TY - JOUR
T1 - Single-photon intensity interferometry (SPIIFY)
T2 - Utilizing available telescopes
AU - Pilyavsky, Genady
AU - Mauskopf, Philip
AU - Smith, Nathan
AU - Schroeder, Edward
AU - Sinclair, Adrian
AU - van Belle, Gerard T.
AU - Hinkel, Natalie
AU - Scowen, Paul
N1 - Publisher Copyright:
© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
PY - 2017/6/1
Y1 - 2017/6/1
N2 - One of the main scientific goals of optical interferometers is to measure the angular diameters of stars. These measurements, combined with precise distance measurements, such as those from the upcoming Gaia satellite, can provide improved constraints on stellar linear diameters and effective temperature. We describe a modular intensity interferometer system using commercially available single-photon detectors. We present our calculations on the sensitivity and uv-plane coverage using these modules mounted on existing telescopes on Kitt Peak, Arizona. Determining accurate stellar properties is important for testing models of stellar evolution as well as for deriving physical properties of transiting exoplanets. Our simulations indicate that we should be able to measure stellar diameters of bright stars with AB magnitude ≤6 with a precision of ≥5 per cent in a single night of observation.
AB - One of the main scientific goals of optical interferometers is to measure the angular diameters of stars. These measurements, combined with precise distance measurements, such as those from the upcoming Gaia satellite, can provide improved constraints on stellar linear diameters and effective temperature. We describe a modular intensity interferometer system using commercially available single-photon detectors. We present our calculations on the sensitivity and uv-plane coverage using these modules mounted on existing telescopes on Kitt Peak, Arizona. Determining accurate stellar properties is important for testing models of stellar evolution as well as for deriving physical properties of transiting exoplanets. Our simulations indicate that we should be able to measure stellar diameters of bright stars with AB magnitude ≤6 with a precision of ≥5 per cent in a single night of observation.
KW - Instrumentation: high angular resolution
KW - Instrumentation: interferometers
KW - Methods: data analysis
KW - Stars: fundamental parameters
KW - Techniques: high angular resolution
KW - Techniques: interferometric
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U2 - 10.1093/mnras/stx272
DO - 10.1093/mnras/stx272
M3 - Article
AN - SCOPUS:85045940539
SN - 0035-8711
VL - 467
SP - 3048
EP - 3055
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -