Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes
- Autores
- Oknyansky, V. L.; Gaskell, C. M.; Mikailov, K. M.; Lipunov, V. M.; Shatsky, N. I.; Tsygankov, S. S.; Gorbovskoy, E. S.; Tatarnikov, A. M.; Metlov, V. G.; Malanchev, K. L.; Brotherton, M. B.; Kasper, D.; Du, P.; Chen, X.; Burlak, M. A.; Buckley, D. A. H.; Rebolo, R.; Serra-Ricart, M.; Podestá, Ricardo César; Levato, Orlando Hugo
- Año de publicación
- 2017
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Optical and near-infrared photometry, optical spectroscopy, and soft X-ray and UV monitoring of the changing-look active galactic nucleus NGC 2617 show that it continues to have the appearance of a type-1 Seyfert galaxy. An optical light curve for 2010-2017 indicates that the change of type probably occurred between 2010 October and 2012 February and was not related to the brightening in 2013. In 2016 and 2017 NGC 2617 brightened again to a level of activity close to that in 2013 April. However, in 2017 from the end of the March to end of July 2017 it was in very low level and starting to change back to a Seyfert 1.8. We find variations in all passbands and in both the intensities and profiles of the broad Balmer lines. A new displaced emission peak has appeared in Hβ. X-ray variations are well correlated with UV-optical variability and possibly lead by ̃2-3 d. The K band lags the J band by about 21.5 ± 2.5 d and lags the combined B + J bands by ̃25 d. J lags B by about 3 d. This could be because J-band variability arises predominantly from the outer part of the accretion disc, while K-band variability is dominated by thermal re-emission by dust. We propose that spectral-type changes are a result of increasing central luminosity causing sublimation of the innermost dust in the hollow bi-conical outflow. We briefly discuss various other possible reasons that might explain the dramatic changes in NGC 2617.
Fil: Oknyansky, V. L.. Sternberg Astronomical Institute; Rusia
Fil: Gaskell, C. M.. Department of Astronomy and Astrophysics. University of California. Santa Cruz; Estados Unidos
Fil: Mikailov, K. M.. Shamakhy Astrophysical Observatory, National Academy of Sciences. Pirkuli; Azerbaiyán
Fil: Lipunov, V. M.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University ; Rusia
Fil: Shatsky, N. I.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia
Fil: Tsygankov, S. S.. Tuorla Observatory, Department of Physics and Astronomy. University of Turku.; Finlandia
Fil: Gorbovskoy, E. S.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia
Fil: Tatarnikov, A. M.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia
Fil: Metlov, V. G.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia
Fil: Malanchev, K. L.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia
Fil: Brotherton, M.B.. University of Wyoming; Estados Unidos
Fil: Kasper, D.. University of Wyoming; Estados Unidos
Fil: Du, P.. Institute of High Energy Physics. Chinese Academy of Sciences; China
Fil: Chen, X.. School of Space Science and Physics. Shandong University; China
Fil: Burlak, M. A.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia
Fil: Buckley, D. A. H.. The South African Astronomical Observatory; Sudáfrica
Fil: Rebolo, R.. Instituto de Astrofisica de Canarias; España
Fil: Serra-Ricart, M.. Instituto de Astrofisica de Canarias; España
Fil: Podestá, R.. Universidad Nacional de San Juan; Argentina
Fil: Levato, O. H.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina - Materia
-
Agn
X-Ray
Uv
Photometry - 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:11336/99644
Ver los metadatos del registro completo
| id |
CONICETDig_2d667d8ea1684f15f9f2b783880e1353 |
|---|---|
| oai_identifier_str |
oai:ri.conicet.gov.ar:11336/99644 |
| network_acronym_str |
CONICETDig |
| repository_id_str |
3498 |
| network_name_str |
CONICET Digital (CONICET) |
| spelling |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State ChangesOknyansky, V. L.Gaskell, C. M.Mikailov, K. M.Lipunov, V. M.Shatsky, N. I.Tsygankov, S. S.Gorbovskoy, E. S.Tatarnikov, A. M.Metlov, V. G.Malanchev, K. L.Brotherton, M. B.Kasper, D.Du, P.Chen, X.Burlak, M. A.Buckley, D. A. H.Rebolo, R.Serra-Ricart, M.Podestá, Ricardo CésarLevato, Orlando HugoAgnX-RayUvPhotometryhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Optical and near-infrared photometry, optical spectroscopy, and soft X-ray and UV monitoring of the changing-look active galactic nucleus NGC 2617 show that it continues to have the appearance of a type-1 Seyfert galaxy. An optical light curve for 2010-2017 indicates that the change of type probably occurred between 2010 October and 2012 February and was not related to the brightening in 2013. In 2016 and 2017 NGC 2617 brightened again to a level of activity close to that in 2013 April. However, in 2017 from the end of the March to end of July 2017 it was in very low level and starting to change back to a Seyfert 1.8. We find variations in all passbands and in both the intensities and profiles of the broad Balmer lines. A new displaced emission peak has appeared in Hβ. X-ray variations are well correlated with UV-optical variability and possibly lead by ̃2-3 d. The K band lags the J band by about 21.5 ± 2.5 d and lags the combined B + J bands by ̃25 d. J lags B by about 3 d. This could be because J-band variability arises predominantly from the outer part of the accretion disc, while K-band variability is dominated by thermal re-emission by dust. We propose that spectral-type changes are a result of increasing central luminosity causing sublimation of the innermost dust in the hollow bi-conical outflow. We briefly discuss various other possible reasons that might explain the dramatic changes in NGC 2617.Fil: Oknyansky, V. L.. Sternberg Astronomical Institute; RusiaFil: Gaskell, C. M.. Department of Astronomy and Astrophysics. University of California. Santa Cruz; Estados UnidosFil: Mikailov, K. M.. Shamakhy Astrophysical Observatory, National Academy of Sciences. Pirkuli; AzerbaiyánFil: Lipunov, V. M.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University ; RusiaFil: Shatsky, N. I.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; RusiaFil: Tsygankov, S. S.. Tuorla Observatory, Department of Physics and Astronomy. University of Turku.; FinlandiaFil: Gorbovskoy, E. S.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; RusiaFil: Tatarnikov, A. M.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; RusiaFil: Metlov, V. G.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; RusiaFil: Malanchev, K. L.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; RusiaFil: Brotherton, M.B.. University of Wyoming; Estados UnidosFil: Kasper, D.. University of Wyoming; Estados UnidosFil: Du, P.. Institute of High Energy Physics. Chinese Academy of Sciences; ChinaFil: Chen, X.. School of Space Science and Physics. Shandong University; ChinaFil: Burlak, M. A.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; RusiaFil: Buckley, D. A. H.. The South African Astronomical Observatory; SudáfricaFil: Rebolo, R.. Instituto de Astrofisica de Canarias; EspañaFil: Serra-Ricart, M.. Instituto de Astrofisica de Canarias; EspañaFil: Podestá, R.. Universidad Nacional de San Juan; ArgentinaFil: Levato, O. H.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaOdessa National University2017-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/99644Oknyansky, V. L.; Gaskell, C. M.; Mikailov, K. M.; Lipunov, V. M.; Shatsky, N. I.; et al.; Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes; Odessa National University; Odessa Astronomical Publications; 30; 11-2017; 117-1201810-4215CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.18524/1810-4215.2017.30.114366info:eu-repo/semantics/altIdentifier/url/http://oap.onu.edu.ua/article/view/114366info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:46:33Zoai:ri.conicet.gov.ar:11336/99644instacron: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:34982025-09-29 09:46:33.339CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes |
| title |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes |
| spellingShingle |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes Oknyansky, V. L. Agn X-Ray Uv Photometry |
| title_short |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes |
| title_full |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes |
| title_fullStr |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes |
| title_full_unstemmed |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes |
| title_sort |
Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes |
| dc.creator.none.fl_str_mv |
Oknyansky, V. L. Gaskell, C. M. Mikailov, K. M. Lipunov, V. M. Shatsky, N. I. Tsygankov, S. S. Gorbovskoy, E. S. Tatarnikov, A. M. Metlov, V. G. Malanchev, K. L. Brotherton, M. B. Kasper, D. Du, P. Chen, X. Burlak, M. A. Buckley, D. A. H. Rebolo, R. Serra-Ricart, M. Podestá, Ricardo César Levato, Orlando Hugo |
| author |
Oknyansky, V. L. |
| author_facet |
Oknyansky, V. L. Gaskell, C. M. Mikailov, K. M. Lipunov, V. M. Shatsky, N. I. Tsygankov, S. S. Gorbovskoy, E. S. Tatarnikov, A. M. Metlov, V. G. Malanchev, K. L. Brotherton, M. B. Kasper, D. Du, P. Chen, X. Burlak, M. A. Buckley, D. A. H. Rebolo, R. Serra-Ricart, M. Podestá, Ricardo César Levato, Orlando Hugo |
| author_role |
author |
| author2 |
Gaskell, C. M. Mikailov, K. M. Lipunov, V. M. Shatsky, N. I. Tsygankov, S. S. Gorbovskoy, E. S. Tatarnikov, A. M. Metlov, V. G. Malanchev, K. L. Brotherton, M. B. Kasper, D. Du, P. Chen, X. Burlak, M. A. Buckley, D. A. H. Rebolo, R. Serra-Ricart, M. Podestá, Ricardo César Levato, Orlando Hugo |
| author2_role |
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 |
Agn X-Ray Uv Photometry |
| topic |
Agn X-Ray Uv Photometry |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
Optical and near-infrared photometry, optical spectroscopy, and soft X-ray and UV monitoring of the changing-look active galactic nucleus NGC 2617 show that it continues to have the appearance of a type-1 Seyfert galaxy. An optical light curve for 2010-2017 indicates that the change of type probably occurred between 2010 October and 2012 February and was not related to the brightening in 2013. In 2016 and 2017 NGC 2617 brightened again to a level of activity close to that in 2013 April. However, in 2017 from the end of the March to end of July 2017 it was in very low level and starting to change back to a Seyfert 1.8. We find variations in all passbands and in both the intensities and profiles of the broad Balmer lines. A new displaced emission peak has appeared in Hβ. X-ray variations are well correlated with UV-optical variability and possibly lead by ̃2-3 d. The K band lags the J band by about 21.5 ± 2.5 d and lags the combined B + J bands by ̃25 d. J lags B by about 3 d. This could be because J-band variability arises predominantly from the outer part of the accretion disc, while K-band variability is dominated by thermal re-emission by dust. We propose that spectral-type changes are a result of increasing central luminosity causing sublimation of the innermost dust in the hollow bi-conical outflow. We briefly discuss various other possible reasons that might explain the dramatic changes in NGC 2617. Fil: Oknyansky, V. L.. Sternberg Astronomical Institute; Rusia Fil: Gaskell, C. M.. Department of Astronomy and Astrophysics. University of California. Santa Cruz; Estados Unidos Fil: Mikailov, K. M.. Shamakhy Astrophysical Observatory, National Academy of Sciences. Pirkuli; Azerbaiyán Fil: Lipunov, V. M.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University ; Rusia Fil: Shatsky, N. I.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia Fil: Tsygankov, S. S.. Tuorla Observatory, Department of Physics and Astronomy. University of Turku.; Finlandia Fil: Gorbovskoy, E. S.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia Fil: Tatarnikov, A. M.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia Fil: Metlov, V. G.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia Fil: Malanchev, K. L.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia Fil: Brotherton, M.B.. University of Wyoming; Estados Unidos Fil: Kasper, D.. University of Wyoming; Estados Unidos Fil: Du, P.. Institute of High Energy Physics. Chinese Academy of Sciences; China Fil: Chen, X.. School of Space Science and Physics. Shandong University; China Fil: Burlak, M. A.. Sternberg Astronomical Institute. M.V.Lomonosov Moscow State University; Rusia Fil: Buckley, D. A. H.. The South African Astronomical Observatory; Sudáfrica Fil: Rebolo, R.. Instituto de Astrofisica de Canarias; España Fil: Serra-Ricart, M.. Instituto de Astrofisica de Canarias; España Fil: Podestá, R.. Universidad Nacional de San Juan; Argentina Fil: Levato, O. H.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina |
| description |
Optical and near-infrared photometry, optical spectroscopy, and soft X-ray and UV monitoring of the changing-look active galactic nucleus NGC 2617 show that it continues to have the appearance of a type-1 Seyfert galaxy. An optical light curve for 2010-2017 indicates that the change of type probably occurred between 2010 October and 2012 February and was not related to the brightening in 2013. In 2016 and 2017 NGC 2617 brightened again to a level of activity close to that in 2013 April. However, in 2017 from the end of the March to end of July 2017 it was in very low level and starting to change back to a Seyfert 1.8. We find variations in all passbands and in both the intensities and profiles of the broad Balmer lines. A new displaced emission peak has appeared in Hβ. X-ray variations are well correlated with UV-optical variability and possibly lead by ̃2-3 d. The K band lags the J band by about 21.5 ± 2.5 d and lags the combined B + J bands by ̃25 d. J lags B by about 3 d. This could be because J-band variability arises predominantly from the outer part of the accretion disc, while K-band variability is dominated by thermal re-emission by dust. We propose that spectral-type changes are a result of increasing central luminosity causing sublimation of the innermost dust in the hollow bi-conical outflow. We briefly discuss various other possible reasons that might explain the dramatic changes in NGC 2617. |
| publishDate |
2017 |
| dc.date.none.fl_str_mv |
2017-11 |
| 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/11336/99644 Oknyansky, V. L.; Gaskell, C. M.; Mikailov, K. M.; Lipunov, V. M.; Shatsky, N. I.; et al.; Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes; Odessa National University; Odessa Astronomical Publications; 30; 11-2017; 117-120 1810-4215 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/99644 |
| identifier_str_mv |
Oknyansky, V. L.; Gaskell, C. M.; Mikailov, K. M.; Lipunov, V. M.; Shatsky, N. I.; et al.; Multi-Wavelength Monitoring of the Changing-Look AGN NGC 2617 during State Changes; Odessa National University; Odessa Astronomical Publications; 30; 11-2017; 117-120 1810-4215 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.18524/1810-4215.2017.30.114366 info:eu-repo/semantics/altIdentifier/url/http://oap.onu.edu.ua/article/view/114366 |
| dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
| eu_rights_str_mv |
openAccess |
| rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
| dc.format.none.fl_str_mv |
application/pdf application/pdf application/pdf |
| dc.publisher.none.fl_str_mv |
Odessa National University |
| publisher.none.fl_str_mv |
Odessa National University |
| dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
| reponame_str |
CONICET Digital (CONICET) |
| collection |
CONICET Digital (CONICET) |
| instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
| repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
| repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
| _version_ |
1844613453755449344 |
| score |
13.070432 |