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Date and Time of the Query: 2019-06-20 T03:29:04 PDT
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Notes for object NGC 5954

9 note(s) found in NED.


1. 2005MNRAS.364.1253V
Re:NGC 5954
NGC 5953/4 is also in the IRS SLUGS sample. While D00 used colour-corrected IRAS
fluxes as listed in the IRAS Bright Galaxy Sample (from Soifer et al. 1989) we
present here, as for all the OS sample, fluxes from the IRAS FSC.

2. 2004AJ....127.3235S
Re:NGC 5954
NGC 5954. Given as CPG 468 by Domingue et al. (2003). The HIRES data
agree with the higher resolution ISOPHOT data indicating the dominance
of the southwestern component.

3. 2002AJ....124..675C
Re:UGC 09904
UGC 09904 also contributes to F15322+1521, whose principal
identification is UGC 09903. VLA C-array map in Condon et al.
(1990).

4. 1997ApJS..108..155G
Re:NGC 5954
NGC 5953 - NGC 5954. NGC 5953 is an S2 nucleus in an Sa galaxy in
interaction with NGC 5954 that has a LINER nucleus in an Scd galaxy. Both
galaxies are experiencing a burst of star formation in the circumnuclear
region. In NGC 5953, all the emission is within the central 10" (1.3
kpc). The nucleus is also extended to the north. The [O III] image is
also extended to the northeast, aligned with the companion. Long-slit
spectroscopy shows that in the circumnuclear region a starburst coexists
with high-excitation gas ionized by the active nucleus (see Gonzalez
Delgado & Perez 1996c).

5. 1995A&AS..110..131R
Re:NGC 5954
NGC 5954: The morphology and internal patchiness are reminiscent of the
Seyfert galaxy NGC 7603. In this case, however, it is the companion that
is classified as a Seyfert. We observed this galaxy along the major axis
(Fig. 6). The gas and the stars show similar steep rotation curves in the
central 5 arcsec. Actually we measure very few stellar velocity values.
The rotation curve of the gas is peculiar for two reasons: 1) the
velocity field is truncated on the SW side and 2) the symmetry axis of
the central part of the curve is displaced towards the SW with respect to
the barycenter of the starlight. It is not clear if these features are
related to considerable dust obscuration in the spiral. The galaxy is
very disturbed and a bridge of stars "connect" it to NGC 5953.
N II]/H{alpha} (Fig.12) ratio is consistent with emission from HII regions
as previously noted by Jenkins (1984). The central velocity dispersion is
consistent with the value measured by Bonfanti (1994) (106+/-11 km s^-1^)
if we assume that our peak value is displaced from the barycenter of the
light (135+/-17 km s^-1^). The Reshetnikov (1993) spectra show (similarly
to NGC 5953) a maximum velocity gradient near 200 km s^-1^. The
"turnover" on the side towards the companion (near the pair axis) shows
significant evidence for noncircular motions. The velocity excess is
toward larger velocity values that indicate either contamination from the
higher velocity S0 neighbor or a velocity-continuous cross fuelling
process.

6. 1976RC2...C...0000d
Re:NGC 5954
= Holm 714a
in Arp 091
in VV 244
in Kara[72] 468
Colliding or strongly interacting pair at 0.8 arcmin
Radio Observations:
M.N.R.A.S., 167, 251, 1974.

7. 1973UGC...C...0000N
Re:UGC 09904
VV 244b, Arp 91
Sc (de Vaucouleurs)
See UGC 09903

8. 1964RC1...C...0000d
Re:NGC 5954
= Holm 714a
Pair with NGC 5953 at 0.8 arcmin.
Spectrum:
Ap. J., 116, 66, 1962.
P.A.S.P., 168, 386, 1957.

9. 1959VV....C...0000V
Re:VV 244b
= NGC 5954
V = +2,170 km/sec from H{alpha}, [NII], {lambda}3727
(Page, T., Ap. J., 116, 63, 1952).


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