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errata, addenda, techniques: radial velocities, planets and satellites: detection, stars: activity, methods: statistical, stars: rotation, instrumentation: spectrographs

This is an erratum to the paper titled ‘Trio of super-Earth candidates orbiting K-Dwarf HD 48948: a new habitable zone candidate’, published in MNRAS 531, 4464–4481 (2024) with 10.1093/mnras/stae1367. We have identified and corrected errors in table 3 of the original publication. The incident flux and temperature values for the three planetary candidates were incorrectly calculated due to a mathematical error. Additionally, we discovered a typographical mistake in the eccentricity values for candidates c and d in the tweaks analysis. The accurate and updated values are provided in the Table 1. While these errors do not alter the overall conclusions of the paper, the corrected values provide a more accurate representation of the data and should be used for reference in future research.

Table 1.
Open in new tab

The table displays the results of three Keplerian models, as discussed in sections 7.1, 7.2, and 7.3. The values and uncertainties of each parameter are derived from their respective posterior distributions, with the 50|$^{\rm {th}}$| percentile representing the central value and the 16|$^{\rm {th}}$| to 84|$^{\rm {th}}$| percentile range indicating 1σ uncertainty. Additionally, the derived parameters, as explained in section 7.3, are also included in this table. The maximum equilibrium temperature is calculated assuming an albedo (A|$_{B}$|⁠) of 0 and isotropic re-emission and uniform equilibrium temperature.

ParameterSymbolUnitHD48948 bHD48948 cHD48948 d
Three Keplerians-only analysis on YV2 RVs
Orbital periodPdays|$7.33982_{-0.00085}^{+0.00082}$||$37.998_{-0.019}^{+0.018}$||$151.12_{-0.49}^{+0.56}$|
RV amplitudeK|$\rm m\, s^{-1}$||$1.35_{-0.17}^{+0.18}$||$1.71_{-0.22}^{+0.20}$||$1.09\pm 0.19$|
Eccentricitye|$0.06_{-0.05}^{+0.10}$||$0.06_{-0.05}^{+0.09}$||$0.10_{-0.09}^{+0.18}$|
Argument of periastron|$\omega$|rad|$0.83_{-1.28}^{+1.27}$||$-1.06_{-1.00}^{+1.24}$||$-1.02_{-1.11}^{+1.43}$|
|$\sqrt{e}\cos \omega$||$0.07_{-0.16}^{+0.19}$||$0.04_{-0.20}^{+0.15}$||$0.04_{-0.30}^{+0.17}$|
|$\sqrt{e}\sin \omega$||$0.09_{-0.15}^{+0.20}$||$-0.11_{-0.19}^{+0.13}$||$-0.14_{-0.27}^{+0.18}$|
Time of periastron|$t_{\rm p}$|BJD|$2456574.05_{-1.49}^{+1.53}$||$2456570.22_{-7.11}^{+5.98}$||$2456564.06_{-31.89}^{+18.67}$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$3.18\pm 0.41$||$6.97_{-0.89}^{+0.82}$||$6.93_{-1.24}^{+1.21}$|
One-dimensional GP analysis on YVA RVs
Orbital periodPdays|$7.34012_{-0.00046}^{+0.00052}$||$37.99_{-0.22}^{+0.16}$||$150.28\pm 0.69$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.07_{-0.17}^{+0.15}$||$1.06\pm 0.69$||$1.55_{-0.38}^{+0.35}$|
Eccentricitye|$0.08_{-0.05}^{+0.06}$||$0.23_{-0.19}^{+0.14}$||$0.15_{-0.10}^{+0.17}$|
Argument of periastron|$\omega$|rad|$0.55_{-0.92}^{+0.95}$||$-0.48_{-1.40}^{+1.81}$||$-1.05{-0.79}^{+0.96}$|
|$\sqrt{e}\cos \omega$||$0.16_{-0.18}^{+0.13}$||$0.13_{-0.40}^{+0.34}$||$0.10_{-0.33}^{+0.20}$|
|$\sqrt{e}\sin \omega$||$0.11_{-0.18}^{+0.14}$||$-0.11_{-0.33}^{+0.46}$||$-0.25_{-0.20}^{+0.23}$|
Time of periastron|$t_{\rm p}$|BJD|$2456573.74_{87}^{+1.05}$||$2456571.71_{-9.80}^{+10.5}$||$2456571.52\pm 15.3$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$4.86_{-0.39}^{+0.35}$||$3.94_{-2.85}^{+3.02}$||$9.72_{-2.56}^{+2.26}$|
Multidimensional GP analysis on YVA RVs
Orbital periodPdays|$7.34013_{-0.00040}^{+0.00040}$||$37.920_{-0.024}^{+0.026}$||$150.95_{-0.41}^{+0.45}$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.11\pm 0.13$||$1.75\pm 0.25$||$1.72\pm 0.22$|
Eccentricitye|$0.078_{-0.050}^{+0.058}$||$0.22_{-0.11}^{+0.10}$||$0.12_{-0.08}^{+0.12}$|
Argument of periastron|$\omega$|rad|$0.68_{-0.77}^{+0.84}$||$1.76_{-0.54}^{+0.66}$||$4.69_{-1.21}^{+1.19}$|
|$\sqrt{e}\cos \omega$||$0.17_{-0.18}^{+0.13}$||$-0.08_{-0.22}^{+0.23}$||$0.01\pm 0.24$|
|$\sqrt{e}\sin \omega$||$0.14_{-0.17}^{+0.13}$||$0.41_{-0.21}^{+0.13}$||$0.21_{-0.19}^{+0.25}$|
Time of periastron|$t_{\rm p}$|BJD|$2459003.44 _{ -0.83 }^{+ 1.06}$||$2459019.8 _{ -2.7 }^{+ 3.5}$||$2459107 _{ -42 }^{+ 24}$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$4.96\pm 0.32$||$6.9\pm 1.0$||$11.0\pm 1.5$|
tweaksanalysis ontweaksRVs
Orbital periodPdays|$7.34013 \pm 0.00040$||$38.06 \pm 0.06$||$151.92 \pm 0.44$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.28\pm 0.15$||$1.48\pm 0.39$||$1.55\pm 0.34$|
Eccentricitye|$0.055 \pm 0.043$||$0.11 \pm 0.08$||$0.13 \pm 0.11$|
Argument of periastron|$\omega$|rad|$0.68_{-0.77}^{+0.84}$||$1.76_{-0.54}^{+0.66}$||$4.69_{-1.21}^{+1.19}$|
Time of periastron|$t_{\rm p}$|BJD|$2456567.026 \pm 1.72$||$2456557.14 \pm 12.5$||$2456494.34 \pm 20.1$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$5.43\pm 0.30$||$6.33\pm 1.6$||$10.05\pm 2.27$|
Derived parameters
Semimajor axisaau|$0.0652\pm 0.0005$||$0.1951\pm 0.0016$||$0.4894\pm 0.0042$|
Semimajor axisaarcsec0.00390.01160.0291
Scaled semimajor axis|$a/R_\star$||$20.65\pm 0.21$||$61.79\pm 0.62$||$154.97\pm 1.61$|
Incident flux|$F_{\rm inc}$||$F_{\rm inc,{\oplus }}$||$43.33\pm 2.41$||$4.84\pm 0.27$||$0.77\pm 0.04$|
Equilibrium temperature|$T_{\rm eq}$|K|$715\pm 10$||$413\pm 6$||$261\pm 4$|
ParameterSymbolUnitHD48948 bHD48948 cHD48948 d
Three Keplerians-only analysis on YV2 RVs
Orbital periodPdays|$7.33982_{-0.00085}^{+0.00082}$||$37.998_{-0.019}^{+0.018}$||$151.12_{-0.49}^{+0.56}$|
RV amplitudeK|$\rm m\, s^{-1}$||$1.35_{-0.17}^{+0.18}$||$1.71_{-0.22}^{+0.20}$||$1.09\pm 0.19$|
Eccentricitye|$0.06_{-0.05}^{+0.10}$||$0.06_{-0.05}^{+0.09}$||$0.10_{-0.09}^{+0.18}$|
Argument of periastron|$\omega$|rad|$0.83_{-1.28}^{+1.27}$||$-1.06_{-1.00}^{+1.24}$||$-1.02_{-1.11}^{+1.43}$|
|$\sqrt{e}\cos \omega$||$0.07_{-0.16}^{+0.19}$||$0.04_{-0.20}^{+0.15}$||$0.04_{-0.30}^{+0.17}$|
|$\sqrt{e}\sin \omega$||$0.09_{-0.15}^{+0.20}$||$-0.11_{-0.19}^{+0.13}$||$-0.14_{-0.27}^{+0.18}$|
Time of periastron|$t_{\rm p}$|BJD|$2456574.05_{-1.49}^{+1.53}$||$2456570.22_{-7.11}^{+5.98}$||$2456564.06_{-31.89}^{+18.67}$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$3.18\pm 0.41$||$6.97_{-0.89}^{+0.82}$||$6.93_{-1.24}^{+1.21}$|
One-dimensional GP analysis on YVA RVs
Orbital periodPdays|$7.34012_{-0.00046}^{+0.00052}$||$37.99_{-0.22}^{+0.16}$||$150.28\pm 0.69$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.07_{-0.17}^{+0.15}$||$1.06\pm 0.69$||$1.55_{-0.38}^{+0.35}$|
Eccentricitye|$0.08_{-0.05}^{+0.06}$||$0.23_{-0.19}^{+0.14}$||$0.15_{-0.10}^{+0.17}$|
Argument of periastron|$\omega$|rad|$0.55_{-0.92}^{+0.95}$||$-0.48_{-1.40}^{+1.81}$||$-1.05{-0.79}^{+0.96}$|
|$\sqrt{e}\cos \omega$||$0.16_{-0.18}^{+0.13}$||$0.13_{-0.40}^{+0.34}$||$0.10_{-0.33}^{+0.20}$|
|$\sqrt{e}\sin \omega$||$0.11_{-0.18}^{+0.14}$||$-0.11_{-0.33}^{+0.46}$||$-0.25_{-0.20}^{+0.23}$|
Time of periastron|$t_{\rm p}$|BJD|$2456573.74_{87}^{+1.05}$||$2456571.71_{-9.80}^{+10.5}$||$2456571.52\pm 15.3$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$4.86_{-0.39}^{+0.35}$||$3.94_{-2.85}^{+3.02}$||$9.72_{-2.56}^{+2.26}$|
Multidimensional GP analysis on YVA RVs
Orbital periodPdays|$7.34013_{-0.00040}^{+0.00040}$||$37.920_{-0.024}^{+0.026}$||$150.95_{-0.41}^{+0.45}$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.11\pm 0.13$||$1.75\pm 0.25$||$1.72\pm 0.22$|
Eccentricitye|$0.078_{-0.050}^{+0.058}$||$0.22_{-0.11}^{+0.10}$||$0.12_{-0.08}^{+0.12}$|
Argument of periastron|$\omega$|rad|$0.68_{-0.77}^{+0.84}$||$1.76_{-0.54}^{+0.66}$||$4.69_{-1.21}^{+1.19}$|
|$\sqrt{e}\cos \omega$||$0.17_{-0.18}^{+0.13}$||$-0.08_{-0.22}^{+0.23}$||$0.01\pm 0.24$|
|$\sqrt{e}\sin \omega$||$0.14_{-0.17}^{+0.13}$||$0.41_{-0.21}^{+0.13}$||$0.21_{-0.19}^{+0.25}$|
Time of periastron|$t_{\rm p}$|BJD|$2459003.44 _{ -0.83 }^{+ 1.06}$||$2459019.8 _{ -2.7 }^{+ 3.5}$||$2459107 _{ -42 }^{+ 24}$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$4.96\pm 0.32$||$6.9\pm 1.0$||$11.0\pm 1.5$|
tweaksanalysis ontweaksRVs
Orbital periodPdays|$7.34013 \pm 0.00040$||$38.06 \pm 0.06$||$151.92 \pm 0.44$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.28\pm 0.15$||$1.48\pm 0.39$||$1.55\pm 0.34$|
Eccentricitye|$0.055 \pm 0.043$||$0.11 \pm 0.08$||$0.13 \pm 0.11$|
Argument of periastron|$\omega$|rad|$0.68_{-0.77}^{+0.84}$||$1.76_{-0.54}^{+0.66}$||$4.69_{-1.21}^{+1.19}$|
Time of periastron|$t_{\rm p}$|BJD|$2456567.026 \pm 1.72$||$2456557.14 \pm 12.5$||$2456494.34 \pm 20.1$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$5.43\pm 0.30$||$6.33\pm 1.6$||$10.05\pm 2.27$|
Derived parameters
Semimajor axisaau|$0.0652\pm 0.0005$||$0.1951\pm 0.0016$||$0.4894\pm 0.0042$|
Semimajor axisaarcsec0.00390.01160.0291
Scaled semimajor axis|$a/R_\star$||$20.65\pm 0.21$||$61.79\pm 0.62$||$154.97\pm 1.61$|
Incident flux|$F_{\rm inc}$||$F_{\rm inc,{\oplus }}$||$43.33\pm 2.41$||$4.84\pm 0.27$||$0.77\pm 0.04$|
Equilibrium temperature|$T_{\rm eq}$|K|$715\pm 10$||$413\pm 6$||$261\pm 4$|
Table 1.
Open in new tab

The table displays the results of three Keplerian models, as discussed in sections 7.1, 7.2, and 7.3. The values and uncertainties of each parameter are derived from their respective posterior distributions, with the 50|$^{\rm {th}}$| percentile representing the central value and the 16|$^{\rm {th}}$| to 84|$^{\rm {th}}$| percentile range indicating 1σ uncertainty. Additionally, the derived parameters, as explained in section 7.3, are also included in this table. The maximum equilibrium temperature is calculated assuming an albedo (A|$_{B}$|⁠) of 0 and isotropic re-emission and uniform equilibrium temperature.

ParameterSymbolUnitHD48948 bHD48948 cHD48948 d
Three Keplerians-only analysis on YV2 RVs
Orbital periodPdays|$7.33982_{-0.00085}^{+0.00082}$||$37.998_{-0.019}^{+0.018}$||$151.12_{-0.49}^{+0.56}$|
RV amplitudeK|$\rm m\, s^{-1}$||$1.35_{-0.17}^{+0.18}$||$1.71_{-0.22}^{+0.20}$||$1.09\pm 0.19$|
Eccentricitye|$0.06_{-0.05}^{+0.10}$||$0.06_{-0.05}^{+0.09}$||$0.10_{-0.09}^{+0.18}$|
Argument of periastron|$\omega$|rad|$0.83_{-1.28}^{+1.27}$||$-1.06_{-1.00}^{+1.24}$||$-1.02_{-1.11}^{+1.43}$|
|$\sqrt{e}\cos \omega$||$0.07_{-0.16}^{+0.19}$||$0.04_{-0.20}^{+0.15}$||$0.04_{-0.30}^{+0.17}$|
|$\sqrt{e}\sin \omega$||$0.09_{-0.15}^{+0.20}$||$-0.11_{-0.19}^{+0.13}$||$-0.14_{-0.27}^{+0.18}$|
Time of periastron|$t_{\rm p}$|BJD|$2456574.05_{-1.49}^{+1.53}$||$2456570.22_{-7.11}^{+5.98}$||$2456564.06_{-31.89}^{+18.67}$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$3.18\pm 0.41$||$6.97_{-0.89}^{+0.82}$||$6.93_{-1.24}^{+1.21}$|
One-dimensional GP analysis on YVA RVs
Orbital periodPdays|$7.34012_{-0.00046}^{+0.00052}$||$37.99_{-0.22}^{+0.16}$||$150.28\pm 0.69$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.07_{-0.17}^{+0.15}$||$1.06\pm 0.69$||$1.55_{-0.38}^{+0.35}$|
Eccentricitye|$0.08_{-0.05}^{+0.06}$||$0.23_{-0.19}^{+0.14}$||$0.15_{-0.10}^{+0.17}$|
Argument of periastron|$\omega$|rad|$0.55_{-0.92}^{+0.95}$||$-0.48_{-1.40}^{+1.81}$||$-1.05{-0.79}^{+0.96}$|
|$\sqrt{e}\cos \omega$||$0.16_{-0.18}^{+0.13}$||$0.13_{-0.40}^{+0.34}$||$0.10_{-0.33}^{+0.20}$|
|$\sqrt{e}\sin \omega$||$0.11_{-0.18}^{+0.14}$||$-0.11_{-0.33}^{+0.46}$||$-0.25_{-0.20}^{+0.23}$|
Time of periastron|$t_{\rm p}$|BJD|$2456573.74_{87}^{+1.05}$||$2456571.71_{-9.80}^{+10.5}$||$2456571.52\pm 15.3$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$4.86_{-0.39}^{+0.35}$||$3.94_{-2.85}^{+3.02}$||$9.72_{-2.56}^{+2.26}$|
Multidimensional GP analysis on YVA RVs
Orbital periodPdays|$7.34013_{-0.00040}^{+0.00040}$||$37.920_{-0.024}^{+0.026}$||$150.95_{-0.41}^{+0.45}$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.11\pm 0.13$||$1.75\pm 0.25$||$1.72\pm 0.22$|
Eccentricitye|$0.078_{-0.050}^{+0.058}$||$0.22_{-0.11}^{+0.10}$||$0.12_{-0.08}^{+0.12}$|
Argument of periastron|$\omega$|rad|$0.68_{-0.77}^{+0.84}$||$1.76_{-0.54}^{+0.66}$||$4.69_{-1.21}^{+1.19}$|
|$\sqrt{e}\cos \omega$||$0.17_{-0.18}^{+0.13}$||$-0.08_{-0.22}^{+0.23}$||$0.01\pm 0.24$|
|$\sqrt{e}\sin \omega$||$0.14_{-0.17}^{+0.13}$||$0.41_{-0.21}^{+0.13}$||$0.21_{-0.19}^{+0.25}$|
Time of periastron|$t_{\rm p}$|BJD|$2459003.44 _{ -0.83 }^{+ 1.06}$||$2459019.8 _{ -2.7 }^{+ 3.5}$||$2459107 _{ -42 }^{+ 24}$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$4.96\pm 0.32$||$6.9\pm 1.0$||$11.0\pm 1.5$|
tweaksanalysis ontweaksRVs
Orbital periodPdays|$7.34013 \pm 0.00040$||$38.06 \pm 0.06$||$151.92 \pm 0.44$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.28\pm 0.15$||$1.48\pm 0.39$||$1.55\pm 0.34$|
Eccentricitye|$0.055 \pm 0.043$||$0.11 \pm 0.08$||$0.13 \pm 0.11$|
Argument of periastron|$\omega$|rad|$0.68_{-0.77}^{+0.84}$||$1.76_{-0.54}^{+0.66}$||$4.69_{-1.21}^{+1.19}$|
Time of periastron|$t_{\rm p}$|BJD|$2456567.026 \pm 1.72$||$2456557.14 \pm 12.5$||$2456494.34 \pm 20.1$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$5.43\pm 0.30$||$6.33\pm 1.6$||$10.05\pm 2.27$|
Derived parameters
Semimajor axisaau|$0.0652\pm 0.0005$||$0.1951\pm 0.0016$||$0.4894\pm 0.0042$|
Semimajor axisaarcsec0.00390.01160.0291
Scaled semimajor axis|$a/R_\star$||$20.65\pm 0.21$||$61.79\pm 0.62$||$154.97\pm 1.61$|
Incident flux|$F_{\rm inc}$||$F_{\rm inc,{\oplus }}$||$43.33\pm 2.41$||$4.84\pm 0.27$||$0.77\pm 0.04$|
Equilibrium temperature|$T_{\rm eq}$|K|$715\pm 10$||$413\pm 6$||$261\pm 4$|
ParameterSymbolUnitHD48948 bHD48948 cHD48948 d
Three Keplerians-only analysis on YV2 RVs
Orbital periodPdays|$7.33982_{-0.00085}^{+0.00082}$||$37.998_{-0.019}^{+0.018}$||$151.12_{-0.49}^{+0.56}$|
RV amplitudeK|$\rm m\, s^{-1}$||$1.35_{-0.17}^{+0.18}$||$1.71_{-0.22}^{+0.20}$||$1.09\pm 0.19$|
Eccentricitye|$0.06_{-0.05}^{+0.10}$||$0.06_{-0.05}^{+0.09}$||$0.10_{-0.09}^{+0.18}$|
Argument of periastron|$\omega$|rad|$0.83_{-1.28}^{+1.27}$||$-1.06_{-1.00}^{+1.24}$||$-1.02_{-1.11}^{+1.43}$|
|$\sqrt{e}\cos \omega$||$0.07_{-0.16}^{+0.19}$||$0.04_{-0.20}^{+0.15}$||$0.04_{-0.30}^{+0.17}$|
|$\sqrt{e}\sin \omega$||$0.09_{-0.15}^{+0.20}$||$-0.11_{-0.19}^{+0.13}$||$-0.14_{-0.27}^{+0.18}$|
Time of periastron|$t_{\rm p}$|BJD|$2456574.05_{-1.49}^{+1.53}$||$2456570.22_{-7.11}^{+5.98}$||$2456564.06_{-31.89}^{+18.67}$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$3.18\pm 0.41$||$6.97_{-0.89}^{+0.82}$||$6.93_{-1.24}^{+1.21}$|
One-dimensional GP analysis on YVA RVs
Orbital periodPdays|$7.34012_{-0.00046}^{+0.00052}$||$37.99_{-0.22}^{+0.16}$||$150.28\pm 0.69$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.07_{-0.17}^{+0.15}$||$1.06\pm 0.69$||$1.55_{-0.38}^{+0.35}$|
Eccentricitye|$0.08_{-0.05}^{+0.06}$||$0.23_{-0.19}^{+0.14}$||$0.15_{-0.10}^{+0.17}$|
Argument of periastron|$\omega$|rad|$0.55_{-0.92}^{+0.95}$||$-0.48_{-1.40}^{+1.81}$||$-1.05{-0.79}^{+0.96}$|
|$\sqrt{e}\cos \omega$||$0.16_{-0.18}^{+0.13}$||$0.13_{-0.40}^{+0.34}$||$0.10_{-0.33}^{+0.20}$|
|$\sqrt{e}\sin \omega$||$0.11_{-0.18}^{+0.14}$||$-0.11_{-0.33}^{+0.46}$||$-0.25_{-0.20}^{+0.23}$|
Time of periastron|$t_{\rm p}$|BJD|$2456573.74_{87}^{+1.05}$||$2456571.71_{-9.80}^{+10.5}$||$2456571.52\pm 15.3$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$4.86_{-0.39}^{+0.35}$||$3.94_{-2.85}^{+3.02}$||$9.72_{-2.56}^{+2.26}$|
Multidimensional GP analysis on YVA RVs
Orbital periodPdays|$7.34013_{-0.00040}^{+0.00040}$||$37.920_{-0.024}^{+0.026}$||$150.95_{-0.41}^{+0.45}$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.11\pm 0.13$||$1.75\pm 0.25$||$1.72\pm 0.22$|
Eccentricitye|$0.078_{-0.050}^{+0.058}$||$0.22_{-0.11}^{+0.10}$||$0.12_{-0.08}^{+0.12}$|
Argument of periastron|$\omega$|rad|$0.68_{-0.77}^{+0.84}$||$1.76_{-0.54}^{+0.66}$||$4.69_{-1.21}^{+1.19}$|
|$\sqrt{e}\cos \omega$||$0.17_{-0.18}^{+0.13}$||$-0.08_{-0.22}^{+0.23}$||$0.01\pm 0.24$|
|$\sqrt{e}\sin \omega$||$0.14_{-0.17}^{+0.13}$||$0.41_{-0.21}^{+0.13}$||$0.21_{-0.19}^{+0.25}$|
Time of periastron|$t_{\rm p}$|BJD|$2459003.44 _{ -0.83 }^{+ 1.06}$||$2459019.8 _{ -2.7 }^{+ 3.5}$||$2459107 _{ -42 }^{+ 24}$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$4.96\pm 0.32$||$6.9\pm 1.0$||$11.0\pm 1.5$|
tweaksanalysis ontweaksRVs
Orbital periodPdays|$7.34013 \pm 0.00040$||$38.06 \pm 0.06$||$151.92 \pm 0.44$|
RV amplitudeK|$\rm m\, s^{-1}$||$2.28\pm 0.15$||$1.48\pm 0.39$||$1.55\pm 0.34$|
Eccentricitye|$0.055 \pm 0.043$||$0.11 \pm 0.08$||$0.13 \pm 0.11$|
Argument of periastron|$\omega$|rad|$0.68_{-0.77}^{+0.84}$||$1.76_{-0.54}^{+0.66}$||$4.69_{-1.21}^{+1.19}$|
Time of periastron|$t_{\rm p}$|BJD|$2456567.026 \pm 1.72$||$2456557.14 \pm 12.5$||$2456494.34 \pm 20.1$|
Minimum mass|$m\sin (i)$|M|$_{{\oplus }}$||$5.43\pm 0.30$||$6.33\pm 1.6$||$10.05\pm 2.27$|
Derived parameters
Semimajor axisaau|$0.0652\pm 0.0005$||$0.1951\pm 0.0016$||$0.4894\pm 0.0042$|
Semimajor axisaarcsec0.00390.01160.0291
Scaled semimajor axis|$a/R_\star$||$20.65\pm 0.21$||$61.79\pm 0.62$||$154.97\pm 1.61$|
Incident flux|$F_{\rm inc}$||$F_{\rm inc,{\oplus }}$||$43.33\pm 2.41$||$4.84\pm 0.27$||$0.77\pm 0.04$|
Equilibrium temperature|$T_{\rm eq}$|K|$715\pm 10$||$413\pm 6$||$261\pm 4$|

Author notes

STFC Ernest Rutherford Fellow

© 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.
This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
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