dark energy tucson 2004 snls the good, the bad, and the ugly chris pritchet snls west u. victoria...
TRANSCRIPT
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Dark Energy Tucson 2004Dark Energy Tucson 2004
SNLS The Good, the Bad, and the Ugly
Chris PritchetU. Victoria (SNLS WestSNLS West)
CFHTLS SN Survey
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Some history …
Riess et al. 1998Riess et al. 1998Perlmutter et al. 1998Perlmutter et al. 1998
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Dark Energy Tucson 2004Dark Energy Tucson 2004
““Size matters Size matters …”…” Anon.
MegaCam – 1 deg x 1 degMegaCam – 1 deg x 1 deg
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Dark Energy Tucson 2004Dark Energy Tucson 2004
MegaCam at CFHT
40 x (2048 x 4612) chips (~ 400Megapixels) good blue response
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Dark Energy Tucson 2004Dark Energy Tucson 2004
MegaCam at CFHT
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Dark Energy Tucson 2004Dark Energy Tucson 2004
CFHT Legacy Survey
470 nights (dark-grey) over 5 years (2003-2008)470 nights (dark-grey) over 5 years (2003-2008) SNLS - Deep SNLS - Deep (“SNe + galaxy evolution”)(“SNe + galaxy evolution”)
202 nights over 5 years202 nights over 5 years four 1 degfour 1 deg² ² fields (0226-04, 1000+02, 1419+53, 2215-18)fields (0226-04, 1000+02, 1419+53, 2215-18)
XMM deepVIMOSSWIREGALEX
Cosmos/ACSVIMOSSIRTFXMM …
Groth stripDeep2ACS …
XMM deep
repeated observations in ugriz filters (360-950nm)repeated observations in ugriz filters (360-950nm)depth i’>24.5 (S/N=8, 1 hr); r’ > 28 in final stacked imagedepth i’>24.5 (S/N=8, 1 hr); r’ > 28 in final stacked imagesuperb image quality (0.5-0.6 arcsec expected)superb image quality (0.5-0.6 arcsec expected)queue scheduling, excellent temporal samplingqueue scheduling, excellent temporal sampling~1000 SNeIa over 5 yrs~1000 SNeIa over 5 yrsspectroscopic followup plan (VLT, Gemini, Keck, Magellan)spectroscopic followup plan (VLT, Gemini, Keck, Magellan)
Wide (“lensing’) 172 deg² in 3 patches
Very Wide (“KBO”) 1300 deg², +-2 deg from ecliptic, short exposures
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Dark Energy Tucson 2004Dark Energy Tucson 2004
The Team(s)
France: R. Pain (CB Chair), P. Astier, J. Rich …
Canada - U. Toronto: R. Carlberg, A. Howell, T. Merrall,K. Perrett, M. Sullivan
Canada - U. Victoria: C. Pritchet (SN Coordinator), D. Balam,D. Neill (Aug 2004)
US: S. Perlmutter + …
UK: I. Hook + …
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Goals of SN observations – 1.1. CosmologyCosmology Λ, w=P/ρ from Type Ia SNe (exploding white dwarfs)
P = wρ(a) ~ a -3(1+w) w = 0 matter
w = -1 w = 1/3 radiation
a(z) w !
Linder 2002 relative to
w = -0.7 model
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Science goals
beat down intrinsic dispersion (±0.1–0.2 mag per SN) as N1/2
goal: ±0.01 mag error in a z bin
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Expected precision on m, , w
Flat
Flat, m=0.03
1000 up to z=0.9
Pain 2004Pain 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
2. SFR(z) – Type II SNe (core collapse)SFR(z) – Type II SNe (core collapse)
IaIa IIII
progenitorprogenitor 1 or 2 white dwarfs
massive star
mechanismmechanism mass transfer or merger
core collapse
progenitor progenitor ageage
~1010 yr ~107 yr
evolution evolution with zwith z
little (1+z) 2-4 :
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Other applications
SNeII cosmology: v(exp) gives intrinsic luminosity
galaxy evolution, correlation functions (deep stacked images)
variable AGN’s
other variable objects
SN properties vs galaxy properties
rates Sullivan et al 2002Perlmutter et al 1998
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Dark Energy Tucson 2004Dark Energy Tucson 2004
The Stacks
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Dark Energy Tucson 2004Dark Energy Tucson 2004
SNLS - Current Status First SN discovered Mar 2003 Survey underway officially since Aug 2003
Mar 2003 Feb 2003 diff
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Dark Energy Tucson 2004Dark Energy Tucson 2004
2 real time detection pipelines working well - Ca-Fr agree to i’=+24
psfmatch2 at work
diff 1999-20001999 2000 6hr I band 100''×100''
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Detections
143 in 03B (candidates) 80-90% overlap Ca-Fr to
i’=24
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Reliability of Faint Detections
What fraction of i’=24.5 detections are real?What fraction of i’=24.5 detections are real?
AnswerAnswer:: of 45 objects i’>24.5:45 objects i’>24.5:
• 2 psfmatch errors• 2 other/unknown• others (89%) showed real light variations (though
not necessarily SNe)
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Detections vs radius [deg]
R [deg]
R [deg]
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Dark Energy Tucson 2004Dark Energy Tucson 2004
i’ detections vs. seeing
Complex!
(# of new detections) ~ (# nights elapsed since last detections)
Normalize # by dt before comparing with seeing
median ~0.4 SNe/night/field
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Spectral successes
working scheme for coordination of working scheme for coordination of telescopestelescopes
Getting the spectroscopy time in the first Getting the spectroscopy time in the first place!place!
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Dark Energy Tucson 2004Dark Energy Tucson 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Spectral successes
working scheme for coordination of telescopes
Nod & shuffle at GeminiNod & shuffle at Gemini
Getting the spectroscopy time in the first place!
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Nod and Shuffle – Gemini+GMOS
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Spectral successes
Toronto program for predicting type/phaseToronto program for predicting type/phase
working scheme for coordination of telescopes
Nod & shuffle at Gemini
Getting the spectroscopy time in the first place!
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Spec-z / Photo-z
Slight over-estimate in photo-z, indicating that
photometry is systematically faint
But this should be improved once we switch
to Elixir
Uses only two epochs of SNaproc photometry!
Sullivan, Howell et al 2004
+ SNIa SNII AGN�Spec confirmed
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Pre-screening candidates – AGN
AGN
what comes out of fitting code without knowing the true z
blue = AGN
red = Ia
green = II
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Pre-screening candidates – SN/AGN?
SN/AGN?
purple = AGN
red = Ia
green = II
(from spec)
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Spectra Statistics
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Dark Energy Tucson 2004Dark Energy Tucson 2004
z=0.84 composite (4)
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Recent Light Curves
Perlmutter 2004
z=0.4-0.7
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Light curves
Howell, Sullivan et al 2004
0.270
0.497
0.695
0.87
0.93z
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Dark Energy Tucson 2004Dark Energy Tucson 2004
June 2003 i’ 1 hr (c030622-07)
z=0.281 SN Iap t=-7d
Sainton 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
R6D4-9 = c030903-1
time
i’max= 24.05z=0.95
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Rudimentary Hubble diagram
Absolute calibration unknownRelative filter-to-filter calibration not yet confirmedBias to brighter objects at higher-redshiftPreliminary photometry
Howell, Sullivan et al 2004
= wrong z, not Ia
EdS
ΛCDM
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Web pages
www.cfht.hawaii.edu/CFHTLS http://legacy.astro.utoronto.ca – photometry,
spectroscopy, finder charts, light curves, calendar, …
http://makiki.cfht.hawaii.edu:872/sne/
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Dark Energy Tucson 2004Dark Energy Tucson 2004
6. Issues
““The Dirty Dozen”The Dirty Dozen”
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Dark Energy Tucson 2004Dark Energy Tucson 2004
LS LS vsvs. PI. PI
Program Allocated Validated % validated
DeepL01+L04 138 hr 91 hr 66%
WideL02+L05 110 hr 40 hr 36%
Very-Wide L03+L06 71 hr 21 hr 30%
Total LSTotal LS 318 hr318 hr 152 hr152 hr 48%48%
PIPI 375 hr375 hr 185 hr185 hr 49%49%
•weather•instrument failures •engineering•validation rate•seeing•focus overheads
r’ i’ , less g’z’r’ i’ , less g’z’
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Dark Energy Tucson 2004Dark Energy Tucson 2004
LS Deep - i’ and z’
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Dark Energy Tucson 2004Dark Energy Tucson 2004
2. Scheduling Issues – 2. Scheduling Issues – QSO has worked well, but …
how to handle demands of other surveys in bad weather? how to get more g’z’ in bad weather?
3.3. Image Quality - Image Quality - corrector problems
4. Calibration4. Calibration
• how achievable is 0.01 mag precision?• zeropoints – esp.in colour (matching k-corr’s at
different redshifts)• uniformity across array• variation in colour terms (esp u* and z’)• CFHT preprocessing pipeline (“Elixir”)• “phase closure”
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Conclusions
““The Ugly”:The Ugly”: • less data than hoped for in 2003B• less g’z’
““The Bad”:The Bad”: • IQ – natural seeing and corrector• calibration/photometry issues to solve
““The Good”:The Good”:• team• detection pipelines• spectroscopy • ““ugly” and “bad” mostly understood and preventable ugly” and “bad” mostly understood and preventable
in 2004Ain 2004A
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Dark Energy Tucson 2004Dark Energy Tucson 2004
--
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Dark Energy Tucson 2004Dark Energy Tucson 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Telescope Aperture vs. Focal Plane Area
total CCD area [Megapix]
total area in 3m+ telescopes [m2]
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Dark Energy Tucson 2004Dark Energy Tucson 2004
Light-curve coverage at low redshift encompasses up to 15 epochs
French and Canadian photometry not yet completely consistent, should be improved once we switch to Elixir.
Howell, Sullivan et al 2004
“Real” fits
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Dark Energy Tucson 2004Dark Energy Tucson 2004
“Real” fits
Moving up in redshift
Coverage is still good
Howell, Sullivan et al 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
“Real” fits
Intermediate redshift
Howell, Sullivan et al 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
“Real” fits
…and higher redshift…
Howell, Sullivan et al 2004
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Dark Energy Tucson 2004Dark Energy Tucson 2004
“Real” fits
And “high” redshift.
Photometry is much nosier. Peak in i is
about 24.2
Howell, Sullivan et al 2004