Telescope and Instrument Performance Summary (TIPS) 16 Jan 2003 AGENDA. 1. Type 1a SuperNovae Adam Riess 2. JWST s NIR Detectors Bernie Rauscher

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1 Telescope and Instrument Performance Summary (TIPS) 16 Jan 2003 AGENDA 1. Type 1a SuperNovae Adam Riess 2. JWST s NIR Detectors Bernie Rauscher

2 Adam G. Riess Space Telescope Science Institute

3 How (we think) Nature makes a SN Ia 51 Homogeneity: 1.4 Mo, 10 ergs Negligible hydrogen, lots of IME Mature progenitors Models (delayed-detonation) good fit to observations

4 Standard Candles dust Bright=near dim=far dim & red=closer!

5 Expansion History of the Universe, Ω < 1 M (redshift), Ω = 1 M, Ω > 1 M Mass is destiny (Distance)

6 The Accelerating Universe By 1998 two teams measured ~100 SNe Ia at 0.01 <z<1.0 Surprise! The Universe is accelerating, propelled by dark energy. High-z SCP

7 Searching for the Epoch of a required feature of a mixed dark matter/dark energy Universe ρ ρ M,0 M = (1 + ρ Λ ρ Λ z) 3 z ρ M ρλ

8 ρ Searching for the Epoch of ρ M,0 M = (1 + ρ Λ ρ Λ z) 3 z ρ M ρλ Our current goal: 6-8 SNe Ia at 1.2<z<1.8

9 Difficulty ( 1+ z) 6 Or why its so hard to find type Ia supernovae at z>1.2 Effect geometrical dilution Factors of (1+z) 2 redshift of energy density dilation of integration time Decline of SN Ia SED ~ µ Decline in QE of detectors ~ µ 1 1 ~1 ~1 Finding SNe Ia Total= 6 SNe Ia at 1.2<z<1.8 is 10 to 40 times harder than at z=0.5 (a.k.a., 1998)

10 The GOODs ACS Treasury Program and The Hubble Higher-z Supernova Search Team A Higher-z Supernova Search Piggybacking on the ACS Survey 134 orbits ToO for 6-8 SNe Ia at 1.2<z<1.8 Riess (STScI) Strolger (STScI) Tonry (UH) Filippenko (UCB) Kirshner, (CfA) Challis, (CfA) Casertano, (STScI) Dickinson (STScI) Giavalisco (STScI) Ferguson (STScI) 399 orbits of deep imaging for extragalactic studies

11 Searching for SNe Ia with ACS 5 z-band epochs, spaced by 45 days, simultaneous v,i band, 120 tiles CDFS=08/02-02/03 HDFN=11/02-05/03

12 What we are finding ~5-6 SNe per search epoch (~0.3 SNe/ACS pointing) ~1/2 type Ia, ~1/2 core-collapse, 0.3<z<1.8, <z>=1

13 SN Color Differences SN Ia UV deficit v i z Most Common SN types: type Ia and type II

14 Color Discrimination

15 Our first higher-z SN Ia, Aphrodite Aphrodite (1<z<1.5) ACS F850lp ACS grism spectrum NICMOS F110W viz

16 The Rise and Fall of Aphrodite Aug Sept Oct Nov

17 Our Second Higher-z SN Ia, Thoth Epoch 2 Epoch 3 Epoch 3-2 red, elliptical host Keck VLT z=1.3

18 Our Third Higher-z SN Ia, Nanna Epoch 1 Epoch 2 difference OII, Keck

19 And Some Even More Distant Athena: phot-z: 1.8<z<2.2 Colors, mag SN Ia at z~1.8 Osiris: Colors, mag SN Ia at 1.5<z<1.8 ACS f850lp viz We are off to a great start results coming soon to a journal near you

20 Dilution of Light or Gravity Depends on the Number of Dimensions Either Sees Number of Dimensions Intensity/Distance Law Independent of Distance (I ~ 1/R 0) Reciprocal of Distance I ~ 1/R 1 Inverse Square Law I ~ 1/R 2 Essential component of String Theory: photons move in 3 dimensions, Gravitons leaks into 5,10 or 11 D long-range decay of gravity (Dvali et al 2001)

21 The Future Is Bright for SNe Ia! New tests of the new cosmology (searching for past deceleration) Deeper understanding of SNe Ia (progenitors) Probing the nature of Dark Energy

22 The End

23 JWST's Near-Infrared Detectors: Ultra-Low Background Operation and Testing And coming soon! Bernie Rauscher, Don Figer, Mike Regan, Sito Balleza, Robert Barkhouser, Eddie Bergeron, Gretchen Greene, Ernie Morse, Steve McCandliss, Russ Pelton & Tom Reeves 16 January 2003 STScI TIPS 1

24 Outline What is a Near-Infrared Array Detector? JWST Science Drivers Detector Requirements Detector testing at STScI/JHU Optimal Use Summary 16 January 2003 STScI TIPS 2

25 JWST s IR Arrays are Hybrid Sensors PN junctions are bump bonded to a silicon readout multiplexer (MUX). Silicon technology is more advanced than other semiconductor electronics technology. The bump bonds are made of indium. 16 January 2003 STScI TIPS 3

26 JWST Needs Very Good Near Infrared Detectors! Completing the JWST Design Reference Mission on time requires background limited nearinfrared (NIR) broadband imaging Zodiacal light is the dominant background component in the NIR The total NIR detector noise requirement is therefore =10 e- rms in a t=1000 seconds exposure. NIRSpec will probably be detector noise limited. The total noise goal is =3 e- rms per 1000 seconds exposure Signal [e-/sec/pix] 1.E+02 1.E+01 1.E+00 1.E-01 1.E-02 1.E-03 1.E-04 Sunshield JWST requirement JWST goal R=5 Zodiacal Light R= Wavelength [µm] 16 January 2003 STScI TIPS 4

27 JWST Near Infrared (NIR) Detector Requirements Parameter Requirement Goal InSb Status HgCdTe Detector Noise per image 9 e RMS 2.5 e RMS 10.8 e RMS 6.7 e RMS Read Noise (n Fowler 16) NR NR 10.6 e RMS 4.6 e RMS Dark Current NR NR e /s 0.02 e /s QE 0.6 µ m < λ < 1.0 µ m 70% 90% unknown unknown 95% 1.0 µ m < λ < 5.0 µ m 80% 95% >80% >80% ~74% Pixel-to-pixel uniformity TBD TBD ~10% ~10% ~74% Operability 98% 99.5% NA NA Latent Image 0.1% 0 <0.5% <0.5 % Fill Factor >95% 100% >98 >98% Radiation Immunity <4% inop EOM no effect unknown unknown Frame Time 12 s <12 s <12s <12 s Temperature 30 K < T < 37 K allow ± 2 K in range in range MTF 0.53 >0.53 unknown unknown a Assumes 1000 second exposure and quadrature sum of read noise and shot noise from dark current. 16 January 2003 STScI TIPS 5

28 Detector Testing at STScI/JHU: Independent Detector Testing Laboratory 16 January 2003 STScI TIPS 6

29 Past and present personnel Eddie Bergeron Data Analyst Tom Reeves Lab Technician Robert Barkhouser Optical Engineer Mike Telewicz Intern Bernie Rauscher Project Scientist Utkarsh Sharma Graduate Student Gretchen Greene Mechanical Engineer Steve McCandliss JHU Lead Ernie Morse Data Analyst Monica Rivera Intern Scott Fels Intern Don Figer Director Russ Pelton Technician Sito Balleza Systems Engineer Mike Regan System Scientist 16 January 2003 STScI TIPS 7

30 IDTL Experiments Read noise Conversion Gain Dark current Linearity Electronic Gain Latent charge (persistence) Relative and Absolute Quantum efficiency (QE) Intra-pixel sensitivity 16 January 2003 STScI TIPS 8

31 Dark Current Lowest measured dark current is ~0.006 e /s/pixel. 16 January 2003 STScI TIPS 9

32 IDTL Measurements: Read Noise Read noise is ~10 e for Fowler-8. (system read noise is ~2.5 e ) 16 January 2003 STScI TIPS 10

33 Per correlated double sample IDTL Measurements: Conversion Gain 16 January 2003 STScI TIPS 11

34 IDTL Test System Hawaii Shirt Hawaii Detector 16 January 2003 STScI TIPS 12

35 Then & Now November 2000 November January 2003 STScI TIPS 13

36 IDTL First Light Images Raytheon ALADDIN Rockwell HAWAII-1R Rockwell HAWAII-1RG Jan. 01 (MUX) Feb. 02 (MUX) Apr. 02 (SCA) Jun. 02 (MUX) Jul. 02 (SCA) Raytheon SB-304 Rockwell HAWAII-2RG Nov. 02 (MUX) Jan. 03 (MUX) 16 January 2003 STScI TIPS 14

37 IDTL Test System Leach II Controller Electronics Dewar Entrance Window Vacuum Hose He Lines 16 January 2003 STScI TIPS 15

38 Detector Readout System T=30-50 K Unix Instrument Control Computer Warm Harness COTS Leach II IR Array Controller T~293 K JWST SCA Detector Customization Circuit Cryogenic Harness 16 January 2003 STScI TIPS 16