Date and Time of the Query: 2022-01-19 T03:58:16 PST
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Notes for object UGC 01032

9 note(s) found in NED.

1. 2002AJ....124..675C
Re:UGC 01032
Unusually warm FIR source: alpha(25,60) = 1.08.

2. 2001A&A...372..730V
Re:MRK 0359
Mark 359 (0124+18) is an NLS1 (Osterbrock & Pogge 1985). The FWHM of the
broad H{alpha} component is 780 km s^-1^; the forbidden lines are
exceptionally narrow (FWHM ~ 100 km s^-1^) (Veilleux 1991a). Discrepent
values have been published for R_4570_: 0.62 (Goodrich 1989) and <0.08
(Osterbrock & Pogge 1985). The coronal lines are very strong (Veilleux
1988; Erkens et al. 1997).

3. 1999ApJS..120..209N
Re:MRK 0359
Mrk 359 (type 1.5; Fig. 3) - The 20cm nuclear source sits on a
plateau of faint, possibly real emission. Gaussian deconvolution
suggests the nuclear source is extended in P.A. ~69^deg^, but the
source size is less than half the beam size. Gaussian deconvolution of
the 3.6cm source suggests that it is unresolved; however, the contours
show a faint extension in P.A. ~80^deg^, more or less consistent with
the P.A. in the 20cm map. We therefore list the source as "(S)" and
adopt an overall radio P.A. of 75^deg^. There is a strong (800 mJy at
20cm) double-lobed confusing source, IC 0115, some 10' away that is
difficult to clean out. Mrk 359 is a narrow-line Seyfert 1 (Veilleux

4. 1998AJ....116.2682C
Re:IRAS 01248+1855
UGC 01032, Mrk 359. Seyfert 1.5. Heavily resolved with the C

5. 1997A&A...319...52V
Re:MRK 0359
Mark 359(0124+18), an SB0 galaxy (Nuchra, 1977), was shown by Osterbrock &
Pogge (1985) and MacAlpine et al. (1985) to have line ratios rather similar to
those of a HII region. Davidson & Kinman (1978) and Veilleux (1991) were able
to separate the broad and narrow components of the lines; the line ratios of
the narrow line region are typical of Seyfert 2s.

6. 1996ApJS..102..309M
Re:MRK 0359
Both the [O III] and H{alpha} images show extension in this galaxy. The
excitation map follows the [O III] morphology, with elongation towards the
south. The color map indicates a blue excess, both on the nucleus and near the
ends of the galactic bar.

7. 1996A&A...305...53B
Re:MRK 0359
Mrk 359, 1E 0919+515, MRK 1044 (MCG -2-7-24), Mrk 42, Mrk 896, and MRK 493
These objects show some evidence for X-ray variability as well, but with a
comparatively slow rate of change (cf. Table 1 and Figs. 3-5). Mrk 359 has the
smallest broad-line widths of any known Seyfert 1 and its narrow lines are
also among the narrowest (Veilleux 1991). Veilleux (1991) argues that the
abnormally small width of the broad H{alpha} line is difficult to explain via
aspect effects alone and that there is probably a deficit of high velocity
line emitting gas in the center of Mrk 359. It was detected in X-rays during
the Einstein slew survey (Elvis et al. 1992) and it is unusual among the NLS1
in our sample since it has both a relatively flat spectral shape and a
relatively small Fe II/H{beta} ratio. 1E 0919+515 shows X-ray flux variations
by a factor of five on a time scale of about 1.5x10^6^ s. Mrk 1044 and Mrk 42
have been classified as NLS1 in Osterbrock & Pogge (1985).

8. 1973UGC...C...0000N
Re:UGC 01032
Main body 0.55 x 0.35, very bright elongated central region
Several galaxies near

9. 1971Afz.....7..299M
Re:MRK 0359
Almost spherical galaxy with a corona, which judging from the
spectrum, it should have a weak stellar nucleus.

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