VTXO: The Virtual Telescope for X-ray Observations
John F. Krizmanic, Neerav Shah, Philip C. Calhoun, Alice K. Harding, Lloyd R. Purves, Cassandra M. Webster, Michael F. Corcoran, Chris R. Shrader, Steven J. Sto… 展开作者
John F. Krizmanic, Neerav Shah, Philip C. Calhoun, Alice K. Harding, Lloyd R. Purves, Cassandra M. Webster, Michael F. Corcoran, Chris R. Shrader, Steven J. Stochaj, Kyle A. Rankin, Daniel T. Smith, Hyeongjun Park, Laura E. Boucheron, Krishna Kota, Asal Naseri
备注：
6 pages, 7 figures, corrected version, Proceedings Volume 11444, Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray; 114447V (2020). arXiv admin note: text overlap with arXiv:2006.12174
The Virtual Telescope for X-ray Observations (VTXO) will use lightweight Phase Fresnel Lenses (PFLs) in a virtual X-ray telescope with $\sim$1 km focal length and with $\sim$50 milli-arcsecond angular resolution. VTXO is formed by using precision formation flying of two SmallSats: a smaller OpticsSat that houses the PFLs and navigation beacons while a larger DetectorSat contains an X-ray camera, a precision start tracker, and the propulsion for the formation flying. The baseline flight dynamics uses a highly elliptical supersynchronous orbit allow the formation to hold in an inertial frame around the 90,000 km apogee for 10 hours of the 32.5 hour orbit with nearly a year mission lifetime. VTXO's fine angular resolution enables measuring the environments close to the central engines of bright compact X-ray sources. This X-ray imaging capability allows for the study of the effects of dust scattering near to the central objects such as Cyg X-3 and GX 5-1, for the search for jet structure near to the compact object in X-ray novae such as Cyg X-1 and GRS 1915+105, and for the search for structure in the termination shock of in the Crab pulsar wind nebula. The VTXO SmallSat and instrument designs, mission parameters, and science performance are described. VTXO development was supported as one of the selected 2018 NASA Astrophysics SmallSat Study (AS$^3$) missions.
Optical frequency comb integration in radio telescopes: advancing signal generation and phase calibration
Korea Advanced Institute of Science and Technology (KAIST)（韩国科学技术院）；Korea Astronomy and Space Science Institute (KASI)（韩国天文学与空间科学研究所）；University of Science and Technology (UST)（科学技术联合大学院大学）；Max-Planck Institute for Radio Astronomy（马克斯·普朗克射电天文研究所）；Korea Research Institute of Standards and Science (KRISS)（韩国标准与科学研究院）
Using U-Nets to Create High-Fidelity Virtual Observations of the Solar Corona
NASA Frontier Development Lab（NASA前沿发展实验室）；IQVIA（艾昆纬）；Rosseland Center for Solar Physics（罗瑟兰太阳物理中心）；University of Oslo（奥斯陆大学）；IACS - The Catholic University of America（美国天主教大学计算科学研究所）；NASA - Goddard Space Flight Center（NASA戈达德太空飞行中心）；Lockheed Martin Solar and Astrophysics Laboratory（洛克希德·马丁太阳与天体物理实验室）；Stanford University（斯坦福大学）；Institut d’Astrophysique Spatiale, Université Paris-Sud（巴黎南大学空间天体物理研究所）；University of Oxford（牛津大学）；SETI（搜寻地外文明研究所）
