The Carnegie Supernova Program (CSP). People and Institutions People: R. Carlberg, A. Filippenko, G....
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Transcript of The Carnegie Supernova Program (CSP). People and Institutions People: R. Carlberg, A. Filippenko, G....
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The Carnegie Supernova Program (CSP)
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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
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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
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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)
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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
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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-m Du Pont 2.5-m Magellan 6.5-m
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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.
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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
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OperationSelection 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
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Proposed Organization Scheme for Data Reductions
Optical Photometry (head: Mario; backup: ???)
Ftp data to csp1Process 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 csp1Process 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 csp1Process 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)
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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
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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
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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