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The CoRoT ground-based complementary archive

The CoRoT ground-based complementary archive. Monica Rainer, Ennio Poretti M. Rosa Panzera, Angelo Mistò INAF OABrera. M. Rainer acknowledges support from the SPACEINN grant entitled ” Exploitation of the HARPS-ESO spectra collected in the CoRoT ground based activities ”.

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The CoRoT ground-based complementary archive

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  1. The CoRoTground-based complementaryarchive Monica Rainer, Ennio Poretti M. Rosa Panzera, Angelo Mistò INAF OABrera M. Raineracknowledgessupportfrom the SPACEINN grantentitled ”Exploitationof the HARPS-ESO spectracollected in the CoRoTgroundbasedactivities”

  2. The CoRoT ground-based complementary archive A large ground-based high-resolution spectroscopic campaign has been performed from the launch of the CoRoT satellite (27th December 2006) up to January 2013. The spectroscopy complements the photometric CoRoT observations of asteroseismic targets. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  3. Ground-based spectroscopy P.I. Ennio Poretti FEROS@2.2m ESO-LaSilla HARPS@3.6m ESO-LaSilla P.I. Philippe Mathias SOPHIE@1.9m OHP P.I. Pedro Amado FOCES@2.2m Calar Alto P.I. KatrienUytterhoeven FIES@NOT ORM P.I. ConnyAerts HERMES@MERCATOR ORM CORALIE@1.2m ESO-LaSilla P.I. Karen Pollard HERCULES@1m Mt. John Obs. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  4. Main studies Most of the spectra are already been used for dedicated studies. This large dataset of variable objects can still be exploited either for more detailed single studies or for statistical and comparative analysis. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  5. HARPS spectra For now we will build our archive using only the HARPS spectra, that are homogenoeusly reduced and normalised. 7150 spectra 269 objects Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  6. The ESO archive The HARPS spectra are already stored in the ESO archive, where both the raw data and the spectra reduced by the HARPS pipeline at the telescope can be found. We have reduced the spectra with a different method, using a semi-automated pipeline developed at the Brera Observatory. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  7. Reduced HARPS spectra Automated pipeline result Our pipeline result Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  8. Normalised HARPS spectra All the HARPS spectra have been normalised in an automated way. The normalisation procedure has some problems with the first orders, but it is averall quite good. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  9. Physical parameters The already normalised spectra are very useful in the determination of the stellar physical parameters. HD 50870 Mantegazza et al., 2012, A&A 542, 24 Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  10. Format of the spectra • 5-columns ASCII files with wavelength, reduced flux, normalised flux, signal-to-noise error and number of the echelle order. • 2-columns ASCII files with wavelength and normalised flux. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  11. The SPACEINN archive Other than the reduced spectra, the goal of our SPACEINN archive is to provide many additional information, concerning both the targets and the single spectra. The objects will be categorised by the variability class and, if possible, information about the time series will be given. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  12. Mean line profiles The mean line profile of each spectrum will be computed and uploaded in the archive. The profiles are obtained using the LSD technique (Donati et al., 1997, MNRAS 291, 658) on a sub-region of the normalised, non-merged spectra. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  13. Mean line profiles The mean line profile fo each spectrum will be computed and uploaded in the archive. The profiles are obtained using the LSD technique (Donati et al., 1997, MNRAS 291, 658) on a sub-region of the normalised, non-merged spectra. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  14. Mean line profiles The high signal-to-noise ratio of the mean line profiles enables a more sensitive study of the line profile variations. HR 6139 Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  15. Pulsating binary systems Creevey et al., 2009, A&A 507 901 Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  16. Multiple systems HD 170200 Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  17. Variable classes In the SPACEINN archive the stars will be characterized by their variable class, in order to enable statistical analysis of objects of the same kinds. Some information on the most peculiar characteristic of the variable will be given. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  18. Be stars HD 49330 Floquet et al., 2009, A&A 506, 103 In the case of the Be stars, we would like to give some information on the strength and symmetry of the H-alpha emission. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  19. δ Scuti stars Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  20. δ Scuti stars Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  21. Activity index It is possible to compute an activity index from the CaII H and K lines to be stored in the SPACEINN archive. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  22. The files • For each observed spectrum, the archive will contain three different FITS files, with VO-compliant headers: • a 5-field table with wavelength, reduced flux, normalised flux, signal-to-noise ratio and echelle order; • a 2-field table with wavelength and normalised flux, where the echelle orders have been merged; • a 2-field table (velocity and normalised flux) storing the mean line profile computed using the LSD software. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  23. Information on the object • Looking for a variable class will return a list of objects with their physical parameters, such as: • effective temperature, logg, metallicity; • binarity flag (none, SB1, SB2) • spectral type • information on the pulsational content of the time series, if more than a few spectra are present in the archive. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  24. Information on the spectrum • Looking for an object will return a list of spectra with some characterizing information such as: • date of the observation, HARPS mode; • signal-to-noise ratio at a predefined wavelength; • radial velocity and vsini; • activity index, emission index (Be), tbd. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  25. Other capabilities The user should be able to plot the spectra and the mean line profiles and zoom them. We would like to offer the possibility of either plotting or downloading radial velocity curves and other relevant quantities. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  26. Study example We hope that this archive will be useful for comparative or statistical studies. The spectra are already being used in this way, but the web interface will allow much easier access. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  27. Milestones • T0 + 12 • Availability of the reduced spectra with full indicators • T0 + 18 • Availability of simultaneous photometric and • spectroscopic curves • T0 + 24 • Definition of the query interface • T0 + 30 • Opening to the community Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  28. Conclusion: what we have • The reduced data and large part of the mean line profiles. • An estimate of the physical paramenters for many objects, but we would like to complete the work on the whole database. • Reliable HARPS radial velocities for the objects observed in HAM mode (R = 115,000), but we will need to compute them for the ones observed in the EGGS mode (R = 80,000). • Binarity flags for most of the objects. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

  29. Conclusion: work to do • Complete the previous work. • Calibrate a reliable activity index. • Determine ad hoc information on the time series in order to give an hint on the pulsational content (i.e., the standard deviation of the mean line profiles from the average mean line profile). • Defining the archive interface and the kind of output given. Monica Rainer – The CoRoT ground-based complementary archive – 21 October 2013

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