NUMERICAL GRIDS OF QSO BROAD EMISSION-LINE STRENGTHS by Kirk Korista, Jack Baldwin, Gary Ferland and Dima Verner 1. INTRODUCTION This directory contains the full contents of the 9 photoionization grids presented in the paper "An Atlas of Computed Equivalent Widths of Quasar Broad Emission Lines", by Korista et al. (1997, ApJS, 108, 401). Here, we give the equivalent widths (defined below) of 218 emission lines and diffuse continuum measures, at 841 points on a grid of log(hydrogen ionizing photon flux) vs. log(hydrogen density) for several cloud column densities, incident continuum shapes, and a case of high metallicity (Z = 5 Z_sun). A simple recipe to convert these equivalent widths to fluxes is provided. These data should prove useful in the analysis of quasar emission line data and in the detailed modeling of quasar broad emission line regions. *********************************************************************** ****************************GRID HISTORY******************************* The history of the quasar emission line photoionization grids will be listed at this location. In the near term, only the results of the calculations presented in Korista et al. (1997) will be available. At future times, further grids may be made available as well, and will be noted here. If significant changes in CLOUDY warrant a revision of the grids, the revision will be noted here. ****Current Status**** 25.November.1996.: The current version of the QSO emission line grid set was run using CLOUDY version 90.02d. Several significant ``bugs'' in the code have been uncovered and fixed since submission of manuscript to the ApJS (which used version 90.01). However, most results changed very little (the results of the newer calculations were resubmitted to ApJS). 17.June.1997.: Minor modifications to this document. Most importantly: Phi_H is the hydrogen ionizing photon FLUX, not density, as was previously noted. Grids are scheduled to be updated at the end of Summer 1997 when CLOUDY 90.03 is stabilized. Additional grids may be added at this time. Line files should be smaller by 27% with updated write format. *********************************************************************** **************************GENERAL CAUTION****************************** Some individual lines may appear anomalously bright or dim at a single coordinate in the density-flux plane --- anomalous compared to what would be expected from its neighbors. This can happen when the optical depth scale of the model does not fully converge. Failure to converge is nearly always due to a numerical oscillation in the ionization near an imminent ionization front at the back of the cloud (the ionization front moves in and out of the cloud in sequential iterations). This generally occurs in a handful of models in any one grid, and almost never affects strongly the strengths of the emission lines; the O I line emission is one exception since it depends so critically upon the hydrogen ionization. *********************************************************************** **********************QUESTIONS AND COMMENTS*************************** Please send, via email, your questions and comments regarding these grids (including possible ``bugs'' present in the grids) to either Kirk Korista (korista@cloud9.pa.uky.edu) or Gary Ferland (gary@cloud9.pa.uky.edu). *********************************************************************** 2. AVAILABLE DATA SETS. Each of the 9 data sets is contained in a separate compressed tar file. Each tar file will generate a subdirectory containing 218 separate ascii files, one for each emission line or continuum measure. The following table gives the association between the names of the tar files, the sub-directories they will create, and the column density and continuum-shape parameters (as defined in the Korista et al. paper and in Section 5 below) used to generate the data set. The parameter k is described in Section 6 below. TABLE 1. Data Sets. File Name Sub-directory Col.Density E_peak alpha(o-x) k agn1_23.tar.Z ./agn1/stop_23 1.E23 44 -1.2 10.758 agn2_23.tar.Z ./agn2/stop_23 1.E23 22 -1.2 10.656 agn3_22.tar.Z ./agn3/stop_22 1.E22 44 -1.4 10.741 agn3_23.tar.Z ./agn3/stop_23 1.E23 44 -1.4 10.741 agn3_24.tar.Z ./agn3/stop_24 1.E24 44 -1.4 10.741 agn4_23.tar.Z ./agn4/stop_23 1.E23 22 -1.4 10.629 agn5_23.tar.Z ./agn5/stop_23 1.E23 44 -1.6 10.736 agn6_23.tar.Z ./agn6/stop_23 1.E23 22 -1.6 10.619 E_peak is the peak of the UV bump (in lambda*F_lambda) in units of eV, and alpha(o-x) is a measure of the relative strength of the X-ray power law to that of the UV bump component; these are discussed in more detail in Korista et al. (1997). These are all for solar metallicity; the data set for the 5 x solar metallicity case described in the paper is: agn3_23_Z05.tar.Z ./agn3/hiZ05 1.E23 44 -1.4 10.741 ==> CONSUMER WARNING: Each compressed tar file contains about 1.15 Mbytes, which expands into 6.921 Mbytes when uncompressed. For all 9 data sets together, this works out to 10.34 Mbytes compressed or about 62.29 Mbytes uncompressed. Our data are great and all that, but do you *really* want all nine datasets? 3. CONTENTS OF THE COMPRESSED TAR FILES. After ftp-ing the tar files into your directory, use the unix commands: uncompress dataset.tar.Z tar -xvf dataset.tar This will generate a new subdirectory with the name given in the above table, containing 218 separate ascii files. The ascii files have names fort.11, fort.12 ... fort.xxx 4. CONTENTS OF INDIVIDUAL ASCII FILES. The ascii files contain *normalized* dimensionless equivalent widths (hereafter: "EW"), defined as an emission-line strength divided by a continuum measure. The continuum measure used was always "inci 1215", the continuum level at 1215A in units of lambda*F_lambda, measured at the face of each cloud. Each file starts with a line identifying which emission line is described by the file, and the continuum measure it has been divided by: (emission line) (continuum) Example: totl 1216 inci 1215 indicates that the file contains the equivalent width of the Ly-alpha line computed by dividing the Cloudy output parameter "totl 1216" by the Cloudy output parameter "inci 1215". This results in a *normalized* dimensionless EW, referenced to the incident continuum at 1215 Angstroms. There are then two lines containing the words: H-density ionizing photon flux They describe the first two columns of the output to follow. This is followed by 841 lines giving the emission-line equivalent width at each point on the density-flux plane. The format is: log(n_H) log(Phi_H) EW where n_H and Phi_H are, respectively, the hydrogen number density and ionizing photon number flux as defined in the paper, and EW is the *normalized* dimensionless equivalent width as defined above. log(n_H) ranges from 7.000 to 14.000 in steps of .25. log(Phi_H) ranges from 17.000 to 24.000 ion steps of .25. Note that the normalized equivalent width is a linear (not logarithmic) value. The equivalent widths are the values predicted for full coverage of the continuum source (covering factor = 1, or 4*pi steradians of sky covered as seen from the continuum source). They are calculated for each line using the continuum at 1215A, not the local continuum. At the end of this document we append a long listing of the emission line or continuum measure corresponding to each fort file, using the emission-line and continuum-measure names from the Cloudy output, and giving a brief definition of each. Many emission lines appear (in separate fort files) as both "Totl" and "Inwd" values, corresponding respectively to the total emission in the inward plus outward directions from the cloud (the clouds are assumed plane-parallel), and to the emission from just the inward (illuminated) face. All lines are total fluxes unless "Inwd" is specifically stated. For some lines which are doublets, the Totl flux from each member is given sepearatly, followed by Totl and Inwd fluxes for the sum of the members. A "level 2 line" designation means that the line's gf-lambda are not precise and the line is not properly transferred. Note that the physics of the Fe II, Si II, and O I emission is complicated and the predicted emission for these lines is expected to have large uncertainties. Note too, that Fe III emission is expected to be important in many AGN/QSO spectra, especially near 1900A and 2080A, but these lines are, as of yet, unpredicted by CLOUDY. For further information about how the emission lines and continuum measures are defined, see Vol. IV of "Hazy, a Brief Introduction to Cloudy" and (as of 03.October.96.) the expanded Lines section, both available from (http://www.pa.uky.edu/~gary/cloudy). 5. DEFINITION OF CONTINUUM SHAPES The 44 eV UV bump peak with alpha_ox = -1.2 continuum was generated by CLOUDY with the command: agn kelvin 6.00 -1.20 -0.50 -1.00 The 22 eV UV bump peak with alpha_ox = -1.4 continuum was generated by CLOUDY with the command: agn kelvin 5.70 -1.40 -0.50 -1.00 etc. The -0.50 and -1.00 describe the power law slope in the optical/UV (alpha_uv) and X-ray (alpha_x), respectively. The optical/UV power law is cut off by an exponential with a characteristic temperature (T_cut) whose log is given as the first entry. alpha_ox, which normalizes the X-ray power law to the UV bump, is the second entry. The following represents the general analytic form of the continuum: f_nu ~ nu^alpha_uv * exp(-hnu/kT_cut) + nu^alpha_x See HAZY, volume 1, (CLOUDY homepage) for further details of how this command works. For those who require knowledge of average ionizing photon energy, _ion, in the incident continuum, in order to convert the number flux into an energy flux, 4*pi*r**2 * Phi_H = Q(H) = L_ion/_ion, we supply the _ion in eV for each continuum shape considered here: File Name Sub-directory _ion(eV) agn1_23.tar.Z ./agn1/stop_23 55.811 agn2_23.tar.Z ./agn2/stop_23 54.151 agn3_22.tar.Z ./agn3/stop_22 44.355 agn3_23.tar.Z ./agn3/stop_23 44.355 agn3_24.tar.Z ./agn3/stop_24 44.355 agn4_23.tar.Z ./agn4/stop_23 38.205 agn5_23.tar.Z ./agn5/stop_23 40.518 agn6_23.tar.Z ./agn6/stop_23 32.668 agn3_23_Z05.tar.Z ./agn3/hiZ05 44.355 6. CONVERTING NORMALIZED EQUIVALENT WIDTH TO CLOUD SURFACE FLUX. To convert to emitted flux F erg cm-2 s-1 at the surface of the cloud: F = EW * 10**(log Phi_H - k) where k is of order 10.7 and depends on the shape of the incident continuum. For clarity, Table 1 (Section 2 above) lists the value of k for each data set. To generate the intensity ratio of two emission lines, just take the ratio of their normalized equivalent width values. 7. PGPLOT PROGRAM FOR CONTOUR PLOTS The file pgcont.for in this directory contains a fortran program which calls pgplot subroutines to plot up to 100 contours of emission line EWs or ratios in the density--flux plane. Each page of plotted output will contain 6 grids of n_H vs. Phi_H in the same format used in the Korista et al. paper. 8. CONVERTING TO IRAF IMAGES FOR CONTOUR PLOTTING, ETC. Alternatively, you may find it convienient to convert the grids to IRAF images. You can then use IRAF tasks such as implot, splot, contour, imarith, imreplace, and stsdas routines such as imcalc to view and manipulate the results. Here is an iraf script that will find all of the files in the current directory with names fitting the template fort.* and create corresponding iraf images with names in the form "ifort.nn.imh"; i.e fort.11 gets turned into the image ifort.11.imh, etc: ######################################################################## procedure locim # iraf task to make an image from every ascii file with name fort.nn # note that the dimensions 29 x 29 are built in string filename struct *fortlist begin delete ("tmpfortlist", ver-) files("fort.*", > "tmpfortlist") fortlist="tmpfortlist" while (fscan(fortlist, file) !=EOF) { delete ("tmpfortjunk", ver-) fields (file, 3, > "tmpfortjunk") rtextimage ("tmpfortjunk", "i"//file, otype="real", head-, nskip=3, dim="29,29", pix+) imtranspose ("i"//file, "i"//file) print ("i"//file) } delete ("tmpfortjunk", ver-) delete ("tmpfortlist", ver-) end ######################################################################## To use this, while in IRAF type: task locim=locim.cl (or use a fuller pathname if locim.cl is not in the same directory as the data) locim The resulting images have log(n_H) increasing in the positive-x direction and log(Phi_H) decreasing in the positive-y direction (same orientation as in the Korista et al. paper). Note that the equivalent widths are on a linear scale, not a log scale as in the plots in the Korista et al. paper. If you wish to convert them to a log scale, try the IRAF task imfunction. APPENDIX - LISTING OF ASCII FILE CONTENTS The basic listing was made using "head -1 fort.* > index", and then annotated by hand. See Section 4 for further information. # Begin CLOUDY grid output line list... ==> fort.11 <== FeKa 2 inci 1215 Iron K-alpha line (near 6.4 keV) ==> fort.12 <== o 8r 19 inci 1215 O VIII 19A X-ray line ==> fort.13 <== o 4 609 inci 1215 total flux of O IV 609A; level 2 line ==> fort.14 <== mg10 610 inci 1215 total Mg X 610 ==> fort.15 <== mg10 625 inci 1215 total Mg X 625 ==> fort.16 <== totl 615 inci 1215 total of sum of both Mg X components ==> fort.17 <== o 5 630 inci 1215 total O V 630 ==> fort.18 <== s 4 655 inci 1215 total S IV 655; level 2 line ==> fort.19 <== n 3 678 inci 1215 total N III 679; level 2 line ==> fort.20 <== o 3 698 inci 1215 total O III 703; level 2 line ==> fort.21 <== s 4 737 inci 1215 total S IV 737; level 2 line ==> fort.22 <== n 3 752 inci 1215 total N III 764; level 2 line ==> fort.23 <== n 4 765 inci 1215 total N IV 765 ==> fort.24 <== ne 8 770 inci 1215 total Ne VIII 770 ==> fort.25 <== ne 8 780 inci 1215 total Ne VIII 780 ==> fort.26 <== totl 774 inci 1215 total of sum of both Ne VIII components ==> fort.27 <== inwd 774 inci 1215 inward flux of sum of both Ne VIII components ==> fort.28 <== s 5 786 inci 1215 total S V 786 ==> fort.29 <== o 4 789 inci 1215 total O IV 789 ==> fort.30 <== s 4 798 inci 1215 total S IV 798 ==> fort.31 <== o 3 835 inci 1215 total O III 834 ==> fort.32 <== totl 895 inci 1215 total Ne VII] 895 ==> fort.33 <== s 6 933 inci 1215 total S VI 933 ==> fort.34 <== s 6 944 inci 1215 total S VI 944 ==> fort.35 <== totl 933 inci 1215 total of sum of both S VI components ==> fort.36 <== p 4 950 inci 1215 total P IV 950; level 2 line ==> fort.37 <== totl 972 inci 1215 total Lyman-gamma 972 ==> fort.38 <== inwd 972 inci 1215 inward flux of Lyman-gamma 972 ==> fort.39 <== c 3 977 inci 1215 total C III 977 ==> fort.40 <== n 3 990 inci 1215 total N III 990 ==> fort.41 <== totl 1025 inci 1215 total Lyman-beta 1025 ==> fort.42 <== inwd 1025 inci 1215 inward flux of Lyman-beta 1025 ==> fort.43 <== o 6 1032 inci 1215 total O VI 1032 ==> fort.44 <== o 6 1037 inci 1215 total O VI 1037 ==> fort.45 <== totl 1035 inci 1215 total of sum of both O VI components ==> fort.46 <== inwd 1035 inci 1215 inward flux of sum of both O VI components ==> fort.47 <== 6lev 1039 inci 1215 total O I 1039 ==> fort.48 <== totl 1085 inci 1215 total He II Balmer-gamma 1085 ==> fort.49 <== n 2 1085 inci 1215 total N II 1085 ==> fort.50 <== s 4 1086 inci 1215 total S IV 1086; level 2 line ==> fort.51 <== p 5 1121 inci 1215 total P V 1121; level 2 line ==> fort.52 <== fe 3 1122 inci 1215 total Fe III 1122 ==> fort.53 <== ne 5 1141 inci 1215 total Ne V 1141 ==> fort.54 <== c 3 1176 inci 1215 total C III* 1176 ==> fort.55 <== s 3 1194 inci 1215 total S III 1194 ==> fort.56 <== totl 1198 inci 1215 total S V 1198 ==> fort.57 <== si 3 1207 inci 1215 total Si III 1207 ==> fort.58 <== inci 1215 inci 1215 incident continuum at 1215 Angstroms in units of nuF(nu) ==> fort.59 <== totl 1216 inci 1215 total Lyman-alpha 1215.67 ==> fort.60 <== inwd 1216 inci 1215 inward flux of Lyman-alpha ==> fort.61 <== totl 1217 inci 1215 total He II Balmer-beta 1216 ==> fort.62 <== totl 1218 inci 1215 total of sum of O V] 1218 + [O V] 1218 ==> fort.63 <== n 5 1239 inci 1215 total N V 1238.82 ==> fort.64 <== n 5 1243 inci 1215 total N V 1242.80 ==> fort.65 <== totl 1240 inci 1215 total of sum of both N V components ==> fort.66 <== inwd 1240 inci 1215 inward flux of sum of both N V components ==> fort.67 <== s 2 1256 inci 1215 total S II 1256 ==> fort.68 <== si 2 1260 inci 1215 total Si II 1260 + 1263 ==> fort.69 <== 6lev 1304 inci 1215 total O I 1302 + 1305 ==> fort.70 <== si 2 1305 inci 1215 total Si II 1305 ==> fort.71 <== c 2 1335 inci 1215 total C II 1335 + 1336 ==> fort.72 <== si 4 1394 inci 1215 total Si IV 1394 ==> fort.73 <== si 4 1403 inci 1215 total Si IV 1403 ==> fort.74 <== totl 1397 inci 1215 total of sum of both Si IV components ==> fort.75 <== inwd 1397 inci 1215 inward flux of sum of both Si IV components ==> fort.76 <== o 4 1402 inci 1215 total O IV] 1402 (5 components to line: 1397.2, 1399.77, 1401.16, 1404.81, 1407.39 -- not computed individually) ==> fort.77 <== s 4 1406 inci 1215 total S IV 1406 ==> fort.78 <== totl 1486 inci 1215 total of sum of N IV] 1486 + [N IV] ==> fort.79 <== si 2 1527 inci 1215 total Si II 1527 + 1533 ==> fort.80 <== c 4 1548 inci 1215 total C IV 1548.19 ==> fort.81 <== c 4 1551 inci 1215 total C IV 1550.77 ==> fort.82 <== totl 1549 inci 1215 total of sum of both C IV components ==> fort.83 <== inwd 1549 inci 1215 inward flux of sum of both C IV components ==> fort.84 <== totl 1640 inci 1215 total He II Balmer-alpha 1640 ==> fort.85 <== inwd 1640 inci 1215 inward flux of He II Balmer-alpha 1640 ==> fort.86 <== o 3 1661 inci 1215 total O III] 1663 ==> fort.87 <== o 3 1666 inci 1215 total O III] 1666 ==> fort.88 <== totl 1665 inci 1215 total of sum of both O III] components ==> fort.89 <== al 2 1670 inci 1215 total Al II 1670.8; level 2 line ==> fort.90 <== n 4 1718 inci 1215 total N IV 1718.55; level 2 line ==> fort.91 <== s 3 1720 inci 1215 total S III 1720 ==> fort.92 <== n 3 1750 inci 1215 total N III] 1750 (all components; not computed seperately) ==> fort.93 <== fe 2 1787 inci 1215 total Fe II 1787 (probably selectively excited) ==> fort.94 <== si 2 1808 inci 1215 total Si II 1814 (1808.0 + 1816.9 + 1817.5) ==> fort.95 <== al 3 1855 inci 1215 total Al III 1855 ==> fort.96 <== al 3 1863 inci 1215 total Al III 1863 ==> fort.97 <== totl 1860 inci 1215 total sum of both Al III components ==> fort.98 <== inwd 1860 inci 1215 inward flux of sum of both Al III components ==> fort.99 <== totl 1888 inci 1215 total of sum of Si III] 1892 + [Si III] ==> fort.100 <== totl 1909 inci 1215 total of sum of C III] 1908.73 + [C III] ==> fort.101 <== n 2 2140 inci 1215 total sum of N II] 2139.01, 2142.77 ==> fort.102 <== c 3 2297 inci 1215 total C III 2297; level 2 line ==> fort.103 <== c 2 2326 inci 1215 total C II] 2324.69 + 2328.12 ==> fort.104 <== si 2 2335 inci 1215 total Si II] 2335 ==> fort.105 <== totl 2665 inci 1215 total of sum of Al II] 2669 + [Al II] ==> fort.106 <== mg 2 2796 inci 1215 total Mg II 2796 of the doublet ==> fort.107 <== mg 2 2804 inci 1215 total Mg II 2804 of the doublet ==> fort.108 <== totl 2798 inci 1215 total of sum of both Mg II components ==> fort.109 <== inwd 2798 inci 1215 inward flux of sum of both Mg II components ==> fort.110 <== BA C 0 inci 1215 total of integrated H balmer continuum ==> fort.111 <== BaC 3646 inci 1215 total of nuFnu of Balmer jump at 3646 above the underlying Paschen continuum ==> fort.112 <== ca2k 3934 inci 1215 total Ca II 3934 emission ==> fort.113 <== ca2h 3969 inci 1215 total Ca II 3969 emission ==> fort.114 <== totl 4102 inci 1215 total H-delta ==> fort.115 <== inwd 4102 inci 1215 inward flux of H-delta ==> fort.116 <== totl 4340 inci 1215 total H-gamma ==> fort.117 <== inwd 4340 inci 1215 inward flux of H-gamma ==> fort.118 <== o 2 4341 inci 1215 total O II 4341; level 2 line ==> fort.119 <== 6lev 4368 inci 1215 total O I 4368 ==> fort.120 <== He I 4471 inci 1215 total He I 4471 ==> fort.121 <== o 2 4651 inci 1215 O II 4651; level 2 line ==> fort.122 <== totl 4686 inci 1215 total He II 4686 ==> fort.123 <== inwd 4686 inci 1215 inward flux of He II 4686 ==> fort.124 <== totl 4861 inci 1215 total H-beta 4861 ==> fort.125 <== inwd 4861 inci 1215 inward flux of H-beta 4861 ==> fort.126 <== totl 5876 inci 1215 total He I 5876 ==> fort.127 <== inwd 5876 inci 1215 inward flux of He I 5876 ==> fort.128 <== na 1 5895 inci 1215 total Na ID 5895 ==> fort.129 <== totl 6563 inci 1215 total H-alpha 6563 ==> fort.130 <== inwd 6563 inci 1215 inward flux of H-alpha 6563 ==> fort.131 <== k 1 7745 inci 1215 total K I 7745 ==> fort.132 <== 6lev 8446 inci 1215 total O I 8446 ==> fort.133 <== ca2x 8498 inci 1215 total Ca II 8498 ==> fort.134 <== ca2y 8542 inci 1215 total Ca II 8542 ==> fort.135 <== ca2z 8662 inci 1215 total Ca II 8662 ==> fort.136 <== PA C 0 inci 1215 total of integrated H Paschen continuum ==> fort.137 <== totl 10830 inci 1215 total He I 10,830A ==> fort.138 <== totl 18752 inci 1215 total H Paschen-alpha # The following 11 "lines" represent emission by a "6-level" Fe II atom # of Hamann & Ferland, a modification of the Wills, Netzer, and Wills. # See HAZY for some details. ==> fort.139 <== fe 2 6200 inci 1215 ==> fort.140 <== fe 2 4300 inci 1215 ==> fort.141 <== fe 2 2400 inci 1215 ==> fort.142 <== fe 2 1100 inci 1215 ==> fort.143 <== fe 2 1500 inci 1215 ==> fort.144 <== fe 2 11500 inci 1215 ==> fort.145 <== fe 2 2500 inci 1215 ==> fort.146 <== fe 2 2300 inci 1215 ==> fort.147 <== fe 2 8900 inci 1215 ==> fort.148 <== fe 2 1216 inci 1215 pumping of the Fe II atom via H Lya 1216 ==> fort.149 <== fe2c 0 inci 1215 cooling from the Fe II atom ==> fort.150 <== ne 5 3426 inci 1215 total [Ne V] 3426 ==> fort.151 <== ne 3 3869 inci 1215 total [Ne III] 3869 ==> fort.152 <== totl 4363 inci 1215 total [O III] 4363 ==> fort.153 <== o 3 5007 inci 1215 total [O III] 5007 ==> fort.154 <== Fe14 5303 inci 1215 total [Fe XIV] 5303 ==> fort.155 <== o 1 5577 inci 1215 total [O I] 5577 ==> fort.156 <== Fe 7 6087 inci 1215 total [Fe VII] 6087 ==> fort.157 <== o 1 6300 inci 1215 total [O I] 6300 ==> fort.158 <== Fe10 6375 inci 1215 total [Fe X] 6375 ==> fort.159 <== Fe11 7892 inci 1215 total [Fe XI] 7892 ==> fort.160 <== inci 4860 inci 1215 incident continuum at 4860 Angstroms in units of nuF(nu) # The following are the total non-line emission from the cloud # (diffuse + reflected continuum) at a given wavelength in Angstroms. ==> fort.161 <== nFnu 11186 inci 1215 ==> fort.162 <== nFnu 8220 inci 1215 ==> fort.163 <== nFnu 8205 inci 1215 ==> fort.164 <== nFnu 6209 inci 1215 ==> fort.165 <== nFnu 4885 inci 1215 ==> fort.166 <== nFnu 3649 inci 1215 ==> fort.167 <== nFnu 3644 inci 1215 ==> fort.168 <== nFnu 2392 inci 1215 ==> fort.169 <== nFnu 2071 inci 1215 ==> fort.170 <== nFnu 2052 inci 1215 ==> fort.171 <== nFnu 1793 inci 1215 # In optically thick clouds of significant H I columns, Lya "Rayleigh # scattering" of incident continuum becomes important beginning here and # extending down to the Lyman limit. ==> fort.172 <== nFnu 1458 inci 1215 ==> fort.173 <== nFnu 1356 inci 1215 ==> fort.174 <== nFnu 1297 inci 1215 ==> fort.175 <== nFnu 1262 inci 1215 ==> fort.176 <== nFnu 1218 inci 1215 ==> fort.177 <== nFnu 1196 inci 1215 ==> fort.178 <== nFnu 1175 inci 1215 ==> fort.179 <== nFnu 1143 inci 1215 ==> fort.180 <== nFnu 1113 inci 1215 ==> fort.181 <== nFnu 1103 inci 1215 ==> fort.182 <== nFnu 1073 inci 1215 ==> fort.183 <== nFnu 1064 inci 1215 ==> fort.184 <== nFnu 1035 inci 1215 ==> fort.185 <== nFnu 1000 inci 1215 ==> fort.186 <== nFnu 913 inci 1215 ==> fort.187 <== nFnu 911 inci 1215 ==> fort.188 <== nFnu 760 inci 1215 ==> fort.189 <== nFnu 701 inci 1215 ==> fort.190 <== nFnu 608 inci 1215 ==> fort.191 <== nFnu 575 inci 1215 ==> fort.192 <== nFnu 505 inci 1215 ==> fort.193 <== nFnu 503 inci 1215 ==> fort.194 <== nFnu 399 inci 1215 # The following are the inward directed non-line emission from the cloud # (diffuse + reflected continuum) at a given wavelength in Angstroms. ==> fort.195 <== InwT 11186 inci 1215 ==> fort.196 <== InwT 8220 inci 1215 ==> fort.197 <== InwT 8205 inci 1215 ==> fort.198 <== InwT 6209 inci 1215 ==> fort.199 <== InwT 4885 inci 1215 ==> fort.200 <== InwT 3649 inci 1215 ==> fort.201 <== InwT 3644 inci 1215 ==> fort.202 <== InwT 2392 inci 1215 ==> fort.203 <== InwT 2071 inci 1215 ==> fort.204 <== InwT 2052 inci 1215 ==> fort.205 <== InwT 1793 inci 1215 ==> fort.206 <== InwT 1458 inci 1215 ==> fort.207 <== InwT 1356 inci 1215 ==> fort.208 <== InwT 1297 inci 1215 ==> fort.209 <== InwT 1262 inci 1215 ==> fort.210 <== InwT 1218 inci 1215 ==> fort.211 <== InwT 1196 inci 1215 ==> fort.212 <== InwT 1175 inci 1215 ==> fort.213 <== InwT 1143 inci 1215 ==> fort.214 <== InwT 1113 inci 1215 ==> fort.215 <== InwT 1103 inci 1215 ==> fort.216 <== InwT 1073 inci 1215 ==> fort.217 <== InwT 1064 inci 1215 ==> fort.218 <== InwT 1035 inci 1215 ==> fort.219 <== InwT 1000 inci 1215 ==> fort.220 <== InwT 913 inci 1215 ==> fort.221 <== InwT 911 inci 1215 ==> fort.222 <== InwT 760 inci 1215 ==> fort.223 <== InwT 701 inci 1215 ==> fort.224 <== InwT 608 inci 1215 ==> fort.225 <== InwT 575 inci 1215 ==> fort.226 <== InwT 505 inci 1215 ==> fort.227 <== InwT 503 inci 1215 ==> fort.228 <== InwT 399 inci 1215 # End of CLOUDY grid output...