1. The Carnegie Supernova Project Wendy Freedman Carnegie Observatories Cosmology 2007 San Servolo, Italy August 30, 2007

2. State of the Art (2007): Type Ia Supernovae Riess et al. 2004 HST ACS data Knop et al. 2003Astier et al. 2006 Wood-Vasey et al. 2007WLF et al. 2007

3. Carnegie Supernova Project: Primary Goals 1.Reduce systematics (reddening, calibration, K-corrections…) 2.I-band restframe Hubble diagram => observations in the near-IR (>1  m) “Y”, J bands (To date only UBV restframe…)

4. Carnegie Supernova Project Swope 1-meterMagellan 6.5-meterDupont 2.5-meter Low z:High z: u’BVg’r’i’YJHK photometry 2.5-meter spectroscopy YJ photometry Magellan 6.5-meter C40 9 month campaigns over 5 years (1350 nights) densely sampled photometry and spectroscopy 0 < z < 0.1 100 SNe Ia, 100 SNe II ~100 SNe Ia at completion observations near max 0.2 < z < 0.8

5. Carnegie Supernova Project (CSP) Chris Burns Carlos Contreras Gaston Folatelli Wendy Freedman (PI, High z) Mario Hamuy Barry Madore Nidia Morell Eric Persson Mark Phillips (PI, Low z) Miguel Roth Nick Suntzeff Pamela Wyatt Collaborators: Ray Carlberg, Chris Pritchet, Mark Sullivan, Kathy Perrett, Andy Howell (CFHT SN Legacy) Alex Filippenko, Weidong Li (LOSS) Nick Suntzeff (ESSENCE) Josh Friemann, Masao Sato (SDSS-II) Dan Kelson, Eric Hsiao http://www.ociw.edu/csp/

6. CFHT Legacy Survey ESSENCE CSP Collaborations LOTOSS (KAIT) SN Factory High z: Low z: Intermediate z: SDSS-II CSP followup and collaboration

7. Carnegie Supernova Project: Systematics Nugent et al (2002) 1.Galactic reddening 2.Host reddening 3.Supernova Dust 1.Reddening 2.K-corrections 3.Environment 4.Calibration ** Minimize effects due to: Overview: WLF 2005, astro-ph/0411176

8. 1. Galactic Extinction Law Cardelli, Clayton and Mathis 1989 A B / E(B-V) = 4.1 A I / E(B-V) = 1.7 B I V R V = A V / E(B-V) A U / E(B-V) = 4.9 U

9. 2. Improved K-corrections Eric Hsiao Univ. Victoria astro-ph 0703529 Thesis: Improvement to Standard (Nugent) K-corrections New spectra, at many epochs and including i-band coverage (including CSP low-z data). CSP { Ca triplet

10. CSP Low z Targets Low z supernovae

11. Examples of CSP Low-z Light Curves

12. SN 2006X NGC 4321 (M100) Type Ia Spectra from du Pont and Magellan / LDSS2 Carnegie Supernova Project Nidia Morell SN2006X

13. d149wcc4_11 (ESSENCE) z ~ 0.3 c040117-14 (CFHT Legacy) z ~ 0.6 Magellan High-z IR Observations: Two Examples TargetTemplateDifference

14. Carnegie Supernova Project: High z SNLS SDSS-II ESSENCE Redshift z 58 SN Ia as of 3/07 41 with templates  16 with complete reductions, reddenings Number

15. Carnegie Supernova Project: High z Redshift i’-band light curves: low z High z: Observe pre- maximum Follow 3-7 epochs  Less than 10 days after maximum Gaps less than 5 days 1 st peak 2 nd peak

16. Carnegie Supernova Project: High z z = 0.59 z = 0.43z = 0.52 z = 0.62 ri: SNLS YJ: Magellan z = 0.32 gri : SDSS-II Y: Magellan.. J Y i r Y i r g C. Burns

17. Carnegie Supernova Project: High z YJ Use optical data to determine decline rates (  m15(B) ). Use both optical and near-IR data to solve for reddening. Use YJ light curves to solve for the distance modulus. Template light curves from Prieto et al. (2006) nearby sample.

18. Carnegie Supernova Project: High z Redshift *PRELIMINARY* 16 Type Ia supernovae First I-band Hubble diagram at z > 0.07 Magellan Riess et al. gold Astier et al. small scatter at I better than current low-z sample

19. Carnegie Supernova Project: Fisher-Matrix Constraints on w o and   Current CSP (50 SN Ia) 100 SN Ia 150 SN Ia Stage I SNLS (71 SN Ia) Astier et al (2006) Chris Burns WMAP plus H 0 Key Project priors 95% confidence contours CSP Allows for k-correction and color errors**

20. Carnegie Supernova Project: Fisher-Matrix Constraints on w o and   Current CSP (50 SN Ia) 100 SN Ia 150 SN Ia Stage II SNLS (700 SN Ia) Chris Burns WMAP plus H 0 Key Project priors 95% confidence contours

21. Carnegie Supernova Project: High z Assumption: flat universe *PRELIMINARY* maximum likelihood CSP+BAO:  M = 0.3 ± 0.1 w = -0.9 ± 0.2 95% confidence W = P / 

22. SNe Ia & The GMT 0.5  seeing HST 1.5  m GMT AO SNe studies are limited by confusion GMT AO will address this GMT Science Working Group --P. McCarthy

23. The Giant Magellan Telescope (GMT) Alt-az structure Seven 8.4-m primary mirrors Cast borosilicate honeycomb 25.3-m enclosed diameter 24.5-m diffraction equivalent 21.5-m equivalent aperture 3.2-m adaptive Gregorian secondary mirror

24. GMT Institutions Australia Carnegie Observatories Harvard University Smithsonian Astrophysical Observatory Texas A&M University University of Arizona University of Michigan University of Texas, Austin + …OTHERS TBD

25. Summary  First restframe I-band Hubble diagram for 0.2 < z < 0.7  Dispersion lower than for UBV  Lower sensitivity to reddening  Improved K-corrections  Preliminary Results: w = -0.9 § 0.2 (95% confidence)  Final sample 4-5 times greater Low redshift : tests of systematics High redshift: I-band Hubble diagram “Local” calibration for JDEM