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我们的赫歇尔开放时间观测提案得到了批准

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我们的赫歇尔开放时间观测提案得到了批准

Posted by Maohai Huang at November 16. 2010

7 月份使劲忙活了一阵。基本要点比较早就形成了,但确定细节和落在纸面上还是有不少工作。不少时间花在了把内容控制在页数限制范围内。得到了所要的全部观测时间还是比较满意的。


下面是建议书的cover page




GRB Afterglow Photometry with Herschel Infrared Cameras


Principal Investigator: Maohai Huang
Institution: National Astronomical Observatories of China
E−mail address: m-------------.cn
Co−Investigators: Bing Zhang, Dept. of Physics and Astronomy of Univ. of Nevada
Jinsong Deng, National Astronomical Observatories of CAS
Yulei Qiu, National Astronomical Observatories of CAS
Liping Xin, National Astronomical Observatories of CAS
Dong Xu, Weizmann Institute of Science
Science Category: Extra Galactic: Extra−Galactic Other
Observing Modes: PACS Photometer, SPIRE Photometer
Hours Requested: 23.6


Abstract:
GRB Afterglow Photometry with Herschel Infrared Cameras (GRAPHICS)
Gamma−ray bursts (GRBs) are the most luminous explosions in the universe. It has been difficult to obtain a full spectral picture of the phenomena in the short period when GRBs become ‘‘alive’’, i.e. when they generate bursts in Gamma−ray and produce afterglows in other wavelengths. Between NIR (12micron) and submillimeter (850micron) there lies nearly two orders of magnitude of spectral range where GRB afterglows have never been detected. Herschel is unique in its cutting edge sensitivity, efficiency, and readiness in FIR observations, and is capable of detecting GRB afterglows. Observing GRB afterglows with Herschel would greatly enrich our understanding of GRB physics and conditions of the Universe in early epochs.
We propose Target of Opportunity studies using the SPIRE and PACS instruments of Herschel to observe 3 bright GRB afterglows, each within a few hours to a few tens of days after burst. We will make follow−up observations after the initial one to photometrically measure GRB light curves and IR SEDs. We will make ground optical observations to compliment Herschel data, and have the the GRB community informed. Observing the forward shock peak in the FIR light curve and compare it (both the flux and time) with those in the optical and radio bands would give a unambiguous test to the fireball model, and offer a direct measurement of the density profile of the circumburst material. Catching the short−lived reverse shock emission and measure its magnitude would lead to constraints on some important parameters of the GRB ejecta and address the unknown composition of GRBs, baryonic vs. magnetic.


 


 


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