1. The Carnegie Supernova Program (CSP)

2. People and Institutions People: R. Carlberg, A. Filippenko, G. Folatelli, W. Freedman, S. Gonzalez, M. Hamuy, W. Krzeminski, W. Li, J. Maza, N. Morrell, D. Murphy, M. Phillips, G. Oemler, E. Persson, P. Pinto, M. Roth, S. Shectman, N. Suntzeff Institutions: Carnegie/Las Campanas Observatories Cerro Tololo Inter-American Observatory University of California at Berkeley University of Chile The University of Arizona

3. Goals During the next 5 years we want to obtain high-quality gap- free optical/NIR light-curves and spectro-photometry of: >100 nearby (z<0.07) Type Ia supernovae >100 nearby (z<0.05) Type II supernovae >20 nearby (z<0.05) Type Ibc supernovae with the purpose to: Establish and refine methods for obtaining distances (study of local galaxy flows, a reddening-free determination of the Hubble constant, provide a fundamental reference for observations of high-z supernovae to solve for w, w’?) Gain insight into the progenitors and explosion mechanisms of supernovae

4. Resources Carnegie telescopes (1-m, 2.5-m, Magellan 6.5-m) and instruments (cameras and spectrographs) will permit us to use > 300 nights/year NSF grant (2004-2006) will allow us to hire personnel (2 observers and 1 post-doc) STScI and Carnegie provide one post-doc fellow (2004- 2006)

5. Implementation (Search) LOTOSS (Lick Observatory) KAIT 0.8-m telescope ~ 60 SNe/year south of δ=+20 degrees z<0.05 OGLE III (Las Campanas) Warsaw 1.3-m telescope several SNe/year near the LMC and SMC z < 0.1

6. Implementation (Follow-up) Optical (u’BVg’r’i’) Photometry: Las Campanas Swope 1-m telescope + CCD (151 nights) Infrared (YJsHKs) Photometry: Las Campanas Swope 1-m telescope + RetroCam (YJsH) (151 nights) Las Campanas du Pont 2.5-m telescope + WIRC (YJsHKs) (34 nights) Optical (0.32-1.0 μm) Spectroscopy: Las Campanas du Pont 2.5-m telescope + WFCCD (or Modspec) (15 nights) Magellan + LDSS2 (or B&C and IMACS) NEED TELESCOPE PROPOSAL One 9-month campaign per year Swope 1-mDu Pont 2.5-mMagellan 6.5-m

7. Implementation: RetroCam (E. Persson, D. Murphy) Machining: 99% done Array: fine Electronics and data system: done C40 Mountain base has been modified and a swivel mechanism has been added SLOAN filters have arrived and filter holders have been built Control software is far advanced C40 secondary was coated at Livermore Commissioning starts March 27 Science observations start April 1 or so.

8. Implementation (Computers) 2 Linux PCs at El Pino + 2 PCs for the C40 (1 linux + 1 windows) + 1 linux PC for the mountain (hot spare that needs a home). csp1: 2.3 GHz processor + 1 Gb RAM, dual 250 Gb data disk (permits nightly incremental backup) + DVD drive csp2: 2.3 GHz processor + 1 Gb RAM, dual 160 Gb data disk (permits nightly incremental backup) + DVD drive 500 DVS + jewel boxes User account: cspuser1 (username) + csp_pass (password) Web site is (will be): http://csp1.lco.cl/~cspuser1 SN list + finding charts Observers schedule (Sergio) Observing procedures Observing Program Observing logs IAUCs database: csp1 will host the database with all optical + IR direct images (one subdirectory/SN) and all spectra

9. Operation Selection of targets: web site administrator must make list of SNe with finding charts and prepare observing plan for the night (need administrator) Observations: Observers must use list of SNe and priorities, execute the program accordingly, and save raw data in a DVD (need to fill out observer’s schedule: Sergio, Wojtek, et al.) Data Reductions: Need to be done during the day following the night and the reduced data must be immediately incorporated into the database (otherwise we will die)  Need to get organized

10. Proposed Organization Scheme for Data Reductions Optical Photometry (head: Mario; backup: ???) Ftp data to csp1 Process data through [OTZF] (pipeline? yes) Spread processed data in database (pipeline? yes) Photometric calibration (pipeline? yes) Quick-look photometry (pipeline? yes) Update web site (observing logs) Infrared Photometry (head: Gaston; backup: ???) Ftp data to csp1 Process data through [OTZF] (pipeline? no) Spread processed data in database (pipeline? yes) Photometric calibration (pipeline? yes) Quick-look photometry (pipeline? yes) Update web site (observing logs) Optical Spectroscopy (head: Nidia; backup: ???) Ftp data to csp1 Process data through [OTZF] (pipeline? almost) Extract 1-D spectra, wavelength and flux calibration (pipeline? no) Spread processed data in database (pipeline? no) Update web site (observing logs)

11. Why Type Ia supernovae? Distances derived from Type Ia supernovae light curves play a central role in the determination of cosmological parameters, but these measurements could be biased due to systematic errors: Photometric errors (S-corrections) Reddening corrections Evolutionary effects (age, metallicity) Need to address these issues Which are the progenitors? What causes the diversity? Cosmology Nature

12. Why Type II supernovae? Type II plateau supernovae can be used in the determination of extra-galactic distances, thus offering an independent route to cosmological parameters via: Standardized Candle Method (SCM) σ=15% Expanding Photosphere Method (EPM) σ=20-25% Spectral Expanding Atmosphere Method (SEAM) Light-curves and spectra provide constraints on physical parameters of the progenitor (mass, initial radius) and the explosion (energy, nucleo-synthesis) What causes the photometric and spectroscopic diversity? Cosmology Nature

13. Why Type Ibc supernovae? Probably not There are only a handful of Type Ibc supernovae with good light-curves and spectroscopic follow-up What causes the photometric and spectroscopic diversity? Is there He in Type Ic supernovae? Is there H in Type Ib supernovae? Cosmology Nature