1. Multi-Messenger Astronomy AY 17 10/19/2011

2. Outline What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return

3. Outline What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return

4. What is Multi-Messenger Astronomy? It’s Astronomy with multiple messengers! – One of the first instances of a clear cut meaning in an astronomical definition Informs you about different conditions in the same object – Photons come from the surface of the Sun – But neutrinos are made from the nuclear reactions in the core

5. Outline What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return

6. Photons Most widely used messenger particle in Astronomy – Easy to detect (unlike neutrinos) – Can travel long distances (unlike nuclear messenger particles) However…. – Not all frequencies are created equal

7. Photons Astronomers are merely fleas on the dog of industry – Cheap Silicon Optical – Radar Radio – Nuclear Testing Gamma rays

8. Photons X-Ray Astronomy – Began as a series of Balloon and V-2 Rocket experiments in the 1960s Usually a single astronomical instrument tagging along with various other experiments (atmospheric measurements, NIH experiments, etc.) Initially measured the Sun, and eventually led to the discovery of bright X-ray sources in the Milky Way

9. Photons Chandra X-Ray Observatory – 3-10 keV – Launched in 1999 – Plane parallel mirrors

10. Photons Galactic and Extragalactic X-Ray Astronomy – 10 keV / k b ~ 10 8 K

11. Photons

12. Intra-Cluster Gas – Cooled by Thermal Bremsstrahlung Evidence for metal lines in the Intra- cluster gas – How did they get there?

13. Photons X-Ray emission within Galaxies? – Supernovae – Accreting Black holes – X-ray binaries NS+NS NS+Blackhole NS+WD etc

14. Outline What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return

15. Cosmic Rays What are Cosmic Rays – Highly Energetic atomic and subatomic particles – ~90% Protons, 9% He, 1% other (mostly heavy elements)

16. Cosmic Rays

18. Galactic Cosmic Rays – Originate in supernova remnants – Accelerated by magnetic fields – Localization is hard Deflected by magnetic fields in the galaxy – Can fragment as travel

19. Cosmic Rays Extragalactic Cosmic Rays – Some cosmic rays have enough energy to leave the galaxy 1 / m^2 / yr hits the Earth – Little is known about their composition (statisitics problem) – Some evidence they come from AGN – Could also come from colliding galaxies, the early universe, decay of superheavy particles

20. Cosmic Rays

21. Cosmic Rays and You

22. Outline What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return

23. Neutrinos 86 Holes 5160 Optical Sensors Sensitive to high energy neutrinos

24. Neutrinos Solar Observation – Super-Kamiokande produced a neutrino image of the Sun

25. Neutrinos

26. Supernova Early Warning System – Neutrinos were detected from SN 1987A before the optical counterpart was discovered – IceCube and other neutrino experiments are poised to detect the neutrinos from the next nearby (galactic) supernova – Icecube will have the ability to pinpoint the neutrino origin accurately

27. Neutrinos Avoiding Cosmic Ray Confusion – IceCube also has a cosmic ray detector array on the Antarctic surface Coincidence between cosmic ray detection and “neutrino” detection lowers confusion rates This “junk” is interesting to some people!

28. Cosmic Rays with IceCube

29. Local Magnetic fields? Stellar magnetic fields? A handful of close pulsars?

30. Outline What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return

31. Gravity Waves

36. Gravitational Waves What the gravity wave sky actually looks like:

37. Gravity Waves

39. Advanced LIGO Bigger, Better, Stronger – 20x stronger laser – Seismically isolated from 40 Hz down to 10 Hz – Reduced thermal noise – An actual detection likely! – 2015* *Actual finish time may vary

40. Outline What is Multi-messenger astronomy? Photons Cosmic Rays Neutrinos Gravity-Waves Sample-Return

41. Sample Return

43. Collect cometary and interstellar dust particles in aerogel Return the sample to Earth Take millions of photographs of aerogel to identify dust grains – stardust@home 45 interstellar dust grains identified!

44. Sample Return

45. List of findings: – Organic compounds – Amorphous silicates – Olivine and pyroxene (Solar system matter well mixed with ISM)

46. Sample Return Supernova Debris – Fe-60 has a half life of 2.6 Myr (all of it that formed with the Earth is gone)

47. Sample Return This points to a core-collapse supernova within a few 10s of parsecs of the Earth exploding several million years ago Contributed to the “Local Bubble” of the ISM – We are in a low density, high temperature, ~150 light year region of the ISM