Suzaku observation of TeV blazar the 1ES 1218+304

Clues on particle acceleration in an extreme TeV blazar

R. Sato, Jun Kataoka, T. Takahashi, G. M. Medejski, S. Rügamer, S. J. Wagner

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

We observed the TeV blazar 1ES 1218+304 with the X-ray astronomy satellite Suzaku in May 2006. At the beginning of the two-day continuous observation, we detected a large flare in which the 5-10 keV flux changed by a factor of ∼2 on a timescale of 5×10 4 s. During the flare, the increase in the hard X-ray flux clearly lagged behind that observed in the soft X-rays, with the maximum lag of 2.3 ×10 4 s observed between the 0.3-1 keV and 5-10 keV bands. Furthermore we discovered that the temporal profile of the flare clearly changes with energy, being more symmetric at higher energies. From the spectral fitting of multi-wavelength data assuming a one-zone, homogeneous synchrotron self-Compton model, we obtain a magnetic field strength B - 0.047 G, an emission region size R = 3.0 × 10 16 cm for an appropriate beaming with a Doppler factor of δ = 20. This value of B is in good agreement with an independent estimate through the model fit to the observed time lag ascribing the energy-dependent variability to differential acceleration timescale of relativistic electrons provided that the gyro-factor ξ is 10 5.

Original languageEnglish
Title of host publicationAIP Conference Proceedings
Pages447-450
Number of pages4
Volume1085
DOIs
Publication statusPublished - 2009
Externally publishedYes
Event4th International Meeting on High Energy Gamma-Ray Astronomy - Heidelberg, Germany
Duration: 2008 Jul 72008 Jul 11

Other

Other4th International Meeting on High Energy Gamma-Ray Astronomy
CountryGermany
CityHeidelberg
Period08/7/708/7/11

Fingerprint

particle acceleration
flares
time lag
x rays
astronomy
energy
field strength
synchrotrons
estimates
profiles
magnetic fields
wavelengths
electrons

Keywords

  • BL lacertae objects
  • Individual (1ES 1218+304)

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Sato, R., Kataoka, J., Takahashi, T., Medejski, G. M., Rügamer, S., & Wagner, S. J. (2009). Suzaku observation of TeV blazar the 1ES 1218+304: Clues on particle acceleration in an extreme TeV blazar. In AIP Conference Proceedings (Vol. 1085, pp. 447-450) https://doi.org/10.1063/1.3076704

Suzaku observation of TeV blazar the 1ES 1218+304 : Clues on particle acceleration in an extreme TeV blazar. / Sato, R.; Kataoka, Jun; Takahashi, T.; Medejski, G. M.; Rügamer, S.; Wagner, S. J.

AIP Conference Proceedings. Vol. 1085 2009. p. 447-450.

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Sato, R, Kataoka, J, Takahashi, T, Medejski, GM, Rügamer, S & Wagner, SJ 2009, Suzaku observation of TeV blazar the 1ES 1218+304: Clues on particle acceleration in an extreme TeV blazar. in AIP Conference Proceedings. vol. 1085, pp. 447-450, 4th International Meeting on High Energy Gamma-Ray Astronomy, Heidelberg, Germany, 08/7/7. https://doi.org/10.1063/1.3076704
Sato R, Kataoka J, Takahashi T, Medejski GM, Rügamer S, Wagner SJ. Suzaku observation of TeV blazar the 1ES 1218+304: Clues on particle acceleration in an extreme TeV blazar. In AIP Conference Proceedings. Vol. 1085. 2009. p. 447-450 https://doi.org/10.1063/1.3076704
Sato, R. ; Kataoka, Jun ; Takahashi, T. ; Medejski, G. M. ; Rügamer, S. ; Wagner, S. J. / Suzaku observation of TeV blazar the 1ES 1218+304 : Clues on particle acceleration in an extreme TeV blazar. AIP Conference Proceedings. Vol. 1085 2009. pp. 447-450
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AB - We observed the TeV blazar 1ES 1218+304 with the X-ray astronomy satellite Suzaku in May 2006. At the beginning of the two-day continuous observation, we detected a large flare in which the 5-10 keV flux changed by a factor of ∼2 on a timescale of 5×10 4 s. During the flare, the increase in the hard X-ray flux clearly lagged behind that observed in the soft X-rays, with the maximum lag of 2.3 ×10 4 s observed between the 0.3-1 keV and 5-10 keV bands. Furthermore we discovered that the temporal profile of the flare clearly changes with energy, being more symmetric at higher energies. From the spectral fitting of multi-wavelength data assuming a one-zone, homogeneous synchrotron self-Compton model, we obtain a magnetic field strength B - 0.047 G, an emission region size R = 3.0 × 10 16 cm for an appropriate beaming with a Doppler factor of δ = 20. This value of B is in good agreement with an independent estimate through the model fit to the observed time lag ascribing the energy-dependent variability to differential acceleration timescale of relativistic electrons provided that the gyro-factor ξ is 10 5.

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