FUNCTION xrt_flux1102_slmd_fctm, te, fw1, fw2, time, $ cal = cal, $ index=index, $ vem=vem, cem=cem, electron=electron, datapoint=datapoint, $ contamination_thickness=contamination_thickness, $ info=info, message=message, $ lambda_spectrum = lambda_spectrum, $ te_spectrum = te_spectrum, spectrum = spectrum, $ apac_spectrum = apac_spectrum, eff_area = eff_area, $ ; corona=corona, hybrid=hybrid, photospheric=photospheric, $ cr2012=cr2012, ioneq_v6=ioneq_v6, ph2009=ph2009, ph2011=ph2011, $ cr1992=cr1992, ph2015=ph2015, spe_file=spe_file, $ sp_info=sp_info, $ ; frac_open=frac_open, fctm_fact=fctm_fact ; ========================================================================= ;+ ; PROJECT: ; ; Solar-B / XRT ; ; NAME: ; ; XRT_FLUX (with frac_open and fctm_fact keywords) ; ; CATEGORY: ; ; XRT RESPONSE ; ; PURPOSE: ; ; Get the data number (DN) flux [sec^-1 pixel^-1] ; when XRT observes the solar plasma at an inputed temperature (for CEM = 1 [cm^-5] in default), ; i.e., get the XRT temperature response. ; Covered temperature range is from 10^5.0 to 10^8.0 [K]. ; ; In default, this program use the solar spectrum ; calculated with CHIANTI database ver. 10.0. ; (density: 10^9 [cm^-3], ionization equilibrium: chianti.ioneq, abundance: sun_coronal_ext.abund). ; ; CALLING SEQUENCE: ; ; result = XRT_FLUX_slmd_fctm(te, fw1, fw2, time, [index=index], $ ; [vem=vem], [cem=cem], [/electron], [/datapoint], $ ; [contamination_thickness=contamination_thickness], [/info], $ ; [lambda_spectrum = lambda_spectrum, te_spectrum = te_spectrum, spectrum = spectrum], $ ; [/apac_spectrum], [eff_area = eff_area]) ; ; INPUTS: ; ; TE - (float array) log Temperature with a range from 5.0 to 8.0. ; FW1 - (long) Filter No. on filter wheel 1. ; FW2 - (long) Filter No. on filter wheel 2. ; TIME - (string) Time when you want to calcurate the XRT flux, ; because XRT flux influenced by contamination is a function of time. ; This time is used to derive the thickness of contaminant. ; If you directly give the contamination thickness with CONTAMINATION_THICKNESS ; keyword, you should omit this TIME input. ; FRAC_OPEN - (float) Open fraction of pre-fileter (0.0 : no opening -- 1.0 : fully open) ; FCTAM_FACT - (float) Filter contamination enhancement factor ; ; KEYWORDS: ; ; CAL - [Optional input] If set as "cal = 1", the flux is calculated based on the calibration in Narukage et al. (2011). ; If set as "cal = 2", the flux is calculated based on the calibration in Narukage et al. (2013). ; Default is "cal = 2" to use the latest calibration result of Narukage et al. (2013). ; INDEX - [Optional input] (structure) If set, you can omit the inputs of FW1, FW2 and TIME. ; VEM - [Optional input] (float) volume emission measure [cm^-3] of solar plasma in logalithmic scale (e.g., VEM = 44. for 1e44 [cm^-3]). ; CEM - [Optional input] (float) column emission measure [cm^-5] of solar plasma in logalithmic scale (e.g., CEM = 26. for 1e26 [cm^-5]). ; /ELECTRON - [Optional] (Boolean) If set, unit of return value is [electron sec^-1 pixel^-1]. ; /DATAPOINT - [Optional] (Boolean) ; If set, result is calculated at the data point of temperature and ; the data point is inputed into "te" parameter. ; The data point of temperature is from 10^5.0 to 10^8.0 [K] with 10^0.05 [K] resolution. ; CONTAMINATION_THICKNESS - [Optional input] (float) ; You can directly give the contamination thickness. ; When you use this keyword, you should omit the input of TIME. ; /INFO - [Optional] (Boolean) If set, information is shown. ; LAMBDA_SPECTRUM - [Optional input] (float array) wavelength for SPECTRUM in an unit of [A]. ; TE_SPECTRUM - [Optional input] (float array) temperature for SPECTRUM in an unit of [log K]. ; SPECTRUM - [Optional input] (2-dim float array, [lambda_spectrum, te_spectrum]) photon number spectrum from solar plasma in an unit of [cm^3 s^-1 sr^-1]. ; We recommend that ; (1) The data point of wavelength is from 1 to 400 [A] with 0.1 [A] resolution. ; (2) The data point of temperature is from 10^5.0 to 10^8.0 [K] with 10^0.05 [K] resolution. ; /APAC_SPECTRUM - [Optional] (Boolean) If set, solar spectrum calculated with APAC database is used. (in default, solar spectrum is calculated with CHIANTI database.) ; EFF_AREA - [Optional] (Structure) You can input the output (effective area) from MAKE_XRT_WAVE_RESP.PRO. ; ; OUTPUTS: ; ; return - (float array) DN flux [DN sec^-1 pixel^-1] (for CEM = 1 [cm^-5] in default). ; ; EXAMPLES: ; ; Get X-ray flux [DN sec^-1 pixel^-1] observed with thin-Al-poly filter ; at 11-Mar-2007 00:55:00 from the solar plasma (CEM=1 [cm^-5]): ; IDL> te = 5.+findgen(61)*0.05 ; IDL> flux = xrt_flux(te, 1, 0, '11-Mar-2007 00:55:00') ; ; Get X-ray flux [DN sec^-1 pixel^-1] with index from the solar plasma (VEM = 10^44 [cm^-3]): ; IDL> te = 5.+findgen(61)*0.05 ; IDL> flux = xrt_flux(te, index = index, vem = 44.) ; ; IDL> ofrac=get_pf_openfrac(index) ; IDL> fctm=get_fctm_fact7_xx(index) ; xx: filter pair ; IDL> flux = xrt_flux1102_slmd_fctm(te, index = index, vem = 44., $ ; /corona, frac_open=ofrac, fctm_fact=fctm) ; ; COMMON BLOCKS: ; ; none ; ; NOTES: ; ; filter on filter wheel 1 ; 0: open ; 1: thin-Al-poly ; 2: C-poly ; 3: thin-Be ; 4: med-Be ; 5: med-Al ; ; filter on filter wheel 2 ; 0: open ; 1: thin-Al-mesh ; 2: Ti-poly ; 3: G-band (optical) ; 4: thick-Al ; 5: thick-Be ; ; The detail of calibrated temperature response function of the Hinode/XRT is described in ; Narukage et al. 2011, Solar Phys., 269, 169. ; http://adsabs.harvard.edu/doi/10.1007/s11207-010-9685-2 ; and ; Narukage et al. 2013, Solar Phys., in press ; http://adsabs.harvard.edu/doi/10.1007/s11207-013-0368-7 ; These two papers are the reference papers of this program. ; ; CONTACT: ; ; Comments, feedback, and bug reports regarding this routine may be ; directed to this email address: ; noriyuki.narukage ~at~ nao.ac.jp ; ; MODIFICATION HISTORY: ; progver = 'v2007-May-17' ;--- (N.Narukage (ISAS/JAXA)) Written. progver = 'v2009-Jul-27' ;--- (N.Narukage (NAOJ)) Updated to consider the contamination on focal-plane analysis filters and CCD. progver = 'v2010-Jul-30' ;--- (N.Narukage (NAOJ)) Updated to input the solar spectrum. ; And added the option to select the APAC database. progver = 'v2010-Aug-04' ;--- (N.Narukage (NAOJ)) Updated to input the output from MAKE_XRT_WAVE_RESP.PRO. progver = 'v2011-Jan-31' ;--- (N.Narukage (NAOJ)) Modified the manual. progver = 'v2011-Feb-17' ;--- (N.Narukage (NAOJ)) Added the information on the reference paper. progver = 'v2013-Nov-04' ;--- (N.Narukage (NAOJ)) Updated to use the calibration result of Narukage et al. (2013). ; Added the keyword of "cal" to select the calibration result. ; And modified for the message from the program. ; '2014-Feb-24' ;--- (Aki Takeda (MSU)) added keywords to accept various solar_spectrum files. ; AkT version created to study new XRT response functions. ; XRT_TEEM_CH713 does not use this function for Te&EM calculation. ; '2014-Feb-27' ;--- (Aki Takeda (MSU)) added spe_file keywords. ; '2015-Sep-11' ;--- (Aki Takeda (MSU)) modified to calculate flux with partially opened pre-filter. ; '2020-Jun-19' ;--- (Aki Takeda (MSU)) modified to use newer Chianti DB (ver.7.1.3 --> 9.0.1). ; '2021-Mar-12' ;--- (Aki Takeda (MSU)) modified to use keyword, FCTAM_FACT. ; '2022-Jan-02' ;--- (Aki Takeda (MSU)) Modified and renamed to use Chianti DB (ver.9.0.1 --> 10.0). ; '2023-Aug-12' ;--- (Aki Takeda (MSU)) Modified and renamed to use Chianti DB (ver.10.0 --> 10.1). ; added /cr1992 keyword for coronal abundance by Feldman 1992. ; added /ph2015 keyword for photospheric abundance by Scott 2015. ; '2025-Oct-03' ;--- (Aki Takeda (MSU)) Modified and renamed to use Chianti DB (ver.10.1 --> 11.02). ;- ; ========================================================================= ps = path_sep() file_prefix = get_logenv('$SSW_XRT') + ps + 'idl' + ps + 'response' + ps + 'j' + ps ; --- setting for message ------------------------------------------------- if not keyword_set(message) then message = ['XRT_FLUX'] ; --- read filter config data --------------------------------------------- config = xrt_config(cal = cal) ; --- process of option --------------------------------------------------- if keyword_set(index) then begin time = anytim(index.date_obs, /ecs) fw1 = index.ec_fw1 fw2 = index.ec_fw2 endif ; --- read solar spectrum ------------------------------------------------- if not(keyword_set(lambda_spectrum) and keyword_set(te_spectrum) and keyword_set(spectrum)) then begin if keyword_set(apac_spectrum) then begin temp = get_xrt_spec_genx() dl = temp.wave[1] - temp.wave[0] lambda_spectrum = temp.wave[0:temp.WLENGTH-1.] te_spectrum = temp.temp[0:temp.TLENGTH-1.] spectrum = temp.spec[0:temp.WLENGTH-1., 0:temp.TLENGTH-1.] * dl endif else begin dir_sp = '/home/takeda/idlpro/xrt/xrt_resp/solar_spectrum/' ; dir_sp = '/disk/yla/software/xrt_ssw/solar_spectrum/' ; solar_spe_file = 'XRT_solar_spe-chianti_6.0.1-edensity_1e9-chianti.ioneq-sun_coronal_ext.abund' solar_spe_file = dir_sp+'solspec_ch1102_cr2021chianti_adv' ; if keyword_set(corona) then solar_spe_file = dir_sp+'solspec_ch1102_cr2021chianti_adv' if keyword_set(photospheric) then solar_spe_file = dir_sp+'solspec_ch1102_ph2021asplund_adv.genx' if keyword_set(cr1992) then solar_spe_file = dir_sp+'solspec_ch1102_cr1992feldman_adv.genx' if keyword_set(hybrid) then solar_spe_file = dir_sp+'solspec_ch1102_cr2012schmelz_adv.genx' if keyword_set(cr2012) then solar_spe_file = dir_sp+'solspec_ch1102_cr2012schmelz_adv.genx' ; if keyword_set(ph2015) then solar_spe_file = dir_sp+'solspec_ch1010_ph2015scott_chianti.genx' ; if keyword_set(ph2009) then solar_spe_file = dir_sp+'solspec_ch1000_ph2009asplund_chianti.genx' ; if keyword_set(ph2011) then solar_spe_file = dir_sp+'solspec_ch1000_ph2011caffau_chianti.genx' if keyword_set(spe_file) then solar_spe_file = spe_file print,'*** Assumed spectrum file : ', solar_spe_file ; restgen, te_spectrum, lambda_spectrum, spectrum, file=solar_spe_file ; restgenx, te_spectrum, lambda_spectrum, spectrum, $ ; file = file_prefix + 'database' + ps + 'solar_spe' + ps + solar_spe_file ; spectrum : photon number spectrum from solar plasma (n = 10^9 [cm^-3]) [cm^3 s^-1 sr^-1] endelse endif ; --- calculate flux ------------------------------------------------------ p = config.ccd.plate_scale ; XRT CCD plate scale [arcsec] s = (config.ccd.pixel_size / 1.e4)^2. ; area of 1 pixel on CCD [cm^2] f = config.var.focal_length ; focal length of XRT [cm] if keyword_set(eff_area) then begin temp = fltarr(6,6) temp[*,*] = -1. temp[0,1] = 0. ; Al-mesh temp[1,0] = 1. ; Al-poly temp[2,0] = 2. ; C-poly temp[0,2] = 3. ; Ti-poly temp[3,0] = 4. ; Be-thin temp[4,0] = 5. ; Be-med temp[5,0] = 6. ; Al-med temp[0,4] = 7. ; Al-thick temp[0,5] = 8. ; Be-thick temp[1,1] = 9. ; Al-poly/Al-mesh temp[1,2] = 10. ; Al-poly/Ti-poly temp[1,4] = 11. ; Al-poly/Al-thick temp[1,5] = 12. ; Al-poly/Be-thick temp[2,2] = 13. ; C-poly/Ti-poly temp[2,4] = 14. ; C-poly/Al-thick if temp[fw1, fw2] ne -1 then begin temp = eff_area[temp[fw1, fw2]].effar ea = interpol(temp.eff_area[0:temp.length-1], temp.wave[0:temp.length-1], lambda_spectrum) > 0. if keyword_set(info) and n_elements(temp.name) ne 0 then begin print print, temp.name print endif endif else begin ea = fltarr(n_elements(lambda_spectrum)) ea[*] = 0. message = [message, ''] message = [message, '***** WARNING from XRT_FLUX.PRO *****************************************'] message = [message, 'Your inputted EFF_AREA as a keyword does not contain'] message = [message, ' the effective area information about'] message = [message, ' '+config.filter1[fw1].name+' (FW1) / '+config.filter2[fw2].name+' (FW2).'] message = [message, '***************************************** WARNING from XRT_FLUX.PRO *****'] endelse endif else begin ea = xrt_eff_area_slmd_fctm(lambda_spectrum, fw1, fw2, time, cal=cal, $ index=index, $ ; contamination_thickness=contamination_thickness, $ info=info, message=message, frac_open=frac_open, fctm_fact=fctm_fact) print,'frac_open assumed: ', frac_open print,'fctm_fact assumed: ', fctm_fact endelse ea = rebin( ea, n_elements(lambda_spectrum), n_elements(te_spectrum) ) ; effective area [cm ^ 2] FP = spectrum * s * ea / (f^2.) ; photon number flux detected by CCD 1 pixel from CEM = 1 [cm^-5] plasma h = 6.6261e-27 ; plank constant c = 2.9979e10 ; speed of light [cm/s] cf = rebin( (h*c/(lambda_spectrum*1.e-8)), n_elements(lambda_spectrum), n_elements(te_spectrum) ) ; factor to convert photon count to erg FE = FP * cf ; energy flux detected by CCD 1 pixel from CEM = 1 [cm^-5] plasma cf = 3.65*1.602*1.e-12 ; factor to convert erg to electron count EC = FE / cf ; electron count from CCD 1 pixel from CEM = 1 [cm^-5] plasma if (n_elements(cem) eq 0) then cem = 0. cf = 10.^cem ; factor to convert CEM if (n_elements(vem) ne 0) then begin if keyword_set(index) then time = anytim(index.date_obs, /ecs) if keyword_set(time) then l = 696000.e5 / get_rb0p(time, /radius, /quiet) else l = 726.e5 cf = 10.^( vem - (alog10(p*l)*2.) ) ; factor to convert VEM endif flux = total(EC,1) * cf gain = config.ccd.gain if not keyword_set(electron) then flux = flux / gain ; convert electron count to DN. if keyword_set(datapoint) then te = te_spectrum else flux = INTERPOL( flux, te_spectrum, te ) ; --- filter name ------------------------------------------------------------ fw1name = config.filter1[fw1].name fw2name = config.filter2[fw2].name ; print, 'filter (FW1/FW2): '+fw1name+' / '+fw2name ; --- show message ------------------------------------------------------------ if n_elements(message) ge 2 then begin if message[0] eq 'XRT_FLUX' then hprint, [message[1:*], ''] endif ; --- return result ----------------------------------------------------------- return, flux END