The Carnegie Supernova Program Zwicky Symposium Saturday, January 17, 2004 Carnegie Observatories

Type Ia Supernovae for Cosmology Advantages: small dispersion single objects (simpler than galaxies) can be observed over wide z range Challenges: dust (grey dust) chemical composition evolution photometric calibration environmental differences

Carnegie Supernova Project Infrared observations of Type Ia & II supernovae High and low z (0 < z < 0.8) : improved constraints on w I-band Hubble diagram Gaston Folatelli Wendy Freedman Mario Hamuy Barry Madore Nidia Morell Eric Persson Mark Phillips Nick Suntzeff Pamela Wyatt Ray Carlberg (CFHT Legacy) Alex Filippenko, Weidong Li (KAIT) Nick Suntzeff (ESSENCE) CSP coI’s:

Carnegie Supernova Project Advantages: - dust - chemical composition - low dispersion => reduce systematics Why an I-band Hubble diagram?

Barris et al. (2003) unbinned binned (median)

Overview of Carnegie Supernova Project Swope 1-meter (C40) Low z: u’BVr’i’ CCD photometry YJH IR array RAPID SWITCHING (< 15min) C40 9 month campaigns over 5 years densely sampled (every 2 nd night) photometry SNIa and SNII

Overview of Carnegie Supernova Project Dupont 2.5-meter densely sampled photometry and spectroscopy 0 < z < 0.2 well-determined k-corrections SNIa and SNII u ’ BVr ’ i ’ CCD photometry YJH IR array spectroscopy

Overview of Carnegie Supernova Project Magellan 6.5-meter High z: RIYJ photometry Magellan spectroscopy ~200 nights over 5 years ~200 SNIa 0.2 < z < 0.8

Overview of Carnegie Supernova Project Swope 1-meter (C40)Magellan 6.5-meterDupont 2.5-meter Low z:High z: u’BVr’I’YJH photometry Dupont spectroscopy r’i’YJ photometry Magellan spectroscopy ~200 nights over 5 years ~200 SNIa 0.2 < z < 0.8 C40 9 month campaigns over 5 years densely sampled photometry and spectroscopy 0 < z < 0.2 SNIa and SNII

Goals: minimize systematics accurate reddenings, K-corrections H 0 (H-band observations for Cepheids + SNIa)   peculiar flows physics of SNI and II Carnegie Supernova Project Magellan

~30 observed to date UBVRIJHK light curves excellent sampling Carnegie Supernova Project Krisciunas et al. (2002) SN2001el Nearby supernovae:

decline rate versus magnitude BVIH H-band promising as distance indicator Carnegie Supernova Project Mark Phillips et al.

Carnegie Supernova Project Krisciunas et al. H-band Hubble diagram Log velocity (km/sec) Distance Modulus (mag)

CFHT Legacy Survey : ugriz light curves CFHT MegaCam 2000 SN over 5 years 0.1 < z < 1 Ongoing Supernova Searches ESSENCE : VRI light curves CTIO 4m Mosaic Imager 200 SN over 5 years 0.15 < z < 0.75 LOTOSS (KAIT) : UBVRI light curves Lick 0 < z < ~0.15 High z: Low z: SN Factory: spectophotometry, UH 3200 – A o NEAT, Palomar ***E.g., redshifts posted on web within 2 days!!!!!

CFHT Legacy Survey : Success! CFHT Legacy candidates: September 03 finding ~ 15 SN1a per month generally finding ~ 2 mag before peak collaboration with Carlberg et al. followup SN1a 0.2 < z < 0.8 at RIYJ

CFHT Legacy Survey : Success! CFHT Legacy candidates: September 03 REFERENCEDIFFERENCE Try to catch supernovae on the rise for followup. I AB ~ 22 – 25 mag

 SN Ia spectrum z = 0.54 t = 20 min VLT FORSI Followup Spectroscopy: ESSENCE & CFHTLS VLT Gemini Magellan SNIa e.g.:

PANIC: Magellan 6.5-meter IR Imager PANIC: Eric Persson Antennae 1024 x 1024 array 1 – 2.5 micron imager 2 ’ x 2 ’ FOV “ /pixel

PANIC: Magellan IR Imager 35 nights of Magellan time November 03 through March 04 optical r ’ I ’ imaging near-IR YJ imaging optical spectroscopy

IMACS: Inamori Magellan Areal Camera and Spectrograph installed August, 2003 Followup spectroscopy RI photometry 2 cameras f/4 : 15 ’ FOV f/2 : 30 ’ FOV 8192 x 8192 CCD array Alan Dressler, Bruce Bigelow

Magellan SNIa Observations z ID I-mag Discovery 0.20 e132.wcc1_ Essence 0.30 d149.wcc4_ Essence 0.30 e108.wdd8_ Essence 0.55 c Legacy 0.69 c031217_ Legacy

First Magellan PANIC Images ESSENCE SNIa : z = 0.33 (d149) 36-minute dithered exposures J-bandY-band November 3, 2003

First Magellan PANIC Images CFHT SNIa : z = 0.55 (1022) 36-minute dithered exposures (total exposures 2 hours per filter) J-bandY-band November 3, 2003 Stay tuned …