ESO & ITALYESO & ITALYSAItSAIt 2003 Meeting2003 Meeting

TriesteTrieste

Catherine Catherine CesarskyCesarsky

The Making of ESOEarly Phases

1952-1962 Preparatory Discussions1962 ESO Convention

(Belgium, France, Germany, Netherlands, Sweden)

1964 La Silla(Chile)

The Making of ESO

Catching up

1967 Denmark enters

1970 -80 CERN umbrella and collaboration

1976 Completion of 3.6-m telescope at La Silla

The Making of ESO

Transition Phase: 1980-1990Novel developments

1982 Italy and Switzerland enterDecision to construct 3.5-m New Technology Telescope (NTT)

1984 ESO invents and demonstrates “Active Optics” (computer-controlled, thin and large mirrors)

1987 Decision to construct 4 x 8.2-m Very Large Telescope Array (VLT)

1989 First light of NTT – the VLT Prototype and Testbench

The Making of ESO

VLT Construction 1990-2001Taking the lead

May 1998 First light 1st telescopeMarch 1999 Inauguration of Paranal ObservatorySeptember 2000 First Light 4th telescope2001 Portugal entersAugust 2001 All four telescopes in operationOctober 2001 First successes with interferometryDecember 2001 “Adaptive optics” installed at VLT

The Making of ESO2002 to…Expanding

2002 United Kingdom entersFebruary 2003 ALMA Agreement Signed

with NSF

New instruments: NACO, VIMOS, FLAMES, MIDI, HARPS

Distribution of International Staff Members by Nationality as of December 2002

Belgium5,5%

Switzerland1,1%

Germ any32,5%

Others10,2%

France17,9%

Netherlands3,3%

Italy18,2%

Great Britain5,1%

Denm ark3,6%

Portugal0,4%

Sweden2,2%

Distribution of ESO Staff Astonomers by nationality as of December 2002

Germ any21,0%

Italy29,0%

France16,1%

Netherlands1,6%

Portugal1,6%

Belgium3,2%

Switzerland1,6%

Denm ark4,8%

Others11,3%

Great Britain9,7%

19%19%6363332332

24%24%662525StudentsStudents

22%22%773232FellowsFellows

18%18%5050275275Int. Staff MembersInt. Staff Members

%%Italian Italian nationalitynationalityTotalTotalCategoryCategory

Members of the Personnel:Members of the Personnel:

ContractContract / / CountryCountry of of OriginOrigin -- ITALYITALY

19.6719.6781,579.1081,579.101.01.1983 1.01.1983 –– 31.12.200131.12.2001

24.6724.677,523.907,523.901.01. 1.01. –– 31.12.200131.12.2001

20.6920.693,779.703,779.701.01. 1.01. –– 31.12.200031.12.2000

4.424.421,043.201,043.201.01. 1.01. -- 3131--11--22--19991999

Share in %Share in %(of all (of all ContractsContracts placedplacedin ESO in ESO MemberMember StatesStates))

EUREUR((€ 1.000)€ 1.000)

PeriodPeriod

+ APEX (2003)

acquired 1964construction from 1965first telescope 19673.6-m in 19753.5-m NTT in 1990now 825 sq. km

La SillaLa Silla

ESO & Italy : the NTT

The membership fee of Italy and Switzerland were used to pay for the 3.5m NTT (1988)

This telescope was the first based on the innovative active optics and open dome concepts. It projected ESO to the forefront of world astronomy

Italian industry contributed to a major share of the project building the telescope mechanics and the enclosure NTT at La Silla Obs

SAIt- 15.4.2003

The NTT (pathfinder for the VLT)The NTT (pathfinder for the VLT)The Italian membership to ESO bought the NTT and brought the The Italian membership to ESO bought the NTT and brought the ideas for active optics to the mainstream of telescope design.ideas for active optics to the mainstream of telescope design.The New Technology Telescope incorporated a multitude of novel The New Technology Telescope incorporated a multitude of novel features:features:

Active support of the primary mirror with force actuators designActive support of the primary mirror with force actuators designed to ed to correct the mirror shape as opposed to passive supports employedcorrect the mirror shape as opposed to passive supports employed in in the past designed to maintain the mirror shape.the past designed to maintain the mirror shape.Active positioning of the secondary to ensure that collimation wActive positioning of the secondary to ensure that collimation was as maintained at all times relaxed the mechanical constraints on thmaintained at all times relaxed the mechanical constraints on the e SerrurierSerrurier truss. truss. Closed loop monitoring and correction of the image quality of thClosed loop monitoring and correction of the image quality of the e telescope through a Shacktelescope through a Shack--Hartmann sensor incorporated in the Hartmann sensor incorporated in the telescope functions.telescope functions.Day time airDay time air--conditioning of the enclosure to ensure minimal thermal conditioning of the enclosure to ensure minimal thermal differentials at start of operationdifferentials at start of operationActive heat extraction from electronics in the telescope areaActive heat extraction from electronics in the telescope areaMinimal dome with good ventilationMinimal dome with good ventilationDistributed control systemDistributed control system

thereof placed in Italy: EUR 5.061.790 (approx. 40 %)

Total Value NTT Contracts placed in ESO Member States: EUR 12.680.000

Telescope EnclosureMECNAFER

Adapter RotOFFICINE GALILEO ators

5 Altitude and 5 Azimuth ServodrivesBERENGO

M3 Support UnitMACDIT ITALIANA

M2 StructureADS Italia

M1 Cell / M1 Support SystemANSALDO

Telescope StructureINNSE

PROJECTFIRMS

NTTNTTNTT first light was in 1989. Images of NTT first light was in 1989. Images of 0.3 0.3 arcsecarcsec became a reality for ground became a reality for ground based observations and set the based observations and set the standard for all future telescopes.standard for all future telescopes.All drawings and technical information All drawings and technical information were provided to the TNG project. were provided to the TNG project. Upgrade project in 1996 to full VLT Upgrade project in 1996 to full VLT compliance and VLT operationscompliance and VLT operationsNTT has been working well with NTT has been working well with impressive scientific returns both before impressive scientific returns both before and after the upgrade project (e.g. SN and after the upgrade project (e.g. SN 1987A and the NTT deep field)1987A and the NTT deep field)

SAIt- 15.4.2003

Wide Field Imager (January 1999 at 2.2-m )•4x2 mosaic of eight 2Kx4K CCDs• 67 million pixels• 33 arc min field of viewINAF Capodimonte . - P.I. D. ManciniContribution: 1 person year (10%) + M€ 0.25 (35%)

The NTT Deep Field, a program in collaboration between ESO and OA Roma astronomers, opened the way todeep imaging at ESO (1997)

ESO & Italy: CCDs Cameras at LaSilla Obs.

SUSI2 -upgrade, based on 4k x4k CCD Camera(Febr 1998 at NTT)

This was the first CCD control system FIERA andthe first CCD mosaic implemented by ESO

INAF- Rome Obs- P.I. E. Giallongo , Contribution: 2 person years (25%) + M€ 0.16 (40%)

WideWide--field imagingfield imaging::MPIA/ESO 2.2MPIA/ESO 2.2--mm

8k x 8k 8k x 8k -- FOV: 34’ x 34’FOV: 34’ x 34’

La Silla InstrumentsLa Silla Instruments

HighHigh--Precision Precision Spectrometer Spectrometer at the 3.6at the 3.6--m telescopem telescope

~ 1 m/sec~ 1 m/secHigh stabilityHigh stabilityAccurate calibrationAccurate calibrationIodine CellIodine CellFiber feedFiber feed

HARPSHARPS

HARPSHARPSAssembledAssembledAlignedAlignedDetector optimizedDetector optimizedFIRST LIGHT FIRST LIGHT on Feb. 12, 2003on Feb. 12, 2003Press Release Press Release soonsoonCommissioning Commissioning nownowOperation from Oct. 1Operation from Oct. 1

HARPS Spectrum of HD 100623 HARPS Spectrum of HD 100623 (K0V)(K0V)

Paranal Observatory

in theAtacama

Desert

View towards East

Gerd Hudepohl (ESO)

Installing the ESO Very Large Telescope

Transformation of the Paranal Mountain

What is Paranal?What is Paranal?Telescopes: 8.2-m UT1, UT2, UT3, UT4 (more 8-m’s than the others combine), 1.8-m AT1, AT2, AT3, AT4 (more than the others have outriggers), DIMM, SID1, SID2, and survey telescopes VST, VISTA (more AΩ than most)Instruments: ISAAC, FORS1, FORS2, UVES, VIMOS, NACO, FLAMES, VISIR, SINFONI, CRIRES, TC1/2, VINCI, MIDI, AMBER, PRIMA, GENIE, Ω-CAM and VISTA-Cam.Other items: 3+3 delay lines, 4 adaptive optics coude systems (2 tip-tilts installed), LGSF, MMU

158 mirrors1+1 coating chambersMore computers than you want to knowAll kept going 24 hours a day, 365 days a year

in the middle of the most arid desert on the planet…..

Who is Paranal?Who is Paranal?

67 engineers and technicians41 astronomers, fellows, etc.3 logistics support staff

With an 8+6 turno for technical staff and 50-50 for most astronomers, the observatory has less than half of these people present at any given time.Outsourcing of most services

• ANTU, KUEYEN,MELIPAL, YEPUN

• 430 tons (total 542 tons)• 8.2-m main mirror(22 tons - Zerodur)

• 1.1-m secondary mirror(50 kg - Beryllium)

• Cassegrain focus• 45º tertiary mirror• Nasmyth focus• Fixed instruments• Active Optics• Adaptive Optics• Interferometer (VLTI) with

4 movable 1.8-m ATs• Observations from the VLT

Control Room

VLT Active Optics System

A Consortium of Italian industrial companies designed, produced and commissioned the four alt-azmounts of the VLT telescope (~ 11% of the total VLT project cost)

The design encompasses some unique features which have made the VLT a telescope with unprecedented performances.

The drive system is based on direct motors that deliver high precision movement s (now adopted also in GranTeCan , the 10m spanishtelescope, and in the ALMA European Antenna).

The compact mechanical structure allows for cost reduction and high eigenfrequencies

ESO & Italy: the VLT

UT Structure

SAIt- 15.4.2003

ESO & Italy : VLT Enclosures

A Consortium of Italian industries was responsible for the design,manufacture and erection on Paranal of the four Telescope Enclosures (contract value ~ 4% of the VLT project cost)

Main Characteristics of the Enclosure

30 meter diameter rotating dome with 9.5 meter wide observing slit and various ventilation openings like louvers and doors. Total rotating mass about 240 tons. High quality steel construction with aluminum sandwich panel cladding. Fully computer controlled operation of all functions. Very smooth and precise rotation and movements due to passive vibration damping systems. Highly reliable operations and low maintenance effort.

VLT Enclosures

SAIt- 15.4.2003

ESO & Italy: 1st Gen VLT Instruments UVES

INAF OA Trieste

Development and Commissioning of Observing Software, Maintenance Software, Secondary Guiding Software, Templates.

P.I. P. Santin

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ESO & Italy: 1st Gen. VLT instruments FLAMES

ItalConsortium: INAF Bologna, Cagliari, Palermo, Trieste, P.I. C.Cacciari; provided 7% of project cost + 8 personyears

Workpackages: UVES fiber DRS, UVESfiber OCS, FLAMES templates

INAF-OA Trieste, P.I.: P.SantinWorkpages: Super OS, FLAMES OCS, GIRAFFE ICS, OCS

SAIt- 15.4.2003

ESO & Italy: 1st Gen. VLT instruments VIMOS and Mask Manufacturing Unit

Built by French-Italian Consortium( P.I. O. Lefevre) with major contribution from Italian Institutes. coPI: P.Vettolani.

• IASF-CNR Milano (D.Maccagni)- MMU; OCS,DRS Software, Templates

•IRA-CNR Bologna - OCS, DRS

•INAF OA Cap. (D.Mancini)-Mechanics, Electronics, ICS

•INAF- OA Brera (F.Zerbi) Optical components

SAIt- 15.4.2003

VIMOS VIMOS –– the Cosmology the Cosmology MachineMachine

First LightFeb. 26, 2002

VLT MELIPAL

Multi-spectra

1000 galaxy spectra

6400 IFU spectra in 56x56 arcsec area

The Antennae GalaxiesThe Antennae Galaxies

IFU spectra of centreMELIPAL + VIMOS

VLTI

“First Light”in March 2001

d = 0.00929”±0.00017”

VLTI “First Light” on 17th March 2001

VLTI First Generation VLTI First Generation InstrumentationInstrumentation

Near Infrared: Near Infrared: AMBERAMBER•• J, H, K bands, 3 beams (closure phase), K J, H, K bands, 3 beams (closure phase), K = 11= 11--2020**,,spectroscopy with R = 10000spectroscopy with R = 10000

Mid Infrared: Mid Infrared: MIDIMIDI•• N band, 2 beams, N = 4N band, 2 beams, N = 4--9, moderate 9, moderate spectroscopyspectroscopy

OnOn--axis fringe tracker: axis fringe tracker: FINITOFINITO•• H band, H = 12H band, H = 12

DualDual--feed facility feed facility PRIMAPRIMA•• OffOff--axis fringe tracker for MIDI and axis fringe tracker for MIDI and AMBER, AMBER,

First Light for MIDI at VLTI

1.5 x 2.1 m optical tableWeighs 1.5 tons6 million €ESO + 11 institutesEspecially useful for the

study of stellar accretion disks (in which planetary formation may be ongoing)

December 15, 20028.2-m ANTU + MELIPALBaseline 102 metresWavelength 10 µmFringes of star ε Carinae

ESO & Italy : the VLTI

Fringe Tracker FINITO: ESO & INAF- OA Torino. First Fringes in Jan 03 in Garching. P.I. M. Gai

AMBER Cooled Spectrograph (to work with up to 3 combined beams, in the 1-2.5µm range).Provided by INAF- OA Arcetri within the F/D/It AMBER consortium(~17% of project, P.I.: F.Lisi) . Paranal FL 4Q2003

PRIMA Fringe Sensor UnitDesigned and manufactured by Alenia Spazio. 2.3 M€ contract, delivery in 2005

Amber View during integration

SAIt- 15.4.2003

VSTVSTA collaborative project between ESO and OAC to place A collaborative project between ESO and OAC to place a powerful optical wide field telescope into operation on a powerful optical wide field telescope into operation on Paranal.Paranal.The The OsservatorioOsservatorio didi CapodimonteCapodimonte is responsible for the is responsible for the construction, erection and commissioning of the construction, erection and commissioning of the telescope at Paranal.telescope at Paranal.ESO provides the site, the civil works, the infrastructure ESO provides the site, the civil works, the infrastructure and the enclosure.and the enclosure.ESO also has undertaken to support the construction of ESO also has undertaken to support the construction of the camera to be used.the camera to be used.ESO will operate the telescope on behalf of all parties.ESO will operate the telescope on behalf of all parties.

VST enclosureVST enclosure

ESO & Italy: Omega CAM

• 8x4 mosaic of thirty-two 2Kx4K CCDs, to be installed at the 2.6m VST in 3Q 2004

• 268 million pixels, 1 square degree field of view

• Italian contribution: 14 person years (~20%) + M€ 0.75 (25%).

INAF- OA Padova, OA Capodimonte, OA Bologna; coPI : E. Cappellaro

SAIt- 15.4.2003

A visual impression of the size of the

Omega CAM shutterand CCD mosaic.

Paranal Additions in 2003

VISIR commissioning (VLT)MIDI commissioning (VLTI)2 Auxiliary Telescopes for the VLTI2 MACAO for the VLTILGSF (NACO upgrade to LGSs)VLT Survey Telescope +AMBER installation (VLTI)

Italy and ParanalItaly and ParanalAES consortium built and erected the main structures for AES consortium built and erected the main structures for the four 8the four 8--m telescopesm telescopesSEBIS consortium built and erected the enclosures for SEBIS consortium built and erected the enclosures for the the UTsUTsSOIMI performed some of the civil worksSOIMI performed some of the civil worksVIMOS (VIMOS (NapoliNapoli, , MilanoMilano))FINITO (FINITO (TorinoTorino))UVES, FLAMES (Trieste)UVES, FLAMES (Trieste)BerengoBerengo is building the enclosure for the VST and is part is building the enclosure for the VST and is part of the group awarded the contract for the VISTA of the group awarded the contract for the VISTA enclosure.enclosure.CapodimonteCapodimonte is building the VSTis building the VST

MUSE X-Shooter Planet Finder-I Planet Finder-IIKMOS-I KMOS-II

Phase A Phase A Phase A Assessment Phase A Phase A

Call for VLT Second Generation Instruments (Nov. 2001)Call for VLT Second Generation Instruments (Nov. 2001)

STC April ‘03

Sep. ’03 Reviewgo/no go

July. ’04 ReviewSelection Sep. ’04 Review

go/no goSelection

Preliminary ProposalsPreliminary Proposals

ESO & Italy:

2nd Gen. VLT Instruments Studies

•X-shooter: high efficiency, intermediate resolution, UV, Vis, J+R Cass Spectrograph.

INAF-Brera, -Catania, -Palermo and Trieste; CoPI R. Pallavicini.

•K-MOS -2: multi-object, 1-2.5µm Nasmyth Spectrograph IASFC Milano, IRA Bologna, IFSI Roma, INAF Arcetri; P.I. D.Maccagni

•Planet-Finder -1: “Non classical” AO system, differential polarimeter & IF spectro-imager

INAF-Padova, coPI M.Turatto (spectrograph)

SAIt- 15.4.2003

4x MACAO-VLTI4x MACAO-VLTINACONACO

SINFONISINFONI

CRIRES AO

AO:The initial

burst

The Adaptive Optics Pipeline

• OWL Ground layer correction• OWL SAO in K-band• OWL MCAO in K-band• OWL XAO <K-band• R&Ds

Analysis2nd generation systems

• Planet finder (03-04)• MUSE MCAO system (03)• MCAO (Falcon) (03-04)• VLT Adaptive Secondary (03-04)

Study

FDRPAE

PAC

Status: March 03

Approval

Final PreliminarySINFONI 2K (04) CAMCAO (04)MAD (04)

DesignDevelopment•SPIFFI GI (Now)•MACAO-VLTI #1 (4/03)

Commissioning

• NACO (P70)

Operation

AIT DevelopmentMACAO#2 (08.03) MACAO#3 & 4 (04)SPIFFI (04) CRIRES-AO systemSINFONI AO (04) NAOS-LGS (early 04)

SINFONI-LGS (late 04)

• Research Training Network of EC on “AO for ELT” ->2004• MCAO concept study & simulations (INAF – Arcetri)• Large Deformable Mirrors (INAF – Arcetri)

• Development of the Layer Oriented Wavefront Sensor for the MCAO Demonstrator (MAD)

• LOWFS opto-mechanics, control algorithms,simulations (INAF – Arcetri)• MAD Control SW (INAF – Padova)P.I. R. RagazzoniTest in Paranal 2Q2004

ESO & Italy: Adaptive Optics Development

SAIt- 15.4.2003

A 100-m Ground-Based Visual/IR Telescope Project

Jupiter Earth

OWL 100mJ Band80% Strehl104 sec0.4’’ seeing

O.1’’

ImageProfiles

One of the “great goals” of astronomy today…

To take a spectrum and analyze the atmosphere of an Earth-like planet

located at a distance of 10 pc (~30 light-years)

you need a 100-m telescope

Search for Search for ExoExo--Biospheres:Biospheres:Solar System from 30 lightSolar System from 30 light--yearsyears

OWL OWL -- Current Design Current Design StatusStatus

6-mirrors optical designSpherical primaryFlat secondary 4-elements correctorNear-IR MCAO

Low cost sliding enclosure, open-air operation

Low cost sliding enclosure, open-air operation

LightweightAlt-Az mount,Modular design,Friction drives

LightweightAlt-Az mount,Modular design,Friction drives

Maintenance building,Mirror covers (mirror maintenance,local air conditioning)

Maintenance building,Mirror covers (mirror maintenance,local air conditioning)

95-m

Study in Phase A (end in 2004)Study in Phase A (end in 2004)Endorsed by ESO’s Scientific & Technical Committee (STC)Endorsed by ESO’s Scientific & Technical Committee (STC)

Science Science -- OpticonOpticon endorsementendorsementEdinburgh (Sep 2000) and Edinburgh (Sep 2000) and LeidenLeiden (May 2001) workshops(May 2001) workshops

MultiMulti--Conjugated Adaptive OpticsConjugated Adaptive OpticsMCAO Demonstrator for the VLT, first light Q4/2003MCAO Demonstrator for the VLT, first light Q4/2003

CollaborationsCollaborationsRTN on AORTN on AOOPTICON (Science case in FP5, RTD request in FP6)OPTICON (Science case in FP5, RTD request in FP6)ESO/AURA discussion on specific technical issuesESO/AURA discussion on specific technical issues

Industrial studies ongoingIndustrial studies ongoingBlank production, wind effects, Blank production, wind effects, SiCSiC, mechanics modules, mechanics modules

Industry confirms cost estimates of main itemsIndustry confirms cost estimates of main items

Status of OWL Status of OWL StudyStudy

ESO & Italy: Collaborations within OPTICON

Joint Research Activities involving Italy, ESO, others (OPTICON JRA proposals for FP6)

•JRA #1: Adaptive Optics (led by ESO): INAF Arcetri; DIAMP Milano, Microgate

•JRA #4: Interferometry : INAF Torino

•JRA #5: Smart Focal Planes: INAF Padova, IASF CNR Milano

•JRA #6: Volume Phase Holographic Gratings: INAF-OABr, LSMPM-Milano

SAIt- 15.4.2003

The ALMA ProjectThe ALMA ProjectAtacama Large Atacama Large MillimeterMillimeter ArrayArray

[ESO + Spain] & [USA + Canada] [ESO + Spain] & [USA + Canada] & (Japan & (Japan -- 2004?)2004?)64 x 1264 x 12--m antennasm antennas7000 square metres total area7000 square metres total areaBaselines to 10 km (10 Baselines to 10 km (10 millimilli--arcsecarcsecresolution)resolution)30 30 -- 900 GHz frequency coverage900 GHz frequency coverageChajnantorChajnantor site at 5050 metres altitudesite at 5050 metres altitudeFirstFirst phase operations 2007phase operations 2007 ready 2011ready 2011

The ALMA Project

New Science with ALMANew Science with ALMA

Cosmology & Extragalactic projectsCosmology & Extragalactic projectsThe early Universe, Gravitational The early Universe, Gravitational lensinglensing, , Absorption lines in quasars, AGN, Normal Absorption lines in quasars, AGN, Normal galaxies, the galaxies, the MagellanicMagellanic CloudsClouds

Star & Planet FormationStar & Planet FormationProtostarsProtostars and and YSOsYSOs, Accretion Disks , Accretion Disks Exoplanets, Small Bodies, DustExoplanets, Small Bodies, Dust

Molecular Clouds & Molecular Clouds & AstrochemistryAstrochemistry

Galaxy Formation in the Very Early Universe

Star & Planet Formation

z = 2.55 z ~ 0.7-2.5

ALMA and ItalyALMA and ItalyALMA governing bodies and committeesALMA governing bodies and committees

•• EAB: G. EAB: G. TofaniTofani, ASAC: M. , ASAC: M. WalmsleyWalmsley, AMAC: S. , AMAC: S. BertiniBertiniParticipating institutionsParticipating institutions

•• ArcetriArcetri: Back End Electronics: G. : Back End Electronics: G. ComorettoComoretto

Industries Industries -- prototype antennaprototype antenna•• EIE EIE -- design, engineering, and integrationdesign, engineering, and integration•• GalbiattiGalbiatti -- steel structures and integration facilitysteel structures and integration facility•• ATR ATR -- CFRP backup structureCFRP backup structure•• PlyformPlyform -- CFRP receiver cabinCFRP receiver cabin•• MediaMedia--LarioLario -- reflector panelsreflector panels•• RIC RIC -- panel adjusterspanel adjusters•• MicrogateMicrogate -- antenna control unitantenna control unit•• ADS ADS -- SubreflectorSubreflector and shutter mechanismsand shutter mechanisms•• FAPS FAPS -- CFRP CFRP quadrupodquadrupod•• Phase Phase -- drive motorsdrive motors

ALMA Antenna PrototypeALMA Antenna PrototypeInnovative design with technologies used by Italian industry in Optical Telescopes projects

Antenna structure during preAntenna structure during pre--assembly at assembly at GalbiatiGalbiati factory (factory (LeccoLecco))

ALMA Antenna Prototype ALMA Antenna Prototype Receiver CabinReceiver Cabin

New design of the receiver cabin based on Carbon New design of the receiver cabin based on Carbon FiberFibertechnology. Mass and inertia very low and expected to enhance technology. Mass and inertia very low and expected to enhance the antenna performance. the antenna performance. Cabin manufactured by Cabin manufactured by PlyformPlyform ((NovaraNovara), assembled and ), assembled and machined at the machined at the GalbiatiGalbiati factory (factory (OggionoOggiono, LC), now undergoing , LC), now undergoing Aluminium flame spray for Radio Frequency immunity. Aluminium flame spray for Radio Frequency immunity.

ALMA Antenna PrototypeALMA Antenna PrototypeBackup StructureBackup Structure

Backup structure manufactured by ATR (San Backup structure manufactured by ATR (San BenedettoBenedetto del del TrontoTronto) in ) in 16 slices, with very tight dimensioning tolerances. 16 slices, with very tight dimensioning tolerances. Finally assembled into two separate BUS halves for reasons of Finally assembled into two separate BUS halves for reasons of transport. transport. BUS supporting the panels with stability of the order of 15 micrBUS supporting the panels with stability of the order of 15 microns. ons.

ALMA Antenna PrototypeALMA Antenna PrototypeReflector PanelsReflector Panels

• Panels manufactured By Media Lario (Lecco) based on their proprietary Nickel replication technology

• Panels are afterwards coated with Rhodium to guarantee thermo-optical properties. Able to sustain extreme temperatures variation, hailstones and snow.

• Extremely high precision (6 to 8 microns) coupled with rapid serial production.

APEX APEX -- THE ATACAMA THE ATACAMA PATHFINDER EXPERIMENTPATHFINDER EXPERIMENT

APEX is a collaboration between Germany APEX is a collaboration between Germany MPG/MPG/MPIfRMPIfR/AIRUB (50%), ESO (27%) and /AIRUB (50%), ESO (27%) and Sweden/OSO (23%).Sweden/OSO (23%).The project consists of the installation of a 12The project consists of the installation of a 12--m ALMA VERTEX prototype antenna at the m ALMA VERTEX prototype antenna at the ALMA site at ALMA site at ChajnantorChajnantor, in order to use the , in order to use the excellent atmospheric conditions for subexcellent atmospheric conditions for sub--mm mm and THz observations.and THz observations.Agreement signed in January 2003.Agreement signed in January 2003.

View from San Pedro towards View from San Pedro towards ChajnantorChajnantor

APEX

Italian science with the VLTItalian science with the VLTOut of the 20 top cited papers with data from the VLT in 2000 anOut of the 20 top cited papers with data from the VLT in 2000 and 2001 d 2001

the following 11 papers have astronomers based in Italy as firstthe following 11 papers have astronomers based in Italy as firstauthors or coauthors or co--authors.authors.

MolaroMolaro ApJApJ 541 : 54 541 : 54 Andersen A&A 364 : L54 Andersen A&A 364 : L54 KudritzkiKudritzki ApJApJ 536 : 19 536 : 19 MoorwoodMoorwood A&A 362 : 9A&A 362 : 9GiacconiGiacconi ApJApJ 551 : 624 551 : 624 TurattoTuratto ApJApJ 534 : L57 534 : L57 GrattonGratton A&A 369 :87 A&A 369 :87 MaoliMaoli A&A 368 766A&A 368 766IsraelianIsraelian ApJApJ 551 : 833 551 : 833 VreeswijkVreeswijk ApJApJ 546 : 672 546 : 672 TozziTozzi ApJApJ 562 : 42 29562 : 42 29