%0 Generic %1 luo2021binary %A Luo, Feng %A Zhao, Yong-Heng %A Li, Jiao %A Guo, Yan-Jun %A Liu, Chao %D 2021 %K multiplicity %T Binary fraction of O and B-type stars from LAMOST data %U http://arxiv.org/abs/2108.11120 %X Binary stars plays important role in the evolution of stellar populations . The intrinsic binary fraction ($f_bin$) of O and B-type (OB) stars in LAMOST DR5 was investigated in this work. We employed a cross-correlation approach to estimate relative radial velocities for each of the stellar spectra. The algorithm described by 2013A&A...550A.107S was implemented and several simulations were made to assess the performance of the approach. Binary fraction of the OB stars are estimated through comparing the uni-distribution between observations and simulations with the Kolmogorov-Smirnov tests. Simulations show that it is reliable for stars most of whom have $6,7$ and $8$ repeated observations. The uncertainty of orbital parameters of binarity become larger when observational frequencies decrease. By adopting the fixed power exponents of $\pi=-0.45$ and $\kappa=-1$ for period and mass ratio distributions, respectively, we obtain that $f_bin=0.4_-0.06^+0.05$ for the samples with more than 3 observations. When we consider the full samples with at least 2 observations, the binary fraction turns out to be $0.37_-0.03^+0.03$. These two results are consistent with each other in $1\sigma$.

@misc{luo2021binary, abstract = {Binary stars plays important role in the evolution of stellar populations . The intrinsic binary fraction ($f_{bin}$) of O and B-type (OB) stars in LAMOST DR5 was investigated in this work. We employed a cross-correlation approach to estimate relative radial velocities for each of the stellar spectra. The algorithm described by \cite{2013A&A...550A.107S} was implemented and several simulations were made to assess the performance of the approach. Binary fraction of the OB stars are estimated through comparing the uni-distribution between observations and simulations with the Kolmogorov-Smirnov tests. Simulations show that it is reliable for stars most of whom have $6,7$ and $8$ repeated observations. The uncertainty of orbital parameters of binarity become larger when observational frequencies decrease. By adopting the fixed power exponents of $\pi=-0.45$ and $\kappa=-1$ for period and mass ratio distributions, respectively, we obtain that $f_{bin}=0.4_{-0.06}^{+0.05}$ for the samples with more than 3 observations. When we consider the full samples with at least 2 observations, the binary fraction turns out to be $0.37_{-0.03}^{+0.03}$. These two results are consistent with each other in $1\sigma$.}, added-at = {2021-08-26T17:44:57.000+0200}, author = {Luo, Feng and Zhao, Yong-Heng and Li, Jiao and Guo, Yan-Jun and Liu, Chao}, biburl = {https://www.bibsonomy.org/bibtex/2093e2629e7861095d486ea3f3fe0642c/superjenwinters}, description = {Binary fraction of O and B-type stars from LAMOST data}, interhash = {852bb4499207397450957779f2702c47}, intrahash = {093e2629e7861095d486ea3f3fe0642c}, keywords = {multiplicity}, note = {cite arxiv:2108.11120}, timestamp = {2021-08-26T17:44:57.000+0200}, title = {Binary fraction of O and B-type stars from LAMOST data}, url = {http://arxiv.org/abs/2108.11120}, year = 2021 }