Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Observations used to confirm the transiting planet system HATS-74A, excluding data from the NASA TESS mission that are shown in Figure 5. Top left: phase-folded unbinned HATSouth light curve. The top panel shows the full light curve, the middle panel shows the light curve zoomed in on the transit, and the bottom panel shows the residuals from the best-fit model zoomed in on the transit. The solid lines show the model fits to the light curves. The dark filled circles show the light curves binned in phase with a bin size of 0.002. Top right: unbinned follow-up transit light curves corrected for instrumental trends fitted simultaneously with the transit model, which is overplotted. The dates, filters, and instruments used are indicated. The residuals 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 up in the fitting procedure to achieve a reduced χ2 of unity, but the uncertainties shown in the plot have not been scaled. Bottom left: radial velocities and bisector span measurements from ESPRESSO/VLT phased with respect to the midtransit time. The top panel shows the phased radial velocity measurements together with the best-fit model. The center-of-mass velocity has been subtracted. The middle panel shows the 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 phased bisector span measurements. Bottom right: color-magnitude diagram (CMD) and spectral energy distribution (SED). The top panel shows the absolute G magnitude vs. the dereddened G − KS 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 Gyr, 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 Gyr of each isochrone labeled on the plot. The filled blue circles show the measured reddening- and distance-corrected values from Gaia DR2 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 DR2) 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.