Date and Time of the Query: 2019-06-16 T00:49:56 PDT
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Notes for object 2MASX J00215355-7910077

5 note(s) found in NED.

1. 2004MNRAS.353.1151S
Re:PGC 089877
F00198-7926. Has been studied as part of the H_2_0 maser emission survey
by Greenhill et al. (2002) as well as part of a study on compact radio
cores performed by Roy et al. (1994).

2. 2003MNRAS.343..585F
Re:IRAS 00198-7926
00198-7926. This source is a double-nucleus system with a large tail,
with a Sy2 optical spectrum. The second nucleus is probably a large
region of extranuclear unobscured star formation, and there are a number
of H II regions embedded in the tail (Heisler & Vader 1994). A deep
Bepposax observation gave no detection, giving an upper limit to the
X-ray flux of F_2-10_ < 1 x 10^-13^ erg cm^-2^ s^-1^ (Risaliti et
al. 2000). From our results, the properties of this object mark it as
unusual. We find that the IR emission from this object is mostly
starburst in origin. The starburst is comparatively old, and can thus
account for both the submillimetre emission and all of the unobscured
star formation observed by Heisler & Vader (1994). We interpret the
'warm' infrared colour of this object as being due to the old starburst
rather than an AGN. There is, however, comparatively little IR data
available for this object and the resulting AGN upper limit is weak. The
best-fitting model, shown in Fig. 1, includes an AGN component.

3. 2001MNRAS.327..459L
Re:IRAS 00198-7926
0019-7926: As noted in Section 2.5, both de Grijp et al. (1992) and
Vader et al. (1993) present spectra of this object showing clearer
Seyfert characteristics. From the data in Vader et al. we estimate that
W_{lambda}5007_ ~ 200 A, and the intrinsic line luminosity is ~6 times
larger than that reported here. This would move 0019-7926 in Fig. 8 from
the non-HBLR region into the HBLR one. We therefore suspect that new
spectropolarimetric observations may detect an HBLR in this system. If
true, this would increase the distinction between the HBLRs and non-HBLRs
in terms of L_{lambda}5007_, but would not significantly change our other

4. 2000A&A...357...13R
Re:IRAS 00198-7926
IRAS 00198-7926: The source IRAS 00198-7926 was observed by the BeppoSAX
instruments for ~ 20000 seconds and was not detected. From this
non-detection we estimate an upper limit to the 2-10 keV flux,
F_2-10_ > 1 x 10^-13^ erg cm^-2^ s^-1^.

5. 1994AJ....107...35H
Re:IRAS 00198-7926
00198-7926. A large tail with an almost 90^deg^ bend, extends to the
northwest of the main body of this very peculiar galaxy. A contour plot
suggests that either a second nucleus or a large extranuclear region of
star formation is present [Fig. 15(a)]. A masked B image, and a B-R color
map reveal many knots which are presumably H II regions embedded in the
tails of this galaxy.

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