Transcript NIRISS: The Near InfraRed Imager & Slitless Spectrograph Alex Fullerton STScI TIPS / JIM 2013 June 20

NIRISS:
The Near InfraRed Imager & Slitless Spectrograph
Alex Fullerton
STScI
TIPS / JIM
2013 June 20
Outline
a)
b)
c)
d)
e)
What is NIRISS?
What can it do?
Who is on the NIRISS Team?
What are we doing now?
What’s coming up?
Previous TIPS / JIM Presentations on NIRISS
TIPS / JIM
2013 June 20
2013 April 11
Single-Object Slitless Spectroscopy with NIRISS (Kevin Volk)
2012 Sept. 20
The Wide-Field Slitless Spectroscopy Mode of NIRISS (Van Dixon)
2012 Aug. 16
The Delivery of FGS/NIRISS to GSFC (Alex Fullerton)
2012 June 21
NIRISS NRM Bad Pixel Tolerance Analysis (Anand Sivaramakrishnan)
2012 March 15
Aperture Synthesis Imaging with JWST NIRISS’ NRM (Anand Sivaramakrishnan)
2011 Sept. 15
Introducing JWST’s NIRISS: The Near Infrared Imager and Slitless Spectrograph (Alex Fullerton)
FGS / NIRISS
Fine Guidance Sensor (FGS)
PI: John Hutchings (NRC-Herzberg)
René Doyon (U de M)
Optical Bench
Near-Infrared Imager
and
Slitless Spectrograph
(NIRISS)
PI: René Doyon (U de M)
TIPS / JIM
2013 June 20
Optical Layout of NIRISS
TIPS
/ JIM
TIPS/JIM
2013
June 20
2011 September
15
The Near-Infrared Imager and Slitless Spectrograph (NIRISS)
At a glance:
Optical Layout
Detector
Teledyne HAWAII-2RG
HgCdTe with 5.2μm cutoff
2048 × 2048 pixels
Field of View
2.2´ × 2.2´
Plate scale
0.065 arcsec / pixel
Pupil Wheel
“Blue” filters
Grism GR700XD
Aperture Mask NRM
Filter Wheel
“Red” filters
Grisms GR150C,R
Pick-Off Mirror
Kinematic Mounts
(3 pairs)
Collimator
Camera
Pupil Wheel
Filter Wheel
Detector
Pupil / Filter Wheel
!
Observing Modes
“R”
Imaging
Point-Source Sensitivity:
S/N=10 in 10 ks
Filter
nJy
m(Vega)
F090W
11.28
28.28
F115W
11.22
28.06
F150W
9.19
27.83
F200W
7.81
27.54
F277W
6.63
27.09
F356W
6.89
26.56
F444W
12.29
25.49
NIRISS Pocket Guide v1.0 (2013 May)
“C”
Wide-Field
Slitless Spectroscopy
GR150{R,C} grisms + “Blue” Filters
Resolving Power (1st order): ~150
Spectral coverage (1st order): 0.8 – 2.2
μm
{Row, Column} orientations provide
orthogonal dispersion directions on the
detector to mitigate blending. Blocking
filters isolate wavelengths of interest.
Fiducial sensitivity (unresolved line):
5 ×10-18 erg/s/cm2 with S/N=10 in 10 ks
Single-Object
Slitless Spectroscopy
Aperture Masking
Interferometry
GR700XD grism + CLEAR
Three cross-dispersed orders
Spectral coverage 0.6 – 2.5 μm
Resolving Power (1st order): 300 – 800
The orders are broadened in the crossdispersion direction by 30 – 40 pixels.
NRM + Medium “Red” Filters
7-hole aperture mask with 21 baselines;
all have different (“non-redundant”) lengths.
Subarray readout formats through 1 or 4
pre-amps optimize SOSS for exoplanet
transit spectroscopy. No slit losses;
target acquisition provides repeatability.
Estimated J-band bright limits (G2 V star):
Subarray
1 pre-amp 4 pre-amps
2048 × 256
8.2
6.7
2048 × 80
6.9
5.5
Michelson:
δθ = 0.5 λ / D
Mask
Interferogram
AMI with NIRISS enables the
detection of exoplanets at
3.8, 4.3, and 4.8 μm around
stars as bright as M’ ~ 5 with:
Contrast: ~2×10-5 (S/N~5)
Separations: 70 – 400 mas
Fourier
Aperture synthesis imaging
Transform
(of. e.g., AGN) is also enabled.
http://www.stsci.edu/jwst/instruments/niriss
A Niche for AMI
70 mas
400 mas
NIRCam soft occulting spot inner
working angle
(IWA; 50% transmission point)
TIPS / JIM
2013 June 20
The Near-Infrared Imager and Slitless Spectrograph (NIRISS)
At a glance:
Optical Layout
Detector
Teledyne HAWAII-2RG
HgCdTe with 5.2μm cutoff
2048 × 2048 pixels
Field of View
2.2´ × 2.2´
Plate scale
0.065 arcsec / pixel
Pupil Wheel
“Blue” filters
Grism GR700XD
Aperture Mask NRM
Filter Wheel
“Red” filters
Grisms GR150C,R
Pick-Off Mirror
Kinematic Mounts
(3 pairs)
Collimator
Camera
Pupil Wheel
Filter Wheel
Detector
Pupil / Filter Wheel
!
Observing Modes
“R”
Imaging
Point-Source Sensitivity:
S/N=10 in 10 ks
Filter
nJy
m(Vega)
F090W
11.28
28.28
F115W
11.22
28.06
F150W
9.19
27.83
F200W
7.81
27.54
F277W
6.63
27.09
F356W
6.89
26.56
F444W
12.29
25.49
NIRISS Pocket Guide v1.0 (2013 May)
“C”
Wide-Field
Slitless Spectroscopy
GR150{R,C} grisms + “Blue” Filters
Resolving Power (1st order): ~150
Spectral coverage (1st order): 0.8 – 2.2
μm
{Row, Column} orientations provide
orthogonal dispersion directions on the
detector to mitigate blending. Blocking
filters isolate wavelengths of interest.
Fiducial sensitivity (unresolved line):
5 ×10-18 erg/s/cm2 with S/N=10 in 10 ks
Single-Object
Slitless Spectroscopy
Aperture Masking
Interferometry
GR700XD grism + CLEAR
Three cross-dispersed orders
Spectral coverage 0.6 – 2.5 μm
Resolving Power (1st order): 300 – 800
The orders are broadened in the crossdispersion direction by 30 – 40 pixels.
NRM + Medium “Red” Filters
7-hole aperture mask with 21 baselines;
all have different (“non-redundant”) lengths.
Subarray readout formats through 1 or 4
pre-amps optimize SOSS for exoplanet
transit spectroscopy. No slit losses;
target acquisition provides repeatability.
Estimated J-band bright limits (G2 V star):
Subarray
1 pre-amp 4 pre-amps
2048 × 256
8.2
6.7
2048 × 80
6.9
5.5
Michelson:
δθ = 0.5 λ / D
Mask
Interferogram
AMI with NIRISS enables the
detection of exoplanets at
3.8, 4.3, and 4.8 μm around
stars as bright as M’ ~ 5 with:
Contrast: ~2×10-5 (S/N~5)
Separations: 70 – 400 mas
Fourier
Aperture synthesis imaging
Transform
(of. e.g., AGN) is also enabled.
http://www.stsci.edu/jwst/instruments/niriss
Current Flight Grism (Bach Corp.)
weak
cylindrical
surface
Rλ 300 – 800 in 1st order
Unruled Perimeter
TIPS / JIM
2013 June 20
Spectral Traces
Spectral traces are
shown for the nominal
target acquisition
location
2500 nm
500 nm
500 nm
1300 nm
order 1
order 3
order 2
order 0
The Near-Infrared Imager and Slitless Spectrograph (NIRISS)
At a glance:
Optical Layout
Detector
Teledyne HAWAII-2RG
HgCdTe with 5.2μm cutoff
2048 × 2048 pixels
Field of View
2.2´ × 2.2´
Plate scale
0.065 arcsec / pixel
Pupil Wheel
“Blue” filters
Grism GR700XD
Aperture Mask NRM
Filter Wheel
“Red” filters
Grisms GR150C,R
Pick-Off Mirror
Kinematic Mounts
(3 pairs)
Collimator
Camera
Pupil Wheel
Filter Wheel
Detector
Pupil / Filter Wheel
!
Observing Modes
“R”
Imaging
Point-Source Sensitivity:
S/N=10 in 10 ks
Filter
nJy
m(Vega)
F090W
11.28
28.28
F115W
11.22
28.06
F150W
9.19
27.83
F200W
7.81
27.54
F277W
6.63
27.09
F356W
6.89
26.56
F444W
12.29
25.49
NIRISS Pocket Guide v1.0 (2013 May)
“C”
Wide-Field
Slitless Spectroscopy
GR150{R,C} grisms + “Blue” Filters
Resolving Power (1st order): ~150
Spectral coverage (1st order): 0.8 – 2.2
μm
{Row, Column} orientations provide
orthogonal dispersion directions on the
detector to mitigate blending. Blocking
filters isolate wavelengths of interest.
Fiducial sensitivity (unresolved line):
5 ×10-18 erg/s/cm2 with S/N=10 in 10 ks
Single-Object
Slitless Spectroscopy
Aperture Masking
Interferometry
GR700XD grism + CLEAR
Three cross-dispersed orders
Spectral coverage 0.6 – 2.5 μm
Resolving Power (1st order): 300 – 800
The orders are broadened in the crossdispersion direction by 30 – 40 pixels.
NRM + Medium “Red” Filters
7-hole aperture mask with 21 baselines;
all have different (“non-redundant”) lengths.
Subarray readout formats through 1 or 4
pre-amps optimize SOSS for exoplanet
transit spectroscopy. No slit losses;
target acquisition provides repeatability.
Estimated J-band bright limits (G2 V star):
Subarray
1 pre-amp 4 pre-amps
2048 × 256
8.2
6.7
2048 × 80
6.9
5.5
Michelson:
δθ = 0.5 λ / D
Mask
Interferogram
AMI with NIRISS enables the
detection of exoplanets at
3.8, 4.3, and 4.8 μm around
stars as bright as M’ ~ 5 with:
Contrast: ~2×10-5 (S/N~5)
Separations: 70 – 400 mas
Fourier
Aperture synthesis imaging
Transform
(of. e.g., AGN) is also enabled.
http://www.stsci.edu/jwst/instruments/niriss
Wide-Field Slitless Spectroscopy with NIRISS:
Simulations of MACS J0647+7015
Image: F200W
Spectra: GR150C, F200W
Spectra: GR150R, F200W
Layout of Spectral Orders
Filter Transmission Profiles
GR150R
Detector Pixels
GR150C
The Near-Infrared Imager and Slitless Spectrograph (NIRISS)
At a glance:
Optical Layout
Detector
Teledyne HAWAII-2RG
HgCdTe with 5.2μm cutoff
2048 × 2048 pixels
Field of View
2.2´ × 2.2´
Plate scale
0.065 arcsec / pixel
Pupil Wheel
“Blue” filters
Grism GR700XD
Aperture Mask NRM
Filter Wheel
“Red” filters
Grisms GR150C,R
Pick-Off Mirror
Kinematic Mounts
(3 pairs)
Collimator
Camera
Pupil Wheel
Filter Wheel
Detector
Pupil / Filter Wheel
!
Observing Modes
“R”
Imaging
Point-Source Sensitivity:
S/N=10 in 10 ks
Filter
nJy
m(Vega)
F090W
11.28
28.28
F115W
11.22
28.06
F150W
9.19
27.83
F200W
7.81
27.54
F277W
6.63
27.09
F356W
6.89
26.56
F444W
12.29
25.49
NIRISS Pocket Guide v1.0 (2013 May)
“C”
Wide-Field
Slitless Spectroscopy
GR150{R,C} grisms + “Blue” Filters
Resolving Power (1st order): ~150
Spectral coverage (1st order): 0.8 – 2.2
μm
{Row, Column} orientations provide
orthogonal dispersion directions on the
detector to mitigate blending. Blocking
filters isolate wavelengths of interest.
Fiducial sensitivity (unresolved line):
5 ×10-18 erg/s/cm2 with S/N=10 in 10 ks
Single-Object
Slitless Spectroscopy
Aperture Masking
Interferometry
GR700XD grism + CLEAR
Three cross-dispersed orders
Spectral coverage 0.6 – 2.5 μm
Resolving Power (1st order): 300 – 800
The orders are broadened in the crossdispersion direction by 30 – 40 pixels.
NRM + Medium “Red” Filters
7-hole aperture mask with 21 baselines;
all have different (“non-redundant”) lengths.
Subarray readout formats through 1 or 4
pre-amps optimize SOSS for exoplanet
transit spectroscopy. No slit losses;
target acquisition provides repeatability.
Estimated J-band bright limits (G2 V star):
Subarray
1 pre-amp 4 pre-amps
2048 × 256
8.2
6.7
2048 × 80
6.9
5.5
Michelson:
δθ = 0.5 λ / D
Mask
Interferogram
AMI with NIRISS enables the
detection of exoplanets at
3.8, 4.3, and 4.8 μm around
stars as bright as M’ ~ 5 with:
Contrast: ~2×10-5 (S/N~5)
Separations: 70 – 400 mas
Fourier
Aperture synthesis imaging
Transform
(of. e.g., AGN) is also enabled.
http://www.stsci.edu/jwst/instruments/niriss
NIRISS Instrument Team @ STScI
Van Dixon
Alex Fullerton
Paul Goudfrooij
PhD Astronomy
Johns Hopkins (1995)
PhD Astronomy
Toronto (1990)
PhD Astronomy
Amsterdam (1994)
Team Lead
Operations Lead
WFSS Simulations
Pipeline Development
Efficiency WG
PPS WG
ISIM CV Planning
Sherie Holfeltz
André Martel
Swara Ravindranath
BSc Astronomy
Utah (1990)
PhD Astronomy
UC Santa Cruz (1996)
PhD Astronomy
IIA Bangalore (2000)
ISIM CV Test Planning
On-Orbit Commissioning
Algorithm development
Data Analysis
Most recent arrival!
Tasks TBD
SID Archive Ingest
Data Simulations
Data Analysis
Anand Sivaramarkrishnan
Deepashri Thatte
Kevin Volk
PhD Astronomy
UT Austin (1983)
MSc Physics
South Carolina (2004)
PhD Astronomy
Calgary (1986)
Aperture Masking:
Operations
Calibration
JAM / JAMEx WG
NIRISS Science Team
TIPS / JIM
2013 June 20
Aperture Masking:
Simulations & Tests
Website Curation
Calibration Planning
Cal Pipeline
Reference Files
Data Analysis
S&OC: How the Work Gets Done
NIRISS
S&OC Subsystems
Interfaces
Ops-04 GTO Science Program
SR-01
PPS
Sci Rationale
Science Team
Observing
Mode
Astronomer’s Proposal Tool
Exposure Time Calculator
Instrument Website
Instrument Handbook
Help Desk
MESA-PPS WG
ETC Algorithms WG
Backgrounds WG
OSS
Ops-02B OCD
Instrument Definition Team
CSA
ComDev
U de M
HIA / NRC
Ops-01B User Manual
TIPS / JIM
2013 June 20
Operations WG
Efficiency WG
JAM / JAMEx
DMS
SR-04B Cal Req
SR-05B Data Proc Req
OPS-03B Cal Plan
Mikulski Archive for Space Telescopes
Instrument Website
Instrument Data Handbook
Help Desk
GSW-01B Data Pipeline Inputs
GSW-02B Reference Files
Cal & Com WG
Cal Pipeline WG
NIRISS Team: Working Groups at STScI
Working Group
Proposal Planning
Lead
Backup
Products
Fullerton
Goudfrooij
Reports; Refined Concepts; Improved APT
Goudfrooij
Fullerton
Reports; Refined Ops Concepts; Cross-instrument Ops
Martel
Volk
Reports; Algorithms; Reference Files; etc.
Volk
Lead: Dixon
Martel
Reports; User Handbooks
Fullerton
Goudfrooij
Reports; Improved Ops Concepts
Martel
Fullerton
Reports; Training; Test Support
Forum to discuss all aspects of
proposal planning from the
perspective of a user
Operations
Development forum for cross-SI
issues
Calibration & Commissioning
Design/Evaluate algorithms
Oversee creation of reference files
Track calibration error budget
Maintain commissioning plan
Maintain Cycle 1 calibration plan
Define calibration standards
Calibration Pipeline
Test pipeline implementation
Document pipeline
Observatory Efficiency
Maintain SO-DRM 2012
Use SO-DRM to study efficiency and
related issues, including trade-offs
ISIM I&T
Coordinate STScI inputs to ISIM CVs
Coronagraphy & High-Contrast Imaging
Refine ops and cal concepts
Sivaramakrishnan
Reports; Improved Ops Concepts
JAM / JAMEx
Sivaramakrishnan
Reports; Ops and Calibration Concepts
Martel
Reports; Instrument Simulator; Improved ETCs
JWST Backgrounds
Martel
Reports; Algorithms; Data; Improved background model
SID Archive
Holfeltz
Improved ingest process; Improved data retrieval
Explore ops & cal concepts for AMI
ETC Algorithms
Define algorithms for ETC
TIPS / JIM
2013 June 20
What’s Coming Up?
2013–03–01: ISIM Integration of NIRISS / FGS
TIPS / JIM
2013 June 20