HamStar_eRASS1_Main_Possible_Identifications_v1.1.fitsContent of the page (HDU means "Header Data Unit" of a fits file).
Catalog table
| Name | Type | Unit | Description |
|---|---|---|---|
| ERO_IAUNAME | char[23] | None | IAU name of the eRASS1 sources (IAUNAME) |
| ERO_DETUID | char[32] | None | Unique detection ID of the eRASS1 sources (DETUID) |
| ERO_MJD | float32 | mjd | Epoch of the observation of the eRASS1 source (MJD) |
| ERO_POS_ERR | float32 | arcsec | Positional uncertainty of the eRASS1 source (POS_ERR) |
| CTP_RANK | int32 | None | Rank of the counterpart that increase for less likely alternative counterparts |
| CTP_ID | int64 | None | Identifier of the counterpart (source_id if Gaia source, otherwise combination of TYC1, TYC2, TYC3; for Tycho-2 only sources CTP_ID < 1e10) |
| CTP_SEP | float32 | arcsec | Proper motion corrected angular separation between eRASS1 source and counterpart adopting the observation time of the eRASS1 source as provided by ERO_MJD |
| p_coronal | float64 | None | Probability of the eRASS1 source to be coronal |
| p_ij | float64 | None | Probability of the counterpart to be associated to the eRASS1 source |
| CTP_RA | float64 | deg | Proper motion corrected right ascension of the counterpart adopting the observation time of the eRASS1 source as provided by ERO_MJD |
| CTP_DEC | float64 | deg | Proper motion corrected declination of the counterpart adopting the observation time of the eRASS1 source as provided by ERO_MJD |
| Fx | float64 | erg/s/cm2 | X-ray flux in the 0.2 - 2.3 keV band assuming a coronal spectrum |
| G | float64 | mag | G band magnitude of the counterpart |
| BP_RP | float64 | mag | BP-RP color of the counterpart |
| PLX | float64 | mas | Parallax of the counterpart |
| SIMBAD_NAME | char[40] | None | Name of the Simbad identification if available |
| SIMBAD_OTYPE | char[20] | None | Classification in the Simbad database if available |
| TRAIN_SET | bool | None | True if counterpart to an eRASS:4 training set source |
| CORONAL | bool | None | False if the properties are untypical for coronal X-ray emitters |
| OB_STAR | bool | None | True for likely reddened OB stars |
| FLAG_OPT | bool | None | True if the source is affected by optical loading, adopted from the eRASS1 catalog |
| NWAY_DIFFCTP | bool | None | True if NWAY provides a different best counterpart |
Gaia Collaboration et al., Gaia Data Release 3, A&A, 674A, 1, (2023)
Predehl, P., et al., The eROSITA X-ray telescope on SRG, A&A, 647A, 1 (2021)
We thank Andrea Merloni for very helpful comments and suggestions.
SF gratefully acknowledge supports through the Integrationsamt Hildesheim and the ZAV of Bundesagentur für Arbeit, SC by DFG under grant CZ 222/5-1, JR by DLR under grant 50 QR 2105, and PCS by DLR under grant 50 OR 1901 and 50 OR 2102. SF thanks Gabriele Uth and Maria Theresa Lehmann for their support.
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/NRTA software system developed by the German eROSITA consortium.
This work has made use of data from the European Space Agency (ESA) mission
Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia
Data Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC
has been provided by national institutions, in particular the institutions
participating in the Gaia Multilateral Agreement.
This research has made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive.
This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
This research has made use of the VizieR catalogue access tool, CDS,
Strasbourg, France (DOI : 10.26093/cds/vizier). The original description
of the VizieR service was published in 2000, A&AS 143, 23