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Date and Time of the Query: 2019-06-24 T02:50:32 PDT
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Notes for object NGC 5854

6 note(s) found in NED.


1. 2001A&A...374..421B
Re:NGC 5854
4.8 NGC 5854
NGC 5854 is an early spiral (Sa) characterized by a low gas content and the
absence of current star formation. Haynes et al. (2000) have studied the
stellar kinematics, using H{alpha} and MgIb optical absorption lines, and
the kinematics of ionized gas, using the N[II] and O[III] optical emission
lines. These data reveal the existence of a counterrotating gas disk
extending up to r ~ 7" (0.8 kpc), with a total velocity range of
120 km s^-1^. The stellar velocities measured at r ~ 40" (4.5 kpc) reach
+/-160 km s^-1^. Although HI content is low, Magri (1994) detected a signal
in the nucleus. The HI profile is centered at 166 km s^-1^, close to the
optically determined value for v_sys = 1669 +/- 30 km s^-1^ (Fouque et al.
1992). The narrowness of the HI spectrum (FWHM ~ 100 km s^-1^, namely, less
than the measured stellar velocity spread) suggests a close association of
the HI component with the counterrotating ionized gas (see discussion in
Haynes et al. 2000).
Although weak, the ^12^CO(J = 1 - 0) spectrum shows the existence of
H_2_ gas within r = 2.3 kpc. There is a hint of a double-horned profile,
with two velocity components at v = 1539 km s^-1^ (with
FWHM ~ 100 km s^-1^) and v = 1930 km s^-1^ (with FWHM ~ 170 km s^-1^),
equidistant from v = 1735 km s^-1^. The CO spectrum in the J = 2 - 1 line
confirms the detection of molecular gas. Not surprisingly, the J = 2 - 1
and J = 1 - 0 profiles differ. The J = 2 - 1 line shows hints of two
velocity components, although with a smaller velocity spread
(v = 1630 km s^-1^ and 1740 km s^-1^) and is centered at v ~ 1690 km s^-1^,
in reasonable agreement with HI. However the larger velocity spread of the
J = 1 - 0 spectrum would suggest that, compared to the counterrotating
ionized gas core, the H_2_ disk may extend farther out. The molecular gas
mass within the central r = 2.3 kpc was derived from the ^12^CO(J = 1 - 0)
integrated intensity giving; M_mol_ = 1.6 x 10^8^ M_sun_.

2. 2001A&A...374..394V
Re:NGC 5854
NGC 3368, NGC 3810 and NGC 5854: Our major-axis kinematics are in good
agreement with the literature. This is also true for the V_*_ we measured
along the minor axis of NGC 5854.

3. 1996AJ....112..937D
Re:NGC 5854
11: NGC 5854 (S0). A number of upper limits have been reported for this galaxy
along with a flux of 0.43 Jy km s^-1^ reported at Arecibo and 3 Jy km s^-1^
found at Effelsberg. We detect no extended emission in neighboring points that
might account for the discrepancy. Unfortunately, uncertain baseline
subtraction at the position of the galaxy itself does not allow us to confirm
either flux measurement.

4. 1994CAG1..B...0000S
Re:NGC 5854
Sa
(E,S/I,0)
PH-8022-S
April 27/28, 1979
103aO
10 min
There are two spiral patterns in NGC 5854.
One is very close to the center, and the other is
traceable on the original plate to at least the
outermost of the two faint stars slightly above the
major axis on the left-hand side of the print.
The inner spiral pattern is in the bulge (it
forms the bulge) and has the form and the sense
of the opening of a stubby S. The outer arms are
smooth and massive. They open in the same sense
as that of the bulge. Their surface brightness is
exceedingly low, but they can be seen beyond the
moderately high surface brightness lens to a
distance of about twice the diameter of the lens.
The high-surface-brightness bulge has a diameter
about half that of the lens.
The intensity distribution on the original
plate gives the impression of three discrete
components, the inner two of which (the bulge and
the lens) have sharp edges. But this is probably
a subjective description of what is a continuous
gradient to the intensity distribution. The eye
and brain take the first derivative of an intensity
field; a change of the luminosity gradient appears
as an edge to the eye.

5. 1973UGC...C...0000N
Re:UGC 09726
SB(s)0+ (de Vaucouleurs)

6. 1964RC1...C...0000d
Re:NGC 5854
Very small diffuse nucleus in a bright smooth lens: 0.85 arcmin x 0.25 arcmin
with a suggestion of a bar and spiral pattern. Faint, smooth whorls in a
bright envelope.
In the NGC 5846 Group with NGC 5839, NGC 5845, NGC 5846, and NGC 5850.


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