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Date and Time of the Query: 2019-02-23 T10:34:19 PST
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Notes for object Leo III

10 note(s) found in NED.


1. 1999ApJ...519...89C
Re:Leo A
Leo A.-This dwarf Irr galaxy is a possible member of the Local
Group. We did not find any X-ray emission from this galaxy.

2. 1999AJ....118.1657C
Re:Leo A
Leo A provides a stark contrast to the other galaxies in this
sample. The color-magnitude data are from Tolstoy et al. (1998). The
smallest, most isolated galaxy in the sample, the CMD of Leo A shows the
unusual feature of a dominant blue supergiant branch, evidence for
strong recent star formation. Leo A's giant branch lies to the blue of
IC 1613's, indicating its lower metallicity (and/or age). The blue,
vertically extended RC in Leo A suggests that this galaxy is dominated
by an ~1 Gyr population. Deep WIYN and Multiple Mirror Telescope images
of Leo A have failed to reveal an extended Baade's sheet population of
red giants that would be indicative of significant early star formation
(A. Saha 1998, private communication; Tolstoy et al. 1998). The low
metallicity and high gas fraction of Leo A are all consistent with a
galaxy that has not had a major star formation episode until quite
recently. Leo A is even more isolated than IC 1613 (its nearest
neighbors are the Leo I and Leo II dwarf spheroidals, more than 450 kpc
away), and it must stand as a counterexample to the Tucana dwarf, a
purely old system (Da Costa 1998), in evolutionary studies of small,
isolated galaxies.

3. 1997AstL...23..656G
Re:Leo A
Leo A. Demers et al. (1984) (photographic photometry). The estimates of V(5)
obtained from the color-magnitude diagrams of Hoessel (1986) and Sandage (1986)
are the same.

4. 1997AstL...23..644G
Re:Leo A
LeoA. Sandage (1986) (Cepheids); Sandage (1986) (nos. 90, 30, 52), (nos. 65,
64, 39). Not all of the bright stars were photometered by Demers et al. (1984).

5. 1994CAG1..B...0000S
Re:Leo A
ImV
PH-95-S
Jan 3/4, 1952
103aO + WG2
15 min
The dwarf galaxy Leo A (RA_50_ = 9^h^ 57.55^m^,
Dec_50_ = +30^deg^ 59.2') was discovered by Zwicky
(1942) in one of the first surveys done with the
Palomar 18-inch Schmidt beginning in 1936.
Photometry of the stellar content (Sandage
1986b) shows that the brightest blue stars begin
to resolve at B = 19 and the brightest red
supergiants at V = 19. Leo A is one of the faintest
dwarfs of type Im in or near the Local Group. If
the distance modulus is m - M = 26 (Sandage
1986b), its absolute magnitude is M_B_ = -13.
Leo A has a redshift relative to the centroid
of the Local Group of v_o = -32 km/s (Sandage
1986a). It is, therefore, a Local Group member
near the zero velocity surface that separates the
Local Group from the cosmological expansion
field. It is evident from the velocity and distance
data that the kinematic radius of the Local Group
in the direction of Leo A extends to a distance of
about 1.6 Mpc from the Sun.

6. 1994AJ....107.1328v
Re:LEO A
Leo A = DDO 69
This dwarf irregular galaxy is listed as a local Group member by
Kraan-Korteweg & Tammann (1979). However, Demers et al. (1984) obtain
(m - M)_0_ = 26.8+/-0.4, corresponding to a distance of 2.3+/-0.4 Mpc. A
slightly smaller, but very uncertain, distance modulus (m - M)_0_ = 26+/-1
has been advocated by Sandage (1986a). The position of Leo A in the
V_sun_ versus cos{theta} plot is consistent with membership in the local
Group.

7. 1976RC2...C...0000d
Re:[RC2] A0956+30
= DDO 069
Dwarf Leo A system.

8. 1973UGC...C...0000N
Re:UGC 05364
DDO 69, A0956 in RC1
Ir I (Holmberg)
Ir V (DDO)

9. 1966AJ.....71..922v
Re:DDO 069
= Leo A
= Leo III.
Possible member of Local Group.

10. 1964RC1...C...0000d
Re:[RC1] A0956
= Zwicky Object in Leo
= Leo A
Photograph:
Sci. Monthly, 51, 400, 1940.
Applied Mech., Th. Von Karman Anniv. Vol., p.137, Plate I, 1941.
Magnitude and Distance:
Mt. Wilson Report, 20, 1939-1940.


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