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NIR studies of galactic giant HII regions

Published online by Cambridge University Press:  08 November 2005

A. Damineli ,
R. D. Blum ,
E. Figuerêdo  and
P. S. Conti
A. Damineli
Affiliation:
IAGUSP, University of São Paulo, 05508-900, Brazil email: damineli@astro.iag.usp.br
R. D. Blum
Affiliation:
Cerro Tololo Interamerican Observatory, Casilla 603, La Serena, Chile email: Blum@noao.edu
E. Figuerêdo
Affiliation:
IAGUSP, University of São Paulo, 05508-900, Brazil email: damineli@astro.iag.usp.br
P. S. Conti
Affiliation:
JILA, University of Colorado, Campus Box 440, Boulder, CO, 80309, USA email: Pconti@jila.colorado.edu
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Abstract

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We present results from our ongoing survey of Galactic Giant HII Regions in the near-infrared. The luminosity function indicates that the IMF is uniform, independent of the galactocentric distance and compatible with Salpeter (1955) slope. Distances measured by the spectroscopic parallax method are systematically smaller than kinematic distances derived from radio techniques. As a consequence, the number of ionizing photons and the star formation rate is much lower than that derived from rotation models. Although the luminosities of the giant HII regions obtained from this method are lower than by other methods, the morphological type of the Milky Way is well in line of previous results, close to Sbc or Sc types.

Keywords

surveysstars: distancesstars: early typestars: formation(ISM): HII regionsGalaxy: diskinfrared: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S227: Massive Star Birth: A Crossroads of Astrophysics , May 2005 , pp. 407 - 412
Copyright
© 2005 International Astronomical Union