Date and Time of the Query: 2019-05-26 T16:07:52 PDT
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Notes for object NGC 3898

15 note(s) found in NED.

1. 2012ApJ...754...67F
Re:NGC 3898
NGC 3898 .SAS2..-Outer disk dust spiral transitions into weak dust lanes over a
smooth and classical bulge morphology in HST F606W. The rotation curve rises
slowly out to r ~= 10" and flattens at about the bulge radius of ~=15.7". The
velocity dispersion profile is strongly centrally peaked and rises smoothly from
~=140 km s^-1^ to ~=220 km s^-1^ in the center. The h_3_ moments are
anti-correlated with velocity and reach local maximum at r ~= 10", the same
radius where the flattening of the rotation curve sets in.

2. 2008MNRAS.388..500E
Re:UGC 06787
UGC 6787 (NGC 3898). Because of the interference filter used for this
observation, which was not perfectly centred on the systemic velocity of the
galaxy, the H{alpha} emission from the eastern side was not transmitted through
the filter (a good H{alpha} image could be found in Pignatelli et al. 2001). As
a consequence, our H{alpha} rotation curve is only traced with the approaching
side but seems acceptable anyway. It reaches a plateau within the optical radius
(D_25_/2) and seems to decrease beyond, in agreement with the H I data from
WHISP (Noordermeer et al. 2005). However, the H I data suggest that the rotation
curve climbs again beyond 2 arcmin to recover the same velocity level. Also, the
steep inner rise of the velocities seen in the H I position-velocity diagram
from WHISP is not detected in our H{alpha} position-velocity diagram, which is
probably due to a too low signal-to-noise ratio of the optical observations. The
H{alpha} velocities remain constant in the approaching half of the diagram,
whereas the H I velocities increase in the same region.

3. 2007MNRAS.376.1513N
Re:UGC 06787
The rotation curve of UGC 6787 (NGC 3898) is well resolved and shows some
characteristic 'wiggles' with an amplitude of 30-50 km s^-1^. The kinematics in
the central parts are only barely resolved in the optical spectrum, and due to
the high inclination angle and resulting line-of-sight integration effects, the
central line-profiles are strongly broadened. After the initial rise of the
rotation curve to the peak velocity of 270 km s^-1^, the rotation velocities
drop to approximately 220 km s^-1^ at a radius of 30 arcsec (~2.75 kpc), after
which they gradually rise again to 250 km s^-1^ at R ~= 100 arcsec (~9 kpc). The
rotation velocities then drop again to 220 km s^-1^, after which they rise again
to reach a more or less flat plateau at 250 km s^-1^. Although there are clear
indications that the gas disc of UGC 6787 is warped, the locations of the
'wiggles' in the rotation curve do not coincide with the radii where the
position angle and the inclination chan ge and the variations in the rotation
velocity seem real. This is further confirmed by the fact that the variations
occur symmetrically at all position angles over the velocity field.
The discrepancy between the kinematic inclination angle derived here and the
optical inclination from Paper II can be explained by the dominance of the bulge
in the optical image. As was noted in Paper II, the optical image of this galaxy
is dominated by the spheroidal bulge out to large radii, which makes it
impossible to obtain a reliable estimate for the inclination from the isophotes.
The kinematical inclination derived here is free of such effects and thus
reflects the true orientation of this galaxy more accurately.

4. 2002ApJS..142..223F
Re:NGC 3898
NGC 3898. NVSS reports an 8.7 mJy source and FIRST a 2.4 mJy source.
The 1.4 GHz, 54" resolution observations of Condon (1987) detect an
uncertain 6.3 mJy source, spatially confused by a strong, nearby,
unrelated core. The same radio structure is seen in the Gioia &
Fabbiano (1987) map.

5. 2002AJ....123..159C
Re:NGC 3898
Red (dusty) center; red nuclear elongated feature; larger scale
southeast-northwest red (dust?) disk/barlike feature connects with red
spiral feature northeast of center

6. 2002A&A...388...50F
Re:NGC 3898
The ionized-gas distribution and kinematics of this Sa galaxy
have recently been studied in detail by Pignatelli et al. (2001).
They found that in the innermost region (|r|<~8") of NGC 3898,
the ionized gas is rotating more slowly than the circular
velocity predicted by dynamical modelling based on stellar
kinematics and photometry. The fingerprint of such a
"slowly-rising'' rotation curve (according to Kent 1988
definition) can be recognized in the decrease of the velocity
gradient at smaller radii. The two-component shape of the PV
diagram results from the bright nuclear emission and not the
increase of velocity gradient or the velocity dispersion. This
is a Type III PV diagram and its similarity to the PV diagram
of NGC 4419 is remarkable.

7. 2001MNRAS.325..385T
Re:NGC 3898
NGC 3898 is centred just off this field to the east, and is only partly
visible. It is a member of the nearby 12-3 Group and has a heliocentric
velocity of 1176 km s^-1^.

8. 2001A&A...374..394V
Re:NGC 3898
NGC 3898: The H I distribution and velocity field have been studied in
detail by van Driel & van Woerden (1994). The comparison of these data with
our ionized-gas kinematics and the H{alpha}-imaging by Pignatelli et al.
(2001) suggests that both ionized and neutral hydrogen have a regular
velocity field and a smooth distribution.

9. 2001A&A...368...16M
Re:NGC 3898
28. NGC 3898 is an Sa spiral of medium inclination with multiple thin arms.
Carollo & Stiavelli (1998) found on HST images the continuation of the
R^1/4^ density profile of the bulge to less than 1" radius.

10. 1999A&A...349...88K
Re:NGC 3898
4.5. NGC 3898
There have been several studies of this galaxy in the optical (e.g.,
Burbidge & Burbidge 1965, Barbon et al. 1978, Mizuno & Hamajima 1986,
and references given in van Driel & van Woerden 1994). H97 tentatively
concluded that broad H{alpha} is absent from the optical spectrum.
21 cm HI observations with the WRST were presented by van Driel &
van Woerden (1994).
The source is quite weak with only about 50 detected photons, very
close to the limits of meaningful {chi}^2^ spectral fits. Therefore, we
only applied a powerlaw model with fixed Galactic absorption. This
results in {GAMMA}_X_ = -2.1 and gives an acceptable fit.

11. 1997ApJS..112..391H
Re:NGC 3898
NGC 3898.--The profiles of the [S II] lines do not match those of narrow
H{alpha} and [N II] in detail. This, coupled with the fact that the spectrum
does not have very high S/N, leads to ambiguity regarding the detection of
broad H{alpha} (Fig. 10g). We will adopt the more conservative assumption that
broad H{alpha} is not present; it would be highly desirable to verify this with
data of higher S/N.

12. 1994CAG1..B...0000S
Re:NGC 3898
Hubble Atlas, p. 10
March 25/26, 1955
103aO + Wr2
30 min
NGC 3898 is described in the Hubble Atlas
(p. 10) as the prototype Sa galaxy with multiple
arms (MAS type), whose later type-example is
NGC 2841 (Sb; Hubble Atlas, p. 14; panels 142,
S4, S12 here). The reproduction here is from the
same 200-inch plate used in the Hubble Atlas.
The galaxy is similar to NGC 4698 at the lower
left but is later along the Sa section.
Two very thin outer arms, outlined only by
knots (HII regions), are just barely seen in the
print here and in the Hubble Atlas. Both arms
are on the same side of the image below and
above the left half of the major axis. The arms
have a wider pitch angle than the inner tightly
wound arms. They extend far beyond the main
The innermost of these thin outer arms
sweeps outward slightly above the field star that
is close to the minor axis near the top of the print.
This arm can be faintly traced here from the
seven HII knots that are just visible, the outer
three of which are to the right and slightly above
the bright field star. The same feature is present
in the Hubble Atlas print. The arm that is still
more distant runs approximately parallel to the
arm just described, but it is more distant from
the center in the same ratio as the first of the two
arms. If the knots are HII regions, star formation
is occurring in these outer, very-low-surface-brightness
arms. The outer arms here are similar
to the outlying thin arms in IC 5267 in the
negative print below.

13. 1976RC2...C...0000d
Re:NGC 3898
Brightest of NGC 3846-3898 Group.
Non-interacting pair with NGC 3888 at 16 arcmin

14. 1973UGC...C...0000N
Re:UGC 06787
SA(s)ab (de Vaucouleurs), Sa (Holmberg)
Companion 5.0, 60, 0.7 x 0.12, early

15. 1964RC1...C...0000d
Re:NGC 3898
Very bright, large nucleus: 0.6 arcmin x 0.35 arcmin. Bright inner spiral
structure. Pseudo (r): 2.3 arcmin x 0.9 arcmin in a lens: 2.55 arcmin x
1.05 arcmin. Very faint, partially resolved outer arms.
Brightest of NGC 3846-3898 Group.
Non-interacting pair with NGC 3888 at 16 arcmin.
Lund 9, Heidelberg Veroff. Vol. 9, 1926 and HA 88, 2 dimensions are for the
bright part (the lens) only.
Ap. J., 85, 325, 1937.

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