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Astrophysics Source Code Library

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Searching for codes credited to 'Hernandez, J.'

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[ascl:1705.005] SPTCLASS: SPecTral CLASSificator code

SPTCLASS assigns semi-automatic spectral types to a sample of stars. The main code includes three spectral classification schemes: the first one is optimized to classify stars in the mass range of TTS (K5 or later, hereafter LATE-type scheme); the second one is optimized to classify stars in the mass range of IMTTS (F late to K early, hereafter Gtype scheme), and the third one is optimized to classify stars in the mass range of HAeBe (F5 or earlier, hereafter HAeBe scheme). SPTCLASS has an interactive module that allows the user to select the best result from the three schemes and analyze the input spectra.

[submitted] APPHi: An Automated Photometry Pipeline for High Cadence, Large Volume Data

The software package APPHi (Automated Photometry Pipeline for High Cadence, Large Volume Data), developed to carry out the aperture and differential photometry of the data to be produced
by the TAOS-II project. It is computationally efficient manner and as such, it can be used also with other astronomical wide field image data. The main features of the APPHi software are: its computational speed, the capacity to work with large volumes of data and that it can handle both FITS and HDF5 formats. Due the large number of stars that the software has to handle in an enormous number of frames, it is optimized to automatically find the best value for parameters to carry out the photometry as: mask size for aperture, size of window for extraction of a single star and number of counts for the threshold for detecting a faint star. Using images with similar features to those that will be collected by TAOS-II, we made a comparative performance with IRAF, and found that APPHi can obtain light curves of comparable quality in terms of the SNR, but up to 300 times faster. In addition to its efficiency,
the carried out tests prove that APPHi, although intended to work with the
TAOS-II data, can also be used to analyze any set of astronomical images,
being a robust and versatile tool to perform stellar aperture,
differential photometry.