[[PageOutline]]

= Challenger =

 * This is the top level page that describes my Pan-STARRS adventure. 
 * The ultimate goal is to provide a set of tools for accurate photometry of large galaxies.
 * Using ISP (Imaging Sky Probe) data for better evaluation of the sky background. 
[created in January 2016 - Ehsan Kourkchi]

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== Useful tools to work with SDSS data:

 * Quick looK: http://cas.sdss.org/dr12/en/tools/quicklook
 * Table Descriptions: http://skyserver.sdss.org/dr12/en/help/docs/tabledesc.aspx
 * SQL (test queries): http://skyserver.sdss.org/dr12/en/tools/search/sql.aspx
 * DR12 Science Archive Server (SAS): http://data.sdss3.org/
  * Single Field Search — Imaging: http://data.sdss3.org/fields
  * Coverage Check — Imaging: http://data.sdss3.org/coverageCheck




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== Sample Galaxies ==

These galaxies are all taken from '''Brent-9060''' HI catalog, when cross-matching with other catalogs.

A few galaxies to work with.
 * Sample (15 galaxies): [wiki:sample]

 * Hall 2012 (SDSS Catalog): [wiki:hall_sdss] [[br]]
 SDSS Imaging Data: M. Hall et al. 2012, MNRAS,425,2741
 
 * All galaxies: http://www.ifa.hawaii.edu/~ehsan/html_tables/all_brent_9060.html
 * All galaxies (with SDSS data): http://www.ifa.hawaii.edu/~ehsan/html_tables/sdss_brent_9060.html


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== Data Exploration ==

We have a catalog of 9060 galaxies with available HI data, but 8179 lie above dec -30: 

Goals:
 * Measuring their g,r,i magnitudes
 * Measuring their inclinations

Catalog: 
 * Good HI profiles
 * Types Sa and later
 * Inclinations greater than 45 degrees from face on, i.e. b/a > 1/sqrt(2)


This is the distribution of the magnitude of the galaxies. For those galaxies for which we have no magnitude data, the adopted value for the magnitude is zero. That' why we see a peak at zero.
 * (Bt) B mag from RC3
 * (It) I mag from RC3
[[Image(magnitude_distribution.v03.jpg)]]

Size distribution:
 * diameter at B 25 mag/as^2^ from RC3
[[Image(size_distribution.jpg)]]


The distribution of axial ratios: 
 * (b/a) axial ratio from RC3
 * (b/a2) axial ratio from Spitzer
 * (Wj/Wn ) axial ratio WISE
[[Image(axial_ratio_all.v02.jpg)]]



Distribution of Numeric type from RC3

[[Image(type_distribution.jpg)]]

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= How to install the pipeline (IPP) =

 1. Getting access to PS server
{{{
ssh -X username@ippc??
}}}
 2. Download the pipeline into your home directory 
{{{
svn co http://svn.pan-starrs.ifa.hawaii.edu/repo/ipp/trunk
}}}
 3. To properly install the code, follow the instruction in README in the root directory of the pipeline. 
{{{
cd $TRUNK/psconfig
}}}
and follow INSTALL instruction. TRUNK is the path-address of the pipeline. At this stage, all necessary executable (binary) files would be compiled.
   *  Note: Use "{{{psbuild -dev -extbuild}}}" in order to compile everything.
   *  This step is fragile, as people may constantly change the codes. If the compilation process fails at some point, report the failure.
   *  If you have access to a working version, do not remove it until you make sure that the newer version works as good.
{{{
psbuild -dev -extbuild
}}}
 4. Modify {{{.tcshrc}}} in your home directory. This is where all necessary environmental variables are initialize for the shell you are using. Also see here: http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/IPP_on_ifaps1

Usually, looking at `~ipp/.tcshrc` will give you an idea how to set-up your own `~/.tcshrc`

 5. Source `.tcshrc` or open another `tcsh` sehll by running `tcsh`
{{{
source ~/.tcshrc
}}}

 6. After all, you may find you cannot still run your desired IPP commands, therefore you may need to either modify your `.tcshrc` or compile some extra packages. Normally all packages should be installed all at once, unless some last minute changes have been introduced to some components.

 7. Consult to an IPP expert if you are stuck.