Gaia RVS instrument for the study of stellar populations

Details Gaia RVS instrument for the study of stellar populations Gaia RVS instrument for the study of stellar populations

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011hsa6.conf..777m&link_type=abstract

Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society (SEA), held

Astronomy and Astrophysics

Astrophysics

Scientific paper

Gaia spacecraft will be launched by Spring 2012 and will measure astrometry with unprecedentedaccuracy for a significant 1% of the objects in the Milky Way. Additionally,two spectrophotometers will determine the SEDs of the objects in the region of 0.3 to1 microns, and a radial velocity spectrograph (RVS) will provide spectra in the near IR CaII triplet region with an expected SNR between 100 and 20 for F-G-K stars with visual magnitude between 8 and 15. We have been testing several analysis techniques in order to be prepared to extract all possible astrophysical information from RVS stellar spectra.A combination of data processing in transformed domains (Fourier analysis andWavelet multilevel decomposition) and connectionist systems (Artificial Neural Networks)have proven to be a good approach to derive the fundamental stellar parameters,T_{eff}, log g, [Fe/H], and [alpha/Fe], on the basis of RVS synthetic spectra blurred with noiseat different SNR. Signal processing techniques allowed us to estimate and categorizethe SNR, which in turn is found to be essential since the optimal algorithm for parameterizationis highly dependent on SNR. In the case of low SNR (5-25) spectra, it isfound that the wavelet transform provides a competitive approach for parameterization.The derivation of the stellar parameters is performed by the use of ANNs trained withthe error backpropagation algorithm. The accuracy in the derivation of parameters ispresented for typical galaxy populations.

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