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

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

Collaborators Dpto. Astrofísica, F. Físicas

Universidad Complutense de Madrid, UCM

David Montes, Alexis Klutsch, Hugo M. Tabernero,F. Javier Alonso-Floriano,M. Cortés-Contreras,

Raquel M. Martínez-Arnáiz,Javier López-Santiago.

Universidad Autónoma de Madrid, UAM

CAB (Centro de Astrobiologia) Madrid

Carlos Eiroa,Jesús Maldonado.

Benjamín Montesinos, and DUNES team.

Observatoire Astronomique,

Université de Strasbourg

Osservatorio Astrofisico di Catania

Patrick Guillout, Rubens Freire Ferrero, F.-X. Pineau, N. Grosso,Antonio Frasca, Ettore Marilli.

CAB (Centro de Astrobiologia) Madrid José Antonio Caballero.

IAC (Instituto de Astrofísica de Canarias) Jonay I. González Hernández.

http://www.ucm.es/info/ucmp/

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

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)

ORM: CAHA:

Intermediate-resolution spectroscopyIntermediate-resolution optical and NIR spectrographs R < 20000 (> 0.3 Å) – future

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)

6 m - HEXA(an instrument for spectroscopic surveys)

ORM: CAHA:

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


7


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

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).

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

Spectroscopic Analysis

• Kinematics (U, V, W).

• Radial velocity (Vr) • Age (LiI 6707.8Å).

• Chromospheric activity

• CaII H&K to CaII IRT

• Rotation (vseni).• Activity – rotación relation

• Absolute and differential abudances.• Chemical tagging

• Stellar parameters.• T

eff, log g, ξ and [Fe/H]

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 χ vs 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.

Fe, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, and Ni

- EW method in a line-by-line basis with ARES code (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.

Chemical abundances Fe, Na, Mg …..

[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).

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 Fe abundance results. In this subsample another 1-rms diagnostic has been applied in order to prove homogeneity in each element.

Differential abundances Δ[X/H]

Stellar Kinematics Groups

Montes et al. 2001 MNRAS.328...45

• Moving group (Supercluster) Eggen (1994)

Group of stars gravitationally unbound that share the same kinematics and may occupy extended regions in the Galaxy

Stellar Kinematics Groups

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).

Chemical TaggingThe 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) sowing the abundances of HR1614 MG stars (De Silva et al. 2007b, triangles) compared to the Hyades (De Silva et al. 2006, circles) and Collinder 261 (De Silva et al. 2007a, squares) open clusters. The smaller open symbols represent background field stars (Reddy et al. 2003; Allende Prieto et al. 2004; Edvardsson et al. 1993). The dotted lines mark the solar value.

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 kinematically selected stars and De Silva et al. (2011) analyses 26 southern giant candidates. Found 10 % and a 15 % membership respectively .

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. 61 single 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.

Gaia ESO Spectroscopic Survey (GES)

• 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

Will start to provide large amount of dataWill start to provide large amount of data

Gaia ESO Spectroscopic Survey (GES)

But additional observations are neededBut 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

Characterization of the CARMENES sample

• 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

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 binariesBecause 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.

FGKT

eff, 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.



• 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



• 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

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 T

eff 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)

Future long-term projects

More spectroscopic observations of FGKs will be needed:

Future long-term projects

• 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…)

Present instruments:

Large number of stars&

High-Res


High-Res

R > 40000, but only V<10-12

Future Long-term projects



• 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



• 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



• 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.

Future instruments:


High-Res


High-Res


But R < 20000

But only V<16


High-Res & faint stars: High-Res & faint stars:

R = 40 - 80000

Large number of dataLarge number of data

North Spectroscopic survey


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

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