Quasar SP-2721 User Manual

ResearchDuringthefirstpartoftheyearCometHalleystoodatthecentreofattentionofmanyobservers.Accu-ratepositionsweredeterminedatthetimethecometreappearedfr

formeris"new",coming for thefirst time from theouterreachesofthe solar system, while the latterhas been close to the sunmanytimes.Also in th

Thispholoofomet HalleyinSagilla-ril1swas obtained byT.HäfnerOllMa"ch2/.The photo, a 10-minuleexposureoncolour reversal film, wassubsequelllly enh

A new molecule was discovered inthe interstellar absorption spec-trumofzetaOphiuchi.This spec-trumhad been studied extensivelyat various observatories

obtained in the opticaldomainonthe star beta Pictoris. With the 2.2 mtelescope, an occulting mask and asophisticated image analysis, a disklikestructu

30DoradusNebulaintheLargeMagellanicCloud.Innine regions,theelemental abundanceswerefoundtobe similartothoseinthecore.Thisindicatesthatmeasure-mentswit

star. Results like thiscouldneverhave beenobtainedbya singleobserver- unlessequippedwithhisOwntelescope.Onthe basisofobservationswithCASPECat the 3.6

numberofvery high velocity starshas been found, includingonewitha radial velocityof595km/sec, thehighestknownfor any galactic star.FromCASPECspectra i

A search has been made with theCAT/CESfor the [Fe XIV]coro-nal emission line at 5303 A inthespectrumofzeta Puppis.ThesoftX-ray flux,wheninterpreted in

Withdata from radio telescopes,ESO,IUEandEXOSAT,studieshave been madeofthecontinuumemission from the quasar3C273.Large variations werefoundinhardX-ray

COVFRPICTURFT!Jisillji'drcd i/l/Il?,e (2.2fJ../I/)0{l!Jeillllcrlt/ost regiollort!Jeg,i/'lctic cellIre(j,hlSo!Jtdilledwit!Jl!Je2.2-/1/ le/esc

ThescaleoftheUniverse(HubbleConstant)remains amuchdebateditem, in particular becauseofitsrelationtothe ageofthe Universe.Fromstudiesofgiant H II regio

night.Inthe cluster A 370witharedshiftof0.374, some 90 spectrahave been obtained atESOand attheCFHT.Anunexpected percen-tageofspiraltypegalaxies (50(1

1.64microns;withan intensitycomparabletoH beta. A detailedmapofthis linecouldbeobtainedinpartofRCW103. Severalother[FeI1]lines were also detected inth

2ndESO-CERNSymposiumon"Cosmology,AstronomyandFundamentalPhysics", Garching,17-21 March.ESO-ESAWorkshopon"Interre-lationofGroundBased an

upgradedbyexchangingboththeVAX11/780 andVAX111785with VAX 8600computers.Thisincreasedthetotal capacityoftheVAX clusterbya factorofmorethan three.TheVA

AportableversionofMIDASisbeing developed,whichwillrunonbothVAX/VMSandUNIXsystems, for release in the springof1988.N ew mechanics and optics wereimplem

lates an observationofan astro-physical targetwithanyoftheSTinstruments.Thesimulationincludes effects like diffractionpatterns in the telescope and in

planned to load theIUE"Iine-by-line" imagesonthe opticaldiskoComputerCommunicationswithEuropeanand American Instituteshave considerablyimpro

FacilitiestelescopesVLY':Followingthe workshop in Venice'onthe VLT, work was started on,t~e'preparation of the "Proposaltorthe con

structureswithlowthermal inertiaandlowwinddragbutwithhighstiffness.Thetubehas a massof109tonswitha first eigenfrequencyof10Hz,the fork a massof110 ton

Annual Report / Rapportannuel/Jahresbericht1986presentedtothe Council by the Director Generalpresente au ConseilparleDirecteur generaldem Rat vorgeleg

tion willbemade use ofina mostefficient manner.Extensive site studies contil1lledinthe north of Chile,inparticular atParanal. Results about c10ud cove

The meleorological condiliollsalPara-nal areclIreJIIII)'mOllitored severallimcs cver)'da)'.Lesrelcves meteorologiqHcsSill'Icsitede

Tbe tower/0/'the small telescope to beillstalled/01'seeing measlfrementsIn/987. The necessary eleetronics IShOlfsedinthe container blfilding

The SEST nearingiLscomple/ion.SESTThemountofthe15 mSwedish-ESOSub-millimetreTelescopewaserectedduringthefirst halfoftheyear.Subsequently,astartwasmade

MOlln/ing /he reflec/ive panels0//heET.Mon/agedespannellllX rf!flec/e/lrsSIIrleSET.Monlage der RefleklorelemenledeET.extenivepointinotests and beampr

TheEroCechellespeclmmoftheQSO1208+1011.Theobjeet has avisualmagui-tudeof17.5andoneofIhe highest redshiflSknown(z = 3.8). Thisimageistheaver-ageoftwo90

These two figllres illllstrate theuseoftheWoilastOllprismillEFOS for areapolarimetryofextellded objects. Theleft-handfigureisan[011lj,5-milluteexposll

Muchprogress was made in theconstructionofDISCO,the newCCDdirect imaging camerawithan imagemotioncorrection capa-bility.Thefast movingmirrorwasprocure

theotherhas been installed at theDanish 1.54 m telescope.WithproductionofCCDsforastronomical applications beingstopped by some manufacturersRCA) and b

Max-Planck-Institut fürAstrono-mie in Heidelberg.SomeIRarrays were received andare undergoing extensive tests inGarching.Muchelectronics hadtobe built

Tableof ContentsINTRODUCTION. . . ...5RESEARCH9Joint ResearchwithChilean Institutes ...21Conferences andWorkshops.21Sky Survey . . . . . . . . . ...22

At the 2.2 m telescope, theCCDimaging camera and theCCDspec-trograph continued to occupymostof theESOobserving time with43% and 37 % respectively. The

betweenmoonlitand moonlessperiods, itisexpectedthatat the 3.5mNTTinstrumentchanges willbecome rare, since at thetwoN as-mythfocitwodifferent instru-me

Telescope Use / Utilisation de telescopes /Verwendungder TeleskopeTelescope ITelescope I Teleskop3.62.21.51.5DCAT1.0OtherNights INuitsINächte365271365

involve scientists from theESOcountries.ltisevident from thesefiguresthatESOasaninstitutioniswell integratedintoits largercom-munity.Atthesame time, t

orothercollaboratorstakes place,the actualnumberofscientistsbenefittingfromLaSillashouldsubstantiallyexceedthe612 inthetable.d'analyseyfontsuite,

Europe/EuropaElectronics /ElectroniqueIElektronikOpticalInstrumentationGroup/Grouped'instrumentationoptiqueIOptischeInstrumentations-GruppeInfrar

Halfofthelattermaybe consideredto be relatedtotelescopes and theotherhalftothe scientificpro-grammeofESO.Ifthings are ap-POrtioned in thisway,wecometo

Assistants.Tothis areaddedtheapportionedcostsoftheEuropeantechnicaldepartmentsandthegeneral(T.R.S.+112Astronomy)costsattributedtoeach telescope.Thelat

cost appearstovaryastheinversesquarerootofthetelescope diame-ter.Ofcourse,thefigures givenwil1changefromyeartoyear:thehigh costofthe2.2 m telescope fo

enceroom,above whichisthe newspace for the image processing ter-minals.Thetwotopfloors containa totalof22new offices.Ontheothersideofthe building anad

This pieture01NG104, 01' 47 Tltca-nae,isa coIour composite madelromB,ValidR plates obtailled with the[SOSchmidt telescope. Observer:G.Piz-zaro; c

FinancialandOrganizationalMattersThe reviewoftheESOStaffRegu-lations,announcedinthe1985AnnualReport,startedin 1986withthepresentationofproposalsto the

As usual, the following tablesshowasummaryofthe financial situationin 1986 and the forecast for 1987.50Commed'habitude, la situationbudgetairepou

Budget Statement1986/ Situation budgetaire de1986Haushaltsituation1986(inDM1000 I en milliers deDM)Expenditure I Depenses I AusgabenBudgetHeadingAppro

Budgetfor1987/Budgetpour1987/Haushaltfür1987(inDM1000 I en milliers deDM)Expenditure/ Dcpenses / AusgabenBudget HeadingRubrique du budgetKapitelEurope

Appendixes',lAnnexes/Anhang

\Jl-""APPENDIX1-UseofTelescopes /ANNEXE1-Utilisation des telescopesANHANGI- Verwendung der TeleskopeUseofthe3.6 m Telescope I Utilisationdut

\Jl\JlPeriod/ periode/ ZeitObserver/ Observateur/ Beobachter Institute/ InstitutProgramme/ Programm InstrumentIII28-30Bouchet"- (EncrenazlLecache

V10'Useofthe3.6 m Telescope (Continued) I UtilisationdutcHescopede 3,6 m (continuation) IVerwendungdes 3,6-m-Teleskops (Fortsetzung)PeriodI perio

V1'-IPeriodI PeriodeI Zeit Observerj ObservateurI BeobachterInstituteI InstitutProgrammeI Programm InstrumentX 05-08MighelllButcherlBuonannolGath

U100Useofthe2.2 m Telescope I Utilisation du telescope de 2,2 m IVerwendungdes 2,2-m-TeleskopsPeriodI periode I Zeit ObserverI ObservateurI Beobachter

IntroductionIn lateSeptember1986,ESOcon-vokedabouteighty scientists andengineers to aworkshopin Veniceonthe16m equivalent VLT.TheESOprojectgrouppresen

\Jl'-DPeriodI PeriodeI ZeitObserverI ObservateurI Beobachter InstituteI InstitutProgrammeI Programm InstrumentV 04-06Galletta Padova Discstructur

0'ClUseofthe2.2 m Telescope (Continued) I Utilisationdutelescope de 2,2 m (continuation) IVerwendungdes 2,2-m-Teleskops (Fortsetzung)PeriodI Peri

0'UseoEthe1.52 m Telescope / Utilisationdutelescopede1,52 m IVerwendungdes 1,52-m-TeleskopsPeriod I PeriodeI ZeitObserverI ObservateurI Beobachte

0'NUseofthe1.52 m Telescope (Cominued) IUtilisationdutelescope de 1,52 m (continuation) IVerwendungdes 1,52-m-Teleskops(Fortsetzung)Period I peri

'"V>Period/ Periode / ZeitObserver/ Observateur/ BeobachterInstitute/ InstitutProgramme/ ProgrammInstrumentX31-XI03VitonlPrevotlSivan Mar

0-~Useofthe1.4 mCAT+CES(Continued) IUtilisationduCATde 1,4 m +CES(continuation) IVerwendungdes1,4-m-CAT+CES(Fortsetzung)Period/P~riode/Z6tObserverI Ob

C1'!JlPeriod/ Periode/ZeitObserver/Observateur/BeobachterInstitute/ InstitutProgramme/ProgrammInstrumentIX03-09BarbierilBenacchiolCristianilNotaP

0'0'Useofthe1 rn Telescope /UtilisationduteIescope de 1rn/Verwendungdes I-rn-TeleskopsPeriod / Periode/ Zeit Observer/ Observateur/ Beobacht

0''-JIPeriod / Periode / ZeitObserver/ Observateur/ Beobachter Institute/ InstitutProgramme/ Programm InstrumentV28-VI02deMuizon/D'Hend

ü'00Useofthe1rnTelescope (Continued) IUtilisationduteIescope de 1rn(continuation) IVerwendungdes I-rn-Teleskops (Fortsetzung)PeriodI periode I Ze

site testing campaign was contin-ued innorthernChile, and also atLa Silla, with a varietyofinstru-ments inorderto obtain a betterunderstandingofthe st

er-'oDPeriod / Periode / ZeitObserver/ Observateur/ Beobachter Institute/ Institut Programme / Programm Instrument1118-III20DKIII20-25Heydari-Mal

'JoESOUseoftheDanish1.54 m Telescope (Continued) IUtilisationparI'ESOdutelescope danois de 1,54 m (continuation) IVerwendungdes dänischen 1,

APPENDIXlI/ANNEXE11-ProgrammesANHANG11-ProgrammeI.Galaxies / GalaxienE:Antonello/P.Conconi/G.L.Chincarini(Merate):Super-glant stars asdistanceindicato

D.Kunth/P.Arnault/I.Tarrab(Paris):Nearinfraredphoto-metryofbluecompactgalaxies (3.6 m).D.Kunth(Paris)/W.L. Sargcnt (Pasadcna):Scarch forCaII Hand Kabs

R.Falomo(Asiago)/P.Bouchet(ESO)/L.Maraschi/E.G.Tanzi/A. Treves (Milano):Studyofthe optical-infrared conti-nuumofBLLacertae objects (1.5 m).K.j.Fricke/

M.Heydari-Malayeri(ESO)/G.Testor(Meudon):Studyofcompactexcited blobs in the MagellanicCloudsandoftheirnebular and stellarenvironment(1.5 m).F. P. Isra

~.McNally/I.A.Crawford(London):Studyofthed.iff~seInterstellarmediuminthedirectionoftheScoOBIassoClation(1.4 mCAT).M. deMuizon(Leiden)/L.d'Hendeco

galaetic centreandoftheRAqrjetwithan infrared camera at2.2,3.5and 5 microns (2.2 m).W.Liller/G.Alcaino (Santiago):VRIphotometryofglobularclusterstanda

W.H.Lewin(MPIGarching)/H.Pedersen(ESO)/].van Para-dijs(Amsterdam):A searchforfast optical quasi-periodicoscillations in ScoX-I(1.5 m D).G.Noci(firenze

A. M. vanGenderen/W.J. G. Steemers (Leiden)/K. A. van derHucht(Utrecht): Study of the optical micro-variability ofWolf- Rayet stars(91cm Du).M. Gerbal

TheE T phologwphcd dHrillgIheonslmcliOIlperiocl.LeESTphologrrlphicrllI1't1l1llt1periodecleCO11sImcliOIl.DasE TwiilnemlriesZHsanllllclI-balls.mirr

M. T.Ruiz/].Melnick/P.Ortiz(Santiago):Monitoringoftime variationsofthe Balmer line profilesfromTlCar(1.4 mCAT).M.Scardia (Merate):Mesuresmicrometrique

E. W. Eist (Uccle): Investigation of the orbit of the Troyansand calculation of the massofJupiter(GPO).Th. Encrenaz/J. Lecacheux/M. Combes (Meudon): I

APPENDIX111/ ANNEXE111-PublicationsANHANG111-VeröffentlichungenVisiting Astronomers / Astronomes visiteursGastastronomenAlcaino,G.,Liller,W.:BVRICCDph

distanc<~ofDXDei, and theproblemofthe mean absolutemagnitudeofRRLyrae stars.AA,159,255-260.Burki,G.,Meylan,G.:RRLyrae, 8 Seuti,SXPhoenieis starsand

Fricke,K.j.,Kollatschny,W.,Loose,H.-H.:Groupsaroundbright Seyfert galaxies. In: StructureandEvolutionofActiveGalaetic Nuclei,eds. G. Giuricin,F.Mardir

tudes, and from stars in the Mathewson and Ford polariza-tion eatalogue.AASuppl., 64, 487-494.Krautter,].:Th28: a new bipolarHerbig-Harojet.AA,161,195

on "ESO's Very Large Telescope", eds.S.D'Odoricoandj.-P.Swings, p. 269-277.Roddier,F.:Guidelines for a site testing campaign and t

Telescope", eds.S.D'Odoricoand]'-P.Swings, p.289-296.Weigelt,G.,Baier,G.,Ebersberger,].,Fleischmann,F.,Hof-mann,K.-H.,Ladebeck,R.:Highr

Crane, P., Hegyi,D.].,Mandolesi,N.,Danks, A. c.: Cos-mic background radiation temperature fromCNabsorp-tion. AstrophysicalJournal, 309, 822-827.Crane,

Garay,G.,Rodriguez,L.F., vanGorkom,J.H.:Rotatingand cxpanding ultracompact H II regions.AstrophysicalJournal,309, 553-563.Andersson, M., Garay,G.:A wa

Muchworkwas donebyESOstaffandbystaff ofthe ESO-ESAEuro-pean Coordinating Facility for theSpace Telescope (ST-ECF)onthefurther expansion of the MIDASim

Ochsenbein, F.: Data storage and retrieval in astronomy. In:Proceedings lInd Int. Workshop on "Data Analysis inAstronomy", p. 305-313.Oliva,

ray emissionandits correlationwiththeultraviolet inNGC4151. AstrophysicalJournal, 306, 508-521.Morini,M.,Scarsi,1.,Molteni,D.,Salvati,M.,Perola,G.C.,P

418.D.Baade:Nonradialand Radial OscillationsObservedinNon-EmissionLineOBDwarfsand Giants. Invited talkpresentedatJointDiscussion III "Solar and S

461. L. Binette and A. Robinson: Fossil Nebulae in theCon-text of Active Galaxies.1.Time Evolutionofa SingleCloud. AA. August1986.462.D. Baade: Ground

APPENDIXIV- Council and CommitteeMemberson1.1.1987ANNEXEIV- Membres du Conseil et des Comites au1.1.1987ANHANGIV - Rats- und Ausschußmitglieder am1.1.

OBSERVINGPROGRAMMESCOMMITTEE/COMITEDESPROGRAMMESD'OBSERVATIONAUSSCHUSSFÜRBEOBACHTUNGSPROGRAMMEMembers / Membres / MitgliederD. Reimers (1987-91)M

VLT WorkingGroups/ Groupes de travail du VLT / VLT-ArbeitsgruppenSITESELECTION/SELECTIONDUSITE /STANDORT-AUSWAHLA.Ardeberg (Lund)M.Sarazin (ESO)H. van

ESOAddrcsses / Adrcsscs dc]'ESO/ESO-AdrcssenFUROPEIEUROPAKarl-Schwarzschild-Str. 2D-8046GARCHINGb.MünchenfederalRepublicofGermanyTelephone:(089)3

ISSN 0531-4496