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--- work:wp6 [2015/03/13 12:54] – jcsuarez
+++ work:wp6 [2015/03/30 13:43] (current) – persia
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+==== WP6. Spectroscopic analysis ====
+^Responsible: INAF |
+|Ennio Poretti |
+The space mission CoRoT and Kepler observed hundreds of A-F type stars locate
+inside the instability strip. Spectroscopic campaigns in the framework\\
+of three ESO Large Programmes (LPs)  were performed and some papers were published (see below). \\
+They discuss in details the comparison between the models and the results from spectroscopic\\
+mode identification. This task was very difficult due to the extreme complexity\\
+of the pulsational content and a full comprehension of the rotational effects.\\
+As a final output, the most powerful results were obtained on stars with a \\
+clear frequency pattern only.\\
+\\
+The HARPS spectra  of A-F stars are now included in the spectroscopic\\
+archive built in the context of the FP7-Space SpaceInn project. The spectra\\
+are fully reduced in terms of careful determination of the physical parameters,\\
+rotational velocities, and mean line-profiles. No extra work is foreseen on the \\
+determination of these quantities. The goal of the SpaceInn archive is to make\\
+the spectra available to the community for a deep analysis in function of \\
+the spectral class and/or variability type. This is what we intend to perform in \\
+the PERSIA project for A-F stars. Unexploited  \\
+spectra are available on HD 181555, HD 172189, HD 171834, HD 174532, HD 44195, \\
+HD 170699, HD 43338, and HD 170133. The spectra of \\
+HD 49434 (Uytterhoeven et al. 2008, A&A 489, 1213), \\
+HD 50844 (Poretti et al.  2009, A&A 506, 85), \\
+HD 174936 (Garcia Hernandez et al. 2009, A&A 506, 79),\\
+HD 50870 (Mantegazza et al. 2012, A&A 542, A24), \\
+HD 174966 (Garcia Hernandez et al. 2013, A&A 559, A63),\\
+HD 51844 (Hareter et al. 2014, A&A 567, 124), and \\
+HD 144277 (Zwintz et al. 2014, A&A 567, A4) \\
+are also available for this kind of new  analysis.\\
+\\
+When developing the tools of a more detailed \\
+comprehension of the rotational effects the INAF team will go back to the spectra and \\
+compare predictions with observations in order to test we are going in the\\
+right direction. These kind of tests  will be performed by means of   \\
+codes supplied by other partners and existing software (e.g., FAMIAS). This will give us \\
+back  tighter constraints on the models, in a sort of virtuous circle. \\
+\\
+Without the efforts programmed in the PERSIA project the pulsational\\
+content of A-F stars will still remain not understood and this will have a \\
+negative feedback in future missions, PLATO in particular. This should be\\
+a frustrating insuccess for the asteroseismology technique, especially if\\
+considering the large spectroscopic database available and the richness of\\
+physical information contained in the line-profile variations.\\
+For instance the age determination will remain limited to the lower part of the \\
+Main Sequence, leaving the datation of the exoplanetary systems\\
+around A-F stars an inaccurate technique.
+=== Tasks  (TBD) ===
+    * Proposals, observations, data reduction
+    * …TBD
+=== Deliverables ===
+    * Particular spectroscopic time series of interest for theoretical models
+    * Partial mode identification for a small set of stars
+    * …TBD
+\\