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A&A
Volume 633, January 2020
Article Number A30
Number of page(s) 12
Section Planets and planetary systems
DOI https://doi.org/10.1051/0004-6361/201936532
Published online 03 January 2020

© ESO 2019

1 Introduction

After almost 20 yr of initially pioneering and then systematic operations, ground-based surveys, based on single or on an array of small automated telescopes or telephoto lenses, have made a huge contribution to the discovery of exoplanets. They open the way to current and next generation space-telescope surveys for transiting exoplanets. Nevertheless, the work of robotic telescopes is far from finished as they are exceptionally well-suited to detecting hot giant planets. Given that hot giant planets are known to be relatively rare from both RV surveys (Mayor et al. 2011; Wright et al. 2012) and transit surveys (Fressin et al. 2013; Fulton & Petigura 2018), in order to discover such planets it is necessary to scan the sky with wide-field instruments that are sensitive to various ranges of stellar magnitudes. For this purpose, nearly 10-yr long observational campaigns have been carried out by ground based observatories, equipped with small automated telescopes (e.g. Bakos et al. 2004; Pollacco et al. 2006; Pepper et al. 2007). More recently, this approach of multiple, wide-field, small aperture telescopes has been adopted from a space environment with the successful TESS1 mission (Ricker et al. 2015).

The formation, evolution and possible migration of hot giant exoplanets are complex phenomena, due to many interacting astrophysical processes. Observational constraints are thus necessary to discriminate the best theoretical models among the competing ones that have been proposed. A large sample of giant exoplanets, whose physical properties are well known, is needed for obtaining good statistics, and very accurate measurements of their mass and radius is crucial for this purpose. However, the complete characterization of an exoplanetary system requires, in many cases, additional observational data and modeling.

Recently, the WASP team announced the discovery of a transiting exoplanet orbiting the star WASP-174 (Temple et al. 2018), whose main parameters are summarised in Table 1. This planetary system was reported as composed by a F6 V star and a near-grazing transiting planet, which rotates on a moderately misaligned and (assumed) circular orbit in 4.23 days, but with only an upper limit on the mass (Mp < 1.3 MJup) due to the relatively low precision of the radial velocity measurements over most of the orbital phase (> 50 m s−1). Also the radius of the planet was difficult to constrain precisely (0.7 < Rp∕RJup < 1.7), because the transit is either grazing or near-grazing and does not show the second and third contact points. The planetary nature of the planet was in fact confirmed by taking a continuous series of spectra during a transit event with the HARPS high-resolution spectrograph and performing the Doppler tomographic method (Temple et al. 2018).

Similar to the case of WASP-67b (Hellier et al. 2012), WASP-174b seems to satisfy the criterion for a grazing transiting planet, that is b + (Rp∕R⋆) > 1, where b is the impact parameter. In a such grazing orbit, the second and third contact points are missing and the transit light curve has a V shape, similar to that of an eclipsing binary. Consequently the photometric parameters, like Rp ∕R⋆ and b, are difficult to constrain and we needvery high-quality light curves to reduce the uncertainties to levels similar to those of the other well-studied, non-grazing, transiting exoplanets (≲20%).

WASP-174b was detected independently as a candidate transiting planet from HATSouth2 survey3, and thus we have observations dating back to 2011 for discovery photometry and 2014 for follow-up spectroscopy and photometry. Here, we use these observations, in conjunction with other data, including TESS data, to perform a comprehensive study of the WASP-174 system, which allows us to much better characterize the physical parameters of this planetary system.

Table 1

Astrometric, photometric and spectroscopic parameters for WASP-174.

2 Observations

2.1 The HAT South survey

HATSouth (Bakos et al. 2013) is a three-station network of ground-based, automated wide-field telescopes. The stations are placed in the southern hemisphere, on three different continents (South America, Africa and Australia). Each station hosts two units composed of a single mount, on which four 18 cm Takahashi astrographs are placed; 24 telescopes in total. Each of the six units can monitor a region on the celestial sphere of 8° × 8°. The large separation in longitude of the three stations allows us to monitor the same stellar field for 24 h per day without interruptions, except for bad weather. The images are recorded by Apogee U16M Alta CCD cameras, automatically calibrated and then stored in the HATSouth archive at Princeton University. Aperture photometry is performed for extracting light curves, which are then analysed with the aim to find periodic signals due to transiting exoplanets. Finally, the most promising candidates undergo spectral reconnaissance, radial-velocity (RV) measurements and precise photometric follow-up observations with larger telescopes to confirm they are real exoplanets. The entire process is exhaustively described, step by step, in Bakos et al. (2013) and summarised in most of the previous works of the HATSouth team4.

Table 2

Summary of photometric observations from the HATSouth survey.

thumbnail Fig. 1

Phase-folded unbinned HATSouth light curves for WASP-174. Top panel: full light curve, while middle panel: light curve zoomed-in on the transit. The solid line shows the model fit to the light curve. The residuals of the fit are shown in the bottom panel. The dark filled circles in the bottom panels show the light curves binned in phase with a bin size of 0.002.

2.2 Photometric detection

WASP-174 (aka 2MASS 13031055-4123053, aka HATS700-010) was observed, through a Sloan-r filter, by the HATSouth telescopes between April 2011 and July 2012 (see Table 2 for details). The subsequent analysis of its light curve, which is plotted in Fig. 1, resulted in a typical transiting-planet signal with a period of ≈ 4.23 days. WASP-174 was thus flagged as planetary-system candidate and underwent follow-up observations for confirming its planetary nature.

2.3 Spectroscopic observations

We acquired 16 RV measurements of WASP-174 by using the FEROS high-resolution spectrograph at the MPG 2.2 m telescope. Comprehensive details about the instrument, data reduction, and corresponding RV extracting method can be found in the previous works of the HATSouth team (see footnote #3), and are largely based on the CERES pipeline (Brahm et al. 2017). Details concerning the observations are summarized in Table 3, while the values of the RV measurements are reported in Table A.1 together with those from HARPS and Coralie taken from Temple et al. (2018). The phase-foldedRVs of WASP-174 are plotted in Fig. 2 together with bisector spans (BS). The measurement of the Rossiter-McLaughlin effect by Temple et al. (2018) is highlighted in Fig. 3 (see discussion in Sect. 4).

2.4 Photometric follow-up observations

Broad-band photometric follow-up observations of several transit events of WASP-174b were also obtained with larger telescopes (see Table 4), with the aim to obtain a better determination of the photometric parameters. In particular, a complete transit was simultaneously observed with the AAT 3.9 m and PEST 0.3 m telescopes and another complete transit was recorded with the LCOGT 1 m.

More recently, we obtained high-quality, optical light curves of another transit event, by using the GROND multi-band camera mounted on the MPG 2.2 m telescope at the ESO Observatory in La Silla, during a photometric night with good seeing (≈ 0.5′′). GROND is an instrument which is capable of simultaneous observations in four optical (similar to Sloan g′, r′, i′, z′) and three NIR (J, H, K) passbands (Greiner et al. 2008). It was conceived for observing transient events, but it turned out to be an optimum instrument for monitoring planetary transits too (e.g. Mohler-Fischer et al. 2013). Several points were cut from the final light curves due to tracking issues before and after the transit. Again, details about the telescopes and data reduction are reported in the previous works of theHATSouth team (for the GROND-data reduction, see also Mancini et al. 2019). The corresponding light curves can be examined in Fig. 4.

2.5 Limb darkening and transit depth

We plotted the four optical GROND light curves superimposed in Fig. 5 to highlight the differences of the transit depth among the four passbands. For normal transiting-planet systems, in which the orbital inclination is ≈ 90° and it is possibleto precisely measure the timings of the four contact points, it is well known that the transit depth gradually decreases moving from blue to red bands (e.g. Knutson et al. 2007); actually, the limb radiation of a star is characteristically cooler than that from its centre and, hence, is slightly redder. Here, instead, we observe the opposite effect. Since WASP-174b is a grazing transiting planet, during its transits it only covers the limb of its parent start, which is fainter in blue than in red wavelengths, resulting in shallower eclipses in the bluest bands for this system. This behavior is similar to that of WASP-67b, another grazing transiting planet (Mancini et al. 2014) (see also Perryman et al. 2018, pag. 224).

Table 3

Summary of spectroscopy observations.

thumbnail Fig. 2

Phased high-precision RV measurements for WASP-174. The instruments used are labelled in the plots. Top panel: phased measurements together with our best-fit model. Zero-phase corresponds to the time of mid-transit. The center-of-mass velocity has been subtracted. The solid line shows the best-fitting model (see discussion in Sect. 3). Second panel: velocity O-C residuals from the best fit. Third panel: bisector spans (BS). Note the differentvertical scales of the panels.

2.6 TESS photometry

WASP-174 was also observed by TESS (Ricker et al. 2015) during Sector 10 of its primary mission. Near continuous observations of the target star from 2019-03-29 to 2019-04-22 were obtained through Camera 2, CCD 3 of the spacecraft, and downlinked via the ~30 min cadenced Full Frame Images (FFI).

The light curve was extracted using the calibrated FFIs from the TESS Science Processing Operations Center (Jenkins et al. 2016). A cut out of10 × 10 pixels around the target star was downloaded via the TESScut tool from the Mikulski Archive for Space Telescopes (MAST) archives. Aperture photometry was performed using the lightkurve package (Barentsen et al. 2019), with the aperture manually selected to best avoid the Tmag = 12.7 variable star 24.5′′ away from WASP-174. The light curve was detrended via a set of cubic splines, fitted with the known transits and spacecraft momentum dumps masked out. Finally, the light curve was adjusted for third light blending due to nearby starsvia the TIC-6 catalogue (Stassun et al. 2018). The last step was necessary, because this nearby 12.7-mag star is somewhat variable, causing contamination on the WASP-174 star. While no clear hints of occultation are present, a very clear transitsignal was obtained (Fig. 6), which is in close agreement to the transits presented in the previous sections.

thumbnail Fig. 3

Zoom of Fig. 2 to highlight our fit of the 23 HARPS RVs, which were taken by the WASP team during a transit event (Temple et al. 2018), and the moderately misalignment of the orbit of WASP-174b.

3 Physical properties

The observational data, which were presented in the previous section, were modeled to refine the main physical properties of the WASP-174 system. The modeling was performed following the procedure described in detail in Hartman et al. (2019) with a few modifications that we discuss here. We carry out a joint fit of the available light curves, RV observations, broad-band catalog photometry, and spectroscopically determined stellar atmospheric parameters using a Differential Evolution Markov chain Monte Carlo (DEMCMC) procedure. We constrain the physical parameters of the star (and planet) using two different methods: (1) an isochrone-based method where we use the PARSEC stellar evolution models (Marigo et al. 2017) and perform an interpolation within a pre-computed grid of these isochrones at each step in the Markov chain using the stellar effective temperature, density and metallicity (which are varied in the fit) as look-up parameters; (2) an empirical model where we use the stellar radius (determined from the temperature and luminosity, which is constrained primarily by the Gaia observations) and density to empirically determine the stellar mass. In this paper we differ from Hartman et al. (2019) in using a newer version of the PARSEC models obtained through the CMD v3.2 web-interface5, adopting an updated set of bolometric corrections for the Gaia DR2 photometric bandpasses (Maíz Apellániz & Weiler 2018), and incorporating infrared photometry from the WISE mission (Cutri et al. 2014) into the fit as well. Incorporating the WISE photometry allows for a more direct constraint on the extinction AV, whereas thiswas previously constrained primarily through the MWDUST 3D dust model of the Galaxy (Bovy et al. 2016). We still use the MWDUST model as a prior, but it is less informative on the value than in our previous analyses. To model the Rossiter-McLaughlin effect observed in the HARPS measurements presented by Temple et al. (2018), which we fit in the joint analysis (see Fig. 3), we use the ARoME package (Boué et al. 2013), utilizing the modeling branch appropriate for RV observations obtained through the cross-correlation function (CCF) method. In fitting the TESS light curve, the model is integrated over the 30 min full-frame image exposure time. We also fit the detrended TESS light curve, rather than detrending simultaneously with the fit, see Fig. 6.

One other difference from Hartman et al. (2019) is that we allow the quadratic limb darkening coefficients to vary in the fit, whereas previously we held them fixed to theoretically expected values. Here we allow them to vary, but use the tabulations from Claret et al. (2012, 2013) and Claret (2018) to place Gaussian priors on their values.

The stellar parameters for the star and the planet are shown in Tables 5 and 6, respectively. We reported both the isochrone- and empirical-model results and compared them with those from the discovery paper. The results from the two models are consistent with each other to within 2σ, with the isochrone models being somewhat more precise. We adopt the sets of parameters coming from the isochrone model as the final ones for consistency with our previous works, for which the isochrone was always our default fiducial model. The location of WASP-174 on the absolute G-magnitude versus Gaia DR2 BP − RP color in illustrated in Fig. 7 (top panel), while the broadband spectral energy distribution (SED) fits to the observed bands is plotted in the bottom panel of the same figure.

Our analysis gives a grazing solution with a confidence greater than 5σ, that is b + (Rp∕R⋆) = 1.0628 ± 0.0094, which is larger than 1 and, therefore, indicates that the transits of WASP-174b are grazing. Using plane geometry and circle–circle intersection formulae (Lillo-Box et al. 2015), we estimate that roughly 76% of the planetary disc transits the parent star at each mid-transit time. Specifically, Aecl∕Ap = 0.76 ± 0.12, where Ap is the full area of the disk of the planet, while Aecl is the area of the part of the planetary disk that actually eclipses the parent star.

With our new data, we are able to constrain the mass and radius of the planet. Based on the results from the isochrone model, we find that WASP-174b has Mp = 0.330 ± 0.091 MJup and Rp = 1.437 ± 0.050 RJup, and is therefore a very low-density, inflated hot giant planet with Teq = 1528 ± 17 K. It is worth noting that the empirical model points towards a planet with greater gravity and density, even though the differences versus the fiducial parameters are within the error bars.

Table 4

Summary of photometric follow-up observations.

thumbnail Fig. 4

Unbinned transit light curves for WASP-174. The dates of the events, filters and instruments used are indicated. Light curves following the first are displaced vertically for clarity. Our best fit from the global modeling is shown by the solid lines. The residuals from the best-fitting model are shown on the right-hand-side in the same order as the original light curves. Note the precision of the GROND light curves, which have point-to-point scatters between 0.37 and 0.52 mmag.
thumbnail Fig. 5

Simultaneous four optical light curves of a transit of WASP-174b obtained with GROND. Top panel: individual light-curves with arbitrary offsets for clarity. Bottom panel: all light-curves superimposed for comparison purposes. The passbands and their central wavelengths are labelled. Note how the transit light curve shape changes with wavelength. Contrary to higher-inclination transiting planetary systems, the transit in the g′ band is shallower than the other bands, because the transit is grazing and the limb darkening is stronger at bluer wavelengths. The same effect was observed in only another case, that is WASP-67b (Mancini et al. 2014).
thumbnail Fig. 6

TESSlight curve of WASP-174 and our best fit from the global modeling (solid lines). The full un-phased light curve is plotted in the top panel. Left-hand middle panel: full phase-folded light curve, while left-hand bottom panel: phase-foldedlight curve zoomed-in on the secondary eclipse Right-hand middle panel: phase-folded light curve zoomed-in on the transit, while right-hand bottom panel: corresponding residuals from the best-fitting model.
Table 5

Derived stellar parameters for WASP-174.

Table 6

Orbital and planetary parameters for WASP-174b.

thumbnail Fig. 7

Top panel: color-magnitude diagram of WASP-174 compared to theoretical isochrones (black lines) and stellar evolution tracks (green lines) from the PARSEC models interpolated at its metallicity, which was spectroscopically determined. The stellar mass of each evolution track is reported in green in solar mass units, while the black numbers denote the age of of each isochrone in Gyr. The blue circle shows the measured reddening- and distance-corrected value from Gaia DR2, together with 1σ and 2σ confidence regions (blue lines). Bottom panels: broadband spectral energy distribution (black points) as photometrically measured through the observed filters, compared with model SEDs (gray lines), followed by the O–C residuals from the best-fit model.

4 Summary and discussion

In this paper we have refined the physical parameters of the transiting planetary system WASP-174, which was a HATSouth transiting planet candidate at the time its discovery was announced by the WASP team in Temple et al. (2018). In particular, using the data from the HATSouth survey and those from spectroscopic and photometric follow-up observations, we were able to confirm that the WASP-174b is transiting in front of its parent star every ≈ 4.2 days and the semi-major axis of its orbit is ≈0.055 au. We also confirm the main characteristics of the host star, a F6 V dwarf star with M⋆ = 1.240 ± 0.038 M⊙ and R⋆ = 1.347 ± 0.018 R⊙ (Table 5). Most importantly, we were able to obtain a much better characterization of the physical parameters of the exoplanet WASP-174b with respect to the values reported in Temple et al. (2018), see Table 6 and Fig. 8.

Moreover, while Temple et al. (2018) were not able to precisely distinguish between a grazing or near-grazing solution, we have found that b + (Rp∕R⋆) > 1 at more than 5σ confidence level, which definitively points towards a grazing nature for the WASP-174b transits. We have estimated that at mid-transit roughly 76% of the planetary disk eclipses the host star. The grazing scenario is also suggested by observing the shape and the depth of the grazing transits of WASP-174b (see Fig. 5) that change with the wavelength in a reverse way with respect to normal cases of a planetary transit, where the disk of the planet is entirely inside the disk of its parent star. Here, instead, the transits are grazing and the planet covers only the limb of the star, causing an increasing of the transit depth moving from blue to red bands.

Having measured the RV phase curve of the parent star (see Fig. 2), we have also determined that the mass of WASP-174b is Mp = 0.330 ± 0.091 MJup, which, together with a more precise measurement of its radius, Rp = 1.437 ± 0.050 RJup, indicates that WASP-174b is an extremely low-density giant planet at the border between Saturn- and Jupiter-type planets (Fig. 9). The inflated size of WASP-174b is evident from Fig. 8. Figures 10 and 11 show its position in the radius-gravity and mass-density diagrams of the currently known transiting exoplanets. In the latter diagram, the position of the planet is compared with five different theoretical models, taken from Fortney et al. (2007), having different core of heavy-elements: 0, 10, 25, 50, and 100 Earth mass. The models were estimated for a planet at 0.045 au from a parent star, with an age of 3.16 Gyr. WASP-174b has a density comparable with the model related to core-free planets.

Since WASP-174b is a very inflated planet, it could be a favorable target for probing its atmosphere through the transmission spectroscopy method. An estimation of the expected signal of its transmission spectrum, Aabs, can be generally obtained by deriving the contrast in area between the annular region of the planetary atmosphere and that of the star, during a transit event. This can be obtained from the characteristic length scale of the planetary atmosphere (see e.g. Bento et al. 2014), i.e. A abs = π ( R p +H) 2 −π R p 2 π R ⋆ 2 . \begin{equation*} A_{\textrm{abs}}=\frac{\pi(R_{\textrm{p}}&#x002B;H)^2-\pi R_{\textrm{p}}^2}{\pi R_{\star}^2}.\end{equation*}(1)

In the latter equation H is the pressure scale height of the planetary atmosphere, that is H = kBTeq∕μm gp, where kB is Boltzmann’s constant and μm is the mean molecular weight, for which the value of 2.3 amu is usually adopted for giant-planet atmospheres dominated by H2 and He (Lecavelier des Etangs et al. 2008). Because of the transits of WASP-174b are grazing, we have to slightly modify Eq. (1) for this planet in order to take into account that only a portion of its atmosfere can absorb the light coming from the parent star. This portion is just equal to Aecl∕Ap and, therefore, we have

thumbnail Fig. 12

Parent-star V magnitude as a function of the expected transmission spectral signal of 1 atmospheric scale height for transiting exoplanets. Data are taken from TEPCat. The curves are adopted from Sing (2018) and give an indication of constant values for S/N and spectral resolution (see also Heng & Winn 2015). The numbers in red and blue refer to HST and JWST, respectively. The region of the diagram in which exoplanetary atmospheres are unobservable, due to low S/N, is marked in gray. The position of WASP-174 is highlighted together with those of other selected transiting exoplanets.
thumbnail Fig. 13

Left-hand panel: complete light curves recorded by the LCOGT/sinistro (i) and MPG 2.2 m/GROND (i′, r′, i′, z′, J) are plotted together with the best-fitting models, which were obtained fixing all the parameters except Rp ∕R⋆. Right-hand panel: residual from the best fit models for the corresponding filters.
A abs = π ( R p +H) 2 −π R p 2 π R ⋆ 2 ( A ecl A p ). \begin{equation*} A_{\textrm{abs}}=\frac{\pi(R_{\textrm{p}}&#x002B;H)^2-\pi R_{\textrm{p}}^2}{\pi R_{\star}^2} \left(\frac{A_{\textrm{ecl}}}{A_{\textrm{p}}}\right).\end{equation*}(2)

Assuming that H ≪ Rp, then Eq. (2) is simply A abs = 2 R p k B T eq μ m   g p R ⋆ 2 ( A ecl A p ). \begin{equation*} A_{\textrm{abs}}=\frac{2 R_{\textrm{p}}k_{\textrm{B}}T_{\textrm{eq}}}{\mu_{\textrm{m}}\,g_{\textrm{p}}R_{\star}^2}\left(\frac{A_{\textrm{ecl}}}{A_{\textrm{p}}}\right).\end{equation*}(3)

In order to compare the relative signal-to-noise of WASP-174b with those of the other transiting exoplanets, we plotted the absorption signal, Aabs, against the magnitude of the host stars in Fig. 12. We can see that the expected atmospheric signal for WASP-174b during its transits, in terms of expected S/N, is similar to that of HAT-P-26b, for which evidences of water has been convincingly found with the HST (Wakeford et al. 2017). WASP-174b is, therefore, another interesting close-in giant planet, whose atmospheric composition can be probed via the transmission-spectroscopy technique.

Exploiting our multi-band photometric observations, we attempted to estimate an observational transmission spectrum of WASP-174b. Following the general approach, we made a new fit of each of our complete light curves, which were obtained with the LCGOT/sinistro and the MPG 2.2 m/GROND facilities, including the NIR data, and fixing the parameters to the values reported in Table 6, with the exception of Rp ∕R⋆, whose uncertainties were estimated by performing 20 000 Monte Carlo simulations.

The light curves and the best-fitting models are plotted in Fig. 13, with the exception of the H and K light curves, because the lower values that we obtained from them are not physically justifiable (the data are simply too noisy to extract reliable results).

The values of Rp∕R⋆ are reported in Table 7 and shown in Fig. 14, where the vertical errorbars represent the relative errors in the measurements and the horizontal errorbars are related to the FWHM transmission of the passbands used. Just for illustration, we also plotted a model atmosphere calculated by Fortney et al. (2010) for a giant planet with a surface gravity of gp = 10 ms−2, a base radius of 1.25 RJup at 10 bar, and Teq = 1000 K. Clearly, the quality of the data do not allow to characterize the transmission spectrum of WASP-174b and we can only conclude that our observational points do not indicate any large variation of the radius of the planet and are compatible with a flat transmission spectrum. More accurate data are required for effectively studying the atmospheric composition of WASP-174b.

thumbnail Fig. 8

Masses and radii of the known transiting extrasolar planets. The plot is restricted to exoplanets with values of the mass until 2.5 MJup and radius until 2.0 RJup. Grey points denote values taken from the Transiting Extrasolar Planet Catalogue (TEPCat)5, (Southworth 2011). Their error bars have been suppressed for clarity. The green point with error bars refers to the position of WASP-174b in the diagram (this work), compared to the possible values of the two parameters reported in the discovery paper (light-red box; Temple et al. 2018). Dotted lines show where density is 2.5, 1.0, 0.5, 0.25 and 0.1 ρJup.
thumbnail Fig. 9

Mass-period diagram of all known transiting hot giants, i.e. transiting exoplanets in the mass range 0.1 MJup < Mp < 5 MJup and with an orbital period ≤10 days. The planets are represented by circles, whose size is proportional to their radius. Color indicates equilibrium temperature. The error bars have been suppressed for clarity. The positions of WASP-174b is highlighted. Data taken from TEPCat. The horizontal dashed line indicates the mass limit of Jupiter planets (0.3 MJup) according tothe definition given by Hatzes & Rauer (2015).
thumbnail Fig. 10

Radius-gravity diagram of the currently known transiting exoplanets with precisely measured mass and radius. The grey points denote values taken from TEPCat. Their error bars have been suppressed for clarity. The position of WASP-174bis shown in green with error bars.
thumbnail Fig. 11

Mass-density diagram of the currently known transiting exoplanets with precisely measured mass and radius. The grey points denote values taken from TEPCat. Their error bars have been suppressed for clarity. The position of WASP-174bis shown in green with error bars. Four planetary models, with various heavy-element core masses (10, 25, 50, and 100 Earth mass) and another without a core are plotted for comparison. They were estimated for a planet at 0.045 au from a parent star with an age of 3.16 Gyr (Fortney et al. 2007).
Table 7

Values of Rp∕R⋆ for each of the passbands.

thumbnail Fig. 14

Variation of the planet/star radius ratio with wavelength. The colors are the same as in Fig. 4. The vertical bars represent the errors in the measurements and the horizontal bars show the FWHM transmission of the passbands used. The observational points are compared with an atmosphere model from Fortney et al. (2010). The transmission curve for the Sloan i filter and the total efficiencies of the GROND filters are shown in the bottom panel.

Acknowledgements

Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations have been supported by NASA grants NNX09AB29G, NNX12AH91H, and NNX17AB61G, and follow-up observations have received partial support from grant NSF/AST-1108686. GROND was built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO, and is operated as a PI-instrument at the MPG 2.2 m telescope. L.M. acknowledges support from the University of Rome “Tor Vergata” through “Mission: Sustainability 2017” fund. A.J. acknowledges support from FONDECYT project 1171208, and by the Ministry for the Economy, Development, and Tourism’s Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). K.P. acknowledges support from NASA grants 80NSSC18K1009 and NNX17AB94G. We thank Jorge Lillo-Box, Elyar Sedaghati and the anonymous referee for their suggestions and comments.

Appendix A Additional table

Table A.1

Relative radial velocities and bisector spans for WASP-174.

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1

Transiting Exoplanet Survey Satellite.

2

The HATSouth network is operated by a collaboration consisting of Princeton University (PU), the Max Planck Institute for Astronomy (MPIA), the Australian National University (ANU), and the Pontificia Universidad Católica de Chile (PUC). The station at Las Campanas Observatory (LCO) of the Carnegie Institute is operated by PU in conjunction with PUC, the station at the High Energy Spectroscopic Survey (H.E.S.S.) site is operated in conjunction with MPIA, and the station at Siding Spring Observatory (SSO) is operated jointly with ANU. Based on observations made with the MPG 2.2 m Telescope at the ESO Observatory in La Silla. Based in part on observations made with TESS, the facilities of the Las Cumbres Observatory Global Telescope, the Perth Exoplanet Survey Telescope, and the 3.9 m Anglo-Australian Telescope at SSO.

4

The complete list of the HATSouth discovery papers is available on http://hatsouth.org/planets/

All Tables

Table 1

Astrometric, photometric and spectroscopic parameters for WASP-174.

In the text
Table 2

Summary of photometric observations from the HATSouth survey.

In the text
Table 3

Summary of spectroscopy observations.

In the text
Table 4

Summary of photometric follow-up observations.

In the text
Table 5

Derived stellar parameters for WASP-174.

In the text
Table 6

Orbital and planetary parameters for WASP-174b.

In the text
Table 7

Values of Rp∕R⋆ for each of the passbands.

In the text
Table A.1

Relative radial velocities and bisector spans for WASP-174.

In the text

All Figures

thumbnail Fig. 1

Phase-folded unbinned HATSouth light curves for WASP-174. Top panel: full light curve, while middle panel: light curve zoomed-in on the transit. The solid line shows the model fit to the light curve. The residuals of the fit are shown in the bottom panel. The dark filled circles in the bottom panels show the light curves binned in phase with a bin size of 0.002.
In the text
thumbnail Fig. 2

Phased high-precision RV measurements for WASP-174. The instruments used are labelled in the plots. Top panel: phased measurements together with our best-fit model. Zero-phase corresponds to the time of mid-transit. The center-of-mass velocity has been subtracted. The solid line shows the best-fitting model (see discussion in Sect. 3). Second panel: velocity O-C residuals from the best fit. Third panel: bisector spans (BS). Note the differentvertical scales of the panels.
In the text
thumbnail Fig. 3

Zoom of Fig. 2 to highlight our fit of the 23 HARPS RVs, which were taken by the WASP team during a transit event (Temple et al. 2018), and the moderately misalignment of the orbit of WASP-174b.
In the text
thumbnail Fig. 4

Unbinned transit light curves for WASP-174. The dates of the events, filters and instruments used are indicated. Light curves following the first are displaced vertically for clarity. Our best fit from the global modeling is shown by the solid lines. The residuals from the best-fitting model are shown on the right-hand-side in the same order as the original light curves. Note the precision of the GROND light curves, which have point-to-point scatters between 0.37 and 0.52 mmag.
In the text
thumbnail Fig. 5

Simultaneous four optical light curves of a transit of WASP-174b obtained with GROND. Top panel: individual light-curves with arbitrary offsets for clarity. Bottom panel: all light-curves superimposed for comparison purposes. The passbands and their central wavelengths are labelled. Note how the transit light curve shape changes with wavelength. Contrary to higher-inclination transiting planetary systems, the transit in the g′ band is shallower than the other bands, because the transit is grazing and the limb darkening is stronger at bluer wavelengths. The same effect was observed in only another case, that is WASP-67b (Mancini et al. 2014).
In the text
thumbnail Fig. 6

TESSlight curve of WASP-174 and our best fit from the global modeling (solid lines). The full un-phased light curve is plotted in the top panel. Left-hand middle panel: full phase-folded light curve, while left-hand bottom panel: phase-foldedlight curve zoomed-in on the secondary eclipse Right-hand middle panel: phase-folded light curve zoomed-in on the transit, while right-hand bottom panel: corresponding residuals from the best-fitting model.
In the text
thumbnail Fig. 7

Top panel: color-magnitude diagram of WASP-174 compared to theoretical isochrones (black lines) and stellar evolution tracks (green lines) from the PARSEC models interpolated at its metallicity, which was spectroscopically determined. The stellar mass of each evolution track is reported in green in solar mass units, while the black numbers denote the age of of each isochrone in Gyr. The blue circle shows the measured reddening- and distance-corrected value from Gaia DR2, together with 1σ and 2σ confidence regions (blue lines). Bottom panels: broadband spectral energy distribution (black points) as photometrically measured through the observed filters, compared with model SEDs (gray lines), followed by the O–C residuals from the best-fit model.
In the text
thumbnail Fig. 8

Masses and radii of the known transiting extrasolar planets. The plot is restricted to exoplanets with values of the mass until 2.5 MJup and radius until 2.0 RJup. Grey points denote values taken from the Transiting Extrasolar Planet Catalogue (TEPCat)5, (Southworth 2011). Their error bars have been suppressed for clarity. The green point with error bars refers to the position of WASP-174b in the diagram (this work), compared to the possible values of the two parameters reported in the discovery paper (light-red box; Temple et al. 2018). Dotted lines show where density is 2.5, 1.0, 0.5, 0.25 and 0.1 ρJup.
In the text
thumbnail Fig. 9

Mass-period diagram of all known transiting hot giants, i.e. transiting exoplanets in the mass range 0.1 MJup < Mp < 5 MJup and with an orbital period ≤10 days. The planets are represented by circles, whose size is proportional to their radius. Color indicates equilibrium temperature. The error bars have been suppressed for clarity. The positions of WASP-174b is highlighted. Data taken from TEPCat. The horizontal dashed line indicates the mass limit of Jupiter planets (0.3 MJup) according tothe definition given by Hatzes & Rauer (2015).
In the text
thumbnail Fig. 10

Radius-gravity diagram of the currently known transiting exoplanets with precisely measured mass and radius. The grey points denote values taken from TEPCat. Their error bars have been suppressed for clarity. The position of WASP-174bis shown in green with error bars.
In the text
thumbnail Fig. 11

Mass-density diagram of the currently known transiting exoplanets with precisely measured mass and radius. The grey points denote values taken from TEPCat. Their error bars have been suppressed for clarity. The position of WASP-174bis shown in green with error bars. Four planetary models, with various heavy-element core masses (10, 25, 50, and 100 Earth mass) and another without a core are plotted for comparison. They were estimated for a planet at 0.045 au from a parent star with an age of 3.16 Gyr (Fortney et al. 2007).
In the text
thumbnail Fig. 12

Parent-star V magnitude as a function of the expected transmission spectral signal of 1 atmospheric scale height for transiting exoplanets. Data are taken from TEPCat. The curves are adopted from Sing (2018) and give an indication of constant values for S/N and spectral resolution (see also Heng & Winn 2015). The numbers in red and blue refer to HST and JWST, respectively. The region of the diagram in which exoplanetary atmospheres are unobservable, due to low S/N, is marked in gray. The position of WASP-174 is highlighted together with those of other selected transiting exoplanets.
In the text
thumbnail Fig. 13

Left-hand panel: complete light curves recorded by the LCOGT/sinistro (i) and MPG 2.2 m/GROND (i′, r′, i′, z′, J) are plotted together with the best-fitting models, which were obtained fixing all the parameters except Rp ∕R⋆. Right-hand panel: residual from the best fit models for the corresponding filters.
In the text
thumbnail Fig. 14

Variation of the planet/star radius ratio with wavelength. The colors are the same as in Fig. 4. The vertical bars represent the errors in the measurements and the horizontal bars show the FWHM transmission of the passbands used. The observational points are compared with an atmosphere model from Fortney et al. (2010). The transmission curve for the Sloan i filter and the total efficiencies of the GROND filters are shown in the bottom panel.
In the text

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