Run D75 GALEX images through to get SB HXZ: 02/25/10 Get exposure times: (Check exp FITS images) NGA_SextansA-fd-exp.fits 1663.32 NGA_SextansA-nd-exp.fits 1512.36 ======> fuv: 1663.32 s; nuv: 1512.36 s 1)Cut out smaller images: cutout subimage size: 800*800 centered around the galaxy center of cutout: 1947; 1894 imcopy NGA_SextansA-fd-int.fits[1445:2444,1395:2394] d75fcut.fit imcopy NGA_SextansA-nd-int.fits[1445:2444,1395:2394] d75ncut.fit -------------------------------------------- 2)Remove foreground stars and background galaxies: imedit d75fcut.fit d75fcl.fit logfile=fcut.log imedit d75ncut.fit d75ncl.fit logfile=ncut.log ========> d75ncl.fit; d75fcl.fit ---------------------------------------------------------- 3)Get the background now that the extraneous stuff has been removed: #Note: #The low counts rates in GALEX images leads to poisson, rather than gaussian noise. #which leads to the failure of using the usual sky-fitting routines in IRAF #Fit the sky of the original images usually failed. #So I selected many sky regions around the galaxy to get a mean sky level and the associated variance # #Here I first average the original images with 10*10 bin size ======= blkavg d75fcl.fit d75fblkav.fit 10 10 blkavg d75ncl.fit d75nblkav.fit 10 10 ========> d75fblkav.fit; d75nblkav.fit #Then use ELLIPSE to get mean pixel intensity and the associated rms in the elliptical annular sky regions around the galaxy. #I fixed the ELLIPSE parameters to that used to do surface photometry. # PACKAGE = isophote TASK = geompar (x0 = 40.497172) initial isophote center X (y0 = 40.479586) initial isophote center Y (ellip0 = 0.5) initial ellipticity (pa0 = 45.6) initial position angle (degrees) (sma0 = 10.) initial semi-major axis lenght (minsma = 10.) minimum semi-major axis lenght (maxsma = 30.) maximum semi-major axis lenght (step = 3.) sma step between successive ellipses (linear = yes) linear sma step ? (maxrit = INDEF) maximum sma lenght for iterative mode (recente= no) allows finding routine to re-center x0-y0 ? (xylearn= no) updates pset with new x0-y0 ? (physica= no) physical coordinate system ? (mode = al) ------- ellip d75fblkav.fit fsky_ell ellip d75nblkav.fit nsky_ell tprint fsky_ell.tab columns='sma,intens,pix_var,ndata' > fsky_ell.lst tprint nsky_ell.tab columns='sma,intens,pix_var,ndata' > nsky_ell.lst # I choose the surface photometry intensity on the 7.5 arcmin annulus (6th annul in *_ell.lst) # The sky variations around the galaxy are -- 5.13E-5 for FUV, 2.29E-4 for NUV imarith d75fcl.fit - 3.42E-4 d75fms.fit imarith d75ncl.fit - 0.00297 d75nms.fit =========> d75nms.fit; d75fms.fit #Add SKYMEAN keyword to these fits headers sethead d75fms.fit skymean=3.42E-4 sethead d75nms.fit skymean=0.00297 ------------------------------------------- #Geometrically transform the NUV and FUV images to match the pixel scale and orientation of # the original V image: #I use 5 field stars in v and nuv images center d75ncut.fit center d75v.fits txdump d75v.fits.ctr.1 xc,yc yes > v.xy txdump d75ncut.fit.ctr.1 xc,yc yes > n.xy joinlines v.xy n.xy > vn.xy imheader d75v.fits d75v.fits[1620,1844][real]: Sex A V geomap vn.xy vn.geomap 1 1620 1 1844 fitgeo=general functio=polyn xxorder=2 xyorder=2 xxterms=half =====> V image is 1620 * 1844. rms in geomap is 0.156 and 0.061 for x and y geotran d75fms.fit d75fms_geo.fit vn.geomap vn.xy geotran d75nms.fit d75nms_geo.fit vn.geomap vn.xy geotran d75fcut.fit d75fcut_geo.fit vn.geomap vn.xy geotran d75ncut.fit d75ncut_geo.fit vn.geomap vn.xy =====> d75fms_geo.fit; d75nms_geo.fit; d75fcut.fit; d75ncut_geo.fit ---------------------------------------------------------------------------------------- Ellipse photometry: ### #Use d75ncl.tab as inellip to do photometry # copy ddo75fms_geo.pl/ddo75nms_geo.pl (the original mask file) to the new GALEX directory # as d75fms_geo.pl/d75nms_geo.pl. ellipse d75fms_geo.fit d75f_ell inellip=d75ncl.tab inter- region+ ellipse d75nms_geo.fit d75n_ell inellip=d75ncl.tab inter- region+ ====> d75f_ell.tab; d75n_ell.tab isoexam d75f_ell.tab isoexam d75n_ell.tab ====> d75f_ell.ps; d75n_ell.ps tprint d75f_ell.tab > d75f.phot tprint d75n_ell.tab > d75n.phot ====> d75f.phot; d75n.phot ---------------------------------------------------------------------------------------- Create input_galex file: FUV photometry file: 0=no FUV NUV photometry file: 0=no NUV Final output file Number of ellipses Integration time --- FUV Integration time --- NUV Average sky (counts/s/pixel) --- FUV Average sky (counts/s/pixel) --- NUV b/a D(Mpc) E(B-V) total scale of V image in "/pixel R_25 (arcsec), 9999.9 if none R_D (arcsec), 9999.9 if none The original input_galex file should work fine, but change to whatever filenames you are using. d75f.phot d75n.phot d75uv.final82 15 1663.32 1512.36 2.32379e-05 0.000201803 0.85 1.3 0.068 0.391 142.5 35.4 The sky is determined by scaling the sky to the V-band pixel size. implot d75nms and d75fms and measure sky in the middle of the galaxy. Then scale as (V-band pixel size/1.5)**2. =====> input_galex ---------------------------------------------------------------------------------------- Calibrate the photometry and determine surface brightnesses: ../annuli_galex82.exe =====> d75uv.final82 ---------------------------------------------------------------------------------------- Plot: uv_82.sm sm input uv_82.sm =====> d75uv_82.eps -------------------------------------- Fit exponential disk: fields d75uv.final82 2,5 lines="24-31" | polyfit stdin 1 > d75n_inner.expfit This gives you mu_NUV = mu_NUV^0 + slope * R(arcmin) ../expfit.exe ### This calculates R_D for you. give it d75n_inner.expfit mv expfit.out82 d75n_inner.expout fields d75uv.final82 2,5 lines="32-36" | polyfit stdin 1 > d75n_outer.expfit ../expfit.exe ### This calculates R_D for you. give it d75n_outer.expfit mv expfit.out82 d75n_outer.expout # Calculate the radius R_Br and surface brightness where they intersect. ../intersect.exe 1st file returned by POLYFIT: d75n_inner.expfit 2nd file returned by POLYFIT: d75n_outer.expfit ======> intersection x0 : 1.777 intersection x0 in Kpc: 0.672 intersection y0: 24.122 # =====> R_Br= 1.777 arcmin = 0.672 kpc at mu_NUV = 24.122 R_D inner = 2.281 +/- 0.327 arcmin = 0.863 +/- 0.124 kpc mu_NUV^0 inner = 24.967 +/- 0.072 R_D outer = 0.485 +/- 0.032 arcmin = 0.183 +/- 0.012 kpc y(100 kpc) outer = 612.56 ----------------------------------- Color: ../avecolors.exe Final file=d75uv.final82 Beg line for FUV-NUV(0=none)=24 End line for FUV-NUV(0=none)=36 =======>Ave FUV-NUV= 0.073 +/- 0.080 fields d75uv.final82 3,9 lines="24-31" | polyfit stdin 1 > d75fmn_inner.expfit This calculates FUV-NUV = zeropt + slope * R(kpc) =====> zeropt = 0.2423824 +/- 0.02141076; slope = -0.4032824 +/- 0.05382204 fields d75uv.final82 3,9 lines="32-36" | polyfit stdin 1 > d75fmn_outer.expfit This calculates FUV-NUV = zeropt + slope * R(kpc) =====> zeropt = -0.05788586 +/- 0.1595362; slope = 0.09170625 +/- 0.1744863 # ../intersect.exe Intersect at R_colBR= 0.229 kpc at FUV-NUV=-0.002 # fields d75uv.final82 3,9 lines="24-36" | polyfit stdin 1 > d75fmn_.expfit ======> zeropt= 0.1782625 +/- 0.03139764; slope= -0.1872993 +/- 0.04851029 y (100 kpc) = -18.5517 ---------------- Revise the FUV-NUV lines in uv_82.sm update : line 107 , line 108 , line 109 for NUV SB fitting plot. update : line 182 , line 183 for UV color plot with new Ave color ------------------------------------------ Combine with other photometry: Enter in galex2/photfiles_rev.list and cp to tempfiles.list and edit out all but galaxy that you are working on, or do them all at the end. ./collectv_lt.exe =====> d75allphot82.dat