From paco@usmu01.usm.uni-muenchen.deTue Sep 23 11:08:24 1997 Date: Tue, 23 Sep 1997 08:10:13 +0200 (MET DST) From: Francisco Najarro To: Ian Howarth Subject: Wrong figure. Hi Ian, I've just found out that I gave to you a wrong ps figure. In figure_2_b I sent to you I had convolved the HeI profiles with 200km/s resolution, while the H ones (figure_2_a) where unconvolved. I've also found a couple of new typos (I was not able to write HDE316285 twice in a row correctly). Please find enclosed the new figure_2_b.ps file and the tex file. Cheers Paco *************************** BEGIN figure_2_b.ps *********************** %!PS-Adobe-3.0 %%BoundingBox: 54 127 465 679 %%Title: Graphics produced by IDL %%For: paco@hal2.usm.uni-muenchen.de, /e/ud2/users/paco/modpro/pcyg/profi %%Creator: IDL Version 4.0 (OSF alpha) %%CreationDate: Mon Sep 22 21:23:45 1997 %%DocumentData: Clean7bit %%LanguageLevel: 1 %%PageOrder: Ascend %%Pages: (atend) %%DocumentNeededResources: (atend) %%EndComments %%BeginProlog %+ prolog.ps -- Prolog for IDL generated PostScript files %+ Copyright (c) 1988-1993 Research Systems, Inc. All Rights Reserved. %v 3 save /$IDL_DICT 40 dict def $IDL_DICT begin /bdef { bind def } bind def /C {currentpoint newpath moveto} bdef /CP {currentpoint} bdef /D {currentpoint stroke moveto} bdef /F {closepath fill} bdef /K { setgray } bdef /M {moveto} bdef /N {rmoveto} bdef /P {lineto} bdef /R {rlineto} bdef /S {gsave show grestore} bdef /X {currentpoint pop} bdef /Z {gsave currentpoint lineto 20 setlinewidth 1 setlinecap stroke grestore} bdef /L0 {[] 0 setdash} bdef /L1 {[40 100] 0 setdash} bdef /L2 {[200 200] 0 setdash} bdef /L3 {[200 100 50 100] 0 setdash} bdef /L4 {[300 100 50 100 50 100 50 100] 0 setdash} bdef /L5 {[400 200] 0 setdash} bdef /STDFONT { findfont exch scalefont setfont } bdef /ISOFONT { findfont dup length dict begin { 1 index /FID ne {def} {pop pop} ifelse } forall /Encoding ISOLatin1Encoding def currentdict end /idltmpfont exch definefont exch scalefont setfont } bdef /ISOBULLET { gsave /Helvetica findfont exch scalefont setfont (\267) show currentpoint grestore moveto} bdef end 2.5 setmiterlimit %%EndProlog %%Page: 0 1 %%PageResources: (atend) %%PageOrientation: Portrait %%PageBoundingBox: 54 127 465 679 %%BeginPageSetup save $IDL_DICT begin 54 127 translate 0.0283465 dup scale %%IncludeResource: font Helvetica 423.333 /Helvetica STDFONT %%EndPageSetup 20 setlinewidth L0 0.000 K 666 13264 M 6417 0 R D 666 13264 M 0 108 R D 2270 13264 M 0 108 R D 3874 13264 M 0 108 R D 5479 13264 M 0 108 R D 7083 13264 M 0 108 R D 1067 13264 M 0 54 R D 1468 13264 M 0 54 R D 1869 13264 M 0 54 R D 2671 13264 M 0 54 R D 3072 13264 M 0 54 R D 3473 13264 M 0 54 R D 4275 13264 M 0 54 R D 4677 13264 M 0 54 R D 5078 13264 M 0 54 R D 5880 13264 M 0 54 R D 6281 13264 M 0 54 R D 6682 13264 M 0 54 R D 666 18708 M 6417 0 R D 666 18708 M 0 -109 R D 2270 18708 M 0 -109 R D 3874 18708 M 0 -109 R D 5479 18708 M 0 -109 R D 7083 18708 M 0 -109 R D 1067 18708 M 0 -55 R D 1468 18708 M 0 -55 R D 1869 18708 M 0 -55 R D 2671 18708 M 0 -55 R D 3072 18708 M 0 -55 R D 3473 18708 M 0 -55 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26 26 R 0 -184 R D 354 6332 M -8 -8 R 8 -9 R 9 9 R -9 8 R D 442 6499 M 97 0 R -53 -70 R 26 0 R 18 -9 R 9 -9 R 8 -26 R 0 -18 R -8 -26 R -18 -17 R -26 -9 R -27 0 R -26 9 R -9 8 R -8 18 R D 666 1148 M 64 0 R D 666 1505 M 64 0 R D 666 1862 M 64 0 R D 666 2575 M 64 0 R D 666 2932 M 64 0 R D 666 3289 M 64 0 R D 666 4002 M 64 0 R D 666 4359 M 64 0 R D 666 4716 M 64 0 R D 666 5429 M 64 0 R D 666 5786 M 64 0 R D 666 6143 M 64 0 R D -289 3356 M 184 0 R D -324 3567 M 290 -158 R D -289 3619 M 184 0 R D -201 3786 M -18 -18 R -8 -17 R 0 -27 R 8 -17 R 18 -18 R 26 -8 R 18 0 R 26 8 R 18 18 R 8 17 R 0 27 R -8 17 R -18 18 R D 7083 792 M 0 5708 R D 7083 792 M -128 0 R D 7083 2219 M -128 0 R D 7083 3646 M -128 0 R D 7083 5073 M -128 0 R D 7083 6500 M -128 0 R D 7083 1148 M -64 0 R D 7083 1505 M -64 0 R D 7083 1862 M -64 0 R D 7083 2575 M -64 0 R D 7083 2932 M -64 0 R D 7083 3289 M -64 0 R D 7083 4002 M -64 0 R D 7083 4359 M -64 0 R D 7083 4716 M -64 0 R D 7083 5429 M -64 0 R D 7083 5786 M -64 0 R D 7083 6143 M -64 0 R D 666 4359 M 200 0 R 201 0 R 200 0 R 201 0 R 200 0 R 201 0 R 200 -1 R 201 -31 R 32 -19 R 32 -29 R 32 -40 R 32 -55 R 32 -72 R 32 -92 R 33 -113 R 32 -134 R 32 -154 R 32 -170 R 32 -182 R 32 -189 R 32 -190 R 32 -186 R 32 -176 R 32 -163 R 32 -149 R 32 -133 R 33 -116 R 32 -99 R 32 -83 R 32 -67 R 32 -51 R 32 -36 R 32 -20 R 32 -6 R 32 9 R 32 23 R 32 36 R 33 49 R 32 60 R 32 70 R 32 78 R 32 83 R 32 86 R 32 90 R 32 90 R 32 89 R 32 88 R 32 87 R 33 85 R 32 84 R 32 81 R 32 79 R 32 76 R 32 75 R 32 73 R 32 70 R 32 68 R 32 66 R 32 64 R 32 62 R 33 60 R 32 57 R 32 55 R 32 53 R 32 51 R 32 49 R 32 47 R 32 45 R 32 42 R 32 40 R 32 39 R 33 36 R 32 34 R 32 32 R 32 31 R 32 28 R 32 26 R 32 24 R 32 23 R 32 20 R 32 19 R 32 17 R 33 16 R 32 14 R 32 12 R 32 11 R 32 10 R 32 8 R 32 7 R 32 6 R 32 5 R 32 4 R 32 4 R 33 3 R 32 2 R 32 1 R 32 2 R 32 1 R 32 0 R 32 1 R 32 0 R 32 0 R 32 0 R 32 0 R 32 0 R 33 0 R 32 0 R 32 0 R 200 0 R 201 0 R 200 0 R 201 0 R 200 0 R 201 0 R 201 0 R 200 0 R D 5306 5554 M 0 -196 R D 5437 5554 M 0 -196 R D 5306 5461 M 131 0 R D 5502 5433 M 113 0 R 0 18 R -10 19 R -9 10 R -19 9 R -28 0 R -18 -9 R -19 -19 R -10 -28 R 0 -19 R 10 -28 R 19 -19 R 18 -9 R 28 0 R 19 9 R 19 19 R D 5680 5554 M 0 -196 R D 5989 5554 M -94 -131 R 140 0 R D 5989 5554 M 0 -196 R D 6175 5554 M -93 -131 R 140 0 R D 6175 5554 M 0 -196 R D 6288 5377 M -10 -10 R 10 -9 R 9 9 R -9 10 R D 6419 5554 M -29 -9 R -18 -28 R -10 -47 R 0 -28 R 10 -47 R 18 -28 R 29 -9 R 18 0 R 28 9 R 19 28 R 9 47 R 0 28 R -9 47 R -19 28 R -28 9 R -18 0 R D 6587 5489 M -56 -206 R D 6577 5451 M -9 -46 R 0 -28 R 19 -19 R 18 0 R 19 9 R 19 19 R 19 37 R 18 66 R D 6662 5423 M -10 -37 R 0 -19 R 10 -9 R 18 0 R 19 19 R 9 18 R D 7916 792 M 6417 0 R D 7916 792 M 0 114 R D 7565 474 M 158 0 R D 7872 580 M -88 -123 R 132 0 R D 7872 580 M 0 -184 R D 8012 580 M -26 -9 R -18 -26 R -9 -44 R 0 -27 R 9 -43 R 18 -27 R 26 -8 R 17 0 R 27 8 R 17 27 R 9 43 R 0 27 R -9 44 R -17 26 R -27 9 R -17 0 R D 8187 580 M -26 -9 R -18 -26 R -8 -44 R 0 -27 R 8 -43 R 18 -27 R 26 -8 R 18 0 R 26 8 R 18 27 R 8 43 R 0 27 R -8 44 R -18 26 R -26 9 R -18 0 R D 9520 792 M 0 114 R D 9169 474 M 158 0 R D 9397 536 M 0 9 R 9 17 R 9 9 R 17 9 R 35 0 R 18 -9 R 9 -9 R 8 -17 R 0 -18 R -8 -17 R -18 -27 R -87 -87 R 122 0 R D 9616 580 M -26 -9 R -17 -26 R -9 -44 R 0 -27 R 9 -43 R 17 -27 R 26 -8 R 18 0 R 26 8 R 18 27 R 8 43 R 0 27 R -8 44 R -18 26 R -26 9 R -18 0 R D 9792 580 M -27 -9 R -17 -26 R -9 -44 R 0 -27 R 9 -43 R 17 -27 R 27 -8 R 17 0 R 26 8 R 18 27 R 9 43 R 0 27 R -9 44 R -18 26 R -26 9 R -17 0 R D 11124 792 M 0 114 R D 11107 580 M -26 -9 R -18 -26 R -9 -44 R 0 -27 R 9 -43 R 18 -27 R 26 -8 R 17 0 R 27 8 R 17 27 R 9 43 R 0 27 R -9 44 R -17 26 R -27 9 R -17 0 R D 12729 792 M 0 114 R D 12492 536 M 0 9 R 9 17 R 9 9 R 17 9 R 35 0 R 18 -9 R 8 -9 R 9 -17 R 0 -18 R -9 -17 R -17 -27 R -88 -87 R 123 0 R D 12711 580 M -26 -9 R -18 -26 R -8 -44 R 0 -27 R 8 -43 R 18 -27 R 26 -8 R 18 0 R 26 8 R 18 27 R 8 43 R 0 27 R -8 44 R -18 26 R -26 9 R -18 0 R D 12886 580 M -26 -9 R -17 -26 R -9 -44 R 0 -27 R 9 -43 R 17 -27 R 26 -8 R 18 0 R 26 8 R 18 27 R 9 43 R 0 27 R -9 44 R -18 26 R -26 9 R -18 0 R D 14333 792 M 0 114 R D 14175 580 M -87 -123 R 131 0 R D 14175 580 M 0 -184 R D 14316 580 M -27 -9 R -17 -26 R -9 -44 R 0 -27 R 9 -43 R 17 -27 R 27 -8 R 17 0 R 26 8 R 18 27 R 9 43 R 0 27 R -9 44 R -18 26 R -26 9 R -17 0 R D 14491 580 M -26 -9 R -18 -26 R -9 -44 R 0 -27 R 9 -43 R 18 -27 R 26 -8 R 17 0 R 27 8 R 17 27 R 9 43 R 0 27 R -9 44 R -17 26 R -27 9 R -17 0 R D 8317 792 M 0 57 R D 8718 792 M 0 57 R D 9119 792 M 0 57 R D 9921 792 M 0 57 R D 10322 792 M 0 57 R D 10723 792 M 0 57 R D 11525 792 M 0 57 R D 11927 792 M 0 57 R D 12328 792 M 0 57 R D 13130 792 M 0 57 R D 13531 792 M 0 57 R D 13932 792 M 0 57 R D 10518 236 M 70 -184 R 70 184 R D 10903 271 M -17 -17 R -18 -26 R -17 -35 R -9 -44 R 0 -35 R 9 -44 R 17 -44 R 18 -26 R 17 -17 R D 10965 236 M 0 -184 R D 11052 175 M -87 -88 R D 11000 123 M 61 -71 R D 11113 175 M 0 -123 R D 11113 140 M 27 26 R 17 9 R 27 0 R 17 -9 R 9 -26 R 0 -88 R D 11210 140 M 26 26 R 18 9 R 26 0 R 18 -9 R 8 -26 R 0 -88 R D 11464 149 M -9 17 R -26 9 R -26 0 R -27 -9 R -8 -17 R 8 -18 R 18 -8 R 44 -9 R 17 -9 R 9 -18 R 0 -8 R -9 -18 R -26 -9 R -26 0 R -27 9 R -8 18 R D 11515 234 M 98 0 R D 11667 278 M 11 5 R 16 17 R 0 -114 R D 11766 271 M 18 -17 R 17 -26 R 18 -35 R 8 -44 R 0 -35 R -8 -44 R -18 -44 R -17 -26 R -18 -17 R D 7916 6500 M 6417 0 R D 7916 6500 M 0 -115 R D 9520 6500 M 0 -115 R D 11124 6500 M 0 -115 R D 12729 6500 M 0 -115 R D 14333 6500 M 0 -115 R D 8317 6500 M 0 -57 R D 8718 6500 M 0 -57 R D 9119 6500 M 0 -57 R D 9921 6500 M 0 -57 R D 10322 6500 M 0 -57 R D 10723 6500 M 0 -57 R D 11525 6500 M 0 -57 R D 11927 6500 M 0 -57 R D 12328 6500 M 0 -57 R D 13130 6500 M 0 -57 R D 13531 6500 M 0 -57 R D 13932 6500 M 0 -57 R D 7916 792 M 0 5708 R D 7916 792 M 128 0 R D 7289 976 M -26 -9 R -18 -26 R -9 -44 R 0 -27 R 9 -43 R 18 -27 R 26 -8 R 18 0 R 26 8 R 17 27 R 9 43 R 0 27 R -9 44 R -17 26 R -26 9 R -18 0 R D 7429 809 M -9 -9 R 9 -8 R 9 8 R -9 9 R D 7613 914 M -9 -26 R -17 -18 R -26 -8 R -9 0 R -26 8 R -18 18 R -9 26 R 0 9 R 9 26 R 18 18 R 26 9 R 9 0 R 26 -9 R 17 -18 R 9 -35 R 0 -44 R -9 -43 R -17 -27 R -26 -8 R -18 0 R -26 8 R -9 18 R D 7780 976 M -88 0 R -9 -79 R 9 9 R 26 8 R 27 0 R 26 -8 R 18 -18 R 8 -26 R 0 -18 R -8 -26 R -18 -18 R -26 -8 R -27 0 R -26 8 R -9 9 R -8 18 R D 7916 2219 M 128 0 R D 7263 2262 M 17 9 R 27 26 R 0 -184 R D 7429 2131 M -9 -9 R 9 -9 R 9 9 R -9 9 R D 7552 2297 M -26 -9 R -18 -26 R -9 -44 R 0 -26 R 9 -44 R 18 -26 R 26 -9 R 17 0 R 27 9 R 17 26 R 9 44 R 0 26 R -9 44 R -17 26 R -27 9 R -17 0 R D 7727 2297 M -26 -9 R -18 -26 R -8 -44 R 0 -26 R 8 -44 R 18 -26 R 26 -9 R 18 0 R 26 9 R 18 26 R 8 44 R 0 26 R -8 44 R -18 26 R -26 9 R -18 0 R D 7916 3646 M 128 0 R D 7263 3689 M 17 9 R 27 26 R 0 -184 R D 7429 3558 M -9 -9 R 9 -9 R 9 9 R -9 9 R D 7552 3724 M -26 -9 R -18 -26 R -9 -44 R 0 -26 R 9 -44 R 18 -26 R 26 -9 R 17 0 R 27 9 R 17 26 R 9 44 R 0 26 R -9 44 R -17 26 R -27 9 R -17 0 R D 7780 3724 M -88 0 R -9 -79 R 9 9 R 26 9 R 27 0 R 26 -9 R 18 -18 R 8 -26 R 0 -17 R -8 -27 R -18 -17 R -26 -9 R -27 0 R -26 9 R -9 9 R -8 17 R D 7916 5073 M 128 0 R D 7263 5116 M 17 9 R 27 26 R 0 -184 R D 7429 4985 M -9 -9 R 9 -9 R 9 9 R -9 9 R D 7526 5116 M 17 9 R 26 26 R 0 -184 R D 7727 5151 M -26 -9 R -18 -26 R -8 -44 R 0 -26 R 8 -44 R 18 -26 R 26 -9 R 18 0 R 26 9 R 18 26 R 8 44 R 0 26 R -8 44 R -18 26 R -26 9 R -18 0 R D 7916 6500 M 128 0 R D 7263 6464 M 17 9 R 27 26 R 0 -184 R D 7429 6332 M -9 -8 R 9 -9 R 9 9 R -9 8 R D 7526 6464 M 17 9 R 26 26 R 0 -184 R D 7780 6499 M -88 0 R -9 -79 R 9 9 R 26 8 R 27 0 R 26 -8 R 18 -18 R 8 -26 R 0 -18 R -8 -26 R -18 -17 R -26 -9 R -27 0 R -26 9 R -9 8 R -8 18 R D 7916 1148 M 64 0 R D 7916 1505 M 64 0 R D 7916 1862 M 64 0 R D 7916 2575 M 64 0 R D 7916 2932 M 64 0 R D 7916 3289 M 64 0 R D 7916 4002 M 64 0 R D 7916 4359 M 64 0 R D 7916 4716 M 64 0 R D 7916 5429 M 64 0 R D 7916 5786 M 64 0 R D 7916 6143 M 64 0 R D 14333 792 M 0 5708 R D 14333 792 M -128 0 R D 14333 2219 M -128 0 R D 14333 3646 M -128 0 R D 14333 5073 M -128 0 R D 14333 6500 M -128 0 R D 14333 1148 M -64 0 R D 14333 1505 M -64 0 R D 14333 1862 M -64 0 R D 14333 2575 M -64 0 R D 14333 2932 M -64 0 R D 14333 3289 M -64 0 R D 14333 4002 M -64 0 R D 14333 4359 M -64 0 R D 14333 4716 M -64 0 R D 14333 5429 M -64 0 R D 14333 5786 M -64 0 R D 14333 6143 M -64 0 R D 7916 2219 M 200 0 R 201 0 R 200 0 R 201 0 R 200 0 R 201 0 R 200 1 R 201 42 R 32 26 R 32 37 R 32 53 R 32 71 R 32 95 R 32 120 R 33 149 R 32 180 R 32 210 R 32 240 R 32 267 R 32 289 R 32 306 R 32 314 R 32 314 R 32 305 R 32 284 R 32 255 R 33 216 R 32 173 R 32 125 R 32 76 R 32 28 R 32 -16 R 32 -54 R 32 -85 R 32 -109 R 32 -128 R 32 -140 R 33 -145 R 32 -148 R 32 -146 R 32 -143 R 32 -137 R 32 -132 R 32 -124 R 32 -118 R 32 -111 R 32 -105 R 32 -99 R 33 -94 R 32 -89 R 32 -84 R 32 -80 R 32 -76 R 32 -73 R 32 -70 R 32 -67 R 32 -64 R 32 -62 R 32 -59 R 32 -57 R 33 -56 R 32 -54 R 32 -52 R 32 -51 R 32 -50 R 32 -48 R 32 -48 R 32 -47 R 32 -45 R 32 -45 R 32 -44 R 33 -43 R 32 -42 R 32 -41 R 32 -40 R 32 -39 R 32 -38 R 32 -37 R 32 -36 R 32 -35 R 32 -33 R 32 -33 R 33 -31 R 32 -30 R 32 -28 R 32 -28 R 32 -26 R 32 -25 R 32 -24 R 32 -22 R 32 -22 R 32 -20 R 32 -19 R 33 -18 R 32 -16 R 32 -15 R 32 -14 R 32 -12 R 32 -11 R 32 -9 R 32 -8 R 32 -7 R 32 -5 R 32 -4 R 32 -3 R 33 -2 R 32 -2 R 32 -1 R 200 -2 R 201 0 R 200 0 R 201 0 R 200 0 R 201 0 R 201 0 R 200 0 R D 12556 5554 M 0 -196 R D 12687 5554 M 0 -196 R D 12556 5461 M 131 0 R D 12752 5433 M 113 0 R 0 18 R -10 19 R -9 10 R -19 9 R -28 0 R -18 -9 R -19 -19 R -10 -28 R 0 -19 R 10 -28 R 19 -19 R 18 -9 R 28 0 R 19 9 R 19 19 R D 12930 5554 M 0 -196 R D 13164 5554 M 103 0 R -56 -74 R 28 0 R 18 -10 R 10 -9 R 9 -28 R 0 -19 R -9 -28 R -19 -19 R -28 -9 R -28 0 R -28 9 R -10 10 R -9 18 R D 13444 5554 M -93 0 R -10 -84 R 10 10 R 28 9 R 28 0 R 28 -9 R 19 -19 R 9 -28 R 0 -19 R -9 -28 R -19 -19 R -28 -9 R -28 0 R -28 9 R -10 10 R -9 18 R D 13538 5377 M -10 -10 R 10 -9 R 9 9 R -9 10 R D 13659 5554 M -28 -9 R -9 -19 R 0 -18 R 9 -19 R 19 -9 R 37 -10 R 28 -9 R 19 -19 R 9 -19 R 0 -28 R -9 -18 R -9 -10 R -28 -9 R -38 0 R -28 9 R -9 10 R -10 18 R 0 28 R 10 19 R 18 19 R 29 9 R 37 10 R 19 9 R 9 19 R 0 18 R -9 19 R -28 9 R -38 0 R D 13837 5489 M -56 -206 R D 13827 5451 M -9 -46 R 0 -28 R 19 -19 R 18 0 R 19 9 R 19 19 R 19 37 R 18 66 R D 13912 5423 M -10 -37 R 0 -19 R 10 -9 R 18 0 R 19 19 R 9 18 R D %%PageTrailer showpage end restore %%PageResources: font Helvetica %%Trailer restore %%Pages: 1 %%DocumentNeededResources: font Helvetica %%EOF ************************************* BEGIN TEX FILE ********************8 \documentstyle[11pt,paspconf,psfig]{article} %Checked for refs %***************** BEGIN Paco's definitions \def\my{\hbox{\rm $\mu$m}} \def\arcsec{\hbox{\rm \char '175}} \def\opahei{\hbox{$\chi_{504}$}} \def\pfga{\hbox{\rm Pf${\gamma}$}} \def\bgam{\hbox{\rm Br${\gamma}$}} \def\hap{\hbox{\rm H${\alpha}$}} \def\hab{\hbox{\rm H${\beta}$}} \def\hag{\hbox{\rm H${\gamma}$}} \def\had{\hbox{\rm H${\delta}$}} \def\bap{\hbox{\rm Br${\alpha}$}} \def\pap{\hbox{\rm P${\alpha}$}} \def\heone{\hbox{\rm \HeI\ 584\AA}} \def\hedubt{\hbox{\rm \HeI\ ${2.112\mu}$m}} \def\hedubi{\hbox{\rm \HeI\ ${2.112/3\mu}$m}} \def\hetrit{\hbox{\rm \HeI\ ${1.700\mu}$m}} \def\hetwot{\hbox{\rm \HeI\ ${2.058\mu}$m}} \def\henue{\hbox{\HeI$_{1.909\mu m}$}} \def\henuet{\hbox{\rm \HeI\ ${1.909\mu}$m}} \def\hetwo{\hbox{\HeI$_{2.058\mu m}$}} \def\hetri{\hbox{\HeI$_{1.700\mu m}$}} \def\hedub{\hbox{\HeI$_{2.112\mu m}$}} \def\rheh{\hbox{\rm \HeI$_{2.06}/B{\gamma}$}} \def\el{\hbox{\rm \={e}}} \def\ne{\hbox{\rm n$_{\rm e}$}} \def\np{\hbox{\rm n$_{\rm p}$}} \def\pdos{\hbox{\rm $2^{1}P$}} \def\pdose{\hbox{\rm $2P$}} \def\pdop{\hbox{\rm \scriptsize {\pdos}}} \def\pdope{\hbox{\rm \scriptsize {\pdose}}} \def\sdos{\hbox{\rm $2^{1}S$}} \def\sdost{\hbox{\rm $2^{3}S$}} \def\sdose{\hbox{\rm $2S$}} \def\suno{\hbox{\rm $1^{1}S$}} \def\sunoe{\hbox{\rm $1S$}} \def\ltres{\hbox{\rm \pdos-\sdos}} \def\ltrese{\hbox{\rm \pdose-\sdose}} \def\ltrep{\hbox{\rm \scriptsize {\ltres}}} \def\ltrepe{\hbox{\rm \scriptsize {\ltrese}}} \def\luno{\hbox{\rm \pdos-\suno}} \def\lunoe{\hbox{\rm \pdose-\sunoe}} \def\lunop{\hbox{\rm \scriptsize {\luno}}} \def\lunope{\hbox{\rm \scriptsize {\lunoe}}} \def\ofr{\sc (r)} \def\tc504{\hbox{$\tau_{\rm 504}$}} \def\ngst{\hbox{\rm $n_{1S}$}} \def\taunu{\hbox{$\tau_{\nu}$}} \def\taunur{\hbox{$\tau_{\nu}$(r)}} \def\taues{\hbox{$\tau_{\rm es}$}} \def\tauro{\hbox{$\tau_{\rm R}$}} \def\tauL{\hbox{$\tau_{\rm L}$}} \def\taumax{\hbox{$\tau_{\rm max}$}} \def\tauo{\hbox{$\tau_{0}$}} \def\taucon{\hbox{$\tau_{\rm cont}$}} \def\taurtt{{\footnotesize \hbox{$\tau$=2/3}}} \def\taur23{ \hbox{$\tau$=2/3}} \def\nuo{\hbox{$\nu_{0}$}} \def\Vo{\hbox{$v_{0}$}} \def\Vsound{\hbox{V$_{\rm s}$}} \def\Vrad{\hbox{V$_{\rm rad}$}} \def\Vesc{\hbox{V$_{\rm es}$}} \def\Vcore{\hbox{V$_{\rm core}$}} \def\Heff{\hbox{$h_{\rm eff}$}} \def\Vray{\hbox{V$_{\rm ray}$}} \def\Vnew{\hbox{V$_{\rm new}$}} \def\Vold{\hbox{V$_{\rm old}$}} \def\Rmax{\hbox{R$_{\rm max}$}} \def\Bij{\hbox{\rm B$_{\rm ij}$}} \def\Bji{\hbox{\rm B$_{\rm ji}$}} \def\Aji{\hbox{\rm A$_{\rm ji}$}} \def\Rij{\hbox{\rm R$_{\rm ij}$}} \def\Rji{\hbox{\rm R$_{\rm ji}$}} \def\Rik{\hbox{\rm R$_{\rm ik}$}} \def\Rki{\hbox{\rm R$_{\rm ki}$}} \def\Ripi{\hbox{\rm R$_{{\rm i}^{\prime}{\rm i}}$}} \def\Riip{\hbox{\rm R$_{{\rm ii}^{\prime}}$}} \def\Rippi{\hbox{\rm R$_{{\rm i}^{\prime\prime}{\rm i}}$}} \def\Riipp{\hbox{\rm R$_{{\rm ii}^{\prime\prime}}$}} \def\nip{\hbox{\rm n$_{{\rm i}^{\prime}}$}} \def\nipp{\hbox{\rm n$_{{\rm i}^{\prime\prime}}$}} \def\Cij{\hbox{\rm C$_{\rm ij}$}} \def\Cji{\hbox{\rm C$_{\rm ji}$}} \def\Cik{\hbox{\rm C$_{\rm ik}$}} \def\Cki{\hbox{\rm C$_{\rm ki}$}} \def\Cipi{\hbox{\rm C$_{{\rm i}^{\prime}{\rm i}}$}} \def\Ciip{\hbox{\rm C$_{{\rm ii}^{\prime}}$}} \def\Cippi{\hbox{\rm C$_{{\rm i}^{\prime\prime}{\rm i}}$}} \def\Pij{\hbox{\rm P$_{\rm ij}$}} \def\Pji{\hbox{\rm P$_{\rm ji}$}} \def\Zji{\hbox{\rm Z$_{\rm ji}$}} \def\Yij{\hbox{\rm Y$_{\rm ij}$}} \def\SL{\hbox{S$_{\rm L}$}} \def\Sij{\hbox{\rm S$_{\rm ij}$}} \def\Snu{\hbox{S$_{\nu}$}} \def\Sdma{\hbox{$ \bar{\mbox{\boldmath $S$}}_d$}} \def\Ndma{\hbox{$ \bar{\mbox{\boldmath $N$}}_d$}} \def\Jlma{\hbox{$ \bar{\mbox{\boldmath $J$}}_l$}} \def\Jlksma{\hbox{$ \bar{\mbox{\boldmath $J$}}_{lks}$ }} \def\Jlksmap{\hbox{$ \bar{\mbox{\boldmath $J$}}_{lks}^{'}$ }} \def\Jlksmapp{\hbox{$ \bar{\mbox{\boldmath $J$}}_{lks}^{''}$ }} \def\Jlkjma{\hbox{$ \bar{\mbox{\boldmath $J$}}_{lkj}$ }} \def\Jlkjmap{\hbox{$ \bar{\mbox{\boldmath $J$}}_{lkj}^{'}$ }} \def\Jlkjmapp{\hbox{$ \bar{\mbox{\boldmath $J$}}_{lkj}^{''}$ }} \def\fij{\hbox{\rm f$_{\rm ij}$}} \def\chiL{\hbox{$\chi_{\rm L}$}} \def\chiij{\hbox{$\chi_{\rm ij}$}} \def\chinu{\hbox{$\chi_{\nu}$}} \def\chiros{\hbox{$\chi_{R}$}} \def\chic{\hbox{$\chi_{\rm c}$}} \def\chies{\hbox{$\chi_{\rm es}$}} \def\etaL{\hbox{$\eta_{\rm L}$}} \def\etaij{\hbox{$\eta_{\rm ij}$}} \def\etanu{\hbox{$\eta_{\nu}$}} \def\etac{\hbox{$\eta_{\rm c}$}} \def\etaes{\hbox{$\eta_{\rm es}$}} \def\Jbar{\hbox{$\overline{\rm J}$}} \def\JbarL{\hbox{$\overline{{\rm J}_{\rm l}}$}} \def\Jbarij{\hbox{$\overline{{\rm J}}_{\rm ij}$}} \def\Jres{\hbox{J$_{\rm Res}$}} \def\Jdel{\hbox{J$_{\Delta}$}} \def\Jc{\hbox{J$_{\rm c}$}} \def\Jnu{\hbox{J$_{\nu}$}} \def\Inu{\hbox{I$_{\nu}$}} \def\Imunu{\hbox{I$_{\mu\nu}$}} \def\Inup{\hbox{I$_{\nu}^+$}} \def\Inum{\hbox{I$_{\nu}^-$}} \def\Hnu{\hbox{H$_{\nu}$}} \def\Hc{\hbox{H$_{\rm c}$}} \def\Knu{\hbox{K$_{\nu}$}} \def\fnu{\hbox{f$_{\nu}$}} \def\Bnu{\hbox{B$_{\nu}$}} \def\nuij{\hbox{$\nu_{\rm ij}$}} \def\nud{\hbox{$\nu_{\rm D}$}} \def\dnud{\hbox{$\Delta\nu_{\rm D}$}} \def\alphaij{\hbox{$\alpha_{\rm ij}$}} \def\alphaijnu{\hbox{$\alpha_{\rm ij} (\nu)$}} \def\alphaik{\hbox{$\alpha_{\rm ik}$}} \def\alphaiknu{\hbox{$\alpha_{\rm ik} (\nu)$}} \def\sigmaij{\hbox{$\sigma_{\rm ij}$}} \def\sigmaijv{\hbox{$\sigma_{\rm ij} (v)$}} \def\sigmaik{\hbox{$\sigma_{\rm ik}$}} \def\sigmaikv{\hbox{$\sigma_{\rm ik} (v)$}} \def\qij{\hbox{\rm q$_{\rm ij}$}} \def\qijt{\hbox{\rm q$_{\rm ij} ({\rm T})$}} \def\sige{\hbox{$\sigma_{\rm e}$}} \def\phinu{\hbox{$\phi_{\nu}$}} \def\psinu{\hbox{$\psi_{\nu}$}} \def\qnu{\hbox{q$_{\nu}$}} \def\bi{\hbox{\rm b$_{\rm i}$}} \def\bj{\hbox{\rm b$_{\rm j}$}} \def\gi{\hbox{\rm g$_{\rm i}$}} \def\gijk{\hbox{\rm g$_{\rm ijk}$}} \def\gojk{\hbox{\rm g$_{\rm 0jk}$}} \def\gojpk{\hbox{\rm g$_{\rm 0j+1k}$}} \def\gj{\hbox{\rm g$_{\rm j}$}} \def\chiijk{\hbox{$\chi_{\rm ijk}$}} \def\chiIjk{\hbox{$\chi_{\rm Ijk}$}} \def\Ni{\hbox{\rm N$_{\rm i}$}} \def\Nj{\hbox{\rm N$_{\rm j}$}} \def\Njk{\hbox{\rm N$_{\rm jk}$}} \def\Nk{\hbox{\rm N$_{\rm k}$}} \def\ni{\hbox{\rm n$_{\rm i}$}} \def\nj{\hbox{\rm n$_{\rm j}$}} \def\nk{\hbox{\rm n$_{\rm k}$}} \def\nijk{\hbox{\rm n$_{\rm ijk}$}} \def\nojk{\hbox{\rm n$_{\rm 0jk}$}} \def\nojpk{\hbox{\rm n$_{\rm 0j+1k}$}} \def\nij{\hbox{\rm n$_{\rm ij}$}} \def\nik{\hbox{\rm n$_{\rm ik}$}} \def\njk{\hbox{\rm n$_{\rm jk}$}} \def\NH{\hbox{N$_{\hbox{H}}$}} \def\NHe{\hbox{N$_{\hbox{He}}$}} \def\Fnu{\hbox{F$_{\nu}$}} \def\Fc{\hbox{F$_{\rm c}$}} \def\nheh{\hbox{$n_{\rm He}/n_{\rm H}$}} \def\nnihe{\hbox{$n_{\rm N}/n_{\rm He}$}} \def\nnih{\hbox{$n_{\rm N}/n_{\rm H}$}} \def\nmax{\hbox{$n_{\rm max}$}} \def\nl{\hbox{$n_{\rm l}$}} \def\Mbol{\hbox{$M_{\hbox{\sc bol}}$}} \def\EBV{\hbox{$E(B-V)$}} \def\Mdot{\hbox{$\dot{M}$}} \def\Rsun{\hbox{$R_\odot$}} \def\Mstar{\hbox{$M_*$}} \def\Rstar{\hbox{$R_*$}} \def\Rt{\hbox{$R_{\rm T}$}} \def\Rro23{\hbox{$R_{\tauro=2/3}$}} \def\R23{\hbox{$R_{2/3}$}} \def\Reff{\hbox{$r_{\rm eff}$}} \def\Lsun{\hbox{$L_\odot$}} \def\Lstar{\hbox{$L_*$}} \def\Msun{\hbox{$M_\odot$}} \def\Msunyr{\hbox{$M_\odot\,$yr$^{-1}$}} \def\Teff{\hbox{$T_{\rm eff}$}} \def\Tstar{\hbox{$T_*$}} \def\T23{\hbox{$T_{2/3}$}} \def\Te{\hbox{$T_{\rm e}$}} \def\Logg{\hbox{$\log{g}$}} \def\grad{\hbox{$g_{\rm rad}$}} \def\gcont{\hbox{$g_{\rm cont}$}} \def\gline{\hbox{$g_{\rm line}$}} \def\Loggeff{\hbox{$\log{\g}_{\rm eff}$}} \def\geff{\hbox{$g_{\rm eff}$}} \def\Vtur{\hbox{$V_{\rm tur}$}} \def\Vesc{\hbox{$V_{\rm esc}$}} \def\Vinf{\hbox{$v_\infty$}} \def\kms{\hbox{km$\,$s$^{-1}$}} \def\kpc{\hbox{kpc}} \def\Hz{\hbox{Hz}} \def\mum{\hbox{$\mu$m}} \def\yr{\hbox{yr$^{-1}$}} \def\Gam{\hbox{$\Gamma$}} \def\Game{\hbox{$\Gamma_{\rm e}$}} \def\qdef{\hbox{$\delta_{\rm nlS}$}} \def\qnef{\hbox{$\nu_{\rm nlS}$}} \def\HeI{He\,{\sc i}} \def\HeII{He\,{\sc ii}} \def\HeIII{He\,{\sc iii}} \def\HII{H\,{\sc ii}} \def\HI{H\,{\sc i}} \def\CI{C\,{\sc i}} \def\CII{C\,{\sc ii}} \def\CIII{C\,{\sc iii}} \def\CIV{C\,{\sc iv}} \def\NI{N\,{\sc i}} \def\NII{N\,{\sc ii}} \def\NIII{N\,{\sc iii}} \def\NIV{N\,{\sc iv}} \def\NV{N\,{\sc v}} \def\OI{O\,{\sc i}} \def\OII{O\,{\sc ii}} \def\OIII{O\,{\sc iii}} \def\OIV{O\,{\sc iv}} \def\OV{O\,{\sc v}} \def\OVI{O\,{\sc vi}} \def\MgII{Mg\,{\sc ii}} \def\FeII{Fe\,{\sc ii}} \def\FeIII{Fe\,{\sc iii}} \def\ArIII{Ar\,{\sc iii}} \def\NiII{Ni\,{\sc ii}} \def\SiIV{Si\,{\sc iv}} \def\SiIII{Si\,{\sc iii}} \def\SII{S\,{\sc ii}} \def\CrII{Cr\,{\sc ii}} \def\CaII{Ca\,{\sc ii}} \def\FeXIV{Fe\,{\sc XIV}} \def\ie{\hbox{i.e.,}} \def\eg{\hbox{e.g.,}} \def\etal{\hbox{et~al.}} \def\etc{\hbox{etc.}} \def\cm{\hbox{\rm cm}} \def\Kel{\hbox{\rm K}} \def\keV{\hbox{\rm keV}} \def\eV{\hbox{\rm eV}} \def\dim{\hbox{\rm erg$\,$cm$^{-2}\,$s$^{-1}$}} \def\sec{\hbox{\rm $s^{-1}$}} \def\scm{\hbox{\rm s$^{-1}\,$cm$^3 $}} \def\cmcube{\hbox{\rm cm$^{-3}$}} \def\etadim{\hbox{\rm erg$\,$cm$^{-3}\,$sr$^{-1}\,$Hz$^{-1}\,$s$^{-1}$}} \def\etaldim{\hbox{\rm erg$\,$cm$^{-3}\,$sr$^{-1}\,$s$^{-1}$}} \def\Ang{\hbox{\AA}} \def\arcsec{$^{''}$} \def\Av{\hbox{$A_V$}} %***************** END Paco's definitions \begin{document} \title{Quantitative IR Spectroscopy of Hot Stars Observed by ISO} \author{F.~Najarro and R.-P.~Kudritzki\altaffilmark{1}} \affil{Universit\"ats-Sternwarte, Scheinerstrasse 1, 81679 Munich, Germany} \author{D.\,J.~Hillier} \affil{Department of Physics and Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USA} \author{H.\,J.\,G.\,L.\,M.~Lamers\altaffilmark{2}, R.\,H.\,M.~Voors, and P.\,W.~Morris\altaffilmark{3}} \affil{SRON Laboratory for Space Research, Sorbonnelaan 2, NL-3584 CA, Utrecht, The Netherlands} \author{L.\,B.\,F.\,M.~Waters\altaffilmark{4}} \affil{Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, NL-1098 SJ, Amsterdam, NL} \altaffiltext{1}{Max-Planck-Institut f\"ur Astrophysik, 85740 Garching bei M\"unchen, Germany} \altaffiltext{2}{Astronomical Institute, University of Utrecht, Princetonplein 5, NL-3584 CC, Utrecht, NL} \altaffiltext{3}{ISO SOC, Astrophysics Division of ESA, PO Box 50727, E-28080 Villafranca, Madrid, Spain} \altaffiltext{4}{SRON Laboratory for Space Research, PO Box 800, NL-9700 AV, Groningen, The Netherlands} \begin{abstract} In this paper we present quantitative infrared spectroscopic analyses of hot stars based on ISO data. In a pilot study, we first investigate in detail the ISO--SWS spectrum of P~Cygni and the consistency of the results obtained from IR spectroscopy with those from optical studies. Then we present preliminary results from ISO--SWS observations for three more hot stars. \end{abstract} \section{Introduction} \label{Intro} The dramatic progress of ground based IR astronomy in this decade has lead to a severe revision of the status of quantitative IR spectroscopy of hot stars, which was clearly lagging behind. Triggered by the detection of the \HeI\ cluster at the Galactic centre by Krabbe et~al.\ (1991), recent systematic observational studies in the $J, H,$ and $K$ bands (e.g., Morris et~al.\ 1996, Hanson et~al.\ 1996; Figer et~al.\ 1997; Fullerton \& Najarro 1997) have supplied the input for quantitative spectroscopy of early-type stars. The relatively narrow IR window accessible from Earth has been considerably enlarged since the launch of the Infrared Space Observatory (ISO) which is providing, indeed, new light for our understanding of the stellar winds of early-type stars. The SWS (2.38--45.2\mum) instrument on board ISO not only opens a new spectral window for quantitative spectroscopy, but also imposes severe new constraints, as we must now be able to reproduce stellar spectra over a very wide spectral range. Once we achieve this, we may then confidently perform infrared quantitative spectroscopy to derive properties of objects in highly obscured regions for which only IR spectra are observable. We present here, therefore, first results on quantitative infrared spectroscopy of a sample of hot stars observed with SWS. In a pilot study, we will first investigate in detail the stellar properties of the Luminous Blue Variable P~Cygni from ISO and check its consistency with those obtained by modeling the optical and near-IR H and \HeI\ lines. Once we gain some insight into the processes controlling the formation of the IR line profiles, we may confidently proceed to analyse other objects. Preliminary results are presented here for HDE~316285 (P-Cyg-type star), HD~152408 (O8\,Iafpe), and $\lambda$~Cep (O6\,I(n)fpe). \section{IR Continuum and Lines as Diagnostic Tools} \label{ircoli} >From the observational point of view, the IR represents an alternative spectral window for those objects which suffer from high interstellar extinction (e.g., the Galactic centre). The observational relevance of the latter is shown in Fig.~\ref{fig-redenpp}a, where we see how the peak of the continuum energy distribution of an object with \Teff$\simeq$30kK is shifted to the IR region even for \Av$\geq$5. >From the theoretical point of view, both the IR {\it continuum}\/ and {\it lines}\/ of hot stars are powerful diagnostics for the investigation of the stellar winds surrounding these objects. \begin{itemize} \item{ An {\it IR continuum flux excess}\/ is shown by all early-type stars undergoing moderate mass-loss, which is attributed to the bound-free and free-free emission processes in the stellar wind (e.g., Wright \& Barlow 1975, Panagia \& Felli 1975). This is also shown in Fig.~\ref{fig-redenpp}a, where we clearly see how the IR continuum energy distribution takes off from the blackbody distribution. The behavior of the IR excess yields important information to constrain the structure of the stellar wind.} \item{The {\it IR line profiles}\/ are even better diagnostic tools. As $h\nu/kT>1$ in the IR, non-LTE effects in the line profiles are magnified (Mihalas 1978), and even in the case of very {\it thin}\/ winds, the IR spectral lines become ideal tracers of the presence of the stellar wind. This is illustrated in Fig.~\ref{fig-redenpp}b, where we see how, for a typical $\beta$-Cephei star ($T_{\rm eff}=18$kK, $\log{g}=3.8$, $R_*=8R_\odot$), the \bap\ line is more sensitive to changes in \Mdot\ than \hap. In the case of {\it dense}\/ winds, both the lines and the continuum are formed in the wind and the behavior of continuum opacity with wavelength gives rise to a {\it zoology}\/ of spectral lines. This is shown in Fig.~\ref{fig-mulhydhe}, where we see how the shapes of the hydrogen and helium profiles are affected as a result of the combination of the line and continuum opacities for an extreme B1 supergiant. The different positions of the profile maxima/minima shown in Fig.~\ref{fig-mulhydhe} demonstrate the importance of the IR line profiles in constraining the wind velocity structure.} \end{itemize} \begin{figure} \vspace{-.5cm} \hbox{\hspace{3.3cm}{\bf a}\hspace{6.1cm}{\bf b}} \vspace{-.1cm} \hbox{\hspace{-.35cm} \psfig{figure=figure_1_a.ps,width=6.2cm,angle=90} \hspace{-.55cm} \psfig{figure=figure_1_b1.ps,width=4.0cm,angle=0} \hspace{-.65cm} \psfig{figure=figure_1_b2.ps,width=4.0cm,angle=0}} \vspace{-.4cm} \caption[]{(a) Continuum-flux energy distribution (solid line) of a \Teff=28kK model with a dense stellar wind, compared with the black-body distribution; note the IR~excess. Also shown are the effects of the interstellar reddening for two \Av\ values: \Av=5 (dashed) and \Av=25 ({dashed-dotted}); the latter is characteristic of the Galactic centre. (b)~\bap\ and \hap\ profiles as tracers of a thin stellar wind for a $\beta$-Cephei star. The \bap\ profile is more sensitive (see text).} \label{fig-redenpp} \end{figure} \section{Observations and Model for P~Cygni} \label{sec-obsred} ISO--SWS observations and data reduction for P~Cygni and other LBVs have been described by Lamers, Morris, et~al.\ (1996). P~Cygni's ISO--SWS spectrum (2.38--45.2\mum) is dominated by H and \HeI\ emission lines and some strong forbidden emission lines of [Fe\,{\sc ii}], [Fe\,{\sc iii}], [Ni\,{\sc ii}], [Ne\,{\sc ii}], [Ne\,{\sc iii}], and [Si\,{\sc ii}]. In addition, we have used the averaged high-resolution ($R=12\,000$) optical and near-IR spectra (4060--8900{\AA}) from the long-term spectroscopic monitoring of P~Cygni carried out by Stahl et~al.\ (1993). \begin{figure} \vspace{-.5cm} \hbox{\hspace{-.25cm} \psfig{figure=figure_2_a.ps,width=6.5cm,angle=0} \hspace{-.1cm} \psfig{figure=figure_2_b.ps,width=6.5cm,angle=0}} \vspace{-.4cm} \caption[]{ {\rm Zoology} of H and \HeI\ IR-profiles for an extreme B1-supergiant model. The shapes of the profiles are controlled by the effects of continuum opacity and the ratio of the line to continuum opacity.} \label{fig-mulhydhe} \end{figure} For the spectroscopic analysis we proceed as described by Najarro et al.\ (1994) and use the iterative, non-LTE method presented by Hillier (1987, 1990) %XXXHillier 1990 not in ref list. DONE !! to solve the radiative-transfer equation for the expanding atmospheres of early-type stars in spherical geometry, subject to the constraints of statistical and radiative equilibrium. Steady state is assumed, and the density structure is set by the mass-loss rate and the velocity field via the equation of continuity. The velocity law (Hillier 1989) is characterized by an isothermal effective scale height in the inner atmosphere, \Heff, and becomes a $\beta$ law in the wind (e.g., Lamers, Najarro, et~al.\ 1996). The atmosphere is considered to consist of hydrogen, helium, and nitrogen (N\,{\sc ii}--N\,{\sc iii}). The model atoms consisted of 15 H, 51~\HeI\ ($n\leq11$), 5~\HeII, 43~\NII\, and 11~\NIII\ levels. The model is then prescribed by the stellar radius, \Rstar, the stellar luminosity, \Lstar, the mass-loss rate, \Mdot, the helium and nitrogen abundances, \nheh\ and \nnih, and the velocity field, $v(r)$. We started the analysis with the stellar parameters derived by Najarro (1995), based on a spectroscopic investigation of data from Stahl et~al.\ (1993), from which we obtained a value for the terminal velocity (\Vinf=185~\kms), while the stellar radius was assumed to be \Rstar=76\Rsun\ (Lamers et al. 1983). We then relaxed all other stellar parameters and proceeded to model the IR spectra of P~Cygni in detail. The main observational constraints were set by the H and \HeI\ profiles measured with ISO, but consistency with the optical spectra was also required. Table~1 shows the model parameters which best reproduce the ISO--SWS lines, together with those obtained by Najarro et~al.\ (1997) %XXXNajarro et al. 1996 not in ref list DONE (najarro 1997) from the optical spectroscopic investigation. Notice that the stellar parameters obtained from both analyses agree fairly well. The main difference between the two models is the velocity field in the supersonic part of the wind. To match high Paschen-series lines in the optical we require a steep velocity field close to the photosphere, which switches to a flatter velocity law with $\beta= 4.5$ around \Vo=80 \kms (see Fig.~\ref{fig-velofig}). However, this velocity field results in much larger equivalent widths for the IR lines in the 2--7\my\ region than observed, as shown in Figure~\ref{fig-velofig}. In this spectral range the line-formation regions of the main H and \HeI\ lines are located at $v(r)>0.5 \Vinf$, i.e., well beyond the transition zone between photosphere and wind, whereas the continuum is formed around \Vo. Hence, if the velocity field is varied in the transition zone, the resulting changes in the equivalent widths will be primarily controlled by the variation of the continuum flux. Therefore, to reduce the computed equivalent widths in the 2--7\my\ region, a lower value of \Vo\ (and hence a higher density and continuum flux) is required. {\protect \small \begin{table}[hb] \caption[]{Derived stellar parameters for P~Cygni from optical and infrared observations; $\beta$ is the steepness parameter of the velocity field.} \label{tab-stelpar} \begin{center} \begin{tabular}{lcccccccc} \hline \vspace{-7pt} \\ ~Model & \Rstar & \Lstar & \Teff & \nheh & \nnih & \Mdot & \Vinf & $\beta$ \\ & (\Rsun) & (\Lsun) & $(10^{4}$K) & & $(10^{-4}$&\Msunyr) &(km/s) & \\ \hline \noalign{\smallskip}Optical & 76 & 7.0$\times10^{5}$ & 1.92 & 0.29 & 5.8 & 3.2$\times10^{-5}$ & 185 & 4.5 \\ ISO--SWS & 76 & 5.6$\times10^{5}$ & 1.81 & 0.30 & 6.0 &3.0$\times10^{-5}$ & 185 & 2.5 \\ \tableline \tableline \end{tabular} \end{center} \end{table} \begin{figure} \vspace{-.5cm} \hbox{\hspace{-.65cm} \psfig{figure=figure_3_a.ps,width=6.75cm,angle=90}} \vspace{-6.0cm} \hbox{\hspace{4.75cm} \psfig{figure=figure_3_b.ps,width=15.1cm,angle=0}} \vspace{-15.4cm} \caption[]{Influence of the velocity field on the IR~profiles. Left: velocity field derived from the ISO (solid) and optical (dashed) investigations. Right: the higher transition velocity for the optical models (dashed) produces too-strong emission components in the (2--7\mum) range when compared with the observations (solid), while the lower transition velocity of the ISO (dotted) is able to reproduce the observations quite well.} \label{fig-velofig} \end{figure} \normalsize} This is achieved in our ISO--SWS model where the transition between the steep photospheric velocity field and the wind regime occurs at about 30 \kms\ and the wind velocity law is steeper ($\beta=2.5$) than that derived from the optical spectrum. Due to the difference in the velocity and density structure of both models we derive a slightly lower effective temperature ($\Delta$\Teff=1\,000~K) for the model based on the IR observations. Figure~\ref{fig-pcyisofits} shows the excellent agreement of our calculations with the observations. Our model reproduces not only the profiles of the H and \HeI\ lines over the whole 2.5--28\my\ range, but also the optical lines. The model also accounts for the broad electron-scattering wings of the strongest lines. The only discrepancies between our model and the observations are found for the \HeI\ $3^3$S--$3^3$P line at 4.29\my\, which is overestimated, and the absorption components of the high Paschen-series members, which are slightly underestimated. This is due to the lack of metal-line blanketing in our models (for further discussion see Najarro 1995; Lamers, Najarro, et~al.\ 1996). \begin{figure} \vspace{-1.5cm} \hbox{\hspace{-1.cm} \psfig{figure=figure_4_a.ps,width=13.9cm,angle=0}} \vspace{-11.3cm} \hbox{\hspace{-1.cm} \psfig{figure=figure_4_b.ps,width=13.9cm,angle=0}} \vspace{-10.6cm} \caption[]{Top: profile fits (dashed) to the main IR H and \HeI\ lines of P~Cygni observed with ISO--SWS (solid). Computed profiles have been degraded to the corresponding instrumental resolution. Each profile is labeled with the contributing component(s). Hydrogen-profile fits include the corresponding \HeI\ components (see text). Bottom: fits to the averaged optical H and \HeI\ lines.} \label{fig-pcyisofits} \end{figure} Good agreement is also found between our model and published photometric observations ranging from the UV to radio (Najarro 1995; Lamers, Najarro, et~al.\ 1996). We derive an extinction of $E(B-V)=0.51$ which results in a distance of 1.71 kpc. This is within the uncertainty of the cluster distance of 1.8 kpc (Lamers et al. 1983). {\protect \begin{figure} %\vspace{-.3cm} \vspace{-1.cm} \hbox{\hspace{-.45cm} \psfig{figure=figure_5_a.ps,width=4.7cm,angle=0} \hspace{-.8cm} \psfig{figure=figure_5_b.ps,width=4.7cm,angle=0} \hspace{-.8cm} \psfig{figure=figure_5_c.ps,width=4.7cm,angle=0} } \vspace{-.3cm} \hbox{\hspace{-.45cm} \psfig{figure=figure_5_d.ps,width=4.7cm,angle=0} \hspace{-.8cm} \psfig{figure=figure_5_e.ps,width=4.7cm,angle=0} \hspace{-.8cm} \psfig{figure=figure_5_f.ps,width=4.7cm,angle=0} } \vspace{-.3cm} \hbox{\hspace{-.45cm} \psfig{figure=figure_5_g.ps,width=4.7cm,angle=0} \hspace{-.8cm} \psfig{figure=figure_5_h.ps,width=4.7cm,angle=0} \hspace{-.8cm} \psfig{figure=figure_5_i.ps,width=4.7cm,angle=0} } \vspace{-.4cm} \caption[]{Profile fits to the main H and \HeI\ lines observed with ISO--SWS. {Top,} HDE~316285; {middle,} HD~152408; {bottom,} HD~210839.} \label{fig-otherisofits} \end{figure} \small \begin{table}[hbt] \caption[]{Preliminary stellar parameters derived for HDE~316285, HD~152408 and HD~210839 from ISO--SWS observations. Stellar parameters are consistent with those obtained from optical studies (see text).} \label{tab-othstelpar} \begin{center} \begin{tabular}{lccccccl} \hline \vspace{-7pt} \\ ~Model & \Rstar & \Lstar & \Teff & \nnih & \Mdot & \Vinf & \,$\beta$ \\ & (\Rsun) & (\Lsun) & $(10^{4}$K) & &(\Msunyr) &(km/s) & \\ \hline \vspace{-7pt} \\ HDE~316285 & 75 & 2.8$\times10^{5}$ & 1.53 & $0.67$ & 2.4$\times10^{-4}$ & 410 & 2.5 \\ HD~152408 & 33 & 6.1$\times10^{5}$ & 2.80 & $0.55$ &2.4$\times10^{-5}$ & 955 & 1.25 \\ HD~210839 & 19 & 6.6$\times10^{5}$ & 3.77 & $\phantom{5}0.125$ &5.3$\times10^{-6}$ & $\phantom{0}$2250 & 1.3 \\ \tableline\tableline \end{tabular} \end{center} \end{table} \normalsize } \section{Preliminary Results for Other Early-Type Stars} New ISO--SWS observations have been obtained recently for three other objects, namely HDE~316285 (B1\,Ia$^+$), HD~152408 (O8:\,Iafpe), and HD~210839. For HDE~316285, SWS-01 ($R\simeq800$) observations were obtained for the full SWS range. Since HD~152408 and HD~210839 are relatively weak sources for SWS we observed only the full first SWS band (2.38--4.1\my) with SWS-06 and the strongest lines in band~2 (i.e., Pf$\alpha$). Data reduction was as described by Lamers, Morris, et~al.\ (1996). Table~2 shows stellar parameters derived from a preliminary investigation of these objects. Fits to the observed profiles are shown in Figure~\ref{fig-otherisofits}. {\it Our results based in ISO--SWS observations confirm those obtained from optical studies}\/ (e.g., Crowther \& Bohannan 1997 for HD~152408; Puls et~al.\ 1996 for HD~210839; and own analysis for HDE~316285). The above result is extremely important, not only because we are able to reproduce the stellar spectra from the UV to the IR, but also as it provides us with an important degree of confidence to carry out infrared quantitative spectroscopy when, for instance, due to high extinction only this spectral region is accessible. HD~210839, HD~152408, and HDE~316285 are the first objects in our long list of early-type stars from O6 to A3 that will be observed by ISO, which is, indeed, providing new, crucial insights in quantitative infrared spectroscopy. \acknowledgments F.\,N.\ wishes to thank Allan Willis for maintaining the (s)cat(t)ering among the members of the after-dinner sessions. He also acknowledges a grant from the DARA under WE2-~50~OR~9413~6. \begin{references} \reference Crowther, P.\,A., Bohannan, B., 1997, \aap, 317, 532 \reference Figer, D.\,F., McLean, I.\,S., Najarro, F., 1997, \apj, 486, 420 \reference Fullerton, A.\,W., Najarro, F., 1997, in Boulder-Munich II: Properties of Hot, Luminous Stars (ASP Conf.\ Series, Vol.~XXX), ed. I.\,D.~Howarth (ASP, San Francisco), p.~XXX \reference Hanson, M.\,M., Conti, P.\,S, Rieke, M.\,J, 1996, \apjs, 107, 281 \reference Hillier, D.\,J., 1987, \apjs, 63, 947 \reference Hillier, D.\,J., 1989, \apjs, 347, 392 \reference Hillier D.\,J., 1990, \aap, 231, 116 \reference Krabbe, A., Genzel, R., Drapatz, S., Rotaciuc, V., 1991, \apj, 382, L19 %\reference %Lamers, H.\,J.\,G.\,L.\,M., de Groot, M.\,J.\,H., 1992, \aap, 257, 153 %XXXNot cited in paper . Remove \reference Lamers, H.\,J.\,G.\,L.\,M., de Groot, M.\,J.\,H., Cassatella, A., 1983, \aap, 128, 299 \reference Lamers, H.\,J.\,G.\,L.\,M., Morris, P.\,W., et al., 1996, \aap, 315, L225 \reference Lamers, H.\,J.\,G.\,L.\,M., Najarro, F., et al., 1996, \aap, 315, L229 %\reference %Langer, N., Hamann, W.-R., Lennon, M., Najarro, F., Pauldrach, A.W.A., %Puls, J., 1994,A\&A, 290, 819 \reference Mihalas, D., 1978, Stellar Atmospheres, 2nd Edition (Freeman, San Francisco) % Mihalas \reference Morris, P.\,W., Eenens, P.\,R.\,J, Hanson, M.\,M., Conti, P.\,S., Blum, R.\,D., 1996, \apj, 470, 597 \reference Najarro, F., 1995, PhD Thesis, University of Munich \reference Najarro, F., Hillier, D.\,J., Stahl, O., 1997, \aap, 236, 1117 %XXXNot cited in paper. DONE \reference Najarro, F., Hillier, D.\,J., Kudritzki, R.\,P., Krabbe, A., Genzel, R., Lutz, D., Drapatz, S., Geballe, T.\,R., 1994, \aap, 285, 573 \reference Panagia, N., Felli, M., 1975, \aap, 39, 1 \reference Puls, J., Kudritzki, R.\,P., Herrero, A., et~al., 1996, \aap, 305, 171 \reference Stahl, O., Mandel, H., Wolf, B., G\"ang, Th., Kaufer, A., Kneer, R., Szeifert, Th., Zhao, F., 1993, \aaps, 99, 167 \reference Wright, A.\,E., Barlow, M.\,J., 1975, \mnras, 170, 41 \end{references} \bigskip \centerline{\bf Discussion} \medskip \noindent{\bf Langer:} You seem to get very large values for the acceleration parameter, $\beta$, in the B hypergiants. Is that something you expect from radiation-pressure theory? \noindent{\bf Najarro:} We carried out an investigation for P~Cygni, with Adi Pauldrach's code, and the velocity structure I was getting from the spectroscopic analysis was more or less the same as he was getting from the multi-line models. It's a pretty flat velocity law, and can be approximated with such a $\beta$~value. \noindent{\bf Kudritzki:} When you include the ISO infra-red, it goes the other way round; the exponent becomes smaller than you might expect from wind models \noindent{\bf Najarro:} Yes, in the case of P~Cyg. But when you use Adi's models you get very similar results. \noindent{\bf Kaper:} It looks like not only $\beta$, but also $v_0$ has decreased dramatically, from something like 80~km$\;$s$^{-1}$ if you use only optical data? \noindent{\bf Najarro:} The reason for that large value was the high members of the Paschen series, which were observed to have high-velocity absorption dips. One way to explain that was to have the high transition velocity between wind and photosphere. \noindent{\bf Walborn:} With regard to $\lambda$~Cep, the reason for the classification that you quote, O(n)fpe, was exactly for the reason of the peculiar profiles; $\zeta$~Pup is another example. Those stars (the class Conti called Oef) have reverse $\lambda$4686; also, as a class they have broadened absorption lines -- rapid rotation. Additionally, the profiles tend to vary, so the timing of your observations may be important. \noindent{\bf Najarro:} Yes, that's true. As far as I remember, it's only ever been observed once that the red peak was higher than the blue peak in $\lambda$4686 for $\lambda$~Cep. \noindent{\bf Owocki:} These models are still one-dimensional, right? You haven't been able to investigate rotational effects? \noindent{\bf Najarro:} That's right. \end{document}