© Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México R Morelia, Nacional the they cen and kno lengths and Barlo classic evista 2 1 tly Since Univ Cen wn ultra c homogeneous hemical can w , tro w massiv ersidad Mic electron (1975), Mexic Aut´ through ork violet winds b de hoac´ e onoma of studied Radioastronom comp Cyg observ estos traba results p densities, en Key duran para assumptions jetos desviaciones p there parameters and on of v ana e an, ariations Mic P osibles ossess 1. from radiation it the anagia the la temp their VER de M INTR w hoacana de WR Wor OB2 flo osition. cada jo cuy sup te ob ´ El The as exico. exist ado M winds winds assumption hot for ws observ Astr winds ´ exico, presen erature, jetos asimetr la p mo ds: o free-free osici´ 147 & sizes, ODUCTION Y ossible No. in classical y massiv with uno 3 vien ob ultima ´ onom from delo allo ´ F ıa de ST P — deriv confirman of brigh ha the w LAR In on Morelia, elli ationally p that jects (WN8h+B0.5V). tamos 12 R ere y CYGNI, oseen to de v w these ARS: ´ San sp ıas, ST this constan e e de ´ est´ Astrof ıa (1975) flux c to amos degree e M. the (B5Ie, ectral t emission. eive us no treated of deviate b ellos. d ARS: mo whose GE andar y sources: un inhomogeneidades een ´ obtain ecada Nicol´ w E. a Mic resultados hot to vien Astr densities. se underlying d a ´ del ısica, EARL stationary y el vien FR at un t 2003 Con , and hoac´ are questioned indices as analyze comp LBV?) of ARRA Estos massiv based tos v tama of W for wind radio from para as comp elo estas a to OM de ´ Univ ısic ionized treras, an, ionization W OLF-RA P Un v Octob isotropic que Y-TYPE cit free-free orta estacionario, alue righ no, ˜ Hidalgo, a Cyg M the par´ on la These b ersidad and e til y ortamien These para , w y sup , p ´ exico. eha star, 40 MASSIVE stars. se a isotropic Y and ossible 1 WR emisi´ t el ABSTRA the ametros er v for re- como RESUMEN basic b in osiciones G. e- & (B1Ia, , mass vior y ´ desv ındice OBSER tres 53–60 OB2 13; emission YET hot y features the Mon 147 on — v assumptions. ´ to ıan deviates lo ac ariaciones asymmetries, loss fuen massiv libre-libre and last LBV), isotr´ NO. esp distin tes, nos c (WN8h+B0.5V). the 1998; 2002). emission ev of w Cherepashc ual Radio sumptions tions. b firm (2004) CT ST predice epte de een ell han er, tes rates ectral material 1,2 ARS: homogeneous confirm The from V decade. opico mass p blobs lo d evidence (1981), ST 12) to ermiten studied, e A since brillan from F. sido observ Cyg 2004 Con esp ob TIONS In al for en ARS el existence ionized y P — loss de lines y jects INDIVIDUAL erado. cl´ (Moffat . W w treras the mo la the OB2 cuestionadas. la h eac the the inhomogeneities Wilkin January homog asico ere tes: mo who uc ations vien e In ST for tasa rate b detectar densidad delo ha h k oth optical w are ving ha nonclassical standard not this ARS: v stellar No. tos deviations ork of (1990) wind. P found Se en e v & Rep OF M ´ de eneo. 1 e of observ & seem est´ obtained the ˙ v Cyg suggested ionizados alid, ha w estos with 22 of b Ro 12 from p Rob ortamos andar. p ork, een ´ erdida region, la MASS de ossible targets. Ho Abb winds WINDS that dr rep studied (B5Ie, to (B1Ia, Sin ationally mo v presencia ´ ıguez ert w vien Existen the flujo. rep arious radio detect ortado w from (WR147, ev ott, b del, radio e in and em eha orted de er, 1994). is En tos. to p se wind presen el inhomogeneities LBV?) some LOSS LBV), bargo, eaks the These Bieging, based 1999; these Estas observ viour masa these authors since basa time flujo (marginally) represen este flux que and ob- de to discrepancy (Skinner t cases sup basic Theoretically theoretically ations. Exter erp ha & t these v assump- Ch osed individ- e found et et blobs Ho urc has b as- on al. al. w- 53 h- e- . , © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México viations. rep in t 54 it with geneities ing WR loss b v that a emission 1997). that the sources: rate. rates mal an et the sev b a cal surface can et b w y ations erger et y binary v a een . 3 al. the Asso asymmetric al. Note. ery eral w orted Cyg P Source WR WR W V The The wind stellar b with wind. the rates, V as een He 147, these ariable e Ho Cyg e 1990, are ery the 1981; form ciated go due This 2002). m National presen ev hot National OB2 147 147 − at study w concluded system, the P lines mo uc can o a making firm usually In en ev exp Decon d Large v Th w winds 0.7, Cyg to h ariations 1994; S N stationary massiv er, v of del e Univ example t radio No. this in Con ariabilit as explain w us, ected the t migh should of blobs. evidence o stellar the the Radio 3.5, 2. Science t 80% , v is ersities w 12 where stellar treras the olv in Cyg pap Arra (Girard the Luehrs orbital deriv o v OBSER e emission v t that absence ery and ed order ariabilit and sets stars of b main are y er this Astronom of 0 WR 0.06 wind tak In 0 OB2 y e F size . ed suggests wind. . the there Inc. 06 [arcsec][deg] imp θ 04 winds, oundation. et explained w the a 0 a of (VLA) due fact, 6 e sw of 1997; . e discrepancy to × 7 & assuming non-classical V × × including star assumptions errors mo al. mass in cm in ortan under presen No. eeping · cm A an observ observ of 0 y has 0 · 0.05(22) determine Willson to is to . TIONS . · rotation. 03 y (P in del 03(32) Williams It 1996; in the an of of Georgiev asymmetric Observ a that accoun 12, A) of the trinsic b (42) t of are co has c this t including een in three b ations ed b hanging of optical the op y and new CONTRERAS, teraction ecause the observ a ∼ P w Williams erativ this 1987; X-ra the b atory detected binary e and classical SOUR wind t 0. een Cyg 0.37 0 0 In reliable 0.25 v wind of 00 are et WR brigh . p . VLA ariabilit NRA 01. & 13 19 presence tak [arcsec][deg] in θ ossible y e the v the 3 ed al. suggested is mass mass ariabilit prop teraction Williams . not Ko agreemen × × × luminos- 6 could × (Abb inhomo- wind en op 147. CE source. t surface system cm optical 0.21(120) O 0 0 case (1997) 0.30(110) classi- obser- enigs- . . et erated radio mass 12(103) ther- deal- 13(160) 3 from (P with osed y loss loss SIZES de- ott A) al. on b T in of of of y e t ABLE MONTES, a AND 0 0.46 0.49 0 . 6 2005+403 configuration ∼ 1999 1328+307 F hours observ ∼ During densities and observ tiv the a opacit flux sizes Astronomical in zenith follo terminal soft calibrating sume data order 2D-Gaussian pure BUST w F ha 1 . 24 [arcsec][deg] 22 or or eigh θ small tegrated cm. v 0. ely 6 1 × × Data CLEANed e w × × 00 second the w cm P densit FLUXES 2.54 2 & hour 0.35(163) are 0 uniform used (T t 0 ed w June 0.21(93) y to . to ed, ed. and During (P for . optical 12(176) and Cyg b = 19(29) eigh WILKIN correction the able dep first et A)  ha of for v obtain standard while 0, w the y and for elo 0 The the reduction for flux and and v ting ∼ first endence run . een 28 and the 03 of e 2) season, 2005+403 Figures cit fit w 0. giving b depth eac minimized 2015+371: second. AIPS 0137+331 1.99 maps 00 Image eigh total oth and densities mJy imaging. for Natural y during only 2015+371 observing 4 NRA 36.6 Cyg sc to flux 9.0 9.7 h S v for for [mJy] hemes 0  alues ting all · ep source the . of 7   · VLA Septem the of 0 on-source  at IMFIT angular 2005+403 · w O. atmospheric 1 OB2 densities o eac cm . 1 2 w 2 01 sources. the ere c . . the Pro τ w . 5 1 source, and w Amplitude 0.7, hs as and 2 observ A h (T ere: w A = and as the at according 1.35 run t ere ap cessing t for the second w pro obtained No. on able 0.1. b 24.5 preferred 0.7 3.6 Uniform p 5.9 8.0 9.3 3.5 2), 3.6, a pro er erture S resolutions exp phase v erformed 1.18 [mJy]  all cedures 3 the tak arra ed elength, eac in . and w 12, w cm, 6  Distances   0 cm cedure. In 1) 3  while and tegration . e ected and cm as 0 0 0 three 09 en  b 0 h only . . . at first y this . ha 1 2 and 2 o System calibrators 0 1 w an efficiency calibrators w source observ otstrapp . w observing at to using from as w 6 06, v e (Figure 6 0.7, as e for as WR in ha trop sources w 22.1 10.8 cm resp for run 0.7 decon 4.2 6.0 obtained. cm, the Based determined using of a termediate in 2.01 [mJy] S used v y and WR the 6 ed time e 3.6, ,   differen cm. sizes w ospheric ectiv ∼ the  147  and editing, cm w applied (AIPS) using . resp source. ed 0 0 e  v 0 0 and 3). e . . 0. olv . . (R 1 1 liter- wind 0 2 w w w ha 2 on run. 147, 00 “A” pre- flux and w w . F ely the ere 02, ere ere 1.5 05, ec- w O- ed v In as as or a a a e e t . © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México 60 IMA at ature Fig. of S-E. are times with magnitude. but and mass-loss tries WR WR Cyg P Source P µ 0.7 not Cyg Jy 1. GR they W Cyg Both the or

50 © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México OB2 147 147 (Con cm. VLA b righ DECLINATION (B1950) DECLINATION (B1950) corrected eam 37 5237.0 41 0415.0 inhomogeneities with w µ relation are rates w 20 1556.65 N S e 11.5 12.0 12.5 13.0 13.5 14.0 14.5 33.5 34.0 34.5 35.0 35.5 36.0 36.5 Jy t 20 3053.35 Con No. treras eak maps − DERIVED can & 1 an b exp at eam tours Barlo 12 emission for see 56.60 in 53.30 6 of ected for deriv et α termediate 0.26 0.25 0.12 − cm, eac P a 0 1 56.55 . w for 53.25 7 T al. (B1950) p the Cyg and − · h ABLE ossible −   ·  ed (1975), 3 · to 56.50 P regions Cyg . ob 3,3,4,8,12,16,30,40,60,80 0 0 0 1996); 6 53.20 ARAMETERS effects (e.g., . . . and − cm 10 04 13 b Cyg OB2No.12 ject b y 3,3,4,5,6,7,8 56.45 e 53.15 OB2 data − blob P 2 Cyg 0.63 0.18 0.50 correct P Cyg α 0.25 (T anagia allo are Skinner 56.40 these 6 cm 6 cm 53.10 3 of . able 6 No. OB2 w to −  IONIZED   w ∼ p 56.35  6 eigh 53.05 ed 0 0 0 ossible the 0 3 cm . . . 06 02 05 12 data, to . 2). & − 04 No. © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México times us t et N-E 4 are (R F an [10 Our σ to elli 12 M 2.7 1.0 0.5 al. 20 1556.65 OBUST=0). asymme- ˙ ab 20 3053.35 together − order − 0 · in 0.6 at deriv WINDS    . 5 · 7 (1975) o 3,3,4,6,8,10, 1998), v · M 1.0 0.4 0.2 v the times alues all cm e mJy

56.60 the 53.30 ed ] observ of wind, 70 b 56.55 corresp 53.25 OF RIGHT ASCENSION(B1950) eam µ ed Con as 56.50 Jy 53.20 MASSIVE − 20,40,60,80 kind (1998) mined from ha able found the flux our creased v ters 1996). the early sities observ da w Cyg OB2No.12 w 1 b ariations tours onding a 56.45 ell eam at 53.15 v ys. v This e elengths. first 2D observ (ionization P Cyg densit c as 6, of 3.6 cm 3.6 cm b their with 56.40 hanges 1980’s − 53.10 ed that een for flux Sev 3.6, 1 Gaussian one in b b time map B1 at eha y 56.35 on 53.05 P ed their times ST previous eral y are 1995 prop 3.6 ∼ and in densities , Ia P vior Cyg All when a © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México with noise. in v ARS 3.1 b 70%, the star ariable cm time Cyg as explanations eha 41 0413.4 37 5235.4 0.7 degree, osed, the maps 20 1556.53 long-term . v 60 has fits. are alues Cyg 12.9 13.0 13.1 13.2 13.3 34.8 34.9 35.0 35.1 35.2 35.3 and large vior. v has cm, P Abb ∼ µ ones, ariations 3. sp sho scale 20 3053.23 Jy − at b Cyg w radio but Comparing − 35%, OB2 ectral RESUL een 3,3,4,6,8,10,15,20,40,60,80 b resp ere ws ott (Con 56.52 wind 3,3,4,5,6 as b 0.7, een In eam w probably (B1Ia, none obtained observ ∼ e ectiv imp No. et deep this emission. and 53.22 studied RIGHT ASCENSION(B1950) 56.51 treras 3.6, found related indices v − of 50% al. TS elo 1 ortan 12 ely , times of w 20 ∼ 53.21 and − cit ed 56.50 radio (1981) LBV) Cyg OB2No.12 ork these . map 3,3,6,10,20,40,60,70 them 34%, that without using et − In as y in b (Con to t , y 6 50% 0.7 53.20 Radio al. w mass-loss 56.49 the c radio P Cyg 0.7 cm short at wind Skinner hanges cm, study new e they 0.7 cm resp AIPS rep mJy seems 1996). treras 6 ha 3.6 frequen 53.19 56.48 cm, consider- v based orted flux since emission as parame- ha ectiv . e cm b routine eam deter- v to in a They to et times et rate) e This den- map few ely the de- the for tly its al. on al. 55 − fit 1 , © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México found tinct emitting the 10 Fig. 56 − in dex altered star, sp b Skinner mal sp one lengths the one p abilit at of are (2001) serv to cen 6 seems again lations Genderen, lengths eha o 3,3,4,6,8, termediate cm ectral ectral 00 orly these 0.7 c tly Regarding Regarding hanges ed star, observing outer in v 2. wind. can close vior y arying regions is maps, , the to t cm radius) in correlated has long-term w ha VLA that b © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México almost sample b et regions index, new y o index, ha exp seems is eing v

the DECLINATION (B1950) prop region to the o 10,15,20 differen 40 1041 e The Sterk al. b v in consisten curring P data sho with e een CLEANed describ ect around studies, zero. 20 3454.1 outer 35 36 37 38 39 40 a (1998) decrease Cyg sp a morphology the osed more presen coming 0 to flat wn to non-isotropic differen coming en, observ rapid ectral . that w of 7 optical or a t the eigh b wind times − undergo in ed v in completely explanations & regions e (T the In en t ob alues P ts 3 prop the it south 54.0 flux Fig. t de able . with the tirely c v maps from 6 ed indices, Cyg: viously of t a our (R hange arious from w parameters. 0.6 cm photometric regions Gro sp the opp ould osed, at OBUST=0). , corresp inner 1. es densit RIGHT ASCENSION(B1950) 53.9 2) of w of the ectral mJy case regions sp of uncorrelated. the other ot e 0.7 osite: wind whic a In the the while in ectral t b WR presen elongated Skinner differen since sho yp 0.6 region (2002) e 53.8 region, inner b these cm y men in the the WR onding eam h index useful es wind. w at ws c CONTRERAS, v 147 the farther the could hanges flux a alue the of index tioned differen t v sp all wind studies 53.7 − Th WR 147 star. a region Con elengths. t maps, closer and 1 0.7, at 0 et ectral , but of time-scale), sp three us, . densit 3 6 cm to at Wind to 7 for at . b 0.7 tours al. 6 ectral Then, 53.6 0.8 − has out e 6 emission de examine 3.6, t ab ma − in not t w 0.7 related a (ab and b 3 P (1998) to and w w o . y index Jager (eac o y while oscil- 6 ther- 6 y from b v view . are v a a Cyg 53.5 and dis- v Re- ari- een out the ob- e. v v cm cm cm in- As w 0.7 an b 6 e- e- h e e © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México − MONTES, cm. 3,3,4,6,8,10,15,20,40,80,100,150,200 cm, 40 1038.0 20 3453.89 Maps resp 37.0 37.1 37.2 37.3 37.4 37.5 37.6 37.7 37.8 37.9 y the asymmetric 1 1998. sults p emission one. 0.7 et somewhat wind more lar the where observ inner ∼ ula can ten termediate emission ing NE men denser from is et ortan − more 16 al. ectiv 53.88 ths wind The to to of w cm tary 1999 around hardly 3 error, & − ere the P (1996), of detailed is nebula × P ed Since its b t 53.87 90 than ely of 18 WILKIN Cygni’s also e ob flux Skinner decrease Cyg. deriv 10 source. obtained 00 at at cen . wind con ma 00 explained. mass-loss an . 53.86 vious − In lo in and see scale a v the Although structure 5 P our inhomogeneous. tral RIGHT ASCENSION(B1950) jor/minor w tamination densit is arious arcsec (as ed 4 the 53.85 study This diameter er M σ asymmetry Cyg still what surrounding -lev in wind t also

Moreo et star, defined mass-loss w 6 53.84 b than using in our y et o inhomogeneit cm yr consisten al. el rate scales: in b is 1999), w v 53.83 to could − ecause consisten and surrounding alues of whic in een map 1 3.6 diameter, v (1998), v 0.7 cm WR 147 axis AIPS that and er, ery a a 53.82 rep (whic b is our v y small asso cm oid h the is they w b rate a lo it ratio times w an Skinner orted 53.81 wind, the t inhomogeneous indicates rep e e routine 0.7 w consisten ere compact with map. is h ciated can emission p er t cen who outer 53.80 orted ossible radio condensation found y not for sho and with is obtained an 70 than tral is evidence b see the that 2 y w found Here µ ab IMA et inner P surprising nebula (T nebula 6 ed Jy v Skinner t that t b compact w core core that out ariabilit the al. the Cyg cm able non-thermal y v with from o b GR alue a w eam fain Con 1998) nebula a using 0. e v at maps of v previous the of and 00 2). ery extend- alue sligh , with can or require 6 the t within a − a to an treras a et while y 1 a small blob blob neb- stel- that The w fila- few and has im- the the the the see tly re- in- w al. an a of of y e © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México thermal southern (Con v In new 28, from 24.9 maps presence all emission fine 1990; asymmetric that (W WR+OB of gion denser OB2 but that 6 tio its (Fig. Cyg ho a sho fluxes VLA source 3.6, T sian tiv tral index Our has (1996), v ariable alue able spherical cm w a ely w C7d+O4-5) this wn angular Individual This V Maps of ev decreased  structure. indices 1999) homogeneous rather and a 0.7, at OB2 to treras flux ariable this fit , No. 1). the v for observ 0.1 w has 2 er, emission Doughert ha 1. elengths, while than in (Setia 6 e the b 3.2 (T w to v v 3.6, radio a cm ecoming radiation can 6 dep of F protub ork, 12 The densities radio ery at W e decreased Figs. colliding at No. mJy able rom thermal . 3.3 and cm south. the & decreased wind sho size to olf-Ra a ations its radio Cyg wind, the deviates ends 6 its and see the in . wind Ro from Guna flux 12 flux c w ws cm emission flux 1). surroundings. a teresting do WR hange y source. 1 comp for is 20.2 whic erance e at 6 source b dr OB2 at 2D 6 do et emission and y es more on three oth cm presen wind. F a The ´ its also wind its et(WR) v the cm w ıguez all densit that wind (north w urthermore, in densities. es to 0.7 ariations the  147 al. h ere kind not Gaussian an onen densit from teraction b 0.3 flux as comp shap No. 2. is shap three data a not y has could con sho arc consisten and 2003). rep of (WN8h+B0.5V) observing rather as obtained not t These et system first w ∼ 1999; y ha binaries t Based mJy of ell. maps het has 12 has 0.6, the a tour sho w e e y radio v 60% orted onen v w star, al. (Figs. (WR alues 3.6 the w ma e w as enhanced is ell b some Th ha yp (B5Ie, a w observing The ould Both b a e fit, standard while increased v W flat 2003), region fluxes It jor-to-minor for ob map een S v ts cm if case. elengths; is e and explained us, an as t on smo obtained e and b atson comp of star) IONIZED 2 viously the from ∝ clearly for w with y and one (Williams y 3 caused v w v rep b inhomogeneities the and the (Figs. e its . alue Con 0.7 ariation whic the ∼ n oth 6 a sho LBV?) deviation e ha emitting Since WR v source e 2 are curving − and of some orted onen elengths elongated , 18%, morphology emission et sho the wind a v 3). ws and second treras 0 assumption w 6 b of h o run e the . sho 2D it y 7 v elongated e al. 1 sho the cm from as ws 147S obtained al WR our − 0.3 that classical free-free t). In prop ∼ axis WINDS of and is for resp 3.6 had ws at of kno 3 a 2002). wn Gaus- et shap (June index  . time- these sp et a 12%. their clear from 6 non- blob Cyg new w this 0.7, 0.1. run 140 our the the are are ose wn cm cm ra- ec- ec- re- 2); Its al. an al. a at in y e , OF MASSIVE can b densities (Septem data data that with ence sion. ond angular sisten pro b of eate 9.2 cm, tia (T terial in observ the for (2002) north (northern flux ha its et the though 3.6 using the 147S its pap As Con v flux et w gated treras et tion in ations e oth as terv able v al. WR al. al. the  v made 1996 1996 the Morphologically Guna e discussed cm er treras presen cause 3.6 southern whic e densit v clearly 0.1 run, w of of flux and sets. the (1997) for t ariations remained A al radio (2002) the (2001) comp MERLIN inside rep in ations eak & wind at 1), with v flux 147S. inhomogeneities w WR w cm b precise of resolution. ariations mJy h w v v Ro the obtained measuring e 1995 e er orts b the WR measured alue. alues. resp densit quite t y comp an ST & emissions, w ∼ traces ecause Although confirm . still onen dr densit asymmetric. flux comp w e 3, and the of the 147S sho As E-W Ro ARS 3 find of same and Therefore, ork et b ´ source, ıguez cannot an ectiv 147N, y observ 1999). v yr. WR comparison onen constan random do dr y alue w t Williams This W al. data 1998 the densit wind, Con increase Th onen the of finds in ed y v ´ 8.4 ıguez those v atson from v direction, On ely w ariabilit not , ariabilit that 2001). ariabilit sho (1999) flux us, Ho the the 147S v t) and a are that  treras (Con esp ed the the ariation outer see . v v are flux and ts F the y ariation 0.4 elength. w ws app a cannot t, find or the its system, (1999). v densities, In radio asymmetric. at data the in ev et ecially w of (Williams fitting ariations an decrease With com smaller of at high while treras et within e rep a mJy other WR again er, Although ears found y al. 3.6 the 3.6 y T regions. y WR y concatenation & of ha an the decrease northern 6 able at the al. bined orted has significan prop rep w flux this (2002) v cm Ro y our cm, y wind cm our confirms ere 147N e for resolution ob the Th 6 radio the from Ho et purp hand, (1997) clear 147N, et the dimensions orted no dr used the than and b viously they 1 b in osed at us, in new 6 w flux b whic the ´ tak een oth b ıguez new al. one data et northern w clear e ev cm y of Setia oses. the sho the 6 ha of our Ho flux emission error, source e it asymmetry observ 21 en the W the er, t previously 1996) al. help cm, first ours compared the v sources, h v rep densit b to and ∼ presen ma w VLA flux v c alue e the atson y radio same do new k cm (1999), ariation traces elongation at elongated. ev this v of 14% 1997; suggested com WR the Guna ed MERLIN orted y alues Williams the WR W to and er, b o W not the ed a deriv b sugges- is densit for cannot is v ecause y e source region v obser- e t delin- south latter bined er atson emis- lo while radio et alues pres- elon- Con- 147S from note that ma con- at WR w star ma- flux sec- t w im- the are Se- w for al- an b al. an ed 57 to er in in y y y o 6 © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México they et at the sho clear − P sion maps 1999, Based rep three Fig. 58 part gion gested MERLIN, b has Giv directly to detect, densations e 3,3,4,5,6,8,10,12,20,30,60,100,150,200,250 al. differen Cyg’s the a ort w en WR not 3. structures at clump resolv at that (2002) radio w observ and South the on b the e at b 6 star y the to VLA een wind, can t cm Setia b w MERLIN a inclination w e decon in high the oth emission as en ed and e ha 3-4 N-E out detected at see (Fig. the tering CLEANed suggest obtained v w are but radio σ south Guna e 3.6 a resolution v a a extended southern found

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This a o -2.0 and t that north-south blobs What (2002) indices of p the Based w indices tak ossesses W p emission, b e (1999), clump R osition flux e eha they en exp do w OBUST=-1. of observ sho is ell ha vior on emission in are not ected v most w for v ariabilit seem with in e a based as June these a preferen ed, can sho suggested, exp whic the negativ the set those v surprising alue to an wn then ect of b S-W and to southern v h on y e y alues, lie Con fitting is at explained rep the in them tial for e of data it consisten Septem almost direction, index all tours T orted the the a south ma outflo able w classi- curv ab w tak to e com- y WR a t can out b v are w in- b b b en in es er e- 2. of w if y o e e t © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México assumption to greater the (2003) in of ters consisten will the latter under & b Raga c colliding with Although system. ratio b (1996) our northeastern adopt the jection ing to v This the ing with η tion, resp sev Williams the nation WR distance tion p view R This obtained hrotron ariations, y , o eak ◦ w w Ro P the eral agreemen Con the W from a stagnation stars. brigh wind e onds collision new normal neglect of of sho 147S, of ratio emission the new dr e but a the non-axisymmetric then = et b the the treras inclination to the for ha metho ´ p eing radio the v ıguez momen than b 3.4 c alues oin and 1350 t D al. maps, winds test est k the In north v to et from collision system. is repro assumption our exact v e calculated , the within . is Considering as t alue wings t t, 0. w the sho is inhomogeneities t 1997). and previously al. also w Fitting order the 00 thermal surface wing fit orbital indep & source d o 1999). part morphology w 556 o with and of φ of yr v tum w p collision duce the describ stars, ell (Raga c (1997). w alid Ro angle stars, oin solutions of estern k of stagnation = the WR supp φ e (v are  error. app as angle has of dr v enden to no t. measure η φ In (Fig. loss 30 ratio an elo that the Along b ´ of the sp 0. ıguez stagnation and Giv emission. the the the 0. w differs If ecause 147N ◦ 00 b orted of apply ears obtained = et ed the 00 our cit t eeds. 020. der fitted et wing the w an 635 rates WR surface, curv the W morphology rederiv steady t en observ of al. w 30 pro o y orbital 3). used b R wind the Our of e of y of to (1999) een winds the estimated fit, ◦ fundamen ◦ is Huc the corresp w  the stars obtain p b 1997). /D e Wilkin Can its . 147 jected an from and wind A of b the a eak η y Reasonable oin WR The plane 0. greatest is e , , the revised b e ed colliding line 00 w collision Our Th h sim for thin and impro the isotropic p more y analytic p 020 and t t´ er = motion t e in parameters Bow angle o, are osition collide oin p of IONIZED 5 us, is the Doughert symmetry 2002), observ 147N onds sp assume ulated ossible sho η Giv 15 wind, η . assumption joining go (1997) Raga, of the b GHz 0.01, w t shell 1 in tal apply eeds separated Although = w o op v / ◦ orbital o Sho as is a c one w 2 tuitiv ed the en v at ould d at k / ≤ 0 angle alue surface en, wind to of parameters lo at head-on (1 tak (Con ed . relativ winds: mo sho surface agreemen ck fits radio but 02 the η a qualit mo images this are mass w whic & φ (see the the obtained sky that the the distance + suggest- y v er en e, ma del, b WINDS separa-  c for Wilkin ≤ alue del is axis p to k, mo e is φ treras η . et latter m erio since stag- h driv- lo 0 limit from y , also, 1 ana- b that e syn- pro- cen- 30 y 40 also cor- still loss . uc / the the W the the the the y ca- del 01. for for w w 2 al. b to at of of of of ◦ ◦ ). h d a e e e e t , . 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M.E.C, commen from Ciencias thank Program w ort o theoretical o o w Stapp a constrain non-classical e all this orted c All In W structure. ed inclination man same k a a w non-spherical the ed mo sho for in onen DGAP the e has φ of b region this fain observ higher a W Our giv line v v teresting the e of ys w thank of ariable ariations. dels previously ts a F.P y ers c e observ the the a ork, the B´ based for ks en surrounding b wind t north-south t direction confirm ST 30 our free w asicas from b clump emission. een on new emission and .W., NSF-In using A-P 2002). deriv a y ma suc the − +10 ed (Wilkin financial (north first WR ARS b wind y suggestion w 15 , Con o observ Luis sev This ed angle parameters source, rep y w e h our API on inhomogeneous. b wind w b winds. binary presen degrees the and ed eha est b a detect a (40864-F). crossing time sho eral elongation our star. treras 4. that v orted e momen W ternational but high source Ho mo new elengths from IT radio and generated F. v vior p fitting e of SUMMAR ed standard c 2000), source. ariabilit G.M. eak supp w preferen k wind new del found t b v systems. (IN107202) that is at ev the Ro ersions curv oth VLA angular P of ob t whic These maps at p observ & w of er, comp tum still lo with osition a at this ort. dr o Cyg jects to W VLA orbit. high Ro curv thank cated lo material. in Cyg e these ´ suc and ıguez p it is h F.P y atson that 6 WR w data attempt tial ossible to consisten for dr ratio, (see zone. its giv ations onen additional Researc due w mo er Y has blobs h cm deviates e of A ´ Additionally .W. are ıguez resolution angular ould the data. in OB2 as to corresp non-axisymmetric es resolution radio mo outflo del: Cyg financial highly 147 three confirm and for Gaensler, the et to t) b and its a η the clear those W northern een also dels of clumps , are b seems a lo al. (1999). Th hers No. is a than e e his t OB2 CONA morphologi- w man spatially flux w its blob These N-E, w onds ha in in in unique within resolution. structured one previously us, er (2002) kinematic almost wishes axis. in e examples teresting teresting rep the v observ 12 v supp wind at tro uscript. limit the suggest F e densit aluable w , to No. denser w Jones, in ello of whic it e fitted CyT- to orted radio is e least duce This data non- p The still one is the the the ort os- so- re- re- re- ws an an 12 59 to to a- in is h y a © Copyright 2004: Instituto de Astronomía, Universidad Nacional Autónoma de México Exter, Con Gaensler, Con Doughert Cherepashc Georgiev, Girard, Can Raga, de P Abb Luehrs, 60 Ma. Moffat, anagia, Jager, 409, quez, Ser. 2002, R. eds. 2000: Sterk ApJ, ASP), ApJ, (m.con trof treras, treras, t´ ott, o, Eugenia A. F., K. J., ´ ısica, A. V T., S. A. 217 en D. 580, 250, y A. N.,& MNRAS, 400 ol. C., B. M., Williams, 393 C. , L., Raga, 1997, M. treras;g.mon M. F. h F. 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