Date and Time of the Query: 2019-07-20 T05:53:35 PDT
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Notes for object MESSIER 110

16 note(s) found in NED.

1. 2009MNRAS.397.2148G
Re:NGC 0205
In addition to M33, NGC 205 also has only an upper limit to the mass of any
potential BH at its centre (Valluri et al. 2005). It does however possess a very
obvious nuclear star cluster (e.g. Carter & Sadler 1990). From the F814W surface
brightness profile in Fig. A6, the inner nuclear component has an absolute
magnitude of -10.42 I-mag (using a distance of 0.82 Mpc).^9^ There is some
evidence for excess light from ~0.5 to 3 arcsec, and Butler & Martinez-Delgado
(2005) have remarked that there may be a nuclear disc present. Using M/L_I_=
1.6(* 0.95) = 1.52 from Valluri et al. (2005), the associated mass of the NC is
0.8 * 10^6^ M_{sun}_, in fair agreement with our adopted (dynamical) value of
1.4 * 10^6^ M_{sun}_from De Rijcke et al. (2006a).
For a 13-Gyr-old spheroid population, M/L_B_~ 2.5, which is in good
agreement with our adopted value of 2.7 from De Rijcke et al. (2006a).

2. 2007MNRAS.382.1552L
Re:NGC 0205
NGC 205 - M 110: Bica et al. 1990 performed population synthesis of the nuclear
spectra and inferred that the dominant stellar population has an age between 0.1
and 0.5 Gyr, with subsolar metallicities. This is in very good agreement with
our population-synthesis results, except for the derived metallicities. A modest
burst of star formation also took place ~50 -100 Myr ago (Peletier 1993;
Cappellari et al. 1999).

3. 2004A&A...416...41X
Re:NGC 0205
NGC 205. This is also a dwarf elliptical galaxy which shows similar
characteristics to NGC 185. The bright blue stars observed in this
galaxy (Hodge 1973) as well as detailed study of the color profiles
(Peletier 1993), show that star formation activity is still taking place
in this galaxy. The atomic hydrogen in this galaxy is distributed in an
elongated structure which is curved and extends about twice as far to
the south of the optical center as it does to the north of the optical
center (Young & Lo 1997). CO observations show that the molecular gas is
associated with the dust clouds (Welch et al. 1998; Young & Lo 1996;
Young & Lo 1997). The 15 micron emission (Fig. A.1) is associated with
the dust clouds.

4. 2001ApJ...556...24Z
Re:NGC 0205
While there are no detected sources down to ML = 6 within ~1.4' of the
optical position, the contours hint at the possibility of some diffuse
emission in the central area. The upper limit derived from the ROSAT HRI
observation is a factor of 8 below that determined from Einstein HRI data
(Markert & Donahue 1985). NGC 205 also occurs in two PSPC pointings of the
first ROSAT M31 survey (ROR 600067 and 600068; Supper et al. 1997), around
a 40' off-axis angle. No sources associated with NGC 205 are found in these
two PSPC frames. The upper limits are in these cases a factor of 3 higher
than our HRI upper limit and are thus not as constraining as the one derived
from the HRI exposure.

5. 2000MNRAS.319...17L
Re:NGC 0205
NGC 205 (M 110): This small elliptical galaxy was observed with the
Einstein HRI and no X-ray sources were detected with a
flux > 1.8 x 10^-12^ erg s^-1^ cm^-2^ in the 0.5-4.0 keV bandpass
(Markert & Donahue 1985; Fabbiano, Kim & Trinchieri 1992). The ROSAT
HRI observations of NGC 205 reported here give an upper limit of
6.78 x 10^-14^ erg s^-1^ cm^-2^ for the flux of any point source in the
nuclear region. The only source seen in Fig. 3 lies 2.7 arcmin away from
the nucleus and is probably not associated with the galaxy.

6. 1999ApJ...519...89C
Re:NGC 0205
NGC 205 (M110).-This is a normal dwarf galaxy and is one of the two
elliptical companions to M31. There is no previous evidence for a
central black hole, and we do not detect a compact X-ray source.

7. 1995ApJS...98..477H
Re:NGC 0205
The well-defined nucleus exhibits a blue continuum and prominent Balmer
absorption lines, indicating a young stellar population. Emission lines
are very weak or absent, however, implying that there is either not much
gas present or a deficit of O-type stars in this dwarf elliptical system.
Hodge (1989) cites additional evidence for a young stellar population in
NGC 205, and discusses its probable star formation history.

8. 1994CAG1..B...0000S
Re:NGC 0205
Local Group
Hubble Atlas, p. 3
S0/E pec
(dE,N pec)
Aug 21/22, 1952
103aD + GG11
75 min
NGC 205, the companion to M31 (Hubble
Atlas, p. 18; panel 149 here), was first resolved
into individual stars by Baade (1944a) with the
Mount Wilson 100-inch Hooker Telescope using
red-sensitive plates. The print here was made
from a Palomar 200-inch plate taken by Baade
on a yellow-sensitive emulsion. This plate is not
the same used in the Hubble Atlas (p. 3), which
was also taken by Baade at Palomar but on a
red-sensitive emulsion.
Resolution into stars occurs suddenly at a
threshold apparent magnitude of V = 22 (Mould,
Kristian, and Da Costa 1984). It is the red color
of the stars and the presence of the sharp upper
luminosity threshold for resolution that led
Baade to identify the population properties of the
resolved stars with the evolutionary stage of old
stellar systems such as globular clusters.
The integrated absolute magnitude of NGC
205 is faint at M_B_T_ = -16. The appearance of
NGC 205 on small-scale plates (cf. Zinnecker
and Cannon 1985) is consistent with this faint
intrinsic luminosity, as judged by the low surface
brightness. The image shown there is prototypical
of nucleated dE,N dwarf ellipticals of the type
that define the class (Sandage and Binggeli
1984). However, on large-scale plates the
well-known dust patches in NGC 205 (Baade 1951;
Hodge 1973) are prominent, seen also in the
print here. The two main patches are to the lower
right and near the top of the bright part of the
bulge in this print. Dust patches are not typical
in prototype dE,N galaxies.

9. 1994CAG1..B...0000S
Re:NGC 0205
Local Group
Hubble Atlas, p. 3
S0/E pec
(dE,N pec)
Aug 21/22, 1952
103aD + GG11
75 min
A portion of the image from the same plate
used for the main print of NGC 205 at the left is
shown here to see better the brightest globular
clusters associated with this galaxy (Hubble
1932; Hodge 1973).
The brightest cluster is slightly to the right
of the major axis, about one-third the way from
the lower border of this print. This, and clusters
like it in the body of the M31 disk, were important
for Baade's (1944a) case, justifying his
identification of the resolved stars as similar to
stars at the tip of the giant branches in globular
clusters. His point was that on the original plates
where the resolution into stars in the outskirts of
the globular clusters themselves was seen, the
cluster stars resolved at the same magnitude as
the stars over the image of NGC 205 itself. A hint
of that fact can be imagined from the image of the
globular cluster in the print here.

10. 1994CAG1..B...0000S
Re:NGC 0205
Local Group
Hubble Atlas, p. 3
S0/E pec
Sep 6/7, 1921
80 min
There was, however, an early false clue
concerning the nature of the stellar content of NGC
205, and from it, a mistaken generalized uncertainty
concerning the stellar content of all E
galaxies. Both here and in NGC 4486 (the
prototype giant E galaxy, panel 17), resolution
occurred into a few outstandingly bright images.
(In the case of NGC 4486, the objects are
globular clusters, not individual stars.)
The same situation was known for NGC 205
even from the earliest Mount Wilson plates, c. 1920.
It was known that very bright starlike
images exist near the center of NGC 205. The
Mount Wilson plate used for the image on the
facing page here, taken by Hubble with the
100-inch Hooker Telescope in 1921, clearly shows
their existence.
From a spectacular, near-ultraviolet plate
by Baade (1951), it finally became understood
that these images are of hot, young,
high-luminosity stars that have just formed.
This is one of the few known cases of recent
star formation in an apparently old E galaxy
environment. But because NGC 205 is so close,
and therefore can be studied with unusual detail,
it may be that the presence of dust and a low rate
of current star formation are more common in E
galaxies than is now (1990) believed.
The colors of the young-star-forming regions
in NGC 205, and the ages that can be inferred
from them, have been discussed by Price and
Grasdalen (1983). Early measurements of the
neutral hydrogen content of NGC 205 were made
by Johnson and Gottesman (1983).

11. 1976RC2...C...0000d
Re:NGC 0205
Interacting pair with NGC 0224 in M31 Group.
MCG dimensions for NGC 0205 and NGC 0221 are interchanged.
P.A.S.P., 78, 495, 1966.
Observatory, 88, 91, 1968.
Ann. Rev. Astr. & Ap., 9, 35, 1971.
Ap. J. (Letters), 183, L73, 1973.
Photometry: (12 colors)
Ap. J., 145, 36, 1966.
Photometry: (5 colors)
A.J., 73, 313, 1968.
Photometry: (UBV)
IAU Symp. No.44, 46, 1972.
P.A.S.P., 85, 286, 1973.
Photometry: (10 colors)
Ap. J., 179, 731, 1973.
Globular Clusters:
Ap. J., 182, 671, 1973.
Ap. J., 139, 532, 1965.
Ap. J., 177, 285, 1972.
Astrofizika, 4, 409, 1968.
Rotation Curve and Systemic Velocity:
Astr. Ap., 8, 364, 1970.
Planetary Nebulae:
Bull. A.A.S., 5, 13, 1973.
Ap. J. (Letters), 183, L73, 1973.
HI 21cm: (upper limits)
Observatory, 83, 245, 1963.
Astr. Ap., 29, 335, 1973.
M.N.R.A.S., 169, 607, 1974.
Radio Observations: (upper limits)
Astrophys. Lett., 11, 173, 1972.
Astrophys. Lett., 13, 65, 1973.

12. 1973UGC...C...0000N
Re:UGC 00426
E5 pec (de Vaucouleurs), E pec (Holmberg)
Companion to UGC 00454 = Messier 31 at 37, 134
Identity M 110 suggested by Kenneth Glyn Jones, see Sky and Telescope,
Vol XXXIII, page 156

13. 1964RC1...C...0000d
Re:NGC 0205
Interacting pair with NGC 0224.
In the M31 (Local) Group.
(B-V) increases with log A/D(0); interpolated value.
Ap. J., 76, 44, 1932. = MWC 452.
Publ. Michigan X, 10, 1951.
Ap. J., 100, 137, 1944. = MWC 696.
M.N.R.A.S., 94, 519, 1934.
M.N.R.A.S., 98, 618, 1938.
Medd. Lund, II, 128, 1950.
Sov. A.J., 20, 54, 1943.
A.J., 61, 97, 1956.
Bull. Abastumani, No.18, 15, 1955.

14. 1961Hubbl.B...0000S
Re:NGC 0205
E pec / S01
July 20/21, 1950
85 min
Enlarged 2.8X
NGC 0205 is one of the two elliptical companions of M31.
Note how the outer parts of NGC 0205 are highly resolved into
stars on this 200-inch plate. The brightest of these stars
are all of about the same apparent brightness. This explains
the observational fact that resolution does not occur
until a critical exposure time is reached, at which
time the entire smooth image of the galaxy breaks up into
individual stars.
NGC 0205 has two features uncommon to pure elliptical systems.
(1) There are two dust patches near the centerof the galaxy.
They are not completely opaque. They do not show
in this illustration because of the high stellar
density near the center, but a negative reproduction of a
good 100-inch plate taken by Hubble and published in
Sky and Telescope, January 1954, does show the feature.
(2) A few blue supergiant stars appear to be associated
with dust patches in the center of NGC 0205. A negative
print from an ultraviolet plate taken by Baade with the
100-inch is given in Pub. Michigan Obs., 10, 10.
The intensity gradient of NGC 0205 suggests the pres-
ence of an outer envelope similar to that of S01 galaxies.
perhaps this is a transition case.
NGC 3898
Mar. 25/26, 1955
103aO + WG2
30 min
Enlarged 6.0X
NGC 3898 is the Sa prototype of multiple-arm spirals of
the NGC 2841 [Sb, pg. 14] type. The arms in NGC 3898 are
very tightly wound about a large amorphous center. The
arms themselves are made up of individual segments
which cannot be traced as complete arcs for more than
20" to 30". NGC 3898 is one of the earliest members of a
sequence of multiple-arm spirals which can be traced from
late Sc to early Sa. Among the members of this sequence
are M1O1 (pg. 27), NGC 5055 (pg. 15), 488 (pg. 15) 2841
(pg. 14), NGC 3898 (this galaxy), NGC 2811 (pg. 11), and
NGC 1302 (pg. 9).

15. 1956AJ.....61...97H
Re:NGC 0205
HMS Note No. 004
Hydrogen lines unusually strong (HMS Plate IVb).

16. 1918PLicO..13....9C
Re:NGC 0205
The companion n.p. the nebula in Andromeda. The bright central portion is
about 2' in diameter, showing traces of rather irregular spiral structure; the
nucleus is almost stellar. There are two small dark patches near the brighter
central portion. Very much fainter matter forms the outer portion of the
nebula in an oval about 8' x 3'; no whorls can be made out in this outer
portion; doubtless a spiral of the Andromeda type. 2 s.n.

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