1. Team L Supernovae Mark Blount Elizabeth Brooks Blaze Campbell Sonia Vazquez Yanet Zavala

2. Goal  To learn about stellar evolution theory  To discover how elements spread across our galaxy after a supernova explosion.  To draw conclusions from supernova remnants that we studied, specifically Cassiopeia A (Cas A) and Tycho.

3.  What is a supernova?  How are supernovae formed?  Stars make energy through fusion reactions in the core.  Internal structure has layers of chemicals like an onion.  Supernova explosion spreads the chemicals into space. Introduction SN 1987a - Type II before supernova

4. Introduction Cont.  Why are supernovae remnants important?  The chemicals spread by SNRs are the building blocks of life anywhere in our universe.  Supernovae remnants  Shells of gas that expand into space

5. Materials  DS9 computer program from NASA  Chandra X-ray Satellite archives  DS9 instruction handbook  Horizons Text book by: Michael Seeds  Lecture Notes by M. Richards  NASA Chandra Education webpage (http://chandra-ed.harvard.edu/activities.html)

6. Procedures  Use DS9 computer program to analyze SNR data  Load, select, and examine SNR using DS9  Qualitative Analysis  Quantitative Analysis

7. Procedures Cont.  Calculate distance to supernova remnant  Use angular size of SNR and expansion speed over 10 years  Calculate date when supernova occurred  Calculate time that a knot takes to move a certain distance  Determine size of remnant  Measure width of SNR in pixels and convert to light years  Calculate luminosity from flux  Examine radial intensity profile  Examine energy spectrum

8. Results Cas ATycho Distance in light years (ly)11,4007,500 Date of explosion1667 A.D.1572 A.D. Size of remnant 6.16 pc 18.57 ly 6.97 pc 20.07 ly Luminosity (ergs/sec)4.54 x 10 36 4.98 x 10 36 Luminosity (L sun )11951311

9. Cas ATycho

10. Conclusions  Our results confirm the spread of the elements from a supernova event.  Accuracy and precision play an important role in our measurements and calculations because of the large distances and small angles in astronomy.  Further Analysis  Long term monitoring of SNRs.  Determine rate of expansion  Detailed examination of the composition of elements

11. QUESTIONS?

12. Thank you... Dr. Daniel Larson, Dean of the Eberly College of Science Dr. Mercedes Richards Ms. Jody Markley Ms. Annie Holmes Mr. Craig Keiser Ms. Skyra Blanchard All UBMS Staff This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory Dr. W. Terrell Jones, Vice Provost for Educational Equity