The SDSS-HET Survey of Kepler Eclipsing Binaries. Description of the Survey and First Results. (arXiv:2004.02962v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mahadevan_S/0/1/0/all/0/1">Suvrath Mahadevan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bender_C/0/1/0/all/0/1">Chad F. Bender</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hambleton_K/0/1/0/all/0/1">Kelly Hambleton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fleming_S/0/1/0/all/0/1">Scott W. Fleming</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deshpande_R/0/1/0/all/0/1">Rohit Deshpande</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conroy_K/0/1/0/all/0/1">Kyle Conroy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matijevic_G/0/1/0/all/0/1">Gal Matijevič</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hebb_L/0/1/0/all/0/1">Leslie Hebb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roy_A/0/1/0/all/0/1">Arpita Roy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ak_H/0/1/0/all/0/1">Hasan Ak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leban_B/0/1/0/all/0/1">Blaž Leban</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prsa_A/0/1/0/all/0/1">Andrej Prša</a>
The Kepler mission has provided a treasure trove of eclipsing binaries (EBs),
observed at extremely high photometric precision, nearly continuously for
several years. We are carrying out a survey of ~100 of these EBs to derive
dynamical masses and radii with precisions of 3% or better. We use multiplexed
near-infrared H band spectroscopy from the SDSS-III and -IV APOGEE instrument
and optical spectroscopy from the HET High-Resolution Spectrograph to derive
double-lined spectroscopic orbits and dynamical mass-ratios for the EB sample.
This information is combined with Kepler photometry to derive orbital
inclination, dynamical masses of the components, radii and temperatures. These
measurements are directly applicable for benchmarking stellar models that are
integrating the next generation of improvements, such as the magnetic
suppression of convection efficiency, updated opacity tables, and fine-tuned
equations of state. We selected our EB sample to include systems with low-mass
($M lt 0.8 ; M_{odot}$) primary or secondary components, many expected to
populate the relatively sparse parameter space below $0.5 ; M_{odot}$. In
this paper, we describe our EB sample and the analysis techniques we are
utilizing, and present masses and radii for two systems that inhabit
particularly underpopulated regions of mass-radius-period space: KIC 2445134
and KIC 3003991. Our analysis of KIC 2445134 ($q=0.411 pm 0.001$) yields
masses and radii of $M_A = 1.29 pm 0.03 ; M_{odot}$, $M_B = 0.53 pm 0.01 ;
M_{odot}$, $R_A = 1.42 pm 0.01 ; R_{odot}$, $R_B = 0.510 pm 0.004 ;
R_{odot}$, and a temperature ratio of $T_B/T_A = 0.635 pm 0.001$; our
analysis of KIC 3003991 ($q=0.298 pm 0.006$) yields $M_A = 0.74 pm ; 0.04
M_{odot}$, $M_B = 0.222 pm ; 0.007 M_{odot}$, $R_A = 0.84 pm 0.01 ;
R_{odot}$, $R_B = 0.250 pm 0.004 ; R_{odot}$, and a temperature ratio of
$T_B/T_A= 0.662 pm 0.001$.
The Kepler mission has provided a treasure trove of eclipsing binaries (EBs),
observed at extremely high photometric precision, nearly continuously for
several years. We are carrying out a survey of ~100 of these EBs to derive
dynamical masses and radii with precisions of 3% or better. We use multiplexed
near-infrared H band spectroscopy from the SDSS-III and -IV APOGEE instrument
and optical spectroscopy from the HET High-Resolution Spectrograph to derive
double-lined spectroscopic orbits and dynamical mass-ratios for the EB sample.
This information is combined with Kepler photometry to derive orbital
inclination, dynamical masses of the components, radii and temperatures. These
measurements are directly applicable for benchmarking stellar models that are
integrating the next generation of improvements, such as the magnetic
suppression of convection efficiency, updated opacity tables, and fine-tuned
equations of state. We selected our EB sample to include systems with low-mass
($M lt 0.8 ; M_{odot}$) primary or secondary components, many expected to
populate the relatively sparse parameter space below $0.5 ; M_{odot}$. In
this paper, we describe our EB sample and the analysis techniques we are
utilizing, and present masses and radii for two systems that inhabit
particularly underpopulated regions of mass-radius-period space: KIC 2445134
and KIC 3003991. Our analysis of KIC 2445134 ($q=0.411 pm 0.001$) yields
masses and radii of $M_A = 1.29 pm 0.03 ; M_{odot}$, $M_B = 0.53 pm 0.01 ;
M_{odot}$, $R_A = 1.42 pm 0.01 ; R_{odot}$, $R_B = 0.510 pm 0.004 ;
R_{odot}$, and a temperature ratio of $T_B/T_A = 0.635 pm 0.001$; our
analysis of KIC 3003991 ($q=0.298 pm 0.006$) yields $M_A = 0.74 pm ; 0.04
M_{odot}$, $M_B = 0.222 pm ; 0.007 M_{odot}$, $R_A = 0.84 pm 0.01 ;
R_{odot}$, $R_B = 0.250 pm 0.004 ; R_{odot}$, and a temperature ratio of
$T_B/T_A= 0.662 pm 0.001$.
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