ó 2~ÇTc@sbddlZddlZddlZddlTgZdZd„Zd„Zd„Zd„Z dS(iÿÿÿÿN(t*icCsq|dkri}tddƒ}|jƒ}x=|dkrltj|ƒ}|d||d<|jƒ}q0W|jƒ|dd}|dd}|dd } |dd } |dd } |d d |d d?dƒtd@dAƒtdBdCƒtdDƒdEGHtƒdFGHtƒ|dGkrQdHGHtƒn6|dIkrldJGHtƒn|dKkr‡dJGHtƒndLGHtƒ|dMkr®dNGHtƒnt ƒtdOƒt t | ƒdPƒtƒt t |ƒƒtƒ|dGkrt t |ƒd!ƒtƒn@|dIkr;t dQƒtƒn |dKkr[t dRƒtƒnt t |ƒd7ƒtƒ|dMkrœt t |ƒƒtƒnt ƒtdSƒdTGHtƒ|dUksÑ|dVkràdWGHtƒn dXGHtƒt ƒtdYƒt t |ƒdZƒtƒ|dUks0|dVkrNd[|}%t |%ƒtƒnt t |ƒdZƒtƒt ƒtd=ƒt ƒnÁd} d }"d }#dG|GH|dkr·d\G|GHn|dkrØd GHd]G|Gd^GHn|dkr|dkrd#GHd_G|Gd`GHdaG|GdbGHdcG|GddGHnde||fGHd(G|GHdfG| GHd,G| GH|ddkrd-G| GdgGHd.G|Gd`GHd/G|GdhGHd1G|GdiGHndjG| GdkGHdFG|GH|dGkrÂdHG|GdlGHn(|dIkrÖdmGHn|dKkrêdnGHn|dMkr dNG|GHndLG|GdgGHdoG|GH|dUks0 |dVkr< dp|GHn dq|GH|dkrà t| drƒ}&|&jds|dtƒ|dkr™ |&jdu|dtƒn|dkrÊ |&jdƒ|&jdv|dwƒn|dkr1 |dkr1 |&jd‘ƒ|&jdx|dyƒ|&jdz|d{ƒ|&jd||d}ƒn|&jd~||fƒ|&jd|ƒ|&jd€| dtƒ|&jd| dtƒ|ddkrÚ |&jd‚| ƒ|&jdƒ|ƒ|&jd„|ƒ|&jd…|ƒn|&jd†| ƒ|&jd‡|ƒ|dGkr |&jdˆ|ƒn8|dIkr8 |&jd‰ƒn|dKkrT |&jdŠƒn|dMkrt |&jd‹|ƒn|&jdŒ|ƒ|&jd|ƒ|dUks® |dVkr |&jdŽ|ƒn|&jd|ƒ|&jƒndS(’Nis output.iniRRiRs table.csvRsplot.pngsplot.pltRs index.htmltheadline_objectsObject characteristicstheadline_hardwaresHardware characteristicst object_leftsSource geometry:s Source type:tbttsSource magnitude (%s-filter):s Temperature:sLine wavelength:s Line flux:s Line width:t object_rightsTemplate spectrum, tgalaxyiÿÿÿÿs, z= t Blackbodys mags Ks Single lines microns erg/s/cm²s Åt hardware_lefts LUCIFER No.:sDetector full well:sDetector Readout Noise:sFilter:sCamera:s Slit width:s'Central Wavelength of the grating unit:sNumber of lines per milimeter:s Dispersion:s Plate scale:thardware_rights%.0f e-s Fullwell_%ds %.0f e- rmssRON_%ds arcsecs l/mms%4.2fgˆÃ@s Å/pixels arcsec/pixeltclears80%tcentertheadline_atmospheresAtmospheric conditionstheadline_exposuresParameters of exposuretatmosphere_lefts Water vapor:sAirmass:t0sSky brightness:iåÿÿÿsSky background:iïÿÿÿsSeeing:s-1sStrehl:tatmosphere_rights mmtFilet Theoreticalt exposure_leftsDIT: iisSNR:sTotal exposure time:texposure_rights secs%.1fsSource type: Template spectrum,sBlackbody Temperature:tKsLine_wavelength:tmicrons Line_flux:s erg/s/cm^2s Line_width:tAs&Source magnitude (%s-filter): %.2f magsFilter of LUCIFER:tarcsecsl/mms arcsec/pixels Water vapour:tmmtmagsSky background: FilesSky background: TheoreticalsDIT:s SNR: %.2f sTotal exposure time: %.2f tasSource geometry: s s Source type: Template spectrum, sBlackbody Temperature: s K sLine_wavelength: s micron s Line_flux: s erg/s/cm^2 s Line_width: s As'Source magnitude (%s-filter): %.2f mag sLUCIFER No.: %s sFilter used in LUCIFER: sCamera: sSlit width: %s arcsec s4Central Wavelength of the grating unit: %.2f micron s'Number of lines per milimeter: %s l/mm sPlate scale: %.2f arcsec/pixel sWater vapor: %.1f mm sAirmass: %.2f sSky brightness: %.1f mag sSky background: File sSky background: Theoretical s Strehl: %.2f sSeeing: %.2f arcsec sDIT: %.2e sec s SNR: %.2f sTotal exposure time: %.2e sec s Blackbody s Single line (R R R RRt headline_lefttheadline_righttpartnewlinetcoda_partemphtfindtstrtintRR('RtSourcetObject_choice_0tObject_choice_1tObject_choice_2t Filter_magtObject_brightness_choicetDetectortHawaii_conditionst Filter_choicet Camera_choicet Slit_widthtDispersion_choicet Water_vaportAirmasstBackground_choicetSky_brightnesstStrehltSeeingtCentral_wavelengthtLpmmtSNtDITtTautScaletModeRRRRRRRRRR R!tStringR"((s*/users/jheidt/cgi-bin/calculator/output.pytoutput_summary/s                                                                                                     c!Cs¡|dkr·i}tddƒ}|jƒ}x=|dkrltj|ƒ}|d||d<|jƒ}q0W|jƒ|dd}|dd}|dd }|dd }|dd }|d d |d | krWd?|t j || ƒ| f}|j |ƒ|d@| dA}qW|jƒt|dBƒ} | j dC|dDƒ| j dEƒ| j dFƒ| j dGƒ| j dHƒt j |d@| dA| ƒ| }| j dI|ƒ| j dJ|dKƒ| j dLƒ| jƒdM|}tj|ƒ|dkrtdƒdN| dOGHtƒtdPdQƒt|ƒtd-ƒtƒtdRƒt|dSƒndS(TNis output.iniRRiRs table.csvRsplot.pngsplot.pltRs index.htmls80%R/sCalculated valuest2tfivet output_leftiisExposure time:sSNR:sTotal object flux:sTotal sky flux:s3Electrons from object+sky inside the central pixel:s;Electrons from object+sky inside the central pixel per DIT:sObject central pixel:sSky background:t output_rights%.2fs secs Point sources e-s e-/pixels%0.2f e-s%0.2f e-/pixels%.2f e-s Fullwell_%ssLinearity_start_%ssLinearity_end_%ss %.2f e-/DITs)%s !! saturated !!s;%s !! Linearity is not within 5%% !!s%.2f e-/pix/DITR.s.Total number of electrons from source: %.2e e-sExposure time: %.2e secs SNR: %.2es;Electrons from object+sky inside the central pixel: %.2e e-sSNR for the central pixel: %.2esBackground: %.2e e-/pixel/secR?s/Total number of electrons from source: %.2f e- sExposure time: %.2f sec s SNR: %.2f s<Electrons from object+sky inside the central pixel: %.2e e- s SNR for the central pixel: %.2f sBackground: %.2f e-/pixel/sec s sexposure time / sec SNR gÐ?gü?s %.2e %.7f gø?g4@R s set output 's' s set term png sset style data lines s!set xlabel 'exposure time [sec]' sset ylabel 'SNR' sset yrange[*:%s] splot 's' using ($1):($2) stitle 'LUCIFER-ETC SNR' sgnuplot s\The SNR is calculated over %d pixels in the PSF area including 93.8 % of the total flux.gà?sSignal-To-Noise plotRtasciis ASCII-file(R R R RRRRRBRDRCRERtmathtsqrttostsystemtimagetlink(!RRIRORPtPhotons_object_tautPhotons_sky_tautCenter_pixel_tauR]t SN_center_tauR^tSN_DITR_RatN_pixRZRRRRRRRRR tTemptTemp1tTemp4tTemp2tTemp3R"tiRbt Gnuplot_write((s*/users/jheidt/cgi-bin/calculator/output.pytoutput_imagingRs                                                  !      #           c 'Csd} d}d}|dkräi}tddƒ}|jƒ}x=|dkr~tj|ƒ}|d||d<|jƒ}qBW|jƒ|dd }|d d }|dd }|d d }|d d }|d d|d ƒndS(?Niôgis output.iniRRiRs table.csvRsplot.pngsplot.pltRs index.htmlR R?sWL/micron SN Pixel g@gà?gð¿s %s %.4f %d g@g@s set output 's' s set term png sset style data lines sset xlabel 'Pixel' s"set x2label 'wavelength [micron]' s'set ylabel 'SNR (total exposure time)' s set x2tics 0,s s set x2range[t:s] sset xtics nomirror sset xrange[-%s:%s] sset yrange[0:*] splot 's*' using ($3):($2) title 'LUCIFER-ETC SNR' sgnuplot s80%R/sCalculated valuesRdReRfsObject signal at %4.2f micron:sSNR at %4.2f micron:s%Maximum count rate from object + sky:s"Maximum sky level at %4.4f micron:Rgs %3.2f e-/DITs%3.2fs%3.2f e-/DIT/pixs Fullwell_%ss&!! saturated !!stThe SNR and the object signal is calculated for one pixel in dispersion direction and %d pixel in spatial direction.sSignal-To-Noise plotRRhs ASCII-file(R R R RRtkeystsortRRHtatofRGRkRlRRRBRDRCRERmRn('RRORPR]tPhotons_object_dittPhotons_sky_ditRTtPixelRtR[R^R_tPhotons_max_ditt Pixel_shifttWavelength_starttWavelength_endRRRRRRRRR R{R"tListetPhotons_sky_maxRztjtWavelength_sky_maxRbtPhotons_object_cwtPhotons_sky_cwtSN_cwtWavelength_stepRuRv((s*/users/jheidt/cgi-bin/calculator/output.pytoutput_spectrums       ) (            )                           ( R RkRit html_elementstContentR!R#RcR|R(((s*/users/jheidt/cgi-bin/calculator/output.pyts$  & ÿ$ °