Subject: LSST stellar populations panel summary

From: Knut Olsen

Submitted: Wed, 26 Mar 2003 01:20:22 -0400

Message number: 103 (previous: 102, next: 104 up: Index)

On March 19-20, we met in Tucson to discuss in depth the stellar
populations science case for LSST.  In attendance were You-Hua Chu (by
phone), Chuck Claver, Kem Cook, Andy Dolphin, Raja Guhathakurta,
Rodrigo Ibata (by phone), Dave Monet, Knut Olsen (chair), Ed
Olszewski, Abi Saha, and Nick Suntzeff (by video).  As a result of our
discussions, we have produced an outline which describes what we
believe are exciting stellar populations projects that will be possible
with
LSST.  The projects are organized around two broad themes, 1) the
structure and accretion history of the Local Group, and 2) expanding
the solar neighborhood through astrometry.  We also have projects that
do not fit neatly within either theme, but that we also found
important.

We aim to produce a first draft of a detailed document following this
outline by April 30.  We will devote 2-3 pages to each of the items
below, which will include a description of the scientific motivation and

a discussion of the science requirements, following the format which
Michael
Strauss presented to the SWG and included in his latest message.
We have placed the initials of people with writing responsibility next
to
each item; while we do not have any unclaimed items, we welcome
participation
from any interested member of the SWG.  Please contact Knut Olsen
(kolsen@ctio.noao.edu) if you would like to contribute.



Outline of the LSST stellar populations panel discussion
========================================================

  Participants: YC,CC,KC,AD,RG,RI,DM,KO,EO,AS,NS

Introduction - KO
------------

  New observational parameter space:
  - the combination of deep photometry and accurate astrometry as a
function
    of time
  - ultra-wide field

Structure and Accretion History of the Local Group
--------------------------------------------------

  1.  Milky Way halo-
      - the distant halo-EO
      - the nearby halo-DM
  2.  The MWG and its dwarf galaxy system (incl. MCs)-YC+RG+RI
  3.  M31 halo-RI+RG
  4.  The dwarf galaxies within 4 Mpc-AD+NS+AS

Expanding the solar neighborhood through astrometry
---------------------------------------------------

  Kinematic groups: Galaxy Genesis II-KO+NS

  The stellar luminosity function of:
    a.  10^4 white dwarfs (200 pc volume)-CC+DM
    b.  sub T dwarfs-DM
    c.  the nearby members of the halo-DM

  Planets and companions through astrometric wiggles-DM


Other
-----
1.  Microlensing-KC
2.  Finding all galaxies within ~10 Mpc: the temperature of the Hubble
flow-
    NS+AS+AD+(Alan Whiting)
3.  The variable star zoo-NS+AS+KC
4.  Planetary transits-KC


Format:

2-3 pages
Sections:
A.       Motivation, including uniqueness of problem to LSST
B.       Experimental design and technical issues, including:
   1. Sample size: the area of sky imaged at any given time, and
             the total area of sky to be covered.
   2. The depth and dynamic range needed in a single exposure.
   3. The depth and dynamic range needed in stacked exposure.
   4. Length of individual exposures.
   5. Requirements on slew time.
   6. The requirements on seeing, PSF, and pixel size: uniformity
      of PSF, aberrations of PSF, all as function of wavelength.
   7. The filters needed/on what cadence?
   8. The need, if any, to stack the data
   9. The photometric accuracy needed (both relative and absolute).
   10. The astrometric accuracy needed (both relative and absolute).
   11. Tails of the astrometric and photometric error distribution.
   12. The filters needed.
   13. The cadence of observations needed (very different for moving
       objects and, e.g., distant galaxies).   Should the cadence
       be dynamic?
   14. Requirements of sky darkness and photometricity.
   15. Requirements on the speed of data reduction needed, and the
       nature of the measured quantities.
   16. Auxiliary data needed (e.g., follow-up spectroscopy,
       observations at non-optical wavebands, and/or
       a priori calibrating data)
   17. Specialized data analysis tools needed to carry out the
       science.



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