NGC 4260 .SBS1..-Strongly barred. The bulge morphology is generally smooth.
Martini et al. (2003) acknowledge the presence of dust structures in the central
region but claim that they do not imply a sense of rotation. The bulge is
classified as a classical bulge by Fisher & Drory (2008). The velocity
dispersion profile is somewhat irregular and S-shaped within the bulge region.
The h_3_ moments are small and mostly compatible with zero, The h_4_ moments
show a gradual drop from a central value of zero to about -0.06 at about 10".
VCC 341: We did not detect this galaxy, with an rms noise level of 0.76 mJy. Its
optical redshift is 1827+/-60 km s^-1^. The Effelsberg H I detection reported by
Huchtmeier (1982) at 1846 km s^-1^, with W_50_ = 465 km s^-1^ and I_HI_ =
3.0+/-1.5 Jy km s^-1^, i.e. an average line strength of 6.5 mJy, appears
spurious given its low signal-to-noise ratio.
NGC 4260 (C)
Dust structures are visible in the circumnuclear region, but they are
not of sufficient contrast to classify easily. Those present do not
imply any sense of rotation; we therefore classify this as a chaotic
The regular bulge is embedded in an early-type bar. The profile is
fitted by an R ^1/4^ law with R_e_ =36" and V_F606W_ =11.2. This fit
clearly includes the bar component, and it has therefore been
omitted from our analysis.
5: NGC 4260(Sa). An upper limit of 0.7 Jy km s^-1^ was reported at Arecibo
while a detection of 3 Jy km s^-1^ was reported at Effelsberg. The nearby
galaxy UGC 7349 also had an Arecibo detection at 5500 km s^-1^ and one at
Parkes at 980 km s^-1^. We detect nothing at the positions of NGC 4260 or
UGC 7349 (up to a velocity of 3600 km s^-1^). In the general vicinity, four
objects listed in the Virgo Cluster Catalog (Binggeli et al. 1985, hereafter
referred to as VCC) have possible detections. A fifth possible source
(1218+0615) was found near a position where a very faint, uncataloged
(possibly background) galaxy appears on the Palomar plate. VCC 329 and 340
have previous detections consistent with our measurements after accounting for
the offsets in our positions from the galaxy centers. It appears possible that
the detection at Effelsberg was caused by confusion with VCC 340. VCC 379 and
405 are listed as dwarf ellipticals, which would make H I detections
surprising, but we caution that none of these positions has been reobserved.
April 27/28, 1979
NGC 4260 is in the W Cloud region of the
Virgo complex. Its high redshift, v_o = 1806 km/s,
suggests it is at the greater distance of the W
Cloud rather than that of the Virgo Cluster core.
NGC 4260 is one of the prototype smooth-armed
SBa's in the RSA that have often been
used in discussions of the origin of smooth-armed
early-type galaxies (Sandage 1983a). Are such
galaxies generic to the classification sequence or
are they results of environmental processes?
NGC 4260 is important for the question. The
answer is seen from the fact that, as with NGC
7743, NGC 6942, and NGC 1022 on preceding
panels, NGC 4260 is not in the Virgo Cluster; it
is moderately isolated and shows no evidence of
environmental effects such as tides by a close
encounter. Its smooth arms must then be generic
to the formation process for NGC 4260 itself.
The very-high-surface-brightness central
region containing the bar is burned out in the
print here. The bar itself is not as well defined as
in the prototype SBb galaxy NGC 1300 (Hubble
Atlas, p. 45; panels 154, S8 here), but NGC
4260 has bright asymmetrical parts that
resemble bright massive spiral stubs, the most
prominent of which is seen here to the upper left
of the bright central bulge.
Well-defined dust lanes exist on the inside
edges of the outer smooth arms.
SB(s)a (de Vaucouleurs)
Small, very bright nucleus in a bright broad bar with blobs. Pseudo (r):
1.1 arcmin x - . 2 regular, smooth arms.