학술논문
A Search for Technosignatures Around 11,680 Stars with the Green Bank Telescope at 1.15–1.73 GHz
Document Type
article
Author
Margot, Jean-Luc; Li, Megan G; Pinchuk, Pavlo; Myhrvold, Nathan; Lesyna, Larry; Alcantara, Lea E; Andrakin, Megan T; Arunseangroj, Jeth; Baclet, Damien S; Belk, Madison H; Bhadha, Zerxes R; Brandis, Nicholas W; Carey, Robert E; Cassar, Harrison P; Chava, Sai S; Chen, Calvin; Chen, James; Cheng, Kellen T; Cimbri, Alessia; Cloutier, Benjamin; Combitsis, Jordan A; Couvrette, Kelly L; Coy, Brandon P; Davis, Kyle W; Delcayre, Antoine F; Du, Michelle R; Feil, Sarah E; Fu, Danning; Gilmore, Travis J; Grahill-Bland, Emery; Iglesias, Laura M; Juneau, Zoe; Karapetian, Anthony G; Karfakis, George; Lambert, Christopher T; Lazbin, Eric A; Li, Jian H; Li, Zhuofu Chester; Liskij, Nicholas M; Lopilato, Anthony V; Lu, Darren J; Ma, Detao; Mathur, Vedant; Minasyan, Mary H; Muller, Maxwell K; Nasielski, Mark T; Nguyen, Janice T; Nicholson, Lorraine M; Niemoeller, Samantha; Ohri, Divij; Padhye, Atharva U; Penmetcha, Supreethi V; Prakash, Yugantar; Qi, Xinyi Cindy; Rindt, Liam; Sahu, Vedant; Scally, Joshua A; Scott, Zefyr; Seddon, Trevor J; Shohet, Lara-Lynn V; Sinha, Anchal; Sinigiani, Anthony E; Song, Jiuxu; Stice, Spencer M; Tabucol, Nadine M; Uplisashvili, Andria; Vanga, Krishna; Vazquez, Amaury G; Vetushko, George; Villa, Valeria; Vincent, Maria; Waasdorp, Ian J; Wagaman, Ian B; Wang, Amanda; Wight, Jade C; Wong, Ella; Yamaguchi, Natsuko; Zhang, Zijin; Zhao, Junyang; Lynch, Ryan S
Source
The Astronomical Journal. 166(5)
Subject
Language
Abstract
Abstract: We conducted a search for narrowband radio signals over four observing sessions in 2020–2023 with the L-band receiver (1.15–1.73 GHz) of the 100 m diameter Green Bank Telescope. We pointed the telescope in the directions of 62 TESS Objects of Interest, capturing radio emissions from a total of ∼11,680 stars and planetary systems in the ∼9′ beam of the telescope. All detections were either automatically rejected or visually inspected and confirmed to be of anthropogenic nature. We also quantified the end-to-end efficiency of radio SETI pipelines with a signal injection and recovery analysis. The UCLA SETI pipeline recovers 94.0% of the injected signals over the usable frequency range of the receiver and 98.7% of the injections when regions of dense radio frequency interference are excluded. In another pipeline that uses incoherent sums of 51 consecutive spectra, the recovery rate is ∼15 times smaller at ∼6%. The pipeline efficiency affects calculations of transmitter prevalence and SETI search volume. Accordingly, we developed an improved Drake figure of merit and a formalism to place upper limits on transmitter prevalence that take the pipeline efficiency and transmitter duty cycle into account. Based on our observations, we can state at the 95% confidence level that fewer than 6.6% of stars within 100 pc host a transmitter that is continuously transmitting a narrowband signal with an equivalent isotropic radiated power (EIRP) > 1013 W. For stars within 20,000 ly, the fraction of stars with detectable transmitters (EIRP > 5 × 1016 W) is at most 3 × 10−4. Finally, we showed that the UCLA SETI pipeline natively detects the signals detected with AI techniques by Ma et al.