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Timestamp:
Mar 1, 2013, 4:10:47 PM (13 years ago)
Author:
eugene
Message:

adding links to flesh out the public data pages

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branches/eam_branches/ipp-20130207/dvodist/ippdata/docs
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  • branches/eam_branches/ipp-20130207/dvodist/ippdata/docs/index.mkd

    r35170 r35219  
    33# DVO Documentation
    44
    5 ## Release Notes on 3pi.20120525
     5(up to [PS1 Data Release](/ippdata/index.php))
    66
    7 This database contains PS1 3pi observations through 2012/01/21.  The
    8 ubercal zero points have been applied to all exposures included in
    9 that analysis.  The remaining exposures have been tied to the ubercal
    10 system via relative photometry.  The ubercal measurements are given
    11 10x their poisson weight to ensure they drive the photometric
    12 solution.
     7Below are links to documentation related to the distributed data
    138
    14 The database has been merged with the PS1 Synthetic photometry
    15 database (based on 2MASS and USNO-B).  For objects brighter than the
    16 saturation limit, the Synthetic photometry has been used for the mean
    17 magnitudes (these can be identified by having bit 0x04 raised in the
    18 mean filter flags).  Objects which used ubercal photometry have the
    19 bit 0x08 raised in the mean filter flags. 
     9* [Photometric Reference Ladder, Release 12.01 Notes](photladder.php)
     10* [Photometric Reference Ladder, Release 12.01 Paper (pdf)](photladder-1206.20121230.pdf)
    2011
    21 This database has also been merged with the 2MASS, WISE, and
    22 SuperCOSMOS databases.  The following photcodes are used for those
    23 external photometric sources:
     12* [PS1 Photometric System](http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/PS1_Photometric_System)
     13* [Tonry et al paper on the PS1 Photometric System](http://adsabs.harvard.edu/abs/2012ApJ...750...99T)
    2414
    25 <table class="page">
    26 <tr><th> Source </th><th> Photcode </th></tr>
    27 <tr><td> 2MASS_J </td><td> 2011 </td></tr>   
    28 <tr><td> 2MASS_H </td><td> 2012 </td></tr>   
    29 <tr><td> 2MASS_K </td><td> 2013 </td></tr>   
    30 <tr><td> WISE_W1 </td><td> 2014 </td></tr>   
    31 <tr><td> WISE_W2 </td><td> 2015 </td></tr>   
    32 <tr><td> WISE_W3 </td><td> 2016 </td></tr>   
    33 <tr><td> WISE_W4 </td><td> 2017 </td></tr>   
    34 <tr><td> SYNTH.g </td><td> 3001 </td></tr>   
    35 <tr><td> SYNTH.r </td><td> 3002 </td></tr>   
    36 <tr><td> SYNTH.i </td><td> 3003 </td></tr>   
    37 <tr><td> SYNTH.z </td><td> 3004 </td></tr>   
    38 <tr><td> SYNTH.y </td><td> 3005 </td></tr>
    39 <tr><td> SCOS.103a.E       </td><td>      1150  </td></tr>
    40 <tr><td> SCOS.4414.OG590   </td><td>      1151  </td></tr>
    41 <tr><td> SCOS.4415.OG590   </td><td>      1152  </td></tr>
    42 <tr><td> SCOS.IIIaF.OG590  </td><td>      1153  </td></tr>
    43 <tr><td> SCOS.IIIaF.RG610  </td><td>      1154  </td></tr>
    44 <tr><td> SCOS.IIIaF.RG630  </td><td>      1155  </td></tr>
    45 <tr><td> SCOS.IIIaJ.GG385  </td><td>      1156  </td></tr>
    46 <tr><td> SCOS.IIIaJ.GG395  </td><td>      1157  </td></tr>
    47 <tr><td> SCOS.IVN.RG715    </td><td>      1158  </td></tr>
    48 <tr><td> SCOS.IVN.RG9      </td><td>      1159  </td></tr>
    49 </table>
    50 
    51 <img width=1000px src="relphot.20120528/sigma.i.ubercal.20120528.v0.png"><br>
    52 Map of the mean per-star residual (inst mag brighter than -10) for
    53 i-band (ubercal data only).
    54 <br>
    55 
    56 <img width=1000px src="relphot.20120528/sigma.g.ubercal.20120528.v0.png"><br>
    57 Map of the mean per-star residual (inst mag brighter than -10) for
    58 g-band (ubercal data only).
    59 <br>
    60 
    61 <h3>Comparison with 2MASS</h3>
    62 
    63 The plots below compare the PS1 grizy photometry with 2MASS photometry
    64 by examining the location of the color-color locus for early (&lt; K0)
    65 main sequence stars.
    66 
    67 For each pixel (0.5 degree on a side), I select all objects with PS1 r
    68 &lt; 20 and detected JHK magnitudes, keeping only those with S/N in
    69 the mean &gt; 50 and standard deviations less than 0.05 magnitudes.  I
    70 then fit the stellar locus in g-r,r-i for the g-r range 0.2 to 1.0,
    71 and keep only objects that fall within 0.05 of that (linear) stellar
    72 locus fit.<br>
    73 
    74 I then fit the stellar locus with a line in each of the color-color diagrams
    75 g-i,i-J; g-i,i-H; g-i,i-K.  I measure the mean i-J color expected from
    76 the fit for stars with g-i = 0.5.  The figures below show the maps of
    77 the i-J, i-H, and i-K offsets as well as the J-H and H-K offsets at
    78 g-i = 0.5.  The center of these maps is RA,DEC = 0,0, (east is left,
    79 north is up).  The pixels are 0.5 degrees on a side.<br>
    80 
    81 These maps show three main features.  The Galactic Plane is quite
    82 clear, and not surprising: this test is particularly sensitive to
    83 reddening. <br>
    84 
    85 Several large scale patches are also visible (eg, the black patch near
    86 RA ~ 150 deg).  Disappointingly, these correspond to areas without
    87 good ubercal ties -- in other words, these are regions in which the
    88 data were obtained in non-photometric conditions.  This shows the
    89 limitation of using relative photometry to tie across individual
    90 exposures.  If the exposures have an extinction gradient, the
    91 correction far from the photometrically tied region can drift from the
    92 correct value.  The largest region at RA ~ 150 matches a section with
    93 poor i-band photometry and has a depth of roughly 0.1 magnitudes in
    94 i-J.  Assuming this is completely due to i-band errors, this
    95 corresponds to about 0.06 magnitudes of drift to the center of this
    96 region. <br>
    97 
    98 The third pattern is at a lower level of intensity: N-S strips with
    99 roughly E-W bands.  They are most noticable in K and H-K.  These
    100 appear to correspond well to the 2MASS scanning pattern, and have an
    101 amplitude corresponding to about 0.02 - 0.04 magnitudes of offset in
    102 K.  <br>
    103 
    104 <img width=1000px src="relphot.20120528/dJ.allsky.20120528.v3.png"><br>
    105 Map of the i-J color at g-i = 0.5.
    106 <br>
    107 
    108 <img width=1000px src="relphot.20120528/dH.allsky.20120528.v3.png"><br>
    109 Map of the i-H color at g-i = 0.5.
    110 <br>
    111 
    112 <img width=1000px src="relphot.20120528/dK.allsky.20120528.v3.png"><br>
    113 Map of the i-K color at g-i = 0.5.
    114 <br>
    115 
    116 Combinations of the above maps can highlight any problems in 2MASS
    117 which are driven by the color rather than the mean magnitudes.
    118 
    119 <img width=1000px src="relphot.20120528/dJH.allsky.20120528.v3.png"><br>
    120 Map of the J-H color at g-i = 0.5.
    121 <br>
    122 
    123 <img width=1000px src="relphot.20120528/dHK.allsky.20120528.v3.png"><br>
    124 Map of the H-K color at g-i = 0.5.
    125 <br>
     15* [Schlafly et al ubercal paper](http://adsabs.harvard.edu/abs/2012ApJ...756..158S)
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