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Science team George Rieke (U of A, Lead) Gillian Wright (ROE, Instrument PI and Co-lead) Tom Greene (NASA-Ames) Margaret Meixner (STScI) Mike Ressler (NASA-JPL, Instrument Scientist) Torsten Boeker (ESA-ESTEC) Thomas Henning (MPIA) Luis Colina (CSIC-IEM) STScI Instrument team

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Miri observing templates

Science team

George Rieke (U of A, Lead)

Gillian Wright (ROE, Instrument PI and Co-lead)

Tom Greene (NASA-Ames)

Margaret Meixner (STScI)

Mike Ressler (NASA-JPL, Instrument Scientist)

Torsten Boeker (ESA-ESTEC)

Thomas Henning (MPIA)

Luis Colina (CSIC-IEM)

STScI Instrument team

Christine Chen (APT/ETC)

Scott Friedman (Commissioning)

Karl Gordon (Calibration)

Dean Hines (Operations)

Rachel Anderson

Misty Cracraft

MIRI is a NASA/JPL-led partnership with a European Consortium sponsored by ESA

NASA provides focal planes, signal chain

Consortium provides optical bench assembly

MIRI Observing Templates

C. H. Chen


Miri operating configurations
MIRI Operating Configurations

  • Imaging

    •  = 5 - 27 m wavelength range

    • Diffraction limited imaging with 0.11” pixels

    • ~2 square arcmin field of view

  • Coronagraphy

    • Three 4 Quadrant Phase Masks (10.65, 11.4, and 15.5 m)

    • One Lyot Coronagraph (23 m)

  • Low Resolution Spectroscopy (LRS)

    • R ~ 100 from  = 5 - 10 m

  • Medium Resolution Spectroscopy (MRS)

    •  = 5 - 27 m wavelength range, goal to reach  = 28.3 m

    • Integral field spectroscopy with fields of view of 3” or more

    • R ~ 3000 - 1000 from  = 5 - 27 m

C. H. Chen


Miri fov on the sky
MIRI FOV on the Sky

  • For more information, see “Mid-infrared Instrument (MIRI) Operations Concept Document” Rev C edited by C. H. Chen JWST-STScI-00910

C. H. Chen


Miri data format
MIRI Data Format

Nominal Data File Coordinates

In Final Format

Nominal Data File Coordinates

(w/Ref Output)

  • Reference Pixels - four pixels at the beginning and end of each row with no light sensitivity, one for each data output

  • Reference Output pixels - “blind” pixels interleaved with light-sensitive pixels that use a separate data output

C. H. Chen


Miri readout patterns
MIRI Readout Patterns

  • FASTMode

    • Each pixel in the (sub-)array is sampled once and that value is returned

    • Full frame time 2.775 sec

    • Will be used to observe bright targets

  • SLOWMode

    • Each pixel in the (sub-)array is sampled 10 times, the middle 8 samples are averaged together and returned

    • Full frame time 27.75 sec

    • Will be used to observe faint targets

C. H. Chen


Imaging astronomical observation requests
Imaging Astronomical Observation Requests

  • Target acquisition

    • Current implementation does not include target acquisition for direct imaging

    • The smallest subarrays (SUB64 and SUB128) may require target acquisition

    • User will specify TA source coordinates, TA filter, and expected brightness for the TA source in TA filter

  • Filter

    • User will select based on the science justification

  • Subarray

    • User will select based on the science justification and the brightness of the target, with guidance from ETC/APT software

  • Readout Pattern

    • User will select based on the science justification and the brightness of the target with guidence from ETC/APT software

  • Dither Pattern

    • User will select based on science justification

C. H. Chen



Imaging subarray selection
Imaging: Subarray Selection

  • For more information, see “MIRI Subarrays for Planetary Transits and Other Bright Objects” Rev. A by C. H. Chen, G. H. Rieke, & K. D. Gordon, JWST-STScI-001757

C. H. Chen


Imaging dither pattern selection
Imaging: Dither Pattern Selection

  • Available Patterns

    • No Dither (for transiting extra-solar planets)

    • 5-Point Gaussian (SUB64, SUB128)

    • 12-Point Reauleaux (SUB256, BRIGHTSKY, or FULL array)

    • 311-Point Cycling Pattern (SUB256, BRIGHTSKY, or FULL array)

      • User specifies starting position in list of offsets and number of dither positions required

  • Available Pattern Sizes: S, M, L

  • Optimal pattern sizes exist based on the

  • For more information, see “MIRI Imaging Dither Patterns” Rev A by C. H Chen JWST-STScI-001657

C. H. Chen


Coronagraphic astronomical observation requests
Coronagraphic Astronomical Observation Requests

  • Target acquisition

    • User will specify TA source coordinates, TA filter, and expected brightness for the TA source in TA filter

    • For more information, see “Mid-Infrared Instrument (MIRI) Target Acquisition Strategies and Use Cases” by Gordon & Meixner, 2008, JWST-001407

  • Coronagraph/Filter

    • User will select based on the science justification

  • Subarray

    • Will be automatically selected based on Coronagraph/Filter selection

  • Readout Pattern

    • User will select based on the science justification and the brightness of the target with guidance from ETC/APT software

  • Dither Pattern

    • No dither pattern is allowed

C. H. Chen


Coronagraph coronagraph filter selection
Coronagraph: Coronagraph/Filter Selection

4QPM

Lyot

  • User must select which of the following coronagraphs they would like to use: 4QPM at 10.65, 11.4, or 15.5 m or Lyot Coronagraph at 23 m

C. H. Chen


Lrs astronomical observation requests
LRS Astronomical Observation Requests

  • Target acquisition

    • User will specify TA source coordinates, TA filter, and expected brightness for the TA source in TA filter

    • For more information, see “Mid-Infrared Instrument (MIRI) Low Resolution Target Acquisition for Faint Sources” by Gordon, 2008, JWST-STScI-001347

  • Filter

    • Is automatically set to “LRS Prism”

  • Subarray

    • User will select (either LRS-Slit or LRS-Slitless) based on the science justification and the brightness of the target, with guidance from ETC/APT software

  • Readout Pattern

    • User will select based on the science justification and the brightness of the target given guidance from ETC/APT software

  • Dither Pattern

    • If LRS-Slit, then user will select based on science justification

C. H. Chen


Lrs slit vs lrs slitless observations
LRS Slit vs LRS Slitless Observations

Slitless

Slit

Target placed in the slit

Target placed in the Lyot FOV

  • LRS Slit

    • LRS Slit Target Acquisition

    • FULL frame is readout

  • LRS Slitless

    • LRS Slitless Target Acquisition TBD

    • SLITLESSPRISM subarray is readout

C. H. Chen


Lrs slit observations dither pattern selection
LRS Slit Observations: Dither Pattern Selection

  • Point Source/Staring

    • Always two positions in the slit

    • Always 1/3 and 2/3 of the way along the slit

  • Extended Source/Mapping

    • Customizable grid of positions

    • User gives number of positions parallel and perpendicular to the slit

    • User gives offset between slit positions in direction parallel and perpendicular to the slit

  • For more information, see “The LRS Dither Pattern ” by C. H. Chen JWST-STScI-001634

C. H. Chen


Mrs astronomical observation requests
MRS Astronomical Observation Requests

  • Target acquisition

    • User will specify TA source coordinates, TA filter, and expected brightness for the TA source in TA filter

    • For more information, see “Mid-Infrared Instrument (MIRI) Target Acquisition Strategies and Use Cases” by Gordon & Meixner, 2008, JWST-001407

  • Grating

    • User will select based on the science justification

  • Subarray

    • Only FULL array observations are allowed

  • Readout Pattern

    • User will select based on the science justification and the brightness of the target with guidance from ETC/APT software

  • Dither Pattern

    • User will select based on science justification

C. H. Chen


Mrs overview

10 arcseconds

Each channel’s field of view is

sliced, dispersed and detected.

Channel 1

(4.9 - 7.7 mm)

Channel 2

(7.4 - 11.8 mm)

Channel 3

(11.4 - 18.2 mm)

Channel 4

(17.5 - 28.8 mm)

Wavelength/Velocity

MRS Overview

C. H. Chen


Mrs grating selection
MRS: Grating Selection

  • Select one sub-band at a time (A-”short”,B-”medium”, or C-”long”) or ALL

C. H. Chen


Mrs dither pattern selection tbd
MRS: Dither Pattern Selection (TBD)

Pattern 2

Pattern 1

  • Pattern 1 - improved spatial sampling for all channels simultaneously

  • Pattern 2 - improved spatial and spectra sampling for one channel at a time (Ch 1, 2, 3, and 4 optimized patterns)

  • For more information, see “MIRI MRS Dither Patterns” by C. H. Chen & A. Glasse JWST-STScI-001871

C. H. Chen


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