gaia and ground based spectroscopic surveys: science synergies · gaia and ground based...
TRANSCRIPT
Gaia and ground based spectroscopic surveys: science synergies
Alejandra Recio-Blanco Observatoire de la Côte d’Azur (Nice, France)
Outline !
1. Stars as fossils !
2. Observation thresholds in Galactic archaeology (4 levels of information) ! - Data (Gaia and ground-based surveys) !
- Physical properties of the Galaxy
What we would like to know !
- Physical processes of Galaxy evolution
What we would like to understand !
3. Conclusions
1. Stars as fossils
Stars are fossils we can work with: - A star of 0.8Mo leaves more than 13Gyr ! - ages z ≥ 6.
1. Stars as fossils
Fossil information about Galactic (sub)populations: 1. Position and Kinematics:
1. Stars as fossils
Fossil information about Galactic (sub)populations: 2. Chemical composition
Chemical tagging Free parameters of an isolated system: star formation rate, initial mass function, galactic winds…
How to disentangle this fossil record to arrive to this ? !
How to disentangle this fossil record? !
Observational thresholds of Galactic Archaeology and what do they tell us?
First threshold: Positions & magnitudes
1. Data 2. Phy. properties 3. Phy. processes
On the Construction of the Heavens. By William Herschel, Esq. F. R. S. Philosophical Transactions of the Royal Society of London, Vol. 75. (1785), pp. 213-266.
First threshold: Positions & magnitudes
1. Data 2. Phy. properties 3. Phy. processes
VISTA
First threshold: Positions & magnitudes
1. Data 2. Phy. properties 3. Phy. processes
Gaia: Positions, Gmag
First threshold: Positions & magnitudes
1. Data 2. Phy. properties 3. Phy. processes
Gaia: BPRP data
First threshold: Positions & magnitudes
1. Data 2. Phy. properties 3. Phy. processes
- 2D spatial distributions !
- Photometric stellar atmospheric parameters
González et al. (2013) VVV Bulge metallicity distribution
Ivezic et al. (2008) SDSS
First threshold: Positions & magnitudes
1. Data 2. Phy. properties 3. Phy. processes
- 2D spatial distributions !
- Photometrical stellar atmospheric parameters
Bailer-Jones et al. (2013) Gaia BPRP based expected parameter accuracies !Down to G~19
First threshold: Positions & magnitudes
1. Data 2. Phy. properties 3. Phy. processes
- 2D spatial distributions !
- Photometrical stellar atmospheric parameters
Bailer-Jones et al. (2013) Gaia BPRP based expected parameter accuracies !Down to G~19
First threshold: Positions & magnitudes
1. Data 2. Phy. properties 3. Phy. processes
- Recent accretions (streams)Belokurov et al. (2006) Ivezic et al. (2008)
2nd threshold:Distances & propermotions
1. Data 2. Phy. properties 3. Phy. processes
- Parallaxes (distances) - Proper motions
Credits François Mignard
Gaia huge step forward
2nd threshold:Distances & propermotions
1. Data 2. Phy. properties 3. Phy. processes
HR diagrams
Baade, 1944
2nd threshold:Distances & propermotions
1. Data 2. Phy. properties 3. Phy. processes
3D distributions
Hyades in 3D Credits Anthony Brown
2nd threshold:Distances & propermotions
1. Data 2. Phy. properties 3. Phy. processes
- Stellar cluster’s studies (membership) !
- Disc evolution processes (photometric metallicity gradients): migration, disc heating by mergers,… !
- Stellar structure and evolution models
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
- Radial velocities - Spectroscopic stellar parameters - Individual element abundances
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
- Stellar parameters, chemical compositions - 3D kinematics - Dynamics (orbits) !
Chemo-dynamical constraints to models
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
Gaia: Apsis pipeline - GSPspec (Bailer-Jones et al. 2013) (Recio-Blanco et al. 2014b, sub.)
Credits O. Marchal & D. Katz
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processesGaia GSPspec performances (Recio-Blanco et al. 2014b, sub.)
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processesGaia GSPspec performances (Recio-Blanco et al. 2014b, sub.)
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
G-type dwarfs
early-type stars
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
Late-type stars - Errors in metallicity lower than ~0.1 dex for
G_RVS < 12-13 - Good recovery of the [alpha/Fe] - Performances degrade for fainter stars but still
good parametrization ! Early-type stars
- Very good results down to GRVS ~ 13 - Very good log g recovery thanks to Paschen lines
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes - Stellar parameters, chemical compositions
Gaia: GSPspec (Recio-Blanco et al. 2014b, sub.)
- Important contribution for bright stars (added scientific value on Teff (->ages), metallicity and individual abundances
!
- Help to GSPphot parametrization on Teff-extiction degeneracy
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
GES: VLT/Giraffe spectra (performances) Recio-Blanco & GES consortium, in prep.
3nd threshold: Spectroscopy
1. Data 2. Phy. properties 3. Phy. processes
GES: Thin to thick disc transition Recio-Blanco et al. 2014
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Recio-Blanco et al. 2014
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition ESO FEROS+HARPS archive homogeneous analysis
AMBRE project (P.I. de Laverny)
8105 stars solar neighborhood
Mikolaitis+ in prep.
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Recio-Blanco et al. 2014
The thick disc seems to lie in thinner and thinner layers as metallicity increases.!
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Guiglion et al. 2014, in prep.
Detailed study of disc rotational velocity
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Guiglion et al. 2014, in prep.
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Guiglion et al. 2014, in prep.
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Guiglion et al. 2014, in prep.
Minchev+ 2014
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Recio-Blanco et al. 2014
The eccentricity distribution of the thick disc peaks at higher values than the thin disc one
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Recio-Blanco et al. 2014
Metallicity dependence of eccentricity : thick disc -> yes thin disc -> no !
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Thin to thick disc transition Recio-Blanco et al. 2014
Metallicity dependence of eccentricity : thick disc -> yes thin disc -> no !But need of more accurate distances for dynamics !!
Gaia accurate distances needed
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Metallicity gradients in the disc Mikolaitis et al. 2014
Mikolaitis et al. 2014
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Metallicity gradients in the disc Mikolaitis et al. 2014
Mikolaitis et al. 2014
1. Data 2. Phy. properties 3. Phy. processes
3nd threshold: Spectroscopy
GES: Metallicity gradients in the disc
Mikolaitis et al. 2014
1. Data 2. Phy. properties 3. Phy. processes
4th threshold: Ages
Gaia revolution with important synergies with ground-based data
Direct constraints on the time-evolving chemo-dynamical picture of the Milky Way
Conclusions
- Gaia will induce a strong quantitative and qualitative change:
* completeness * spatial distributions, kinematics * [Fe/H] and [alpha/Fe] (bright part) * dynamics ! * ages !! !
- Ground-based spectroscopic surveys : * complete chemical information in the Gaia sphere of accurate ages * Vrad and chemical information for fainter stars
Conclusions
- Future ground-based surveys (eg. 4MOST, WEAVE…) covering the halo will complete the present ones.
!
- IR surveys as APOGEE (I&II) important to cover the bulge.
Available positions at the Observatoire de la Côte d’Azur (Nice, France) !
1) Post-doc for 2 years 2) Phd grant !
Starting date ~ 1st October 2015 !Deadline: 1st February 2015