A method to deconvolve mass ratio distribution of binary stars
Aims. It is important to know the binary mass-ratio distribution to better understand the evolution of stars in binary systems and to constrain their formation. However, in most cases, that is, for single-lined spectroscopic binaries, the mass ratio cannot be measured directly, but can only be deriv...
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| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_00046361_v573_n_p_Cure |
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todo:paper_00046361_v573_n_p_Cure2023-10-03T14:00:52Z A method to deconvolve mass ratio distribution of binary stars Curé, M. Rial, D.F. Cassetti, J. Christen, A. Boffin, H.M.J. Binaries: general Methods: analytical Methods: data analysis Methods: numerical Methods: statistical Stars: fundamental parameters Distribution functions Inverse problems Stars Systems (metallurgical) Binaries: general Methods: numericals Methods:analytical Methods:data analysis Methods:statistical Stars:fundamental parameters Numerical methods Aims. It is important to know the binary mass-ratio distribution to better understand the evolution of stars in binary systems and to constrain their formation. However, in most cases, that is, for single-lined spectroscopic binaries, the mass ratio cannot be measured directly, but can only be derived as the convolution of a function that depends on the mass ratio and on the unknown inclination angle of the orbit on the plane of the sky. Methods. We extend our previous method for deconvolving this inverse problem by obtaining the cumulative distribution function (CDF) for the mass-ratio distribution as an integral. Results. After a suitable transformation of variables, this problem becomes the same as the problem of rotational velocities vsini, allowing a close analytic formulation for the CDF. We here apply our method to two real datasets: a sample of Am star binary systems, and a sample of massive spectroscopic binaries in the Cyg OB2 association. Conclusions. We are able to reproduce previous results for the sample of Am stars. In addition, the mass-ratio distribution of massive stars shows an excess of systems with a low mass ratio, in contrast to what was claimed elsewhere. Our method proves to be very reliable and deconvolves the distribution from a sample in one single step. © 2014 ESO. Fil:Rial, D.F. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v573_n_p_Cure |
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Universidad de Buenos Aires |
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I-28 |
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R-134 |
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Binaries: general Methods: analytical Methods: data analysis Methods: numerical Methods: statistical Stars: fundamental parameters Distribution functions Inverse problems Stars Systems (metallurgical) Binaries: general Methods: numericals Methods:analytical Methods:data analysis Methods:statistical Stars:fundamental parameters Numerical methods |
| spellingShingle |
Binaries: general Methods: analytical Methods: data analysis Methods: numerical Methods: statistical Stars: fundamental parameters Distribution functions Inverse problems Stars Systems (metallurgical) Binaries: general Methods: numericals Methods:analytical Methods:data analysis Methods:statistical Stars:fundamental parameters Numerical methods Curé, M. Rial, D.F. Cassetti, J. Christen, A. Boffin, H.M.J. A method to deconvolve mass ratio distribution of binary stars |
| topic_facet |
Binaries: general Methods: analytical Methods: data analysis Methods: numerical Methods: statistical Stars: fundamental parameters Distribution functions Inverse problems Stars Systems (metallurgical) Binaries: general Methods: numericals Methods:analytical Methods:data analysis Methods:statistical Stars:fundamental parameters Numerical methods |
| description |
Aims. It is important to know the binary mass-ratio distribution to better understand the evolution of stars in binary systems and to constrain their formation. However, in most cases, that is, for single-lined spectroscopic binaries, the mass ratio cannot be measured directly, but can only be derived as the convolution of a function that depends on the mass ratio and on the unknown inclination angle of the orbit on the plane of the sky. Methods. We extend our previous method for deconvolving this inverse problem by obtaining the cumulative distribution function (CDF) for the mass-ratio distribution as an integral. Results. After a suitable transformation of variables, this problem becomes the same as the problem of rotational velocities vsini, allowing a close analytic formulation for the CDF. We here apply our method to two real datasets: a sample of Am star binary systems, and a sample of massive spectroscopic binaries in the Cyg OB2 association. Conclusions. We are able to reproduce previous results for the sample of Am stars. In addition, the mass-ratio distribution of massive stars shows an excess of systems with a low mass ratio, in contrast to what was claimed elsewhere. Our method proves to be very reliable and deconvolves the distribution from a sample in one single step. © 2014 ESO. |
| format |
JOUR |
| author |
Curé, M. Rial, D.F. Cassetti, J. Christen, A. Boffin, H.M.J. |
| author_facet |
Curé, M. Rial, D.F. Cassetti, J. Christen, A. Boffin, H.M.J. |
| author_sort |
Curé, M. |
| title |
A method to deconvolve mass ratio distribution of binary stars |
| title_short |
A method to deconvolve mass ratio distribution of binary stars |
| title_full |
A method to deconvolve mass ratio distribution of binary stars |
| title_fullStr |
A method to deconvolve mass ratio distribution of binary stars |
| title_full_unstemmed |
A method to deconvolve mass ratio distribution of binary stars |
| title_sort |
method to deconvolve mass ratio distribution of binary stars |
| url |
http://hdl.handle.net/20.500.12110/paper_00046361_v573_n_p_Cure |
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