Collaboration Priorities

  • Crowded­ field photometry/astrometry (Example action items: DECam precursor studies of Galactic bulge/plane to estimate the source density as a function of position; Use ImSim pipeline to create synthetic images of crowded fields and test LSST’s astrometry and photometry on resultant CMDs).
  • Star­galaxy separation (Example action items: HST archival project to generate a point source/extended source truth table; Use of SMASH survey of Magellanic Clouds to empirically benchmark impact of unresolved galaxies on LSB structure mapping; Multi-color deep wide­field surveys of known LSB systems to test star­galaxy separation algorithms; Use ImSim input catalog to test star­galaxy separation algorithms).
  • Photometric metallicity calibration (Example action items: Assemble relevant spectral and photometric datasets. Compare to existing efforts from SDSS, including Ivezic metallicities for FGK stars, and Mann, Lepine and West calibrations for M dwarfs. What are the ranges in mass/color where these relations are valid? Extend these applications to LSST, assuming a LSST­SDSS transformation is robust. Using archival spectra or PanSTARRS data, test how y­band photometry can improve the photometric metallicity estimate. How can time­series information be used to improve metallicity estimates (e.g., Miller, Richards, Bloom et al).
  • y4 filter calibration (Example action items: Ground based/space based y4 investigations; Can PanSTARRS experience be leveraged for y­band calibration? How does varying the water column change the spectral response. SImulate the effect of a varying water column on the y4 filter using existing spectra of FGKM stars.).
  • Cadence Planning (Example action items: Build the case for Magellanic Clouds cadence; Develop the science and technical case for MW disk and bulge cadence; Develop and test cadence metrics for astrometry).
  • Stellar variability classification (Example action items: Define classification metrics required for your specific science goals, see example in Near­Field Cosmology roadmap; Develop light curve classifiers + period finders and test on existing datasets [e.g. LINEAR]; coordinate with Transients science collaboration and tools from EB factory ­ general purpose light curve classifier and intelligent period finder; DECam Bulge survey).
  • Subgroup ­specific technical needs (Action items: As defined by individual collaboration members and Working group leads, e.g. photometry of nebulae.).
  • Theoretical predictions for LSST Milky Way science (Example action items: As defined by individual collaboration members and Working group leads, e.g., simulations that make predictions for LSST; coordinate with Justin Read’s Gaia challenges).