Panchromatic Observations of SN2011dh Point to a Compact Progenitor Star

• Published in: NASA Center for AeroSpace Information (CASI). Misc. Resources
• Main Authors: Soderberg, A M, Margutti, R, Hurley, K, Barthelmy, S, Toizumi, T, Morii, M, Chevalier, R A, Gurwell, M, Petitpas, G, Rupen, M, Alexander, T, Levesque, E M, Zauerer, B A, Fransson, C, Brunthaler, A, Bietenholz, M F, Chugai, N, Cline, T, Krauss, M, Katz, B, Chomiuk, L, Dittmann, J A, Nakar, E, Sakamoto, T, Kawai, N
• Format: Web Resource
• Language: English
• Published: Hampton NASA/Langley Research Center 11.07.2011
• Subjects: Binary stars; Companion stars; Elastic scattering; Emission; Gamma rays; High energy astronomy; Missions; Optical properties; Photometry; Photons; Stellar winds; Supernovae; Wind speed

We report the discovery and detailed monitoring of X-ray emission associated with the Type IIb SN2011dh using data from the Swift and Chandra satellites, placing it among the best studied X-ray supernovae to date. We further present millimeter and radio data obtained with the SMA, CARMA, and EVLA during the first three weeks after explosion. Combining these observations with early optical photometry, we show that the panchromatic dataset is well-described by non-thermal synchrotron emission (radio/mm) with inverse Compton scattering (X-ray) of a thermal population of optical photons. We derive the properties of the shockwave and the circumstellar environment and find a time-averaged shock velocity of v approximately equals 0.1c and a progenitor mass loss rate of M-dot approximately equals 6 X 10 (exp 5) Solar M/ yr (wind velocity, v(sub w) = 1000 km/s). We show that these properties are consistent with the sub-class of Type IIb supernovae characterized by compact progenitors (Type cIIb) and dissimilar from those with extended progenitors (Type eIIb). Furthermore, we consider the early optical emission in the context of a cooling envelope model to estimate a progenitor radius of R(sub star) approximately equals 10(exp 11) cm, in line with the expectations for a Type cIIb supernova. Together, these diagnostics suggest that the putative yellow supergiant progenitor star identified in archival HST observations is instead a binary companion or unrelated to the supernova. Finally, we searched for the high energy shock breakout pulse using X-ray and gamma-ray observations obtained during the purported explosion date range. Based on the compact radius of the progenitor, we estimate that the shock breakout pulse was detectable with current instruments but likely missed due to their limited temporal/ spatial coverage. Future all-sky missions will regularly detect shock breakout emission from compact SN progenitors enabling prompt follow-up observations of the shockwave with the EVLA and ALMA.