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The Carnegie Supernova Program

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)

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The Carnegie Supernova Program

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

  2. 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

  3. 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 CSP coI’s: 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)

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

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

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

  7. Overview of Carnegie Supernova Project Dupont 2.5-meter • u’BVr’i’CCDphotometry • YJHIR array • spectroscopy • densely sampled photometry • and spectroscopy 0 < z < 0.2 • well-determined k-corrections • SNIa and SNII

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

  9. Overview of Carnegie Supernova Project Swope 1-meter (C40) Dupont 2.5-meter Magellan 6.5-meter Low z: High z: • u’BVr’I’YJHphotometry • 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

  10. Carnegie Supernova Project • Goals: • minimize systematics • accurate reddenings, • K-corrections • H0 (H-band observations • for Cepheids + SNIa) • WL • peculiar flows • physics of SNI and II Magellan

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

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

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

  14. Ongoing Supernova Searches High z: Low z: • CFHT Legacy Survey : • ugriz light curves • CFHT MegaCam • 2000 SN over 5 years • 0.1 < z < 1 • LOTOSS (KAIT) : • UBVRIlight curves • Lick • 0 < z < ~0.15 • ESSENCE : • VRIlight curves • CTIO 4m Mosaic Imager • 200 SN over 5 years • 0.15 < z < 0.75 • SN Factory: • spectophotometry, UH • 3200 – 10000 Ao • NEAT, Palomar • ***E.g., redshifts posted on web within 2 days!!!!!

  15. 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

  16. CFHT Legacy Survey : Success! CFHT Legacy candidates: September 03 REFERENCE DIFFERENCE • Try to catch supernovae on • the rise for followup. • IAB ~ 22 – 25 mag

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

  18. PANIC: Magellan 6.5-meter IR Imager Antennae • 1024 x 1024 array • 1 – 2.5 micron imager • 2’ x 2’ FOV • 0.125 “/pixel PANIC: Eric Persson

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

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

  21. Magellan SNIa Observations z ID I-mag Discovery 0.20 e132.wcc1_7 21.3 Essence 0.30 d149.wcc4_11 19.5 Essence 0.30 e108.wdd8_4 21.8 Essence 0.55 c031022-02 23.0 Legacy 0.69 c031217_23 23.9 Legacy

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

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

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