SIMBAD references

2016ApJ...823..115D - Astrophys. J., 823, 115 (2016/June-1)

Doppler monitoring of five K2 transiting planetary systems.

DAI F., WINN J.N., ALBRECHT S., ARRIAGADA P., BIERYLA A., BUTLER R.P., CRANE J.D., HIRANO T., JOHNSON J.A., KIILERICH A., LATHAM D.W., NARITA N., NOWAK G., PALLE E., RIBAS I., ROGERS L.A., SANCHIS-OJEDA R., SHECTMAN S.A., TESKE J.K., THOMPSON I.B., VAN EYLEN V., VANDERBURG A., WITTENMYER R.A. and YU L.

Abstract (from CDS):

In an effort to measure the masses of planets discovered by the NASA K2 mission, we have conducted precise Doppler observations of five stars with transiting planets. We present the results of a joint analysis of these new data and previously published Doppler data. The first star, an M dwarf known as K2-3 or EPIC 201367065, has three transiting planets ("b," with radius 2.1 {R}_⊕; "c," 1.7 {R}_⊕; and "d," 1.5 {R}_⊕ ). Our analysis leads to the mass constraints: {M}\={8.1}{-1.9}^{+2.0} {M}_⊕ and M_ c_ M (95% confidence). The mass of planet d is poorly constrained because its orbital period is close to the stellar rotation period, making it difficult to disentangle the planetary signal from spurious Doppler shifts due to stellar activity. The second star, a G dwarf known as K2-19 or EPIC 201505350, has two planets ("b," 7.7 R; and "c," 4.9 R) in a 3:2 mean-motion resonance, as well as a shorter-period planet ("d," 1.1 R). We find M_ b_= {28.5}{–5.0}{+5.4} {M}_⊕ , M_ c_= {25.6}{–7.1}{+7.1} {M}_⊕ and M_ d_ M (95% conf.). The third star, a G dwarf known as K2-24 or EPIC 203771098, hosts two transiting planets ("b," 5.7 R; and "c," 7.8 R) with orbital periods in a nearly 2:1 ratio. We find M_ b_= {19.8}{–4.4}{+4.5} {M}_⊕ and M_ c_= {26.0}{–6.1}{+5.8} {M}_⊕ . The fourth star, a G dwarf known as EPIC 204129699, hosts a hot Jupiter for which we measured the mass to be {1.857}{–0.081}{+0.081} {M}_Jup . The fifth star, a G dwarf known as EPIC 205071984, contains three transiting planets ("b," 5.4 R; "c," 3.5 R; and "d," 3.8 R), the outer two of which have a nearly 2:1 period ratio. We find M_ b_= {21.1}{–5.9}{+5.9} {M}_⊕ , M_ c_ (95% conf.) and M_ d_ M (95% conf.).

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): planetary systems - planets and satellites: composition - techniques: radial velocities

Simbad objects: 21

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2021.01.27-20:28:00

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