2XMM Flares Detected from Tycho-2 Stars

This table contains the results from a uniform, large-scale survey of X-ray flare emission, based on the XMM-Newton Serendipitous Source Catalog (2XMM) and its associated data products. This survey comprises both XMM-targeted active stars and those observed serendipitously in the half-degree diameter field-of-view of an observation. The 2XMM Catalog and the associated time-series ('light-curve') data products have been used as the basis for the survey of X-ray flares from cool stars in the Hipparcos Tycho-2 catalog. In addition, the authors have generated and analyzed spectrally-resolved (i.e. hardness-ratio) X-ray light-curves. Where available, they have compared XMM OM UV/optical data with the X-ray light-curves. Their sample contains ~130 flares with well-observed profiles; they originate from ~70 stars. The flares range in duration from ~10<sup>3</sup> to ~10<sup>4</sup> s, have peak X-ray fluxes from ~10<sup>-13</sup> to ~10<sup>-11</sup> erg cm<sup>-2</sup> s<sup>-1</sup>, peak X-ray luminosities from ~10<sup>29</sup> to ~10<sup>32</sup> erg s<sup>-1</sup>, and X-ray energy output from ~10<sup>32</sup> to ~10<sup>35</sup> erg. Most of the ~30 serendipitously-observed (target_flag = 'N') stars have little previously reported information. The hardness-ratio plots clearly illustrate the spectral (and hence inferred temperature) variations characteristic of many flares, and provide an easily accessible overview of the data. In the reference paper, the authors present flare frequency distributions from both target and serendipitous observations. The latter provide an unbiased (with respect to stellar activity) study of flare energetics; in addition, they allow the authors to predict the numbers of stellar flares that may be detected in future X-ray wide-field surveys. The serendipitous sample demonstrates the need for care when calculating flaring rates, especially when normalizing the number of flares to a total exposure time, where it is important to consider both the stars seen to flare and those from which variability was not detected (i.e., measured as non-variable), since in the present survey, the latter outnumber the former by more than a factor of ten.

Source https://heasarc.gsfc.nasa.gov/W3Browse/all/xmmt2flare.html
Metadata Access http://dc.g-vo.org/rr/q/pmh/pubreg.xml?verb=GetRecord&metadataPrefix=oai_datacite&identifier=ivo://nasa.heasarc/xmmt2flare
Creator Pye et al.
Publication Year 2020
Contact Michael Preciado <Michael.E.Preciado@nasa.gov>
Resource Type AstroObjects
Format text/xml
Discipline Various