The Pan-STARRS1 Photometric System

The Pan-STARRS1 survey is collecting multi-epoch, multi-color observations of the sky north of declination -30 deg to unprecedented depths. These data are being photometrically and astrometrically calibrated and will serve as a reference for many other purposes. In this paper we present our determination of the Pan-STARRS photometric system: gp1, rp1, ip1, zp1, yp1, and wp1. The Pan-STARRS photometric system is fundamentally based on the HST Calspec spectrophotometric observations, which in turn are fundamentally based on models of white dwarf atmospheres. We define the Pan-STARRS magnitude system, and describe in detail our measurement of the system passbands, including both the instrumental sensitivity and atmospheric transmission functions. Byproducts, including transformations to other photometric systems, galactic extinction, and stellar locus are also provided. We close with a discussion of remaining systematic errors.Comment: 39 pages, 9 figures, machine readable table of bandpasses, accepted for publication in Ap

Results of Periodontal Therapy Related to Tooth Type

Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/142120/1/jper0270.pd

Short Term Results of Three Modalities of Periodontal Treatment

Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/141914/1/jper0131.pd

Longitudinal Study of Periodontal Therapy

Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/142010/1/jper0066.pd

Results Following Three Modalities of Periodontal Therapy

Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/141627/1/jper0522.pd

Properties of M31. II: A Cepheid disk sample derived from the first year of PS1 PAndromeda data

We present a sample of Cepheid variable stars towards M31 based on the first year of regular M31 observations of the PS1 survey in the r_P1 and i_P1 filters. We describe the selection procedure for Cepheid variable stars from the overall variable source sample and develop an automatic classification scheme using Fourier decomposition and the location of the instability strip. We find 1440 fundamental mode (classical \delta) Cep stars, 126 Cepheids in the first overtone mode, and 147 belonging to the Population II types. 296 Cepheids could not be assigned to one of these classes and 354 Cepheids were found in other surveys. These 2009 Cepheids constitute the largest Cepheid sample in M31 known so far and the full catalog is presented in this paper. We briefly describe the properties of our sample in its spatial distribution throughout the M31 galaxy, in its age properties, and we derive an apparent period-luminosity relation (PLR) in our two bands. The Population I Cepheids nicely follow the dust pattern of the M31 disk, whereas the 147 Type II Cepheids are distributed throughout the halo of M31. We outline the time evolution of the star formation in the major ring found previously and find an age gradient. A comparison of our PLR to previous results indicates a curvature term in the PLR

Results of Periodontal Treatment Related to Pocket Depth and Attachment Level. Eight Years

Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/141007/1/jper0225.pd