SCSI: the Southern Connecticut Stellar Interferometer

Horch, Elliott; Weiss, Samuel A.; Rupert, J.; DiMaio, Alex J.; Nusdeo, Daniel A.; Peronio, Pietro; Rech, Ivan; Gulinatti, Angelo; Giudice, Andrea

doi:10.1117/12.2232659

Cited by 4 publications

(2 citation statements)

References 16 publications

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“…The basic idea has been discussed in the context of intensity interferometry (see fig. 3 in Horch et al 2016). Even though the implementation of such technology on current telescope arrays seems ambitious, it does not have to be implemented now, but rather in a dozen or so years.…”

Section: Discussionmentioning

confidence: 99%

Towards a polarization prediction for LISA via intensity interferometry

Baumgartner

Bernardini

Cuissa

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Compact Galactic binary systems with orbital periods of a few hours are expected to be detected in gravitational waves (GW) by LISA or a similar mission. At present, these so-called verification binaries provide predictions for GW frequency and amplitude. A full polarisation prediction would provide a new method to calibrate LISA and other GW observatories, but requires resolving the orientation of the binary on the sky, which is not currently possible. We suggest a method to determine the elusive binary orientation and hence predict the GW polarisation, using km-scale optical intensity interferometry. The most promising candidate is CD–30○ 11223, consisting of a hot helium subdwarf with mB = 12 and a much fainter white dwarf companion, in a nearly edge-on orbit with period 70.5 min. We estimate that the brighter star is tidally stretched by 6%. Resolving the tidal stretching would provide the binary orientation. The resolution needed is far beyond any current instrument, but not beyond current technology. We consider scenarios where an array of telescopes with km-scale baselines and/or the Very Large Telescope (VLT) and Extremely Large Telescope (ELT) are equipped with recently-developed kilo-pixel sub-ns single-photon counters and used for intensity interferometry. We estimate that a team-up of the VLT and ELT could measure the orientation to ±1○ at 2σ confidence in 24 hours of observation.

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Section: Discussionmentioning

confidence: 99%

Towards a polarization prediction for LISA via intensity interferometry

Baumgartner

Bernardini

Cuissa

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…A [35]. The baselines for the NSII were adapted by having the telescopes able to move along a 188 m diameter circular railroad track, but can as easily be done with static telescopes and digital delays in this day and age [36,37,38,39,40,41,42].…”

Section: Pos(icrc2019)007mentioning

confidence: 99%

Non-Gamma-ray Applications of TeV Telescopes

Daniel¹

2019

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019)

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Imaging Atmospheric Cherenkov Telescopes (IACTs) are instruments for the indirect detection of very high energy cosmic and gamma rays, since they are essentially very large light buckets used to gather the optical Cherenkov photons generated within extensive air showers. Whilst the imaging quality of their reflective surfaces may be crude it should not be forgotten that they are in actuality amongst the largest optical telescopes ever constructed-with sensitive camera equipment ideal for application to high time resolution optical astronomical research from scales of seconds down to nanoseconds. Recent advances in instrumentation have resulted in the VER-ITAS IACTs making sub-milliarcsecond resolution observations through the revived technique of intensity interferometry and obtaining the smallest optical angular resolution measurements to date in direct measurements of stellar diameters at the ∼100 micro-arcsecond scale from observations of asteroid occultations of stars. There are many further diverse non-gamma-ray applications that these types of telescopes are starting to contribute to: from the simultaneous search for optical counterparts to Fast Radio Bursts, to the search for extraterrestrial intelligence. This increased range of utility for these form of telescope expands their potential remit from facilities for specialised purposes to observatories for a wider scientific community in prime locations around the world.

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