Transcript Diapositiva 1 - Isaac Newton Group of Telescopes
REG Red Española de Gaia
La contribución de las ICTS españolas a 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.
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Dos telescopios: espejos primarios de 1.45 0.50 m 2 Eje de rotación (6 h), precesión (63 día) Monitor del ángulo de base Estructura toroïdal de SiC Bipods Plano focal combinado 2 FoV, con 106 CCD Radial-Velocity Spectrograph (RVS) Superposición de los dos FoV
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Figure courtesy EADS Astrium 2/22
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All 10 mirrors integrated on the optical bench
Alignment of the two telescopes in progress, tolerance 3 mm
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Focal plane
106 CCD, 938 milions of pixels, 2800 cm 2
104,26cm Detection Astrometry Image motion Spectrophotometry
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Spectroscopy 4/22
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Focal Plane Assembly
Completion of mechanical and thermal tests; delivery for integration in the PLM
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Summary of status
Industrial development is overall good
: no major issues unresolved Completion of the FPA mechanical tests and thermal tests Completion of the alignment of the two telescopes Launch in 2013
Data processing preparation is in good health
GSIR successful end-to-end tests ongoing First steps for CU9: GAP, GENIUS
Scientific exploitation
Data releases scenario established GREAT & REG: meetings, exchange of visits, ESRs FP7 Additional spectroscopic survey: Gaia-ESO Contribution to the scientific case of WEAVE
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REG Red Española de Gaia First release:
launch + 22 Months Aug-2013 June-2015
Second release:
launch + 28 Months Dec-2015
Third release:
launch + 40 Months Dec-2016
Data release scenario (I)
• Positions ( a,d ) and G-mag for single-like stars (90% of the sky) • the Hundred Thousand Proper Motions (HTPM) catalogue based on the Hipparcos stars • • Updates of above +
Mean radial velocities for stars
with non-variable radial velocity (90% of the sky) •
Positions (
a,d
), 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
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launch + 65 Months Jan-2019
Final release:
End Mission + 3 years (36 months)
Aug-2021/2022
Data release scenario (II)
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
photometry as available, and the epoch •
Solar system results
with preliminary orbital solutions and individual epoch observations • Non-single star catalogue 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)
+ early releases of transient sources and Near Earth Objects to IMMCE
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Gaia capabilities
• Positions, proper motions and parallaxes for 1 billion stars (G < 20) • Low resolution spectrophotometry for 1 billion stars, allowing estimations of T eff , logg, A velocities for 5 million stars (G RVS v and [Fe/H] • Radial velocities for 150 million stars (G < 12) RVS < 17) • Atmospheric parameters, reddening and rotational • Detailed chemical abundances for 2 million stars (G RVS < 11)
…but is going to need some help
~90% of stars without radial velocities > 90% without accurate chemical composition additional characterization, time sampling
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On-ground observations
1.Data processing and mission operations 2.Science exploitation: ongoing projects 3.Science exploitation: future projects
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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/s variability 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)
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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
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2. Science exploitation
• Gaia science is unique, very wide and even unexpected • Complementary observations to reinforce the scientific return: photometry and spectroscopy in many cases multi-epoch observations optic, NIR, IR • Rather different needs depending on the science topic ongoing projects (surveys or specific objects) projects for the future • preparing for Gaia data, and • when Gaia data will be available (see all talks)
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Requirements and recommendations
• R=5000: for completion of the 6D phase space information for stars with 16 < G < 20 5·10 6 stars; 2-3 km/s v rad ; 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 bulge 5·10 4 stars + 5·10 4 stars ; 1-2 km/s v rad ; 0.1 dex [Fe/H]; a /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) 2·10 5 stars; < 0.05 dex [Fe/H]; a /Fe; r-s processes
Optical + IR
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2. Science exploitation: ongoing projects
GES:
Gaia ESO spectroscopic survey
(FLAMES@VLT) ~300 people, 300 nights in 5 years, field stars + open clusters >10 5 Giraffe spectra (R ~ 16,000 - 25,000) >10 4 UVES spectra (R ~ 47,000) 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) ?
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2. Science exploitation: ongoing projects
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
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2. Science exploitation: ongoing projects
Characterization of galactic structures
: arms, moving groups Cygnus arm through open clusters photometry (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 regions modern wide field images in IR proper motions Obscured massive clusters multiplexing in the NIR at moderate resolution R=10 000 - 20 000
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2. Science exploitation: ongoing projects
Characterization of solar system objects
Shapes, orientations and albedos photometry 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 ?
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3. Science exploitation: Future projects during 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
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3. Science exploitation: Future projects
•
GES-like in the North
•
Characterization of outliers (UaC leading the processing in DPAC)
5% of sources, grouped into families Photometry, intermediate and high resolution spectroscopy •
Characterization of ultra faint dwarf galaxies
Deep colour-magnitude diagram (V,I) for stellar population synthesis MOS •
Characterization of kinematic groups
Mid & High resolution spect for age and detailed chemical composition R ~20000, 40000 – 80000 •
Characterization of NEAs, NEOs, asteroids
photometry and UV spectroscopy
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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
large projects surveys need
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
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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)
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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 regime
Could 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 tools A “letter of support” is needed / desirable ? does REG wish to do it ?
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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)
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Contribution to next discussion
• Prepare well defined projects •
ICTS in “danger” or unclear situation
(letters of support) • Long-term projects / Legacy projects CAHA 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)
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Gaia capabilities
• Positions, proper motions and parallaxes for 1 billion stars (G < 20) • Low resolution spectrophotometry for 1 billion stars, allowing estimations of T eff , logg, A velocities for 5 million stars (G RVS v and [Fe/H] • Radial velocities for 150 million stars (G < 12) RVS < 17) • Atmospheric parameters, reddening and rotational • Detailed chemical abundances for 2 million stars (G RVS < 11)
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RVS design
• R = 11500 G RVS • binning by 3 pixels G RVS • range 847-874 nm < 10 > 10 27 nm
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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”
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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=2deg 2 stars V<14 1 million • 4-MOST at NTT 1500 fibres FoV=3deg 2 LR+HR • MOONS 500 fibres IR VLT -> inner disk and bulge • WEAVE at WHT 1000 fibres FoV=2deg 2 LR+HR • LAMOST 4000 fibres FoV=5deg 2 LR(+HR)
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Star density
latitude 0-5 deg 100,000 stars /deg 2 5-10 80,000 10-20 31,000 20-30 11,000 30-90 3,800 G =< 20 open clusters, globular clusters, halo streams, dwarf satellites
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High-Res
post-Gaia
More spectroscopic observations of FGKs will be needed:
Large number of stars
But R < 20000
High-Res:
But only V<10-12
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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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