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Date and Time of the Query: 2019-05-20 T20:06:37 PDT
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Notes for object NGC 3497

5 note(s) found in NED.


1. 2001A&A...374..421B
Re:NGC 3497
4.6 NGC 3497
NGC 3497 is a major-axis dust lane elliptical known by different names
(NGC 3525 = NGC 3528 = IC 2624). The ringed dusty disk shown in the B - R
color maps of Ebneter & Balick (1985) seems to have the same extent as the
stellar disk (diameter ~70"). As with all major-axis dust-lane ellipticals,
e.g. ESO 263-48 in this paper, the dust signature is interpreted to be the
result of an accretion episode. The galaxy has a fainter galaxy at 2'
(named NPM1G-19.0362) and a companion with similar redshift at 5'
(NGC 3529 = IC 2625).
Stellar and gas rotation curves have been derived by Bertola et al.
(1988a), who measured a radial velocity difference of ~240 +/- 30 km s^-1^
between the western and eastern sides of the major axis (on the NE side
stars are receding). The measured systemic velocity is
v_sys_ = 3672 +/- 25 km s^-1^. No X-ray, IR or HI data are available in
the literature.
The emission of both lines of ^12^CO were observed in three positions
located along the major axis of the disk: the (0,0) offset centered on the
galaxy nucleus and two off-centered positions at r = +/-22". The J = 2 - 1
and J = 1 - 0 spectra shown in Fig. 1 reveal the presence of molecular gas
in the central region (up to r = 5 kpc) and also the detection of the
J = 1 - 0 line of ^12^CO in the NE offset. In the SW position, however,
CO emission was not detected. The ^12^CO(J = 1 - 0) central spectrum is
fitted well by a single Gaussian profile, centered at 3774 km s^-1^ and
with FWHM = 600 km s^-1^ (~1000 km s^-1^ at zero power); therefore, it is
100 km s^-1^ redshifted with respect to v_sys_. In contrast, the J = 2 - 1
profile shows three velocity components at v = 3497 km s^-1^,
v = 3693 km s^-1^ (close to the optically determined ) and
v = 3497 km s^-1^. The velocity asymmetry in the central J = 1 - 0
spectrum may indicate that H_2_ distribution is slightly asymmetrical in
the disk within r = 5 kpc.
A comparison between the radial velocity measured on the CO spectrum
(~3570 km s^-1^) and the stellar velocities observed in the NE side of the
major axis (redshifted with respect to v_sys_), indicates that molecular
gas is counterrotating with respect to the stars.
The molecular gas mass within the central r = 5 kpc, derived from the
^12^CO(J = 1 - 0) integrated intensity, would be
M_mol_ = 1.4 x 10^9^ M_sun_. The amount of molecular gas detected in the
NE offset is M_mol_ = 2.7 x 10^8^ M_sun_.

2. 1994AJ....108.2128C
Re:PGC 033667
PGC 033667 = NGC 3528 = NGC 3525 = NGC 3497 = IC 2624.

3. 1985SGC...C...0000C
Re:NGC 3528
Plate 4205
= NGC 3497 = NGC 3525 = IC 2624. Overexposed center with strong dust lane,
much extended corona. Small companion 2.0 north-following. Interacting(?)
pair with NGC 3529 at 4.9; 1st in group.

4. 1982ESOU..C...0000L
Re:ESO 110450-1912.1
=ESO 570- G 06
absorption lane
pair with ESO 570- G 07
in cluster
IC 2624 Dec 5' off
NGC 3497 RA 5.9 minutes off
NGC 3525 RA 0.9 minutes off

5. 1968MCG4..C...0000V
Re:MCG -03-28-037
Pair with MCG -03-28-038. {rho}=5.1 arcmin. Gradient of brightness
in MCG -03-28-037 is very steep - not like in a galaxy E, although
on the red print it resembles E; it does not have a dusky belt. On the
blue print, it is of the same type as NGC 4753.


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