© 2008: Instituto de Astronomía, UNAM - Massive : Fundamental Parameters and Circumstellar Interactions Ed. Paula Benaglia, Guillermo Bosch, & Cristina Cappa lo con de Luego They in definitiv un ciones Key p ha Since (WR) ings. this ation ra and that kno discordance. nary recurren R Casilla the still mass-loss sidad and na de imp Belgium. THE erio evMexAA cidad y v v 5 1 4 2 3 Li the en os HD sistema R. Massiv The e Europ Departamen F Institut Las wledge ortan ev un WR+O Wor ` searc ege, fragmen acultad ob te w Nacional d nature a X are and, Despite olution the Gamen, 601, are de p ould dynamic Campanas of 980, strong ject 93162, p radial eri´ ely aso tly FIRST ds: All parameters ean er t hed que, ab the rate, e imp disco La ´ odicas ıo d’Astroph ´ ee of impact. through La binario ciada predicted de binaries: pro in stars sho (Serie out allo Southern binaries tary do de Serena, du for ma these W to of Serena, 1 mec que Ciencias ortan median the la order v ws 1. although v La orbital ws E. e e 208 and 6 . de Observ ery a jor p of hemos de a INTR the deriv hanical Ao p erio Plata, imp massiv that de Gosset, us con HD F ysique , t ermitieran sp ob their Chile. su ´ source ısica, sp da ut, ˆ In Observ are Chile that to c with ob te b to Confer ectral Astron´ hemical susp dicities. jects atory ectroscopic ortance y ys. v ed cercano 93162 colisi´ 17, jects ODUCTION this in observ the elo k Argen observ determine some rotation ey e Univ h et v impact ([email protected]). 2 radial predominan ected atory EINSTEIN , uge estigate B-4000, cidad of and omicas The N. de t on ob W AL encias) con yp that tina. ersidad (WR ionizing authors aciones olf-Ra ev demostrar ado jects of , F G mass-loss I. de a es Carnegie are text, Chile. of or ´ eoph binary olution radial v Morrell, los — could on massiv SOLUTION BINAR pla O elo Li y vien their the minim esp 25), its , b ` its Geof ege stars: de and y ysique, their 208 y cities ecause 33 et massiv , tly del to ectrosc´ tos. and p first a La mass que (Sart of reiteradamen also ´ , nature Observ ısicas, ossible e ev star of W crucial b d rates, 91–93 3 um esta sat ´ determine Serena, individual surround- ıas. e stars, strong olution olf-Ra Sin UV V. from Univ . dem time, a Y their ha Tilman), e ´ elite and and masses opicamen WR Univ colliding-wind atories, hip´ S. O+O v em ha radi- HD ersit they uestran (2008) v e role ABSTRA our sp ariabilit Niemela, y Be- otesis. bi- RESUMEN EINSTEIN p v its G. an bargo, er- X-ra et is 25 e erio ectroscopic ´ F e (HD nev te R. OR 93162 is y te dic se que Soliv er Con actually emission hasta y 93162) desde 4 ha tions the for 50 serv rio tions v b this rep in brigh indep massiv motion inclination, if from CT radial-v THE b and elo H. een WR een binary , com ella supuesto dicit el the high-, orted W T HD se ( t atories t cities Sana, star ahora w data w ≡ o ob t to — el a enden e the larger (see 4 found descubriera o 25 o bined e in an y ( matter WR observ jeto 2. asso elo (Moffat 93162 an˜ MASSIVE V stars: groups pro sp star v o system. could es R 8 2,5 radial estigate v measured acquired o RESUL details eccen cit ectra no V = er and tly medium- vide un ciated que absolute de 1994 than so with Y. y researc studies the 8.1) 25) ed se W (WR of explorar sistema v collected far. b with w tric 1978; esta ariations Naz olf-Ra v hab acquired an e WR ere debate Ho past elo hasta TS the in la tec the found galactic with mainly ´ ´ e, W h answ ıan binary 25 w existencia cit in estrella Gamen v com and masses. hniques AND ha 2 y arious ev exp Con 25 e groups region. 10 binary et binario y COLLIDING-WIND G. eac in la la v detectado sp er, HD for bined. er e un (R from high-resolution 12 are ected y ti in p ectroscopically v fec h Rau ears. not radial-v b CONCLUSIONS an W V) osible til system to et man deb lo instrumen et et 93162, data 1973), ha, detected. olf-Ra of to status w-resolution Its w de the w, 1994 der de the al. orbital rev al. errors, er een Although Li y extract 2 encon alta ´ in naturaleza binary ıa set v 1979). ` ege ealed y data R. elo Huc ab ariaciones 2006), with tensa y ears. to this at formar 1994 et of o cit H. excen sho and v tal solution trando h no 2006 Our differen e-men star WR obtained t y an Barb´ ob a the nature w emisi´ Previously sp monitored 2001) and configura- v single the obtaining ed y La sp ariations probable tricidad, ject parte ectra analysis (except lo 25, binaria orbital orbital ectra. tioned a, de radial v v on Plata cated 2006, t aria- aria- and, 1 w is has ob- the p v b de de 91 as of e- e- y a © 2008: Instituto de Astronomía, UNAM - Massive Stars: Fundamental Parameters and Circumstellar Interactions Ed. Paula Benaglia, Guillermo Bosch, & Cristina Cappa the al. sorption stars lution 75 an rio parameters 92 (a ing ations line allo exact companion and w p with suremen the the sp semi-amplitudes out phase sp they He Campanas, sisting around larger at roughly to emission a the R go help sp lo obtained osition V ere w most ectiv ectiv ectra  o d least 55 monitor eccen i After A W w d full to on WR 1999), 7 N lo i resulting resolution the is orbit, ed the ab had pleasan kno absorption e w agreemen M and orbital preliminary than a plot with giv iv narro ely ely Ma of determined probable out phase dataset us a

t obtained, eccen w great tric of confirming comp wn line, redder this . in line es errors. a mass λ eigh the y + 27 to (Figure the particulary They c.f. 4058 , star. WR a and with found large a this w in Ma high tly binary  2006. 21 conclude study solution factor tricit orbital p t similarit represen onen 1.0. 50 sho 3 and binary N data erio t t Rau y giv will M La surprised one wice 25 M lines ( emission issue. will iv p with W this impact K high-resolution w and 1973 are

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en and t , orbital d 1). strong The W ed e the Silla during w O system λ observing 2. b seeming the e (errors in binary probably of first for /K 4058 that e semiamplitude. e do to systems the et = p d remained y ting sho that our This R concerning WR could R analysed. and The erio noted ab published The b WR Vs P Observ 0 the published V deblend al. these on et . analyzed c p when out of line enough 56 emission solution king an = orbital of d the erio WR (Gamen w ) system 25. means April larger do most the WN 1996; the to een  turns gap “fill” 208.3 presen WR exp time 208 that in b wn and data d atories 0 WN e b minim 25 The w uncertain, . O eccen our WR elong 01; P in revised and sp e ected could The 2001, imp to da data, 25 solution, to  than the Sc presen =207.7 out that the star. the at orbit. in noted line He the w ectra, t ted et and in 0.5 w ys the preliminary h minimize as 25 measuring CASLEO, tricit the − ortan an um w o Although w most al. high to data to gap the i indicativ minim b 120 eic the N comp i b as a d. 10 although but deriv and This ratio do O ecause ts 80-da e b λ an that  O 2006). masses khardt obtaining clear iv y allo e Also, 5411 wn our solution, t But, with km stars filled R 0.1 WR km set mass massiv did star are at despite and WR O-t V orbital onen ed p λ um of GAMEN cated when y some mea- oin 4058 least v da data s con- s this e yp t gap Las ari- has not − the ab- the the the the p − us- so- w re- re- w b on 22 ys in et 1 of of of of ts ts e- 1 y o e e e ) , ET Sc Rau Rau Rau P Moffat, v Gamen, Con Bonanos, from 2005 ing line. our sp Fig. P emission 82 orbit the deblended The tion Could comp marks? an ollo ollo AL. h ectrum & w Magain, 1093 228, M On ti, X-ra w, w, w, the der 1. ephemeris eic c and star ( c onen colliding-wind W

k, as φ k P G. G., The G., khardt, the the A. . olf, ≡ Huc 206 systemic R., (Rau A. y T & some S., of sho A. a th 2008, 0 o domain due ts et F. He V . M. B. basis h refinemen WR et WN P Niemela, 11), Corcoran us answ Z., reux, ws t, al. ., of J. w i al. 1999, to i corrections T., K. & J., is RevMexAA corresp ho et 1978, λ 2004, and et WR 25 comp their 4541 2006, Ro er of v brigh w A. al. Sc J.-M., on & REFERENCES elo is al. A&A, the the c this, hm Ma V. theories 2001, Corcoran, ho 2004, v 20a. JD t A&A, cit A&A, absorption extreme ariable. onen (2006) ter onds A&A, of wicz, utz, y S., 2004; lines y existing , 2 Gosset, w 2006 the and 347, & 452 NewA at ha ApJ, e (SC), t Their W., 68, 420, from to W K. v need 460, in (c.f. p Bonanos newly e 843 found orbital alb ( the 127 WR eriastron M. 41 φ a 1996, Stahl, 611, to WR line 9 XMM-Newton E., Rev., 33, ≡ orn, b p 777 masses whic F. Rau an use oth eriastron b 25 0 observ e 65 33 . Hutsem determined A&A, 2006, 97). that radial 25 N. orbital O., made w comp w 45, of h et as R. as according 2008). break an The are Szeifert, 135 ed brigh al. the A&A, 1979, 306, onen v predicted ´ ek emission concern- elo passage. on inclina- ers, 83 b 2004). cities. X-ra ottom April, ter those ts data, 771 ApJ, SB2 445, and are D., T., to in y © 2008: Instituto de Astronomía, UNAM - Massive Stars: Fundamental Parameters and Circumstellar Interactions Ed. Paula Benaglia, Guillermo Bosch, & Cristina Cappa corresp latter a images, together. eccen G. higher in indicator These R. G. N. imp near R. sa ob line P. lines R. where A. has (w stellar WR it stars N. ev for core, y hard en is e!) jects: WR Moffat Massey Gamen Gamen Walb Gamen Walb R R the ortan an b v 25 auw alw auw future, do. more tric alue? een compared A1 will ything correctly 4 first in ev onds sp primary 25 in orn orn a un stars HD t (eclipsan olution. ys - sitting - than SB2 the ectrum. - The the go to til to MISSING extreme - - Y - - Congratulations recognized, a - - including to W W ou A Did 93162 ab searc expanding bac The sho no I constitute go t with galaxy e e the motiv v w sho inferred out to this of w. ery see ha o on w k ould y d t, narro h The ou Ho Balmer R the v w and (WR directly (higher an high-qualit the en’t idea V these P massiv for momen ed ation 145, w an set is =3.77 lik a 3 ev O Carina w including w, the He optical to photometric a atmosphere. done e sligh a der that er, e 25) the main-sequence lines, masses to single absorption symetrical, w sequence e, R examine i luminosit t v that on as lines? there d, ery Huc with emphasize tly single-star 145 w γ an differen y e Nebula fine a L eclipses, v i.e. y FER nice elo only fain sp h x they CWR of in the t consideration nev w ∼ ectrum, collab cit He has these eak o 30 of ter y follo v OS L t results lines, measured er , no y er unshifted mo i x en is indep Doradus higher ORBIT in WNLh of that emission λ quoted wind v w had of 100 companion. sp v w v orativ ery 4471, the terpretation (then elop e the protot ectra WR whic b up. with enden for y b this M brief most mass mass). een e O analogy e AL

b spread a the do h the N ab 25!) dev (LMC) ecome w yp of lines, star is the are WN+O4f displa iv ork t in an out ?? loss. p e SOLUTION WR DISCUSSION elopmen not N detection groups o y λ WR and O2If* indicated. emission?It Finally w These iv to with 4058 of nicely the out evidence and with erful, wider y just that WR 25 emission that the a C 22. systemic in man strong for HD w selectiv t star ( t another , wide WR I P yp the 25 ork X-ra at nearb the near of of NGC men =9 some y e 92340 for is similar the HD the rough observ on F on 22, Carina ys. is line. companions v also d, p tioned e OR y elo a v 3603 eriastron, imp secondary emission the N 5 WR the elo 93129A. lab L in companion Ha cit (WR y iv x the Of WR atories! p cit ears, mass ortan whic oratory v same ≥ y eriastron!) basis Nebula. also star, v y e y course, gradien alue, esterda second 4 y 22), of h 25 ou times t unable and line con In but thing. do of the the but to star I’d measured or for HD addition, tains from Moffat’s not y do t W is luminosit w most they O emission , a just did L in e in e that a although and to 93131 x k that star. will I no affect ey suc b the either of 3 y get do lik etter am X-ra ou w WNLh v ob h purp WR e do erify to the He sp not W ha there sp y a (WR also to use ject and . y the ectra e photospheric v an close clear radial ectra i R WR men ose, luminous e i 25). Balmer deblend ha y the lines. to preliminary impressed 145 extensiv WNh stars our absorption are v 24) e tion dissipation, p the understand where 22 and F a v to erio do results. or v 3 elo with erage Can in is absorption ev do issue. that luminous es as hence the d. cities WR also e its olution the app w that. study strong and But y ho ell former O. absorption v ou lines results star, Of ery an w ear It originate O3 or as Sc v massiv but already no similar elo is course (80 in whic direct hn WNL dense He to mo lines. w stars lines with also cit and the the urr for 93 b he d) v I h y e e e I