Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· On-line Data
· References in the article
· Citations to the Article (97) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (82)
· NED Objects (1)
· Also-Read Articles (Reads History)
· Translate This Page
NGC 3603 and its Wolf-Rayet stars: Galactic clone of R136 at the core of 30 Doradus, but without the massive surrounding cluster halo
Moffat, Anthony F. J.; Drissen, Laurent; Shara, Michael M.
AA(Université de Montreal, Montreal, Canada), AB(Université de Montreal, Montreal, Canada), AC(Space Telescope Science Inst., Baltimore, MD, US)
Astrophysical Journal, Part 1 (ISSN 0004-367X), vol. 436, no. 1, p. 183-193 (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Density Measurement, H Ii Regions, Star Clusters, Stellar Mass, Hubble Space Telescope, Local Group (Astronomy), Statistical Distributions, Stellar Spectra, Wolf-Rayet Stars
Bibliographic Code:


Hubble Space Telescope/Planetary Camera (HST/PC) images of the dense stellar cluster at the center of the Galaxy's most massive visible H II region, NGC 3603, reveal remarkable similarity to the dense core R136 in the Local Group's most massive Giant H II region, 30 Dor. The projected star density for stars brighter than MV = -5.0 in both objects increases inwards to the last data bin in both objects at r = 0.033 pc with a power-law of slope close to -1.8. Even the central star density in NGC 3603 is similar to that found in R136. Outside r approximately equals 1 pc, NGC 3603 plummets to zero density, at least for its massive stars, while 30 Dor continues to decrease with similar power-law slope out to r approximately equals 130 pc. Narrowband He II 4686 A images reveal that NGC 3603 contains three WR stars; they stand out as the brightest members of NGC 3603, all located within the central 0.1 pc. However, while R136 also contains three bright WR stars within 0.1 pc of its center, they are almost a magnitude fainter than NGC 3603's WR stars. Reasons for these differences are probably related to the different environments and ages of the two objects.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences

More Article Retrieval Options

HELP for Article Retrieval

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints