V407 Lup, an intermediate polar nova
- Autores
- Orio, M.; Melicherčík, M.; Ciroi, S.; Canton, V.; Aydi, E.; Buckley, D. A. H.; Dobrotka, A.; Luna, Gerardo Juan Manuel; Ness, J.
- Año de publicación
- 2024
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present X-ray and optical observations of nova V407 Lup (Nova Lup 2016), previously well monitored in outburst, as it returned to quiescent accretion. The X-ray light curve in 2020 February revealed a clear flux modulation with a stable period of 564.64±0.64 s, corresponding to the period measured in outburst and attributed to the spin of a magnetized white dwarf in an intermediate polar (IP) system. This detection in quiescence is consistent with the IP classification proposed after the nova eruption. The XMM-Newton EPIC X-ray flux is is ≃ 1.3 × 10-12 erg cm-2 s-1 at a distance, most likely, larger than 5 kpc, emitted in the whole 0.2-12 keV range without a significant cut-off energy. The X-ray spectra are complex; they can be fitted including a power law component with a relatively flat slope (a power law index ≃1), although, alternatively, a hard thermal component at kT≥19 keV also yields a good fit. The SALT optical spectra obtained in 2019 March and 2022 May are quite typical of IPs, with strong emission lines, including some due to a high ionization potential, like He II at 4685.7 Å. Nebular lines of O [III] were prominent in 2019 March, but their intensity and equivalent width appeared to be decreasing during that month, and they were no longer detectable in 2022, indicating that the nova ejecta dispersed. Complex profiles of the He II lines of V407 Lup are also characteristic of IPs, giving further evidence for this classification.
Fil: Orio, M.. Istituto Nazionale di Astrofisica; Italia. University of Wisconsin; Estados Unidos
Fil: Melicherčík, M.. Advanced Technologies Research Institut; Eslovaquia
Fil: Ciroi, S.. Università di Padova; Italia
Fil: Canton, V.. Università di Padova; Italia
Fil: Aydi, E.. Michigan State University; Estados Unidos
Fil: Buckley, D. A. H.. University of Cape Town; Sudáfrica
Fil: Dobrotka, A.. Advanced Technologies Research Institut; Eslovaquia
Fil: Luna, Gerardo Juan Manuel. Secretaria de Investigacion ; Universidad Nacional de Hurlingham; . Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Ness, J.. Agencia Espacial Europea. European Space Research And Technology Centre.; Países Bajos - Materia
-
novae, cataclysmic variable
stars: magnetic field
X-rays: individual (V407 Lup) - 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:11336/243644
Ver los metadatos del registro completo
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V407 Lup, an intermediate polar novaOrio, M.Melicherčík, M.Ciroi, S.Canton, V.Aydi, E.Buckley, D. A. H.Dobrotka, A.Luna, Gerardo Juan ManuelNess, J.novae, cataclysmic variablestars: magnetic fieldX-rays: individual (V407 Lup)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present X-ray and optical observations of nova V407 Lup (Nova Lup 2016), previously well monitored in outburst, as it returned to quiescent accretion. The X-ray light curve in 2020 February revealed a clear flux modulation with a stable period of 564.64±0.64 s, corresponding to the period measured in outburst and attributed to the spin of a magnetized white dwarf in an intermediate polar (IP) system. This detection in quiescence is consistent with the IP classification proposed after the nova eruption. The XMM-Newton EPIC X-ray flux is is ≃ 1.3 × 10-12 erg cm-2 s-1 at a distance, most likely, larger than 5 kpc, emitted in the whole 0.2-12 keV range without a significant cut-off energy. The X-ray spectra are complex; they can be fitted including a power law component with a relatively flat slope (a power law index ≃1), although, alternatively, a hard thermal component at kT≥19 keV also yields a good fit. The SALT optical spectra obtained in 2019 March and 2022 May are quite typical of IPs, with strong emission lines, including some due to a high ionization potential, like He II at 4685.7 Å. Nebular lines of O [III] were prominent in 2019 March, but their intensity and equivalent width appeared to be decreasing during that month, and they were no longer detectable in 2022, indicating that the nova ejecta dispersed. Complex profiles of the He II lines of V407 Lup are also characteristic of IPs, giving further evidence for this classification.Fil: Orio, M.. Istituto Nazionale di Astrofisica; Italia. University of Wisconsin; Estados UnidosFil: Melicherčík, M.. Advanced Technologies Research Institut; EslovaquiaFil: Ciroi, S.. Università di Padova; ItaliaFil: Canton, V.. Università di Padova; ItaliaFil: Aydi, E.. Michigan State University; Estados UnidosFil: Buckley, D. A. H.. University of Cape Town; SudáfricaFil: Dobrotka, A.. Advanced Technologies Research Institut; EslovaquiaFil: Luna, Gerardo Juan Manuel. Secretaria de Investigacion ; Universidad Nacional de Hurlingham; . Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Ness, J.. Agencia Espacial Europea. European Space Research And Technology Centre.; Países BajosWiley Blackwell Publishing, Inc2024-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/243644Orio, M.; Melicherčík, M.; Ciroi, S.; Canton, V.; Aydi, E.; et al.; V407 Lup, an intermediate polar nova; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 533; 2; 9-2024; 1541-15490035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/533/2/1541/7731135info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stae1922info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:07:55Zoai:ri.conicet.gov.ar:11336/243644instacron: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 10:07:55.475CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
V407 Lup, an intermediate polar nova |
| title |
V407 Lup, an intermediate polar nova |
| spellingShingle |
V407 Lup, an intermediate polar nova Orio, M. novae, cataclysmic variable stars: magnetic field X-rays: individual (V407 Lup) |
| title_short |
V407 Lup, an intermediate polar nova |
| title_full |
V407 Lup, an intermediate polar nova |
| title_fullStr |
V407 Lup, an intermediate polar nova |
| title_full_unstemmed |
V407 Lup, an intermediate polar nova |
| title_sort |
V407 Lup, an intermediate polar nova |
| dc.creator.none.fl_str_mv |
Orio, M. Melicherčík, M. Ciroi, S. Canton, V. Aydi, E. Buckley, D. A. H. Dobrotka, A. Luna, Gerardo Juan Manuel Ness, J. |
| author |
Orio, M. |
| author_facet |
Orio, M. Melicherčík, M. Ciroi, S. Canton, V. Aydi, E. Buckley, D. A. H. Dobrotka, A. Luna, Gerardo Juan Manuel Ness, J. |
| author_role |
author |
| author2 |
Melicherčík, M. Ciroi, S. Canton, V. Aydi, E. Buckley, D. A. H. Dobrotka, A. Luna, Gerardo Juan Manuel Ness, J. |
| author2_role |
author author author author author author author author |
| dc.subject.none.fl_str_mv |
novae, cataclysmic variable stars: magnetic field X-rays: individual (V407 Lup) |
| topic |
novae, cataclysmic variable stars: magnetic field X-rays: individual (V407 Lup) |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
We present X-ray and optical observations of nova V407 Lup (Nova Lup 2016), previously well monitored in outburst, as it returned to quiescent accretion. The X-ray light curve in 2020 February revealed a clear flux modulation with a stable period of 564.64±0.64 s, corresponding to the period measured in outburst and attributed to the spin of a magnetized white dwarf in an intermediate polar (IP) system. This detection in quiescence is consistent with the IP classification proposed after the nova eruption. The XMM-Newton EPIC X-ray flux is is ≃ 1.3 × 10-12 erg cm-2 s-1 at a distance, most likely, larger than 5 kpc, emitted in the whole 0.2-12 keV range without a significant cut-off energy. The X-ray spectra are complex; they can be fitted including a power law component with a relatively flat slope (a power law index ≃1), although, alternatively, a hard thermal component at kT≥19 keV also yields a good fit. The SALT optical spectra obtained in 2019 March and 2022 May are quite typical of IPs, with strong emission lines, including some due to a high ionization potential, like He II at 4685.7 Å. Nebular lines of O [III] were prominent in 2019 March, but their intensity and equivalent width appeared to be decreasing during that month, and they were no longer detectable in 2022, indicating that the nova ejecta dispersed. Complex profiles of the He II lines of V407 Lup are also characteristic of IPs, giving further evidence for this classification. Fil: Orio, M.. Istituto Nazionale di Astrofisica; Italia. University of Wisconsin; Estados Unidos Fil: Melicherčík, M.. Advanced Technologies Research Institut; Eslovaquia Fil: Ciroi, S.. Università di Padova; Italia Fil: Canton, V.. Università di Padova; Italia Fil: Aydi, E.. Michigan State University; Estados Unidos Fil: Buckley, D. A. H.. University of Cape Town; Sudáfrica Fil: Dobrotka, A.. Advanced Technologies Research Institut; Eslovaquia Fil: Luna, Gerardo Juan Manuel. Secretaria de Investigacion ; Universidad Nacional de Hurlingham; . Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina Fil: Ness, J.. Agencia Espacial Europea. European Space Research And Technology Centre.; Países Bajos |
| description |
We present X-ray and optical observations of nova V407 Lup (Nova Lup 2016), previously well monitored in outburst, as it returned to quiescent accretion. The X-ray light curve in 2020 February revealed a clear flux modulation with a stable period of 564.64±0.64 s, corresponding to the period measured in outburst and attributed to the spin of a magnetized white dwarf in an intermediate polar (IP) system. This detection in quiescence is consistent with the IP classification proposed after the nova eruption. The XMM-Newton EPIC X-ray flux is is ≃ 1.3 × 10-12 erg cm-2 s-1 at a distance, most likely, larger than 5 kpc, emitted in the whole 0.2-12 keV range without a significant cut-off energy. The X-ray spectra are complex; they can be fitted including a power law component with a relatively flat slope (a power law index ≃1), although, alternatively, a hard thermal component at kT≥19 keV also yields a good fit. The SALT optical spectra obtained in 2019 March and 2022 May are quite typical of IPs, with strong emission lines, including some due to a high ionization potential, like He II at 4685.7 Å. Nebular lines of O [III] were prominent in 2019 March, but their intensity and equivalent width appeared to be decreasing during that month, and they were no longer detectable in 2022, indicating that the nova ejecta dispersed. Complex profiles of the He II lines of V407 Lup are also characteristic of IPs, giving further evidence for this classification. |
| publishDate |
2024 |
| dc.date.none.fl_str_mv |
2024-09 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
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publishedVersion |
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http://hdl.handle.net/11336/243644 Orio, M.; Melicherčík, M.; Ciroi, S.; Canton, V.; Aydi, E.; et al.; V407 Lup, an intermediate polar nova; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 533; 2; 9-2024; 1541-1549 0035-8711 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/243644 |
| identifier_str_mv |
Orio, M.; Melicherčík, M.; Ciroi, S.; Canton, V.; Aydi, E.; et al.; V407 Lup, an intermediate polar nova; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 533; 2; 9-2024; 1541-1549 0035-8711 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/533/2/1541/7731135 info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stae1922 |
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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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Wiley Blackwell Publishing, Inc |
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Wiley Blackwell Publishing, Inc |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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