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Date and Time of the Query: 2019-08-20 T06:40:55 PDT
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Notes for object UGC 03374

11 note(s) found in NED.


1. 2003ApJS..148..327S
Re:MCG +08-11-011
5.19. MCG +08-11-011
Previous HST images obtained with WF/PC1 did not show any extended
[O III] emission (Bower et al. 1994; SK96) which was probably due to
the strong spherical aberration of the pre-COSTAR images. Radio
images from Schmitt et al. 2001b show 3.6 cm emission extended for
3.5" along the N-S direction. Closer to the nucleus Ulvestad & Wilson
(1986) showed that the radio structure consists of a triple source
extended by ~1" along P.A. = 127^deg^. The top left panel of Figure 8
presents the [O III] image of this Seyfert 1 galaxy. We can see that
most of the emission is extended close to the N-S direction, along
P.A. = 20^deg^, aligned with the large-scale radio emission. The
total extent of the emission in this direction is 3.6" (1450 pc) and
3" (1210 pc) along the perpendicular direction. South of the nucleus
we see a CCD defect which could not be removed from the data, but
which also does not influence the results. A large portion of the
emission is concentrated at the nucleus with a second blob of
emission located at 0.7" north of it. Closer to the nucleus, we see
two blobs of emission, one to each side of it, separated by ~1" along
P.A. = 130^deg^. These structures may be related to the nuclear
triple radio source detected by Ulvestad & Wilson (1986).

2. 2002AJ....124..675C
Re:UGC 03374
Seyfert 1.5. Unusually warm FIR source: alpha(25,60) =0.50.

3. 2002A&A...389..802P
Re:MCG +08-11-011
MCG 8-11-11. This observation was published by
Perola et al. (2000), to which we refer for the
choice of neglecting in the fit the LECS counts
below 0.4 keV. N_s_ is negligible compared to
N_g_, the warm absorber N_W_=(6^+9^_-6_) x 10^20^
has cm^-2^ with X_i_ ~ 7 erg cm s^-1^. The iron
line is not resolved, the upper limit on its width
is comparable to that of the lines resolved in our
sample.

4. 2001ApJS..132..199S
Re:MCG +08-11-011
4.2.20. MCG +8-11-11
The first radio observations of this galaxy were done by Wilson &
Willis (1981), using the VLA at 6 cm, which showed a strong nuclear source
and some extended emission in the north-south direction. Ulvestad & Wilson
(1986) presented a VLA image at 2 cm, showing a triple radio source,
extended by ~1" along P.A. = 127^deg^. Our radio image at 3.6 cm shows a
central component extended along P.A. = 128^deg^, surrounded by diffuse
emission along the north-south direction, with a total extent of 1230 pc.
This structure is similar to the one observed by Ulvestad & Wilson (1986)
at 6 cm. The HST [O III] and H{alpha} images of this galaxy show no
evidence of extended emission (Bower et al. 1994; Schmitt & Kinney 1996).

5. 2001ApJ...550..261W
Re:MCG +08-11-011
3.3.2. MCG +8-11-11
Between the two observations of MCG +8-11-11 (taken less than 3 days
apart), no change is observed in the 2-10 keV flux, line energy, or line
flux (Fig. 8b). The low EW reported for the 1995 September 3 observation
is a result of a large absorption correction. When we measure the EW
without correcting for this absorption, we find a value of 306 +/- 84 eV,
which is consistent with that obtained for the other observation.

6. 1999ApJS..125..409C
Re:UGC 03374
UGC 03374. - The BOPOS position is not of the nucleus.

7. 1999ApJ...516...97N
Re:MCG +08-11-011
MCG 8-11-11: RC3 and UGC list major axis P.A. = 90 ^deg^. UGC lists a
diameter of 2.82' x 2.51' in B. A second generation DSS image shows the
galaxy to be near circular at a diameter of about 2'.

8. 1997A&A...327..493R
Re:MCG +08-11-011
MCG 8-11-11 was detected in HI emission with a FWZI line width of 450 km/sec.
This compares well with the 500 km/sec CO FWZI, given that both detections are
at 3{sigma} level. There is also agreement in the profiles of the two emission
lines.

9. 1996ApJ...463..498S
Re:UGC 03374
A20. UGC 3374
This galaxy was observed through a medium-band filter that had the same
transmittance for [O III] {lambda}{lambda}4959, 5007 and H{beta} Using the flux
values of Whittle (1992), we can calculate that the H{beta} emission is
responsible for 28% of the total emission in the image. The deconvolution of
this galaxy images contained residuals, so that subtraction of the continuum
from the emission-line image was impossible. The emission in this object is
pointlike, with the bulk of the emission having a maximum, extent of 0.4"
(160 pc). As Bower et al. (1994) have already pointed out, there is no
emission related to the radio lobes observed by Ulvestad & Wilson (1986). See
Bower et al. (1994) for more details on the WF/PC images of this galaxy.

10. 1995ApJ...447..121W
Re:MCG +08-11-011
MCG 8-11-11.-We detect an Fe K line in this Seyfert 1 galaxy at 97%
significance. There was a marginal detection of an Fe K line with EXOSAT
(Leighly, Pounds, & Turner 1989).

11. 1973UGC...C...0000N
Re:UGC 03374
Bright stellar nuclear region in diffuse bar


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