radio emition of normal galaxies

8/13/2019 Radio Emition of Normal Galaxies

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Annu Re Astrn Astrphs 99 55prht 99 Annu Rees n A rhts reere

RADIO EMIION FROMNORMAL GALAXIE

J. J Codo

Naona Rado Asronoy Observaory, 20 Edgeon Road,Charoesve, Vrgna 220-247KY WORS os rs reeree esso rre ro sr oo

oo o

IOUCIOIf he rado energy source n a gaay s no a superassve back hoe or

reaed nucear "onser, hen ha gaay s caed nora n hsrevew, regardess of s opca orphoogy. Neary a of he rado esson fro nora gaaes s synchroron radaon fro reavsc eecrons and feefree esson fro H II regons. Thera reradaon osargh by dus qucky overwhes hese coponens above v 200GHz 1 ), denng a pracca upper bound o he frequences o"rado observaons Typca reave nenses of synchroron radaon,free-free esson, and dus reradaon are shown n he rado/far-nfraed(FIR) specu of M82 (Fgure 1 ) Te rado connuu fro a noragaay s ceary jus a racer accounng for

0 K to be a starburst However an 8.44 GHz VA ap aewit 02 resolution (Figure sow tat tis source is extene an itspea brigtness teperature is only 0 K Therefore a at spectrueven at GHz frequencies is not sucient to prove tat a raio source ispowere by an AGN Flatspectru sources prouce by onsters inSeyfert galaxies classical raio galaxies quasars etc generall are synchrotron selfabsorbe Tus igresolution aps capable of separating

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88 CONDON585'"

0

8u

7Q

694

ll5444 44 non

4419500 e uleu o 69 i typial o e briget ad mo ompa our oud

i "omal galaxie GH brige temperature i oly 0 o i relaivelya radio ptrum idiae reree aborpio by termal elero wi tmperaure 0 o ycoo laboptio by lait leco i tc tmpau > mk 0' logarimi oour are eparaed by aor o 2 i brigead te lowe oour i 0 my bam

souces wt 1 K fo tose wt > K cf os et l99) soul be able to stngus between at-spectu stabusts anonstes But t s not enoug to sow tat K at g fequences GHz to eject stabusts cf Caal et al 99 Capan et al1 99); stabust galaxes uc bgte tan M82 o exst SYNCROTRON RAATIONSyncoton aaton fo ultaeatvstc (E mec2) electons o

nates te ao esson fo ost noa gaaxes at fequences beow 3 GHz Caculatons of patce lfetes, enegy enstes, etc aeoe eanngfu fo te ao souces n noa gaaxes tan fo soucesn classcal ao galaxes a quasas because tey ay be copaewt ect obsevatons of cosc ays n ou galaxy an b equpattonbetween e an patcle enegy enstes pobaby ols n noalgaaxes see Secton On te ote an, ao spectal sgnatues ofcosc-ay enegy loss an tanspot pocesses ae elusve an tacng tecosc ays to te soces s st ct

Basi Equations

Electons wt enegy E ovng at ptc angle n a agnetc el ofstengt B et ost of e enegy nea te ctca fequency e

Annu.Rev

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RADO MSSO ROM ORMA GAAXS 89

or a ypcal pral el rengh

G ynchroron eon nhe freqency range of . GHz generae by elecron n he: energy range GeV. he ynchroron poer ee by eachelecron d dt n E GeV 3 .8 GeV 8.or oropcally rbe elecron eloce ch a obere near hen n

2/3. The ynchroron fee rs

E/ldE/dtlrs n yr fG GH 9.

hch abo yr a . GHz for G InereCoponloe hae he ae energy epenence an he rao of ynchroron o nereCopon loe eqal o he rao of agnec energy enyU /8) (U erg c n he Gaaxy) o raaon energy

eny Ucroae bacgron aon fro ar (Uof coc ray n he olar neghborhoo ece fro Be ecay 2 yr GarcaMnoz e a 977) or ore Doge 99) o ynchroron an nereCopon loe ay be gncan a GHz freqence.he raaon energyeny n copac aeer D pc) lralno log LFIR/Lo) . here Lo 3.83 arbr o large (U 3 erg c ) ha he nereCopon lfee ofrelac elecron eng a

GHz only abo yr Conone a 99c) .An eneble of relac elecron can be ecrbe by he nbereny NE)dE of elecron h energe beeen E an E+ dE. If

NE) NEY an he elecron hae an oropc eocy rbonher ynchroron eon coecen .

here [ he angle beeen he agnec el an he l ne of gh o heoberer. he ynchroron raaon fro an elecron of energy

E

conne o a bea of h f /E raan parallel o he elecron elocy. An oberer ee raaon exclely fro hoe eecronhoe elocy ecor nearly cro h neofgh o [ an ony he

Annu.Rev.

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9 ONDONcoponen of he agnec el pojece ono he y plane conrbeo he oberve raaon h qaon l ncae ha he oberve

brghne of a orce epen on he recon of any orere el coponen even hogh he elecron are ovng oropcally. or exaplef he coponen of he agnec el gncan n he halo of galaxe ynchroron halo ll appear brghe n egeon ye anll be fane n faceon ye eg obervaon of or galaxy nrecon near pole)ynchroron elfaborpon only poran for orce h brighne eperare > mc/k K vale apparenly never aaneby noral galaxe. The pecral nex of he nonheral eon fro

a noral galaxy herefore

-

/

2 ally

.8 a GHz freqence plyng 2 6 a GeV energe.Maheon e al 972) ree ha he ynchroron evy qeenve o change n he agnec el rengh e BH an henceo copreon of he eng vole conanng boh el an parcle x+a for a copreon facor x. They acrbe brgh rge ofynchroron raaon concng h he lane on he nner ege ofspira arms in to compression of the iterstear mediu (both par-cle an el) by pral ar hoc Laer ap ae h hgherreolon ho ha he nonheral ar hape are no conen hple copreon Tlan e al 988) The non heral neny graen are eeper on he oe ege han on he ne ege an heneny pea j ne he lane. The ga conanng he relavcelecron oe no appear o be hoce pobly becae on pee he Alfvn pee B/(4np S n he ho onzenerellar e In boh M Tlan & Allen 989) an M8 Kafan e al 989) he non heral ar are cenere on he rge of yongar an H II regon no on he H I velocy hoc fron. Th arforaon ore poran han copreon for procng rao pralar n noral galaxe.If he procon rae of relavc elecron q(E an he oalelecron energy lo rae (E epen on energy alone hen he eqlbr bon of relavc elecron N(E Jq(EdE. Thehree er n he approxaon (E --E -E correpon oonzaon loe relavc brerahlng pl aabac loean ynchroron pl nvereCopon raaon repecvely orq(E E, he eqlbr rbon of relavc elecron

.Becae he onzaon an brerahlng lo rae have eren energyepenence brerahlng loe excee onzaon loe a energe


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AO MO OM OMA AAX 591e he heisi eegy 0. GeV (f iesell me sisig pimily f hyge). The espig iil fequey i 5

0 G els is

0 MHz s iizi lsses i rl glies usully e eglee. eliisi emsshlug lsses i he isk f ugly e ply seee sie he smi-y me fee ph is5 g m (Gi-Muz e l 9) e f mgiue smlleh he 50 g m - ii legh i he iesell meium.The mie syh plus i esemp lsses eee he eliisi emsshlug plus ii lsses eegies > heiil fequey (qui ) espig / is lle heek fequey Wih he ppimi h eliisi elesie ly hei iil fequeies, Equi yiels f he herml speum

oSN + /" .

whee ()/2 1/2 is he sympi hge i spelie The spel seepeig fm + is ily sughy sees euse migh fll i he sele GHz feqey ge.

Hwee qui 1 shws h his ek is elly ly ey gle lgely euse V sfms smll eegy ge i lgefequey ge. I is s gul, ufuely h i is usele wihhe uy fequey ege f eisig u-esiy mesuemesf ml glies. This pi is illuse y he w mel spe iFigue 6 Wee (988) esies he ele iuly f isiguishighges i fm hges i i he speum fNG 461 . Neheless, spel seepeig sis wih 0.5 wih z i he isk/hlspe f he ege- glies NG 89 1 NG 46 hs ee epe

(Humme11). Magneti Fieldssimes f he mgei el segh B e usully eie fm hessumpi f miimum l eegy ( ) V, whee is heeliisi pile eegy esiy, is he mgei eegy esiy V is he se lume (Buige 956). The l eegy f giesyh lumisiy is miimize whe U U/4. This is ey lse eegy equipii ( ) ls pessue equliy Pm Ppsie

Pm

U P

/ f uleliisi piles. The lulemmumeegy el B epes wekly he sue gemey heheml spel ie he fequey ge i ig syh ii usully ke e 0.0100 GHz. I ls epes he

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592 CONDON

I 1

lilt ! 11

(z)

111

6 e oninuou uve e eum o a galaxy wi = 22 eal bend = /2 eneed on = 5 GHz and emal/nonemal u aio / a V = IGHz e boen uve oeond o a owelaw nonemal eum w = lu a weaker ermal onibuin / 5 a = G. e eral bend aued byynoon ad nveeComon loe i oo gadual o ee ea o be dnguiedobevaonally Aba eueny GHz dnae: elave ux deniy abay uni

iisic /c c i f, which S f 40 i gxy (W 99 1 ). F isk wih 0.5(BmiO)

5( 1+f)217(Tb)1(_V )11/14( )-1,G 4 K GHz kc .

wh Tb /(2kQ is h s h yighJsighss fqcy

is h h f h c gh if-sgh. qiy Tb is h fc ighss 2 k c (c B 1 985 H 1 990) is yic iskhickss. h i fc ighss f si gxis isTb . 5 GHz, s s si isks chciz y sghs i h g 50 G (Sf 986 H 1988).Th ii-gy i h c gi fM82 Jy GHz f 0 0 gi hs 0 5 kc hick) is Bmo OO G h sghs i h ighs cc scs ssci wih

gxis ch 1000 G ( 99c). N h h y s i Eqi 3 is Tb (h hickss is siy if f hss isis f h s) s h cc s f Bmil i h ss f sych sfc ghss. h


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RDO MSSO FROM NORM GXS 593g ss liv h h ul mgi l sghs i h isksf ml glis ls Bmin. hul B Bm u(Pp/P (4/9 (B/B7

wul m lg h smi ys wuli ul pll fm h isk Pk 965) h mgi is vy ssiiv pssu gul f livisi pils Thls pils h pl ly y h wigh f hisll mium Pk 1966) s B Bm is ls ulikly.Th lgsl mgi l suus f spil glis i fm muli fquy plizi mps s Kus 990 Bk 1991 f viws). Th iisi g f li plizif pilly hi syh ii fm pwlw isiui f

livisi ls i vuum is

3 + 3)/3 + 7). Th svg is u y Fy plizi y viis i hmgi l ii wihi h m glviz l 976). Diskmgi ls glly m uifm i s f lw s fmih u isk im gis) m uul wh h sfmi is high spil ms wih lg H II gis mlllus h ulus Kus l 989 ukum All 1989Niig l 199) Th iisi psii gl f is ppiul h pji f h sky. Th s psii gl mus f Fy i whih is fiml ppil

A

mulipli y h i msuRM eBld whB is h mgil mp plll h lifsigh. Highslui mps m w m sh A ; 0 m) wvlghs shw h lg-sl iskmgi ls f spil glis mlly u lms plll h spilms Th l li s my spil iw uw his 80 miguiy sv i slighly ili glis us h sig f h RMhgs wih h sig f hB pji Aisymmi isk ls lwyspiig ih iw uw) us h RM sig hg vy180 f gly zimuh

RM

sig hgs vy 90 ii isymmils lig i ii. Aisymmi ls hv sv iM1 Bk 98 Bk l 989) I 4 Kus l 989isymmi ls i M5 Hllu l 1 990) M8 Kus l989). Hwv h lgsl l suu s lwys ysimpl isymmi isymmi ym ml H l 989)Th uply high RM sg Fy plizi fu ih suhws qu f h NG 6946 isk suggs lg vilmp h isk l gli l hl Bk 199). ysmi viis f

RM

ss h isk f M83 ls vl sigi mps m is g-s isk suu Niig 1 99 Mgi l suu v lwh isk msu y mulifquy plizi mps f g

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594 gx. h mnnt tn N 81 t r t th k (An & Sukumr 1991), ut th n n thxtn r h NG 461 (Humm t 1 99 1 ) nt yutwr. Cosm-ay Soures and TransportI th m ry n ur gxy v tt nrgy 10 g n nvg g 10 y th u mut t m ry t nvrg wr v x 1 0 rg . y II n y I unvrmnnt hrt-v 8 (Knnutt 1984) t r th ngtr nt u hy u unt mhn ngyn hk n r th trngt nnthrm ur n th xy (nzug Syrvtk 1964) y I urnv mnnt ng rm nr tr utn r mrtnt rtr m ry nnm gx. It nw tht y I unv r much mmn n tty gx (vn n Bgh & mmnn 191); nmny ur r rm th qutr n thr rnt gxy whrth mnt nttr nty w. y I SN mght ntrutt wk u n g wt y w urrnt tnrt.

But rt urnv rmnnt thmv mt ny m tn th ntgt nn thm ux m M1 (Py 1 69) n thrnry gx (Ivky & quux 17 Brmnn 1976). Mt thnnthm mn mth y my trnt tht tht tutn t u nt u n t. uux(1971) un tht th g t trutn yung tr n nnthrm ntnuum r rrt n th k gx n h rtht urnv rmnnt t mt th m ry rvthrughut th k. Vn ut t (1977) untr tht th rtrutn nnthrm ntnuum n N 6946 mr y mthth tutn t ght u y th r k tr utn, whh thy uggt h my u. Nw th m mny nrm gxy k r v t r tht th nnthrm ngth uy gtr thn th th t ngth th k t n th FR ngth trng vryyung t (By & H 10) h y u my rgtn xn th vum u y m y trn.hrr, ngth nnt rty u t tnguhtwn yung n r t utn. Dur t ( 1 86) vht th nn thrm mn n N 10 y mr y rrt wth th (r) rm thn wth H II rgn r thr trr rnt tr rmtn n Du (186) r r hk g-

Annu.Rev





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RAO MSSO ROM ORMA GAAXS 595it elertrs f smi rys i rml glies with high shkspees. Hwever the gs tiig smi rys my t e shke

(Seti 4.) Als Giurii et (989) rik et (1989) fu rrelti f ri rightess r the ri/ue rti with spir rmprmiee i smpes f rml glies. Hrwit et l (98) suggestetht viet fe- lisis etwee the mleulr isks f glieselerte the reltivisti eletrs i ultrlumius strursts. Suhsures wu e very shrt live prly less mpt th serve( et 991).he ther ri lumisities f rm glies re rrelte tieret egrees with lumisities i mst ther wves these

lumisity rreltis hve ee use t supprt ieret ter ppultis s sures f smi rys. Hummel (98) e fvre the lisk ppulti euse the ri ptil lumisities f rmgies re rrete whie the isk ri rightess is t lery rrelte with (B- V) lr (ut see Keiutt 198) r rm prmiee.he ri/lue lumisity rrelti is hwever quite r lier ( 1989) sie the mst itese str frmti is hieehi usty mleulr lus. Klei ( 982) i rrelti f rirightess with ptil lr fr ue mpt glies s fvre yuger stelr ppulti. Keiutt (198) te tht the premity therml .4 GHz u esities f rml glies rerrelte with their H ues ue tht the reltivisti eletrsrespsie fr the therml ri emissi re elerte y theppulti f mssive shrtlive iizig strs rther thy the l isk ppulti. he X-ry lumisities f rml gliesre etter rrelte with ue th with ri lumisities, s Fi & rihieri (1985) suggeste tht lw-mss X-ry iries (lerisk strs) elerte mst f the smi rys. he Xry lumisitiesf strurst ulei re ls rrelte with Br umi sities trer fmssive strs (Wr 1988). he est rreti with thermri lumisity is the e with FI lumisity esrie i Seti5; it fvrs very yug stelr ppulti (f e g et 985). Hummel et (988) stress the rrelti f ri surfe rightess withFI ust lr temperture s eiee fr ri emissi frmyug strs A sphistite ve (ri, FI, er ifrre lue Xry) stuy f umisity rretis i spirls le Fi et l( 988) t ue tht the ri emissi frm strursts must rigitei the yug stelr ppulti ut ler usi e rw frmthe lumisty rreltis i ess tive spirl gies. Sie there is e t rretis with ri lumisities, this is prly the mst tht e si with ee.

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596 CONDON

Radio supernovae are compact synchrotron sources that appear anddisappear within a period of months to years following Type II or Type Ibsupernovae; no radio emission has been detected from ype Ia supernovae(Weiler et al 18). he poer source appears to e the supernova shock

that propaates into the dense circumstellar wind (Chevalier 982 or H IIregion (McKee 988, Chevalier & Laing 989 produced by the supergiantprogenitor star before it exploded Too few radio supernovae ave beenobserved to establish radio supernova rates in galaxies hey do not appearto contribute a sinicant fraction of the average radio luminosities ofnormal alaies althouh a sine radio supernova may have a radioluminosity L 2 h- W Hz- (Rupen et al 987 for a few yearsSupernova remnants become radio surces aout 50 yr aer he explosion(Gull 13 as Rayleih-aylor instailities develop in the boundary

beeen the shoc and the ambient interstellar medium and radio SNRsremain visile for hundrds or thousands of yars About 40 young SNRs

are conspicuous in highresolution maps o M8 at Gz (Kronberg etal 1 98 and 84 GHz (Figure an radio SNRs are just visible in NGC23 (ntonucci Ulvestad 1988) and NGC 3448 (Noreau & Kronberg1987).

SNRs account for < % of th radio luminosities o f normal gaaxiesbut they can be used to estimate supernova rates Shlovsky ( 1 968) shoedthat an optically thin youn radio SNR expanding adiabatically wth

constant speed and conservin manetic ux will decay exponentially inluminosity Its age t can be estimated from its radio halflife T with the

- I M 8

d 655'" 0

50 0 @

c

I

.9 5 ' " . c5"u

Q 56 C54 55 I I I

m44 43 Rh scnson ( 1 )

Figure 7 The compact sources visible in this 44 GHz VA map (Z-P. Huang, unpublseddata) of the cente o ae ado SNRs he fanest of whch ae aout as luminous a Gala N apa A T lam a paa by fa f 2 '/n bghtness and he lowes conour is mJy eam '.

Annu.

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RAO MSSON ROM NORMA GAAS 97eqaio t 2(2+ )/l2 ere i e pecral idex Kroberg &Sramek (198) moiored Hz x deiie of e e roge SR iM82 ad fod alf-lie

yr c lead o aerage aget

1 yr e radio peroa rae i M82 lie i e rage 14 yrdepedig o eer or o e e roge SR are e e yogeVLBI meareme ad loer limi for e aglar diameer of SRi M82 yied a radio peroa rae 1 yr if eir radii gro 1 km S (Barel e al 1 98 Wilkio & de Bry 199)Mo comic ray ecape eir pare SR llig e galaxy dikad alo I diio model comic-ay propagaio i pecied by aempirical eergy-depede diio coecie () For or galaxy() 1

cm

S

if eV ad () 1(/eV) cm

S

if > eV (izbrg e a 1 98) Aer ime e comic ray die adiace d () akig 4 eV for elecro radiaig a 149Hz ad 2 x 1 yr i e olar eigborood idicae d 3 kpci i cie o make e oermal radio dik moo ad icreaei radial cale leg igicaly alog e ycroro brigecale leg i orer a e eqipariio comicray or mageic eldcale leg (cfHmmel & re 1 99 Hmme 1 99 b) Brig compacorce i galacic clei mc malle a 3 kpc are poible becaeeir comic ray ae or ycroro ad iere-ompo lifeime(odo e al 1991c) Simple diio pread e comic ray from apoi orce io a aia dribio b Bicay & elo (199) foda coolig e FIR brige diribio (ake o be e orcebrige diribio) of earby face-o piral galaxie i aiadi o yied good o obered radio brige diribioAleaely comic ray ca ream a e Alf peed VA 1 km i e ioized ierellar medim ad rael 2 kpc i 2 x 1 yromic a may alo die io a aic alo or coec ay from e

dik io a dyamic alo e eec of comic ray propagaio o eoemal adio emiio from alo ere died i ome deail byLerce & Sclickeier ( 1 98 1 982) Eergy-depede diio ad adiabaic loe fro coecio prodce pecral bed of e form gie byEqaio 12 i aympoic pecral-idex cage 1/4 e pecral bed are ery gradal oeer realiic imlaio o oly malldierece beee e pecra of edge-o galaxie i aic or dyamicalo (a der Wa 199) e radio pecra of e be-obered aloi 891 (Hmmel e al 1991b) ad 431 (Hmmel & Demar199) are coie i coecio Oer ig of coecio or idare ycroro prorio from edge-o dik (odo 1983 Reer eal 1991 Seai & Odegard 1991) ad ordered alo mageic eld(Hmmel Demar 199 Hmme e al 1988b 199a) Oberable


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98 COOdtncton beteen tatc and dynamc ao ere recenty reeed byBoemen ( 1 99 1 a).

T R/RO CORRLTON correation beteen te A 10 m mdinfrared and 141 MHz radiouminote of Seyfert gaaxy ncei a dcoered by an der Kruit( 1 97 1 ) and oon extended to te nuce of norma pra gaaxe (an derKruit 1 97 ). t rt bot te nfrared and radio emiion ere tougt tobe yncrotron radation from reatitic eectron acceerated by nucearmonter (e.g mae back oe in Seyfert gaaxie or oter AGN)Ten Harit

Pacin ( 97) propod at te infrared i erma reradiaton from duty H II region ie te 14 MHz uminoty domnatedby yncrotron radation from reatitc eectron acceerated n SNRfrom te ame popuaion of mae tar tat eat and ionze te H IIregion ondon et a (1982) caied te uminou centra ource inpra gaaxie a eiter tarburt or monter by teir radio ze andmopooge and tey uggeted tat te nfrared/rado rato coud beued to ditingi tarurt from monter ine te coeation amuc tgter for nucear tarburt tan for monter Rckard & Harey

( 184) found tat te FIR/rado correation appe to te dik of normagaaxie a eTe rea gnicance of te FIR/radio correaton for norma gaaxietat it o tgt and o unieraa not appreciated unti te argeIAurey appeared Te IRAx denitie at A 60 m and A 100m can be ued to cacuate te quantty FIR R 26 10 28pm+m m x y 4.ic te tota ux beteen

A 40 m and

A

20 m IR meaurete majority of te ux reradated by dut in norma gaaxe (eou et a 988) Heo et a ( 198) dened te parameter I ) S )q og .7 1 0 m og m z

ere v 14 GHz une oteie pecid a a ogatc meaureof te FIR/rado ux-denty ratio. Te dtbuton of q a found to be

quite narro (rm catterq ;

02 about te medianq

2.3 at

1 .4GHz) among pira gaaxie in Virgo (Heou et a 1 98) a arge inomogeneou ampe of pra and rreguar gaaxe (underc et 1987) Sbcgaaxie (Humme et a 1 988a) E/S gaaxie t cuent tar fomaton

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O O O O GX 99Dr 988 rob & c 988 99) xtragaacc FR ourcctd at 60 m odo & Brodrc 986 99) ad rado uxmd amp o orma gaax odo

&Brodrc 988 odo a 99b) T FIR/rado corrato odo t a 99 a) or gaax rd S BGS Sor a 989) pottd Fgu 8Sc ycroro mty por radatd pr ut oum) proproa o s+ ) B' +a or a g dty NE o rattc cro Equato 0) t a propod umm 986 umm t a 988a)a dao o ddua gaax rom t arag FIR/rado raorct arato Ba. T FIR/rado rato o o to b arycotat or a rag o' 0 B2 B odo t a 99c)

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'.

1 0 lg h2L

2Figure The /radio correlation for strong sources selected at = 6 Jm and nocotainin known monsters (e. eyfert nuclei) or opticay thick to free-free absorption at = 9 Gz The measuremen errors are smaller than the intrinsic scatter for this sample.bscissa: lo uminosity in solar units Ordiate lo 49 Gz luminosty (W z )

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600 COOere i agai te magetic eegy deity o ti doe ot eem tobe te cae If te comic-ray prodctio rate i proportioal to FR te

FIR/radio correlatio actally reqire tat te total radiog

emittedper relatiitic electro drig it lietime be early idepedet of bt it doe ot cotrai te itataeo radio emitted by eacelectro Apparetly galaxie copire to x te ratio of ycrotroergy loe to te radioqiet lo from iereompto catterigbremtralg ioizatio adiabatc expaio ad ecape ito itergalactic pace.Seeral explaatio for ti copircy ae bee propoed lk( 989) arged ta te break freqecie (Eqatio 2) of ormal galaxie

are

GHz; tat i galaxie are "calorimeter or "beam dmp iic relatiitic electro loe mot of teir eergy to ycrotro adiereompto radiatio Te ratio of ycrotro to total eergy loi terefore /( ) ere i te radiatio eergy deity icmt be early cotat to ae e FIR/radio correlatio Star are tedomiat orce for te radiatio eergy deity i mot ormalgalaxie at lo redi altog te idepedet cotribtio to fromte comic microae bacgro gro a + Z a mg qecte raio emiio at rei z Trblece aociated it tarformatio cold amplify te magetic eergy deity (Ko

&Parker 989)til i t i comparable it te itertellar trblet prere pv/3ere te rm trblet elocity v 1 i abot 0 km i or galaxyTi mecaim ill ted to keep te ratio /( U) cotat if tetarformatio rate arie oeer it may be dict to recocie botte FIR/radio correlatio (ic reqire tat te radio eergy deity berogly proportioal to ) ad a cotat /( ) it miimmeergy or eqpartio magetic eld ice te relatio betee te miimmeergy magetic eergy deity ad radio eergy deity Vradio

i ot liearVmin V:iO

(Eqatio ). Alo te FIR/radio correlatioold at freqecie a lo a 0 1 GHz (ox et a 988) ad te oberedoteral pectral idice of ormal galaxie ell belo GHz are ota teep a migt be epected If Y 2 (Bell 98) te for Vb.i & Wolfedale ( 990) ietigated model i ic relatiitic electrodie ot of all bt te mot lmio galaxie to get otermal pectralidice i better agreemet it te oberatio Tey amed U Uo U/U + U) /2 atomatically Teir amed diio coecieti proportioal to U o tat coic ray ecape ore qicky fro galaieit trog magetic eld altog erce

&Sclickeier (980) aearged tat te diio coeciet old decreae it B Fially teradio emittig olme a claimed to be proportioal to & Tte emiiity i early idepedet of lmioity i cotrat it te

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RAO ESSON RO NORA GAAES 0 obervatio tat ource it iger R ave maller volume ad veryig emiivitie (odo et al 1990) ee aumptio are o trog

tat tey leave little room for departure from te FIR/radio correlatiobut tey may ot be valid for real galaxie.e oberved FIR/radio correlatio i ot preciely liear epecially ioptically elected ample cotaiig very lo-lumioity galaxie (Fitt etal 988 ox et al 1 988 Devereux ale 989). alaxie it lo FIRlumioitie ave eve loer radio lumioitie ta expected. Suc aoliearity ould occur if eiter te FIR or radio lumioity i otdirecty proportioal to te tar-formatio rate. e tocompoetmodel for FIR emiio (elou 198 odale-Pero elou 1987)iclude a arm "active compoet fom duty molecular cloud eatedby te maive youg tar repoible for radio emiio plu a coolcirru compoet of dut eated by te geeral itertellar radiatioeld. If te cirru compoet of galaxie i a quiecet pae i eatedprimariy y te oer radio-uiet tar popuatio te cirru cotributio to I ould be ubtracted to make te FIR/radio correlatioliear Fitt et al ( 988) attempted to correct te FIR/radio corelatio byuig te oberved FIR color temperature to etimate ad ubtract teFIR emiio fro te cool (tey aued 0 K) dut copoet of

eac galaxy. Devereux

ale (989) argued tat te iteity of teradiatio eld eatig te cirru compoet i proportioal to te bluelumioity ad tey ubtracted a xed ractio of te blue lumioity fromte FIR lumioity of eac galaxy to learize te FIR/radio correlatio.Alteratively i Wolfedale ( 990) aumed tat te FIR lumioityi proportioal to te curret rate of maive tar formatio ad ececomicray productio but tat te radio lumioity migt be deciet ilolumioity galaxie becaue te comic ray are more likely to ecapey diio (or covecio). ey corrected te oberved radio lumioitie for teir etimate of tee loe to make te FIR/radio correlatioliear. odo et al (991a) ivetigated te FIR/radio correlatio forto elldeed ample of ormal galaxieoptically elected piralgalaxie briter a BT + d te IRAS Reved Brit aaxySample it S60m 5.24 yit ucietly accurate 1.49 z uxdeitie fo idividual meauremet error i q to be maller ta teitriic catter i te q ditributio. ey foud tat oe of te correctio decribed above ca imultaeouly liearize te FIR/radio correlatio ad reduce te oberved catter for bot galaxy ample. A

empirical correctio toq

a foud tat deped o te blueradio ratioit ca imultaeouly liearize te correlatio ad reduce te catter. egalaxie eedig te larget correctio geerally ave te loet radioad ifrared lumioitie but ormal blue lumioitie ugetig tat


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602 OOther crret tarformato rate may be oer tha the average over theat 0 yr. Tu te emprca correcto cotet t eou1986

tocompoet mode bt oy f the radooud popuato ofmave ; 8 tar eat bot te arm dut II rego adcotrbute gcaty to heatg te crru dut hc eed ot be verycoo. u 990 a recety argued tat te crru heated by oozg from ortved tar te 20 rage. Devereux & Youg 99ed the ()/ rato to gget that the dt cotrbtg to heated prmary by tar th ; 6 at eat gaaxe th > 0 Both ad te podcto rate of comc ray thappear to be drecty proportoa to te recet formato rate of mavetar mot orma gaaxe. oever th ot ucet to eure atght FIR/rado correato t t eceary to ho that the othermarado eergy produced per reatvtc eectro doe ot vary gcatyfrom gaaxy to gaaxy. Ideed comcray ecape or oter oe may bea factor te hg FIR/rado rato of o-umoty ( < 0)gaaxe epecay darf gaaxe th reatvey at rado pectra (Keet a 98 RADIO EMISSIO AD STAR ORMATIO

Nonhermal Lumnoy and he Supernova RaeThe fetme of the mave tar repobe for mot of the rado emofrom norma gaaxe are mch horte tha a bbe tme o the crretrado moty proportoa to te recet tarformato rate. Berma 96 rt cded terma ad otherma rado ux meauremet quattatve gaaxy mode becaue tey had attaed a precohch comparabe to or ome cae ceary better tha the precoof optca mearemet Th poeerg ork compared B- coorth bue/rado ux rato. Berma amed a tmedepedet poera M F () Y th ope y = ad pper ma mt u Atar t N ' 6 ere premed to produce radoemttgperova remat o the rado perova rae iMUVN tdM 6 xtme tegra for each perova remat. Jy yr at 5

Gz he ee from a dtace d

20 Mpc a extrapoato ofte oberved (ark & ae 96 urface brghtedameter -Dreato for Gaactc upeova remat Berma oted that te oerma mt N for rado perova more crtca tha N

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RIO EISSION RO NORA GAXIES 603bcau tp IMF op pl ta ot rado upoa progtora a jut abo N T rut od coud b ad to agr

t t obvd bu/rado rato oy if t aud otra radorgy pr upoa r crad by a factor of tA ry clar driato of t rato bt t uproa ratad t o ta radio uioity iplid by t rlato agi by tad (1982) T 408 MHz data idicat (W Hz r ) ' 10[(pc)] ad (pc) ' 043[(c )][(yr) r t xploo rgy i uit of 10 rg abtpartc dty ad t i t t c t uproa xpoio (lark &al 1976) If t uproa rat i a rado ourc oly durg tadiabatc ft (yr) ' 2

x

10 [(c )] t 1at 408 MHz ltad (1982) ud a rlato lar to quato 1 todri VN fro t obrd rado uioiti of Syfrt aax Hcad t frard/optca uoit fro t clac Rk t al (1980)od D fo M82 t VN ad foud t to xcd t obrd alu

by at at a factor of t T proptd uggtio tat t radoourc ot Syfrt alaxi ar pord by AG tad of tarGrz t al (1983) cotructd a tadytat od for t copacttarburt i G 3690 tat uid fatur of t arr odl adty ud t FIR luoity a t b tat of t bolomtrc uoty of a tarburt Grz t al (1983) copad H FIR, ad radocotiuu uot ofG 3690 t tarburt odl paratrzdby drt IMF op y ad a it ML, Mu Ty alo foud itdicut to rcoc t g uproa rat dd to xpai t ota rado io t t obrd FIR ad H luioiti Truccfu odl a a ry tp (y 3) ad ry trucatd(M ' 2) IMF plu a loM ' Suc odl faor VN izig t bootic uoity ad N Ty caot b appd toa galax c t dicory of Wof-Rayt tar o FIR uougalax (Au t a1 1988) pro tat t IMF do xtd byod 25M galax obyg t ubiquitou FIRrado corrlatoT ad rlatd dculti ar uaoidabl if t SR tlar rqurd to prod al of t ota rado io fro oalgaaxi Hcka t al (1983) argud tat otr AG ot tarburt por trog ucar ourc piral gaax c t aragado pctra d


30/37

64 COOcoul not econcle the hh supenova ate eque to explan the nonthea ao lunosty of the noal spal alaxy GC 93 wth ts

H an boloetc lunostes conclun that "no explanaton can befoun fo the ao esson onbe & Beann 19) foun excessve consupton of H ass by the stabust nucleus ofGC 46 othe LN X 1 W Hz nontheal lunosy of ou alaxy at 4MHz Behusen 94) Equaton 17 ples an excessve ao supenova ate VN .4 y Ths s uch hhe than the Type supenovaate VN y estate by Taann 1 9) o the Galactc pulsabthate 1 3 y yne et a 1 9). Even the ao counts of younGalactc s suest a ao supenova ate VN .3 y Caswell&eche 1979) albet wth lae uncetanty Geen 194) upenovaenants ay acceleate the elatvstc electons poucn the nontheal ao esson n spal alaxes but > 9% of ths esson ustbe pouce lon ate the nvual supenova enants have fae outan the electons have use thouhou the alaxya ol Pooley1969 Ilovasy & equeux 197) but oten ovelooe esult TheefoeConon n 199) oppe Equaton 17 n favo of the obseve

Galai lai bw ad wi imli

1 Equaton 1 pobably apples to ost noal alaxes snce sncantvaatons the ato LN/vN fo alaxy to alaxy woul volate theobseve /ao coelaton Also l et al 1 99) have aue thatthe coscay eney poucton pe supenova s the sae n the stabustalaxy M as n ou alaxy.

ASmpl Modl /or Rado Emon /rom Normal

GalaxThe lobal ao nontheal an theal lunostes plus the F/aoato fo ost noal alaxes can be appoxate by a sple oelwth only one fee paaete the aveae foaton ate of stas oeassve tha [ R( 5o J IMu Mt(M) dM.y J5MG 9The "extene Mllecalo 979) IM (M) M- s tuncate atMu 1 All stas oe assve than MN becoe aoAnnu.Rev.Astro.Astrophys.1992.30:575-611.Downloadedfromwww.ann

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RAO MO ROM ORMA GAAX 605pro o t rdio pro rt VSN i dtrmid dircly by trformtio rt:( VS ) [SFR(M 5M] .41 M yr yr 20. orml lmioity L c t b obtid from Eqtio 8 i i( LN )

X2 1 (_V )-'[SFR(M 5Mo]W H 1 5 3 10 H M Z o yr

wr a 0.8 i t orml pcrl idx.

2 .

T rdio trml frcio c b imd from llr modl for md lctro tmprr e 10 K if dt borptio of Lymcoi poto i gligil rlt o it ( ly[LHO)] 4.4 x 0F( 5W yrT Eqtio 2, 3 d 4 yild( LT ) 5.5 x0 2 o _)- O. I [SFRM 5Mo].WHz Hz o yr- I

22

23 trm frctio implid by t rio of Eqio 1 d 23 grwll wit t rg obrd l (Eqtio 5 T ioizio rt iuv) 3 .5x10[SFR(MMo] . I Moyr I 24.

Bl lmioiy i poor qtitti mr of ry rc 1 yrtr formtio bc of tictio i molclr clod pl cofioby oldr (p o 1 yr obcrd tlr popltio of bl tr (Sg oloo 98 Mi r r formd i dty git molclrclod from wic oly mll frcio of t V or opticl (gH) poto ctlly cp o t rly ll of lmioiy prodcdby tr i H II rgio mrg i t FIR For ypicl dt mprtrd miiii bot 2/3 of i miio ppr i FR bdbtw

4 m d

2 m (Hlo t l 88 orly moo t lmioiy i d mrd y FR i from dt td bytr or i t (r og 1 1.For tim-idpdt IMF

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606

LI 3 M)LM)M) dM

2.

whr eM) is th lifti of a star with ass M an LM) is i ts avragbolotric luinosity Th total nrgy LM)rM) itt by a asivstar uring its ainsqunc lif Mar 1 8) can b approxiat byL 96MMo)32Lo yr If th IMF lop i for M ; Mothn ach logarithic tllar a rang contribut qualy to LI an

6.

Both L + L T an LI ar proportional to th tarforation rat o thiol ipli a linar FIR/raio corrlation Th FIR/raio ratio atv 1 .4 Gz prict by Equations 2 1 23 an 6 is q 4 clos to thavrag obsrv valu q 2.3 or oratly luinous L :9Lo) galaxis (Conon t a 1 l a) Also th ratio La)L .fro quations an 6 is in rasonabl agrnt with th ata inrux on (1990nc SFRM M0 s th only r paratr only on obrvablg th raio luinosity at on fruncy) pr galaxy is n to trin its ol paratrs. For xapl, th aur raio luinosity ofM8 i L L T 10 1 W H at v = .4 GHz Th atio LN/L T 8ollows fro ithr quation or th ratio of quation 1 an . hol hn prict th ar-foration rat SRM . Myr, th raio uprnova rat V . yr th ionization ratN 8 10 an th FIR luinoity Li 4 x OL Thsvalus ar all in vry goo agrn with th ata.Th rlativ contributions to V L L an N L T ro tarsin irt rangs of log

M Mar plott or this ol in Figur inc th rang of tllar ass contriuting ost to V falls within thbro rang of a proucing L, th FIR/raio ratio houl brlativly innitiv to ti variability or lop chang in th auMF. Th thral raction LTL + LT) i lss robust bcus thr i lssovrlap btwn th stllar as rang rsponsibl for suprnova anionizatio. Th taytat ol o Lithrr (10) inicat that achang in th IMF slop chang th log of th thral fracton byapproxiatly / bout x 6 yr ar th trination o a

starburt th ionization rat ithrr 1 0) an hnc th thrmal luinosity all prcipitouly whil th uprnova rat an nonthral isionprist hu it is unlikly that th sharp spctral cuto at v 8 Gzrport or NG 16 i a consqunc of rlativitic lctron nrgy

Annu.Rev





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O IIO O O 60 '

N

- - / - - - -i

.

: ii

M Meure he eave onibions o he spenova ae V he ainae minosi and he ionzaon ae (he as om Leihee 990) pe logahmi ineval oa ma o a mindndn < M/2 uncaed a M = 00 M bsissaog sella mas in sola mass nis dinae elaive onibion pe logaihmi massran

losss in a poststarburst alaxy (Isral & Bruyn 88 sinc NGC 6still as a noral tral fraction7 SUMMARYIprssiv avancs in bot obsrvation an ntrprtaton av bna in t t snc t nral rviw of rao sson fro spralalaxis by van r Krut & Alln 76. T VA as prov t spto ap unrs of alaxis n coplt sapls, t snstvity to tcton o niiual rao suprnoa an SNs in xtrnal alaxis, trsolution t ap narby alaxs in tail an to rsolv vn t ostcopact nuclar starbursts an t ability to a aps at svral frquncis wt silar u )plan covra. Equally iportant is lRAS,wos F sy surcy provi complt sapls of normal alaxsranin fro t quiscnt to t ultraluinous L > 0L ansow tat t FI/raio corrlaton is rarably stron an unvrsal.T FI/rao corrlaton s t sinl ost portant factor in t wspra accptanc of assiv stars as t nry sourc for bot t FIan nontral raio sson from noral alaxs It also suststat t starforation rat

SFR(M

M

s t onant varablcontrolln t ran of FI an raio lunosts obs Otrfactors suc as antc l strnt itr play a nor rol or onot vary sinicantly fro orinary is alaxs to lunous nuclarstarbursts.


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608 CONDONMol rlating th thra raio non thral raio an FR luinoiti o galai to SRM 5M an no b ontru tht ar

oitt it but ot ruir by th ata For ap t piriarlation btn th uprnova rat an nonthral raio luinoityEuation 8) o not plain ho i ray ar gnrat in uprnovarnant propagat in th intrtlar iu an lo thir nrgy orap ro th gaay it rly p th probl unr th rug.But uh ol o highlight th pobl that rain to b olv bybttr analyi an obrvation iting ata on th trong narby ourin M8 iniat hat ight b on ith othr noral gaai uingiprov intrunt in th nar utur. Dirt tiat o th uprnovarat ar baly n to pin on th rlation btn non thral raiouinoity an th SR. Th VLA i apab o onitoring th nubro NR in M8 thir u niti an vn thir angular iz PrioiVLA obrvation o othr narby galai oul b nitiv nough tott n raio uprnova an trin thir avrag raio uprnovarat ithou th optia iiation o onuion by tarlight an intionby u At ot hav an otli at mght b oy th utur ibring th ul pitur o hat ust b.CKNOLEDGMENS

Th Nationa Rio Atronoy Obrvatory i opr by Aoiatnivriti n unr ooprativ agrnt ith th National inFounation. thank Pat Cran org Hlou Allan anag JoanWrobl an pialy Ko Hu or any valuabl uggtion anont.Lterature Cted

llen R J. Suuma S 99 See Bloeme

99b pp 28794nonu R R J lvesad S 988 ApJ. ett 0 9700

mus L Heman . M le G 988 Ap J ett 2 4-49

Banes . , Henqui E 99 Ap ett 70 -8

Bael N., Rane Roges Shapiro Bonometti R et a 987Ap 2 5

Bec R 982 Astron. Astrophys 0 2 32

Bec R 99 Astro. Astrophs 25 -2Be R en ause M 985

Astron. Astrophs. 2 2749Be R oiseau N Hummel , Be

huijsn, v R al 989Astr Astrphys 222 58-68

Bell R 978 MNRAS 82 47-56

Behuijsen M 984 Astro Astrphys4 4 40Beuemann K, anbah G Behujsen

M 985 Astr Astrphys. 5 7-4Biay M D Helu G 990 Ap J 2

597Bierman 97 Asto Astrophs.

295-Bomn H 99a Sc D & Cran 99

pp 276Blemen H d. 99 The Interstellar

Dk-Hal Cectn Galaxes Dodh: Kuwr

Baun R 99 Ap Suppl 72 76-75Bucl U R. 988 Astron Astrophs

25 294Bubig 9 Ap_ J. 24 429Cane H V 979 NRAS 89 465-78

Annu.Rev





35/37

O IIO O O 609Capa, ., Deaeg, L 1 86. Asron

Asrophs 155 27-313Castom, . E., obeg, . 1 1 . Ap.

. 366 22- 1Caa, ., Tue, . L., Ho, . T. 10.

Ap . 362 32Caswe, . L., Lece, 17. MNRAS 187

201-16Capa, 1 M SaeySt, Axo,

D. ., ge, S W., Coe, . 1. e a.1 0. MNRAS 2 281 0

Ceae, . A. 182. Ap. . 25: 3021 0Cee, . A, Lag, E. . 1 8. Ap .

3: 3320C, X Woedae, A W. 1 0. MNRAS

25 101-7Cak, D. H, Caswe, L. 176. MNRAS

1 7 267-305Codo, . . 1 83 Ap . Sppl 53: 5

95Codo, . 187. Ap . Sppl 65: 85

51Codo, . . 18. Ap. . 338 1 3-23odo, J J Adeso M. L., Heou, G.

11a Ap 376 5-103Codo, . ., Bodeck, . 1. 186. Asron

J 2 102Codo, . ., Bodeck, . . 188. Asron

J. 6 306 1Codo, 1 , Bodeck, 1 1 1 . Asron.

102 1637Codo, . Codo M. A., Gse G.,

usce, . 182 Ap 252 102-2Codo, 1. aye, D. T, Bodeck, 1 . 1 .11b. Asron 101 362-0

Codo, Heou, G., Sdes, D 8Soe, B. T. 10 Ap . Sppl 73 35-00

Codo, . . Hug, Z.., Y, Q. . ,Tu, T X 11c. Ap . 3 78 6576

Codo 1 Y 10 p 357710

Cowe, ., Bu . 18. yntssImagng n Rado Asronom, ed. A.eey, Scwab, A. H. Bde, pp.1 67-83 Sa acsco: Asto. Soc. ac.

Cox, M. 1. Eaes, S. A. E, Aexade, .,, A. 188. MNRAS 235: 12273

de Gjp, M. H. ., Mey, G ., Lub, .187. stro stroys 70 51 1

de Gjp, M ., Mey, G ., Lub, 1. de og, T. 1 8 5. Nate 3 1: 202

de og, T., e, U , We1ebsk, Wudec, E. 185. Asron Asrophs 17L6

Deeeux N Eaes S A 1 8 Ap .30: 70812

Deeeux, N . A. , oug, S . 10. Ap. . 350 L25-28Doge!, V A. 1 0 See B1ee 1 1, pp.175-86

Dowes, D., Wso, T. L, Begg,

Wk, . 1 80 Asron Asrophs Sppl0 37

Desse, L. L 188. Ap. 32 L6-73

Duc, N 186. Ap. . 30: 61 1 0Duc, N., Boueu, E., Gegoy, C.

188. Asron . 6 811Duc, N. , Cae, . C., ed. 1 1 . h

Inerpreaon of Mode Snhss Obsrvaons ofSpral Galaxes. Sa acsoAso. Soc ac.

Du, N., Dma M. . 188. Ap . e332 L67-70

Duc, N., Sequst, E. ., Cae, . c,Das, L. E. 1 86. Ap. . 30: 82-5

abbao G. Tce, G. 1 85. Ap . 26306

aao, G., Goa, M., Tce, G.188. Ap. 32: 7-66

, A. J Aede, ., Co, M. . 1 88 .MNRAS 233 0721GacMuoz, M., Mas, G M.

Smpso . A 177. Ap. 217 85-77Gez, . D. Samek, . A., Weedma, D.

W 83 67 5516Gzbug, V L., aza, Y. M., usk,

V S 180. stroys ae S 68 23 1

Gug V L. , Syos, S . 16. ThOrgn of Cosm Ras New Yok egao

Goa M. Gego L. , e, 1 82

Asron. Asrophs 1 16: 1 67Guc, G., Madossa, . Mee, M18. Asron Asrophs 208: 273 1

Ge, ., e, U., Weesk, 10.Asron. Asrophs 238 3

Gee, D. A 1 8. MNRAS 20 -78Gu S F 173. MNRAS 1 6 1 7-6Haett, Beck, ., Buczowsk, U. .

8 sron roph 33Haw, M, Houck . , Soe, 8 T.,

uo, G G. C. 1 87. J. 315 285

Haw, M., , 175. p J. 200L1272

asa, , soe, 17Nare 327 21 1-1

Heckma, T. M ., a Beuge, W., Mey, G.., Buce H 183 stron J 881077-87

Heou, G. 186. Ap . 1 1 L33-36Heou, G., a, ., Maek, L., Boee,

L 188. . 68 151-72Heou, G., Soe, 8 T., owaobso,

M 185. Ap. . e 28 L7- 1 1Hequst, L. 18. Nare 30 6871Hoeou, c Beck, ., e, . 1 0

Gala and Inrgala agne elds

ed. . Beck . . obeg, We1esk, pp 1 1 12. Dodect uweHumme, E 181. As/ron. Asrophs. 3 3

105

Annu.Rev.



ualreviews.org

byU



seonly.


36/37

60 OOumme E 1986 Aston Astophys 60:

ummel E 990 Windows on Galaxies,

ed. G. Faao J S Gallage ARe pp 141-55 odech Kuwe

umme E 1991 Aston Astophys 251 442

ummel E 1991b See Boeme 99b, pp25766

ummel E Bec R Dahlem M 199Aston Astophys 248 2329

umme E . Dahlem M va de uls JM Suuma S 1991b Aston Astophys 246 10 20

ummel E Daves R D WosecroR. D va de uls J M Pedla A1988 Aston Astophys 99 9 104

umme E Dema R. 990 AonAtophys. 236 3346

ummel E Gve R. 1990 Aston Astophys. 228 3 526ummel E esch Weles R

Schlcese R 1988b Aston Astophys197 L23 1

umme E va de us J . M Kecu R Kel W 99Aston Astophys 236 33345

Hm D G., toy J 987 MNRAS224 80120

Iovasy S A eueux J 972 AstonAstophys. 20 34756

srae F P de Buy A G 98 8 As/onAstophys 198 10915

srae F P Maoey M J 990 Ap J352 3043

srael F P va de uls J M 1983Aston J 88 73648

Jes R 984 Ap J 277 5012Kauma M Bash N e Ros

A Elmegre D M e al 989 ApJ. 345 67496

Kcu R 983 Ap J. 272 5467Kecu R 983b. n. Asph.

2 2922Kecu R 984 p. J. 277 3666Kecu R 989 Ap. J. 344 685

703Kecu R c, Pogge R W 990 AstoJ 99 670

Kle U 982 Aston Astophys 6 1 7578

Kle U Bec R Buclow U R Weles R 1982 Aston Astophys 10876 87

Ke U Emeso T 1981 AstonAstophys 94 2944

Kle U Gve R 986 As/on Astophys 16 15568

Kle U Wead Brs E 199 Aston Astophys 246 32340

Kl U Weles R ayes R. FMal D F 1989 Aton. Astophys 2 1 2892

Ke U Wees R Mos W1988 Aton Atophys. 90 6

Kle U Wees R Thua T X984 Aston. Astophys 4 244

Ko M Pae E N 1989 Ap. 341 82831

Krause M 990 Galati and Intealacti Maneti Fields, ed R Bec PP Kroeg R Wes 8796.Dodec Kuwe

Kause M Bec R umme E 989Aston Astophys 217 730

Kause M ummel E Bec R 989b.Aston Astophys. 217 4

Koeg P P Bema P 98 Ap J243 8996

Koerg P P Bema P Scwa FR 1 985 Ap J 29 693707

Kroerg P P Same R A 985. S

227 2831eer 990 Ap. J pp 73 -2eueux 197 1 Aston Astophys 5 42

49erche Sclcese R 1980 Ap J. 239

089 06che I Sclcese R 1982. Aton

Astophys 07 1480ogar M S 98 Hih Eney Asto

physis. amdg amge Uess

osdale J. acg P B orow TP RowaRoso M 1990. Ap J 358680

osdaePesso J elou G 1987 Ap 2

ye A G Maces R N Tayo J 198 MNAS 2 3 6 339

Maede A 1987 Aston Astophys 17324762

Mahewso D S va dr Ku Bouw W N 972. Aston. Astophys 1746886

MKee F. 988. Spenova emnantsand the ntestella edim, ed R S.Roge T L adece pp 0 amrdge: amdge Uv Pess

Mller G E Sca J M. 1979 Ap J Sppl4 51 347Nege N Kle U Bec R We

les R 99 Nate 352 7883Nlso P 973 Uppsala Geneal Catalo of

alaxies Uppsala Uppsala Aso sNoeau Koeg P P 1987 Aston. J

93 0453Nos R P Alle D A Sam R A

Keseve M . J Toup E R 990. Ap J359 29195

Pacocy A G 1970 adio Astophysis.Sa racso Freema

Pae E N 965 Ap J 142 58490Parer E 966. Ap J 45 8 33Pooley G G 1969. MNAS 144 1027Puxley P J Bad P W J . Mooe T

Annu.Rev





37/37

IO IIO O O I 61 1J T Mountan C M Nakai N et al1989 Ap J 345: 63-68

Reuter rause M Wielensk RLesch 99 Asron Asrophys 48:

Rickard L J arve M 984 Asron 89 5Rieke G eosk M J Thompson

R Low J Tokunaga A T 98Ap J 8 4

Ruin R H 968 Ap 54: 9-95Rupen M van Gorkom J H napp

G R Gunn J E Schneider D 987Asron J 94 6-7

Sage L J Solomon M 989 Ap J e34 Ll5-8

Sandage A Tammann G A 98 ARevsed hapeyAmes Caao of Brh

Gaaes. Wshngton DC: Carnegie nstWashingtonSaunders W RowanRoinson M Law

rence A Etathiou G aiser N et al1990 MNRAS 242: 3 8-37

Scovile N Z Sargent A Sanders DB Sofer B T 99 Ap. J. . 66:L5-9

Seaust R degard N 99 Ap J369

Segalovitz A Shane W W de Brun AG 976 Nare 64 -6

Shklovsk S 968 pernovae London:Wle nterscience

Sironi G 974 MNRA 66 45-53Skiman ein 988 Asron

Asrophys 99: 666Sofue Y Fuimoto M Wieleinski R

986 Ann Rev Asron. Asrophys. 4:45997

oifer B Boehmer eugeaue Sanders D B 989 Asron J 98 76697

Sopp M Alexander 99 MNRA5 - 8

Sukumar S Alen R J 989 Nare 34:537-39

Sukumar S en Grve R 987

Asron Asrophys 84 778Tammann G A 98 n peovae Arvey ofCrren Researh ed M J Rees J Stoneham pp 7-4 DordrechtReidel

Tilanus P J llen R J 99 Ap Je. 339: L57-6

Tianus R J Allen R J van der HustJ M Crane C ennicutt R C 988Ap J : 6677

lvestad J S 98 Ap. J. 59: 96ranik M Beck R ein Grve R

989 Asrophys pae 56: 9598van den Bergh S Tammann G A 99 Ann Rev Asron Asrophys 9: 363-47

van der ulst J M nnicutt R CCrane C Rots A H 988 AsronAsrophys 95: 38-5

van der ruit C 97 Asron. Asrophys5 :

van der ruit C 97 Asron. Asrophys9: 6-75

van der ruit c Allen R J 976 AnnRev Asron Asrophys 4 4745

van der ruit C Allen R J Rots A 977 Asron Asrophys 55: 43van der Wat D J 99 Asrophys pae

68: 337Viallefond F 99 Du & Ca 99

pp 799Vk J 989 Asron Asrphys 8: 67-

7Vk J ein Welesk 989

Asron Asrophys L-4Ward M J 988 MNRA 3 : p5pWeer W R 99 See Durc & Crane

99 pp 374Wester A 97 Asrophys e 5: 89-

92Wester A S 974 MNRA 66 357Weier W Sramek R A anagia N

van de r Hulst J M Salvat M 9 86 ApJ : 798

Werner W 988 Asron Asrophys -8

Wilknson N de Brun A G 99MNRA 4: 5934

Willner S Soifer B T Russell R WJoce R R Giett F C 977 Ap J 7: L4

Wroe J M Heeschen D S 988 Ap

335 677-87Wroe J M eeschen D S 99 AsronJ : 4869

Wundelch len Welensk R987 Asron Asrophys. pp 69: 487-54

Xu C 99 Ap J e 365: L47-5

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