Edward Brown edited integration-lecture-lab.tex  about 9 years ago

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The first two weeks of lecture now discusses angular coordinates, right ascension and declination, sidereal time, and parallax. In the first lab, students find objects on the sky using with the \href{http://www.stellarium.org/}{\verb|Stellarium| planetarium software}; in the second lab, the students determine which celestial objects are visible from the MSU campus observatory. The lectures then discuss the inverse-square-law for flux, magnitude, and the distance modulus. A discussion of the wave nature of light, in particular diffraction, then follows. This dovetails with the lab, in which students use the \href{http://ds9.si.edu/site/Home.html}{\verb|ds9| visualization software} to measure point-spread functions.  Following these topics, the next three weeks of lectures are devoted to probability and statistics, with course notes drawn from \citet{Taylor1997An-Introduction} and \citet{Durrett1994The-Essentials-}. Starting with a derivation of probability rules from set-theoretical concepts, we discuss combinatorics and then build to a derivation of the binomial distribution in the context of the random walk. The small-probability limit as a Poisson distribution is introduced, and then we imagine measurement fluctuations as a random walk with a corresponding normal distribution. From there, we derive the uncertainty in the mean, propagation of uncertainties, and the use of the $\chi^2$-statistic. $\chi^2$-statistic (see Figure~\ref{fig:sample-datasets}).  In parallel, the students work through a multi-part lab in which they determine the distance to the Hyades and its age. This puts into practice the statistical concepts discussed in lecture.  At this point, the lectures and lab diverge, as the discussion in the lectures turns to detection of exoplanets. We continue to pose questions relating to probability, so that the students must review previously discussed topics. For example, one exercise asks students to compute the probability that a planetary mass, detected via Doppler velocity measurements of the host star, exceeds a certain value.