VizieR Online Data Catalog: Search for flares and CMEs in SDSS data (Koller+, 2021)
Abstract
This file contains the complete list of flares found by this work and their most important derived or collected parameters. The in-depth description of the derivation of these parameters is given in the article.
The optical spectra by SDSSS data release 14 (2018ApJS..235...42A) that we used in this work consist of several single spectra, which are combined to a final coadded spectrum for each observed object. We used the single spectra to find temporal changes in Balmer lines, indicating flaring events. With the latest GAIA data release (2018A&A...616A...1G), we were able to derive energy and luminosity values for the flares. We focused on the Halpha Balmer line due to the better S/N. Our methods were based on line fitting algorithms to detect changes from one observation to another. Similar to the work by Hilton et al. (2010, Cat. J/AJ/140/1402) we give stellar coordinates as RAdeg and DEdeg as the first parameters to distinguish between the objects. In addition to that, the Plate-MJD-Fiber number serves as a unique identifier for the flaring SDSS spectrum. The stellar position is not enough because objects can be observed multiple times at different surveys by SDSS, resulting in different sets of single spectra. The method and the categorization of the S/N bins are defined in the article. The spectral type classified by SDSS and by other literature is given. The distance and the source for the value is given when possible. The defined quiet flag and the consideration flag give insight on the reliability of the derived values. Whether a flare was also detected in Hilton et al. (2010, Cat. J/AJ/140/1402) is given in a separate column. The flare energy, the luminosity, and the associated errors were derived using the SDSS spectra as is described in the article (see Sect.4.2.2) and given here in units of W and W/s (J). The peak spectrum and the spectrum used in the calculation as the reference are given. Their number refer to the chronological order of the single spectra. The number of available single spectra (in the optical red domain containing Halpha) and the number of single spectra in a flaring state are given. The overall time of these flaring spectra is summed and given in units of minutes. Additional comments made during the visual inspection of all flaring spectra are added. (1 data file).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- November 2020
- DOI:
- 10.26093/cds/vizier.36460034
- Bibcode:
- 2020yCat..36460034K
- Keywords:
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- Stars: flare;
- Stars: late-type;
- Balmer lines