NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2022-01-17 T09:27:35 PST
Help | Comment | NED Home

## 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 SB0_1_(5) (P) PH-164-S 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 here. 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 component. 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. Photometry: 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.

Back to NED Home