Date and Time of the Query: 2019-04-25 T07:15:57 PDT
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Notes for object NGC 2974

16 note(s) found in NED.

1. 2008MNRAS.386.2242H
Re:NGC 2974
The black hole masses of NGC 2974, NGC 3414, NGC 4552, NGC 4621, NGC
5813 and NGC 5846 are taken from Cappellari et al. (2007b) with a formal
error of 10 per cent (1{sigma} CL), which is approximately converted
from the 30 per cent error at 3{sigma} CL.

2. 2008MNRAS.386.2242H
Re:NGC 2974
The black hole masses of NGC 2974, NGC 3414, NGC 4552, NGC 4621, NGC 5813 and
NGC 5846 are taken from Cappellari et al. (2007b) with a formal error of 10 per
cent (1{sigma} CL), which is approximately converted from the 30 per cent error
at 3{sigma} CL.

3. 2006MNRAS.369..497K
Re:NGC 2974
This rapidly rotating galaxy shows evidence of enhanced metal line strength
along the rotation direction. The H{beta} map appears relatively flat. The
long-slit observations of Rampazzo et al. (2005) show declining H{beta} strength
with radius while Carollo et al. (1993) data suggest a modest increase with
radius. Our emission-line maps (Paper V) show significant [O III] and H{beta}
emission basically over the full FoV, and thus different H{beta} emission
corrections are likely the cause of the literature disagreement on H{beta}
absorption strengths.

4. 2006MNRAS.366.1151S
Re:NGC 2974
SAURON observations for this galaxy were previously discussed in detail in
Krajnovic et al. (2005). Here we note how the EW maps highlight the presence of
a nuclear bar surrounded by a ring and of two spiral arms connecting to the
outer parts of the field where emission remains strong. The presence of nested
bars within this galaxy is discussed in the light of the SAURON and HST
observations by Krajnovic et al. and Emsellem et al. (2003). The inner bar is
responsible in particular for the observed twist within the central 4 arcsec in
the velocity field, which is otherwise very regular. The velocity dispersion of
the gas rises up to 250 km s^-1^ and remains moderately high (~100 km s^-1^)
also in the rest of the map. The possibility of a dynamical support for the gas
motions was first investigated by Cinzano & van der Marel (1994) and recently
also by Krajnovic et al. Although not perfectly regular, the dust distribution
appears to trace the general orientation of the gaseous disc, following in
particular part of the EW ring.

5. 2004MNRAS.352..721E
Re:NGC 2974
NGC 2974: A very rapidly rotating galaxy which has an h_3_ field with one
of the strongest amplitudes. The h_4_ map exhibits a central dip, as
found by, e.g. Cinzano & van der Marel (1994), but stays positive, in
contrast to the data of Bender et al. (1994).

6. 1998A&AS..128...75P
Re:NGC 2974
4.3.4. NGC 2974
This isolated galaxy is one of the brightest objects of the sample. HI emission
was discovered and an atomic gas disk has been put in evidence by Kim (1988).
Ionized gas has been shown by Demoulin et al. (1984), Kim (1989) and Goudfrooij
et al. (1994). Ionized gas kinematics has been studied by Bettoni (1992). This
object also shows an X-ray emission (Forman et al. 1985). Contrary to most of
elliptical galaxies, ionized gas and HI gas components MA of NGC 2974 are
aligned with respect to stars. The {phi} viewing angle is not constrained at
all because of small difference between MA of gas and stars. This object is a
good carididate for an internal origin of ionized gas.

7. 1996A&AS..120..257Z
Re:NGC 2974
3.2. NGC 2974
The line emission is found to extend out to 30" from the galaxy nucleus. From
the analysis of the radial intensity profiles of the [NII] {lambda}6583.4 A
line a position angle of ~48^deg^ for the gaseous disk is derived and an
inclination of i=49^deg^, The velocity and the velocity dispersion fields are
symmetric around the center of the galaxy indicating that the gas is moving in
ordered orbits. The presence of a significant velocity gradient
(~50 km/s/arcsec) along the minor axis of the gaseous disk (PA=135^deg^)
indicates as in the case of NGC 1453 a probably non-axisymmetric galaxy
potential. A maximum velocity of Vmax=250 km/s is measured at PA=25^deg^. The
velocity dispersion profile of the gas has a central peak of ~250 km/s and
then falls rapidly off to a constant level of ~70 km/s in the outer parts of
the galaxy. Because of the high velocity gradient the value of the central
velocity dispersion may be overestimated due to seeing effects and due to the
finite slit width.

8. 1996A&AS..120..257Z
Re:NGC 2974
NGC 2974 is the only galaxy of the sample which is also detected at 21 cm. The
orientation and kinematics of the neutral gas disk (i=55^deg^, PA=45^deg^,
Vmax=355+/-60 km/s (290 km/s projected) (Kim et al. 1988) are in good
agreement with the present data which confirm also previous kinematical
studies of the ionized gas component (Demoulin-Ulrich et al. 1984; Kim 1989).
NGC 2974 has a unresolved continuum source coincident with the galaxy cnter
and is an X-ray source which has an extended halo (Forman et al. 1985).
In contrast to other elliptlcals the gaseous disk is very well aligned with
the stellar component and shares also similar kinematic properties. Perhaps
not surprisingly, the galaxy also has a faint stellar disk (Scorza 1993;
Cinzano & van der Marel 1994). Evidence for spiral arm structures has been
found in NGC 2974 (Bregman et al. 1992, Paper I).

9. 1994CAG1..B...0000S
Re:NGC 2974
March 21/22, 1980
103aD + GG495
45 min
NGC 2974 is a prototypical normal E4 galaxy of average
compactness. It is isolated; no other Dreyer galaxy is within several

10. 1994A&AS..105..481M
Re:NGC 2974
NGC 2974: This diE is somewhat atypical, because the axis-ratio fails
to increase rapidly in the envelope. The disk is perhaps more important
than in other diE objects. See detailed study by Cinzano & van der Marel

11. 1994A&AS..105..341G
Re:NGC 2974
The HI 21 cm line has been detected in this galaxy with a rather regular
distribution which is consistent with a rotating disk or ring along the
(apparent) major axis of the galaxy (Kim et al. 1988}). Previous imaging
studies have shown the existence of a dust lane and ionized gas along the
major axis (e.g., Kim 1989}). The present B-I image reveals a similar
distribution of the dust absorption, with some additional amorphous
substructure at ~10" northeast of the nucleus. The H{alpha}+[NII] image
shows a rather regular gas disk associated with the dust lane, with
additional evidence for warped outer structure. The emission-line
spectrum exhibits very broad wings to the H{alpha} line. X-ray source
with extended halo (Forman et al. 1985}). Nuclear radio source. Detected
by IRAS at 60 and 100 microns. Our broad-band images confirm the
presence of weak spiral arm structure as was previously reported in this
galaxy (see Roberts et al. 1993}).

12. 1994A&AS..104..179G
Re:NGC 2974
Significant third order Fourier terms in inner region due to dustlane
(cf. Kim 1989). Detected by IRAS at 60 & 100 microns.

13. 1993A&A...280..409B
Re:NGC 2974
NGC 2974: The ionized gas in this galaxy, which has also been studied
by DBB, Kim (1989), TdiSA and Shields (1991), appears to lie in a
fundamentally regular elongated structure with some peripheral fainter
filaments. The latter could be related to the presence of X-ray emission
(Canizares et al. 1987). Kim (1989) noted the presence of a small major-
axis dust lane. Analysis of the continuum image using the earlier
described adaptive filter reveals a complex substructure with a lens-like
feature from which two distinct spiral arm-like structures originate.
Schweizer (1992, priv. comm.) and Bregman et al. (1992) also reported
evidence for spiral structure in this galaxy. NGC 2974 has also been
detected in HI by Kim et al. (1988). These authors note that the HI disk
is regular, appears undisturbed and lies along the stellar major axis.
The total HI mass is 2 x 10^9^ M_sun_ for our adopted distance of 38 Mpc.
Perhaps not surprisingly, NGC 2974 also has a faint stellar disk (Scorza
1993; Cinzano & van der Marel 1993).

14. 1976RC2...C...0000d
Re:NGC 2974
87 arcmin from the Quintet A0936-04A,B,C,D,E.
See Ap. J., 185, 797, 1973.
Radio Observations:
Ap. J., 183, 791, 1973.

15. 1974UGCA..C...0000N
Re:UGCA 172
UGCA 172:
= NGC 2974
E4 (RC1)

16. 1964RC1...C...0000d
Re:NGC 2974
Very bright nucleus. There is a star at 0.7 arcmin.

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