Abstract

To observe the early optical emissions from gamma ray bursts (GRBs), we built the Slew Mirror Telescope. It utilizes a 150 mm motorized mirror to redirect incoming photons from astrophysical objects within seconds and to track them as compensating satellite movements. The SMT is a major component of the UFFO-pathfinder payload, which was launched on April 28, 2016, onboard the Lomonosov satellite. For the first time, the slewing mirror system has been proven for the precision tracking of astrophysical objects during space operation. We confirmed that the SMT has 1.4 seconds of response time to the X-gamma-ray trigger, and is able to compensate for satellite drift and to track astrophysical objects with magnitudes from 7 to 18.

Highlights

  • One of most important astrophysical objects for emerging multi-messenger astronomy are Gamma-Ray Bursts (GRBs) [1]

  • We confirmed that the Slewing Mirror Telescope (SMT) has 1.4 seconds of response time to the X-gamma-ray trigger, and is able to compensate for satellite drift and to track astrophysical objects with magnitudes from 7 to 18

  • We have demonstrated the validity of slewing mirror telescope technology, the key concept of UFFO-pathfinder instrument

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Summary

Introduction

One of most important astrophysical objects for emerging multi-messenger astronomy are Gamma-Ray Bursts (GRBs) [1]. The UBAT employs 48 × 48 YSO scintillator crystal array connected to photomultipliers, with 191 cm of total detection area and a 5 ∼ 150 KeV sensitivity range Both the UBAT and the SMT are controlled by the UFFO-pathfinder Data Acquisition system (UDAQ) [22]. Commercial rotary encoders and the stepping motors with sealed bearing systems provide a sufficiently rapid response to meet the UFFO-pathfinder scientific requirements. They are simple, robust and mostly space qualified. The SMT employs Field-Programmable Gate Array (FPGA) as its main processing component, and is able to achieve faster response times for incoming triggers while simultaneously running many additional processes (data taking and sending, mirror moving, housekeeping monitoring and so on).

Expected source rates and backgrounds
Performance in space
Observed issues
Rapid slewing capability after trigger
Tracking performance toward astrophysical object
Measured photon flux in the SMT FoV
Discussion
Conclusions
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