Blazar天体的光变及多波段能谱特性
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摘要
本文综述了活动星系核，特别是blazar天体的研究现状，对blazar天体的
多波段观测与多波段能谱特性研究进行了较为详细的评述。主要的研究工作包括
以下内容：（一）γ噪blazar天体的短时标光变研究，通过对16个γ噪blazar
天体（其中包括全部已证认和观测到VHEγ射线爆发的可能甚高能γ射线源）
自1998年的光学观测及光变分析研究表明，短时标光变（小时量级）是GeVγ
噪blazar天体的普遍特性，光变幅度通常可达0.6星等/小时，对PKS 1510-089
类星体的观测发现在一个小时内对象变暗2个星等，对如此激烈的光变变暗目前
的理论还不能很好的解释，但它同样反映了辐射区域的内部结构；而对TBLs的
监测表明，其光学波段的短时标光变没有其他对象激烈，出现的频度和振幅变化
都较小；（二）在研究γ噪blazar天体光变时，研究了寄主星系对光变的影响，
得到了1ES 2344+514的光变与PSF的FWHM的关联，表明随着大气视宁度
的下降（即FWHM变大），对象变暗，即由于寄主星系的影响从而导致假光变的
产生；（三）引进两个多波段复合谱指数，α_(xox)=α_(ox)-α_x及α_(oro)=α_(or)-α_o。
对样本的统计研究表明，RBLs是能谱特性界于XBLs和OVVs之间的一类中
间态，所得结果支持了Sambruna et al.（1996）大样本多波段能谱分布特性的统
计研究结果。（四）我们对地面探测器对blazar天体甚高能波段的观测做了较为
详细的了解，由于blazar天体在全波段上都观测到光变，所以这类对象是多波段
观测研究最完全的。地面望远镜对小时量级的光变很敏感，所以，对低流量源的
直到10TeV或更高能谱的测量是多波段研究的重要扩展，特别地，如果γ射线
的辐射是通过康普顿散射提升低能同步辐射光子产生的，即SSC模型产生，那
么，VHEγ射线的观测和低能同步辐射的观测就可能估计喷流内的磁场强度、
Doppler因子等。对我们今后的光学波段的观测工作提出了新的课题。
In the present thesis, we reviewed the basic properties and studying results
about the active galactic nuclei (AGNs), specially, we focus on the multiband ob-
servations and the properties of multiband spectral energy distributions (SEDs)
of biazars that would constraint the emission models of blazars. Our main works
and results are as follow: (1) studying on short timescale variability of y-ray
blazars. Our CCD monitoring campaign from 1998 have monitored the y-ray
blazars sample of 16 objects, including all TeV sources and some suspicious TeV
objects. The observational results show that the short timescale (about 1 hour)
variability is the common property for the GeV y ray blazars, the amplitude
variations in each optical band (B,V,l{,I) reach to 0.6 mag/hour. The GeV 7-
ray-loud source, PKS 1510?89, was very active during our observation period,
it showed an apparent variation of 2.0 mag within 41 minutes in the R band.
This is the most violently rapid variability in optical monitoring program since
1982 in our group. For this rapid dimming variability phenomenon, there is not
any suitable theoretical explanation, but this is also the reflection of emission
region structure. As for the TeV 7-ray blazars, the short timescale variability
in optical band is less drastic than GeV 7-ray blazars in both the amplitude
and timescale; (2) The influence of variable seeing conditions on the observations
was investigated. There is weak correlation between the observed variability and
the local seeing conditions for the objects 1ES 2344?14. This implies that the
source brightness decreased, while the FWHM of PSF increased, removing more
light from the aperture, e.g. there would be some spurious variation influenced
by variable seeing conditions. (3)We introduce two composite color梒olor indices
= ?a~ and &oro = aor ?a~. The statistical results for selected sample
show that RBLs are intermediate between XBLs and OVV quasars, which have
been given by Sumbruna et al. (1996). (4)We present the overview of the VHE
7-ray observations by using the ground based Cerenkov imaging telescope and
other detector. Because of their variability at all wavelengths, blazars can best
be understood through multi-wavelength observations. The sensitivity of VHE
telescopes to sub-hour scale variability, their ability to detect low source fluxes,
and the measurement of spectra up to 10 TeV or more make the VilE observa-
tions an important addition to multi-wavelength campaigns. In particular, if the
7-ray emission arises from inverse Compton scattering of the same electron pop-
ulation which produces the low energy synchrotron emission, the combination of
VHE 7-ray and synchrotron observations permit the estimation of the magnetic
field strength and Doppler factor in the jet where the 7-ray emission is produced.
It is a guide to our future optical observational campaign.
多波段观测与多波段能谱特性研究进行了较为详细的评述。主要的研究工作包括
以下内容：（一）γ噪blazar天体的短时标光变研究，通过对16个γ噪blazar
天体（其中包括全部已证认和观测到VHEγ射线爆发的可能甚高能γ射线源）
自1998年的光学观测及光变分析研究表明，短时标光变（小时量级）是GeVγ
噪blazar天体的普遍特性，光变幅度通常可达0.6星等/小时，对PKS 1510-089
类星体的观测发现在一个小时内对象变暗2个星等，对如此激烈的光变变暗目前
的理论还不能很好的解释，但它同样反映了辐射区域的内部结构；而对TBLs的
监测表明，其光学波段的短时标光变没有其他对象激烈，出现的频度和振幅变化
都较小；（二）在研究γ噪blazar天体光变时，研究了寄主星系对光变的影响，
得到了1ES 2344+514的光变与PSF的FWHM的关联，表明随着大气视宁度
的下降（即FWHM变大），对象变暗，即由于寄主星系的影响从而导致假光变的
产生；（三）引进两个多波段复合谱指数，α_(xox)=α_(ox)-α_x及α_(oro)=α_(or)-α_o。
对样本的统计研究表明，RBLs是能谱特性界于XBLs和OVVs之间的一类中
间态，所得结果支持了Sambruna et al.（1996）大样本多波段能谱分布特性的统
计研究结果。（四）我们对地面探测器对blazar天体甚高能波段的观测做了较为
详细的了解，由于blazar天体在全波段上都观测到光变，所以这类对象是多波段
观测研究最完全的。地面望远镜对小时量级的光变很敏感，所以，对低流量源的
直到10TeV或更高能谱的测量是多波段研究的重要扩展，特别地，如果γ射线
的辐射是通过康普顿散射提升低能同步辐射光子产生的，即SSC模型产生，那
么，VHEγ射线的观测和低能同步辐射的观测就可能估计喷流内的磁场强度、
Doppler因子等。对我们今后的光学波段的观测工作提出了新的课题。
In the present thesis, we reviewed the basic properties and studying results
about the active galactic nuclei (AGNs), specially, we focus on the multiband ob-
servations and the properties of multiband spectral energy distributions (SEDs)
of biazars that would constraint the emission models of blazars. Our main works
and results are as follow: (1) studying on short timescale variability of y-ray
blazars. Our CCD monitoring campaign from 1998 have monitored the y-ray
blazars sample of 16 objects, including all TeV sources and some suspicious TeV
objects. The observational results show that the short timescale (about 1 hour)
variability is the common property for the GeV y ray blazars, the amplitude
variations in each optical band (B,V,l{,I) reach to 0.6 mag/hour. The GeV 7-
ray-loud source, PKS 1510?89, was very active during our observation period,
it showed an apparent variation of 2.0 mag within 41 minutes in the R band.
This is the most violently rapid variability in optical monitoring program since
1982 in our group. For this rapid dimming variability phenomenon, there is not
any suitable theoretical explanation, but this is also the reflection of emission
region structure. As for the TeV 7-ray blazars, the short timescale variability
in optical band is less drastic than GeV 7-ray blazars in both the amplitude
and timescale; (2) The influence of variable seeing conditions on the observations
was investigated. There is weak correlation between the observed variability and
the local seeing conditions for the objects 1ES 2344?14. This implies that the
source brightness decreased, while the FWHM of PSF increased, removing more
light from the aperture, e.g. there would be some spurious variation influenced
by variable seeing conditions. (3)We introduce two composite color梒olor indices
= ?a~ and &oro = aor ?a~. The statistical results for selected sample
show that RBLs are intermediate between XBLs and OVV quasars, which have
been given by Sumbruna et al. (1996). (4)We present the overview of the VHE
7-ray observations by using the ground based Cerenkov imaging telescope and
other detector. Because of their variability at all wavelengths, blazars can best
be understood through multi-wavelength observations. The sensitivity of VHE
telescopes to sub-hour scale variability, their ability to detect low source fluxes,
and the measurement of spectra up to 10 TeV or more make the VilE observa-
tions an important addition to multi-wavelength campaigns. In particular, if the
7-ray emission arises from inverse Compton scattering of the same electron pop-
ulation which produces the low energy synchrotron emission, the combination of
VHE 7-ray and synchrotron observations permit the estimation of the magnetic
field strength and Doppler factor in the jet where the 7-ray emission is produced.
It is a guide to our future optical observational campaign.
引文
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