Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2005-23.pdf Дата изменения: Thu Nov 29 08:57:17 2007 Дата индексирования: Sun Dec 23 01:36:53 2007 Кодировка: Поисковые слова: http www.stsci.edu science starburst

Instrument Science Report WFC3 2005-23

Optical Properties of Blocking Glass in the WFC3 IR Channel
D.F. Figer & S. Baggett August 16, 2005 ABSTRACT RG830 and IR80 will be used as the optical blocking glass in the WFC3/IR channel to ensure that short-wavelength (optical) light does not reach the detector. This is necessary because the substrate-removed detector will be sensitive to wavelengths below 0.8 µm. This ISR gives the expected transmission of these glasses. It also gives the maximum expected ratio of light leaking through at optical wavelengths for infrared narrow-band filters in the case that those filters provide no blocking of their own.

Introduction
The WFC3 IR channel contains a HgCdTe detector for sensing light from 0.8 µm to 1.7 µm. This type of detector is grown on a substrate to provide mechanical integrity during the manufacturing process. Examples of such substrate material include Sapphire and CdZnTe. The latter has been used for the WFC3/IR detectors. Recently, radiation testing has shown that this substrate material has an undesirable effect. It appears to produce secondary light emission when struck by high energy protons. Because of this effect, the substrate will be removed from the flight detector. When this is done, the detector will be sensitive to optical light, at least down to 400 nm. Because of this, the infrared channel optical train must contain an optical blocking filter. In fact, most of the filters are deposited on 3.66 mm thick IR80; the exceptions are F093W, F110W, and F125W, which are on fused silica. In the future, any replacements will be made of RG830. The following web page gives transmission characteristics of 3 mm thick RG830, as given by Schott. http://www.optical-filters.com/rg830.html

Copyright 1999 The Association of Universities for Research in Astronomy, Inc. All Rights Reserved.


Instrument Science Report WFC3 2005-00N The contents of this web page are reproduced below. As can be seen, the transmission through RG830 is very low at wavelengths below about 760 nm, thus providing blocking at optical wavelengths.

Figure 1. Characteristics of RG830 glass from Schott.

Figure 2 shows the optical density (OD) of 3mm thick witness sample of IR80, as measured at GSFC. Note that OD= -LOG(T), i.e. OD=0 for 100% transmission.

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IR80 Glass

8 7 6 Optical Density 5 4 3 2 1 0 0 200 400 600 Wavelength (nm) 800 1000 1200

-log(T_ave)

Figure 2. Optical density of 3mm thick IR80, as measured at GSFC.

Model
Does the blocking glass provide "enough" blocking? To answer this question, we wrote a program (see Appendix) to count the number of photons in an optical bandpass that make it to the detector after having passed through the blocking glass, and assuming no out-of-band blocking from the infrared filter in the WFC3/IR channel beam. To take an extreme case, we assumed an O-star, using a non line-blanketed Kurucz model, and a narrow-band (R=100) infrared filter. Figure 3 shows the result of this calculation. The "leakage" percentage increases with wavelength because the number of in-band photons decreases at longer wavelengths for the chosen source (O-star). In all cases, the percentage is less than 0.1% for an out of band transmission of 1e-6. We also simulated the effects for an A-type star and found results about a factor of two lower in leakage percentage. Of course, the realized leakage should be much less, given that the narrow-band filters should provide some amount of blocking on their own.

Conclusions
Contamination from a "blue leak" in the WFC3 filters should provide little contamination to photometry, certainly less than 0.1% for the hottest sources.

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Figure 3. Percentage of number of photons through RG830 within 400 and 800 nm versus the number transmitted through an R=100 narrow-band filter versus center wavelength.

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Appendix
pro RG830ratio ; This program computes the ratio of out-of-band flux to in-band flux, assuming ; a WFC3/IR filter and RG830 blocking glass. set_plot,'ps' device,file='ratios.ps',/landscape !p.thick=5.0 !p.charsize=1.4 !x.thick=8.0 !y.thick=8.0 !p.charthick=6 !P.FONT=1 !X.CHARSIZE=1.4 !Y.CHARSIZE=1.4 ; set integration limits RG830lambda2=8000.*1.e-8 RG830lambda1=4000.*1.e-8 ; cm ; cm

plot,[0.8,1.8],[0.1,100],xrange=[0.8,1.8],xtitle='Narrow band wavelength (um)',/nodata,/ylog,$ ytitle='F('+strtrim(string(RG830lambda1/1e-4,format='(F3.1)'),2)+' to '+strtrim(string(RG830lambda2/1.e-4,format='(F3.1)'),2)+' um)/F(Narrow band)*100' ; set range of possible throughputs throughputs=[1e-4,1e-5,1e-6] ; loop over possible throughputs for z=0,2 do begin lambdanarrowcenters=9000*1.e-8*(1+indgen(10)/10.) cd,'c:\figerdev\WFC3 ; read in stellar energy distribution for hot (50,000 K) star from http://www.stsci.edu/science/starburst/Kurucz.html ; l is in angstroms, and f is in erg/s/cm/cm/A ;readcol,'t50000g50p00.dat',l,f readcol,'t50000g50p00.dat',l,f ; increase density of points by a factor of 100 newl=interpol(l,indgen(n_elements(l)),indgen(n_elements(l)*100)/100.) f=interpol(f,indgen(n_elements(l)),indgen(n_elements(l)*100)/100.) l=newl ; define constants h=0.0000000000000000000000000066260755 ; erg*s c=3.e10 ; cm/s lambda=l*1e-10*100 ; cm nu=c/lambda dlambda=(lambda(1:n_elements(lambda)-1)-lambda(0:n_elements(lambda)-2))/1e-8 ; A dnu=-c/lambda(1:n_elements(lambda)-1)+c/lambda(0:n_elements(lambda)-2) dnu=[dnu,dnu(n_elements(dnu)-1)] dlambda=[dlambda,dlambda(n_elements(dlambda)-1)] photons=f/(h*nu)*dlambda ; photons/s/cm/cm ; define vector of transmission values for all lambda RG830throughput=fltarr(n_elements(l)) RG830throughput(*)=throughputs(z) ; integrate flux through RG830 glass RG830region=where(lambda lt RG830lambda2 and lambda gt RG830lambda1) RG830photons=total(photons(RG830region)*RG830throughput(RG830region)) ; loop over set of narrow band filters ratios=fltarr(n_elements(lambdanarrowcenters)) for i=0,n_elements(lambdanarrowcenters)-1 do begin ; define infrared narrow band filter and integrate flux through it, assuming 100% transmission lambdanarrowcenter=lambdanarrowcenters(i) bandpassnarrow=lambdanarrowcenter/100. narrowregion=where(lambda gt lambdanarrowcenter-bandpassnarrow/2. and lambda lt lambdanarrowcenter+bandpassnarrow/2.) narrowphotons=total(photons(narrowregion))

; cm

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; store result ratios(i)=rg830photons/narrowphotons*100. ; print result print,'ratio= ',ratios(i),'%',format='(A,F5.2,A)' endfor ; plot data oplot,lambdanarrowcenters*1e4,ratios xyouts,lambdanarrowcenters(0)*1e4,ratios(0)/1.3,'throughput='+strtrim(string(throughpu ts(z),format='(e11.1)'),2) endfor device,/close end

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