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

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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
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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 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.
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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-MUSIC
OS (MUlti SIte COntinuous Spectroscopy)
NOT-SOFIN (SOviet FINish spectrograph)
NOT-FIES (FIber fed Echelle Spectrograph) TNG-S
ARG (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)
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Intermediate-resolution spectroscopy
Intermediate-resolution optical and NIR
spectrographs R lt 20000 (gt 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)
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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

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2.2m-FOCES, (until 2009), (Fibre Optics
Cassegrain Echelle Spectrograph)
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2.2m-FOCES, (until 2009), (Fibre Optics
Cassegrain Echelle Spectrograph)
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Survey of FGK stars in MGs
? Survey late-type stars in Moving Groups
(MGs) 1999- 2002 - 144 FGKM stars - Montes et
al. 2001, AA, 379, 976 - López-Santiago et al.
2005, PhD Thesis UCM 2006, ApJ, 643, 1160
2009, AA, 499, 129 2010, AA, 514, A97
http//www.ucm.es/info/Astrof/invest/actividad/skg
/skg_SS.html
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Survey Nearby FGK stars
? Survey of FGK stars in the solar neighbourhood
(d lt 25 pc), including the DUNES sample 2005-
2009 450 FGKM stars - Martínez-Arnáiz et al.
2010, AA, 520, A79 2011, MNRAS, 414, 2629,
2011, PhD Thesis UCM - Maldonado et al. 2010,
AA, 521, A12
FGK stars in the solar neighbourhood (d lt 25 pc)
which include the DUNES sample, an approved
Herschel OTKP with the aim of detecting cool
faint dusty disks (Eiroa et al. 2010).
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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

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Spectroscopic Analysis

• Kinematics (U, V, W).
• Radial velocity (Vr)

• Age (LiI 6707.8Å).

• Chromospheric activity
• CaII HK to CaII IRT

• Rotation (vseni).
• Activity rotación relation

• Stellar parameters.
• Teff, log g, ? and Fe/H

• Absolute and differential abudances.
• Chemical tagging

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Stellar parameters
Teff, log g, ? and Fe/H

• Stellar atmospheric parameters (Teff, log g, ?
  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 ? vs log(?(Fe I))
• and log(EW/?) vs log(?(Fe I)) where zero
• - ionization equilibrium
• log(?(Fe I)) log(?(Fe II)).
• - 2-s rejection of Fe I and Fe II lines after a
  first determination of the parameters

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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).
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Differential abundances
?X/H

• Differential abundances ?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.

?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.
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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
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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).

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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.
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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 .

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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.
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Gaia ESO Spectroscopic Survey (GES)
Will start to provide large amount of data

• Public large spectroscopic survey with
  FLAMES_at_VLT
• 300 nights (30n/semester) over 5 (41) years
• start 1/2012 (P88), end 9/2016 (P97) visitor
  mode
• - Stellar atmospheric parameters (Teff, log g, ?
  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
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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

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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

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

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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) 10528 133 nights
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Future long-term projects

• Spectroscopic surveys of FGKs to complement the
  deficits of Gaia
• RV of fainter stars G gt 17
• (completion of the 6D phase space)
• Atmosph param (Teff, log g, ? and Fe/H), and
  vsini (G gt 12)
• (Gaia good Teff limited for log g and Fe/H)
• Chemical tagging, detailed chemical abundances
  (G gt 11)
• (Gaia only very bright stars)
• (R 20000, precision 0.1 0.15 dex)
• (R gt 40000, precision lt 0.05 dex)

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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)

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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 gt 40000, but only Vlt10-12
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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

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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

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Future Long-term projects
More spectroscopic observations of FGKs will be
needed

• Telescope time needed (for a large Gaia support
  project)
• 300 nights (with lt 2-4m telescopes, High-Res
  but not MOS, Vlt12)
• ? only 5000 stars V lt 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 lt 15 and and 2000
  cluster stars down to Vlt16.5.

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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 Vlt16
But R lt 20000
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Future Long-term projects
More spectroscopic observations of FGKs will be
needed
High-Res spectrographs (10m tel) GTC-HORUS ?
High-Res faint stars
R 40 - 80000
Large number of data
Large dedicated program Queue observing
mode Automatic pipelines
North Spectroscopic survey
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The End