1. APT Overview for Transiting Exoplanet Proposals Chris Moriarty – APT Developer

2. Outline Overview of using APT for JWST APT support for Transiting Exoplanet Proposals Example realistic JWST Exoplanet Proposal

3. APT for JWST Single Stream Processing – Rather than the two phase HST process – Proposals now will be “Flight Ready” APT already supports JWST proposals – Free Beta testers are most welcome

4. JWST Proposal Unlike HST proposals, where individual exposures are defined, JWST proposals are similar to Spitzer proposals, where individual observations are defined. Observations allow one Template – Structures the forms per science use case.

5. JWST Templates Selected based on an observing strategy (e.g. MIRI imaging, MIRI low resolution spectroscopy) – First select instrument. – Then select observation strategy. Provides only the necessary information to generate the observing sequence to execute on the telescope. – Including somewhat standardized concept of exposure specifications

7. Exposure Specifications Part of Template in which you specify how one or more exposures will execute. Note – One exposure spec does not imply only one exposure – Ex: When Mosaics and Dithers are used. Templates have either Single or Multiple exposure specs – Ex: Changing Filters. Exposure Time Calculator (ETC) helps craft exposure specs.

8. JWST Visits Set of exposures (with overheads) obtained on the same Guide Star without scheduled interruption. APT manages visits for you based on the specification of the Observation. – Automated visit splitting Visits in APT are not editable.

9. Observation Target Instrument Template Exposure Specification Template Specific Fields JWST Proposal Targets Target1 Target2

10. JWST Proposal Targets Target1 Target2

11. Visit 3 Visit 2 Observation JWST Proposal XML Times Report Pointings Report Visit 1 Data Volume Durations Visualization Visit Planner

12. Exposure Specification Terms Number of Integrations – Single set of non-destructive samples of the detector. – “Sample-up-the-ramp” – Each integration is preceded by a reset. Each integration consists of one or more group – Which is made up of one or more frame. A frame is a non-destructive read of the signal on each pixel. Readout Pattern is how the frame is read out – Instrument dependent

13. INTS & GROUPS

14. Special Requirements Tab Add timing, offset and other constraints

15. Templates for Exoplanets Niriss Single Object Slitless Spectroscopy Miri Low Resolution Spectroscopy Nirspec Bright Object Time Series Nircam Time Series Nircam Grism Time Series

16. Niriss Single Object Slitless Spectroscopy Foreseen to be used for high-cadence spectroscopic observations of single bright stars of late spectral types (e.g., M, K, G) with magnitudes in the range 6 ≤ J ≤ 15.

17. Miri Low Resolution Spectroscopy The mode has been designed specifically for compact (<2”) or point sources, and will be critical for high redshift and Kuiper belt objects (when used in the background limited case).

18. Nirspec Bright Object Time Series Used to study high S/N spectrophotometric observations of exoplanet transits

19. Nircam Time Series Used to study high S/N spectrophotometric observations of exoplanet transits, stellar occultations, and solar system observations.

20. Nircam Grism Time Series Used to study high S/N spectrophotometric observations of exoplanet transits, stellar occultations, and solar system observations.

21. Rules of Thumb Bright Targets could saturate the array – Example: Greater than J = 7 Long transits may not be practical – Example: Greater than 5 hours. Sensitive Observations – 30 minute settling period before observations – “NO PARALLEL” special req recommended

22. In the near future, within our own galaxy, still pretty far away…

23. SODRM 3054 OBSERVING TEMPLATE: NIRISS SOSS Characterize the atmosphere (composition and structure) of several exoplanets using NIRISS transit spectroscopy. The observations will begin with a target acquisition to position the star precisely at a predefined location on the array. Then the G700XD element will be inserted into the beam. A long, uninterrupted sequence of several integrations will then be acquired spanning twice the transit duration (to get sufficient off-transit baseline coverage) and approximately centered on the mid-transit time with a 30 minute settling period allocated at the start of the observations. Individual sequences will typically last for 3-9 hours.

24. Proposal Details NIRISS Single Object Slitless Spectroscopy NIRSRAPID Readout Pattern 15 targets – The 5 brightest systems with a hot Jupiter. – The 5 brightest with a hot Neptune. – The 5 brightest with a hot super-Earth.

32. References and Links Download APT – http://www.stsci.edu/hst/proposing/apt JWST APT Proposal Instructions – http://www.stsci.edu/institute/org/oed/JWST_PPS_Design/proposal_instructions_html Exposure Time Calculator – http://jwstetc.stsci.edu/etc/ Beichman, Charles, et al. "Observations of Transiting Exoplanets with the James Webb Space Telescope (JWST)." Publications of the Astronomical Society of the Pacific 126.946 (2014): 1134-1173 SODRM Proposal 3054