1. Introduction
2. Data sources
2.1. First eROSITA all-sky survey
2.2. Gaia DR3
3. The HamStar identification procedure
3.1. Data selection
3.2. Coronal probabilities
3.3. Bayes map construction
4. Results
4.1. Number of coronal eRASS1 sources and the coronal fraction
4.2. Completeness and reliability
4.3. Comparison with Chandra detections
4.4. Comparison with identifications from NWAY
4.5. Catalog of the coronal identifications
5. Properties of the coronal eRASS1 sources
5.1. Noncoronal contamination
5.2. Multiplicity
5.3. Color–magnitude diagram
5.4. X-ray over bolometric flux
5.5. Rotation–activity relation
6. Discussion of error and caveats
7. Conclusions and outlook