Progenitor Constraint with Circumstellar Material for the Magnetar-hosting Supernova Remnant RCW 103

Stellar winds blown out from massive stars (greater than or similar to 10 M (circle dot)) contain precious information on the progenitor itself, and in this context the most important elements are carbon (C), nitrogen (N), and oxygen (O), which are produced by the CNO cycle in the H-burning layer. Although their X-ray fluorescence lines are expected to be detected in swept-up shock-heated circumstellar materials in supernova remnants, those of C and N have been particularly difficult to detect so far. Here, we present high-resolution spectroscopy of the young magnetar-hosting supernova remnant RCW 103 with the Reflection Grating Spectrometer on board XMM-Newton and report on the detection of the N vii Ly alpha (0.50 keV) line for the first time. By comparing the obtained abundance ratio of N to O (N/O = 3.8 +/- 0.1) with various stellar evolution models, we show that the progenitor of RCW 103 is likely to have a low mass (10-12 M (circle dot)) and medium rotation velocity (less than or similar to 100 km s(-1)). The results also rule out the possibility of dynamo effects in massive (>= 35 M (circle dot)) stars as a mechanism for forming the associated magnetar 1E 161348-5055. Our method is useful for estimating various progenitor parameters for future missions with microcalorimeters such as XRISM and Athena.

Automated summary

Stellar winds from massive stars contain important information about the stars themselves, particularly carbon, nitrogen, and oxygen. Detecting and studying these elements in supernova remnants is challenging. In this study, the N vii Ly alpha line was detected for the first time in the young magnetar-hosting supernova remnant RCW 103. By comparing the abundance ratio of nitrogen to oxygen, the progenitor of RCW 103 was estimated to be a low mass star with medium rotation velocity. This study has implications for future missions in estimating progenitor parameters.