Date and Time of the Query: 2018-12-16 T20:49:11 PST
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Notes for object NGC 1313

16 note(s) found in NED.

1. 2005ApJS..157...59L
Re:NGC 1313
Three ULXs are associated with the barred Sd galaxy NGC 1313 (at a distance of
3.7 Mpc), which shows scattered star-forming regions outside its D_25_ isophote.
ULX1 (IXO 7) is close to but definitely not the nucleus, and it exhibits
extremely high luminosities with L_X_ > 10^40^ ergs s^-1^. During 6 years of
observations, its luminosities vary by more than 50% and showed a dramatic
decrease from 10^40^ to ~4 * 10^39^ ergs s^-1^ in less than a month. Pakull &
Mirioni (2002, hereafter PM2002) found a H{alpha} nebula around this ULX. ULX2
is identified as SN 1978K in a star-forming region outside the D_25_ isophote.
ULX3 (IXO 8) is in another star-forming region outside the D_25_ isophote.
During the observations, it has shown variations of more than 50%. It has been
identified with a R = 21.6 mag stellar-like object (Zampieri et al. 2004) within
a bubble nebula (PM2002). Both ULX1 and ULX3 are variable on timescales of a few
tens of days.

2. 2004AJ....128...16K
Re:NGC 1313
NGC 1313 (HIPASS J0317-66) is a late-type barred spiral galaxy, which
has been studied in detail by Ryder et al. (1995) who find a large H I
disk extending roughly 18' x 10' (24 kpc x 13 kpc). We measure an
integrated H I flux density of 463+-33 Jy km s^-1^ in agreement with
F_HI_ = 484 Jy km s^-1^ obtained by Ryder et al. (1995).

3. 2002A&A...391...83B
Re:NGC 1313
NGC 1313 (Fig. 16) exhibits strong radio emission from the bar and
star-forming regions. No polarization has been detected.

4. 2001ApJS..137..139S
Re:NGC 1313
NGC 1313. - Ryder et al. (1995) cite a mean distance of 4.5 Mpc based on
tertiary distance estimators. They further state that there is no
discrepancy between the long- and short-scale distance camps in the cited

5. 1999ApJ...519...89C
Re:NGC 1313
NGC 1313.-NGC 1313 is a nearby normal spiral galaxy with many H II
regions. Colbert et al. (1995) found that the central bright X-ray
source was offset ~1 kpc from the photometric center, from analysis of
ROSAT PSPC data. They argued that the X-ray source was an
accretion-powered black hole of mass ~10^3^-10^4^ M_sun_ (for an
Eddington ratio ~10^-2^-10^-1^), but unlike an AGN since there is no
evidence for a BLR, NLR, or accretion disk. ASCA observations of the
central X-ray source in this galaxy are discussed in section 5. A
previous analysis of one of the ASCA observations was published in Petre
et al. (1994).

6. 1999A&AS..136...35S
Re:NGC 1313
NGC 1313 -- WR features are found in two regions at large galactocentric
radii of this Transition Magellanic galaxy (Walsh & Roy 1997). For
region #28 both He II {lambda}4686 and C IV {lambda}5808 are found. No
detailed information is provided about region #3. Pindao et al. (1999)
also signal the possible detection of broad He II {lambda}4686; exact
position unknown.

7. 1995A&AS..114..147B
Re:NGC 1313
This galaxy, classified in the RC3 as SB(s)d, has been defined by Sersic
(1968) as very complex. It resembles the Large Magellanic Cloud. Marcelin
& Athanassoula (1982) derived the velocity field from eight
interferograms in H{alpha}. They concluded that the rotation centre is
outside the bar, 1' south-west from the nucleus. A displacement of the
rotation centre had been previously indicated by Carranza & Aguero
(1977), but in the opposite direction. Peters et al. (1994) observed the
HI in this galaxy with the Two Element Synthesis Telescope with an
angular resolution of about 50". They concluded that within the
observational errors, in fact the nucleus is the centre of rotation.
Harnett (1987) observed this galaxy in the radio continuum at 843
MHz. Extended radio emission is detected from the whole galaxy as well as
numerous regions of enhanced radio emission. B79 and RMGWS82 observed
NGC 1313 in the HI line. A detailed optical and HI study is published by
Ryder et al. (1995).

8. 1994CAG1..B...0000S
Re:NGC 1313
Oct 4/5, 1978
103aD + Wr12
60 min
The resolution into individual stars in NGC 1313
is exquisite. Brightest stars begin to resolve
at about B = 17, similar to the level in members
of the South Polar Group such as NGC 55, NGC 247,
and NGC 300 for which distance moduli of
about m - M = 26.5 have been adopted.
The brightest stars occur in the bar and in
a compact association in one of the two stubby
inner arms that start from the ends of the bar.
These arms, and the resolution of stars in the
bar, are seen best in the shallow print on the
right. Both prints here have been made from the
same original plate taken in the V photometric
The chaotic nature of the outer regions of
NGC 1313 is seen in the heavy print on the left.
A semicircular arc near the lower border of the
print, similar to Constellation III in the LMC,
contains a bright association and provides good
resolution into stars. Similar resolution into
fainter stars continues to the plate limit over the
entire face of the galaxy.
The small redshift of v_o = 261 km/s is
consistent with the small distance inferred from
the magnitude of B = 17 for the brightest
resolved stars.
Note that the prints here have been made
from a yellow-sensitive emulsion rather than
blue. This tends to suppress the contrast between
the young blue individual stars and the underlying
older disk.

9. 1993ApJS...88..415R
Re:NGC 1313
NGC 1313 represents an interesting transition object between the late-
type spirals and the Magellanic Irregulars. Coincidentally, it sits
midway between the Large and Small Magellanic Clouds, but at a distance
of ~4.5 Mpc (de Vaucouleurs 1963a). The H II region luminosity function
has been compiled from this data (Ryder & Dopita 1991) and found to have
a power-law slope of -1.9, consistent with the trend with Hubble subtype
found by Kennicutt, Edgar, & Hodge (1989). The most luminous H II regions
outline the two main arms and bar, with a break near the optical nucleus.
Isolated patches of star formation are found to the southwest, as well as
beyond the tip of the northern arm. A low surface brightness envelope of
diffuse H{alpha} emission underlies nearly the entire main body of NGC
1313, and exhibits many filaments, arcs, and shells. In addition, this
image led indirectly to the discovery of Supernova 1978K (Ryder et al.
1993), which is indicated on the H{alpha} image by an arrow.

10. 1993ApJS...86....5K
Re:NGC 1313
NGC 1313; SBdm, H II.
The small apparent discontinuity between the short- and the
long-wavelength spectra could be due to typical pointing errors of 1"-2",
or to the difficulty of extracting flux with high background (see Fig.
17). Marcelin & Gondoin(1983) map some of the many H II regions of NGC
1313 in the optical and show that they extend well outside the range of
the IUE aperture. Although this object has been included in the Rosa,
Joubert, & Benvenuti (1984) catalog of H II regions, the spectrum does
not have the blue slope typical of H II regions.

11. 1985SGC...C...0000C
Re:NGC 1313
Plate 932
Extreme outer dimensions: 17' x 10'.
Plate 958
Overall dimensions: 16.0: x 10.5:. Low surface brightness faint
dwarf 19.5 north-following.
Plate 1871
Overall dimensions: 15.5 x 10.0. Low surface brightness dwarf 19.5

12. 1979AJ.....84..472S
Re:NGC 1313
Many resolved HII regions located in high-surface-brightness
spiral arms which promise significant resolution into stars
at deeper penetration and higher scale.

13. 1977A&AS...28....1V
Re:VV 436
Plate 10 Galaxies of the M51 Type.
NGC 1313, 9.5m 3h17.6m -66^deg^40', V_0_=+47 (R).
Photo and photometry by Sersic (1968), M=-18.7, D=4.5 MPc, SN 1962.

14. 1976RC2...C...0000d
Re:NGC 1313
NGC 1313A at 16.5 arcmin south-following (with corrected coordinates).
Vistas in Ast., Vol. 14, 210, 1972.
Zeit. fur Ap., 69, 242, 1968.
Vistas in Ast., Vol. 14, 224, 1972.
Observatory, 94, 7, 1974.
J.R.A.S. Canada, 68, 177, 1974.
Atlas Gal. Australis, 1968.
Vistas in Ast., Vol. 14, 231, 1972.
Photometry: (2.2 micron upper limit)
M.N.R.A.S., 164, 155, 1973.
Mt. Stromlo velocity (Source H) rejected.
Misidentified V_0 of HII region NGC 1313-I = 516 +/- 85 km/sec.
Cordoba interferometic velocity (Source P4) corrected to +507 km/sec.
See Observatory, 95, 178, 1975.
Interferometry, Rotation Curve and Mass Determination:
Observatory, 94, 7, 1974.
HII Regions:
Zeit. fur Ap., 69, 242, 1968.
Cordoba Obs. Rep. No. 119, 1963.
M.N.R.A.S., 131, 155, 1965.
M.N.R.A.S., 158, 375, 1972.
Radio Observations:
Austral. J. Phys., 16, 360, 1963. 19, 883, 1966.

15. 1964RC1...C...0000d
Re:NGC 1313
Very small, bright nucleus
Fairly bright bar: 1.1 arcmin x 0.4 arcmin.
2 main knotty, partially resolved arms, one stronger.
Very asymmetric.
Many outlying knots and partially resolved groups of star.
Anonymous, small spiral at 16.5 arcmin [south-following].
Mt. Stromlo velocity for emission nebulo. 1.4 arcmin [south-south-following]
Central bar.
Photograph and Photometry:
Ap. J., 137, 720, 1963.
SN 1962
Discussed by Sersic, (unpublished)

16. 1957HPh....53..275d
Re:NGC 1313
(Plate 32)
Only a very small nucleus remains in the center of the bar
from which emerge two, short arms, broken up into clumpy
sections. The rest of the spiral pattern is weak, very
irregular and strongly asymmetrical.
Note also the asymmetrical half-ring on one side of the bar.
This is the transition stage towards the Magellanic irregulars.
Compare with NGC 7741 (Plate 31), SMC (Plate 36),
and IC 1613 (Plate 37).

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