- Sarah Kendrew
- Leonardo Ubeda
- Everett Schlawin
- Brian Brooks
- Nikolay Nikolov
- Stephan Birkmann
- Nestor Espinoza
- Knicole Colon
- Jeroen Bouwman
- News & Announcements (all).
- TSO WG work updates:
(a) TSO visits/schedule monitor (Nikolov)
(b) Non-linearity as measured by TSOs (Espinoza)
(c) 1/f noise work updates (Espinoza)
(d) Zodiacal background measurements (all)
- Roundtable check-in (all) – out of time!
1. News & announcements
|2. TSO work tasks updates|
(a) TSO visit/schedule monitor (Nikolay Nikolov )
developed code to run via cron job every 4 hours. pulls from the visit status page. new searching & organisation options. for programs that had failures, we can also see the repeats.
Plan: put somewhere visible to everyone. right now using an internal server in NN's home directory.
Improvement: work better for MIRI; for MIRI is harder to filter. also look at the APT files but that would be slower; right now already takes a while.
Suggestions & feedback welcome!
NE: can parse the PDF of the APT instead of the APT file itself? TSO setting is included in the Special Requirements box in the APT - would make it faster. this is how did the web scraper in the past.
NN: ok can look into it
NN contacted the web team to see if we can host this in a location on the webpages that is accessible to the institute (like JWQL, not open to the world). NE will talk to Mees who has done this for JWQL.
|(b) Non-linearity as measured by TSOs (Espinoza)|
no updates so far - we have measurements from the NIR instruments, need to put this into report. (deadline is not until Sep)
|(c) 1/f noise update||Nestor Espinoza|
reanalyzing all NIR data from commissioning. data looks great. will deliver on characterization + will work on best practices.
part 2 - how to implement into the pipeline. two steps:
1 pre-amp reset (every read has a jump on the pedestal) - for data without reference pixels, the data look v bad. need to get this implemented in the pipeline. working with L Ubeda on this part - testing using the pixels at the edges of the subarrays to correct the pre-amp reset. using different sizes of edge regions. Taking larger region decreases scatter on the time series; but have to trade off against contamination from the source spectrum.
SB: this is not a TSO specific issue - also relevant for other observations.
Need to work with the pipeline to get this included.
|(d) Zodiacal background measurements||all|
plans for better zodiac calibration with TSO modes?
NE: even if background is constant then can still introduce dilution as a function of wavelength that affects the transit spectrum. saw this for NIRISS SOSS. but background might also change during an observation. have we looked at that?
SK looked at it for MIRI (not to huge depth) and did not see any clear temporal variations
NN: also have to consider the quality of the background-only frame: if not high enough precision then we can end up injecting additional noise into the science data. would be constant but would introduce pixel-to-pixel variations.
JB: even if we have a higher px-to-px response due to flat field errors, given the pointing stability, wouldn't affect us too much. but yes, need more dedicated investigation.
NE: understanding shape of the background is very important as allows you to smooth it out. didn't need the strict per-pixel SNR, as the background is so smooth you can smooth it out. Could be 2-stage process together optimal subtraction.
|2 mins||4. Closing Remarks||Sarah Kendrew|
special visitor next week!