1 / 17

BAOs

BAOs. SDSS, DES, WFMOS teams (Bob Nichol, ICG Portsmouth). Understanding Dark Energy. Observers Prospective. We can make progress on questions: Is DE just a cosmological constant (w(z)=-1)? (Make better observations and push to higher z)

foster
Télécharger la présentation

BAOs

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. BAOs SDSS, DES, WFMOS teams (Bob Nichol, ICG Portsmouth)

  2. Understanding Dark Energy Observers Prospective • We can make progress on questions: • Is DE just a cosmological constant (w(z)=-1)? • (Make better observations and push to higher z) • Is DE a new form of matter (with negative effective pressure) or a breakdown of GR? • (Study DE using different probes) • But there are only two broad avenues: • Geometrical tests (SN, BAO) • Growth of structure (ISW, lensing, clusters) No compelling theory, must be observational driven

  3. DETF Report (Kolb et al) 138 pages condensed to this column SN & BAO - safe, but only 100% improvement CL & WL - risky, but big gains Clear recommendation to do multiple measurement with one being the growth of structure to test GR

  4. Baryon Acoustic Oscillations m=0.24 best fit WMAP model Miller et al. 2001, Percival et al. 2001, Tegmark et al. 2001, 2006 Cole et al. 2005, Eisenstein et al. 2005, Hutsei 2006, Blake et al. 2006, Padmanabhan et al. 2006 WMAP3 Power spectrum of galaxy clustering. Smooth component removed Percival et al. 2006 SDSS DR5 520k galaxies

  5. Cosmological Constraints Standard ruler (flat,h=0.73,b=0.17) 99.74% detection Percival et al. (2006) h=0.72±0.08 HST m=0.256+0.049-0.029 Best fit m=0.26 Sullivan et al. (2003) m0.275h WMAP3 m=0.256+0.029-0.024 mh2 WMAP3 m=0.256+0.019-0.023

  6. BAO with Redshift Measure ratio of volume averaged distance D0.35 /D0.2 = 1.812 ± 0.060 Flat CDM = 1.67 Systematics (damping, BAO fitting) also ~1Next set of measurements will need to worry about this 99.74% detection z~0.2 143k + 465k 79k z~0.35 Percival et al. (2006) Percival et al. 2007

  7. Cosmological Constraints Flatness assumed, constant w With CMB Only D0.35 /D0.2 W 3 1 Favors w<-1 at 1.4 2 m

  8. Cosmological Constraints Flatness assumed m = 0.249 ± 0.018 w = -1.004 ± 0.089 With CMB Only D0.35 /D0.2 W W 3 1 D0.35 /D0.2 = 1.66 ± 0.01 2 m m

  9. Discrepancy! What Discrepancy? • 2.4 difference between SN & BAO. The BAO want more acceleration at z<0.3 than predicted by z>0.3 SNe (revisit with SDSS SNe) • ~1 possible from details of BAO damping - more complex then we thought • Assumption of flatness and constant w needs to be revisited

  10. Dark Energy Survey (DES) • 5000 sq deg multiband (g,r,i,z,Y) survey of SGP using CTIO Blanco with a new wide-field camera • VISTA will image same area in JHK • ~10 sq deg time domain search for SNe • Cluster counts from optical+SPT • Weak lensing maps • SNe Ia distance measurement study from 1400 SNe • Galaxy angular power spectrum for 300 million galaxies Each will independently constrain the dark energy eqn of state <10% DES on-sky in 2011

  11. DES SN Survey SN surveys are systematics limited Provide a large sample of high-redshift SN Ia (redshift > 0.7) with good rest-frame g-band (observer-frame z-band) light curves . Possible with enhanced red sensitivity of DECam. • 750 hrs time • ~10 deg2 • 4 - 6 days in riz • Possible Y • 1400 Ia’s • 0.2 < z < 1

  12. DES SN Survey Spectroscopic Follow-up Focus spectroscopy on 300 Ia’s in elliptical hosts as less dust and no SNII Target high-z clusters Monte Carlos simulations underway Sullivan et al. (2003)

  13. DES Forecasts Forecasts DETF FoM • Nearly factor of 5 improvement in FoM (Stage III) • These predictions include systematic errors as well

  14. Proposed MOS on Subaru via an international collaboration of Gemini and Japanese astronomers 1.5deg FOV with 4500 fibres feeding 10 low-res spectrographs and 1 high-res spectrograph ~20000 spectra a night (2dfGRS at z~1 in 10 nights) >105 redshifts for photo-z’s (Peacock et al. report) DE science, Galactic archeology, galaxy formation studies and lots of ancillary science from database Design studies underway; on-sky by 2013 Next Generation VLT instruments; meetings in Marseilles & Garching WFMOS

  15. Parkinson et al. (2007) Emission-line galaxies 5600 deg2 at z=1.1 (dz = 0.3) > 5 million galaxies 150 deg2 at z=3.15 (dz = 0.2) FoM an order of magnitude larger than SDSS Optimum is broadly peaked and insensitive to other surveys Now investigating curvature and other w(z) models (Clarkson et al. 2007) WFMOS Surveys Optimize instrument parameters

  16. 99.74% detection z~0.2 143k + 465k 79k z~0.35 Percival et al. (2006) Percival et al. 2007 Future BAO w=-1 WFMOS 2009 now 2011 +VISTA

  17. SDSS BAO measures are delivering sub 10% measurements of cosmological parameters 2 discrepancy with SNe? Curvature / w(z)? WFMOS and AS2 will move BAO to 1% level Conclusions

More Related