There is a strong confusing source ~4' away that is very
difficult to clean out. Miyaji, Wilson, & Perez-Fournon (1992) present
deeper radio images of this source that reveal a P.A. of 10^deg^ for
the central source and a larger scale northern extension, the P.A. of
which increases from 10^deg^ to 20^deg^ with increasing distance from
the nucleus. We measure a radio extent of 0.65" (0.17 kpc) in our 20cm
map but use an extent of 4 kpc from Miyaji et al. (1992). Miyaji
et al. (1992) measured fluxes at 20cm of 4.31 and 2.17 mJy for the
north and south components of the central source, respectively. We do
not completely resolve these two components, but our total flux of 9.4
mJy is significantly higher than the sum of Miyaji et al.'s (1992)
fluxes. UGC lists a host galaxy major axis P.A. of 55^deg^, a blue
size of 2.1^deg^ x 1.8^deg^, and a red size of 2.3' x 2.0'. However,
RC3 does not list a P.A. for the major axis. Thompson & Martin (1988)
used enlarged sky survey prints to derive a P.A. of 55^deg^ for the
brighter isophotes, but they list this as an unsure determination. We
used a POSS-E red plate from DSS to measure a P.A. of 55^deg^. Arribas
et al. (1997) find the stellar-kinematic line of nodes to be 53^deg^
+/- 5^deg^ over the inner ~10" of the galaxy. Since the kinematic and
photometric axes are in close agreement, we use a major axis P.A. of
55^deg^ with a quality flag of "a." Ho et al. (1997) use the criterion
of Whittle (1992a) to classify this object as a Seyfert 1.2, which
agrees with the classification in Whittle (1992a).

19. 1999ApJ...526L...9P
Re:NGC 3516
This is a Seyfert 1 galaxy for which Nagar et al. (1999) found that
the radio jet is along P.A. = 10^deg^. The parameters derived by Kinney
et al. (1999) are i = 37^deg^ and {delta} = 46^deg^. Nandra et al.
(1999) found that the Fe K{alpha} line could be fitted by an inner disk
inclination (+/-{phi}) of i_disk_ = 35^+1^_-2_ degrees. The inspection
of the HST image (Malkan et al. 1998) shows that the north side of the
galaxy is closer, so the jet is projected against the nearer side of the
galaxy. Applying equation (3) to this data, we find that
{beta} ~ 66^deg^.

20. 1999AJ....117.2676R
Re:NGC 3516
A single spiral dust pattern dominates the morphology of the S0
galaxy, NGC 3516. The main red dust lane emerges from the blue feature
north of the nucleus at a radius of ~3". It then appears to spiral
around the nucleus and get closer until it is lost in the diffraction
effects ~0.5" from the nucleus. The extinction in the map is very
asymmetric with the majority being concentrated in north of the
nucleus. The saturated nucleus in the WFPC2 image creates several
artifacts in the color map. These are the blue cross and the very blue
east-west ridge. A fainter red linear feature to the north and south is
due to the diffraction spikes in the NICMOS image.
There seems to be a connection between the dust lane to the north
of the nucleus seen in extinction and a blue feature to the northeast of
the nucleus. The morphology of the blue feature is not consistent with
it arising from star formation since it shows a filamentary structure.
The blue emission to the southwest of the nucleus also is more extended
than the diffraction spikes. The diffuse blue emission ~1.5" southwest
of the nucleus appears to connect to the red excess seen 5"
west-southwest of the nucleus.

21. 1998ApJS..114...73G
Re:NGC 3516
Section A5. NGC 3516
This source, one of the original galaxies classified by Seyfert (1943) as a
type 1.0 galaxy, was first detected in X-rays by Einstein (Maccacaro,
Garilli, & Mereghetti 1987). In our analysis of the data from an ASCA
observation performed in 1994 April, we find no model in Section 5 that
satisfies our formal criteria for acceptability. Nevertheless, we find model
B(i) to provide a significant improvement over models A(i) and A(ii),
offering clear evidence for ionized gas and confirming the results of R97 and
those from a second ASCA observation carried out in 1995 March (Kriss et al.
1996a). However, while a single-zone photoionization model clearly reveals a
strong "~1 keV deficit" in this source, we find that despite providing a vast
improvement, a satisfactory fit is still not obtained with the inclusion of
an additional absorption edge (Section 6.2). Interestingly, we note that
neither R97 nor Kriss et al. (1996a) were able to find a solution that
satsifies our criteria for acceptability. We find a derived index
({GAMMA} ~ 1.9), steeper than that which has been claimed from previous
Einstein (Kruper, Canizares, & Urry 1990), EXOSAT (Ghosh &
Soundararajaperumal 1991), and Ginga (Kolman et al. 1993) observations in the
2-10 keV band. However, all these observations required a neutral
N_H,0_ >> N^gal^_H,0_, undoubtedly due to the incorrect modeling of the deep
O VII and O VIII edges in this source with neutral gas. A steeper index
({GAMMA} >~ 2.4) is implied when a single power-law model is applied to the
ROSAT PSPC data (Boller et al. 1992), again probably the result of the deep
O VII and O VIII edges. For models B(i)-C(ii), we find a neutral
N_H, 0_ ~ 5 x 10^20^ cm^-2^ and an ionized N_H, z_ ~ 9 x 10^21^ cm^-2^, with
U_X_ ~ 0.1. For comparison, R97 find N_H, z_ ~ 10^22^ cm^-2^, {GAMMA} ~ 1.7,
and U^R97^_X_ ~ 0.06 from an independent analysis of the ASCA data set
obtained in 1994 April and assuming a single-zone model. Kriss et al. (1996b)
have performed a detailed analysis of the 1995 March observation (using
XSTAR) and for a single-zone model find U_X_ ~ 0.03 (assuming their quoted
spectrum), N_H, z_ ~ 10^22^ cm^-2^ and {GAMMA} ~ 2.0. These workers also find
adding a second zone of ionized gas significantly improves the fit, obtaining
a best-fitting solution with U_X_ ~ 0.1, N_H, z_ ~ 1.4 x 10^22^ cm^-2^, and
U_X_ ~ 0.02, N_H_, z ~ 7 x 10^21^ cm^-2^ for the two zones. Nandra et al.
(1997c) have recently shown the Fe emission line varied significantly between
the two ASCA observations. Evidence for absorption by ionized gas was found
in three Ginga observations of NGC 3516, with N_H, z_ ~ 2-3 x 10^23^ cm^-2^
(Kolman et al. 1993). We also note that ROSAT HRI observations show possible
evidence for elongation of some fraction of the soft X-ray emission in
NGC 3516 in a direction consistent with the extended narrow-line region
(Morse et al. 1995).
NGC 3516 has long been known to exhibit deep, variable absorption lines in
the UV (Koratkar et al. 1996; Kriss et al. 1996a and references therein)
with at least four distinct radial components visible in C IV (Crenshaw et
al. 1998). From the combined analysis of the simultaneous ASCA and HUT,
Kriss et al. (1996b) conclude that a range of column densities and
ionization parameters are required to explain the depths of all the X-ray
and UV absorption features seen in NGC 3516 (see also Mathur, Wilkes, &
Aldcroft 1997).

22. 1998ApJ...500..685P
Re:NGC 3516
3. NGC 3516.--NGC 3516 has a type 1 Seyfert nucleus in an S0 galaxy. The optical
nucleus is very prominent in the optical broadband images that show no dust
features. This is the only galaxy studied for which only two components are
needed to fit its SED, a cold component at 49 K, with total width of ~19 K, and
a warm component at 153 K, with a ~50 K width. Both components have similar

23. 1998AJ....116.2682C
Re:IRAS 11033+7250
NGC 3516. Seyfert 1.5. Radio images suggesting outflow in Wrobel &
Heeschen (1988), Miyaji, Wilson, & Perez-Fournon (1992), and Baum et al.

24. 1997MNRAS.286..513R
Re:NGC 3516
7.1.6 NGC 3516
Kriss et al. (1996a) present an analysis of a later ASCA observation (1995
March 11/12) of the Seyfert 1 galaxy NGC 3516 than that presented here (1994
April 2). It is found that the source has a similar luminosity in both epochs.
The inferred oxygen edge depths are also consistent with not having changed
between the two epochs. Simultaneous observations with the Hopkins Ultraviolet
Telescope (HUT) were also performed (Kriss et al. 1996b). Kriss et al. show
that the UV and X-ray data combined strongly argue for a multizone ionized
absorber containing a large range of ionization states. They also show how
detailed photoionization modelling of the 1995 ASCA data hints at a multizone

25. 1997ApJS..112..391H
Re:NGC 3516
NGC 3516.--We determined the narrow-line spectrum of this well-known Seyfert 1
nucleus (Boksenberg & Netzer 1977) quite accurately, using a model derived from
[S II] (Fig. 6c). The resulting fits give ([N II] {lambda}6583)/H{alpha}=1.3,
([S II] {lambda}{lambda}6716, 6731)/H{alpha}=0.70, and ([O I] {lambda}6300)/
H{alpha}=0.15. The broad-line component is also clearly present in H{beta} and

26. 1997ApJS..110..299M
Re:NGC 3516
Bar is visible in both the ellipse fits and the K_S_image.

27. 1997ApJS..108..155G
Re:NGC 3516
This is a S1 galaxy in a S0 host galaxy. It is one of the galaxies in the
original list of Seyfert (1943) and was reported as the first emission-
line variable galaxy (Andrillat & Souffrin 1968). The H{alpha} image
shows circumnuclear emission extended ~20" in a Z-shaped structure,
elongated at P.A. = 45^deg^ (Fig. 11b). Narrow-band H{alpha} and [O III]
images have been reported previously by Pogge (1989a), Miyaji, Wilson, &
Perez-Fournon (1992), and Wanders et al. (1994). The radio continuum map
reveals an elongated structure aligned and cospatial with one of the
sides of the Z structure (Miyaji et al. 1992). The velocity of these
structures shows large departures from rotation, which are explained by a
bipolar outflow from the nucleus (Mulchaey et al. 1992; Veilleux, Tully,
& Bland-Hawthorn 1993). No H II regions are detected in the disk.

28. 1997A&A...319...33A
Re:NGC 3516
NGC 3516 This is a strong X-ray Seyfert (C=2582) with sources inside ~r=11'
aligned NW-SE. At r=22.5' along this line to the NW is encountered a very
strong, C=155.7 source which is a catalogued Sey. 1 of V=16.40 mag., z=.089, or
about 10 times the redshift of NGC 3516. Similar objects found in our Seyfert
sample are listed in Table 2 and discussed in the summary. The inner sources
pictured in Fig. 11 are all identified accurately with BSO's as indicated in
Table 3. Note the probability of a double quasar for C=3.1
Also note the very similar BSO's, C=6.6 N and 6.6 S, extremely well aligned
across the brighter BSO, C=7.1. This could represent another case of a
secondary alignment originating from a larger, active companion as in NGC 5273
and NGC 5548 following.

29. 1995MNRAS.276.1262K
Re:NGC 3516
NGC 3516:Type 1(1.5). Host galaxy: lenticular with bar and ring (CPG), SB0
(UGC). Radio: Baum et al. (1993) found radio emission with a total extent
of 45 arcsec at 6 cm, centred on an unresolved flat-spectrum radio core
which is coincident with the optical nucleus (Ulvestad & Wilson 1984b).
The surface brightness of the extended structure is too low for it to be
detected in the present 8.4-GHz observations and both maps show only the
central object, which is unresolved by both C- and A-configurations
(although the flux ratio of ~3:1 implies that there is emission on
intermediate scales). The positions agree well with the optical position
(Clements 1981), but differ from that of Edelson (1987) by ~3 arcsec.

30. 1994CAG1..B...0000S
Re:NGC 3516
Feb 11/12, 1980
12 min
The partial external ring that is
semi-detached from the main body in NGC 3516 is
well seen in this negative print. The two opposite
regions of decreased luminosity between the
outer edge of the inner disk and the external ring
is shown here at position angles 4 and 10 o'clock
in the orientation of the print. The axis of the line
through these two regions of decreased
luminosity makes an angle of about 20 deg with the
axis of the bar. The bar is burned out on this
negative print. However, it is well formed and is
almost vertical in the print here.

31. 1993ApJ...419..553B
Re:NGC 3516
NGC 3516 (UGC 06153)
Subarcsecond VLA images of the Seyfert 1 galaxy NGC 3516 have faced to
resolve the nucleus but show instead only a flat spectrum radio core
centered on the optical nucleus (Ulvestad & Wilson l984b). However, VLA
C-array images taken by Wrobel & Heeschen (1988) have revealed the
presence of a linear radio source on the tens of arcsecond scale. Our
full resolution WSRT images (Fig. 7a, 4.1" x 4.3" resolution) confirm the
results of Wrobel & Heeschen and show the radio structure with somewhat
better resolution and signal-to-noise. The tapered image (Fig. 7b, 6.0" x
6.4" resolution) reveals that the source has a total extent of ~45" (~8.5
kpc) and is oriented along P.A. 44^deg^. The radio emission is aligned
with the extended [O III] emission detected by, for example, Pogge (1989)
and Miyaji, Wilson, & Perez-Fournon (1992). However, the radio emission
appears to extend beyond the currently observed inner "Z" in the [O III]
emission and exhibits an additional "wiggle" giving the radio source a
"corkscrew" appearance. The radio structure is not symmetric about the
radio core but is brighter to the northeast of the nucleus and fainter
and more diffuse to the southwest. Long-slit optical spectroscopic
observation provide evidence that the gas within ~0.5 kpc of the nucleus
in NGC 3516 exhibits the kinematic signature of a low-velocity (several
100 km s^-1^) bipolar outflow (e.g., Goad & Gallagher 1987: Mulchaey et
al. 1992).

32. 1976RC2...C...0000d
Re:NGC 3516
Type 1 Seyfert,
B(nucleus) = 14.0 - 16.0
B_T(excluding nucleus) = 12.60.
Diameter of nucleus:
A.J., 73, S175, 1968.
"Nuclei of Galaxies", 27, 1971.
Publ.Dept. A. Univ. Texas, II, 2, No. 7, 1968.
A.J., 73, 858, 1968.
Photometry (UBV):
A.J., 73, 866, 1958.
Astrophys. Lett., 1, 171, 1968.
Astrophys. Lett., 12, 1, 1972.
Ast. Tsirk., No. 620, 1971.
Sov. A.J., 16, 763, 1973.
Sov. A.J., 17, 169, 1973.
M.N.R.A.S., 169, 357, 1974.
Att...Conv. Sci. Osserv. Cima Ekar, Padova-Asiago, 101, 1973.
= Cont. Asiago No. 300b.
Photometry (I.R. 1-10 microns):
A.J., 73, 866, 1968.
Ap. J. (Letters), 176, L95, 1972.
M.N.R.A.S., 169, 357, 1974.
A.J., 73, 862, 897, 1968.
Astrophys. Lett., 1, 111, 1968.
Astrophys. Lett., 8, 161, 1971.
Astrophys Lett., 13, 165, 1973.
Ap. J., 174, 483, 1972.
Astr. Ap., 22, 343, 1973.
Ast. Tsirk., No. 688, 1972.
Ast. Tsirk., No. 831, 1974.
Ast. Tsirk. No 467, 1968.
Ap. J., 162, 743, 1970.
Ann.Ap., 31, 569, 1968.
Sov. A.J., 11, 767, 1968.
Astr. Ap., 1, 305, 1969.
Astr. Ap., 27, 433, 1973.
IAU Symp. No.29, 82, 1968.
"Nuclei of Galaxies", 151, 1971.
Pol.Ast. Tsirk., No 454, 1967.
Astrofizika, 7, 417, 1971.
Astrofizika, 8, 509, 1972.
Radio Observations:
Astr. Ap., 15, 110, 1971.

33. 1973UGC...C...0000N
Re:UGC 06153
(R)SB(s)0/a: (de Vaucouleurs)
11 02.5 +72 46 at 4.6, 236, 0.35 x 0.30, m=15.4

34. 1964RC1...C...0000d
Re:NGC 3516
Extremely bright nucleus on a short bright bar: 0.4 arcmin x 0.1 arcmin.
Very faint (R): 0.95 arcmin x 0.95 arcmin.
Heidelberg Veroff. Vol. 9, 1926 dimensions are for the nucleus or lens only.
P.A.S.P., 53, 231, 1941.
Ap. J., 97, 28, 1943.

35. 1956AJ.....61...97H
Re:NGC 3516
HMS Note No. 108
This nebula is one of the uncommon, highly concentrated types
whose nucleus shows a spectrum of very broad bright bands.
It isone of those studied spectrophotometrically
by Seyfert, C.K. (1943, Ap. J., 97, 28)

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