广西大学天体物理学科介绍
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z peak
( , z) ˆ ( 2, 100.15z ) ( 2)
1
Free parameters 2
in our models:
Lb
15
MC Result
{α1=0.70, α2=1.9} Lb~ 1046 erg s-1
Our Monte Carlo (MC) simulations suggest that a intrinsic broken power-law luminosity function can well reproduced the observed magnitude distributi1o6ns.
科学意义
恒星 物理
高能 辐射 过程
引力 物理
星系 物理
伽玛暴
宇宙 学
中心能源？ 喷流形成和演化？ 火球动能辐射？ 各种成份的物理起源？
…….
伽玛暴光变曲线
Shallowwk.baidu.comDecay
Distinct origins of various components ?
luminosity functions (LF) at t<1h ?
6
Data selection
Sample:
Full sample of GRBs with optical afterglow detection from 1997-2012, 230 GRBs included
146 well-sampled LCs for our analysis. Most of them were observed in the R-band.
Function 3. MC simulation 4. Robotic 60-cm Telescopes of GXU-NAOC Center 5. Summary and Discussion
14
MC simulation Model
(1)Optical luminosity function:
Optical data, prompt gamma-ray dataand redshift.
Corrections:
k-correction, Galactic extinction (No correction for host galaxy extinction )
7
光度分布
Global lightcurves
8
光度分布
Onset
9
光度分布
shallow Decay
10
光度分布
11
Optical prompt emission of GRBs
目前已探测到伽玛暴～4000个； 但探测到爆发时光学辐射的<10个:
✓ GRB 990123, 041219, 050401, 050820A, 060111B, 061121, 080913B ✓ 其中仅仅 GRB 080913B有无时延观测！
GRB 080913B
Summary for the observations:
The observed distributions of R-band magnitude are roughly a Gaussian function. About 90% of GRBs in the above samples have R<20. This may be due to instrumental selection effect (only small robotic telescope can rapidly response to the GRB triggers).
伽玛暴光学余辉光度函数 和60 cm 光学望远镜
王祥高
广西大学—国家天文台天体物理与空间科学研究中心 China-VO and Astroinformatics 2012·2012.11.28-12.02·三峡大学
Outline
1. GRB and it’s optical emission 2. Observed GRB Optical Brightness Distribution
Oneset
Li, Liang et al. 2012, arXiv1203.2332
5
Outline
1. GRB and it’s optical emission 2. Observed GRB Optical Brightness Distribution
Function 3. MC simulation 4. Robotic 60-cm Telescopes of GXU-NAOC Center 5. Summary and Discussion
( L)
0
[(
L Lb
)1
( L Lb
)2 ]1
(2)GRB rate: dN RGRB (z) dV (z)
dzdt 1 z dz
RGRB (z) RSFR (z)( , z)
(3)Extinction:
RSFR
(
z)
(1 (1
z
z)3.44 , z ) , 3.44
peak
z
z
peak
Prompt Optical Flares: More luminous, and the burst time is more early
13
Outline
1. A generic Optical Lightcurves of GRBs 2. Observed GRB Optical Brightness Distribution
Function 3. MC simulation 4. Robotic 60-cm Telescopes of GXU-NAOC Center 5. Summary and Discussion
2
1.伽玛暴
伽玛射线暴(Gamma-Ray Burst，GRB) 是宇宙学距离上的宇宙大爆炸以来的最 强的能量爆发事件，它的主要特点是伽 玛射线波段流量突然增强，以及具有的 瞬时性，能量高，时标短，光变曲线复 杂多变等特点。
Outline
1. GRB and it’s optical emission 2. Observed GRB Optical Brightness Distribution
Function 3. MC simulation 4. Robotic 60-cm Telescopes of GXU-NAOC Center (Robotic Autonomous Observatory) 5. Summary and Discussion
( , z) ˆ ( 2, 100.15z ) ( 2)
1
Free parameters 2
in our models:
Lb
15
MC Result
{α1=0.70, α2=1.9} Lb~ 1046 erg s-1
Our Monte Carlo (MC) simulations suggest that a intrinsic broken power-law luminosity function can well reproduced the observed magnitude distributi1o6ns.
科学意义
恒星 物理
高能 辐射 过程
引力 物理
星系 物理
伽玛暴
宇宙 学
中心能源？ 喷流形成和演化？ 火球动能辐射？ 各种成份的物理起源？
…….
伽玛暴光变曲线
Shallowwk.baidu.comDecay
Distinct origins of various components ?
luminosity functions (LF) at t<1h ?
6
Data selection
Sample:
Full sample of GRBs with optical afterglow detection from 1997-2012, 230 GRBs included
146 well-sampled LCs for our analysis. Most of them were observed in the R-band.
Function 3. MC simulation 4. Robotic 60-cm Telescopes of GXU-NAOC Center 5. Summary and Discussion
14
MC simulation Model
(1)Optical luminosity function:
Optical data, prompt gamma-ray dataand redshift.
Corrections:
k-correction, Galactic extinction (No correction for host galaxy extinction )
7
光度分布
Global lightcurves
8
光度分布
Onset
9
光度分布
shallow Decay
10
光度分布
11
Optical prompt emission of GRBs
目前已探测到伽玛暴～4000个； 但探测到爆发时光学辐射的<10个:
✓ GRB 990123, 041219, 050401, 050820A, 060111B, 061121, 080913B ✓ 其中仅仅 GRB 080913B有无时延观测！
GRB 080913B
Summary for the observations:
The observed distributions of R-band magnitude are roughly a Gaussian function. About 90% of GRBs in the above samples have R<20. This may be due to instrumental selection effect (only small robotic telescope can rapidly response to the GRB triggers).
伽玛暴光学余辉光度函数 和60 cm 光学望远镜
王祥高
广西大学—国家天文台天体物理与空间科学研究中心 China-VO and Astroinformatics 2012·2012.11.28-12.02·三峡大学
Outline
1. GRB and it’s optical emission 2. Observed GRB Optical Brightness Distribution
Oneset
Li, Liang et al. 2012, arXiv1203.2332
5
Outline
1. GRB and it’s optical emission 2. Observed GRB Optical Brightness Distribution
Function 3. MC simulation 4. Robotic 60-cm Telescopes of GXU-NAOC Center 5. Summary and Discussion
( L)
0
[(
L Lb
)1
( L Lb
)2 ]1
(2)GRB rate: dN RGRB (z) dV (z)
dzdt 1 z dz
RGRB (z) RSFR (z)( , z)
(3)Extinction:
RSFR
(
z)
(1 (1
z
z)3.44 , z ) , 3.44
peak
z
z
peak
Prompt Optical Flares: More luminous, and the burst time is more early
13
Outline
1. A generic Optical Lightcurves of GRBs 2. Observed GRB Optical Brightness Distribution
Function 3. MC simulation 4. Robotic 60-cm Telescopes of GXU-NAOC Center 5. Summary and Discussion
2
1.伽玛暴
伽玛射线暴(Gamma-Ray Burst，GRB) 是宇宙学距离上的宇宙大爆炸以来的最 强的能量爆发事件，它的主要特点是伽 玛射线波段流量突然增强，以及具有的 瞬时性，能量高，时标短，光变曲线复 杂多变等特点。
Outline
1. GRB and it’s optical emission 2. Observed GRB Optical Brightness Distribution
Function 3. MC simulation 4. Robotic 60-cm Telescopes of GXU-NAOC Center (Robotic Autonomous Observatory) 5. Summary and Discussion