© 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya con in scale p galaxy morphology Key tam F trends 200 framew abnormalit L´ non-star-forming to n 500 to t clusters apparen disk-wide compactos resultados alb se 44 densit acerca Duran M agotada que estrellas Luis la los R yp uev or M82 or actea. evMexAA ´ exico v 1 distribuci´ cono the estigar the eit tin e Lo morfologistas Instituto bi la decades, Myr c Wor la os Enrique um 17.6 ´ under ´ en y cated uamen te . at com (ydm@inao exp line raz´ cen de ork ce resultados and tly The in La ds: ulos AS en duran p d ago, lo p on ´ burst o ecadas que ected el tral la imp binacion the y c 100 of similares w distinct of co formaci´ galaxies: galaxies: Nacional on (Serie the the at te and efecto situation arcsec to Erro estelares galaxia the principal A M82 lev with sigh te usual ortan Milky M82 500 radial 1. p Ma only in form for lies ep.mx). name or els, GALAXY: un stellar n a v spiral el INTR 1, t. nos. uclear ˜ estigate concernien − de on as the p global in un normal morphological tes de no n mo 1 de in structure en individual a c en T The o W of tro en ; ucleo ´ de Confer a ccurring onan estelar j´ is F zone, giga distance extinci´ ov Irr detr´ sobre the es do Astrof a disk El the su arm, ODUCTION reedman galaxy masa ducir y con general. c la , enes. starburst hanging halo una de de registro tzin but con I the galaxies form as de rotation densidad a I ten star ´ ısica encias) no. ˜ that la hidden brote in tes tla, que on or un tenido de p . starburst galaxia (M82) an of t teracciones o morfolog El con ero of It v MORPHOLOGY formation Examinamos of amorphous. y of al et Optica erall su tip ´ M82 C.P order subsiste En con disco f´ o app is tin 3.63 una hace osil has h al. that un v its esquema , curv o aparen from er undreds . kno del 37 — estelar tains uously los Y. morfol´ earance effect que 72840, 1994), del is orden disk pron the tak ´ of , Mp y cerca ıa con galaxies: had en e. wn gas 44–55 D. also ultimos ´ Electr´ the magnitude DISK y brote est´ en en siga The te more completely c last la tiene unciada and el for Ma of prompted con ogico y for general a (image of de M82 Puebla, de la all div optical galaxia un con cuidadosamen It are la in onica, restringida los yy disk (2009) decade, almost compact estelar ev 500 usual o halo. magnitud ABSTRA teraction evidencia ersa starburst un than the is RESUMEN forma tenido v a a its is oluci´ acorde er nos AND ˜ patrones 1 no formed inclinaci´ brazo Ma and de limeligh view y p a morfolog M82 w ounger. 200 in quenc the eculiar In la half on en nos, giga ˜ with de estelar M82 AND b Luis star its denominado situaci´ el this — tire mak burst giv with one CT eing de morphologists on a b espiral de y ha HALO m´ la a almost y y oung te disco con esp hed on una stellar ear. t as galaxies: e the M82. the cen curv como a clusters, formaci´ star ´ acaparado Carrasco e of ıa, in review, range cada The it del understo the erados com en j´ and on la it ov around STELLAR tury regi´ the publication M82 ev y es compact a sin a W formation la formaci´ disco enes, ace all an presen bination con ha olution filamen galaxia. de una e visually su on the most direcci´ of on formaci´ that star of carefully IrrI en with w en in rotaci´ 1 similar ten cam historia cen o electromagnetic y e its 100 de que teresting estelar to asso la d forma t galaxias I del on t, clusters discuss observ tary M82 tral biado star star of in stars las o that on atenci´ v with on. of Myr on of Desde los ery history estelar ciated app tro halo. amorfo. M82. in de anormalidades extinction de some formation de examine clusters. distribution p as de CONTENT estelar, duce c El through ed the ealing little eculiar mass con ago. um ´ on evidence la — these 500 ob cien normales, a ba En disco , hace ob galactic en visual. ulos galaxy galaxies: in ject main radial imp a jo la Ahora jects. tos ´ p discussion esta The v el to separate c estig´ morphology no recen niv publicaci´ de eac sp ortan cerca a disco form´ globulares que The of and that de is burst revisi´ visible for reasons ectrum. fossil el distribution El formaci´ h do restricted andose sup of The study c se lo t stellar um ´ con observ que o high of t esn’t disk halo star completamen of findings de dust, que ha morphological erwinds casi results on OF mo ulos record the tiene on n on the en ha medio uclear establecido discutimos inclination on in , formation, b con de de m follo condujo con adas de to M82 de ehind It observ el not estelares but o globular uy THE en the das estelar, currido M82 m´ around tains ten on la optico ´ is in v of of w along tirely as arios p star- para siglo only as also t V o one gas the the the the sus en- its de ed co — ´ es te ıa a a a © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya discuss a cleus cen is disk the our and disk of of cuss w b cally & (1978) ma H recen rest and Ho fully § under burst then, co of prominen a 500 arc mass or of more M82 b gered ac sim y oth as α v 7. galaxy v hew Miller compact the to the in w ast y het a ery tral ulations In The The Though Holm 2.1 n filamen neigh p ev “Amorphous” , b termitten referred its Concluding (1–3 and the b ucleus. t phenomenon mem explaining and to than summarize y c in M82 activit yp b e ma the stars . er, § brigh y 1977; the y and of the in these kiloparsec, curren n ears. exotic witnessing 2. The . stars e 2, its significance b the (1964) uclear an t b jorit kp the b in erg size, a for orho 200 n THE bursts framew w ts ers star classical w test formed suggest terest there uclear c) Riek neigh y encoun Y as halo nucle bridge to e prop There bar. y t that t (F¨ un, (1950), in the idea are of compact briefly o bursts of and starburst giv ev clusters due as infrared all d. CENTRAL orster remarks e the the the b o are exist ar them olutionary erties Ho, discussed ork in starburst The en et related ccurring or b an w whic the region on ter in The the that y are harb to w of ere M81 starburst of n M82 discussed kno al. a orks M81 Sandage the ucleus the explo I0 for & discuss of the b formation prop inn Sc in the h imp morphological discuss clusters, influenc suggestions in principal in et though the ors ob wn Lo (1980), tergalactic o are hreib b a group includes bursts the nature w umerable as of ccupies the to y of disco the jects presence and ortan in ding erties een starburst in starburst 1993). phenomenon. KILOP around prop de is status giv O’Connell a M82 the last the disk. and the er §§ framew & in the going t galaxy e v M82 (Gottesman en subsequen V p in are t ery galaxy of to 3 the et Brucato of erties of § aim starburst aucouleurs opularly last a 30 observ the prop its n and is in 5. the M82 region ARSEC that M82 are studies al. a b the uclear concen 6 of of gas and Myr, on e latter § considered in mo new ork lar 10 In of × class starburst is high a 4. erties ejected sky 2001). 8. discussed of inner & b M82 in w ge-sc 10 in ed § this as Myr. del. p connecting gro y NGC3077, of The (1979). ere t opulation of . 6, Mangano galaxy kno M82 starburst 8 with trated the The M82, Sandage a on activit of features success- v M82 Histori- & wing N-b M82 around M w elo galaxy is review ale (1959) stellar put of wn e outer W Since Irr Most M82, Star- form from

trig- cit and o dis- dis- t n the eli- w w dy AS an as as u- to in in in in of I It y y o e I . A GALAXY and ev iden w Sup et p emitting & minor than siv 10 a the burst 43–52 Sc dius H (color) H left ance at origin stitutes of sists tion panel cen fact uum in the gated dust in that sp tablished Sc infrared stars co The tec 2.2 erwinds, ere α α en to patc v hreib hmidt ectra 2 half W e al. broad-line hnology kp the er tly . The The It tified tually images obscuring er Spitzer images panel called stars observ a disco ea (Shen the The kinematical of rotates in and emission c 4 orbiting is a 2008, region, of h bubbles, (Sandage Star bip mag Oh axis v maxim ab y comp er halo. filamen bar mag in nature the er of almost t these bands, Figure v et w disk app called teresting c gas y them o olar ered the in that of et entr the o whic v ama ations w & tak Clusters telescop 1999). if b of of al. e SSCs). halo these ere slo Figure osite al. comp earance of ecame compact there um the dust (at Lo dust H as b ligh ∼ Bland outflo al in the en arising tary halo b of Sup (1976) m y wly h α and et y 1 dust-free visual allo 2001). historically 1 & galactic uc the as the radial 1995). (FWHM) data cone-shap b the to galactic with are FWHM (Engelbrac t kp image, emitting erclusters onen al. clusters y , resides galaxy Miller The is h is w e with 2 tak The 1 scattered w narro note is a the Visv c Hubble same off-planar ed in ha v ob & of (O’Connell (2002) mixed (Oh a traced from length and ailable o illustrated extinction are ts: Subaru en Surrounding the jects v v molecular the cen orbits T T the The that energy second er e anathan the formed w-line c vision elesco y name. ully 1964). plane in b omp up 300 confirmed the is ama Scarrott fully almost tral ed y Bulge cone < the argued optical Space a on a h halo with established disk. Carrasco released b as patc recen t fain 200 to at b foreground onents: y along (1988) telescop structures first the km structures y surfaces et starburst et (Lehnert, lib so emission et comp of consisten are the using distances these Ho et T t h & a in the if H km the al. on ring photographic al. t erated The elescop y al. to s bands M82 exp decade α comp et − Sandage al. w the observ the the illustrated optical this the H et 2006). as 1 s b ev 2002). onen as emission dust stars (1991) and ) − The al. e, α onen the e of 1995; w mid al. er, 1 of the and ma that of in galactic b activ e a presence ) in onen (full t and screen seen bar region 400 from with ottom-left v (1991) Hec along b t organized (HST) (1986) ations t B explosiv as elengths. more p efore with Bar the tial particles w jorit (F¨ the imaging infrared consists app olariza- , (1972), con o Ma it e to V kman, t (Wills p far orster images width X-ra in more elon- mas- c star- is near con- con- halo y as top- and ear- they and and dis- tin- yy has the the the had and su- ra- es- re- b 45 as in of of y y a a e © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya Fig. 46 ( estimated bi-conical due dynamical et p part seen with minor ab most w tral normal in the profiles from B onen as o al. V the Ho v to en 1. 2 probably of e that most and prominen 2000). Ma t axis w righ tire kp the that the Multi-band at late (see big yy c. structure H the t fact a of these HST of galaxy a, mass α exp panel A mass is t ) The the Figure yp this bar Carrasco, t M82’s in Subaru that near ected e I-band structure terpreted w galaxy in bar galaxy dominates of of mass a views as along v individual the infrared ∼ elengths. Figure 2) bulge? con for the image 10 image in sho concen . cen of & the tributes 10 is an The the bulge as w M82 Luna tral M the 1, minor Sofue o exp (top-left), (NIR) is stars an coming v

Spitzer where near trated er sho cen illustrating region. for onen of excess (2005) substan a wn tral (1998) and axis. smo what infrared the comp it image, tial within in from bar, compact w can oth en n Sofue In the e is tially uclear disk, osite w in tire see the the as b presen disk whic MA the terpreted b trace in e the ottom-righ galaxy tensit the once clearly (1998) NIR in image to whic YY bulge star h com- ligh terpla cen- the is the ted stellar A ( h y a clusters completely t J , & distribution H y t CARRASCO K b panel. disk et ; w top-righ explained face cleus the and M82 ha comp mass dust are een 3.1 and v Detailed e obscured resolv Notice observ . photometric ga stars, along of is onen lo and with Optic the v t), ok P hindered e 3. MORPHOLOGY AH ed ed the and t an in ed the gas dust a al the THE b in in y optical maxim particles for terms excess upp and bar. Spitzer grain and Sofue this the line lanes, kinematical INNER analysis er b ne dust. image. Gaffney y y optical of um of ar (1998). n surface limit app the and 3.6 uclear with sigh the infr size In earance µ obscuration (1–3 hot of image. t, m con of , the ar the AND Lester, of the photometric whic Ho ligh (b e 10 dust. evidence tribution d 7.5 KPC) color ottom-left) H w 7 of surfac t profiles α ev h D Filamen M can p the emission A YNAMICS er, is & c. comp

zo DISK: exp e T caused image, a b for for om elesco from e photometry detailed suggest osite ts ected completely analysis images, the the of along tracing whic the the b (1993) optical y bulge bulge giv that sur- SW h n the the the en u- of is a © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya w confirm the tiv R as ure attempt brigh ligh found whic these the illustrated steep at tronographic suffers Fig. R the to those the the tral images M82. cated sky-plane a G G the v ely shorter a Blac t. obscuring elengths, < large part. inner ∼ disk 2), n 2. h tness bump increase ucleus. bands. exp of The bluer 90 radii It that can 90 considerably ev Multi-band kman, where their 00 normal, to can of onen inclination − en comp w (77 and n in b is a obtain um the in — M82, 150 there e Notice v at also of suggesting ◦ Figure tial images elengths. not dust On findings attributed ). R b w Axon, the a onen 00 in 2 ers profiles G e . c tensities scale late Disk haracteristic b kp using the affected can > is can The radial the a radial e at t lo c 1. of detailed 210 noticed in evidence or w & t the length ( other gradual yp b using outside clearly ∼ the The er bump for e the that 00 the T disk surface e to in easily 120 in top-righ extinction are a b spiral ylor disk tensit the galacto bar y scattering B photographic hand, in new in the 00 b surface indistinguishable flattening is ) the see y prop the for arcseconds and NIR this traced is of (1979) distance brigh stronger dust excess y t galaxies. digital resp the the dust. cen cen corner an the ert profiles V bands figure, — tness photometry -bands. onsible particles. y tral tric galaxy in enhancemen enhancemen of of made NIR nev ligh of the a data in the ligh corresp These at in w profiles and distances starburst scattered ertheless Bet t that b the a M82 the shorter surface optical et y is profiles t for a to They (Fig- w w from from from rela- elec- indi- first cen- ond een een the W the are the AS of of e t t A GALAXY tion a images, spiral alw whic to burst sim irregular from tral spiral mem ties bled t Mangano presence suggested (1979), b tered morphological smo lengths, ages phous profiles images tions exp prop of exp The an the individual whic the atically morphological (I) distribution. where images phous of yp eing 3.2 metho M82, the Figure a e ulations Ma The It onen ected excess band bar, othen defining of ys h h t ert . shortest b of that is (Sc/Irr) yp sev suggested (b ers ligh ma arms The NGC arms yy app end it the is app M82 susp y (Mutc caused fain based sho classification e– increasing and at d ottom-left tial breaks eral first a, pa of is y c asso galaxy as to t of of p (1978) haracteristic 1. the earance that earance of observ spir R of w are stars t ving opularized b Carrasco, spiral ected difficult progressiv of (Y function, using late-t 972 in –its M81 can G represen e photographic criteria kiloparsec In noticed scale-length hler ciated the NIR on A the galaxies. images. un the al structures b recalled class > comparable M82 do t the . the the y (Ma the the mass, b arms or ed ha mid in bar yp 1999); arms, group 60 wn et The the in graininess the e at seen on ligh panel o v v presence teraction 00 e this to seen scale-length al. stellar with v b radial yy ery e assigned t of w shorter b for at (Barnes ely with & spiral unsharp erall y can infrared dust the b y The t noted a presence and the a explain of luminosit Irr 2007), y on that y one distances Blac analyzing the predicted Luna T amorphous cen feeding o the et and Da in decreases of is v elesco the dust to ground-based b I the the images er scale-length in structure the con scattering I to tral complexes” e al. galaxies, of reac resolution vid the kman, Figure w tensit do the of ev that Irr visualize of individual v & the cen esp to y (2005) masking a the tribution ground scale-lengths those ery w Irr the en 1998). es v spiral part, this Malin of hed disks et of Hernquist b y a elengths (47 I “failure tral M82. ecially , v ottom-righ to not I the exp clearest y the (Malin II deep at elengths, w spiral al. the size, transp Axon, at (or 1). galaxy: 00 galaxy profile ell in all of of rather classific there disco arms, con starburst arcsec onen (Ev whic (1991). = gross for generation based of longer O’Connell n the the tec fitted of M82 amorphous) normal the w uclear J mean in of stars. optical The The 0 tradict HST/A arms ans — H to ort as amplifica- 1978). . hnique v & tial examples the h 8 the is the 1992). analysis, K with ered inheren K without than system- N-b w prop t again Spitzer kp acts ation images resolv resolu- clearly one resem- T -band, 1994). of amor- amor- a b -band w panel sp a F814 mass scat- y disk, star- y w c) a ylor o and late im- gas the the the ere CS v ec- er- up dy an an — 47 In to of of e- & is a e t © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya tected b optical with 1984). comp it disk galaxy some than decreased cally searc fects ligh ago, ages. ev emission M82 star-forming quires forming the image. with M82 preferred arms. relativ Figure b rotation traced Fig. 48 scale K y y -band er, is mass subtracting Late-t In t, arms. 3. not hing the as mak the image is has onen can less the times (1) and ely Ho one only normal Illustration The in Ho 3, is images a The will residual of surprising stars b neutral gross in e w yp stopp asso w the prominen late-t the b abnormally w surroundings op t eing spiral con stars (3) to ev 3.3 e e the ev sho after W ev absence ev the e en ellipse b displa partly er, HI H trace er, ciation trast e en spiral high e . en at the ws an as prop yp galaxies, ed an α arms exp The detection I find optical discussed image gas arms subtracting most NIR in b presen and e regions, high the of exp forming imp ey nearly y ected t that with obscuration the of spiral erties the o galaxies of extending gas the ond, the at that v of (pitc onen spiral the the gas-ric band ercome ossible of — (con as a underlying t. the and NIR the making spiral the and arro for mo the the dominating 30–40% spirals the discussed edge-on tial h (SBc), B arms of the in In the tours), stars star NIR arms deled trailing -band angle=14 spiral NIR ws has h images. disk dust the are the § spiral fact, task. optical arms disk b arms disco all with 4. y indicates forming due caused the a smo at w ric that are w whic gas spiral using whic image the c (Y a arms images orien In stellar dis-adv a ontent from the of spiral h v v around The ab v arms to the of oung elengths. oth ery spirals elengths. generally is ◦ disk. in bulge, M82. the w h h b o ) en the est a M82 tation concen v the b is w could suggest arms regions gas the y of gas first e. exp the of y tire arms. as con absence an due up & consisten are matc MA the M82 The scattered dust, 100 arms NIR con observ obtained tage onen in and fraction Sco sense are tin to, t disk in b trated w trinsi- to of YY Th easily spiral Ho bluer h e gra ten uum with o Myr that ville as and tial im- not the the the the de- the (2) us, for re- A ef- w- ed of of y- of t, a t & CARRASCO with of lo are v in CO age. zone former. optical that in length matter consisten the cen profile. radius, et 170 whereas distribution emission up the used sev are rotation suggests ing (2) suggest Na idences the from in and for the tribution in of 1993; this ery cit the the the the the al. the eral tral 00 W The Almost the to sp absorption dust sho cluster direction ∼ literature b mass y , the radius The little the y the the for e long-slit (1990) ectral Ma W starburst spiral measured cen disk disk. 50% a rotation wn 48 Sofue 3.4 tracers, with studies presence bar compiled halo, Significan are: their alter, rotation Ho the curv halo, radius at a t y and an CO data disk 00 resulting of tral . is all , with in to visual colors w of all can parsec The but lo the energy the Ro of masses exp arms. ev concen e obtained (1) (1998)) (1960) and w Figure of and absorption the in M82 1 and mass with of W has p using er, sp mass. er. lines, dr with terstellar b curv region an kp of ermit most mass onen its v mass of eiss, using sp e the ectra ´ alue extinction curv all ıguez-Merino tly suggest observ hence H b c b fits re-calculated scales asso 170 Ho Sofue is exp dust ectra companion trated distribution oth estimated HI een , outside e I region. estimated the 4. b tial the H is whose gas-p there In distribution e & w lines. of oth is and deriv to a 00 outside I is onen α the ciated substan and ev It . of the mo result ed regions in the rotation the Sco reac a it lines, the emission reliable mass (Ma all (1998) origin the er, stellar can Ma factor M82 mass-to-light within o the deled cold is ed is tial v tracers ville or. There strength of this radial m In en elo the hed observ there yy y presence no w with ulti-band b b that from all the a ∼ tire whereas inner tially distribution M81 all et arp cities. mass y a e has of (Go gas not the mass 1 w radius found and of to evidence 2002). at curv v Go seen et outside (1960) al. the lies a mag elo these zone exists the ed is n the mass the ed 2.5 y giv obtain the uclear etz a al. (Y b tracers etz maxim ev higher disk. ample gaseous surface and cit e to een 2010), south of rotation radius in e cen that of disk un, en The higher inferred stars using that (see 2008). Sofue con y b et et K a r photometry studies, 4 3 Th the outside gas extinguish- atio et and tral this detectable line × deriv data for maxim -band These the al. Ho, kp al. starburst w tributing um w the obtained p us evidence than of the 10 (HI and most een and n eak densit outside ards c of tracers optical for a (1998) (1990) radius ucleus 1990), Go 1 9 radial width scale- curv m ed & sho mass mass M p from dark con- 30 and kp uc 70– eak im- gas um the the the the ev- v (3) etz Lo

in in of e- 00 w h y e c , , © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya is dius The & band 15% of stars stellar v with t exp ties galaxy the zone, lo Giv mass sisten (solid 48 in tion line main Fig. The ing zon denote (b and ypical elo cities ottom) 00 in the Sco M tal W ected en cold corresp is the cities. circular 4. measured effect that resulting of of the /L almost the that t of e and luminosit ville b sho cone error that absorption the with The 1 b o obtained range measured stars the K 2 dy gas y kp A–F v wn is form × to also elo of are Morgan onds errors indicates 1984). en of c rotation b disk bars inside, 10 the the (top) b adding cit v b oth b of are tirely y elo gas v more sp e 9 y along b of y alue y to radius the v same, y M com ectral more denote mass the measuremen cities alues in the in solar-lik the that b atomic and F the lines

and (1958). y solid concen or the massiv an curv is the bining the M that these outside HI rotation in where 0 in comparison, optical stellar deriv represen is classification exp in /L Keplerian . measured the suc e 15 same line. the off-planar and outflo the e. trated and and K the onen the e  h tracers b the ed the b than ts. The of eam 0 as CO this radial and ottom curv mass . radial tracers, molecular plane. b 05 disk tial wing tativ the disk measured the The y within size v M ha outside observ e Go the ISM zone, elo ma disk streamers, for disk mo M

Balmer panel. v e is zone mass v from assigned etz zone e cities. ertical /L in Sun, y /L of a del Hence, dominated absorption b esp the of not whic mass ed K the outside een et K the v this outside gas the and

scale for (70–170 elo ecially The al. consisten 30 = lo . represen error lines, The top h detected distribu- cities A w M82 00 M82 circular (Y n 1 for radius). (1990). the the is v t dotted uclear length radius elo if v panel oung a least hori- con- alue bars this 70 line the the are v K ra- us- 00 re- AS ci- b e- ). y 00 t t - A GALAXY corresp o threw lar. obtained resp the million around optical 60 halo. tus tion to color-magnitude can tion star-burst. relativ The that along is dances w to signatures of sp tra nan ric with suggests 0 More inner mean mo for 4.3 v . as 9 er ectra 00 sho hed that the 4. a del,  A Ma Comparison F t the iden to of . ect b radius The 4.1 part features rom p a almost that stellar late-t e Sp THE mean 0 wn In recen disk osition the age, e imp the yy those more (Origlia . width inner onding found . 1 0.5 of patc giv y disk to of atial tification (2–2.7 in this outer ears, 4.2 a A that b Gyr. in the of tensities ma is ortan inner elemen the es ge y yp the of Gyr. t on of as INNER et Detailed . h p ages all ly Figure a ligh a from study in disk, section, marginally e are opulation of an jor of Glob a v of in discussions kno M82 the compared al. the inner the inner terior burst sp eraging to r et galaxy the disk tly kp esolve 40–50 of t the and slit Ma The age diagrams ectra axis sho ts of greater wn radius al (2006) not al. , c α a northeast p the burst b of observ has (1–3 yy ostp some 6. dominant in Single the y radial along wn part seen disk elemen Star outer lasting mo of w to resulting 2004). as CONTENT d . star 00 of a only the Da features sho e the . cold, F star on 0.5 et a deling oning 110 in discuss “M82-B”. urther M82 Detailed more KPC) sp ≤ Sp ha to vidge sp of of immediately used formation ab than ed w lo c Ca al. the either Figure long-slit for disk, ectra Stellar zone) ving ts ounting 110 ectrum on ectra. 00 Gyr the w those the o formation a These for side w stellar v radius (2006). to are sligh stel I star e, the arm the M ma ev of the 00 in I the (2008a) DISK: 0.7 age-sensitiv details the disk, only but completely for age /L olv are it K side are encloses these suggest the lar jor systematically 5. for analysis P discussions resolv t formation ev are The corresp and is Gyr. sp long-slit K results mass ed & opulation difference history the also (i.e. Eac strikingly date olutionary p a , axis not with observ of ectra a clear opulation STELLAR after H history unmistak of and as data few using four normal neutral the ed p h that lines, of opulations the the consisten < a the as The compared onding sp an p e of red spatially that h a ed n the a stopp ertinen p absorp- suggest ectra sp sp 2 undred history w ucleus. the opula- brigh mo age y ma of (SSP) of in abun- domi- fr ell kp sp ectra ectra simi- oung stars 160 with able om disk disk gas, sta- the the the the en- del ec- jor c). IR ed 49 as to of is 00 t t t © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya in formed stars Sup p magnitude lished iso predicted A tion genitors to the the the (A results image w galacto the Deep T R WIR Fig. 50 the opulating elescop ere GB -band. GBs) the c the One hrones er burst brigh brigh detection disk 5. limits Cam used. that wide-field phase are en cen the Gian burst for relativ Blue of in e of tire ter test is tric sho Sp nature instrumen the b are (CFHT) absence of these of M82. the diagrams The the ts y at not ecifically wn A part disk. mo distances Girardi the stars ely outer us of (RSGs). older GBs these aims CMDs images exp b del, exp stars the y recen of (Ma of CFHT He the of osures seen b disk ected w star ts than ages, the the , of eing (CMDs), asymptotic ere et yy are these found r of tly on arro are tak 0 Da a , ma F al. and longw formation 60 disk , observ rom the 0.5 used whic of i sligh en suc w to ws. et vidge’s 0 the 00 jor , (2002), ere , relativ a halo that z with 110 Gyr. Canada-F h con al. should few 0 h Prominen ard tly the Da axis A , in as ations. long are GB J 00 tain to 2006). vidge gian , the OB , more solar the his study of ely analysis and According sp stars in H the ab enough stars. mostly ectra the t brigh stars, stars Me w the o y and 160 rance-Ha Additionally t firmly v branc masses, next ounger ork massiv e w age-sensitiv are gaCam traditional According 00 inner the as MA extracted test The K of that are and to to section. in con h to -bands to estab- detec- YY color- e allo trace sho stars stars stars their with pro- disk w Red tain test and and the are A aii wn. w , e & on features Appro CARRASCO either of y repro (2–4 Fig. ounger ximate the are side The 6. duces kp observ indicated. c) Star of i as 0 p -band ositions is the b compared est ed repro formation cen disk the luminosit ter duced of observ mass the at to history extracted three in the is ed y pro function the prop relativ radial of duced top erties. the sp panel ely ectra for zones in disk More fain the the on of of cen ter burst. inner an Figure M82 than tered A optical GBs. disk 90% that at 7. © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya the is part half B information t in than 4 that mass the exactly p could con could (SFHs). as it mo brigh 100 tion dynamical ually than older observ tributed the stars dication wise, more nitude of p and lution It with due ab magnitude, solv yp eak eak. y -band kp as out has stars this compared del. e tin The Another Th at previous ed Myr pre-burst one-to-one to of the c. can the 5. galaxies. ter of 10% the 4 big the y predicted after corresp than than uation b us, ations of b the ounger a ∼ The the the stellar during kp The galaxy e THE e that It the short dropping presen surface p disk of b b The A than ago, disk burst accommo as 0 star c sligh y eak of e GB absence seems . disk. incompleteness mass it a 5 ∼ as a brigh used the suggesting disk disk 6 the sections exp finding on onds 5.1 decrease OUTER of observ in p to Gyr . can magnitude stellar terminating than 5 at formation i 1 the tly stars, p As stars. scale the eak t as 0 tensit 0 mo stars b relation opulation . the ected our presen F brigh Gyr. ∼ the status for y tness (6.9 to size i the at The a rom 0 compared ed higher significan outer ago. to b del A dated us. of 22 = ∼ consequence infer ed e burst galacto the length GB-phase, do mass mo y in older disk at burst p a defined these tness kp Th 23 100 in outer used for mag, w DISK no ertained luminosit falls tly Ho corresp that not of p del, our ∼ e inner . c). There disk. b history us the 4 w-on-w the eak with brigh than w a et had w to observ understanding Myr. exists is 0 abruptly on than mag, ev allo strength cen more older of ould . tly burst falls w the implying the to implies 5 stel Th study to n star AND in relativ een in er, as the um disk. onding Gyr, the prop sligh tric ter w us are the on to fine that the lar ab y excellen p ards, the mass deriv most the exceed the ed to a b the rapidly only stars. formation eak fain mo the function basically out the er than M82 conclusiv either THE distances tly osed. is disk hardly ely con disk 10% luminosit 25 Data at that starburst decreased radius tune n de in densit detection ter ed is w the um to that of age in 1 discussions for more this tin mag y e the normal of t real Gyr. disk the mass from ounger the HALO side. the with of b refer these the of side These giv uing absence agreemen er the SFH. and resem the an y age. the only observ at arcsec e histories the the detailed and limiting e mass M82 of p densit y greater implies y answ M Other- the is radius of to Giv an eak whic activ- up burst grad- inner inner func- mag- stars stars stars limit /L late- ages con- ev disk The new The bles less not the the re- in- AS − ed en to er in o- of of K is h y 2 t A GALAXY magnitudes the the the outer far ∼ three A sp formation LF Fig. largest (2008a) nen in also disk, mass-to-ligh b ( or tra not scale A lar fers commonly suc µ et GB GB ectroscopic B 100 the HI, w h Did The t for out p outer p that inner a an 7. een lac > opulations stellar v eak a similar starburst disk, panels stars stars M82 ailable. Myr, three The and k alternativ 22 for tec as presen the 0 CMD stars could of and disk disk. mag activit hnique, 12 more disk. used there i hence are are p 0 the t whic outer at radial -band of to opulation ratios. 2 kp ages, t-da of older is larger arcsec p the Figure detected b LF the In follo tracer details. n and c er h qualitativ y e resolv is e 0 the disk y from . suggest Luminosit w 0.5 5 in zones Da the used a brigh shifting appro than results a wing is telescop Ho clear SFH radius. − y the vidge dynamical i 2 the ed of 0 7. also figure, to could ) w the mag to test are ev the ev is rotation last ximate stars It determine the n lac ely complete of en found er, um age systematically participate c y cen (2008a) can p displa es. hallenging The burst? k NIR b the F er 100 v w at b in the e unctions of ery ter. in er e date arcmin teraction? estimated b mass radial ages existence stars In outer can for the e of curv Myr. y stars outer similar ed seen Throughout cessation Obtaining stars the found the the the NIR see in 2 e of estimates y (LFs) . in ev disk. in distances ounger The suc ages disk the the See the absence inner with outer a en the to to the bands using of h that trend Do Da b i SFH for that of of lac promi- as fain a of 0 ottom -band Using large- r outer sp vidge p disk. es than 0 stars stel- disk ks star H − eak the the the the are ter ec- of- 51 α as of of of of it i a , 0 © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. 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Mayya that M82 axis (TR are et the resolv in tude of the in t V a p 7 resp the stars, the band ate is south their evidence the and halo. of region men 500 are in ing to around 10 un ha 52 that tematically a b formation w opulation efore teraction. teraction burst kp serious v o consisten til the b and A the al. kp Saito Sak In The e the age e disk, burst northeast p formed sev t, onsible GB) Myr GB fields, then c of globular the (Da they started exp opulation in correct, c ed images Da fields 2008), distances a red where of and the in in ai I eral the triggering distance 1 p mo these -band ab more most vidge stars, tra-group stellar vidge ected ago. opulations. the for et stars the stars, & disp or couldn’t are problem p in 50% o de, galaxy also t they with in opulation earlier v isolated in for al. passed Madore 2 the they around e these including with halo M82 at then corrob activ ersed clusters recen part fields The the magnitudes argued images and situ indicating 2008b). of ages for (2005) confusion residing p its 5.2 and candidates ab 0 from presence the opulations detected . . y of 08 found at halo. the farther e disk out it ounger . ha age medium parts A triggering. the of that t in in to through the p orated w should 00 The Orion-lik GB calls mem 3 the a (1999) w Da v erio is as the the that to FWHM e defining had small form idea at ork, pro Gyr the of one tip plane, burst. vidge as in b the It significan around of stars stel study cro d limit een the b for the the halo. A cen out jected ages old deep large disk the rep the ers of with ma of ago. Da the GB that ∼ b for of the of wding observ used lar asso a e ter, the star burst e triggered presence in et y extreme orted 6 vidge w the as using M81 of ma new suggests t M82 and halo Ho considered are er. disk the the w plane. A star-forming stars. The ere diffusely halo observ b kp the al. the 1 distance ciations quan o 3 M81 GB the e off-planar formation tly the w jorit ed red magnitude c If Gyr, adjacen also mo of noted prop ev found in detected TR (2004) w group along also the disk. (2008a) limiting in the to higher they burst en er, tities trend stars. HST/WFPC2 y stars the deling ations group teraction But GB. gian of south b that t found the of erties disco then y o H distributed through if or of in A that ccurred conclusiv inner the halo (de are ten the t MA studied t unlik seems the t termedi- south suggests and of w w In ∼ fields fraction the HI clusters studied ev regard- that regions around around One v magni- branc clearly as tativ as of in minor of YY ery b found Mello latest 1 there en R stars b elo bulk disk star fila- sys- e w kp K GB not oth the the the A an go as to at in in in of of of e, w 0 h a c e - & CARRASCO as around function the decreasing are cuss of maxim p are optical their more outer Hence, distances clusters is clusters, brigh of whic the distribution ure scopic (Konstan around side p Clusters nit the M82. putting starburst imaging ev the external w galaxy that where starburst et of 6. oin opulation ere er, M81 not al. these y the the THE There A One consisten published bar 1 necessit visual disco t of h to the can tness formed, than prop 1995). all (brigh of disk total . can SSCs um the hea ages maxim clusters. searc group, the 0.5 6 colors ends. Da prop is of situated capabilit view some with SUPER of galaxies, IN v top or these kp b greater follo are n vily ery erties n a b is giv e extinction within vidge almost kp of ucleus the non-detection its of y ucleus. are c e t h of magnitude THE SSCs. of oulos in t candidates If erties in no um distance easily c p en and none of condition for wing the The in clusters with then of can distance doubts affected triguing. 653 oin the the distance large ob biggest a M82 detectable including Both v in Ma (2008a) y the ST than outside the mass ailable jects ts). POST-ST are of outer 200 frequen et monotonically mean of disk of of b n its In an clusters it Figure noticed AR yy Starburst e um SSCs M82 n the al. the the as is blue of addition, still along um in The a 4 used age the is regarding p of fain b ac b lie from of v from c for CLUSTER for teraction kp a disk, et 2008). y around er cluster ery cluster clusters indeed only the also A b hiev tly clusters of of M82 is galaxy surviving. of in V their ers the c. in 8. compact ter CS details al. clusters and their ARBURST in globular for w the compact lik one the the the less − the n referred The ere emen the encoun The for the than the are (2008). uclear pro activit obscuration ely suffered giv I estimating Giv ma deriv p mass . disco ev . 1 disk cen n older of n than their formation opulation found, a and with vided are A direction The ucleus, b ucleus, found detection en of that olutionary mag. ts cluster jor at in en ottom-righ handful CS the POPULA ter. star tered clusters. y ed the the zone. v of The of clusters the the decreases as galacto B ered, 0.5 than axis Here, that mean the affiliation images sev seems a M82. DISK first an mass the − (O’Connell Sup lo nearly searc The clusters large-scale inner just highest thereafter Gyr, wide densit eral w 5 mem on opp V the from b Sp 200 the of and of some limit HST y ob er w regions surface as cen TION A status in of where h colors ectro- either radial t to e Ho co SSCs these M81, dust, ortu- disk. jects with ages Myr Star field b Fig- disk as w ric and y dis- tric 400 the the the the v ers w- b ell at to er in of is is is h a e © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya Da whic the nique galaxy K NGC that in ters brigh are is (b t The b Fig. co ones. the w either preferen bulge destro the massiv distances, yp ottom ere sho ottom) v -band) 100 150 200 the vidge 50 ered e Ho The The similar. disk 3 4 5 6 7 0 destruction 8. formation is mean h M82’s wn 0 for t formed 2403 y as w and follo also is e b Radial A ed. with panel ev tially ecause spiral lo absence b GB and of M82. comparable (2008a) in of y in w er, mass making wing consisten relativ M82 ( the stellar M82. the ∼ inferred the stars mass in more M82 divides distribution destro 1000 7. arms 14 The solid of of the the Sup w with b outer M82 of y ely kp compared a the SSCs p He them disk differs similar ys: extended er er relativ tidal outer SSCs conditions line. y t all c), the ed. to mass, op NGC with cluster also AS unit Star disks disks extends p inferred 2000 en more the or n oin The On of forces. from uclear disk, A in e to found a surface cluster nature the 2403, that t absence scarcit size of GALAXY the late p the an of at dotted that to and opulation normal normal n w they at a M82 larger using clusters a um of stellar ere morphological outer v the Th that a 3000 more erage late least of p y brigh of the b late opulation v us, er of of could not ertical M82. SSCs and the the the morphological spiral spiral galacto (top) globular disk stellar a at up vulnerable prop t ev SSCs from tness yp suitable dominating NGC same en eac newly n ha to e He line there um 4000 could and erties galaxies galaxies isolated M82 h v the if in 12 are cen (in disk e b found radius in SSCs t tec b M82. clus- er 2403 mass yp kp disk dis- less tric een the are the for AS b to h- of of of e. c, e A GALAXY that high-surface nario. tion small, gas-ric w t NGC for generated presence in fore a (Sofue b Xu presen at prop in supp ∼ v Y ing deviate metal y ing acting pre-burst b rise first along pro ric disk cen w the ing stellar (2) are 7.1 w ast oung een elo oung as as teraction big een 10 h the detecting t cess If It Mihos kno . et the unin stellar c it w. con galaxy to in gas-p the erties 10 in amoun ort haracterized ma stars 100 the Gas a 4676 the with is bulge, al. trinsically t: h w consequen ric galaxies global in 1998). ages as wn gas-ric & t M galactic trary collision. from jor as w of terrupted in for LSB burst tra-group h examples of 2000). pre-collisional Myr

disk-wide o o Sco ac 0.5 stars. teresting . (Mirab that are in disk, LSBs or formation, (1999) a the ts for (Barnes ev p of suc cr the W (Karac , brigh a it ossibilities: the ville normal the h parameters: galaxy en to etion of Ho Gyr. there e > formed is in stellar h metal-enric also its w fa LSB discuss disks t existence then This gas tly b w of normal ould w turned 5 a v Alternativ As el the of b in tness egin (1984). ev ors o ould relativ medium y Gyr hen discussed , b disk lo v sho starburst terstellar and et to 2004). . This are er, as pre-collisional eing star er galaxy of star w late-t kind w is If disk disk star al. ha with tsev in w note with, e these it the galaxy surface the (Kennicutt b no probably through starburst galaxy the on no v galaxies should ely disk-wide e 1998; (1) formation a NGC drifted formation e p of hed w of formation yp Deep with it of . required eculiar et Hubble observ burst ely surviv in of the that stars pre-collisional suc Ev three lo there it widespread the e is happ medium M82 pre-collisional al. , gas the w M81 with Hibbard 4038/9, galaxy en migh brigh M82 h should to starburst prop b observ observ through in a pre-collisional 2004). estimated induced e in ed with a formed ed o if w cases ened cen SFH M82 star is n and time, et able the disk. in as as a to t brigh that the um tness an could bulge erties in the , no ter. big ha al. a stripp follo suggested ations test ations mean but b formation b relations Arp the & LSB in most individually should LSB mak v to e purely star er in comp with is t 1994). e the This bulge in Y b b (LSB), the He a of b wing M82 teraction exp infer and y acquired disk, un this eing of con its 299 mass e es ed normal the galaxy M82 forma- galaxy galaxy sho age clouds of aimed of in found exist- in mean elling ected 1999; giv tin disk, ha M82 dur- disk or gas- also sce- and had ter- the the the the the the b b c On re- b 53 v ks as or at u- es of e- e- is y a e © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya 54 tection in un p three b galaxy bined for tablished v in 7.2 y of b the it immediately in these mass ies the fields this stellar formed On stripp the curv should p of tection this, stars stripp mass medium. stars, est ations ounger eculiar een e othesis y teraction. , usual its the the old . witnessing seen While In Studies M82 Ho 8. its in bulge the short pre-collisional target e. h R else acquired in tergalactic are main yp (No disk, ed ed mo studies whic ejuvenate SUMMAR w effect the disk M81 stars pre-collisional b distinct in disk. limit of fa ev other othesis. at the 7.3 resem e than optical stars. stars they dels star-formation stellar dominated v esk Sak formation. that w er, (Wills scale dominated scenario R h or of redshifts . probably and e in sequence GB of group. halo In are e is A Instead, ai can of the outside not that prop HST so w bles the hand, are recen stars et dust M82 It d not other ne ould & historical length, the the also app stars Y con medium et F far not star at starburst arby al. should all exp Madore or last osed the in prop AND stars al. observ halo exp tly scattering, ten In earance, HST a is b 0.2–1.0 ha b ha not in the 2006). t the example, rule stars, If w b y eing the stars ected formation the ypical in radial . luminous y 2000). a v galaxy decade ords, v t recen ected the this a the osed here, e e should those late history detected the FUTURE b stars and in are a con old out n observ ations. classification, rep disk e n v (1999) formed uclear in bar ailable whic are uclear debris to the is noted in t bulges, M82 b distance tributed Th halo stars t whic orted underneath ma completely exp in a y yp v y the ha t b ha according dominating p high elo ypical ears exp M81 . b gas-ric us e Sofue h blue ations. oten in formation? e jorit v e ving ected m detected starburst could h e in cit are of Ho case, left that spiral from for found region data The in ected a uc RESEAR the undoubtedly and w inclination, sev y group tial the compact y M82 w stripp to h as of of M82, b h (1998), high the b ev field of eral the elo then farther ehind to the disco b the LSB disk The is to the bulge 2 rather in er, resp none galaxy somewhere to to e the the w are ma da tra-group kp MA first e the the had b a the ma luminos- stripp d rotation and fields w this v none b of e y the v the CH onsible c. brigh nearb mo y elo of e stel e galax- obser- ery a in newly YY of jorit stars. m R R fa com- . b than than ligh ha time M82 ma lo disk The cit and del. uc GB GB lo een v h the the the de- de- lar es- Its A w- ed v or y- in of of w t- h y y y y e t & CARRASCO galaxy in dius. is data mo the rather quenc the lac it outer radii. around the sible mencemen burst burst cen indicate at is coun mation 1 10 b happ factor p disk burst stars ated propagated b NGC tain sem the photometric ages. collisional ence tection cup b of the y est opulation e y Gyr not applicable k distances normal the the del kp tly It The ying Sofue bled t starburst of pre-burst observ disk. inner ter y fits are of ened b on of that seems c , hed The , activit disk, is Th w started efore true 3077. surest of w than around the ago. CMD. data a stars formed the 300 of as started the pre-burst the as in b that w the no that us t et (1998), follo a t m disk star-formation ed the The w suc disk. late triggered w general for y seems whic initially inner glare in w the outer to of Myr. observ o. the y uc con farther main tec can w y een from of w Numerical M w related h the as stopp stellar wing According around ounger h the starburst The 300 b a the ards, ell data (radius t most latest If in tin y hniques h /L a a e stellar yp b These far of b for to parts efore as last M82 lo disk then The stellar disk the ational w burst uously established the K sequence Myr outer the e e consisten ed the w detection the e prop out b , then old seem out b testing galaxies. reconciled p to of e encoun surface tak than whic y encoun systematically in 800 opulation duration, outer cen using mo p is as the and suggest stars burst, < ago. burst an teraction is the as in w opulation activit its osed disk, sim disk e in in the to data o old ere related v ter, 3 y h to difficult Myr v the 3 in ed presen ∼ the t er stars its ulations the the and earlier In kp in ma disk, ter. the to Gyr. are ter burst the brigh stars. suggest as mainly of with limit based as 100 where progressiv teraction. that ma for y the c). disk. The the that y neigh disk with existence accoun ago, 1 M82 disk as in evidenced happ red first exp W traditional scenario t jorit b the in Gyr. happ to and Myr So tness ages the should Hubble burst e estimates due as encoun the w Ho the in Iden the disk-wide on ected w the It at uncertain ell b a gian constrained of and most the y as if inner ened started that y the as w ors ounger idea t the subsequen ened burst ma CMD an A earlier the in to the burst burst ev of as Y ely tification galaxy bulk this 12 mo completely t t of un The ywhere ha latest er, encoun lasted ter? y M81 to the the distances prop the the time the branc lik from study more disk, that star to data del the v kp b around surface or e (1999) ely b uncer- recen mo mo in e w of activ- times burst burst . inner inner A same c e pres- initi- com- star- b osed ould that p pre- and w De- for- lik GB y hes the the the the the en- o del de, os- ter ra- for tly re- re- on b as in of of c- y a e t © 2010: Instituto de Astronomía, UNAM - A Long Walk Through Astronomy: A Celebration of Luis Carrasco’s 60th Birthday Ed. E. Recillas, A. Luna, & Y. D. Mayya Carrasco, Bland, Barnes, Barnes, Karac Blac on Da Holm Girardi, v some Hibbard, Gottesman, Go co-author Gaffney Ro the w for 58956-F. F the review. Ev constrain F¨ tip tection ery carried of Engelbrac de of Da these Da radius sequence de ery reedman, orster as ans, HST/A vidge, vidge, Mello, etz, V vidge R dr the nic RAS, 128, 407, 1990, D., Moun Herriot, discussions W of of ev starburst, kman, supp aucouleurs, GB ´ m b ıguez, hen e stars. k, part olutionary erg, the R & uc J., R. greater , M., NIR out Sc thank J. J. 1 L57 of GB L., N. J. tain, A&A, tsev, T. 189, J. stars orted h Stern T. W ts D. h Finally L., (2008a) turn-off hreib 1994, & . CS E., E. in t, W. R R C. E. 1986, Luis. I., G. McKeith, et e 2008b, E., of S. only Abraham J. on The F., GB GBs. astronom T stars Recillas-Cruz, J., C. all 2004, 751 & ac M., Lester, ully P 1950, observ I. al. L., T., b 2008a, 2004, the Alessandro er, but & b in ., on than 240, erg, Smith, MNRAS, W., the G. the Sto kno Hernquist, D., y , RevMexAA, stars. limiting for 2002, Axon, It , Y et state & it & (Sak N. the CONA magnitude, a w ApJ, B. REFERENCES 1959, MNRAS, Hence, un, w esz, also wledge is w et A. 52 is mass Lund as al. Karac v Harb P W the ations ork 2 D. AJ, ariet M., orks C. 1988, ASP, y y a eliac Luna al. disk L. ai M. 2001, A&A, kp ou 1994, not of J., As D. 678, F., pleasure w and halo, Handbuc D., ec presen 266, & J., CyT 136, 2006, magnitude Genzel, c ould hen y of S. Medd. M82. related who E., hew, these L. Rigaut, J., k, Bressan & 116, Nature, of could of the Madore will of deep Sabbi, 350, L85 and Do ApJ, 1999, M82. ApJ, the 12, tsev 391, T D. Cruz-Gonzalez, 1992, 511 2502 no & M82 resulting topics (M but elesco, help ApJ, motiv wnes, ted L. 1 con R. w, not 135 T a, images 798 to h Rob Astron. stars R., ´ exico) 195 to b 552, enough a 427, AJ, 1977, E., are der F., ylor, 334, e V. ARA&A, 2008, is tribution thank suc here. and in 1999). M82. 642, for ated only discussed used Lutz, erto C. D., ab E., Gallagher, 118, 544 V Ph 628 understanding w h formed 43 in ApJ, eran, M. K. pro p o ell esp Daniel L127 AJ, a Obs. ysik, & v oin Huc me Romano m to the put for Thank e This 162 D., study 1979, 1993, b Detection ject ecially Grev y the I., t 30, elo 135, 211, M82 h iden to J.-P of (YDM) sources the disco 53, Ser. tmeier, Kunze, & strong in b w gran 705 main Rosa w w efore e, J. Lino ApJ, MN- Mel- ., this 548 w y L57 275 tify ork ork the de- AS ou S., I A. as at v- in & I, t A GALAXY T Visv Y W Sofue, Y Shen, Riek Origlia, Y Wills, Oh Sc Xu, Scarrott, Sandage, Sak Ro Saito, Sandage, Ma Mihos, Mutc Ma Mirab O’Connell, Morgan, No Ma O’Connell, Ma Ma Malin, Konstan Lehnert, Kennicutt, elesco, un, un, oung, alter, hmidt, dr esk y yy yy yy y yy Campins, ApJ, 2004, at & 252, F. Sanders Colley 37, at AJ, ApJ, Luna, Sanders L33 Martinez, ApJ, c ApJ, 2008, W. ai, ama, all, anathan, ho, C., e, ´ ıguez-Merino, hler, M. a, a, a, a, M. Domingue, e, el, J., Lo Lo J., Y., K. S., Y. 56 D. K., G. J. 116, J. F., Y. Gao, G., N. Y. 12 Y. top K. Y. L., w w S., 206, 679, 523, 435, W. M. I. S. C. ApJ, ApJ, & S. G. , & C. A. A., Y., A., 1998, & A., et S., F. M., H., W. & D., and and U. D., R. F., R. R. W G., D., oulos, W M., D., (Dordrec (Dordrec Lo, Ho, T 1999, 1999, D., Madore, Ranalli, D., 1671 R., W. al. 1978, M., & et et Mak okunaga, Y., H. & eiss, L. 888 404 575 22 N., estmo Carrasco, W., 1960, W., et C., N. Leb Carrasco, et 606, 674, Bressan, et Ra High High P Eaton, Brucato, K. Romano, 2005, al. al. Sco Angel, Hec P & 1958, 2006, 1991, al. ASJ, Mazzarella, D. al. . & 1995, aro al. in Jo I. T A., vindranath, ofsky IA Gallagher, & T. Miller, Y. Nature, 2002, 2000, ville, L. am 862 846 kman, quette, Sandage, Ann. 2007, y IA S., L. 1998, h h v, U 2006, Redshift, Redshift, Mangano, , P B. P t: t: ApJ, & 1995, P ApJ, H., ApJ, blyn, 50, ., U N., J. ., A. 2000, , D. M., ApJ, Symp. ASP, Bastian, Klu Klu A., Sco F. L., L., N. & M. Symp. Comastri, P MNRAS, R. R. d’Ap., R., W. T. P 227 et ASJ, T. A&A, I. & ApJ, 1999, 276, 621, M. Lo, ASP, ville, w w 649, Z. ApJ, 369, Carrasco, & 1979, & P Dietz, P 2004, J., Axon, 446, 1980, ApJ, J., er), er), al. J. M., A. 70, ., ., C. Ro 1984, Luna, S., 186, S., ed. ed. Rosa-Gonz´ K. & & 186, J. S., 54, 591 750 Thompson, Lu, 640, 2010, 23, 1972, 172 N., 135 dr 1964, N. 333, ApJ, 364 81 205 119, & 445, L1 & Crom AJ, Congdon, J. & Y. J. J. AJ, ´ 541, 316, ıguez-Merino, I ApJ, D. 891 K., Galaxy W A., I 2002, 344 Galaxy Gallagher, N., Smith, ApJ, I, 1978, Carrasco, E. E. A. L143 1993, L1 ea 1 L., L99 84, J. ApJ, 526, RevMexAA(SC), Science 127, Hun w 644 33 & v Barnes Barnes Sulen 2005, Dec 238, 1991, ell, er, alez, & ApJ, 472 287, ApJ, Maiolino, ter, ApJ, 599 2031 In In L. her, 176, Hernandez- R. K. C. R. 24 tic, teractions teractions ApJ, MNRAS, 144, J., 153 D. D. 580, J. L. A. H. E. & & I., 221, 411, 57 R., J. L. S., T A., D. D. 2008, 1998, 1999, 1976, 1994, Lo 405 628, ran- L21 W., H., I 62 55 R. 17 w, B. B. & & I I