Early-Time Observations of Supernovae and Gamma-Ray Burst Afterglows at Gunma Astronomical Observatory

Details Early-Time Observations of Supernovae and Gamma-Ray Burst Afterglows at Gunma Astronomical Observatory Early-Time Observations of Supernovae and Gamma-Ray Burst Afterglows at Gunma Astronomical Observatory

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...9e..38k&link_type=abstract

Supernovae: One Millennium After SN1006, 26th meeting of the IAU, Joint Discussion 9, 17-18 August 2006, Prague, Czech Republic,

Astronomy and Astrophysics

Astronomy

Scientific paper

I have performed the observations of supernovae (SNe) and gamma-ray burst (GRB) afterglows at Gunma Astronomical Observatory (GAO). The key sentence of the observations is "Quick is important". GAO is a public observational facility founded in 1999 by Gunma Prefecture local government in Japan. The observatory is designed for both astronomical research and public use. It is equipped with a various size of telescopes needed to conduct observational research, including a 1.5 m reflectors and a small automatic telescope. It is more flexible to allocate the observation time for the quick observations than common-use observatories by proposals, except for a star-gazing time for public. Because the SNe and GRB afterglows are rapidly fading, the observable time is limited. Therefore, the early-time observations are very important for these objects. For GRB afterglows, as earlier responses can detect brighter ones, which sometimes observable with small telescopes. Also, SNe evolve faster at the earlier phase. The earlier information is sometimes clue to resolve the nature of the objects. Moreover, it can take a trigger of more detailed observations with the larger telescopes. We have reported some earliest observation results of SNe and the GRB afterglows in the IAU and GCN circulars. In the case of a hypernova, SN2002ap, our report was a trigger of many observations in the world. Moreover, the following sequential spectroscopy could reveal the early evolution and a variety of hypernovae (Kinugasa et al. 2002). In this presentation, I will introduce our facilities, observation results and the current status of the observations.

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