allnewdr1cvs_fin_2cds.fitsContent of the page (HDU means "Header Data Unit" of a fits file).
Primary header
| Key | Value | Type | Comment |
|---|
New CVs identified in eRASS1, with X-ray and optical properties together with CV type, periods and notes on entries
| Key | Value | Type | Comment |
|---|
| Name | Type | Unit | Description |
|---|---|---|---|
| IAUNAME | char[23] | None | Name of system from the eRASS1 catalog |
| RA_x | float64 | degrees | Right ascension in eRASS1 |
| DEC_x | float64 | degrees | Declination in eRASS1 |
| GaiaID | int64 | None | Source ID in Gaia DR3 |
| RA_epoch2000 | float64 | degrees | Right ascension in Gaia DR3 |
| DEC_epoch2000 | float64 | degrees | Declination in Gaia DR3 |
| Separation_xo | float64 | arcsec | Positional offset between X-ray and optical coordinates |
| G | float64 | mag | Mean Gaia G band magnitude |
| BP-RP | float64 | mag | Difference between Gaia B-band and Gaia R-band magnitudes |
| ML_cts | float32 | None | Total number of X-ray source photons between 0.2 keV and 2.3 keV |
| ML_FLUX | float32 | erg s**(−1) cm**(−2) | eROSITA DR1 X-ray flux in the 0.2 − 2.3 keV band |
| Distance | float64 | pc | rgeo distance from Bailer-Jones et al. (2021) |
| logLx | float64 | erg s**(−1) | Logarithm of the X-ray luminosity in the energy band 0.2 − 2.3 keV |
| log(fx/fopt) | float64 | None | Logarithm of fx to optical using G |
| Gabs | float64 | mag | Absolute G-magnitude based on G and rgeo |
| SubType | char[9] | None | Main type that the CV belongs to |
| Note | char[30] | None | Brief comment on the target |
| Period | float64 | hours | Main period regarded as the orbital period |
| Period2 | float64 | minutes | Secondary period associated with the spin of the WD or a superhump |
We thank an anonymous referee for constructive criticism that helped improving the quality of the paper. This work is based on data from eROSITA, the soft X-ray instrument aboard SRG, a joint Russian-German science mission supported by the Russian Space Agency (Roskosmos), in the interests of the Russian Academy of Sciences represented by its Space Research Institute (IKI), and the Deutsches Zentrum für Luft- und Raumfahrt (DLR). The SRG spacecraft was built by Lavochkin Association (NPOL) and its subcontractors, and is operated by NPOL with support from the Max Planck Institute for Extraterrestrial Physics (MPE). The development and construction of the eROSITA X-ray instrument was led by MPE, with contributions from the Dr. Karl Remeis Observatory Bamberg & ECAP (FAU Erlangen-Nuernberg), the University of Hamburg Observatory, the Leibniz Institute for Astrophysics Potsdam (AIP), and the Institute for Astronomy and Astrophysics of the University of Tübingen, with the support of DLR and the Max Planck Society. The Argelander Institute for Astronomy of the University of Bonn and the Ludwig Maximilians Universität Munich also participated in the science preparation for eROSITA. The eROSITA data shown here were processed using the eSASS software system developed by the German eROSITA consortium. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under program IDs 110.24DX, 111.24Q0, 114.27SL, 115.28JL, and 116.29JQ. This work was supported by the research unit FOR2990 (eRO-STEP: Stellar endpoints with eROSITA) funded by the Deutsche Forschungsgemeinschaft. GL, KK, and VC were supported by the Deutsches Zentrum für Luft- und Raumfahrt (DLR) under Contract Nos. 50 QR 2504, 50 OX 2301, and 50 OR 2405. This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. The Asteroid Terrestrial-impact Last Alert System (ATLAS) project is primarily funded to search for near earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogs from the survey area. This work was partially funded by Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889, and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen’s University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and The Millennium Institute of Astrophysics (MAS), Chile.