The role of 4m class telescopes at ESO

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2 The role of 4m class telescopes at ESO The three ESO 4m class telescopes & instruments Their research programs Their future

3 The 4m class telescopes at ESO

4 VISTA + VIRCAM

5 3.6m+HARPS +visitor instruments

6 NTT+EFOSC2,SOFI (SUSI2) + visitor instruments

7 LS as platform for experiments

8 Visiting Instruments 3.6m PolCor ( Coronagraph with a polarizing mode) NTT ULTRACAM ASTRALUX IQEYE ExAO (WineRed)

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10 Back to ESO instruments And their science LS instruments VISTA

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13 In order of importance: HARPS (and FEROS in the past) C (ISM, star formation and planetary systems) D (Stellar evolution)

14 HARPS (2003)

15 HARPS - basic performances HARPS is an exceptionally STABLE spectrograph: - the spectrograph bench is under vacuum (10 3 mbar); - three layers of temperature controlled environments; - temperature RMS at the grating < 7mK in one month, typical ~1mK in one night. For reference, 7mK temperature change introduces a drift of ~ 1m/s. RV accuracy: ~ 0.2m/s on the short term (instrument, guiding, ThAr, atmosphere); m/s on the medium term (2 years, Lovis 2006, Nature); System efficiency: 7% at peak (after M2 upgrade). Limiting magnitude: 17 (S/N ~ 1, Texp~ 1h, RV ~ 100m/s). online pipeline to obtain precise RVs within one minute to spectrum acquisition raw and reduced data published in the ESO archive within few hours (proprietary rights!) Recent upgrades: new fiber link for improved scrambling capabilities and increased throughput (by 20% 30%) laser frequency comb installed and still under test before making it finally available to the Community.

16 HARPS C = ISM, star formation and planetary systems spectro-polarimetry exoplanets around stars with jitter Herbig Ae/Be SF via accretion SF via accretion ZAMS Spectro-Thosimult + spectro-obja(b) exoplanets stellar abundances stellar jitter stellar multiplicity sun (reflected on moon) DIB

17 In order of importance: EFOSC2 D (Stellar evolution) A (Cosmology) C (ISM, star formation and planetary systems) B (Galaxies and galactic nuclei)

18 EFOSC2 (1989)

19 EFOSC2: Instrument Overview EFOSC2 consists of the following elements : - slit wheel Quarter+ - filter wheel - grism wheel - collimator - half & quarter wave plate for polarimetry - He and Ar arc lamps - quartz lamp for internal flat fields - camera unit The camera is opened to F/4.9 with a focal length of 200mm.

20 EFOSC2 CCD #40 Loral/Lesser, Thinned, AR coated, UV flooded, MPP chip E2V Multi-AR CCD231-84

21 EFOSC2 Category D: Stellar Evolution Long slit: source identification/classification X ray variable sources from Swift & Chandra Gaia transients (e.g., accreting binaries) Wolf Rayet and early O supergiant candidates cluster candidates found in the 2MASS all sky survey OB Runaway Stars Inside SNRs UV excess objects detected with the GALEX (compact pulsators and binary targets ) confirmation of wide binaries via RV to complement p.m. white dwarf candidates, identified in the ATLAS magnitudes system massive stars, accreting binaries and hot white/sub dwarfs from VPHAS+ candidate White Dwarfs from GALEX and APASS

22 In order of importance: SOFI C (ISM, star formation and planetary systems) D (Stellar evolution) A (Cosmology) B (Galaxies and galactic nuclei)

23 SOFI (1997)

24 SofI Instrument Overview - imaging: with plate scales of 0.144, and arcsec/pixel, using broad and narrow band filters in the microns range, largest FoV 4.92 x 4.92 arcmin - spectroscopy: low (R~900) & medium resolution (R~ ), micron range, fixed width 0.6, 1, and 2 slits; slit length 4.92 arcmin - imaging polarimetry: micron

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26 SOFI C: C ISM, star formation and planetary systems Spectroscopy long slit source identification/classification ages of Myr old M dwarfs; candidates via GALEX and WISE satellites;spectral features such as Hydrogen line emission, K and Na absorption strength, and the shape of the H band spectral types, effective temperatures, masses and ages of newly discovered YSOs; identified from 2MASS and AllWISE infrared photometry confirmation of planetary mass objects in Chamaeleon I confirmation of wide very low mass binaries and multiple systems in the VISTA Hemisphere Survey and 2MASS confirmation of M dwarf candidates in moving groups via metallicity of ultracool dwarfs (UCDs) and brown dwarfs (BDs) confirmation of ultra cool dwarfs (UCDs) in multi epoch, high spatial resolution VVV Survey and WISE mission (low surface gravity)

27 More science with LS instruments: Public spectroscopic surveys

28 ESO Public Survey: Status Report Prepared by Magda Arnaboldi, Head - Archive Science Group ESO Survey Team leader marnabol@eso.org EST (M. Arnaboldi, M. Hilker, G. Hussain, M. Petr-Gotzens, M. Rejkuba) ASG (M. Arnaboldi, N. Delmotte. L. Mascetti, A. Micol, J. Retzlaff)

29 2012 PESSTO

30 ESO Public Spectroscopic Surveys PESSTO The PESSTO survey started operation on April 1st 2012, on EFOSC and SOFI at NTT on La Silla yrs The time allocation of the survey include 90 nights each year, with allocation 60/30 nights in odd and even periods Thus far 350 nights were allocated to this survey

31 VIRCAM (2009)

32 VIRCAM (VISTA InfraRed CAMera) 1.65 degree diameter field of view 67 million pixels of mean size arcsec broad band filters Z,Y,J,H,Ks narrow band filters at 0.98, 0.99, and 1.18 micron. wide-field corrector lens system (3 infrasil lenses), mounts to the rotator on the back of the primary mirror cell The telescope has an altitude-azimuth mount, and quasi-ritcheychretien optics fast f/1 primary mirror f/3.25 focus to the instrument at Cassegrain. autoguider and active optics sensors

33 Current VISTA

34 VISTA Public Surveys Surveys Area (deg2) Filters Magnitude limit 5σ (AB), 10σ (AB) x VMC Observation hours taken (Apr 16) 1.7 deep Y J H Ks 25.7, 25.5, 25.1, ultra-deep Y J H Ks 26.7, 26.6, 26.1, VHS Y J H Ks 21.2, 21.1, 20.6, VIDEO 12.0 Z Y J H Ks VVV 560 Z Y J H Ks Comp. VIKING 1500 Z Y J H Ks VMC 180 Y J Ks 21.9, 21.4, Deep high z Whole Sky UltraVISTA 1801 NB118 Galactic Extragalactic Resolved SFH

35 ESO/VISTA Public Survey status Estimated completion year

36 Phase 3 releases from ESO Public Surveys For imaging surveys, we are at: VISTA DR3 VST DR2 For spectroscopic surveys, we are at DR2 GaiaESO, PESSTO Sky coverage >11500 sq.deg Opt./NIR: 4336 / 9445 sq.deg Tot. data volume: >35 TB; 270k+ files; >29k spectra High-level science catalogs for all surveys Including light curves for variable sources!

37 Phase 3 releases from ESO Public Surveys The VISTA & VST public survey DPs released through the Phase 3 process in 2014/2015 cover almost square degrees of the Southern Hemisphere. VPHAS+ VIDEO VVV VHS KiDS VIKING, VMC - blue UltraVISTA ATLAS STATUS: more than 35 TB of SDPs have been ingested and published through the ESO SAF in 2014/2015

38 Statistics: ESO Science Archive Facility -Access and Download Data volume download from ESO SAF of public survey products: all surveys have been accessed by archive users VHS VVV UltraVISTA VMC VIDEO 8000 VIKING 6000 VPHAS KiDS 2000 V-ATLAS 0 Gaia - ESO PESSTO

39 # of publications (April 2016) Spectroscopic VISTA VST

40 # of publications (April 2016) Archive users query for reduced products more than once (~7 times, on average) The number of archive users using reduced products for their science is more than twice the number of listed PIs/CoIs of ESO public surveys proposals Spectroscopic VISTA VST

41 The future of 4m telescopes High-level: Science Priorities at ESO From 85th Meeting Of SCIENTIFIC TECHNICAL COMMITTEE Garching, April 2015

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48 Second VISTA call for ESO Public Survey 2015 July: call for start in P98 (October 2016) 3y duration (then 4MOST) Oct 15: 13 Letters of Intent received by OPO And PIs of current VISTA surveys submitted extended reports, with requests for compensation/extension of their programs Total time requested hrs (+30); 7470 (available (2490h x 3yrs) => factor 2 oversubscription) Seven teams have be invited to submit proposals for P98 (after review of Public Survey Panel)

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50 4MOST 4m Multi-Object Spectroscopic Telescope P.I. Roelof de Jong(AIP) Fabian+03 VISTA

51 4MOST timeline Fabian+03 June 2016: Preliminary Design Review 2018: Final Design Review 2019: Call for Proposal for Community surveys 2020: Preliminary Acceptance Europe 2021: Start of operations

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53 4MOST GTO Galactic Surveys Fabian+03 Milky Way Halo Low Resolution Survey: characterization of the MW dark matter halo Milky Way Halo High Resolution Survey: chemical composition of the oldest and most metal poor stars Milky Way Bulge and Disk Low Resolution Survey: constrain the formation of the MW bulge and disk complement astrometric information from Gaia with high-precision chemical abundances for 2 million stars

54 4MOST GTO Extra-galactic Surveys Fabian+03 erosita follow-up surveys: Clusters and AGNs: follow-up of >50,000 X-ray selected clusters and 1 million AGNs up to z~6 Galaxy Evolution Survey (WAVES): WAVES-Deep: 100 deg2 to r<22, and SDSS-like out to z~1 WAVES-Wide: 1500 deg2 to r<22 with photo-z preselection (z<0.13) Cosmology Redshift Survey Mapping the 3d matter distribution: 2M LRGs and 13M elgs

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57 By 2016 cost reduced to 1.5 MEUR/year through Increased external contributions to the site operation costs of the NTT and 3.6m telescope. HARPS is expected to retain a key role for another decade, but the instrumentation on the NTT is aging and will not remain competitive much longer. ESO's community of astronomers continues to grow, and the NTT is one of the best 4m class telescopes in the Southern Hemisphere. For this reason it makes good sense to consider new long term goals for the NTT. no resources for in house instrumentation programme new instrumentation for the NTT if funded mostly externally La Silla s future after 2020 will strongly depend on the success to continue to attract competitive science projects that are carried out at the 4m class telescopes.

58 LPRS distribution by Type Nr. of problems Instrumentation comp HW Electronic Software Network DHA Oper. Eng. Mechanic Maintenance Tel. Oper. Electric Type of problem Logistics

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61 2014 March 1: call June 9: 7 letters of intent shortlisted 2015 February 13: closing date for detailed proposals April: STC June: Council

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67 And for more future directions See community poll

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