William James Parker
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- School: Southern University and A&M College
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- Department: Mathematics
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Location:
801 Harding Blvd
Baton Rouge, LA - 70807 - Dates at Southern University and A&M College: -
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Biography
Southern University and A&M College - Mathematics
Educator and Researcher
William
Parker
Baton Rouge, Louisiana
Experienced Math Instructor with a Masters in Mathematics
Experience
East Baton Rouge Parish School System
Substitute Teacher
• Used variety of teaching techniques to encourage student critical thinking and discussion in Mathematics.
• Instructed 10-11th grade levels of Algebra I and Algebra II to a class of 30 students.
Education
Southern University and Agricultural and Mechanical College at Baton Rouge
Bachelor of Arts (BA)
Mathematics
Study Math and Physics President of SPSSouthern University and Agricultural and Mechanical College at Baton Rouge
Master of Science (MS)
Mathematics
Publications
Observation of Gravitational Waves from a Binary Black Hole Merger
American Physical Society
OnSeptember14,2015at09:50:45UTCthetwodetectorsoftheLaserInterferometerGravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0 × 10−21. It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203000 years, equivalent to a significance greater than5.1σ.Thesourceliesataluminositydistanceof410þ160 −180 Mpccorrespondingtoaredshiftz¼ 0.09þ0.03 −0.04. In the source frame, the initial black hole masses are 36þ5 −4M⊙ and 29þ4 −4M⊙, and the final black hole massis 62þ4 −4M⊙, with3.0þ0.5 −0.5M⊙c2 radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass blackhole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger
Observation of Gravitational Waves from a Binary Black Hole Merger
American Physical Society
OnSeptember14,2015at09:50:45UTCthetwodetectorsoftheLaserInterferometerGravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0 × 10−21. It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203000 years, equivalent to a significance greater than5.1σ.Thesourceliesataluminositydistanceof410þ160 −180 Mpccorrespondingtoaredshiftz¼ 0.09þ0.03 −0.04. In the source frame, the initial black hole masses are 36þ5 −4M⊙ and 29þ4 −4M⊙, and the final black hole massis 62þ4 −4M⊙, with3.0þ0.5 −0.5M⊙c2 radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass blackhole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger
Observation of Gravitational Waves from a Binary Black Hole Merger
American Physical Society
OnSeptember14,2015at09:50:45UTCthetwodetectorsoftheLaserInterferometerGravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0 × 10−21. It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203000 years, equivalent to a significance greater than5.1σ.Thesourceliesataluminositydistanceof410þ160 −180 Mpccorrespondingtoaredshiftz¼ 0.09þ0.03 −0.04. In the source frame, the initial black hole masses are 36þ5 −4M⊙ and 29þ4 −4M⊙, and the final black hole massis 62þ4 −4M⊙, with3.0þ0.5 −0.5M⊙c2 radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass blackhole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger