Elias Kammoun, T. Kawamuro, Koichi Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, Michael Eracleous, Oluwashina Adegoke, E. Bertola, Peter Boorman, V. Braito, G. Bruni, A. Comastri, Pierpaolo Condó, M. Dadina, Teruaki Enoto, Javier A. García, V. E. Gianolli, Fiona Harrison, G. Lanzuisi, M. Laurenti, Andrea Marinucci, Guglielmo Mastroserio, Hironori Matsumoto, G. Matt, G. A. Matzeu, R. Middei, E. Nardini, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, F. Panessa, E. Piconcelli, C. Pinto, Joanna M. Piotrowska, G. Ponti, Cláudio Ricci, R. Ricci, Roberto Serafinelli, Fangzheng Shi, Daniel Stern, A. Tanimoto, Yuichi Terashima, Ryota Tomaru, Francesco Tombesi, A. Tortosa, Yoshihiro Ueda, F. Ursini, C. Vignali, Satoshi Yamada, S. Yamada
Abstract We present the first high-resolution X-ray spectrum of NGC 7213 obtained with XRISM/Resolve, supported by simultaneous XMM-Newton, NuSTAR, and SOAR optical data. The XRISM spectrum resolves the neutral Fe K α into two components: a narrow core ( FWHM = 65 0 − 220 + 240 km s − 1 ), consistent with emission at the dust sublimation radius, and a broader asymmetric line, best described by disklike emission from ∼100 R g . This disk component mirrors the profile of the double-peaked H α line observed in the optical. In addition, we detect broadened Fe xxv and Fe xxvi emission lines, whose inferred locations bridge the gap between the inner disk and the optical broad-line region. The weak narrow Fe K α equivalent width (EW = 32 ± 6 eV) and the absence of a Compton hump imply a low-covering-fraction, Compton-thin torus. Together, these results reveal a radially stratified structure in NGC 7213, spanning nearly 4 orders of magnitude in radius, and place the source in an intermediate-accretion state ( λ Edd = 0.1%–1%), where the inner disk and broad-line region remain, while the torus shows signs of dissipation.