We present different aspects of the ground-based observational counterpart of
the CoRoT satellite mission. We give an overview of the selected asteroseismic
targets, the numerous instruments and observatories involved, and the first
scientific results.Comment: 3 pages, 2 tables, 1 figure, to be published in the conference
  proceedings 'Stellar Pulsation: Challenges for Theory and Observation' (31
  May - 5 June, Santa Fe, New Mexico, US), publishers: American Institute of
  Physic

C. Catala

C. Maceroni

C. Neiner

E. Poretti

E. Rodríguez

I. Ribas

Joyce Ann Guzik

K. Pollard

K. Uytterhoeven

L. Balaguer-Nuñez

M. Paparó

M. Rainer

null null

P. Amado

P. Mathias

Paul A. Bradley

R. A. García

S. Martín-Ruiz

English

arXiv

Crossref

The asteroseismic ground-based observational counterpart of CoRoT

International audienceWe present different aspects of the ground-based observational counterpart of the CoRoT satellite mission. We give an overview of the selected asteroseismic targets, the numerous instruments and observatories involved, and the first scientific results

Uytterhoeven, K.

Poretti, Ennio

Mathias, P.

Amado, P.

Rainer, Monica

Martin-Ruiz, Susana

Rodríguez, E.

Paparó, M.

Pollard, Karen R.

Maceroni, Christian

Balaguer-Núñez, L.

Ribas, Ignasi

Catala, Claude

Neiner, Coralie

Garcia, Rafael A.

HAL-INSU

arXiv:0907.3363v1  [astro-ph.SR]  20 Jul 2009The asteroseismic ground-based observational counterpart ofCoRoTK. Uytterhoeven∗,†, E. Poretti†, P. Mathias∗∗,‡, P. Amado§, M. Rainer†,S. Martín-Ruiz§, E. Rodríguez§, M. Paparó¶, K. Pollard‖, C. Maceroni††, L.Balaguer-Nuñez‡‡,§§, I. Ribas§§,¶¶, C. Catala∗∗∗, C. Neiner†††, R.A. García∗ and theCoRoT/SWG Ground-based Observations Working Group‡‡‡∗Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot;CEA, IRFU, SAp, centre de Saclay, 91191,Gif-sur-Yvette, France†INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46,23807 Merate, Italy∗∗UMR 6525 H. Fizeau, UNS, CNRS, OCA, Campus Valrose, 06108 Nice Cedex 2, France‡Observatoire Midi Pyrenees, Laboratoire d’Astrophysique-LATT, 57 Avenue Azereix, 65000 Tarbes, France§Instituto de Astrofísica de Andalucía (CSIC), Apartado 3004, 18080 Granada, Spain¶Konkoly Observatory, P.O. Box 67, 1525 Budapest, Hungary‖Dep. of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand††INAF-Osservatorio Astronomico di Roma, via Frascati-33, Monteporzio Catone, Italy‡‡DAM.Universitat de Barcelona, Diagonal 647, 08028, Barcelona, Spain§§Institut d’Estudis Espacials de Catalunya, c/ Gran Capità 2- 4, 08034 Barcelona, Spain¶¶Institut de Ciències de l’Espai, CSIC, Facultat de Ciències, UAB, 08193 Bellaterra, Spain∗∗∗LESIA, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France†††GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France‡‡‡Abstract. We present different aspects of the ground-based observational counterpart of the CoRoT satellite mission. We givean overview of the selected asteroseismic targets, the numero s instruments and observatories involved, and the first scientificresults.Keywords: asteroseismology, high-resolution spectroscopy, multi-co our photometry, spectropolarimetry, variable starsPACS: 95.75.Fg, 95.75.De, 95.85.Kr, 97.10.Tk, 97.20.Ec, 97.20.Ge, 97.30.Dg, 97.30.EhCOROT’S SIMULTANEOUSGROUND-BASED OBSERVATIONSThe CoRoT/SWG Ground-Based Observations WorkingGroup is undertaking huge efforts to complement theCoRoT space data (e.g. [1]) with simultaneous ground-based data1 to guarantee an optimal scientific outcome ofthe asteroseismic part of the CoRoT mission. Activitiesare strongly focused on selected targets in the seismocore program, but include also the characterisation ofstars in the exoplanet fields.1 Observations are performed at the following observatories: Euro-pean Southern Observatory (ESO), La Silla and Paranal, Chile; Ob-servatoire de Haute Provence (OHP), France; Calar Alto Astronom-ical Observatory (CAHA), Spain; Mount John University Observa-tory (MJUO), New Zealand; Observatorio Roque de los Muchachos(ORM), La Palma, Spain; Konkoly Observatory (KO), Hungary;Ob-servatorio de Sierra Nevada (OSN), Spain; Observatorio SanPedroMártir (OSPM), Mexico; Observatoire du Pic du Midi (OPM), France.The ground-based counterpart of CoRoT’sseismo core programmeSeveral CoRoT asteroseismic targets are selected fora simultaneous follow-up from the ground. Table 1 givesan overview of theδ Sct, γ Dor, β Cep, Be, Ap, andsolar-like stars, eclipsing binaries (EB) and double-linedspectroscopic binaries (SB2) that were observed betweenDecember 2006 and June 2009 (i.e. time of writing) us-ing several high-resolution spectrographs, multi-colourphotometers and/or spectropolarimeters. To ensure anunraveling of the beat frequencies multi-site campaignshave been set up, including several Large Programs. Theinstruments involved are listed in Table 2. The comple-mentary character of each project with respect to theCoRoT space data can be summarised as follows:• High-resolution spectroscopy (Panel A of Table 2):From time-series of high-resolution spectra valu-able information on the mode parameters(ℓ,m) canbe extracted. Figure 1 illustrates the number of spec-tra obtained so far.• Multi-colour photometry (Panel B of Table 2):Time-series of multi-colour observations provideadditional information on the degreeℓ of the modes,that cannot be derived from the CoRoT ’white’lightcurve.• Spectropolarimetry (Panel C of Table 2): By meansof spectropolarimetric measurements, signatures ofmagnetic fields are detected and studied.Characterisation of asteroseismic andbinary targets in CoRoT’s exoplanet fieldsThe CoRoT exoplanet fields reveal a goldmine of newvariable stars. However, the CoRoT lightcurves are notsufficient to characterize them. Therefore the followingobserving programs have been set up (Panel D of Table2):• Multi-Object spectrography: Spectra are obtainedfor many exoplanet field stars simultaneously,which are used to identify the pulsator type and todetermine fundamental stellar parameters.• Wide Field Camera: The complete exoplanet fieldsare observed in the Strömgrenuvby−β filters. Thecolours provide information on the physical param-eters and reddening of the targets.• Multi-colour photometry: Johnson BVRI coloursare observed for selected newly discoveredδ Sctand RR Lyrae variables in the exoplanet fields, tocharacterize the stars and to provide additional in-formation on the degreeℓ of the modes.FIRST SCIENTIFIC RESULTS BASEDON THE OBSERVATIONSFor the first scientific results obtained from the ground-based observations presented here, we refer, e.g., to thefollowing publications:• HD 49434: [2]• HD 180642: [3]• HD 50844: [4]• HD 49330: [5]• HD 50209: [6]• HD 181231: [7]• HD 51106 and HD 50747: [8]• HD 50846 (AU Mon): [9]• Wide Field Camera data: [10]Also, analysis results have been presented at severalconferences, e.g. [11], [12], [13], [14], [15], [16], [17].ACKNOWLEDGMENTSThis work was supported by the italian ESS project, con-tract ASI/INAF I/015/07/0, WP 03170, by the HungarianESA PECS project No 98022 and by the European Helio-and Asteroseismology Network (HELAS), a major inter-national collaboration funded by the European Commis-sion’s Sixth Framework Programme. The FEROS andHARPS data are being obtained as part of the ESO LargeProgrammes LP178.D-0361 and LP182.D-0356. KU ac-knowledges financial support from aEuropean Commu-nity Marie Curie Intra-European Fellowship, contractnumber MEIF-CT-2006-024476. PJA acknowledges fi-nancial support from a Ramon y Cajal contract of theSpanish Ministry of Education and Science.REFERENCES1. A. Baglin, M. Auvergne, P. Barge, et al., inESA SP1306,33 (2006)2. K. Uytterhoeven, P. Mathias, E. Poretti, et al.,A&A 489,2213–1224 (2008a)3. M. Briquet, K. Uytterhoeven, T. Morel, et al.,A&A, inpress (2009) (arXiv:0906.3626)4. E. Poretti, E. Michel, R. Garrido, et al.,A&A, in press(2009) (arXiv:0906.2628)5. M. Floquet, A.-M. Hubert, A.-L. Huat, et al.,A&A, inpress (2009)6. P. D. Diago, J. Gutíerrez-Soto, M. Auvergne, et al.,A&A,in press (2009)7. C. Neiner, J. Gutíerrez-Soto, B. de Batz, et al.,A&A, inpress (2009)8. N. Dolez, S. Vauclair, E. Michel, et al.,A&A, in press(2009)9. M. Desmet, Y. Frémat, F. Baudin, et al.,MNRAS, in press(2009)10. P. Degroote, C. Aerts, M. Ollivier, et al.,A&A, in press(2009) (arXiv:0907.2183)11. K. Uytterhoeven, E. Poretti, M. Rainer, et al.,Journal ofPhysics Conference Series118, 012077 (2008b)12. C. Neiner, J. Gutíerrez-Soto, Y. Frémat, et al.,CoAst157,349-350 (2008)13. J. Gutíerrez-Soto, C. Neiner, A.-M. Hubert, et al.,CoAst157, 70-74 (2008)14. P. Degroote, A. Miglio, J. Debosscher, et al.,CoAst158,167 (2009)15. L. Lefèvre, E. Michel, C. Aerts, et al.,CoAst158, 189(2009)16. M. Briquet, K. Uytterhoeven, T. Morel, et al.,AmericanInstitute of Physics, these proceedings17. E. Poretti, L. Mantegazza, M. Rainer, et al.,AmericanInstitute of Physics, these proceedingsTABLE 1. Overview of the targets, their variable type, and the CoRoT field. The last three columnsindicate if the star is observed spectroscopically (if yes,the amount of spectra is given), photometricallyand/or spectropolarimetrically.Target Type Field # spectra Photom. TBL Target Type Field # spectra Photom. TBLHD 50844 δ Sct IR01 231 yes - HD 50170 solar-like LRa2 - - yesHD 50846 EB IR01 32 - - HD 50870 δ Sct LRa2 209 yes -HD 49330 Be LRa1 127 - yesHD 51452 Be LRa2 145 - yesHD 49933 solar-like LRa1 - yes yesHD 51193 Be LRa2 145 - yesHD 49294 δ Sct LRa1 86 yes - HD 52265 solar-like LRa2 - - yesHD 49434 γ Dor LRa1 1487 yes - HD170987 solar-like LRc2 - - yesHD 50209 Be LRa1 68 - yesHD171586 Ap LRc2 40 - -HD 50747 SB2 LRa1 37 - - HD171834 γ Dor LRc2 1347 yes -HD 50773 Ap LRa1 - - yesHD172189 δ Sct LRc2 176 yes -HD 51106 SB2 LRa1 33 - - HD175726 solar-like LRc2 - - yesHD174936 δ Sct LRc1 - yes - HD181420 solar-like LRc2 - - yesHD174966 δ Sct LRc1 365 yes - HD174532 δ Sct SRc2 329 - -HD180642 β Cep LRc1 248 - - HD 44195 hybrid LRa3 - yes -HD181231 Be LRc1 72 - - HD 44283 δ Sct LRa3 - yes -HD181555 δ Sct LRc1 694 yes - HD170580 β Cep LRc4 98 - -FIGURE 1. Accumulative histograms indicating the number of spectra obt ined (from December 2006 to June 2009) for selectedδ Sct,γ Dor,β Cep, Be and Ap stars with FEROS, SOPHIE, FOCES, HERCULES, HARPS and FIES. The colour code is explainedin the left panel. Note the different scales on the Y-axis forthe different panels. The target names are given above each column.TABLE 2. Observatories, instruments and telescopes involved in theCoRoT ground-based campaign. The characteristics ofthe instruments (e.g. spectral resolution R, photometric filters) are given, as well as the amount of observing time awarded tothe project. In the last column the P.I.s of the observationsare listed.Obs. Instrument Telescope Characteristics # nights per semester/year P.I.A. High-resolution spectrographs:ESO FEROS 2.2m ESO/MPI R∼48,000 2006-2008: 15n per sem. E. PorettiOHP SOPHIE 1.93m R∼70,000 2007-ongoing: 20n per sem. P. MathiasCAHA FOCES 2.2m R∼40,000 2007-ongoing: 10n per sem. P. AmadoESO HARPS 3.6m R∼80,000 2008-2010: 15n per sem. E. PorettiMJUO HERCULES 1.0m McLellen R∼35,000 2007-ongoing: 15-30n per sem. K. PollardORM FIES 2.56m NOT R∼67,000 2009: 4n per sem. K. UytterhoevenORM HERMES 1.2m Mercator R∼85,000 2009: 6n per sem. K. UytterhoevenB. Multi-colour photometers:OSN Danish photometer 0.9m uvby−β 2006-ongoing: 75-100n per yr S. Martín-Ruiz, E. RodríguezOSPM Danish photometer 1.5m uvby−β 2006-ongoing: 18n per yr E. PorettiKO CCD 1m RCC BVRI 2006-ongoing: 14-30n per sem. M. PaparóC. Spectropolarimeter:OPM NARVAL TBL 2007-ongoing: 15n per sem. C. CatalaD. Multi-object spectrograph and (Wide Field) CCD cameras:ESO FLAMES VLT UT2 2008-ongoing:∼3n per sem. C. NeinerORM WFC 2.5m INT uvby−β 2007-ongoing: 2-4n per sem. I. Ribas, C. Maceroni, L. Balaguer, K. UytterhoevenKO CCD 1m RCC telescope BVRI 2008-ongoing: 14-30n per sem. M. Paparó

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The asteroseismic ground-based observational counterpart of CoRoT

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