Date and Time of the Query: 2022-01-17 T09:27:35 PST
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Notes for object NGC 1023

15 note(s) found in NED.

1. 2012ApJ...754...67F
Re:NGC 1023
NGC 1023 .LBT-..-Clean classical morphology in HST F555W. The rotation curve
steps rapidly from ~=+60 km s^-1^ to ~=-60 km s^-1^ in the central two
arcseconds and then rises gradually to a value of ~=200 km s^-1^ at 50". The
h_3_ profile shows an equally fast change within the inner ~=2" from -0.03 to
0.03 with opposite sign. Like Emsellem et al. (2004) we see that the v/h_3_
anti-correlation turns into a correlation outward of ~=10". The velocity
dispersion profile rises all the way to the center. Outside of 50" the velocity
dispersion profile flattens out at about 100 km s^-1^ which coincides with a
flattening in the rotation curve. This is significantly beyond the bulge radius
of ~=19". The minor axis rotation is mostly close to zero at larger radii but
becomes negative inward of 4" (~=-25 km s^-1^ at the center). The acquisition
image does not show an obvious offset of the minor axis slit but we note that
due to the rapid rise of major axis rotation in the central arcseconds already a
small offset of (~=0.5") to the west suffices to explain the observed behavior.
The h_3_ moments become positive in the same radial range, which is expected if
the velocity offset is due to actual rotation. The minor axis h_4_ moments show
a double peak at +/-7" with maximum values of h_4_ ~= 0.04. The continuously
centrally rising velocity dispersion of the major axis is reproduced on the
minor axis.

2. 2009MNRAS.397.2148G
Re:NGC 1023
Bower et al. (2001) show that the average V-I colour within 1.0 (0.1) arcsec
is 1.4 (1.25). From the innermost colour, our adopted stellar population models
tell us that the metallicity is super-solar and that the population must be of
an intermediate to old age, in agreement with the 7-Gyr-old age from Sil'chenko
(1999). From Fig. A1, the associated V-band, stellar M/L ratio is in the range
0.2 < log[M/L_V_] < 0.6, and we adopt M/L_V_= 2.5 for the NC magnitude from
Bower et al. (2001, their equation 2). Faber et al. (1997) report B-V= 0.93
for this galaxy, a typical colour for an old population. Assuming a 13-Gyr-old
stellar population, we have applied a K-band stellar M/L ratio of 1.0 to the
K-band bulge magnitude tabulated in Marconi & Hunt (2003).

3. 2006MNRAS.369..497K
Re:NGC 1023
This SB0 galaxy, with a prominent twist in the central velocity field (see Paper
III), shows a central concentration in all metal lines. The metal line strength
at larger radii appears flat and even tend to rise again at the edges of the
FoV. The H{beta} map is consistent with a constant value over the full FoV.

4. 2006MNRAS.366.1151S
Re:NGC 1023
This galaxy displays [O III] emission that remains strong in the outer regions,
with a distribution that appears to be skewed with respect the galaxy major
axis. Yet, the gas shows a coherent, although not perfectly regular, velocity
field with a reasonably defined zero-velocity curve, which indicates a mild
kinematic misalignment between gas and stars. The approaching south-eastern arm
indicates that the angular momentum of the gas may vary in the outermost parts
of the galaxy. This would be consistent with the complex neutral hydrogen
morphology and kinematics found by Sancisi et al. (1984), suggesting an
interaction with three nearby companion galaxies. No noticeable absorption
feature is visible in the HST image, which also in this case reveals the
presence of a nuclear stellar disc.

5. 2005A&A...442..137N
Re:UGC 02154
UGC 2154 (NGC 1023) is the brightest galaxy of a nearby group of 13 galaxies
(Tully 1980). The total H I-flux for this galaxy is quite large (80.13 Jy km
s^-1^), but the gas is scattered over a large area, has a very low
column-density and does not reside in a regular disk. It seems most likely the
result of a recent merger or accretion event, possibly with one of the other
group members (cf. Sancisi et al. 1984).

6. 2004MNRAS.352..721E
Re:NGC 1023
NGC 1023 This is an example of an SB0 galaxy showing h 3 anticorrelated
with V inside ~10 arcsec, and correlated outside (Bower et
al. 2001). There is a strong twist of the zero-velocity curve near the
centre. Stellar kinematics has been previously published by Simien &
Prugniel (1997b), Neistein et al. (1999), Sil'chenko (1999), including
multiple long-slit data parallel to the major axis (Debattista, Corsini
& Aguerri 2002). The h_3_ and h_4_ maps show significantly negative values
on the western side of the galaxy which are not observed by Debattista
et al. (2002). The cause for this discrepancy is not known, so these
features should be confirmed.

7. 2002ApJ...574..740T
Re:NGC 1023
NGC 1023.
Both the velocity dispersion and black hole mass are from
Bower et al. (2001).

8. 2001AJ....121.2974L
Re:NGC 1023
NGC 1023: At 9.8 Mpc, NGC 1023 is the nearest S0 galaxy. It is the
brightest galaxy in a group of 13 galaxies (Tully 1980). Its GC system has
been studied recently by using HST by Larsen & Brodie (2000). As well as
the expected blue and red GC subpopulations, they identified a third
subpopulation of red spatially extended clusters. The origin of these
extended clusters is currently unknown.

9. 2001A&A...368...16M
Re:NGC 1023
4. NGC 1023 is one of the few S0 (SB0) galaxies in our sample. It has a
very good distance determination (11.11 Mpc) by Ferrarese et al. (2000).
The residua show a dipole structure near the centre, probably due to the
central nuclear disk (Sil'chenko 1999) which we did not consider in the fit
procedure. From our disk-bulge decomposition we obtained a half-light
radius of the bulge of 30 to 35" which is in fairly good agreement with the
corresponding bulge radius obtained from stellar velocity dispersion
profiles (50", Simien & Prugniel 1997).

10. 1994CAG1..B...0000S
Re:NGC 1023
NGC 1023 Group
Sep 22/23, 1952
103ao + Wr2c
20 min
NGC 1023 may be the brightest member of
a group identified by Humason, Mayall, and
Sandage (1956). Two possible dwarfs (Im types),
of the eight such dwarfs mentioned in the Hubble
Atlas as group candidates, are shown in the
Hubble Atlas (p. 40).
The deviation of the intermediate-zone
orientation from that of both the central nuclear
region (shown in the insert) and the outer
extended envelope (shown in the main print) is
characteristic of SB0 types.
A low-surface-brightness Im dwarf
companion is to the left and slightly below the major
axis of the NGC 1023 envelope in the main print

11. 1993ApJS...86....5K
Re:NGC 1023
NGC 1023; SB0.
The long-wavelength spectrum of NGC 1023 is apparently dominated by F and
G stars. NGC 1023 is a normal SB0 galaxy in a group of 13 gravitationally
bound galaxies (Tully 1980). Since NGC 1023 lies at Galactic latitude
b = 19^deg^, the strong absorption line of Mg II is very likely to be from
our Galaxy. In contrast, Mg I is so strong that it is unlikely to be from
just the Milky Way ISM, implying that there is an intrinsic Mg I

12. 1976RC2...C...0000d
Re:NGC 1023
= Arp 135
Brightest of NGC 1023 Group.
Faint elliptical satellite at the eastern end of the major axis.
Photometry: (5 Color)
A.J., 73, 313, 1968.
Photometry: (UBV)
Trudy Ast. Obs. Leningrad, 28, 32, 1971.
HI 21cm:
A.J., 79, 767, 1974.

13. 1973UGC...C...0000N
Re:UGC 02154
Arp 135
SB(rs)0- (de Vaucouleurs), S0 (Holmberg)
Faint diffuse companion attached following
`Similar nebulosity about one diameter further east' (Arp)
8 dwarf members known in NGC 1023 group
UGC 02080 at 46.3

14. 1964RC1...C...0000d
Re:NGC 1023
Brightest member in the NGC 1023 Group.
Extremely bright nucleus
in the center of a diffuse bar: 1.3 arcmin x 1.0 arcmin
near the minor axis of the projected lens.
Very faint asymmetric extension or satellite
near one end of major axis.
See also Ap. J., 46, 30, 1917 = MWC 132.
Ap. J., 120, 439, 1954.
Radio Emission: (upper limit)
M.N.R.A.S., 123, 279, 1961.

15. 1918PLicO..13....9C
Re:NGC 1023
6' x 1.3' in p.a. 80^deg^. Center very bright, with perhaps an almost stellar
nucleus. While no spiral whorls are discernible, it is probably a spiral of the
Andromeda type. 13 s.n.

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