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.
CAB (Centro de Astrobiologia) Madrid
José Antonio Caballero.
IAC (Instituto de Astrofísica de Canarias)
Jonay I. González Hernández.
Universidad Autónoma de Madrid, UAM
Carlos Eiroa,
Jesús Maldonado.
CAB (Centro de Astrobiologia) Madrid
Observatoire Astronomique,
Université de Strasbourg
Osservatorio Astrofisico di Catania
Benjamín Montesinos,
and DUNES team.
Patrick Guillout,
Rubens Freire Ferrero,
F.-X. Pineau,
N. Grosso,
Antonio Frasca,
Ettore Marilli.
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
ORM:
WHT-UES
(Utrecht Echelle Spectrograph)
INT-MUSICOS
(MUlti SIte COntinuous Spectroscopy)
CAHA:
2.2m-FOCES, (until 2009),
(Fibre Optics Cassegrain Echelle Spectrograph)
NOT-SOFIN
2.2m-CAFE, (2011- )
(SOviet FINish spectrograph)
(Calar Alto Fiber-fed Echelle 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
3.5m-CARMENES (2014 - )
(Calar Alto high-Resolution search for M dwarfs with
Exoearths with Near-infrared and optical Échelle
Spectrographs)
Intermediate-resolution spectroscopy
Intermediate-resolution optical and NIR spectrographs
R < 20000 (> 0.3 Å) – future
ORM:
CAHA:
WHT- WEAVE
(wide-field multi-object spectrograph)
6 m - HEXA
(an instrument for spectroscopic surveys)
GTC - MEGARA
(Multi-Espectrógrafo en GTC de Alta
Resolución para Astronomía)
GTC - MIRADAS
(Mid-resolution InfRAreD Astronomical
Spectrograph)
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 –
• Survey of late-type (F-M) stars in MGs –
1997 – 1999
1999 - 2002
• Survey of FGK in the solar neighbourhood (DUNES) – 2005-2009
2.2m-FOCES, (until 2009),
(Fibre Optics Cassegrain Echelle Spectrograph)
6
2.2m-FOCES, (until 2009),
(Fibre Optics Cassegrain Echelle Spectrograph)
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 –
• Searching “isolated” very young star –
2009 -
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
• Stellar parameters.
• Teff, log g, ξ and [Fe/H]
• Absolute and differential abudances.
• Chemical tagging
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.
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 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.
[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]
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.
Δ[Fe/H] differential abundance vs Teff. 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.
Stellar Kinematics Groups
• 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
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 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) 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)
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
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
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
Characterization of the CARMENES sample
Calar Alto high-Resolution search for M dwarfs with Exoearths
with Near-infrared and optical Échelle Spectrographs
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
separated by at least 5′′
photometry
spec indexes
Previous M-dwarf metallicity calibrations (Bean et al. 2006a; Bonfils et al. 2005; Johnson & Apps 2009; RojasAyala et al. 2010) but with atmospheric parameters and abundances not determined in an uniform way.
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
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
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)
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…)
Future Long-term projects
Present instruments:
Large number of stars
&
High-Res
R > 40000, but only V<10-12
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
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
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.
Future Long-term projects
Future instruments:
Large number of stars
&
High-Res
But only V<16
But R < 20000
Future Long-term projects
More spectroscopic observations of FGKs will be needed:
High-Res & faint stars:
R = 40 - 80000
Large number of data
North Spectroscopic survey
The End