Date and Time of the Query: 2019-03-24 T16:10:49 PDT
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Notes for object IC 0750

7 note(s) found in NED.

1. 2001A&A...379...54H
Re:KPG 313B
KPG313B. The galaxy is classified as Sab:sp. Our sharp/filtered and (B-I)
images show an inclined galaxy with extended and apparently warped arms.
The (B-V)_T_^0^ colour is redder than that corresponding to its
morphological type. RC3 reports total asymptotic B and V magnitudes with
associated errors of 0.15 mag that imply a (B-V) colour in agreement to
our observed value. The I/A class for the pair is DI.

2. 1999A&AS..135..429B
Re:PGC 037719
May be confused by galaxies with unknown radial velocity and/or
morphological type.

3. 1994CAG1..B...0000S
Re:IC 0750
Karachentsev 313 [with IC 0749]
Aug 7/8, 1980
103aO + GG385
45 min
IC 750 forms a close pair with IC 749 (SBc;
panel 306) at a separation of 3.3'. The redshifts
are closely the same, v_o(749) = 827 km/s and
v_o(750) = 742 km/s. At the mean redshift
distance of 16 Mpc, the projected linear separation
is small, at 15 kpc.
The morphology of IC 750 is similar to that
of both NGC 4522 and NGC 4433 on the
preceding panel. The surface brightness of the
central parts of IC 750 is very high, but the
resolution into individual HII regions is not nearly
as great as it is in the companion. The normal
morphology of IC 749 shows no evidence of tidal
perturbation, but, like the morphology of NGC 4522
and NGC 4433, the form of IC 750 is
outside the ridge-line of the classification
sequence (i.e., it is outside the middle line through
the morphological box).

4. 1993A&AS...97..887B
Re:IC 0750
IC 749/750 are two strongly interacting galaxies separated by about 3.5'
(11 kpc). We have observed both galaxy nuclei in CO(1-0) and CO(2-1)
along with a cut from one center to the other, taking spectra every 20".
While little molecular gas was found in IC 749, IC 750 appears very rich
in molecular gas, although not at the central coordinates taken. The
molecular gas appears to be on the side opposite IC 749, which is why the
spectra shown are convolved about (7,-7). From Keel et al. (1985) the
nuclear (0.3 kpc) H{alpha} emission from IC 750 is nearly ten times as
great as from IC 749 but they class the stellar continuum of IC 750 as
coming from an older population, close to that of an elliptical galaxy
and the H{alpha} width is less than that of IC 749. The radio continuum
in IC 750 (H87) reveals a strong 10 mJy nuclear source about 0.5" in size
(coinciding with our 0,0 coordinates) with a total flux density of 84
mJy. The 1.49 GHz emission from IC 750 lies roughly perpendicular to the
line between the galaxy centers and does not coincide with the CO
emission. The CO(2-1) emission at the (0,0) position is actually quite
weak. Van Driel et al. (in prep.) discuss the effect of the interaction
on the HI and H_2_ distributions.

5. 1976RC2...C...0000d
Re:IC 0750
= Holm 313b
= Kara[72] 313b
Pair with IC 0749 at 3.3 arcmin

6. 1973UGC...C...0000N
Re:UGC 06973
Very red object
Smooth halo or outer disk
See UGC 06962

7. 1964RC1...C...0000d
Re:IC 0750
= Holm 313b
Pair with IC 0749 at 3.3 arcmin.
See also HA, 105, 230, 1937.

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