000006826 001__ 6826
000006826 005__ 20240217082932.0
000006826 0247_ $$2DOI$$a10.1093/mnras/stad1027
000006826 037__ $$aSCART-2024-0086
000006826 100__ $$aNarang, Mayank 
000006826 245__ $$auGMRT obser v ations of the hot-Saturn WASP-69b: Radio-Loud Exoplanet–Exomoon Sur v ey II (RLEES II)
000006826 260__ $$c2023
000006826 520__ $$aExomoons have so far eluded ongoing searches. Several studies have exploited transit and transit timing variations and high-resolution spectroscopy to identify potential exomoon candidates. One method of detecting and confirming these exomoons is to search for signals of planet-moon interactions. In this work, we present the first radio observations of the exomoon candidate system WASP-69b. Based on the detection of alkali metals in the transmission spectra of WASP-69b, it was deduced that the system might be hosting an exomoon. WASP-69b is also one of the exoplanet systems that will be observed as part of JWST cycle-1 GTO. This makes the system an excellent target to observe and follow up. We observed the system for 32 h at 150 and 218 MHz using the upgraded Giant Metrewave Radio Telescope (uGMRT). Though we do not detect radio emission from the systems, we place strong 3σ upper limits of 3.3 mJy at 150 MHz and 0.9 mJy at 218 MHz. We then use these upper limits to estimate the maximum mass-loss from the exomoon candidate.
000006826 536__ $$aFED-tWIN STELLA/$$cFED-tWIN STELLA/$$fFED-tWIN STELLA
000006826 594__ $$aNO
000006826 700__ $$aOza, Apurva V. 
000006826 700__ $$aHakim, Kaustubh 
000006826 700__ $$aManoj, P. 
000006826 700__ $$aTyagi, Himanshu
000006826 700__ $$aBanerjee, Bihan 
000006826 700__ $$aSurya, Arun 
000006826 700__ $$aNayak, Prasanta K. 
000006826 700__ $$aBanyal, Ravinder K. 
000006826 700__ $$aThorngren, Daniel P.
000006826 773__ $$c1662–1668$$n2$$pMonthly Notices of the Royal Astronomical Society$$v522$$y2023
000006826 8560_ $$fkaustubh.hakim@ksb-orb.be
000006826 85642 $$ahttps://doi.org/10.1093/mnras/stad1027
000006826 905__ $$apublished in
000006826 980__ $$aREFERD