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Notes for object MESSIER 083

26 note(s) found in NED.


1. 2008ApJ...679..310G
Re:MESSIER 083
M83 (Figs. 22 and 23).-M83 is a spiral galaxy that is similar in several aspects
to M51. Its band ratios (Fig. 22) and the spatial distribution of its PAH
emission (Fig. 24) have the same properties qualitatively. The average centroid
of the 7.7 micron is identical to that for M51 and M83 ({lambda}_7.7_) ~= 7.72
microns;Table 2).

2. 2008A&A...484..341R
Re:MESSIER 083
Figure A.5. This near, face-on barred spiral galaxy shows mostly extended
emission surrounding a faint central object. The extended emission is dominated
by PAHs which account for the majority if the MIR luminosity (Vogler et al.
2005). The micron flux measured, 232 mJy, is identical with the micron flux
measured by Siebenmorgen et al. (2004). Our images, however, show a clear,
although faint, central source, while Siebenmorgen et al. (2004) report only
fuzzy extended emission. The LW3 filter (12-18 micron) of Vogler et al. (2005)
show the emission clearly tracing the spiral arms of M 83, which is not seen in
our image.

3. 2007MNRAS.382.1552L
Re:NGC 5236
NGC 5236 - M 83: Fig. 2 shows that the centre of this galaxy has complex
structure in the optical and NIR (Gallais et al. 1991; Elmegreen et al. 1998).
The radio emission from the central region is also complex, with multiple
sources (Turner & Ho 1994; Harris et al. 2001; Maddox et al. 2006). The optical
and NIR nucleus is coincident with the third brightest radio-peak (Maddox et al.
2006). NIR imaging (Elmegreen et al. 1998) shows two dust lanes going into the
centre from opposite directions, and forming a circumnuclear ring in the centre.
This ring is possibly joined to an inner ring by a nuclear bar. The main
star-forming region is a partial arc lying between these two red rings and south
of the nucleus. The crosses in Fig. 2 mark the 6-cm radio peaks from Turner & Ho
(1994); however, there is also extended emission throughout the region. The
radio peak positions are shifted slightly to correctly align the optical and
radio sources (Gallais et al. 1991).

4. 2007ApJS..173..538T
Re:NGC 5236
NGC 5236 [M83] (Fig. 16.26).-The prototypical XUV-disk galaxy [SAB(s)c; H II
starburst] exhibits clumpy SF complexes associated with local maxima throughout
an extensive, filamentary H I disk (Thilker et al. 2005a). The distribution of
UV complexes is sparse, with a low surface covering factor, although there are
many sites of recent star formation. Some of the XUV complexes do contain faint
H II regions, which have low abundance (~Z_sun_/10) and are often ionized by
single massive stars (Gil de Paz et al. 2007b). Past interaction with other
members of the Centaurus A group, including NGC 5253 and KK 208 (Karachentseva &
Karachentsev 1998), is considered likely. More details on NGC 5236 are presented
by Thilker et al. (2005a) and Gil de Paz et al. (2007b).

5. 2006ApJS..165..307M
Re:NGC 5236
HIPASS J1337-29 (NGC 5236).The well-studied Messier 83 is a large face-on SBb.
The thick bar is 199" long and contains numerous dust lanes. The bar dust lanes
terminate in a central, knotty very HSB region (in both R band and H{alpha}) 14"
across-the central starburst. Numerous bright H II regions have a high covering
factor, especially along the two arms, out to R ~ 290". There the H{alpha}
distribution is largely truncated, as pointed out by Kennicutt (1989) and Martin
& Kennicutt (2001), while the UV light profile shows no truncation (Thilker et
al. 2005). However, a few fainter H II regions can be seen out to the edge of
our frame.

6. 2005ApJS..157...59L
Re:NGC 5236
NGC 5236 (M83) is a starburst barred Sc spiral galaxy at a distance of 4.7 Mpc
with very luminous spiral arms. ULX1 (IXO 82) is located on the edge of a spiral
arm, and its luminosity showed an increase from 1.5 * 10^39^ to 2.5 * 10^39^
ergs s^-1^ between two observations separated by 600 days.

7. 2004AJ....128...16K
Re:NGC 5236
NGC 5236 (M83, HIPASS J0317-41) is a nearly face-on, gas-rich spiral
galaxy located within a loose group of galaxies (see Fig. 28). We
measure an integrated H I flux density of 1630+-96 Jy km s^-1^ and a
deconvolved Gaussian H I diameter of 31.2' x 21.4' (40 kpc x 28 kpc).
Huchtmeier & Bohnenstengel (1981) measure a maximum H I extent of
95' x 76'. Park et al. (2001) obtained a large H I mosaic with the ATCA
and Parkes showing an extent of at least 60'. The dwarf companions
NGC 5253 (HIPASS J1339-31A) and NGC 5264 (HIPASS J1341-29) lie at
projected distances of 113' and 60' from NGC 5236, respectively
(see also Banks et al. 1999 and Koribalski 2002).

8. 2004A&A...419..501F
Re:NGC 5236
NGC 5236- Genzel et al. (1998) report in the SWS 14" x 20" aperture an
extinction of 5 mag, larger than the value adopted here. The ratio
[N II]{lambda}6583 {Angstrom}/(H{alpha} + [N II] {lambda}6583 {Angstrom})
{approx}0.3 in the central{approx} 5" (Keel 1984; Veron-Cetty & Veron
1986). The nucleus is saturated in the ISOCAM LW2 and LW3 maps, more
severely for LW3. We thus used maps simulated from the CVF spectral cube
to measure the LW2 and LW3 fluxes. We estimate in this way that the
missing flux fractions due to saturation are 11% and 34% respectively,
assuming that the effects discussed in Sect. 3.1, making photometry from
CVFs uncertain by 10-20%, are negligible.

9. 2003ApJS..146....1W
Re:NGC 5236
NGC5236(M83). This galaxy is a nearby, large starburst (velocity
516 km s^-1^, diameter 16.1 kpc or 1.2' at its distance of 4.7 Mpc).
The FUSE aperture covers only part of the galaxy. The flux is
probably due to a mixture of many O stars. Very strong O VI
absorption is seen between -200 and 740 km s^-1^, but the
Galactic contribution is unclear. This sight line was therefore
excluded from the final sample.

10. 2002ApJS..140..303L
Re:NGC 5236
NGC 5236 (Fig. 37).-NGC 5236 is a prototypical starburst galaxy, and
the HUT spectrum displays spectacular hot-star lines. Note the striking
O VI P Cyg profile. All absorption lines are broader than in any other
galaxy. This is due to two reasons: NGC 5236 was observed in part
through the 32" aperture and is extremely metal-rich. The high
metallicity may explain the apparent weakness of the C IV emission. The
surrounding photospheric Fe lines cause a significant depression of the
flux level, which is not the case in the solar metallicity model.
Nevertheless, a characteristic age of 10 Myr can be derived.

11. 2000MNRAS.319...17L
Re:NGC 5236
NGC 5236 (M 83): The very complex X-ray emission in this galaxy can be
appreciated in Fig. 25. Several X-ray knots are distributed on top of
bright, uneven extended emission. Comparison between the two ROSAT HRI
observations reveals that at least three of the eight detected point
sources are variable. Table 7 shows the count rates observed in 1993
January and 1994 July. Sources X1, X7 and X8 are not detected during the
observations obtained in 1994 July, but are among the brightest objects
seen in 1993 January.
Trinchieri, Fabbiano & Paulumbo (1985) reported on the Einstein HRI
observations of this galaxy. From their observations (obtained in 1980
January and 1981 February) only three sources were detected in the nuclear
region of the galaxy. Two correspond to the ROSAT sources X3 (the nucleus)
and X6, which are the brightest sources observed in the ROSAT HRI data (see
Table 7). Their fluxes in the Einstein (0.5-3.0 keV) bandpass are in good
agreement with the fluxes given in Table 4. The third source had a
luminosity of 2.3 x 10^38^ erg s^-1^ in the Einstein bandpass (for a
distance to NGC 5236 of 3.75 Mpc as assumed by Trinchieri et al. 1985),
and it is not detected in the ROSAT data. It probably corresponds to a
transient XRB.
Ehle et al. (1998) report on ROSAT PSPC observations of NGC 5236
obtained between 1992 January and 1993 January. They find a luminosity for
the nuclear source of 7 x 10^-13^ erg s^-1^ cm^-2^, in good agreement
with the measurement in Table 4. They also detect all the point sources
seen in the HRI observations, with the exception of X5, which corresponds
to the faintest source in the nuclear region. This suggests that the
variable sources X1, X7 and X8 were detectable for at least a year (from
the beginning of 1992 until the beginning of 1993), before fading away,
becoming undetectable by 1994 July.
The diffuse emission from the central region of NGC 5236 can be
appreciated in Fig. 36. From the PSPC observations Ehle et al. (1998) find
that the soft 0.1-0.4 keV diffuse component accounts for almost half of
the total X-ray emission, and argue that most of it is due to hot gas in
a superbubble with radius ~10-15 kpc. Evidence of vigorous starburst
activity comes from observations of the nuclear and circumnuclear regions
of NGC 5236, which have intricate morphologies in the UV, optical and
infrared (Bohlin et al. 1983; Gallais et al. 1991; Johnson 1997).
Finally, several historic supernovae have been observed in this galaxy,
but none of them is consistent with the positions of the point X-ray
sources.

12. 1999A&AS..138..253B
Re:NGC 5236
NGC 5236 (M83) - SNe 1923A, 1950B, 1957D, 1968L, 1983N: all patches at
all locations appear to be very bright and blue (both in the B-V and in
the V-R colors). At the site of SN 1983N two compact patches are
visible. Note that the positions of these supernovae are known
accurately (see Sect. 4.1). In all these cases the SN star progenitors
are likely to have been massive (two SNe are confirmed Type II's and one
is a Type Ib; SN 1957D is likely to be a Type II, as possibly inferred
from the radio data, see Weiler et al. 1986). Around such progenitors
dense circumstellar and possibly interstellar environments are expected,
thus allowing for the formation of light echoes. The best bets may be
SNe 1957D and 1983N. SNe 1957D and 1983N are classified as candidates
(see Table 3).

13. 1999A&AS..136...35S
Re:Messier 083
M 83 -- From eight giant HII regions surveyed by Rosa & D'Odorico (1986)
in this galaxy, three exhibit a broad emission feature at the blue WR
bump.

14. 1998ApJS..118..275K
Re:MRC 1334-296
This is the well-known galaxy M83 (NGC 5236). For VLA maps at several
radio frequencies, see Neininger et al. (1993).

15. 1998A&A...335..807A
Re:NGC 5236
This galaxy, also known as M83, is one of the closest spirals with a
prominent bar (Adamson et al. 1987). At optical and near infrared
wavelengths the galaxy exhibits an amorphous structure within the
central 16" (Gallais et al. 1991) and this can almost certainly be
associated with a mild nuclear starburst. There is bright emission in
our FIR maps of M83 and some evidence for a bar structure in the 100
micron image. The 200 micron emission appears very extended with respect
to the optical disk. Intriguingly, M83 is known to have a remarkably
extensive HI disk containing 80% of its mass outside the optical
diameter (Huchtmeier & Bohnenstengel 1981).

16. 1997A&AS..125..479J
Re:NGC 5236
NGC 5236 (M 83) (SABc, I=21.0^deg^)
The nuclear structure of this nearby "hot-spot" starburst galaxy (e.g. Telesco
et al. 1993) is complex also in our JHK images and the ellipse fitting in the
central region not too meaningful (it even fails in J). The structure, patchy
but dissimilar from optical and mid-IR will be analyzed elsewhere.

17. 1996ApJS..103...81C
Re:NGC 5236
NGC 5236.--M83. Polarization maps in Neininger et al. (1993). VLA maps showing
the core and supernova remnants in Cowan, Roberts, & Branch (1994).

18. 1994CAG1..B...0000S
Re:NGC 5236
M83
Centaurus A Group
Hubble Atlas, p. 28
SBc(s)II
CD-1320-S/Br
March 12/13, 1980
103aO + GG385
45 min
NGC 5236 is the brightest spiral in the
nearby group whose brightest member is
NGC 5128 (Cen A; S0 + S pec; panels 45, 46). The
mean redshift of the group is about = 280
km/s. Because the group is so nearby, most
members are highly resolved and are important
for the calibration of the extragalactic distance
scale.
The surface brightness of NGC 5236 is
exceedingly high in the arms, which are massive in
the sense of Reynolds (1927a,b) and therefore
cover most of the disk.
The dust lanes are intricate and, in general,
are closely associated with the luminous arms on
the insides of these arms, as usual.
The range of the surface-brightness scale is
so large that two levels of the image from the
original negative are illustrated. The heavy image
is on this panel; a lighter print showing the dust
lanes and the central regions is on the following
panel.
Far-outlying associations exist beyond the
borders of this print. They are similar to the
associations in M31 Field IV of Baade and Swope
(1963), which is 96' from the center of M31. It
is in these outlying fields, where the surface
brightness of the background disk of M83 is low
and the dust is negligible, that searches for
Cepheids will be made. Several such remote
associations exist; the farthest, easily visible on
the Las Campanas 100-inch plates, is at a radial
distance of 11' from the center, off the borders
of this print. At the estimated distance of 6 Mpc
for M83 this angular distance corresponds to a
linear distance from the center of 20 kpc. The
distance of Field IV from the center of M31 is
similar, at 24 kpc.

19. 1994CAG1..B...0000S
Re:NGC 5236
M83
Centaurus A Group
Hubble Atlas, p. 28
SBc(s)II
CD-1320-S/Br
March 12/13, 1980
103aO + GG385
45 min
This light print of M83 shows the intricate
dust lanes and the central oval luminosity
distribution requiring the barred classification.
Consistent with this classification are the two
major thin dust lanes in the central oval. The
dust lane pattern, the signature of a bar potential,
is due to the response of the interstellar gas
to that potential, resulting in two hydrodynamic
shock fronts that appear as straight dust lanes.
The pattern has been discussed in many of the
previous descriptions of prototypical SBb
galaxies such as NGC 1300 (panels 154, S8).
One of the central dust lanes cuts across the
front of the nuclear region; the other appears to
duck behind. The pattern is identical to that in
the prototypical SBb galaxy NGC 5383 (panel
168).
The brightest individual stars are easily
resolved throughout the image of M83. However,
their photometry in the high-surface-brightness
central regions is difficult to interpret because of
the evident high internal absorption throughout
the inner disk and arms. We estimate that the
brightest stars begin to resolve at about B = 17.

20. 1993ApJS...86....5K
Re:NGC 5236
NGC 5236 (M83); SBc, starburst.
M83 is a nearby, bright southern galaxy which is almost face-on and which
belongs to a class of galaxies with an "amorphous" nucleus (Sersic &
Pastoriza 1965). M83 is undergoing a burst of star formation in the
nucleus and in the spiral arms, possibly triggered by its companion NGC
5253 (Condon et al. 1982). Associated with the star formation is strong
emission in the radio (Condon et al. 1982), in the infrared (Telesco &
Houper 1980), and in the X-ray (Trinchieri, Fabbiano, & Palumbo 1985).
The UV absorption lines, which have a strong similarity to those of NGC
7714, suggest that M83 is a starburst with an evolved population of
supergiants, whose signature is the P Cygni profiles of Si IV
{lambda}{lambda}1397, 1402 and C IV {lambda}1550 (Bohlin et al. 1983). A
large number of supernovae have been observed in this galaxy (five since
1923, among which the one detected in the nucleus [1968L]) is a Type II
supernova. The association of the Type II supernova with H II regions in
the spiral arms and in the nucleus is in agreement with the general
scenario of a starburst (Richter & Rosa 1984). Although the UV spectrum
does not show a marked 2200A dust absorption, observation in optical
wavelengths indicates a value for intrinsic E(B - V) ~ 0.3 mag (Pastoriza
1975).

21. 1985SGC...C...0000C
Re:NGC 5236
Plate 494
Patchy arms, plate defect superposed?

22. 1976RC2...C...0000d
Re:NGC 5236
= M83
= PKS 1334-29
Description and Classification:
P.A.S.P., 77, 287, 1965.
P.A.S.P., 79, 152, 1967.
IAU Symp. 38, 29, 1970.
Photograph:
P.A.S.P., 77, 287, 1965.
Astr. Ap., 12, 379, 1971.
Ap. J., 194, 559, 1974.
M.N.R.A.S., 167, 13, 1974.
Photometry:
Atlas Gal. Austr., 1968.
Photometry (UBV):
A.J., 74, 335, 1969.
Photometry (I.R., 1-21 microns):
Ap. J. (Letters), 159, L165, 1970.
Ap. J. (Letters), 176, L95, 1972.
Ap. J. (Letters), 191, L20, 1974.
M.N.R.A.S., 164, 155, 1973.
Spectrum:
Observatory, 87, 38, 225, 1967.
Dynamics and Mass Determination:
Proc. A.S. Austr., 1, 288, 1969.
HII Regions and Distance Modulus:
Ap. J., 194, 554, 1974.
Interferometry H{alpha}:
Bol. A.A. Argentina, No. 14, 38, 1968.
Astr. Ap., 12, 379, 1971.
SN1923A
Ann. Rev. Ast. Ap., 2, 249, 1964.
"Supernovae & SN Remnants", Ap.& Space Sc. Lib., 45, 203, 1974.
SN1950B
P.A.S.P., 65, 242, 1953.
SN1957D (noted 1958 in RC1)
IAU Circ. No. 1643, 1958.
Zeit. f. Ap., 49, 202, 1961.
SN1968L
IAU Circ. No. 2085, 1968.
Ast. Tsirk., No. 474, 1968.
B.A.A. Circ. No. 501, 1968.
M.S.A.S.S.A., 27, 105, 1968.
Sky & Tel., 36, 295, 1968.
Astr. Ap., 19, 99, 1972.
M.N.R.A.S., 167, 13, 1974.
"Supernovae & SN Remnants", Ap. & Space Sc. Lib., 45, 119, 1974.
HI 21cm:
Proc. A.S.Austr., 1, 104, 1968.
Astr. Ap., 29, 425, 1973.
Ap. J., 193, 309, 1974.
Radio Observations:
Australian J.Phys., 16, 360, 1863.
M.N.R.A.S., 152, 439, 1971.
Proc. S.A.Australia, 2, 159, 1972.

23. 1974UGCA..C...0000N
Re:UGCA 366
UGCA 366:
= NGC 5236 = M 83
SAB(s)c (RC1)
magnificent!; northern part much more patchy and irregular than southern part;
a very irregular, almost radial pattern on preceding side;
fairly bright out to 11 x 11 arcmin, but a faint halo is visible outside;
the galaxy is probably much larger than 14 x 14 arcmin

24. 1964RC1...C...0000d
Re:NGC 5236
= Messier 083
Extremely bright nucleus in a bright complex bar with dark lanes. 2 main,
partially resolved arms, with many branchings.
(B-V)(0) interpolated.
Photograph:
M.N.R.A.S., 85, 1019, 1925.
P.N.A.S., 26, 33, 1940.
Radio Emission:
Handbuch der Phys., 53, 253, 1959.
M.N.R.A.S., 122, 479, 1961.
P.A.S.P., 72, 368, 1960.
Observatory, 83, 20, 1963.
HI Emission:
Epstein, Harvard Thesis. 1962.
SN 1923
P.A.S.P., 35, 166, 1923.
P.A.S.P., 48, 320, 1936.
H.B. 786, 787, 1923.
Ap. J., 88, 293, 1938.
SN 1950
H.A.C. 1074, 1950.
SN 1958 (or Nova?)
H.A.C. 1394, 1958.
Sky & Telescope, 17, 287, 1958.

25. 1961Hubbl.B...0000S
Re:NGC 5236
Messier 083
Sc/SBb
H-540-H
Mar. 2/3, 1925
E40
100 min
Enlarged 3.3X
NGC 5236 is a magnificent southern spiral with multiple
arms. The present illustration does not do justice to the
intricate dust lanes or to the fainter spiral arms.
The galaxy has certain features common to an SBb,
such as the straightness of the two dust lanes coming
from the nucleus on opposite sides of a region of somewhat
enhanced luminosity. On short-exposure plates,
one lane appears to cut in front of the nucleus and the
other goes behind. The pattern is similar to that of NGC 5383
on page 46. There are two bright spiral arms and a
number of arm fragments of lower surface brightness on
the outside of the principal arms. The dust lanes that
emerge from the nucleus follow the inside of the two bright
arms. This is a general characteristic of most galaxies
having opaque dust lanes. But dust is by no means concentrated
in these two lanes; it is spread in spiral patterns
over the entire face of the central lens. The segments are
branched as in M51 and M101. The luminous spiral arms
generally follow the branching of the dust lanes. Reproductions
of M83 are also given by Shapley in his "Galaxies",
page 22, and as Figure 2 of his "The Inner Metagalaxy".

26. 1918PLicO..13....9C
Re:NGC 5236
A bright and unusually beautiful spiral 10' x 8'. The nucleus is 20" in diameter
and very bright; in a 2m exposure it shows as a faint disk with a bright
peripheral streak or whorl. A large number of almost stellar condensations in
the rather open whorls of this fine object. See figure 7. 18 s.n.


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