Marrone, Daniel P.
Carlstrom, John E.
Doeleman, Sheperd S.
Folkers, Thomas W.
Greer, Christopher H.
Lauria, Eugene F.
Massingill, Kyle D.
Nguyen, Chi H.
Stark, Antony A.
AffiliationUniv Arizona, Steward Observ
Univ Arizona, Dept Astron
MetadataShow full item record
PublisherSPIE-INT SOC OPTICAL ENGINEERING
CitationJunhan Kim, Daniel P. Marrone, Christopher Beaudoin, John E. Carlstrom, Shepherd S. Doeleman, Thomas W. Folkers, David Forbes, Christopher H. Greer, Eugene F. Lauria, Kyle D. Massingill, Evan Mayer, Chi H. Nguyen, George Reiland, Jason SooHoo, Antony A. Stark, Laura Vertatschitsch, Jonathan Weintroub, and André Young "A VLBI receiving system for the South Pole Telescope", Proc. SPIE 10708, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX, 107082S (9 July 2018); doi: 10.1117/12.2301005; https://doi.org/10.1117/12.2301005
Rights© (2018) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE).
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractThe Event Horizon Telescope (EHT) is a very-long-baseline interferometry (VLBI) experiment that aims to observe supermassive black holes with an angular resolution that is comparable to the event horizon scale. The South Pole occupies an important position in the array, greatly increasing its north-south extent and therefore its resolution. The South Pole Telescope (SPT) is a 10-meter diameter, millimeter-wavelength telescope equipped for bolometric observations of the cosmic microwave background. To enable VLBI observations with the SPT we have constructed a coherent signal chain suitable for the South Pole environment. The dual-frequency receiver incorporates state-of-the-art SIS mixers and is installed in the SPT receiver cabin. The VLBI signal chain also includes a recording system and reference frequency generator tied to a hydrogen maser. Here we describe the SPT VLBI system design in detail and present both the lab measurements and on-sky results.
VersionFinal published version
SponsorsNSF [AST-1207752, AST-1440254]; National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation