The result is truncated. The full result is available at the Resource Link. Copyright 2019-2026 Caltech, Support from NASA is acknowledged. This information is taken from a collection created and curated by the NASA/IPAC Extragalactic Database (NED), operated by the California Institute of Technology (Caltech). If your research benefits from the use of NED, the following acknowledgement in your paper would be appreciated: "This research has made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology." See: https://ned.ipac.caltech.edu/Documents/Overview/Acknowledgments A row number applicable to this list only Bibliographic reference code Object name in NED standard format Note about the object, as transcribed from the referenced catalog or publication

1	2009MNRAS.397.2148G	MESSIER 031	NGC 224, better known as Andromeda, has not been included because the nucleus is not a pressure-supported star cluster in which the stars have random motions but is a rotationally supported nuclear disc.
2	2008MNRAS.386.2242H	NGC 0224	NGC 224 (M31), NGC 3031 (M81) and NGC 3115 in our sample are typical classical bulges listed in KK04.
3	2008MNRAS.386.2242H	NGC 0224	NGC 224 (M31), NGC 3031 (M81) and NGC 3115 in our sample are typical classical bulges listed in KK04.
4	2007MNRAS.382.1552L	NGC 0224	NGC 224 - M 31: The M31 nucleus is highly compact, and is the prototype of the central luminous star clusters found in many galaxies. The bulk of its stellar population corresponds to an old (>~10 Gyr) metal-rich component (Bica et al. 1990). This is also reproduced by our synthesis analysis. The central 1 kpc of M 31 contains several ionized gas clouds, which interestingly have different line ratios, placing them in the Seyfert, LINER or star-forming regions of line ratio diagrams (delBurgo et al. 2000).
5	2002ApJ...574..740T	MESSIER 031	M31. The modeling is complicated by the double nucleus. Kormendy & Bender (1999) find M_BH_ = (3.0 +/- 1.5) x 10^7^ M_sun_, although this result relies heavily on the small displacement between the center of light of the nucleus and bulge. Tremaine (1995) and Bacon et al. (2001) find M ~ 7 x 10^7^ M_sun_ but without detailed model fitting. We adopt the range (2.0-8.5) x 10^7^ M_sun_.
6	2002AJ....124..675C	UGC 00454	M31. The 1.4 GHz flux density is from the NRAO 91 m telescope (Dennison et al. 1975).
7	2001ApJS..132..129M	NGC 0224	Outside the bulge, the MUV light profile roughly parallels the R-band profile. However, the FUV profile flattens and even rises slightly with increasing radius, meaning that the (FUV-MUV) color becomes systematically bluer with radius. This result is preliminary because of the difficulty in determining the sky background (see section 4). The existence of a smooth radial distribution of FUV emission at small radii suggests the presence of an FUV-bright inner disk which spatially overlaps with the outer bulge. Such an inner disk is not seen in the case of M81 (NGC 3031, see Fig. 17a), where the combined FUV light of the bulge and disk is undetectable at inner radii (r < 3.5' = ~3.5 kpc). The surface brightness profiles are quite different between these two objects, despite the fact that M81 is only slightly earlier in Hubble type (Sab rather than Sb). The outer disk of M31 is rich in UV-bright massive stars, the brightest concentration of which is NGC 206, located ~5' from the southwestern edge of the mosaics shown in Figures 5a-5b. Hill et al. (1992a) provide UV photometry of 30 resolved stars in NGC 206; most are evolved OB stars with 30 <~ M/M_sun_ <~ 60. Hill et al. (1993c, 1995b) presented enlargements of the UIT images for some 60 OB associations in M31 and photometered individual stars and integrated light. They infer a maximum stellar mass of 85 M_sun_. Only about 40% of the integrated MUV light and 20% of the FUV light of a typical association comes directly from the resolved stars; the remainder may be dust-scattered starlight with a smaller contribution from fainter stars with T >~ 10,000 K. Bohlin et al. (1993) obtained UV photometry for 43 compact clusters; most of these are old globulars, but seven appear to be compact young clusters. The disk shows a strong (FUV-MUV) color gradient, becoming systematically bluer from r ~ 3' to r ~ 50' (~10 kpc) by about 2 mag. This reflects the increasing contribution of OB associations to the total integrated light at larger radii.
8	2001ApJS..132..129M	NGC 0224	NGC 224 (M31). - The Andromeda galaxy, a member of the Local Group, is a disk system, type SA(s)b, ~690 kpc in distance, and inclined 78^deg^ to our line of sight. Several low-resolution, wide field UV images of M31 were obtained with both balloon (Deharveng et al. 1980) and rocket experiments (Deharveng et al. 1976; Carruthers, Heckathorn, & Opal 1978; Bohlin et al. 1985; Bohlin et al. 1988), the latter two in both FUV and MUV bands. The best of these images achieved a spatial resolution of ~15" and showed that the UV emission from M31 is dominated by the bulge and a broken ring of OB associations. UIT imagery was obtained in two overlapping fields during Astro-1; M31 completely fills the field of view in both. One field is centered on the bulge; the other is centered ~40' to the southwest along the major axis. Images in each filter have been combined and are displayed as mosaics in Figures 5a-5b. The radial UV surface brightness and color profiles plotted in Figures 5a-5b, respectively, are based on mean values within those segments of the elliptical apertures which lie within our mosaic. The profiles therefore reflect behavior only near the southwestern major axis for r < 50'. The R-band profile shown in Figures 5a5b was interpolated from the major axis profile data taken from Kent (1987). The bulge is extended in both FUV and MUV and displays a relatively smooth appearance; neither bright substructure nor dust lanes are evident. As in the case of M81, the bulge of M31 is considerably more prominent at longer wavelengths, though the contrast is not as extreme as in M81. In both FUV and MUV light, the inner bulge follows a reasonably good de Vaucouleurs r^0.25^ profile to r ~ 90". Except at very small radii where the spatial resolution of the data are mismatched, the bulge shows only a small color gradient in (25-R). However, the FUV light is more centrally concentrated, producing a strong radial color gradient in (FUV-MUV) for 0 <~ r <~ 150", in which the light gets redder with increasing radius. This behavior is typical of large spiral bulges and elliptical galaxies but is much larger in amplitude and is reversed in sense from gradients in the optical bands such as (B-V) or (V-K) (O'Connell et al. 1992; Ohl et al. 1998). There are no detected UV point sources in the bulge, even though individual stars as faint as B1 V (m(MUV) ~ 18.4) would be above the MUV threshold (O'Connell et al. 1992). If the FUV light from the bulge originated in recently formed massive stars with a normal initial mass function, there would be ~200 OB stars visible within r <~ 2'. Their absence supports the interpretation of the FUV light as originating from low-mass, post-giant branch stars (e.g., Greggio & Renzini 1990; O'Connell 1999). HST UV observations of the core of M31 have been presented by King et al. (1992); Bertola et al. (1995); King, Stanford, & Crane (1995); and Brown et al. (1998). At HST resolution, the nucleus of M31 is double, and the component coincident with the dynamical center has UV colors which are bluer than those of the background bulge and therefore may contain massive stars formed through stellar collisions (King et al. 1995; Lauer et al. 1998). The second, off-nuclear component has UV colors similar to the bulge. These sources are not resolved in the UIT photometry. Brown et al. (1998) have partially resolved the hot stellar population responsible for the FUV light in the central 14" x 14" using HST/FOC images. Color-magnitude diagrams of the resolved stars are consistent with objects that have evolved from the extreme horizontal branch.
9	2001A&A...374..394V	NGC 0224	NGC 224: The discrepancy observed along the NE axis between our data and those by Kormendy (1988) and by Dressler and Richstone (1988) may be the result of an incorrect sky subtraction in our data. An overestimation of the sky level due to the large size of the galaxy covering all the slit area may produce the higher {sigma}_*_ and shift in V_*_ we actually measure.
10	2000MNRAS.319...17L	NGC 0224	NGC 224 (M 31): No analysis of X-ray data for this galaxy has been done in this paper. Einstein and ROSAT HRI observations of M 31 have detected over 100 individual sources with luminosities 10^36^ <~ L_X_ <~ 10^38^ erg s^-1^ (Trinchieri & Fabbiano 1991; Primini, Forman & Jones 1993). The ROSAT PSPC, which is more sensitive than the HRI (but with worse spatial resolution), gives an upper limit for a diffuse component associated with the galactic bulge of 2.6 x 10^38^ erg s^-1^ (Supper et al. 1997). The point sources are associated with two components, the disc and the bulge, and are strongly concentrated towards the centre. PSPC data show that the bulge and disc components account for about one and two thirds of the total emission, respectively (Supper et al. 1997). Ginga (2-20 keV) and BeppoSAX (0.1-10 keV) observations have shown that this emission from the galaxy is consistent with a population of low-mass X-ray binaries (LMXRBs) (Makishima et al. 1989; Trinchieri et al. 1999). A list of the sources found within ~6 arcmin of the nucleus is shown in Table 6. The source coincident with the galactic nucleus has been reported to vary (Primini et al. 1993), and is probably an XRB.