1. Status of the JWST mission, and planning (AGN) observations
Alvaro Labiano Ortega
La Laguna, Oct 27, 2016

2. Acknowledgements
All along this presentation you will see results from work conducted by a large number of teams in Europe, USA and Canada.
Many (most?) elements of this presentation are based on existing presentations prepared by other members of the JWST instrument teams.

3. JWST Key Figures James Webb Space Telescope
joint ESA-NASA-CSA collaboration
One of the “great observatories” of the next decade.
>15% total observing time to ESA state applicants.
6.5 m Diameter Primary Mirror
18 hexagonal Segments (1.3 m flat to flat, Beryllium)
Spatial Resolution: 0.02”-0.9”
Observable Wavelength: 0.6 μm-28 μm
Operating Temperature: < 50 K
Passive cooling with sunshield of 22 m x 10 m
Active Cooling to 7 K for MIRI
Launch: Oct. 2018, Ariane V.
5-10 years mission.

4. Coming Together! OTE/ISIM TESTING Cryo Optics Test ISIM I&T
Completes 2017
OTE/ISIM
TESTING
Cryo Optics Test
Completes 2015
Completes 2016
ISIM I&T
Spacecraft Panel I&T
OTE
I&T
Sunshield I&T
OTE Structure I&T
Spacecraft Element I&T
Facility
I&T Responsibility
Execution
GSFC
NGAS
ITT
ESA / Arianespace
Completes 2018
Complete Observatory I&T
Launch Site I&T
LV Integ
Launch
Completed
Sunshield Pathfinders (EPF/IVA)
Observatory EM Test Bed (EMTB)
Completed 2014
OTE Pathfinder
Structure
Pathfinder Optics Integration
Pathfinder Cryo Optics & Thermal Tests
Propulsion Module I&T
JSC
N/A
Oct. 2018

5. OSIM ready to be delivered…

6. … to Johnson Space Center

7. JWST Observing Modes

8. NIRCam JWST’s primary visible and near-IR wavelength imager
Low-res slitless spectroscopy, and Lyot coronagraphy
Two fully redundant MODULES A/B, each 2.2’ x 2.2’ separated by 44”, observing simultaneously.
Each module has one SW ( μm) and one LW ( μm) channel that have the same 2’ x 2’ FoV
SW channel has four pixel SCA separated by 5 arcsec; LW has one pixel SCA
Pixel scales of 0.032″/pix and 0.065″/pix provide Nyquist sampling at λ = 2.0 and 4.0 μm in the short- and long-wavelength channels, respectively. The short-wavelength channel provides five wide-band (R ~ 4), 4 medium (R~10), and three narrow-band (R~100) filters, while the long-wavelength channel contains three wide, eight medium, and four narrow-band filters.
, coronagraphy for high-dynamic-range imaging of faint sources near bright sources (e.g. exoplanets or debris disks), and slitless spectroscopy at 2.4–5 μm with a resolving power R ~ 1700.

9. NIRCam FoV
If full-field imaging is not required, individual modules or smaller subarrays may be used to increase readout speeds and reduce data volumes.

10. NIRCam Imaging

11. NIRSpec
Multi-object dispersive spectrograph, including single-slit, an integral field unit, and multi-object mode.
The multi-object mode allows for simultaneously observing more than 100 sources over a field of view (FOV) larger than 3 arcmin square
NIRSpec's IFU consists of 30 slices, over a region 3”x3”, with spatial sampling every 0.1 arcsec.
Several conventional fixed slits (largest 1.6”x1.6”)
Detectors: Two Teledyne Hawaii- 2RG; HgCdTe arrays with 5.3μm cutoff; 2048 × 2048 pixels each
Overall eld of view: 2.2 × 2.4 arcmin
Plate scale: arcsec/pixel
Dispersers: One prism (R=100) and two sets of gratings (R=1000 and 2700)

12. NIRISS
Near-InfraRed Imager and Slitless Spectrograph (NIRISS) [+ Fine-Guidance Sensor (FGS)].
Wide-field slitless spectroscopy with R~150 from 1.0 to 2.5 µm, with two orthogonally-oriented grisms.
Single-object cross-dispersed slitless grism spectroscopy with R~700 from 0.6 to 2.8 µm.
Aperture-masking interferometry at 2.7 & 4.8 µm.
Broad-band imaging across its 2.2' x 2.2' field between µm.
Functionally independent

13. Mid Infrared Instrument
Only instrument covering wavelengths > 5μm
Coldest instrument at 7 K requiring a dedicated cooler
4 instruments in one
Classical Imager with 9 filters, 5-25μm, 74" x 113"
Coronagraph
Long Slit Spectrograph
Integral Field Spectrograph

14. MIRI Focal Plane Overview
1 arcminute
Three 4QPM Coronagraphs
24 x 24 arcsec
Low Resolution Spectrometer
5 x 0.6 arcsec
Imager
75 x 113 arcsec field
0.11 arcseconds/pixel
Nyquist sampled at 7 mm
R ~ 3000, 4 Channel Integral Field Spectrometer
Lyot Mask 23mm
30” x 30”
MIRI FM Imager
Channel 1 & 2
Channel 4 & 3
MRS: diffraction limited integral field spectrograph from 5 to 28.5 μm.
The light get s split into 4 channels, each with 3 sub-bands.
Concentric FOVs on the sky ranging from 3.7”x3.7” to 7.7”x7.9”, and slice widths from 0.18” to 0.64” (scales with diffraction limit)
6.7
10.2
15.7
24.5
l/ mm
l/ mm
l/ mm
5.6
8.6
13.3
20.5 14

15. MRS-Imager Simultaneous Observations (SIMO)
Imager has better PSF and larger FoV -> We can refine the MRS astrometry!
Very useful for dithers, mosaics, and deep observations:
Combine cubes of faint or undetected sources from different visits
Mosaics of diffuse emission
Serendipitous discovery of asteroids.
Extra data for only 30 seconds per filter!
[≠ parallel]
Are overheads TBC?
More details on Macarena and Alistair talks 15
Image: STScI

16. Focal plane map

17. NIRCam – MIRI parallels
JWST will offer limited coordinated science parallels in Cycle 1
Pure parallel GO programs will be also available

19. Spectral power

20. Ferruit– ESAC 16, Milam+15

21. JWST Science Programs

22. Four JWST science themes
End of the dark ages: First light and reionization
Assembly of galaxies
Four JWST science themes
Birth of stars and protoplanetary systems
Planetary systems and the origin of life

23. JWST Science Programs Guest Observer (GO programs)
Open access for the community
~80% of time in Cycles 1 through 5
Guaranteed Time Observer (GTO) programs
4020 hours allocated over first 30 months (i.e. Cycles 1 through 3)
NASA policy constraints on time/cycle
Director’s Discretionary Time (DD) programs
Up to 10%/cycle i.e. ≤877 hours
Rapid response observations & targeted science programs, such as Early Release Science program
Reid- Science Policies – ESAC 16

24. JWST GO Program Types
4 size categories: Small, Medium, Large, Very Large; with a balanced distribution in over all cycles
Especialized categories:
Long-term programs  Science requires observations in future cycles.
Treasury/Legacy programs  Broad science reach, providing higher-level data products for the community.
ToO programs.
Archival & theory research programs.
Joint programs with other facilities will not be available until Cycle 2.
STScI and JSTAC continue to refine these.
STScI anticipates…
Reid- Science Policies – ESAC 16

25. GTO proposal submission
GTO proposal submission deadline is April
Cycle 1 GTO comprise 25% to 49% of the total time available to GO & GTO in Cycle 1
~5500 hours remain for Cycle 1 GO programs (similar to HST GO time/year)
A full list of GTO Cycle 1 targets will be published by June
GTO programs have priority on specific observations of specific targets. A full list for Cycle 1 will be made available to the community no later than June
Reid- Science Policies – ESAC 16

26. Early Release Science (ERS)
Accelerate the diffusion of JWST know-how, to maximize the science return of the mission.
Expand early opportunities for the community to gain experience with JWST data and scientific analysis.
ERS programs are pathfinders for the community: How will you help your colleagues exploit JWST?
In addition to immediate release of data, ERS activities provide focal point for organization of GO user support and dissemination of information on JWST performance and results.

27. STScI Director Ken Sembach will allocate ~500 hours of Director’s Discretionary time for an Early Release Science (DD-ERS) program to prepare the community for Cycle 2
Resources are allocated to support up to 15 teams. Proposals will be selected in research areas spanning the science themes of JWST :
A multi-disciplinary committee of experts will recommend a suite of proposals that both fulfills the goals of the DD-ERS and makes optimal use of the available time for observation and funding.
Reid- Science Policies – ESAC 16

28. JWST Science Timeline – Sep 16
DD-ERS NoI due 2017Mar03
DD-ERS TAC 2017Oct
GO CP
2017Nov30
GO Cy1
deadline
2018Mar02
ERS Call 2017Apr01
Call for DD-ERS Notices of Intent ERS draft call
2017Jan06
commissioning
(6 mo)
DD-ERS
deadline
2017Aug18
GO TAC
2018May
2016
2017
2018
2019
GTO Call
2017Jan06
launch
2018Oct
Cycle 1 obs. begin
2019Apr
GTO APT
submissions
2017Sept01
GTO
props due
2017Apr01
GTO Cy1
observations
published
2017Jun15
Detailed schedule subject to change
Reid- Science Policies – ESAC 16

29. Summary JWST is on its way All Instruments perform really well
Most hardware built
Key critical technology is developed and tested
Sufficient Schedule margin to meet launch date 2018
All Instruments perform really well
Optical performance is excellent
All effects well characterized
Data reduction and analysis tools coming
Calls for proposals next year!

30. Thank you Image & Video Credits:
NASA/Goddard Space Flight Center, NASA/Northrop Grumman, Scientific Visualization Studio, MIRI European Consortium, ESA, EADS, STScI, CSA

31. DD-ERS proposal requirements (not your standard GO proposal…)
Justification for ERS time
How will your program help the community learn to do science with JWST and prepare for Cy2? What science-enabling products are proposed for development and release? How will your program demonstrate baseline JW science capabilities?
2. Project Management Plan & Budget
Data processing and analysis plan, roles, responsibilities, work schedule, budget. Identification of core team responsible for science-enabling product development and delivery.
3. Scientific Justification
Why are the observations scientifically compelling and require JWST?.
4. Description of the Observations
Establish feasibility for early execution, and flexibility in target selection to accommodate any change to start date for Cy1 science obs.
5. Team Diversity
Description of how the proposing team represents and has input from diversity of experts with broad demographics within sub-discipline
Reid- Science Policies – ESAC 16