1 SDSS Supernova Survey Josh Frieman Supernova Rates 2008, Florence May 19, 2008.
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Transcript of 1 SDSS Supernova Survey Josh Frieman Supernova Rates 2008, Florence May 19, 2008.
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SDSS Supernova Survey
Josh FriemanSupernova Rates 2008, Florence
May 19, 2008
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Dark Energy and Dark Matter
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SDSS II Supernova Survey Goals• Obtain few hundred high-quality SNe Ia light curves in the `redshift
desert’ z~0.05-0.35 for continuous Hubble diagram• Detailed spectroscopic follow-up, including some with multiple
epochs, to study evolution and diversity of SN features• Probe Dark Energy in z regime complementary to other surveys• Well-observed sample to anchor Hubble diagram & train light-curve
fitters • Rolling search: determine SN/SF rates/properties vs. z, environment• Rest-frame u-band templates for z >1 surveys • Large survey volume: rare & peculiar SNe, probe outliers of
population• Enable time-domain science both in real time* & after the fact** *candidates immediately on the web+IAU circulars+VOEventNet **SN images & object catalogs all available publicly w/in ~2 months
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Spectroscopic follow-up telescopes
R. Miquel, M. Molla
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SDSS 2.5 meter telescope SDSS-I: 2000-5Apache Point Observatory SDSS-II: 2005-8New Mexico
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<#>
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Stripe 82
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Frieman, et al (2008); Sako, et al (2008)
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Search Template Difference
g
r
i
Searching For Supernovae
• 2005– 190,020 objects
scanned
– 11,385 unique candidates
– 130 confirmed Ia
• 2006– 14,441 objects
scanned
– 3,694 unique candidates
– 193 confirmed Ia
• 2007 – 171 confirmed Ia
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Spectroscopic Target Selection2 Epochs
SN Ia Fit
SN Ibc Fit
SN II Fit
31 Epochs
SN Ia Fit
SN Ibc Fit
SN II Fit
Fit with template library
Classification>90%accurate after 2-3 epochs
Redshifts 5-10% accurate
Sako etal 2008
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SN 2005 gb
z = 0.086, confirmed at ARC 3.5mPreliminary gri light curve and fit from low-z templates
Before After
Composite gri
images
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SN and Host Spectroscopy
MDM 2.4m
NOT 2.6m
APO 3.5m
NTT 3.6m
KPNO 4m
WHT 4.2m
Subaru 8.2m
HET 9.2m
Keck 10m
Magellan 6m
TNG
SALT 10m
2005+2006
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Spectroscopic Follow-up
•1325 spectra taken over 3 seasons•Multi-epoch spectroscopy of selected low-redshift SNe
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Spectroscopic Deconstruction
SN modelHost galaxy modelCombined model
Zheng, et al (2008)
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Rolling survey leads to well-sampled*, well-constrained light curves
peaked after Sept. 7 peaked before Sept. 7
r=22.5*9 epochs of imaging per SN (median)
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SDSS low-redshiftlight curvesfrom 2005 well-sampled, multi-band (u,z not shown)
Will use to trainLC fitters & anchor HubbleDiagram
2005-07:83 confirmedSNe Ia at z<0.12
gri
Dilday et al (2007) submitted
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SDSS SN Photometry: Holtzman et al. (2007) submitted ``Scene modeling”
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B.
Dild
ay
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Redshift Distribution for SNe Ia
and counting
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Peculiar SNe from SDSS
2005gj: SN Ia in dense circumstellar environment or SN IIn; more luminous than any normal Ia; Prieto et al (2007)
2005hk: underluminous; pure deflagration? Phillips et al (2007)
Collaborations with Carnegie Supernova Project
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Light Curve Fitting with MLCS2k2 and SALT-II
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Model Survey Efficiency
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Monte Carlo Simulations match data distributions
Use actual observing conditions (sky, zero-points, PSF, etc)
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Extract RV distribution from SDSS SN data
D. Cinabro
€
RV =AV
E(B −V )=1.87 ± 0.59
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Extract AV Distribution from SDSS
(no prior)
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Future: Improved SN Ia Distances
TrainFitters
Fit Cosmology
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The Dark Energy Survey• Study Dark Energy using 4 complementary*
techniques: I. Cluster Counts II. Weak Lensing III. Baryon Acoustic
Oscillations IV. Supernovae
• Two multiband surveys: 5000 deg2 g, r, i, z, Y
to 24th mag Smaller area repeat for
SNe
• Build new 3 deg2 camera and Data management sytem Survey late 2011-2016 (525
nights) Response to NOAO AO
Blanco 4-meter at CTIO
*in systematics & in cosmological parameter degeneracies*geometric+structure growth: test Dark Energy vs. Gravity
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The DES Collaboration
FermilabUniversity of Illinois at Urbana-ChampaignUniversity of ChicagoLawrence Berkeley National LabNOAO/CTIODES Spain ConsortiumDES United Kingdom ConsortiumUniversity of MichiganOhio State UniversityUniversity of PennsylvaniaDES Brazil ConsortiumArgonne National Laboratory
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The DES Instrument: DECam
3556 mm
1575 mm
Hexapod
Optical Lenses
F8 Mirror
CCDRead out
Filters Shutter
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DES CCDs
• 62 2kx4k fully depleted CCDs:
520 Megapixels
• Excellent red sensitivity
• Developed by LBNL
0
10
20
30
40
50
60
70
80
90
100
300 400 500 600 700 800 900 1000 1100
Wavelength (nm)
Quantum Efficiency (%)
Thinned CCD Deep DepletedLBNL high resistivity
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DES Supernovae
• Baseline survey: ~1000 hours over 5 years (5 months per yr), roughly evenly split between photometric and non-photometric; ~5 visits per lunation in griz(Y); 2 deep fields, 3 shallow fields (3 sq deg per field); some possible NIR follow-up on VISTA
• ~3500 well-measured SN Ia lightcurves to z~1
• Larger sample, improved z-band response (fully depleted CCDs) compared to ESSENCE, SNLS: reduce dependence on rest-frame u-band and Malmquist bias
• Spectroscopic follow-up of SN Ia subsample+`complete’ host galaxies (LBT, Magellan, Gemini, Keck, VLT,…) e.g., focus on ellipticals (low dust extinction)?
• What strategy would be optimal for rate measurements? What questions will you want to ask?
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Forecast Redshift Distribution