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Request for AIP4WIN and other CCD photometry software Dear Colleagues, While writing a comment on NMO Campaign (not directly relevant), an idea comes to my mind. Present-day (amateur) CCD observations heavily rely on automated CCD photometry programs. I have a concern whether the available features in such programs have forced the style of CCD observers into a very specialized form. For many CCD photometry programs, time-series analyses of a long run on a single object is an easy task, and people becoming familiar with CCD observations are getting more involved in this type of observation than other forms of observation, but this is not the only method of variable star observing. With the present-day automatic pointing of the telescope, one can reasonably get images over 100 objects within a single night. These observations will enable us to detect many outbursts of CVs, long-term light curve of long- or intermediate-period variable stars, both of which are very traditional style of variable star observing, but are not reasonably supported by current CCD photometry programs. I thereby request to authors of these programs to implement a function to make photometry of many targets (i.e. many variable stars) within the same night, without bothering to issue many independent commands or time-consuming eye examination of individual images. There will be two approaches. One will be to equip present variable star charts or sequences (or photometric standards), with which one can automatically measure any variable star which is included in these chart/sequence collections once the observer get a CCD image of the field. This is an extention of the traditional style of variable star observing. For CVs, Henden/Sumner/Misselt sequences (and future extensions) will be sufficient. We may need a similar public database of sequences for other types of variable stars until we can get all-sky reliable photometric catalogs. The other is an extention of time-series studies. Once the observer selects a set of comparisons for a certain object, the program automatically uses this set for the same object on later observing nights. The set of comparison stars can be redefined later when the initial set becomes inadequate. After operating with this style, the observer can get a fair collection of personal sequences for many variable stars with necessary precision and consistency what the observer expects for time-series photometry. The second approach would be similar to what RoboScope has been doing for long-term activities of CVs. Writing such functions would be, by themselves, a difficult task, but once they are implemented, they will be a far greater tool for all CCD variable star observers, and I would surely recommend such a tool for all observers starting with a CCD. I wonder whether such an idea has already proposed by other variable star organizations. Any further suggestions or comments are welcome. Regards, Taichi Kato
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