NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-08-20 T21:57:27 PDT
Help | Comment | NED Home

Notes for object NGC 0262

21 note(s) found in NED.


1. 2006A&A...457...61R
Re:NGC 0262
NGC 262. This CfA galaxy hosts a Sy 2 nucleus with strong emission
lines. In polarized light, it presents a broad H{alpha} component (
FWHM=8400 km s^-1^) and an underlying featureless continuum (Miller &
Goodrich 1990). A hard X-ray detection (Awaki et al. 1991) supports the
idea that NGC 262 harbors an obscured Seyfert 1 nucleus. The J-band
spectroscopy of Veilleux et al. (1997) reports the presence of a faint
blue-wing emission with FWHM approx 900-1600 km s^-1^ in Pa{beta} and
He I 10818 Angstrom, which is not seen in the forbidden lines. The NIR
spectrum of this source has been studied in separated works (Veilleux
et al. 1997; Imanishi & Alonso-Herrero 2004; Sosa-Brito et al. 2001),
but the one presented here is the first one covering the JHK-bands
simultaneously. We find that the NIR continuum emission is essentially
flat. A rich emission line spectrum was detected with strong forbidden
lines of [S III] and [Fe II], as well as [C I] 9850 Angstrom and [P II]
11 886 Angstrom. High ionization lines such as [Si VI] 19 630 Angstrom,
[S VIII] 9912 Angstrom and [Si X] 14300 Angstrom, are also present. No
evidence of broad components or wings are found either in Br{gamma}
(FWHM=520 km s^-1^) or Pa{beta} (FHWM=400 k)m s^-1^. We attribute the
blue wing reported by Veilleux et al. (1997) in Pa{beta}to [Fe II] 12
788 Angstrom, which contaminates the blue profile of the former. For
comparison, [S III] displays an FWHM of 560 km s^-1^. Faint absorption
lines, mainly in the H-band, were detected.

2. 2005A&A...442..137N
Re:UGC 00499
UGC 499 (NGC 262), also known as Markarian 348, is a well-known Seyfert 2 galaxy
(Koski 1978). We detect H I emission out to distances of 100 kpc from the
center, but it is clearly distorted and does not rotate regularly around the
center.

3. 2004MNRAS.352..112B
Re:TXS 0046+316
3.1.2 0046+316 This radio source is classified as a type 2 Seyfert
galaxy (NGC 262) at z= 0.015 (1 mas ~= 0.30 pc). On the larger scale,
the multi-element radio-linked interferometer network (MERLIN)
interferometer detects a bright core and two symmetrically placed
components at about 130 mas from the central core in roughly the
north-south direction (e.g. Unger et al. 1984; Augusto, Wilkinson &
Browne 1998). The southernmost MERLIN component is polarized at a level
of 5 per cent (Anton et al. 2002). Our VLBA image shows that the radio
core is resolved in the north-south direction and, even if it cannot be
properly imaged, there is some weak and diffuse emission all the way
from the core to the position of the components detected by MERLIN. No
significant polarized flux is detected in the VLBA observation.

4. 2003ApJS..148..327S
Re:Mrk 0348
5.1. Mrk 348
This is a Seyfert 2 galaxy with polarized broad emission lines
(Tran 1995). The HST [O III] and H{alpha} + [N II] images were
studied by Capetti et al. (1996) and Falcke et al. (1998). The
[O III] emission (Fig. 5, top left) is extended by 2.85" (840 pc)
along P.A. = 185^deg^, with a blob of emission at approximately 0.9"
south of the nucleus. Along the perpendicular direction the emission
is extended by 1.75" (510 pc). Close to the nucleus, the emission is
extended along P.A. ~ -10^deg^, which is similar to the direction of
the radio emission observed by Ulvestad et al. (1999). It is possible
to draw a cone with opening angle 60^deg^ on top of the extended
[O III] emission.

5. 2001ApJS..136...61S
Re:MRK 0348
5.1. Mrk 348 (=NGC 262 = UGC 499)
This galaxy hosts a Seyfert 2 nucleus with strong emission lines and
underlying featureless continuum in the optical (Koski 1978). The host
galaxy is an early-type spiral galaxy which is oriented nearly face-on
and has a nearby companion galaxy, NGC 266 (Heckman et al. 1982;
Simkin et al. 1987). A broad H{alpha} component has been found in
polarized light with a FWHM of 8400 km s^-1^ (Miller & Goodrich 1990).
Veilleux, Goodrich, & Hill (1997) do not find broad Br{gamma} in their
IR spectrum but find a Br{gamma} profile broader than that of
H_2_ 1-0 S(1). Our K-band spectrum superficially agrees with theirs,
although the lower S/N of our spectrum does not permit more conclusive
comparisons. A hard X-ray detection (Awaki et al. 1991) gives
N_H_ = 1.1 +/- 0.2 x 10^23^ cm^-2^ and supports the idea that Mrk 348
harbors an obscured Seyfert 1 nucleus. Neff & de Bruyn (1983) report
that its nuclear radio source consists of a compact core plus two knots
aligned along position angle 168^deg^, with a total size of about 0.15".
They also report variation at 6 and 21 cm on timescales of months. A
high-resolution HST image published by Capetti et al. (1996b) shows a
linear structure of narrowband [O III] {lambda}5007 emission extended
0.45" at a position angle of ~155^deg^.

6. 2000ApJ...544..747S
Re:MRK 0348
Markarian 348
CR is 0.72 for this galaxy, thus indicating the presence of a PL/YS
component contributing with 30% in flux at 4020 A and in approximate
agreement with the W values. Figure 14c also shows that the overall
spectrum is well reproduced by this combination, taking into account that
there is some emission in H9 and probably also in H10, making it impossible
to detect the HOBL in absorption, if any. Ne III {lambda}3968 + H {epsilon}
emission completely dominates the Ca II H + H{epsilon} absorption.

7. 1999ApJS..120..209N
Re:MRK 0348
Mrk 348 (type 2; Fig. 2) - Gaussian deconvolution suggests that the
bright core of the source is unresolved in both the 3.6 and 20cm maps.
There appear to be faint extensions to the north-northeast and
south-southwest at 20cm. Our measured fluxes of 238 and 302 mJy at 3.6
and 20cm, respectively, are low compared with some previous
measurements; earlier observations of this source (Paper V) gave fluxes
of 480 and 565 mJy at 6 and 2 cm, respectively. VLBI observations of
the source (Neff & de Bruyn 1983) reveal a triple structure in P.A.
170^deg^. The radio source structure is therefore classified as "L."
The P.A. of the major axis of the galaxy is not listed in RC3 or UGC.
Heckman et al. (1982) mapped the H I in this galaxy and derived P.A.
~0^deg^ for the outer H I ring. A deeper H I map (Simkin et al. 1987)
reveals a complex kinematic structure (their Fig. 3) in which the
kinematic major axis appears to be along P.A. 170^deg^ Falcke et al.
(1998) and Capetti et al. (1996) have used high-resolution radio and
optical images to investigate the detailed correlation of radio
structure and ionized gas in this galaxy.

8. 1999ApJ...524..684G
Re:MRK 0348
Mrk 348 (NGC 262) is a Seyfert 2 galaxy that is unusual in two
respects. First, it has a very large H I disk grown perhaps by a tidal
encounter with a neighboring spiral (Heckman et al. 1982; Simkin et al.
1987). Second, there is evidence for a hidden BLR in this source (e.g.,
Miller & Goodrich 1990. Although the nucleus hosts a very bright
subarcsecond radio triple (e.g., Neff & de Bruyn 1983), we detect no H I
absorption in this experiment. Halkides, Ulvestad, & Roy (1997) report
evidence for free-free absorption below 6 cm wavelength, but it is
unclear which components of the radio triple might be absorbed. (This
result is consistent with the spectral decomposition of Neff & de Bruyn
1983). The lack of H I absorption from the medium obscuring the BLR
might again be ascribed to free-free suppression of the nuclear radio
continuum source at 21 cm wavelength.

9. 1998MNRAS.299.1159A
Re:TXS 0046+316
B0046+316: The source is identified with a Seyfert II galaxy at
z = 0015. It was observed and mapped partly as a quality control for
comparison with the map presented by Unger et al. (1984) - their
Fig. 1(c). Both maps (and the model in Table 3) show a bright compact
central component flanked by weaker, more extended components. The
overall extent of ~ 300 mas corresponds to ~ 90 pc and hence we classify
it as a low-luminosity CSO with a bright core.

10. 1998MNRAS.297..579C
Re:MRK 0348
Mrk 348. This is a Seyfert 2 galaxy with evidence of broad H{alpah} (De Robertis
& Osterbrock 1986b), He I 10830-A and Pa{beta} lines (Ruiz, Rieke & Schmidt
1994). Koski (1978) observed this galaxy through a 2.7x4 arcsec^2^
aperture. obtaining a 14 per cent contribution from an FC at 5000A. Kay (1994)
estimated an FC contribution of 35 per cent to the flux at 4400 A, while Tran
(1995a) found 27 per cent at 5500 A. Mrk 348 is one of the Seyfert 2 galaxies
that had a hidden Seyfert 1 nucleus revealed by spectropolarimetry (Miller &
Goodrich 1990).
The Ws and continuum ratios of this galaxy are shown in Fig. 10. The Ws have
values similar to those of an S4 template, without any noticeable gradient in
the inner 8 arcsec. From the results of Koski (1978), Kay(1994) and Tran(1995a),
we would expect the Ws to be substantially diluted in the nuclear region, but
this is not detected. One possibility would be that the FC is extended,
diluting all the Ws. However, the narrow-line region of this galaxy is extended
by less than 2 arcsec (Schmitt & Kinney 1996), and the FC would have to be
extended by ~8 arcsec.
The continuum ratios show a gradient, having values similar to those of an S4
template at the nucleus and becoming bluer farther out, reaching values similar
to those of S5-S6 templates. The continuum behaviour of Mrk 348 is intriguing,
due to the fact that outside the nucleus it indicates bluer templates than those
expected from the analysis of the Ws. This behaviour is also seen in many other
objects in the present sample, particularly Seyfert 2s.

11. 1998ApJ...495..196A
Re:MRK 0348
3.5.1. Mrk 348
The near-IR and optical properties of the Seyfert 2 galaxy Mrk 348 have been
extensively discussed by Simpson et al. (1996). To summarize, after subtracting
a model for the surface brightness of the galactic bulge, they found a red
linear structure (interpreted as an edge-on disk) in the near-IR continuum
which runs approximately 2" (800 pc) east-west and is unresolved in the
north-south direction. An HST [O III] {lambda}5007 image (Capetti et al. 1996)
shows that the central emission is confined to a linear structure 0.45" in
size, with P.A.=155^deg^, while on a larger scale, the [O III] {lambda}5007/
H{alpha}+[N II] emission is extended over several arcseconds and shows a
biconical morphology with axis at P.A.~170^deg^ (Simpson et al. 1996; Mulchaey,
Wilson, & Tsvetanov 1996). Capetti et al.'s (1996) optical continuum image
reveals obscuration across the nuclear region with a scale of less than 50 pc.
The resolution of our images is not good enough to determine whether this
obscuration is associated with the elongated red feature seen in the near-IR
images.
In Figure 4a we show the ellipticity and major axis P.A. as a function of the
semimajor axis of the fitted ellipse in the J band. The P.A. of the 5" scale
isophote in the J-, H-, and K-band images is close to 90^deg^ (consistent with
the orientation of the elongated red feature found by Simpson et al. 1996).
However, the fitted P.A. should be taken with caution because of the low values
of the ellipticity. Within a region of size equal to or smaller than 3" (1.3
kpc), 90% of the L'-band emission appears to be unresolved.

12. 1997ApJS..108..155G
Re:NGC 0262
This S2 nucleus is in an S0 host galaxy. It shows circumnuclear emission
in the form of a faint ring of unresolved H II regions at 2.3 kpc from
the nucleus.

13. 1997ApJ...477..631V
Re:MRK 0348
MRK 348 = NGC 262
Mrk 348 is a Seyfert 2 galaxy that exhibits very broad H{alpha} in
polarized light (FWHM = 8400 km s^-1^; Miller & Goodrich 1990; Tran
1995a). The existence of this broad H{alpha} emission was first suspected
by De Robertis & Osterbrock (1986). Ruiz et al. (1994) recently reported
the detection of faint blue-wing emission with FWHM ~ 900 - 1600 km s^-1^
in the profiles of He I{lambda}1.083 and Pa{beta}. Our J-band spectrum
confirms the presence of this excess of emission in the blue wing of
Pa{beta} (Fig. 2e). This excess emission is not visible in
[Fe II]{lambda}1.2567 or fourth-order [S III]{lambda}0.9532.
Unfortunately, it is not clear whether this excess emission corresponds
to broad Pa{beta} emission or represents contamination by
He I{lambda}1.27887. The K-band spectrum does not clarify the situation
(Fig 2f). The profile of Br{gamma} appears broader at the base than that
of H_2_{lambda}2.121, but structure in the K-band continuum prevents
us from making a firm statement. A two-Gaussian decomposition of the
Pa{beta} and Br{gamma} profiles provides upper limits to the broad-line
flux in this galaxy: F(Pa{beta}_b_) <~ 1 x 10^-14^ ergs s^-1^ cm^-2^,
F(Br{gamma}_b_) <~ 7 x 10^-16^ ergs s^-1^ cm^-2^, FWHM(Pa{beta}_b_)
~ 1,850 km s^-1^, and FWHM(Br{gamma}_b_ ~ 2500 km s^-1^. Data of
higher S/N will be needed to better assess the importance and origin of
this excess emission.

14. 1996ApJS..102..309M
Re:MRK 0348
Mrk 348 is a well-studied, luminous Seyfert 2. Although the host galaxy has
been classified as a SA0/a, our H{alpha} images reveal faint spiral arms (not
visible on the scales shown in Figure 6), suggesting Sa might be a more
appropriate classification. Spectropolarimetry has revealed a hidden BLR in
this object (Miller and Goodrich 1990). Further evidence of an obscured
Seyfert 1 nucleus includes the detection of a hard x-ray continuum with
photoelectric absorption corresponding to a column of
N_H_ = 1.1+/-0.2x10^23^ cm^-2^ (Awaki et al. 1991).
This galaxy has previously been imaged in the lines of [O III] and H{alpha} by
Tran (1995) and our results are consistent with his. Both the [O III] and
H{alpha} emission are extended in Mrk 348, although the nuclear emission-line
gas does not display the linear or conical morphology common to many other
Seyfert 2's. Instead, the gas has a "halo"-like morphology. The H{alpha}
emission extends on larger scales than the [O III] gas and develops a knotty
morphology beyond the [O III] emission. This morphology is suggestive of a
partial ring of HII regions. The excitation map reveals peaks in high
excitation gas on either side of the nucleus in the north-south direction.
Thus, the high excitation gas is somewhat bi-conical in morphology despite the
overall halo morphology of the [O III] gas. The elongation of the high
excitation gas is along a similar direction to that of the linear radio
structure(PA_2 cm_ ~ 168^deg^; Ulvestad & Wilson 1984). There is also evidence
for a slight blue excess coincident with the southern excitation peak, which
could represent scattered nuclear continuum emission as similar blue features
are seen along the radio axis in a few other Seyfert 2's (Pogge & De Robertis
1993).

15. 1996ApJ...463..498S
Re:MRK 0348
A15. MRK 348
This galaxy was observed with a medium-band filter that includes both [O III]
{lambda}{lambda}4959, 5007 and H{beta}. H{beta} contributes to 8.5% of the
total emission in the image. The [O III] emission is composed of two blobs
separated by 0.15" (45 pc) along PA 150^deg^, with the nucleus close to the
northern component and the total extent of the emission being 0.6" (180 pc)
along this direction. There is also some faint emission at 0.9" (270 pc) south
of the nucleus, but it does not appear to be correlated with the nuclear
emission. Assuming that the southern emission has a conical shape, the opening
angle is measured to be 60^deg^. The cone's base extension is 0.4" (120 pc).

16. 1993ApJS...86....5K
Re:NGC 0262
NGC 262 (Mrk 348); S0, Seyfert 2.
The short-wavelength spectrum of Mrk 348 is flat (F_{lambda}_ is
proportional to {lambda}^0^) with strong emission lines. This Seyfert 2
nucleus resides in a face-on early-type (Sa) spiral, which has a
companion, NGC 266 (Garcia-Vargas et al. 1989). Mrk 348 has been shown
by Miller & Goodrich( 1990) to have broad Seyfert 1 type emission lines
in polarized flux, with a FWHM for H{alpha} of 7400 km s^-1^. IUE data on
Mrk 348 were first reported by Ferland & Osterbrock (1986), who found a
value of {alpha} = -0.9 for the UV spectral index, which is within the
errors of the Kinney et al. (1991a) value of {alpha} = -1.4 +/- 0.5
(F_{nu} is proportional to {nu}^-1.4+/-.5^). Kinney et al. (1991a)
found that the number of recombination photons is larger than predicted
from the number of ionizing photons, implying that the photoionizing
continuum is obscured. Thus, Mrk 348 displays evidence of harboring a
Seyfert 1 galaxy with broad H{alpha} emission lines and with some of the
ultraviolet continuum flux blocked from our line of sight.

17. 1993ApJ...419..553B
Re:MRK 0348
Mrk 348 (UGC 00499; NGC 0262)
Mrk 348 is a Seyfert 2 and is an early-type disk galaxy (S0/a or Sa)
(Huchra 1980; Adams 1977). Heckman et al. (1982) present WSRT 21 cm line
imaging of the large (175 x 115 kpc) atomic hydrogen halo surrounding
this galaxy. This large H I halo may have been produced by the
interaction of Mrk 348 with its companion NGC 266 (Heckman et al. 1982;
Simkin et al. 1987). Both the morphology and axial ratio of the optical
disk and the kinematics of the H disk suggest that the galaxy is seen
within 20^deg^ of face-on. Miller & Goodrich (1990) have shown that the
very intense narrow H{alpha} line in Mrk 348 has broad polarized wings
suggesting that Mrk 348 contains a hidden broad line region.
Neff & de Bruyn (1983) present VLBI 21 cm continuum image of the
compact radio core showing a linear triple source with projected length
of about ~0.2" (56 pc) at position angle (P.A.) 170^deg^. MERLIN
observations of the component are presented by Unger et al. (1984). Neff
& de Bruyn also present extensive radio observations of the variability
of the compact radio source. They suggest that the VLBI morphology, high-
amplitude variability, and inverted spectrum of the compact radio source
are most consistent with an AGN rather than a starburst origin for the
compact radio source.
Our 6 cm WSRT image (Fig. 1, full resolution 3,5 x 6,8 resolution)
shows the radio structure after the central 50 pc radio source is
subtracted out. We find extended radio emission straddling the central
source at P.A.~13^deg^ with a total extent of ~18" (5 kpc) This emission
was resolved out in the VLA A-configuration observations of Ulvestad &
Wilson (1984a). The extended emission is confirmed by our tapered image
(not shown, resolution 6.1" x 11.5"). This is in agreement with the 21 cm
WSRT image of Neff& de Bruyn (1983) which shows emission extended ~20"
(5.6 kpc) to the southwest of the core at P.A. ~210^deg^.

18. 1993AJ....106.1405P
Re:NGC 0262
NGC 262 (Mrk 348). This is a tidally distorted galaxy (Simkin et al.
1987) with a strong Seyfert 2 nucleus (e.g., Koski 1978). Our images of
this interacting galaxy show long, faint spiral arms that appear to be
tidally stretched toward its east companion. This galaxy may once have
been S0, but its tidal peculiarity lead us to eject it from the sample on
the grounds of highly anomalous morphology.

19. 1976RC2...C...0000d
Re:NGC 0262
= MRK 0348
Type 2 Seyfert galaxy.
Spectrum and Photograph:
Ap. J., 192, 581, 1974.
Radio Observations: (variability)
Ap. J. (Letters), 191, L13, 1974.
P.A.S.P., 86, 649, 1974.

20. 1973UGC...C...0000N
Re:UGC 00499
(R)?
Companions 1.1, 326, 0.3 x 0.1; and 1.2, 86, 0.5 x 0.25

21. 1971Afz.....7..299M
Re:MRK 0348
Spherical with a corona.
Red on the whole; the data refer to the nucleus.
H{alpha} and (N_1 + N_2 + H{beta}) are observed in the spectrum.


Back to NED Home