Classical Observations of Visual Binary and Multiple Stars

The database of visual double star data has experienced tremendous changes, doubling in size during the last 25 years and growing at an ever increasing rate. Interferometric techniques have allowed the database to extend to much closer separation (and shorter periods), while longer timebases and higher-precision wide-field surveys have increased our knowledge of common proper motion pairs at the widest separations. These changes in the database are highlighted, describing the evolution of methods of observation (both historically and the past few years) and the effectiveness of these various methods in different regimes of separation/ period space. The various niches for wide- and narrow-field work as applied to double and multiple stars are examined and the different types of information which each can provide are also highlighted. After more than 20 years of successful work, speckle interferometry and conventional CCD astrometry have replaced filar micrometry and photography as the preferred classical techniques. Indeed, most work in filar micrometry is now being done by amateurs, although much of that community is also switching to CCDs and other electronic techniques. Despite the significant growth of the double star database, much still remains to be done, such as finding lost pairs, filling in missing parameters so that observing programs may be more efficient at observing stars appropriate to their capabilities, and providing at least approximate kinematic descriptions. Work on pairs described as neglected at the time of the last major WDS data release (2001) is given as a specific example of recent improvements, and finally the continued need to publish data using classical double star parameters is discussed.