Date and Time of the Query: 2019-06-19 T08:45:10 PDT
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Notes for object UGC 08850

15 note(s) found in NED.

1. 2008A&A...484..341R
Re:MRK 0463
The image of this double-nuclei Seyfert 2 galaxy shows an unresolved core at
11.9 micron, measuring 338 mJy.

2. 2007A&A...461.1209D
Re:MRK 0463
MARK 463: The MECS field containing MARK 463 is populated by 3 other
sources, one of which (PG 1352+183) is brighter than MARK 463 (Landi &
Bassani 2001).

3. 2004AJ....128..969D
Re:IRAS F13536+1836
F13536+1836: No radio data. Object from sample of Condon et al. (1995).

4. 2004A&A...418..465L
Re:MRK 0463
Mrk 463 has a very strong mid-IR AGN continuum but the relatively lowest
absorption corrected hard X-ray emission compared to the average
relation. The X-ray column may be underestimated.

5. 2003AJ....126.2237D
Re:Mrk 0463
4.2. Seyfert Galaxies
Mrk 463 (F13536+1836) contains two nuclei that are separated by ~5.9
kpc and embedded in a common envelope (Mazzarella & Boroson 1993).
Both nuclei have Seyfert 2 optical spectra (Shuder & Osterbrock 1981),
though the eastern nucleus, Mrk 463E, has a Seyfert 1 nucleus observed
in polarized light (Veilleux, Sanders, & Kim 1997). Both nuclei are
radio sources. Mrk 463E has a luminous steep-spectrum core and weak
radio lobes with extent ~27 kpc (Mazzarella et al. 1991). Mazzarella
et al. (1991) suggest Mrk 463E may be a transition object between the
smaller, weaker radio sources seen in Seyfert galaxies and extended
powerful radio galaxies. At high resolution the core is found to be a
compact double with extent ~1.8 kpc (Thean et al. 2000). Mrk 463W has
a weaker radio source with a flatter spectrum (Mazzarella et al.
1991). Overall, Mrk 463 appears in our sample as a moderately powerful
radio source [L_{nu}_(4.8 GHz) = 10^24.1^ W Hz-1] with high FIR
luminosity [{nu}L_{nu}_(60 micron) = 10^11.5^L_solar_] and an
intermediate radio excess (u = 1.30).

6. 2001ApJS..136...61S
Re:MRK 0463
5.26. Mrk 463 (=UGC 8850)
Mrk 463 consists of two nuclei, Mrk 463W and E, separated by about 4"
(Adams 1977, see also our K-band image). Without distinguishing between
the two nuclei, Lutz, Veilleux, & Genzel (1999) use newly developed
mid-infrared tools to classify Mrk 463 as an AGN. Indeed, Mrk 463E is
classified by most authors as a Seyfert 2 (e.g., Schuder & Osterbrock
1981; Hutchings & Neff 1989) and shows in HST direct imaging what was
initially described as a 0.84" long optical jet directed toward the south
of the nucleus (Uomoto et al. 1993). The Seyfert 2 nucleus appears as a
Seyfert 1 in reflected polarized light (Miller & Goodrich 1990), and more
recent HST imaging polarimetry has revealed that the "optical jet" is in
fact a cone of polarized light extending northward from the Seyfert 1
nucleus (Tremonti et al. 1996). In addition, the eastern component is seen
to have broad Pa{alpha} emission (Veilleux et al. 1999, consistent with
our data which include only the red side of the line). Mrk 463W, on the
other hand, is classified as either a Seyfert 2 (Schuder & Osterbrock 1981;
Mazzarella et al. 1991) or as a LINER (Blanco 1991). Although there are
arguments in favor of other classifications, we adopt the Seyfert 2
classification for both nuclei. The unresolved nuclei seen in our K-band
data have been shown to be unresolved at higher spatial resolution
(Mazzarella et al. 1991).

7. 2001ApJS..133..269L
Re:MRK 0463
5.9. Mrk 463
Mrk 463 has two nuclei, and one of them, Mrk 463 E, has been observed
to have broad optical lines in polarized light (Miller & Goodrich 1990).
The three-component model of a scattered power law and thermal emission
fits Mrk 463. Thermal emission accounts for 31% of the soft X-rays. The
theoretical PSF of the PSPC does not fit Mrk 463 well, suggesting that the
X-ray emission is extended on scales of 48 kpc, but the observed radial
profile is also consistent with a point source.

8. 2001A&A...368...64V
Re:MRK 0463
13. Mrk 463 The Arecibo detection of Mrk 463 (Hutchings et al. 1987)
at 0.2 Jy km s^-1^ is at the 4{sigma} level, with a peak flux density
of 1.6 mJy; the authors note that the profile was detected in both
observing runs. Heckman et al. (1978) note that their Green Bank flux
measurement is relatively uncertain, 6.0 +/- 2.3 Jy km s^-1^, and that it
would imply a very high M_HI_/L_B_ ratio for Mrk 463 if all gas detected
resides in this galaxy. The reported Green Bank flux is 30 times higher
than the Arecibo value, and the central velocities of these detections seem
incompatible: 14702 and 15230 km s^-1^, respectively
({DELTA}V = 528 km s^-1^), for a W_20_ profile width of 200 km s^-1^ measured
at Arecibo. Inside the Green Bank HPBW but well outside the Arecibo beam, the
DSS shows only one other galaxy that might be a source of confusion in the
Green Bank H I spectrum: CGCG 103-016, 6.1' to the SE of the target galaxy,
a B_T_ 15.5 object of 0.4' diameter and unknown redshift. If it were the sole
source of H I emission within the Green Bank beam, it would have an M_HI_/L_B_
ratio of 1.4 M_sun_/L_sun,B_, which is about 4 times the mean ratio for an Sc
spiral (Roberts & Haynes 1994), but not unheard of for late-type galaxies. The
morphology of CGCG 103-016 is hard to discern, however, as a relatively
bright star is situated close to its centre. In conclusion, CGCG 103-016
may be the cause of the discrepant Green Bank flux. For the total H I mass,
we used the Arecibo detection by Hutchings et al. (1987).

9. 2000MNRAS.314..573T
Re:MRK 0463
Markarian 463 (UGC 8850): Three aligned north-south radio components are
detected in this well-studied double-nucleus galaxy. North-south radio
structures have previously been observed from VLBI scales
(Hummel et al. 1982; Kukula et al. 1999) to up to 18 kpc south of the
nucleus (Mazzarella et al. 1991). The new observations match the 6-cm
radio structure observed by Mazzarella et al., with the exception of the
weak central radio component which appears to coincide with a bright knot
in the aligned optical jet (Uomoto et al. 1993). This is the second most
radio-luminous Seyfert in the extended 12-mm sample.

10. 2000AJ....120..604S
Re:Mrk 0463
Mrk 463.-The eastern nucleus is distinctly elongated north-south,
and the western nucleus is elongated east-west exactly as expected from
the WFPC2 images of Paper I. Nearly all of the U' emission in the
eastern nucleus comes from the position of the northern "knot" and not
the southern infrared "nucleus" (Surace & Sanders 1999), which is
consistent with its interpretation as an AGN ionization feature.
Although the eastern nucleus is physically smaller and hence has a
higher peak surface brightness, it is the western nucleus that dominates
in overall luminosity at U'. All of the "knots" identified in the tidal
ring structure are extremely luminous at U'. Their colors indicate ages
less than 10 Myr.

11. 1998ApJ...492..116S
Re:MRK 0463
Mrk 463=UGC 8850.--The eastern nucleus is optically classified as a Seyfert 1
galaxy (Miller & Goodrich 1990). A radio luminosity density, aligned radio
structures, and optical/near-infrared colors that have been interpreted by
Mazzarella et al. (1991) as representative of a dusty QSO are associated with
this nucleus. An optical "jet" seen by Uomoto et al. (1993) resembles in our
data an X-shaped structure dominated by a central peak. Tremonti et al. (1996)
report that the bright object to its north is highly polarized and reflects a
hidden Seyfert 1 nucleus lying in this X-structure. This is confirmed by
high-resolution near-infrared observations (Surace et al. 1997) that indicate
that the near-infrared luminosity is centered on the X. The entire eastern
nucleus lies on a plateau of extended emission in which there are several
bright knots. The western nucleus is optically classified as a Seyfert 2. There
seem to be two principal components to the western nucleus: a dominant source
that is distinctly elongated in the E-W direction and a more compact, very blue
source 1" to its west. Two arcs of star-forming knots to the north and south of
the two dominant components of the western nucleus are also in this region.
Both of these arcs form a sharp edge to a fan of emission centered on the
dominant nuclear components.

12. 1994AJ....107...35H
Re:IRAS 13536+1836
13536+1836 (Mkn 463). This well-studied double-nucleus galaxy (e.g.,
Kollatschny & Fricke 1984, Hutchings & Neff 1988, Neff & Ulvestad 1988,
Mazzarella et al. 1991) has three low surface brightness tails as
revealed by deep exposure CCD images. The optical nuclei are separated by
approximately 4 arcsec corresponding to ~4 kpc. Each nucleus has optical
emission lines typical of Seyfert type 2 galaxies, but when viewed in
polarized light this galaxy has the spectrum of a Seyfert 1 (Miller &
Goodrich 1987). A two-color map uncovers many bright knots, arcs, and
dust patches. This galaxy has a double radio source separated by 1.3" at
6 cm (Ulvestad & Wilson 1984).

13. 1993ApJS...86....5K
Re:UGC 08850
UGC 8850 (Mrk 463); Seyfert 2.
Extensive observations of this double nucleus galaxy in the optical,
near-IR, and radio (Mazzarella et al. 1991) and in polarized light
(Miller & Goodrich 1990), and studies of its featureless continuum in UV
+ optical and of its hydrogen lines (Kinney et al. 1991a), suggest that
Mrk 463E is probably a dust-obscured Seyfert 1 nucleus. The presence of a
large amount of dust surrounding Mrk 463E is also confirmed by the strong
far-infrared luminosity of the galaxy [log (L_FIR_/L_sun_) = 11.77;
Sanders et al. 1988]. The nature of Mrk 463W is ambiguous; it could be
either a Seyfert 2 nucleus or a powerful starburst.
The extended radio emission and the far-infrared luminosity may be
enhanced by the merging process (Mazzarella et al. 1991), as manifested
by the tidal tails and by the existence of a small difference in the
recession velocity of the two nuclei ({delta}v ~ 50 km s^-1^; Hutchings &
Neff 1987). The two nuclei are separated by 3 kpc and are both included
in the IUE slit.

14. 1992A&A...265..429A
Re:Mrk 0463
Sanders et al. (1988a) found CO emission at 15,300 km s^-1^ using the
NRAO 12-m. Reobserving with the IBM telescope, Sanders et al. (1989a)
give a revised redshift velocity of 15,250 km s^-1^ and a FWHM of 292 km
s^-1^.The latter paper also notes that Mrk 463 has a double nucleus and
that the diameter of its host galaxy is 40". The highest accuracy claimed
for an optical velocity is 15,032+/-9 km s^-1^ from [OIII] (E nucleus) by
Whittle (1985). It is based on 40 km s^-1^ resolution data. Other careful
studies of this object include that of Hutchings & Neff (1989). They find
15,205 km s^-1^ for [O III] from the E nucleus, and 15,235 km s^-1^ from
the W. They also note that the narrow H{beta} line is ~100 km s^-1^ lower
in velocity at both nuclei. The CfA Redshift Catalog value is
15,149 km s^-1^. H I 21 cm radiation has been detected by Hutchings et
al. (1987) who find a central velocity of 15,230 km s^-1^ with a full
width at 20% intensity (FW20) of 200 km s^-1^. The CO emission extends
approximately from 15,000 km s^-1^ to 15,530 km s^-1^, similar to the
H I. Whittle's velocity is near the blue limit of this range.

15. 1973UGC...C...0000N
Re:UGC 08850
Main body 0.45 x 0.25 with diffuse streamer southwestwards

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