{"about":{"site":"https://codewithpapers.app","non_affiliation":"Code with Papers and Syntology are not affiliated with, endorsed by, or sponsored by Papers with Code, Meta, or the pwc-archive mirror.","licence":"CC BY-SA 4.0","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","attribution":"https://codewithpapers.app/attribution","modified":"archive material modified by Syntology; see the attribution page"},"url":"/paper/the-size-of-accretion-disks-from-self","title":"The size of accretion disks from self-consistent X-ray spectra and UV/optical/NIR photometry fitting: applications to ASASSN-14li and HLX-1","arxiv_id":"2408.17296","date":"2024-08-30","proceeding":null,"authors":["Muryel Guolo","Andrew Mummery"],"abstract":"We implement a standard thin disk model with the outer disk radius ($R_{\\rm out}$) as a free parameter, integrating it into standard X-ray fitting package to enable self-consistent and simultaneous fitting of X-ray spectra and UV/optical/NIR photometry. We apply the model to the late-time data ($\\Delta t \\approx 350-1300$ days) of the tidal disruption event (TDE) ASASSN-14li. We show that at these late-times the multi-wavelength emission of the source can be fully described by a bare compact accretion disk. We obtain a black hole mass ($M_{\\rm BH}$) of $7^{+3}_{-2}\\times10^{6} M_{\\odot}$, consistent with host-galaxy scaling relations; and an $R_{\\rm out}$ of $45 \\pm 13 \\, R_{\\rm g}$, consistent with the circularization radius, with possible expansion at the latest epoch. We discuss how simplistic models, such as a single-temperature blackbody fitted to either X-ray spectra or UV/optical photometry, lead to erroneous interpretations on the scale/energetics of TDE emission. We also apply the model to the soft/high state of the intermediate-mass black hole (IMBH) candidate HLX-1. The model fits the full spectral energy distribution (from X-rays to NIR) without needing an additional stellar population component. We investigate how relativistic effects improve our results by implementing a version of the model with full ray tracing calculations in the Kerr metric. For HLX-1, we find $M_{\\rm BH} = 4^{+3}_{-1} \\times 10^{4} M_{\\odot}$ and $R_{\\rm out} \\approx {\\rm few} \\times 10^{3} \\, R_{\\rm g}$, in agreement with previous findings. The relativistic model can constrain the inclination ($i$) of HLX-1 to be $10^o \\leq i \\leq 70^o$.","url_abs":"https://arxiv.org/abs/2408.17296v3","url_pdf":"https://arxiv.org/pdf/2408.17296v3.pdf","source":{"archive":"pwc-archive (Hugging Face), CC BY-SA 4.0","snapshot":"2025-07-28","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","row_kind":"links_only","authors_date_abstract":"arXiv metadata, CC0 1.0 (https://info.arxiv.org/help/license), from the Kaggle arXiv metadata snapshot of 2026-09-12"},"code_links":[{"paper_slug":"the-size-of-accretion-disks-from-self","repo_url":"https://github.com/muryelgp/disksed","is_official":1,"mentioned_in_paper":1,"mentioned_in_github":1,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"syntology_url":null,"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}