© Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México R example, the ies. can Ra ha to this brigh motions evista v y detect In The e et analysis mission b Some ter measured e this obtained Hipparcos Mexic than of b at pap y ob with 118,218 of and obscuration radio jects estudiadas con Los son est la sistema nar tiemp Arra their arc de T prop within b motions with sup Key binary 12.5. ana er y radio o 1. RADIO prop m ´ e hiv radio una w in Hipparcos erno v accurately sus mo INTR v ellos, uestra, de y estacionaria er Wor e erify satellite w arias resp prop that F o Presen W man e de presen er a ain vimien motions noise, data. system remanen Astr stars del of v mo v e binario con for a ds: elengths seis motions ect ter ODUCTION six er presen den y the are Univ remnan vimien v or orden p onom y tin eces cases WR tamos or motions. t PR obtained estrellas W stars to with tos tro with encon large and the metho fain uum formed for Hipparcos ersidad determined olf-Ra se te R its t ´ m´ en propios ıa 145a tos de del OPER e these and t. form´ from analysis t the de c w the w as those el tramos distances) visual eive lo emission y in ere su 10 e Cen d, propios. ruido y an´ cal sup Astr W precisos T rep accurate analysis et prop b = o first the marco d Nacional a previous ypically ob not w y alisis olf-Ra — p tro of erno de stars 20 standard 2008 Cyg e ort or direct of y jects magnitudes of S. que visible b radio MOTIONS er observ included ´ studied Hipparcos. time ısic WR a rep de y colapso that six nos. ˜ v their de Dzib T y are motions us de X-3 with a. que July et los a , ´ Radioastronom of prop ortamos do ıpicamen , collapse observ W these 145a Aut´ are stud- con rep from ha con acional. easy 45 P observ (for mo ABSTRA not are olf- of and los prop RESUMEN radio b ara 2; v er , tin directo a oso onoma y WR e vimien emisi´ 3–12 rest = few ac observ consisten determinados aciones uum: L. v The er Cyg sus te, lo c ations erificar emission, of epte 140 times F. cal and motions Las on (2009) OF estas a de de tos additional for parcos. and fiv c b determination the V though prop mo CT other ations X-3 hec Ro stars d een de ery massiv y ´ ıa in e tomadas una M otras suggest vimien 2008 t tak The the propios sugieren more dr el k W radio, y stars their er y ´ exico, son observ with the ears, Large observ ´ the ıguez m fiv — with en Astrof estrella co for motions. OLF-RA first it ´ e eto Septemb cinco p e consisten Besides accurate v sample, tec tos reliabilit from star, has or prop ha er the con WR the examples that Morelia, aciones do, the with determinados del ed Arra time, hniques: WR que v ´ ısica p Hipparcos propios e an erio source estrellas el masiv er (P incluimos first purp with arc without stars the visual the er y prop´ el 140 the erryman determining accurate motions tes y ds and than, w hiv YET (VLA) cubren ho 17 e of V time. ose Mexico blac a, high of of w w con ery o p osito in also b purp y the as or magnitudes ere sin o found eing del terferometric WR 10 of the and expulsion y k negro a included que Large primera p tec determining angular had consisten la ST ose hole are to et The p not Hipparcos in de WR or V stationary er relativ consisten no ery expulsi´ hnique 20 al. la ´ that determi- sev nosotros ıo ARS their not an of studied en in prop 140 dos fueron fuen Arra y Large eral ears. 1997), determining in of este v in this ely rep resolution the tes larger ez. on de en terest used. te er prop our y a t o prop orted small ccasions in study er The than er in order motions b class motion finding y at , other their ev Hip- o 12.5 the v en to er of 3 © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México at VLA all massiv stars 4 configuration with in tines b Arra ter). used source, Moffat ep BnA. ep y o o 1 T Asso least ep The W T The c c able the hs h y o in tak o Calibrator of e F (VLA) 2001.14. e c ciated obtain et 1990.43 National hs. all searc w or National data three the en runa 1, e al. ep most required with F with Astronomical Univ hed or o w w (1998). of of ep accurate c ere a hs. eac Radio 2. Science and In y o the the the ersities Man high of a in c Angular stars, calibrated OBSER Calibrator h hs 1820 1925+211 2007+404 2007+404 2007+404 2007+404 these These EQUA the the the 1999.76, latest NRA VLA, source ual Astronom fulfilling angular F − a Inc. absolute oundation. F same observ WR WR WR WR WR WR arc suc 254 cases adopted rom O phase TORIAL V distance Image refined except Star 1 under presen hiv A h using 147 146 112 140 145a 125 for TIONS and Doughert y resolution phase as ation the these es 18 19 20 20 20 20 Observ calibrators astrometry observ co h h h h h h those Pro of in for ted for α p 20 25 07 07 07 07 configuration b the op (2000) ositions PR et 79.846 79.848 80.561 12.146 80.930 54.445 the m m m m m m calibrator requiremen the w erativ cessing WR WR atory w ( here, Adopted 57. 59. 44. 44. 44. 44. y e ◦ l standard OPER ations een ) discussed s s s s s s et reduction (0. used V 849 605 945 945 945 945 e 112 140 ery 00 PHASE al. is the are w agreemen from 4 DZIB for − − op e System or of 2005. the 0.700 0.445 4.177 1.058 MOTIONS 0.315 1.186 in in P found phase Large ( listed erated − +21 +40 +40 +40 +40 to ◦ b ts. eac osition rou- WR b ) w 25 the the the et- b b T T as & of δ A ◦ ◦ ◦ ◦ ◦ ◦ h y e CALIBRA t (2000) ABLE ABLE 28 06 29 29 29 29 calibrator R 0 0 0 0 0 0 (kp ODR 12. 26. 48. 48. 48. 48. 1.85 0.65 4.15 9.00 0.72 3.06 d 00 00 00 00 00 00 c) 584 162 604 604 604 604 OF a in galactic and for motions, (AIPS). al. 7 tion v p w ble from of fitting in for 1 2 ´ an IGUEZ ected ere of the the galactic TORS the (2005). In A The whic w (mas and THE − der T the mo − − − − − cos( e added Observ Dehnen 11.2 able comparison WR145a WR112 WR125 WR147 WR146 WR140 T 2.0 2.5 5.2 2.7 linear 5.0 Source Sun also task six galactic del the Huc able h equatorial Systematic δ prop exp yr       WR ) and the µ 3) WR 0.6 0.2 0.3 0.5 0.2 − 3.1 co with giv of source. α ed JMFIT h in 1 ected least 3 t indicates ) ordinates, er & distance Brand e ST (2001), quadrature the w stars the prop motions resp Binney e Angular (mas − ARS − − − − − b squares giv motions. 13.5 prop difference et distances 5.1 4.3 2.5 5.7 1.2 3. to errors ect er µ are & w e yr δ with      RESUL  that STUDIED obtain een w ( the motions 6.7 6.6 1.7 7.5 7.5 4.8 Blitz er the 1.0 0.3 2.1 0.6 ◦ 0.1 − 5.5 to (1998). as giv ) Distance 1 w a fits ) motions to of the e the the observ tak four en exp T the used the (1993) to TS to reduced b o en in measured lo exception et ected the obtain (WR (see the order cal formal w T from ed the een able determined stars, and standard prop prop Columns galactic 125, χ of galactic Doughert the the 2. 2 errors the and 5 er of tak er v In WR to alues exp WR observ motions. motions v en this the 20 prop elo of of 6 b ected 145a, rota- from y 140, mas y of rest and cit the ex- ta- ed us er et y 1 © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México This p t order consider where cases separation equiv sho rest then one as serv tic ences than stars WR WR their ypical ected a prop c All ed or k v b c a criterion 140 146, alen b resp 42 angular Difference ask elo Observ Exp of b WR WR WR WR WR WR 4 region. eing b the galactic et to six er p × oth cit Star km WR this ositional w t and ectiv ected if motions, b 10 and 146 147 140 125 145a 112 een y to appro systems is binary e, ed stars, s the 14 (Moffat − 140, binary WR of for for separation e ∼ the 1 In galactic galactic WR b cm, prop lo 0.001 from et radio order ximately cos( a distances cal (mas the − errors or w WR exp − − − − − 112, separation as runa 17.2 een the studied 147) er 4.9 5.1 5.3 3.8 6.3 GALA as ev et b standard a discussed ) its case ected mas Ma prop prop µ emission 1983 1990 1999 2004 2006 yr en      10 112, motions  the a al. w w l angular ( 0.3 1.7 0.9 0.1 0.6 − ( 5.1 exp is e 11 o a jor p of ∼ stationary from 1 ) y er oin er of CTIC 1998). ) observ a of obtain at 10–20 Oct Jun Oct Oct Apr m and WR are cm star ected the axis motions. motions PR WR uc t order Ep is of a (mas b the source. − +3.4 +2.7 − +3.5 − 30 03 18 07 22 h consisten is the separations (Ac elo binaries. OPER o distance ed × rest. six exp 125, µ to 0.5 1.5 0.3 PR c mas) smaller b significan (1983.83) (1999.76) (2004.80) (1990.43) lo 145a, (2006.31) h originating w. in ( minor and 1 h       depart yr o observ cal ected OPER with stars teracting ) terb from 0.2 3.8 1.3 0.8 0.2 0.5 kp a and − In AR W 1 Ev the and MOTIONS standard ) c e the t the erg axis; CHIVE resp ha of mo or en than WR ed ha with to One b exp t cos( MOTIONS (mas v w y are case 9 v binary del larger, 1989), e in differ- galac- ect VH54G e b Pro e p BD114 AB252 BB117 more AJ315 wind ected from used − − − − − − kp e 146, b osition can can our the the ob- ) discussed ex- 4.2 1.1 2.8 2.5 4.4 4.5 µ yr T T to ject of of of c. D l ABLE ABLE ( − A OF e galactic 1 ) T ) b angle. A W OF W F (mas in determined 74 vidually b for with These p of of lar significan to p correct smaller a 3 4 OLF-RA OR v y (cm) erform ositional 3.6 6.0 3.6 3.6 6.0 µ elength THE prop 4. text. the − − − − − − WR  allo Doughert b In In This the resolution ( 0.2 0.3 2.1 2.3 0.8 0.5 COMMENTS WR e yr a 11 ) order the w authors er 7.9 northern b − 147, WR . than for M 1 individual is motions. separate YET tly ) 140 y

next errors, ear 0. 0. 0. 0. 0. a this to , the y ST 00 00 00 00 00 the ∆[cos( alter in ∼ and Angular 36 47 31 26 22 WR+O et of c find ST 30 p ARS hec the section × × × × sho × (mas erio prop − al. effect angular ∼ Beam − − − +0.6 − ARS a but mas. 16.1 imaging 0. 0. 0. 0. 0. our k 300 b 0.7 2.3 2.8 1.8 a astrometry 00 00 00 00 ON 00 4.1 distance c ) plane (2005) d the µ 33; 36; 24; 11; 17; k STUDIED semima er yr Size      l  that m . ( colliding-wind in and results. mas. o 0.3 0.9 1.7 0.6 0.1 − w 5.1 This INDIVIDUAL motions WR reliabilit uc − teraction − 1 19 68 79 71 e a separation ) of 7 h has with e of discuss ◦ ◦ ◦ ◦ ◦ assume )] the smaller of jor is 140 W c the b for 1 comparable e VLBA axis Finally een . sky y ∆[ of 85 are southern (mas of zone, eac +3.7 − +1.3 +5.0 +0.2 +4.3 eac µ ,  this studied that 0.3 of is b than our a then ( binary h h 0 o SOUR , total  observ      large 9 yr . comp − 16 source . and metho star, 3.8 0.2 0.8 1.3 0.5 0.2 in 0 − it e our  unable 1 )] kp ) with star the in will c 0 mass enough w system onen CES ations. c. . whic 5 detail angu- e d, indi- case mas and can our not w t. to of h 5 e © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México v 0 µ 0 More few W men ∼ dicates p (2005) for plus obtained den lev first the of et − dio are in ing nations. p has and Fig. 6 elo . . ected ositions δ 58 66 0 e el. Figure . 1.85 34 al. = Comparison Using 84 frecuencies. the cit times the ts cos( obtained previously 1. ∆ only radio Pie studied mas mas −  recen  µ y and Righ galactic 1 b ha 1997), 0 that δ kp wind-collision 2 is . T . W ) ' 2 b of 46 observ µ more v yr yr 1. o y c VLBA km emission coincides  tly e e in t α wn, +4 the − − mas us. is ascension used WR b 0 determined cos( The 1 1 = the . y Bob . s whic 1 3 rep equiv accurate prop to and and − star ations They b − the yr  mas 1 δ et 140 the direction . is prop 5 orted measure ) oltz observ − 0 µ h w . 44 er . 1 as 43 with alen µ µ originates. α 2 Hipparcos Practically een , yr δ δ yielded (left) ep obtained has ◦ and region, mas motions er = et a  obtained − = = 51 t o than optical ations, function 1 the them c 0 − al. motions accurate 0 . to hs a th . . − − and 25 its yr 5 of Our The . 2 1 us p 0 (2007), giv a observ − the . . cos( eculiar 37 89 prop p mas from 1  at declination cos( v giv p satellite ositiv , and en ery dashed all eculiar determination during Doughert 0 Their   previous that of δ the en . of ) er 2 δ in prop yr µ ed 0 0 of time similar ) where radio . . used α e mas µ this in motion 49 64 − 1 motion T at α the 1 and galactic able lines to = er v T (P v = the mas mas a and alues, are able elo star (righ yr measure- the 2- y determi- − DZIB erryman − distance p motions most to the − σ 4. are cit 5 eculiar 4 sho et nigh of at 1 . µ . those yr yr VLA error t) 26 3 72 w y The δ and is lat- least − − ex- us- wn ere ra- or- in- of al. & of of   = 1 1 t, a . . WR R squares ODR 140 these v and will motions star comparison the with prop for of cen galactic is et with itude. b motions culiar ing lision 1996). ma ∼ et ´ l IGUEZ = as 50 ' pro al. al. fits 4.15 jor timeter Insp In WR a +4. ep a fall as ∆ er a − a w runa M dense duced large v zone (2002) order µ to o (1999) function axis 320 p a ◦ a Assuming elo motions

c ection b y Since kp 2, erio in 112 plane, of hs of function the ' w for cit from  c these the of w order a of WR prop d giv +3 b to b dust 100 y are y data. a b suggest et the of ∼ elongs indicates v y WR a is star. of en category . measure of elength near w 7 30 ∼ an indicates dust results er massiv b 112 km equiv een  cos( system, time. Figure that of 25 elo in en A motions 3 140 4.2 original U. time l v s w . to y observ in T 8 b − that elop = formed ears. alen )∆ able . the 1 our emission. The The e mas the a suggest the declination of WR +80. is and 2 µ binary are non this es that t this v l the adopted at suggests ed Assuming small ariable righ 5. prop radio ' to yr are ◦ p (v v sho 112 thermal 9. osition in b p a − − and runa WR an is p The t erio 1 ' that 16 wn confirmed, In eculiar er galactic system, , the ascension a group study 74 that . der exp motions, infrared 1 an d WR+OB w v 112 in are p that elo  it  a wind-wind implies ositions y lo a nature y Figure ected 76 ma 5 Huc at cated cit case, total not of stars. has of v . 1 Marc elo latitude the km y a y is Chapman W mas h emission criterion WR distance b cities smo p t w 20 galactic mass C a the system for e 2. eculiar prop s in e of henk et − h semi- mo stars yr used 1 The oth. 20 col- 112 the the the . p al. − v- er of of of e- m If o 1 © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México the Monnier of (2002) to the jor motion) of abrupt that A of and More and Fig. U. the one WR ≤ axis other the observ 2. 1.2 Since 2004.72. at than sky of Righ found 112. declination c a is y v hange et the . turned ears, elo distance this ed only This a t al. cities mem ascension This smo an p This p (2002) it osition in osition ∼ abrupt off optical oth b implies 30 of separation p is of ers b osition c − order A a hange ecause 4.15 gradien ha Ma (left) 18 of 2000 2001 2002 2003 2004 2005 2006 U. shift. shift c v ◦ companion hange the jor e (assuming W 58 kp 1,300 prop Oct F Ma Jul Sep Jan Apr b and is their allace, to 0 axis eb binary t, c et . is PR Finally Ep y ok The of is w 06 there cannot 21 12 21 17 22 osed declination to 07 een km × o equiv OPER place the estimated (2003.51) c o (2004.72) (2005.03) (2001.14) (2000.80) (2006.31) h dashed (2002.35) minor Moffat, turning large ab s ep a that , seems − order alen 1 w out b AR true o o e v e c in MOTIONS axis; hs er WR attributed to lines CHIVE t note (righ the 0. & to semima- on a of to ph 00 2003.51 explain 94 p p Shara 112 Pro AM661 AM793 AM831 AM727 AM661 AM766 AM793 b ysical plane 0. ∼ while are erio t) osition e that 00 SW 330 08, of an ject T least D is d ABLE WR A OF T angle. A squares W W 112 F a the et system p ma nary source. could of structures asso 5 OLF-RA v OR (cm) osition 3.6 3.6 3.6 3.6 3.6 3.6 3.6 elength as al. WR y In WR ep ciated fits a WR pro systems 1994; o b order function c with e 104 In to hs 125 duce shift YET related 112 the that summary with giv 0. 0. 0. 0. 0. 0. 0. and v to 00 00 00 00 00 00 00 is a an 69 37 36 36 36 38 36 Angular (Monnier in en shifts data. p ST measure of b erio × surround × × × × × × a der WR eliev WR in to time. Beam ARS 0. 0. 0. 0. 0. 0. 0. “pin 00 00 00 00 00 00 00 T 4.3 d , the Huc in 49; 20; 20; 20; 20; 30; 18; ed able 98a). 112 w larger Size . wheel” e The the the et to − colliding WR h conclude − − − − +3 − t a should 6. 80 a al. 7 9 9 9 2 b 2001). apparen These righ prop ◦ ◦ ◦ ◦ ◦ ◦ ◦ few than e The 125 2002). a t W er WR ascension b p winds 18 e are that ositions C7+O9I motions, t studied y p Their stars ears (as spiral osition the found is is (Williams as I and observ presence I the further. w 18 gaseous a binary e of h in func- used that case 16 the bi- ed m 7 © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México exp tion ing and Fig. 8 surrounding ject, (Sc a p Its ep in ception a ossibilities significan WR+C o Figure hm p This T ected c that the 3. hs of erio o in utz, Righ time measure giv declination of this d this system galactic 4 en is system, the Geballe, t t exhibit cannot are medium. ∼ deviation ascension case source in 4.8 p giv T oin the is prop able hours. most is en 4.4 where t b also a & is 19 e at a prop in . smo er Ma (left) 7. excluded 1985 1993 2000 2002 2004 2006 stationary ◦ Sc in WR ep lik Figure 33 motions kno The hild jor declination C er oth o 0 ely . c F Jan Oct Mar Dec F and 145a h stands wn axis eb eb The motions, prop 1996), Ep b 2000.81, a eha 16 16 18 3. 19 06 (Stark declination 03 as o × massiv agree dashed with c The (1993.04) (1985.13) (2006.13) (2000.80) er (2004.93) h vior (2002.17) minor for Cyg although motions from & AR w resp observ w compact e whic with lines ell, e X-3. Saia axis; blac CHIVE (righ the ect used DZIB suggest- h the are ed k sho 2003). sho p Pro A A A A A A to other main t) osition It W638 W546 W563 W672 hole V193 C116 and least ob- the ex- wn ws of its ject T & D is ABLE WR A R T squares ODR angle. A W 125 F a ejection caula trend. that With tion − ably ties particular galactic consisten runa in tionary 6 v OR (cm) ´ IGUEZ 6.0 6.0 6.0 6.0 6.0 6.0 elength 0 as our fits . Comparison One 7 of w a  WR with WR affected the a (2001). v to function fits. 0 y l This with . prop 3 of ev = t the adopted stars 125 145a mas resp with the en 0. 0. 0. 1. − 0. 0. the 00 00 00 00 00 00 data. 30 t resp 42 36 39 ep er 11 39 Angular 37 the declination, ect Since of yr studied  is this o × × × has × × × curren b motions c 13 − Beam ect time. et h distance 0. 0. 0. the 0. 0. determination 0. 1 to 00 00 00 00 00 00 w system km corresp 35; 34; 33; and 34; a 34; 34; een to this its Size so-called tly relativ The b s its − − − − ∆ y − en the giv a 36 62 27 16 ejection 1 1 µ accepted 5 of this Mart lo b onds vironmen ◦ and righ ◦ ◦ ◦ ◦ ◦ b en eing cal ely 9 observ = kp t p in ´ v − ı, Blaau standard oin ascension b small to c, of appro 0 P = T ev . 3 w ed t aredes, able the the explanation t, en  − e is w 13 obtain and 0 t ximately p cos( not . north-south p 2 eculiar kic most  3 osition, of is mas 9 indicates exp b k: included & 19 )∆ km rest. v h prob- P elo ected yr µ mass s era- mo- sta- 28 l − − for ci- in = 1 1 m . , © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México Kalogera are massiv sho with cussed authors b lo the momen at Fig. ev and no ejected e cities en v the a w a exp the t mec 4. ed sup no and explosion e Righ fiv tum time ected declination in sup suddenly that hanism erno prop blac e is (2001). binaries binary t erno not opp v k of ascension ose t if a w holes they ejection. o included explosion. v osite forces b a that y of Mirab and is systems explosion, with whic 40 them w ( a to ≥ Ma (left) ◦ ere in 1983 1985 1987 1997 2000 2004 2006 symmetrically the 57 el in a h 10 that jor the So, blac 0 formed are Dha & the . they with Sep Mar Aug Jan Oct Sep Ma and binary M The axis Ro as formation k PR one of Ep fit.

y not w 15 13 10 declination 21 hole prop ), 28 05 drigues 16 an p form × o a OPER the oin The b c (1983.71) (2004.70) (1997.03) exp (2000.81) no runa (1987.66) (1985.18) h blac (2006.37) y minor to et comp t osed direct un for ects kic al. b is dashed AR recoil k y w b (2003) of MOTIONS k b 2000.81 a ound axis; hole, (2007) b the onen CHIVE ys. eliev (righ y recoil v the collapse, elo F with lines ry sup p These t, Pro AM669 A AM858 ed AH172 AR545 A t) cities mass since most mea- osition AJ95 er W426 C204 (indicated and dis- v of er- D ject T to are & e- a ABLE A WR OF T least angle. A W 145a W F a with ra without sources et of b b for ities. motion blac sured without OR 7 squares OLF-RA v (cm) y e 6.0 6.0 6.0 6.0 3.6 3.6 6.0 elength y as al. this In GRS WR them k bursts WR an a The hole, 2006; summary the function kind empt fits ma could asso 145a a YET 145a 1915+105 a Cyg prop significan y 0. 0. 0. 0. 0. 0. to and 0. of y Fyn “dark 00 00 00 00 00 00 ciated 00 of b 40 43 24 42 40 26 Angular square) 22 app the e b long ST X-3 of er massiv , e the found b × × × × × × × the o Beam ARS ear data. due time. 0. 0. 0. 0. 0. 0. motion 0. birth”. luminous 00 00 00 00 00 00 et 00 system ones t duration (Dha 36; 36; 24; 36; 34; 19; 20; kinematics w to Size al. natal e to no as The blac − − − − − − indicate resp tak a w 2006; a evidence 37 69 45 61 23 78 of 4 an dynamical ma ◦ righ ◦ ◦ ◦ ◦ ◦ ◦ k Another en kic sup onsible Cyg in hole y et during k. t Mirab b erno that ascension the that al. e Its X-1, of formation, another v for a near example w p el ae small 2007). it diffusion eculiar ma e a 2008). the (Della also determined jor ∼ is Univ example gamma- p 20 ejection 10 formed eculiar These v called h could V elo erse, pro- M 32 alle c- m

9 © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México and Fig. 10 cess, GRS It companion (1996) is This the 5. the suc 1915+105. Righ and declination h brigh is as a t confirmed w WR+O ascension discussed as test first WR is 4.5 41 system a a rep b (left) Ma Ma . star 1985 1995 1996 1999 1991 1996 2004 ◦ y b WR 22 y orted Niemela jor jor 0 Dha at . F Jul Dec Sep and Jul Oct Oct with axis axis The eb 146 radio Ep Ep w 21 12 b 03 16 26 1 declination 14 an y o o × × dashed a (2004.75) c c (1995.55) (1991.53) et (1999.67) (1985.13) (1996.82) (1996.95) h h Doughert 30.8 minor minor et w al. a al. v AR AR elengths. y lines (1998). ear axis; axis; (2007) CHIVE CHIVE (righ DZIB y p are Pro AM305 Pro AM482 AD391 AD502 erio A A A p p et t) osition osition C468 C116 C530 least for Its ject ject of al. T T & d. D D ABLE ABLE WR A A R T T squares ODR angle. angle. A A W W 146 F F a a tions w b motion tions relativ runa 9 8 v v (cm) (cm) OR OR ´ IGUEZ et 6.0 3.6 3.6 3.6 6.0 6.0 3.6 elength elength e as fits w used In w een a WR WR giv are a ely order to function y in the en observ the star. sho 147 146 small b 0. 0. 0. 0. 0. 0. 0. in 00 00 00 00 00 ep 00 00 to is data. wn 22 48 37 22 43 22 20 Angular Angular T o of ∼ ed measure able c × × × × × × × and hs in Beam Beam time. 16 0. 0. 0. 0. 0. 0. 0. and 00 00 00 00 00 00 00 giv Figure 19; 36; 30; 18; 35; 12; 17; 3,  w Size Size en e w exp 5 The − − − − − e the conclude in km a a 44 17 33 17 50 54 15 conclude ected 5. ◦ ◦ ◦ ◦ righ ◦ ◦ ◦ T galactic able s − F t 1 rom galactic . ascension 8. that This that The the prop this difference the comparison prop prop er is p is 20 motion, eculiar er er h not mo- mo- 35 m is a © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México 147S images An cated colliding on classified Fig. Fig. and companion as a the This earlier the 6. 7. function is ≈ basis Righ Relativ clearly the declination 0 system wind as . 64 O8-O9 WN8 t whose of a of ascension arcsec e B0.5V rev Hubble sho time. prop consists star eal winds c V-I is k. er 4.6 north The 40 a star (v I The (left) motions Space . I ◦ second an WR are sp 21 of dashed b of der 0 ectral southern y . and a in the T The 147 Williams WN8 PR teracting in Huc source elescop declination lines WN righ OPER t dashed yp h t star t comp e 2001). are (WR star e ascension w et (HST) to as lines MOTIONS plus least al. onen whic pro (righ 147N) prop Near-IR (1997). are an squares duce obser- t h t) (left) osed WR w OB least of lo- as a WR OF and fits squares 147S W to declination of v al. the are exp ciated. WR tions. OLF-RA the ations WR as fits In ected 1998), sho ep data. 147S a order to o wn function 147N (Niemela c hs the YET (righ galactic in do confirming giv to data. es Figure t) and ST en measure of of not et ARS time. prop WR in WR al. ha 6. T that able v er 147N 147S Comparing The 1998). the e motions, large they prop righ 9. with are The t The p er are similar ascension eculiar resp w motions, the E ph e prop ect ( B conclude ysically observ (Niemela − to prop er is V WR motions w 20 ) er ed e v h alues asso- used 147S that mo- 36 and 11 et m © Copyright 2009: Instituto de Astronomía, Universidad Nacional Autónoma de México Sergio SIMBAD Ac F cyt sidad with the quite LFR in a a do it 12 p & WR that prop the 145a, tions sp lo in rotation with radio of motion − obtaining prop rance. eculiar 0 cit teraction sup dark ect is h rest Ro the . not (sdzib, cional W The The The W 4 terb true (M northern y ose er the mo  a 145a, the erno ac dr e e due large. to Nacional WR source of galactic runa 0 from motions ´ exico). birth, ´ erg, measured kno measure thank ıguez (see ving measuremen . prop Dzib radio prop that prop 6 the p mo the exp v to osition cos( mas database, a l.ro 146 wledges Aut´ w the A. zone del This Dehnen Figure lo ected ejection. a the er a Sun er er this 1999). 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