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Galaxy Tutorial
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residuals

Bell et al

(2007)

Slide 32

Stellar streams

Stellar streams

Belokurov et al (2007)

Slide 33

Tidal streams (Pal 5)

Tidal streams (Pal 5)

Sloan digital sky survey (SDSS)

Slide 34

Dark Halo

Dark Halo

Hard to track around MW

NGC 3198

Milky Way

Slide 35

Dark halos cuspy?

Dark halos cuspy?

Slide 36

Gravitational microlensing

Gravitational microlensing

Microlensing and magnitude of non-circular motions imply little DM at r<5kpc

Slide 37

Conclude

Conclude

Halo rather spherical

Counts of gravitational microlensing events imply that its mass is not in stellar or planetary objects

Slide 38

DM Searches

DM Searches

If m~GeV/c2, ~106 /cm2/s at ~300 km/s

Seasonal variation in flux

Slide 39

If particles weakly-interacting, one occasionally impacts atomic nucleus

If particles weakly-interacting, one occasionally impacts atomic nucleus

look for events deep underground (shielded from cosmic rays)

Boulby, Yorks

Slide 40

UKDMF Boulby

UKDMF Boulby

Slide 41

Limits on cross section

Limits on cross section

CDMS Collaboration (06)

SSM

Slide 42

Conclusion

Conclusion

Understanding the Milky Way key for understanding the Universe

Provides probe of constitution of Universe

Much progress in the last decade

Still many unresolved questions

Will remain on the frontier of physics & astronomy for the foreseeable future

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