The Structure of the Relativistic Fe Line in GX 340+0 as Viewed with XRISM/Resolve, NICER, and NuSTAR
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| Main Authors: | , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866909679729246208 |
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| author | Ludlam, R. M. Ballhausen, R. Chakraborty, P. Costantini, E. Corrales, L. Hall, H. Kilbourne, C. Moutard, D. L. Nakagawa, T. Porter, F. S. Psaradaki, I. Sudha, M. Smith, R. K. Takahashi, H. Done, C. García, J. A. |
| author_facet | Ludlam, R. M. Ballhausen, R. Chakraborty, P. Costantini, E. Corrales, L. Hall, H. Kilbourne, C. Moutard, D. L. Nakagawa, T. Porter, F. S. Psaradaki, I. Sudha, M. Smith, R. K. Takahashi, H. Done, C. García, J. A. |
| contents | We present a 152 ks XRISM/Resolve observation of the persistently accreting Z source GX 340+0. Simultaneous observations also occurred with NuSTAR and NICER for 22.47 ks and 2.7 ks, respectively. The source covered the normal branch to the flaring branching during the observations. The data from all three missions were modeled concurrently for each spectral branch. The superior energy resolution of XRISM/Resolve reveals structure within the iron emission line complex regardless of spectral state. We model the reprocessed Fe K line with a reflection model tailored for thermal illumination of the accretion disk by a neutron star. The currently available model encompasses the broad components, but narrow emission features remain at the ~5% level. These remaining features may be described by the presence of an ionized plasma in the system as has been observed in the Z source Cygnus X-2, but subsequent updates to the reflection model code may be able to explain these features. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_06289 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Structure of the Relativistic Fe Line in GX 340+0 as Viewed with XRISM/Resolve, NICER, and NuSTAR Ludlam, R. M. Ballhausen, R. Chakraborty, P. Costantini, E. Corrales, L. Hall, H. Kilbourne, C. Moutard, D. L. Nakagawa, T. Porter, F. S. Psaradaki, I. Sudha, M. Smith, R. K. Takahashi, H. Done, C. García, J. A. High Energy Astrophysical Phenomena We present a 152 ks XRISM/Resolve observation of the persistently accreting Z source GX 340+0. Simultaneous observations also occurred with NuSTAR and NICER for 22.47 ks and 2.7 ks, respectively. The source covered the normal branch to the flaring branching during the observations. The data from all three missions were modeled concurrently for each spectral branch. The superior energy resolution of XRISM/Resolve reveals structure within the iron emission line complex regardless of spectral state. We model the reprocessed Fe K line with a reflection model tailored for thermal illumination of the accretion disk by a neutron star. The currently available model encompasses the broad components, but narrow emission features remain at the ~5% level. These remaining features may be described by the presence of an ionized plasma in the system as has been observed in the Z source Cygnus X-2, but subsequent updates to the reflection model code may be able to explain these features. |
| title | The Structure of the Relativistic Fe Line in GX 340+0 as Viewed with XRISM/Resolve, NICER, and NuSTAR |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2507.06289 |