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Notes for object NGC 5548

34 note(s) found in NED.

1. 2009ApJ...705..962C
Re:NGC 5548
This sight line shows some evidence for high-velocity gas, but the absorption
only extends out to V_LSR_ = -125 km s^-1^ in the Si III profile. The feature is
not seen in low ions, although low ion absorption features do extend out to
nearly V_LSR_ = -100 km s^-1^. Although we see absorption out to V_LSR_ = -125
km s^-1^ in O VI, it was reported as a high-velocity non-detection by S03. Owing
to the weakness of the absorption and the small extent into the "high-velocity"
range, we report this sight line as a Si III non-detection. We estimate an upper
limit on high-velocity N_Si III_ by assuming 100 km s^-1^ width for any possible

2. 2009ApJ...705..199B
Re:NGC 5548
The current low-luminosity state of NGC 5548 has resulted in a very low, broad
H{beta} line profile which extends under the [O III] doublet. As the [O III]
lines in this object are quite strong, we attempted to subtract them from each
spectrum using a very localized linear continuum (which actually includes the
red wing of the H{beta} profile) before creating the light curves for the four
velocity bins. Only the most redward velocity bin is affected by the [O III]
lines, and so the measured lag time for that bin may be somewhat suspect. The
average lag time for each bin is shown in Figure 15, where there does not seem
to be an ordered behavior. In this object as well, each of the measured lag
times is generally consistent with the others within the errors, rendering
interpretation as somewhat ambiguous.

3. 2007AJ....134.1061D
Re:NGC 5548
NGC 5548 was found to be intrinsically absorbing by Shull & Sachs (1993) in data
from IUE along with evidence of X-ray warm absorption (George et al. 1998).
Crenshaw et al. (1999) found absorption in FOS data as well. More recently
Crenshaw et al. (2003) saw five blended and broad components in data from STIS.
We see a case similar to what Crenshaw et al. did in the FUSE data, with five
blended and broad components.
Brotherton et al. (2002) examined the FUSE data available prior to 2002
and found intrinsic absorption spanning the range between 0 and -1300 km s^-1^,
which is coincident with what we have found in our co-added spectrum.

4. 2007AJ....134..648M
Re:NGC 5548
NGC 5548 (Figs. 7.11, 9.11, 20.11): This is a face-on spiral with a very bright
nucleus. Several hundred parsecs to the north of the nucleus there is an arc of
star formation, plus several scattered and relatively isolated stellar clusters
still farther away.

5. 2007A&A...461.1209D
Re:NGC 5548
NGC 5548: The BeppoSAX data acquired during the 1997 observations were
divided into 4 observations. Nicastro et al. (2000) summed these
datasets to perform the spectral analysis, while here they were
analyzed separately. Nicastro et al. (2002) found that the source X-ray
spectrum is well modeled, adding a reflection component to a power law
continuum with a high-energy cut-off. This is in agrement with the
results presented here. On the contrary, Nicastro et al. (2002) found
signatures of the presence of a warm absorber below ~ 2.5 keV that are
negligible once the LECS data are excluded by the spectral analysis. The
same results are also obtained for the last two observations.

6. 2006A&A...457...61R
Re:NGC 5548
NGC 5548. The NIR spectrum of this well-studied and known Seyfert 1 is
dominated by the He I 1.083 microns and [S III] 9531 Angstrom lines. It
also shows very broad components in the permitted lines (H I and He I),
of complex structure, similar to that observed in double-peaked
profiles. It is worth to mention that similar reports of double-peak
lines exist in the optical region on this object. In fact, due to the
high variability shown by NGC 5548, the double-peak in the optical
lines is not always detected. The coronal emission line spectrum is
remarkably strong, with [S VIII] 9912 Angstrom, [S IX] 12 520 Angstrom,
[Si X] 14 300 Angstrom, [Si VI] 19 630 Angstrom and [Ca VIII] 23210
clearly detected. The continuum emission displays a clear turnover at
13 000 Angstrom, which is rather steep to the blue. Redwards of the
turnover, the continuum emission rises steeply to the red, very likely
due to dust emission, similar to the one reported in Mrk 1239. The
stellar contribution to the observed spectrum seems rather low, with
only a few weak C O bands in H detected

7. 2004ApJ...613..682P
Re:NGC 5548
NGC 5548. Some comments on this object appear in {section}5. There are
more published variability data, by far, on this object than any other,
and most of the data are very good. Only a few problems need to be
pointed out. First, the H{alpha} region of the rms spectrum from the
Wise Observatory campaign (Netzer et al. 1990) has strong narrow-line
residuals that render the line-width measures unusable. The CCCD for the
associated time series is also rather ambiguous, so we do not include
these measurements in the mass determination. The H{beta} profile in the
rms spectrum from the fifth year of AGN Watch monitoring (i.e.,
JD 2,448,954-2,449,255) is very unusual, as shown in Figure 14; there are
two peaks, a strong central peak and a weak blue peak. The FWHM
measurement is thus meaningless. Finally, He II {lambda}4686 is
prominent in the rms spectrum for the first year of the AGN Watch
campaign (JD 2,447,509- 2,447,809), but is too heavily blended with the
optical Fe II blends to measure in the mean spectrum; this line is not
included in this part of the analysis (see Figs. 4 and 5).

8. 2004ApJ...607..309I
Re:NGC 5548
NGC 5548.-The integrated values for N V and C IV column densities are in
agreement with Savage et al. (1997) along the unremarkable sight line
toward this Seyfert I galaxy.

9. 2004A&A...422...65B
Re:NGC 5548
3.3.4 NGC 5548 This simultaneous observation was already published by
Pounds et al. (2003). The BMS gives an acceptable fit ({chi}^2^=206/192).
The parameters, shown in Table 2, are consistent with those found by
Pounds et al. (2003). In particular, the line width is marginally
resolved, with a value consistent with that measured by Chandra (Yaqoob
et al. 2001). These results are in contrast to the broad line found by
ASCA (Nandra et al. 1997). However, an analysis on eight ASCA
observations revealed a possible variability in the line flux, but no
evidence for a broad line (Weaver et al. 2001).

10. 2003ApJS..148..327S
Re:NGC 5548
5.43. NGC 5548
The [O III] emission from this Seyfert 1 galaxy has a halo-like
morphology (Fig. 12, top left), with a diameter of 1.3" (450 pc)
around the nucleus. It also presents some low surface brightness
fingers of emission extending by 2.7" (900 pc) in the N-S direction.
The radio emission extends for 18" along P.A. = -15^deg^ (Wilson &
Ulvestad 1982a). Ground-based observations (Wilson et al. 1989)
detected low-intensity [O III] emission that is not detected by the
current observations. This could be due to differences in the
sensitivity of the two observations.

11. 2003ApJS..146..353M
Re:NGC 5548
NGC 5548 (TW)
The extremely prominent nucleus of this Seyfert 1 galaxy at both V and
H obscures the central 500 pc with diffraction rings and other PSF
artifacts. On larger scales, a tightly wound spiral is apparent, and
this spiral may change from a one-arm to a two-arm spiral at a radius
of about 1 kpc.

12. 2003ApJS..146....1W
Re:NGC 5548
NGC 5548.-The O VI absorption looks narrower in the LiF2B segment than
in the LiF1A segment, but both segments were combined to create the
final spectrum.

13. 2002ApJS..143..257K
Re:NGC 5548
1417+2508rb.---A merger of 40 spectra of NGC 5548, which is known to
have variable luminosity and emission line profiles.

14. 2002AJ....124..675C
Re:UGC 09149
Unusually warm FIR source, low FIR/radio ratio for a spiral. Seyfert

15. 2002A&A...389..802P
Re:NGC 5548
NGC 5548. This observation was published by Nicastro et al. (2000).
They find internally evidence of a correlation between
{GAMMA} and the flux (previously discovered in Ginga observations
by Magdziarz et al. 1998, confirmed with RossiXTE observations by
Chiang et al. 2000), which has some impact on the quality of our
fit. In a Chandra LETGS observation Kaastra et al. (2002) find
evidence of a very complex warm absorber, of a soft excess and of
low energy emission lines. Following Kaastra & Barr (1989), who
first reported a soft excess in EXOSAT observations, they model
it as a "modified black body'' with temperature kT ~ 0.1 keV. They
suggest that the NVII emission line at 0.5 keV could be identified
with the low energy line detected by Nicastro et al. (2000) in the
BeppoSAX observation. We therefore added to the BMS a soft component,
as described by the module DISKBB in XSPEC, with kT fixed at 0.1 keV,
and a line with E_l_ fixed at 0.5 keV. The fit yields
W_l_ = 76 ^+61^_54_ eV, compatible with the Chandra result. N_s_ turns
out negligible compared to N_g_, while N_W_ =(2.4+/-0.7)x10^21^ cm^-2^
(with X_i_~14 erg cm s^-1^) is marginally consistent with the column
density of the dominant component in the warm absorber as estimated by
Kaastra et al. (2002). The iron line is unresolved and significantly
narrower (less than 0.13 keV) than in any of the other sample objects.
A Chandra HETGS observation (Yaqoob et al. 2001), with the source at a
flux level about 30% lower, has revealed a narrow line at 6.4 keV with
{sigma}_{alpha} = 41 ^+32^_-24_ eV, corresponding to a velocity spread
consistent with an origin in the outer BLR (a substantial contribution
to the line from thick matter beyond that region is not excluded). The
intensity of this line matches the one measured by us. Using the same
prescriptions for a relativistic disk line used by Yaqoob et al. (2001)
to obtain an upper limit of 7x10^-5^ cm^-2^ s^-1^, we find a more
stringent limit of 4x10^-5^ cm^-2^ s^-1^: this is a factor about 2 less
than in earlier ASCA records of a substantially broader line, as
reported in Yaqoob et al. (2001) or in Chiang et al. (2000). In a
spectral variabilty study with RossiXTE, Chiang et al. (2000) found
the intriguingly paradoxical (for the reprocessing paradigm) result
that W_{alpha}_ is anticorrelated to R.

16. 2001ApJS..133...77H
Re:NGC 5548
NGC 5548 (S1.5). - The classic triple linear structure of NGC 5548,
consisting of a compact core and oppositely directed lobes, is well known
(Wilson & Ulvestad 1982a; Kukula et al. 1995; Nagar et al. 1999; Wrobel
2000). Our maps are consistent with those of previous studies. The core is
unresolved at our resolution, and the total extent of the jets is
~15" (5 kpc) along P.A. = 163^deg^. We find evidence for weak
(S_pol,6_^P^ ~ S_pol,20_^P^ ~ 0.2 mJy beam^-1^) linearly polarized
emission associated with the extended emission (Fig. 16k).

17. 2001ApJ...550..261W
Re:NGC 5548
3.3.11. NGC 5548
The 2-10 keV flux varies by ~50% (Fig. 8k). When the iron line is
detected, its energy and flux remain constant. However, the Fe K line is
detected in only four of the eight observations. To derive upper limits,
we fix the line energy at its mean observed value. In these cases, we find
that the line flux and EW have decreased significantly (with 99%
confidence), in particular for observation 7 when the source is returning
to its bright state. (See line EW vs. continuum correlation in Fig. 9d.)
We have examined whether the disappearance of the line can result from
our technique of fitting a narrow Gaussian profile to a line that has
become extremely broadened. From a series of fits using a broad Gaussian,
both with and without the high-energy power-law component, we find no
evidence for a broad line for cases in which the narrow line has vanished.

18. 2001AJ....122..653R
Re:NGC 5548
NGC 5548: The extremely bright Seyfert nucleus dominates the bulge light
of NGC 5548 for radii <~ 1"-2". The Nuker parameters are thus quite
uncertain. No useful (unsaturated) optical image was found in the archive.

19. 1999ApJS..120..209N
Re:NGC 5548
NGC 5548 (type 1.2; Fig. 14) - The northern component seen in the
20cm map is limb-brightened, whereas the nuclear component is
unresolved (see Wilson & Ulvestad 1982). The P.A.'s of the peaks of the
northern and southern extensions relative to the core are 348^deg^ and
170^deg^, respectively. Neither of the extensions are detected in the
3.6cm map. There are two other sources in the field, one at {alpha} =
14^h^15^m^39.76^s^, {delta} = 25^deg^21'56.0" (B1950.0) and a double
source at {alpha} = 14^h^15^m^35.82^s^, {delta} = 25^deg^22'08.3"
(B1950.0). There is also a confusing source ~4' away. The radio sources
in the field around NGC 5548 are discussed in detail by Wilson
& Ulvestad (1982). The flux ratio R = F_[O III]_/F_H{beta}_ listed by
Whittle (1992a) leads to a classification of Seyfert 1.2, whereas Ho
et al. (1997) use the criterion of Whittle (1992a) to classify this
object as a Seyfert 1.5. We use a classification of Seyfert 1.2 as
long-term monitoring of the broad-line region in NGC 5548 (Peterson
et al. 1991) consistently gives R ~< 0.75. UGC lists a major axis P.A.
of 110^deg^ at an extent of 1.7' x 1.5'. The optical morphology of this
galaxy is, however, complex, and we do not list a major axis P.A. for

20. 1998ApJS..114...73G
Re:NGC 5548
Section A13. NGC 5548
This Seyfert 1.2 galaxy was first detected in X-rays by OSO 7 (Hayes et al.
1980). Absorption by ionized gas in NGC 5548 was first suggested by Ginga
observations (Nandra et al. 1991) and confirmed by the ROSAT PSPC (Nandra et
al. 1993). In our analysis of the data from ASCA observation performed in
1993 July, we find acceptable solutions with U_X_ ~ 0.1, N_H, z_ ~ 3 x 10^21^
cm^-2^, and {GAMMA} ~ 1.9 for all models B(i) and C(i). Consistent results
are also obtained for model B(ii), with no requirement for an unattenuated
(D_f_ = 0) component. This confirms the results of R97 who found the addition
of O VII and O VIII edges ({tau}_O7_ ~ 0.25 and {tau}_O8_ ~ 0.16)
significantly improved their fit to a single-power-law model ({GAMMA} ~ 1.9)
to these ASCA data. R97 also fitted a single-zone photoionization model and
found U^ R97^_X ~ 0.08, N_H, z_ ~ 5 x 10^21^ cm^-2^, assuming a single
optical-X-ray continuum {GAMMA} ~ 1.9. Mathur et al. (1995) have also
presented photoionization calculations based on previously published ASCA
results and obtain U_X_ ~ 0.06 (for their quoted optical-X-ray continuum)
assuming N_H_, z ~ 4 x 10^21^ cm^-2^.
We find a significant improvement in the goodness of fit is achieved assuming
model C(ii). However, the best-fitting solution occupies the region of
high-N_H, z_, high-UX, high-D_f_ parameter space and does not extrapolate
well <0.6 keV (Fig. 12). A yet superior improvement was found in
Section 6.4.2 consisting of the combination of a steep power law
({GAMMA}_s_ ~ 3.2) dominating the lowest energies and a flatter power law
({GAMMA}_h_ ~ 1.5) dominating at highest energies. The ionized gas in this
case has U_X_ ~ 0.2, N_H, z_ ~ 7 x 10^21^ cm^-2^ but also requires a neutral
column density (N_H_, 0 ~ 1.7 x 10^21^ cm^-2^) far in excess of N^gal^_H,0_.
A spectral flattening toward higher energies also seen in HEAO 1 (W95) and
Ginga (NP94) along with evidence for absorption by ionized gas, with
N_H, z_ ~ 5 x 10^22^ cm^-2^. A "soft excess" has been proposed in NGC 5548
from the analysis of EXOSAT (TP89) and ROSAT (Nandra et al. 1993; Done et al.
1995) data sets, but we find any such component to be insignificant >0.6 keV
from the analysis presented here.
NGC 5548 has been observed to have variable absorption lines of C IV, N V,
and Ly{alpha} in the UV (Shull & Sachs 1993; Mathur et al. 1995). A detailed
comparison between the UV and X-ray absorption systems indicates the same gas
is probably responsible (Mathur et al. 1995).

21. 1998AJ....116.2682C
Re:IRAS 14156+2522
NGC 5548. Seyfert 1. Optical position from Clements (1981). Only the
eastern VLA component is associated with NGC 5548. VLA A-configuration
maps at 1.465 and 4.885 GHz in Wilson & Ulvestad (1982).

22. 1997MNRAS.286..513R
Re:NGC 5548
7.1.11 NGC 5548
The oxygen edges of the warm absorber in the famous Seyfert 1 galaxy NGC 5548
were first found by the ROSAT PSPC (Nandra et al. 1993). A single-edge fit to
the ROSAT data yields an edge depth of {tau}~0.4, consistent with the values
found here and reported in Table 3. The ROSAT data also find a soft excess
component which, when modelled as a blackbody, has a best-fitting temperature
of kT=60_-20_^+13^ eV. This is rather softer than the values found from the
ASCA data (kT=240_-20_^+30^ eV) and suggests either some spectral variability
of the soft excess or a complex soft excess. For example. a blackbody soft
excess with a hard tail could reproduce these results, owing to the different
bandpasses of ROSAT and ASCA.
The ASCA data presented here have been previously reported by Fabian et al.
(1994b). These authors agree with the results obtained here.

23. 1997ApJS..112..391H
Re:NGC 5548
NGC 5548.This famous Seyfert 1 galaxy has been the target of recent intensive
variability monitoring aimed at determining the size and structure of its BLR
(see Peterson 1993 for a review). The [S II] lines have FWHM~300 km s^-1^ and
display an obvious blue wing. Constraining the narrow H{alpha} and [N II] lines
to have the same profiles, we subtracted suitably scaled versions of the [S II]
profile from the H{alpha}+[N II] complex (Fig. 6h). The final strengths of the
narrow lines, taken such that the broad profile be as smooth as possible at
their positions, yield the following narrow-line intensity ratios: ([N II]
{lambda}6583)/H{alpha}=0.9, ([S II] {lambda}{lambda}6716, 6731)/H{alpha}=0.7,
([O I] {lambda}6300)/H{alpha}=0.4, and ([O III] {lambda}5007)/ H{beta}=10. In
addition to the narrow and broad components of H, there is clearly also
substantial emission from a distinct component with intermediate velocities
(FWHM~1000 km s^-1^). Although the intermediate-width component is much less
prominent in H{beta}, comparison of the profile of [O III] {lambda}5007 with
that of the central peak of H{beta} suggests that it might be present. Broad
H{beta} and H{gamma} are present in the blue spectrum, as is an Fe II complex
centered near 4550 A and possibly also He II {lambda}4686.

24. 1997ApJS..108..155G
Re:NGC 5548
This is a well-known Seyfert 1 galaxy, subject of extensive monitoring
campaigns because of its spectroscopic variability (e.g., Peterson et al.
1994). It is a bright X-ray source (Mushotzsky et al. 1980). In radio
continuum emission, three radio sources are detected extended 13" in
total (Wilson & Ulvestad 1982). The narrow-band H{alpha} and [O III]
images and long-slit spectroscopy, reported by Wilson et al. (1989), show
an extended circumnuclear emission, with one high-excitation component
presumably ionized by radiation escaping from the nucleus, and another
low-excitation component ionized by hot stars. Our H{alpha} image shows
an extended nebulosity of 8" around the bright nucleus, but our image
does not have enough signal-to-noise to show the weak extended nebulosity
in the northeast detected by Wilson et al. (1989).

25. 1997A&A...319...33A
Re:NGC 5548
NGC 5548 Fig. 4 shows the disposition of the many strong sources around this
strong X-ray Seyfert. Only the brighter, outer sources are labelled in Fig. 4.
The inner sources are shown below in an enlargement of the X-ray map (Fig. 20).
Identifications are given in Table 3.

26. 1996ApJS..104...37M
Re:NGC 5548
NGC 5548.--It is interesting to compare the different widths of the narrow
components of He II {lambda}1640 and O III] {lambda}1663: 5.3 A versus 9.5 A
(not corrected for instrumental profile). This is a clear-cut example showing
that, while He II {lambda}1640 is often made up by a narrow component, and a
very distinct, very broad component, O III] {lambda}1663 is semibroad. There
is no evidence of a broad component for O III] {lambda}1663 in NGC 5548 nor in
any other object considered in this investigation. Fe II_UV_ is certainly

27. 1995MNRAS.276.1262K
Re:NGC 5548
NGC 5548: Type 1(1.5). Host galaxy: spiral with ring (CPG), Sa (UGC).
Radio: At 6 cm Wilson & Ulvestad (1982a), using the VLA, and Baum et al.
(1993), with the Westerbork Synthesis Radio Telescope (WSRT), report a
central component with bright radio lobes to the north and south - a
structure also seen in the current C-array map. The central component
appears as a point source with A-array, but the rest of the C-array
structure has been resolved out.

28. 1995ApJ...447..121W
Re:NGC 5548
NGC 5548.-We confirm spectral flattening at high energies for this
Seyfert 1 galaxy. The upper limit on N_HFe_ is roughly consistent with
Ginga (NP94).

29. 1994CAG1..B...0000S
Re:NGC 5548
April 27/28, 1979
10 min
NGC 5548 is a Seyfert galaxy with a starlike
unresolved nucleus. It has multiple fragments of
spiral arms. The outermost fragment is almost
circular, with a 180 deg wrap, as shown in this print
in the upper center. However, all fragments are
in a spiral pattern, connecting to the bulge at its
rim. Small-scale images might suggest that the
outer brightest arm is a broken ring (hence the
classification of PS0/a in the RC2), but the
pattern is spiral beyond doubt.

30. 1993ApJ...419..553B
Re:NGC 5548
NGC 5548 (UGC 09249)
Wilson & Ulvestad (1982a) published a paper on the optical and radio
morphology of the Seyfert 1.2 galaxy NGC 5548. The extended emission line
nebula has also been studied by Wilson et al. (1989). The Wilson &
Ulvestad VLA radio images (reproduced in Figs. 10a and 10c) show the
presence of an unresolved core which is straddled by two diffuse lobes of
radio emission along a P.A. of 155^deg^. Their images show that these
lobes" have edgebrightened or "bubble-like" appearances. The total
source.extent as seen in their images is 12" (~400 Pc). Our WSRT 6 cm
image (Fig. 10c; 3.5" x 8.5" resolution) shows additional emission with
total extent ~20" (~600 Pc) along P.A.~158^deg^. Our tapered WSRT 6 cm
image (Fig. 10d; 6.0" x 14.5" resolution) reveals that the source has a
total extent of ~30" (~1 kpc) with faint extensions to the west from the
northern tip of the source and to the east from the southern edge of the
source. These additional "wiggles" combined with those seen in the VLA
images (Figs. 10a and 10b) give the source a "corkscrew" appearance.
Wilson & Ulvestad argued that the radio lobes in this source originate
from the nuclear AGN and represent low-luminosity counterparts to the
radio jets/lobes seen in powerful radio galaxies. Interestingly, NGC 5548
has an unusually low far-IR luminosity for a Seyfert galaxy as well as a
flat 60-25 micron spectral index. Like powerful radio galaxies, its radio
luminosity is dominated by the extended (and not nuclear) radio flux. In
these respects, it is similar to a low-power radio galaxy.

31. 1985AnTok..202.237T
Re:KUG 1415+253
Seyfert galaxy?

32. 1976RC2...C...0000d
Re:NGC 5548
Type 1 Seyfert nucleus.
Diameter of Nucleus:
A.J., 73, S175, 1968.
B(nucleus) = 14.8-15.8.
B_T(excluding nucleus) = 13.30.
Astr. Ap., 15, 110, 1971.
Photometry (UBV):
A.J., 73, 858, 866, 870, 1968.
Publ. Dept. A. Univ. Texas, II, 2, No. 7, 1968. ,
Astrophys. Lett., 12, 1 1972.
Sov. A.J., 16, 763, 1973.
Sov. A.J., 17, 169, 1973.
M.N.R.A.S., 169, 357, 1974.
Ast. Tsirk., No. 620, 1971.
Ast. Tsirk., 777, 1973.
IAU Circ. No. 2529, 1973.
"Att...Conv.Sci.Osserv. Cima Ekar, Padova-Asiago", 101, 1973
= Cont. Asiago No. 300bis.
Photometry (I.R., 1-20 Microns):
A.J., 73, 866, 870, 1968.
Ap. J. (Letters), 159, L165, 1970.
Ap. J. (Letters), 161, L203, 1970.
Ap. J. (Letters), 176, L95, 1972.
M.N.R.A.S., 169, 357, 1974.
Ap. J., 169, 449, 1971.
Ap. J., 174, 483, 1972.
Ap. J. (Letters), 179, L89, 1973.
IAU Symp. No.44, 155, 1972.
Ap. J. (Letters), 154, L53, 1968.
Ap. J., 162, 743, 1970.
Ap. J., 164, 1, 1971.
Ap. J., 171, 5, 1972.
C.R.Acad. Sc. Paris, (B), 265, 1149, 1967.
Sov. A.J., 11, 553, 1968.
Astrofizika, 7, 389, 1971.
Ast.Tsirk. No. 467, 1968.
"Nuclei of Galaxies", 151, 1971.
Ap. J., 151, 71, 1968.
Radio Observations:
J.Phys., 19, 565, 1966.
A.J., 73, 876, 1968.
Astr. Ap., 15, 110, 1971.

33. 1973UGC...C...0000N
Re:UGC 09149
{(R')}SA(s)0/a (de Vaucouleurs)
Slightly asymmetric
{UGC incorrectly notes "Pec". H. Corwin}

34. 1964RC1...C...0000d
Re:NGC 5548
Extremely bright nucleus. Faint spiral pattern in lens: 0.5 arcmin x
0.5 arcmin. Outer whorls form pseudo (R): 1.0 arcmin x 0.85 arcmin.
Heidelberg Veroff. Vol. 9, 1926 and Lund 9 dimensions are for the lens only.
Broad emission lines in the nucleus.
L'Astronomie, 73, 3, 1959.

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