Paper: TOI 762 A b and TIC 46432937 b: Two Giant Planets Transiting M-dwarf Stars
Authors: Joel D. Hartman, Daniel Bayliss, Rafael Brahm, Edward M. Bryant, Andrés Jordán, Gáspár Á. Bakos, Melissa J. Hobson, Elyar Sedaghati, Xavier Bonfils, Marion Cointepas, Jose Manuel Almenara, Khalid Barkaoui, Mathilde Timmermans, George Dransfield, Elsa Ducrot, Sebastián Zúñiga-Fernández, Matthew J. Hooton, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Amaury H. M. J. Triaud, Michaël Gillon, Emmanuel Jehin, William C. Waalkes, Zachory K. Berta-Thompson, Steve B. Howell, Elise Furlan, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David Rapetti, Karen A. Collins, David Charbonneau, Christopher J. Burke, David R. Rodriguez
Figure caption: Observations incorporated into the analysis of the transiting planet system TOI 762 A. Additional light curves are shown in Figure 3. Top: transit light curves with best-fitted model (maximum likelihood) overplotted. The dates, filters, and instruments used are indicated. The term z − H used for the ExTrA light curves refers to the full bandpass not the color. For TESS we phase-fold the data, and plot the unbinned observations in gray, with the phase-binned values overplotted in blue. The residuals for each light curve are shown on the right-hand side in the same order as the original light curves. The error bars represent the photon and background shot noise, plus the readout noise. Note that these uncertainties are scaled in the fitting procedure to achieve a reduced χ 2 of unity, but the uncertainties shown in the plot have not been scaled. Bottom left: high-precision RVs phased with respect to the mid-transit time. The top panel shows the phased measurements together with the best-fit (maximum-likelihood) model with no eccentricity. The grayscale curves show 1000 models randomly selected from the MCMC posterior distribution generated when the eccentricity is allowed to vary. The center-of-mass velocity has been subtracted. The middle panel shows the phase-folded velocity O − C residuals. The error bars include the estimated jitter, which is varied as a free parameter in the fitting. The bottom panel shows the O − C residuals as a function of time. Bottom right: color–magnitude diagram (CMD) and spectral energy distribution (SED). The top panel shows the absolute G magnitude vs. the dereddened G − K  S  color compared to theoretical isochrones (black lines) and stellar evolution tracks (green lines) from the MIST models interpolated at the best-estimate value for the metallicity of the host. The age of each isochrone is listed in black in billions of years, while the mass of each evolution track is listed in green in solar masses. The solid red lines show isochrones at higher and lower metallicities than the best-estimate value, with the metallicity and age in billions of years of each isochrone labeled on the plot. The filled blue circles show the measured reddening- and distance-corrected values from Gaia DR3 and 2MASS, while the blue lines indicate the 1σ and 2σ confidence regions, including the estimated systematic errors in the photometry. The middle panel shows the SED as measured via broadband photometry through the listed filters. Here we plot the observed magnitudes without correcting for distance or extinction. Overplotted are 200 model SEDs randomly selected from the MCMC posterior distribution produced through the global analysis (gray lines). The model makes use of the predicted absolute magnitudes in each bandpass from the MIST isochrones, the distance to the system (constrained largely via Gaia DR3), and extinction (constrained from the SED with a prior coming from the MWDUST 3D Galactic extinction model). The bottom panel shows the O − C residuals from the best-fit model SED. The errors listed in the catalogs for the broadband photometry measurements are shown with black lines, while the errors including an assumed 0.02 mag systematic uncertainty, which is added in quadrature to the listed uncertainties, are shown with red lines. These latter uncertainties are what we use in the fit.