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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


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