© Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México phologies ing the Bubble tributed of no mainly terstellar noma R evista v massiv 2 3 1 4 5 a Photoionizing Instituto Lab Based LAM, Univ morphology KINEMA HI explosions de I oratoire formed ersidad M Mexic and regions to e Observ on ´ exico, medium are P stars. . observ stellar de sup Am difficult Key form bubble p unrev remnan b and formadas is en v con de m primera naturaleza, p morphology art ana d’Astroph Ib e b y atoire eculiar ero Mexico. Astronom uy of from at to eroamericana, y erbubble bro ´ reflejada los ıculo TIC una Induced the ations radiation, ionized ev n de bubble-lik Wor (ISM) tam 1. pro their p winds, ealed. uestros differen La The cio-Cruz, filamen eculiar, olution de t around massiv Astr action explosi´ GENERAL to vide v radial es ysique bi ds: of done Marseille, nebulosa FIELD ez ´ p ıa, ´ b en nebula or explain. prop of formaci´ bubbles onom an en star oundaries, formation N119 difficult una and H kinematics t Univ kinematic tos encon los resultados, at of e a stellar e dif on de Mexico. of su v bubble-lik 2,5 h the I stars elo nebulae orcionar galaxy La I yp formation N119. d R burbuja ´ vien ´ sup ıcil Grenoble, ıa ersidad camp the de ´ ebiles, seems F M. regions N119 e cit erno on Silla WR tramos N119 rance. c filled y OF eive erno to de tos hip winds transform y Rosado, stellar Astr y is o but field, v The (ESO). explain in ev data star and explicar d and a erno in estelares to Nacional los de e v datos THE to with generally N119 alrededor en oluci´ a 2007 F of explosion. — otras can regions, rance. the con other and v ´ p explosions ısic cuales a rings dynamics sho Br v la elo that winds eculiar a. 2 ISM: medium hot on. tain explain with a Large cinem´ A. Octob the parece cidades Nub wing 21, sup comp , con S-SHAPED En Aut´ mor- de ha 44 could gas. La La forman ABSTRA at- three in- er- RESUMEN de inside and from bubbles e v- classical , estrellas o- spiral el los sev v er aticos Indeed, onen p 355–364 Magellanic al, Ma — la eculiar con curso radiales, 30; place eral another mo 4 estrella expanding y W ISM: the tes diferen tener E. or shap delos olf-Ra ac que matic and of ( cated of enigma. a sho b giv ab cult & ula CT expansions — mo O, α Le de w cuy de e N119 c constrain morfolog plethora (2008) o rotation epte this Newton e sup e e = ws explained The In v ISM: WR dels. puedan 3 Coarer, este el is N of comp ha tes WR Magallanes e o to rise cl´ y Cloud NEBULA 05 v nebulosas erno origen et d seen data cual the asicos. (Georgelin a v ery w this 119 nebula. h bubble-shap explain regiones e aim y 2008 eird 18 estudio spiral The and to Br individual It detected onen ´ quiz´ ıa v ts close Large of . of m 1984; pro of nebula 3 a 4 that sho sho dar bubble is of espiral 21. m no uestra nebula on D. ring-shap remnan the b the aim July O El as t , jected y also the ws ws δ with morphology ( est´ the Russeil, restricciones whose en en stars, tiene ∼ hemos un could one ob = Magellanic Rosado disk fain of et is 15 a 22 a for presen a forma N119 de jetiv ed − v imp formation. forma p nature, claro. in (N the also arias 0 ts v the t in al. osible of 69 v ery to of esta filamen the nebulae una ed ery the place and origin ortan ◦ fron o detectado 4 119) the presen the the 15 classical reflected t 1986). de 1983; nebulae and del conspicuous expansiones first de De nebulosa pap 0 LMC. conspicuous IN morfolog remanen t a formation southeast) mec in LMC burbujas, whic t Cloud constrain of sobre — presen ts p burbuja remains acuerdo P t er formed to J2000 ossible time . the THE Indeed, whic Meaburn, pap hanisms Amram h ISM: Ho is The note ev whose in (Kim p still bar su to or ´ se er te w te (LMC) ıa en h a a ev equino ts nebula ts pro to the of LMC er, et remains form, this 4 origins on that men vide the the al. Mc the lo there x) the nebula tioned cation cen N LMC. 1998) could 1 kine- is diffi- Gee, neb- can 119 355 na- ter lo- an is © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México scrib observ section, Fig. 356 teristics matics ture, to emission, (b) presen scanning tiv DEM photon-coun resolution. the giving of to the tained × Am The der op b tak observ 7200s [O een 2. erated 254 ely view, i a the en The W i bro H H Europ to OBSER i 1. nebular discussion es ]( α scanned . formation e α L132a,b and ations ations ts b λ sampling × cio-Cruz Consequen c 3D Mono of the Cassegrain emission. efore line 5007 ha observ hec w and the and a 24. F under N e ean v v 8000s sho abry-P v k e elo giv V and elo 119. The c ting data conclusions the carried hromatic for and A of an A). ˚ obtained and ws in ations Southern cit e TIONS cit of and et sp 24 7 the the information lo the p angular for y free In In detector y tly erot WR after cub The the ossible km ectral cal al. cub fo differen field P § , brigh H ev out on same H cus es anel the 3 sp kinematic en α images s nebula (1997). (FP) olution es AND i − calibration the FP N119 i w ha Observ of ectral vironmen and 1 in resolutions of t sampling with FP of e flexures region (a) for v and the used t conditions presen order this nebular e data etalon in the [O D are data of ab total w the the terferometer With of nebula. A this broad range ere atory i the out w T of i results. 36 mark N N103 i to ork. t p A t cub [O ], of cub carried exp osition spacing angular data the resolution of 9 field 119. exp resp the cm REDUCTION of obtain a 00 i arc the at i es ed of , N e i as osure 38 16 § ] main osures w describ sizes La F around ectiv telescop line, and in 119. 5 the at 0 AMBR cub In Finally equipmen e during abry-P km × of out is P p the ha Silla field attac the H anel 38 times b dev es the ositions FP ely c are resp s § α v sho harac- with of − 0 in ed e 4 kine- N . w next , 1 oted OCIO-CR field e erot CO and and and hed 254 (b). has ws the the ob- de- § ere or- ec- for 119. in of of t. 6 a the clouds The fain UZ 1993) in three tion measured length co and the rectly ula. photometry L130 50 the comp liott, “mono denomination. comp tral constrained FP all ing t scale is east v 3. neigh sho kp these erage Calibrating The The ET new data sp radial part this and Although ENVIR MAIN onen onen , & c is according nebulae wn filamen ecialized c whic generally calibration, for AL. hromatic” the b HI Meaburn IA data nebulae decomp oring of of soft cub b ts ts b U I v y the y h same elo N119. the 3.1 region CHARA ONMENT is exists. b circles; nomenclature, t. p w es. Caplan reduction y allo ossible. DEM found are cit N LMC p . N The soft the adjusting nebula, to ositions, with Ionize for osition. y The 119 ws as 119 1976). and N construction w profile the w bubble lab F eac fluxes N e in L132a,b, CTERISTICS distance, are & flat or 119 is forms HI decomp d “con el 119 also h sev Deharv DEM Since OF smaller w N119 information I gas CIGALE map. Hereafter sce facilitating (Henize as fielding extraction regions eral the DEM follo tin ma B051842-6918 THE a w p morpholo sho p catalogue ere osition erformed uum” w DEM w y radial and min eng (a) eculiar, wing e e (131 ws of L123 b NEBULA ha 1956) for ha e able [OI um correction, the (1985) (Le including w the AND v v done images L123 × and e v their the on e I whic e and um of gy elo I] will v in 175 used strong Coarer to go elo b or, (Da emission the profiles tricate cit usual y fitting. the LOCAL n in h o consists only and iden cit construct designate um d means p follo y from vies, absolute N the the v c, ∼ profiles y nebulae spatial elo cen b tifica- 119 w 80 DEM et maps using LMC er wing indi- neb- cen- a flux cit w and Us- tral the El- v al. p as of of of e- y c © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México of sp (hereafter lo extremit ure cub Fig. matic can c ula, of hannels oks ectiv filamen w W In es 1), b 2. it eak e e lik Figure in images, is ely). with Some appreciated can er e y sho the remark tary a (hereafter called filamen w large w see These w of 1 the a extensions) extracted a vy the the y able a “strong and bubbles discussed ts. filamen brigh conspicuous arcs [OI in called for brigh The I the I] presen t, its from KINEMA DEM v t. cen than elo [OI elongated, t the NE p in filamen On tral eculiar cit I t our § I] L132a NE morphology y the ramifications arc 2. the and emission”, c [OI hannels TIC and 30 tary is other spiral and I H cen Doradus I] 15 α FIELD SW arcs and 0 tral DEM mono in hand, long, shap of arcs, see N on H formed region N α 119. c L123 e. Neb- OF eac hro- Fig- and 119 the FP re- h THE The and upp the S-SHAPED of also brigh SW (a east whic a sho arcs form DEM kinematically er lo brigh filamen and w w c arc h and er rev hannels a tness: four the L132b, includes t c fain b eals hannels has and (2) ts in lo bubble-lik t NEBULA (1) cations whic a a that sho Figure filamen broad DEM iden series more the sho a w h brigh N the tified “strong w are L123 arc of rounded t of 1). e 119 the N119 bubble seems clearly structures. fain these t can in WR “S-shap and An is t § cen constituted b filamen 4. DEM bubble. structure: insp bubbles to WR e differen tral seen, close ed ection nebula) emission” L132b; Figures ts main whereas tiated whic (DEM the to b of y structure” the h whic structure the Figure t 1 b seem w and y L132a, middle to o and w h their sets est, 357 the the are to 2 1 © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México Gee, direction the more than 7 HDE269333 Fig. 358 of (see of a sp whic Massey grade this Ardeb sp the ha et ha Massey sho dial 0 ectral ectrum). × “c” v v the al. ws, the The The Among In The e e optical star 3. star; 4 h v Figure measured 14 Bro 0 massiv elo determined most 2000), erg the . notes is 18 qualit this , 1989). Most SDor-t sole thermal an mag t cit LH 0 t W oks, w of × ho yp case et o 18 y aterhouse, luminous WR OB nebula As w the 3). e decrease e the stellar y 41 or are al. more of 0 ev (Luc of stars & WN3+B1Ia DSS yp of F to Figure asso − er a strong +268 R87) star east, the 3.2 radio lo Batc (1972) e. massiv the radial 32 k these this a cated image N e luminous asso . ciation are stars is stars. sp & of Stel 119. star from Thac helor is km The 2 lo cen con & ectral determination lo ciation Ho O4I authors e sho v cated a ha of inside lar elo cated tral of DeGioia-East s Sk tin W dge k v stars, with N − “a” (W ws, first I 1972) era e cit LH41 1 I c − olf-Ra uum 119 stars ontent measured emission; sp t alb inside (based 69 y 1970), y yp inside to this outside the , 52 ha ectral ◦ of sho one & orn e 104 is “d”). Br21 source v are y mem to +286 132b W e massiv wing of et the asso attributed N 1977; esselink spreading only is (HDE269357), the lo (their (WR) t O7I w this b yp ho 119 a cated WR As the (Sk ciated ers SDor Bubble. o AMBR MC30 km w o e e stellar south I up d ev I(f emission Figure Con is star p (Massey − brigh nebula. ositions qualit s on star (1960) er, (2000) 69 LH41, − ) in itself 1 with ti only OCIO-CR o (Mc ◦ and and one the the v are 95, ter ra- for er of & y 3 UZ has case, analysis M 23 shell Szeifert able − p α emission-line 10 (DEM from ern with (1 to its Stothers nen t than data fluctuating arc of absorption regions but an (218 km Sterk men a far star 1999) nebula. (HDE269321 more (Sk our the Stahl (data more w c) 69 helio w . 0 BOL − o = sigh 5) − SDor Israel Figure F for ts ET M ards (DEM ligh arc 4 H s south ◦ b tioned it comp and in sho rom − p − 10 69 candidates are en, the 05 een the α this data

southern M northern et along 1 c), a rep is t cen = SDor. L123 ˙ 10 ), (Figure t . v the 0 ◦ AL. image. sourrounding h wing LB 00 of ailable N et 94, al. to 16 of DEM collected & & 132a − et Rohlfs curv t classified − ort and classical onen HI tric star yp of W 00 L132a) 4 119, V o the Kim 5 m 9 al. HR b from SDor de Chin al. min lines, the (1984) . J2000 HD35343 and esselink M sho 3.3 fain 57 e efore. 7, the at a observ The or es, v only radial ts bubble, F is

strong W Gro s 1). elo (1993) FI-t cloud. L132b (1996) T t diagram cloud, . at presen ws line et , = et w t asso R85, L eff DEM strong yr δ e 9000 related Gase v (1996) that and corresp o cit for other ariable in cases, +213 can al. These NASA ( al. ot and as one yp − = Spitzer suggested 10 ∼ = of ations of v y F 1 ciated T the (1956) elo measuring . e − rom (1997) a cen − ha +275 ous t mark (1984) 13600 them (1999) able determined see K The (GS54; or and its the sigh of L132b), the 6 HI Recen R=50 sp only B5I 69 cen SDor-t v cit is ha to ionized authors onding or km tral to M e R88); ectrum, that +295 arc ◦ with mass-loss Envir comp t 132b higher y close with v observ detected 09 ed with tral 1. of third temp

the km lo that b 20 e of small K of has ha hiv ha t y ha 0 emission s that cated p carried 45 +275 as yr − α the observ yp the c). Arp 000 corresp and v +279 v a onment s v emission SDor 1 onen e) the to bubble to 00 km DEM e an − e erature gas a − e . ha it cloud = LBV ation e measured smaller 1 1 found nev v spatial photo determined, this cataloged J2000 a northern y sup the resolution ) star that ariations. v K. is along R (1992). three 05 to matc p V rate km e t and v s stellar ations km er osition − v out an elo an also along = erimp h onding D L123 and According ariables in star 1 at is M 18 is and disso of observ t s ˙ 135 cit comp of D (Figure s w h also SDor and − and, CO Genderen, LB lo the amplitude Figure m Sk a resolution − 8 measured o 1 P-Cygni. v southern y ( 1 cated 42 (Massey is sp SDor microns mass a osed nebulae (GS ∼ ery . the the − V comp 2 for R ciation for of max In clouds north- of s to These either R=85 v 69 ectral onen mean +245 ed

gian , from from aries v with δ w this an line . ari- 123 ◦ the the the 15 51; 1), 3); on ell 92 so to to o- of = = It is y t t 0 © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México Gee ula files N the nebulosities W Fig. In whic 132b cen lineated, e 119. this tral In The Figure can and whole 4. et h sho bubble general, sho Con al. figure see emission w thermal DEM the w 1972) a tour 2 nebulosit that 4. and mark presen main some nebula it THE L123. the map is the the * is radio and Detected ed DEM DEM DEM DEM RADIAL seen v asso emission H ts elo photo of y 123 VELOCITY as α con the arcs, Spitzer at cit and ciated con that bubbles L132a L130 L123 L132b nebula. tains y an disso [OI KINEMA tin cloud [OI comp whic HELIOCENTRIC in separated a I uum observ four with I] v ciation GAS I addition erage I] 132a, FP without Israel h onen radial FIELD fain source are the TIC ation v SEEN elo regions helio t 132b, et ter optical quite b detected 275 279 CO cit to FIELD v v y * al. at elo elo bubble-lik MC30 cen y 7 the ON 8 WR (1993) cit c cit surrounding km w microns hannels tric nebula y ell strong y VELOCITIES THE OF measuremen neb- o pro- (Mc s v de- − v T er e- 1 e ABLE THE . Rohlfs (data LINE the 246, 244, S-SHAPED a it regular features, analyzed ha plex p dial violen en v 2 resp and lo et OF 1 v t. 266 266 ionized elo onen ailable HI y in cit t v al. (km field e 274 275 cit ectiv Figure morphological SIGHT y v 7 v plotted elo (1984) t t, elo of km y motions and at s the of cit gas comp +279 cit ely − in sho s 1 NASA y the − NEBULA 5). y ) radial § matc OF has 1 (this profiles wing OF profiles radial 4.3, onen for km S-shap In Kim N a inside h arc THE the addition corresp s v there single ts that v 119 − elo features ery hiv v 1 app et that and H elo ed N119 and cit 271 271 e) NEUTRAL HI α al. them. w sup are cit ear cen y v ell onds sup and suggesting elo are (1999) profiles with to y erimp tral with bubbles complex. erp and cit profiles this [OI coinciden to The y osed FWHM b the comp I osed that profile main o I] sho dy p v on presen 132a the , of elo erturb w In whic onen on mak our v t sev the of cit elo that existence Figure with bubble, the 20 y H ting eral h e t cit ed differen α profiles, n is the km will y um image. differ- v zones other quite com- com- elo 5 359 s b the ra- w − b er of c- e e 1 t © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México v cen matics stars in Fig. 360 and are is mark H cated can ble North in oted α tensit the Figure tral In In image. m 2. b 5. DEM ed uc e main asso within to is Figure the Some Indeed, y asso of as b h at of the o fain ciated 3. dy No. these The follo the comp the L123 ciated examples . study N ter 2 0 top x line wing w 119, the -co onen and 4.1 distinct e than with men with and ha ordinate in of . bubbles whose t 1 section v Stel arbitrary tioned of the found the e in eac east some the detected the lar bubbles, kinematics h S-shap is in p H in nebula ositions Bubbles 132a, H b w α to of the efore α e the units. and the the will radial ed profiles for whole while 132b, [O left. cen are are massiv Profiles are study of the i v i tral i elo the listed ] sho field giv also § WR radial AMBR first cit e 4.3 es b wn. the S-shap mark y stars o (see mark the dy nebula time in profiles is v kine- elo OCIO-CR The and text). helio ed T de- lo- ed ed a- cit a with y cen are profiles The tric * nigh UZ are v nebular that ing winds prising lo gas, bubbles its nebula, seem bubble solid ery radial cit t-sky of computed H On ET wind-blo y α w as massiv line the to that a profiles radial v the AL. y around b lines. and can cen elo con are , ecause differen corresp w cit in other tral e e tain w b differen wn v teract y exp The stars e e age. elo in of will b the seen t onds WR an cit bubbles ect o km hand, features v the dy y elo y that The sho with WR t the s profiles. in to in are and cit − from bubbles w terior 1 the the y DEM undergo Figure existence and that the star also of (W comp Of sum those N radial the ea surrounding The exciting sho it stars Br21, 119 L123 v onen and is 5, of er y wn. expansion -co v of a sup all of elo v where et t ha WR elo of ordinate nebula inside the mark bubbles the erimp cit This v star. al. cities e the y nebula neigh comp v comp ISM, ed t ery 1977). is ypical osed the S-shap do motions, giv as in not around onen b strong es onen form- No. es giv N119 on these oring sur- not v the en ed ts. an In e- ts 2 © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México in b found parameters ble, lo one from p whose the massiv exciting p second), excess et S LH41 the (1987) plan The WR DEM DEM DEM H oundaries osition onen cit Figure al. α Bubble The On one . nebula deriv name exciting y Lyman & our ts, (1972) (1.05 profiles this signature e L132b L123 L132a of the from deriv Deharv star, Lyman stars of V ed implying the 5. H kinematic min basis × (see the α of the from flux + * In ed UV star 10 (2.4 Mec nebula linear DEM DEM DEM WR Dynamic flux at the Sk-69 and is LH Sk-69 T Exciting 51 eng from v § Bubble exciting of S is Br measured able flux name elo × hanical observ the SN? star more our denomination, 4) photons nebula bubbles Dor 41-32 the 10 H V that is P L123 L132b L132a 21 ◦ (1985, cit radius, ◦ α N ARAMETERS 104 max the cen 50 92 evidence 2 H for 7.1 y presence and timescale. 119 α w ations than photons , the profiles ter luminosit 6-cm × e KINEMA star), flux the and 05 05 05 05 05 10 rep suc p b 1986) H has R, km y of er h h h h h UV of 49 β 18 19 18 18 17 enough α V 272 285 279 285 h ort MAIN Smith, (1.3 132a H observ of extreme for the second) 2000 photometry sys star m m m m m b s of as: α photons while − are p een sp 19 1 59 14 56 y the flux as the × 1 er surface the . splitting 9 bubbles TIC of ectral . . . . name 10 3 5 4 1 s bubble single. ations E second) DERIVED deduced s s s s CHARA OB Cornett, main the km to bubbles 50 of ( at V B is v − − − − − 20 27 26 34 FIELD − elo exp photons the p photoionize stellar s larger the 69 69 69 69 69 t of asso brigh V − er of yp , measured of δ of (near ) cit 1 ◦ ◦ ◦ ◦ ◦ obtained the W the 2000 11 13 12 15 16 star and e = in second; McGee CTERISTICS ciation bubble the b y e sho & of 0 0 0 0 0 tness, terior y cm 41 07 55 01 03 wind. color com- 0.15. OF bub- than ha FR 10 19 20 n Hill Ca- p the the the 8 v wn 00 00 00 00 00 e − v T T er e- 3 e OM ABLE ABLE THE Sp O7I SNR? O4I WN3 LBV LBV t cm ectral yp 2.5 2.6 1.2 1.7 F n I I(f ABR o S-SHAPED − I e I obtainded the to sho luminosit in stellar al. Sc prop this scale. umn sho ters Garman Column b b photon they temp 3 3 2 ) een een OF haerer, Column driv ws c (1977). The T On Y-PER Radius 10 total k listed erties able (p v erature 2 driv iden cannot t 13 18 THE 79 26 26 44 5 alue + 6 5 e the densit wind-driv giv c) the In yr flux, y the systemic 3 , en y tified 3 H & es in from Column & OT of rms 8 of NEBULA lists, giv α other BUBBLES corresp Hillier b km measured 10 the y of an T but V con y Sh the emission. the 247 253 230 236 es 36 able min OBSER and the the in electron s ull the estimate systemic in en − tribute 13 12 44 15 erg the terior L bubbles hand, it winds 1 v 2005) onds Column wind SDor elo 1996). 2 bubbles 7 a is Column s km v w − expansion N119 V the cities erage bubble p V 299 307 298 275 1 e max to ossible The from A is densit of s to can v to or of − TIONS v ariable b wind the 10 giv 1 elo Ho the y 1, an the the dev of helio an 36 expansion deduce applying 6 L the en. 10 cit 0.2–2 w the expansion bubble y 100 O3V earlier mec the erg that ev , 13 elop the a − – yield y O3I luminosit v v cen Column 5 stars er measured bubble elo * ailable of erg s ionized − ed or dynamical tric no this sev cit the 1 star cm phase 132a. of indicates the O4I S b 3.3 6.6 4.9 5.4 y v eral OB H y , − v ionized is elo the name. α mec bubble y elo 2 5 Column W I mo (Martins, obtained; I gas s cit required of parame- the The star ph − ea cities (V hanical Lyman 1 dels y v SDor. ysical , acca, sr er w time that Col- pre- gas, w 361 lo has has − ere as et 1 of of w 4 © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México 362 from s et obtained mo n an the ing 10 electron mec dynamic with from of L W sion star the lo nosit the Ko comparable the at t required fully s eral WR driv lo L123 formed al. tral this of where km giv N c 4.2 , − − hanical o cit cated e 36 1 1 = 119. 10 a is al. 10 e esterk dels, . = . . In Bubble In In initial (1999) hanical a e p s WR tak am bubble. y p WN3 t figure the could y star. 36 − accoun the motion. 3 erg 4 osition obtained An n the yp The the The ositions shell ( undergo of . the 1 Figure the t e 35 C of 1977) K bien e . b ergs In e to the is and S stellar dimensions y O7 densit e luminosit phase, s timescale estimate to C Con measured The × as: and the /V − is case mass sup pre-sho the star) et in addition, the accoun S case but, it thic t 1 DEM ted luminosit 10 lifespan and to S driv s m of V medium is Th − = ti where can al. ernova ) units winds, es V 5, in action V − uc required 2 F exp 1 y NW the kness as of a wind for n & S obtained , , 7 exp urthermore, unfortunately is 10 us, it of of e O4 h ubble R e =V the an R HI n (1991). c t L123, the , b y Underhill 0 b the 5 of 2 is k b e matc required larger 55 bubble e km . y where amply of n bubble in , = sup of y 59 the × of V of of exp gian this expansion of from densit o prop r y ∆ appreciated the [OI L has assuming S the WR emnant V and R 10 p 10 M WR the (V a the mec the DEM R the of ergian S . s wind c, hes 3 is /V expansion also − I 6 t 5

WR , b optical a max The in I] = b osed than 1 The the W n C shell v y where yrs. the S y for S-shap nebula, WR y V HI stellar een DEM expansion = terior (the ailable o w nebula. ears, , for wind S v S ( alb (1988) taking from (W mark R elo ell L123 in t , n luminosit star – 0 dynamical stellar shell. is c pro is sho stars) o / mass-loss these that . andidate Consequen ev orn the an phase an cataloged motion 5 , cit 3(1 cm with ea V t the ring the L ypical R O aluated ed has p wind L132b ducing that min M c ed v of y isothermal Maeders’s the mec o are am − k ˙ of er et calibrations. sup wind is the + in w this 3 cen profiles sound Th authors the the the wind v sho in )/2. V er is coincides b for al. bien this giv and et elo V C p y hanical w sho a bubble of een ergian 2 S us, terminal tral v b obtained 2 2 c (L) initial Figure DEM bubble c AMBR v in (asso duration ailable en rate same )) a the ecause cit (1995) in time al. the luminosit k b b alue and tly wn. t bubble V y y star (L The obtained sp the y order (W v medium S units to in b , Kim at elo assum- cen t expan- do mec o (1996) sho eed 1977), in as comes ciated in of V DEM stars. scale, L123 F lumi- dy ea sp driv units mass with with 2, OCIO-CR cit S WR rom sev- and me- rms w tral ) not the the the km km v v ec- c as: as to et in er in of of k: of e- y is is is y e . UZ kinematic profiles zone v a On E km results cen al. assumption et (Lozinsk s ble 1999) nebulosit comp Figure blueshifted phase cen is b LMC, tiv bubble; sion detected b h an are this ticed quoted L123 ting tak fain ties O6 sion sion, [OI stellar there 4.3 − alue yp e een o main a 1 al. ely , ev fully e ter tric I . The As The ET t but erno measured s sup sup 1990), the I] required for are kind and of is − The en of as stars ha onen prop that w is 1997), and is 1 in (this as v of wind of not men ould t the ergian erno AL. in 5). v elo v more v no measured v the and these a in other the H rep a accoun +299 e is elo elo y the a broadening is y inside Chev velo this of α t T difference osed ma other cit a field b at is ab evidence though the explosion plausible, tioned S-shap the able orted one v cit cit presen of corresp een H On and th nebular & ev with mo w a lo same y y an to city out t complex α stars in y nebula. y an e hand, us alier remnan en km cated con Moiseev profiles ted case to outer stars, displa is dels detected obtain a comp and 2 explain this the similar of the t, [OI v 10 energy require in field a parameters ed +247 while b t tribute erage w b s for onds for suc sho (1974) e ab 51 − FWHM of efore, o of a I in T to [OI other at [OI in systemic 1 cen v if nebula. I] candidates y ys could since onen regions while able t out erg. er [OI the h b that of w The strong in 10 (with of as the w (SNR) sev the radial y large I 2007), the km helio I the tral simple input to as I] tensities I] e (Ric UV the at 52 the to I a the for t bubble for +279 eral I] in Ho hand, 3. line assume the eastern v comp non-thermal energetic most t case, accoun deriv s detected erg there least partially of bubble elo ypical b − cen v S-shapp her emission en S/N=6) diameter for w N103 a surrounding addition stellar elo bubbles o W v 1 b v A then, but 20 places. ev t dy near elo cit SNR tire elo y and as ypical (with tric t e to ed km cit this onen et er, redshifted a the , the extreme N186E b y km most, cit are see the cit t whic no et sup that p y SN old (Am ph al. field energetics. v profiles, narro b the it for eriphery y winds in e y w s o nebula elo ionize profiles. input t y presence energetics d , − s that S/N=4). v and ysical other initial no (P een presen should F erno v profiles bubbles − explosion. the to 2001). er n applying 1 SNRs h c the alue urthermore, cit bro this geometrical 1 , this um entr radio a ark (Rosado at w has blue the and whic the y the v a the v radiativ group is applying cio-Cruz the in b elo H a er v v a of signs are prop al of energy resp t cen er bubble nebula elo elo found. of α b a explo- in whole helio- DEM emis- emis- +279 split- et cities 7 h of main sho most e stars b bub- ha suc S/N 2 The also o this cit cit and tral can the the no- km ec- dy er- w al. 44 v in et of of A w h y y e e e , © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México time The (DEM N119 and this nen winds range the s mec (1.05 where ratio cen 119 shap from densit bles from lar trying with tion ogy ph the sp SNR, the t (2.4 The N bubbles [SI a flux idence in sion. w − terior SNR, ectiv 1 o ysical 119 I]/H 5. tral )(profiles Figure In N119 The The winds t × hanisms strong nature northern of can of (1.3 could nature ed comp of p × blueshifted a in the of the Ho 10 UV nebula, DISCUSSION y-b or the ossible the 10 of to from b the L132b). ely). them α for bubble sev b 50 nebulae Lyman conspicuous y the 330, suc OB × w (DEM b prop p o 51 line-ratios, ounded seems 6 in surrounding e next the ev (DEM observ Ch dy ossibly 10 onen S/N ph eral b the S-shap stellar 5 of h terpret cm of in ph e field er, , 50 W stars taking The can and u also 3 erties as terpreted and detection and resp Bubble naturally s the v around ∼ olf-Ra − t, p section, & ph t no observ Indeed, elo flux L123) s and yp to 1 ossibilit 6. ations non-thermal formed 4. − L132b b is nebula, ) v the other ed the energy Mac winds ectiv 1 w largest sho other that cit southern e elo s es and CONCLUSIONS ) the con − of e 277–281 place measured formed ha 4 shap cen OF y 1 y is suggest emission cit of ws remnan DEM NEBULAE ations et ). these imply tain the ISM. ely of v Lo kinematic a the of v w ha larger as redshifted formed y y tral of e Bubble bubbles signatures of b alues So THE discussion (WR KINEMA e the requiremen e at w . nebula b y in Figure v that the comp WR a diffuse ha the of een e one three w the (1990) L123 least b bubbles regions b this W km of result the t not v that y e the v o radio b e OB than ORIGIN of of elo e dy massiv of found. bubble) this ha the y McGee star deriv b onen detected action and s formed ha y (DEM existence complex. Smith a the nebular 5) in b expanding − cit v is field the of it X-ra TIC e ( the een asso 1 of h v is of Of will emission ∼ nebula still . y Br some the of e is yp ts ed and are WR here ts N fain +395 the a e the In Consequen estimated profiles. a main and and y in erno ciation the detected of of 119. et in 21 marginal from FIELD b ( and L123) et OF WR one uncertain. b teraction ∼ detected emission ter addition sho e for terior presence nebula, complex a y directions. one the sup al. al. +255 inside presen of The WR morphol- v S-shap is case km differen THE a wn the regions, O bubble- comp nebula. deriv or our sev erp an (1972) (1987) stellar explo- of is LH41 stars stars OF bub- high s stel- that first The of still eral y osi- − tly ted the the the H km old ev- re- et. ed ed to in o- in 1 of of N α a t ) , THE S-SHAPED F ation Georgelin, w Da 123 Ardeb Caplan, M Henize, Am a N119 uncertain; the Arp, Con that from effect, the tion). lision bubbles. t Another Con to from Ch only brigh no coincide sev Chev ha b tion ral w east, o ell h ´ exico. v v o dy) vies, u, the eral yp RAS, MNRAS, NASA) P G., 1972, and bro shap a According F The According e ti, ti, minim nebula. main of . alier, w of rom with H. Y.-H., tness explosion apparen differen DGAP erno regions 1997, erg, gran could b M. e P cio-Cruz, and In & b P in the et W an R. K. bubbles . 1992, ha J., y e . A&AS, 81, spatially teraction S., p Rosado, W., w observ olf-Ra adition, authors of S., v R. . A., the the In v ts D., ossibilit Y. b G. um original of een w consequen & a four NEBULA 1986, A&A, e & o b & 89 N119 A, 121, e t A. detected; explosion. dy Thac the 46054-F e Deharv surrounding fa t MNRAS, & 1956, M., Brunet, Elliott, Mac suggest 132a ionization, to Massey systemic complexit to the due y v or of P Univ ations 1974, at bubbles et 6, Underhill, or (pressumably A&A, 337 ., zone. these M. . 319, Georgelin, k these some the y could REFERENCES 249 can Lo Stars of differen era La differen molecular ApJS, The to ac of bubble,the is eng, 1983, ersidad w, tly , K. v ApJ, kno the y J. N119 973 the differen al, that this that at P from 258, , this results, b 155, Ho , . of M. A. spiral v M., (NASA results, b P e y L. can the 1989, wledge 8 elo A., 2, ., e sev winds w in the A&AS, t t the due 188, D., of A. microns ho 1990, scenario 800 1985, it the pro ev 297 Maurice, teraction 315 & Y. systemic nebulae cities Conacyt h Nacional eral Marcelin, b w the t is cloud er, ionized yp , & B. Meaburn, e massiv shap ApJ, w duced ev P 501 to systemic 132b shap SP-497) a the seen W ., e and othesis ApJ, the A&AS, some er, (ed.) expanding 54, v p financial think and esselink, the La elo osible e the 337, (no e zone is do w E., v 459 bubble of spiral e p as v b gas of cit al, 365, of and eak M., ossible of elo Aut´ in y they es 1988, in the w photo N119 of (W J. that the y 62, a & 251 teraction N119 the v terior the A., not matc cities. remnan ens. the elo of pro & profiles a 510 1976, onoma A. ashington: Pr IN100606 increased 63 shap detected ma true p and cities supp Monnet, bubbles bubbles Amram, in O the disso ´ ev explain J. cen jection can erfora- h h is terac- y stars. ot, yp 1960, Stars Mm- v e spi- tral col- due t 363 not the ery ort er- ci- b de in L. of of of of e © Copyright 2008: Instituto de Astronomía, Universidad Nacional Autónoma de México Massey Martins, Luc McGee, Massey Maeder, Meaburn, Lozinsk Le Ko P 364 P Israel, Kim, E. Kim, M. . . Am esterk Amram, Coarer, Ev d’Astroph 26 2000, lo 436, Aust. 503, RAS, & Sc Saulte, M. Rosado: k M D.F., P CEDEX ([email protected]). e, Lecoarer: q., aseo S., hm ´ S., Goldes, exico, olution, bro F. 1999, , , P a 1049 674 R. P y . Sta utz, A. W e, P AJ, F., Dopita, 206, J. a, P . B., Mexico J., ., cio-Cruz: de J., olf-Ra ., 1999, X., E., 1996, v L., T. Ph W D.F., Instituto AJ, eley-Smith, et A. Sc McGee, W. ysique), 4, & 119, Kestev la G. 705 aterhouse, ys., ed. A., Bro Rosado, haerer, al. Ho F Hamann, La Reforma y 1991, 118, IA 1993, Lab rance Pro M. et 2214 ([email protected]). & 1993, Mexico 25, dge, oks, J. v U al, en, Instituto Stars Moiseev, c. R. A., oratoire 39 2797 M. Circ., 581 de A&A, A&A, D., J. 33rd P ([email protected]). M., M., and X., A&A, L., . Sta Astronom V E., W., W. 880, W.-R., in & ([email protected]) reux, & & Dopita, 7290, Georgelin, v Li D. 248, 280, eley-Smith, Hillier, the & A. 1970, McConnell, Newton, & de ` ege 276, Lomas d’Astroph Russeil: DeGioia-East V. Batc et Astronom 1 166 F 365 In W ramew ´ M. 25 AJ, 2007, ıa, al. tern. essolo D. helor, L. Y. A., de Univ (Li 75, J. LAM, MNRAS, L., M. ork Astroph. D. P San wski, F ` ysique ege: AMBR 2005, ., 171 R. reeman, ´ ıa, ersidad 1998, 1984, & Viale, w of ta A. o Univ Institut Bessell, o Observ Stellar U., F A&A, d, 1972, ApJ, e, MN- OCIO-CR Col- 381, de K., A., Nacional ersidad K. 01210, & atoire Grenoble, and M Nacional UZ P Ric Rosado, Rohlfs, Rosado, W Smith, W Stahl, Stothers, Szeifert, V W W V Aut´ ´ exico, ark de acca, an Dpto. esselink, ea alb alb her, the Hesser, F Mo J., 320, Stahl, R., 131 A&A, 460, ET v Genderen, er, onoma eitzinger, Marseille, orn, orn, er, O., & ore, W. & Magellanic A. M. J. AL. D.F., B.P 609 914 de M. M., K., Aut´ de R., T., R. V N. N. 318, O., W W., D., M., A. R. o & G., F . 1986, Gro els, olf, de B., et ´ R. R., ısica, onoma Humphreys, Mc Kreitsc D. W J. 1977, Garman Mexico. et J. 81 Cornett, et 53 A. al. M ot, 1977, olf, B., S. & 2, Lennon, 1956, Bohlender al. V. ´ Cra al. exico, A&A, M., 1990, Clouds, Chin, 1995, Univ Place M. Leitherer, B., ApJ, 1999, 1984, Grenoble hmann, 2001, de y ApJ, y , Sterk MNRAS, 1984, , & R. M ersidad R., Ap C. A&A, 160, P C. D. 218, IA Le A&A, ASP ´ R., exico, Zic ed. A&A, H., D., 215, en, (San do. 1996, U Castor, J., A&A, 211 kgraf, V J., C., Y.-H. 377 Da , Symp. & 238, C., & errier, 70-264, Haser, 107, 53 116, Ib CEDEX 137, F Ap vidson, Sh 370, Zic Hill, ApJ, rancisco: Siegman, & eroamericana, 140, ull, 315 F. Ch do. kgraf, 104 J., de 3 343 190, 34 S. 13248 R. 1996, u, 468, J. 04510, Gro 459 70-264, Shapiro, K., M., N. M. S. New F., ASP), ot, 9, 842 Sun 1987, A&A, B. 1996, Kudritzki, Jones, Marseille Krautter, M. M Views tzeff, F 04510, C., ´ exico, rance P 237 Prol. 1997, ApJ, ApJ, ., 314, T., of J. & &