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Notes for object NGC 1073

14 note(s) found in NED.

1. 2005ApJS..157...59L
Re:NGC 1073
NGC 1073 (at a distance of 15.2 Mpc) is a barred Sc spiral galaxy. ULX1(IXO 5)
is close to a star-forming knot on the spiral arm, and its luminosities
increased by more than 50% between two observations separated by half a year.

2. 2005A&A...437..837D
Re:NGC 1073
Figure 10 shows the observational gradients of [N II]/[O III] and [O
III]/H{beta} and our model results for NGC 1073. The angular scale 1" = 55.4 pc
(Martin & Roy 1994) was assumed. The four innermost points represent H II
regions located in the bar of NGC 1073, which may have a secondary ionization
source (Martin & Roy 1994), so our analysis did not extend to these points. The
observational data do not include the emission lines needed for sulfur abundance
determinations, so all models were built considering a solar S/O ratio. We
derive an effective temperature gradient represented by T_eff_ (10^4^ K) =
(0.073 +/- 0.004) R (kpc) + (3.89 +/- 0.02) and a mean ionization parameter of
log U ~~ -2.80 +/- 0.05. The absence of an observational [O II]/[O III] line
ratio can make these results somewhat uncertain, because this ratio is strongly
dependent on those two parameters (Dors & Copetti 2003; Morisset et al. 2004).
In Fig. 11 our O/H gradient is compared with the one obtained by Martin & Roy
(1994) via a [O III]/H{beta} vs. O/H calibration. For NGC 1073 we derive an O/H
gradient of 12+log (O/H) = (-0.048 +/- 0.012) R (kpc) + (8.74 +/-0.06), very
consistent with the one derived by Martin & Roy (1994).
We obtained a mean value of log (N/O)= -1.05 +/- 0.05 and no systematic
variation of N/O with R was found. The N/O abundances obtained for H II regions
in NGC 1073 are larger than the ones for similar oxygen abundance objects found
in other galaxies. In order to prove that this overabundance of nitrogen is not
an artefact of our models, we use Fig. 12 to plot [N II]/[O III] vs. [O
III]/H{beta}, in order to show that the [N II] lines measured by Martin & Roy
(1994) in H II regions of NGC 1073 are relatively stronger than the ones
obtained in 34 other spiral galaxies by Bresolin et al. (1999), van Zee et al.
(1998), Edmunds & Pagel (1984), Deharveng et al. (1988), Henry et al. (1992),
and Ferguson et al. (1998). England et al. (1990) suggested that NGC 1073 may
have suffered an interaction in the past, and Martin & Roy (1994) pointed out
that the intense star formation activity in its bar can be a signature of this
interaction. As a result, the overabundance of nitrogen in the NGC 1073 disk
could have possibly been yielded by a distinct chemical evolution due to an
encounter with another galaxy. Further abundance studies based on emission-line
measurements obtained with a more reliable observational technique than the one
used by Martin & Roy (1994) are necessary to confirm the N/O overabundance in H
II regions of NGC 1073.

3. 2004A&A...418..877A
Re:NGC 1073
NGC 1073: in the CP02 catalog there are two X-ray sources in this galaxy
which are at about the same distance from the nucleus and much brighter
in X-rays than the source which they designated IXO5 (this is associated
to a HII region if our identification was correct, as said). These two
were not include in the IXO CP02 catalog because it was known that they
were quasars (Arp & Sulentic 1979; Burbidge et al. 1979). But clearly
these fit the definition of ULXs and are listed in Table 1. Also
included in Table 1 is the third known quasar in NGC 1073 which has
log L_X = 38.7 erg s^-1^ only slightly above the general criterion for
ULXs. The strong X-ray quasar with z = 1.411 is also a strong radio
source. Since high redshift compact objects which are strong in both
X-ray and radio are generally now regarded as BL Lac type objects it is
noted in the last column of Table 1.

4. 2002ApJS..143...73E
Re:NGC 1073
NGC 1073.---SB(r)ab: Strong, thin bar, and very elliptical bulge. Weak
grand-design arms form an inner ring. Arms originate at the ends of
the bar and are roughly at right angles to the bar. The B-band type is
SBc for all classifiers. We classify NGC 1073 substantially earlier in
the H band because the outer, open spiral arms are very faint in the
near-IR, leaving the inner arm/ring structure as the spiral feature
that dominates the classification.

5. 2002AJ....124..675C
Re:UGC 02210
Diffuse radio source. The compact radio source in the southern arm of
UGC 02210 = NGC 1073 is quasar (Arp & Sulentic 1979).

6. 1999A&AS..138..253B
Re:NGC 1073
NGC 1073 - SN 1962L: no patches are visible in the immediate
surroundings of the SN. An extended patch instead is visible off the 5
arcsec ring to the south-east of the SN position.

7. 1997A&A...326..449M
Re:NGC 1073
NGC 1073. There is a clear SF asymmetry in the bar with the two brightest HII
regions located to the SW. A faint "bridge" appears between these regions but
it could be an artifact of the continuum subtraction. The H II regions are
confined to one axis. No SF enhancement is observed at the end of the stellar
bar. Although there are no obvious companions near the galaxy (Martin & Roy
1994), England et al. (1990) found an asymmetry in the HI distribution and
suggested that an interaction may have perturbed the galaxy in the recent past.
Indeed, simulations of a strong interaction between a large galaxy and a small
one by Noguchi (1988) revealed striking morphological similarities with NGC
1073. The central part of the galaxy is moderately gas-rich (Hunter & Gottesman
1996). Neither Kaufman & Contopoulos (1996) or England et al. (1990) mention
the presence of inner Lindblad resonances (ILRs) in NGC 1073. The radial O/H
gradient across the disc is shallow, suggesting strong radial gas flows (Martin
& Roy 1994).

8. 1994CAG1..B...0000S
Re:NGC 1073
NGC 1068 Group
Hubble Atlas, p. 49
Nov 6/7, 1980
12 min
NGC 1073 is the prototype SBc galaxy. The
arm pattern is open. The bar contains HII
regions, unlike the situation in most SBb galaxies
where no recent star formation occurs, evidenced
by the smoothness of the bar light.
The redshift listed for NGC 1073 in the
RSA2 is v_o = 1318 km/s; evidently the velocity
listed in Humason, Mayall, and Sandage (1956)
is incorrect.
NGC 1073 has been considered a member
of the NGC 1068 group, which also contains the
RSA galaxies NGC 1055 (Sbc; panel 194),
NGC 1087 (Sc; panel 279), and perhaps NGC 936
(SB0/SBa; panel 106) and NGC 941 (Scd; panel
The arms in NGC 1073 are well resolved
into bright HII regions, the largest of which have
halo diameters of about 2". Individual brightest
stars appear to resolve starting at about B = 21,
but unambiguous discrimination of HII regions
from stars has not been done by the standard
methods at this writing (1991).

9. 1993A&AS...97..887B
Re:NGC 1073
NGC 1073 is a strongly barred SBc(rs)II with generally weak emission at
all wavelengths. Our CO detection is dubious. The optical magnitude,
size, color indices and IRAS data are essentially identical to NGC 1042.
The two real differences are the bar and the larger HI column density in
NGC 1073. The line widths and inclinations are similar.

10. 1976RC2...C...0000d
Re:NGC 1073
In the NGC 1068 Group.
Coll.Int. CNRS, Paris, 194, 1965.
IAU Symp. No.38, 23, 1970.
Ap. J., 194, 559, 1974.
Photometry: (7 Color)
Izv. Crimea Obs., 45, 162, 1972.
IAU Symp. No.44, 62, 1972.
Old HMS velocity (Source C) rejected.
See A.J., 76, 22, 1971.
HII Regions:
"Atlas and Catalogue", Univ. Washington,Seattle, 1966.
Ap. J., 155, 417, 1969.
Ap. J., 194, 559, 1974.
Distance Modulus:
Ap. J., 194, 559, 1974.
C.R. Acad. Sc. Paris, 256, 5284, 1963 = Publ. O.H.P., 6, No. 41.
Ann. Ap., 27, 327, 1964 = Publ. O.H.P., 7, No. 24.
Ann. Ap., 27, 319, 1964 = Contr. Asiago. No. 159.
Coll.Int. Novae & SN CNRS, Paris, pp.194-202, 1965.
Abh. Univ. Kasan, 125 No. 7, 1965.
Bull. Kasan Obs., No. 38, 1965.
Tokyo Ast. Bull., No. 176, 1967.
Radio Observations:
Austral. J. Phys., 19, 883, 1966.

11. 1973UGC...C...0000N
Re:UGC 02210
SB(rs)c (de Vaucouleurs), Sc+ (Holmberg)
SN 1962l
(rs) 2.5 x 2.0, inner diameter 1.7 x 1.4
UGC 02188 = NGC 1068 at 1^deg^24'

12. 1964RC1...C...0000d
Re:NGC 1073
In the NGC 1068 Group.
Very small, bright nucleus
in narrow bar: 1.2 arcmin x 0.2 arcmin (with bright knots).
Smooth, partially resolved (r): 1.7 arcmin x 1.6 arcmin,
Many filamentary arms.
SN 1962
H.A.C. 1577, 1962.
L'Astronomie, 76, 392, 1962.
I.A.U. Circ. 1809, 1962.
I.A.U. Circ. 1820, 1963.
I.A.U. Circ. 1821, 1963.

13. 1961Hubbl.B...0000S
Re:NGC 1073
Nov. 11/12, 1950
30 min
Enlarged 2.5X
The arms do not begin from the ends of the bar but rather
about 30 degrees from the bar's termination. There is no
complete circular ring. The arms and the bar are resolved
into many knots. There are no straight absorption lanes
in the bar.

14. 1956AJ.....61...97H
Re:NGC 1073
HMS Note No. 017
Slit on central bar.

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