The 5 to 28 micron imager and spectrometer that is slated to fly aboard the JWST in 2018, MIRI (Mid-Infrared Instrument), is equipped with three  flight detector arrays, each 1024 × 1024 pixels, Si:As impurity band conductors, developed by Raytheon Vision Systems.

La salle de contrôle à JPL

JPL, in conjunction with the MIRI science team, has selected the three flight arrays along with their spares.

A tutorial on how these detectors work (from M. Ressler, JPL) is available at: Detector Handout. For a thorough review of the detectors characteristics and performances, see Rieke et al., 2015 and Ressler et al., 2015.

In parallel, and in addition, to the tests performed at the Goddard Space Flight Center (GSFC, see report in the same page), several members of MICE supported the continued characterization at the Jet Propulsion Lab de la NASA (JPL, Pasadena en Californie), of the state-of-the-art Si:As detectors and its associated focal plane electronics (FPE), in view of understanding better the detectors behaviour and specific related issues. The goals of these tests are to: characterize the performance of readout modes; establish subarray operations; characterize changes to performance when switching between subarrays and/or readout modes; fine tune detector settings to mitigate residual artifacts; optimize anneal effectiveness; and characterize persistence. These tests are part of a continuing effort to support the MIRI pipeline development. They are being followed by an extensive analysis. Thus, MIRI team members not only staffed shifts during the testing but are are also collaborating in analyzing the data taken. The 8th campaign at JPL took place during the first 2 weeks of March, 2018.

La pièce de JPL où est installé le détecteur

The list below includes reports based on tests made at GSFC during which MIRI was inside ISIM (CV1, CV2, CV3), and on the 8 tests performed at JPL. The following reports are NOT intended for the general public, but rather for the professionals.

MIRI-TR-00003-CEA: Study of the Signal to Noise Ratio, Drifts and other odd behaviours (Aug. 2012)

MIRI-TR-00004-CEA: A Further Analysis of MIRI High Signal to Noise Data (Aug. 2012)

MIRI-TR-00005-CEA: Impact on a Fluctuating Focal Plane Temperature on the Integration Ramps (Oct. 2012)

MIRI-TR-00006-CEA: Signal drifts (July. 2013)

MIRI-TR-00007-CEA: Scattered Light (July 2013)

MIRI-TR-00008-CEA: Latents in darks (Aug. 2014)

MIRI-TR-00009-CEA:Latents decay timescales (March 2015)

MIRI-TR-00010-CEA: Slow Drifts (July 2015)

MIRI-TR-00011-CEA: Fast Latents (Sept. 2015)

MIRI-TR-00012-CEA: Slow Latents (Sept. 2015)

MIRI-TR-00013-CEA: Sensitivity Baseline (in colaboration with M. Garcia-Marin (ESA) and Ori Fox (STScI)) (March 2016)

MIRI-TR-00014-CEA: Electronic Anneal (April 2016)

MIRI-TR-00015-CEA: Long Timescale Latents (March 2018)

MIRI-TR-00016-CEA: Trap Mechanisms (Nov. 2016)

MIRI-TR-00017-CEA: Dark Persistence (Feb. 2014)

MIRI-TR-00018-CEA: Fast vs. Slow Mode (Jan. 2018, Draft)

MIRI-TR-00019-CEA: Dwell Time (Jan. 2018, Draft)

MIRI-TR-00020-CEA: Imprints (Jan 2018, Draft)

And from Macarena Garcia-Marin (ESA) on BIAS Levels (July 2015).

Publié dans Expertise