Date and Time of the Query: 2019-05-25 T18:36:05 PDT
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Notes for object NGC 3110

5 note(s) found in NED.

1. 2004AJ....127..736H
Re:NGC 3110
A12. NGC 3110 NGC 3110 (Fig. 1l) is a distorted spiral galaxy with a
small companion ~1.8' (~36 kpc) to the southwest (MCG-01-26-013). An
H{alpha}+[N II] image of this galaxy (Dopita et al. 2002) shows bright
H{alpha} knots along the two spiral arms. Our H{alpha} image also shows
the knots, as well as a possible barlike structure through the nucleus
with P.A. ~ 60deg and length ~20". The barlike structure cannot be seen
in our continuum image. Zink et al. (2000) investigated the distribution
of 100 micron emission and concluded that the disk or arms of NGC 3110
contribute up to 35% of the total FIR flux.
The companion galaxy MCG-01-26-013 (Fig. 2a) shows H{alpha} emission
associated with the nucleus (Dopita et al. 2002). There is also an
H{alpha} source ~3" east of the nucleus.

2. 2002ApJS..143...47D
Re:IRAS 10015-0614
IRAS 10015-0614 (NGC 3110).---This galaxy is paired with MCG
-01-26-013 at a separation of 1.9'. Both the R-band continuum and
H{alpha} images exhibit strong knots in the spiral arms of NGC 3110.
The H{alpha} emission in MCG -01-26-013, however, is concentrated
toward its nucleus. The IRAS source has been associated with NGC 3110
rather than its companion (Zink et al. 2000). NGC 3110 has been
classified as H II region--like by Corbett et al. (2002b) using
optical spectral diagnostics.

3. 2000ApJS..131..413Z
Re:NGC 3110
5.2.7. NGC 3110
NGC 3110 is a low-inclination spiral with a companion about 2' to the
southwest near the end of one of its two distinct spiral arms (Fig. 8).
The system has a log (L_FIR_/L_sun_) = 10.96 and a rather large gas mass
(as estimated from CO detection by Sanders et al. 1991) of
2 x 10^10^ M_sun_. This galaxy presents a fairly unique opportunity. Since
it is not too far away (65 Mpc; CHSS), it subtends a substantial angle
across the sky (>60" x 30"), but it is still very luminous. It provides a
good opportunity to resolve a fairly typical FIR luminous galaxy.
The core of NGC 3110 is clearly resolved (Fig. 8) and our observations
indicate D_g_ ~ 24" and a D_e_ ~ 13". However, the photometry strongly
suggests even further extension. The detector 5 flux (corrected for minor
miscentering) and sum of detectors 1-10 flux both are ~33% below the IRAS
flux (Table 4). This suggests that not only the core that was resolved is
extended, but also that the FIR emission area is extended enough that a
substantial portion of the FIR flux escaped of our detector array entirely.
From the flux received in detectors 11-20 (not shown here; perhaps 5 Jy)
and assuming a similar amount of FIR-emitting area is spread on the other
side of the detector 1-10 arm (to the east), much of the flux discrepancy
can be accounted for. The almost exact coincidence of the IRAS source with
NGC 3110 suggests that little of the IRAS flux comes from the companion to
the southwest. So it can be concluded that the core of NGC 3110 is extended
at least on a scale of 13", and beyond the core, the disk or arms of the
galaxy contribute up to 35% of the total FIR flux.
Using the derived sizes of the core, our array-summed 100 micron flux,
and a 60 micron flux scaled so that the S_100_/S_60_ ratio remains the
same as for the BGS fluxes as well as a 1.25 mm point (Carico et al. 1992)
scaled similarly, one obtains a core dust temperature of 32.1 K and a
rather high A_V_ of 8.3. The CHSS radio flux includes both the core and
the disk so one only has the system q of 2.22 using BGS fluxes.

4. 1997ApJS..108..449G
Re:NGC 3110
The spectrum is of the brighter galaxy, oriented approximately north-
south. We note that our measured line strengths are much fainter than
those of Marconi et al. (1994). Since our line measurements would show
this galaxy to have among the weakest emission lines in our sample, the
spectrum in this paper may be in error.

5. 1963MCG3..C...0000V
Re:MCG -01-26-014
Pair with MCG -01-26-013, {rho} = 1.9 arcmin.

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