Matthias Steinmetz. 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 1

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1 Matthias Steinmetz 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 1

2 The RAVE Survey Spectroscopic high latitude survey of the MW 9 < I < 13 GAIA spectral range and resolution Ca triplet region ( Å), Reff=7500 6dF at the 1.2m UKST in Australia fibres 38 sqdeg FoV Scheduled operation: nights per lunation up to 8/ nights per lunation since 8/ spectra (Aug 2012) 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 2

3 Radial Velocities: DR4 Internal errors Number per 0.2 km s 1 bin Cum. Frac DR1 DR2 DR3 DR4/ rv (km s 1 ) 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 3

4 : current status 2003/04/11 to 2005/04/02 Aug 2012: 560,000 Spectra 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 4

5 Trends with S/N DR3 140 DR4 120 SNR (Kordopatis) DR calibrated [M/H] (kordopatis) 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 5

6 RAVE DR4 stellar parameters 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 6

7 Chemical abundances with λ range: Å (Gaia wavelength range) Resolution R=7500 at 8600Å; Dispersion = 0.4Å/pix From the RAVE spectra we obtain: radial velocities stellar parameters (effective temperature, gravity and metallicity) chemical abundances 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 7

8 DR4 stellar parameters 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 8

9 Going 6D: Distances of RAVE stars Fit Y 2 -isochrones to RAVE data/ deduced stellar parameters + J- K colors J-Magnitude Error in J-Magnitude Check by Monte-Carlo sampling Result: 1/7 better 25% 1/3 better 37.5% 2/3 better 50% Breddels et al, 2009 Zwitter et al, 2010 Burnett et al, Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 9

10 Verification for stars with Hipparcos distances Breddels et al, Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 10

11 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 11

12 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 12

13 Comparison of RV-surveys 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 13

14 Kinematics vs Chemistry of thin disk, thick disk and halo [α/fe] [α/fe] [α/fe] thin disk thick disk halo [Fe/H] highest quality Rave Spectra (S/N >80) giants (1.0 < log g < 3.5); 4000 < T eff (K) < 5500 best chemical elements Fe, Mg other 5 elements available Boeche et al., 2012 for the ompo- 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 14 Fig. 10. As in Figure 9 but for the abundance ratio [α/fe] now as function of [Fe/H]. This figure correspond to Figure 3 of G03.

15 Kinematics vs Chemistry of thin disk, thick disk and halo Z max [α/fe] [α/fe] [α/fe] N= 122 (g) N= 262 (h) N= 195 (i) N= 641 (d) N= 879 (e) N= 367 (f) N= 3453 (a) N= 1575 (b) N= 311 (c) [Fe/H] e = Boeche et al., Oct 2012 Science from 0.3 N= 122 the Next Generation (g) N= 262 Imaging and (h) N= 195 Spectroscopic Surveys (i) [Fe/H] [Fe/H] Ntot

16 Dissecting the Milky Way <V φ > (km s 1 ) <σ(v φ )> (km s 1 ) Z (kpc) 0 Z (kpc) R (kpc) R (kpc) Williams et al., Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 16

17 Radial velocity gradient in the extended SN (Siebert et al 2011) <V R > (km s 1 ) Q1 Q2 Y (kpc) 0 1 Q X (kpc) Assume R 0 = 7.8 kpc, v c0 = V LSR = 247 km/s, U LSR = 0 km/s (U,V,W) = (11,12,7) km/s 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 17 Q3

18 <V R > (km s 1 ) Z (kpc) R (kpc) 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 18

19 Velocity Substructure in RAVE Williams et al, Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 19

20 Wylie-deBoer et al 2012: 6 Aquarius stars: -1.28<[Fe/H]<0.98 deboer et al., Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 20

21 Follow-up Spectroscopy (Wylie-deBoer et al, 2012) [Na/Fe] [Ni/Fe] 0.0!0.2!0.2!0.4!0.4!0.6!1.0! [O/Fe]!1.0!0.8!0.6!0.4! [Na/Fe] Aquarius stream stars globular clusters field stars dsph stars 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 21

22 Local sample, RAVE vs GCS Wavelet analysis via a trous algorithm (Starck & Murthag, 2002) 1: Coma Berenice; 2: Hyades; 3: Sirius; 4: Pleiades; 6: Hercules Antoja et al., Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 22

23 Non-local samples first non-local detection of moving groups local kinematic groups are large scale features 1kpc from the Sun in R 0.7kpc below the plane Known groups are shifted in velocity (e.g. 4.) Dynamical/resonant origin 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 23

24 Summary RAVE survey: more than 500,000 spectra taken Radial velocities (1km/s) Stellar parameters Distances Abundances Kinematical Tomography of the galactic disks Substructure and tidal debris can be found in the galactic disks (Aquarius) Detection of large-scale non-axisymmetry of the velocity field in the solar neighborhood Apparent asymmetry above vs below the plane 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 24