München, January 31, 2018 GW meeting

SON OF X-SHOOTER

SOXS

SERGIO CAMPANA OSSERVATORIO ASTRONOMICO DI BRERA

ON BEHALF OF THE SOXS CONSORTIUM HISTORY

ESO call for new instruments at NTT (06/2014)

Proposal submission (02/2015)

SOXS selected by ESO (05/2015) out of 19

J. Vernet et al.: X-shooter, the new wide band intermediate resolution spectrograph at the ESO Very Large Telescope 3

instrument shutter Th-Ar, D2 lamps

Calibration unit calibration mirrors Ar Hg Ne Xe lamps FF lamps

A&G Similar to X-shooter camera acq. pin. mon. 50/50 A&G 3 positions mirror pellicle IFU CCD FF .. but also different, only two arms filter wheel lamp piezo. 1 CCD FF lamp exposure VIS slit dichro. 1 ADC focus shutter carriage ADC UV with overlap around 850 nm spectro piezo. 2 UV slit exposure focus carriage shutter VIS dichro. 2 piezo. 3 to cross-calibrate spectra spectro. COLD NIR slit wheel NIR spectro. X-shooter

Fig. 2. Functional diagram of X-shooter. The light path runs from the top to the bottom of the figure. Each element is described in Sect. 2.

In this section, we give an overview of the design of X- The optical design allows the introduction of two short- shooter following photons coming from the telescope. For more wavelength atmospheric dispersion correctors (ADC) and the fo- detailed discussions of specific aspects and the manufacturing cusing of the target on the slit units at the entrance of the respec- process please refer to the following publications: Spano` et al. tive arms. (2006) for the optical design; Rasmussen et al. (2008) for the backbone and the UVB and VIS spectrographs; Navarro et al. (2006, 2008) for the NIR spectrograph; Roelfsema et al. (2008) The size, weight and flexure restrictions implied a very com- for the cryogenic design; Guinouard et al. (2006) for the Integral pact optical design of the spectrographs, requiring an ecient Field Unit; Vidali et al. (2006) for the control software; Goldoni folding of the light path, especially for the NIR-arm. The solu- et al. (2006) and Modigliani et al. (2010) for the data reduction tion was found in selecting the “4C” design described in Delabre software. et al. (1989).

2.1. Key design choices The inclusion of the K band was the subject of a complex A number of key design choices were made in the phases of trade-o↵. With its uncooled optics in the pre-slit area the instru- the project definition. Possibly the most crucial design choice ment could not be optimized for a low thermal background. On was on the method used to split the incoming beam from the the other hand the K band did fit well in the spectral format on telescope between the three spectral arms. The option to use a the detector and had a potentially high eciency. It was finally single slit in the telescope focal plane was rejected because of decided to include the band, but its inclusion should not reduce the diculty of designing a highly ecient relay system and at- the performance in the J- and H-bands. It was also decided not mospheric dispersion correction for the full spectral range, and to cool the instrument pre-slit optics. the need for work-packages with clean interfaces to be handled by the di↵erent consortium partners, which is not possible when spectrographs are sharing a single slit. The solution that was fi- Another key design choice was the spectral resolution in the nally adopted is based on the sequential use of two dichroics three arms. The goal was to build an instrument which reaches after the focal plane, used at 15 rather than 45 to minimize the dark sky noise limit in about 30 minutes, while still provid- polarization e↵ects. The beams toward the UVB and VIS spec- ing medium resolution to do quantitative work on emission and trographs are then deviated to 90 with folding mirrors. These absorption lines. In the NIR the resolution of 5600 for 0.900 slit two folding mirrors together with one in the NIR path are ac- permits the full separation (and subtraction) of the sky emission tively controlled to compensate for small motions due to flex- lines. At UVB and VIS wavelengths, specific scientific programs ures in the backbone of the instrument and guarantee that the did call for higher resolving power, e.g. to optimally measure three target images all remain centered on the three slit units as abundances. The final choices (see Table 4) are obviously a com- the telescope is tracking (see Sect. 3.5.2). promise to cover a broad range of astrophysical programs. SOXS@NTT IN A NUTSHELL

- Broad band spectrograph 350-2000 nm

- R~4,500 (3,500-6,000)

- Two arms (UV-VIS + NIR)

- S/N~10 spectrum - 1 hr exposure for R~20

- Acquisition camera to perform photometry ugrizY (3’x3’) WHY SOXS?

New deeper survey: PanSTARSS, DES, ZTF, LSST, … Space optical missions: Gaia, EUCLID, … Space high-energy missions: Swift, Fermi, SVOM, … Radio new facilities: MeerKAT, SKA, … VHE: CTA Messengers: aLIGO-Virgo, KM3Net, ANTARES, …

SOXS@NTT will have ~170-180 n/yr (for 5 yr) ~3,000 - 4,000 spectra/yr SPECTROSCOPIC BOTTLENECK

• New transients need to be classified (& redshift) and studied over time in details

• PESSTO/ePESSTO (Large ESO program 90n/yr): - initially focussed on SN, now open to more science cases - service classification activity - 64 papers in 5 years and ~600 ATel SOXS SCIENCE CASES

• Classification (service) • SN (all flavours) • GW & � • TDE & Nuclear transients • GRB & FRB • X-ray binaries & novae, magnetars • Asteroids & Comets • Young Stellar Objects & stars • Blazars & AGN • Unknown SOXS (ON PAPER) UV-VIS ARM

A Pickup mirror from slit

B OAP

C Dichroic

D Mirror

E Grang

F Aspheric corrector

G Field flaener

H Mangin Mirror UV-VIS ARM

u g r i

Camera 0.920 0.920 0.920 0.920

UV-VIS Spectrograph 0.656 0.668 0.655 0.652

No Conngency 0.756 0.770 0.755 0.751

Common Path 0.820 0.820 0.820 0.820

Telescope 0.510 0.510 0.510 0.510 Overall 0.274 0.279 0.274 0.272 No Conngency 0.316 0.322 0.316 0.314 NIR ARM

ORDER FSR MIN WL BLAZE WL MAX WL 10 (0.193) (1833) 1.930 (2.016) 11 0.159 1.674 1.754 1.834 12 0.134 1.541 1.608 1.675 13 0.114 1.427 1.484 1.541 14 0.098 1.329 1.378 1.428 15 0.086 1.244 1.286 1.329 16 0.075 1.168 1.206 1.244 17 0.067 1.102 1.135 1.168 18 0.06 1.042 1.072 1.102 19 0.053 0.989 1.016 1.042 20 0.048 0.941 0.965 0.989 21 0.044 0.897 0.919 0.941 22 0.04 0.857 0.877 0.897 23 0.036 0.821 0.839 0.857 24 0.034 0.787 0.804 0.821 NIR ARM TIMELINE (TIGHT!)

Date to be operational on sky: end 2020

PDR July 2017, 21-22 ✓ FDR July 2018 End of Procurement April 2019 AIT & Test in Europe June 2020 Instrument in Chile August 2020 End of Commissioning December 2020

LSST - CTA - SKA good timing with GW experiments (4 detectors) - Consortium structure CONSORTIUM STRUCTURE

P. Schipani R. Claudi

S. Campana

E. Cappellaro (INAF-OAPadova) - Italy M. Della Valle (INAF-OANapoli) - Italy A. Gal-Yam (Weizmann) – Israel S. Smartt (Univ. Belfast) – UK I. Arcavi (Tel Aviv University) – Israel S. Mattila (FINCA) – Finland J. Fynbo (NBI) - Denmark S. Campana (INAF-OABrera) - Italy RESPONSIBILITIES

Italy ~ 50% (CP, NIR-arm, integration, management, etc.)

Israel ~25% (UV-VIS arm optics and mechanics)

Chile ~10% (Acquisition camera)

UK ~10% (VIS-CCD, reduction pipeline)

Finland ~5% (Calibration Unit) OPERATIONS ESO will reward the SOXS consortium with NTT observing time: now ePESSTO 90n/yr — future SOXS ~180n/yr.

SOXS consortium responsible for the operations. Flexible schedule of a day-by-day basis (one day in advance) SOXS+ESO targets). SOXS team (3 people) on weekly rounds to cope with observations (schedule, classification, etc.) and on call for reaction to GW (GRBs, etc.) with fast (<1hr) ToO and problems. ESO-TNO to carry out observations.

<5% of the consortium time open to the community as ToO (Swift-like) observations (public data).

Relevant information (classification, peculiar sources, etc.) announced in real time through GCN, ATel, IAUC, etc.

Consortium data public after a short (6-12 months TBD) proprietary period. SOXS FOR GW Pian et al. 2017

High priority targets

Spectroscopic study of GW candidates

Deep follow-up of GW counterparts Figure 4: Spectroscopic data and model fits a: Spectroscopic data from +1.4 to +4.4 daysSmartt after et al. 2017 | discovery, showing the fast evolution of the SED. The points are coeval UgrizJHK photometry. b: Com- parison of the +1.4 day spectrum with a TARDIS spectral model that includes Cs I and Te I [see text].

Thin vetical lines indicate the positions of spectral lines blueshifted by 0.2 c, corresponding to the photo- spheric velocity of the model (the adopted black-body continuum model is also shown for reference). c: The

Xshooter spectrum at +2.4 days, also shows Cs I and Te I lines that are consistent with the broad features observed in the optical and near infra-red (here, the lines are indicated at velocities of 0.13 c and we include additional, longer wavelength transitions to supplement those in B.).

23 SUMMARY

SOXS @ NTT from 2021 Medium resolution (~4,500) Broad-band (350-2000 nm) ugrizY imaging (3’x3’) Dedicated to transient astrophysics

Possibility to trigger every night Fast reaction (probably the only instrument mounted at NTT)

GW is one of the main SOXS science cases Thanks The Organisation de Zeeuw T., Reaching New Heights in Astronomy

measurements and continues to be main- tained and upgraded in collaboration with external institutes. The NTT operates EGP/ESO with the ESO Faint Object Spectrograph and Camera 2 (EFOSC2) and the Son of ISAAC infrared camera (SOFI), and the telescope is still much in demand by the community. It is currently used for the PESSTO survey (Smartt et al., 2013) and also provides opportunities for novel instrumentation by offering a visitor focus.

A call for new instruments was made in 2014, aimed primarily at replacing the ageing instrumentation at the NTT. The medium-resolution (R = 5000) optical and near-infrared (0.4–1.8 μm) spectrograph SOXS (Son of X-shooter) was selected as the future workhorse instrument at the NTT. SOXS addresses in particular — but eight years and operation was discontin- Figure 9. The new solar photovoltaic plant at not exclusively — the needs of the time- ued as planned at the end of March La Silla. The Organisation domainde Zeeuw research T., Reaching community. New Heights Further in- Astronomy2016. Recently, the Universidad Católica more, the high-speed, triple-beam imager Norte in collaboration with the Pontifcia ULTRACAM, a visitor instrument,The Organisation was Universidad Católicade deZeeuw Chile T., hasReaching New HeightsThe science in Astronomy operations model for La Silla offered for up to 25 % of NTT time in upgraded the ESO 1-metre telescope — and the corresponding infrastructure exchange for cash contributions to NTT and installed the FIber Dual Echelle support — are being evolved to maintain operations. In addition, the Near Infra-Red Optical Spectrograph (FIDEOS). basic compatibility with its Paranal coun- Planet Searcher (NIRPS) was selected as terpart, so that the overall ESO end-to- the near-infrared extension of HARPS on Two new projects, ExTrA (Exoplanets end operations also encompass the the 3.6-metre telescope, creating the most in Transit and their Atmospheres) and ESO-operated facilities at La Silla. This powerful optical to near-infrared precision MASCARA (Multi-site All-Sky CAmeRA), support includes the tools and methods radial velocity machine for exoplanet are currently being added to the suite used by the community to prepare and measurements and continues to be main-research in the southern hemisphere. of hosted telescopes. All these projects execute observations at La Silla, or to tained and upgraded in collaboration with external institutes. The NTT operates measurements and continuescan be to kept be main cost-neutral- to ESO throughEGP/ESO exploit the data in the SAF. with the ESO Faint Object Spectrograph An increasing number of tainedsmall-telescope and upgraded infnancial collaboration contributions by the project and Camera 2 (EFOSC2) and the Son projects are hosted at La Silla.with external These institutes. teamsThe NTT to operates the site operations costs, as The availability of SOXS on the NTT (and EGP/ESO of ISAAC infrared camera (SOFI), and the scientifc projects are developedwith the ESO by Faint Objectlong Spectrograph as the NTT and the 3.6-metre tele- X-shooter on the VLT) will put the ESO telescope is still much in demand by the teams in the community;and they Camera are funded 2 (EFOSC2) scope and the are Son operated by ESO. An increas- community in an excellent position to fol- community. It is currently used for the by national institutes or byof theISAAC European infrared cameraing (SOFI), fraction and of the the projects offer access low up the most interesting transients to PESSTO survey (Smartt et al., 2013) and Research Council or via privatetelescope dona is still- much into demand their high-level by the data products via the be discovered by the LSST from 2023 community. It is currently used for the also provides opportunities for novel tions, and take advantage of the excellent SAF in return for lowered hosting fees. onwards. The combination of HARPS and instrumentation by offering a visitor focus. PESSTO survey (Smartt et al., 2013) and atmospheric conditions, alsothe availableMESSENGERprovides opportunities for novel N.166NIRPS on the 3.6-metre telescope is cru- A call for new instruments was made in infrastructure and the leaninstrumentation operation- by offeringThe aLa Silla visitor focus. 2010+ plan was envisaged cial for providing critical ground-based 2014, aimed primarily at replacing the support model. for an initial period of fve years without complementary data for the ESA/Swiss ageing instrumentation at the NTT. The A call for new instrumentsmajor was re-investment made in into the site infra- mission CHaracterising ExOPlanet Satel- medium-resolution (R = 5000) optical andLa Silla hosts the the Max2014, Planck aimed primarily atstructure. replacing theModest re-investment is now lite (CHEOPS) and for PLATO. near-infrared (0.4–1.8 μm) spectrograph Gesellschaft MPG/ESO 2.2-metreageing instrumentation tele- neededat the NTT. to Themaintain the site infrastructure SOXS (Son of X-shooter) was selected as medium-resolution (R = 5000) optical and scope, the Danish 1.54-metre,near-infrared the Swiss (0.4–1.8 μm) at thespectrograph level required by the continued The extension of La Silla operations the future workhorse instrument at the 1.2-metre Leonard Euler, the ESO operation of the 3.6-metre, the NTT and beyond 2020 as described above NTT. SOXS addresses in particular — but eight years and operationSOXS was (Sondiscontin of X-shooter)- Figure 9. was Theselected new solar as photovoltaic plant at 1-metre, the Rapid Eye Mountthe future (REM), workhorse the instrumentthe hosted at the telescopes. Operation-critical requires both NIRPS and SOXS to be not exclusively — the needs of the time- ued as planned at the end of March La Silla. Télescope à Action RapideNTT. pour SOXS les addresses ininformation particular — technology but eight (IT)years infrastructure and operation wassuccessful. discontin- IfFigure 9. NIRPS The were new solarto fail photovoltaic for some plant at domain research community. Further- 2016. Recently, the Universidad Católica not exclusively — the needs of the time- ued as planned at the end of March La Silla. more, the high-speed, triple-beam imagerObjets Norte Transitoires in collaboration (TAROT-S) with the andPontifcia the has been renewed during 2016. Savings unforeseen reason, then the 3.6-metre domain research community. Further- 2016. Recently, the Universidad Católica ULTRACAM, a visitor instrument, was TRAnsitingUniversidad Planets Católica and de Plane Chile thas esImals Thehave science been operations made on modelelectrical for La Silla power telescope with HARPS would still be more, the high-speed, triple-beam imager Norte in collaboration with the Pontifcia offered for up to 25 % of NTT time in Smallupgraded Telescope the ESO (TRAPPIST), 1-metre telescope all with —costs, and the as corresponding La Silla became infrastructure a regulated valuable for exoplanet research, but it ULTRACAM, a visitor instrument, was Universidad Católica de Chile has The science operations model for La Silla dedicated instruments. An increasing client in June 2015 in return for support- would be reasonable for ESO to require exchange for cash contributions to NTT and installed the FIber Dualoffered Echelle for up to 25 %support of NTT time— are in being evolvedupgraded to maintainthe ESO 1-metre telescope — and the corresponding infrastructure operations. In addition, the Near Infra-Rednumber Optical of Spectrograph these telescopes (FIDEOS).exchange are operated for cash contributions basicing thecompatibility installation to NTT with ofand its a Paranalinstalledphotovoltaic counthe FIber- solar Dual Echelleexternal contributionssupport — to are the being operation evolved to maintain Planet Searcher (NIRPS) was selected asremotely. The QUEST surveyoperations. project In addition,terpart, powerthe Near so plant Infra-Redthat theon theoverall Opticalpremises. ESO Spectrograph end-to- The plant (FIDEOS). costs. If SOXSbasic were compatibility to fail, then with the its future Paranal coun- the near-infrared extension of HARPS on on theTwo 1-metrenew projects, ESO ExTrASchmidtPlanet (Exoplanets telescope Searcher (NIRPS) endstarted was operations selected producing also as encompass power in mid-2016the of the NTT wouldterpart, be so in that serious the overall doubt. ESO end-to- the 3.6-metre telescope, creating the most (Baltay in Transit et al., and 2012) their was Atmospheres) completedthe near-infrared and after extension ESO-operated(Figure 9). of HARPS facilities on Two at La Silla. new projects, This ExTrA (ExoplanetsThis would threatenend operations the viability also encompass of the the powerful optical to near-infrared precision MASCARA (Multi-site All-Sky CAmeRA), support includes the tools and methods the 3.6-metre telescope, creating the most in Transit and their Atmospheres)entire and La Silla ESO-operatedoperations model, facilities as atit isLa Silla. The This availability of state-of-the-art detec- and the Operations Support Facility (OSF) radial velocity machine for exoplanet are currently being addedpowerful to the suiteoptical to near-infraredused by the precision community MASCARA to prepare (Multi-site and All-Sky CAmeRA), support includes the tools and methods research in the southern hemisphere. of hosted telescopes. All these projects execute observations at La Silla, or to not cost-effective for ESO to run the tors is critical for ESO. Infrared devices at 2950 metres formally ended in Decem- radial velocity machine for exoplanet are currently being added to thecomplete suite site usedfor a bysingle the communitymedium-sized to prepare have and traditionally been single-source pro- ber 2013, except for, as regards ESO, can be kept cost-neutralresearch to ESO throughin the southern exploit hemisphere. the data in the SAF.of hosted telescopes. All these projects execute observations at La Silla, or to The Messenger 166 – December 2016 telescope. External funding or support curements from US companies who the ALMA Residence and a site-security An increasing number of small-telescope 12 fnancial contributions by the project can be kept cost-neutral to ESO through exploit the data in the SAF. projects are hosted at La Silla. These teams to the site operationsAn increasing costs, as numberThe of small-telescope availability of SOXS fnancial on the NTTcontributions (and by the projectcould come from (consortia of) institutes serve the defence market and are under surveillance system. NAOJ completed scientifc projects are developed by long as the NTT and theprojects 3.6-metre are tele hosted- atX-shooter La Silla. These on the VLT) willteams put to the the ESO site operations costs,in the as Member The States, availability or from of SOXSpartners on the NTTsignifcant (and ITAR (International Traffc in delivery of the Band 4, 8 and 10 receivers teams in the community; they are funded scope are operated by ESO. scientifc An increas projects- are communitydeveloped byin an excellentlong position as the NTT to fol and- the 3.6-metreelsewhere tele- includingX-shooter the on Host the StateVLT) will Chile. put the ArmsESO Regulations) restrictions. The next- soon after this date. NRAO continued by national institutes or by the European ing fraction of the projectsteams offer in access the community; low theyup the are most funded interesting scope transients are operated to by ESO. An increas- community in an excellent positiongeneration to fol- devices are extremely expen- after 2013 with the investigation of the Research Council or via private dona- to their high-level data productsby national via institutes the orbe by discovered the European by the LSSTing fraction from 2023 of the projects offer access low up the most interesting transientssive toand start to dominate the budgets astigmatism affecting the North American tions, and take advantage of the excellent SAF in return for loweredResearch hosting fees.Council or viaonwards. private Thedona combination- to their of HARPShigh-level and data products2.4 via Technology the be developmentdiscovered by programmethe LSST from 2023and limit the scope of new instruments. In antenna performance and a number of atmospheric conditions, the available tions, and take advantageNIRPS of onthe the excellent 3.6-metre SAF telescope in return is for cru lowered- hosting fees. onwards. The combination of HARPSthe optical,and the situation is less urgent, other activities. Commissioning activities infrastructure and the lean operation- The La Silla 2010+ plan atmosphericwas envisaged conditions, cial thefor availableproviding critical ground-based It is critical to NIRPSdevelop on and the 3.6-metresecure key telescope but is cruthe- traditional charge-coupled device of the array are continuing and extend support model. for an initial period of fveinfrastructure years without and thecomplementary lean operation- data forThe the La Silla ESA/Swiss 2010+ plan was envisagedtechnologies whichcial for willproviding maintain critical the ground-based(CCD) technology is now being replaced into the operations phase for more major re-investment intosupport the site model.infra- mission CHaracterisingfor ExOPlanet an initial periodSatel- of fve yearsObservatories without complementary at the cutting edgedata for of the ESA/Swisswith Complementary Metal Oxide Semi- advanced observing modes, including La Silla hosts the the Max Planck structure. Modest re-investment is now lite (CHEOPS) and for PLATO.major re-investment into the siteastronomy infra- andmission so contribute CHaracterising to achieving ExOPlanet conductor Satel- (CMOS) technology. This repre- solar observations and participation in La Silla hosts the the Max Planck structure. Modest re-investment is now lite (CHEOPS) and for PLATO. Gesellschaft MPG/ESO 2.2-metre tele- needed to maintain the site infrastructure ESO’s mission. In practice, this means sents a viable alternative for commercial global very long baseline interferometry Gesellschaft MPG/ESO 2.2-metre tele- needed to maintain the site infrastructure scope, the Danish 1.54-metre, the Swiss at the level required by the continued The extension of La Silla operations taking those that are at low levels of tech- applications and in principle also for (VLBI) experiments. 1.2-metre Leonard Euler, the ESO operation of the 3.6-metre,scope, the theNTT Danish and 1.54-metre,beyond 2020 the Swiss as described at the above level required by the continued The extension of La Silla operations nology readiness and developing them to astronomy, but currently no such devices 1-metre, the Rapid Eye Mount (REM), the the hosted telescopes. Operation-critical1.2-metre Leonard Euler,requires the ESO both NIRPS andoperation SOXS toof bethe 3.6-metre, the NTT and beyond 2020 as described above a level suffcient to be incorporated within meet ESO’s needs. A frst step in mitigat- The ALMA Residence will be completed Télescope à Action Rapide pour les information technology (IT)1-metre, infrastructure the Rapid Eyesuccessful. Mount (REM), If NIRPS the werethe hostedto fail for telescopes. some Operation-critical requires both NIRPS and SOXS to be Objets Transitoires (TAROT-S) and the has been renewed duringTélescope 2016. Savings à Action Rapideunforeseen pour les reason, theninformation the 3.6-metre technology (IT) infrastructurenew projects withsuccessful. manageable If NIRPS risk. were The to fail foring some these risks is participation in the and handed over to ALMA in early 2017, TRAnsiting Planets and Plane t esImals have been made on electricalObjets power Transitoires (TAROT-S)telescope and with the HARPS haswould been still renewed be during 2016.requirement Savings tounforeseen not only develop reason, thenbut alsothe 3.6-metre ATTRACT initiative, which aims to obtain and procurement of the site-security Small Telescope (TRAPPIST), all with costs, as La Silla becameTRAnsiting a regulated Planets and valuable Plane t esImalsfor exoplanet research,have been but made it on electrical securepower technologytelescope for the with future HARPS means would still fundingbe from the European Commission surveillance system will follow. The per- dedicated instruments. An increasing client in June 2015 in returnSmall for Telescope support- (TRAPPIST),would be all reasonable with forcosts, ESO as to La Sillarequire became a regulatedthat only rarely valuable will a technology for exoplanet develop research,- butfor itdeveloping imaging and detection manent power system started operations number of these telescopes are operated ing the installation of a photovoltaicdedicated instruments. solar external An increasing contributions to client the inoperation June 2015 in return forment support project- takewould the be form reasonable of a conven for ESO- to requiretechnologies in Europe. in November 2012 and is now in reliable remotely. The QUEST survey project power plant on the premises.number The of plantthese telescopescosts. Ifare SOXS operated were to ingfail, the then installation the future of a photovoltaictional solarprocurement external from contributions industry or to instithe -operation 24/7 operation, after some initial techni- on the 1-metre ESO Schmidt telescope started producing powerremotely. in mid-2016 The QUESTof survey the NTT project would be inpower serious plant doubt. on the premises. tutes.The plant Usually costs.a collaborative If SOXS were approach to fail, then the future cal and operational diffculties in 2013. (Baltay et al., 2012) was completed after (Figure 9). on the 1-metre ESO SchmidtThis would telescope threaten thestarted viability producing of the power in mid-2016is required to ofensure the NTT that would the intellectual be in serious doubt.3. Submillimetre Programmes Previous ESO infrastructure deliveries (Baltay et al., 2012) was completed after (Figure 9). This would threaten the viability of the property developed in the project is either include the Technical Building for the transferred to ESO, or another scheme ESO’s activities in the submillimetre OSF, the Santiago Central Offce (SCO) at is used to ensure that the technology will wavelength regime, traditionally associ- the ESO Vitacura premises, 192 antenna 12 The Messenger 166 – December 2016 12 The Messenger 166 – December 2016 be available and further developed over ated with radio-astronomy, started with foundations, and the access road to the the period of time that it is needed. This the Swedish-ESO Submillimetre Tele- OSF and AOS. approach requires long-term planning to scope (SEST) on La Silla (1987–2003). address risks such as obsolescence, loss This led to participation in ALMA and Front End and Back End deliveries were of external manufacturers, and uncertain APEX (Figure 10). complete by the end of 2013. These requirements for future development. included 73 receiver cartridges each for Band 7 and Band 9, 58 water vapour In addition to enabling ESO’s mission, 3.1 Chajnantor — ALMA radiometers, 83 Front End power supplies, technology development also has a role 26 fully integrated and tested Front End in enhancing the skills, and increasing the ALMA evolved from separate regional assemblies, 70 cryostats, more than 500 motivation, of staff within ESO. Although plans to a global partnership between cartridge bodies, more than 600 photo this aspect will not drive the selection of ESO (37.5 %), the US National Science mixers, the complete fbre management specifc projects, it will be considered Foundation (NSF, representing USA, system, 550 tuneable flter boards, and when deciding where and how the devel- Canada and Taiwan; 37.5 %) and the 58 sets of cryogenic helium lines. Two opment will be carried out. National Institutes of Natural Sciences in custom-made antenna transporters have Japan (NINS, representing Japan, South been in routine operation since 2008. The The funding for technology development Korea and Taiwan; 25 %). The host state contract with the AEM Consortium for the has been consolidated from a variety Chile receives 10 % of the observing antennas provided by ESO was formally of small R&D budgets across the Directo- time. ESO’s counterparts at the executive closed in early 2016, when the warranty rates of Programmes and Engineering, level are the US National Radio Astronomy period of the twenty-ffth antenna expired. from the enabling technology budget for Observatory (NRAO), managed by the All AEM antennas are within specifcation the VLT and from the enabling technology Association of Universities Inc. (AUI), and and operating reliably. programme formerly planned for the ELT. the National Astronomical Observatory of Current projects include the development Japan (NAOJ). Council set the cost-to-completion for of deformable mirrors for future ESO ESO’s ALMA construction in 2005, at an projects, detector development, laser amount equal to 489.5 MEUR in 2014 R&D, ELT real-time computing and wave- 3.1.1 Construction prices. The entire programme was deliv- front-sensor camera development, and ALMA construction on the Array Opera- ered over the next nine years with only R&D for the ELT EPICS instrument. tions Site (AOS) at 5050 metres altitude a 1.5 % cost increase. A workshop on

The Messenger 166 – December 2016 13 PRELIMINARY

Unknown 300 hr