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--- tests:streams [2015/08/31 14:25] – ahwkuepper
+++ tests:streams [2022/10/24 12:10] (current) – external edit 127.0.0.1
@@ Line 65: / Line 65: @@
   * IDstream: progenitor ID. Stars with same IDstream come were accreted in the same progenitor.
-For a detailed description of how these catalogues were produced, please see go to the [[:tests:streams:challenges:#error-convolved_mock_catalogue_of_individual_halo_stellar_tracers|the Aquarius Error-convolved mocks Section in this Wiki]].
+For a detailed description of how these catalogues were produced, please go to [[:tests:streams:challenges:#error-convolved_mock_catalogue_of_individual_halo_stellar_tracers|the Aquarius Error-convolved mocks Section in this Wiki]].
 The file AqA2KIII.nGC3.IDpole.log is a log that contains IDstream, IDpole and purity. Purity is the fraction of stars in IDpole that come from the progenitor IDstream. Frec is the fraction of stars from the progenitor IDstream that lie in the IDpole detection. The full pole-count map showing the IDpole detections is available [[https://www.dropbox.com/s/ua1cxt5q31u6sfv/AquariusA2KIII.FULL.pe.t2d.mu0.5.new.fx50.ngc3.npa.cl.png?dl=0|here]].
@@ Line 79: / Line 79: @@
 When making use of data in this part of the challenge, please cite the Gaia Challenge Wiki and Mateu et al. in prep.
 For any questions please feel free to contact Cecilia Mateu (cmateu@astrosen.unam.mx). For details about the Aquarius and LJMU simulations please contact Andrew Cooper (a.p.cooper@durham.ac.uk) and Andreea Font (A.S.Font@ljmu.ac.uk) respectively.
+=== Detection of halo streams in the local halo ===
+We provide three catalogs based on high-resolution N-body simulations of the interaction between a
+Milky-Way like disk galaxy within a dark matter halo and orbiting dwarf galaxies with four representative cases of merging histories in term of dynamical friction properties (see [[ftp://ftp.oato.inaf.it/astrometria/paola/InnerHaloModel/mergingsatellites_4.6Gyr.jpg|figure]]).
+These catalogs include the 3D position and 3D velocities of the accreted particles within 3 kpc of the Sun after 4.63 Gyr:
+ * [[ftp://ftp.oato.inaf.it/astrometria/paola/InnerHaloModel/SIMULATION_SATS_HALO_OERR_GAIA.dat | Gaia-like errors for FGK dwars ]]
+ * [[ftp://ftp.oato.inaf.it/astrometria/paola/InnerHaloModel/SIMULATION_SATS_HALO_OERR_GSCII-SDSS.dat | current ground-based errors]]
+ * [[ftp://ftp.oato.inaf.it/astrometria/paola/InnerHaloModel/SIMULATION_SATS_HALO_OERR_TRUE.dat | 'true' values ]]
+The format of the ASCII files is:
+  cols 1-6, x,y,z (kpc), vx,vy,vz (km/s), in the galactic reference frame
+  col 7, particle id, as follow:
+     id=31 counter-rotating satellite, high inclination (60 deg)
+     id=32 prograde-rotating satellite, high inclination (60 deg)
+     id=33 counter-rotating satellite, low inclination (10 deg)
+     id=34 prograde-rotating satellite, low inclination (10 deg)
+     id=1  local smooth halo (mock catalog)
+Further details are given in [[http://adsabs.harvard.edu/abs/2015arXiv150803736R|Re Fiorentin et al. (2015)]].  The N-body simulations are from [[http://adsabs.harvard.edu/abs/2010ApJ...716L.115M | Murante et al. 2010]].
+For any questions please feel free to contact Alessandro Spagna (spagna@oato.inaf.it) or Paola Re Fiorentin (re_fiorentin@oato.inaf.it).
 ===== 3. Determining the Potential=====