Solar energy paper index
eROSITA all-sky survey - stars and optical loading
One-line summary
A solar energy research paper on eROSITA all-sky survey - stars and optical loading.
Engineering notes
Engineering notes will be added by the Power for Solar editorial team.
Chinese explanation / 中文解读
中文解读待补充：本站会优先为光伏效率、钙钛矿太阳能电池、储能技术、太阳能热利用、BIPV、并网技术等高价值论文补充中文说明。
Original abstract
eROSITA (extended ROentgen Survey with an Imaging Telescope Array) on board the Spectrum-Roentgen-Gamma (SRG) spacecraft has performed the eROSITA All-Sky Survey (eRASS) at X-ray energies. We study the brighter stars to assess the impact of optical loading in the eROSITA all-sky survey, here specifically the eRASS:3. Further we use thermal plasma models to investigate the general properties of stellar eRASS sources and compare optical loading affected stars to coronal sources. We compare data from Gaia DR3, Tycho-2, 2MASS and the SIMBAD database with the eRASS count rates of brighter stars. We analyze X-ray images, light curves and spectra for sources suspected to be affected by optical loading and determine their properties. eROSITA source properties are checked in comparison to genuine coronal sources with generated sets of APEC model spectra, where we determine rate conversion factors and hardness ratios for stellar X-ray emitter. Regarding optical loading we find a clear correlation between optical brightness and observed minimum count rate in the range of about 2\,--\,5 mag (V/G band), which then saturates for very bright sources. While magnitude and color are the main determinants, exposure depth and specific scanning paths also matter. For intrinsic X-ray emitters, optical contamination is likewise observed. We characterize the fake X-ray sources, address pseudo variability and spectral properties. To interpret stellar eRASS data, hardness ratios and count rate conversions for thermal plasma models are provided. The eROSITA data is prone to optical loading, which was studied in greater detail. The optical loading flag for the DR2 is set, if sources are brighter than 5.0~mag (B, V, G) or 3.5~mag (J). It is somewhat dependent on exposure depth, but we expect only minor changes for future data releases.
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