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Notes for object WLM

11 note(s) found in NED.


1. 2009AJ....138.1203M
Re:WLM
A.3. WLM WLM was the third most populous galaxy in our survey with 191 regions
marked, 165 of which made it into our final data set. Its distance was typical
at 1.0 Mpc. This galaxy is distinct in having the oldest average star-forming
regions in all our sample. The cluster formation rate appears to have been
relatively constant until it stopped about 22 Myr ago. The minimum detectable
mass at 500 Myr is about 1 * 10^3^ M_sun_. This galaxy has a large fraction of
star-forming regions beyond R_H{alpha}_: 31 out of the total 165. UV regions are
seen to a radius of 7.4', while H{alpha} drops out beyond 4.2'. In Figure 3,
there appears to be a slight drop in the mass beyond R_H{alpha}_, amounting to a
factor of ~3.

2. 2004ApJ...608...42S
Re:WLM
WLM. A distance to this galaxy was calculated by Lee et al. (1993) based
on I-band data, adopting an absorption A(I) = 0.04 mag. Furthermore, all
of the Cepheids have periods less than 8 days, preventing us from
calculating a new distance for this galaxy.

3. 2004AJ....128...16K
Re:WLM
The Wolf-Lundmark Melotte (DDO 221, HIPASS J0001-15) is a Local Group
dwarf irregular galaxy at a distance of ~900 kpc (Mateo 1998; Dolphin
2000; Rejkuba et al. 2000). Despite its large optical diameter of
12' x 4', it appears unresolved in HIPASS. However, using Effelsberg H I
data, Huchtmeier et al. (1981) find a total H I extent of 45' (12 kpc)
and an H I mass of 5.3 x 10^7^ M_sun_. We obtained a lower value of
M_HI_ = 4.7 x 10^7^ M_sun_. Note that the WLM is, in projection, located
just northeast of the Magellanic Stream.

4. 2001ApJ...556...24Z
Re:WLM
One source (with ML = 18.1 in the longer HRI observation at
{alpha}_2000_ = 00h01m58.24", {delta}_2000_ = -15^deg^27'56.7") is closely
coincident with the cataloged optical position (Fig. 3) at 7.6" from the
SIMBAD position. The near coincidence of an X-ray source elsewhere in this
field with a moderately bright star (GSC 0583800179) of magnitude 13.3
exhibits an offset of 3.3" essentially only in declination. This is comparable
to the positional error of this X-ray source (2.7" in right ascension,
2.4" in declination), indicating that no significant systematic error has
affected the position of the central source. Otherwise, theinformation on
this central source is less than in the case of NGC 6822 (see above): There
are only HRI observations; thus, hardness ratios or spectra are not available.
The source shows no variation between the two HRI exposures that are half a
year apart. The luminosity of 3.4 x 10^36^ ergs s^-1^ is very similar to the
central source in NGC 6822, which could be right for a low-level nuclear
source. Since WLM is also an irregular galaxy, we can again only consider
it a suspicious core candidate. The flux and luminosity quoted in Table 2
refer to this source; upper limit determinations around this source yield
stricter limits for the flux and luminosity of 0.34 x 10^-14^ ergs cm^-2^ s^-1^
and 0.35 x 10^36^ ergs s^-1^, respectively.

5. 1997AstL...23..656G
Re:WLM
WLM. We use the rough estimate of V(5) that is based on the LF of Hoessel
(1986) for B magnitudes. The CCD photometry of Ferraro et al. (1989) covers
about 40% of the galaxy; if we multiply all values of the LF by 2.5, the
magnitude V(5) will be 0.2^m^ fainter. After their reduction to the CCD scale
of Ferraro et al. (1989) (by adding 0.4^m^), the photographic data of Sandage
and Carlson (l985b) yield V(5) that is 0.4^m^ fainter than the magnitude
obtained from Hoessel's data. Our estimate of V(5) is unreliable. The LF of WLM
is similar in shape to that of UGC 6572 (Fig. 1e), and the estimate of V(5) is
unstable against a small change in the number of stars used. In Karachentsev
and Tikhonov (1994) and Rozanski and Rowen-Robinson ([994), WLM markedly
deviates from the calibration relations and could be a galaxy with a deficit of
blue stars that is similar to Sextans B and Pegasus (see below).

6. 1997AstL...23..644G
Re:WLM
WLM. Sandage and Carlson (1985b) (Cepheids); Sandage and Carlson (1985b) (63V,
6V, no. 11), (nos. 22, 61, 30). The CCD photometry of Ferraro et al. (1989)
does not cover the entire galaxy. So far, no complete CCD survey of this galaxy
has been made.

7. 1976RC2...C...0000d
Re:[RC2] A2359-15
= DDO 221
= Wolf-Lundmark-Melotte System
Dwarf Im galaxy in Local Group.
Photograph:
Vistas in Astr., 14, 222, 1972.
HI 21cm:
Ap. J., 150, 8, 1967.

8. 1974UGCA..C...0000N
Re:UGCA 444
UGCA 444:
= WLM = Wolf-Lundmark-Melotte system = DDO 221 = An 2359 in RC2
Im (RC1)

9. 1968MCG4..C...0000V
Re:MCG -03-01-015
A member of the local group of galaxies, this system is described
by Wolf, and then by Lundmark and Melott (MN 86, 636, 1926). According to
de Vaucouleurs the type is Im. Redshift: +3, F; CI=0.27, Cp'=0.17.

10. 1966AJ.....71..922v
Re:DDO 221
Wolf-Lundmark-Melotte system.
Possible member of Local Group.

11. 1964RC1...C...0000d
Re:[RC1] A2359
= Wolf-Lundmark-Melotte System (= WLM)
Dwarf Im in Local Group.
See M.N.R.A.S., 86, 636, 1926.
Mt. Wilson velocities are for 2 emission patches north of the center and for a
cluster preceding the center.
Photometry:
Medd. Lund II, 128, 1950.
Star Counts:
V.J.S., 68, Heft 4, 1933 = Lund Medd. I, No 135, 1933.


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