• Corpus ID: 1153539

Joint Efficient Dark-energy Investigation (JEDI): a Candidate Implementation of the NASA-DOE Joint Dark Energy Mission (JDEM)

@article{Crotts2005JointED,
  title={Joint Efficient Dark-energy Investigation (JEDI): a Candidate Implementation of the NASA-DOE Joint Dark Energy Mission (JDEM)},
  author={Arlin P. S. Crotts and Peter M. Garnavich and William Priedhorsky and Salman Habib and Katrin Heitmann and Yun Wang and Edward A. Baron and David Branch and Harvey S. Moseley and Alexander S. Kutyrev and Chris Blake and Edward Cheng and Ian P. Dell’Antonio and John W. MacKenty and Gordon K. Squires and Max Tegmark and Craig Wheeler and Ned Wright},
  journal={arXiv: Astrophysics},
  year={2005}
}
JEDI will probe dark energy in three independent ways by measuring the expansion history of the universe: (1) using type Ia supernovae as cosmological standard candles over a range of distances, (2) using baryon oscillations as a cosmological standard ruler over a range of cosmic epochs, (3) mapping the weak gravitational lensing distortion by foreground galaxies of the images of background galaxies at different distances. JEDI will unravel the nature of dark energy with accuracy and precision… 

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References

SHOWING 1-6 OF 6 REFERENCES
Astrophys.J
  • Astrophys.J
  • 2000
Astrophys.J.Suppl
  • Astrophys.J.Suppl
  • 2003
astro-ph/0504097, Nature, in press
  • 2005
Phys. Rev. D
  • Phys. Rev. D
  • 2005
Phys.Rev
  • Phys.Rev
  • 2004
We thank Pier-Stefano Corasaniti for sending us the Fisher matrices of (w 0 , w ′ ) for the JEDI SNe Ia
  • We thank Pier-Stefano Corasaniti for sending us the Fisher matrices of (w 0 , w ′ ) for the JEDI SNe Ia