Standard

A new activity phase of the blazar 3C 454.3 : Multifrequency observations by the WEBT and XMM-Newton in 2007-2008. / Raiteri, C. M.; Villata, M.; Larionov, V. M.; Gurwell, M. A.; Chen, W. P.; Kurtanidze, O. M.; Aller, M. F.; Böttcher, M.; Calcidese, P.; Hroch, F.; Lähteenmäki, A.; Nilsson, K.; Ohlert, J.; Papadakis, I. E.; Agudo, I.; Aller, H. D.; Angelakis, E.; Arkharov, A. A.; Bach, U.; Bachev, R.; Berdyugin, A.; Buemi, C. S.; Carosati, D.; Charlot, P.; Chatzopoulos, E.; Forné, E.; Frasca, A.; Fuhrmann, L.; Gómez, J. L.; Gupta, A. C.; Hagen-Thorn, V. A.; Hsiao, W. S.; Jordan, B.; Jorstad, S. G.; Konstantinova, T. S.; Kopatskaya, E. N.; Krichbaum, T. P.; Lanteri, L.; Larionova, L. V.; Latev, G.; Le Campion, J. F.; Leto, P.; Marchili, N.; Marilli, E.; Marscher, A. P.; McBreen, B.; Mihov, B.; Nesci, R.; Nicastro, F.; Nikolashvili, M. G.; Novak, R.; Ovcharov, E.; Pian, E.; Principe, D.; Pursimo, T.; Ragozzine, B.; Ros, J. A.; Sadun, A. C.; Sagar, R.; Semkov, E.; Smart, R. L.; Smith, N.; Strigachev, A.; Takalo, L. O.; Tavani, M.; Tornikoski, M.; Trigilio, C.; Uckert, K.; Umana, G.; Valcheva, A.; Vercellone, S.; Volvach, A.; Wiesemeyer, H.

в: Astronomy and Astrophysics, Том 491, № 3, 12.2008, стр. 755-766.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Raiteri, CM, Villata, M, Larionov, VM, Gurwell, MA, Chen, WP, Kurtanidze, OM, Aller, MF, Böttcher, M, Calcidese, P, Hroch, F, Lähteenmäki, A, Nilsson, K, Ohlert, J, Papadakis, IE, Agudo, I, Aller, HD, Angelakis, E, Arkharov, AA, Bach, U, Bachev, R, Berdyugin, A, Buemi, CS, Carosati, D, Charlot, P, Chatzopoulos, E, Forné, E, Frasca, A, Fuhrmann, L, Gómez, JL, Gupta, AC, Hagen-Thorn, VA, Hsiao, WS, Jordan, B, Jorstad, SG, Konstantinova, TS, Kopatskaya, EN, Krichbaum, TP, Lanteri, L, Larionova, LV, Latev, G, Le Campion, JF, Leto, P, Marchili, N, Marilli, E, Marscher, AP, McBreen, B, Mihov, B, Nesci, R, Nicastro, F, Nikolashvili, MG, Novak, R, Ovcharov, E, Pian, E, Principe, D, Pursimo, T, Ragozzine, B, Ros, JA, Sadun, AC, Sagar, R, Semkov, E, Smart, RL, Smith, N, Strigachev, A, Takalo, LO, Tavani, M, Tornikoski, M, Trigilio, C, Uckert, K, Umana, G, Valcheva, A, Vercellone, S, Volvach, A & Wiesemeyer, H 2008, 'A new activity phase of the blazar 3C 454.3: Multifrequency observations by the WEBT and XMM-Newton in 2007-2008', Astronomy and Astrophysics, Том. 491, № 3, стр. 755-766. https://doi.org/10.1051/0004-6361:200810869

APA

Raiteri, C. M., Villata, M., Larionov, V. M., Gurwell, M. A., Chen, W. P., Kurtanidze, O. M., Aller, M. F., Böttcher, M., Calcidese, P., Hroch, F., Lähteenmäki, A., Nilsson, K., Ohlert, J., Papadakis, I. E., Agudo, I., Aller, H. D., Angelakis, E., Arkharov, A. A., Bach, U., ... Wiesemeyer, H. (2008). A new activity phase of the blazar 3C 454.3: Multifrequency observations by the WEBT and XMM-Newton in 2007-2008. Astronomy and Astrophysics, 491(3), 755-766. https://doi.org/10.1051/0004-6361:200810869

Vancouver

Raiteri CM, Villata M, Larionov VM, Gurwell MA, Chen WP, Kurtanidze OM и пр. A new activity phase of the blazar 3C 454.3: Multifrequency observations by the WEBT and XMM-Newton in 2007-2008. Astronomy and Astrophysics. 2008 Дек.;491(3):755-766. https://doi.org/10.1051/0004-6361:200810869

Author

Raiteri, C. M. ; Villata, M. ; Larionov, V. M. ; Gurwell, M. A. ; Chen, W. P. ; Kurtanidze, O. M. ; Aller, M. F. ; Böttcher, M. ; Calcidese, P. ; Hroch, F. ; Lähteenmäki, A. ; Nilsson, K. ; Ohlert, J. ; Papadakis, I. E. ; Agudo, I. ; Aller, H. D. ; Angelakis, E. ; Arkharov, A. A. ; Bach, U. ; Bachev, R. ; Berdyugin, A. ; Buemi, C. S. ; Carosati, D. ; Charlot, P. ; Chatzopoulos, E. ; Forné, E. ; Frasca, A. ; Fuhrmann, L. ; Gómez, J. L. ; Gupta, A. C. ; Hagen-Thorn, V. A. ; Hsiao, W. S. ; Jordan, B. ; Jorstad, S. G. ; Konstantinova, T. S. ; Kopatskaya, E. N. ; Krichbaum, T. P. ; Lanteri, L. ; Larionova, L. V. ; Latev, G. ; Le Campion, J. F. ; Leto, P. ; Marchili, N. ; Marilli, E. ; Marscher, A. P. ; McBreen, B. ; Mihov, B. ; Nesci, R. ; Nicastro, F. ; Nikolashvili, M. G. ; Novak, R. ; Ovcharov, E. ; Pian, E. ; Principe, D. ; Pursimo, T. ; Ragozzine, B. ; Ros, J. A. ; Sadun, A. C. ; Sagar, R. ; Semkov, E. ; Smart, R. L. ; Smith, N. ; Strigachev, A. ; Takalo, L. O. ; Tavani, M. ; Tornikoski, M. ; Trigilio, C. ; Uckert, K. ; Umana, G. ; Valcheva, A. ; Vercellone, S. ; Volvach, A. ; Wiesemeyer, H. / A new activity phase of the blazar 3C 454.3 : Multifrequency observations by the WEBT and XMM-Newton in 2007-2008. в: Astronomy and Astrophysics. 2008 ; Том 491, № 3. стр. 755-766.

BibTeX

@article{10d14ba6d0644516b201f68c2cd3297b,
title = "A new activity phase of the blazar 3C 454.3: Multifrequency observations by the WEBT and XMM-Newton in 2007-2008",
abstract = "Aims. The Whole Earth Blazar Telescope (WEBT) consortium has been monitoring the blazar 3C 454.3 from the radio to the optical bands since 2004 to study its emission variability properties.Methods. We present and analyse the multifrequency results of the 2007-2008 observing season, including XMM-Newton observations and near-IR spectroscopic monitoring, and compare the recent emission behaviour with the past one. The historical mm light curve is presented here for the first time.Results. In the optical band we observed a multi-peak outburst in July-August 2007, and other faster events in November 2007-February 2008. During these outburst phases, several episodes of intranight variability were detected. A mm outburst was observed starting from mid 2007, whose rising phase was contemporaneous to the optical brightening. A slower flux increase also affected the higher radio frequencies, the flux enhancement disappearing below 8 GHz. The analysis of the optical-radio correlation and time delays, as well as the behaviour of the mm light curve, confirm our previous predictions, suggesting that changes in the jet orientation likely occurred in the last few years. The historical multiwavelength behaviour indicates that a significant variation in the viewing angle may have happened around year 2000. Colour analysis confirms a general redder-when-brighter trend, which reaches a {"}saturation{"} at R ∼ 14 and possibly turns into a bluer-when-brighter trend in bright states. This behaviour is due to the interplay of different emission components, the synchrotron one possibly being characterised by an intrinsically variable spectrum. All the near-IR spectra show a prominent Hα emission line (EWobs = 50-120 {\AA}), whose flux appears nearly constant, indicating that the broad line region is not affected by the jet emission. We show the broad-band SEDs corresponding to the epochs of the XMM-Newton pointings and compare them to those obtained at other epochs, when the source was in different brightness states. A double power-law fit to the EPIC spectra including extra absorption suggests that the soft-X-ray spectrum is concave, and that the curvature becomes more pronounced as the flux decreases. This connects fairly well with the UV excess, which becomes more prominent with decreasing flux. The most obvious interpretation implies that, as the beamed synchrotron radiation from the jet dims, we can see both the head and the tail of the big blue bump. The X-ray flux correlates with the optical flux, suggesting that in the inverse-Compton process either the seed photons are synchrotron photons at IR-optical frequencies or the relativistic electrons are those that produce the optical synchrotron emission. The X-ray radiation would thus be produced in the jet region from where the IR-optical emission comes..",
keywords = "Galaxies: active, Galaxies: jets, Galaxies: quasars: general, Galaxies: quasars: individual: 3C 454.3",
author = "Raiteri, {C. M.} and M. Villata and Larionov, {V. M.} and Gurwell, {M. A.} and Chen, {W. P.} and Kurtanidze, {O. M.} and Aller, {M. F.} and M. B{\"o}ttcher and P. Calcidese and F. Hroch and A. L{\"a}hteenm{\"a}ki and K. Nilsson and J. Ohlert and Papadakis, {I. E.} and I. Agudo and Aller, {H. D.} and E. Angelakis and Arkharov, {A. A.} and U. Bach and R. Bachev and A. Berdyugin and Buemi, {C. S.} and D. Carosati and P. Charlot and E. Chatzopoulos and E. Forn{\'e} and A. Frasca and L. Fuhrmann and G{\'o}mez, {J. L.} and Gupta, {A. C.} and Hagen-Thorn, {V. A.} and Hsiao, {W. S.} and B. Jordan and Jorstad, {S. G.} and Konstantinova, {T. S.} and Kopatskaya, {E. N.} and Krichbaum, {T. P.} and L. Lanteri and Larionova, {L. V.} and G. Latev and {Le Campion}, {J. F.} and P. Leto and N. Marchili and E. Marilli and Marscher, {A. P.} and B. McBreen and B. Mihov and R. Nesci and F. Nicastro and Nikolashvili, {M. G.} and R. Novak and E. Ovcharov and E. Pian and D. Principe and T. Pursimo and B. Ragozzine and Ros, {J. A.} and Sadun, {A. C.} and R. Sagar and E. Semkov and Smart, {R. L.} and N. Smith and A. Strigachev and Takalo, {L. O.} and M. Tavani and M. Tornikoski and C. Trigilio and K. Uckert and G. Umana and A. Valcheva and S. Vercellone and A. Volvach and H. Wiesemeyer",
year = "2008",
month = dec,
doi = "10.1051/0004-6361:200810869",
language = "English",
volume = "491",
pages = "755--766",
journal = "ASTRONOMY & ASTROPHYSICS",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "3",

}

RIS

TY - JOUR

T1 - A new activity phase of the blazar 3C 454.3

T2 - Multifrequency observations by the WEBT and XMM-Newton in 2007-2008

AU - Raiteri, C. M.

AU - Villata, M.

AU - Larionov, V. M.

AU - Gurwell, M. A.

AU - Chen, W. P.

AU - Kurtanidze, O. M.

AU - Aller, M. F.

AU - Böttcher, M.

AU - Calcidese, P.

AU - Hroch, F.

AU - Lähteenmäki, A.

AU - Nilsson, K.

AU - Ohlert, J.

AU - Papadakis, I. E.

AU - Agudo, I.

AU - Aller, H. D.

AU - Angelakis, E.

AU - Arkharov, A. A.

AU - Bach, U.

AU - Bachev, R.

AU - Berdyugin, A.

AU - Buemi, C. S.

AU - Carosati, D.

AU - Charlot, P.

AU - Chatzopoulos, E.

AU - Forné, E.

AU - Frasca, A.

AU - Fuhrmann, L.

AU - Gómez, J. L.

AU - Gupta, A. C.

AU - Hagen-Thorn, V. A.

AU - Hsiao, W. S.

AU - Jordan, B.

AU - Jorstad, S. G.

AU - Konstantinova, T. S.

AU - Kopatskaya, E. N.

AU - Krichbaum, T. P.

AU - Lanteri, L.

AU - Larionova, L. V.

AU - Latev, G.

AU - Le Campion, J. F.

AU - Leto, P.

AU - Marchili, N.

AU - Marilli, E.

AU - Marscher, A. P.

AU - McBreen, B.

AU - Mihov, B.

AU - Nesci, R.

AU - Nicastro, F.

AU - Nikolashvili, M. G.

AU - Novak, R.

AU - Ovcharov, E.

AU - Pian, E.

AU - Principe, D.

AU - Pursimo, T.

AU - Ragozzine, B.

AU - Ros, J. A.

AU - Sadun, A. C.

AU - Sagar, R.

AU - Semkov, E.

AU - Smart, R. L.

AU - Smith, N.

AU - Strigachev, A.

AU - Takalo, L. O.

AU - Tavani, M.

AU - Tornikoski, M.

AU - Trigilio, C.

AU - Uckert, K.

AU - Umana, G.

AU - Valcheva, A.

AU - Vercellone, S.

AU - Volvach, A.

AU - Wiesemeyer, H.

PY - 2008/12

Y1 - 2008/12

N2 - Aims. The Whole Earth Blazar Telescope (WEBT) consortium has been monitoring the blazar 3C 454.3 from the radio to the optical bands since 2004 to study its emission variability properties.Methods. We present and analyse the multifrequency results of the 2007-2008 observing season, including XMM-Newton observations and near-IR spectroscopic monitoring, and compare the recent emission behaviour with the past one. The historical mm light curve is presented here for the first time.Results. In the optical band we observed a multi-peak outburst in July-August 2007, and other faster events in November 2007-February 2008. During these outburst phases, several episodes of intranight variability were detected. A mm outburst was observed starting from mid 2007, whose rising phase was contemporaneous to the optical brightening. A slower flux increase also affected the higher radio frequencies, the flux enhancement disappearing below 8 GHz. The analysis of the optical-radio correlation and time delays, as well as the behaviour of the mm light curve, confirm our previous predictions, suggesting that changes in the jet orientation likely occurred in the last few years. The historical multiwavelength behaviour indicates that a significant variation in the viewing angle may have happened around year 2000. Colour analysis confirms a general redder-when-brighter trend, which reaches a "saturation" at R ∼ 14 and possibly turns into a bluer-when-brighter trend in bright states. This behaviour is due to the interplay of different emission components, the synchrotron one possibly being characterised by an intrinsically variable spectrum. All the near-IR spectra show a prominent Hα emission line (EWobs = 50-120 Å), whose flux appears nearly constant, indicating that the broad line region is not affected by the jet emission. We show the broad-band SEDs corresponding to the epochs of the XMM-Newton pointings and compare them to those obtained at other epochs, when the source was in different brightness states. A double power-law fit to the EPIC spectra including extra absorption suggests that the soft-X-ray spectrum is concave, and that the curvature becomes more pronounced as the flux decreases. This connects fairly well with the UV excess, which becomes more prominent with decreasing flux. The most obvious interpretation implies that, as the beamed synchrotron radiation from the jet dims, we can see both the head and the tail of the big blue bump. The X-ray flux correlates with the optical flux, suggesting that in the inverse-Compton process either the seed photons are synchrotron photons at IR-optical frequencies or the relativistic electrons are those that produce the optical synchrotron emission. The X-ray radiation would thus be produced in the jet region from where the IR-optical emission comes..

AB - Aims. The Whole Earth Blazar Telescope (WEBT) consortium has been monitoring the blazar 3C 454.3 from the radio to the optical bands since 2004 to study its emission variability properties.Methods. We present and analyse the multifrequency results of the 2007-2008 observing season, including XMM-Newton observations and near-IR spectroscopic monitoring, and compare the recent emission behaviour with the past one. The historical mm light curve is presented here for the first time.Results. In the optical band we observed a multi-peak outburst in July-August 2007, and other faster events in November 2007-February 2008. During these outburst phases, several episodes of intranight variability were detected. A mm outburst was observed starting from mid 2007, whose rising phase was contemporaneous to the optical brightening. A slower flux increase also affected the higher radio frequencies, the flux enhancement disappearing below 8 GHz. The analysis of the optical-radio correlation and time delays, as well as the behaviour of the mm light curve, confirm our previous predictions, suggesting that changes in the jet orientation likely occurred in the last few years. The historical multiwavelength behaviour indicates that a significant variation in the viewing angle may have happened around year 2000. Colour analysis confirms a general redder-when-brighter trend, which reaches a "saturation" at R ∼ 14 and possibly turns into a bluer-when-brighter trend in bright states. This behaviour is due to the interplay of different emission components, the synchrotron one possibly being characterised by an intrinsically variable spectrum. All the near-IR spectra show a prominent Hα emission line (EWobs = 50-120 Å), whose flux appears nearly constant, indicating that the broad line region is not affected by the jet emission. We show the broad-band SEDs corresponding to the epochs of the XMM-Newton pointings and compare them to those obtained at other epochs, when the source was in different brightness states. A double power-law fit to the EPIC spectra including extra absorption suggests that the soft-X-ray spectrum is concave, and that the curvature becomes more pronounced as the flux decreases. This connects fairly well with the UV excess, which becomes more prominent with decreasing flux. The most obvious interpretation implies that, as the beamed synchrotron radiation from the jet dims, we can see both the head and the tail of the big blue bump. The X-ray flux correlates with the optical flux, suggesting that in the inverse-Compton process either the seed photons are synchrotron photons at IR-optical frequencies or the relativistic electrons are those that produce the optical synchrotron emission. The X-ray radiation would thus be produced in the jet region from where the IR-optical emission comes..

KW - Galaxies: active

KW - Galaxies: jets

KW - Galaxies: quasars: general

KW - Galaxies: quasars: individual: 3C 454.3

UR - http://www.scopus.com/inward/record.url?scp=57049086556&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:200810869

DO - 10.1051/0004-6361:200810869

M3 - Article

AN - SCOPUS:57049086556

VL - 491

SP - 755

EP - 766

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

IS - 3

ER -

ID: 88376473