AAS 207th Meeting, 8-12 January 2006
Session 100 Cosmology, Early Universe, Cosmic Distance Scale I
Oral, Tuesday, 2:00-3:30pm, January 10, 2006, Salon 1

Previous   |   Session 100   |   Next  |   Author Index   |   Block Schedule

[100.04] Illuminating Dark Energy with the Joint Efficient Dark-energy Investigation (JEDI)

Y. Wang, E. Baron, D. Branch (Univ. of Oklahoma), S. Casertano (Space Telescope Institute), E. Cheng (Conceptual Analytics), A. Crotts (Columbia), I. Dell'Antonio (Brown Univ.), P.M. Garnavich (Notre Dame), S. Habib (LANL), M. Hamuy (Univ. of Chile), K. Heitmann (LANL), A.S. Kutyrev (GSFC), J.W. MacKenty (Space Telescope Institute), L.A. Moustakas (JPL), C. Papovich (Steward Observatory), M. Phillips (Carnegie Institution of Washington Las Campanas Observatory), W.C. Priedhorsky (LANL), R. Silverberg (GSFC), V. Springel (Max-Planck-Institut fuer Astrophysik), G. Squires (Caltech), M. Tegmark (MIT), C. Wheeler (UT Austin), E. L. Wright (UCLA), JEDI Collaboration

JEDI (Joint Efficient Dark-energy Investigation) is a candidate implementation of the NASA-DOE Joint Dark Energy Mission (JDEM). JEDI will probe dark energy in three independent ways: (1) using Type Ia supernovae as cosmological standard candles over a range of distances, (2) using baryon acoustic 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 by obtaining observations of a quantity and quality only possible with a dedicated space mission.

JEDI is a 2m class space telescope with the unique ability of simultaneous wide-field imaging (0.8-4.2 micron in five bands) and multi-slit spectroscopy (with minimum wavelength coverage 1-2 micron) with a field of view of around 1 square degree. What makes JEDI efficient is its ability to simultaneously obtain high signal-to-noise ratio, moderate resolution slit spectra for all supernovae and ~ 5000 galaxies in its wide field of view, and to combine imaging and spectroscopy to balance the time devoted to each. JEDI will obtain the well-sampled lightcurves in z, j, h, k, l bands and spectra of ~ 5000-20,000 Type Ia supernovae with redshifts ranging from 0 to 2; the redshifts of ~ 100 million galaxies to z ~ 2 over 10,000 square degrees; and measurements of the shapes of galaxies over 10,000 square degrees in z, j, h, k, l bands to H ~ 22-23. We will discuss the JEDI mission concept, and the expected constraints on dark energy from JEDI data.

This work was supported in part by NSF CAREER grant AST-0094335.

If you would like more information about this abstract, please follow the link to http://jedi.nhn.ou.edu/. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

Previous   |   Session 100   |   Next

Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.