Circumstellar stability radius for the higher order systems included in the SPOTS target list.
|TYC 9399 2452 1||0.97 + ?||1.69||9.07||169.90||Quadruple||1,2|
|HIP 46637||0.89 + ?||0.87||14.00||153.41||Triple (wide)||3|
|HIP 49669||3.70||1.10||175.00||>1000||Quadruple||SPOTS II|
|HIP 76629||1.39||0.22||10.00||158.65||Triple (wide)||4|
|HIP 77911||3.14||0.20||7.96||576.09||Triple (wide)||5|
|HIP 78416||1.26 + ?||1.15||6.55||217.10||Triple (wide)||SPOTS I|
|ScoPMS048||1.35 + ?||0.4||3.38||152.03||Triple (wide)||This work, 6|
|ROXs 43A||1.64||0.7||4.48||256.11||Quintuple||This work, 7|
|HIP 84586||2.05||0.25||33.00||178.00||Quadruple||SPOTS II|
|HIP 19591||1.27||0.52||0.31||2.38||Tripled||This work, SPOTS I|
|HIP 12716||1.52||0.58||0.38||3.16||Tripled||This work, SPOTS I|
|HIP 105404||0.8||0.9||0.04||0.27||Tripled||This work, 10|
Notes. (a) Total mass of the inner system (MA + MB from Table B.1). (b) Mass of the additional companion (or total mass of the pair in case of hierarchical systems). (c) Outer limit for orbital stability. If no information on the mass was available (marked with a question mark), a mass equal to half of that of the primary was adopted for the computation of the dynamical stability limit. (d) The circumstellar stability radius for the triple systems will not be considered for the statistical analysis, as we are not sensitive to those separations.
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