The role of 4m class telescopes at ESO

– The three ESO 4m class telescopes & instruments

– Their research programs

– Their future

The 4m class telescopes at ESO

VISTA + VIRCAM

3.6m+HARPS+visitor instruments

NTT+EFOSC2,SOFI (SUSI2)+ visitor instruments

LS as platform for experiments

Visiting InstrumentsVisiting Instruments

3.6m3.6m

– – PolCor ( Coronagraph with a polarizing mode)PolCor ( Coronagraph with a polarizing mode)

NTTNTT– – ULTRACAMULTRACAM

– – ASTRALUXASTRALUX

– – IQEYEIQEYE

– – ExAOExAO

– – (WineRed)(WineRed)

Back to ESO instruments

And their science

– LS instruments– VISTA

●In order of importance:

● HARPS (and FEROS in the past)

● C (ISM, star formation and planetary systems)

● D (Stellar evolution)

HARPS (2003)

HARPS - basic performances• HARPS is an exceptionally STABLE spectrograph:

- the spectrograph bench is under vacuum (10­3 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);- 0.8 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 fiber­link 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.

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

●In order of importance:

● EFOSC2

● D (Stellar evolution)

● A (Cosmology)● C (ISM, star formation and planetary systems)● B (Galaxies and galactic nuclei)

EFOSC2 (1989)

EFOSC2: Instrument Overview

EFOSC2 consists of the following elements :

- slit wheel- 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.

Quarter+

E2VMulti-AR CCD231-84

EFOSC2CCD #40

Loral/Lesser, Thinned, AR coated, UV flooded, MPP chip

EFOSC2 Category D: Stellar Evolution

Long slit: 

• source identification/classification• X­ray variable sources from Swift & Chandra • Gaia transients (e.g., accreting binaries) • Wolf­Rayet and early O supergiant candidates • cluster candidates found in the 2MASS all­sky­survey • OB Runaway Stars Inside SNRs • UV­excess 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/sub­dwarfs from VPHAS+ • candidate White Dwarfs from GALEX and APASS 

● In order of importance:

● SOFI

● C (ISM, star formation and planetary systems)

● D (Stellar evolution)● A (Cosmology)● B (Galaxies and galactic nuclei)

SOFI (1997)

SofI – Instrument Overview

- imaging: with plate scales of 0.144, 0.273 and 0.288 arcsec/pixel, using broad and narrow band filters in the 0.9-2.5 microns range, largest FoV 4.92 x 4.92 arcmin

- spectroscopy: low (R~900) & medium resolution

(R~1400-2200), 0.93-2.54 micron range, fixed width 0.6”, 1”, and 2” slits; slit length 4.92 arcmin

- imaging polarimetry: 0.9-2.5 micron

SOFI C: C ISM, star formation and planetary systems

Spectroscopy­long­slit 

• source identification/classification

• ages of 10­100 Myr­old M­dwarfs; candidates via GALEX and WISE satellites;spectral features such as Hydrogen line emission, K and Na absorption strength, and the shape of the H­band

• spectral types, effective temperatures, masses and ages of newly discovered YSOs; identified from 2MASS and AllWISE infrared photometry

• confirmation of planetary­mass objects in Chamaeleon­I • confirmation of wide very low­mass 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 multi­epoch, 

high spatial resolution VVV Survey and WISE mission (low surface gravity) 

More science with LS instruments:

Public spectroscopic surveys

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)

2012 – PESSTO

The PESSTO survey started operation on April 1st 2012, on EFOSC and SOFI at NTT on La Silla – 4 + 1 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

ESO Public Spectroscopic Surveys –

PESSTO

VIRCAM (2009)

VIRCAM (VISTA InfraRed CAMera)

– 1.65 degree diameter field of view

– 67 million pixels of mean size 0.339 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-Ritchey-Chretien optics

– fast f/1 primary mirror

– f/3.25 focus to the instrument at Cassegrain.

– autoguider and active optics sensors

Current science @ VISTA

VISTA Public Surveys

Surveys Area (deg2) Filters Magnitude limit

5σ (AB), 10σ (AB) x VMC

Observation hours

taken (Apr 16)

Ultra-VISTA

1.7 deep 0.73 ultra-deep

Y J H Ks

Y J H Ks

NB118

25.7, 25.5, 25.1, 24.5

26.7, 26.6, 26.1, 25.6 26.0

1801

VHS 17800 Y J H Ks 21.2, 21.1, 20.6, 20.0 4710

VIDEO 12.0 Z Y J H Ks 25.7 24.6 24.5 24.0 23.5 1942

VVV 560 Z Y J H Ks 21.9 21.1 20.2 18.2 18.1 Comp.

VIKING 1500 Z Y J H Ks 23.1 22.3 22.1 21.5 21.2 2200

VMC 180 Y J Ks 21.9, 21.4, 20.3 1887

Deep high z Whole Sky Galactic Extragalactic Resolved SFH

ESO/VISTA Public Survey status

Estimated completion year

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!

Phase 3 releases from ESO Public Surveys

The VISTA & VST public survey DPs released through the Phase 3 process in 2014/2015 cover almost 11500 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

Phase 3 releases from ESO Public Surveys

Data volume download from ESO SAF of public survey products: all surveys have been accessed by archive users

Statistics: ESO Science Archive Facility -Access and Download

0

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VVV

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VIDEO

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Gaia - ESO

PESSTO

Spectroscopic VISTA VST

# of publications (April 2016)

Spectroscopic VISTA VST

# 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

The future of 4m telescopes

High-level:

Science Priorities at ESO

From 85th Meeting Of SCIENTIFIC TECHNICAL COMMITTEE

Garching, 21-22 April 2015

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 14021 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)

Second VISTA call for ESO Public Survey

Fabian+03

4MOST – 4m Multi-Object Spectroscopic Telescope

P.I. Roelof de Jong(AIP)

VISTA

Fabian+03

4MOST timeline

• June 2016: Preliminary Design Review

• 2018: Final Design Review

• 2019: Call for Proposal for Community surveys

• 2020: Preliminary Acceptance Europe

• 2021: Start of operations

Fabian+03

4MOST GTO Galactic Surveys

• 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

Fabian+03

4MOST GTO Extra-galactic Surveys

• 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

● 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 onthe NTT is aging and will not remain competitive much longer. ESO's community ofastronomers continues to grow, and the NTT is one of the best 4m class telescopes inthe Southern Hemisphere. For this reason it makes good sense to consider new long­term goals for the NTT. 

● no resources for in­house 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.

 

Electronic

InstrumentationSoftware

comp HWNetwork

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LPRS distribution by Type

2013+2014

2013

2014

Type of problem

Nr. of problems

2014

● March 1: call

● June 9: 7 letters of intent shortlisted

2015

● February 13: closing date for detailed proposals

● April: STC

● June: Council

June 2015

SOXS

SOXS

NIRPS

NIRPS

And for more future directionsSee community poll