Date and Time of the Query: 2019-03-26 T13:18:00 PDT
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Notes for object NGC 1140

9 note(s) found in NED.

1. 2007ApJS..173..538T
Re:NGC 1140
NGC 1140 (Fig. 16.39).-GALEX imaging shows additional structure in this IBm
pec:; H II Seyfert 2 galaxy, unrecognized at optical wavelengths, despite its
classification as a Type 2 XUV-disk. The UV-optical morphology is complex, with
a curved (out-of-plane?), clumpy feature oriented to the southwest visible in
both the GALEX and DSS images, plus a set of UV-only (not seen in the DSS)
sources extending north of the galaxy center for nearly 2'. The inner disk has a
diffuse-looking background of NUV bright emission, with very bright central
surface brightness at the nucleus. The peculiar UV-optical morphology of NGC
1140 is suggestive of interaction, although the galaxy is considered isolated in
the NOG catalog. As noted earlier, NGC 4383 and NGC 1140 are similar objects,
even though our classification criteria put them into different XUV classes.

2. 2000ApJ...531..776G
Re:MRK 1063
0252-102 = Mrk 1063.-Broad bump consisting of N V {lambda}4619,
N III {lambda}4640, He II {lambda}4686. Additionally, N III {lambda}4512
Si III {lambda}4565 and Si II {lambda}5046 are observed in
the blue region. The C IV {lambda}5808 line is observed in the red

3. 1999A&AS..136...35S
Re:NGC 1140
NGC 1140 -- A broad WR bump and C IV {lambda}5808 are detected by Guseva
et al. (1998).

4. 1993ApJS...86....5K
Re:NGC 1140
NGC 1140 (Mrk1063); Irr Am BCG.
NGC 1140 is a blue irregular galaxy containing a large blob of ionized
gas in its center, where the IUE aperture has been placed. Lamb, Hunter,
& Gallagher (1986) have studied the IUE spectrum of this galaxy, which
has a continuum slowly rising toward shorter wavelengths that is rich in
absorption features. The above authors have also synthesized the
spectrum, concluding that the galaxy has experienced a single burst of
star formation starting about 3 X 10^6^ yr ago and that its population is
mainly constituted of main-sequence stars with masses <~ 50 M_sun_, with
a contribution from supergiants and, possibly, Wolf-Rayet stars.

5. 1985ApJS...57..643D
Re:VV 482
Spiral with one extension.
Nucleus is approximately 10 arcsec in diameter (elongated).

6. 1977A&AS...28....1V
Re:VV 482
Plate 18 Transport out of Large Companions
MCG -02-08-019 = NGC 1140; 12.7m, V_0_=+1511 (RC1), F2e, V=12.82,
The companions are apparently not related to the spiral systems, yet
are transported out by means (seemingly) of a massive filament. The
photograph is overexposed and may be misinterpreted.

7. 1976RC2...C...0000d
Re:NGC 1140
P(b?) with outlying knots at end of "tail".
D. Wells, Univ. Texas Dissert., Austin, 1972, unpublished.

8. 1968MCG4..C...0000V
Re:MCG -02-08-019
Obvious interaction.
From galaxy F to the north, an arm starts from three bright,
not very compact knots in mutual contact, and connecting it
to a compact galaxy, N [17 mag].
{rho} = 0.7 arcmin.
Sand - Irr
vdB - Pec
Morg - I?p or ??I + tail
deV - Im or Pec?
Redshift = +1,511 km/sec
F2e; Cp'= 0.29.

9. 1964RC1...C...0000d
Re:NGC 1140
Very bright nucleus with traces of spiral structure.
Asymmetric, partially resolved short filamentary arms.
Interacting pair with outlying nebulous knots?

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