1992AJ....104.1721C THE 1721 © ASTRONOMICAL Astron. American originally The function find close images one colors the massive supergiants sustained are on of l(r}a:.rr R136 presence region. predicted determining limit present. Department Kitt Kitt NGC the brightest similar that is Planetary J. companions on is Peak Division Peak of 104 now ofR136, The stellar stars. the ;;.50 of three HUBBLE 3603. of normal over with from identified of National (5), National Astronomical the in Washburn have lower resolved relaxation Physics the component Wolf-Rayet times of A stars color Camera photometry. 130 JOURNAL November stars ground-based Physics r=-1.72±0.06 The Geological the observed narrowband been of evolved end Observatory, Department Observatory, and times that in by SPACE core the and Observatory, within luminosity into Lick Lick Department, of Lowell detected R136a time Astronomy, speckle of speckle components. of ofR136, the of the and luminosity 1992 Observatory, Observatory, stars. structure the two (Wolf-Rayet the DEIDRE the the for The Observatory, TELESCOPE color-magnitude of Planetary area. National He are National observations. ROGER Hubble Society center components. interferometry. Physics, massive the within larger University This per Princeton University II distribution Received of is or An cluster filter the of shown A. University University to unit Optical Sciences, Optical with of LYNDS Space region VOLUME University suggests R136. F336W the HUNTER 1400 Wolf-Rayet star those JAMES and Orion of was 14 EDWARD EDWARD ROBERT University, area 0004-6256/92/111721-22$00.90 of • is cluster Wisconsin, BEL Too ARTHUR to PLANETARY a May In Astronomy Astronomy W. cluster New S.M. ABSTRACT We much Telescope The blue California used The ( Provided of of small have AND is of diagram the - surface Three Mars for of of A. 1992; CAMPBELL that California, California, R. found Mexico, 2 104, cluster present AND stars Maryland, luminosity unless supergiants) all to latter M. pc) FABER WESTPHAL a P.O. smaller at J. J. EARL 30 LAUER Hill type; 475 core revised comparable CODE investigate relaxation NUMBER Observatories/ of Observatories, GROTH least Institute SHAYA of LIGHT Doradus JON within brightness has defined Box corresponds Rd., to 800 N. the case members R136 a Santa Santa color-magnitude of J. with Charter College 24 be by large been than 708, 12 Yale A. CAMERA IMAGES F1agstaff, the O'NEIL, 12 of July per p R136a separate consistent Cruz, Cruz, 0 as HOLTZMAN the Princeton, components Technology, is Blvd., and in two > 5 'c<0.25", the the used effects population 2 Park, area unit 1992 St., R profile 5 X comparable P. P. the that California California 136. Arizona NASA age to Wolf-Rayet identified 0. zero-age 0. Madison, are N. JR. 10 to area Large Maryland and ZAMS components, Box Box lie E., 4 of have New We found obtain vh" is with Pasadena, Albuquerque, 3.5 seven in 26732, 86001 outside 26732, constructed diagrams 0 considerably 95064 are 95064 find of Jersey Magellanic Wisconsin Astrophysics the main-sequence pc- been X from spectral a to 20742 to lower broad previously 10 stellar Tucson, that Tucson, pure times have inner that 08544 3 OF 6 California • that © ground-based yrs very including The and mass the 53706 and R136 New 1992 power luminosities type of that population. 1" for required Arizona Arizona crowded Cloud. implied stars important smaller Orion a Mexico narrowband (0.25 unidentified Am. stars 91125 R136 B3. 1 of luminosity (ZAMS) law the the NOVEMBER in 85726 85726 Data R136a, No Astron. is pc) by but upper 87131 based R inner eight data, than with core also and 136 We red the of in is System Soc. 1992 1721 1992AJ....104.1721C formation can contains gion, ing lines nebula scope spectra. star stars, 30 OB a infrared, R136 suggestion and ceived 1722 R136a tions stars as a/. R136a's Wolf- made. massive type nents self) (LMC) addressed 1985). izing requiring within bers Jl 1985; R136a. tory the tions rounding by cooperative 1991) obtained AURA, Association urhe 1 < Based spectral 1 05. The © Speckle 0 The Doradus Wolf-Rayet ( so be mass) pc stars inferred with 1985) ) for National stars, of of near which could can Rayet American radiation most Neri for (HD (HST) around that on (Rl36al-a8), stars difficulty CAMPBELL The In resolved. resolved region is in Inc., 30 2'-3' This at Wolf-Rayet extreme highly The massive star is numerous composite observations dominated and addition a R136 and the agreement the these that easily identification Doradus of of enough more who most was function a & the interferometric under 38268), of mass extreme make components component (Kennicutt interpretation Universities Optical ionization most spectacular the Space of Grewing optical as Faint WN4.5-5+0B(n) which an Rl36a, difficulty based ionized as show stars for form of R136a of Fully recently the required individual star NASA LMC account concentration > unusually the define to Telescope few and luminous the with having very Nebula spectrum, ET the with Astronomical whose Astronomy 10 Object in I. and R136a by core the formation. in all in are a that end core 3 INTRODUCTION one stellar and contract sufficiently unique the is 1988) as AL: for nitrogen the however, Jl massive into part nebula (Savage of the tight within in which apparent was the early-0 by 1991). example classified to contained concentration and the for National six as Research quarter 0 brightest 03If Science around observations of cluster R was Camera NASA/ESA in objects core HST match the Melnick on luminosity of rich a many 136a (Cassinelli constituents clusters and early once Observatories half the 30 early NAS UV make case minimum as the the originally the of 1", stellar In in The appearing et IMAGES (but spectra Doradus Institute, grouping Science later in Large extreme along itself free of of a NGC in ( WN the 0 a/. the both study 5-26555. addition believed pointlike as very 30 apparent in have images but component 0 < it whole. the the Astronomy, a (1985) central and of 30 3") excluding Hubble a observed 1983). Doradus of likely Society Hubble core evolution. stars supergiant nebular are from (and, extremely spectral of Foundation. the Magellanic 15' et 2070, (Weigelt high total optical with 03 of types Galactic which Wolf-Rayet not are drove of of OF density and a in a/. very at of the (Weigelt the of This to radius UV the appearance stars useful be eight and Space that region deficit operated the least by their R136 massive as mass 1981 Wolf-Rayet which 30 Space features on is be in role large Inc., luminosity R136a ionization, clusters inner present the early-type and R136a classifica inference, operated (Melnick Moffat yet has emission Observa the Doradus and within of & Telescope, the a H massive redden • as compo around labora ) . optical in played Cloud under of super single early ( II Baier near by num eta/. early itself Tele stars been This non been core Provided > per ion star sur has the re 20 the it in of in in by et a a faint ofR136 a heart have stars etry ables lowed attainable images they primary a emission-line filters low of F547M, F469N Wolf-Rayet modulus to age of covery 2.2), taken through for as can core image morphology and deconvolution. F368M tions and was two tiple pixels) pixel color-magnitude stars Therefore: 8/26/90 8/26/90 4/12/91 4/11/91 4/12/91 4/12/91 30 PC6 HST an Five the d&te be 1984). by analyzed is orbits: to removed, of otherwise heretofore stars problematical exposures of is one are we Doradus evaluative F336W, after by possible, scale taken found the stellar of of on with identify on image this compromised PC exposures with the filter and mirror filters to listed use the spherical to and R136 from the cluster 25 F702W F655W F336W F647M F368M F469N four the UV observations stars. extraordinary of filter a identify of NASA in the a later, in TABLE the sharp in photometry He broadband August by and is sine 0.044". is would F555W, to -flooding The been in F368M 2.1 were later LMC the Griffiths although order the were of Wolf-Rayet at 1990 of HST program crowding II summed be Therefore, was a Table were the interpolation, No. diagram Data 300 the higher and aberration ground. due I. F547M 11.4686, core 2. stellar limited aligned narrowband E(B- set stellar obtained images to are have The to placed OBSERVATIONS 1990. Planetary by Astrophysics Although images s telescope, and F702W, it be made I. to examine of of (1989)]. Obtained and of images each the not HST the presented star instituted signal-to-noise is F368M been among 30 content -18.6 observations the data V) by the Furthermore, and which components [Details F547M. (each the stars. in on uncertainties Exposure presented better PC 40300, spherical Doradus and cluster, in were through =0.34 through dynamic the point lack without is Camera luminosity and this photometry F469N also observations. cosmic the the Observations the the and 50100 10150 used in filter one shifted Time image 800 We is and in summed. 140 calibration shortly about 80 26 16 stellar primary 1990 of F469N. Although image obtained, spread (Fitzpatrick very we obtained a (•) high this the X at here. below filters were filter range take aberration Data image on-orbit aberration. distribution. rays that (PC), characteristic to were 800 than to 150 stellar by total are paper brightest the content an HST function. resolution that after taken of The illustrate CCD F368M the function less were Photometry F368M to Flat-fielding mirror. of s. larger the passes made instrument Image is were extent calibrated, which individual were System reddening w0ce0107B w0ce0102B later construct detecting w0ia0102t w0ia010lt w0ia0103t w0ia0104t The photom (see we used distance observa flats than the F336W images & Name flagged as known of of Early stars. made than with tried mul 1722 used Sav data over The part Sec. The and The dis has not the en the the the be 0.2 al for of 1992AJ....104.1721C flooded. clean in tests tinue the bered bered dark dus of individual F368M visible volution with spread ever, sure corrected from from four flats of observations is the the WF F702W to tometry the removing nate broadband based extends CCD list Definition F555W minations, matic rameter would photometry photometry 1723 (Plate 1991 another the view April © In PC In Measurements the tendrils /PC of center quality entire fell CCD's) had in list times flat-fielding current. 100 stars this the response Fig. American addition images in the through routines extreme stars, images V-band 115) in CAMPBELL be cluster function filter of images. and and on to in A produced 1991 the team. by package many extended iterations, the numbering more pixel-to-pixel for speckle a 1 of outside stars PC6 flat Team DAOPHOT fundamental the -60 were filters chips of as shows PC eye of lists same we through the (Plate are F336W is PC6; original in were On-orbit A-D of stars. the obtained region, to correction, tendrils image comers for the In outlined problems, 2.2 broadband chip. We difficult examined filter field in listed to pixels (PSF) fact 80, problems R136 of PC5, wreaking 1992). were Fig. components. of way the the no DAOPHOT photometry finding stars other halos used verify R136a. Data 114) ET Astronomical retained conversion both are Therefore, was scheme. so 16, Because that the the and stellar F555W. of images. in core F368M using in 4 of that made AL: of streak 7, were varies and during that in also limitation for to in Table The this one stars is Obtained 26, of used, narrowband brightnesses radius. frames. their the each and but the of stars with the Fig. are flat-field R136. of The displayed havoc HST Weigelt the filters stars features only chip-to-chip during obtained the shown and can the using region stellar The field the the (Stetson flats they image significantly detector stars near another 8 I. and prelaunch F368M in 3 (see reality excess to The errors, stars; first as IMAGES Rl36 method stars (Plate see cluster cluster, to PSF order 140 A We with results falsely in on collected of did 36, F555W, F336W, it the well. the the the in WF & in halos be which displayed third rest kindly eight the 1991 provided a view the filter on noise the s, also that must the on Society of Baier itself major Fig. a had frame. crowded-field center photometric preflash, CCD's. fitting eliminated mosaic 1987). to /PC 116) respectively. The reasonable of F368M center. variations. of the identify of thermal 11 measurable the the OF accuracy difficulty often produce original appeared stars across are modified of F469N. deconvolution not 2. be the apparent as loaned from Lucy and (1985) Investigation limitation variable on images Rl36 procedure F702W stars of the to The placed not determined a of The The lead stars been a are relatively bias, 30 show Figure image 12 knots the the January vacuum ground PC • already than coordi (1974) a decon in to comes streak of Expo job Dora deter in How April num num a point auto clean were pho only UV Provided near con field PSF PSF four The and and and (all the the the pa the the on of of in in it 2 9 gitimate lists. F336W. DAOPHOT the this the ticular uncertainty parameters both automatic and function, decreasing cally, discussed most matic hand," sured as change outside. filter currently field apply apparent cluded cially corrected ination Thus, January Johnson-Cousins R136 the to were however, the those roughly below. with point, study colors In Investigation tometric (Sec. (see the an The Because The The Note R136 standard very intervening Johnson-Cousins dubious by list. in This time the taken approximate 3.3). noticeable but of system of Johnson to of and as 800 technique of the below) stars any it DAOPHOT stars Omega by photometric in approximates that, the R136 1991 stars To massive core uncertainties, the we described stars zero massive was the F555W known. that we not by below to has after list, the magnitudes stars tenths Omega this the color were of with from measured try toss were star software. 0.01 problems NASA although not created ground-based searching measurement of Definition point at which the was as F555W we optical is the system Cen effective the clean three to in on in R136, the used out a> stars to defined term. detections blue feasible stars In software and mag sorted into desired of observations still magnitudes. the photometry above, V not get Cen CCD's the automatically on the estimate fact, faint 0.6 a a zero magnitude star is months another the UVR to given F702W as ultraviolet, path. 214 through required star. Furthermore, Astrophysics to to is 2 magnitude in a the retained quoted section with Note we as four observations were close quantum Aprill991. Team better eliminate fairly a 0 allow to as to the list ground-based effect that end. points faint stars. broadband are returns made V Even of estimate and our although system, by a filters, This spurious also CCD's. WF/PC magnitude, was those deleted completeness to the box ties cooled frames. star to, on below WF/PC and close, Harris for We that of estimate of in 1992). in knowledge, in B the Outside so, it for that compiled corrects where contamination zero over efficiency. the eliminating the the the the several but computing objects the stars 7.3"X8.7" within even they list goodness have objects R136 however, but for the Since from F336W i.e., The are it and filters are frame. filter flight et luminosity detections. the fitting contamination HST We point For not time definition entirely also filters. the the incompleteness and of are Data a!. more and of we included fairly within on for has transformations measures R136 as photometry observations. the the used the essentially system be R136 corrections this zero magnitudes dozen ( equal F702W are standard eliminates not was This that (see have This avoided procedure 1991 we well. any the of and star luminosities cosmic the photometry dates detected difficult which We luminosity analogs System is close, automati and will fit. the point identical. increases our used ofRI36. function we intrinsic contam WF/PC WF/PC ) effect For number the is stars F555W to, not In are expect, a do These of of the those auto use espe mea pho over very zero 1723 rays par first star "by and can not not the the the the the for for in on le of as of in to to of it 3 1992AJ....104.1721C 1724 through stars edly given Photometry more magnitude tudes respectively. 8 sources and Definition pixel Naturally, to © The the identify individual FIG. in an coordinates American uncertain by as CAMPBELL x,y flat of the 6, 4. underestimate DAOPHOT a uncertainty Team photometry A where level. fielding positions function box for it Figure mosaic PC as than the images defined 1992). However, being on the of ET ( Astronomical and 5 rest -0.08 the of that the given star shows include have AL.: of found four magnitude of shown F702W as of of the number been in HST mag; R136 the the the PC stars the more on the Tables variously CCD in stars true photometric IMAGES uncertainty frame. see PC5, zero is outside the begins crowded for images presented WF/PC uncertainties. is 2-6 figure point Society PC6, rotated That the given with is OF R136 are shown F555W in PC7, ( Rl36 are Investigation in uncertainties is, Rl36 -0.05 in the a in the order at the 5, undoubt Tables for Table or • original a stars magni 6, the origin Other to mag) filter. given PC8, Provided 7 match F555W or 2. is 3 the filter. 0,0 in with box Camera. Table lower Fig. nate region coordinate identified stars. acteristic narrowband the orientation Tables A of stellar Stars in by 3 respect designations 140 corresponds left 7 a 7 each and Fig. the not Figure of s on and on the match 2-6 emission-line closest image system 3 identified chip Wolf-Rayet filter to NASA Figs. has PC's that the sky. 3 is is shows a F469N. of to in to 1 sky. in of position made 6, the is and R136 the the Fig. the Astrophysics 7, the both The the pyramid feature stars. coordinate 0,0 8 1 4 literature. between This are following tables was and orientation angle outside center coordinate identified The filter also He can corner with of star stellar II of of be obtained the These is counterclockwise. 25", here. .1.4686 the the useful number of respect used of Data pyramid of with the Note chip continuum box each stars the to that field for through that PC5 outlined pixel System to and orient chip. Planetary isolating are is the overlap of known to given alter char view 1724 The also also the the the In in 1992AJ....104.1721C 1725 © American CAMPBELL ET ID ID Astronomical 101 100 102 114 113 112 111 110 109 108 107 104 106 105 103 120 119 118 117 116 115 14 16 17 15 13 12 10 11 21 20 19 18 86 35 30 38 34 33 32 31 40 29 28 27 26 25 24 23 22 97 88 87 96 84 95 85 83 82 81 94 93 39 37 36 89 99 90 92 98 91 4 1 8 9 5 7 6 3 2 AL: 346.4 345.7 341.3 338.3 340.4 344.3 342.3 335.9 354.1 361.2 356.5 350.6 338.2 360.1 361.8 360.1 353.5 332.7 365.4 335.5 334.3 322.6 345.2 306.3 347.7 307.2 330.7 311.8 373.2 346.6 359.9 335.5 339.7 362.8 357.3 414.9 349.9 378.5 322.2 368.9 312.0 364.2 366.7 388.0 340.0 323.2 320.1 331.7 321.3 333.5 380.3 275.8 411.8 289.9 356.2 309.8 354.9 368.5 375.3 327.9 319.1 304.5 285.8 263.5 272.5 890.5 317.1 361.1 349.7 337.7 301.5 284.2 374.1 264.4 379.6 363.5 348.5 313.6 288.1 316.5 X X HST 463.4 466.1 467.5 472.6 467.2 464.2 474.3 472.0 472.2 469.1 482.3 477.2 473.3 458.2 461.9 469.1 464.5 442.2 419.3 486.5 484.2 458.6 458.6 517.5 392.0 417.5 436.3 482.2 449.9 473.8 436.3 484.3 464.9 463.0 413.7 506.4 352.5 373.1 413.7 492.4 447.9 459.9 491.4 452.0 440.6 413.0 462.1 488.2 413.9 442.3 497.0 403.0 386.5 546.0 353.4 384.6 491.9 496.7 451.2 491.1 414.3 482.6 451.6 424.9 469.8 403.0 480.1 487.8 458.3 460.0 431.2 376.7 478.6 486.3 408.8 484.7 454.9 499.3 513.3 448.2 y y IMAGES F555W F555W 12.85 13.78 13.73 12.78 13.09 13.56 14.28 14.51 13.58 14.06 12.87 14.68 15.18 15.06 13.92 15.12 14.72 13.83 13.03 12.86 15.20 14.15 15.36 15.05 14.66 15.95 14.58 14.20 14.37 14.26 14.31 14.30 14.28 14.21 14.32 15.93 15.92 15.91 15.99 15.99 15.89 15.85 14.54 15.89 14.52 15.84 15.83 15.81 15.80 14.53 14.47 15.86 15.96 15.88 15.87 15.86 15.82 15.81 14.52 15.89 16.11 15.98 16.05 16.05 16.05 16.04 16.22 16.20 16.19 16.19 16.15 16.13 16.12 16.11 16.09 16.09 16.08 16.08 16.06 16.06 Society 0.10 0.10 0.10 0.11 0.06 0.07 0.07 0.10 0.12 0.04 0.07 0.09 0.06 0.09 0.10 0.09 0.07 0.06 0.04 0.05 0.08 0.05 0.14 0.06 0.06 0.17 O.D7 0.07 0.05 0.05 0.05 0.13 0.05 0.06 0.05 0.06 0.08 0.12 0.12 0.14 0.09 0.06 0.04 0.10 0.11 0.05 0.06 0.06 0.10 0.06 0.17 0.13 0.06 0.05 0.06 0.12 0.05 0.14 0.12 0.04 O.o4 0.08 0.10 0.06 0.17 0.13 0.08 0.19 0.06 0.12 0.10 0.12 0.19 0.18 0.18 0.08 0.09 0.18 0.18 0.21 " cr OF 336-555 336-555 TABLE -1.46 -1.20 -0.85 -0.66 -0.85 -0.78 -0.89 -0.80 -1.05 -0.72 -0.94 -0.79 -1.04 -0.75 -0.76 -0.80 -1.03 -1.01 -0.84 -1.17 -0.72 -1.11 -0.86 -0.71 -0.53 -1.04 -0.84 -0.81 -0.20 -0.87 -0.75 -1.03 -0.78 -1.00 -0.99 -0.76 -0.72 -0.75 -0.89 -0.76 -0.84 -0.87 -0.92 -0.24 -0.73 -1.21 -0.85 -0.95 -0.85 -0.86 -1.09 -0.87 -0.49 -0.73 -0.80 -0.68 -0.86 -0.74 -0.55 -0.70 -1.03 -0.63 -1.09 -1.01 -0.75 -1.24 -0.71 -0.87 -0.68 -0.93 -0.89 -0.35 -0.96 -0.33 -1.01 R136 0.24 2. 555-702 555-702 • Photometry -0.24 -0.19 -0.04 0.58 0.00 0.25 0.23 0.21 0.16 0.35 0.40 0.31 0.16 0.14 0.25 0.33 0.23 0.24 0.08 0.10 0.22 0.09 0.22 0.31 0.28 0.02 0.16 0.36 0.43 0.12 0.06 0.14 0.19 0.18 0.19 0.30 0.27 0.24 0.33 0.36 0.14 0.15 0.03 0.14 0.73 0.31 0.16 0.26 0.30 0.16 0.25 0.16 0.13 0.12 0.11 0.28 0.21 0.32 0.15 0.35 0.02 0.16 0.35 0.31 0.15 0.11 0.06 0.11 0.07 0.24 0.26 0.22 0.33 0.24 0.05 0.14 0.30 0.18 0.00 0.28 Provided (b) Ia I ID ID of 137 136 135 127 130 129 124 126 125 122 128 132 123 121 140 134 139 133 138 145 144 141 131 143 142 154 153 152 151 150 149 148 147 146 159 158 157 156 155 160 41 49 48 47 44 46 45 43 42 50 54 57 56 58 55 53 51 52 59 67 66 65 63 62 61 60 64 68 80 69 74 79 78 75 71 70 77 76 73 72 stars 313.8 366.4 387.3 352.7 349.0 375.0 382.3 362.6 335.3 280.8 293.1 388.4 386.0 301.3 332.6 385.4 376.2 336.8 359.9 390.0 329.2 323.1 323.1 380.8 324.5 396.1 331.8 322.7 415.8 418.3 341.5 329.3 367.9 369.6 376.1 383.6 300.0 315.9 374.1 364.1 370.2 321.1 395.9 333.9 263.5 411.2 304.9 355.1 372.3 359.4 365.3 397.3 363.2 323.3 352.0 387.1 304.4 264.5 297.1 293.7 279.9 330.2 351.9 324.6 385.3 362.9 390.8 413.8 272.5 392.1 323.0 372.2 363.6 363.0 359.7 290.1 324.3 372.2 378.3 384.8 395.6 X by X in 484.0 446.0 448.5 442.9 443.9 437.6 499.1 456.2 388.2 431.9 497.8 445.0 448.8 440.8 527.3 492.1 489.2 434.0 471.1 465.0 430.1 507.1 470.9 455.2 476.7 457.2 395.9 398.7 432.2 456.2 471.6 456.8 479.2 419.2 496.1 487.8 492.8 444.3 403.7 505.6 502.8 373.7 473.4 477.3 460.8 479.2 401.5 422.7 489.4 455.9 485.0 525.9 504.9 511.5 526.8 380.8 502.2 501.8 394.8 385.1 395.1 410.1 499.2 458.1 479.0 491.0 486.6 404.9 366.0 483.0 495.6 Rl36. 397.3 362.6 542.4 483.3 512.1 503.6 393.3 397.3 the y y F555W F555W NASA 14.95 14.92 14.91 14.70 14.90 14.61 14.98 14.79 14.59 15.14 15.00 15.08 15.14 15.19 15.25 14.60 15.Dl 15.29 15.55 15.53 15.47 15.41 15.36 15.53 15.41 15.38 15.49 15.69 15.62 15.55 15.69 15.66 15.64 16.32 15.77 16.32 15.72 15.72 15.66 15.66 16.28 16.35 16.24 15.78 15.76 16.48 16.45 16.45 16.52 16.51 16.45 16.44 16.49 16.37 16.36 16.31 16.31 16.39 16.44 16.29 16.56 16.53 16.55 16.82 16.66 16.63 16.61 17.09 17.08 16.99 16.99 16.91 16.81 16.77 16.75 16.70 16.70 16.67 17.11 16.95 0.07 0.03 0.06 0.08 0.08 0.10 0.08 0.05 0.06 0.04 O.D7 0.11 0.11 0.11 0.09 0.05 0.10 0.09 0.10 0.12 0.16 0.08 0.09 0.09 0.09 0.09 0.10 0.05 0.14 0.06 0.13 0.06 0.10 0.11 0.10 0.11 0.06 0.13 0.08 0.08 0.15 0.11 0.19 0.11 0.05 0.13 0.13 0.07 0.10 0.10 0.15 0.09 0.14 0.21 0.14 0.12 0.23 0.16 0.19 0.10 0.10 0.08 0.07 0.12 0.19 0.12 0.21 0.22 0.29 0.15 0.22 0.18 0.09 0.08 0.11 0.17 0.11 0.08 0.20 0.15 " " Astrophysics 336-555 336-555 -0.80 -1.02 -0.80 -0.95 -0.95 -0.74 -0.90 -1.00 -0.86 -0.74 -1.32 -0.87 -0.87 -0.59 -0.87 -1.00 -0.84 -1.08 -0.93 -1.11 -1.10 -0.92 -1.05 -0.90 -1.20 -0.75 -0.99 -0.67 -0.56 -0.88 -0.82 -0.95 -0.98 -1.07 -0.81 -0.79 -0.86 -1.06 -0.80 -0.81 -1.16 -0.91 -0.63 -1.01 -0.95 -0.54 -0.66 -1.08 -0.75 -0.80 -0.89 -0.79 -0.60 -0.58 -0.94 -0.80 -0.90 -0.86 -0.69 -1.14 -0.82 -0.01 -0.49 -0.86 -1.11 -0.87 -0.78 555-702 555-702 -0.03 -0.05 -0.19 -0.09 -0.07 -0.50 -0.08 -0.02 -0.42 -0.08 0.26 0.23 0.19 0.13 0.22 0.26 0.09 0.18 0.25 0.41 0.10 0.04 0.08 0.19 0.21 0.14 0.18 0.21 0.19 0.16 0.05 0.34 0.18 0.23 0.14 0.16 0.10 0.42 0.26 0.04 0.10 0.12 0.40 0.24 0.04 0.22 0.13 0.05 0.24 0.12 0.46 0.11 0.10 0.24 0.03 0.23 0.16 0.20 0.06 0.33 0.23 0.08 0.13 0.17 0.11 0.33 0.09 0.18 0.21 0.28 0.08 0.22 0.08 0.32 0.19 0.52 0.20 0.44 0.17 0.15 Data System 1725 1992AJ....104.1721C continuum can combination in 1726 resulting tracted passed ary. and fore: doubles R136. Weigelt tight the those dus. lute near ternal gram. reddening 12 (Plate (F336W-F555W), Table © We Before or inner be 214 magnitudes These Fitzpatrick that collection the more stars, American 8, extinction Also confirm CAMPBELL found. by 117). F469N in stars & 8. stars image core R136a the 1.5" we the The Baier 3.2 is was components on 3.1 The of filter can 1, These of in E(B- image PC centered what of The the PC6 shows 3, the Identification subtracted we & is depending of the the center massive ( convert 3. and images. 1985) passband not plot ET Savage Astronomical the Color-Magnitude F336W stars STELLAR have F469N numerous (F555W-F702W) relative cluster ID V) box 171 170 168 178 169 167 181 180 179 177 176 175 174 173 172 166 165 164 163 162 161 187 185 184 183 182 186' those 6 AL.: an starlight is on of =0.34. are include 311.9 266.9 405.4 409.1 347.9 302.7 388.9 310,4 380.9 309.0 304.5 279.9 273.2 292.2 287.7 282.2 288.4 284.5 279.1 407.5 411.1 417.2 410.2 358.5 276.5 280.3 418.6 from and stars. to apparent unusual X (1.9X2.2 a In R136 stars ( HST on from image themselves line and was stars 1984) estimate and to CONTENT 456.0 438.5 468.4 all 518.1 531.2 519.4 508.6 353.6 414.1 493.7 450.4 499.6 479.2 493.5 469.1 475.0 415.6 488.8 464.3 444.7 497.0 533.1 540.2 512.5 460.7 482.0 423.0 their of where y studies speckle R136a that IMAGES at approximated indicating the Components we In is 1, F555W concluded in the F555W single itself magnitudes 17.33 17.18 17.24 17.38 17.38 17.20 17.19 17.16 17.44 17.30 17.38 17.34 17.18 17.11 17.11 17.39 examined 17.63 17.25 17.62 17.16 17.52 17.51 17.50 17.12 17.61 17.46 17.62 the shown 2, magnitudes of count which pc) Fig. 8 you Diagram the F469N and itself Society have star center interferometry. stars clearly is 0.14 0.32 0.16 0.08 0.14 0.32 0.12 0.24 0.20 0.14 0.14 0.17 0.14 0.18 0.13 0.08 0.20 0.15 0.14 0.20 0.22 0.17 0.12 0.16 0.17 0.17 0.17 color--color star, we draw images, external u OF shown 8 in 9 20 R134 He intrinsic breaks concluded that 336-555 use identified (see Fig. we several R136 but of stars image. -0.76 -1.55 -0.24 -0.94 -0.63 -0.52 -0.61 -0.86 -0.96 -0.90 -1.19 -1.09 -0.12 -0.29 -1.64 -0.81 -1.24 II resolved the by in into 30 are to emission in the total the the rather lt an plot and Fig. 7. a • and TABLE bound up within 555-702 Dora Fig. define linear listed UVR abso stars -0.38 -0.26 -0.01 -0.59 Provided sub The into 0.40 0.25 0.18 0.21 0.29 0.21 0.12 0.10 dia 0.06 0.12 0.42 0.11 0.44 0.08 0.03 0.03 0.24 0.40 0.13 0.10 0.13 0.19 0.01 the be 2), in Of by as 6 a 2. (cl (continued) and colors line Johnson that variable stars and adopting massive view have patrick stars. spond from for One E(B- that their measured. the reasonable sequence stars R136 Doradus mostly photometric = ID 206 205 203 202 201 200 204 196 191 189 188 192 199 198 197 193 194 195 214 213 212 211 210 209 208 207 190 1.68, The In low fact because in by for the can the external 32o.9 354.5 355.6 264.8 272.1 268.9 291.2 422.5 410.0 277.4 425.5 408.8 416.2 420.9 423.9 412.1 402.2 405.1 421.4 417.1 406.6 312.3 344.8 375.3 280.8 270.7 287.8 down of simply about Figs. individual and X The approximately V) (Johnson principle and vertical A sequence mass stars the an across stars the see system. that HST region 555 is Fitzpatrick 542.2 541.2 495.8 460.0 400:8 403.6 412.4 448.9 524.7 521.7 539.0 538.5 532.3 538.8 535.3 512.6 510.3 508.0 536.7 534.3 536.4 521.6 384.0 510.9 353.9 390.1 468.5 is R136a y correction In to 9 extinction Savage E(B- = about PC, taken that the 7 - uncertainties adopted NASA in and to stars. in that we 1.04, the F555W colors the 17.98 17.94 18.04 18.17 18.04 18,01 17.90 17.94 17.90 17.68 19.21 19.10 18.86 18.25 18.32 18.87 18.80 18.44 17.80 17.77 18.66 17.75 18.72 18.40 18.31 18.30 17.89 R136 at it. photometric in could the Also the particularly down luminosities. 1968) are are on 10 V) from of 0.5 However, color--color about and the 30 and Therefore, 0.16 0.20 0.14 0.15 0.20 0.16 0.19 0.12 0.18 0.08 0.40 0.39 0.19 0.45 0.24 0.17 0.16 0.22 0.20 0.21 0.23 0.11 0.21 0.19 0.16 0.18 0.09 WF stars B3 not we and u to in the to the of looking Doradus have shown in mag Astrophysics F555W even have to although Edvardsson A R136a ZAMS. /PC Wolf-Rayet 336-555 the show 0.34. even the .. 702 (M and in reddening -0.74 -1.37 -1.08 -1.04 -0.90 -1.34 -1.20 -0.36 -0.74 -1.25 Savage's (M about o.75 wide, not applied vary =0.68. R136 extinction because uncertainties 336 between on filter 336 WF/PC possibly the at color-magnitude Extinction Furthermore, filter. for diagram are -M region 555-702 -M This been the -0.15 -0.08 -0.09 -0.42 - across massive due one 0.18 0.18 0.23 0.29 0.83 0.37 0.10 0.30 0.16 0.59 0.11 O.Ql 0.56 0.38 0.59 0.58 0.23 0.40 0.27 0.21 0.13 0.41 0.10 brightest cover all 555 not system 1. 555 reddening it & or plot the determined confirms ) to stars transformed in must These the 0 ) (cf. due Bell's unusual for filters 0 = 0 one Data the intrinsic the all part is vs -1.5, is are blue supergiant core are Melnick the also stars of we the bear range small known M can ( limits the so for to the 1989) suggestions bulk not will adopt in 555 to stars. R136 System reddening diagrams. reflecting large, in the colors by in see terms stars stars variable a of field known plot to give the of corre 1986) to mind given work M large Fitz 1726 A type that The and the the we we 336 555 be 30 of of of in is a 1992AJ....104.1721C 1727 outside likely stars spread of mass reddening where begins red. Also, 1987). 1992) slightly © This as at loss American to and CAMPBELL the to could At R136 they M be shows curve about could and 555 redder across photometric intrinsic evolve be ~ show convective -6.5 up to due be M stars, the 5001 5002 5009 5010 5006 5004 5003 5005 5007 5008 5015 5016 5017 5012 5011 5013 5014 5025 5018 5019 5021 5020 5023 5026 5027 5028 5029 5022 5024 5082 5083 5081 5084 5031 5085 5032 5030 5033 5034 5035 5037 5086 5088 5087 5089 5090 5091 5036 5092 5038 5039 5040 1D 555 the ET a ID clearly the Astronomical (Stothers to signature since one = cluster. AL.: 494.5 152.1 659.5 724.5 226.6 433.9 293.4 287.7 494.2 149.7 127.7 325.6 462.7 right 582.1 395.1 732.6 320.8 304.8 374.9 208.0 405.5 258.1 133.7 same 639.6 345.7 409.4 404.8 148.0 721.3 290.9 225.0 187.9 175.8 114.8 567.6 328.0 621.1 229.2 232.9 204.3 258.2 141.7 107.0 144.5 126.8 the 84.2 78.1 93.0 presumably uncertainties -2 82.2 51.6 73.7 65.8 X X begins as overshoot the HST natural 423.6 one 585.7 539.6 543.7 360.7 279.5 439.1 459.0 407.1 555.6 775.0 256.0 255.3 129.8 691.8 791.0 608.9 430.7 472.7 195.6 552.2 586.3 613.1 741.3 735.8 125.4 111.5 100.8 519.1 574.6 536.2 392.8 369.5 730.9 260.6 221.6 545.3 672.2 513.8 365.1 501.8 353.8 582.8 773.5 305.7 604.8 295.0 248.0 181.9 164.6 199.8 spread for 63.0 the y y & of relatively However, IMAGES may Chin to cooler, stars main-sequence F~S~W F555W 12.47 14.07 16.19 16.49 16.37 15.30 14.09 14.24 16.50 16.18 15.49 16.06 16.54 16.52 16.78 16.85 16.67 16.98 16.99 16.98 17.04 17.04 16.92 16.87 16.90 17.10 17.00 19.13 19.11 19.16 19.20 17.22 17.10 17.14 17.35 17.16 17.38 19.48 19.20 19.22 19.24 19.27 19.29 17.42 19.33 17.49 19.40 17.57 17.54 17.75 17.74 17.79 spread see as as possibly (Maeder are 1977; undergoing TABLE Society those a the 0.08 0.08 O.Q7 0.08 0.11 0.04 0.08 0.00 0.09 0.06 0.04 0.05 0.04 O.Q7 0.07 0.02 0.06 0.15 0.07 0.07 0.07 0.08 0.07 0.08 0.06 0.17 0.16 0.16 O.Q7 0.21 0.06 0.08 0.06 0.36 0.07 0.10 0.05 0.21 0.19 0.18 0.23 0.22 0.17 0.09 0.19 0.08 0.16 0.20 0.09 0.08 0.09 0.09 lower slight " uncrowded " OF larger. some among main Schaller m 336-555 3. within R136 see -1.01 -0.68 -0.73 -1.04 -0.98 -0.91 -0.84 -1.10 -1.03 -1.16 -1.11 -1.01 -0.87 -0.95 -1.02 -1.45 -0.92 -1.05 -0.78 -0.94 -0.98 -1.14 -0.73 -0.70 -0.79 -2.13 -1.33 -0.87 -1.00 -1.28 -0.85 -1.13 -0.04 -1.51 -0.82 -0.68 -0.95 -0.72 -0.42 0.47 0.44 mass Photometry tum & ~~~ turnoff spread sequence Intrinsic a extreme massive Meynet • clump ~~~ R136, to 555-702 stars. et stars Provided -0.33 -0.29 -0.04 -0.39 0.30 0.21 0.56 0.06 0.32 0.26 0.19 0.11 0.19 0.20 0.20 0.25 0.07 0.14 0.09 0.60 0.07 0.13 0.24 0.22 0.25 0.33 0.15 0.14 0.34 0.34 0.20 0.06 0.13 0.18 0.34 0.46 0.16 0.16 0.19 0.58 0.41 0.14 0.26 0.40 0.00 0.30 0.29 0.11 1.38 0.37 0.25 the 0.32 al. 702 in is of stars Ia) lb region and diagrams one F555W that tum vs the red by R136 outside 5042 5041 5044 5043 5046 5045 5047 5048 5050 5049 5051 5053 5052 5054 5055 5057 5056 5060 5059 5058 5063 5062 5064 5065 5093 5066 5103 5102 5101 5094 5095 5068 5067 5098 5096 5097 5099 5071 5070 5069 5073 5072 5074 5078 5077 5076 5075 5079 5061 5104 5100 5080 lD ID M One Melnick ward can color-magnitude by all to 102 at itself. 299.7 429.6 550.6 651.1 487.3 122.7 139.8 125.8 150.5 192.2 668.1 306.5 248.5 268.9 154.7 130.2 569.1 309.0 548.1 202.1 451.0 465.2 455.2 467.9 754.8 311.3 241.9 496.0 127.0 128.0 524.7 343.5 323.4 320.3 670.2 363.0 618.3 236.0 389.8 385.7 235.0 284.6 459.0 243.3 227.1 286.5 471.6 160.2 157.7 measured 75.4 60.4 75.2 X other 0 R136 X compared the the also plot, the at of and the 608.1 460.5 705.0 606.0 656.1 723.6 793.1 200.6 289.0 214.0 564.7 702.3 386.2 717.9 220.8 419.1 672.8 282.6 711.1 419.4 758.3 355.0 108.2 595.1 566.6 512.0 563.2 597.6 604.0 608.5 679.2 741.3 316.0 710.9 776.2 296.8 276.3 455.9 213.4 281.3 170.6 782.7 523.8 630.2 641.2 722.2 333.0 208.3 bright ( higher 49.8 80.0 84.5 65.4 see y (PCS). y Rl36 1985). the NASA point B faint the ~·~~~w F555W by stars 17.93 17.86 18.11 18.14 18.14 17.96 18.01 18.00 18.09 18.19 18.26 18.20 18.32 18.35 18.44 18.36 18.53 sequence 18.74 18.63 18.57 18.56 18.66 18.63 18.70 18.72 20.22 20.15 20.58 20.06 19.57 19.57 18.74 18.74 19.86 19.70 19.60 19.59 19.79 18.77 18.78 18.81 18.83 13.77 18.86 18.86 19.01 18.88 18.91 18.91 18.96 18.89 19.02 to end. and of photometric star end Melnick No F336W. diagrams interest have Astrophysics 0.10 0.11 0.08 0.08 0.07 0.33 0.08 0.11 0.09 0.09 0.09 0.07 0.12 0.11 0.12 0.11 0.12 0.10 0.10 0.13 0.09 0.12 0.12 0.12 0.14 0.52 0.34 0.48 0.22 0.08 0.31 0.22 0.15 0.13 0.34 0.32 0.21 0.36 0.26 0.12 0.15 0.14 0.10 0.10 0.12 0.12 0.13 0.19 0.13 0.15 0.16 0.12 The Mk9, red although of " " is the 338 basically 336-555 supergiants narrowness (1986). narrower In -0.66 -0.72 -0.70 -1.90 -0.40 -0.72 -0.76 -0.76 -1.03 -0.92 -0.47 -0.55 -0.40 -1.09 -0.57 -1.48 -0.96 -0.23 -0.40 -1.05 -0.74 -1.35 -0.58 -0.71 -0.79 -0.91 -0.87 -0.62 -1.26 -0.77 classified is ~55 stars of the that accuracy it the 555 555-702 does upper the -0.11 -0.05 -0.10 On measured the 0.05 0.34 0.26 0.30 0.52 0.82 0.19 0.29 0.23 0.41 0.64 0.22 0.17 0.15 0.22 0.27 0.20 0.42 0.21 0.10 0.28 0.19 0.00 0.39 0.06 0.05 0.51 0.80 0.51 0.24 0.36 0.17 0.59 0.82 0.52 0.20 0.41 0.11 0.16 0.37 0.23 0.16 1.27 0.19 0.25 0.08 0.22 0.44 0.08 and larger 702 as were show is same Data the color-magnitude an right in due does M (M found F702W 30 the V- of to supergiant outside System 555 not Doradus redward this the R -M within curve color 1727 plot 702 and fact of ) 1992AJ....104.1721C 1728 ©American CAMPBELL ET Astronomical Society "6016 6006 6011 6005 6001 6012 6010 6009 6007 6002 6019 6018 6008 6004 6003 6022 6020 6017 6013 6021 6014 6015 6025. 6024 6023 6026 6035 6027 6039 6033 6028 6037 6036 6034 6030 6029 6040 6038 6031 6032 ID 6082 6081 6084 6083 6086 6088 6087 6090 6091 6092 6095 6096 6100 6099 6098 6097 6085 6101 6089 6094 6093 6108 6113 6107 6106 6105 6104 6110 6109 6102 6103 6118 6117 6116 6115 6114 6112 6111 6120 6119 ID AL.: 542.3 317.2 482.3 128.4 595.4 595.5 568.5 568.1 582.4 608.3 346.3 314.5 388.6 264.0 459.5 199.8 110.4 386.6 294.4 242.0 273.3 286.5 254.4 405.4 192.9 596.2 576.0 599.8 625.9 332.9 710.3 739.8 304.5 285.8 200.9 471.6 499.7 392.8 231.7 434.5 192.2 596.9 561.7 554.9 668.3 304.2 613.2 611.4 250.0 728.5 491.9 485.7 490.7 436.4 483.3 487.8 143.1 526.9 515.4 527.1 438.2 240.0 174.8 195.4 528.2 553.8 366.1 339.5 328.0 322.6 699.0 373.8 242.7 286.3 162.6 194.2 87.5 206.4 76.7 75.5 X HST 395.3 332.0 269.1 243.0 417.4 495.2 568.3 582.8 352.2 696.2 315.7 621.4 327.7 724.7 348.9 736.0 304.2 232.1 434.0 465.4 623.0 686.9 634.5 698.0 603.4 767.1 768.8 609.3 401.3 386.4 566.0 612.3 365.6 775.3 711.7 375.1 702.1 707.2 478.6 446.7 509.8 573.7 371.5 333.6 393.2 386.1 676.1 617.7 464.3 205.6 428.7 399.4 391.8 346.3 641.0 566.0 514.5 633.8 706.1 584.5 553.5 307.7 612.0 488.2 444.8 475.5 155.8 591.2 572.8 662.6 617.6 707.5 400.1 576.6 578.6 579.7 508.5 751.4 66.5 y 78.5 y IMAGES F555W F555W 13.36 13.30 12.57 13.81 14.47 12.94 12.67 13.46 12.95 14.57 14.69 14.40 14.39 14.08 14.01 13.67 13.52 14.66 14.20 14.21 14.21 14.99 14.75 14.99 14.66 15.14 15.02 15.25 15.44 15.39 15.20 15.49 15.45 15.45 15.37 15.50 15.31 15.35 15.34 15.49 16.38 16.41 16.42 16.57 16.45 16.45 16.64 16.48 16.46 16.65 16.48 16.52 16.53 16.75 16.69 16.69 16.68 16.54 16.61 16.64 16.77 16.75 16.67 16.66 16.49 16.53 16.53 16.50 16.51 16.87 16.88 16.85 16.84 16.84 16.84 16.80 16.84 16.80 16.88 16.89 TABLE 0.03 0.03 0.07 0.04 0.03 0.01 0.05 0.05 0.04 0.05 0.06 0.05 0.04 O.Q7 0.07 0.04 0.05 0.05 0.05 0.04 0.06 0.05 0.05 0.05 O.D7 0.05 0.04 0.05 0.06 0.05 0.04 0.04 0.06 0.07 0.03 0.04 0.05 0.07 0.05 O.D7 0.04 0.05 0.05 0.10 0.07 0.06 0.05 0.04 0.06 0.06 0.06 0.06 O.D7 0.08 0.05 0.04 0.06 0.05 0.07 0.12 0.07 0.07 0.05 0.06 0.05 O.Q7 0.03 0.06 0.07 0.07 0.05 0.06 O.D7 0.1-0 0.07 0.06 0.09 0.08 O.Q7 0.07 OF " " 4. 336-555 336-555 R136 -0.88 -0.80 -1.03 -0.70 -1.18 -0.85 -0.73 -1.01 -1.08 -0.98 -0.83 -0.97 -0.88 -0.87 -1.14 -1.02 -0.32 -0.87 -1.05 -0.88 -1.08 -0.91 -0.89 -0.71 -1.08 -1.03 -1.08 -1.00 -0.68 -1.07 -0.89 -1.22 -0.98 -1.00 -0.86 -0.86 -0.93 -0.89 -0.36 Photometry -1.09 -0.73 -0.67 -0.77 -0.22 -0.91 -0.95 -0.93 -0.98 -0.76 -0.65 -1.16 -0.68 -1.16 -0.90 -0.74 -0.42 -0.69 -0.60 -1.08 -0.45 -0.94 -0.87 -0.80 -0.84 -0.69 -0.92 -1.18 -0.20 -1.03 -1.02 -0.89 -0.84 -0.73 -0.56 -1.08 -1.04 -0.85 -0.52 • 555-702 555-702 -0.30 -0.37 Provided 0.32 0.10 0.19 0.17 0.12 0.00 0.09 0.20 0.20 0.28 0.16 0.25 0.32 0.18 0.15 0.32 0.14 0.15 0.20 0.26 0.19 0.17 0.14 0.23 0.14 0.08 0.06 0.13 0.17 0.33 0.14 0.14 0.12 0.15 0.23 0.17 0.12 0.33 0.38 0.19 0.20 0.16 0.15 0.16 0.31 0.11 0.12 0.04 0.12 0.14 0.29 0.18 0.22 0.21 0.27 0.13 0.11 0.27 0.15 0.42 0.18 0.17 0.21 0.13 0.27 0.13 0.16 0.16 0.12 0.23 0.43 0.24 0.34 0.19 0.14 0.08 0.13 0.17 of (a) stars 6046 6045 6050 6044 6049 6048 6043 6054 6047 6042 6041 6059 6058 6057 6056 6055 6051 6060 6053 6052 6061 6065 6064 6063 6062 6066 6074 6073 6068 6078 6075 6070 6069 6067 6071 6072 6077 6079 6076 6080 outside 6152 6149 6148 6147 6146 614G 6144 6143 6142 6141 6140 6139 6138 6137 6132 6131 6130 6128 6127 6126 6125 6124 6123 6122 6121 ID 6154 6153 6151 6150 6155 6136 6135 6134 6133 6157 6156 6129 6158 6160 6159 ID by 556.6 334.2 376.5 314.7 250.7 479.0 543.9 650.8 597.1 606.8 692.7 387.0 425.8 483.3 461.9 400.0 455.8 410.4 153.4 179.8 127.0 138.8 188.1 130.0 118.1 523.1 523.7 663.7 254.5 436.5 478.1 435.4 575.8 564.7 332.8 670.2 280.6 245.0 704.2 222.6 422.1 453.0 483.8 576.2 587.8 539.2 541.7 363.2 318.2 365.8 644.9 433.5 489.0 439.4 456.5 456.8 451.4 418.6 428.3 179.2 607.8 357.4 613.7 693.0 603.5 784.0 724.1 290.6 221.2 493.7 272.5 244.9 437.5 182.5 307.0 304.6 247.0 187.4 63.5 47.2. X R136 the 651.4 459.4 460.7 378.7 395.6 558.8 558.7 508.7 699.8 523.0 581.4 687.2 384.4 381.6 776,8 310.5 723.6 227.3 282.5 447.3 443.0 501.1 601.5 695.5 622.0 641.0 713.8 264.6 551.8 671.4 597.2 337.7 721.5 730.3 400.8 138.4 196.1 546.7 579.3 592.5 671.9 604.6 308.4 306.1 572.1 357.7 330.0 300.8 625.4 469.5 294.4 294.5 424.9 143.8 540.2 316.6 556.2 754.8 364.6 320.2 611.7 645.9 335.6 763.4 214.8 244.9 436.6 177.8 164.2 529.8 500.3 557.5 641.3 344.6 196.8 599.4 53.1 54.5 y 95.8 90.7 y ( PC6). NASA F555W F555W 15.69 15.68 15.62 15.81 15.79 15.98 15.93 15.93 15.93 15.97 15.70 15.70 15.57 15.90 15.82 15.82 15.62 15.60 15.99 16.00 16.20 16.11 16.05 16.03 16.03 16.15 16.12 16.29 16.31 16.35 16.32 16.21 16.20 16.24 16.38 16.37 16.36 16.33 16.32 16.29 16.90 16.89 17.06 17.06 17.05 17.05 17-04 17.01 16.91 16.90 16.92 16.92 16.92 16.96 16.97 16.95 17.10 17.09 16.99 16.99 16.98 16.98 16.97 17.07 17.06 16.97 16.94 16.94 17.D7 17.09 17.13 17.13 17.12 16.97 17.14 17.16 17.19 17.16 17.19 17.21 0.06 0.06 0.06 0.06 0.06 0.06 0.04 0.06 0.05 0.10 0.05 0.04 0.05 0.06 0.05 0.06 0.08 0.04 0.06 0.05 0.06 0.06 O.D7 0.07 0.06 0.07 0.04 0.08 0.06 0.05 0.03 0.07 0.05 0.04 0.05 0.06 0.07 0.05 0.05 0.08 O.Q7 0.06 0.06 0.06 0.03 0.11 O.Q7 0.11 0.09 0.06 0.06 0.04 0.05 0.05 0.06 0.10 0.07 0.06 0.05 0.12 0.06 0.04 0.13 0.07 0.05 0.12 0.10 0.09 0.07 0.08 0.06 0.08 0.06 0.10 0.05 0.06 0.12 0.07 0.08 0.06 " " Astrophysics 336-555 336-555 -0.99 -0.97 -1.16 -0.90 -0.81 -0.96 -1.34 -0.99 -0.74 -1.07 -0.98 -0.96 -0.65 -0.77 -1.04 -0.43 -0.75 -0.96 -1.05 -1.18 -0.72 -0.86 -0.96 -0.62 -0.87 -1.15 -1.09 -0.63 -0.95 -0.53 -0.92 -0.97 -0.87 -0.04 -0.74 -1.21 -1.11 -1.01 -0.56 -0.88 -0.78 -0.60 -0.89 -0.74 -0.69 -0.72 -0.63 -0.47 -0.70 -0.89 -1.02 -0.73 -0.90 -0.70 -0.70 -0.89 -0.92 -1.00 -0.19 -0.68 -0.93 -0.51 -0.91 -0.76 -0.66 -1.06 -0.50 -0.97 -0.86 -0.46 -0.73 -0.88 -0.80 -0.90 -0.47 -0.60 -0.27 555-702 555-702 -0.03 0.30 0.03 0.17 0.47 0.20 0.18 0.21 0.14 0.45 0.23 0.14 0.09 0.24 0.17 O.Q7 0.83 0.24 0.18 0.28 0.06 0.29 0.18 0.27 0.22 0.19 0.19 0.15 0.28 0.09 0.16 0.34 0.15 0.30 0.22 0.24 0.09 0.06 0.19 0.23 0.21 0.17 0.12 0.27 0.27 0.17 0.18 0.18 0.09 0.11 0.15 0.21 0.09 0.21 0.11 0.12 0.16 0.16 0.04 0.12 0.23 0.18 0.03 0.14 0.12 0.27 0.19 0.23 0.21 0.32 1.11 0.18 0.22 0.12 0.21 0.18 0.57 0.17 0.07 0.41 Data System 1728 1992AJ....104.1721C 1729 © American CAMPBELL ET Astronomical 6161 6163 6162 6165 6164 6167 6168 6166 6169 6170 6171 6174 6172 6173 6176 6175 6177 6181 6180 6179 6178 6182 6183 6187 6186 6185 6184 6188 6192 6191 6190 6189 6193 6194 6195 6196 6197 6198 6199 6200 6252 6253 6251 6242 6241 6243 6257 6256 6255 6254 6250 6247 6244 6262 6261 6260 6258 6248 6246 6245 6259 6249 ID 6276 6272 6271 6269 6268 6270 6267 6266 6265 6264 6263 6273 6274 6275 6280 6277 6279 6278 ID AL.: 660.0 486.6 415.7 529.8 364.8 651.1 442.9 256.1 145.7 198.6 527.9 520.2 562.3 522.9 24Q.4 322.6 427.5 178.1 663.2 430.2 473.6 487.7 104.2 317.0 588.3 349.3 681.5 686.7 434.8 414.2 302.4 211.4 514.3 586.8 238.1 253.0 443.2 157.6 35Q.4 650.0 221.9 430.4 434.3 258.1 430.4 649.0 363.9 329.8 310.7 721.3 284.5 296.0 284.8 461.9 450.9 442.5 490.3 496.5 429.2 225.9 430.9 163.6 18D.6 153.4 593.0 564.8 544.1 555.0 654.4 317.5 225.9 209.1 453.3 287.0 131.5 141.9 97.1 31.1 X 84.9 35.9 X HST 552.8 302.1 309.1 691.5 431.4 381.4 756.3 433.2 207.4 414.0 317.6 345.1 259.5 721.2 243.6 453.7 405.2 557.0 765.5 777.8 606.7 288.3 277.6 298.5 444.5 444.1 566.5 613.5 279.5 618.9 425.9 417.4 510.4 592.2 687.9 625.6 311.7 448.8 495.9 492.0 456.1 588.5 570.2 547.4 339.5 694.8 339.4 514.0 566.3 647.9 626.2 781.3 330.9 752.6 204.9 285.3 283.0 289.1 126.2 192.3 391.5 632.9 631.9 310.9 307.0 614.8 363.5 314.3 664.9 242.2 221.2 417.1 676.9 726.2 339.2 704.2 79.7 48.3 63.3 y 97.5 y IMAGES F555W F555W 17.22 17.22 17.24 17.23 17.26 17.25 17.24 17.26 17.28 17.29 17.30 17.34 17.34 17.35 17.33 17.31 17.36 17.36 17.36 17.35 17.38 17.38 17.40 17.42 17.42 17.41 17.44 17.47 17.46 17.47 17.44 17.46 17.48 17.49 17.50 17.52 17.52 17.52 17.53 17.54 17.90 17.82 17.89 17.88 17.83 17.88 17.86 17.83 17.90 17.82 17.91 17.91 17.90 17.83 17.95 17.95 17.90 17.96 17.95 17.92 17.94 17.94 17.93 17.88 18.05 17.97 17.99 17.99 17.97 17.96 17.96 17.97 18.01 17.99 18.02 18.01 18.Q4 18.00 18.00 18.01 Society 0.06 0.17 0.07 0.08 0.21 0.04 0.10 0.08 0.09 0.05 0.09 0.06 0.09 0.09 0.06 0.05 0.09 0.08 0.11 0.14 0.18 0.07 0.08 0.12 0.09 0.06 0.10 O.Q7 0.10 0.07 0.06 0.06 0.09 0.07 0.09 0.06 0.06 0.05 0.13 0.07 0.09 0.19 0.14 0.08 0.08 0.05 0.08 0.08 0.08' 0.10 0.16 0.07 0.10 0.14 0.10 0.10 0.10 0.10 0.25 0.09 0.09 0.08 0.09 0.08 0.07 0.09 0.08 0.08 0.08 0.15 0.14 0.07 0.15 0.07 0.07 0.09 0.13 O.o7 0.07 0.17 OF u u 336-555 336-555 R136 -0.62 -0.79 -0.92 -0.40 -0.71 -0.67 -0.55 -1.18 -0.69 -0.81 -0.73 -0.60 -0.61 -0.85 -0.09 -0.66 -0.82 -1.26 -0.83 -0.18 -0.99 -0.41 -0.72 -0.95 -0.62 -0.67 -0.44 -0.59 -0.62 -1.03 -0.80 -0.99 -0.61 -0.95 -1.01 -0.56 -1.07 -0.91 -0.28 -0.15 -0.77 -1.05 -0.82 -0.64 -0.79 -0.55 -0.95 -0.83 -0.53 -0.10 -0.39 -1.00 -0.91 -0.89 -0.29 -0.29 -0.45 • TABLE 555-702 555-702 Provided -0.05 -0.62 -0.05 -0.05 -0.35 -0.01 0.23 0.22 0.17 0.22 0.20 0.23 0.14 0.10 0.32 0.09 0.24 0.22 0.12 0.12 0.26 0.37 0.17 0.22 0.26 0.38 0.27 0.32 0.24 0.18 0.20 0.16 0.25 0.32 0.40 0.31 0.17 0.28 0.16 0.14 0.23 0.26 0.20 0.19 0.23 0.33 0.15 0.12 0.26 0.17 0.43 0.27 0.38 0.32 0.21 0.17 0.30 0.20 0.46 0.23 0.24 0.16 0.64 0.00 0.30 0.10 0.50 0.40 0.33 0.12 0.33 0.16 0.72 0.33 0.18 0.10 0.20 0.16 0.33 0.27 4. (continued) lei (dl 6203 6202 6201 6204 6205 6206 6207 6208 6209 6213 6212 6211 6214 6216 6215 6210 6217 6218 6219 6220 6221 6222 6225 6224 6223 6227 6226 6230 6231 6232 6228 6229 6233 6236 6235 6234 6237 6240 6239 6238 6290 6289 6287 6292 6291 6282 6281 6288 6293 6285 6284 6283 6295 6294 6286 6300 6299 6298 6297 6296 6302 6303 6301 6304 6305 6306 6310 6309 6307 6308 6311 6313 6312 6314 6316 6315 6317 6318 6319 6320 ID ID by 475.0 564.9 387.5 306.5 310.4 616.8 218.8 485.2 368.4 526.0 711.5 239.9 448.4 411.5 117.9 308.1 200.3 476.4 557.7 310.2 325.4 616.5 222.8 257.2 235.1 474.4 546.7 588.2 313.9 493.1 226.3 188.8 593.0 556.4 530.7 346.5 440.5 474.0 237.1 167.1 513.6 314.4 350.9 367.4 305.9 669.5 324.4 393.0 232.7 209.1 206.9 483.6 290.3 259.2 493.1 196.9 114.4 140.9 153.4 124.8 677.5 356.0 318.5 361.6 509.1 306.3 391.1 235.5 381.6 390.8 466.4 252.7 425.4 289.2 195.2 538.6 45.8 50.3 X 55.9 55.1 X the 689.5 399.2 666.2 311.0 638.0 549.8 774.2 775.3 620.5 796.8 462.8 501.5 642.1 761.3 623.5 623.2 590.6 319.2 413.2 408.2 533.5 616.8 342.7 763.9 604.1 268.1 497.4 565.8 614.8 685.8 649.0 301.2 665.6 215.8 676.7 774.0 436.4 443.5 193.1 548.3 341.0 487.5 439.4 654.0 604.7 600.6 330.7 324.8 639.1 560.0 567.2 505.7 624.4 582.6 653.8 633.3 730.8 571.8 737.6 645.5 302.8 405.1 258.4 405.2 139.3 163.2 574.0 570.3 564.8 669.2 562.0 673.7 388.6 604.8 279.8 344.1 290.4 483.1 123.4 47.1 y y NASA F555W F555W 17.56 17.56 17.55 17.64 17.57 17.58 17.60 17.61 17.62 17.62 17.62 17.64 17.65 17.66 17.67 17.66 17.67 17.67 17.69 17.68 17.70 17.73 17.73 17.70 17.74 17.74 17.74 17.75 17.78 17.77 17.79 17.76 17.80 17.77 17.76 17.80 17.80 17.80 17.75 18.10 18.13 18.12 17.81 18.14 18.13 18.13 18.12 18.11 18.10 18.09 18.11 18.11 18.06 18.05 18.07 18.12 18.07 18.12 18.08 18.07 18.13 18.14 18.14 18.15 18.15 18.15 18.15 18.15 18.18 18.19 18.19 18.20 18.20 18.20 18.25 18.25 18.25 18.26 18.26 18.26 0.13 0.06 0.08 O.Q7 0.06 0.08 0.09 0.19 0.08 0.09 0.08 O.Q7 0.11 0.11 0.13 0.10 0.15 0.31 0.15 0.08 0.10 0.12 0.10 0.08 0.11 0.11 0.10 0.07 0.08 0.08 O.Q7 0.19 0.10 0.12 0.08 0.12 0.13 0.10 0.08 0.13 0.15 0.10 0.12 0.40 0.12 0.10 0.09 0.14 0.12 O.Q7 0.09 0.09 0.09 0.07 0.09 0.08 0.14 0.19 0.18 0.13 0.10 0.23 0.19 0.07 0.18 0.22 0.09 0.14 0.07 0.14 0.18 0.20 0.11 0.08 0.12 0.14 0.30 0.19 0.08 0.15 u u Astrophysics 336-555 336-555 -0.27 -0.61 -1.04 -0.51 -0.74 -0.77 -0.63 -0.14 -0.55 -0.43 -0.88 -1.08 -0.68 -0.32 -0.10 -0.56 -0.86 -0.27 -0.38 -0.46 -0.39 -1.08 -0.57 -0.74 -0.89 -0.96 -1.06 -0.31 -0.08 -0.58 -1.15 -0.77 -0.57 -0.55 -1.46 -0.67 -0.35 -0.85 -0.32 -0.70 -0.87 -0.72 -0.21 -1.09 -0.95 -0.60 -0.84 -0.68 -0.99 -0.65 -1.06 555-702 555-702 -O.o4 -0.20 -0.05 -0.50 0.18 0.20 0.36 0.37 0.22 0.24 0.09 0.25 0.20 0.25 0.12 0.26 0.26 0.29 0.30 0.23 0.00 0.35 0.09 0.25 0.19 0.20 0.29 0.21 0.18 0.28 0.52 0.28 0.29 0.27 0.09 0.34 0.15 O.Q7 0.07 0.38 0.17 0.23 0.46 0.40 0.24 0.11 0.20 0.00 0.80 0.10 0.38 0.24 0.35 0.16 0.24 0.19 0.37 0.28 0.12 0.25 0.19 0.15 0.17 0.43 0.14 0.06 0.52 0.10 0.32 0.03 0.52 0.13 0.15 0.25 0.49 0.04 0.21 0.26 0.53 0.00 Data System 1729 1992AJ....104.1721C 1730 ©American CAMPBELL ET Astronomical Society 6401 6402 6403 6321 6406 6323 6322 6408 6407 6325 6324 6409 6326 6405 6404 6410 6329 6328 6327 6331 6330 6411 6333 6416 6412 6334 6343 6332 6417 6415 6414 6336 6335 6419 6418 6413 6337 6420 6338 6339 6422 6421 6341 6342 6424 6423 6351 6348 6347 6346 6345 6344 6356 6340 6350 6429 6428 6427 6426 6425 6431 6430 6354 6353 6352 6349 6355 6358 6357 6360 6359 6433 6432 6436 6435 6434 6439 6437 6438 ID ID AL.: 546.3 232.9 493.0 328.2 681.7 782.0 370.1 635.9 315.0 678.8 284.1 205.2 426.2 475.6 476.8 433.1 489.1 499.8 430.0 423.2 492.6 132.7 193.6 198.6 552.7 507.7 531.2 652.7 590.6 535.3 607.6 618.3 581.9 744.6 287.0 241.0 496.6 427.1 451.9 490.3 235.3 200.3 510.6 302.6 391.5 729.8 509.0 251.7 212.2 480.6 461.4 498.4 499.3 469.0 194.3 512.5 669.8 592.0 396.4 662.0 578.2 575.9 304.2 254.4 275.4 227.7 402.7 469.9 458.8 290.7 469.2 160.7 783.0 249.6 249.8 439.2 45.8 33.2 99.7 X HST 417.8 547.2 332.3 656.1 295.3 477.0 462.8 573.9 397.0 393.1 381.0 533.7 532.1 334.7 686.6 363.8 719.2 320.0 612.1 689.7 693.6 410.1 441.1 444.2 264.7 495.6 163.1 109.5 138.9 608.3 604.5 565.6 571.4 558.9 302.0 623.9 547.6 319.6 231.0 651.3 476.5 403.2 271.1 483.7 269.3 559.8 543.1 551.2 532.0 362.6 377.9 374.6 524.5 291.8 210.5 285.2 260.0 478.2 477.9 432.0 151.3 178.2 527.3 633.7 344.3 519.4 326.6 706.0 646.3 503.9 564.2 328.1 650.2 524.9 371.9 300.2 711.0 264.8 177.3 y y IMAGES F555W F555W 18.89 18.96 18.90 18.92 18.95 18.91 18.26 18.96 18.29 18.27 18.27 18.96 18.30 18.96 18.31 18.32 18.31 18.30 18.30 18.97 18.34 18.97 18.35 18.98 19.03 18.46 18.45 19.04 18.48 18.46 18.31 18.40 18.34 19.01 19.00 19.00 18.98 18.98 19.01 18.40 19.02 18.41 19.03 18.42 18.44 18.43 19.12 19.11 19.11 19.04 18.50 18.48 18.47 18.47 19.13 19.13 19.10 19.10 18.51 18.50 18.48 18.48 18.52 18.51 18.52 19.15 19.16 19.18 19.17 18.51 19.14 18.52 18.56 18.53 18.56 19.17 19.17 19.20 19.23 0.14 0.20 0.14 0.21 0.09 0.08 0.11 0.12 0.15 0.12 0.14 0.19 0.13 0.24 0.12 0.09 0.11 0.19 0.14 0.12 0.23 0.12 0.14 0.34 0.17 0.18 0.15 0.17 0.24 0.07 0.13 0.22 0.24 0.22 0.34 0.12 0.18 0.14 0.12 0.12 0.11 0.21 0.38 0.17 0.18 0.20 0.17 0.10 0.11 0.15 0.21 0.16 0.16 0.29 0.15 0.15 0.21 0.08 0.15 0.20 0.12 0.12 0.10 0.13 0.14 0.19 0.10 0.08 0.09 0.10 0.15 0.14 0.28 0.20 0.18 0.14 0.26 0.15 0.17 a a OF 336-555 336-555 R136 -0.68 -0.70 -1.62 -1.34 -0.58 -0.49 -1.15 -0.93 -0.78 -1.18 -0.89 -0.90 -1.15 -0.54 -0.74 TABLE • 555-702 555-702 -0.08 -0.03 -0.56 -0.14 -0.02 -0.03 -0.08 0.25 0.04 0.10 0.15 0.23 0.14 0.05 0.53 0.49 0.66 0.34 0.58 0.32 0.09 0.19 0.58 0.42 0.17 0.31 0.64 0.22 0.35 0.45 0.34 0.38 0.17 0.57 0.47 0.09 0.25 0.28 0.31 0.44 0.14 0.16 0.02 0.33 0.18 0.49 0.00 0.30 0.51 0.22 O.Dl 0.30 0.35 0.06 0.12 0.00 0.40 0.28 0.16 0.38 0.34 0.23 0.04 0.14 0.50 0.13 0.44 0.20 0.47 0.43 0.07 0.48 0.13 0.23 0.20 0.42 0.51 0.24 0.39 Provided 4. e (continued) 6441 6362 6361 6440 6442 6443 6444 6446 6445 6368 6367 6363 6369 6366 6365 6364 6371 6370 6447 6448 6449 6450 6451 6453 6455 6454 6457 6459 6461 6462 6463 6372 6373 6374 6376 6375 6380 6379 6378 6377 6385 6382 6381 6384 6383 6452 6456 6458 6460 6465 6464 6467 6466 6389 6388 6387 6386 6391 6390 6395 6471 6476 6475 6474 6472 6473 6469 6468 6470 6392 6398 6397 6394 6393 6400 6399 6396 6477 ID ID 438.6 503.8 604.6 793.7 688.2 484.5 420.8 441.9 451.8 419.8 480.3 573.0 322.6 662.5 389.1 604.6 343.5 295.2 467.1 433.4 481.6 371.5 450.1 447.4 467.8 429.9 232.0 433.6 432.1 124.8 168.5 113.8 371.6 375.5 579.0 514.9 562.8 323.3 445.3 517.8 455.5 256.7 489.1 415.4 460.1 451.1 448.5 175.1 120.8 578.1 352.7 681.5 364.3 573.1 310.7 446.6 730.4 236.4 280.8 444.8 436.8 458.1 102.6 162.9 505.2 371.6 706.7 268.5 213.4 291.8 137.8 199.3 135.5 by 773.0 558.2 87.0 90.4 83.1 X X the 314.5 367.7 551.6 376.5 516.5 379.6 730.8 357.4 589.2 342.8 306.3 241.3 680.9 409.6 576.4 653.9 333.9 603.6 372.5 368.8 633.2 610.5 632.2 292.7 603.3 365.6 343.5 564.0 312.2 736.0 436.0 352.4 480.5 461.4 125.7 286.6 169.9 544.7 717.8 382.7 589.5 528.7 578.0 684.8 461.2 610.4 301.5 745.4 284.5 717.9 272.9 711.8 254.3 252.8 198.0 553.5 515.7 769.4 604.3 336.5 664.9 288.7 288.5 274.6 457.9 459.6 163.8 599.6 304.1 768.4 732.0 439.1 329.6 343.1 389.6 719.7 166.7 64.9 y y NASA F555W F555W 19.26 19.27 19.27 19.29 19.33 19.29 19.33 19.34 19.34 19.35 19.37 19.40 19.37 19.41 19.41 19.40 19.46 19.47 19.48 19.51 18.57 19.60 18.59 18.57 18.60 19.63 18.62 18.58 18.59 19.66 18.65 18.65 18.64 18.65 18.66 19.57 18.58 19.66 19.72 19.72 19.72 18.69 18.68 18.71 18.70 18.75 18.76 18.72 18.72 18.72 19.84 19.78 19.80 19.79 18.71 18.70 18.81 18.80 18.77 18.76 18.74 18.71 18.81 18.83 18.82 18.72 18.83 18.84 18.84 18.83 18.82 18.86 20.29 20.39 20.07 19.95 19.91 19.85 0.33 0.17 0.16 0.21 0.17 0.16 0.24 0.20 0.19 0.25 0.26 0.37 0.20 0.23 0.25 0.23 0.28 0.19 0.23 0.26 0.15 0.31 0.22 0.14 0.13 0.30 0.10 0.13 0.12 0.10 0.30 0.10 0.15 0.11 0.23 0.20 0.24 0.09 0.30 0.21 0.23 0.28 0.14 0.10 0.15 0.16 0.32 0.14 0.14 0.27 0.29 0.35 0.27 0.39 0.27 0.32 0.27 0.15 0.12 0.17 0.17 0.20 0.12 0.13 0.13 0.32 0.23 0.19 0.18 0.11 0.11 0.19 0.20 0.40 0.44 0.30 0.52 0.38 a a Astrophysics 336-555 336-555 -0.98 -1.29 -1.36 -0.92 -1.00 -0.81 -0.77 -0.88 555-702 555-702 -0.13 -0.18 -0.22 -0.02 -0.04 0.33 0.49 0.33 0.06 0.65 0.25 0.20 0.54 0.43 0.21 0.08 0.53 0.30 0.35 0.71 0.89 0.03 0.40 0.22 0.40 0.55 0.35 0.02 0.42 0.40 0.33 0.14 0.75 0.41 0.17 0.44 0.11 0.06 0.50 0.39 0.29 0.30 0.13 0.24 0.26 0.46 0.40 0.17 0.48 0.55 0.30 0.43 0.51 0.61 0.26 0.82 0.13 0.74 0.33 0.50 0.48 0.31 0.63 0.41 0.50 0.15 0.16 0.68 0.29 0.46 0.62 0.40 0.21 0.43 1.16 0.13 0.51 1.43 Data System 1730 1992AJ....104.1721C 1731 © American CAMPBELL ET Astronomical 7092 7089 7093 7091 7090 7086 7085 7084 7088 7087 7083 7082 7081 7105 7104 7102 7103 7006 7005 7004 7096 7101 7100 7099 7098 7003 7002 7001 7097 7095 7094 7007 7109 7108 7107 7106 7016 7015 7014 7008 7010 7009 7110 7013 7012 7011 7115 7114 7113 7112 7021 7020 7019 7018 7017 7116 7111 7117 7120 7119 7118 7027 7026 7025 7023 7024 7022 7028 7029 7039 7030 7036 7034 7033 7032 7031 7038 7037 7040 7035 ID AL.: 577.4 551.5 622.8 314.3 599.9 365.8 637.7 662.4 495.9 205.4 496.3 411.6 140.7 654.5 681.5 535.6 647.3 506.5 510.6 342.2 367.7 390.8 602.9 727.5 377.7 365.7 615.8 325.1 768.2 684.5 455.9 467.6 251.8 298.0 492.0 299.0 460.2 190.1 369.4 526.3 552.5 500.6 637.9 661.2 564.5 309.8 653.1 225.3 754.6 297.5 286.1 402.8 447.1 461.3 291.8 451.2 656.7 407.9 466.2 128.4 186.6 389.5 663.4 660.6 589.5 324.5 483.7 417.1 561.7 375.2 617.2 709.5 211.1 206.0 125.5 188.7 709.1 721.0 98.8 77.2 X HST 482.9 480.5 539.9 559.1 308.4 341.0 703.8 244.4 299.3 262.3 293.7 210.0 465.1 198.4 187.9 150.2 583.4 579.9 650.7 367.2 375.2 340.9 284.5 401.8 442.7 264.3 442.2 480.3 198.9 110.6 172.1 198.3 133.1 608.7 351.6 306.9 262.0 23Q.5 25D.4 204.3 176.7 177.8 122.4 155.1 171.5 174.6 345.0 455.3 4. 14.93 142.8 138.2 580.5 224.9 217.1 408.7 481.3 406.8 483.5 194.3 178.8 631.6 349.2 312.3 269.5 119.6 195.8 52.2 59.8 61.0 97.8 67.4 79.6 48.7 88.9 79.7 73.8 77.9 90.4 55.3 77.6 67.6 y IMAGES F555W 17.25 17.19 17.10 17.22 17.16 17.60 17.59 17.53 13.48 17.52 17.50 17.50 17.47 17.41 17.39 17.35 17.33 17.33 13.28 17.46 17.49 17.48 17.30 17.29 13.26 12.57 11.81 17.25 17.72 17.72 17.71 17.70 17.61 17.60 17.80 17.77 14.65 13.65 13.65 13.61 13.77 14.58 14.49 14.40 13.92 17.80 17.82 14.80 14.72 14.66 17.73 17.73 17.85 17.82 17.94 17.93 17.91 15.22 15.12 15.10 15.08 15.04 14.94 14.91 14.83 15.34 15.27 15.39 15.28 15.57 15.51 15.51 15.42 15.52 15.49 15.93 15.89 15.96 15.93 Society TABLE 0.09 0.08 0.11 0.07 0.06 0.08 0.10 0.09 0.08 0.07 0.16 0.07 0.06 0.10 0.06 0.11 0.10 0.12 0.11 0.10 0.07 0.07 0.09 0.10 0.08 0.08 0.05 0.03 0.10 0.11 0.04 0.06 0.04 0.04 0.05 0.04 0.04 0.04 0.06 0.09 0.11 0.13 0.05 0.05 0.12 0.09 0.14. 0.09 0.11 0.17 0.10 0.18 0.12 0.04 0.05 0.04 0.05 0.04 0.05 0.04 0.06 0.07 0.06 0.05 0.07 0.05 0.05 O.o7 0.06 0.05 0.04 0.10 0.05 0.06 0.05 0.07 0.06 0.07 0.05 0.05 17 OF 336-555 5. R136 -1.10 -0.45 -1.03 -0.83 -1.10 -0.89 -0.88 -1.02 -0.29 -0.75 -0.81 -0.84 -1.00 -1.06 -0.71 -0.86 -0.60 -0.60 -1.15 -0.83 -0.86 -1.02 -1.04 -0.90 -0.96 -1.11 -0.28 -0.26 -0.95 -1.11 -0.84 -0.66 -0.50 -1.11 -0.98 -1.02 -1.09 -1.08 -1.32 -1.13 -1.00 -0.85 -1.06 -1.11 -1.07 -1.21 -1.32 -1.21 -0.34 -0.37 -1.14 -1.04 -1.01 -1.14 -0.89 -1.23 -1.09 -0.71 -1.04 -1.00 -1.19 -1.12 -1.03 -1.03 -0.97 -1.06 -1.03 -1.19 -1.13 Photometry 0.09 • 555-702 -0.03 -0.02 -0.03 Provided -0.12 -0.09 -0.19 -0.06 0.11 0.20 0.13 0.22 0.02 0.13 0.29 0.15 0.05 0.15 0.19 0.41 0.37 0.11 0.00 0.07 1.87 0.25 0.06 0.05 0.20 0.13 0.21 0.07 0.55 0.05 0.16 0.10 0.26 0.06 0.21 0.16 0.24 0.15 0.19 0.20 0.19 0.15 0.26 0.09 0.29 0.47 0.14 0.04 0.19 0.12 0.06 0.18 0.26 0.29 0.25 0.08 0.22 0.09 0.06 0.24 0.09 0.19 0.15 0.09 0.14 0.08 0.40 0.08 0.60 0.29 0.19 0.16 0.14 0.25 0.01 0.08 0.19 of (b) Ia) stars 7141 7140 7130 7138 7135 7133 7132 7131 7129 7125 7124 7123 7136 7134 7128 7126 7147 7146 7145 7144 7143 7142 7045 7044 7139 7043 7042 7041 7047 7137 7127 7122 7121 7148 7153 7154 7152 7048 7054 7046 7155 7151 7150 7149 7049 7157 7156 7160 7053 7051 7050 7162 7161 7159 7158 7052 7061 7060 7059 7062 7058 7057 7056 7055 7066 7065 7064 7067 7063 7069 7068 7080 7079 7078 7070 7076 7075 7074 7073 7072 7071 7077 ID outside by 483.3 368.4 615.6 678.4 644.0 623.6 301.6 335.6 200.3 201.6 473.0 453.9 438.6 483.6 553.0 536.5 377.1 652.2 365.6 716.8 716.6 404.5 443.4 432.0 497.0 455.0 188.2 162.2 157.7 154.9 533.2 750.8 589.1 559.8 628.1 375.6 583.7 312.3 312.1 320.8 280.1 214.1 441.9 185.8 184.3 545.4 582.5 348.2 734.6 250.1 114.2 196.9 112.9 155.1 134.0 139.6 153.2 564.9 536.0 515.2 674.5 373.9 353.1 394.8 707.2 499.7 413.2 144.4 596.7 546.1 624.0 606.4 656.2 757.3 414.7 166.4 157.1 759.7 722.1 47.8 74.0 67.6 X R136 the 499.1 564.5 593.0 520.5 552.7 557.6 627.7 385.0 338.1 324.7 358.2 373.3 422.7 210.2 254.5 465.1 208.0 230.1 463.2 499.0 123.3 118.1 319.8 527.8 316.0 721.8 472.7 267.7 420.0 464.0 415.0 493.0 430.2 136.5 338.8 577.3 684.2 658.2 657.3 386.1 370.0 725.3 207.8 233.5 290.7 469.6 419.6 226.4 263.8 131.7 105.9 184.0 146.0 143.3 141.2 100.7 343.0 264.3 142.9 196.2 343.1 379.9 282.1 179.1 354.7 654.0 718.5 760.9 281.6 260.2 249.7 274.0 211.8 153.6 101.2 94.4 81.9 52.3 43.4 84.0 99.3 66.2 y (PC7). NASA F555W 18.12 18.66 18.55 18.60 18.51 18.51 18.40 18.32 18.06 17.97 17.95 18.50 18.35 18.27 17.94 17.94 18.41 18.37 18.36 18.ol 17.98 17.94 18.97 18.81 18.80 18.70 18.70 19.10 18.45 16.11 15.98 19.11 16.21 16.15 16.12 19.10 19.08 16.47 16.45 16.42 16.22 16.49 16.47 16.25 19.15 19.03 16.31 16.34 19.26 19.01 16.42 16.39 16.36 14.52 14.30 14.27 19.32 19.36 19.73 16.65 16.60 16.52 16.50 16.62 16.74 16.72 16.68 16.67 16.74 16.80 17.07 16.74 17.01 16.91 16.89 16.83 16.91 17.06 17.05 17.10 17.10 16.92 0.11 0.13 0.12 0.14 0.20 0.23 0.09 0.14 0.16 0.28 0.20 0.12 0.23 0.16 0.12 0.20 0.18 0.16 0.21 0.23 0.16 0.19 0.19 0.18 0.13 0.29 0.15 0.05 0.30 0.26 0.20 0.09 0.09 0.05 0.23 0.25 0.19 0.06 0.05 0.06 0.21 0.26 0.06 0.06 0.41 0.07 0.07 0.08 0.06 0.04 0.04 0.58 0.21 0.28 0.06 0.10 0.06 0.06 0.06 0.07 0.05 0.08 0.08 0.11 0.08 0.06 0.04 0.05 0.06 0.07 0.15 0.10 0.08 0.06 0.08 0.08 0.06 0.09 0.08 0.05 0.10 0.08 17 Astrophysics 336-555 -1.28 -1.30 -1.07 -0.54 -1.14 -0.72 -0.86 -0.42 -1.54 -0.93 -1.01 -1.01 -1.20 -1.11 -1.05 -1.01 -0.51 -0.79 -0.78 -0.59 -0.88 -0.99 -0.86 -1.14 -0.99 -0.35 -1.16 -1.02 -1.32 -0.78 -0.51 -0.69 -0.91 -1.04 -0.79 -0.71 -1.10 -1.09 -0.99 -0.53 -1.01 -0.89 -1.22 -0.77 -0.75 -0.56 -0.49 -0.80 -0.61 -0.67 -0.92 -0.74 -1.09 555-' . -0.07 -0.07 -0.08 -0.12 -0.08 -0.01 -0.02 -0.22 0.22 0.14 0.02 0.32 0.18 0.21 0.24 0.13 0.16 0.09 0.20 0.08 0.38 0.28 0.09 0.13 0.05 0.51 0.26 0.28 0.22 0.16 0.14 0.16 0.39 0.09 0.28 0.33 0.74 0.17 0.18 0.78 0.34 0.41 0.04 0.54 0.20 0.06 0.14 0.02 0.10 0.09 0.22 0.06 0.22 0.07 0.19 0.34 0.19 0.12 0.29 0.19 0.27 0.10 0.13 0.12 0.13 0.20 0.10 0.22 0.21 0.19 0.05 0.00 0.40 0.17 0.12 0.15 0.18 0.12 0.04 0.04 0.09 0.07 702 Data System 1731 1992AJ....104.1721C loci R136 than there sparsely dercorrected and of R136 1732 R136 reddening, rily stars. stellar sible among out the seen cause gives vestigation the real. function luminosity R R136 than the 136 the © We current an slopes host of due 8 in but stars M a appears and that A American are are diagram, effects and which medium CAMPBELL points offset have detailed the 555 the more populated. to is counterintuitive of very very outside fall outside = for of shown it function loci Definition the data difficulties CCD counted -4, for between of are the would to such on likely the similar 3.3 8009 8006 8007 8018 8005 8013 8017 8010 8004 8003 8025 8015 8014 8012 8016 8002 8011 8008 8001 8020 8019 8026 8024 8027 8023 8021 8028 8022 8029 similar. ID but within discussion of this winds be reddening further we PCs luminosity ofR136 the in stars of The area chips. a that both 510.9 618.7 213.8 209.1 291.9 223.9 481.2 478.6 581.8 578.5 511.7 520.7 695.2 321.9 501.6 565.6 310.2 362.7 368.2 238.1 457.1 256.6 472.1 118.7 793.4 230.7 107.1 ET Astronomical If 31.1 order 71.3 is explanation X imply Fig. cannot small, R136. stars CCD star between 5, Team the from this shown Luminosity AL.: in outside. In in the 7, are 430.3 490.1 393.6 371.0 377.4 618.7 539.4 289.4 477.6 253.0 484.3 196.6 525.7 322.4 618.5 222.7 224.6 214.6 221.1 110.6 195.1 128.6 i86.1 171.3 away 47.0 84.7 78.8 66.9 63.6 since 11, y but cross-normalizing The the of R136 counts of the and relative in offset that chips. HST -0.05 R136 However, offset be the functions this and (1992; magnitude. F555W 0.5 in on color-magnitude 15.75 15.69 15.23 17.70 17.75 16.13 15.05 14.77 17.57 17.66 17.60 17.69 16.12 14.37 17.60 16.83 15.95 14.18 17.91 17.89 18.60 18.53 18.72 18.28 18.14 18.10 19.05 M 18.80 18.82 M from one 8 flat-fielding sure The the region is IMAGES Fig. concentration 555 although 336 problem. PC6 the is mag from within stars That to to Function that might -M - = due 0.04 0.03 0.06 0.05 0.04 0.05 0.03 0.03 0.03 0.05 0.04 0.03 see 0.05 0.05 0.06 0.05 0.04 0.05 0.05 0.09 0.07 0.07 0.04 0.06 0.05 0.06 stars 0.08 0.10 0.08 the that log log the 0.1 t7 12. fall this within luminosity TABLE Society 555 to the are is, the 7 Chaps. core. to 336-555 of of mag, stars One R136 The the expect and on in OF be color, PCs -1.12 the -0.78 -0.62 -1.28 -1.07 -0.79 -0.78 -0.89 -1.08 -0.99 -0.87 -0.79 -1.08 -1.20 -0.81 -1.01 -1.17 -1.20 -0.83 -0.89 -0.12 -0.74 -0.88 -1.05 -0.45 -0.45 Therefore, offset stars slightly offset the a the problems the the 6. more PC6 offset difference Rl36 and WF on can This stars -4. offset 5 cumulative Photometry of clearly luminosity diagram 6 same 555-702 outside the and flat-fields is however, PCs is /PC and bins massive see without are • 0.26 0.12 0.16 0.36 0.28 0.31 0.32 0.22 0.18 0.19 0.24 0.33 0.18 0.18 0.25 0.34 0.26 0.21 0.36 0.27 0.25 0.34 0.15 0.23 0.32 1.01 0.34 0.18 0.40 Fainter cleared prima is redder that within due in inter 8 with area 5, pos Provided that can 12) un the are In be- for of in to 7, is is of stars 8040 8036 8046 8044 8043 8042 8041 8039 8045 8047 8038 8037 8035 8030 8031 8054 8053 8055 8052 8050 8049 8048 8033 8032 8034 8051 8068 8057 8056 ID come in tions by stars star seeing and artificial tion, F555W R136 tered be because found for ences estimate outside R136 Figure this region noise segregation explore could tamination resulting l>M outside 496.5 457.8 533.1 399.5 599.8 673.6 689.1 319.2 629.8 379.3 756.7 435.7 297.2 429.6 448.6 113.1 186.6 155.9 123.2 505.0 556.0 767.9 711.2 378.3 Fig. 100.5 128.5 123.1 We more For the 37.6 31.4 the X v each finding as by the in to of data on goes incomplete; than are occur how in was estimated very strong 13 automatic 13 the 547.7 577.5 330.6 693.2 201.6 250.6 263.3 217.4 222.8 479.0 452.7 164.4 124.2 183.2 526.5 603.6 336.8 670.2 241.4 219.1 116.9 107.2 548.0 138.8 Rl36 the the of this and the essentially 89.7 91.8 53.1 96.9 70.2 massive stars the apparent y completeness R136 the stars magnitude from within shows for away. to normalized this outside many by range raw from technique crowded luminosity central question F702W anywhere. F555W '19.82 (PC8). inner 20.14 20.13 20.05 19.76 19.98 19.74 19.95 19.14 be 19.96 20.17 20.07 20.22 20.28 20.28 20.99 19.88 19.90 19.55 19.73 19.86 19.85 19.94 19.32 19.98 19.52 19.23 19.37 19.19 NASA stars evidence Galactic with per a region. luminosity obtained Fainter that of dynamical the incompleteness variable M turnover it routine. the region. none 0.19 0.17 0.17 0.16 0.25 0.25 0.27 0.21 0.30 0.18 0.20 0.17 0.12 0.29 0.22 0.25 0.33 0.21 0.23 0.17 0.23 0.11 0.11 0.11 0.11 0.21 0.34 0.41 0.55 within the region magnitude is 555 t7 bin, frames, widths region estimated in there mentioned relative to harder central Astrophysics = corrections function The 100 foreground 336-555 for more of than match incompleteness -4 -0.92 -1.20 -0.91 -1.00 -1.10 in initial 40 of With We seen function. stars the mass is of effects the of number one the to pixels M to detail to a region. R 555-702 20 then artificial approximately errors, in slight future. bin is were lower v- this 136 -7, detect cluster. in at mass segregation. 0.48 0.25 0.17 0.41 0.50 0.11 0.98 0.34 0.34 0.63 0.29 0.51 1.52 1.29 0.51 0.74 0.42 0.51 0.68 0.76 0.26 0.51 O.o7 by 1.09 1.44 0.82 0.34 0.89 1.67 pixels. Fig. 0.3. would in stars Sec. a -3, of with applied Results were than of completeness using the found However, time, the hint mass R136 No function, 11 We so and stars 2.2. stars is it was Data Mass be higher slope For for outside center we is si~nificant expected placed that note the in and measure stars expected are One hs correc these impossible and estimated the in were We do each annuli the segregation l>(log there automatic the System that measured presented the signal-to however, center hundred not for of inside of number hope on correc found. radius differ in R136 outer it. mass faint stars only 1732 N)! con may cen take the the by to to of of 1992AJ....104.1721C 1733 slope see ours direction cations luminosity his nosity and luminosity Doradus 1985). © slope Parker ZAMS for can American CAMPBELL function Melnick, for the but of is be function the 1992). function mass the - core compared outside 0.26, stars plotted LMC however, for of L1. ~ LO LO LO Unfortunately, ET FlO. within within outside Astronomical which (PC7), is in the a Rl36. into similar ( star R136 AL.: Ratnatunga with by S. 12 14 16 region. 18 20 the R136 The and of a uses is cluster Melnick For HST 0 more the that true we in hexagons throughout uncertainty, are core. a This very the are IMAGES crowded shown measured relationship without mass of & same unable ( 2 good would 1986) (PCS). Bahcall .1 Myrs Society with u, R function luminosity 30 136 in OF spectral agreement filled to from Stars imply for the Doradus to region between 'r· translate Rl36 1985). . convert magnitudes circles stars '·. with the • .2 ) (Massey have that • classifi ' • u> range lumi in and This with Provided . (but a M the the 0.6 his higher 30 those as v have a • cr X function .3 uncertainty without X been slope sample sity function function once ity luminosity termines north. (mag) Milky ' !:. Another function eliminated !:. of by comparable of are is Way Reid X star the of X • for similar the triangles •o has a X for xo .4 nearby magnitudes mass a function o t:. o x field region formation et that given from that a NASA X outside outside outside outside al. slope • function (PC5), to stars we magnitude the to galaxies. ( region !:. of that 1987) star for find to 30 .5 of star R136 R136 R136 R136 and X's Astrophysics is !:. filter a X lists. Doradus compiled 1.35. slope for mass and Constellation examined than formation (PC6), by Thus, F55SW. (PC7) (PC6) (PC5) Clearly, (PCS) R Freedman 0 those found of 136 function. .6 squares in 1.0::1:0.3 the by Stars stars stars appears the terms that a Scalo slope slope III, V-band (1985) for (1985) Data From was where of of to ( located 1986) overall of the be undoubtedly this luminosity 0.55. System a shallower luminos Salpeter for a he to inten large This 1733 the de the 1992AJ....104.1721C M slope and mass mation tion tion state than 1734 v- 8002 8003 8001 8004 6002 6018 6001 6013 6007 6006 6005 6004 6003 7002 7009 7006 7006 7003 © .... 11 cFrom 6 NOTE.- ID Mk42 Mk39 Mk37 Mk35S Mk35N Mk35 Mk34 Mk33N Mk33S Mk32 Mk30 Mk26 Mk24 Mk15S Mk15 Mk14N Mk14 Mk13 Mk12 Mk9 Mk7 Mk6 Mk5 'From ' R136b R134 Mk37W Mk8 R142 R141 R136c NOTE.- 26 25 R136a-A Ma.gnitudea to magnitude From 3 2 for difference. Reid of stars the from Rl36a.-A American is -3. CAMPBELL Walborn's the Walborn is Melnick the probably m(469)~mR Literature and slope of are in In et indicate measured Rl36a-B regions Rl34. ring (1985) (1986) (1986). progress fact al. present 4.26: 4.19: 4.62: 4.53: 4.09: 5.51: 0.55 5.03 3.33 3.43 3.19 3.41 3.67 3.84 0.00 0.56 0.40 0.66 0.64 0.90 2.66 2.16 3.27 11 found A 134 Constellation TABLE the refer in around TABLE colon (469)" review. find or due northern Reid the rather Feitzinger to ET Astronomical following net Moffat 8001 8003 8002 5004 5104 5001 5003 6020 6001 6002 6003 6005 6007 6010 6017,6089, 6006 6004 6008, 6009, 7003, 7005 7006 7009 7021, 7160, 7004 ID 25 26 7001 7002· 7. in for to a today. 8. AL.: F469N and et in Identification O.Ql 0.01 0.04 0.04 0.07 0.06 0.08 O.o! 0.06 0.08 0.09 0.01 0.34 0.11 0.09 0.04 0.04 0.14 0.19 0.04 0.44 0.18 0.07 Rl36. Constellation main-sequence et 6014 6013 7019 7029 7161, Tables Emission-line a southern than the et a!. Constellation al.'zt image al. difference HST magnitude 6143,6161,6264 7162 {1985) compiled (1980). 2-6 III For R136 R136a-AS an However, subcomponent (on-band R136 Mk37W Mk33S IMAGES designations. Rl36b R136c Mk42 Mk35 Mk24 Mk26 Mk30 Mk32 Mk34 Mk39 Mk37 .. is R134 Rl41 actual Mk7 Mk6 Mk8 means mo· .. AN that of B a stars. minus stars. in much that Society III a respectively. young WC5+04 initial III; The turnoff continuum) the luminosity this the WN7-A OF where 03If/WN6-A 03If/WN6-A 03If/WN6-A 03If/WN6-A "N" residual older 03 B2: WN7-A WN4.5 B0-0.5 WN7 Spectral 07V OV 03 03 05-6 03 08 03-4 03-4 03-6 03-6 03-4 05-6 0(7) 08-9 05-7: B0.5-0.71 B0.5 more evolutionary difference R136 and WN7-A (Mk33) (Mk37) WN4.5 03-4V 03-4V 0(7)V mass region II II/WN6-A II/WN6-A II/WN6-A II/WN6-A B05.1 WN7 08-9 05-6 0811 Ip? relative is I "S" v v v v v v at star Ia uncertain. • typeb appended region, higher about func func to Provided for the the in emission diction. R136c. Wolf-Rayet nents. slope stars slope additional fainter detected or detected Table R136a R136b Wolf-Rayet to therefore while 1 1984; (cf., component FIG. the (Feitzinger and 2 Several R134 transitional bottom by Walborn and 7. much of Melnick 8, R136b Star than had and R136c are An and R136a the it are image, the on was is panel of stars, enlarged et their in number ground-based spectral indeed more stated star stars magnitudes the stars R136a given. al. luminosity NASA was likely our was 1973; is 1985; stellar is 1980). shown R136a-A. or the F469N most like like emission resolved version 3.4 not. is already were that likely The 3 a net to features itself Moffat Moffat The is transitional type. that R134, Wolf-Rayet contain emission Astrophysics of in Chu Moffat it presence measured of function elongated. net-emission top detected to Figs. known studies In must known Fig. which by image, Outside & be panel et et Rl36c, characteristic addition image. one 6 Seggewiss the al et a 6 al. showing be and is weak-linked spectral type. al.'s we of to Stars is from or 1985). R136b in have PC the (1984) One at of be the much and measure more 7, to image continuum R136: R136a-B, most can into Although only a R136 this confirms Data R136a, Wolf-Rayet Wolf-Rayet the recognized 1983; The type. is see did WN-type of flatter, R136a, image three indeed a that are R136a's we R136b for Wolf-Rayet Wolf-Rayet net weak-lined not Chu image, System The two and the listed this detected we b, R136. compo relative F469N with detect upper and much other et stars stars stars stars have star, and 1734 that pre and and al. c in a 1992AJ....104.1721C stage companion ined that multiple. a argues Ip?." 1735 F702W star © The the is American Given (Maeder 1.2" CAMPBELL that the star and PC5 The time southwest can Rl36a Mk5 does the image image & be peculiar L1. ~ it L1. ~ ll) ll) ...... 0 C\1 ll) not is Meynet I seen formed takes Astronomical ET stars FIG. through reddening for classified of show of -.8 -.6 -.2 -.4 Mk5 AL.: any within .4 . 6 . 8 in 8. 0 3.5 nature Mk5, a the 1987). A 6. up at massive evidence HST line is Mk5 The F336W-F555W o Johnson • t. o X by least in several shown but -2 outside outside outside outside of for colors the IMAGES Walborn 136 the E(B- 3.5 it star F336W system that in is have arcseconds. spectrum, X Society R R136 R136 R136 4.8 Fig. V) 10 • to the 136 X not OF vs =0.34; 6 (Johnson (1986) • -1.5 mag evolve t. image. yrs F555W-F702W 14. star been (PC7) (PC6) (PC5) (PCS) • R136 t. ago, No we fainter ... the X corrected might There • as 1968). to There- curved bright exam 0 since Provided "B2: • that F336W-F555W 0 be in is for ~5 line -1 color-color reddening. designates The by stars fore, and given in remains were 4. • • Fig. The binning STELLAR by center is ~·· • detected the contained X diagram in The F336W 15 at the the unknown. -.5 the ox reason X "# and straight intrinsic (346.26,467.40) the was t. X X tables. • for NASA I DENSITIES X in listed X stellar surface 0 calculated PROFILE • the within X F555W for line UVR XX • 0 stars For in in the t. X photometry given Astrophysics brightness 0 the colors Table the the listed AND 0 but OF peculiar upper from few innermost in ffiE for • in not THE 9. right the Tables 0 stars the The CLUSTER F336W, profile and SURFACE nature system is .5 luminosity B profile 2 in a arcsecond the in for Data of a Tables of Rl36 U- inner BRIGHTNESS was the coordinates centroid System V generated spectrum is of 10" 2 color shown and Rl36 1735 that of of 4. 1992AJ....104.1721C 1736 Table number stars 0.06 consistent consider R136 really reflect comparison. including r= radius, profile -0.80 © Figure -1.72±0.06. pc; and American is 9 have CAMPBELL has the that or have of problematic, a the a poor 15 with half-power been stars profile luminosity central a has shows This been possibility small a statistics assumed. in y pure Description ...... , ~ through Flo. magnitude ..... corrected value with a ~ ET 0 that core Astronomical O core, given however, point, power 9. as AL: weighted -8 -6 -7 the -5 rc=0~25 -4 -3 -2 -1 that of lead at A 6. 0 1 r-+0. The that -3 radial on The color-magnitude rc HST the distribution for of law the us o of t:.. the e o is x points absolute, the given is absorption. Experiments very outside 6. outside outside outside R136 the significantly IMAGES to of right. Poisson bin. is brightness a the conclude profile innermost shown central center. -2.5 shown 6. the The Society form reddening-corrected R136 R136 R136 R136 of small colors diagram statistics OF has stars •• The in X in /(r) region We profile (PC5) (PC6) (PC?) (PCB) that smaller ox with R136 6. structure 6. • r Fig. Fig. have 6. c number in error < thus • with -2 a: X~ 6. • the x!t 6. • R136 0~25 D profiles rr been 15 of of 15 might 0 (MrJJew-Mr555w)o :sf),. F336W-F555W than with Provided core bars also x and the the for 0 >P ~~tft~A magnitude corrected or of of is ~ X