CHRONOS: Towards an auto-consistent and absolute age scale

Transcription

1 CHRONOS: Towards an auto-consistent and absolute age scale David Barrado, Nuria Huélamo, Hervé Bouy CAB (INTA-CSIC), Université de Bordeaux Granada, October 14th, 2016

2 CHRONOS: WHY AND HOW? Ø Age is unarguably one of the most fundamental parameter of any astrophysical object Ø Different age-dating techniques produce values with discrepancies up to 50% Ø The main culprit for this state of affairs is the lack of a universal age scale and the absence of a systematic and robust cross-calibration of the various methods Ø Our goal is to deliver a universal, self-consistent, absolute and accurate age scale over the entire time

3 Ages from isochrones Lithium ages End MS 1 Msun Globular clusters Anchors Universe: Gyr Sun: 4.57 Gyr Rocky planets Disks dissipate Coma Praesepe Hyades Blanco 1 Pleiades APer IC4665 IC2602, IC2391 NGC2547, NGC1960 BPMG TWA Blanco 1 Pleiades APer IC2602 IC2391 IC4665,NGC2547 BPMG, NGC1960 Valid range LDB ages Gas giant planets Class I ends Gaia is almost blind here

4 A(Li) Lithium evolution Age dating techniques Lum Isochrone fitting Teff Teff Rot.Vel Lx Dec ZAMS Gyrochronology Stellar activity Kinematics Teff Teff R.A.

5 The age stairways Others: Lithium FGK, activity, gravity (GES, Kepler K2, APOGEE, CAHA) Binaries (SB2 and EB), multiple systems (GES, Kepler K2, TESS, APOGEE, CAHA) Isochrone fitting (Gaia, DANCe, VISTA) Asteroseismology (Kepler K2, TESS, Gaia) Kinematics (Gaia, DANCe, GES, CAHA) Gyrochronology (Kepler K2, TESS) LDB (DANCe, 8-10m telescopes) Radiometry Λ-CDM ONC, NGC2264 Taurus LOSFR Upper Sco TWA BPMG AB Dor IC4665 IC2391, IC2602 APer Pleiades, Blanco1, M35 Hyades, Coma, Praesepe NGC2158 NGC752 Ru 147 M67 x Sun Globular clusters Universe

6 CHRONOS: CAHA role now i) supplying Lucking Imaging in order to detect visual binaries (2.2m/Astralux) ii) iii) iv) providing high spectral resolution (2.2m/CAFE and CARMENES in few cases) to fully characterize cluster members (lithium in FGK stars, vsini, gravity indicators, stellar activity detecting spectroscopic binaries (an together with Kepler data and Astralux, produce a complete binarity study) measuring accurate radial velocities for faint members not observed by Gaia (for the kinematics). The goal is to observe several hundred members in each of these clusters and to collect high quality (SNR>100), homogeneous, high spectral resolution data together with the Lucky imaging along four semesters, totalling 200 nights. See Barrado D., 2016, Stellar clusters: benchmarks of stellar physics and galactic evolution - EES2015, E. Moraux, Y. Lebreton, and C. Charbonnel (eds.). EAS Publications Series, - arxiv:

7 CHRONOS: CAHA role in the future ASTRONET (specially the Wide Field Spectrograph Working Group): ASTRONET Science Visions updatefuture facilities (as defined in the Science Vision of 2007) A wide-field, highly-multiplexed, low and high resolution spectroscopic survey telescope will be complementary for goals 6 & 7, it will be necessary to disentangle the relations between masses, ages, morphologies, and environments in order to understand the formation of galaxies. ASTRONET: Infrastructure Roadmap update Development of wide-field, multiplexed spectrometers for 8m-class telescopes A very strong scientific case for the development of wide-field, multiplexed spectrometers has existed for many years and was a high priority recommendation of the Roadmap

8 Scientific cases Stellar evolution and the structure of the Galaxy: exoplanets, astroseismology, arqueoastronomy, properties stellar clusters Extragalactic: large scale structure, equation opf state dark energy, properties universe high redshift, metal enrichment of the Universe, etc Exploitation large photometric cartographic studies: VISTA, LSST, PAUCam, J-PLUS, J-PAS Support space missions: Gaia, PLATO, EUCLID, etc

9 CALAR ALTO: m 2.2m 1.23m TCE Califa, Legacy (extragalactic) PMAS Spectroscopy CAFÉ+CAFOS IR Cartography PANIC Image Long-term DLR camera ExoEarths Carmenes? Carmenes Gaia Legacy? Instrument? CEO (MONSUL) pathfinder? Spectroscopic cartrography HEXA+multiplexing 9

10 Field The market Multiplexing (fibers) Resolution Simultaneous coverage LAMOST 5 deg ,000 (future) (50% loses) VISTA 4MOST (South) MMT HECTOECHELLE AAO HERMES (South) WHT WEAVE deg , deg ,000 1 order 2 deg ,000 (50% loses) 1000 A In four orders VPH 2 deg ,000 1 order? VLT MOONS (South) GTC MEGARA 500 arcmin pairs 9, mu mu mu 3.5x3.5 arcmin 92 18, Δvelocity = F(espectral coverage, SNR, resolution)

11 Why HEXA (2012)? Ø Two decades of large photometric surveys: SDSS, 2MASS, WISE, VISTA, VST, Kepler, etc), there is a need of massive spectroscopy. Ø Combination of photometric and spectroscopic data: key problems like the assembly and evolution of galaxies, cosmology, and stellar archeology, among others. Extragalactic science: a) improved spectral resolution (e.g. search for supermassive blackholes), b) with a larger spatial coverage (e.g. IFUs to resolve properties of nearby objects, as it is the case of CALIFA or MaNGA), c) deep enough to observe low surface brightness galaxies (to ensure completeness of galaxy samples at low luminosities). Stellar case will be dominated by the results of the GAIA mission (one billion stars down to magnitude G=20. Initial steps with Gaia-ESO (GES) Ø "Astronet infrastructure road map" and "Science Vision for European Astronomy" reports (e.g. SV B7 at HEXA followed the MICINN/MINECO roadmap for new infrastructures: RIA informed very positively about HEXA

12 HEXA: 6.5m telescope for spectroscopic mapping Base-line: Ø Aperture 6.5m Ø FOV 1.5 deg Ø 500 multiplexing Ø Medium to high-spectral resolution (R= 5,000 and 25,000) Science with HEXA: some examples a) Gaia follow-up: properties and evolution of stars and stellar associations b) Plato: characterization of exoplanets c) Extragalactic: post-califa d) Cosmology: J-PAS, J-PLUS e) Cosmology: dark energy and acustic barionic oscilations

13 Ø Aperture: 6.5m diameter Requirements Summary Ø Output F# number = 3.6. (for the prime focus solution F#2.5 was used) Ø Plate scale for 2M and 3M: 8.84 arcsec/mm (focal length 23.4m, F#3.6). Ø Plate scale for 1M: 12.2 arcsec/mm (focal length m, F#2.5) Ø FOV: 1º to 2º Ø (diameter) Ø Image quality: seeing limited Ø Spectral range: narrow band filters 100 Å in the whole wavelength range : 3800 Å Å Ø Optimized for fibers: Telecentric system and flat focal plane

14 HEXA: a 6.5 m for CAHA

15 Initial instrumental concepts Nasmyth A (Hekatonkheires+Cyclops) ØFiber positioner at Nasmyth: HECATE (Giraffe+Megara) ØMultifiber spectrograph: GYGES ØIFU bundle (PMAS/PPAK-like) ØCamera BRONTESS Nasmyth B (Titans): ØSlitless: GEA (based on Gaia), D. Galadí ØWide Field IFU (Fourier): CEO (MONSUL), J. Iglesias

16 HECATE/GYGES

17 Nasmyth A (Hekatonkheires & Cyclops) Nechelle x CAFE-like R=60,000 NIFU x PMAS-type R=5000 Bundles in 5 arcmin Current Ncells=361 NMOS=358 NIFU=1 Nechelle=1 Ncam=1 Ncells GYGES R=25,000 HECATE positioner NMOS=Ncells-NIFU-Nechelle-Ncam Ncam x BRONTESS camera 1 deg FOV

18 The telescope: phases and milestones We followed the MICINN/MINECO roadmap for new infrastructures. RIA informed very positively about HEXA: En esta línea, la nueva instrumentación de gran campo en fase de estudio (el espectrógrafo multiobjeto el telescopio en fase de definición) son cruciales para estas necesidades y la comunidad REG requiere su uso para grandes surveys. HEXA never obtained a negative report Phase Name Milestone at the end of the phase Abbrev. Phase 1 Conceptual Design System Conceptual Design Review SCDR OK Phase 2 Preliminary Design Preliminary Design Review PDR Phase 3 Detailed Design Critical Design Review CDR Phase 4 Manufacturing and subsystem tests Subsystem Acceptance Reviews SSAR Phase 5 Assembly, Integration and Verification System Preliminary Acceptance Review (at site) SPAR Phase 6 Commissioning System Acceptance Review (SA) at site and on sky (Final Acceptance) FA

19 Detailed spectral characterization Plenty of features Smal equivalent widths Small equivalent widths, blended with other features R=40,000 or larger, SNR>100 or larger

20 Fourier transform spectrometer (see the talk by J. Iglesias) R=1-20,000 in 30 arcmin

21 Multiplexing with masks: Magellan/IMACS A much wider detector is required Confusion Limited resolution Limited packing

22 Echelle: multiple detectors 300 CCDs (fibers) x 20,000 euro/ccd = 6,000,000 Meuro But in fact this design requires a battery of spectrographs

23 HERMES: smart design

24 Summary Ø CHRONOS: 200 nights now for accurate ages Ø HEXA was a very promising concept Ø This four years have changes the technological and scientific landscapes Ø TCE is a qualitative and quantitative leap: instrumental (WEAVE, 4MOST), tecnological (large surface optical elements) and scientific (CHRONOS, BAOs, etc) leap Ø ASTRONET.- The community yearns for it Ø Spanish capacity to accept the challenge Ø Possible international collaborations: UBerkeley, China, Max- Planck