TASK LIST (Summer 2007 / 2007-08 academic year) ----------------------------------------------- URGENT! --> - ApJL on statistics of metal rich streams . What's the status of competing/complementary Font et al paper? *** Karrie will email? - DEIMOS spectroscopy of new DDO51 halo fields (R4/R6, outside S quadrant) . Status of Rachael's scripts? *** Karrie/Raja to email Rachael? . Goals for Karrie's UVa visit . DEIMOS mask design - Strategies for improving yield in DDO51-selected outer halo fields . Changes in dsimulator priority scheme . Longer exposures . Complementing the MMT/Hectospec survey - RGB / dwarf separation in the eight M31 dwarf satellite fields . Merge photometry table with table of velocities and line strengths for all dwarf satellites - after Jason sends dSph phot *** Jason . Evan's X_CMD, Y_CMD, and Fe/H_phot calculation . L pipeline - SB profile from counts of spectroscopically confirmed M31 RGB stars . Need RGB/dwarf separation in dwarf satellite fields (above item) . Finish I mag suppression factor calculations, correct for CMD- (i.e. color-) based selection of And X targets . Make remaining figures! *** Raja . Write text! - And XIV photometry from Keck/DEIMOS images - to be added to Marla's followup up paper - Kinematics of NE and W shelves . Photometry and astrometry of NE shelf with Rachael . Photometry and astrometry of W shelf from Jay's images . DEIMOS mask design . Trethewey is working with Chapman at IoA. No clear detection of W shelf from 3 masks. Ratty data on NE shelf. Collect new data in 2007B? Try to read off their RVs? Combine with m4 result and Mark's latest GSS progenitor model? If they publish NE and W shelf velocity and Fe/H distributions before us, we can still publish our data within the paper(s) Mark is writing on the GSS modelling - just not a stand-alone one. - Kinematics / metallicity in m4 (Priya) . Nature of "Stream C" . Mark's new GSS simulation with a rotating satellite . Update on Trethewey/Chapman spectroscopy of "stream C" at R ~ 60 kpc on the SE minor axis - directly relevant to m4 project. They see two peaks in the RV distribution: v ~ -280 km/s metal poor; v ~ -350 km/s metal rich with large Fe/H spread. This is *exactly* what Priya sees as well! LESS IMMEDIATE --> - Results of telecon with Kathryn, James, and Steve (May 21, 2007) . Comparison of Via Lactea to Johnston/Bullock simulations - former is DM only whereas latter models baryons in dwarf satellites - need to understand this distinction better. Via Lactea is fine for general radial anisotropy study, but not for statistics of substructure? . Their understanding is Karrie will be "observing" their simulations using the parameters (fields, sampling density) of SPLASH . Kathryn's student will look into constraints on the (virial) mass of M31 using the most current / complete set of available tracers - a la Evans et al (2000) - try various *assumed* tangential velocity vectors for M31 in anticipation of our upcoming measurement . James and his student want to do an M31 live disk simulation + GSS progenitor to explore warping / heating of extended stellar disk - have asked him to coordinate with Mark's simulations (GSS progenitor -> central bar -> star-forming ring) - Metallicity trend in the inner spheroid / outer halo transition zone (Jedidah) . Ping Jedidah about star by star metallicity vs radius plot - Response to Koch et al Bonn poster on Gilbert et al 2007 sample . May need to respond right away if Koch et al decide to proceed with a publication . Compare spectroscopic metallicities of stream wraparound debris (and spillover?) on SE minor axis to those of GSS and dynamically hot inner spheroid: Is there a dramatic (1 dex!) radial gradient in the inner spheroid at R ~ 20 kpc as claimed? Is the inner spheroid much more metal-rich than GSS (H13s) as claimed? . See note on CaT-based metallicities below - What is the best way to measure the CaT line strength? . This seems to fit most naturally as a section in one of Evan's papers . Trying coadding CaT lines a la Koch et al - compare to EWs measured as we have in the past with standard weights. Try adding ivar weighting. Use higher S/N Leo I spectra to test effect of Poisson noise. . Try measurement via xcorr of high S/N stellar templates. Use best fit template from spec1d fit. Adjust strength of CaT lines in the template to best match the data? Test something like: [f_nt(\lamb) + x]/(1 + x) where f_nt(\lamd) is the template spectrum with the contimuum normalized to unity in the CaT region. . Monte Carlo error realizations to degrade high S/N spectra (Leo I and/or xcorr templates) to quality (and RV) of each program star - use these to test/compare the different CaT EW measurement methods: our old direct EW method, Koch's line coaddition method, and the xcorr-based method. . Important to obtain careful CaT EW error estimate for each star for Fe/H spec vs phot analysis (see below). - Fe/H spec vs phot analysis . For M31 coadds, make statistical use of the Brown et al MSTO-based age-vs-Fe/H space distributions for inner spheroid, GSS, and (ultimately) halo. Goal: constrain alpha/Fe. Is a logical part of Evan's thesis. . Can this be tried on the dE spectra? Leo I spectra? - Velocity dispersion profile . Way to account for "velocity masking" (or dwarf satellite members, substructure) in the construction of a global velocity histogram - Tangential motion . Plot of delta radial velocity vs azimuth for all tracers (RGB stars, dwarf satellites, GCs) - with symbol size proportional to project radial distance(?) - cut out dwarf satellites and various known substructures - is there a way to account for this velocity masking? . Repeat for various assumed tangential velocity vectors and attempt to detrend and minimize scatter - Organization of SPLASH data (undergrads?) . Installation of zspec (and spec2d/spec1d?) at UCSC *** Marla . Homogenizing the reduction of *all* masks - "delta zspec" of masks already zspec-ed - i.e. focus only on *changes* in velocity or zq resulting from use of Marla's code . Web page design - Improvements to L pipeline (Priya?) . Empirical PDFs . Better matched (more finely subdivided) training sets . Development and use of all 10 *independent* diagnostics - Evan's thesis projects . Design DEIMOS masks for bright GC stars for which detailed chemical abundances have already been measured using HIRES (e.g. M3, M13, M15) . Improvement of dE photometry using (pending) CFHT MegaCam data - Deconvolution of inner bright elliptical portion of star count map into inner spheroid vs disk . Write short ApJL? . Use our data + *all* published RVs from Ibata/Chapman group . Arguments: (1) broad RV distribution in minor axis fields [and underlying dynamically hot (non-rotating on average?) population in all Chapman/Ibata fields?]; (2) predicted SB profiles of inner spheroid and disk (even including possible disk warp) indicate that the disk should be a minor contributor in fields close to the minor axis. ------------------------------------------------------------------------------