A Volume-limited Radio Search for Magnetic Activity in 140 Exoplanets with the Very Large Array

• Published in: The Astronomical journal 2024-09, Vol.168 (3), p.127
• Main Authors: Ortiz Ceballos, Kevin N., Cendes, Yvette, Berger, Edo, Williams, Peter K. G.
• Format: Article
• Language: English
• Subjects: Arrays; Circular polarization; Emissions; Exoplanets; Extrasolar planets; Frequency ranges; Luminosity; Magnetospheric radio emissions; Non-thermal radiation sources; Planetary magnetospheres; Planetary systems; Polarization; Radio emission; Radio sources (astronomy); Searching; Star-planet interactions; Stellar activity; Stellar systems; Target detection
• ISSN: 0004-6256; 1538-3881
• DOI: 10.3847/1538-3881/ad58be

We present results from a search for radio emission in 77 stellar systems hosting 140 exoplanets, predominantly within 17.5 pc using the Very Large Array (VLA) at 4–8 GHz. This is the largest and most sensitive search to date for radio emission in exoplanetary systems in the GHz frequency range. We obtained new observations of 58 systems and analyzed archival observations of an additional 19 systems. Our choice of frequency and volume limit is motivated by radio detections of ultracool dwarfs (UCDs), including T dwarfs with masses at the exoplanet threshold of ∼13 MJ. Our surveyed exoplanets span a mass range of ≈10−3–10 MJ and semimajor axes of ≈10−2–10 au. We detect a single target—GJ 3323 (M4) hosting two exoplanets with minimum masses of 2 and 2.3 M⊕—with a circular polarization fraction of ≈40%; the radio luminosity agrees with its known X-ray luminosity and the Güdel–Benz relation for stellar activity suggesting a likely stellar origin, but the high circular polarization fraction may also be indicative of star–planet interaction. For the remaining sources our 3σ upper limits are generally Lν ≲ 1012.5 erg s−1 Hz−1, comparable to the lowest radio luminosities in UCDs. Our results are consistent with previous targeted searches of individual systems at GHz frequencies while greatly expanding the sample size. Our sensitivity is comparable to predicted fluxes for some systems considered candidates for detectable star–planet interaction. Observations with future instruments such as the Square Kilometre Array and Next-Generation VLA will be necessary to further constrain emission mechanisms from exoplanet systems at GHz frequencies.