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Date and Time of the Query: 2019-05-21 T20:16:59 PDT
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Notes for object NGC 1042

10 note(s) found in NED.


1. 2007MNRAS.380..506G
Re:NGC 1042
NGC 1042 is an Scd galaxy forming a pair with NGC 1035 at a separation of 22
arcmin (corresponding to 177 kpc). It has a bright, small nucleus and otherwise
low surface brightness. Our line strength maps are quite patchy, due to poor S/N
in the data and consequent heavy binning of the spectra. The Mgb index takes on
low values in the very centre, and higher ones around it. H{beta} is high in the
centre and low outside it, being flat over most of the map; as can be seen also
from the line strength profiles in Fig. A1, the line strength indices stay
approximately constant over most of the field, outside a central zone of radius
~=3 arcsec. The age of the stellar populations (one-SSP analysis) reaches a
minimum in the centre. The metallicity is everywhere low, and peaks in the
centre.
The analysis of the {DELTA}{chi}^2^ contours for the central aperture, in the
continuous star formation approach, shows that this galaxy is not well described
by an SSP (see Fig. 29, fifth column). The {tau} map for age fixed to 10 Gyr
(see Fig. 8) shows a peak in the very centre, corresponding to the peak in the
H{beta} and to the minimum in the Mgb maps.

2. 2007ApJS..173..538T
Re:NGC 1042
NGC 1042 (Fig. 16.4).-This SAB(rs)cd NLAGN galaxy has along its perimeter
(predominately to the east and west) an annular zone of reduced SF intensity,
for which both GALEX and H{alpha} data (SINGG; Meurer et al. 2006) indicate a
population of distinctly lower luminosity SF regions. SDSS data does not show
the vast majority of emission features detected by GALEX in this zone. NGC 1042
belongs to a group of 11 galaxies dominated by NGC 988 (Giuricin et al. 2000),
but also containing NGC 991, which we have classified as a Type 2 XUV disk. The
H I disk of NGC 1042 has been studied in detail by Kornreich et al. (2000), who
find that the gas distribution is asymmetric, and conclude that this resulted
from interaction with NGC 1052 (also suggested by van Gorkom et al. 1986).
AlthougH It reaches past the optical disk emission, the relative H I extent is
not particularly large (D_H I_/D_25_ ; Kornreich et al. 2000) in comparison to
other spirals. The outer gas disk also does not appear substantially structured
into fi laments at 20" (~1 kpc) resolution. The net effect of these two factors
is that the XUV-disk emission in NGC 1042 does not attain truly extreme
galactocentric distances, such as found in many of our other objects.

3. 2005ApJS..157...59L
Re:NGC 1042
ULX1 (IXO 4) is on the tip of the spiral arm of this face-on Scd spiral galaxy,
for which the distance is 8.4 Mpc.

4. 2002ApJS..143...73E
Re:NGC 1042
NGC 1042.---SABc: Weak bar. Nuclear point source extends into mildly
elliptical bulge. Classic two-armed spiral. Arm emerging from the NW
side of the bulge has an HSB inner portion, becomes diffuse after
~30deg, and then becomes well defined again after ~180deg. There are
a number of bright star-forming knots in the outer part of this arm.
The NW arm winds through a total of ~270deg before fading. SE arm is
more regular, with an inner HSB region fading into an outer LSB region
and not rebrightening. This arm can also be traced through ~270deg
before fading.

5. 1998ApJ...502..582C
Re:NGC 1042
Much of the spiral structure of this galaxy is faint, diffuse, and
punctuated by bright knots (thus resembling IC 0211). The spiral
structure in the inner disk consists of two short, bright arcs.

6. 1994CAG1..B...0000S
Re:NGC 1042
Sc(rs)I-II
pair
CD-1579-S/Br
Aug 10/11, 1980
103aO + GG385
45 min
NGC 1042, redshift v_o = 1436 km/s,
forms a probable physical pair with NGC 1035
(Sc; panel 291) whose redshift is v_o = 1307 km/s.
The angular separation of 22.5', at a mean
redshift distance of 27 Mpc (H = 50), gives the
projected linear separation of 177 kpc.
Two principal arms begin near the center
but on the rim of a smooth central disk. The arms
branch into fragments, one after a quarter
revolution outward, the other after half a
revolution.
The largest of the HII-region complexes is
about 1" in diameter (core + halo).

7. 1993A&AS...97..887B
Re:NGC 1042
NGC 1042
Both the HI and CO lines are the narrowest of the survey except for
NGC 628. K83 classified the nucleus as HII region like but the H{alpha}
flux estimated is well below their sample average. C87 however detected
it and found a 1.49 GHz peak at 1' from the optical position. Our CO peak
coincides with the optical peak rather than the radio continuum peak. The
CO(1-0) line is clearly observed at exactly the central HI velocity and
is stronger than might be expected for such a low FIR flux. The Full
Width at Zero Intensity (FWZI) of the CO line is 36 km/s (7 channels at
5.2 km/s resolution) but the half power width is essentially the same.
The H_2_ mass implied is about 5 X 10^7^ M_sun_ (at 20 Mpc) or about 100
typical GMCs within a radius of 1 kpc. The velocity dispersion is very
low and the emission could come from either 100 GMCs (and/or some smaller
clouds) or a big nuclear complex although in our galaxy the nuclear
velocity dispersion is much greater.

8. 1976RC2...C...0000d
Re:NGC 1042
In the NGC 1052 Group.

9. 1968MCG4..C...0000V
Re:MCG -02-07-054
Four bright HII regions to the east.
{omega} = 16 degrees, {mu}_1_ = 72 degrees,
{mu}_2_ = 80 degrees, {phi}_1_= 330 degrees, {phi}_2_ = 290 degrees,
l_1_ = 1.8, l_2_ = 1.8.
Type:
Sand - Sc
deV - SAB(rs)cd
Redshift = +334 km/sec
CI = 0.42, Cp'= 0.79.

10. 1964RC1...C...0000d
Re:NGC 1042
In the NGC 1052 Group.
Misidentified as NGC 1048 in HA 88, 2 and also by
Morgan (1959) and by van den Bergh (1960).
Very small, very bright nucleus in smooth lens,
Faint (r): 0.9 arcmin x 0.5 arcmin.
2 main partially resolved, filamentary arms with many branching


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