Krystina Krylova
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The document summarizes the history and current state of optical SETI (OSETI), which searches for signals from extraterrestrial intelligence using lasers and optical telescopes. It notes that OSETI efforts began in the 1960s and discusses various university-based OSETI groups established between 1993-2007 using different detector setups, from elementary detectors to mega detectors composed of many elementary units. It describes simulations of night sky background to optimize detector sensitivity and thresholds. Current work involves building improved double and quad mega detectors to better eliminate background and future directions will depend on available funding.
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The Future of the Internet Enabling New Science
10.04.19
Invited Speaker
San Diego Science Festival
Mark Twain High School
Title: The Future of the Internet Enabling New Science
San Diego, CA
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Predavanje održano 27. septembra 2021. godine u okviru serije naučno-popularnih predavanja povodom obeležavanja 50 godina studija fizike, hemije i matematike na Univerzitetu u Nišu i dana Prirodno-matematičkog fakultetu u Nišu.
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The ExoplanetSat Mission to Detect Transiting Exoplanets with a C
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Cosmology Research in China
ECL 2018 Autumn Workshop
Presentation by Prof. Xuelei Chen
National Astronomical Observatories,
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- 1. OSETI Optical Search for Extra-Terrestrial Intelligence Kristina Krylova(University at Buffalo – SUNY) REU at Case Western Reserve University 27 July, 2010
- 2. Timeline Nationwide OSETI efforts Varieties of detector setups Night Sky Background simulation What’s next? Outline 2/12
- 3. 1959 – Giuseppe Cocconi and Philip Morrison: interstellar communication via radio waves 1960 – Theodore Maiman: first laser in Hughes Research Laboratory 1961 – Robert Schwartz and Charles Townes: paper suggesting use of laser 1993 – Stuart Kingsley: optical SETI in the US Timeline 3/12
- 4. Columbus Observatory, 1993 Harvard, 1998 Princeton, 1999 UC Berkley, 1999 Lick Observatory, 2000 Case Western Reserve, 2007 OSETI groups 4/12
- 6. ≈1.5 inch diameter PMTsData recording every 4 nanoseconds 5/12 Elementary Detector
- 7. 9 elementary detectors = 1 mega detector Threshold set on mega detector to lower background Lower threshold: more background vs. greater sensitivity BAD GOOD 6/12 Mega Detector Facts
- 8. Double Mega Detector 7/12
- 9. Quad Mega Detector 8/12
- 10. 9/12 Night Sky Background Simulation
- 11. Build and install the detectors Start taking data 10/12 What’s next?
- 12. Quad mega detector better eliminates background thus more sensitive to extraterrestrial signal Quad is twice as expensive as double Final detector design will depend on funding 11/12 Summary
- 13. Thank you for being here!kkrylova@buffalo.edu 12/12
Editor's Notes
- High frequency radio wavesHughes Research Laboratory in Californiapaper by Robert Schwartz and Charles Townes People still continued to use radio waves for several decades though until laser technology has been improved October 19, 1998 OSETI at Harvard
- Stuart Kingsley’s Columbus in Bexley, OH near Columbus which is 2 and a half hours south-west of hereLick at the University of California