WASP-69b's Escaping Envelope Is Confined to a Tail Extending at Least 7 R_p

Studying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed as excess H/He absorption during/after transit. Such an outflow has been observed for WASP-69b by multiple groups that disagree on the geometry and velocity structure of the outflow. Here, we report the detection of this planet's outflow using Keck/NIRSPEC for the first time. We observed the outflow 1.28 hr after egress until the target set, demonstrating the outflow extends at least 5.8 x 10(5) km or 7.5 R-p This detection is significantly longer than previous observations, which report an outflow extending similar to 2.2 planet radii just 1 yr prior. The outflow is blueshifted by -23 km s(-1) in the planetary rest frame. We estimate a current mass-loss rate of 1 M-circle plus Gyr(-1). Our observations are most consistent with an outflow that is strongly sculpted by ram pressure from the stellar wind. However, potential variability in the outflow could be due to time-varying interactions with the stellar wind or differences in instrumental precision.