![]() The r CCDs are calibrated by matching up bright stars detected by SDSS with the UCAC astrometric reference catalogs. That is, the positions for SDSS objects are based on the r centroids and calibrations. Any advice which can point me in the right direction would be appreciated, even if you have suggestions for alternative research problems. The r photometric CCDs serve as the astrometric reference CCDs for the SDSS. I've read about maggies but not sure which variation of the unit to use.įor some context, I am trying to establish a research niche by targeting dim spectra in particular, hence my interest in the magnitude measures. Is there a single general unit for the magnitude of the spectra (in terms of brightness I mean).What method is currently used to classify the spectra? Does the SDSS have ML algorithms of its own? I assume they can't all be visually classified given the sheer volume of spectra. This algorithm determines which fields are used as the primary observation of any given region of sky and which catalog entries are the primary detections of the given source.Are the SDSS surveys (eBoss, APOGEE2, etc) spectroscopic or photometric surveys? What is the basic difference between these in terms of what the data for each type would look like?. ![]() ![]() Not sure if this is an appropriate place for these kinds of questions, if not please direct me to a better alternative. we will provide a workflow to query catalogs such as SDSS and Gaia via the. I'm considering doing research on SDSS spectral classification (STAR, GALAXY, QSO) with machine learning for my school dissertation. When absolute astrometry is desired, the images can be aligned to an external.
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