Isabel Rebollido1, Marshall Perrin1, Christine Chen1, Chris Stark2, Paul Kalas3, Laurent Pueyo1, Julien Girard1 1Space Telescope Science Institute, Baltimore, MD, USA, 2NASA Goddard Space Flight Center, Greenbelt, MD, USA 3Astronomy Department, University of California, Berkeley, CA, USA irebollido@stsci.edu Why β Pic? The star, β Pic, (A6V with an estimated age ~20 Myr) is nearby (~19 pc) and bright (V=3.8 mag). High angular resolution scattered light and thermal emission images have revealed a spectacular edge-on disk including a main belt (diameter ~1800 au) and an inner belt (6.4 au) . β Pic also hosts two Jovian-mass planets, β Pic b and β Pic c, with semi-major axes of 9 and 2.8 au respectively. Finally, we have had evidence of dynamical activity in the system for over 30 years, when exocomets were first discovered around β Pic. Observations with HST What do we see in the data? Takeaway message! During the past 25 years, HST has visited beta Pic repeatedly to image its archetypal disk in scattered light. These observations span visible (STIS, ACS) to near-infrared light (NICMOS, WFC3). We present here unpublished WFC3 F160W observations for the first time and an improved reduction of F110W. Although many of the individual observations have been analyzed in detail, the complete set of scattered light images has never been studied self- consistently. We plan to analyze these observations in conjunction with high angular resolution thermal emission images and planned JWST Cycle 1 GTO observations (PID 1411), to study the dust spatial distribution, shape and composition in detail. • Both the SW (a) and the NE (b) sides of the disk have a blue color at distances great than 50 au. • The Disk Flux/Stellar Flux (c) and the Disk Flux/Stellar Flux time the stellar offset squared (d) indicate the presence of a density enhancement at ~100 au. • The disk is asymmetric (e) with the SW side being brighter than the NE. The disk appears more asymmetric at longer wavelengths (~100) au and more asymmetric at shorter wavelengths (~85 au). • We have analyzed HST β Pic images from 3 different instruments: ACS, STIS and WFC3. • We find a density enhancement in the disk at 50-100 au (d). • We find that the asymmetry of the disk (e) is more pronounced and further from the star in the WFC3 data when compared to ACS and STIS. • We plan to self-consistently analyze the scattered light and thermal emission from the β Pic disk to better constrain the overall disk geometry and the properties of the constituent grains (e.g. size, composition). JWST Cycle 1 science observations coming soon, so stay tuned! Images of β Pic observations used in this analysis. Title indicates the instrument and filter (ACS, WFC), or instrument and observation program (STIS). The central wavelength of the filters is shown in the upper right, and the date in the upper left. Images are scaled to show comparable fields of view. a b c d e I have another poster! We detected CO gas in a young debris disk @102.201 IMAGES OF THE β PIC DISK WITH HST RADIAL PROFILES OF THE DISK Some References: Larwood & Kalas, 2001; Okamoto 2004;Lagrange+2008; Apai+2015; Ballering+2016; Lagrange+2019 01-Oct-2003 01-Oct-2003 01-Oct-2003 17-Sep-1997 06-Mar-2012 23-Sep-2013 21-Nov-2009 21-Nov-2009 We are for the first time gathering all Hubble coronagraphy of the famous β Pic debris disk for a joint analysis of the disk as seen in multiple wavelengths and over time