New URL

The URL you are looking for has changed. The new URL is:

http://www.submm.caltech.edu/cso/recent_results/

You will be taken there automatically in 15 seconds. Otherwise, you can click on the link right now.

cso@cco.caltech.edu
The Orion Bar photo-dissociation region (SE of IRc~2) and the ``molecular fingers'' (NW of IRc~2) are clearly visible. Contour levels are 30, 60, 120, 240, and 480~Jy per beam (the lowest contours correspond to about 10 sigma in OMC-1 and 20 sigma in OMC-2/3). This image appears in a paper recently submitted to The Astrophysical Journal by D.C. Lis et al.

An image showing the distribution of the molecule 13CO toward the star-forming region G10.62. The bright 13CO emission peak indicates the high molecular column density toward the ultracompact H II region. The extended halo of emission to the southeast and northwest forms a boundary for the large cavity of ionized material to the northeast as seen in VLA radio continuum images. This image was provided by Todd Hunter.

350 micron emission and polarization of the molecular cloud Sagittarius B2 near the center of the Galaxy. The data were obtained at the CSO with the University of Chicago polarimeter Hertz. The emission (shown by the contours) is from dust grains which are aligned by the magnetic field in the cloud, resulting in a measurable linear polarization. The vectors (straight lines) on the map show the direction of the polarization, which is perpendicular to the magnetic field. Rotating the vectors by 90 degrees yields a magnetic field map. This is one of only a handful of methods of measuring magnetic fields in remote nebulae. This figure appears in a paper recently accepted for publication in The Astrophysical Journal by C.D. Dowell et al.

350 micron polarization measurements of the circumnuclear disk (CND) and 50 km/sec cloud at the center of the Galaxy. For this figure, the polarization vectors have been rotated by 90 degrees to show the direction of the magnetic field. The contours show the dense material emission at a wavelength of 1.3 mm (from Mezger et al. 1989), the shaded area shows the non-thermal 6 cm radio emission from a supernova shell (Ekers et al. 1983), and the dots show the location of young massive stars (Goss et al. 1985). The structure of the magnetic field -- that it follows the ridge of dense material -- supports the idea that the 50 km/sec cloud has been compressed by the expanding supernova, leading to the formation of massive stars. This figure appears in a paper recently submitted to The Astrophysical Journal by G. Novak et al.

A spectrum of the CO (carbon monoxide) J=7-6 line in the Orion-KL star-forming region. This line was observed as part of a spectral line survey project of this region between the frequencies of 795 and 840 GHz. This project used the new 850 GHz receiver of the CSO.

-->