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The Carnegie Supernova Project Wendy Freedman Carnegie Observatories Cosmology 2007 San Servolo, Italy August 30, 2007 State of the Art (2007): Type Ia Supernovae HST ACS data Knop et al. 2003 Riess et al. 2004 Wood-Vasey et al. 2007 Astier et al. 2006 WLF et al. 2007 Carnegie Supernova Project: Primary Goals 1. Reduce systematics (reddening, calibration, K-corrections…) 2. I-band restframe Hubble diagram => observations in the near-IR (>1m) “Y” , J bands (To date only UBV restframe…) Carnegie Supernova Project Swope 1-meter Low z: Dupont 2.5-meter •u’BVg’r’i’YJHK photometry • 2.5-meter • C40 9 month spectroscopy campaigns over 5 years (1350 nights) • densely sampled photometry and spectroscopy 0 < z < 0.1 • 100 SNe Ia, 100 SNe II Magellan 6.5-meter High z: • YJ photometry • Magellan 6.5-meter • ~100 SNe Ia at completion • observations near max • 0.2 < z < 0.8 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 http://www.ociw.edu/csp/ 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 CSP Collaborations High z: • CFHT Legacy Survey • ESSENCE Low z: • LOTOSS (KAIT) • SN Factory Intermediate z: • SDSS-II CSP followup and collaboration Carnegie Supernova Project: Systematics Minimize effects due to: 1. 2. 3. 4. Reddening K-corrections Environment Calibration** Overview: WLF 2005, astro-ph/0411176 1. Galactic reddening 2. Host reddening 3. Supernova Dust Nugent et al (2002) 1. Galactic Extinction Law U B AU / E(B-V) = 4.9 AB / E(B-V) = 4.1 V I AI / E(B-V) = 1.7 R V = AV / E(B-V) Cardelli, Clayton and Mathis 1989 2. Improved K-corrections Eric Hsiao Univ. Victoria astro-ph 0703529 CSP { Ca triplet Thesis: Improvement to Standard (Nugent) K-corrections New spectra, at many epochs and including i-band coverage (including CSP low-z data). CSP Low z Targets Low z supernovae Examples of CSP Low-z Light Curves Carnegie Supernova Project • SN 2006X • NGC 4321 (M100) • Type Ia • Spectra from du Pont and Magellan / LDSS2 SN2006X Nidia Morell Magellan High-z IR Observations: Two Examples d149wcc4_11 (ESSENCE) z ~ 0.3 c040117-14 (CFHT Legacy) z ~ 0.6 Target Template Difference Carnegie Supernova Project: High z SNLS SDSS-II ESSENCE • 58 SN Ia as of 3/07 Number • 41 with templates Redshift z 16 with complete reductions, reddenings Carnegie Supernova Project: High z i’-band light curves: low z High z: 1st peak 2nd peak • Observe premaximum • Follow 3-7 epochs Less than 10 days after maximum • Gaps less than 5 days Redshift Carnegie Supernova Project: High z J z =Y0.59 i r z = 0.62 z = 0.32 . gri : SDSS-II Y: Magellan Y z = 0.52 z = 0.62 i ri: SNLS YJ: Magellan g z = 0.43 . r C. Burns Carnegie Supernova Project: High z Y J • 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 Carnegie Supernova Project: High z *PRELIMINARY* 16 Type Ia supernovae Riess et al. gold Astier et al. Magellan First I-band Hubble diagram at z > 0.07 • small scatter at I • better than current low-z sample Redshift Carnegie Supernova Project: Fisher-Matrix Constraints on wo and Current CSP (50 SN Ia) 100 SN Ia 150 SN Ia Chris Burns WMAP plus H0 Key Project priors 95% confidence contours CSP Allows for k-correction and color errors** Stage I SNLS (71 SN Ia) Astier et al (2006) Carnegie Supernova Project: Fisher-Matrix Constraints on wo and Current CSP (50 SN Ia) 100 SN Ia 150 SN Ia Chris Burns WMAP plus H0 Key Project priors 95% confidence contours Stage II SNLS (700 SN Ia) Carnegie Supernova Project: High z *PRELIMINARY* maximum likelihood CSP+BAO: M = 0.3 ± 0.1 w = -0.9 ± 0.2 95% confidence Assumption: • flat universe W=P/ SNe Ia & The GMT SNe studies are limited by confusion 0.5 seeing HST 1.5m GMT AO GMT AO will address this GMT Science Working Group --P. McCarthy 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 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 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