Statistics
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........14m&link_type=abstract
Thesis (PH.D.)--YALE UNIVERSITY, 1995.Source: Dissertation Abstracts International, Volume: 56-08, Section: B, page: 4374.
Statistics
9
Galactic Structure
Scientific paper
A Galactic Structure and Kinematic Model code (GSKM) is described which predicts the number of stars as a function of apparent magnitude, color, and kinematics by using the fundamental equation of stellar statistics. The kinematic model uses Schwarzschild's velocity ellipsoids to represent the distribution of stars in velocity space and the velocity lag for the disk is computed self -consistently through the asymmetric drift equation and the assumed density function for the disk component. Comparison of the GSKM with low-latitude proper motions toward the open clusters NGC 188 and NGC 3680 show that the model can be used to determine tangential velocities for open clusters with a 5% uncertainty (10% for globular clusters), even in those cases where there are no objects available in the field-of-view to provide a zero-point correction. At the South Galactic Pole (SGP) the GSKM shows that the local relative normalization of thick-disk stars needs to be increased by about 50% above the current estimates of 2%. The absolute proper motion distribution is compatible with a model having a prograde halo with a lag of -170 +/- 50 km/s, if the thick-disk is lagging -70 km/s behind the disk. The preliminary results from the Yale/San Juan Southern Proper Motion program towards the SGP indicate that there is a systematic difference of 2 to 4 mas/yr between the observations and the model. We explore the origin of this discrepancy with the aid of the model. Finally, a new reddening model is developed. Comparison with both star counts at low Galactic latitudes and diffuse star light measurements show excellent agreement between the reddening model predictions and observations. The reddening model will enable us to compute corrections from relative to absolute parallax and proper motion for low Galactic latitude stars.
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