Star formation in the galactic center dust ridge

Details Star formation in the galactic center dust ridge Star formation in the galactic center dust ridge

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...423l..39l&link_type=abstract

Astrophysical Journal, Part 2 - Letters, vol. 423, no. 1, p. L39-L42

Astronomy and Astrophysics

Astronomy

22

Astronomical Maps, Dust, Galaxies, Molecular Clouds, Radio Astronomy, Radio Emission, Ridges, Star Formation, Submillimeter Waves, Water Masers, Bolometers, Data Reduction, Radio Telescopes, Spatial Resolution, Very Large Array (Vla)

Scientific paper

We present multiwavelength submillimeter and radio continuum, as well as 22 GHz H2O line observations of the giant molecular cloud core M0.25 + 0.01 located in the 'dust ridge' near the Galactic center radio arc. At lambda = 350 micrometer the continuum emission region is spatially resolved by our 12 sec beam, and we find no evidence for compact dust sources similar to those found in Sgr B2. Although existing far-infrared data do not allow for accurate determination of the dust temperature, the steep rise of the submillimeter spectrum between 800 and 350 micrometer suggests that the grain emissivity law in the M0.25 + 0.01 core may be significantly steeper than in previously studied Galactic center dust sources. The detection of an H2O maser source located near the 350 micrometer emission peak implies the presence of at least some ongoing low-mass star formation. However, in spite of the relatively large molecular mass of the core implied by the submillimeter observations (approximately equals 1.6 x 105 solar mass), our 8.4 GHz continuum data show that current star formation in the M0.25 + 0.01 core is limited to stars with spectral types later than B0; there is no evidence for more massive young stars. This Greater Magellanic Cloud (GMC) core thus appears distinctly different from the Sgr C and D cores, which, although much less massive, harbor O-type stars.

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