2005-05-251 HAWAII-2RG NOISE SNAP Collaboration Meeting M.Bonati, D.Guzman, R.Smith Caltech.

Slides:



Advertisements
Similar presentations
Toolkit for testing CCD cameras
Advertisements

IP Addressing Terminology
Describe the relationship between x and y.
Name: Date: Read temperatures on a thermometer Independent / Some adult support / A lot of adult support
Worksheets.
Hosted by Type your name here Choice1Choice 2Choice 3Choice
/ 251 Internet Applications Ahmed M. Zeki Sem – / Chapter 8.
Multiplying Powers Dividing Powers Zero ExponentsNegative.
Mr. Smith Cat. 1Cat. 2Cat. 3Cat
Mixed Numbers Equivalent Simplest Form Comparing
$100 $200 $300 $400 $500 $100 $200 $300 $400 $500 $100 $200 $300 $400 $500 $100 $200 $300 $400 $500 $100 $200 $300 $400 $500 $100 $200 $300.
TDC130: High performance Time to Digital Converter in 130 nm
Irradiation of 300 m phi detectors from MICRON and HAMAMATSU cont. Second independent estimate: 6h 2 cycles, 12h 1 cycle, 14h no beam, 5.5h 1cycle estimated.
A 200 Frames per Second, 1-Megapixel, Frame Store CCD camera for X-ray imaging Dionisio Doering (a), Nord Andresen (a), Devis Contarato (a), Peter Denes.
The basics for simulations
CrIMSS EDR Performance Assessment and Tuning Alex Foo, Xialin Ma and Degui Gu Sept 11, 2012.
Cosmic Ray Test of GEM- MPI/TPC in Magnetic Field Hiroshima University Kuroiwa CDC Group Mar
ISIS and SPiDeR Zhige ZHANG STFC Rutherford Appleton Laboratory.
Kailua-Kona, Marcel Trimpl, Bonn University Readout Concept for Future Pixel Detectors based on Current Mode Signal Processing Marcel Trimpl.
Hosted by Lynn Dickson Choice1Choice 2Choice 3Choice
The characteristics of the MA-PMT HAMAMATSU : H for the MINICAL Samuel Kazarian, Volker Korbel, Pavel Murin, Stefan Valkar, Jan Weichert.
Static Equilibrium; Elasticity and Fracture
Chart Deception Main Source: How to Lie with Charts, by Gerald E. Jones Dr. Michael R. Hyman, NMSU.
Schutzvermerk nach DIN 34 beachten 05/04/15 Seite 1 Training EPAM and CANopen Basic Solution: Password * * Level 1 Level 2 * Level 3 Password2 IP-Adr.
C. Beichman, Dimitra Touli, Gautam Vasisht, Roger Smith Tom Greene
16 January 2003STScI TIPS1 JWST's Near-Infrared Detectors: Ultra-Low Background Operation and Testing Bernie Rauscher, Don Figer, Mike Regan, Sito Balleza,
Analysis of chip with 100 events, July 2001 Variation in pixel to pixel average ADC values (fixed pattern noise) Pixel ADC value event to event repeatability.
In situ testing of detector controllers Roger Smith Caltech
Discussion of CalWebb contents M. Robberto (facilitator)
First results from the HEPAPS4 Active Pixel Sensor
CHARGE COUPLING TRUE CDS PIXEL PROCESSING True CDS CMOS pixel noise data 2.8 e- CMOS photon transfer.
Echelle spectra reduction with IRAF*
HgCdTe Noise from µHz to kHz Roger Smith, Gustavo Rahmer, David Hale, Elliott Koch Caltech Detectors for Astronomy Garching,
European Southern Observatory
Jaap Velthuis, University of Bristol SPiDeR SPiDeR (Silicon Pixel Detector Research) at EUDET Telescope Sensor overview with lab results –TPAC –FORTIS.
James Webb Space Telescope : Characterization of Flight Candidate of Raytheon NIR InSb Arrays 5 Aug 2003 Craig McMurtry, William Forrest, Andrew Moore,
JWST Radiation Environment 1March 13, 2003 Reference pixels and readout modes: What we have learned thus far Don Figer, Bernie Rauscher, Mike Regan March.
Detector Assembly Design Pedestal Cold Strap Interface Cable SCA Motherboard Attachment Feet 51 Pin Electrical Connector Cover/Baffle Package designed.
1 Ultra low background characterization of Rockwell Scientific MBE HgCdTe arrays Donald N. B. Hall, University of Hawaii, Institute for Astronomy, Honolulu,
Measurement Results for 4kX2k Frontside Illuminated CCD
Digital Hadron Calorimeter Cosmic Ray Test Stand.
14 January 2003Special LASP Seminar at GSFC1 JWST's Near-Infrared Detectors: Ultra-Low Background Operation and Testing Bernard J. Rauscher Space Telescope.
STAR Collaboration Meeting, Nantes, July2002 SVT Analysis/Status Update Jun Takahashi – University of Sao Paulo.
Rate and Gain Measurements of the 1-m long GEM detector Aiwu Zhang EIC tracking R&D weekly meeting.
Readout Electronics: SIDECAR ASIC Hardware
Super-hot pixels, hot pixels and DSNU on Hawaii-2RG detector
NASSP Masters 5003F - Computational Astronomy Lecture 19 EPIC background Event lists and selection The RGA Calibration quantities Exposure calculations.
Evaluation of Silicon Photomultiplier Arrays for the GlueX Barrel Calorimeter Carl Zorn Radiation Detector & Medical Imaging Group Jefferson Laboratory,
CCD Detectors CCD=“charge coupled device” Readout method:
Telescope Guiding with a HyViSI H2RG Used in Guide Mode Lance Simms Detectors for Astronomy /2/09.
NIRSpec Operations Concept Michael Regan(STScI), Jeff Valenti (STScI) Wolfram Freduling(ECF), Harald Kuntschner(ECF), Robert Fosbury (ECF)
The MPPC Study for the GLD Calorimeter Readout Introduction Measurement of basic characteristics –Gain, Noise Rate, Cross-talk Measurement of uniformity.
Solar-B SOT/FPP 1 SOT April 2006Ted Tarbell FPP CCD Camera Performance Ted Tarbell 17-Apr-2006.
10/26/20151 Observational Astrophysics I Astronomical detectors Kitchin pp
APS-2 Single Pixel Test 7 February 2008 V. Suntharalingam  The Pattern file to capture data from a 256x256 array was modified to address only one pixel.
SNAP Collaboration meeting / Paris 10/20071 SPECTROMETER DETECTORS From science requirements to data storage.
6/15/051 Energetic Cosmic Ray Events in SIPIN-H2RG-015 Device Lance Simms.
Basic Detector Measurements: Photon Transfer Curve, Read Noise, Dark Current, Intrapixel Capacitance, Nonlinearity, Reference Pixels MR – May 19, 2014.
The InGaAs IR Array of Chunghwa Telecom Laboratory Chueh-Jen Lin and Shiang-Yu Wang, Optics and Infrared Laboratory In 2006, Advanced Technology Laboratory.
Installation of the ACS Guido De Marchi – TIPS meeting – Guido De Marchi - ESA/STScI - ACS Group The ACS was installed on board the HST on the.
Scientific DetectorWorkshop, 2005 Taormina Characterization of 1.7um cutoff detectors for SNAP Roger Smith Caltech.
# x pixels Geometry # Detector elements Detector Element Sizes Array Size Detector Element Sizes # Detector elements Pictorial diagram showing detector.
Binomial Distribution Possion Distribution Gaussian Distribution Lorentzian Distribution Error Analysis.
4x8 Mosaic Camera Development
Charge Transfer Efficiency of Charge Coupled Device
Detectors of JWST Near IR Instruments
Preliminary Design Review
Preliminary Design Review
Dark Current Experiment Preliminary Design Review
The MPPC Study for the GLD Calorimeter Readout
Presentation transcript:

HAWAII-2RG NOISE SNAP Collaboration Meeting M.Bonati, D.Guzman, R.Smith Caltech

The questions Is detector material limiting noise performance? Is this a property of the 1.7 m cutoff material/process, or the higher operating temperature? Is the problem with the noise floor or the starting CDS noise? Requirement / Goal = 8e- / fowler ~16...yes …both …CDS too high

Confusing effects Is detector noise floor masked by dark current, mux glow, or particle hits? Is mux degrading detector noise? Is controller degrading mux noise? …slightly. Upgradeable, but not urgent. …not now. RTS may intrude later. …particle hits in substrate are a concern.

How do we know detector material limits noise performance? Image pixel noise >> bare mux, ref pixels Dependence on T, not seen in ref pixels. Excess noise goes away when reset switch is closed.

Temporal noise map shows reference pixels are much quieter than image Need >400 samples to see intrinsic width of histogram

Temporal Noise Histograms vs. T

Fowler Noise at 140K Excess noise goes away when reset switch is closed.

Is it just the temperature?

At 77K CDS noise is still much higher than for 2.5 m HgCdTe. True fowler limit may be due to mux glow, dark current, drift or Cosmic Rays.

Dark current vs. Temperature Modal dark current is negligible. ~0.2e-/read mux glow has small effect at Fowler 64. Dewar showed no light leak previously, but this has not been tested recently.

Sample Up the Ramp Average of all channels is quite linear but individual channels sho considerable scatter. ….Drifts? ….Cosmic ray hits?

K Hot pixels frozen out Dark images vs T Movie 140K lots of hot pixels Many diffuse cosmic ray hits

Cosmic Rays ? Difference of successive 300s dark images 100K Fowler 32 Some are very diffuse Movie

Long darks show flat field pattern Movie Dark Flat

e-/ADU vs T 4% rise from 85 to140K Inverse Gain

Bare mux performance ….Not currently a limitation.

Bare mux 006, ch 1, optimum biases CDS noise (ADU) Reset modeImage pixels spatial temporal Reference pixels spatial temporal Line, Pulsed Global Global + dummy before reset Global + dummy after reset Line, Continuous gain = 1.1 to 1.4 e-/ADU PREVIOUS RESULTS

To reduce bias sensitivity… V load VoVo Column bus CellDrain V reset RG Row Sel Col Sel BiasGate BiasPower CiCi R load OutputDrain VddA BG tracks BP so bias current ~constant. [Can use 32 ch readout] VddA = BP eliminates body effect, but… …. VddA still acts like phantom gate connection here so VddA=BP increases net effect of VddA drift. Vishay J mA, 700K, 0.05%/C 375

Bare mux CDS noise ConfigurationSpatial noise min.exp 300s Temporal (mode) min.exp 300s BG = BP VddA = BP BG = BP Independent VddA ANU bias board BG= BP, VddA=BP ANU bias board Separate BP, BG, VddA Mux030, SDSU biases, BG= BP, Noise in ADU, gain = 1.1 to 1.4 e-/ADU Continuous line reset, all pixels on ch 1, ~1 sec/read. BP=3.3V, BG=2.4V, VR=0.6,

DRIFTS in CDS frames ConfigurationDrift (ADU) RMS of means for 200 frames Min.exp 300s SDSU biases BG= BP, VddA=BP ANU bias board BG= BP, VddA=BP ANU bias board Separate BP, BG, VddA Mux030, SDSU biases, BG= BP, RMS variation of mean in ADU. gain = 1.1 to 1.4 e-/ADU Continuous line reset, all pixels on ch 1, ~1 sec/read. BP=3.3V, BG=2.4V, VR=0.6 Drift reduced by shield installation? …less convection around JFET currrent source?

ANU bias loopback tests ANU drift and noise are dominated by the Leach 8 channel video board drift and noise, so they are indeed very good. We plan to improve the drift of the Leach board by a factor of two by a component change, and will then remeasure.