Circumstellar material (CSM) produced by stellar winds blown out from stars provides
rich information for understanding progenitors of supernova remnants (SNRs). Lighter
elements in CSM such as carbon (C), nitrogen (N), and oxygen (O) critically reflect the
history of the stars and in particular the abundance ratios of N to O (N/O) and N to C
(N/C) of CSM are related to the initial states of the star such as mass, rotation
velocities, and convections (e.g., Maeder et al. 2014). Some previous studies with the
Reflection Grating Spectrometer (RGS) on board XMM-Newton (e.g., Uchida et al. 2019)
have successfully detected lines of C, N, and O around SNRs and the progenitor
constraint with CSM has become available. In this talk, we will introduce the new useful
method of progenitor constraint with CSM for core-collapse (CC) SNRs and report the
results of high-resolution spectroscopy of Galactic CC SNRs RCW 103 (Narita et al. 2023)
and G292.0+1.8 (Narita+ in prep.). We detected the N VII line of these SNRs with RGS for
the first time and found that RCW 103 has the high N/O (=3.8 \pm 0.1) and G292.0+1.8 has
the low N/O (=0.3 \pm 0.1). By comparing our results with several stellar evolution
models, we constrained the progenitor of RCW 103 (a single 10-12 Msun progenitor with a
medium rotation velocity < 100 km/s) and G292.0+1.8 (a progenitor in a binary
system). The progenitor constraint method with CSM established by our studies is useful
for future missions with microcalorimeters such as XRISM and Athena. We will discuss the
future perspectives using CSM such as a companion constraint method with CSM for Type Ia
SNRs.