Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER
- Autores
- König, Ole; Mastroserio, Guglielmo; Dauser, Thomas; Méndez, Mariano; Wang, Jingyi; García, Javier A.; Steiner, James F.; Pottschmidt, Katja; Ballhausen, Ralf; Connors, Riley M.; García, Federico; Grinberg, Victoria; Horn, David; Ingram, Adam; Kara, Erin; Kallman, Timothy R.; Lucchini, Matteo; Nathan, Edward; Nowak, Michael A.; Thalhammer, Philipp; van der Klis, Michiel; Wilms, Jörn
- Año de publicación
- 2024
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The Neutron Star Interior Composition Explorer (NICER) monitoring campaign of Cyg X-1 allows us to study its spectral-timing behavior at energies < 1 keV across all states. The hard state power spectrum can be decomposed into two main broad Lorentzians with a transition at around 1 Hz. The lower-frequency Lorentzian is the dominant component at low energies. The higher-frequency Lorentzian begins to contribute significantly to the variability above 1.5 keV and dominates at high energies. We show that the low- and high-frequency Lorentzians likely represent individual physical processes. The lower-frequency Lorentzian can be associated with a (possibly Comptonized) disk component, while the higher-frequency Lorentzian is clearly associated with the Comptonizing plasma. At the transition of these components, we discover a low-energy timing phenomenon characterized by an abrupt lag change of hard (≳2 keV) with respect to soft (≲1.5 keV) photons, accompanied by a drop in coherence, and a reduction in amplitude of the second broad Lorentzian. The frequency of the phenomenon increases with the frequencies of the Lorentzians as the source softens and cannot be seen when the power spectrum is single-humped. A comparison to transient low-mass X-ray binaries shows that this feature does not only appear in Cyg X-1, but that it is a general property of accreting black hole binaries. In Cyg X-1, we find that the variability at low and high energies is overall highly coherent in the hard and intermediate states. The high coherence shows that there is a process at work which links the variability, suggesting a physical connection between the accretion disk and Comptonizing plasma. This process fundamentally changes in the soft state, where strong red noise at high energies is incoherent to the variability at low energies.
Fil: König, Ole. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania
Fil: Mastroserio, Guglielmo. Università degli Studi di Milano; Italia
Fil: Dauser, Thomas. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania
Fil: Méndez, Mariano. University of Groningen. Kapteyn Astronomical Institute; Alemania
Fil: Wang, Jingyi. Massachusetts Institute of Technology; Estados Unidos
Fil: García, Javier A.. National Aeronautics and Space Administration; Estados Unidos
Fil: Steiner, James F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Pottschmidt, Katja. National Aeronautics and Space Administration; Estados Unidos
Fil: Ballhausen, Ralf. National Aeronautics and Space Administration; Estados Unidos
Fil: Connors, Riley M.. Vilanova University; Estados Unidos
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Grinberg, Victoria. Agencia Espacial Europea. European Space Research And Technology Centre.; Países Bajos
Fil: Horn, David. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania
Fil: Ingram, Adam. University of Newcastle; Reino Unido
Fil: Kara, Erin. Massachusetts Institute of Technology; Estados Unidos
Fil: Kallman, Timothy R.. National Aeronautics and Space Administration; Estados Unidos
Fil: Lucchini, Matteo. University of Amsterdam; Países Bajos
Fil: Nathan, Edward. California Institute of Technology; Estados Unidos
Fil: Nowak, Michael A.. Washington University in St. Louis; Estados Unidos
Fil: Thalhammer, Philipp. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania
Fil: van der Klis, Michiel. University of Amsterdam; Países Bajos
Fil: Wilms, Jörn. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania - Materia
-
ACCRETION, ACCRETION DISKS
STARS: BLACK HOLES
STARS: INDIVIDUAL: CYG X-1
X-RAYS: BINARIES - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/258363
Ver los metadatos del registro completo
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Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICERKönig, OleMastroserio, GuglielmoDauser, ThomasMéndez, MarianoWang, JingyiGarcía, Javier A.Steiner, James F.Pottschmidt, KatjaBallhausen, RalfConnors, Riley M.García, FedericoGrinberg, VictoriaHorn, DavidIngram, AdamKara, ErinKallman, Timothy R.Lucchini, MatteoNathan, EdwardNowak, Michael A.Thalhammer, Philippvan der Klis, MichielWilms, JörnACCRETION, ACCRETION DISKSSTARS: BLACK HOLESSTARS: INDIVIDUAL: CYG X-1X-RAYS: BINARIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The Neutron Star Interior Composition Explorer (NICER) monitoring campaign of Cyg X-1 allows us to study its spectral-timing behavior at energies < 1 keV across all states. The hard state power spectrum can be decomposed into two main broad Lorentzians with a transition at around 1 Hz. The lower-frequency Lorentzian is the dominant component at low energies. The higher-frequency Lorentzian begins to contribute significantly to the variability above 1.5 keV and dominates at high energies. We show that the low- and high-frequency Lorentzians likely represent individual physical processes. The lower-frequency Lorentzian can be associated with a (possibly Comptonized) disk component, while the higher-frequency Lorentzian is clearly associated with the Comptonizing plasma. At the transition of these components, we discover a low-energy timing phenomenon characterized by an abrupt lag change of hard (≳2 keV) with respect to soft (≲1.5 keV) photons, accompanied by a drop in coherence, and a reduction in amplitude of the second broad Lorentzian. The frequency of the phenomenon increases with the frequencies of the Lorentzians as the source softens and cannot be seen when the power spectrum is single-humped. A comparison to transient low-mass X-ray binaries shows that this feature does not only appear in Cyg X-1, but that it is a general property of accreting black hole binaries. In Cyg X-1, we find that the variability at low and high energies is overall highly coherent in the hard and intermediate states. The high coherence shows that there is a process at work which links the variability, suggesting a physical connection between the accretion disk and Comptonizing plasma. This process fundamentally changes in the soft state, where strong red noise at high energies is incoherent to the variability at low energies.Fil: König, Ole. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; AlemaniaFil: Mastroserio, Guglielmo. Università degli Studi di Milano; ItaliaFil: Dauser, Thomas. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; AlemaniaFil: Méndez, Mariano. University of Groningen. Kapteyn Astronomical Institute; AlemaniaFil: Wang, Jingyi. Massachusetts Institute of Technology; Estados UnidosFil: García, Javier A.. National Aeronautics and Space Administration; Estados UnidosFil: Steiner, James F.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Pottschmidt, Katja. National Aeronautics and Space Administration; Estados UnidosFil: Ballhausen, Ralf. National Aeronautics and Space Administration; Estados UnidosFil: Connors, Riley M.. Vilanova University; Estados UnidosFil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Grinberg, Victoria. Agencia Espacial Europea. European Space Research And Technology Centre.; Países BajosFil: Horn, David. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; AlemaniaFil: Ingram, Adam. University of Newcastle; Reino UnidoFil: Kara, Erin. Massachusetts Institute of Technology; Estados UnidosFil: Kallman, Timothy R.. National Aeronautics and Space Administration; Estados UnidosFil: Lucchini, Matteo. University of Amsterdam; Países BajosFil: Nathan, Edward. California Institute of Technology; Estados UnidosFil: Nowak, Michael A.. Washington University in St. Louis; Estados UnidosFil: Thalhammer, Philipp. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; AlemaniaFil: van der Klis, Michiel. University of Amsterdam; Países BajosFil: Wilms, Jörn. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; AlemaniaEDP Sciences2024-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/258363König, Ole; Mastroserio, Guglielmo; Dauser, Thomas; Méndez, Mariano; Wang, Jingyi; et al.; Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER; EDP Sciences; Astronomy and Astrophysics; 687; A284; 7-2024; 1-210004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202449333info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202449333info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:06:24Zoai:ri.conicet.gov.ar:11336/258363instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-03 10:06:24.495CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER |
| title |
Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER |
| spellingShingle |
Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER König, Ole ACCRETION, ACCRETION DISKS STARS: BLACK HOLES STARS: INDIVIDUAL: CYG X-1 X-RAYS: BINARIES |
| title_short |
Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER |
| title_full |
Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER |
| title_fullStr |
Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER |
| title_full_unstemmed |
Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER |
| title_sort |
Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER |
| dc.creator.none.fl_str_mv |
König, Ole Mastroserio, Guglielmo Dauser, Thomas Méndez, Mariano Wang, Jingyi García, Javier A. Steiner, James F. Pottschmidt, Katja Ballhausen, Ralf Connors, Riley M. García, Federico Grinberg, Victoria Horn, David Ingram, Adam Kara, Erin Kallman, Timothy R. Lucchini, Matteo Nathan, Edward Nowak, Michael A. Thalhammer, Philipp van der Klis, Michiel Wilms, Jörn |
| author |
König, Ole |
| author_facet |
König, Ole Mastroserio, Guglielmo Dauser, Thomas Méndez, Mariano Wang, Jingyi García, Javier A. Steiner, James F. Pottschmidt, Katja Ballhausen, Ralf Connors, Riley M. García, Federico Grinberg, Victoria Horn, David Ingram, Adam Kara, Erin Kallman, Timothy R. Lucchini, Matteo Nathan, Edward Nowak, Michael A. Thalhammer, Philipp van der Klis, Michiel Wilms, Jörn |
| author_role |
author |
| author2 |
Mastroserio, Guglielmo Dauser, Thomas Méndez, Mariano Wang, Jingyi García, Javier A. Steiner, James F. Pottschmidt, Katja Ballhausen, Ralf Connors, Riley M. García, Federico Grinberg, Victoria Horn, David Ingram, Adam Kara, Erin Kallman, Timothy R. Lucchini, Matteo Nathan, Edward Nowak, Michael A. Thalhammer, Philipp van der Klis, Michiel Wilms, Jörn |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
ACCRETION, ACCRETION DISKS STARS: BLACK HOLES STARS: INDIVIDUAL: CYG X-1 X-RAYS: BINARIES |
| topic |
ACCRETION, ACCRETION DISKS STARS: BLACK HOLES STARS: INDIVIDUAL: CYG X-1 X-RAYS: BINARIES |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
The Neutron Star Interior Composition Explorer (NICER) monitoring campaign of Cyg X-1 allows us to study its spectral-timing behavior at energies < 1 keV across all states. The hard state power spectrum can be decomposed into two main broad Lorentzians with a transition at around 1 Hz. The lower-frequency Lorentzian is the dominant component at low energies. The higher-frequency Lorentzian begins to contribute significantly to the variability above 1.5 keV and dominates at high energies. We show that the low- and high-frequency Lorentzians likely represent individual physical processes. The lower-frequency Lorentzian can be associated with a (possibly Comptonized) disk component, while the higher-frequency Lorentzian is clearly associated with the Comptonizing plasma. At the transition of these components, we discover a low-energy timing phenomenon characterized by an abrupt lag change of hard (≳2 keV) with respect to soft (≲1.5 keV) photons, accompanied by a drop in coherence, and a reduction in amplitude of the second broad Lorentzian. The frequency of the phenomenon increases with the frequencies of the Lorentzians as the source softens and cannot be seen when the power spectrum is single-humped. A comparison to transient low-mass X-ray binaries shows that this feature does not only appear in Cyg X-1, but that it is a general property of accreting black hole binaries. In Cyg X-1, we find that the variability at low and high energies is overall highly coherent in the hard and intermediate states. The high coherence shows that there is a process at work which links the variability, suggesting a physical connection between the accretion disk and Comptonizing plasma. This process fundamentally changes in the soft state, where strong red noise at high energies is incoherent to the variability at low energies. Fil: König, Ole. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania Fil: Mastroserio, Guglielmo. Università degli Studi di Milano; Italia Fil: Dauser, Thomas. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania Fil: Méndez, Mariano. University of Groningen. Kapteyn Astronomical Institute; Alemania Fil: Wang, Jingyi. Massachusetts Institute of Technology; Estados Unidos Fil: García, Javier A.. National Aeronautics and Space Administration; Estados Unidos Fil: Steiner, James F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Pottschmidt, Katja. National Aeronautics and Space Administration; Estados Unidos Fil: Ballhausen, Ralf. National Aeronautics and Space Administration; Estados Unidos Fil: Connors, Riley M.. Vilanova University; Estados Unidos Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina Fil: Grinberg, Victoria. Agencia Espacial Europea. European Space Research And Technology Centre.; Países Bajos Fil: Horn, David. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania Fil: Ingram, Adam. University of Newcastle; Reino Unido Fil: Kara, Erin. Massachusetts Institute of Technology; Estados Unidos Fil: Kallman, Timothy R.. National Aeronautics and Space Administration; Estados Unidos Fil: Lucchini, Matteo. University of Amsterdam; Países Bajos Fil: Nathan, Edward. California Institute of Technology; Estados Unidos Fil: Nowak, Michael A.. Washington University in St. Louis; Estados Unidos Fil: Thalhammer, Philipp. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania Fil: van der Klis, Michiel. University of Amsterdam; Países Bajos Fil: Wilms, Jörn. Universitat Erlangen-nurmberg. Astronomisches Institut-dr. Karl Remeis-sternwarte & Ecap; Alemania |
| description |
The Neutron Star Interior Composition Explorer (NICER) monitoring campaign of Cyg X-1 allows us to study its spectral-timing behavior at energies < 1 keV across all states. The hard state power spectrum can be decomposed into two main broad Lorentzians with a transition at around 1 Hz. The lower-frequency Lorentzian is the dominant component at low energies. The higher-frequency Lorentzian begins to contribute significantly to the variability above 1.5 keV and dominates at high energies. We show that the low- and high-frequency Lorentzians likely represent individual physical processes. The lower-frequency Lorentzian can be associated with a (possibly Comptonized) disk component, while the higher-frequency Lorentzian is clearly associated with the Comptonizing plasma. At the transition of these components, we discover a low-energy timing phenomenon characterized by an abrupt lag change of hard (≳2 keV) with respect to soft (≲1.5 keV) photons, accompanied by a drop in coherence, and a reduction in amplitude of the second broad Lorentzian. The frequency of the phenomenon increases with the frequencies of the Lorentzians as the source softens and cannot be seen when the power spectrum is single-humped. A comparison to transient low-mass X-ray binaries shows that this feature does not only appear in Cyg X-1, but that it is a general property of accreting black hole binaries. In Cyg X-1, we find that the variability at low and high energies is overall highly coherent in the hard and intermediate states. The high coherence shows that there is a process at work which links the variability, suggesting a physical connection between the accretion disk and Comptonizing plasma. This process fundamentally changes in the soft state, where strong red noise at high energies is incoherent to the variability at low energies. |
| publishDate |
2024 |
| dc.date.none.fl_str_mv |
2024-07 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
| format |
article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/258363 König, Ole; Mastroserio, Guglielmo; Dauser, Thomas; Méndez, Mariano; Wang, Jingyi; et al.; Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER; EDP Sciences; Astronomy and Astrophysics; 687; A284; 7-2024; 1-21 0004-6361 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/258363 |
| identifier_str_mv |
König, Ole; Mastroserio, Guglielmo; Dauser, Thomas; Méndez, Mariano; Wang, Jingyi; et al.; Long term variability of Cygnus X-1: VIII. A spectral-timing look at low energies with NICER; EDP Sciences; Astronomy and Astrophysics; 687; A284; 7-2024; 1-21 0004-6361 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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openAccess |
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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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application/pdf application/pdf |
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EDP Sciences |
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EDP Sciences |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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