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Notes for object NGC 4244

15 note(s) found in NED.


1. 2007MNRAS.382.1552L
Re:NGC 4244
NGC 4244: Fig. 2 shows a prominent nucleus and a central dust lane. The nucleus
of NGC 4244 corresponds to a star-forming region (Ho et al. 1997a).

2. 2004ApJS..151..193S
Re:NGC 4244
4.2.10. NGC 4244 NGC 4244 is a nearby, low-mass, Scd galaxy (M_tot_
{approx} 10^10^ M_{sun}_ Fry et al. 1999) at a distance of 3.6 Mpc. The
current star formation rate is low, based on the low IR (Rice et
al. 1988) and H{alpha} luminosities (Hoopes et al. 1999). No evidence
for a radio, UV, or X-ray-emitting halo has been found (Bregman &
Glassgold 1982; Schlickeiser, Werner, & Wielebinski 1984; Deharveng et
al. 1986; this paper). Deep H{alpha}imaging (Hoopes et al. 1999)
demonstrates that warm ionized gas at T ~ 10^4^ K is confined to within
40" (700 pc) of the disk of the galaxy. No nuclear activity is known in
NGC 4244.
Despite the relatively long Chandra observation, there is a remarkable
lack of X-ray emission from NGC 4244, with little or no concentration of
X-ray point sources within the optical confines of the galaxy (see
Fig. 13). There is only a weak, ~3 {sigma}, detection of residual
emission within the disk after point source removal, and only an upper
limit of fX < 1.6 x 10^-14^ ergs s^-1^ cm^-2^ (3{sigma} upper limits in
the 0.3-2.0 keV energy band, L_X_ < 2.5 x 10^37^ ergs s^-1^) could be
obtained on diffuse emission from the halo.

3. 2003A&A...398..467K
Re:NGC 4244
NGC 4244. A large edge-on Sc galaxy extends far beyond the WFPC2 field.
Its periphery was resolved into stars by Karachentsev & Drozdovsky
(1998), who estimated the galaxy distance to be 4.5 +-0.9 Mpc from the
photometry of the brightest stars. The CM diagram (Fig. 2) shows ~15000
stars, in particular pronounced populations of blue stars and AGB
stars. The TRGB position, 24.25 +- 0.22 mag, corresponds to a distance
of 4.49 +- 0.47 Mpc in close agreement with the distance estimate via
the brightest stars.

4. 2002AJ....124..675C
Re:UGC 07322
Very extended galaxy; the NVSS flux density may be too low.

5. 2000MNRAS.319...17L
Re:NGC 4244
NGC 4244: No emission was detected in the ROSAT HRI observations of this
galaxy. A 2{sigma} upper limit for a point source located in the nuclear
region of the galaxy can be found in Table 5.

6. 1999ApJ...522..669H
Re:NGC 4244
This is a nearby galaxy (3.1 Mpc), so we can resolve a great deal of
detail in the ionized disk (see Fig. 3). The H II regions distribution
is extended in the vertical direction, a result perhaps of a weaker disk
potential (Olling 1996). There are a few H II regions as far as 700 pc
above the midplane. DIG is clearly visible in the disk, spread between
several bright H II regions. It is immediately obvious, however, that an
extensive DIG layer such as in NGC 891 is absent in this galaxy. Some
short filaments exist in the central regions of the galaxy, but overall
the DIG layer is confined to the disk. The galaxy appears quiescent in
H{alpha}, and the low H{alpha} luminosity and low FIR surface brightness
imply that there is relatively little star formation occurring. Most of
the H II regions are small and faint, except for two bright complexes on
either end of the disk. The absence of long bright filaments, such as
those seen in NGC 891 and NGC 4631, imply that the galaxy also lacks any
visible disk-halo interaction.

7. 1994CAG1..B...0000S
Re:NGC 4244
Canes Venatici I Group
Hubble Atlas, p. 25
ScdIII
PH-124-MH
March 20/21, 1950
103aO
30 min
NGC 4244 is a member of the very nearby
CVn I Group (de Vaucouleurs 1975), which is
the B4 Group of Kraan-Korteweg and Tammann
(1979) in the Ursa Major complex. The redshift
of NGC 4244 is v_o = 249 km/s.
The galaxy is highly resolved into individual
stars beginning at about B = 18. However, study
of its stellar content will be difficult because the
galaxy is almost exactly edge on.

8. 1994CAG1..B...0000S
Re:NGC 4244
Canes Venatici I Group
Hubble Atlas, p. 25
ScdIII
H-2507-H
March 5/6, 1948
103aO
30 min
The image of NGC 4244 in the light print at
the bottom of the column was made from a different
original plate than was used for the heavy
print above it.
The dust lane nearly bisects the very thin
plane, showing that the galaxy is closely edge on.
There is neither a central bulge nor a luminous
halo. HII regions are present, the largest of
which resolve at the 5" level.
The angular diameter of the NGC 4244 disk
is large, at D_25_ = 16'.

9. 1976RC2...C...0000d
Re:NGC 4244
Photometry (12 Color):
Ap. J., 145, 36, 1966.
Rotation Curve and Systemic Velocity:
Astr. Ap., 8, 364, 1970.
HII Regions:
"Atlas and Catalogue", Univ. Washington, Seattle, 1966.
HI 21cm:
Ap. J., 142, 616, 1965.
Ap. J., 150, 8, 1967.
Astr. Ap., 23, 93, 1973.
HI 21cm (upper limit in halo):
Phys. Rev. Let., 17, 1203, 1966.

10. 1973UGC...C...0000N
Re:UGC 07322
SA(s)cd: (de Vaucouleurs), Sc+ (Holmberg)

11. 1964RC1...C...0000d
Re:NGC 4244
Very small, bright nucleus or star? Dark lane.
Lick 13, Lund 9, and Lund 10 dimensions are for the bright part only.
(B-V)(interpolated)
Photograph and Orientation:
P.A.S.P., 53, 269, 1941.
Ap. J., 127, 487, 1958.
Radio Emission:
M.N.R.A.S., 122, 479, 1961.
HI Emission:
A.J., 66, 294, 1962.
A.J., 67, 437, 1962.

12. 1961Hubbl.B...0000S
Re:NGC 4244
Sc
PH-151-MH
Apr. 12/13, 1950
103aO
30 min
Enlarged 0.89X
NGC 4244 is undoubtedly a late Sc galaxy seen on edge.
There is no nuclear bulge; the entire surface is resolved
into stars; and the dust lanes, although present, are not
at all conspicuous. This galaxy must be near by because
it is resolved into stars throughout its surface. They are
individual stars and not HII regions. The reproduction
is too overexposed to show the resolution in the nuclear
region which is visible on the original plate. The estimated
distance modulus of NGC 4244is between (m-M) = 26.5
and (m-M) = 27.0. The galaxy is more distant than members
of the Local Group but not so distant as the M81 and
M101 groups.

13. 1957HPh....53..275d
Re:NGC 4244
SA(s:)cd
(Plate 42)
The spheroidal component is now inconspicuous in the center
of a very extensive, flat component in which the spiral
pattern of bright and dark material shows much irregularity
and very many resolved knots.
Compare with NGC 7793 (Plate 20), and NGC 6643 (Plate 24).

14. 1956AJ.....61...97H
Re:NGC 4244
HMS Note No. 133
Redshift is for approximate center of system.

15. 1918PLicO..13....9C
Re:NGC 4244
Vol. VIII, Plate 31. A fine, quite bright, edgewise spiral, 13' x 0.9' in p.a.
50^deg^. An irregular dark lane runs down the middle. A few almost stellar con-
densations. Apparently no nucleus; though there is a star of magn. 14 in this
position. See Abs. Eff. 10 s.n.


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