From 3cb6627b07b41d1a80dcb021e6a001ee914bab84 Mon Sep 17 00:00:00 2001 From: jemorrison Date: Mon, 5 Aug 2024 12:36:18 -0700 Subject: [PATCH] updates to doc --- docs/jwst/tso_photometry/description.rst | 18 +++++++++++------- 1 file changed, 11 insertions(+), 7 deletions(-) diff --git a/docs/jwst/tso_photometry/description.rst b/docs/jwst/tso_photometry/description.rst index efc5321265..75b5a8fea9 100644 --- a/docs/jwst/tso_photometry/description.rst +++ b/docs/jwst/tso_photometry/description.rst @@ -31,13 +31,17 @@ the times will be computed from the exposure start time, the integration time, and the number of integrations. In either case, the times are Modified Julian Date, time scale UTC. -If NaNs exist in the source or background annulus the NaNs are masked out -and the TSO mode photometry will not will not return NaN. -This is different than photometry for imaging mode where a NaN value is returned. -For TSO data it is easier for single pixels to be affected in a given integration -and science analysis will be focused on variability of one source. -In the imaging case the most likely cause of NaN pixels in the annuli -is NaN-valued central saturated pixels in an image with many sources. +If NaNs exist in the source or background annulus, they are masked out and the value +returned is the sum over the real-valued data. +This is different from the convention for photometry in standard imaging mode: +in that case, a NaN value is returned if it is present in any of the pixels in +the source aperture. In the imaging case, the mostly likely cause of NaN pixels +in the aperture is NaN-valued central pixels for a saturating source in an image +with many sources. nFor TSO data it is more likely that single pixels are affected +in a given integration and science analysis will be focused on variability of one source. +If NaNs are present, the absolute flux will be underestimages, the relative values may still +be useful. + The output table contains these fields: