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Joint Efficient Dark-energy Investigation (JEDI): a Candidate Implementation of the NASA-DOE Joint Dark Energy Mission (JDEM) | | Arlin Crotts
; Peter Garnavich
; William Priedhorsky
; Salman Habib
; Katrin Heitmann
; Yun Wang
; Eddie Baron
; David Branch
; Harvey Moseley
; Alexander Kutyrev
; Chris Blake
; Edward Cheng
; Ian Dell’Antonio
; John Mackenty
; Gordon Squires
; Max Tegmark
; Craig Wheeler
; Ned Wright
; | | Date: |
2 Jul 2005 | | Subject: | astro-ph | | Affiliation: | Columbia), Peter Garnavich (Notre Dame), William Priedhorsky, Salman Habib, Katrin Heitmann (LANL), Yun Wang, Eddie Baron, David Branch (OU), Harvey Moseley, Alexander Kutyrev (NASA GSFC), Chris Blake (British Columbia), Edward Cheng (Conceptual Analyt | | Abstract: | 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. 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 (0.8-3.2 micron) with a field of view of 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 so that the appropriate balance of time is devoted to each. JEDI will measure the cosmic expansion history H(z) as a free function to < 2% accuracy in redshift bins of 0.2-0.3. Assuming a flat universe and sigma(Omega_m)=0.01 (0.03), JEDI could measure a departure from a vanilla Lambda CDM model (w_0=-1, w’=0) with sigma(w_0)=0.013 (0.031) and sigma(w’)=0.046 (0.063). JEDI will obtain the well-sampled lightcurves in Z, J, H, K, L bands and spectra of ~ 14,000 type Ia supernovae with redshifts ranging from 0 to 1.7; the redshifts of ~ 10-100 million galaxies to H ~ 23 and z ~ 4 over 1000-10,000 square degrees; and measurements of the shapes of galaxies over 1000-10,000 square degrees in Z,J,H,K,L for > 10^9 galaxies to H 25. | | Source: | arXiv, astro-ph/0507043 | | Services: | Forum | Review | PDF | Favorites | |
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