pro lum_r,kepmag,ext,teff,ra,dec,lumr ; this routine estimates the luminosity (in solar units) of the stars in ; its input vectors, based on a distance estimate derived from the extinction ; ext and on the galactic latitude computed from ra (in decimal hours) and ; dec (in decimal degrees). ; constants k=.001 ; mag extinction per pc in the galactic plane hh=250. ; scale height for dust in pc erat=0.7 ; ratio of extinction in kepler filter to V (???) vsun=4.82 ; solar V abs mag. radian=180./!pi tt=[3170.,3840.,4830.,5310.,5790.,6250.,7000.,8180.,9790.,15200.,20900.] bc=[-2.73,-1.38,-.42,-.4,-.2,-.16,-.11,-.15,-.30,-1.46,-2.35] vmk=[2.6,1.74,.98,.75,.65,.62,.45,.19,.01,-.14,-.21] ; make interpolated values of the BC and V-kepler color for actual teffs bco=interpol(bc,tt,teff) vmko=interpol(vmk,tt,teff) ; make galactic latitude, max allowed extinction glactc,ra,dec,2000.,gl,gb,1 sinb=sin(gb/radian) exmax=k*hh/sinb extc=(ext > 0.) < exmax ; arbitrary increase in extinction for ext>1, to compensate for no ext > 2 ss=where(extc gt 1.,nss) exte=extc if(nss gt 0) then exte(ss)=1.+(ext(ss)-1.)*2. ; make distance estimate, with lower bound dd=(-hh/sinb)*alog(1.-exte*sinb/(k*hh) > .0001) > 100. ; absolute kepler magnitude kpp=kepmag-extc*erat kpp=kpp-5.*alog10(dd)+5. ; estimated V absolute mag, luminosity vv=kpp+vmko lumr=10.^(0.4*(vsun-vv-bco)) end