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Date and Time of the Query: 2019-08-19 T16:02:19 PDT
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Notes for object MRK 0034

4 note(s) found in NED.


1. 2005A&A...436...75H
Re:Mrk 0034
3.2 Mrk 34
Mrk 34 (IRAS 10309+6017), another luminous (~10^11^ L_sun_) FIR source,
is a distant Seyfert 2 galaxy (z=0.0505, D ~200 Mpc; Falcke et al.
1998). The optical galaxy is characterized as having an inclination
angle of 57^deg^ in Whittle (1992), although a second generation Digital
Sky Survey (DSS) image shows the galaxy to be compact, with poorly
defined outer isophotes (Nagar & Wilson 1999). The radio emission has an
extended structure (~2.5"; Ulvestad & Wilson 1984), and strong evidence
for an interaction between the radio jet and NLR clouds has been found
by Falcke et al. (1998).
.
Mrk 34 is one of the most distant and most luminous H_2_O megamasers
ever detected. The maser shows two or three distinct spectral features
(Figs. 3 and 4). One is centered at a velocity of ~14 840 km s^-1^,
another at ~15 770 km s^-1^, and a third one is tentatively seen at
~14 665 km s^-1^. Peak flux densities are up to 10 mJy and total
isotropic luminosities are ~1000 L_sun_.

2. 1999ApJ...516...97N
Re:Mrk 0034
Mrk 34: This galaxy is not listed in the RC3 and UGC catalogs.
Garnier et al. (1996) find the galaxy to have a diameter of
0.63' x 0.44' in B. A second generation DSS image shows the galaxy is
compact, with ill-defined outer isophotes.

3. 1993ApJ...419..553B
Re:MRK 0034
Mrk34
High-resolution VLA observations of the Seyfert 2 galaxy Mrk 34 reveal
a double radio source with separation 2.4"(2.2 kpc) along P.A. 158^deg^
(Ulvestad & Wilson 1984a). Our WSRT 6 cm observations of this source were
plagued by interference. The final image (Fig. 5, 3.9" x 5.8") shows that
the nuclear source is extended along P.A. 140^deg^ (the minor axis of the
host galaxy). This image also shows a second component with a flux
density of 2.5 mJy about 5" to the northwest at P.A. ~60^deg^ (30^deg^
from the galaxy major axis). It is not clear what the secondary component
might be. It did not appear in the earlier VLA image of Ulvestad & Wilson
(1984a). If real, it may therefore be time variable. If the component is
real and is time variable, it might be a radio hypernova. However, its
radio luminosity would then be roughly a factor 10 greater than the most
radio luminous supernova known (e.g., Weiler, Panagia, & Sramek 1990) and
roughly three orders of magnitude brighter than typical supernovae.
However, there were known problems with the radio observations, thus the
reality of this feature is questionable. Due to the uncertain nature of
the radio imaging results for Mrk 34, we do not include it in the
statistical investigations.

4. 1967Afz.....3...55M
Re:MRK 0034
= MCG +10-15-104
Spectral Type: ds1e
Has a faint corona.
H{alpha}, (N_1, N_2, H{beta}) and {lambda}3727 in emission.


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