{"id":1964,"date":"2025-12-05T12:29:22","date_gmt":"2025-12-05T11:29:22","guid":{"rendered":"https:\/\/www.for5195.uni-wuerzburg.de\/?page_id=1964"},"modified":"2026-03-21T13:22:30","modified_gmt":"2026-03-21T12:22:30","slug":"annual-assembly-2026-1","status":"publish","type":"page","link":"https:\/\/www.for5195.uni-wuerzburg.de\/index.php\/annual-assembly-2026-1\/","title":{"rendered":"Annual Assembly 2026"},"content":{"rendered":"\n
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Group picture of participants at the Annual Assembly 2026, Credit: P. G\u00fcnther \/ FOR 5195<\/figcaption><\/figure>\n\n\n\n
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The annual assembly 2026 took place as a three-day meeting on 9 – 11 March in W\u00fcrzburg.<\/strong><\/p>\n\n\n\n

The meeting was the annual gathering of all members and associated researchers of our research unit as well as of selected experts external to the research unit. Participants had the opportunity to present their research topics, their numerical, computational or analytical techniques, their barriers and obstacles to progress, current difficulties and immediate problems as well as their near-future goals. There also was ample space to discuss conceptual models, recent findings up to now, as well as to plan future starting points of research. We have gained insight about different approaches, about solution finding and in particular we planned future collaborations and potential synergies to enrich our colleagues’ work with fruitful hints.<\/p>\n\n\n\n

For additional information and for the schedule, registered participants may visit this page with more detailed information<\/a>.<\/p>\n\n\n\n

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\"Impression
Impressions from the Annual Assembly 2026, Credit: Patrick G\u00fcnther<\/figcaption><\/figure>\n<\/div>\n\n\n\n
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\"Impression<\/figure>\n\n\n\n
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\"Scientists<\/a>
Scientists of our project P2 have examined the X-ray spectrum of the nearby Seyfert-2 galaxy ESO 033-G002, which exhibits prominent relativistic reflection and a strong broad 6.4 keV iron K\u03b1 line. Panel (a) shows data from XMM-Newton and NuSTAR. In a study performed by Alexey Nekrasov, it was demonstrated (panel b) that the spectrum can be reproduced assuming a ring-like primary source that illuminates the accretion disk, resulting both in relativistic reflection (relxill refl) and direct emission (relxill prim), a distant reflector (xillver), a scattered nuclear component (nthComp), as well as emission from collisionally ionised diffuse plasma (apec). It was found that the primary source is located within three gravitational radii from the black hole.
Credit: “Relativistic reflection within an extended hot plasma geometry”,
A. Nekrasov et al., A&A, 2025, DOI: 10.48550\/arXiv.2510.13337 <\/a><\/figcaption><\/figure>\n<\/div>\n<\/div>\n\n\n\n
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DFG Research Unit (Forschungsgruppe) FOR 5195 \u2013 Relativistic Jets in Active Galaxies<\/a><\/h1>\n\n

Funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)<\/p><\/div>\n\n\n\n

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