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Date and Time of the Query: 2019-05-25 T22:09:30 PDT
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Notes for object IC 0010

9 note(s) found in NED.


1. 2005ApJ...622..217W
Re:IC 0010
IC 10
A distance modulus of 24.9 +/- 0.2 is found in Hunter (2001), which
is at variance with the others used here. Extinction is a large
factor in the disagreement.

2. 1997AstL...23..656G
Re:IC 0010
IC 10. There is a great number of blue stars in the color-magnitude diagram of
Massey and Armandroff (1995). By way of illustration, Fig. 1a shows the LF for
which we selected the blue stars using the more rigorous criterion
(B-V)_0_<0.2. Nevertheless, the magnitude V(5) turns out to be approximately
3^m^ brighter than the expected value. In contrast to Georgiev et al. (1997b),
we failed to obtain a satisfactory estimate of the distance modulus. It may be
concluded that either the contribution of blue Milky-Way stars in this case is
particularly large, or IC 10 exhibits a great excess of bright blue stars. We
favor the first of these alternatives. The total magnitude B(g) of this galaxy
may also be insufficiently reliable. In such cases, the LF method is
inapplicable.

3. 1995ApJS...98..477H
Re:IC 0010
This Im galaxy does not have an obvious nucleus. The brightest knot
(Fig. 2) shows extremely strong emission lines. There may be a hint of
features from Wolf-Rayet (W-R) stars; there is a low-contrast, broad
emission complex near 4650 A and a very faint broad base in the
H{alpha} profile. (See notes on NGC 1156 and NGC 4214 for more
information.) Unfortunately, the region around 4650 A happened to have
landed on a defective portion of the chip; thus additional data are
needed to confirm whether the apparent W-R features are real.

4. 1994AJ....108.2128C
Re:PGC 001305
PGC 001305 = IC 10. Type = .IB.9.. (no question mark), B_T_ = 11.81M +-
0.12, (B-V)_T_ = 1.43 +- 0.05, (U-B)_T_ = 0.3 +- 0.1.

5. 1994AJ....107.1328v
Re:IC 0010
IC 10
This galaxy was first mooted as a possible local Group member by
Hubble (1936). From its distance and radial velocity Yahil et al. (1977)
concluded that IC 10 was a probable member of the local Group. A thorough
discussion of the distance to IC 10 is given by Massey et al. (1992) and
by Yang & Skillman (1993). Following Hodge & Lee (1990) a distance of
1.25 Mpc will be adopted for this highly obscured [E(B - V) = 0.87] dwarf
irregular galaxy. The spatial separation between IC 10 and M31 (assumed
to be at a distance of 725 kpc) is only 0.7 Mpc. On the basis of its
small distance and location in the V_sun_ versus cos{theta} diagram IC 10
is almost certainly a physical member of the local Group. `

6. 1976RC2...C...0000d
Re:IC 0010
Local Group Member
Photograph:
P.A.S.P., 77, 272, 1965.
Vistas in Astr., 14, 206, 1972.
Ap. J., 194, 559, 1974.
Photometry:
P.A.S.P., 77, 272 , 1965.
Vistas in Astr., 14, 231, 1972.
HII Regions and Distance Modulus:
Ap. J., 194, 559, 1974.
HI 21cm:
A.J., 69, 490, 1964.
A.J., 69, 521, 1964.
Ap. J., 150, 9, 1967.
Astr. Ap., 18, 321, 1972.
Astr. Ap., 31, 97, 1974.
Radio Observations:
A.J., 78, 18, 1973.

7. 1973UGC...C...0000N
Re:UGC 00192
IBm (de Vaucouleurs)
Strongly obscured, very uncertain diameter
Not in CGCG
Integrated magnitude B(0) = 13.33 in RC1

8. 1964RC1...C...0000d
Re:IC 0010
Member of the Local Group.
Mt. Wilson Velocity for bright emission patch in the south-following part:
V = -88 km/sec.
Photograph:
P.A.S.P., 47, 317, 1935.
A.J., 67, 432, 1962.
Spectrum:
P.A.S.P., 53, 123, 1941.
HI Emission:
A.J., 66, 294, 1962.
A.J., 67, 431, 1962.
Harvard Radio Ast. Rep., 102, 1962.
Epstein, Harvard Thesis, 1962.

9. 1918PLicO..13....9C
Re:IC 0010
A small area of diffuse nebulosity about 3' x 2'; very patchy, with a number of
nebulous condensations. Exceedingly faint. 6 s.n.


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