Date and Time of the Query: 2019-08-18 T07:51:54 PDT
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Notes for object IC 0450

17 note(s) found in NED.

1. 2009ApJ...690.1322W
Re:MRK 0006
MrK 6. This source is known to have a complex absorber, with ASCA and XMM-Newton
spectra well modeled by a double partial covering model (Feldmeier et al. 1999;
Immler et al. 2003). Due to its complex nature, we only include our XRT analysis
with a simple model, for easy comparison with the other sources.

2. 2009ApJ...690.1322W
Re:MRK 0006
Mrk 6. The residuals to this fit show clear evidence of an Fe K{alpha}
line ({DELTA}{chi}^2^ = 10.7). Adding a gaussian for this component, we
find E = 6.41^+0.07^ _-0.06_ keV, {sigma} = 0.09^+0.10^ _-0.05_ keV, and
EW= 498^+264^ _-250_ eV.

3. 2007AJ....134..648M
Re:MRK 0006
Mrk 6 (Figs. 7.1, 9.1, 20.1): This object is a Sy1.5 galaxy with a very bright
saturated core and some surrounding extended emission.

4. 2007A&A...461.1209D
Re:MRK 0006
MARK 6: Malizia et al. (2003) modeled the broad band X-ray spectra of
the source using a complex absorber. This scenario is not required,
excluding the LECS data. Here a reflection component is preferred,
although marginally detected with a significance of ~97%.

5. 2003ApJS..148..327S
Re:Mrk 0006
5.22. Mrk 6
Ground-based observations of this Seyfert 1 galaxy (Haniff et al.
1988) showed only an unresolved nuclear source. Our observations
(Fig. 8, middle right) show [O III] emission extended by 3.2" (1150
pc) along P.A. = -10^deg^, a direction similar to that of the
extended radio emission observed by Schmitt et al. 2001b. The
emission is concentrated at the nucleus, with a series of blobs
around it and a finger of emission extending for 0.5" toward P.A. =
210^deg^. The largest blob is located 0.7" north of the nucleus and
is probably related to the emission detected in the radio. Another
small blob is observed at 0.5" NW of the nucleus and is possibly
related to the beginning of a transverse radio structure observed by
Kukula et al. (1996) and Schmitt et al. 2001b.

6. 2002AJ....124..675C
Re:UGC 03547
Unusually warm FIR source: alpha(25,60) = 0.62. Seyfert 1.5.

7. 2001ApJS..132..199S
Re:MRK 0006
4.2.5. Mrk 6
The radio image of this galaxy presents an intricate morphology, with a
linear double structure along the north-south direction (P.A. = -3^deg^)
and a low surface density structure, similar to a ring, approximately
perpendicular to the jet. This ring structure has been previously detected
by Baum et al. (1993), Kukula et al. (1996), and Xu et al. (1997).
Baum et al. (1993) also detected radio lobes extending up to 40 from the
nucleus. The jet is extended by 440 pc, while the ringlike structure is
extended by ~1800 pc. Neutral hydrogen mapping of the nuclear region by
Gallimore et al. (1999) shows H I absorption against the northern part of
the jet, possibly due to a dust lane crossing north of the nucleus.
Kukula et al. (1996) compared MERLIN high-resolution radio observations and
[O III] {lambda}5007 A images of this galaxy, showing that they are
misaligned. They suggest that this misalignment is due in part to a
projection effect, where the jet is emitted at an angle relative to the
galaxy disk and the gas emission comes from ionized gas in the disk of the

8. 2000MNRAS.314..573T
Re:MRK 0006
Markarian 6 (UGC 3547): This source contains a central, well-collimated
radio structure. On larger scales, features suggestive of shells or
bubbles are seen at varying position angles (Baum et al. 1993; Kukula
et al. 1996).

9. 1999ApJS..120..209N
Re:MRK 0006
Mrk 6 (type 1.5; Fig. 8) - The central source in the 20cm map is
extended in P.A. 177^deg^, in agreement with the P.A. found in Paper
V. The larger scale structure in the 20cm map (listed as "Extended" in
Table 2) has P.A. ~75^deg^, in agreement with the P.A. ~87^deg^
observed by Baum et al. (1993). At 3.6cm, the source is a triple with a
roughly north-south axis. The weak southernmost extension is labeled
"Southwest" in Table 2. Higher resolution radio maps are published in
Kukula et al. (1996).

10. 1999ApJ...524..684G
Re:Mrk 0006
Mrk 6 is a Seyfert 1.5 galaxy. H I absorption was originally reported
by Heckman, Balick, & Sullivan (1978) and Baan & Haschick (1983), whose
detections we confirm. We have reported a more detailed follow-up MERLIN
observation (Gallimore et al. 1998). The nuclear radio source,
marginally resolved by the present observation, collimates into a 1"
(360 pc) radio jet (Kukula et al. 1996). H I absorption is detected
against the northernmost radio component of the 1" nuclear jet. The
offset absorption appears to arise from a 100 pc-scale arm or dust lane
crossing just north of the AGN. The AGN itself may be partially absorbed
by the dust lane, which may lend to its classification as a Seyfert 1.5.
Otherwise, there are no radio candidates for the AGN. Recent ASCA
spectroscopy suggests a high emission measure to the nucleus, so the
radio nucleus may be free-free absorbed (Feldmeier et al. 1999).

11. 1998AJ....116.2682C
Re:IRAS 06457+7429
IC 450, UGC 03547, Mrk 6. Seyfert 1.5. Optical position from Klemola
et al. (1987). WSRT 4874 MHz image with 3.5" resolution in Baum et al.

12. 1994AJ....107...35H
Re:IRAS 06457+7429
06457+7429 (Mkn 6). This well-known galaxy was not observed by us, but
it has been discussed by others (e.g., Neff & Ulvestad 1988). It is a
strong double radio source with components separated by ~1" (570 pc) at
6 cm (Ulvestad et al. 1981).

13. 1993ApJ...419..553B
Re:MRK 0006
Mrk6 (UG6 03547, IC 450)
Early high-resolution observations showed the inner structure of the
Seyfert 1.5 galaxy Mrk 6 to be a simple double with a separation of ~1"
(~360 Pc) at P.C. ~177^deg^ (Ulvestad, Wilson, & Sramek 1981; Ulvestad &
Wilson 1984a; Unger et al. 1986). Previous low-resolution 21 cm WSRT
observations detected structure on the scale of ~30" but could not image
the details of the emission (de Bruyn & Wilson 1976). Our WSRT 6 cm image
(Fig. 4, 3.5" x 3.6" resolution) shows structure on the scale of ~5" at
P.A. ~87^deg^ and larger scale structure with total extent ~38" (~14 kpc)
at P.A. ~30^deg^ which is roughly perpendicular to the major axis of the
galaxy. The emission is diffuse on both sides of the nucleus. The
northern "lobe" shows a "center-darkened" or "edge-brightened" morphology
which suggests a `bubble-like" structure. A bipolar optical emission line
nebula extends out to 22 kpc from the galaxy nucleus and is aligned with
the central radio source (Meaburn, Whitehead, & Pedlar 1989).

14. 1984AnTok..192.595T
Re:KUG 0645+744
Sd/dm according to UGC.

15. 1976RC2...C...0000d
Re:IC 0450
= MRK 0006
Type 2 Seyfert.
Pair with IC 0451 at 6.5 arcmin
Photometry: (UBV)
Ap. J., 171, 5, 1972.
Ap. J., 159, 405, 1970.
Ap. J. (Letters), 164, L109, 1971.
Ap. J. (Letters), 171, L35, 1972.
Ap. J. (Letters), 172, L101, 1972.
Ast. Tsirk. No. 591, 1970.
Astrofizika, 7, 389, 1971.
Astrofizika, 8, 187, 1972.
Astrofizika, 9, 39, 1973.
Astrofizika, 9, 139, 1973.
Ap. J., 171, 5, 1972.
Radio Observations:
Ast. Tsirk. No. 715, 1972.
Ap. J., 191, 633, 1974.

16. 1967Afz.....3...55M
Re:MRK 0006
= IC 0450
= MCG +12-07-018
Spectral Type: s1e
Has a faint corona.
Mainly red in appearance.
Emission in H{alpha}, (N_1, N_2, H{beta}), H{zeta}
and {lambda}3727

17. 1964RC1...C...0000d
Re:IC 0450
IC 0451 at 6.5 arcmin north-following.

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