NGC 741. We extracted spectra in three contiguous, concentric annuli, with
outer radii 0.6', 2.0', and 3.8' (12, 43, and 82 kpc), respectively. In
order to obtain interesting constraints, we tied Z_Fe_ between the inner
two annuli. We found a statistically significant (delta chi^2^ = 10)
improvement in the fit if two, rather than one, hot gas components (kT =
0.67 and 1.2 keV) were used in the innermost bin; there is no evidence for
the cooler component in the outer bins. The best-fitting abundances are
somewhat higher than Z_Fe_ = 0.37^+0.37^_-0.18_ found by Mulchaey et al.
(2003), who fitted ROSAT data with a single MEKAL model (and no undetected
source component). We attribute the discrepancy to the Fe bias.
NGC 741 (UGC 1413). This E0 galaxy has no apparent nuclear dust. It has
a radio core on VLBA scales and a core-jet morphology on VLA scales. The
STIS slits were aligned approximately parallel to the galaxy major axis;
however, a certain degree of freedom was allowed in slit placement to
allow reasonable observing windows. The central kinematic and flux
properties are listed in Table 10. Very few points had sufficient
signal-to-noise to obtain good fits in these data; it has not been
included in further analysis of global kinematic properties. The fit to
the central spectrum is not improved by the addition of a broad
component. Data for this galaxy are shown in Figure 6 (see key in Fig. 1
for an explanation of these plots).
UGC 01413 (NGC 741=4C 05.10)-This galaxy is a member of a pair of
binary galaxies NGC 741/742. The VLA image displays a core residing near
the center of NGC 741 plus a knot 30" to the east of that core
(Birkinshaw & Davis 1985). Our VLBA image marginally detects a core with
no obvious extended structure associated with it.
NGC 741 is the brightest galaxy in a group of galaxies (Zabludoff &
Mulchaey 1998). There is a small apparent elliptical companion at ~8 "
(2.7 kpc assuming the same distance), which is not cataloged in NED. A
second elliptical companion, NGC 742, is located at 48" (16.2 kpc). No
dust is detected in NGC 741. We detect a central peak of emission with
low-level emission filaments extending ~2" (680 pc) toward the north,
east and south. Macchetto et al. (1996) detected an emission-gas disk
from the ground with minor and major diameters of 10.8" (3.7 kpc) and
22.6" (7.7 kpc), respectively, and with an average flux density that is
significantly below our detection threshold. This disk fills most of
the PC. NGC 741 hosts a head-tail radio source (Birkinshaw & Davies
NGC 741. This E0 galaxy is the brightest member of a group of ellipticals.
NGC 741 is situated ~50" from NGC 742, which is a head-tail radio source.
NGC 741 is situated in the tail, and the observed radio continuum fluxes
of NGC 741 (Dressel & Condon 1978; Hummel et al. 1983) may be influenced
by NGC 742. No X-ray emission has been reported and an upper limit to the
HI flux is 1 mJy (Knapp et al. 1978). We do not detect any CO emission in
this galaxy with a three sigma upper limit to the H_2_ mass of
3 x 10^8^M_sun_.
Sep 2/3, 1980
103aD + GG11
NGC 741 is the center of a small group of
compact elliptical galaxies (Humason, Mayall,
and Sandage 1956, Table XI). The mean redshift
of the three brightest group members is
5612 km/s (Palumbo et al. 1983). At this
writing (1990) it is unknown if the faint image to
the immediate right of NGC 741 itself in the
insert print is a star or is the sharp nucleus of a
sinking satellite in the envelope of NGC 741. The
E0 image farther to the right in the main print is
the companion galaxy NGC 742. It and NGC 741
itself compose VV 175 in the catalog of
Vorontsov-Velyaminov (1977). The main galaxy
is also the radio source 4C +05.10.
= III Zw 038
= VV 175
= 4C 05.10
= PKS 0153+05
Brightest E in a group.
NGC 0742 is at 0.8 arcmin, in a commom halo.
Description and Dimensions:
P.A.S.P., 80, 129, 1968.
Ap. J., 173, 485, 1972.
Ap. J., 160, 405, 1970.
A.J., 75, 695, 1970.
Ap. J., 178, 1, 1972
Ap. J., 183, 731, 1973.
Ap. J. (Letters), 179, L93, 1973.
Dynamics and Mass Determination:
Ap. J., 139, 284, 1964.
Ap. J., 157, 481, 1969
Ap. J., 189, 399, 1974.
Sov. A.J., 13, 881, 1970.
Astrophys. Lett., 6, 49, 1970.
A.J., 75, 523, 1970.
M.N.R.A.S., 167, 251, 1974.
VV 175, III Zw 38
E0 (de Vaucouleurs)
`Red elliptical, stellar nucleus' (CGPG)
Extended extremely faint corona outside 3. x 3.
Central object in a group
01 53.6 +05 21 at 3.3, 223, 0.2 x 0.2, compact, m=15.0
01 53.7 +05 25 = IC 1751 at 1.5, 342, 0.8 x 0.3, nuclear condensation
0.2 x 0.2, compact, m=15.1
01 53.9 +05 23 = NGC 742 superimposed preceding part of UGC 01413 at 0.8,
100, 0.2 x 0.2 + envelope, probably interaction, m=14.8
NGC 741 is not IC 1751 (as stated in RC1)
Star at 2.4, 312 appears to be superimposed on a galaxy
III Zw 38
m(pg) = 13.2 [CGCG]
= IC 1751
Brightest galaxy in a group of ellipticals.
NGC 0742 at 0.8 arcmin.
= NGC 0741