First X-ray detection of symbiotic nova CN Cha with eROSITA/SRG

@misc{saeedi2026first,
  title = {{First X-ray detection of symbiotic nova CN Cha with eROSITA/SRG}},
  author = {Sara Saeedi and Jaroslav Merc and Manami Sasaki and Lorenzo Ducci and Michael Freyberg},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.28079},
  eprint = {2609.28079},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.28079},
}

TY  - UNPB
TI  - First X-ray detection of symbiotic nova CN Cha with eROSITA/SRG
AU  - Sara Saeedi
AU  - Jaroslav Merc
AU  - Manami Sasaki
AU  - Lorenzo Ducci
AU  - Michael Freyberg
PY  - 2026
DA  - 2026/09/23
PB  - arXiv
DO  - 10.48550/arxiv.2609.28079
UR  - https://arxiv.org/abs/2609.28079
AB  - Aims. We report on the first X-ray detection of the symbiotic star CN Cha with eROSITA (extended Roentgen Survey with an Imaging Telescope Array) onboard Spektrum-Roentgen Gamma (Spektr-RG). Methods. We analyse the eROSITA observations from eRASS2 to eRASS5 individually, as well as the combined eRASS:5 data of all five surveys in order to investigate the X-ray spectral and timing properties of CN Cha throughout the eRASS. Results. Although CN Cha was not detected during the first eROSITA All-Sky Survey (eRASS1), it was detected for the first time in the second eRASS2. Our analysis shows that the X-ray emission of CN Cha gradually increased from eRASS2 to eRASS5. The X-ray spectrum of the source, with the main emission at <2.4 keV, allows us to classify it as a \b{eta}-type symbiotic star. However, a more detailed analysis suggests that there is very soft component, which may originate either from thermonuclear burning on the white dwarf, or from the wind collisions. Additional X-ray observations are required to better understand the origin and emission mechanisms of the source.
ER  -