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| Autori principali: | , , , , , , , , , , , , , , , , , , |
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| Natura: | Preprint |
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2024
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| Soggetti: | |
| Accesso online: | https://arxiv.org/abs/2409.08822 |
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| _version_ | 1866914033729273856 |
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| author | Arya, Anuraag Bilkhu, Harmanjeet Singh Vishwakarma, Sandeep Belatikar, Hrishikesh Bhalerao, Varun Ghodgaonkar, Abhijeet Koyande, Jayprakash G. Marathe, Aditi Mithun, N. P. S. Narang, Sanjoli Nimbalkar, Sudhanshu Page, Pranav Palit, Sourav Patel, Arpit Shetye, Amit Tallur, Siddharth Tendulkar, Shriharsh Vadawale, Santosh Waratkar, Gaurav |
| author_facet | Arya, Anuraag Bilkhu, Harmanjeet Singh Vishwakarma, Sandeep Belatikar, Hrishikesh Bhalerao, Varun Ghodgaonkar, Abhijeet Koyande, Jayprakash G. Marathe, Aditi Mithun, N. P. S. Narang, Sanjoli Nimbalkar, Sudhanshu Page, Pranav Palit, Sourav Patel, Arpit Shetye, Amit Tallur, Siddharth Tendulkar, Shriharsh Vadawale, Santosh Waratkar, Gaurav |
| contents | Hard X-ray photons with energies in the range of hundreds of keV typically undergo Compton scattering when they are incident on a detector. In this process, an incident photon deposits a fraction of its energy at the point of incidence and continues onwards with a change in direction that depends on the amount of energy deposited. By using a pair of detectors to detect the point of incidence and the direction of the scattered photon, we can calculate the scattering direction and angle. The position of a source in the sky can be reconstructed using many Compton photon pairs from a source. We demonstrate this principle in the laboratory by using a pair of Cadmium Zinc Telluride (CZT) detectors sensitive in the energy range of 20-200 keV, similar to those used in $\textit{AstroSat}$/CZT Imager (CZTI). The laboratory setup consists of the two detectors placed perpendicular to each other in a lead-lined box. The detectors are read out by a custom-programmed Xilinx PYNQ-Z2 FPGA board, and data are then transferred to a personal computer (PC)}. There are two key updates from CZTI: the detectors are read concurrently rather than serially, and the time resolution has been improved from $20~μ$s to $7.5~μ$s. We irradiated the detectors with a collimated $^{133}\mathrm{Ba}$ source and identified Compton scattering events for the 356 keV line. We run a Compton reconstruction algorithm to correctly infer the location of the source in the detector frame, with a location-dependent angular response measure of $16°-30°$. This comprises a successful technology demonstration for a Compton imaging camera in the hard X-ray regime. We present the details of our setup, the data acquisition process, and software algorithms, and showcase our results. We also quantify the limitations of this setup and discuss ways of improving the performance in future experiments. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_08822 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Development of a Compton Imager Setup Arya, Anuraag Bilkhu, Harmanjeet Singh Vishwakarma, Sandeep Belatikar, Hrishikesh Bhalerao, Varun Ghodgaonkar, Abhijeet Koyande, Jayprakash G. Marathe, Aditi Mithun, N. P. S. Narang, Sanjoli Nimbalkar, Sudhanshu Page, Pranav Palit, Sourav Patel, Arpit Shetye, Amit Tallur, Siddharth Tendulkar, Shriharsh Vadawale, Santosh Waratkar, Gaurav Instrumentation and Methods for Astrophysics Hard X-ray photons with energies in the range of hundreds of keV typically undergo Compton scattering when they are incident on a detector. In this process, an incident photon deposits a fraction of its energy at the point of incidence and continues onwards with a change in direction that depends on the amount of energy deposited. By using a pair of detectors to detect the point of incidence and the direction of the scattered photon, we can calculate the scattering direction and angle. The position of a source in the sky can be reconstructed using many Compton photon pairs from a source. We demonstrate this principle in the laboratory by using a pair of Cadmium Zinc Telluride (CZT) detectors sensitive in the energy range of 20-200 keV, similar to those used in $\textit{AstroSat}$/CZT Imager (CZTI). The laboratory setup consists of the two detectors placed perpendicular to each other in a lead-lined box. The detectors are read out by a custom-programmed Xilinx PYNQ-Z2 FPGA board, and data are then transferred to a personal computer (PC)}. There are two key updates from CZTI: the detectors are read concurrently rather than serially, and the time resolution has been improved from $20~μ$s to $7.5~μ$s. We irradiated the detectors with a collimated $^{133}\mathrm{Ba}$ source and identified Compton scattering events for the 356 keV line. We run a Compton reconstruction algorithm to correctly infer the location of the source in the detector frame, with a location-dependent angular response measure of $16°-30°$. This comprises a successful technology demonstration for a Compton imaging camera in the hard X-ray regime. We present the details of our setup, the data acquisition process, and software algorithms, and showcase our results. We also quantify the limitations of this setup and discuss ways of improving the performance in future experiments. |
| title | Development of a Compton Imager Setup |
| topic | Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2409.08822 |