Metrology of type Ia supernovae for cosmology
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Transcript of Metrology of type Ia supernovae for cosmology
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Metrology of type Ia supernovae for cosmology
Claire JURAMY – Supernovae Group – LPNHE/IN2P3/CNRS
ACKS seminar December 7, 2006
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Claire Juramy 2
• Cosmology measurements with type Ia supernovae• Combined « calorimetric » analysis
• Modeling of type Ia supernovae
• Simulation of radioactive products deposition
• Analysis of late time spectra
• « Green ray » estimator
• Instrumentation for a large focal plane camera• ASIC for CCD readout in large mosaic detectors
• Cryogenic test bench
• Calibration by direct illumination with LEDs
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Claire Juramy 3
Expansion and content of the universe
• Homogenous, isotropic universe + general relativity
Friedman equations :
• R : scale factor, H : expansion rate, k : curvature
• Accelerated expansion : Cosmological constant : w = -1, w’(z) = 0
Dark energy : equation of state wX = pX / X < - 1/3
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Cosmological distance measurements • Cosmological redshift :
• Cosmological distances :
– Angular diameter dA
– Proper motion dM
– Luminosity distance dL :
• Comoving density
ztR
tR
e
r
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r 1)(
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24 L
emobs
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AML dzdzd 211
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Observation of SNe Ia in SNLS• Detection
• Spectrum : identification, redshift
• « Multiplexed » follow-up (MegaCam)
Type Ia, z = 0.93, VLT
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Measurements of dL with SNe Ia (1)
• Measurement of flux in several filters (u*g’r’i’z’)
« Flat fields » for detector calibration
Point Spread Function fitting
Calibration with standard stars, atmospheric extinction
Corrections due to differences in filters (UBVRI) and spectra
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Measurements of dL with SNe Ia (2)
• Nearby and distant supernovae : flux in restframe filters, cross-filter calibration
SuperNova Factory : SNe Ia spectrophotometry at low z• Empirical relations to reduce the dispersion of instrinsic
luminosities (Pem) : « stretch » and « color »
SNLS : SALT (Spectral Adaptative Lightcurve Template) : fits measured lightcurves to get mB*, s, c
Distance modulus :
B = mB* - MB = 5 log(dL/10pc)
Absolute magnitude :
MB = M - (s-1) + c
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Cosmological results with SNLS
M = 0.271 + 0.021 (stat) + 0.007 (sys)
w = -1.023 + 0.087 (stat) + 0.054 (sys)
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Claire Juramy 9
• Cosmology measurements with type Ia supernovae• Combined « calorimetric » analysis
• Modeling of type Ia supernovae
• Simulation of radioactive products deposition
• Analysis of late time spectra
• « Green ray » estimator
• Instrumentation for a large focal plane camera• ASIC for CCD readout in large mosaic detectors
• Cryogenic test bench
• Calibration by direct illumination with LEDs
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• White dwarf C+O, companion, Chandrasekhar mass (1.38 M)• Thermonuclear explosion : intermediate mass elements (Si,
Mg, Ca), 56Ni, iron peak elements Ejecta speed ~10,000 km/s• Decay of radioactive elements :
56Ni ( = 8.8 j) → 56Co ( = 111 j) → 56Fe Lightcurves
Type Ia supernovae
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• Photospheric phase, nebular phase
• “Calorimetric” behavior : total energies, nebular phase
Supernova evolution
SN 1990N
Bmax + 255 j
Å
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Model for gamma ray escape• Simulation of the decay of radioactive elements and of the
absorption of the products (, +) in the expanding supernova
• Physical parameters : 56Ni mass, kinetic energy (density profile, maximal speed), stratification
• Photoelectric effect, Compton scattering (E < 4 MeV)
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GRATIS (Gamma Ray Absorption in Type Ia Supernovae)
• Monte-Carlo
• Propagation along a fixed axis : computing speed, decorrelates direction and energy after Compton scattering
Decay total
Absorbed total
Absorbed in Ni
Absorbed in Fe
Absorbed in Si
Monte Carlo
Direct
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Results from GRATIS
• Deposited power depending on nickel mass mNi and ejecta speed vmax
• Simulation based only on physical parameters
mNi = 0.3 to 1.0 MVmax = 11,000 to 19,000 km/s
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Comparing GRATIS to observations• Bolometric lightcurves : SALT, absolute calibration• Agreement (50 % efficiency), dispersions• Relations between parameters (mNi, vmax) and (s,c)• Limits of SALT for bolometry and at late times
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Late-time spectra decomposition• Publicly available SNe Ia spectra : low signal, few spectra,
quality of data
• Normalized in flux on common interval• Very late-time vector (>+200 d) + orthonormal vector (60 to
200 d)
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Co and Fe components• Projection, linear with %Fe in 56Co → 56Fe• Templates for “Co” and “Fe” • Not enough data for “calorimetry” : cannot determine relative
scintillation efficiency of Co and Fe
200 j60 j
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Color during Co Fe phase
• “Lira” relation for unreddened SNe Ia
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“Green ray”• Fast change in color, transition towards emission spectrum
• Optimal estimator : selected peaks, practical : two sharp filters below and above ~5350 Å
• Quantities : speed, phase and height of the color jump
Flux ratio between filters / same around Bmax
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Measurement of the green ray
• SNLS filters : r’/g’ restframe, i’/r’ at z = 0.35
g’ r’ i’ z’
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Green ray time and stretch parameter
• i’/r’ correlates with stretch within redshift range around 0.35
• Common physical origin
Better evaluation of the “stretch” parameter
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• Cosmology measurements with type Ia supernovae• Combined « calorimetric » analysis
• Modeling of type Ia supernovae
• Simulation of radioactive products deposition
• Analysis of late time spectra
• « Green ray » estimator
• Instrumentation for a large focal plane camera• ASIC for CCD readout in large mosaic detectors
• Cryogenic test bench
• Calibration by direct illumination with LEDs
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Large mosaic detectors projects• Possible improvements for cosmology
with supernovae : increase number, higher redshifts, decrease systematic errors
– Large focal plane
– Optical (CCDs) and/or IR detectors
– Dedicated campaigns
• Projects :
– In space : SNAP (~ 700 Mpixel, 0.7deg², CCDs and IR up to 1.7 m), others : JDEM, DUNE
– On the ground : LSST (> 3 Gpixel, 10 deg²), others
SNAP
MegaCam (CFHT)
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Readout electronics for large mosaics• Constraints on front-end electronics : temperature, power,
irradiation (in space)
Integrated electronics : compact, low power, adapted to low temperatures, radiation hardness / extra noise, limited voltage
• « Video » chip : analogic functions, ADC
• First ASIC : testing of analogic functions - AMS 0.35µ
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CCD readout
• Readout capacitor ~ 40 fF, 4 µV/e-
• Reset noise
• Correction strategies :
• Clamp and Sample : reset to reference voltage
• Dual Slope Integrator : measure of reference and signal, subtraction
eVCTkBV 80320/
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DGCS (Dual Gain Clamp and Sample) ASIC • 17-bit dynamic : 2 e- (CCD noise) to 250,000 e- (CCD well
capacity) – 4 µV/ e-
• Voltage range : +1.5 / - 3.5 V or + 2.5 V
• Readout speed (~1MS/s) : ADC comparator limits dynamic to ~14 bits
• Dual gain solution (x 3 et x 96) + 2x 12-bit ADCs
• Clamp / DC restore
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DGCS ASIC : functional testing• Offset and gain problem on high gain channel : x 60, - 600 mV
• Identification and measurement of parasitic resistors
• Linearity up to specifications
Low
gai
nH
igh
gain
LSB 12 bits
parasitic R
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Acquisition for noise measurements
• Measurements to < 1 µV
• Input resistors : simulate detector noise
• Fast digitizing (1 GHz), off-line analysis
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ASIC DGCS : low noise analysis
• Noise spectra• Thermal noise of
input resistors• Intrinsic noise at
optimal readout time (80 µs) : – x 60 : 1.1 µV– x 3 : 1.8 µV
• Simulation package validated
1 MΩ20 kΩ2 kΩ500 Ω50 Ω
parasitic Cparasitic R
Sim
ulat
ion
Mea
sure
s
Low gain High gain
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1/f noise
• 1/f noise dominant at low frequencies (20 kHz) • Conforms to simulation
Measurements
R = 50 to 1 M
Simulation
R = 500 k and 2 k
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Clamp and Sample vs. Dual Slope Integrator
• C&S : longer integration time for equal pixel time, single clock, clamp noise
• DSI : low frequency noise suppression, need DC restore function, need precision on timing
DSI 2 kΩ
DSI 500 Ω
DSI 500 Ω (no aliasing)
C&S 500 Ω
Readout noise Clamp noise
½ e-1 e-
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Cold and irradiation tests
• Functioning down to 130 K
• Irradiation with cobalt 60 source (180 krad) Viable solution for mosaic readout in ground and space projects Future developments : adding ADCs, Low Current Amplifier
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Cryogenic test bench
• Dual cooling system
• Flexibility
• Temperature and pressure monitoring
• Focal plane : detector, calibrated photodiodes, readout ASIC
• Isolation from EM noise
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Cryogenic commissioning• Cold screen ~ 100 K• Cryogenerator : focal plane ~ 70 KAvailable for future electronic tests
95 K
145 K
ASIC
N2 entrance
cold screen
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SNDICE : SuperNova Direct Illumination Calibration Experiment
• Photometric calibration for SNLS : instrumental calibration• LED properties• Direct illumination setup :
– Less stray light– Controlled flux– Alignment
• Wavelength range : ~20 LEDs• Precision, accuracy :
– Calibrated source – Feedback for stability
– Additional check
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Proposed system architecture
(Cooled Large Area Photodiode)
Camera support beam
Focal plane
Out of the light path
LED sourceDACs
computer
LCAs Mux ADC
FPGAx 20
x 20
T
CLAP
(Low Current Amplifier)
MegaCam
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Low Current Amplifier ASIC• Prototype
• Optimization of input transistor for ultra low input current : guard rings
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Developments and tests
• Preliminary calibration work on test bench :– Calibration of LEDs : X, Y, T, spectrum, stability with
feedback
– Cross-calibration of CLAP with NIST standard
x 20 s
70 fA
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First LED test results
• Oversampling of the beam (photodiode: 2.4 mm)• Subtraction of dark current, comparison of flux to
reference at regular intervals
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First LED test results • Irregularities at the percent level• Need to design second diaphragm hole to avoid
glancing reflexions
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Conclusion
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Détecteurs : CCD du LBNL
• CCD épais haute résistivité du LBNL : « back-illuminated », sensibilité de l’UV au proche infra-rouge, pas de « fringing »
• Forte tension de biais, polarité inversée
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Active Pixel Sensor infra-rouge
• Substrat photosensible HgCdTe ou InGaAs
• Matrice de lecture : « BareMux »
• H2RG (Rockwell) : pixels de référence, fenêtres
• Bruit « extra noise » : supprimé par nouveau procédé
Mesuré
Attendu
Objectif
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Banc de test CCD• Refroidissement à l’azote liquide• Suivi de la température et de la pression• Plan focal : photodiodes calibrées• Lecture CCD : contrôleur SDSU,
intégration système LPNHE• Éléments optiques
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Cryogénie du banc CCD• Suivi de la température et de la pression
• Performances du refroidissement : 150 K au niveau du CCD
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Performances du banc infra-rouge• Écran froid
• Refroidissement du plan focal (plaque molybdène)
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Acquisition CCD• Contrôleur SDSU
• Lecture : SDSU, ASIC, DSA
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• Thermonuclear energy ~ 10 x decay energy• 56Ni : lowest energy/A for Z = A/2
Burnt elements
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Comparing GRATIS to observations : total• Bolometric lightcurves : SALT, absolute calibration
• Agreement (50 % efficiency), dispersions
• Relations between parameters (mNi, vmax) and (s,c)
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Comparing GRATIS to observations : power• Same efficiency (50 %)
• Heavy influence of vmax
• Limits of SALT for bolometry and at late times
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Spectres des phases tardives
• Données rares
• Phases :
– Saut de couleur (rayon vert)
– 56Co 56Fe
– Fer dominant
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• Masse de nickel 56
• Système progéniteur, explosion
• Géométrie : non sphérique, étoile compagnon
• Absorption, rougissement par des poussières
• Galaxie hôte
Diversité des supernovae de type Ia
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Proposed system architecture
(Cooled Large Area Photodiode)
(LED source)
Camera support beam (« spider »)
Focal plane
Out of the light path
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Electronic card
• Low Current Amplifier
LED source DACs computer
LCAs Mux ADC
FPGAx 20
x 20
T
CLAP