Minutes for Telecon for March 11, 2003 Present: Churchwell, Whitney, Meade, Indebetouw, Clemens, Kobulnicky, Stolovy, Wolff, Watson, Marston, Ashman, Babler, Wolfire, Benjamin Team meeting in Madison: April 6-7, 2003. Sunday April 6: 9 am. to 5 pm. Monday April 7: 9 am to noon. QLVT integration with the pipeline--------------------Mark Mark was in Madison Feb 27-28. Tuned some Level A, B, C scripts and programs and the QLVT for data "reinsertion" (e.g. back to Level B for reprocessing if image fails LevelA checks). We have a program that, for each IRAC frame, creates corresponding 2MASS and MSX images for that field which gets carried along with the IRAC frames,for use in the QLVT The QLVT will overlay source catalogs on the images (GLIMPSE DAOPHOT results, 2MASS PSC) and there is a slider to change magnitude limit of the sources overlayed. The QLVT can draw arbitrary regions on an image and put that info into a mask file for later use (e.g. areas of stray light) There is an option to select objects to be removed from or added to the source list. We also have a fairly detailed plan for QLVT interaction with levels E-F (evaluate mosaic images and mosaic photometry). Mark has sent the QLVT to the SSC. The IRAC instrument support team is looking at it. Tony says that a new version of the bandmerger is close to being released. Modified AORs-----------------------------------------Christer OSV region AORs for the new launch date were submitted on 3/1/03. The survey goes from 10 - 65 deg and 350 -295 deg. The OSV AORs were also submitted for the G305.2 region. 4 1/2 height AORs repeated 5 times with different overlaps (8 pix, 10, 12, 15, 20) The 2MASS images have been mosaiced for the G305.2 area. See http://www.astro.wisc.edu/sirtf/2massimages/2massimages.html. The roll angle couldn't be much worse for us. Acute to the galactic plane. Observation set for July 16 -18. Will have resubmit the AORs if it can't be observed then. The roll angle changes rapidly. AORs can be re-run quickly on our end but the SSC needs time to re-schedule. We may have a month's advance notice of a change in the OSV time-frame. The IOC/SV is a very packed schedule. Recent pipeline tests---------------------------------Barb & Marilyn 1. Processing Data -- exercising the pipeline FRAMES (Levels A-C) - ran 12 sets of simulated data Levels A-C for C&R work w/synthetic bkg, with & w/o banding (about 4800 frames) - set-up & ran testcase "aor400" to develop and test QLVT interactions; it has 2 frames which fail (by design) LevelA Checks and 6 frames that fail in LevelC Photometry... MOSAICING - currently mosaicing 2MASS quicklook K images in the survey region for use with the QLVT. Ran on 16 processors over the weekend and completed 60% of the southern hemisphere; northern hemisphere is in work. We also plan to mosaic J, H, and K to the same grid (size, position, pixel scale) as our planned IRAC images. also doing 3-color JHK images of misc. objects of interest, e.g. star formation regions. Some of these images are on the website (G305.2, G333, RCW57). http://www.astro.wisc.edu/sirtf/2massimages/2massimages.html PROBLEMS - Processes go absent (remedy: restart process and delete the absent one); happens in Frame processing and mosaicing - In Levels A-C, occasionally 2 instances of the same process grabs the same frame at slightly different times and runs the process twice. (remedy: need to re-run the frame) - In mosaic, occasionally when opus moves the initial starting files (called the done file, of course) to the data directory, another process file tries to grab it before it gets there, and we see the red x. remedy: change the x to w (wait) and it continues. - what this means is you have to babysit the processes a bit. fortunately, this can be done remotely (i.e., from home) with a lot of patience: OPUS is extremely slow remotely but it's okay for these minor problems. - The mosaic background matching is not perfect, especially in star formation regions. in JHK images, it shows up as color variations across the image (e.g., stars are green in some regions, purple in others). IRAC should not have as much background variation as 2MASS. 2. Pipeline Development Progress (besides QLVT) a. New photometry scripts b. Mosaicing Level EB - mosaicing for product OPUS architecture written, programs written & installed Level EC - mosaicing for photometry OPUS architecture written, hope to have programs written & installed this week Level F - photometry on mosaic images OPUS architecture written, some (most?) programs written, photometry scripts installed. For segment overlap regions with different PSFs, the pipeline will produce 2 different mosaic images with the different segments, and bandmerge those sourcelists. There will probably be a PSF for each segment. and we are assuming the PSF is stable across the IRAC frame. For every source we keep track of which PSF we used. c. Database interaction Full database interaction through Level E (mosaicing) Loads and retrieves images and cat files, log files, etc. after position refinement in LevelC Loads and retrieves results from Photometry to DB master source list (used in Bandmerging) Timestamps used for survey tracking and triggering processes (e.g. levels D-F). 3. Documentation Currently updating flow chart Have not started pipeline description doc Status: Reliability & Completeness Calculations---Christer & Remy Using the simulated w51 region and truth list for comparison. Time was spent getting the bandmerger working outside the pipeline. It's been run on a handful of frames outside the pipeline so far. Still need to run on all the frames. We want to evaluate the Reliability criteria for the OSV data. Hope to have analysis done by the team meeting And want to provide an executive summary to the SSC. Ed says we'd like to write up a clear description of the statistics of the proper way to do C & R when we don't have a truth table and maybe write a paper. There are no papers in the literature on this. Simulated data was made with only diffuse bkg. DAOPHOT is finding a few sources in the diffuse bkg: diffuse knots. Found a few 14th & 15th mag sources. A 1st Cycle 24 micron proposal of selected MSF regions?----------Ed Should we write a Cycle 1 proposal for selected objects? not a big survey. A couple of well-chosen SFRs. Susan is a member of the MIPS team and can give us her expert advise. see Felli et al (2002) and Crowther & Conti (2003) Proposals due at L+5 (September). SIRGAL collaboration----------------------------------Ed Alain Omont will be here the end of March and he will also be in Boston. Science: Massive Star Formation Regions-----------Ed, Barb Identification and extraction of extended regions DAOPHOT extracts only point sources. We will get information on the local source density for each source so can tell if looking at a cluster. Dan: BU will work on this over the summer. They have 2 grad students to work on it. Deriving physical parameters (flux densities, sizes, etc) of extended sources Color selection =>flux densities