Date and Time of the Query: 2019-04-25 T06:50:32 PDT
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Notes for object NGC 3384

17 note(s) found in NED.

1. 2012ApJ...754...67F
Re:NGC 3384
NGC 3384 .LBS-*.-Contains a nuclear bar (Fisher & Drory 2010) and a rapidly
rotation disk described by Busarello et al. (1996); Fisher (1997) and Emsellem
et al. (2004) already find strong h_3_ moments in anti-correlation with
velocity. The velocity dispersion profile changes slope at 10" and becomes more
shallow toward smaller radii, but then exhibits a pronounced peak inward of 3"
that is accompanied by a dip (as seen by Fisher 1997 and Emsellem et al. 2004 as
well) in the h_4_ moments that become positive just outside of this region.

2. 2009MNRAS.397.2148G
Re:NGC 3384
We have used the NC's H-band magnitude from Ravindranath et al. (2001). The
nuclear V-I colour of 1.3 from Lauer et al. (2005) implies an H-band M/L ratio
of ~0.60^+0.25^_-0.15_assuming [Fe/H] < 0.56 (Fig. A1). From this, we derive an
NC mass of 2.2 * 10^7^ M_{sun}_. As a check, we note that Lauer et al. (2005,
their Table 8) provide a V-band NC luminosity of 4 * 10^6^ L_{sun}_.Multiplying
by an M/L_V_ ratio of 2.5 gives a mass of 10^7^ M_{sun}_, similar within a
factor of ~2.

3. 2007MNRAS.377..759S
Re:NGC 3384
NGC 3384: the galaxy, also from the Leo I group, is the only S0 of our sample.
It shows a circumnuclear disc (Sil'chenko et al. 2003) and a disc or a secondary
bar aligned with the major axis. This galaxy also has a non-symmetric
distribution of stars in the disc (Busarello et al. 1996). NGC 3384 has been
proposed as a candidate for a pseudo-bulge (Pinkney et al. 2003).

4. 2006MNRAS.369..497K
Re:NGC 3384
This SB0 galaxy shows a dynamically cold component in the central 5 arcsec (see
Paper III), which may correspond to the red major axis disc component found by
(Busarello et al. 1996). The line strength indices have already been presented
in Paper II. The metal line strengths show regular gradients consistent with the
isophotes. The H{beta} absorption map, at moderately elevated values (see also
Kuntschner et al. 2001), appears flat in the inner regions with weak evidence
for increasing H{beta} strength at large radii.

5. 2006MNRAS.366.1151S
Re:NGC 3384
This galaxy shows weak [O III] and H{beta} emission close to our detection
limit. The unsharp-masked image suggests the presence of two, nested, disc
structures. Ravindranath et al. (2001) noticed the same features in
near-infrared HST images.

6. 2004MNRAS.352..721E
Re:NGC 3384
NGC 3384: The dispersion map exhibits a dumbbell-like shape, coincident
with a rapidly rotating component in the central 5 arcsec (Busarello et
al. 1996; Fisher 1997), with a strong anticorrelation signature in h
3. The velocities are nearly cylindrical in the outer part of this
galaxy classified as SB0 (Paper II). Our h_4_ map shows a slight dip at
the centre, consistent with the long-slit profile of Fisher (1997). Our
h_4_ map is consistent with h_4_ being positive everywhere, in contrast
to the measurements of Pinkney et al. (2003).

7. 2004A&A...415..941E
Re:NGC 3384
NGC 3384 (inner disk): Busarello et al. (1996). Outer-bar measurements
are from the ellipse fits of Busarello et al.; a_{epsilon}_ in this
case is actually the ellipticity minimum, which is also the extremum in
the PA twist. Bar PA is from analysis of Busarello et al., which showed
that the best ellipse-fit PA for the bar is ~ 60 deg away from the bar's
true position angle. (The problems with the ellipse fits comes from the
fact that this galaxy is highly inclined, and the bar is very close to
the projected minor axis.) Inner disk measurements are from WFPC2 F814W
and NICMOS2 F160W images. Distance is from Tonry et al. (2001,
surface-brightness fluctuation), and {sigma}_0_ is the average of several
recent measurements (Gebhardt et al. 2003; Fisher 1997; Neistein et al.

8. 2001AJ....122..653R
Re:NGC 3384
NGC 3384: The optical images show no dust features (van Dokkum & Franx
1995; Tomita et al. 2000). The residual image highlights the weak nuclear
and large-scale disks, which are poorly fitted by the Nuker law. The
pointlike nucleus is also incompletely removed by the PSF.

9. 2001AJ....121.2974L
Re:NGC 3384
NGC 3384: Also in the Leo Group, this S0 galaxy has S_N_ ~ 0.9
(Ashman & Zepf 1998). We detect a total of 54 GCs, of which 30 formally
fall in the "blue" category and 24 in the red, but with no statistical
evidence for bimodality.

10. 2000A&AS..141..385V
Re:NGC 3384
C-34 = NGC 3384. (A,G,J,N) Classified as SB01 in the RSA, it shows a
disc-like component in the inner regions along the minor axis (Davoust
et al. 1984). It has a disc-to-bulge luminosity ratio of 0.9, a disc
scalelength of 2.7 kpc (Fisher et al. 1996; Baggett et al. 1998) and a
central stellar velocity dispersion of 150 km s^-1^ (Fisher et al. 1996;
Prugniel & Simien 1996). Near-infrared photometry: see Jungwiert et al.
(1997). Optical spectra: stellar line strengths and their gradients were
measured by Fisher et al. (1996); no emission lines are visible in the
spectra of Ho et al. (1995, 1997). No stellar counter-rotation was found
by Kuijken et al. (1996), only a suggestion of independent kinematical
components like nuclear discs and bars. Member of the LGG 217, or
Messier 96 (Leo I), group (Garcia 1993). Part of a second, stronger,
line profile is seen at the high end of the Nancay band (at 1150-1400
km s^-1^), which is undoubtedly due to NGC 3389, a 12.4 mag Sc spiral at
the edge of the Nancay beam (2.8' E and 5.7' S of C-34) at an H I
redshift of 1298 km s^-1^ with a FWHM of about 245 km s^-1^ (Helou et al.
1981; Staveley-Smith & Davies 1988) and a line flux of about
26 Jy km s^-1^. The PRC object was detected at Nancay (line flux
1.5 Jy km s^-1^), but not at Arecibo - the best published Arecibo upper
limit is 0.62 Jy km s^-1^ (see Table 3). The well-established optical
redshift of the PRC object, 735 +/- 36 km s^-1^, is 170 km s^-1^ lower
than the Nancay value, 903 km s^-1^, and the H I profile is quite narrow,
{DELTA}V_20_ = 93 km s^-1^. Given this descrepancy, the non-detection at
Arecibo and the lack of confusing galaxies in the neighbourhood, we may
have detected a tail or bridge of H I far from the galaxy's center due to
interaction with its nearby companion NGC 3379, a 10.2 mag elliptical at
a redshift of 888 km s^-1^.

11. 1997AJ....113..950F
Re:NGC 3384
NGC 3384. This SB0 shows a rotation curve which temporarily declines with
radius following an initial rapid rise; after reaching a maximum rotation
speed of 92 km s^-1^ at ~4", the rotation speed of NGC 3384 declines to 74 km
s^-1^ at ~10" before rising again to reach V_max_=156 km s^-1^ at the limit of
our observations. This feature is possibly associated with the influence of
the bar or a nuclear disk. A dip in the central velociiy dispersion is also
present along the minor-axis suggesting that the rapidly rotating component
seen along the major axis is kinematically colder than the surrounding stars.
The h_3_ term indicates that strong asymmetries are present in the LOSVD and a
high-speed tail is present along the major axis beyond 7".

12. 1996ApJ...459..110F
Re:NGC 3384
NGC 3384
Our major- and minor-axis line strengths are dominated by light from the bulge
component of NGC 3384, a barred S0.

13. 1994CAG1..B...0000S
Re:NGC 3384
Leo Group #26
Dec 10/11, 1952
103aD + GG11
25 min
NGC 3384 is one of the brightest galaxies in
the Leo Group (Ferguson and Sandage 1990,
where a map is given), whose closest other bright
members are NGC 3379 (E0; panel 1) at 7.2'
separation, and NGC 3389 (Sc; panel 253) at a
6.3' separation from NGC 3384. The mean
redshift for the group listed by Ferguson and
Sandage (1990) is = 909 km/s.
The central circular bulge has two small
luminous projections (position angles at 1 and 7
o'clock in the prints here) that extend to the
periphery of the faint, highly flattened envelope
whose major axis is at right angle to that of the
projections. The form is similar to that of most of
the other galaxies on this page.

14. 1976RC2...C...0000d
Re:NGC 3384
= Holm 212b
In Leo (M96) Group.
Non-interacting pair with NGC 3379 at 7.2 arcmin
Ap. J., 139, 284, 1964.
Photometry (5 Color):
A.J., 73, 313, 1968.
Publ. Byurakan Obs., No. 40, 15, 1969.
Bull. A.A.S., 5, 348, 1973.
A.J., 79, 835, 1974.
Ap. J. Suppl., 26, No. 230, 1973.

15. 1973UGC...C...0000N
Re:UGC 05911
In triple group with UGC 05902 brightest at 7.2, 247
UGC 05914 at 6.5, 156
SB(s)0-: (de Vaucouleurs)
S0 (Holmberg)

16. 1964RC1...C...0000d
Re:NGC 3384
= Holm 212b
Extremely bright nucleus in a short weak bar: 0.7 arcmin x 0.2 arcmin.
Smooth structure.
Lund 9 dimensions are for the bright part only.
Pair with NGC 3379 at 7.2 arcmin.
In the Leo Group.
Photograph and Photometry:
Dennison, Univ. of Michigan Thesis, 1954.
Ap. J., 50, 384, 1919.

17. 1918PLicO..13....9C
Re:NGC 3384
A replica of 3379 except that it is more oval; 3' long. Nucleus very bright
and elongated; no whorls can be distinguished, but it is probably a spiral
of the Andromeda type.

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