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SDSS Supernova Survey Josh Frieman Fermilab and University of Chicago
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Jan. 12, 2005 AAS2 SDSS and SDSS II SDSS I: April 2000-June 2005 SDSS II: July 2005-2008 (contingent on funding): Legacy Survey (complete northern survey) ~10 6 redshifts SEGUE (low-latitude survey of Milky Way) see posters 64.09, 114.03, 142.04 Supernova Survey see poster 114.04 by H. Lampeitl and 71.04 by S. Krughoff
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Jan. 12, 2005 AAS3 Fermilab: Jen Adelman-McCarthy, Fritz DeJongh, Juan Estrada, Hubert Lampeitl, John Marriner, Chris Stoughton, Doug Tucker U. Chicago: Ben Dilday, Rick Kessler, Erin Sheldon, Don York, Gary Kilper, Mark Subbarao U. Washington: Andy Becker, Gajus Miknaitis, Craig Hogan Portsmouth: Bob Nichol, Bruce Bassett NMSU/APO: Jon Holtzman, Bill Ketzeback, Jack Dembicky, Russet McMillan, John Barentine, Scot Kleinman, Howard Brewington, Mike Harvanek, Atsuko Nitta, Stephanie Snedden, Dan Long, Jerzy Krzesinski, Peter Newman Princeton: Dave Johnston, Jim Gunn U. Pittsburgh: Andy Connolly, Simon Krughoff, Ryan Scranton JPG: Mamoru Doi, Naoki Yasuda, Naohiro Takanashi Stanford: Roger Romani, Masao Sako, Jared Kaplan, Roger Blandford, Steve Kahn Ohio State: Darren Depoy, Jennifer Marshall STScI: Adam Riess LBNL: Lifan Wang U. Texas: Peter Hoeflich SF State: Dennis Lamenti SDSS SN Collaborators
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DateSDSS Supernovae4 a(t) Expansion History of the Universe
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Jan. 12, 2005 AAS5 Type Ia Supernovae & Cosmology Advantages: small dispersion in peak brightness (standard candles) single objects (simpler than galaxies) can be observed over wide redshift range (bright) Challenges/Systematic concerns: dust extinction in host galaxy chemical composition variations/evolution evolution of progenitor population photometric calibration Malmquist bias environmental differences K correction uncertainties Need new SN surveys for statistics and systematics
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Jan. 12, 2005 AAS6 Tonry etal ‘03 0.3, 0.7 0.3, 0.0 1.0, 0.0 Brightness relative to empty Universe: ( m = =0) m Compiled Supernovae Ia Sample `Gold’ sample of ~150 SNe included only 5 between z = 0.1-0.3; SDSS naturally fills this gap
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Jan. 12, 2005 AAS7 The SDSS SN Program Repeat ugriz imaging of ~2.5 o x100 o deg. region along celestial equator for three 3-month runs (Sept-Nov. ‘05-’07): 310<RA<50 Frame subtraction in SDSS gri SN Ia selection in 24 hrs Follow-up spectroscopy for SN typing, redshift (other telescopes) Multi-epoch spectrophotometry for improved K-corrections Follow-up NIR imaging for host extinction & properties Obtain ~200 high-quality, densely sampled SN Ia light-curves in the redshift desert z = 0.05 – 0.35 (exposure time 55 sec on 2.5m telescope; limits g~r~22.2 in `good’ seeing) 5-band photometry, large survey volume also allow selection of unusual type II, Ibc, etc., for further study Rapid release of candidates and data
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Jan. 12, 2005 AAS8 Science Goals Probe Dark Energy in z regime less sensitive to evolution than deeper surveys Study SN Ia systematics (critical for SN cosmology) with high photometric accuracy Search for additional parameters to reduce Ia dispersion Determine SN/SF rates/properties vs. z, environment Rest-frame u-band templates for z >1 surveys Study feasibility of cosmology with SN colors Database of Type II and other SN light-curves
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Jan. 12, 2005 AAS9 Monte Carlo Data Distance modulus Simulated redshift distribution and photometric errors for completed SDSS SN sample (here assumed =0.7=1– m H 0 =72)
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Jan. 12, 2005 AAS10 Fall 2004: Early Science & Test Run Imaging: 20 nights of SDSS 2.5m scheduled every other night late Sept.-mid Nov., covered half the survey area: ~1/2 the nights were useable. Follow-up spectroscopy: ARC 3.5m, HET 9.2m Follow-up imaging (during/after run): NMSU 1m, ARC 3.5m Science Goal: ~10 well-measured SN Ia light-curves with confirmed spectroscopic types and redshifts. Yield: 16 confirmed Ia’s: 0.05<z<0.32 with z = 0.15, 5 Type II, 1 luminous Type Ic Engineering goals met: Rapid processing and selection of candidates in g,r (48 hours) Coordinated follow-up observations Study detection efficiency and photometric accuracy under varying conditions
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Jan. 12, 2005 AAS11 SN Ia z=0.0513 3 epochs of spectroscopy
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Jan. 12, 2005 AAS12 Preliminary u+0.25 g r–0.75 i–2 z–3.25 13 14 15 16 17 18 19 20 21 Magnitude
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Jan. 12, 2005 AAS13 SN 83: Observed vs. Synthetic Light-curves (preliminary)
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Jan. 12, 2005 AAS14 Highest redshift Ia from this sample: z=0.32 Luminous Ia: M r ~ –20 Cross-correlation analysis yields best-fit Ia spectral templates separated by 2 days, in excellent agreement with data
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Jan. 12, 2005 AAS15 Type II Type Ic
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Jan. 12, 2005 AAS16 SDSS II SN Follow-up Spectroscopy: SN typing, redshift, multi-epoch spectrophotometry NIR imaging: extinction/reddening and lightcurves Spectroscopy: ARC 3.5m, HET, MDM 2.4m (new high-throughput spectrograph), Subaru, SALT?, Gemini? NIR imaging: Liverpool Telescope, Carnegie Supernova Project, Calar Alto Optical imaging: NMSU 1m, ARC 3.5m, …
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Jan. 12, 2005 AAS17 Conclusions SDSS SN Survey: SDSS 2.5m, ~200 SNe, z = 0.05-0.35, Sept-Nov. 2005-7, fill in the redshift desert Successful early science and test run Fall 2004: results out soon In combination with WMAP CMB data, the SDSS SN survey should determine the Dark Energy equation of state parameter w to ~10-15% statistical accuracy (assuming w constant) and provide new insight into SN Ia systematics. Combining SDSS SN data with that of deeper on-going surveys (ESSENCE, CFHTLS, z=0.3-0.8) should lead to improved cosmological constraints, due to broader redshift leverage.
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