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Supernova Cosmology Program

Supernova Cosmology Program. Saul Perlmutter Mar 2, 2006. Expansion History of Leonard Parker. SN factory. SNLS. HST Cluster SN. SNAP. Baryon Osc. SCP Staff. Current Collaborators Stockholm ESO/Chile IN2P3/Paris Tokyo STScI Toronto Vanderbilt JPL Chicago Michigan.

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Supernova Cosmology Program

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  1. Supernova Cosmology Program Saul Perlmutter Mar 2, 2006

  2. Expansion History of Leonard Parker SN factory SNLS HST Cluster SN SNAP Baryon Osc.

  3. SCP Staff • Current Collaborators • Stockholm • ESO/Chile • IN2P3/Paris • Tokyo • STScI • Toronto • Vanderbilt • JPL • Chicago • Michigan

  4. CMAGIC intrinsic dispersion & CMAGIC in other colors Wang, Strovink, Goldhaber, Siegrist, Perlmutter, Conley

  5. Apply CMAGIC to high redshift SNe • Alternative method provides systematic cross check of previous results • SCP + literature SNe • 21 high z, 31 low z • Cosmology fit done as “blind”analysis - conceal final results while developing analysis A. Conley, PhD thesis. March 2005

  6. Cosmological Parameters A. Conley, PhD thesis. March 2005 ApJ submitted

  7. SuperNova Legacy Survey at CFHT First-year results: Astier et al., A&A 447, 31 (2006) 71 SNe Ia

  8. SuperNova Legacy Survey at CFHT • Started March '03. • 40 (d) nights/year for 5 years • 4 square degrees : u’, g’, r’, i’, z’ • g’,r’,i’,z’ every 2-3 nights for 10 months/yr • 15’, 30’, 1h, 30’ • Detection up to z = 1.2 -1.3 • Multicolor LC follow- up up to z=0.9 • 2000 SN Ia + 2000 SN II ? + AGNs ? + .. • 600 well measured SNIa 0.3<z<0.9

  9. SuperNova Legacy Survey at CFHT

  10. SNe Ia Spectra from Keck Data from LBL group: Kowalski Schlegel Perlmutter Aldering Spectra of some of the SNLS SN candidates obtained during the 2005A Keck LRIS observing campaign. The light-blue lines show the data after host galaxy subtraction (if necessary),rebinned to 10Å. Overplotted in black are the best fit SN templates. The spectra are confirmed by Keck to be Type Ia SNe.

  11. First-year results from SNLS The Supernova Legacy Survey: Measurement of WM, WLand w from the First Year Data Set P. Astier, et al., astro-ph/0510447 71 high redshift type Ia supernovae Hubble diagram of SNLS and nearby SNe Ia, with variouscosmologies superimposed. The bottom plot shows theresiduals for the best fit to a flat cosmology.

  12. First-year results from SNLS Contours at 68.3%, 95.5% and 99.7% confidence levels for the fit to a flat (WM, w) cosmology, from the SNLS Hubble diagram alone, from the SDSS baryon acoustic oscillations alone (Eisenstein et al. 2005), and the joint confidence contours. Contours at 68.3%, 95.5% and 99.7% confidence levels for the fit to an (WM, WL ) cosmology from the SNLS Hubble diagram(solid contours), the SDSS baryon acoustic oscillations(Eisenstein et al. 2005, dotted lines), and the joint confidence contours (dashed lines).

  13. Edge-on Galaxy Dust

  14. Knop et al Lightcurves Knop et al (ApJ, 2003)

  15. Knop: before/after extinction correction Before Extinction Correction After Extinction Correction

  16. Sullivan, et al. (2003)

  17. Decelerating and Dustfree: Targeting SNe in Very High Redshift Galaxy Clusters • Major 219-orbit year-long HST Program in progress in collaboration with several galaxy cluster groups • searching ~ 24 massive galaxy clusters at z > 1 with ACS • Why clusters? • Dominated by nearly dust-free early type galaxies. • 5 times higher density of early type galaxies • SNe in these galaxies have negligible dust extinction • Our Program • image clusters with cadence ~ 20-23 day in z’, i’ bands • follow SNe with NICMOS (J band) • spectroscopy: 20 half-nights on Subaru, ~ 4 nights on Keck • Scientific goals • Significantly improve SN constraints of dark energy - statistical and systematic uncertainties • Cluster studies: weak lensing, galaxy morphology, and color-magnitude relationship.

  18. SCP Recent Accomplishments: HST New large (219-orbit) HST progam underway: A SN search targeting dustfree elliptical galaxiesin high redshift clusters Cycle 14 observations began July 2005

  19. SNe in Very High Redshift Galaxy Clusters Left Panel: Simulated 68% confidence region on w' vs. w0 for the current literature SN sample but with underlying cosmology(w0 = -1; w’ = 0). The parameters are poorly constrained because color errors are magnified by RB ~ 4. Middle Panel: The solid red contour shows reduced uncertainties (excluding systematic bias) using a Bayesian prior on the extinction distribution prior to suppress color errors.The filled gray contour is from Riess et al. 2004 using this prior. The short-dashed contour shows that this approach is also sensitive to shifts in RB with redshift; the example shifts from 4.1to 2.6. Right Panel: The goal of this project is shown as a confidence region for a simulated new sample of 10 z > 1 SNe Ia found in cluster ellipticals, together with 5 in ellipticals from the past and ongoing GOODS searches, as well as 120 SNe Ia in ellipticals at the lower redshifts now being produced by the ground-based CFHT SN Legacy Survey, the CTIO Essence survey, and (at z < 0.1) the Nearby SN Factory

  20. First SN discovered in a cluster in this search preliminary Cluster RCS0221-03 at z = 1.02

  21. SNe discovered in ongoing search z=1.316 preliminary z=0.926 preliminary

  22. SLIDE WITH SUMMARY OF CLUSTER SEARCH TO DATE - FROM TWIKI PAGE: Current Cluster Rate Summary We have 9 SNe to date (15 Feb 2006) * 3 field z<1, hosted by spiral galaxies o N-010, z=0.203: Caught on the way down, can be any type o Lauren, z=0.821: redshift from host o Gabe, z=0.92: redshift from nebulous host, only have z band data * 2 z>~1, hosted by cluster ellipticals o Frida, z=1.01: spectroscopically confirmed o K-000, z=1.41?: no redshift, but host is likely cluster member, low stretch, low peak mag? * 1 z>1, hosted by cluster spiral o Midge, z=0.98: spectroscopically confirmed (thought host was @1.09 though) * 2 z>1, hosted by background elliptical o Maggie, z=1.31: Redshift from host o C-000, z=1.09: Redshift from host, low stretch, little low peak mag, z=1.09 may be in background cluster??? * 1 possible z>1.5 SN (X-018) seen only in one epoch (#5) New Candidates: * F-003: host is early type galaxy with photo z >1, low SNR possible SN detection in discovery epoch * F-004: host is early type galaxy with photo z >1, low SNR possible SN detection in discovery epoch * T-000: Bright 23mag on core, host appears to be low redshift E * E-003: on core of likely cluster elliptical, z=1.03 * C-007: Good candidate, off-core in foreground spiral

  23. Placing SNe on Hubble Diagram preliminary These SNe are found in ellipticalgalaxies - no extinction correction

  24. Polarization versus lightcurve timescale Wang, et al. submitted slow fast

  25. SCP 1999 Low-z SN campaign • Lightcurves - Cross calibration of multiple telescopes • 20 nearby SN observed (0.02 < z < 0.24) • ~2600 images in UBVRI • 17 different instruments • M. Kowalski, B. Farris SN 1999ac SN 1999ao SN 1999bp SN 1999aa SN 1999aw

  26. Spectra of High Redshift Type Ia Supernovae and a Comparison with their Low Redshift Counterparts I. Hook et al., AJ in press, astro-ph/0509041 The time sequence of high redshift SN spectra in order of rest-frame date relative to maximum light as determined from the light curve. Spectra of the nearby Type Ia, SN 1992A are interspersed for comparison. We find no evidence for evolution in SN Ia properties between low and high redshift samples.

  27. Detailed spectroscopic studies of 2 SNe • Spectroscopic Observations and Analysis of the Unusual Type Ia SN 1999ac, • G. Garavini et al., AJ in press. astro-ph/0507288 SN 1999aa • Spectroscopic Observations and Analysis of the Peculiar SN 1999aa, • G. Garavini et al., AJ 128, 387 High S/N spectra allow for identification and temporal evolution of intermediate mass elements SN 1999ac Synthetic spectrum (SYNOW) compared with SN 1999ac spectrum for day -15

  28. SCP SN studies using Subaru 8.2m • Intensive SN search with Subaru/ Suprime-Cam in 2002 • 5 nights in Spring/11 nights in Fall • coordinated spectroscopy with Keck, Gemini, and VLT • Widest field imaging camera on an 8-10m class telescope • FOV of 33 x 26 arcmin. Spectroscopy Obtained Un-typed SNe SNe Ia S. Perlmutter, G. Goldaber, K. Dawson, V. Fadeyev, D.Schlegel, A. Spadafora, Tokyo group

  29. Adding SNe to Hubble diagram at the highest redshifts SCP Subaru data will provide a significant SN sample at z > 1.

  30. Recent SCP Accomplishments: high z Narrowing in Cosmological parameters: New Constraints from HST-observed SNe SNe in elliptical galaxies - study effect of dust Spectroscopy of high redshift SNe: Published large data set in 2 papers Important data sets completed, analysis in progress: SN “Albinoni” from Keck/HST (z = 1.2) ~40 SNe from Subaru/HST (0.8 < z < 1.5) 2 SNe discovered with HST (z ~ 1.6)

  31. Recent SCP Accomplishments: low z SCP Low-z campaign Detailed Analysis of spectra of 2 SNe published Lightcurves obtained from cross-calibrating telescopes used in extensive observing campaign Other studies of systematics First Restframe I-band Hubble diagram submitted for publication CMAGIC: new analysis approach developed with low-z SNe, applied to a set of high-z SNe for cosmology

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