Untitled

Thatte, Niranjan; Genzel, R.; Kroker, H.; Krabbe, A.; Tacconi-Garman, L. E.; Maiolino, R.; Tecza, Matthias

doi:10.1023/a:1000593931795

Cited by 29 publications

(65 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our interpretation of the present data appears to be generally consistent with the conceptual models developed for the evolution of the center of M83 by Gallais et al (1991) and Thatte et al (2000). Starbursts are associated with the rapid astration of molecular clouds.…”

Section: Discussion : the Recent Cluster Formation History Of M83supporting

confidence: 89%

“…The central starburst in M83 spans 20A (D360 pc at 3.7 Mpc) and presents a relatively complex morphology (see Gallais et al 1991 ;Elmegreen, Chromey, & Warren 1998). In contrast to the centrally concentrated starburst of NGC 5253, the optically detected starburst in M83 is contained in a semicircular annulus between 3A and 7A (54 pc and 126 pc at 3.7 Mpc distance) from M83Ïs optical center (Thatte, Tecza, & Genzel 2000). This "" active ringlet ÏÏ region contains almost 400 objects brighter than mag, m F300W \ 21 and 45 of these are bright enough to have been detected in our shallower Wide Field Planetary Camera 2 (WFPC2) F547M and F814W images.…”

Section: Introductionmentioning

confidence: 99%

“…Near infrared spectroscopy by Puxley, Doyon, & Ward (1997) conÐrms that young populations are o †set from the optically visible nucleus, corresponding to the optical starburst ringlet. Spectroscopy by Thatte et al (2000) shows that the nucleus of M83 is a dynamically complex region and may even harbor a second, optically obscured nucleus.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Young Clusters in the Nuclear Starburst of M83

Harris

Calzetti

Gallagher³

et al. 2001

The Astronomical Journal

149

View full text Add to dashboard Cite

We present a photometric catalog of 45 massive star clusters in the nuclear starburst of M83 (NGC 5236), observed with the Hubble Space T elescope Wide Field Planetary Camera 2, in both broadband (F300W, F547M, and F814W) and narrowband (F656N and F487N) Ðlters. By comparing the photometry with theoretical population synthesis models, we estimate the age and mass of each cluster. We Ðnd that over 75% of the star clusters more massive than 2 ] 104 in the central 300 pc of M83 are M _ less than 10 Myr old. Among the clusters younger than 10 Myr and more massive than 5 ] 103 M _ , 70% are between 5 and 7 Myr old. We list an additional 330 objects that are detected in our F300W images but not in the shallower F547M and F814W images. The clusters are distributed throughout a semicircular annulus that identiÐes the active region in the galaxy core, between 50 and 130 pc from the optical center of M83. Clusters younger than 5 Myr are preferentially found along the northwestern end of the semicircular annulus, and the northwest region also corresponds to the highest equivalent widths of the Ha emission [EW(Ha)] values. The cluster ages are consistent with a burst of star formation that began Myr ago. However, the current data cannot exclude a longer duration of activity, because [10 the star clusters may dissolve on a D10 Myr timescale. We discuss both possible scenarios.

show abstract

Section: Discussion : the Recent Cluster Formation History Of M83supporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Young Clusters in the Nuclear Starburst of M83

Harris

Calzetti

Gallagher³

et al. 2001

The Astronomical Journal

149

View full text Add to dashboard Cite

show abstract

“…Infra-red (IR) observations (Gallais et al 1991;Elmegreen et al 1998;Thatte et al 2000) have shown that the nuclear region of M 83 has a complex structure. From measurements of line-of-sight stellar velocities in the inner galactic region, two dynamical centres are inferred.…”

Section: Introductionmentioning

confidence: 99%

“…0 to the West of the IR peak, is not associated with any bright source, but is approximately coincident with the centre of symmetry of the outer isophote ellipses. The stellar velocity dispersion implies that each dynamical centre contains an enclosed mass of ≈1.3 × 10 7 M (Thatte et al 2000).…”

Section: Introductionmentioning

confidence: 99%

X-ray sources in the starburst spiral galaxy M 83

Soria

2002

A&A

View full text Add to dashboard Cite

Abstract. Chandra has resolved the starburst nuclear region of the face-on grand-design spiral M 83. Eighty-one point sources are detected (above 3.5-σ) in the ACIS S3 image, and 15 of them are within the inner 16 region of the galaxy. A point source with Lx ≈ 3 × 10 38 erg s −1 in the 0.3-8.0 keV band is found to coincide with the infra-red nuclear photometric peak, one of the two dynamical nuclei of the galaxy. No point-like sources are resolved (at a 2.5-σ level) at the centre of symmetry of the outer optical isophote ellipses, suspected to be another dynamical nucleus. About 50% of the total emission in the nuclear region is unresolved; of this, about 70% can be attributed to hot thermal plasma, and the rest is probably due to unresolved point sources (e.g., faint X-ray binaries). The azimuthally-averaged radial distribution of the unresolved emission has a King-like profile, with no central cusp. Strong emission lines are seen in the spectrum of the optically thin plasma component. The high abundances of C, Ne, Mg, Si and S with respect to Fe suggest that the interstellar medium in the nucleus is enriched and heated by type-II supernova explosions and winds from massive stars. The cumulative luminosity distribution of the discrete X-ray sources is neither a single nor a broken power law. Separating the sources in the nuclear region (within a distance of 60 from the X-ray centre) from the rest reveals that the two groups have different luminosity distributions. The log N(>S) − log S curve of the sources in the inner region (nucleus and stellar bar) is a single power law, which we interpret as due to continuous, ongoing star formation. Outside the central region, there is a smaller fraction of sources brighter than the Eddington limit for an accreting neutron star.

show abstract

Gemini 3D infrared spectroscopy: Double nucleus in M 83

Díaz¹,

Agüero

Dottori

et al. 2004

Proc. IAU

View full text Add to dashboard Cite

Abstract. We report the status of our study of the central region of M 83. Recently a binary mass concentration at the nucleus was suggested by Thatte et al. (2000), and we determined the possible position of the optically hidden mass concentration with 2D Hα kinematics. We continue our study of this region trough IR 3D spectroscopy performed with CIRPASS, attached to the Gemini South telescope. Almost 1500 spectra were obtained, centered in the wavelength 1.3 µm. The velocity field in a region of 13" × 9" around the optical nucleus is resolved, with 0.36" (6.4 pc) sampling. We confirm that the optical nucleus of M 83 is not located at the most important center of symmetry of the velocity field. The largest black hole that could fit to the circular motion in this kinematic center should have a mass less than 2 × 10 7 M .

show abstract

Untitled

Cited by 29 publications

References 0 publications

Young Clusters in the Nuclear Starburst of M83

Young Clusters in the Nuclear Starburst of M83

X-ray sources in the starburst spiral galaxy M 83

Gemini 3D infrared spectroscopy: Double nucleus in M 83

Contact Info

Product

Resources

About