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--- tests:astropars:challenge1 [2014/10/31 13:43] – [FAKE GROUP GENERATOR] randrae
+++ tests:astropars:challenge1 [2022/10/24 12:26] (current) – external edit 127.0.0.1
@@ Line 18: / Line 18: @@
 (Zuckerman & Song 2004) around the solar peculiar motion.
+{{:tests:uv_groups.png|}}
 Unlike open clusters, association members are very sparse, with their nearest
 stellar neighbours highly unlikely to be group members.
+{{:tests:groupc_xy.png|}}
+{{:tests:groupc_xz.png|}}
@@ Line 30: / Line 35: @@
 over-densities in distance-velocity space (e,g, near U=0 km/s,V=0 km/s).
+{{:tests:groupc_uv_.png|}}
 However, it’s necessary to consider full 3D velocities, as the over-densities are
 not always apparent in some projections:
+{{:tests:groupc_uw_.png|}}
+{{:tests:groupc_uwmemb_.png|}}
 This could obviously be automated with well-known clustering methods.
@@ Line 42: / Line 51: @@
 km/s at these distances and spectral types:
+{{:tests:groupc_rverr.png|}}
+{{:tests:groupc_rv.png|}}
 This has the effect of smearing out the UVW over densities, reducing their contrast
 over the background field stars.
 Young stars are typically several magnitudes above the main sequence and well
@@ Line 85: / Line 97: @@
-{{:tests:cmd_groups.png|}}
-{{:tests:groupc_rverr.png|}}
-{{:tests:groupc_rv.png|}}
-{{:tests:groupc_uv.png|}}
-{{:tests:groupc_uwmemb.png|}}
-{{:tests:groupc_uw.png|}}
-{{:tests:groupc_xy.png|}}
-{{:tests:groupc_xz.png|}}
-{{:tests:uv_groups.png|}}