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A dynamic black hole corona in an active galaxy through X-ray reverberation mapping

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Nature Astronomy 4: 597- 602 (2020)

http://hdl.handle.net/20.500.12666/152

10.1038/s41550-019-1002-x

2397-3366

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(DIGITAL.INTA)

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Title:: A dynamic black hole corona in an active galaxy through X-ray reverberation mapping
Tema:: Black Hole; Active Galaxy; X ray; Reverberation mapping; Galactic Nuclei; Scattering
Description:: Alston, W.N., Fabian, A.C., Kara, E. et al. A dynamic black hole corona in an active galaxy through X-ray reverberation mapping. Nat Astron 4, 597–602 (2020). https://doi.org/10.1038/s41550-019-1002-x; X-ray reverberation echoes are assumed to be produced in the strongly distorted spacetime around accreting supermassive black holes. This signal allows us to spatially map the geometry of the inner accretion flow1,2—a region that cannot yet be spatially resolved by any telescope—and provides a direct measure of the black hole mass and spin. The reverberation timescale is set by the light travel path between the direct emission from a hot X-ray corona and the reprocessed emission from the inner edge of the accretion disk3,4,5,6. However, there is an inherent degeneracy in the reverberation signal between black hole mass, inner disk radius and height of the illuminating corona above the disk. Here we use a long X-ray observation of the highly variable active galaxy IRAS 13224−3809 to track the reverberation signal as the system evolves on timescales of a day7,8. With the inclusion of all the relativistic effects, modelling reveals that the height of the X-ray corona increases with increasing luminosity, providing a dynamic view of the inner accretion region. This simultaneous modelling allows us to break the inherent degeneracies and obtain an independent timing-based estimate for the mass and spin of the black hole. The uncertainty on black hole mass is comparable to the leading optical reverberation method9, making X-ray reverberation a powerful technique, particularly for sources with low optical variability10.; W.N.A. and A.C.F. acknowledge support from the European Research Council through Advanced Grant 340442, on Feedback. M.L.P. and C.P. acknowledge support from ESA Research Fellowships. M.D. and M.D.C.-G. acknowledge support provided by the GA CR grant 18-00533S. M.D.C.-G. acknowledges funding from ESA through a partnership with IAA-CSIC (Spain). D.J.W. and M.J.M. appreciate support from an Ernest Rutherford STFC fellowship. D.J.K.B. acknowledges a Science and Technology Facilities Council studentship. C.S.R. thanks the UK Science and Technology Facilities Council for support under Consolidated Grant ST/R000867/1. This research has been partially funded by the Spanish State Research Agency (AEI) project no. ESP2017-87676-C5-1-R and no. MDM-2017-0737 Unidad de Excelencia "Maria de Maeztu"-Centro de Astrobiologia (CSIC-INTA). G.M. acknowledges funding by the Spanish State Research. Agency (AEI) project no. ESP2017-86582-C4-1-R. B.D.M. acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skodowska-Curie grant agreement no. 798726. This paper is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the United States (NASA).; Peer review
Idioma:: English
Relation:: info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-87676-C5-1-R; info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-86582-C4-1-R/ES/CONTRIBUCION ESPAÑOLA A LAS MISIONES ESPACIALES CRIOGENICAS SPICA Y ATHENA, POST-OPERACIONES DE HERSCHEL Y EXPLOTACION CIENTIFICA MULTIFRECUENCIA/; info:eu-repo/grantAgreement/EC/FP7/340442; info:eu-repo/grantAgreement/EC/H2020/798726
Autor/Productor:: Alston, W. N.; Fabian, A. C.; Kara, E.; Parker, M. L.; Dovciak, M.; Pinto, C.; Jiang, J.; Middleton, M. J.; Miniutti, G.; Walton, D. J.; Wilkins, D. R.; Buisson, D. J.; Caballero García, M. D.; Cackett, E. M.; De Marco, B.; Gallo, L. C.; Lohfink, A. M.; Reynolds, C. S.; Uttley, P.; Young, A. J.; Zogbhi, A.
Publisher:: Springer Nature Research Journals
Otros colaboradores/productores:: Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; 0000-0003-2658-6559; European Research Council (ERC); Science and Technology Facilities Council (STFC); European Space Agency (ESA); European Commission (EC); Agencia Estatal de Investigación (AEI)
Rights:: Copyright © 2020, The Author(s), under exclusive licence to Springer Nature Limited; info:eu-repo/semantics/restrictedAccess
Date:: 2021-04-08T07:28:16Z; 2020-01-20
Tipo de recurso:: info:eu-repo/semantics/article; info:eu-repo/semantics/publishedVersion; http://purl.org/coar/resource_type/c_6501
Format:: application/pdf

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38. <dim:field element="description" lang="es" mdschema="dc">Alston, W.N., Fabian, A.C., Kara, E. et al. A dynamic black hole corona in an active galaxy through X-ray reverberation mapping. Nat Astron 4, 597–602 (2020). https://doi.org/10.1038/s41550-019-1002-x</dim:field>
39. <dim:field element="description" lang="es" mdschema="dc" qualifier="abstract">X-ray reverberation echoes are assumed to be produced in the strongly distorted spacetime around accreting supermassive black holes. This signal allows us to spatially map the geometry of the inner accretion flow1,2—a region that cannot yet be spatially resolved by any telescope—and provides a direct measure of the black hole mass and spin. The reverberation timescale is set by the light travel path between the direct emission from a hot X-ray corona and the reprocessed emission from the inner edge of the accretion disk3,4,5,6. However, there is an inherent degeneracy in the reverberation signal between black hole mass, inner disk radius and height of the illuminating corona above the disk. Here we use a long X-ray observation of the highly variable active galaxy IRAS 13224−3809 to track the reverberation signal as the system evolves on timescales of a day7,8. With the inclusion of all the relativistic effects, modelling reveals that the height of the X-ray corona increases with increasing luminosity, providing a dynamic view of the inner accretion region. This simultaneous modelling allows us to break the inherent degeneracies and obtain an independent timing-based estimate for the mass and spin of the black hole. The uncertainty on black hole mass is comparable to the leading optical reverberation method9, making X-ray reverberation a powerful technique, particularly for sources with low optical variability10.</dim:field>
40. <dim:field element="description" lang="es" mdschema="dc" qualifier="sponsorship">W.N.A. and A.C.F. acknowledge support from the European Research Council through Advanced Grant 340442, on Feedback. M.L.P. and C.P. acknowledge support from ESA Research Fellowships. M.D. and M.D.C.-G. acknowledge support provided by the GA CR grant 18-00533S. M.D.C.-G. acknowledges funding from ESA through a partnership with IAA-CSIC (Spain). D.J.W. and M.J.M. appreciate support from an Ernest Rutherford STFC fellowship. D.J.K.B. acknowledges a Science and Technology Facilities Council studentship. C.S.R. thanks the UK Science and Technology Facilities Council for support under Consolidated Grant ST/R000867/1. This research has been partially funded by the Spanish State Research Agency (AEI) project no. ESP2017-87676-C5-1-R and no. MDM-2017-0737 Unidad de Excelencia "Maria de Maeztu"-Centro de Astrobiologia (CSIC-INTA). G.M. acknowledges funding by the Spanish State Research. Agency (AEI) project no. ESP2017-86582-C4-1-R. B.D.M. acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skodowska-Curie grant agreement no. 798726. This paper is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the United States (NASA).</dim:field>
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1. <title>A dynamic black hole corona in an active galaxy through X-ray reverberation mapping</title>
2. <creator>Alston, W. N.</creator>
3. <creator>Fabian, A. C.</creator>
4. <creator>Kara, E.</creator>
5. <creator>Parker, M. L.</creator>
6. <creator>Dovciak, M.</creator>
7. <creator>Pinto, C.</creator>
8. <creator>Jiang, J.</creator>
9. <creator>Middleton, M. J.</creator>
10. <creator>Miniutti, G.</creator>
11. <creator>Walton, D. J.</creator>
12. <creator>Wilkins, D. R.</creator>
13. <creator>Buisson, D. J.</creator>
14. <creator>Caballero García, M. D.</creator>
15. <creator>Cackett, E. M.</creator>
16. <creator>De Marco, B.</creator>
17. <creator>Gallo, L. C.</creator>
18. <creator>Lohfink, A. M.</creator>
19. <creator>Reynolds, C. S.</creator>
20. <creator>Uttley, P.</creator>
21. <creator>Young, A. J.</creator>
22. <creator>Zogbhi, A.</creator>
23. <contributor>Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737</contributor>
24. <contributor>0000-0003-2658-6559</contributor>
25. <contributor>European Research Council (ERC)</contributor>
26. <contributor>Science and Technology Facilities Council (STFC)</contributor>
27. <contributor>European Space Agency (ESA)</contributor>
28. <contributor>European Commission (EC)</contributor>
29. <contributor>Agencia Estatal de Investigación (AEI)</contributor>
30. <subject>Black Hole</subject>
31. <subject>Active Galaxy</subject>
32. <subject>X ray</subject>
33. <subject>Reverberation mapping</subject>
34. <subject>Galactic Nuclei</subject>
35. <subject>Scattering</subject>
36. <description>Alston, W.N., Fabian, A.C., Kara, E. et al. A dynamic black hole corona in an active galaxy through X-ray reverberation mapping. Nat Astron 4, 597–602 (2020). https://doi.org/10.1038/s41550-019-1002-x</description>
37. <description>X-ray reverberation echoes are assumed to be produced in the strongly distorted spacetime around accreting supermassive black holes. This signal allows us to spatially map the geometry of the inner accretion flow1,2—a region that cannot yet be spatially resolved by any telescope—and provides a direct measure of the black hole mass and spin. The reverberation timescale is set by the light travel path between the direct emission from a hot X-ray corona and the reprocessed emission from the inner edge of the accretion disk3,4,5,6. However, there is an inherent degeneracy in the reverberation signal between black hole mass, inner disk radius and height of the illuminating corona above the disk. Here we use a long X-ray observation of the highly variable active galaxy IRAS 13224−3809 to track the reverberation signal as the system evolves on timescales of a day7,8. With the inclusion of all the relativistic effects, modelling reveals that the height of the X-ray corona increases with increasing luminosity, providing a dynamic view of the inner accretion region. This simultaneous modelling allows us to break the inherent degeneracies and obtain an independent timing-based estimate for the mass and spin of the black hole. The uncertainty on black hole mass is comparable to the leading optical reverberation method9, making X-ray reverberation a powerful technique, particularly for sources with low optical variability10.</description>
38. <date>2021-04-08</date>
39. <date>2021-04-08</date>
40. <date>2020-01-20</date>
41. <type>info:eu-repo/semantics/article</type>
42. <identifier>Nature Astronomy 4: 597- 602 (2020)</identifier>
43. <identifier>http://hdl.handle.net/20.500.12666/152</identifier>
44. <identifier>10.1038/s41550-019-1002-x</identifier>
45. <identifier>2397-3366</identifier>
46. <language>eng</language>
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51. <rights>Copyright © 2020, The Author(s), under exclusive licence to Springer Nature Limited</rights>
52. <rights>info:eu-repo/semantics/restrictedAccess</rights>
53. <publisher>Springer Nature Research Journals</publisher>
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        <mods:name>
        <mods:role>
        <mods:roleTerm type="text">funder</mods:roleTerm>
        </mods:role>
        <mods:namePart>Agencia Estatal de Investigación (AEI)</mods:namePart>
        </mods:name>
        <mods:extension>
        <mods:dateAccessioned encoding="iso8601">2021-04-08T07:28:16Z</mods:dateAccessioned>
        </mods:extension>
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        <mods:dateAvailable encoding="iso8601">2021-04-08T07:28:16Z</mods:dateAvailable>
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        <mods:originInfo>
        <mods:dateIssued encoding="iso8601">2020-01-20</mods:dateIssued>
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        <mods:identifier type="citation">Nature Astronomy 4: 597- 602 (2020)</mods:identifier>
        <mods:identifier type="uri">http://hdl.handle.net/20.500.12666/152</mods:identifier>
        <mods:identifier type="doi">10.1038/s41550-019-1002-x</mods:identifier>
        <mods:identifier type="e-issn">2397-3366</mods:identifier>
        <mods:abstract>X-ray reverberation echoes are assumed to be produced in the strongly distorted spacetime around accreting supermassive black holes. This signal allows us to spatially map the geometry of the inner accretion flow1,2—a region that cannot yet be spatially resolved by any telescope—and provides a direct measure of the black hole mass and spin. The reverberation timescale is set by the light travel path between the direct emission from a hot X-ray corona and the reprocessed emission from the inner edge of the accretion disk3,4,5,6. However, there is an inherent degeneracy in the reverberation signal between black hole mass, inner disk radius and height of the illuminating corona above the disk. Here we use a long X-ray observation of the highly variable active galaxy IRAS 13224−3809 to track the reverberation signal as the system evolves on timescales of a day7,8. With the inclusion of all the relativistic effects, modelling reveals that the height of the X-ray corona increases with increasing luminosity, providing a dynamic view of the inner accretion region. This simultaneous modelling allows us to break the inherent degeneracies and obtain an independent timing-based estimate for the mass and spin of the black hole. The uncertainty on black hole mass is comparable to the leading optical reverberation method9, making X-ray reverberation a powerful technique, particularly for sources with low optical variability10.</mods:abstract>
        <mods:language>
        <mods:languageTerm authority="rfc3066">eng</mods:languageTerm>
        </mods:language>
        <mods:accessCondition type="useAndReproduction" />
        <mods:subject>
        <mods:topic>Black Hole</mods:topic>
        </mods:subject>
        <mods:subject>
        <mods:topic>Active Galaxy</mods:topic>
        </mods:subject>
        <mods:subject>
        <mods:topic>X ray</mods:topic>
        </mods:subject>
        <mods:subject>
        <mods:topic>Reverberation mapping</mods:topic>
        </mods:subject>
        <mods:subject>
        <mods:topic>Galactic Nuclei</mods:topic>
        </mods:subject>
        <mods:subject>
        <mods:topic>Scattering</mods:topic>
        </mods:subject>
        <mods:titleInfo>
        <mods:title>A dynamic black hole corona in an active galaxy through X-ray reverberation mapping</mods:title>
        </mods:titleInfo>
        <mods:genre>info:eu-repo/semantics/article</mods:genre>
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  37. <dc:description>X-ray reverberation echoes are assumed to be produced in the strongly distorted spacetime around accreting supermassive black holes. This signal allows us to spatially map the geometry of the inner accretion flow1,2—a region that cannot yet be spatially resolved by any telescope—and provides a direct measure of the black hole mass and spin. The reverberation timescale is set by the light travel path between the direct emission from a hot X-ray corona and the reprocessed emission from the inner edge of the accretion disk3,4,5,6. However, there is an inherent degeneracy in the reverberation signal between black hole mass, inner disk radius and height of the illuminating corona above the disk. Here we use a long X-ray observation of the highly variable active galaxy IRAS 13224−3809 to track the reverberation signal as the system evolves on timescales of a day7,8. With the inclusion of all the relativistic effects, modelling reveals that the height of the X-ray corona increases with increasing luminosity, providing a dynamic view of the inner accretion region. This simultaneous modelling allows us to break the inherent degeneracies and obtain an independent timing-based estimate for the mass and spin of the black hole. The uncertainty on black hole mass is comparable to the leading optical reverberation method9, making X-ray reverberation a powerful technique, particularly for sources with low optical variability10.</dc:description>
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