Here are some examples of using tskymap
:
stilts tskymap in=iras_psc.fits lon=RA lat=DEC out=iras_map.csv
stilts tskymap in=2mpz.fits icmd='addskycoords fk5 galactic ra dec glon glat' lon=glon lat=glat tiling=hpx6 cols='jCorr-hCorr hCorr-kCorr jCorr-kCorr' combine=median count=false complete=true out=2mpzColors.fits
addskycoords
filter has been used so that the grid
is laid on the sky with galactic coordinates.
Setting complete=true
guarantees that a row is written
to the output file for every sky pixel, including empty ones.
stilts tskymap in=tgas_source.fits tiling=hpx7 lon=l lat=b count=false cols=phot_g_n_obs combine=sum-per-unit perunit=arcmin2 out=obs-density.fits
phot_g_n_obs
values from the
input table that fall into each tile and applying a suitable
scaling factor.
stilts tskymap in=gums_lmc.fits lon=alpha lat=delta tiling=hpx14 complete=false omode=count
complete=false
, only rows for non-empty pixels
are included in the output table. Then, since the output mode is
count
, these rows are just counted, discarding the
pixels themselves, giving the number of level-14 healpix pixels
touched by the sources in this input file.
Note this is not necessarily the most efficient way to caluclate
coverage information.