/
exofast_chi2v2.pro
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exofast_chi2v2.pro
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;+
; NAME:
; EXOFAST_CHI2
;
; PURPOSE:
; Computes the chi2 for a transit and/or RV for a single planet
;
; CALLING SEQUENCE:
; chi2 = exofast_chi2v2(pars)
;
; INPUTS:
;
; PARS - An array of parameters that describes the model. There
; should be one for each parameter in the structure where
; fit==true. This array should be generated by str2pars.pro.
;
; OPTIONAL INPUTS:
;
; PSNAME - If specified, this routine will generate
; postscript figure for each model generated with a
; base of PSNAME.
;
; OPTIONAL OUTPUTS:
;
; DETERMINANT - The determinant of the Jacobian to weight the
; acceptance likelihood in order to impose
; non-uniform priors in the stepping parameters. This
; is equal to 1 (no transformation) unless MIST
; models are used. If MIST models are used,
; DETERMINANT is equal to d(EEP)/d(Age) to transform
; the uniform EEP prior into a uniform Age prior.
; MODELRV - The RV model given the parameters
; MODELFLUX - The Transit model given the parameters
; DERIVED - An array of derived parameters. Nothing is ever
; returned in DERIVED, but this keyword is required
; by EXOFAST_DEMC.
;
; RESULT:
; The chi^2 of the model given the data and parameters.
;
; COMMON BLOCKS:
; CHI2_BLOCK - See exofastv2.pro for definition
;
; MODIFICATION HISTORY
;
; 2018/03 -- Create documentation -- Jason Eastman (CfA)
;-
function exofast_chi2v2, pars, determinant=determinant, $
modelrv=modelrv, modelflux=modelflux, psname=psname, $
derived=derived, loadss=loadss, ss0=ss0
COMMON chi2_block, ss
;; populate the structure with the new parameters
if keyword_set(loadss) then begin
ss = ss0
return, -1
endif
;; this is just a time sink for debugging/evaluating multithreading
;; ss.delay should never be > 0 in production code!!
;for i=0L, 2.5d6 do t = i ;; this takes 0.05 seconds on my machine
;for i=0L, 2.5d7 do t = i ;; this takes 0.5 seconds on my machine
for i=0L, ss.delay do t = i
if n_elements(pars) ne 0 then pars2str, pars, ss
au = ss.constants.au/ss.constants.rsun
;; derive all required parameters
;; (this may change depending on parameterization)
;derivepars, ss
;; initialize the determinant and chi^2
chi2 = 0.d0
determinant = 1d0
if ss.debug or ss.verbose then printandlog, '', ss.logname
;; *** First make sure step parameters are in bounds ***
;; physical limb darkening (Kipping, 2013)
;; http://adsabs.harvard.edu/abs/2013MNRAS.435.2152K, eq 8
if (where(ss.planet.fittran))[0] ne -1 then begin
bad = where(ss.band.u1.value + ss.band.u2.value gt 1d0 or $
ss.band.u1.value lt 0d0 or $
ss.band.u1.value + 2d0*ss.band.u2.value lt 0d0, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, $
strtrim(nbad,2) + ' limb darkening parameters are bad (' + strtrim(ss.band[bad[0]].u1.value,2) + ', ' + strtrim(ss.band[bad[0]].u2.value,2) + ')',ss.logname
return, !values.d_infinity
endif
endif
;; -180 < phase shift < 180
bad = where(abs(ss.band.phaseshift.value) gt 180d0,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'phase shift is bad (' + strtrim(bad,2) + ')', ss.logname
return, !values.d_infinity
endif
;; 0.1 < Period < 10^13 (~age of the universe)
bad = where(ss.planet.logp.value gt 13d0 or ss.planet.logp.value lt -1d0,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'logP is bad (' + strtrim(bad,2) + ')', ss.logname
return, !values.d_infinity
endif
;; -max(period)/2 < ttv < max(period)/2
bad = where(abs(ss.transit.ttv.value) gt max(ss.planet.period.value)/2d0,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'ttv is bad (' + strtrim(ss.transit[bad].ttv.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; older than the universe (too conservative?)
if ss.star.age.value gt 13.82d0 or ss.star.age.value lt 0d0 then begin
if ss.debug or ss.verbose then printandlog, strtrim(nbad,2) + ' age is bad (' + strtrim(bad,2) + ')',ss.logname
return, !values.d_infinity
endif
;; positive extinction
if ss.star.av.value lt 0 or ss.star.av.value gt 1d3 then begin
if ss.debug or ss.verbose then printandlog, 'extinction is bad (' + strtrim(ss.star.av.value,2) + ')',ss.logname
return, !values.d_infinity
endif
;; can't have more than +/-100% dilution
bad = where(ss.band.dilute.fit and (ss.band.dilute.value le -1d0 or ss.band.dilute.value ge 1d0),nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'dilution is bad (' + strtrim(ss.band[bad].dilute.value,2) + ')',ss.logname
return, !values.d_infinity
endif
;; 0.9 AU to the size of the universe
if ss.star.distance.value lt 4d-6 or ss.star.distance.value gt 3d10 then begin
if ss.debug or ss.verbose then printandlog, 'distance is bad (' + strtrim(ss.star.distance.value,2) + ')',ss.logname
return, !values.d_infinity
endif
;; check vcve
bad = where(ss.planet.vcve.value lt 0, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'vcve is bad (' + strtrim(ss.planet[bad].vcve.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; check sign
bad = where(ss.planet.sign.value lt 0 or ss.planet.sign.value ge 2 or ss.planet.sign2.value lt 0 or ss.planet.sign2.value ge 2, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'sign is bad (' + strtrim(ss.planet[bad].sign.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; Omega boundary checking
bad = where(ss.planet.lsinbigomega.value^2 + ss.planet.lsinbigomega.value^2 gt 1d0, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'bigomega is bad', ss.logname
return, !values.d_infinity
endif
;; limit 0 < Omega < 180 if RVs or Transits not fit
bad = where((ss.planet.lsinbigomega.value lt 0d0 or ss.planet.lcosbigomega.value lt 0d0) and (ss.fitrv or ss.fittran), nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'bigomega is bad', ss.logname
return, !values.d_infinity
endif
;; lambda boundary checking
bad = where(ss.planet.lsinlambda.value^2 + ss.planet.lcoslambda.value^2 gt 1d0, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'lambda is bad', ss.logname
return, !values.d_infinity
endif
;; -c < gamma < c
bad = where(abs(ss.telescope.gamma.value) gt ss.constants.c/ss.constants.meter,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'gamma is bad (' + strtrim(ss.telescope[bad].gamma.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; excludes non-transiting planets where the transit is fit
;; NOTE: chord is not derived by step2pars, only check if chord is fit
bad = where((ss.planet.chord.value le 0d0 or ss.planet.chord.value gt (1d0+ss.planet.p.value)) and ss.planet.chord.fit,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'chord is bad (' + strtrim(bad,2) + ')', ss.logname
return, !values.d_infinity
endif
;; -c^2 < jitter^2 < c^2
bad = where(abs(ss.telescope.jittervar.value) gt (ss.constants.c/ss.constants.meter)^2,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'jittervar is bad (' + strtrim(ss.telescope[bad].jittervar.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; abs(slope) < 1d5 m/s/day
if abs(ss.star.slope.value) gt 1d5 then begin
if ss.debug or ss.verbose then printandlog, 'slope is bad (' + strtrim(ss.star.slope.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; abs(quad) < 1d5 m/s/day^2
if abs(ss.star.quad.value) gt 1d5 then begin
if ss.debug or ss.verbose then printandlog, 'quad is bad (' + strtrim(ss.star.quad.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; 0.01 < SED error scaling < 100
if ss.star.errscale.value lt 1d-2 or ss.star.errscale.value gt 1d2 then begin
if ss.debug or ss.verbose then printandlog, 'error scale is bad (' + strtrim(ss.star.errscale.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; -10 < [Fe/H] < 2
if ss.star.feh.value lt -10d0 or ss.star.feh.value gt 2d0 then begin
if ss.debug or ss.verbose then printandlog, 'teff is bad (' + strtrim(ss.star.teff.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; 100 < Teff < 50000
if ss.star.teff.value lt 100 or ss.star.teff.value gt 250000 then begin
if ss.debug or ss.verbose then printandlog, 'teff is bad (' + strtrim(ss.star.teff.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; 100 < Teff < 50000
if ss.star.teffsed.value lt 100 or ss.star.teffsed.value gt 250000 then begin
if ss.debug or ss.verbose then printandlog, 'teffsed is bad (' + strtrim(ss.star.teffsed.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; 10^-6 < rstar < 2000
if ss.star.rstar.value lt 1d-6 or ss.star.rstar.value gt 2000d0 then begin
if ss.debug or ss.verbose then printandlog, 'rstar is bad (' + strtrim(ss.star.rstar.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; 10^-6 < rstar < 2000
if ss.star.rstarsed.value lt 1d-6 or ss.star.rstarsed.value gt 2000d0 then begin
if ss.debug or ss.verbose then printandlog, 'rstarsed is bad (' + strtrim(ss.star.rstar.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; 10^-3 < mstar < 500
if ss.star.logmstar.value lt -3 or ss.star.logmstar.value gt 2.6989700d0 then begin
if ss.debug or ss.verbose then printandlog, 'mstar is bad (' + strtrim(ss.star.mstar.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; bound marginally detected planets to limit (infinite) parameter space at low logmp
;; conservative lower limit of 1 Ceres in 1 year orbit around sun = 10 um/s
;; conservative upper limit corresponds to 500 solar masses (larger
;; than the largest known star)
bad = where((ss.planet.logmp.value lt -9.4d0 or ss.planet.logmp.value gt 2.7d0) and ss.planet.logmp.fit, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'logmp is bad (' + strtrim(ss.planet[bad].logmp.value,2) + ')', ss.logname
return, !values.d_infinity
endif
if ss.nastrom gt 0 then begin
;; 0.01 < astrometric error scaling < 100
bad = where(ss.astrom.astromscale.value lt 1d-2 or ss.astrom.astromscale.value gt 1d2, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'astrometry error scale is bad (' + strtrim(ss.astrom[bad].errscale.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; 0 <= ra+raoffset <= 360
bad = where(ss.star.ra.value + ss.astrom.raoffset.value lt 0 or ss.star.ra.value + ss.astrom.raoffset.value gt 360,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'ra is bad (' + strtrim(ss.star.ra.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; -90 <= dec+decoffset <= 90
bad = where(abs(ss.star.dec.value + ss.astrom.decoffset.value) gt 90,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'dec is bad (' + strtrim(ss.star.dec.value +ss.astrom[bad].decoffset.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; -20000 <= pmra <= 20000 (2x barnard's star)
if abs(ss.star.pmra.value) gt 2d4 then begin
if ss.debug or ss.verbose then printandlog, 'pmra is bad (' + strtrim(ss.star.pmra.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; -20000 <= pmdec <= 20000 (2x barnard's star)
if abs(ss.star.pmdec.value) gt 2d4 then begin
if ss.debug or ss.verbose then printandlog, 'pmdec is bad (' + strtrim(ss.star.pmdec.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; -c <= rvabs <= c
if abs(ss.star.rvabs.value) gt ss.constants.c/ss.constants.meter then begin
if ss.debug or ss.verbose then printandlog, 'pmdec is bad (' + strtrim(ss.star.pmdec.value,2) + ')', ss.logname
return, !values.d_infinity
endif
endif
;; 0.01 < DT error scaling < 100
bad = where(ss.doptom.dtscale.value le 1d-2 or ss.doptom.dtscale.value gt 1d2, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'dtscale is bad (' + strtrim(ss.doptom[bad].dtscale.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; require planets to stay in the same order as they start
if ss.nplanets gt 0 then begin
if max(abs(ss.planetorder - sort(ss.planet.logp.value))) ne 0 then begin
if keyword_set(verbose) then printandlog, 'Planets must remain in the original order! Rejecting step', logname
return, !values.d_infinity
endif
endif
;; limit range of alpha abundance (not used yet)
;if ss.star.alpha.value lt -0.3d0 or ss.star.alpha.value gt 0.7d0 then begin
; if ss.debug or ss.verbose then printandlog, 'alpha is bad (' + strtrim(ss.star.alpha.value,2) + ')', ss.logname
; return, !values.d_infinity
;endif
;; **** Now place additional physical constraints on derived parameters ****
;; derive the model parameters from the step parameters
;; (returns -1 if can't be derived due to non-physical inputs)
if step2pars(ss,verbose=(ss.debug or ss.verbose),logname=ss.logname) eq -1 then begin
if ss.debug or ss.verbose then printandlog, 'stellar system is bad', ss.logname
return, !values.d_infinity
endif
;; check angular parameters
;; omega boundary checking
bad = where(ss.planet.lsinw.value^2 + ss.planet.lcosw.value^2 gt 1d0, nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'omega is bad', ss.logname
return, !values.d_infinity
endif
;; tighter (empirical) constraint on eccentricity (see Eastman 2013)
if ss.tides then begin
bad = where(ss.planet.e.value gt (1d0-3d0/ss.planet.ar.value), nbad)
if nbad ne 0 then begin
if ss.verbose then $
printandlog, 'TIDES flag set and eccentricity (' + strtrim(ss.planet[bad].e.value,2) + $
') exceeds empirical limit (' + strtrim((1d0-3d0/ss.planet[bad].ar.value),2) + ')', ss.logname
return, !values.d_infinity
endif
endif
;; no transit and we're fitting a transit! This causes major
;; problems; exclude this model (but this biases the significance of
;; the detection)
bad = where(ss.planet.fittran and ss.planet.b.value gt (1d0+ss.planet.p.value), nbad)
;; note: this still allows eccentric solutions with only secondary eclipses!
;; these should be excluded with the rejectflattransit input
;bad = where(ss.planet.fittran and ss.planet.b.value gt (1d0+ss.planet.p.value) and ss.planet.bs.value gt (1d0+ss.planet.p.value), nbad)
if nbad ne 0L then begin
if ss.verbose then printandlog, 'Planet does not transit!', ss.logname
return, !values.d_infinity
endif
;; for multi-planet systems, make sure they don't enter each other's hill spheres
;; if mp unknown, mp=0 => hill radius=0 => planets can't cross orbits
;; **** ignores mutual inclination; a priori excludes systems like Neptune and Pluto!! ****
if ~ss.alloworbitcrossing then begin
mindist = dblarr(ss.nplanets>1)
maxdist = dblarr(ss.nplanets>1)
for i=0L, ss.nplanets-1 do begin
hillradius = ((1d0-ss.planet[i].e.value)*ss.planet[i].a.value*(ss.planet[i].mpsun.value/(3d0*ss.star.mstar.value))^(1d0/3d0)) > 0d0
mindist[i] = (1d0-ss.planet[i].e.value)*ss.planet[i].a.value - hillradius
maxdist[i] = (1d0+ss.planet[i].e.value)*ss.planet[i].a.value + hillradius
for j=i-1,0,-1 do begin
if ((mindist[i] ge mindist[j]) and (mindist[i] le maxdist[j])) or $
((maxdist[i] ge mindist[j]) and (maxdist[i] le maxdist[j])) or $
((mindist[j] ge mindist[i]) and (mindist[j] le maxdist[i])) or $
((maxdist[j] ge mindist[i]) and (maxdist[j] le maxdist[i])) then begin
if ss.verbose then printandlog, 'Planets ' + strtrim(j,2) + ' (' + strtrim(mindist[j],2) + ',' + strtrim(maxdist[j],2) + ') and ' + strtrim(i,2) + ' (' + strtrim(mindist[i],2) + ',' + strtrim(maxdist[i],2) + ') cross paths', logname
return, !values.d_infinity
endif
endfor
endfor
endif
;; must do after step2pars -- sometimes tt is derived
;; tt-period/2 < tt < tt+period/2
bad = where(ss.planet.tt.prior ne 0d0 and $
abs(ss.planet.tt.value - ss.planet.tt.prior) gt ss.planet.period.value/2d0,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'tt is bad (' + strtrim(ss.planet[bad].tt.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; must do after step2pars -- sometimes tc is derived
;; tc-period/2 < tc < tc+period/2
bad = where(ss.planet.tc.prior ne 0d0 and $
abs(ss.planet.tc.value - ss.planet.tc.prior) gt ss.planet.period.value/2d0,nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'tc is bad (' + strtrim(ss.planet[bad].tc.value,2) + ')', ss.logname
return, !values.d_infinity
endif
;; must do after step2pars -- sometimes cosi is derived
;; 0 <= cosi <= 1 (or -1 <= cosi <= 1 if i180 keyword set or astrometry fit)
bad = where(ss.planet.cosi.value gt 1 or (ss.planet.cosi.value lt 0 and ~ss.planet.i180) or (ss.planet.cosi.value lt -1),nbad)
if nbad gt 0 then begin
if ss.debug or ss.verbose then printandlog, 'cosi is bad (' + strtrim(bad,2) + ')', ss.logname
return, !values.d_infinity
endif
;; *** Now start penalizing the model ***
;; *** apply prior penalties ***
priors = *(ss.priors)
for i=0, n_elements(priors[0,*])-1 do begin
;; if it's not a detrending variable
if priors[3,i] eq -1 then begin
value = ss.(priors[0,i])[priors[1,i]].(priors[2,i]).value
upperbound = ss.(priors[0,i])[priors[1,i]].(priors[2,i]).upperbound
lowerbound = ss.(priors[0,i])[priors[1,i]].(priors[2,i]).lowerbound
label = ss.(priors[0,i])[priors[1,i]].(priors[2,i]).label + '_' + strtrim(priors[1,i],2)
prior = ss.(priors[0,i])[priors[1,i]].(priors[2,i]).prior
priorwidth = ss.(priors[0,i])[priors[1,i]].(priors[2,i]).priorwidth
unit = strupcase(ss.(priors[0,i])[priors[1,i]].(priors[2,i]).unit)
endif else begin
;; otherwise
value = (*(ss.(priors[0,i])[priors[1,i]].(priors[2,i]))).(priors[3,i])[priors[4,i]].value
upperbound = (*(ss.(priors[0,i])[priors[1,i]].(priors[2,i]))).(priors[3,i])[priors[4,i]].upperbound
lowerbound = (*(ss.(priors[0,i])[priors[1,i]].(priors[2,i]))).(priors[3,i])[priors[4,i]].lowerbound
label = (*(ss.(priors[0,i])[priors[1,i]].(priors[2,i]))).(priors[3,i])[priors[4,i]].label + '_' + strtrim(priors[1,i],2)
prior = (*(ss.(priors[0,i])[priors[1,i]].(priors[2,i]))).(priors[3,i])[priors[4,i]].prior
priorwidth = (*(ss.(priors[0,i])[priors[1,i]].(priors[2,i]))).(priors[3,i])[priors[4,i]].priorwidth
unit = strupcase((*(ss.(priors[0,i])[priors[1,i]].(priors[2,i]))).(priors[3,i])[priors[4,i]].unit)
endelse
;; apply the bounds
if value gt upperbound or value lt lowerbound then begin
if ss.debug or ss.verbose then $
printandlog, label + '( ' + strtrim(value,2) + ') is out of user-defined bounds (' +$
strtrim(lowerbound,2) + ',' + strtrim(upperbound,2) + ')',ss.logname
return, !values.d_infinity
endif
;; apply the Gaussian prior
;; if it's an angular parameter, make sure we handle the boundary
if unit eq 'RADIANS' then begin
chi2 += (atan(sin(value-prior),cos(value-prior))/priorwidth)^2
endif else if unit eq 'DEGREES' then begin
chi2 += (atan(sin((value-prior)*!dpi/180d0),cos((value-prior)*!dpi/180d0))/(priorwidth*!dpi/180d0))^2
endif else begin
chi2 += ((value - prior)/priorwidth)^2
endelse
;; output debugging info if requested
if ss.verbose then begin
str = string(label,((value - prior)/priorwidth)^2, format='(a," penalty = ",f0.6)')
printandlog, str, ss.logname
endif
endfor
;; **** apply corrections to make priors physical ****
; if fitting in v_c/v_e & omega, correct for a uniform eccentricity prior
for i=0, ss.nplanets-1 do begin
;; vcve jacobian
if ss.planet[i].vcve.fit then begin
dvcvede = abs((-sin(ss.planet[i].omega.value)-ss.planet[i].e.value)/$
(sqrt(1d0-ss.planet[i].e.value^2)*(ss.planet[i].esinw.value+1d0)^2))
determinant *= dvcvede
endif
;; chord jacobian
if ss.planet[i].chord.fit then begin
dchorddcosi = ss.planet[i].b.value^2/(ss.planet[i].cosi.value*ss.planet[i].chord.value)
determinant *= dchorddcosi
endif
;; linear eccentricity prior
;; we never fit in ecosw & esinw; a waste of time
;if ss.planet[i].ecosw.fit and ss.planet[i].esinw.fit then begin
; determinant *= ss.planet[i].e.value
;endif
endfor
;; *** Now computing model constraints ***
;; apply YY penalty to constrain stellar parameters
if ss.yy then begin
if keyword_set(psname) then epsname = psname+'.yy.eps'
yychi2 = massradius_yy3(ss.star.mstar.value, ss.star.feh.value, $
ss.star.age.value, ss.star.teff.value,$
yyrstar=yyrstar, debug=ss.debug, psname=epsname, $
sigmab=ss.constants.sigmab/ss.constants.lsun*ss.constants.rsun^2, $
gravitysun=ss.constants.gravitysun)
if ~finite(yychi2) then begin
if ss.debug or ss.verbose then printandlog, 'star not on YY tracks', ss.logname
return, !values.d_infinity
endif
yychi2 += ((ss.star.rstar.value - yyrstar)/(0.03*yyrstar))^2
chi2 += yychi2
if ss.verbose then printandlog, 'YY penalty = ' + strtrim(yychi2,2), ss.logname
endif
;; apply PARSEC penalty to constrain stellar parameters
if ss.parsec then begin
if keyword_set(psname) then epsname = psname+'.parsec.eps'
parsecchi2 = massradius_parsec(ss.star.eep.value, ss.star.mstar.value, ss.star.initfeh.value, $
ss.star.age.value, ss.star.teff.value,$
ss.star.rstar.value, ss.star.feh.value, debug=ss.debug, $
epsname=epsname, gravitysun=ss.constants.gravitysun, $
fitage=ss.star.age.fit, ageweight=ageweight, logname=ss.logname, verbose=ss.verbose,$
tefffloor=ss.teffemfloor, fehfloor=ss.fehemfloor, rstarfloor=ss.rstaremfloor, agefloor=ss.ageemfloor)
chi2 += parsecchi2
if ss.verbose then printandlog, 'PARSEC penalty = ' + strtrim(parsecchi2,2), ss.logname
if ~finite(chi2) then begin
if ss.debug or ss.verbose then printandlog, 'star not on PARSEC tracks', ss.logname
return, !values.d_infinity
endif
determinant *= ageweight ;; correct uniform EEP prior to uniform Age prior
endif
;; apply MIST penalty to constrain stellar parameters
if ss.mist then begin
if keyword_set(psname) then epsname = psname+'.mist.eps'
;************************************
;print, 'this is for making pretty animated gifs. Do not leave it here!
;filebase = "HAT-3b.MIST."
;files = file_search(filebase+'*.png',count=index)
;pngname = string(filebase, index+1,format='(a,i04,".png")')
;************************************
mistchi2 = massradius_mist(ss.star.eep.value, ss.star.mstar.value, ss.star.initfeh.value, $
ss.star.age.value, ss.star.teff.value,$
ss.star.rstar.value, ss.star.feh.value, debug=ss.debug, $
epsname=epsname, gravitysun=ss.constants.gravitysun, $
fitage=ss.star.age.fit, ageweight=ageweight, logname=ss.logname, verbose=ss.verbose,$
tefffloor=ss.teffemfloor, fehfloor=ss.fehemfloor, rstarfloor=ss.rstaremfloor, agefloor=ss.ageemfloor, pngname=pngname)
chi2 += mistchi2
if ss.verbose then printandlog, 'MIST penalty = ' + strtrim(mistchi2,2), ss.logname
if ~finite(chi2) then begin
if ss.debug or ss.verbose then printandlog, 'star not on MIST tracks', ss.logname
return, !values.d_infinity
endif
determinant *= ageweight ;; correct uniform EEP prior to uniform Age prior
endif
;; apply TORRES penalty to constrain stellar parameters
if ss.torres then begin
massradius_torres, ss.star.logg.value, ss.star.teff.value, ss.star.feh.value, mstar_prior, rstar_prior
umstar = 0.027d0
urstar = 0.014d0
if mstar_prior lt 0.6d0 then printandlog, $
'WARNING: Torres not applicable (mstar = ' + $
strtrim(mstar_prior,2) + '); ignore at beginning. Otherwise, ' + $
'use MIST, YY, or impose a prior on mstar/rstar',ss.logname
;; add "prior" penalty
chi2 += (alog10(ss.star.mstar.value/mstar_prior)/umstar)^2
chi2 += (alog10(ss.star.rstar.value/rstar_prior)/urstar)^2
if ss.verbose then $
printandlog, 'Torres penalty: ' + string((alog10(ss.star.mstar.value/mstar_prior)/umstar)^2, $
(alog10(ss.star.rstar.value/rstar_prior)/urstar)^2,format='(f0.6,x,f0.6)'), ss.logname
endif
;; Apply Chen & Kipping Mass-Radius relation
;; http://adsabs.harvard.edu/abs/2017ApJ...834...17C
for j=0, ss.nplanets-1 do begin
if ss.planet[j].chen then begin
;; negative radii are allowed to assess the significance of the
;; transit depth. That breaks these relations, so exclude them here
if ss.planet[j].rpearth.value le 0d0 then begin
if ss.debug or ss.verbose then printandlog, 'rpearth is bad', ss.logname
return, !values.d_infinity
endif
rp = massradius_chen(ss.planet[j].mpearth.value > 1d-10,rperr=rperr)
;; add a chi2 penalty for deviation from the mass-radius relation
;; if the radius is well-constrained (by transit depth), it
;; becomes an implicit constraint on mass. If the mass is well
;; constrained (by RV), it is an explicit constraint on
;; radius
chi2 += ((rp - ss.planet[j].rpearth.value)/rperr)^2
if ss.verbose then printandlog, 'chen penalty = ' + strtrim(((rp - ss.planet[j].rpearth.value)/rperr)^2,2),ss.logname
endif
endfor
;; fit the SED with MIST BC tables
if file_test(ss.star.mistsedfile) or file_test(ss.star.fluxfile) then begin
if keyword_set(psname) then epsname = psname+'.sed.eps'
sedchi2 = 0d0
;; the SED can constrain Teff too precisely
;; (they ignore systematics in interferimetric radii on which they're based).
;; Add a floor for the Teff used everywhere else
if ss.star.teffsed.fit then begin
teffsed = ss.star.teffsed.value
sedchi2 += ((ss.star.teff.value - ss.star.teffsed.value)/(ss.teffsedfloor*ss.star.teffsed.value))^2
endif else teffsed = ss.star.teff.value
if ss.star.fehsed.fit then begin
fehsed = ss.star.fehsed.value
sedchi2 += ((ss.star.feh.value - ss.star.fehsed.value)/ss.fehsedfloor)^2
endif else fehsed = ss.star.feh.value
;; the SED can constrain FBol too precisely
;; Add a floor for the Fbol used everywhere else
if ss.star.rstarsed.fit then begin
rstarsed = ss.star.rstarsed.value
; lstarsed = 4d0*!dpi*rstarsed^2*ss.star.teff.value^4*ss.constants.sigmab/ss.constants.lsun*ss.constants.rsun^2 ;; lsun
lstarsed = 4d0*!dpi*rstarsed^2*teffsed^4*ss.constants.sigmab/ss.constants.lsun*ss.constants.rsun^2 ;; lsun
sedchi2 += ((lstarsed - ss.star.lstar.value)/(ss.fbolsedfloor*lstarsed))^2
endif else begin
rstarsed = ss.star.rstar.value
; lstarsed = 4d0*!dpi*rstarsed^2*ss.star.teff.value^4*ss.constants.sigmab/ss.constants.lsun*ss.constants.rsun^2 ;; lsun
lstarsed = 4d0*!dpi*rstarsed^2*teffsed^4*ss.constants.sigmab/ss.constants.lsun*ss.constants.rsun^2 ;; lsun
endelse
if file_test(ss.star.mistsedfile) then begin
;; MIST BC SED
sedchi2 += mistsed(teffsed, ss.star.logg.value,fehsed, ss.star.av.value, ss.star.distance.value, lstarsed, ss.star.errscale.value, ss.star.mistsedfile, debug=ss.debug, psname=epsname)
endif else begin
;; Keivan Stassun's SED
junk = exofast_sed(ss.star.fluxfile, teffsed, $
rstarsed,$
ss.star.av.value, ss.star.distance.value, $
logg=ss.star.logg.value,met=fehsed,$
alpha=ss.star.alpha.value,verbose=ss.verbose, $
f0=f, fp0=fp, ep0=ep, psname=epsname, $
pc=ss.constants.pc, rsun=ss.constants.rsun, $
logname=logname, debug=ss.debug, oned=ss.oned)
if ~finite(junk) then begin
if ss.debug or ss.verbose then printandlog, 'sed is bad', ss.logname
return, !values.d_infinity
endif
sedchi2 += exofast_like(f-fp,0d0,ss.star.errscale.value*ep,/chi2)
endelse
;; do some error checking
if ~finite(sedchi2) then begin
if ss.debug or ss.verbose then printandlog, 'sed is bad', ss.logname
return, !values.d_infinity
endif
chi2 += sedchi2
if ss.verbose then printandlog, 'SED penalty = ' + strtrim(sedchi2,2), ss.logname
endif
;; RV model (non-interacting planets)
for j=0, ss.ntel-1 do begin
rv = *(ss.telescope[j].rvptrs)
if (where(rv.err^2 + ss.telescope[j].jittervar.value le 0d0))[0] ne -1 then begin
if ss.debug or ss.verbose then printandlog, ss.telescope[j].label + ' variance is bad', ss.logname
return, !values.d_infinity
endif
modelrv = dblarr(n_elements(rv.rv))
for i=0, ss.nplanets-1 do begin
if ss.planet[i].fitrv then begin
;; rvbjd = rv.bjd ;; usually sufficient (See Eastman et al., 2013)
q = ss.star.mstar.value/ss.planet[i].mpsun.value
if rv.planet eq i then begin
;; time in target barycentric frame (expensive)
;; this needs to be debugged
rvbjd = bjd2target(rv.bjd, inclination=ss.planet[i].i.value, $
a=ss.planet[i].a.value, tp=ss.planet[i].tp.value, $
period=ss.planet[i].period.value, e=ss.planet[i].e.value,$
omega=ss.planet[i].omega.value+!dpi,$
c=ss.constants.c/ss.constants.au*ss.constants.day,$
q=ss.star.mstar.value/ss.planet[i].mpsun.value)
;; calculate the RV model
modelrv += exofast_rv(rvbjd,ss.planet[i].tp.value,ss.planet[i].period.value,$
0d0,ss.planet[i].K.value*q,$
ss.planet[i].e.value,ss.planet[i].omega.value+!dpi,$
slope=0d0)
endif else begin
;; time in target barycentric frame (expensive)
rvbjd = bjd2target(rv.bjd, inclination=ss.planet[i].i.value, $
a=ss.planet[i].a.value, tp=ss.planet[i].tp.value, $
period=ss.planet[i].period.value, e=ss.planet[i].e.value,$
omega=ss.planet[i].omega.value,/primary,$
c=ss.constants.c/ss.constants.au*ss.constants.day,$
q=q)
;; calculate the RV model
if ss.planet[i].rossiter then $
u1 = linld(ss.star.logg.value,ss.star.teff.value,ss.star.feh.value,'V') $
else u1 = 0d0
modelrv += exofast_rv(rvbjd,ss.planet[i].tp.value,ss.planet[i].period.value,$
0d0,ss.planet[i].K.value,$
ss.planet[i].e.value,ss.planet[i].omega.value,$
slope=0d0, $
rossiter=ss.planet[i].rossiter, i=ss.planet[i].i.value,a=ss.planet[i].ar.value,$
p=abs(ss.planet[i].p.value),vsini=ss.star.vsini.value,$
lambda=ss.planet[i].lambda.value,$
u1=u1,deltarv=deltarv)
endelse
endif
endfor
;; add instrumental offset, slope, and quadratic term
modelrv += ss.telescope[j].gamma.value
if (*ss.telescope[j].rvptrs).planet eq -1 then $
modelrv += ss.star.slope.value*(rv.bjd-ss.rvepoch) + ss.star.quad.value*(rv.bjd-ss.rvepoch)^2
;; detrending
modelrv += total((*ss.telescope[j].rvptrs).detrendadd*(replicate(1d0,n_elements((*ss.telescope[j].rvptrs).bjd))##(*ss.telescope[j].rvptrs).detrendaddpars.value),1)
modelrv *= (1d0+total((*ss.telescope[j].rvptrs).detrendmult*(replicate(1d0,n_elements((*ss.telescope[j].rvptrs).bjd))##(*ss.telescope[j].rvptrs).detrendmultpars.value),1))
(*ss.telescope[j].rvptrs).residuals = rv.rv - modelrv
if keyword_set(psname) then begin
base = file_dirname(psname) + path_sep() + file_basename(psname,'.model')
exofast_forprint, rv.bjd, rv.rv - modelrv, rv.err, format='(f0.8,x,f0.6,x,f0.6)', textout=base + '.residuals.telescope_' + string(j,format='(i02)') + '.txt', /nocomment,/silent
exofast_forprint, rv.bjd, modelrv, format='(f0.8,x,f0.6)', textout=base + '.model.telescope_' + string(j,format='(i02)') + '.txt', /nocomment,/silent
endif
rvchi2 = exofast_like((*ss.telescope[j].rvptrs).residuals,ss.telescope[j].jittervar.value,rv.err,/chi2)
if ~finite(rvchi2) then stop
chi2 += rvchi2
if ss.verbose then printandlog, ss.telescope[j].label + ' RV penalty = ' + strtrim(rvchi2,2),ss.logname
endfor
;; if at least one RV planet is fit, plot it
if (where(ss.planet.fitrv))[0] ne -1 then begin
if keyword_set(psname) then begin
plotrv, ss, psname=psname + '.rv.ps'
endif else if ss.debug then begin
plotrv, ss
endif
endif
;; Doppler Tomography Model
for i=0, ss.ndt-1 do begin
if keyword_set(psname) then epsname = psname + '.dt_' + string(i,format='(i02)') + '.eps'
dtchi2 = dopptom_chi2(*(ss.doptom[i].dtptrs),$
ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].tc.value, $
ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].period.value, $
ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].e.value,$
ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].omega.value, $
ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].cosi.value, $
ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].p.value,$
ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].ar.value,$
ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].lambda.value, $
ss.star.logg.value, ss.star.teff.value, ss.star.feh.value,$
ss.star.vsini.value/1d3,ss.star.vline.value/1d3,$
ss.doptom[i].dtscale.value, debug=ss.debug,/like,psname=epsname,$
verbose=ss.verbose, logname=ss.logname)
if 0 then begin
stop
npoints = 1000
vsini = 17000d0 + dindgen(npoints)/(npoints-1)*4000d0
vline = 500d0 + dindgen(npoints)/(npoints-1)*10000d0
; vsini = 19000d0 + dindgen(npoints)/(npoints-1)*2000d0
dtchi2 = dblarr(npoints)
for ii=0, npoints-1 do dtchi2[ii] = dopptom_chi2(*(ss.doptom[i].dtptrs),ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].tc.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].period.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].e.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].omega.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].cosi.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].p.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].ar.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].lambda.value,ss.star.logg.value, ss.star.teff.value, ss.star.feh.value,vsini[ii]/1d3,ss.star.vline.value/1d3,ss.doptom[i].dtscale.value, debug=ss.debug,/like,psname=epsname)
plot, vsini, dtchi2
dtchi22 = dblarr(npoints)
for ii=0, npoints-1 do dtchi22[ii] = dopptom_chi2(*(ss.doptom[i].dtptrs),ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].tc.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].period.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].e.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].omega.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].cosi.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].p.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].ar.value,ss.planet[(*(ss.doptom[i].dtptrs)).planetndx].lambda.value,ss.star.logg.value, ss.star.teff.value, ss.star.feh.value,ss.star.vsini.value/1d3,vline[ii]/1d3,ss.doptom[i].dtscale.value, debug=ss.debug,/like,psname=epsname)
plot, vline, dtchi22
endif
if ~finite(dtchi2) then begin
if ss.verbose or ss.debug then printandlog, (*ss.doptom[i].dtptrs).label + ': DT chi2 is bad', ss.logname
return, !values.d_infinity
endif
chi2 += dtchi2
if ss.verbose then printandlog, (*ss.doptom[i].dtptrs).label + ' DT penalty = ' + strtrim(dtchi2,2),ss.logname
endfor
;; Transit model
for j=0, ss.ntran-1 do begin
transit = *(ss.transit[j].transitptrs)
if (where(transit.err^2 + ss.transit[j].variance.value le 0d0))[0] ne -1 then begin
if ss.verbose then printandlog, transit.label + ' variance + err^2 < 0. If this is the starting model, check the supplied errors are accurate and the starting value for variance_' + strtrim(j,2) + ' is sensible; rejecting step', ss.logname
return, !values.d_infinity
endif
band = ss.band[ss.transit[j].bandndx]
;; quadratic limb darkening
if ss.claret then begin
ldcoeffs = quadld(ss.star.logg.value, ss.star.teff.value, ss.star.feh.value, band.name, $
verbose=ss.verbose, logname=ss.logname)
u1claret = ldcoeffs[0]
u2claret = ldcoeffs[1]
if ~finite(u1claret) or ~finite(u2claret) then begin
if ss.verbose then begin
printandlog, band.label + ' limb darkening coefficients are not defined at this ' +$
'Teff (' + strtrim(ss.star.teff.value,2) + ', ' + $
'logg (' + strtrim(ss.star.logg.value,2) + ', and ' + $
'[Fe/H] (' + strtrim(ss.star.feh.value,2) + '; rejecting step',ss.logname
endif
return, !values.d_infinity
endif
u1err = 0.05d0
u2err = 0.05d0
chi2 += ((band.u1.value-u1claret)/u1err)^2
chi2 += ((band.u2.value-u2claret)/u2err)^2
if ss.verbose then printandlog, band.label + ' u1 penalty = ' + strtrim(((band.u1.value-u1claret)/u1err)^2,2),ss.logname
if ss.verbose then printandlog, band.label + ' u2 penalty = ' + strtrim(((band.u2.value-u2claret)/u2err)^2,2),ss.logname
endif
;; Kepler Long candence data; create several model points and average
ninterp = ss.transit[j].ninterp
npoints = n_elements(transit.bjd)
if ninterp gt 1 then begin
transitbjd = transit.bjd#(dblarr(ninterp)+1d0) + $
((dindgen(ninterp)/ninterp-(ninterp-1d0)/(2d0*ninterp))/$
1440d0*ss.transit[j].exptime)##(dblarr(npoints)+1d0)
modelflux = dblarr(npoints,ninterp) + 1d0
endif else begin
transitbjd = transit.bjd
modelflux = dblarr(npoints) + 1d0
endelse
for i=0, ss.nplanets-1 do begin
if ss.planet[i].fittran then begin
tmpmodelflux = (exofast_tran(transitbjd, $
ss.planet[i].i.value + ss.transit[j].tiv.value, $
ss.planet[i].ar.value, $
ss.planet[i].tp.value + ss.transit[j].ttv.value, $
ss.planet[i].period.value, $
ss.planet[i].e.value,$
ss.planet[i].omega.value,$
ss.planet[i].p.value + ss.transit[j].tdeltav.value,$
band.u1.value, $
band.u2.value, $
1d0, $
q=ss.star.mstar.value/ss.planet[i].mpsun.value, $
thermal=band.thermal.value, $
reflect=band.reflect.value, $
phaseshift=band.phaseshift.value, $
beam=ss.planet[i].beam.value,$
dilute=band.dilute.value,$
tc=ss.planet[i].tc.value,$
rstar=ss.star.rstar.value/AU,$
;x1=x1,y1=y1,z1=z1,$
au=au,$
c=ss.constants.c/ss.constants.au*ss.constants.day) - 1d0)
modelflux += tmpmodelflux
endif
endfor
if ss.transit[j].rejectflatmodel then begin
minmodel = min(modelflux,max=maxmodel)
if minmodel eq maxmodel then begin
if ss.verbose then printandlog, ss.transit[j].label + ' transit model is a flat line, which is not allowed by the REJECTFLATMODEL input! This may artificially enhance the significance of the signal', ss.logname
return, !values.d_infinity
endif
endif
;; ellipsoidal variations
if band.ellipsoidal.value ne 0d0 then begin
minperiod = min(ss.planet.period.value,ndx)
modelflux = modelflux * (1d0 - band.ellipsoidal.value/1d6*cos(2d0*!dpi*(transitbjd-ss.planet[ndx].tc.value)/(ss.planet[ndx].period.value/2d0)))
endif
;; now integrate the model points (before detrending)
;; Riemann integration beats trapezoidal and simpsons wins when
;; sampling like above
if ninterp gt 1 then modelflux = total(modelflux,2)/ninterp
;; Trapezoidal integration not as good
;;if ninterp gt 1 then modelflux = (total(modelflux,2) - modelflux[*,0]/2d0 - modelflux[*,-1]/2d0)/(ninterp-1d0)
;; Simpson integration (about 2x worse than trap because it
;; requires sampling at the midpoint, effectively halving our resolution)
;if ninterp gt 1 then modelflux = (4d0*total(modelflux,2) - 3d0*modelflux[*,0] - 3d0*modelflux[*,-1])/(4d0*ninterp - 6d0)
;; detrending
modelflux += total(transit.detrendadd*(replicate(1d0,n_elements(transit.bjd))##transit.detrendaddpars.value),1)
modelflux *= (ss.transit[j].f0.value + $
total(transit.detrendmult*(replicate(1d0,n_elements(transit.bjd))##transit.detrendmultpars.value),1))
;; fit Andrew Vanderburg's keplerspline to the residuals to detrend the lightcurve
if ss.transit[j].fitspline then begin
if transit.breakpts[0] eq -1 then $
norm = keplerspline(transit.bjd, transit.flux-modelflux+1d0, ndays=ss.transit[j].splinespace) $
else norm = keplerspline(transit.bjd, transit.flux-modelflux+1d0, breakp=transit.breakpts, ndays=ss.transit[j].splinespace)
modelflux *= norm
endif else norm = 1d0
phase = (transitbjd - ss.planet[0].tc.value) mod ss.planet[0].period.value
toohigh = where(phase gt ss.planet[0].period.value/2d0)
if toohigh[0] ne -1 then phase[toohigh] -= ss.planet[0].period.value
toolow = where(phase lt -ss.planet[0].period.value/2d0)
if toolow[0] ne -1 then phase[toohigh] += ss.planet[0].period.value
;set_plot, 'ps'
;device, filename='toi2165.ps'
;loadct, 39, /silent
;red = 254
;sorted = sort(phase)
;plot, phase, transit.flux, psym=1, /ynoz, xtitle='phased time', ytitle='Normalized flux'
;oplot, phase[sorted], modelflux[sorted],color=red
;device, /close
;spawn, 'gv toi2165.ps &'
;stop
;; chi^2
if ss.transit[j].sigma_r.fit then begin
transitchi2 = -2d0*exofast_wavelike(transit.flux - modelflux,ss.transit[j].sigma_r.value,mean(transit.err),/zeropad)
endif else begin
transitchi2 = exofast_like(transit.flux - modelflux,ss.transit[j].variance.value,transit.err,/chi2)
endelse
(*ss.transit[j].transitptrs).residuals = transit.flux - modelflux
; (*ss.transit[j].transitptrs).model = modelflux
if keyword_set(psname) then begin
base = file_dirname(psname) + path_sep() + file_basename(psname,'.model')
exofast_forprint, transit.bjd, transit.flux - modelflux, transit.err, format='(f0.8,x,f0.6,x,f0.6)', textout=base + '.residuals.transit_' + string(j,format='(i03)') + '.txt', /nocomment,/silent
exofast_forprint, transit.bjd, modelflux, format='(f0.8,x,f0.6)', textout=base + '.model.transit_' + string(j,format='(i03)')+ '.txt', /nocomment,/silent
if ss.transit[j].fitspline then $
exofast_forprint, transit.bjd, norm, format='(f0.8,x,f0.6)',$
textout=base+'.spline.transit_' + string(j,format='(i03)') + '.txt', /nocomment,/silent
endif
if ~finite(transitchi2) then stop
chi2 += transitchi2
if ss.verbose then printandlog, ss.transit[j].label + ' transit penalty: ' + strtrim(transitchi2,2) + ' ' + strtrim(ss.transit[j].variance.value,2),ss.logname
endfor
;; plot the transit model and data
;; if a transit is fit for at least one planet
if ((where(ss.planet.fittran))[0] ne -1) then begin
if keyword_set(psname) then begin
plottran, ss, psname=psname + '.transit.ps'
endif else if ss.debug then begin
plottran, ss
endif
endif
;; if TTVs are allowed, add a chi2 penalty to the period and t0 from
;; the fit to a linear ephemeris
;; this imposes the constraint of the linear ephemeris while allowing TTVs
for i=0L, ss.nplanets-1L do begin
if ~ss.planet[i].fittran then continue
;; ensure the tdeltavs average to zero
good = where(ss.tdeltavs[*,i],ngood)
if ngood ge 2 then begin
sigma = stdev(ss.transit[good].tdeltav.value)
if sigma gt 0d0 then begin
chi2 += (mean(ss.transit[good].tdeltav.value)/sigma)^2
if ss.verbose then printandlog, 'TDELTAV penalty ' + strtrim((mean(ss.transit[good].tdeltav.value)/sigma)^2,2)
endif
endif else if ngood ne 0 then begin
printandlog, 'ERROR: TDELTAVs are requested for planet ' + strtrim(i,2) + ', but must have at least 2 transits', ss.logname
stop
endif
;; ensure the tivs average to zero
good = where(ss.tivs[*,i],ngood)
if ngood ge 2 then begin
sigma = stdev(ss.transit[good].tiv.value)
if sigma gt 0d0 then begin
chi2 += (mean(ss.transit[good].tiv.value)/sigma)^2
if ss.verbose then printandlog, 'TIV penalty ' + strtrim((mean(ss.transit[good].tiv.value)/sigma)^2,2)
endif