{"paper":{"title":"The geometry of the hot corona in MCG-05-23-16 constrained by X-ray polarimetry","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A. Brez, A. De Rosa, A. Di Marco, A. F. Tennant, A. Ingram, A. L. Peirson, A. Manfreda, A. Marinucci, A. Papitto, A. P. Marscher, A. Possenti, A. Ratheesh, A. Trois, A. Veledina, B. D. Ramsey, C. Oppedisano, C. Panagiotou, C. Sgr\\`o, C. T. Chen, C. Y. Ng, D. A. Swartz, D. E. Kim, D. Harper, D. Tagliacozzo, E. Cavazzuti, E. Costa, E. Del Monte, F. Capitanio, F. Kislat, F. La Monaca, F. Marin, F. Massaro, F. Muleri, F. Tavecchio, F. Tombesi, F. Ursini, F. Xie, G. G. Pavlov, G. Madejski, G. Matt, G. Spandre, H. Krawczynski, H. L. Marshall, I. Agudo, I. Donnarumma, I. Liodakis, I. Mitsuishi, J. A. Garcia, J. Heyl, J. J. Kolodziejczak, J. Podgorny, J. Poutanen, J. Rankin, J. Vink, K. Wu, L. A. Antonelli, L. Baldini, L. Di Gesu, L. Latronico, M. Bachetti, M. C. Weisskopf, M. Dovciak, M. Negro, M. Perri, M. Pesce Rollins, M. Pilia, N. Bucciantini, N. Cavero Rodriguez, N. Di Lalla, N. E. Thomas, N. Omodei, O. J. Roberts, P. Kaaret, P. O. Petrucci, P. Slane, P. Soffitta, R. Bellazzini, R. Bonino, R. Ferrazzoli, R. Middei, R. Taverna, R. Turolla, R. W. Romani, S. Bianchi, S. Castellano, S. Ciprini, S. D. Bongiorno, S. Fabiani, S. G. Jorstad, S. Gunji, S. L. O'Dell, S. Maldera, S. Puccetti, S. R. Ehlert, S. S. Tsygankov, S. Zane, T. Barnouin, T. Enoto, T. Kitaguchi, T. Mizuno, T. Tamagawa, V. Doroshenko, V. Karas, W. H. Baumgartner, W. Iwakiri, W. Zhang, Y. Evangelista, Y. Tawara","submitted_at":"2023-05-17T13:45:08Z","abstract_excerpt":"We report on the second observation of the radio-quiet active galactic nucleus (AGN) MCG-05-23-16 performed with the Imaging X-ray Polarimetry Explorer (IXPE). The observation started on 2022 November 6 for a net observing time of 640 ks, and was partly simultaneous with NuSTAR (86 ks). After combining these data with those obtained in the first IXPE pointing on May 2022 (simultaneous with XMM-Newton and NuSTAR) we find a 2-8 keV polarization degree $\\Pi$ = 1.6 $\\pm$ 0.7 (at 68 per cent confidence level), which corresponds to an upper limit $\\Pi$ = 3.2 per cent (at 99 per cent confidence level"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2305.10213","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2305.10213/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}