Volume 49, Nº 7 (2023)

We describe the methods of the SRGz system for the physical identification of eROSITA point X-ray sources from photometric data in the DESI Legacy Imaging Surveys footprint. We consider the models included in the SRGz system (version 2.1) that have allowed us to obtain accurate measurements of the cosmological redshift and class of an X-ray object (quasar/galaxy/star) from multiwavelength photometric sky surveys (DESI LIS, SDSS, Pan-STARRS, WISE, eROSITA) for 87 %  of the entire eastern extragalactic region (0 < l < 180◦, |b| > 20◦). An important feature of the SRGz system is that its data handling model (identification, classification, photo-z algorithms) is based entirely on heuristic machine learning approaches. For a standard choice of SRGz parameters the optical counterpart identification completeness (recall) in the DESI LIS footprint is 95% (with an optical counterpart selection precision of 94%); the classification completeness (recall) of X-ray sources without optical counterparts in DESI LIS is 82% (85% precision). A high quality of the photometric classification of X-ray source optical counterparts is achieved in SRGz: >99% photometric classification completeness (recall) for extragalactic objects (a quasar or a galaxy) and stars on a test sample of sources with SDSS spectra and GAIA astrometric stars. We present an analysis of the importance of various photometric features for the optical identification and classification of eROSITA X-ray sources. We have shown that the infrared (IR) magnitude W2, the X-ray/optical(IR) ratios, the optical colors (for example, (g − r)), and the IR color (W1-W2) as well as the color distances introduced by us play a significant role in separating the classes of X-ray objects. We use the most important photometric features to interpret the SRGz predictions in this paper. The accuracy of the SRGz photometric redshifts (from DESI LIS, SDSS, Pan-STARRS, and WISE photometric data) has been tested in the Stripe82X field on a sample of 3/4 of the optical counterparts of eROSITA point X-ray sources (for which spectroscopic measurements are available in Stripe82X): σNMAD = 3.1% (the normalized median absolute deviation of the prediction) and n>0.15 = 7.8%  (the fraction of catastrophic outliers). The presented photo-z results for eROSITA X-ray sources in the Stripe82X field are more than a factor of 2 better in both metrics ( σNMAD and n>0.15) than the photo-z results of other groups published in the Stripe82X catalog.

The extreme levels of solar activity on time scales of 300–400 and 9000 years are considered. The total sunspot area AR, a physical index of solar activity, has been estimated using the sunspot number reconstruction from Wu et al. (2018). The main study has been carried out precisely in terms of this index. The variations in solar activity at the epoch of the last 300–400 years represent fairly well its variations on time scales of the order of nine millennia. The maximum level of solar activity for the yearly averages is ARM = 2930 ± 400  m.s.h. (millionths of the solar hemisphere). The upper limit for the daily values is ARM = 7500 ± 2200  m.s.h. for the traditional sunspot areas corrected for the perspective distortion and AROM = 11 400 ± 3300  m.s.d. (millionths of the solar disk) for the so-called ‘‘observed’’ areas—the sunspot projections onto the visible solar disk. The maximum yearly averages of the sunspot number SNM = 258 ± 38 and the sunspot group number GNM = 12.3 ± 2.4; 11.3%  have also been estimated; 11.3% of the time the solar activity is at an extremely high level; 8.5 and 4.5 %  of the time its level corresponds to the Dalton minimum or lower and an extremely low one, respectively. Thus, extremely high levels are more likely for solar activity than extremely low ones.