La contribución de las ICTS españolas a la misión Gaia de ESA

REG Red Española de Gaia

La contribución de las ICTS españolas a la misión Gaia de ESA , 21-23 marzo 2012 1/22

La contribución de las ICTS españolas La contribución de las ICTS españolas a la misión Gaia de ESAa la misión Gaia de ESA

Objetivos: Ofrecer un marco de discusión a la comunidad interesada en la explotación científica de Gaia (REG - GREAT) a cerca de las necesidades de observaciones complementarias a poder llevar a cabo con ICTS españolas.



Dos telescopios: espejos primarios de 1.45 0.50 m2

Plano focal combinado 2 FoV, con 106 CCD

Eje de rotación (6 h), precesión (63 día)

Radial-Velocity Spectrograph (RVS)

Figure courtesy EADS Astrium

Bipods

Estructura toroïdal de SiC

Monitor del ángulo de base

Superposición de los dos FoV



All 10 mirrors integrated on the optical bench

Alignment of the two telescopes in progress, tolerance 3 mm



Focal plane

Blue Photom

eter CC

Ds

Blue Photom

eter CC

Ds

Red Photom

eter CC

Ds

Red Photom

eter CC

Ds

Image motion

2

Radial Velocity Spectrometer CCDs

2

Radial Velocity Spectrometer CCDs

Astrometry

106 CCD, 938 milions of pixels, 2800 cm2 104,26cm

42,3

5cm

Detection Spectrophotometry Spectroscopy



Focal Plane Assembly

Completion of mechanical and thermal tests; delivery for integration in the PLM



Summary of statusIndustrial development is overall good: no major issues unresolved

Completion of the FPA mechanical tests and thermal tests Completion of the alignment of the two telescopesLaunch in 2013

Data processing preparation is in good healthGSIR successfulend-to-end tests ongoingFirst steps for CU9: GAP, GENIUS

Scientific exploitationData releases scenario establishedGREAT & REG: meetings, exchange of visits, ESRs FP7Additional spectroscopic survey: Gaia-ESO

Contribution to the scientific case of WEAVE



First release:launch + 22 MonthsAug-2013 June-2015

• Positions () and G-mag for single-like stars (90% of the sky)

• the Hundred Thousand Proper Motions (HTPM) catalogue based on the Hipparcos stars

Second release:launch + 28 MonthsDec-2015

• Updates of above +• Mean radial velocities for stars with non-variable radial velocity (90% of the sky)

Third release:launch + 40 Months

Dec-2016

• Positions (), proper motions, and parallaxes and G-mag for single stars (90% of the sky)• Orbital solution for period between 2 months and 75% of the observation duration• Integrated photometry RP/BP • Spectrophotometry from RP/BP for sources for which astrophysical parameters are simultaneously released• Source classification based on BP/RP and astrometry for stars with sufficiently high quality data • Mean RVS spectra for sources where single epoch spectra are usable and APs are simultaneously released

Data release scenario (I)



Fourth release:launch + 65 Months

Jan-2019

Updates of all above + • Source classification plus multiple stellar astrophysical parameters derived from BP/RP, RVS and astrometry for the majority of stars• Variable star classifications and parameters as available, and the epoch photometry• Solar system results with preliminary orbital solutions and individual epoch observations• Non-single star catalogue

Final release:End Mission + 3 years (36 months)

Aug-2021/2022

Full astrometric, photometric, radial velocity catalogue• All available variables and non-single stars solutions• Source classifications (probabilities) plus multiple astrophysical parameters derived from BP/RP, RVS and astrometry for stars, unresolved binaries, galaxies and quasars.Precision improved with respect to 4th release. Some parameters may not be available for fainter stars.• Non Single Stars solutions and exo-planet list • All epoch and transit data for all sources• All Ground Based Observations made for data processing purposes (or links to it)

Data release scenario (II)

+ early releases of transient sources and Near Earth Objects to IMMCE



Gaia capabilities •Positions, proper motions and parallaxes for 1 billion stars (G < 20)

•Low resolution spectrophotometry for 1 billion stars, allowing estimations of Teff, logg, Av and [Fe/H]

•Radial velocities for 150 million stars (GRVS < 17)•Atmospheric parameters, reddening and rotational velocities for 5 million stars (GRVS < 12)

•Detailed chemical abundances for 2 million stars (GRVS < 11)…but is going to need some help ~90% of stars without radial velocities

> 90% without accurate chemical composition additional characterization, time sampling



1.Data processing and mission operations

2.Science exploitation: ongoing projects

3.Science exploitation: future projects

On-ground observations



1. Data processing and mission operations (I)

DPAC, data processing GBOG was set up in 2006

• spectrophotometric standards ([email protected], DOLORES@TNG)long-term variability monitoring until 2014, ~200 SPSS, V<14, small telescopes

• 1420 radial velocity standards: stability at 300 m/svariability monitoring until 2018 (1 additional measurement, ~70 nights)

• training data sets (stellar parameterization, asteroid taxonomy DOLORES@TNG)

• reference frame (alignment with VLBI, morphology of QSO)



1. Data processing and mission operations (II)

DPAC, data processing

Support networks:

• Gaia-FUN-SSO, a Gaia Follow-Up Network for the Solar System Objects• GBOT: Optical tracking• Verification of science alerts (first months of mission)

Shall small/medium telescopes become involved ? Strategic decision by the managers of ICTS

DPAC, data validation still open if auxiliary observations are needed



2. Science exploitation

• Gaia science is unique, very wide and even unexpected

• Complementary observations to reinforce the scientific return: photometry and spectroscopyin many cases multi-epoch observationsoptic, NIR, IR

• Rather different needs depending on the science topicongoing projects (surveys or specific objects)projects for the future

• preparing for Gaia data, and• when Gaia data will be available

(see all talks)



Requirements and recommendations•R=5000: for completion of the 6D phase space information for stars with 16 < G < 205·106 stars; 2-3 km/s vrad; 0.2 dex [Fe/H]

•R=20.000 spectroscopy for metal-poor disk and halo stars, dwarfs and giants, stars in nearby dwarf galaxies (large distances with 4m telescopes) and the bulge5·104 stars + 5·104 stars ; 1-2 km/s vrad; 0.1 dex [Fe/H]; /Fe

•R=40.000-60.000 multi-fibre and perhaps single slit spectroscopy of selected populations of metal-rich stars, e.g. disk and outer bulge (4-8m telescope)2·105 stars; < 0.05 dex [Fe/H]; /Fe; r-s processes

Optical + IR





GES: Gaia ESO spectroscopic survey (FLAMES@VLT) ~300 people, 300 nights in 5 years, field stars + open clusters

>105 Giraffe spectra (R ~ 16,000 - 25,000) >104 UVES spectra (R ~ 47,000)

2. Science exploitation: ongoing projects

The counterpart in the Northern hemisphere absolutely needed

There is no suitable multi-object spectrograph available Meanwhile, [email protected]+FIES@NOT (on object-by-object basis: RC in OC)

Future: WEAVE (and others) ?



Stellar characterization: massive, FGK, low-mass stars

massive stars GOSSS, OWN, IACOB, NoMaDS, IACOB-sweG, CAFE-beans:

LR,IR,HR + imaging Astralux FIES@NOT, HERMES@Mercator, ….

FGK stars (age, chromospheric activity, vsini, …) R ~40000 – 80000 échelle spectra

Low-mass stars Radial velocity: CAFÉ, HARPS-N, GIANO, CARMENES, … Transit: SuperWASP+, LCOGT, SONG, XO, Master




Characterization of galactic structures: arms, moving groups

Cygnus arm through open clustersphotometry (1-2m telescopes at CAHA+ORM)spectroscopy (NOT, WHT, INT, Haute-Provence)

Moving groups through age, chromospheric activity, chemical composition of FGK stars

R ~40000 – 80000 échelle spectra

Star forming regionsmodern wide field images in IR proper motions

Obscured massive clustersmultiplexing in the NIR at moderate resolution R=10 000 - 20 000




Characterization of solar system objects

Shapes, orientations and albedosphotometry at given phases

complete light curves with photometry

Taxonomy UV spectroscopy DOLORES@TNG

there is a coordination with SSO network: how can we guarantee the commitment with the network, if needed ?




3. Science exploitation: Future projectsduring Gaia operations

• Follow-up of alerts (transients + SSOs)•Quick reaction from Spanish ICTS? •more than 34 European Observatories in the list •Spanish research groups not identified during the meeting

Shall small/medium telescopes become involved ? Strategic decision by the managers of ICTS

a significant number of time for a valid contribution



3. Science exploitation: Future projects• GES-like in the North

• Characterization of outliers (UaC leading the processing in DPAC)5% of sources, grouped into familiesPhotometry, intermediate and high resolution spectroscopy

• Characterization of ultra faint dwarf galaxiesDeep colour-magnitude diagram (V,I) for stellar population synthesisMOS

• Characterization of kinematic groupsMid & High resolution spect for age and detailed chemical compositionR ~20000, 40000 – 80000

• Characterization of NEAs, NEOs, asteroids photometry and UV spectroscopy



Discussion (I)• To distinguish among existing and future facilities

spectroscopy (no multiplexing available) FIES@NOT, CAFE@CAHA, HARPS-N at TNG,

HERMES@MERCATOR limiting magnitude V~12

clear support to WEAVE needs for R>40,000 for faint stars identified MIRADAS, MEGARA, HEXA, HORUS

• Current ongoing projects are been granted by TACs, but surveys need large projects

could ORM have guarantee time as CAHA ?Number of nights/yr (50 in CAHA: is it enough ?)

Remember: a large survey reduce costs to the ICTS



Discussion (II)• The need to prepare well defined projects for the next 5-10 years was

identified • Spanish groups could join in bigger groups copying GBOG philosophy:

a set of well defined projects (number of nights, instruments, …) a common interest identified it could be the interface with the managers of RIA/ICTS

• Follow-up observations post-Gaia releases REG community should precisely define projects

Ensure that the instrumentation needed will be available at that time

• GES-North has to wait WEAVE (and others)



Discussion (III)• ICTS in “danger” or unclear situation

NOT, Stella, 2.2mCAHA could Gaia community / “Gaia science case” help on this issue ? yes, look for European projects

German-Spain for CAHA Sweden-Spain for NOT

2.2m CAHA could change its regimeCould a well defined “Gaia Science Case” be elaborated by the Spanish-German

communities in the next months ? Commitments by the Scientific Community: data public & reduced in one-year (like

GES-ESO), common pipe-lines, shared toolsA “letter of support” is needed / desirable ? does REG wish to do it ?



Actions on us• Articulate a group of discussion within REG for:

• Reinforce coordination of current applications related with ongoing projects

• Definition and coordination of future mid- and long-term projects a GBOG-like effort (for the next 5-10 years)

• Support to the several instruments under development or in different levels of study (establishment of priorities ?)

WEAVE Spanish group (both scientific and strategic roadmap)

• Identification of instrumentation available for post-Gaia observations (beyond 2022)

• Convenience of defining a “Gaia on-ground observations road map”, accounting for different scenarios

• ICTS in “danger” or unclear situation (letters of support)



Contribution to next discussion

• Prepare well defined projects

• ICTS in “danger” or unclear situation (letters of support)

• Long-term projects / Legacy projectsCAHA 50 nights, enough ?which telescopes/instruments at ORM, OT, …

• Is there interest if Spanish ICTS to become part of Gaia-networks ? (mission preparation and follow-up of transients and SSOs)







Gaia capabilities •Positions, proper motions and parallaxes for 1 billion stars (G < 20)

•Low resolution spectrophotometry for 1 billion stars, allowing estimations of Teff, logg, Av and [Fe/H]

•Radial velocities for 150 million stars (GRVS < 17)•Atmospheric parameters, reddening and rotational velocities for 5 million stars (GRVS < 12)

•Detailed chemical abundances for 2 million stars (GRVS < 11)



RVS design•R = 11500 GRVS < 10•binning by 3 pixels GRVS > 10•range 847-874 nm 27 nm



Requirements and recommendations

ASTRONET: “It is crucial to supplement the Gaia data-set with dedicated ground-based spectroscopic programmes, in order to obtain the radial velocity and detailed chemical abundances for fainter stars”



Current and future instrumentation•Gaia-ESO survey: 100.000 stars and 100 open clusters

UVES V < 16.5 GIRAFFE V < 19

•RAVE Ca II triplet 1 million stars •APOGEE 300 fibres R=20.000 giants with H<13.5•HERMES 400 fibres R=30.000 FoV=2deg2 V<14 1 million stars

•4-MOST at NTT 1500 fibres FoV=3deg2 LR+HR •MOONS 500 fibres IR VLT -> inner disk and bulge•WEAVE at WHT 1000 fibres FoV=2deg2 LR+HR•LAMOST 4000 fibres FoV=5deg2 LR(+HR)



Star density

latitude 0-5 deg 100,000 stars /deg2 G =< 20 5-10 80,000 10-20 31,000 20-30 11,000 30-90 3,800

open clusters, globular clusters, halo streams, dwarf satellites



High-Res post-Gaia More spectroscopic observations of FGKs will be needed:

Large number of stars

High-Res:

But R < 20000

But only V<10-12



High-Res post-Gaia More spectroscopic observations of FGKs will be needed:

High-Res & faint stars:

R = 40 - 80000

Large number of data

North Spectroscopic survey

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La contribución de las ICTS españolas a la misión Gaia de ESA