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Notes for object NGC 0185

13 note(s) found in NED.


1. 2007MNRAS.382.1552L
Re:NGC 0185
NGC 185: Spectra were obtained for four very red knots seen in the J band. Knot
1 is also coincident with a bright optical source, and the other three knots are
close to regions of enhanced optical emission. With M_V_~-5, the knots
probably correspond to stellar clusters in NGC 185 or individual evolved stars
(Davidge 2005). The other bright optical sources seen in the centre of this
galaxy are a mixture of blue star clusters (Martinez-Delgado et al. 1999) and
probably foreground stars. The cross in Fig. 2 marks the position of the 2-cm
radio detection of Nagar et al. (2000). It is not consistent with an obvious
source in any of the images.

2. 2004A&A...416...41X
Re:NGC 0185
NGC 185. This dwarf elliptical galaxy is of great interest not only
because of its proximity to us (only ~0.7 Mpc away) but also
because it contains optical dust clouds (Martinez-Delgado et al. 1999)
and luminous blue stars (Baade 1944; Lee et al. 1993) indicating current
star formation activity. This galaxy shows a centrally concentrated
distribution for the atomic hydrogen which extends further to the
northeast while CO observations show that the molecular gas is closely
associated with the optical dust clouds (Welch et al. 1996; Young & Lo
1997; Young 2001). The 15 micron map presented in this work
(Fig. A.1) is mainly associated with the dust clouds and the molecular
gas but also shows a central concentration.

3. 2001ApJS..133...77H
Re:NGC 0185
NGC 185 (S2). - Not detected. Heckman, Balick, & Crane (1980) also did
not detect the galaxy at 6 cm (S_6_ < 1 mJy; {DELTA}{theta} = 1.7") or
20 cm (S_20_ < 5 mJy; {DELTA}{theta} = 4"). Although the weak emission
lines in this object formally place it in the category of Seyferts, it is
probable that this galaxy does not contain a genuine active nucleus.
Instead, its emission lines may be powered by stellar processes. NGC 185
is one of the companions of M31, and it is morphologically classified as a
dwarf spheroidal galaxy, one with a diffuse center lacking a clear nucleus.

4. 2000MNRAS.319...17L
Re:NGC 0185
NGC 185: As with NGC 147, this galaxy was observed for the first time in
X-rays, and no emission was detected. These observations have also been
reported by Brandt et al. (1997). A 2{sigma} upper limit for the flux of
a point source was found to be 4 x 10^-14^ erg s^-1^ cm^-2^ in the
0.1-2.5 keV bandpass, again in good agreement with the value quoted in
Table 5.

5. 2000ApJ...542..186N
Re:NGC 0185
NGC 185.-The 2 cm source we detect is offset 14.5" west and 4" north
of the optical position determined by Cotton et al. (1999) from digital
sky survey plates. The 1 {sigma} error of the optical position
determination is estimated to be 2.7" in both right ascension and
declination. The galaxy is diffuse, ~12' x 10' in extent, and has a
prominent dust lane to the northwest that may bias the optical position
determination. Overlaying the optical and radio images shows that the
2 cm radio source lies at the southwest tip of the dust lane, and the
offset from the optical center does appear to be more than can be
explained by dust lane obscuration. Furthermore, the radio source has a
very low luminosity (10^16.7^ W Hz^-1^), which can be explained by a
source in the galaxy stellar disk. Hummel (1980) lists a 5 {sigma} upper
limit of 10 mJy in a 23" resolution map at 20 cm, and we find a 2 cm
flux density of 0.8 mJy in our 0.15" map. It is therefore possible that
the source is flat spectrum, but a measurement at a resolution closer to
that of the 2 cm map is required for a definitive result, and for now we
consider this source to have an undetermined spectral index.

6. 1995ApJS...98..477H
Re:NGC 0185
The nucleus of NGC 185 is very ill-defined, and the spectrum has low
S/N. Nevertheless, the presence of faint H II region emission lines
and Balmer absorption lines indicate some ongoing star formation. Like
NGC 205, NGC 185 is a companion of M31; the star formation histories of
the two appear very similar but not identical (Hodge 1989).

7. 1994CAG1..B...0000S
Re:NGC 0185
Local Group
Hubble Atlas, p. 3
dE3
PH-531-B
Sep 9/10, 1951
103aD + GG11
60 min
NGC 185 is one of the five galaxies in the Local Group that Baade
(1944a, b) resolved into stars at Mount Wilson in his well-known
experiment that was the last stage in his development of the
population concept (see Sandage 1986c for a review of this history).
The absolute magnitude is faint at M_T_ = -14.6. The morphological
type is nearly prototypical dE3 (see Sandage and Binggeli 1984 for the
system of dwarf classification), except for the evident dust patches
near the center. The low surface brightness is characteristic of dE
galaxies of this absolute magnitude (Binggeli, Sandage, and Tarenghi
1984, Fig. 8).
The surface brightness distribution was studied early by Hodge
(1963, 1971). Large numbers of RR Lyrae stars have been discovered by
Saha and Hoessel (1990) with a mean magnitude of = 25.0. Planetary
nebulae have also been identified (Ford, Jacoby, and Jenner 1977).
At least three globular clusters can be identified in the image
here; the brightest is below the center at a position angle of about
5:30 o'clock as oriented here. NGC 185 has a similar distance as M31,
and is a companion to it at a projected linear separation of 105 kpc.
Additional photographs are shown in the original paper by Baade
(1944b) and in the Hubble Atlas (p. 3).

8. 1976RC2...C...0000d
Re:NGC 0185
In the M31 Group.
Non-interacting pair with NGC 0147.
Photograph:
Ap. J. (Letters), 183, L73, 1973.
P.A.S.P., 86, 289, 1974.
A.J., 79, 671, 1974.
Photometry: (12 colors)
Ap. J., 145, 36, 1966.
Photometry: (5 colors)
A.J., 73, 313, 1968.
Photometry: (BV)
Ann. Rev. Astr. & Ap., 9, 35, 1971.
IAU Symp. No. 44, 46, 1972.
Isodensitometry:
A.J., 79, 671, 1974.
Globular Clusters:
P.A.S.P., 86, 289, 1974.
Planetary Nebulae:
Bull. A.A.S., 5, 13, 1973.
Ap. J. (Letters), 183, L73, 1973.

9. 1973UGC...C...0000N
Re:UGC 00396
E3 pec (de Vaucouleurs), E pec (Holmberg)
Paired with UGC 00326 = NGC 147 at 58'
`Low surface brightness dwarf, dark markings in bright middle, no definite
nucleus' (de Vaucouleurs)

10. 1964RC1...C...0000d
Re:NGC 0185
Paired with NGC 0147 in M31 Group.
Low surface brightness dwarf.
Dark markings in bright middle.
No definite nucleus.
Additional Mt. Wilson Velocity
for a globular cluster,
1.1 arcmin [south-following] the nucleus: -102 km/sec.
Photograph and Monologue:
Ap. J., 100, 147, 1944. = MWC 697.
Photometry:
Medd. Lund, II, 128, 1950.
A.J., 68, 691, 1963.

11. 1961Hubbl.B...0000S
Re:NGC 0185
E pec
PH-648-B
Aug. 21/22, 1952
103aD + GG11
60 min
Enlarged 3.1X
The three galaxies shown on the facing page illustrate the
resolution of elliptical galaxies into stars. All three are
members of the Local Group. The resolution of NGC 0185
and NGC 0205 was first accomplished by Baade with the
100-inch telescope (Ap. J., 100, 137-150, 1944). The
photographs here of NGC 0185 and NGC 0205 were taken by Baade
with the 200-inch.
NGC 0185 and NGC 0147 together with M31, M32, and
NGC 0205 form a subunit of the Local Group. All five have
distance moduli of about m - M = 24.4 to 24.6.
A dust patch near the center of NGC 0185 is more easily seen
on a photograph by Baade reproduced in the reference cited.

12. 1956AJ.....61...97H
Re:NGC 0185
HMS Note No. 003
Strong auroral spectrum superimposed.

13. 1918PLicO..13....9C
Re:NGC 0185
Rather irregular; slightly oval, 3' long; there are two curious rifts near the
nucleus; it appears to be an irregular spiral. The nebular matter is faint
and diffuse. A star of magn. 14 is north of the very faint nucleus. 30 s.n.


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