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Survey for the Binary Progenitor in SN1006 and Update on SN1572

Published online by Cambridge University Press:  17 January 2013

Pilar Ruiz–Lapuente ,
Jonay González Hernández ,
Hugo Tabernero ,
David Montes ,
Ramon Canal ,
Javier Mendez  and
Luigi Bedin
Pilar Ruiz–Lapuente
Affiliation:
Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Martí i Franqués 1, E-08028 Barcelona, Spain. email: pilar@am.ub.es Max–Planck Institut für Astrophysik, Karl–Schwarzschild-Strasse 1, 85748 Garching, Germany
Jonay González Hernández
Affiliation:
Instituto de Astrofísica de Canarias, c/. Vía Láctea, s/n, E-38200 La Laguna, Spain email: jonay@iac.es
Hugo Tabernero
Affiliation:
Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
David Montes
Affiliation:
Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain
Ramon Canal
Affiliation:
Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Martí i Franqués 1, E-08028 Barcelona, Spain. email: pilar@am.ub.es
Javier Mendez
Affiliation:
Isaac Newton Group, PO Box 321, Santa Cruz de La Palma, Tenerife, Canary Islands, E-38780, Spain
Luigi Bedin
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
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Abstract

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We have completed a survey down to R = 15 mag of the stars within a circle of 4 arcmin radius around the nominal center of the remnant of SN 1006, one of the three historical Type Ia supernovae (the other two being SN 1572 and SN 1604), in search of a possible surviving binary companion of the white dwarf whose explosion gave rise to the supernova. The stellar parameters (effective temperature, surface gravity, and metallicity), as well as the radial velocities of all the stars, have been measured from spectra obtained with the UVES spectrograph at the VLT, and from the former and the available photometry, distances have been determined. Chemical abundances of the Fe-peak elements Cr, Mn, Co, and Ni have also been measured to check for possible contamination of the stellar surface by the supernova ejecta. The limiting magnitude of the survey would allow us to find stellar companions of the red-giant type, subgiant stars, and main–sequence stars down to F5–6. Unlike in SN 1572, where a subgiant of type G0–1 has been proposed as the companion of SN 1572, for SN 1006 we can discard the possibility that SN 1006 had a red giant or subgiant companion.

Keywords

stars: abundancessupernovae — supernova remnants
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 322 - 325
Copyright
Copyright © International Astronomical Union 2013

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