Measures of Dispersion and Variability: Range, QD, AD and SD
Krystina Krylova
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
5.
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
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
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
