Distances of Three High-Galactic Latitude Diffuse Clouds

Details Distances of Three High-Galactic Latitude Diffuse Clouds Distances of Three High-Galactic Latitude Diffuse Clouds

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541523m&link_type=abstract

American Astronomical Society, AAS Meeting #215, #415.23; Bulletin of the American Astronomical Society, Vol. 42, p.264

Astronomy and Astrophysics

Astronomy

Scientific paper

The Sun is embedded within a large, irregularly-shaped region of plasma called the Local Bubble. Lallement et al. (2003) have traced its convoluted boundary by using the equivalent widths of NaD lines in 1005 distant stars. To avoid directional bias, however, they intentionally avoided targeting stars that shared lines-of-sight with clouds visible on IR, X-ray, or radio maps. Thus, to complement their study, we have determined the distances of three diffuse clouds that were also classified as soft X-ray shadows by Snowden et al. (2000). We targeted these objects since X-ray shadows are expected to lie at or near the bubble's boundary. Thus, their distances and radial velocities provide information about the bubble's edge. In addition, a small fraction of the clouds that are also shadows may prove to lie well within the bubble. The number and nature of such interlopers allows us to place constraints on the bubble's history.
To determine the distances and radial velocities, we collected moderately high-resolution spectra of 62 bright, early-type stars lying near the three clouds using the Sandiford Cassegrain-Echelle spectrograph of the 2.1m Otto Struve Telescope. We then searched the stars’ spectra for interstellar Na-D lines and used their known distances to bracket the distances to the clouds.

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