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      Fast Universal Spectrophotopolarimeter for Robotic Telescopes

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          Abstract

          FUSP is the automatic multimode spectrophotopolarimeter aimed to the study of fast optical transients in the photometric, photopolarimetric (instant measurement of linear polarization), and spectropolarimetric (with or without the slit) modes. The mode change is automatic depending on the transient brightness and the purposes of the observations and may be performed in half a second. The instrument may be equipped with either fast EM-CCD or a position-sensitive detector which may provide temporal resolution up to 1 microsecond. FUSP is the robotic instrument for the robotic telescopes.

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          Broadband observations of the naked-eye γ-ray burst GRB 080319B

          J. Racusin, S. V. Karpov, M. Sokolowski … (2008)
          Long-duration gamma-ray bursts (GRBs) release copious amounts of energy across the entire electromagnetic spectrum, and so provide a window into the process of black hole formation from the collapse of massive stars. Previous early optical observations of even the most exceptional GRBs (990123 and 030329) lacked both the temporal resolution to probe the optical flash in detail and the accuracy needed to trace the transition from the prompt emission within the outflow to external shocks caused by interaction with the progenitor environment. Here we report observations of the extraordinarily bright prompt optical and gamma-ray emission of GRB 080319B that provide diagnostics within seconds of its formation, followed by broadband observations of the afterglow decay that continued for weeks. We show that the prompt emission stems from a single physical region, implying an extremely relativistic outflow that propagates within the narrow inner core of a two-component jet.
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            The Physics of Gamma-Ray Bursts

            Tsvi Piran (2004)
            Gamma-Ray Bursts (GRBs), short and intense pulses of low energy gamma-rays, have fascinated astronomers and astrophysicists since their unexpected discovery in the late sixties. During the last decade, several space missions: BATSE (Burst and Transient Source Experiment) on Compton Gamma-Ray Observatory, BeppoSAX and now HETE II (High-Energy Transient Explorer), together with ground optical, infrared and radio observatories have revolutionized our understanding of GRBs showing that they are cosmological, that they are accompanied by long lasting afterglows and that they are associated with core collapse Supernovae. At the same time a theoretical understanding has emerged in the form of the fireball internal-external shocks model. According to this model GRBs are produced when the kinetic energy of an ultra-relativistic flow is dissipated in internal collisions. The afterglow arises when the flow is slowed down by shocks with the surrounding circum-burst matter. This model has numerous successful predictions like the prediction of the afterglow itself, the prediction of jet breaks in the afterglow light curve and of an optical flash that accompanies the GRBs themselves. In this review I focus on theoretical aspects and on physical processes believed to take place in GRBs.
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              Observation of contemporaneous optical radiation from a gamma-ray burst

              J Wren, B. Lee, J. Szymanski … (1999)
              The origin of gamma-ray bursts (GRBs) has been enigmatic since their discovery. The situation improved dramatically in 1997, when the rapid availability of precise coordinates for the bursts allowed the detection of faint optical and radio afterglows - optical spectra thus obtained have demonstrated conclusively that the bursts occur at cosmological distances. But, despite efforts by several groups, optical detection has not hitherto been achieved during the brief duration of a burst. Here we report the detection of bright optical emission from GRB990123 while the burst was still in progress. Our observations begin 22 seconds after the onset of the burst and show an increase in brightness by a factor of 14 during the first 25 seconds; the brightness then declines by a factor of 100, at which point (700 seconds after the burst onset) it falls below our detection threshold. The redshift of this burst, approximately 1.6, implies a peak optical luminosity of 5 times 10^{49} erg per second. Optical emission from gamma-ray bursts has been generally thought to take place at the shock fronts generated by interaction of the primary energy source with the surrounding medium, where the gamma-rays might also be produced. The lack of a significant change in the gamma-ray light curve when the optical emission develops suggests that the gamma-rays are not produced at the shock front, but closer to the site of the original explosion.
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                Author and article information

                Journal
                Title: Advances in Astronomy
                Abbreviated Title: Advances in Astronomy
                Publisher: Hindawi Limited
                ISSN (Print): 1687-7969
                ISSN (Electronic): 1687-7977
                Publication date Created: 2010
                Publication date (Print): 2010
                Volume: 2010
                Issue:
                Pages: 1-6
                Article
                DOI: 10.1155/2010/109681
                SO-VID: 85a1aae8-5120-4f53-b69b-41b3652cb14b
                Copyright © © 2010
                License:

                http://creativecommons.org/licenses/by/3.0/

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