I have only fiddled with Canopus a couple of times and that was a few years ago. Therefore it would be hard for me to compare others to it.
I also found Maxim DL to be very limited particularly since you must have a comparison star to use the photometry tool and the information window aperture tool is not very accurate and is not recommended for photometry. You can't get raw magnitudes, at least I found no way to get them and for certain things like establishing transformation coefficients you don't want to do differential photometry. You want the raw magnitudes.
Many people use AIP4WIN. I have used it in the past and it's pretty good and readily available as freeware. More than 5 years ago I tried a number of different packages and decided I liked Mira-pro the best. It was developed by Michael Newberry, one of the original developers of IRAF. It has robust GUI interfaced algorithms for photometry and other image analysis tasks - including source extractor - and one of the slickest image calibration pipelines I have ever seen. Fujitsu scansnap s1500 software mac download. The problem is it is expensive - on the order of Maxim DL or a bit more if you get the scripting add-ons. This was developed as a Windows program but I think it is also available for the current MAC OS.
Of course there is IRAF itself or the version integrated with Python, PYRAF. If you found Canopus too complicated you will find these ridiculously so. IRAF, however is regarded as the gold standard of Image Reduction and Analysis (Facility) software for astronomy. It is versatile, has lots of add-on packages to do almost anything you can imagine, has a image viewing interface called DS9 that is incredibly versatile but it has a very difficult learning curve. There is also a free package called image J. It was developed for medical imaging photometry as were many of the best photometry packages including Mira-Pro (because that is where the money is). Image J is quite a good package BUT the last time I looked it did not have a conversion into magnitudes. You had to do that as a manual step at the end. It has some very interesting and helpful features, however and it is free.
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Finally, I have used VPhot and have not had unexpected results. It seems to work well. I don't know if there is a version that you can download to your computer. You could in its original implementation as Photometrica and perhaps it still can be. that would be an interesting question to ask on the forum. I don't see a post on that topic. I agree Uploading images to VPhot is a problem. It was bad enough with my old ST7 that was about 0.8 Mbyte per image. With my new camera at 16 Mbyte per image, it is essentially impossible for more than a very few images over my DSL connection at 0.7Mbps. If you have 10 Mbps it might not be such a pain. It would be great if there were a VPhot client that ran on user computers to do all the heavy lifting on the image with automated interfaces to AAVSO for Variable star search comp stars, and reporting. That could also greatly reduce the storage and traffic on AAVSO servers. I am not competent to evaluate the complexity of such a development project, however.
I am sure that I haven't scratched the surface of all the photometry packages that are out there. There are probably a whole bunch I have never heard of or have forgotten about.
Brad Walter
PS:
Perhaps I should be specific about the meaning I apply to 'raw magnitude' what I mean is precisely
-2.5*LOG(Netcounts*GAIN.EXPTIME)
So it is a negative number, or if you offset all measurements by the same sufficiently large constant you can make them positive i.e. -2.5*LOG(Netcounts*GAIN/EXPTIME) + 25
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So not only is it not transformed, it isn't referenced to a comparison star magnitude.
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I use the term 'instrumental magnitude' for a magnitude that is referenced to a comparison or standard star magnitude but which is not transformed.
Tmag_raw - Cmag_raw + Cmag_sequence
A Confusing Vocabulary:
The terms raw, instrumental standard, differential and absolute are not uniformly used and can have conflicting meanings in different contexts or different meanings in the same context when used by different people. It leads to confusion. The term standard as used in the MTYPE field of WebObs, for example is a bit of a misnomer although it is completely explained in the link in the notes, if you read that far. I would only use the term standard to apply to the magnitude of a recognized standard star. I wouldn't even use it to describe a magnitude that had been transformed to a standard magnitude scale. I would use 'transformed' to describe that. I don't even use 'standard' to describe the chart magnitude of a comparison star. I use 'sequence' magnitude or 'reference' magnitude to describe comp star magnitudes (unless they are recognized standard stars) because most sequence star magnitudes are only transformed to a standard magnitude scale. They are not sufficiently measured to qualify as a photometric standard stars.
I certainly would never use the term 'absolute' magnitude to mean anything other than a magnitude transformed to a recognized standard and adjusted for distance and interstellar extinction to an observational distance of 10 parsecs (see 2.3.3 in Binney and Merrifield, for example) but you sometimes see it used to mean an instrumental magnitude,
Tmag_raw -Cmag_raw + Cmag_sequence,
to distinguish it from a differential magnitude,
Tmag_raw - Cmag_raw.
To add to the confusion, either of these two magnitude types are most frequently produced by AAVSO members using differential photometry vs. all-sky photometry. So differential photometry does not necessarily result in a differential magnitude, but it can. It just depends on which formula you use.
Hp photosmart c4599 software download mac software. Some of these distinctions are only the vocabulary choices of one journeyman amateur, but I think they make distinctions much clearer, particularly trying to explain things to someone new to photometry.
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