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Notes for object UGC 01214

23 note(s) found in NED.


1. 2009ApJ...702.1127R
Re:MRK 0573
Mrk 573 is optically classified as a classical Sy2 nucleus (Tsvetanov & Walsh
1992), and Ramos Almeida et al. (2008) recently re-classify it as an obscured
NLSy1 galaxy, based on near-IR spectroscopy and X-ray archival data. The X-ray
observations of Mrk 573 do not straightforwardly reveal the intrinsic luminosity
of this AGN because it suffers from Compton thick obscuration (Guainazzi et al.
2005). The strong soft X-ray emission is likely photoionized line emission. It
is not the AGN continuum in any case, so previous simplified fits of power-law
models over a broad energy range (e.g., Guainazzi et al. 2005; Shu et al. 2007)
fail to accurately measure the AGN. We determine the intrinsic AGN luminosity
from the XMM-Newton observation of Mrk 573 with the pn detector, which offers a
high S/N. We use the reduced data and associated background and calibration
files from XAssist pipeline processing (Ptak & Griffiths 2003). We fit only the
data at energies greater than 3 keV, to avoid confusion from the separate soft
emission sources. The observed continuum is flat and the Fe K{alpha} line
equivalent width (EW) is large, which are characteristic of a purely reflected
(not direct) AGN continuum. We fix the photon index {GAMMA} = 0 and find EW =
2.0 +/- 0.7 keV. The results are similar if a typical AGN continuum slope is
adopted ({GAMMA} = 1.9). We follow the technique of Levenson et al. (2006),
using the Fe line luminosity and EW and to determine the intrinsic AGN
luminosity, finding L^AGN^_X_ = 2.2 * 10^43^ erg s^-1^ in the 2-10 keV bandpass.
We note that the fitted hard continuum directly corresponds to an intrinsic
luminosity that is a factor of 100 smaller.
The IR SED shape of Mrk 573 is practically the same as those of the rest of
Sy2 galaxies in the sample, so we consider it equivalent to the other Sy2. This
galaxy presents a strong symmetric double radio lobe (Nagar et al. 1999),
suggesting that it contains an edge-on torus; the radio lobes would be
asymmetric if the jets were out of the plane of the sky. The SED fit reproduces
all seven data points and also constrains the majority of the parameters. As for
the case of Circinus, we have introduced the inclination angle of the torus as a
Gaussian prior, centered in 85^deg^ with a width of 2^deg^. The
probability distribution of N_0_ present a Gaussian shape, with median value
N_0_ = 6 +/- ^5^_2_ (there is a tail toward large values that enlarges the
error). The {sigma} and q distributions allow us to establish upper limits of
{sigma} < 37{degree} and q < 1.4. The optical depth of each cloud shows a
Gaussian distribution with a median value of {tau}_V_ = 30+/-^10^_8_. The
optical extinction produced by this clumpy torus is A^LOS^_V_ = 185+/-^120^_75_
mag. Mrk 573 has the highest L^AGN^_bol_ of the Sy2 subset (4.3 * 10^44^ erg
s^-1^; Table 9), but due to the low values of N_0_ and {sigma} derived from its
fit, its reprocessing efficiency is low (~15%). The 10 {mu}m silicate feature
appears in shallow absorption in the median-fitted model ({tau}^app^_10 {mu}m_ =
0.44; see Table 8), producing an estimated value of the optical extinction
A^app^_V_ = 11 mag. The hydrogen column density obtained from the modeling along
the LOS (N^LOS^_H_ ~ 3 * 10^23^ cm^-2^) is much lower than the one that obscures
the X-ray emission (N^X-rays^_H_ > 1 * 10^24^ cm^-2^).

2. 2007AJ....134..648M
Re:UGC 01214
UGC 1214 (Figs. 7.72, 8.11, 9.72, 20.72): The nucleus is very bright and is
surrounded by a kiloparsec-scale symmetrical structure that seems to be an
ionization cone.

3. 2006A&A...457...61R
Re:Mrk 0573
Mrk 573. The CfA Seyfert 2 galaxy Mrk 573 (Huchra & Burg 1992) is a
well-studied AGN with two ionization cones seen in [O III] maps (Falcke
et al. 1998; Pogge & De Robertis 1995). It is also known for the bright
high-ionization emission lines displayed in its optical nuclear
spectrum (Durret 1994). Spectropolarimetric observations by Nagao et
al. (2004) show prominent scattered broad H{alpha} emission and
various narrow forbidden emission lines, the degree of polarization of
the latter ones correlated with the ionization potential of the
corresponding line. They interpret this correlation in terms of
obscuration of the stratified NLR by the optically and geometrically
thick dusty torus. The NIR spectrum of Mrk 573 presented in Fig. 1, is
very similar to that of NGC 591. The strong emission lines of [S III],
He I, and H I dominates the J-band. Also, strong high-ionization lines
were detected, including those of [S IX] 12 520 Angstrom, [Si X] 14 300
Angstrom, and [Ca VIII] 23 218 Angstrom. The line profiles are narrow,
with an FWHM typically of 400 km s^-1^. The most prominent stellar
absorption features are the Ca II triplet at the blue end and the 2.3
microns CO bandhead in K.

4. 2004A&A...415..941E
Re:MRK 0573
Mrk 573: Capetti et al. (1996), Alonso-Herrero et al. (1998). Laine et
al. (2002) suggested that this galaxy was triple-barred; however, the
largest of their three bars, identified via ellipse fits, is actually an
outer ring (e.g., Afanasiev et al. 1996). Outer-bar measurements are
from the J-band ellipse fits of Alonso-Herrero et al. (1998), with
inner-bar measurements from a NICMOS1 F160W image; L_bar_ for the inner
bar is from the nuclear ring.

5. 2003ApJS..148..327S
Re:Mrk 0573
5.2. Mrk 573
This is a Seyfert 2 galaxy known from ground-based images to have
extended [O III] emission (Haniff et al. 1988; Pogge et al. 1993,
1995) aligned with the radio triple source observed by Ulvestad &
Wilson (1984) and misaligned by 60^deg^ from the host galaxy major
axis. The HST images of this galaxy were studied in detail by SK96,
Capetti et al. (1996), Falcke et al. (1998), and Ferruit et al.
(1999). Figure 5 (top right) shows that the emission is composed of
several arches around the nucleus, with a total extent of 8.9"
(2980 pc) along P.A. = 120^deg^, and 3.7" (1250 pc) along the
perpendicular direction. A cone with opening angle of 75^deg^ can be
drawn on top of the [O III] emission.

6. 2003ApJS..146..353M
Re:MRK 0573
Mrk 573 (GD)
The grand-design, nuclear dust spiral in this Seyfert galaxy is
particularly striking as these dust lanes are lit up in emission where
they cross the ionization cone from the active nucleus. The inner part
of these spiral arms also appears to trace the leading edges of the
nuclear bar, as discussed by Quillen et al. (1999) and Martini et al.
(2001).

7. 2002AJ....124..675C
Re:UGC 01214
Seyfert 2, Mrk 573.

8. 2001ApJS..136...61S
Re:MRK 0573
5.3. Mrk 573 (=UGC 1214)
Mrk 573 is a Seyfert 2 galaxy showing strong high-ionization emission
lines (Koski 1978; Tsvetanov & Walsh 1992). No hard X-ray flux was detected
by Ginga for this galaxy (Smith & Done 1996). Veilleux et al. (1997) find
that the nuclear near-IR emission from Mrk 573 is dominated by stars, with
faint Br{gamma} and H_2_ 1-0 S(1) emission. Our spectrum shows similar
characteristics with a strong stellar contribution and lack of significant
diluting continuum. The bar within a bar shown, for example, in the K-band
image of Alonso-Herrero et al. (1998) (change from P.A. ~ 0^deg^-10^deg^ in
the outer to P.A. ~ 80^deg^-90^deg^ in the inner isophotes 4.5" from the
center) is also seen in our K-band image, but our field of view is too
small to see the larger-scale bar. Tsvetanov & Walsh (1992) find a
biconical radiation field roughly aligned with radio emission axis of
Mrk 573 found by Ulvestad & Wilson (1984a). Pogge & de Robertis (1995)
present high-quality line maps, which in [O III], for example, show clearly
a biconical shape. They also find two pairs of arclike emission line
features that enclose the nucleus. The innermost of them are within 2" of
the nucleus, which they interpret as bow shocks. Unfortunately, our line
maps are of insufficient signal-to-noise to reveal any possible biconical
emission in Br{gamma} or H_2_ 1-0 S(1).

9. 2001ApJ...562..139M
Re:MRK 0573
Mrk 573. - This is the best example of a double-barred galaxy in the
sample. The nuclear bar candidate previously noticed by Pogge & De Robertis
(1993) and Capetti et al. (1996) is readily apparent in the NIR surface
brightness. The dust lane morphology is similar to Mrk 471, where the dust
lanes trace the edge of the nuclear bar and then turn abruptly to cross the
nucleus perpendicular to the bar position angle as a straight dust lane.

10. 2000ApJ...544..747S
Re:MRK 0573
Markarian 573
H9 is filled by emission. The CR indicates the presence of a PL/YS
component contributing with ~20% in flux at 4020 A. The other two W values
and overall continuum are also well reproduced by this combination (Fig.
14d). The small discrepancy in the Ca II K line profile is explained as
for the radio galaxies above. HOBL are not detected.
Ne III {lambda}3968 + H{epsilon} emission completely dominates the
Ca II H + H {epsilon} absorption.

11. 1999ApJS..120..209N
Re:MRK 0573
Mrk 573 (type 2; Fig. 4) - The 3.6cm map shows both 20cm components
and a third close to the optical nucleus. The northwest and southeast
components are in P.A. 309^deg^ and 120^deg^ relative to the central
source, respectively. An overall radio P.A. of 125^deg^ is adopted, in
excellent agreement with earlier maps (Paper V; Kukula et al. 1995;
Falcke et al. 1998). Our measured fluxes at 3.6cm are similar to
previously measured 3.6cm fluxes of 0.78, 0.63, and 0.53 mJy for the
northwest, central, and southeast components, respectively (Kukula
et al. 1995). Falcke et al. (1998) use higher resolution and
sensitivity radio and HST images to investigate the detailed
correlations between the radio structure and the ionized gas in this
galaxy (see also Capetti et al. 1996). There is a confusing source ~9'
away. The P.A. of the major axis of the host galaxy has not been listed
in the RC3 or UGC catalogs, since both catalogs find the galaxy to be
almost circular. We have confirmed this using a deeper,
second-generation DSS image.

12. 1999AJ....117.2676R
Re:MRK 0573
The is a well-studied Seyfert 2 galaxy with two ionization cones
(Falcke, Wilson, & Simpson 1998; Pogge & De Robertis 1995). The color
map shows both blue color excess (light colors) and red color excess
(dark colors) regions. The region of the blue excess is delimited by two
cones, but there is interesting structure within the blue regions. Since
the position angle of the cones in our color map (123^deg^) agrees well
with the ground-based ionization cone position angle (124^deg^; Pogge &
De Robertis 1995) the ionization cone is the blue feature in our color
map. The excess emission in the F606W filter within the ionization cone
is likely due to H{alpha} emission included in the F606W filter
bandpass.
What is unusual about this galaxy is that the red absorption
features connect to the blue emission features. The strong red feature
to the south of the nucleus can be seen to directly connect to the very
blue feature 2" west of the nucleus. The weaker red dust lane to the
north of the nucleus connects to both a strong blue feature 0.75"
northwest of the nucleus and faintly to the strong ridge of blue
emission 2" east of the nucleus. The two fainter outer red features can
also be seen to connect to the blue feature. The red feature 3" to the
southeast of the nucleus connects to the outer blue ridge, which then
shows a faint connection to a red feature to the northeast of the
nucleus. The broad red feature just to the southeast of the nucleus
shows a faint connection to the broad blue feature east of the nucleus.
A possible reason for the connection between the features is that the
blue features are dust lanes illuminated from a central ionizing
source.
Given the connection between the two types of features we can see
that Markarian 573 has four symmetric spiral dust lanes. Each dust lane
traces about 180 degrees of arc as it spirals into the central region.
The two outer dust lanes seem to have a higher pitch angle since they
reach the same radius as the two inner arms over the same angular extent
even though they start at about twice the radius of the inner arms.

13. 1998MNRAS.297..579C
Re:MRK 0573
Mrk 573. Pogge & De Robertis (1993) found excess near-UV emission, spatially
extended along the [O III] emission, interpreted as scattered nuclear
continuum. Koski (1 978),estimated that the FC contributes 12 per cent of the
light at 5000 A, observed through a 2.7x4.0 arcsec^2^ aperture, while Kay (1994)
finds 20 per cent FC at 4400 A within an aperture of ~2x6 arcsec^2^. She also
estimated, based on spectropol,arimetry, that the FC is polarized by 5.6 per
cent in the 3200-6300 A range, in agreement with the values found by Martin et
al. (1983). The Ws (Fig. 11) show a mild gradient, from an S3 template at the
nucleus to a bluer one, S4, at 5 arcsec. The continuum ratios show a gradient
from an S3-S4 template at the nucleus to a bluer one, S5-S6, at 5 arcsec. Koski
(1978) and Kay's (1994) estimations of the FC contribution to the nuclear
spectrum are not confirmed by our data, which do not show any detectable
dilution in the Ws. This galaxy is another case in which the continuum ratios
outside the nucleus have values bluer than we would expect from the analysis of
Ws.

14. 1998ApJ...495..196A
Re:MRK 0573
3.5.2. Mrk 573
When fitting elliptical isophotes to the J- and K-band images, a remarkable
twist in the major axis of the isophotes is found at a radial distance of 4.5"
(see Fig. 4b), changing rapidly from P.A.~0^deg^-10^deg^ in the outer
isophotes to P.A.~80^deg^-90^deg^ in the inner isophotes. This is consistent
with the presence of a stellar bar extending over approximately 20" (9.8 kpc)
at P.A.=0^deg^ as also found in the HST 5500 A continuum image (Capetti et al.
1996). In addition to this large-scale bar, Pogge & DeRobertis (1995) find
evidence for the presence of an inner stellar bar in this galaxy, oriented
nearly east-west (P.A.~100^deg^), perpendicular to the large-scale bar. Our data
support this result, since the ellipticity increases steeply from the nucleus
out to radial distance r~2", while the P.A. remains approximately constant
(Fig. 4b). This galaxy therefore shows evidence for a "bar within bar"
situation.
Capetti et al. (1996) constructed an axisymmetric model from the HST 5500 A
continuum image and found a dust lane that spans 1" (500 pc) and is
significantly warped. The variation of the P.A. and ellipticity with radius
found by these authors compares well with our results; differences in the
ellipticity of approximately 0.1 are found in the inner 2". The HST [O III]
{lambda}5007 image (Schmitt & Kinney 1996) reveals emission extending 2" to the
northwest with a total opening angle of 70^deg^, whose substructure is
apparently dominated by the interaction of the radio jet with the ISM. The P.A.
of the 5" diameter ellipse at J, H, and K (Table 4) are all similar and
consistent with the orientation of the inner bar.

15. 1998AJ....116.2682C
Re:IRAS 01413+0205
UGC 01214, Mrk 573. Seyfert 2. Optical position from Clements (1981).
Ulvestad & Wilson (1984) resolved the 3" triple radio source at 4.86 GHz
with the VLA A configuration. The VLA D-configuration flux densities are
S = 16.1 +/- 1.1 mJy at 1.46 GHz and S = 7.1 +/- 0.4 mJy at 4.89 GHz
(Edelson 1987).

16. 1997ApJ...477..631V
Re:MRK 0573
Mrk 573 is a high-ionization Seyfert 2 galaxy which shows strong evidence
for a biconical radiation field (see, e.g., Tsvetanov & Walsh 1992; Pogge
& De Robertis 1993). The extended narrow-line emission of Mrk 573 is
roughly aligned with the axis of the triple source at radio wavelengths
(P.A. ~ 124^deg^; Ulvestad & Wilson 1984a). A BLR was tentatively
detected in the polarized light of Mrk 573 (Kay 1994). The Pa{beta}
profile (Fig. 2j) is very similar to that of [Fe II]{lambda}1.2567,
implying F(Pa{beta}_b_) < 5 x 10^-15^ ergs s^-1^ cm^-2^.
He I{lambda}1.27887 and {lambda}1.2528 are detected blueward of Pa{beta}
and [Fe II], respectively. The K-band spectrum of Mrk 573 (Fig. 2k) is
characterized by a strong stellar continuum and relatively faint emission
from Br{gamma} and H_2_{lambda}2.121. Both He I{lambda}2.058 and
H_2_{lambda}2.223 also appear to be present in the spectrum. The flux of
Br{gamma}_b_ is less than 1 x 10^-15^ ergs s^-1^ cm^-2^. A spectrum of
higher S/N will be needed to subtract accurately the underlying stellar
continuum from the spectrum of Mrk 573 and to put stronger constraints on
the contribution of Br{gamma}_b_.

17. 1996ApJ...463..498S
Re:MRK 0573
A18. MRK 573
The [O III] emission is extended along the same direction as the radio
emission (Haniff et al. 1988; Pogge & De Robertis 1995). This galaxy was
observed with a medium-band filter that included [O III]
{lambda}{lambda}4959, 5007 and H{beta}. H{beta} is responsible for 8% of the
total emission. The ground-based data show that this galaxy has an extended
biconical narrow-line region (Pogge & De Robertis 1993). The HST image
presented here shows the edge of the northwest cone detected by Pogge &
De Robertis (1995); the southeast cone lies outside the detector. The total
opening angle of the northwest cone is 70^deg^, and the emission in that
direction extends by 2" (670 pc). The cone's base extension is 1.8" (600 pc).
Note that this measurement includes the northwest blob.

18. 1995MNRAS.276.1262K
Re:MRK 0573
Markarian 573: Type 2. Host galaxy: lenticular (UGC). Radio:
unresolved by C-array, but the A-array map shows a triple source
with the central component coincident with the optical nucleus,
consistent with the 6-cm VLA image of Ulvestad & Wilson (1984a).
The flux ratio between the maps is ~5:3, indicating that there is
extended emission on intermediate scales which has been resolved
in the A-array image.

19. 1995AJ....110...87H
Re:IRAS 01413+0205
01413+0205 (Mkn 573) [Fig. 1(e)]: This galaxy reveals very interesting
structure on our H{alpha} images. We detect a faint ring of H{alpha}
emission which almost encircles the galaxy, similar to that detected on
digitally enhanced blue broadband optical images (paper II). Deeper
imaging by Pogge & De Robertis (1993) reveal that this ring is actually
two inner spiral arms that almost encircle the galaxy. In contrast to
optical broadband images, the H{alpha} emission extends along a bar-like
region, which is oriented at a position angle of roughly ~130^deg^. This
galaxy contains a compact triple radio source that is nearly symmetric
with the optical centre and extends ~1 kpc oriented at a position angle
of 124^deg^ (Ulvestad & Wilson 1984). Thus the H{alpha} bar appears to be
elongated along the radio axis, consistent with the results of Tsvetanov
and Walsh (1992).

20. 1994AJ....107...35H
Re:IRAS 01413+0205
01413+0205 (Mkn 573). The isophotes for this amorphous galaxy are
peculiar in the sense that the major axes of the ellipses in the central
regions are aligned in an east-west direction, while the major axes of
the outer isophotes appear to be aligned in a north-south direction
[Fig.15(e)]. Adjusting the contrast level so that the central portion of
the galaxy is visible uncovers bright condensations (presumably of star
formation) embedded in a ring that almost completely surrounds the
galaxy, which is clearly visible on a masked image [Fig. 4(c)] of the
galaxy. Mkn 573 is a relatively high ionization Seyfert 2 with narrow
emission-line profiles that are believed to have resulted from optically
thick emission-line clouds in high density regions (De Robertis &
Osterbrock 1986). It contains a compact triple radio source that extends
~1 kpc (Ulvestad & Wilson 1984), and is nearly symmetric with the optical
center.

21. 1994A&AS..108...61F
Re:IRAS 01413+0205
IRAS 0141+020 (Markarian 573). The Seyfert-like emission extends out to
3.4" on either side of the nucleus, including relatively strong [O I].
This emission has been examined by Afanasiev & Sil'chenko (1991) and by
Tsvetanov & Walsh (1992) from kinematic and ionization standpoints.

22. 1992MNRAS.256..589P
Re:E 0141+020
E0141+020, z= 0.02. This object is better known as Mkn 573, a Seyfert 2.
It is a very low-redshift USS AGN and the hard X-ray component is strong.
The permitted lines are very narrow: FWHM H{beta} = 300 km s^-1^ and FWHM
He I {lambda}5876 = 460 km s^-1^(De Robertis & Osterbrock 1986). Radio
maps of Mkn 573 at 6 cm (Olvestad & Wilson 1984) reveal a triple source
whose outer radio components are separated by 3 arcsec. The
[O III] {lambda}5007 line emission is aligned with the radio 6-cm
emission, but [O III] {lambda}5007 emission at the position of the outer
radio lobes is relatively weak (Haniff, Wilson & Ward 1988].

23. 1973UGC...C...0000N
Re:UGC 01214
Companion 4.9, 15, 0.5 x 0.3, diffuse


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