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OWLS update: galaxy selection. Feb 2008. CFHT, ugriz magnitudes, D1 field. CFHT, ugriz magnitudes, D3 field. CFHT, ugriz magnitudes, D4 field. G-R vs. U-G, CFHT (D1 sample). (red = zp > 0.3, green = zp <0.3). G-R vs. U-G, CFHT (D1 sample). (red = zp > 0.4, green = zp <0.4).
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OWLS update: galaxy selection Feb 2008
G-R vs. U-G, CFHT (D1 sample) (red = zp > 0.3, green = zp <0.3)
G-R vs. U-G, CFHT (D1 sample) (red = zp > 0.4, green = zp <0.4)
G-R vs. U-G, CFHT (D1 sample) (red = zp > 0.6, green = zp<0.6)
G-R vs. U-G, CFHT (D1 sample) Showing the effect Of “angular” color Cuts in isolating Bkgd sample (Red = zp > 0.3, Green = zp < 0.3 )
CFHT cuts: zp distributions after color cuts (D1 field) Black = all Blue = color-selected foreground Orange = color-selected bkgd
CFHT cuts: zp distributions after color cuts (D3 field) Black = all Blue = color-selected foreground Orange = color-selected bkgd
CFHT cuts: zp distributions after color cuts (D4 field) Black = all Blue = color-selected foreground Orange = color-selected bkgd
U vs. U-G, CFHT D1 Difficult to see in this And all the following Magnitude vs. color Plots how a magnitude Cut will help clean the Sample more than just A color cut as already Shown.
G-R vs. U-G, LBC-SDSS matched objects (red = zp > 0.3, green = zp <0.3)
Umag Dif (SDSS-LBC) Left = without Umag Error cut Right = with Umag Error cut (SDSS Umagerror < 0.5 ) Umag error (x-axis labels are: 0.5, 1, 1.5, 2, 2.5)
G-Diff Left = without Gmag Error cut Right = with Gmag Error cut (SDSS Gmagerror < 0.2 ) Gmag error (x-axis labels are: 0.2, 0.4, 0.6, 0.8)
R-Diff Rmag error (x-axis labels are: 0.2, 0.4, 0.6, 0.8) Left = without Rmag Error cut Right = with Rmag Error cut (SDSS Rmagerror < 0.2 )
For reference: Comparing Iso Mag vs. Aperture Mag (g-band), LBC