Jonay I. González Hernández (Postdoc, IAC)

Jonay I. González Hernández (Postdoc, IAC)

Hugo M. Tabernero (PhD student, UCM)
David Montes (Staff, UCM)
Jonay I. González Hernández (Postdoc, IAC)
• 
WP10 & WP11:
- Survey started in Dec 2011 (5N per month):
- P88 (3 Runs – 15N)
- P89 (6 Runs – 30N)
- P90 (3/4 observing runs so far – 15N)
- First set of data up to mid-June 2012 analysed
for GES meeting in Potsdam
• 
WP10 & WP11:
- Several presentations were given:
- General status
- UVES: S/N~25, GIRAFFE: S/N~20
- Clusters: S/N~40-60
- We will observe twice MW UVES stars
- Data reduction:
- problems with some setups (520nm and 580nm)
- merging of spectral orders (working with 2D spectra)
- Photometric data to get first-guess stellar parameters
• 
WP10 & WP11:
- Several presentations were given:
- Status of:
- WP12 (Pre-­‐main sequence stars) - WP13 (OBA-­‐type stars) - WP14 (Outliers) - WP5 (Calibration) : Benchmark stars
- Linelists: (LUMBA node)
- Master linelist: including molecular data
- Clean linelist: (atomic data) version 3
• 
WP10 & WP11:
- 1st Data Release:
- First 6 months of the GES survey (P88-89)
- We decided not to do more test but to go for a full
production of the 1st Data Release
- Node presentations
- Next meeting:
- 15th February deadline abstract submission
First Results from the Gaia-­‐ESO Survey: all-­‐hands meeting Nice, France 8-­‐11 April 2013
http://ges2013.sciencesconf.org/
• 
Deriving stellar parameters:
- EW-based method: ARES code (Sousa et al. 2007)
- Line lists from VALD and Sousa et al. (2008)
- Automatic local continuum fitting and EW
determination
- Rejecting lines with wrong fitted FWHM
- Automatic code to derive the stellar parameters
from excitation and ionization equilibria of FeI-II
line strengths
- 2-σ rejection of lines with “wrong” EWs after 1st
iteration (StePar: Tabernero et al. 2012)
¡ 
New linelist using the flag Y/Y and removing lines with EWs > 100
Teff logg [Fe/H] vmicro MRD star Computed 5729 ± 90 4.48 ± 0.08 -­‐0.01 ± 0.08 0.762 ± 0.189 Expected 5779 4.44 0.00 -­‐-­‐ MPD star Computed 5284 ± 95 4.42 ± 0.03 -­‐0.84± 0.08 0.307 ± 0.300 Expected 5308 4.41 -­‐0.89 -­‐-­‐ MPG star Computed 4303 ± 97 1.75 ± 0.07 -­‐0.54 ± 0.06 1.586 ± 0.147 Expected 4247 1.59 -­‐0.54 -­‐-­‐ MRG star Computed 4455 ± 196 2.38 ± 0.09 0.30 ± 0.23 1.159 ± 0.436 Expected 4433 2.50 0.29 -­‐-­‐ ¡ 
New linelist using the flag Y/Y and removing lines with EWs > 100
Teff logg [Fe/H] vmicro MRD star (UVES spectrum) Computed 5729 ± 90 4.48 ± 0.08 -­‐0.01 ± 0.08 0.762 ± 0.189 Expected 5779 4.44 0.00 -­‐-­‐ SUN ATLAS (KURUCZ spectrum) Computed 5737± 87 4.36 ± 0.17 0.02± 0.06 0.61 ± 0.16 Expected 5777 4.44 0.00 -­‐-­‐ SUN ATLAS (KURUCZ spectrum at S/N~30) Computed 5738 ± 109 4.34 ± 0.25 0.09 ± 0.08 0.47 ± 0.27 Expected 5777 4.44 0.00 -­‐-­‐ Fe I and FeII abundances versus excitation potential and reduced equivalent width for the Sun using the solar ATLAS spectrum (Kurucz et al. 1984) and this spectrum degraded at S/N ~ 30. ¡ 
SUN ATLAS FeI
FeII
log( (Fe))
7.8
log( (Fe))
SUN ATLAS (S/N ~30) 8.0
7.6
7.4
7.2
FeI
FeII
7.8
7.6
7.4
7.2
0
1
2
3
(eV)
4
5
0
1
2
3
(eV)
4
5
8.0
log( (FeI))
log( (FeI))
7.8
7.6
7.4
7.2
-6.0
7.8
7.6
7.4
7.2
-5.8
-5.6
-5.4
-5.2
log(EW/ )
-5.0
-4.8
-4.6
-6.0
-5.8
-5.6
-5.4
-5.2
log(EW/ )
-5.0
-4.8
-4.6
¡ 
There are 457 stars for which our code has provided results with S/N > 10 60
50
50
40
40
30
30
20
20
10
10
0
0
4000
5000
6000
7000
1
2
T EFF
80
50
60
40
3
log(g)
4
5
30
40
20
20
10
0
0
-3
-2
-1
[Fe/H]
0
1
0
1
2
3
V MICRO
4
5
400
0.8
300
0.6
log(g)
T EFF
There are 457 stars for which our code has provided results with S/N > 10 200
0.4
0.2
100
0.0
0
50 100 150 200 250 300
S/N
0.30
0.25
0
50 100 150 200 250 300
S/N
0
50 100 150 200 250 300
S/N
1.0
0.8
0.20
V MICRO
[Fe/H]
¡ 
0.15
0.10
0.6
0.4
0.2
0.0
0.05
0.00
0
50 100 150 200 250 300
S/N
There are 457 stars for which our code has provided results with S/N > 10 V MICRO < 0.50
3.0
2.5
3.0
2.5
2.0
2.0
V MICRO
V MICRO
V MICRO < 1.00
1.5
1.0
0.5
0.0
1.5
1.0
0.5
0.0
0
1
2
3
log(g)
4
5
0
1
V MICRO < 0.20
2
3
log(g)
4
5
4
5
V MICRO < 0.15
3.0
2.5
3.0
2.5
2.0
2.0
V MICRO
V MICRO
¡ 
1.5
1.0
0.5
0.0
1.5
1.0
0.5
0.0
0
1
2
3
log(g)
4
5
0
1
2
3
log(g)
There are 457 stars for which our code has provided results with S/N > 10 -1.5 < [Fe/H] < -0.5
0
0
1
1
2
2
log(g)
log(g)
-0.5 < [Fe/H] < +0.5
3
4
5
7000
6000
5000
T EFF [K]
3
4
5
7000
4000
-2.5 < [Fe/H] < -1.5
0
1
1
2
2
3
4
5
7000
6000
5000
T EFF [K]
4000
6000
5000
T EFF [K]
4000
-3.5 < [Fe/H] < -2.5
0
log(g)
log(g)
¡ 
3
4
5
7000
6000
5000
T EFF [K]
4000