Long-term projects for the determination of stellar parameters, abundances and kinematics

1. Long-term projects for the determination of stellar parameters, abundances and kinematics David Montes et al. Dpto. Astrofísica, F. Físicas Universidad Complutense de Madrid, UCM, Madrid, Spain RIA Workshop: Ciencia con los telescopios óptico-infrarrojos de CAHA y ORM en la próxima década. 22-23 de marzo 2012, CDTI, Madrid

2. Collaborators

3. High-resolution spectroscopy High-res echelle spectra High-resolution échelle optical and NIR spectrographs R= 85000 – 22000 (0.08-0.3 Å) – Previous, present and future WHT-UES (Utrecht Echelle Spectrograph) INT-MUSICOS (MUlti SIte COntinuous Spectroscopy) NOT-SOFIN (SOviet FINish spectrograph) NOT-FIES (FIber fed Echelle Spectrograph) TNG-SARG (Spettrografo ad Alta Risoluzione Galileo) TNG-HARPS-N (2012 - ) (High-Accuracy Radial velocity Planet Searcher - North) TNG-GIANO (bifront infrared spectrometer) Mercator-HERMES GTC-HORUS ? (High Optical Resolution Ultra-Stable Spectrograph) project for update UES ORM: CAHA: 2.2m-FOCES, (until 2009), (Fibre Optics Cassegrain Echelle Spectrograph) 2.2m-CAFE, (2011- ) (Calar Alto Fiber-fed Echelle spectrograph) 3.5m-CARMENES (2014 - ) (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs)

4. Intermediate-resolution spectroscopy Intermediate-resolution optical and NIR spectrographs R < 20000 (> 0.3 Å) – future ORM: CAHA: 6 m - HEXA (an instrument for spectroscopic surveys) WHT- WEAVE (wide-field multi-object spectrograph) GTC - MEGARA (Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía) GTC - MIRADAS (Mid-resolution InfRAreD Astronomical Spectrograph)

5. Previous long-term projects • High-Res spectroscopic surveys of FGKMs dedicated to: • Detailed analysis of the chromospheric activity – 1990- • Libraries of high resolution spectra of cool stars – 1997 – 1999 • Survey of late-type (F-M) stars in MGs – 1999 - 2002 • Survey of FGK in the solar neighbourhood (DUNES) – 2005-2009

6. 2.2m-FOCES, (until 2009), (Fibre Optics Cassegrain Echelle Spectrograph)

7. 2.2m-FOCES, (until 2009), (Fibre Optics Cassegrain Echelle Spectrograph)

8. Survey of FGK stars in MGs ★ Survey late-type stars in Moving Groups (MGs) 1999- 2002 - 144 FGKM stars - Montes et al. 2001,A&A, 379, 976; - López-Santiago et al. 2005, PhD Thesis UCM; 2006, ApJ, 643, 1160; 2009, A&A, 499, 129; 2010, A&A, 514, A97 http://www.ucm.es/info/Astrof/invest/actividad/skg/skg_SS.html

9. Survey Nearby FGK stars ★ Survey of FGK stars in the solar neighbourhood (d < 25 pc), including the DUNES sample 2005- 2009 – 450 FGKM stars - Martínez-Arnáiz et al. 2010, A&A, 520, A79; 2011, MNRAS, 414, 2629, 2011, PhD Thesis UCM; - Maldonado et al. 2010, A&A, 521, A12 FGK stars in the solar neighbourhood (d < 25 pc) which include the DUNES sample, an approved Herschel OTKP with the aim of detecting cool faint dusty disks (Eiroa et al. 2010).

10. Ongoing long-term projects • High-Res spectroscopic surveys of FGKMs dedicated to: • Confirming members of MGs by Chemical Tagging – 2010 - • RasTyc Survey (young stars, ROSAT All-Sky X-ray sources)– 2000 - 2008 • Survey of co-moving young stars in Cepheus – 2009 - • Searching “isolated” very young star – 2011- • Gaia ESO Spectroscopic Survey (GES) • Characterization of late-type M-dwarfs for CARMENES • Calibrating the metallicity of M dwarfs with wide visual binaries

11. Spectroscopic Analysis • Kinematics (U, V, W). • Radial velocity (Vr) • Age (LiI 6707.8Å). • Chromospheric activity • CaII H&K toCaII IRT • Rotation (vseni). • Activity – rotación relation • Stellar parameters. • Teff, log g, ξ and [Fe/H] • Absolute and differential abudances. • Chemical tagging

12. Stellar parameters Teff, log g, ξ and [Fe/H] • Stellar atmospheric parameters (Teff, log g, ξ and [Fe/H]) • StePar (Tabernero Montes, González Hernández 2011): • - 2002 version of the MOOG code (Sneden 1973). • a grid of Kurucz ATLAS9 plane-parallel model atmospheres (Kurucz 1993). • - The EW determination of the Fe lines with the ARES code (Sousa et al. 2007). • - 263 Fe I and 36 Fe II lines (Sousa et al. 2008). • The code iterates until obtain: • excitation equilibrium: • the slopes of χvs log(є(Fe I)) • and log(EW/λ) vs log(є(Fe I)) where zero • - ionization equilibrium: • log(є(Fe I)) = log(є(Fe II)). • - 2-σ rejection of Fe I and Fe II lines after a first determination of the parameters • - Limitations: spectral types F6 to K4, slow rotators, no veiling.

13. Chemical abundances Fe, Na, Mg ….. • Fe, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, and Ni • EW method in a line-by-line basis with AREScode (Sousa et al. 2007). • Line lists and atomic parameters from (Neves et al. 2009; González Hernández et al. 2010). • - Abundance analysis with MOOG(Sneden 1973) using our determined atmospheric parameters and a solar spectrum taken with the same instrumental configuration. [Ni/Fe] vs [Fe/H]: open diamonds represent the thin disk data (González Hernández et al. 2010), black filled triangles represent Hyades cluster data (Paulson et al. 2003). Red points are our stars compatible with Hyades Fe abundance, and the green ones not compatible. BZ Cet and HD19902 Hyades cluster members are marked with blue circles. Purple starred points represent the giant stars.Black starred points are the candidates selected stars in De Silva et al. (2011), black circles are those selected in Pompéia et al. (2011).

14. Differential abundances Δ[X/H] • Differential abundances Δ[X/H] • determined by comparison with a reference star known to be member of the Hyades cluster (vB 153) in a line-by-line basis (Paulson et al. 2003 and De Silva et al. 2006). • A first candidate selection within the sample has been determined by applying a 1-rms rejection for the Feabundance results. In this subsample another 1-rms diagnostic has been applied in order to prove homogeneity in each element. Δ[Fe/H] differential abundance vsTeff. Dashed-dotted lines represent 1-rms level for the Hyades cluster. The dashed line represents the median abundance. Red points are accepted as a preliminary selection of candidates, while green ones are rejected. The Hyades cluster member BZ Cet and HD19902 are marked with blue points. Purple starred points represent the giant stars.

15. Stellar KinematicsGroups • Moving group (Supercluster) Eggen (1994) • Group of stars gravitationally unbound that share the same kinematics and may occupy extended regions in the Galaxy Montes et al. 2001 MNRAS.328...45

16. Stellar KinematicsGroups Possible origin of the Stellar Kinematics Groups • Dissolution of clusters or kinematical features? • Several studies conclude that those regions of the UV-plane consist of both • field-like stars and young coeval ones. • Famaey et al. 2005, 2007, 2008; • Antoja et al. 2008; • Klement et al. 2008; • Francis & Anderson 2009; • Zhao et al. 2009. • High resolution spectra is needed to determine ages and metallicities and discern between: • field-like stars (associated with dynamical resonances (bar) or spiral structure). • young coeval stars (debris of star-forming aggregates in the disk).

17. Chemical Tagging The detailed analysis of the chemical signatures chemical tagging is another powerful method that provide clear constrains to the membership to these structures. In open clusters (Hyades, Collinder 261) (Pauson et al. 2003, De Silva et al. 2006, 2007a, 2009) high levels of chemical homogeneity showing that chemical information is preserved within the stars and possible effects of any external sources of pollution are negligible. Figure from De Silva et al. (2009) sowingtheabundancesofHR1614 MG stars (De Silva et al. 2007b, triangles) comparedtotheHyades(De Silva et al. 2006, circles) andCollinder 261 (De Silva et al. 2007a, squares) open clusters. Thesmaller open symbolsrepresent background fieldstars (Reddy et al. 2003; Allende Prieto et al. 2004; Edvardsson et al. 1993). Thedottedlinesmarkthe solar value.

18. Chemical Tagging • * In old stellar kinematic groups • - Hercules stream (Bensby et al. 2007) which stars show different ages and chemistry • (associated with dynamical resonances (bar) or spiral structure) . • - HR 1614 (De Silva et al. 2007b, 2009) that appears to be a true MG • (debris of star-forming aggregates in the disk). • Wolf 630 (Bubar & King, 2010) confirm the existence of an abundance homogeneous subsample of 19 stars that could represent a dispersed cluster with an [Fe/H] = -0.01 and an age of 2.7 Gyr. • * Very recently in young kinematics groups • - Hyades Supercluster,Pompéia et al. (2011) study a sample of 21 kinematicallyselected stars and De Silva et al. (2011) analyses 26 southern giant candidates. Found 10 % and a 15 % membership respectively .

19. Chemical Tagging Tabernero, Montes, González Hernández Result of our abundance analysis of possible members of the Hyades Super Cluster (Tabernero, Montes, González Hernández, 2012). New high-R observations: (January, May, and November 2010) 1.2 m Mercator Telescope HERMES spectrograph R = 85000. 92 stars were observed. 61single main sequence stars (F6 to K4) have been analyzed. 41% of the ample are homogeneous in abundances for all the elements we have considered, 5 stars fail to be homogeneous in one element.

20. Gaia ESO Spectroscopic Survey (GES) Will start to provide large amount of data • Public large spectroscopic survey with FLAMES@VLT • 300 nights (30n/semester) over 5 (4+1) years; • start 1/2012 (P88), end 9/2016 (P97)+; visitor mode • - Stellar atmospheric parameters (Teff, log g, ξ and [Fe/H]) • Abundance determination. • Different tests with UVES archive spectra already started. • WG1: Cluster Membership Analysis • WG11: UVES FGK-star Spectrum Analyses • WG12: Pre-Main-Sequence Stars Spectrum Analyses  Combined Gaia and homogeneous spectroscopic dataset full 6D phase space f(x,y,z,vx,vy,vz), plus stellar parameters, and chemistry for a very large number and variety of stars down to the 19 mag: core science plus legacy science

21. Gaia ESO Spectroscopic Survey (GES) But additional observations are needed • Only covers selected targets, selected regions on the sky • Only the South sky • Limiting mag. (R): 16.5 (UVES), 19 (Giraffe) • No follow-up new objects

22. Characterization of the CARMENES sample Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs • Characterization of late-type M-dwarfs • (The sample selection for CARMENES) • - possible new CARMENES targets from Lepine & Gaidos 2011 catalog) • CAFOS/2.2m (CAHA) • (G100 – R =1500, 4250-8600 Å) •  Tsp, activity • 5 nights Spanish time: 11-12 y 14 Nov 2011; 7-8 Dic 2011 • 5 nights guarantied (GTO) German time: Jan; Feb; Mar 2012 • proposal submitted 2012b • CAFE/2.2m (CAHA) • (R =60000, 3950-8600 Å) • vsini • proposal submitted 2012b

23. Characterization of the CARMENES sample Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs

24. Characterization of the CARMENES sample Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs Calibrating the metallicity of M dwarfs with wide visual binaries Because binaries are assumed to be both coeval and have the same metallicity, the composition of the higher mass star (which can be accurately derived from comparison to theoretical models) can be applied to the companion M-dwarf. FGK Teff, log g, ξ and [Fe/H] M photometry spec indexes separated by at least 5′′ Previous M-dwarf metallicity calibrations (Bean et al. 2006a; Bonfils et al. 2005; Johnson & Apps 2009; Rojas-Ayala et al. 2010) but with atmospheric parameters and abundances not determined in an uniform way.

25. Characterization of the CARMENES sample Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs • Telescope time needed (spectroscopy): • 2.2m CAFOS: 10 nights 2012A + 14 nights (2012B) +10 nights (2013) = 34 nights • (Tsp, …) • 2.2m CAFE: 14 nights 2012B + 21 nights (2013) = 35 nights • (vsini, activity….) • 2.2m CAFE: 4 nights 2012A (HERMES) + 4 nights (2013) = 8 nights • (met. visual binaries) • 2.2m FEROS: 75 h = 8 nights 2012B + 175 h = 20 nights (2013) = 28 nights • (vsini, activity….) • Total: 105 nights

26. Characterization of the CARMENES sample Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs • Telescope time needed (image): • 1.5m TCS FastCam: 6 nights 2011B, 6 2012A, 6 nights (2012B) = 18 nights • (binarity) • 2.2m Astralux: 10 nights (2013) = 10 nights • (binarity) • Total: 28 nights Total (spec + imag): 105+28 = 133 nights

27. Future long-term projects • Spectroscopic surveys of FGKs to complement the deficits of Gaia: • RV of fainter stars G > 17 • (completion of the 6D phase space) • Atmosph param (Teff, log g, ξ and [Fe/H]), and vsini (G > 12) • (Gaia good Teff limited for log g and [Fe/H]) • Chemical tagging, detailed chemical abundances (G > 11) • (Gaia only very bright stars) • (R = 20000, precision 0.1 – 0.15 dex) • (R > 40000, precision < 0.05 dex)

28. Future long-term projects More spectroscopic observations of FGKs will be needed: • Detailed abundances analysis. • Follow-up of interesting kinematic objects • (determine stellar properties, ages, etc…). • Confirm “isolated” very young star candidates. • Galactic archaeology • (disk population (thin, thick, halo), kinematic structure, etc…)

29. Future Long-term projects Present instruments: High-Res spectrographs (1.2-2-4m tel) 2.2m - CAFE NOT - FIES TNG - HARPS-N Mercator - HERMES Large number of stars & High-Res R > 40000, but only V<10-12

30. Future Long-term projects More spectroscopic observations of FGKs will be needed: • Telescope time needed (for a conservative specific project): • 2.2m CAFE: • 5 nights / semester (2013-2017 next 5 years) = 50 nights • NOT-FIES: • 3 nights / semester (2013-2017 next 5 years) = 30 nights • TNG-HARPS-N: • 3 nights / semester (2013-2017 next 5 years) = 30 nights • Mercator-HERMES: • 3 nights / semester (next 5 years) = 30 nights • Total: 140 nights

31. Future Long-term projects More spectroscopic observations of FGKs will be needed: • Telescope time needed (for a large Gaia support project): • 2.2m CAFE: • 15 nights / semester (2013-2017 next 5 years) = 150 nights • NOT-FIES: • 6 nights / semester (2013-2017 next 5 years) = 60 nights • TNG-HARPS-N: • 6 nights / semester (2013-2017 next 5 years) = 60 nights • Mercator-HERMES: • 4 nights / semester (next 5 years) = 40 nights • Total: 310 nights

32. Future Long-term projects More spectroscopic observations of FGKs will be needed: • Telescope time needed (for a large Gaia support project): • ≈ 300 nights (with < 2-4m telescopes, High-Res but not MOS, V<12) •  only ≈ 5000 stars V < 12 • Compared with 105 stars in the GES • ≈ 300 nights (with 8m tel, Hig-Res, MOS, R: 16.5 (UVES), 19 (Giraffe)) • UVES: 5000 field stars with V < 15 and and 2000 cluster stars down to V<16.5.

33. Future Long-term projects Future instruments: High-Res spectrographs (4m tel) 3.5m - CARMENES Multi-object spectrographs (MOS) WHT - WEAVE GTC - MEGARA GTC - MIRADAS 6 m-CAHA –HEXA Large number of stars & High-Res But only V<16 But R < 20000

34. Future Long-term projects More spectroscopic observations of FGKs will be needed: High-Res spectrographs (10mtel) GTC-HORUS ? • High-Res & faint stars: R = 40 - 80000 Large number of data Large dedicated program Queue observing mode Automatic pipelines North Spectroscopic survey

35. The End