Issue Tracker

Optimal background subtraction needs to be decided upon and implemented in CALTSO3

• Optimal TSO Spectral Background Subtraction
  

Continuous Integration / Unit testing

• We need to develop a standard set of tests that automatically run on the calibration pipeline whenever there is an update.

ISIM clock is not precise enough for TSO, need to use FPE clock for relative time and S/C clock for reference point

Target acquisition needs to be implemented in APT

Enable TSO mode for MIRI imaging

Tests show long persistence ramp in TSO data, no easy means to pre-flash detector

• Do we need tests during commissioning?

Enable MRS TSO mode

• Caution: data volumes could be too high

Enable SW DHS spectroscopic mode

Enable narrow-band filter option for target acquisition

Enable TA on saturated targets

How do we ensure the target falls in the 1.6” aperture before TA?

Enable WATA on saturated targets

Enable WATA with NGROUPS=1 or 2

Enable mode to use F277W filter to remove spectral overlap as a calibration

Need bias and 1% saturation levels to make target fluence recommendation to observers

NIRCam recommendation: ~35k ADU

No values from other teams

Needs brightest pixel listed in output

APT may be slow to run Visit Planner for short period planets

• Visit planner in APT 25.4.4 gets stuck (or is slow) for some short-period planets
• Karla Peterson and Everett worked out a solution where he multiplied the planet period by 5 and then it works pretty smoothly and since the period is so short there are still plenty of starting windows.
• If this problem persists in APT, perhaps we should have a note somewhere in JDox (and/or APT) that explains this workaround (multiply the period by a small integer) to users for short period ephemerides?

For very long exposures, the APT visit planner fails to satisfy the phase constraint.

• See JWST program 1201 (NEAT), observation 11 (phase curve observation of WASP-121b)
• The phase constraint is correctly set, but the calculated visibility periods do not satisfy it.
  
• The problem appears whenever t_exp > P - w -1048, where t_exp is the total exposure time, P is the planet period, and w is the time width of the of the observing start window specified in the phase constraint, all in seconds.