Figure 1 from CHIME/FRB Detection of the Original Repeating Fast Radio Burst Source FRB 121102

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CHIME/FRB Detection of the Original Repeating Fast Radio Burst Source FRB 121102

Authors: A. Josephy, P. Chawla, E. Fonseca, C. Ng, C. Patel, Z. Pleunis, P. Scholz, B. C. Andersen, K. Bandura, M. Bhardwaj, M. M. Boyce, P. J. Boyle, C. Brar, D. Cubranic, M. Dobbs, B. M. Gaensler, A. Gill, U. Giri, D. C. Good, M. Halpern, G. Hinshaw, V. M. Kaspi, T. L. Landecker, D. A. Lang, H.-H. Lin, K. W. Masui, R. Mckinven, J. Mena-Parra, M. Merryfield, D. Michilli, N. Milutinovic, A. Naidu, U. Pen, M. Rafiei-Ravandi, M. Rahman, S. M. Ransom, A. Renard, S. R. Siegel, K. M. Smith, I. H. Stairs, S. P. Tendulkar, K. Vanderlinde, P. Yadav, and A. V. Zwaniga

2019 The Astrophysical Journal Letters 882 L18.

Provider: AAS Journals

Caption: Figure 1.

Timeline of CHIME/FRB’s daily exposure to FRB 121102 within the FWHM of the telescope’s synthesized beams at 600 MHz. The reduction in daily exposure starting 2018 December 7 is due to the failure of the computing node responsible for processing one of the four FFT-formed beams through which the source transits. The rms noise is estimated relative to that for the day of detection of the FRB 121102 burst using pulsars detected by CHIME/FRB with the marker colors denoting the number of pulsars used for the estimate. The errors on the relative rms noise account only for the day-to-day sensitivity variation and are not representative of the overall error on the fluence threshold. See Section 2.5 for a description of how the fluence threshold and the corresponding error were determined.

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