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Date and Time of the Query: 2019-05-20 T13:08:19 PDT
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Notes for object NGC 3934

4 note(s) found in NED.


1. 2000A&AS..141..385V
Re:NGC 3934
C-38 = NGC 3934. (A,E,G,N) Already recognized as a PRG by Schweizer et
al. (1983); CCD images (PRC) show a structure resembling two crossed
discs in the inner regions, as well as extensive shells in the outer
region. The galaxy was observed at Nancay as the Effelsberg profile is
much stronger (15.9 vs. 5.7 Jy km s^-1^) and wider ({DELTA}V_20_ 317 vs.
91 km s^-1^) than measured at Green Bank; also, the Green Bank spectrum
shows only one peak, while the Effelsberg data show two. The Nancay
spectrum shows 3 peaks, centered at about 3610, 3775 and 3805 km s^-1^;
at Green Bank only the middle peak was detected, while at Effelsberg
both the middle and the lowest-velocity peak were seen. The Green Bank
observations may well be unreliable, however, as they were plagued by
solar interference, affecting the baseline. Published Arecibo detections
(see Table 3) indicate detections of the middle peak only (V=3740
km s^-1^ and {DELTA}V_20 = 290 km s^-1^, I=4.4 Jy km s^-1^). The peaks at
3610 and 3775 km s^-1^ may well be due to confusion by 14.3 mag NGC 3933,
located 2.7' W and 2.6' S of the PRC object, on the edge of the Nancay
beam but well inside the other beams. H I spectra of NGC 3933 (see
Huchtmeier & Richter 1989) show a systemic velocity of about 3731
km s^-1^ and a {DELTA}V_20_ width of 355 km s^-1^, measured with the 1.9'
radius Arecibo beam, and thus in principle free of confusion by C-38 at
a distance of 3.7', unless it has an H I size much larger than its
optical dimensions, about 1' diameter. The question remains why the
narrow peak at 3805 km s^-1^ was observed only at Nancay; no other
galaxies were found within the Nancay search area, and only one
catalogued object of unknown redshift (16 mag UGC 6835) was found at the
edge of the Effelsberg beam, 6.2' from C-38.

2. 1997MNRAS.284..773G
Re:NGC 3934
3.9 NGC 3934
NGC 3934 has an X-shaped structure; the large-scale images published in the PRC
indicate a dark ring running approximately NW-SE. The presence of shells in
deeper images and a blend between many different structures indicates the
possibility of a past merger, instead of an independent ring that is inclined
with respect to the plane of the galaxy. There is one companion, NGC 3433, at
the same redshift (and having a similar magnitude and size) about 4 arcmin
(~57 kpc) away.
We have detected CO at all five observed positions; the interior X-shaped
structure is included in all the pointings because of the small size of the
galaxy on the sky. Two ranges of velocities are apparent from the data: a large
peak at about 3450 km s^-1^, which is more evident at (13 arcsec, -15 arcsec)
(on the dark ring), and a similar peak at about 3800 km s^-1^, which is
stronger to the south-west (along the presumed major axis of the stellar body).
The other side of the ring, which is smoother in the optical images, shows
fainter CO emission. We deduce that the gas motions are quite complex, but we
do not have the spatial resolution to interpret the data unambiguously. The
multiple peaks in the CO data are reminiscent of the NGC 3690 + IC 694 system
(Solomon & Sage 1988), which consists of two interacting galaxies. Although the
CO spectra do not agree - at first glance - with the H I spectrum reported by
RSS, there is some evidence in the latter spectrum for the features seen here.
In particular, note the strong dip in the H I spectrum at ~3600 km s^-1^, which
is quite evident in the CO data. There may also be H I emission extending down
to ~3400 km s^-1^, as is evident in the CO spectra; a different base-lining of
the H I data might bring such a feature to more prominence.
The molecular hydrogen mass was determined assuming an effective beam area of
1.25 arcmin^2^. If the CO peaks at about 3500 and 3800 km s^-1^ arise from gas
within the ring, then ~80 per cent of the molecular gas resides there. The
narrow H I line could then suggest that atomic gas dominates within the galaxy,
with the molecular material in the ring.

3. 1994AJ....107...99R
Re:NGC 3934
C-38 = NGC 3934 = UGC 6841. The GB 140' sees 3.3 x 10^9^ M_sun_ of HI.
The baseline was affected by solar interference. NED lists three other
galaxies within 15'; two are small and quite faint, but the third,
NGC 3933, is only 3' away with a nearly identical radial velocity, and so
may be contributing some of the GB 140' flux.

4. 1973UGC...C...0000N
Re:UGC 06841
Type NGC 2685?
UGC 06839 at 3.5, 224
Companion 1.7, 356, 0.4: x 0.4:, irregular


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