NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-04-19 T21:41:01 PDT
Help | Comment | NED Home

Notes for object NGC 5506

31 note(s) found in NED.


1. 2009ApJ...702.1127R
Re:NGC 5506
The nucleus of this galaxy is classified as a Sy1.9 based on the detection of
broad wings of the Pa{beta} profile in the near-IR (Blanco et al. 1990).
However, more recently, Nagar et al. (2002) presented evidence that NGC 5506 is
an obscured narrow-line Sy1, as a result of the finding of the permitted O I
{lambda}1.129 {mu}m line, together with a broad pedestal of Pa{beta} and rapid
X-ray variability. The clumpy models reproduce the near-IR and the N-band data
points well, while slightly underestimating the Q-band flux. The discrepancy
between the spectral observations and the model fit along with the poor mid-IR
fit together suggest either that additional emission contaminates the near-IR
measurements or that the models cannot produce this observed SED shape (Section
5.2). Based on the detection of a water vapor megamaser (Raluy et al. 1998), we
have introduced the inclination angle to the code as a Gaussian-prior centered
in 85^deg^ with a width of 2^deg^. In the resulting probability distributions,
we find {sigma} = 25{degree} +/- ^9^_7_, q = 2.5+/-^0.3^_0.4_, and the average
number of clouds along an equatorial ray to be less than 2. The optical depth
per cloud {tau}_V_ < 68, and the calculated torus optical extinction is A_V_ <
90 mag. NGC 5506 has the highest L^AGN^_bol_ of the sample (7.3 * 10^44^ erg
s^-1^; Table 9). As a consequence of the low values of N_0_ and {sigma} derived
from its fit, the reprocessing efficiency is low (7%). The galaxy nucleus is
very compact in the mid-IR, with an apparent optical depth of {tau}^app^_10
{mu}m_ ~ 1.4 (Roche et al. 1991, 2007; Siebenmorgen et al. 2004b), although NGC
5506 also shows variations in its silicate absorption depth on parsec scales
(Roche et al. 2007). Unfortunately, the fitted models reproduce the silicate
feature in emission ({tau}^app^_10 {mu}m_ = -0.21), contrary to the
spectroscopic observations. This galaxy has comparable X-ray and mid-IR
absorbing columns, indicating that the dust-free absorption in this galaxy is
lower th an for the Sy2 reported here.

2. 2009ApJ...696.1218Z
Re:NGC 5506
NGC 5506. The optical spectrum for NGC 5506 has strong [O III] and [N II] narrow
lines. The log([O III]/H{beta}) and log([N II]/H{alpha}) line ratios, 0.88 and
-0.09 respectively (Kewley et al. 2001), place it firmly in the Seyfert 2 region
of the BPT diagram. Gu et al. (2006) report an [O III] flux, F[O III] = 1614.0 *
10^-16^ erg s^-1^ cm^-2^ and an X-ray luminosity, log(L_2-10 keV_) = 42.89 erg
s^-1^.

3. 2009ApJ...690.1322W
Re:NGC 5506
NGC 5506. A full description of the X-ray history and properties of
NGC 5506 is found in Bianchi et al. (2003) where BeppoSax observations
are also presented (a strong reflection component is evident).

4. 2008A&A...484..341R
Re:NGC 5506
Figure A.7. For this edge-one irregular Seyfert 1 (S1i) galaxy, we show here the
first high resolution images at 8.6 and 11. 9 micron. The 8.6 micron image shows
an unresolved core while extended emission to the north-east is seen in the
micron image. The 11.9 micron flux measured, 908 mJy, is similar to the
Siebenmorgen et al. (2004) measurement of 1060 mJy.

5. 2007A&A...461.1209D
Re:NGC 5506
NGC 5506: BeppoSAX observed the source 3 times. Data were previously
published in Perola et al. (2002) and Bianchi et al. (2004). The best
fits proposed here are in agreement with what was presented by these
authors. As for IC 4329a, the source displays an almost steady broadband
spectrum that does not significantly change with the flux state (a
variation of ~3.5 in the 2-10 keV flux has been recorded between the 3
BeppoSAX observations of the target).

6. 2006ApJ...638..642B
Re:NGC 5506
NGC 5506 - The JEM-X and ISGRI spectrum of this Seyfert 1.9 (z = 0.006)
shows an absorbed (N_H_ = 2.7^+2.4^_-2.3_ x 10^22^ cm^-2^) high-energy
cutoff spectrum with GAMMA = 1.81^+0.25^_-0.28_ and E^cut^ = 57^+^139_-27_
keV (Chi^2^nu_ = 1.07; Fig. 7). No SPI data are available for this source,
because SPI was undergoing an annealing cycle during the observations of
NGC 5506. The results are consistent with BeppoSAX measurements (Bianchi
et al. 2003), although the iron Kalpha line and the reflection component
are not detectable in the INTEGRAL data.

7. 2005ApJ...633..105D
Re:NGC 5506
4.4. NGC 5506 - In hard X-rays (2-10 keV), NGC 5506 is one of the most luminous
local Seyfert galaxies (Matt et al. 2001), making it rather unusual amongst
type 2s. However, its X-ray properties are more consistent with those of
narrow-line Seyfert 1 galaxies, which, based on its J-band spectrum, NGC 5506
appears to be (Nagar et al. 2002). Our data tend to support this
classification. A detailed study of the kinematics of the double-peaked lines
by Maiolino et al. (1994) suggested that the object is a nearly edge-on
Seyfert. Their model, a refined version of that proposed by Wilson et al.
(1985), has the disk plane inclined by 75^deg^, above and below which ionized
gas is outflowing in cones extend with opening angle ~80^deg^. A highly
inclined geometry is consistent with the hard X-ray spectrum, for which the
lack of evidence for an accretion disk from the ionized component of the 6.4
keV iron line suggests that it must be nearly edge-on (Matt et al. 2001).
Maiolino et al. (1994) also argue that, based on the observed trends in
emission-line ratios, there is significant star formation occurring at
distances of 300-400 pc from the nucleus that can account for about half of the
H? emission. Our data confirm the evidence for active star formation close to
the AGN, showing symmetrical dips in the 1-0 S(1)/Br{gamma} ratio at offsets of
+/-2"-2.5" (250-300 pc) from the nucleus.

8. 2004MNRAS.350.1049G
Re:NGC 5506
9.21 NGC 5506 This is a heavily obscured nucleus, with colours of its
variable part much redder than average in J - H and H - K. A delay of
about 25 d between J and L may be present.

9. 2004A&A...422...65B
Re:NGC 5506
3.3.8 NGC 5506 The simultaneous BeppoSAX/XMM-Newton observation was
analyzed in detail by Matt et al. (2001) and Bianchi et al. (2003a). We
refer the reader to these papers for details on the best fit model for
this source, being one of those whose spectrum below 2.5 keV was
included in the analysis. We only recall, as already pointed out by the
above-mentioned authors, that the inclusion of two narrow lines at 6.68
and 6.97 keV significantly improves the quality of the fit. Moreover,
the neutral iron line and the Compton reflection are likely produced by
a Compton-thick torus, while the source is absorbed by a Compton-thin
material along the line of sight. The parameters listed in Table 2 refer
to this model.

10. 2003ApJS..146..353M
Re:NGC 5506
NGC 5506 (HI/LW)
This galaxy has too high an inclination for reliable classification,
although the dust lanes present to the south of the nucleus suggest a
dust spiral.

11. 2003ApJS..146..249B
Re:NGC 5506
5.15. NGC 5506
The maser in the edge-on Seyfert 1.9 galaxy NGC 5506 has been marked
by several flares which have lasted roughly a year, and then
disappeared. A flare near 1730 km s^-1^ was detected during 1993-1994
and a feature near 1800 km s^-1^ flared spectacularly through 1995.
The numbers in Figure 1 printed adjacent to the flaring features
indicate the peak intensity in janskys for the maser spike in cases
where the plots overlap. Velocity drifts of lines at 1731 and 1799
km s^-1^ are measured to be 0.36 +/- 0.71 and 0.00 +/- 0.29 km s^-1^
yr^-1^, respectively. The isolation and narrow profiles of these lines
inspire confidence that each originates from a single, persistent
feature rather than a blend. The GBT spectrum (Fig. 2) shows a group
of weak, narrow features centered near the systemic velocity of the
galaxy, 1824 km s^-1^.

12. 2003AJ....126.2237D
Re:NGC 5506
.
4.2. Seyfert Galaxies
.
NGC 5506 (F14106-0258) is also a nearby X-ray luminous Seyfert 2
galaxy with a small radio excess of u = 1.68. The radio source has
very low power [L_{nu}_(4.8 GHz) = 10^22.4^ W Hz-1] and is small with
an unresolved core and diffuse emission extending over ~500 pc (Thean
et al. 2000). The host is an Sa galaxy with a moderate FIR luminosity
of {nu}L_{nu}_(60 micron) = 10^10.2^L_solar_.

13. 2002A&A...389..802P
Re:NGC 5506
NGC 5506. The two observations here merged have an almost
identical average flux level, and when fitted individually
yield similar values of the spectral parameters. The BMS fit
with all three instruments gives an unacceptable
{CHI}^2^ = 180/117, due to an excess in the residuals well
below the strong photoelectric cut-off. Since the parameters
of interest do not crucially depend on how this excess is
modeled, we have chosen to present in Table 2 the results
obtained excluding the LECS. This NELG has a substantial
N_s_ = (3.7 +/- 0.2) x 10^22^ cm^-2^, and no signatures of
a warm absorber. The iron line is resolved and E_{alpha}_ is
marginally inconsistent with 6.4 keV. This line is likely a
blend of the two components recently revealed in a
simultaneous XMM-Newton (with EPIC) and BeppoSAX observation
(flux level similar to ours, Matt et al. 2001), one unresolved
at 6.4 keV, the other resolved ({sigma} about 0.25 keV) at
6.75 keV, the two with comparable intensities whose sum is
consistent with the one in our observation. Matt et al. (2001)
present arguments, centred on the interpretation of the iron
edge seen at 7.1 keV, that a substantial fraction of the RC
in this object is very likely associated with the narrow line
component. Evidence supporting this interpretation can be found
in a spectral variability investigation conducted with RossiXTE
by Lamer et al. (2000).

14. 2001ApJS..132..199S
Re:NGC 5506
4.2.16. NGC 5506
According to Braatz, Wilson, & Henkel (1996) this galaxy has an H_2_O
maser. The radio emission shows a linear structure along the east-west
direction, surrounded by diffuse emission, with a total extension of
300 pc. The VLBA image from Roy et al. (2000) shows a double radio source
along P.A. = 70^deg^, which will be used by Kinney et al. (2000). This
galaxy is almost edge-on, and the H I image (Gallimore et al. 1999) shows
absorption against the nuclear source. The hard X-ray spectrum has a flux
F_2-10 keV_ = 8.38 x 10^-11^ ergs cm^-2^ s^-1^ and is absorbed by a column
density N_H_ = 3.4 x 10^22^ cm^-2^ (Bassani et al. 1999). Maiolino et al.
(1994) detected double-peaked line profiles, which they interpreted as
outflow along P.A. = -16^deg^. Colbert et al. (1998) detected extended
soft X-ray emission along the same direction, P.A. = -20^deg^, which is
also coincident with the extended radio emission.

15. 2001A&A...368..797P
Re:NGC 5506
NGC 5506: The soft X-ray spectrum of the Seyfert galaxy NGC 5506 is highly
absorbed and no reliable spectral fit parameters can be obtained. Thus, we
have used for N_H_ = 1.0 x 10^21^ cm^-2^ as a lower limit in Table C.4.

16. 2000MNRAS.314..573T
Re:NGC 5506
NGC 5506: This edge-on galaxy has a compact core surrounded by a diffuse
halo. The 'loop' identified by Wehrle & Morris (1987) is just traceable
to the north-west of the core (see also Colbert et al. 1996).

17. 1999ApJ...526L...9P
Re:NGC 5506
This Seyfert 2 galaxy was studied by Kinney et al. (1999), who found
that the radio jet is extended along P.A. = 70^deg^, i = 82^deg^, and
{delta} = 21^deg^. According to Wang et al. (1999), the Fe K{alpha} line
of this galaxy can be fitted by an accretion disk with
i_disk_ = 40^+10^_-10_ degrees. From inspection of the HST image (Malkan
et al. 1998), we find that the south side is the nearer side, so the
jet is projected against the farthest side of the galaxy. Using equation
(3), we find that {beta} ~ 70^deg^.

18. 1999ApJ...524..684G
Re:NGC 5506
NGC 5506 is an X-ray bright Seyfert 2 galaxy (Wilson et al. 1976; Rubin
1978). H I absorption was originally reported by Thuan & Wadiak (1982).
The radio emission is dominated by a compact radio source, unresolved
at ~0.1" resolution (Wehrle & Morris 1987). A low surface brightness arc
extends ~0.5" north from the nucleus (Unger et al. 1986; Wehrle & Morris
1987), and faint emission extends ~30" from the nucleus (Colbert et al.
1996). The host galaxy is viewed nearly edge-on, and it seems likely
that most of the absorption arises in foreground disk gas.

19. 1999A&A...350....9O
Re:NGC 5506
3.4.2. NGC5506
This Seyfert 2 galaxy is the only AGN in our sample with detectable
Br13, Br14 hydrogen emission lines (see Fig. 2). The optical spectrum is
also characterized by prominent narrow lines over a relatively faint
continuum. The equivalent width of H{alpha} is ~400 A, i.e. among the
largest observed in Sy2's (e.g. Morris & Ward 1988) and comparable to
that found in young starburst galaxies whose spectra are dominated by
HII regions photoionized by massive O stars. However, the large strength
of high excitation lines ([NeV], [FeVII], HeII) argue for a non-stellar
ionizing continuum.
The IR continuum is dominated by emission from hot dust which
strongly dilutes the absorption features even at 1.6 microns (see
Fig. 2). The inferred mass to light ratio, although uncertain, is
compatible with a normal (old) stellar population.

20. 1997ApJ...477..631V
Re:NGC 5506
In Paper I, we argued against the presence of genuine broad Pa{beta}
emission in NGC 5506 based on the fact that the Pa{beta} profile is
continuous and has the same shape as the nearby [Fe II]{lambda}1.2567, a
forbidden line that cannot be produced in the high-density BLR. However,
the NLR profiles were found to become broader at longer wavelengths,
which suggests that the wing emission is highly reddened. We therefore
argued that the "broad" Pa{beta} line reported by Blanco et al. (1990)
and Rix et al. (1990) (and, more recently, by Ruiz et al. 1994)
corresponds to the strong, highly reddened emission in the wings of this
profile.
New spectra centered on Br{gamma} and Br{alpha} were obtained of
NGC 5506; they are shown in Figures 1j and 1k. The lower S/N and absence
of strong forbidden lines in these data prevent us from making strong
statements on the presence of BLR emission in Br{gamma} and Br{alpha}.
The profile of Br{gamma} is similar to that of Pa{beta} (Paper I): it
presents a narrow core superposed on a broad base. This profile is
affected by sky line residuals at 2.188 and 2.206 microns, and structure
in the underlying stellar continuum may also be responsible for the break
around 2.16 microns in the continuum of NGC 5506.
The line fluxes and widths listed in Tables 3 and 4 were derived by
fitting the sum of a Gaussian and a Lorentzian, both with the same FWHM
and the same peak strength. This profile was shown in Paper I to fit the
Pa{beta} profile very well; Br{gamma} and Br{alpha} are also well fitted
by this hybrid profile. The fluxes in the tables are significantly larger
than those obtained by Moorwood & Oliva (1988) and Kawara et al. (1988).
A similar result is found when comparing our Pa{beta} and [Fe II]
{lambda}1.2567 fluxes to those of Blanco et al. (1990) and Rix et al.
(1990). The origin of this discrepancy is unclear, but it may be due at
least in part to differences in the placement of the slit. All of our
spectra were centered on the infrared peak, while the slit was centered
on the optical peak in the other studies. In an edge-on galaxy like
NGC 5506, where the nucleus is undoubtedly obscured by dust in the galaxy
disk, the position of the optical nucleus can differ by a few arcseconds
from that of the infrared nucleus (see, e.g., Veilleux et al. 1994). This
may account for the discrepancy between our data and those obtained
through relatively small apertures (Blanco et al. 1990 and Rix et al.
1990) but has difficulties explaining the difference between our results
and those of Moorwood & Oliva (1988) and Kawara et al. (1989) who used
apertures of 6" x 6" and 10.3" x 20.7", respectively.
The color excesses derived from the fluxes in Tables 3 and 4 are
significantly larger than the value derived from the Balmer decrement.
There are relatively little variations in the colors excesses derived
from Pa{beta}, Br{gamma}, and Br{alpha}. Once again, this result
suggests that an unreddened source dominates the optical line emission in
NGC 5506, while the infrared line emission is produced in a stronger,
reddened source but not in what would be termed a BLR (see discussion in
Paper I).

21. 1997A&A...327..493R
Re:NGC 5506
NGC 5506 is an example of a galaxy where HI has also been detected in
absorption (Thuan & Wadiak 1982, Dickey 1982). Since the width of the HI
absorption line is only 48+/-15 km/sec, it is difficult to draw any conclusions
on whether this is due to internal motions of the gas clouds near the active
nucleus, or is originating from intervening clouds far from the active nuclei.
NGC 5506 is an edge-on galaxy.

22. 1996ApJS..105...75C
Re:NGC 5506
4.1.13. NGC 5506
Emission-line nebulae extend along the minor axis, ~5" (0.6 kpc) north and
south of the nuclear region (see Fig. 1k). Wilson et al. (1985) first noted
double-peaked [O III] {lambda}5007 and H{beta} emission lines in spectra of the
ELRs >~5" north and south of the nuclear region. Our spectra from these
positions (see Fig. 1k) also show double-peaked H{alpha}, [N II], and [S II]
emission lines. A "loop" of radio continuum emission extends to the north from
the nuclear region (Wehrle & Morris 1987; see also Paper II). These features
imply the presence of a minor axis wind which is blowing a shell of material
northward (and perhaps southward) from the nucleus. Thus, there is very good
evidence for a minor axis outflow in NGC 5506.

23. 1996ApJ...467..551C
Re:NGC 5506
3.1.16. NGC 5506
We show contour maps of the large-scale radio emission from NGC 5506 in Figure
1l. Diffuse, bubble-like radio structures extend out of the disk to radii ~30"
(3.6 kpc) from the nucleus in P.A. ~140^deg^. At higher resolution, the nuclear
source resolves into a compact core plus diffuse halo (Ulvestad, Wilson, &
Sramek 1981; Unger et al. 1986, 1987) extending in the same direction as the
large-scale "bubbles." Wehrle & Morris (1987) have mapped the small-scale radio
halo and have identified a "loop" of diameter ~100 pc that originates at the
compact source. They attribute this loop to either a bubble of hot plasma
rising from the nucleus or a magnetically dominated coronal arch.

24. 1995ApJ...447..121W
Re:NGC 5506
NGC 5506.-We measure an Fe K emission line and find evidence of
reflection. The upper limit on N_HFe_ is consistent with Gina (NP94).

25. 1991ApJ...381...85T
Re:NGC 5506
This highly absorbed Seyfert shows a spectral slope significantly flatter than
that observed by EXOSAT (Fig. 3), although the absorbing column shows no
evidence for variability. An IPC+MPC observation of this source claims an
excess characterized as a blackbody of temperature 10 eV. Such an excess is too
cool to show up in the SSS+MPC data. A HEAO 1 observation gave {GAMMA}=1.75,
suggesting that this source fluctuates between steep and flat states, although
there is no correlation between index and flux level in this source. Analysis
of EXOSAT data base observations of this source shows that the spectral index
also varied among the EXOSAT observations (time scales of weeks).

26. 1988A&AS...75..273D
Re:NGC 5506
NGC 5506 is a dusty edge-on irregular or early type spiral galaxy
first identified to the X-ray source 3U 1410-03 by Bahcall et al.
(1975). This identification is strengthened by the presence of a
Seyfert type 2 spectrum in the nucleus (Wilson et al., 1976). Its
X-ray emission is similar to that of Seyfert type 1 galaxies
(Mushotzky, 1982) with photoelectric absorption (Reichert et al.,
1985), and it is variable (Barr and Mushotzky, 1986). NGC 5506 has
also been detected in the UV (Bergeron et al., 1981). It is a compact
radio source (de Bruyn and Wilson, 1976, Ulvestad et al., 1981,
Ulvestad and Wilson, 1984b) with a diffuse radio halo a few arcseconds
in extent (Unger et al., 1986) and a peculiar radio loop to the
north-west (Wehrle and Morris, 1987). One or possibly two absorption
components have been detected in HI (Dickey, 1986), and NGC 5506 is
rich in CO (Sanders and Mirabel, 1985). It has a nearby companion,
NGC 5507, their velocity difference being 480 km s^-1^ (Dahari,
1985).
The optical properties of NGC 5506 have been discussed by several
authors. Wilson et al. (1976) stated that its morphology resembles
that of M82, while its spectrum reveals a number of high excitation
emission lines. Heckman et al. (1983) have shown that the line
profiles in NGC 5506 were unusual and composite, with at least three
components. Wilson et al. (1985, hereafter WBU85), have performed a
very detailed kinematic and profile analysis study of the ionized gas
around NGC 5506, both using narrow and broad band imaging techniques,
and high spectral resolution long slit spectroscopy. However, only
the strongest emission lines have until now been measured outside the
nucleus.
We find a nuclear redshift z = 0.0059 + 0.0002, corresponding to a
galactocentric velocity of 1718 km s^-1^ and to a distance of 34.4
Mpc.
We have observed ionized gas over 24" (4.0 kpc) along both the
east-west and north-south directions respectively (see Tab. XII and
Fig. 10), that is sizes somewhat larger than found by WBU85. We have
applied to all the optical data the correction factor of 5.1 (given by
Bergeron et al., 1981) needed for the nuclear optical spectrum to be
connected smoothly to the UV. Such a large correction was due to the
poor photometric conditions of the observations. The [OI] 6363 line is
indicated as blended to [FeX] 6374 in table XII, but as mentioned by
Penston et al. (1984) the contribution of [FeX] must be very weak.

27. 1988A&AS...75..273D
Re:NGC 5506
The reddening is large in NGC 5506, as this galaxy is seen close to
edge-on. Wilson et al. (1976) derived an extinction A_v_ = 1.9 mag,
corresponding to E(B-V) = 0.6, close to our estimate from the narrow
H{alpha}/H{beta} ratio. We have used the values of E(B-V) given in
table Xa to derive T_e_ and n_e_ although they are smaller than the
value of E(B-V) = 1.0 derived from the [SII] (4069 + 4076)/(6716 +
6731) ratio by Malkan (1983). The [OIII] line ratio then gives T_e_ =
14900 K in the nucleus, and T_e_ = 15300 K in region S (Tab. XIIa).
The relative line intensities measured in the nucleus of NGC 5506
agree within 25% with those previously measured by other authors
(Wilson et al., 1976, Shuder, 1980, Malkan, 1986, Morris and Ward,
1988).
The excitation level of the gas is higher in the nucleus than
further out, and as WBU85 we find a somewhat higher excitation of the
gas south of the nucleus. Some differenceS in the [NII] 6584/H{alpha}
ratios can also be observed between the different regions.
The problem of NGC 5506 being an obscured Seyfert 1 has been
discussed by several authors. Shuder (1980) first mentioned the
existence of a broad component in H{alpha}, but was contradicted by
Veron et al. (1980), who fitted narrow Voigt profiles to the lines and
found no residuals. The same result was later achieved by Whittle
(1985a and b), using high spectral resolution data. On the other hand,
BD86 have shown that the H{alpha} line did seem to show a broad
component, and that the overall far-UV to far-IR spectrum of NGC 5506
was typically that of an obscured type 1 Seyfert. The detection of the
OI 8446 line, originating in high optical depth gas, made by Morris
and Ward (1985), also favours an obscured broad line nucleus.
The velocity field of NGC 5506 has been thoroughly analyzed by
WBU85, who performed high spectral resolution long slit spectroscopy
of this galaxy with quite a number of slit positions. They found that
the ionized gas had a complex velocity field probably consisting of
normal rotation in a plane with a major axis close to the east-west
direction (which is the photometric axis of the galaxy), together with
a second component which they interpreted as due either to expansion
on the surface of a hollow or partially filled cone or to high
velocity clouds symmetrically disposed far out of the galaxy plane.
We have estimated the velocity field from the [OII] 3727 emission
line instead of [OIII] 5007, because the latter line is heavily
saturated in our data. Along PA = 271^deg^ the velocity amplitude is
at most 110 km s^-1^ and the velocity gradient is 25 km s^-1^ kpc^-1^
(Tab. XIIb). Along PA = 360^deg^, about the direction of the minor
axis as found by WBU85, we indeed observe a roughly constant velocity
in the central 14" (3 kpc) region, but further out on both sides there
are steep velocity gradients with a total velocity amplitude:
{delta}v = 500 km s^-1^. WBU85 also observe some differences between
the velocity ranges present for the [OIII] and Balmer lines; our
results derived from [OII] are similar to those they infer from
[OIII].

28. 1976RC2...C...0000d
Re:NGC 5506
= Holm 604a
= Kara[72] 419a
Pair with NGC 5507 at 4 arcmin

29. 1974UGCA..C...0000N
Re:UGCA 387
UGCA 387:
= NGC 5506
S..? (RC1)
disturbed?
paired with
UGCA 388 at 3.7, 020

30. 1964RC1...C...0000d
Re:NGC 5506
= Holm 604a
Non-interacting pair with NGC 5507 at 4 arcmin.
IC 0985 at 25 arcmin.

31. 1918PLicO..13....9C
Re:NGC 5506
A rather faint, irregular spiral 2' x 0.5' in p.a. 90^deg^; rather bright
stellar nucleus. Absorption lane down the middle. See Abs. Eff. 7 s.n.


Back to NED Home