head 1.1; access; symbols; locks http:1.1; strict; comment @# @; expand @b@; 1.1 date 2004.01.28.13.38.25; author NicholasWalton; state Exp; branches; next ; desc @none @ 1.1 log @none @ text @ࡱ> 8 9 !"#$%&'()*+,-./01234567Root EntrydO)zPowerPoint Document(3SummaryInformation(2DocumentSummaryInformation8( `/ 0DArialNew &(0(z[ 0 "DTimes New Roman(0(z[ 0 @@ .  @@n?" dd@@  @@@@`` ($ 0z$ 0AA@@ʚ;ʚ;g4BdBd@@z[ 0 ppp@@ <4ddddl 0&80___PPT10 ?  %h  ` 33` Sf3f` 33g` f` www3PP` ZXdbmo` \ғ3y`Ӣ` 3f3ff` 3f3FKf` hk]wwwfܹ` ff>>\`Y{ff` R>&- {p_/̴>?" dd@@,|?" dd@@   " @@ ` n?" dd@@   @@@@``PR    @@ ` ` p>> f(    6b  `}  T Click to edit Master title style! !  0  `  RClick to edit Master text styles Second level Third level Fourth level Fifth level!     S  0` ^ `  >*  0 ^   @@*  0 ^ `  @@*H  0޽h ? 3380___PPT10.; Default Designg ~v y(  r  S p>  r  S  `    p 0V6 y #"" " <l??_V6 @@  @@` ! <?+ _6 >rAdd time axis Produce time-SED table Visualize time SED Model fit (see above cases) Variability tests and modelinge  ## # #  ## ##  # $$   <@@p?_+ 6 !Spectral time variability of AGNs$"!#  <]? V_ 8Provide stellar spectra libraries Spectral res. metadataP" !## #  ~  <HI?+ _ ~Same as above Access stellar spectra libraries Convolve model with spectral resolution as well as other instrumental responsespq  ## # #  O#  <4? + _ oDetermine stellar population parameters (age, metallicity, mass) plus internal kinematics from high res spectraP(H '## G#  ,. + E  <#?uV  aProvide instrument function Service for generating standard models with users provided parametersTF ## E# #  C  <x?+ u  KAstrometry visualizer Propagation of errors Use standard SSP libraries (e.g. Bruzual & Charlot; Pegase; starburst99) Service for generating standard models with users provided parameters Allow user to upload/publish models in the VO Convolve model with instrument function Generate SED from archival data Fit convolved model to SED6 ## # #  H## E## - # $#$ '(#(,#, 0#04#4 8#8<<P 8N  <?u+  LDetermine stellar population parameters (age, metallicity, extinction, mass)P(% '## $#  .   <?0Vu TArchive Requirements$#  <,?+ 0u PAVO Requirements$#  <$?0+ u L Science Case$ #ZB ) s *1 ?0V0ZB * s *1 ?6V6ZB + s *1 ?06ZB , s *1 ?V0V6ZB / s *1 ?uVuZB 1 s *1 ?+ 0+ 6ZB 4 s *1 ?06ZB 8 s *1 ? V ZB E s *1 ?_V_H  0޽h ? 33___PPT10i.=+D=' = @@B +f }u0#  (   x  c $>  x  c $ `     h U+o #  #"K6q    <?)+o > @@`   <@@? )o > @@`   <?U) o > @@`   <?+) g'Provide PSF/ beam information in images$('#d   <M? )  Cross ID statistics  expected number of outliers; probability for each ID Source detection / extraction should make use of PSF info. Take into account instrumental beams and source extension in cross-ID Allow filtering options during cross-ID Morphology asymmetry measureK J## :# #  E## '##  # $#$ 2   <