Author: "Gillon, M." - Searchworks@Jio Institute Digital Library Search Results

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1,916 results on '"Gillon, M."'

301. Improved parameters for the transiting planet HD 17156b: a high-density giant planet with a very eccentric orbit

Author: Gillon, M., Triaud, A. H. M. J., Mayor, M., Queloz, D., Udry, S., and North, P.
Subjects: Astrophysics
Abstract: We report high-precision transit photometry for the recently detected planet HD 17156b. Using these new data with previously published transit photometry and radial velocity measurements, we perform a combined analysis based on a Markov Chain Monte Carlo approach. The resulting mass M_p = 3.09 (+0.22-0.17) M_Jup and radius R_p = 1.23 (+0.17-0.20) R_Jup for the planet places it at the outer edge of the density distribution of known transiting planets with rho_p = 1.66 (+1.37-0.60) rho_Jup. The obtained transit ephemeris is T_tr = 2454438.48271 (+0.00077-0.00057) + N x 21.21747 (+0.00070-0.00067) BJD. The derived plausible tidal circularization time scales for HD 17156b are larger than the age of the host star. The measured high orbital eccentricity e = 0.6719 (+0.0052-0.0063) can thus not be interpreted as the clear sign of the presence of another body in the system., Comment: 6 pages, 3 figures, 1 table. Accepted for publication in A&A
Published: 2007
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302. OGLE-TR-211 - a new transiting inflated hot Jupiter from the OGLE survey and ESO LP666 spectroscopic follow-up program

Author: Udalski, A., Pont, F., Naef, D., Melo, C., Bouchy, F., Santos, N. C., Moutou, C., Diaz, R. F., Gieren, W., Gillon, M., Hoyer, S., Mayor, M., Mazeh, T., Minniti, D., Pietrzynski, G., Queloz, D., Ramirez, S., Ruiz, M. T., Tamuz, O., Udry, S., Zoccali, M., Kubiak, M., Szymanski, M. K., Soszynski, I., Szewczyk, O., Ulaczyk, K., and Wyrzykowski, L.
Subjects: Astrophysics
Abstract: We present results of the photometric campaign for planetary and low-luminosity object transits conducted by the OGLE survey in 2005 season (Campaign #5). About twenty most promising candidates discovered in these data were subsequently verified spectroscopically with the VLT/FLAMES spectrograph. One of the candidates, OGLE-TR-211, reveals clear changes of radial velocity with small amplitude of 82 m/sec, varying in phase with photometric transit ephemeris. Thus, we confirm the planetary nature of the OGLE-TR-211 system. Follow-up precise photometry of OGLE-TR-211 with VLT/FORS together with radial velocity spectroscopy supplemented with high resolution, high S/N VLT/UVES spectra allowed us to derive parameters of the planet and host star. OGLE-TR-211b is a hot Jupiter orbiting a F7-8 spectral type dwarf star with the period of 3.68 days. The mass of the planet is equal to 1.03+/-0.20 M_Jup while its radius 1.36+0.18-0.09 R_Jup. The radius is about 20% larger than the typical radius of hot Jupiters of similar mass. OGLE-TR-211b is, then, another example of inflated hot Jupiters - a small group of seven exoplanets with large radii and unusually small densities - objects being a challenge to the current models of exoplanets., Comment: 6 pages. Submitted to Astronomy and Astrophysics
Published: 2007
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303. A transiting planet among 23 new near-threshold candidates from the OGLE survey - OGLE-TR-182

Author: Pont, F., Tamuz, O., Udalski, A., Mazeh, T., Bouchy, F., Melo, C., Naef, D., Santos, N. C., Moutou, C., Diaz, R., Gieren, W., Gillon, M., Hoyer, S., Kubiak, M., Mayor, M., Minniti, D., Pietrzynski, G., Queloz, D., Ramirez, S., Ruiz, M. T., Soszynski, I., Szewczyk, O., Szymanski, M. K., Udry, S., Ulaczyk, K., Wyrzykowski, L., and Zoccali, M.
Subjects: Astrophysics
Abstract: By re-processing the data of the second season of the OGLE survey for planetary transits and adding new mesurements on the same fields gathered in subsequent years with the OGLE telescope, we have identified 23 new transit candidates, recorded as OGLE-TR-178 to OGLE-TR-200. We studied the nature of these objects with the FLAMES/UVES multi-fiber spectrograph on the VLT. One of the candidates, OGLE-TR-182, was confirmed as a transiting gas giant planet on a 4-day orbit. We characterised it with further observations using the FORS1 camera and UVES spectrograph on the VLT. OGLE-TR-182b is a typical ``hot Jupiter'' with an orbital period of 3.98 days, a mass of 1.01 +- 0.15 MJup and a radius of 1.13 (+0.24-0.08) RJup. Confirming this transiting planet required a large investment in telescope time with the best instruments available, and we comment on the difficulty of the confirmation process for transiting planets in the OGLE survey. We delienate the zone were confirmation is difficult or impossible, and discuss the implications for the Corot space mission in its quest for transiting telluric planets., Comment: 7 pages, submitted to Astronomy and Astrophysics
Published: 2007
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304. Characterization of the hot Neptune GJ 436b with Spitzer and ground-based observations

Author: Demory, B. -O., Gillon, M., Barman, T., Bonfils, X., Mayor, M., Mazeh, T., Queloz, D., Udry, S., Bouchy, F., Delfosse, X., Forveille, T., Mallmann, F., Pepe, F., and Perrier, C.
Subjects: Astrophysics
Abstract: We present Spitzer Space Telescope infrared photometry of a secondary eclipse of the hot Neptune GJ436b. The observations were obtained using the 8-micron band of the InfraRed Array Camera (IRAC). The data spanning the predicted time of secondary eclipse show a clear flux decrement with the expected shape and duration. The observed eclipse depth of 0.58 mmag allows us to estimate a blackbody brightness temperature of T_p = 717 +- 35 K at 8 microns. We compare this infrared flux measurement to a model of the planetary thermal emission, and show that this model reproduces properly the observed flux decrement. The timing of the secondary eclipse confirms the non-zero orbital eccentricity of the planet, while also increasing its precision (e = 0.14 +- 0.01). Additional new spectroscopic and photometric observations allow us to estimate the rotational period of the star and to assess the potential presence of another planet., Comment: Accepted for publication in A&A on 11/09/2007; 7 pages, 6 figures
Published: 2007
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305. Accurate Spitzer infrared radius measurement for the hot Neptune GJ 436b

Author: Gillon, M., Demory, B. -O., Barman, T., Bonfils, X., Mazeh, T., Pont, F., Udry, S., Mayor, M., and Queloz, D.
Subjects: Astrophysics
Abstract: We present Spitzer Space Telescope infrared photometry of a primary transit of the hot Neptune GJ 436b. The observations were obtained using the 8 microns band of the InfraRed Array Camera (IRAC). The high accuracy of the transit data and the weak limb-darkening in the 8 microns IRAC band allow us to derive (assuming M = 0.44 +- 0.04 Msun for the primary) a precise value for the planetary radius (4.19 +0.21-0.16 Rearth), the stellar radius (0.463 +0.022-0.017 Rsun), the orbital inclination (85.90 +0.19-0.18 degrees) and transit timing (2454280.78186 +0.00015-0.00008 HJD). Assuming current planet models, an internal structure similar to that of Neptune with a small H/He envelope is necessary to account for the measured radius of GJ 436b., Comment: Accepted for publication in A&A on 21/07/2007; 5 pages, 3 figures
Published: 2007
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306. Detection of transits of the nearby hot Neptune GJ 436 b

Author: Gillon, M., Pont, F., Demory, B. -O., Mallmann, F., Mayor, M., Mazeh, T., Queloz, D., Shporer, A., Udry, S., and Vuissoz, C.
Subjects: Astrophysics
Abstract: This Letter reports on the photometric detection of transits of the Neptune-mass planet orbiting the nearby M-dwarf star GJ 436. It is by far the closest, smallest and least massive transiting planet detected so far. Its mass is slightly larger than Neptune's at M = 22.6 +- 1.9 M_earth. The shape and depth of the transit lightcurves show that it is crossing the host star disc near its limb (impact parameter 0.84 +- 0.03) and that the planet size is comparable to that of Uranus and Neptune, R = 25200 +- 2200 km = 3.95 +- 0.35 R_earth. Its main constituant is therefore very likely to be water ice. If the current planet structure models are correct, an outer layer of H/He constituting up to ten percent in mass is probably needed on top of the ice to account for the observed radius., Comment: 4 pages, 3 figures. Accepted for publication in A&A Letters
Published: 2007
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307. The HARPS search for southern extra-solar planets. X. A m sin i = 11 Mearth planet around the nearby spotted M dwarf GJ 674

Author: Bonfils, X., Mayor, M., Delfosse, X., Forveille, T., Gillon, M., Perrier, C., Udry, S., Bouchy, F., Lovis, C., Pepe, F., Queloz, D., Santos, N. C., and Bertaux, J. -L.
Subjects: Astrophysics
Abstract: Context: How planet properties depend on stellar mass is a key diagnostic of planetary formation mechanisms. Aims: This motivates planet searches around stars which are significantly more massive or less massive than the Sun, and in particular our radial velocity search for planets around very-low mass stars. Methods: As part of that program, we obtained measurements of GJ 674, an M2.5 dwarf at d=4.5 pc, which have a dispersion much in excess of their internal errors. An intensive observing campaign demonstrates that the excess dispersion is due to two superimposed coherent signals, with periods of 4.69 and 35 days. Results: These data are well described by a 2-planet Keplerian model where each planet has a ~11 Mearth minimum mass. A careful analysis of the (low level) magnetic activity of GJ 674 however demonstrates that the 35-day period coincides with the stellar rotation period. This signal therefore originates in a spot inhomogeneity modulated by stellar rotation. The 4.69-day signal on the other hand is caused by a bona-fide planet, GJ 674b. Conclusion: Its detection adds to the growing number of Neptune-mass planets around M-dwarfs, and reinforces the emerging conclusion that this mass domain is much more populated than the jovian mass range. We discuss the metallicity distributions of M dwarf with and without planets and find a low 11% probability that they are drawn from the same parent distribution. Moreover, we find tentative evidence that the host star metallicity correlates with the total mass of their planetary system., Comment: submitted to A&A (January 09, 2007)
Published: 2007
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308. The transiting planet OGLE-TR-132b revisited with new spectroscopy and deconvolution photometry

Author: Gillon, M., Pont, F., Moutou, C., Santos, N. C., Bouchy, F., Hartman, J. D., Mayor, M., Melo, C., Queloz, D., Udry, S., and Magain, P.
Subjects: Astrophysics
Abstract: OGLE-TR-132b transits a very metal-rich F dwarf about 2000 pc from the Sun, in the Galactic disc towards Carina. It orbits very close to its host star (a = 0.03 AU) and has an equilibrium temperature of nearly 2000 K. Using rapid-cadence transit photometry from the FORS2 camera on the VLT and SUSI2 on the NTT, and high-resolution spectroscopy with UVES on the VLT, we refine the shape of the transit light curve and the parameters of the system. In particular, we improve the planetary radius estimate, R=1.18 +- 0.07 R_J and provide very precise ephemeris, T_tr=2453142.59123 +- 0.0003 BJD and P=1.689868 +- 0.000003 days. The obtained planetary mass is 1.14 +- 0.12 M_J. Our results give a slightly smaller and lighter star, and bigger planet, than previous values. As the VLT/FORS2 light curve obtained in this analysis with the deconvolution photometry algorithm DECPHOT shows a transit depth in disagreement with the one obtained by a previous study using the same data, we analyze them with two other reduction methods (aperture and image subtraction). The light curves obtained with the three methods are in good agreement, though deconvolution-based photometry is significantly more precise. It appears from these results that the smaller transit depth obtained in the previous study was due to a normalisation problem inherent to the reduction procedure used., Comment: 7 pages, 6 figures. Accepted for publication in A&A
Published: 2007
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309. DECPHOT: an optimal deconvolution-based photometric reduction method

Author: Gillon, M., Magain, P., Chantry, V., Letawe, G., Sohy, S., Courbin, F., Pont, F., and Moutou, C.
Subjects: Astrophysics
Abstract: A high accuracy photometric reduction method is needed to take full advantage of the potential of the transit method for the detection and characterization of exoplanets, especially in deep crowded fields. In this context, we present DECPHOT, a new deconvolution-based photometry algorithm able to deal with a very high level of crowding and large variations of seeing. It also increases the resolution of astronomical images, an important advantage for the discrimination of false positives in transit photometry., Comment: 6 pages, 2 figures; to be published in Transiting Extrasolar Planets Workshop, Eds: Cristina Afonso, David Weldrake & Thomas Henning
Published: 2007

310. On the influence of blends on the potential of ground-based transit surveys

Author: Gillon, M. and Magain, P.
Subjects: Astrophysics
Abstract: Transit surveys have to observe many stars all at once in order to compensate for the rarity of the searched events. Such surveys, especially the ones observing a deep field of view and/or broadening their stellar images, have to deal with a relatively high level of crowding. This crowding could lead to a reduction of the number of detectable transits, and the estimation of the potential of such surveys without taking into account the influence of blends could give overoptimistic results. We have developed a code which allows to estimate the extent by which such a survey is affected by the crowding of the field of view. Our results show that the influence of blends is important only for severe levels of crowding and is in general much less crucial than the influence of red noise., Comment: 6 pages, 4 figures; to be published in Transiting Extrasolar Planets Workshop, Eds: Cristina Afonso, David Weldrake & Thomas Henning
Published: 2007

311. WASP-1b and WASP-2b: Two new transiting exoplanets detected with SuperWASP and SOPHIE

Author: Cameron, A. Collier, Bouchy, F., Hebrard, G., Maxted, P., Pollacco, D., Pont, F., Skillen, I., Smalley, B., Street, R. A., West, R. G., Wilson, D. M., Aigrain, S., Christian, D. J., Clarkson, W. I., Enoch, B., Evans, A., Fitzsimmons, A., Fleenor, M., Gillon, M., Haswell, C. A., Hebb, L., Hellier, C., Hodgkin, S. T., Horne, K., Irwin, J., Kane, S. R., Keenan, F. P., Loeillet, B., Lister, T. A., Mayor, M., Moutou, C., Norton, A. J., Osborne, J., Parley, N., Queloz, D., Ryans, R., Triaud, A. H. M. J., Udry, S., and Wheatley, P. J.
Subjects: Astrophysics
Abstract: We have detected low-amplitude radial-velocity variations in two stars, USNO-B1.0 1219-0005465 (GSC 02265-00107 = WASP-1) and USNO-B1.0 0964-0543604 (GSC 00522-01199 = WASP-2). Both stars were identified as being likely host stars of transiting exoplanets in the 2004 SuperWASP wide-field transit survey. Using the newly-commissioned radial-velocity spectrograph SOPHIE at the Observatoire de Haute-Provence, we found that both objects exhibit reflex orbital radial-velocity variations with amplitudes characteristic of planetary-mass companions and in-phase with the photometric orbits. Line-bisector studies rule out faint blended binaries as the cause of either the radial-velocity variations or the transits. We perform preliminary spectral analyses of the host stars, which together with their radial-velocity variations and fits to the transit light curves, yield estimates of the planetary masses and radii. WASP-1b and WASP-2b have orbital periods of 2.52 and 2.15 days respectively. Given mass estimates for their F7V and K1V primaries we derive planet masses 0.80 to 0.98 and 0.81 to 0.95 times that of Jupiter respectively. WASP-1b appears to have an inflated radius of at least 1.33 R_Jup, whereas WASP-2b has a radius in the range 0.65 to 1.26 R_Jup., Comment: 7 pages, 3 figures, MNRAS (accepted); new Table 1 added to summarise results for all stars surveyed; new plots of unphased RV curves added; text updated in response to referee's comments
Published: 2006
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312. A deconvolution-based algorithm for crowded field photometry with unknown Point Spread Function

Author: Magain, P., Courbin, F., Gillon, M., Sohy, S., Letawe, G., Chantry, V., and Letawe, Y.
Subjects: Astrophysics
Abstract: A new method is presented for determining the Point Spread Function (PSF) of images that lack bright and isolated stars. It is based on the same principles as the MCS (Magain, Courbin, Sohy, 1998) image deconvolution algorithm. It uses the information contained in all stellar images to achieve the double task of reconstructing the PSFs for single or multiple exposures of the same field and to extract the photometry of all point sources in the field of view. The use of the full information available allows to construct an accurate PSF. The possibility to simultaneously consider several exposures makes it very well suited to the measurement of the light curves of blended point sources from data that would be very difficult or even impossible to analyse with traditional PSF fitting techniques. The potential of the method for the analysis of ground-based and space-based data is tested on artificial images and illustrated by several examples, including HST/NICMOS images of a lensed quasar and VLT/ISAAC images of a faint blended Mira star in the halo of the giant elliptical galaxy NGC5128 (Cen A)., Comment: Institutes: (1) Institut d'Astrophysique et de Geophysique, Universite de Liege, allee du 6 Aout 17, B-4000 Liege, Belgium; (2) Ecole Polytechnique Federale de Lausanne (EPFL), Laboratoire d'Astrophysique, Observatoire, CH-1290 Sauverny, Switzerland; (3) Observatoire de Geneve, 51 Chemin des Maillettes, CH-1290 Sauverny, Switzerland. 8 pages, 8 figures. Accepted for publication in A&A
Published: 2006
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313. High accuracy transit photometry of the planet OGLE-TR-113b with a new deconvolution-based method

Author: Gillon, M., Pont, F., Moutou, C., Bouchy, F., Courbin, F., Sohy, S., and Magain, P.
Subjects: Astrophysics
Abstract: A high accuracy photometry algorithm is needed to take full advantage of the potential of the transit method for the characterization of exoplanets, especially in deep crowded fields. It has to reduce to the lowest possible level the negative influence of systematic effects on the photometric accuracy. It should also be able to cope with a high level of crowding and with large scale variations of the spatial resolution from one image to another. A recent deconvolution-based photometry algorithm fulfills all these requirements, and it also increases the resolution of astronomical images, which is an important advantage for the detection of blends and the discrimination of false positives in transit photometry. We made some changes to this algorithm in order to optimize it for transit photometry and used it to reduce NTT/SUSI2 observations of two transits of OGLE-TR-113b. This reduction has led to two very high precision transit light curves with a low level of systematic residuals, used together with former photometric and spectroscopic measurements to derive new stellar and planetary parameters in excellent agreement with previous ones, but significantly more precise., Comment: 8 pages, 4 figures
Published: 2006
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314. High precision determination of the atmospheric parameters and abundances of the COROT main targets

Author: Gillon, M. and Magain, P.
Subjects: Astrophysics
Abstract: One of the main goals of the COROT mission is to get precise photometric observations of selected bright stars in order to allow the modelling of their interior through asteroseismology. However, in order to interpret the asteroseismological data, the effective temperature, surface gravity, and chemical composition of the stars must be known with sufficient accuracy. To carry out this task, we have developed a spectroscopic method called APASS (Atmospheric Parameters and Abundances from Synthetic Spectra) which allows precise analysis of stars with a moderate to high rotational velocity, which is the case for most primary COROT targets. Our method is based on synthetic spectra and works differentially with respect to the Sun. Using high signal-to-noise spectra and the APASS method, we determined the atmospheric parameters and chemical abundances of 13 primary COROT targets. Our results agree well with those obtained by Bruntt using his software VWA and with those obtained with the software TEMPLOGG. However, in both cases, our error bars are significantly smaller than those of other methods. Our effective temperatures are also in excellent agreement with those obtained with the IR photometry method. For five stars with relatively low rotational velocity, we also performed an analysis with a classical equivalent-width method to test agreement with APASS results. We show that equivalent-width measurements by Gaussian or Voigt profile-fitting are sensitive to the rotational broadening, leading to systematic errors whenever the projected rotation velocity is non-negligible. The APASS method appears superior in all cases and should thus be preferred., Comment: 12 pages, 6 figures, 4 tables. Accepted in A&A
Published: 2005
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315. On the potential of extrasolar planet transit surveys

Author: Gillon, M., Courbin, F., Magain, P., and Borguet, B.
Subjects: Astrophysics
Abstract: We analyse the respective benefits and drawbacks of ground-based and space-based transit surveys for extrasolar planets. Based on simple but realistic assumptions about the fraction of lower main sequence stars harboring telluric and giant planets within the outer limit of the habitable zone, we predict the harvests of fictitious surveys with three existing wide field optical and near-IR cameras: the CFHT-Megacam, SUBARU-Suprime and VISTA-IR. An additional promising instrument is considered, VISTA-Vis, currently under development. The results are compared with the harvests predicted under exactly the same assumptions, for the space missions COROT and KEPLER. We show that ground-based wide field surveys may discover more giant planets than space missions. However, space surveys seem to constitute the best strategy to search for telluric planets. In this respect, the KEPLER mission appears 50 times more efficient than any of the ground--based surveys considered here. KEPLER might even discover telluric planets in the habitable zone of their host star., Comment: accepted in AA
Published: 2005
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316. Abundance analysis of targets for the COROT / MONS asteroseismology missions II. Abundance analysis of the COROT main targets

Author: Bruntt, H., Bikmaev, I. F., Catala, C., Solano, E., Gillon, M., Magain, P., Veer-Menneret, C. Van't, Stuetz, Ch., Weiss, W. W., Ballereau, D., Bouret, J. C., Charpinet, S., Hua, T., Katz, D., Lignieres, F., and Lueftinger, T.
Subjects: Astrophysics
Abstract: One of the goals of the ground-based support program for the COROT and Roemer satellite missions is to characterize suitable target stars for the part of the missions dedicated to asteroseismology. We present the detailed abundance analysis of nine of the potential COROT main targets using the semi-automatic software VWA. For two additional COROT targets we could not perform the analysis due to the high rotational velocity of these stars. For five stars with low rotational velocity we have also performed abundance analysis by a classical equivalent width method in order to test the reliability of the VWA software. The agreement between the different methods is good. We find that it is necessary to measure abundances extracted from each line relative to the abundances found from a spectrum of the Sun in order to remove systematic errors. We have constrained the global atmospheric parameters Teff, log g, and [Fe/H] to within 70-100 K, 0.1-0.2 dex, and 0.1 dex for five stars which are slow rotators (v sin i < 15 km/s). For most of the stars stars we find good agreement with the parameters found from line depth ratios, H-alpha lines, Str\"omgren indices, previous spectroscopic studies, and also log g determined from the HIPPARCOS parallaxes. For the fast rotators v sin i > 60 km/s it is not possible to constrain the atmospheric parameters., Comment: 14 pages, 6 figures, accepted 11th of June 2004 by A&A
Published: 2004
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317. EPOXI: COMET 103P/HARTLEY 2 OBSERVATIONS FROM A WORLDWIDE CAMPAIGN

Author: Meech, KJ, A’Hearn, MF, Adams, JA, Bacci, P, Bai, J, Barrera, L, Battelino, M, Bauer, JM, Becklin, E, Bhatt, B, Biver, N, Bockelée-Morvan, D, Bodewits, D, Böhnhardt, H, Boissier, J, Bonev, BP, Borghini, W, Brucato, JR, Bryssinck, E, Buie, MW, Canovas, H, Castellano, D, Charnley, SB, Chen, WP, Chiang, P, Choi, Y-J, Christian, DJ, Chuang, Y-L, Cochran, AL, Colom, P, Combi, MR, Coulson, IM, Crovisier, J, Dello Russo, N, Dennerl, K, DeWahl, K, DiSanti, MA, Facchini, M, Farnham, TL, Fernández, Y, Florén, HG, Frisk, U, Fujiyoshi, T, Furusho, R, Fuse, T, Galli, G, García-Hernández, DA, Gersch, A, Getu, Z, Gibb, EL, Gillon, M, Guido, E, Guillermo, RA, Hadamcik, E, Hainaut, O, Hammel, HB, Harker, DE, Harmon, JK, Harris, WM, Hartogh, P, Hashimoto, M, Häusler, B, Herter, T, Hjalmarson, A, Holland, ST, Honda, M, Hosseini, S, Howell, ES, Howes, N, Hsieh, HH, Hsiao, H-Y, Hutsemékers, D, Immler, SM, Jackson, WM, Jeffers, SV, Jehin, E, Jones, TJ, de Juan Ovelar, M, Kaluna, HM, Karlsson, T, Kawakita, H, Keane, JV, Keller, LD, Kelley, MS, Kinoshita, D, Kiselev, NN, Kleyna, J, Knight, MM, Kobayashi, H, Kobulnicky, HA, Kolokolova, L, Kreiny, M, Kuan, Y-J, Küppers, M, Lacruz, JM, Landsman, WB, Lara, LM, Lecacheux, A, Levasseur-Regourd, AC, and Li, B
Subjects: comets: individual, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: Earth- and space-based observations provide synergistic information for space mission encounters by providing data over longer timescales, at different wavelengths and using techniques that are impossible with an in situ flyby. We report here such observations in support of the EPOXI spacecraft flyby of comet 103P/Hartley 2. The nucleus is small and dark, and exhibited a very rapidly changing rotation period. Prior to the onset of activity, the period was 16.4hr. Starting in 2010 August the period changed from 16.6hr to near 19hr in December. With respect to dust composition, most volatiles and carbon and nitrogen isotope ratios, the comet is similar to other Jupiter-family comets. What is unusual is the dominance of CO 2 -driven activity near perihelion, which likely persists out to aphelion. Near perihelion the comet nucleus was surrounded by a large halo of water-ice grains that contributed significantly to the total water production. © 2011. The American Astronomical Society. All rights reserved..
Published: 2011

318. Characterising TOI-732 b and c: New insights into the M-dwarf radius and density valley

Author: Bonfanti, A., primary, Brady, M., additional, Wilson, T.G., additional, Venturini, J., additional, Egger, J.A., additional, Brandeker, A., additional, Sousa, S.G., additional, Lendl, M., additional, Simon, A.E., additional, Queloz, D., additional, Olofsson, G., additional, Adibekyan, V., additional, Alibert, Y., additional, Fossati, L., additional, Hooton, M.J., additional, Kubyshkina, D., additional, Luque, R., additional, Murgas, F., additional, Mustill, A.J., additional, Santos, N.C., additional, Van Grootel, V., additional, Alonso, R., additional, Asquier, J., additional, Bandy, T., additional, Bárczy, T., additional, Barrado Navascues, D., additional, Barros, S.C., additional, Baumjohann, W., additional, Bean, J., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Bergomi, M., additional, Billot, N., additional, Borsato, L., additional, Broeg, C., additional, Collier Cameron, A., additional, Csizmadia, Sz., additional, Cubillos, P.E., additional, Davies, M.B., additional, Deleuil, M., additional, Deline, A., additional, Delrez, L., additional, Demangeon, O.D.S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Fortier, A., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Günther, M.N., additional, Heitzmann, A., additional, Helling, Ch., additional, Hoyer, S., additional, Isaak, K.G., additional, Kasper, D., additional, Kiss, L., additional, Lam, K.W.F., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Magrin, D., additional, Maxted, P.F.L., additional, Mordasini, C., additional, Nascimbeni, V., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Scandariato, G., additional, Ségransan, D., additional, Seifahrt, A., additional, Smith, A.M.S., additional, Stalport, M., additional, Stefánsson, G., additional, Steinberger, M., additional, Stürmer, J., additional, Szabó, M. Gy., additional, Thomas, N., additional, Udry, S., additional, Villaver, E., additional, Walton, N.A., additional, Westerdorff, K., additional, and Zingales, T., additional
Published: 2023
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319. A resonant sextuplet of sub-Neptunes transiting the bright star HD 110067

Author: Luque, R., primary, Osborn, H. P., additional, Leleu, A., additional, Pallé, E., additional, Bonfanti, A., additional, Barragán, O., additional, Wilson, T. G., additional, Broeg, C., additional, Cameron, A. Collier, additional, Lendl, M., additional, Maxted, P. F. L., additional, Alibert, Y., additional, Gandolfi, D., additional, Delisle, J.-B., additional, Hooton, M. J., additional, Egger, J. A., additional, Nowak, G., additional, Lafarga, M., additional, Rapetti, D., additional, Twicken, J. D., additional, Morales, J. C., additional, Carleo, I., additional, Orell-Miquel, J., additional, Adibekyan, V., additional, Alonso, R., additional, Alqasim, A., additional, Amado, P. J., additional, Anderson, D. R., additional, Anglada-Escudé, G., additional, Bandy, T., additional, Bárczy, T., additional, Barrado Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Bayliss, D., additional, Bean, J. L., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Billot, N., additional, Bonfils, X., additional, Borsato, L., additional, Boyle, A. W., additional, Brandeker, A., additional, Bryant, E. M., additional, Cabrera, J., additional, Carrazco-Gaxiola, S., additional, Charbonneau, D., additional, Charnoz, S., additional, Ciardi, D. R., additional, Cochran, W. D., additional, Collins, K. A., additional, Crossfield, I. J. M., additional, Csizmadia, Sz., additional, Cubillos, P. E., additional, Dai, F., additional, Davies, M. B., additional, Deeg, H. J., additional, Deleuil, M., additional, Deline, A., additional, Delrez, L., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Esparza-Borges, E., additional, Falk, B., additional, Fortier, A., additional, Fossati, L., additional, Fridlund, M., additional, Fukui, A., additional, Garcia-Mejia, J., additional, Gill, S., additional, Gillon, M., additional, Goffo, E., additional, Gómez Maqueo Chew, Y., additional, Güdel, M., additional, Guenther, E. W., additional, Günther, M. N., additional, Hatzes, A. P., additional, Helling, Ch., additional, Hesse, K. M., additional, Howell, S. B., additional, Hoyer, S., additional, Ikuta, K., additional, Isaak, K. G., additional, Jenkins, J. M., additional, Kagetani, T., additional, Kiss, L. L., additional, Kodama, T., additional, Korth, J., additional, Lam, K. W. F., additional, Laskar, J., additional, Latham, D. W., additional, Lecavelier des Etangs, A., additional, Leon, J. P. D., additional, Livingston, J. H., additional, Magrin, D., additional, Matson, R. A., additional, Matthews, E. C., additional, Mordasini, C., additional, Mori, M., additional, Moyano, M., additional, Munari, M., additional, Murgas, F., additional, Narita, N., additional, Nascimbeni, V., additional, Olofsson, G., additional, Osborne, H. L. M., additional, Ottensamer, R., additional, Pagano, I., additional, Parviainen, H., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Quinn, S. N., additional, Quirrenbach, A., additional, Ragazzoni, R., additional, Rando, N., additional, Ratti, F., additional, Rauer, H., additional, Redfield, S., additional, Ribas, I., additional, Ricker, G. R., additional, Rudat, A., additional, Sabin, L., additional, Salmon, S., additional, Santos, N. C., additional, Scandariato, G., additional, Schanche, N., additional, Schlieder, J. E., additional, Seager, S., additional, Ségransan, D., additional, Shporer, A., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sousa, S. G., additional, Stalport, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Tuson, A., additional, Udry, S., additional, Vanderburg, A. M., additional, Van Eylen, V., additional, Van Grootel, V., additional, Venturini, J., additional, Walter, I., additional, Walton, N. A., additional, Watanabe, N., additional, Winn, J. N., additional, and Zingales, T., additional
Published: 2023
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320. cheops observations of An aligned orbit and signs of variability from a reflective day side.

Author: Singh, V., primary, Scandariato, G., additional, Smith, A.M.S., additional, Cubillos, P.E., additional, Lendl, M., additional, Billot, N., additional, Fortier, A., additional, Queloz, D., additional, Sousa, S.G., additional, Csizmadia, Sz., additional, Brandeker, A., additional, Carone, L., additional, Wilson, T.G., additional, Akinsanmi, B., additional, Patel, J.A., additional, Krenn, A., additional, Demangeon, O.D.S., additional, Bruno, G., additional, Pagano, I., additional, Hooton, M.J., additional, Cabrera, J., additional, Santos, N.C., additional, Alibert, Y., additional, Alonso, R., additional, Asquier, J., additional, Bárczy, T., additional, Barrado Navascues, D., additional, Barros, S.C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Bergomi, M., additional, Bonfanti, A., additional, Bonfils, X., additional, Borsato, L., additional, Broeg, C., additional, Charnoz, S., additional, Collier Cameron, A., additional, Davies, M.B., additional, Deleuil, M., additional, Deline, A., additional, Delrez, L., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Günther, M.N., additional, Harre, J.-V., additional, Heitzmann, A., additional, Helling, Ch., additional, Hoyer, S., additional, Isaak, K.G., additional, Kiss, L., additional, Lam, K.W.F., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Magrin, D., additional, Maxted, P.F.L., additional, Mischler, H., additional, Mordasini, C., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Salmon, S., additional, Ségransan, D., additional, Simon, A.E., additional, Stalport, M., additional, Steinberger, M., additional, Szabó, M. Gy., additional, Thomas, N., additional, Udry, S., additional, Ulmer, B., additional, Van Grootel, V., additional, Venturini, J., additional, Villaver, E., additional, Walton, N.A., additional, and Zingales, T., additional
Published: 2023
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321. Constraining the reflective properties of using CHEOPS photometry

Author: Pagano, I., primary, Scandariato, G., additional, Singh, V., additional, Lendl, M., additional, Queloz, D., additional, Simon, A.E., additional, Sousa, S.G., additional, Brandeker, A., additional, Collier Cameron, A., additional, Sulis, S., additional, Van Grootel, V., additional, Wilson, T.G., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Bárczy, T., additional, Barrado Navascues, D., additional, Barros, S.C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Billot, N., additional, Bonfils, X., additional, Borsato, L., additional, Broeg, C., additional, Bruno, G., additional, Carone, L., additional, Charnoz, S., additional, Corral van Damme, C., additional, Csizmadia, Sz., additional, Cubillos, P.E., additional, Davies, M.B., additional, Deleuil, M., additional, Deline, A., additional, Delrez, L., additional, Demangeon, O.D.S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Fortier, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Günther, M.N., additional, Helling, Ch., additional, Hoyer, S., additional, Isaak, K.G., additional, Kiss, L., additional, Kopp, E., additional, Lam, K.W.F., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Magrin, D., additional, Maxted, P.F.L., additional, Mordasini, C., additional, Munari, M., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Reimers, C., additional, Ribas, I., additional, Rieder, M., additional, Santos, N.C., additional, Ségransan, D., additional, Smith, A.M.S., additional, Stalport, M., additional, Steller, M., additional, Szabó, M. Gy., additional, Thomas, N., additional, Udry, S., additional, Venturini, J., additional, and Walton, N.A., additional
Published: 2023
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322. CHEOPS and TESS view of the ultra-short-period super-Earth TOI-561 b

Author: Patel, J. A., primary, Egger, J. A., additional, Wilson, T. G., additional, Bourrier, V., additional, Carone, L., additional, Beck, M., additional, Ehrenreich, D., additional, Sousa, S. G., additional, Benz, W., additional, Brandeker, A., additional, Deline, A., additional, Alibert, Y., additional, Lam, K. W. F., additional, Lendl, M., additional, Alonso, R., additional, Anglada, G., additional, Bárczy, T., additional, Barrado, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, T., additional, Billot, N., additional, Bonfils, X., additional, Broeg, C., additional, Busch, M.-D., additional, Cabrera, J., additional, Charnoz, S., additional, Collier Cameron, A., additional, Csizmadia, Sz., additional, Davies, M. B., additional, Deleuil, M., additional, Delrez, L., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Erikson, A., additional, Fortier, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Heng, K., additional, Hoyer, S., additional, Isaak, K. G., additional, Kiss, L. L., additional, Kopp, E., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lovis, C., additional, Magrin, D., additional, Maxted, P. F. L., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Ratti, F., additional, Rauer, H., additional, Ribas, I., additional, Santos, N. C., additional, Scandariato, G., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Ulmer, B., additional, Van Grootel, V., additional, Viotto, V., additional, and Walton, N. A., additional
Published: 2023
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323. Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations

Author: Pereira, C L, primary, Braga-Ribas, F, additional, Sicardy, B, additional, Gomes-Júnior, A R, additional, Ortiz, J L, additional, Branco, H C, additional, Camargo, J I B, additional, Morgado, B E, additional, Vieira-Martins, R, additional, Assafin, M, additional, Benedetti-Rossi, G, additional, Desmars, J, additional, Emilio, M, additional, Morales, R, additional, Rommel, F L, additional, Hayamizu, T, additional, Gondou, T, additional, Jehin, E, additional, Artola, R A, additional, Asai, A, additional, Colazo, C, additional, Ducrot, E, additional, Duffard, R, additional, Fabrega, J, additional, Fernandez-Valenzuela, E, additional, Gillon, M, additional, Horaguchi, T, additional, Ida, M, additional, Kitazaki, K, additional, Mammana, L A, additional, Maury, A, additional, Melita, M, additional, Morales, N, additional, Moya-Sierralta, C, additional, Owada, M, additional, Pollock, J, additional, Sanchez, J L, additional, Santos-Sanz, P, additional, Sasanuma, N, additional, Sebastian, D, additional, Triaud, A, additional, Uchiyama, S, additional, Vanzi, L, additional, Watanabe, H, additional, and Yamamura, H, additional
Published: 2023
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324. Refining the properties of the TOI-178 system with CHEOPS and TESS

Author: Delrez, L., primary, Leleu, A., additional, Brandeker, A., additional, Gillon, M., additional, Hooton, M. J., additional, Collier Cameron, A., additional, Deline, A., additional, Fortier, A., additional, Queloz, D., additional, Bonfanti, A., additional, Van Grootel, V., additional, Wilson, T. G., additional, Egger, J. A., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Asquier, J., additional, Bárczy, T., additional, Barrado y Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Billot, N., additional, Bonfıls, X., additional, Borsato, L., additional, Broeg, C., additional, Buder, M., additional, Cabrera, J., additional, Cessa, V., additional, Charnoz, S., additional, Csizmadia, Sz., additional, Cubillos, P. E., additional, Davies, M. B., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Güdel, M., additional, Hasiba, J., additional, Hoyer, S., additional, Isaak, K. G., additional, Jenkins, J. M., additional, Kiss, L. L., additional, Laskar, J., additional, Latham, D. W., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, Lovis, C., additional, Luque, R., additional, Magrin, D., additional, Maxted, P. F. L., additional, Mordasini, C., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Ricker, G., additional, Santos, N. C., additional, Scandariato, G., additional, Seager, S., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Sousa, S. G., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Vanderspek, R., additional, Venturini, J., additional, Viotto, V., additional, Walton, N. A., additional, and Winn, J. N., additional
Published: 2023
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325. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Author: Rommel, F. L., primary, Braga-Ribas, F., additional, Ortiz, J. L., additional, Sicardy, B., additional, Santos-Sanz, P., additional, Desmars, J., additional, Camargo, J. I. B., additional, Vieira-Martins, R., additional, Assafin, M., additional, Morgado, B. E., additional, Boufleur, R. C., additional, Benedetti-Rossi, G., additional, Gomes-Júnior, A. R., additional, Fernández-Valenzuela, E., additional, Holler, B. J., additional, Souami, D., additional, Duffard, R., additional, Margoti, G., additional, Vara-Lubiano, M., additional, Lecacheux, J., additional, Plouvier, J. L., additional, Morales, N., additional, Maury, A., additional, Fabrega, J., additional, Ceravolo, P., additional, Jehin, E., additional, Albanese, D., additional, Mariey, H., additional, Cikota, S., additional, Ruždjak, D., additional, Cikota, A., additional, Szakáts, R., additional, Baba Aissa, D., additional, Gringahcene, Z., additional, Kashuba, V., additional, Koshkin, N., additional, Zhukov, V., additional, Fişek, S., additional, Çakir, O., additional, Özer, S., additional, Schnabel, C., additional, Schnabel, M., additional, Signoret, F., additional, Morrone, L., additional, Santana-Ros, T., additional, Pereira, C. L., additional, Emilio, M., additional, Burdanov, A. Y., additional, de Wit, J., additional, Barkaoui, K., additional, Gillon, M., additional, Leto, G., additional, Frasca, A., additional, Catanzaro, G., additional, Sanchez, R. Zanmar, additional, Tagliaferri, U., additional, Di Sora, M., additional, Isopi, G., additional, Krugly, Y., additional, Slyusarev, I., additional, Chiorny, V., additional, Mikuž, H., additional, Bacci, P., additional, Maestripieri, M., additional, Grazia, M. D., additional, de la Cueva, I., additional, Yuste-Moreno, M., additional, Ciabattari, F., additional, Kozhukhov, O. M., additional, Serra-Ricart, M., additional, Alarcon, M. R., additional, Licandro, J., additional, Masi, G., additional, Bacci, R., additional, Bosch, J. M., additional, Behem, R., additional, Prost, J.-P., additional, Renner, S., additional, Conjat, M., additional, Bachini, M., additional, Succi, G., additional, Stoian, L., additional, Juravle, A., additional, Carosati, D., additional, Gowe, B., additional, Carrillo, J., additional, Zheleznyak, A. P., additional, Montigiani, N., additional, Foster, C. R., additional, Mannucci, M., additional, Ruocco, N., additional, Cuevas, F., additional, Di Marcantonio, P., additional, Coretti, I., additional, Iafrate, G., additional, Baldini, V., additional, Collins, M., additional, Pál, A., additional, Csák, B., additional, Fernández-Garcia, E., additional, Castro-Tirado, A. J., additional, Hudin, L., additional, Madiedo, J. M., additional, Anghel, R. M., additional, Calvo-Fernández, J. F., additional, Valvasori, A., additional, Guido, E., additional, Gherase, R. M., additional, Kamoun, S., additional, Fafet, R., additional, Sánchez-González, M., additional, Curelaru, L., additional, Vîntdevară, C. D., additional, Danescu, C. A., additional, Gout, J.-F., additional, Schmitz, C. J., additional, Sota, A., additional, Belskaya, I., additional, Rodríguez-Marco, M., additional, Kilic, Y., additional, Frappa, E., additional, Klotz, A., additional, Lavayssière, M., additional, Oliveira, J. Marques, additional, Popescu, M., additional, Mammana, L. A., additional, Fernández-Lajús, E., additional, Schmidt, M., additional, Hopp, U., additional, Komžík, R., additional, Pribulla, T., additional, Tomko, D., additional, Husárik, M., additional, Erece, O., additional, Eryilmaz, S., additional, Buzzi, L., additional, Gährken, B., additional, Nardiello, D., additional, Hornoch, K., additional, Sonbas, E., additional, Er, H., additional, Burwitz, V., additional, Sybilski, P. Waldemar, additional, Bykowski, W., additional, Müller, T. G., additional, Ogloza, W., additional, Gonçalves, R., additional, Ferreira, J. F., additional, Ferreira, M., additional, Bento, M., additional, Meister, S., additional, Bagiran, M. N., additional, Tekeş, M., additional, Marciniak, A., additional, Moravec, Z., additional, Delinčák, P., additional, Gianni, G., additional, Casalnuovo, G. B., additional, Boutet, M., additional, Sanchez, J., additional, Klemt, B., additional, Wuensche, N., additional, Burzynski, W., additional, Borkowski, M., additional, Serrau, M., additional, Dangl, G., additional, Klös, O., additional, Weber, C., additional, Urbaník, M., additional, Rousselot, L., additional, Kubánek, J., additional, André, P., additional, Colazo, C., additional, Spagnotto, J., additional, Sickafoose, A. A., additional, Hueso, R., additional, Sánchez-Lavega, A., additional, Fisher, R. S., additional, Rengstorf, A. W., additional, Perelló, C., additional, Dascalu, M., additional, Altan, M., additional, Gazeas, K., additional, de Santana, T., additional, Sfair, R., additional, Winter, O. C., additional, Kalkan, S., additional, Canales-Moreno, O., additional, Trigo-Rodríguez, J. M., additional, Tsamis, V., additional, Tigani, K., additional, Sioulas, N., additional, Lekkas, G., additional, Bertesteanu, D. N., additional, Dumitrescu, V., additional, Wilberger, A. J., additional, Barnes, J. W., additional, Fieber-Beyer, S. K., additional, Swaney, R. L., additional, Fuentes, C., additional, Mendez, R. A., additional, Dumitru, B. D., additional, Flynn, R. L., additional, and Wake, D. A., additional
Published: 2023
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326. Space-based infrared interferometry to study exoplanetary atmospheres

Author: Defrère, D., Léger, A., Absil, O., Beichman, C., Biller, B., Danchi, W. C., Ergenzinger, K., Eiroa, C., Ertel, S., Fridlund, M., Muñoz, A. García, Gillon, M., Glasse, A., Godolt, M., Grenfell, J. L., Kraus, S., Labadie, L., Lacour, S., Liseau, R., Martin, G., Mennesson, B., Micela, G., Minardi, S., Quanz, S. P., Rauer, H., Rinehart, S., Santos, N. C., Selsis, F., Surdej, J., Tian, F., Villaver, E., Wheatley, P. J., and Wyatt, M.
Published: 2018
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327. Investigating the visible phase-curve variability of 55 Cnc e

Author: Meier Valdés, E. A., primary, Morris, B. M., additional, Demory, B.-O., additional, Brandeker, A., additional, Kitzmann, D., additional, Benz, W., additional, Deline, A., additional, Florén, H.-G., additional, Sousa, S. G., additional, Bourrier, V., additional, Singh, V., additional, Heng, K., additional, Strugarek, A., additional, Bower, D. J., additional, Jäggi, N., additional, Carone, L., additional, Lendl, M., additional, Jones, K., additional, Oza, A. V., additional, Demangeon, O. D. S., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Asquier, J., additional, Bárczy, T., additional, Barrado Navascues, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Billot, N., additional, Bonfils, X., additional, Borsato, L., additional, Broeg, C., additional, Cabrera, J., additional, Charnoz, S., additional, Collier Cameron, A., additional, Csizmadia, Sz., additional, Cubillos, P. E., additional, Davies, M. B., additional, Deleuil, M., additional, Delrez, L., additional, Ehrenreich, D., additional, Erikson, A., additional, Fortier, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Günther, M. N., additional, Hoyer, S., additional, Isaak, K. G., additional, Kiss, L. L., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lovis, C., additional, Magrin, D., additional, Maxted, P. F. L., additional, Mordasini, C., additional, Nascimbeni, V., additional, Olofsson, G., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Ribas, I., additional, Santos, N. C., additional, Sarajlic, M., additional, Scandariato, G., additional, Ségransan, D., additional, Sicilia, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Udry, S., additional, Ulmer, B., additional, Van Grootel, V., additional, Venturini, J., additional, Walton, N. A., additional, Wilson, T. G., additional, and Wolter, D., additional
Published: 2023
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328. TOI-2084 b and TOI-4184 b: Two new sub-Neptunes around M dwarf stars

Author: Barkaoui, K., primary, Timmermans, M., additional, Soubkiou, A., additional, Rackham, B. V., additional, Burgasser, A. J., additional, Chouqar, J., additional, Pozuelos, F. J., additional, Collins, K. A., additional, Howell, S. B., additional, Simcoe, R., additional, Melis, C., additional, Stassun, K. G., additional, Tregloan-Reed, J., additional, Cointepas, M., additional, Gillon, M., additional, Bonfils, X., additional, Furlan, E., additional, Gnilka, C. L., additional, Almenara, J. M., additional, Alonso, R., additional, Benkhaldoun, Z., additional, Bonavita, M., additional, Bouchy, F., additional, Burdanov, A., additional, Chinchilla, P., additional, Davoudi, F., additional, Delrez, L., additional, Demangeon, O., additional, Dominik, M., additional, Demory, B.-O., additional, de Wit, J., additional, Dransfield, G., additional, Ducrot, E., additional, Fukui, A., additional, Hinse, T. C., additional, Hooton, M. J., additional, Jehin, E., additional, Jenkins, J. M., additional, Jørgensen, U. G., additional, Latham, D. W., additional, Garcia, L., additional, Carrazco-Gaxiola, S., additional, Ghachoui, M., additional, Gómez Maqueo Chew, Y., additional, Günther, M. N., additional, McCormac, J., additional, Murgas, F., additional, Murray, C. A., additional, Narita, N., additional, Niraula, P., additional, Pedersen, P. P., additional, Queloz, D., additional, Rebolo-López, R., additional, Ricker, G., additional, Sabin, L., additional, Sajadian, S., additional, Schanche, N., additional, Schwarz, R. P., additional, Seager, S., additional, Sebastian, D., additional, Sefako, R., additional, Sohy, S., additional, Southworth, J., additional, Srdoc, G., additional, Thompson, S. J., additional, Triaud, A. H. M. J., additional, Vanderspek, R., additional, Wells, R. D., additional, Winn, J. N., additional, and Zúñiga-Fernández, S., additional
Published: 2023
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329. TESS discovery of a super-Earth orbiting the M-dwarf star TOI-1680

Author: Ghachoui, M., primary, Soubkiou, A., additional, Wells, R. D., additional, Rackham, B. V., additional, Triaud, A. H. M. J., additional, Sebastian, D., additional, Giacalone, S., additional, Stassun, K. G., additional, Ciardi, D. R., additional, Collins, K. A., additional, Liu, A., additional, Gómez Maqueo Chew, Y., additional, Gillon, M., additional, Benkhaldoun, Z., additional, Delrez, L., additional, Eastman, J. D., additional, Demangeon, O., additional, Barkaoui, K., additional, Burdanov, A., additional, Demory, B.-O., additional, de Wit, J., additional, Dransfield, G., additional, Ducrot, E., additional, Garcia, L., additional, Gómez-Muñoz, M. A., additional, Hooton, M. J., additional, Jehin, E., additional, Murray, C. A., additional, Pedersen, P. P., additional, Pozuelos, F. J., additional, Queloz, D., additional, Sabin, L., additional, Schanche, N., additional, Timmermans, M., additional, Gonzales, E. J., additional, Dressing, C. D., additional, Aganze, C., additional, Burgasser, A. J., additional, Gerasimov, R., additional, Hsu, C., additional, Theissen, C. A., additional, Charbonneau, D., additional, Jenkins, J. M., additional, Latham, D. W., additional, Ricker, G., additional, Seager, S., additional, Shporer, A., additional, Twicken, J. D., additional, Vanderspek, R., additional, Winn, J. N., additional, Collins, K. I., additional, Fukui, A., additional, Gan, T., additional, Narita, N., additional, and Schwarz, R. P., additional
Published: 2023
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330. The planetary system around HD 190622 (TOI-1054)

Author: Cabrera, J., primary, Gandolfi, D., additional, Serrano, L. M., additional, Csizmadia, Sz., additional, Egger, J. A., additional, Baumeister, Ph., additional, Krenn, A., additional, Benz, W., additional, Deline, A., additional, Florén, H.-G., additional, Collier Cameron, A., additional, Adibekyan, V., additional, Alibert, Y., additional, Bellomo, S. E., additional, Delrez, L., additional, Fossati, L., additional, Fortier, A., additional, Grziwa, S., additional, Hoyer, S., additional, Bonfanti, A., additional, Salmon, S., additional, Sousa, S. G., additional, Wilson, T. G., additional, Alarcón, J., additional, Alonso, R., additional, Anglada Escudé, G., additional, Bárczy, T., additional, Barragán, O., additional, Barrado, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Bernabò, L. M., additional, Billot, N., additional, Bonfils, X., additional, Borsato, L., additional, Brandeker, A., additional, Broeg, C., additional, Carrión-González, O., additional, Charnoz, S., additional, Ciardi, D. R., additional, Cochran, W. D., additional, Collins, K. A., additional, Collins, K. I., additional, Conti, D. M., additional, Davies, M. B., additional, Deeg, H. J., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Demory, B.-O., additional, Ehrenreich, D., additional, Erikson, A., additional, Esposito, M., additional, Fridlund, M., additional, Gillon, M., additional, Goffo, E., additional, Güdel, M., additional, Guenther, E. W., additional, Harre, J.-V., additional, Heng, K., additional, Hooton, M. J., additional, Isaak, K. G., additional, Jenkins, J. M., additional, Kiss, L. L., additional, Knudstrup, E., additional, Lam, K. W. F., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, Lovis, C., additional, Luque, R., additional, Magrin, D., additional, Maxted, P. F. L., additional, Muresan, A., additional, Nascimbeni, V., additional, Olofsson, G., additional, Osborn, H. P., additional, Osborne, H. L. M., additional, Ottensamer, R., additional, Pagano, I., additional, Pallé, E., additional, Persson, C. M., additional, Peter, G., additional, Piotto, G., additional, Pollacco, D., additional, Queloz, D., additional, Ragazzoni, R., additional, Rando, N., additional, Rauer, H., additional, Redfield, S., additional, Ribas, I., additional, Ricker, G. R., additional, Rodler, F., additional, Santos, N. C., additional, Scandariato, G., additional, Seager, S., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, Gy. M., additional, Thomas, N., additional, Tosi, N., additional, Twicken, J. D., additional, Udry, S., additional, Van Eylen, V., additional, Van Grootel, V., additional, Walton, N. A., additional, and Winn, J. N., additional
Published: 2023
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331. TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star

Author: Hobson, MJ, Jordán, A, Bryant, EM, Brahm, R, Bayliss, D, Hartman, JD, Bakos, GI, Henning, T, Almenara, JM, Barkaoui, K, Benkhaldoun, Z, Bonfils, X, Bouchy, F, Charbonneau, D, Cointepas, M, Collins, KA, Eastman, JD, Ghachoui, M, Gillon, M, Goeke, RF, Horne, K, Irwin, JM, Jehin, E, Jenkins, JM, Latham, DW, Moldovan, D, Murgas, F, Pozuelos, FJ, Ricker, GR, Schwarz, RP, Seager, S, Srdoc, G, Striegel, S, Timmermans, M, Vanderburg, A, Vanderspek, R, Winn, JN, Hobson, MJ [0000-0002-5945-7975], Jordán, A [0000-0002-5389-3944], Bryant, EM [0000-0001-7904-4441], Brahm, R [0000-0002-9158-7315], Bayliss, D [0000-0001-6023-1335], Hartman, JD [0000-0001-8732-6166], Bakos, GI [0000-0001-7204-6727], Henning, T [0000-0002-1493-300X], Almenara, JM [0000-0003-3208-9815], Barkaoui, K [0000-0003-1464-9276], Benkhaldoun, Z [0000-0001-6285-9847], Bonfils, X [0000-0001-9003-8894], Bouchy, F [0000-0002-7613-393X], Charbonneau, D [0000-0002-9003-484X], Collins, KA [0000-0001-6588-9574], Eastman, JD [0000-0003-3773-5142], Ghachoui, M [0000-0003-3986-0297], Gillon, M [0000-0003-1462-7739], Horne, K [0000-0003-1728-0304], Jehin, E [0000-0001-8923-488X], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Murgas, F [0000-0001-9087-1245], Pozuelos, FJ [0000-0003-1572-7707], Ricker, GR [0000-0003-2058-6662], Schwarz, RP [0000-0001-8227-1020], Seager, S [0000-0002-6892-6948], Vanderburg, A [0000-0001-7246-5438], Vanderspek, R [0000-0001-6763-6562], Winn, JN [0000-0002-4265-047X], Apollo - University of Cambridge Repository, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, 5101 Astronomical Sciences, MCP, FOS: Physical sciences, Astronomy and Astrophysics, 3rd-DAS, 5109 Space Sciences, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of TOI-3235 b, a short-period Jupiter orbiting an M-dwarf with a stellar mass close to the critical mass at which stars transition from partially to fully convective. TOI-3235 b was first identified as a candidate from TESS photometry, and confirmed with radial velocities from ESPRESSO, and ground-based photometry from HATSouth, MEarth-South, TRAPPIST-South, LCOGT, and ExTrA. We find that the planet has a mass of $\mathrm{0.665\pm0.025\,M_J}$ and a radius of $\mathrm{1.017\pm0.044\,R_J}$. It orbits close to its host star, with an orbital period of $\mathrm{2.5926\,d}$, but has an equilibrium temperature of $\mathrm{\approx 604 \, K}$, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of $\mathrm{0.3939\pm0.0030\,M_\odot}$, a radius of $\mathrm{0.3697\pm0.0018\,R_\odot}$, an effective temperature of $\mathrm{3389 \, K}$, and a J-band magnitude of $\mathrm{11.706\pm0.025}$. Current planet formation models do not predict the existence of gas giants such as TOI-3235 b around such low-mass stars. With a high transmission spectroscopy metric, TOI-3235 b is one of the best-suited giants orbiting M-dwarfs for atmospheric characterization., 15 pages, 4 figures. Accepted for publication in APJL
Published: 2023

332. WASP-157b, a Transiting Hot Jupiter Observed with K2

Author: Močnik, T., Anderson, D. R., Brown, D. J. A., Cameron, A. Collier, Delrez, L., Gillon, M., Hellier, C., Jehin, E., Lendl, M., Maxted, P. F. L., Neveu-VanMalle, M., Pepe, F., Pollacco, D., Queloz, D., Ségransan, D., Smalley, B., Southworth, J., Triaud, A. H. M. J., Udry, S., and West, R. G.
Published: 2016

333. WASP-120b, WASP-122b, and WASP-123b : Three Newly Discovered Planets from the WASP-South Survey

Author: Turner, O. D., Anderson, D. R., Cameron, A. Collier, Delrez, L., Evans, D. F., Gillon, M., Hellier, C., Jehin, E., Lendl, M., Maxted, P. F. L., Pepe, F., Pollacco, D., Queloz, D., Ségransan, D., Smalley, B., Smith, A. M. S., Triaud, A. H. M. J., Udry, S., and West, R. G.
Published: 2016

334. TESS and CHEOPS discover two warm sub-Neptunes transiting the bright K-dwarf HD 15906

Author: Tuson, A, Queloz, D, Osborn, H P, Wilson, T G, Hooton, M J, Beck, M, Lendl, M, Olofsson, G, Fortier, A, Bonfanti, A, Brandeker, A, Buchhave, L A, Collier Cameron, A, Ciardi, D R, Collins, K A, Gandolfi, D, Garai, Z, Giacalone, S, Gomes da Silva, J, Howell, S B, Patel, J A, Persson, C M, Serrano, L M, Sousa, S G, Ulmer-Moll, S, Vanderburg, A, Ziegler, C, Alibert, Y, Alonso, R, Anglada, G, Bárczy, T, Barrado Navascues, D, Barros, S C C, Baumjohann, W, Beck, T, Benz, W, Billot, N, Bonfils, X, Borsato, L, Broeg, C, Cabrera, J, Charnoz, S, Conti, D M, Csizmadia, Sz, Cubillos, P E, Davies, M B, Deleuil, M, Delrez, L, Demangeon, O D S, Demory, B-O, Dragomir, D, Dressing, C D, Ehrenreich, D, Erikson, A, Essack, Z, Farinato, J, Fossati, L, Fridlund, M, Furlan, E, Gill, H, Gillon, M, Gnilka, C L, Gonzales, E, Güdel, M, Günther, M N, Hoyer, S, Isaak, K G, Jenkins, J M, Kiss, L L, Laskar, J, Latham, D W, Law, N, Lecavelier des Etangs, A, Curto, G Lo, Lovis, C, Luque, R, Magrin, D, Mann, A W, Maxted, P F L, Mayor, M, McDermott, S, Mecina, M, Mordasini, C, Mortier, A, Nascimbeni, V, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Pritchard, T, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Ricker, G R, Rieder, M, Santos, N C, Savel, A B, Scandariato, G, Schwarz, R P, Seager, S, Ségransan, D, Shporer, A, Simon, A E, Smith, A M S, Steller, M, Stockdale, C, Szabó, Gy M, Thomas, N, Torres, G, Tronsgaard, R, Udry, S, Ulmer, B, Van Grootel, V, Vanderspek, R, Venturini, J, Walton, N A, Winn, J N, Wohler, B, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: MCP, DAS
Abstract: We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by ∼ 734 d, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS, and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 ± 0.08 R⊕ and a period of 10.924709 ± 0.000032 d, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R⊕ and a period of 21.583298$^{+0.000052}_{-0.000055}$ d. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 ± 13 K and 532 ± 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm (≲ 700 K) sub-Neptune sized planets transiting a bright star (G ≤ 10 mag). It is an excellent target for detailed characterization studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution. Publisher PDF
Published: 2023

335. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Rommel, F.L., Braga-Ribas, F., Ortiz Moreno, José Luis, Sicardy, Bruno, Santos Sanz, Pablo, Desmars, Josselin, Camargo, J.I.B., Vieira-Martins, R., Assafin, M., Morgado, B.E., Boufleur, R.C., Fişek, S., Çakir, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, Toni, Pereira, C.L., Grazia, M.D., Burwitz, V., Calvo-Fernández, J.F., Carosati, D., Emilio, M., Burdanov, A.Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Waldemar Sybilski, P., Carrillo, J., Zanmar Sanchez, R., Tagliaferri, U., Gowe, B., Valvasori, A., Klemt, B., de la Cueva, I., Guido, E., Yuste-Moreno, M., Ciabattari, F., Bykowski, W., Kozhukhov, O.M., Serra-Ricart, M., Alarcon, Miguel R., Licandro, Javier, Masi, G., Bacci, Roberto, Wuensche, N., Kamoun, S., Bosch, Josep M., Behem, R., Müller, Thomas G., Gherase, R.M., Prost, J.-P., Altan, M., Zheleznyak, A.P., Montigiani, N., Foster, C.R., Mannucci, M., Burzynski, W., Ruocco, Nello, Cuevas, F., Ogloza, W., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Gazeas, K., Fafet, R., Collins, M., Pál, András, Borkowski, M., Csák, B., Gonçalves, R., Fernández-García, Emilio, Benedetti-Rossi, G., Sánchez-González, M., Curelaru, L., Vîntdevară, C.D., Danescu, C.A., de Santana, T., Gout, J.-F., Schmitz, C.J., Serrau, M., Ferreira, J.F., Sota, Alfredo, Belskaya, Irina, Rodríguez-Marco, M., Kilic, Y., Gomes-Júnior, A.R., Frappa, E., Klotz, A., Lavayssière, M., Sfair, R., Marques Oliveira, J., Ferreira, M., Dangl, G., Popescu, Marcel, Mammana, L.A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Fernández-Valenzuela, Estela, Pribulla, T., Tomko, D., Bento, M., Winter, O.C., Klös, O., Husárik, Marek, Erece, O., Eryilmaz, S., Buzzi, Luca, Gährken, B., Nardiello, D., Hornoch, Kamil, Sonbas, E., Urbaník, M., Holler, B.J., Er, H., Weber, C., Kalkan, S., Di Sora, M., Souami, Damya, Canales-Moreno, O., Meister, S., Bagiran, M.N., Tekeş, M., Marciniak, Anna, Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G.B., Isopi, G., Tsamis, V., Boutet, M., Sanchez, J., Trigo-Rodríguez, Josep M., Duffard, René, Renner, S., Rousselot, L., Margoti, G., Kubánek, J., André, P., Krugly, Yurij, Colazo, C., Spagnotto, J., Sickafoose, A.A., Hueso, R., Sánchez-Lavega, A., Fisher, R.S., Conjat, M., Lecacheux, J., Rengstorf, A.W., Perelló, C., Slyusarev, I., Vara-Lubiano, M., Dascalu, M., Castro-Tirado, Alberto J., Tigani, K., Sioulas, Nick, Lekkas, G., Bertesteanu, D.N., Bachini, M., Dumitrescu, V., Wilberger, A.J., Chiorny, V., Barnes, J.W., Fieber-Beyer, S.K., Swaney, R.L., Fuentes, C., Hudin, L., Plouvier, J.L., Mendez, R.A., Dumitru, B.D., Succi, G., Flynn, R.L., Mikuz, H., Wake, D.A., Morales, Nicolás, Maury, Alain, Fabrega, J., Ceravolo, P., Jehin, Emmanuel, Madiedo, J.M., Albanese, D., Mariey, H., Stoian, L., Bacci, P., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, Róbert, Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Anghel, R.M., Zhukov, V., Maestripieri, M., Juravle, A., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Rommel, F.L., Braga-Ribas, F., Ortiz Moreno, José Luis, Sicardy, Bruno, Santos Sanz, Pablo, Desmars, Josselin, Camargo, J.I.B., Vieira-Martins, R., Assafin, M., Morgado, B.E., Boufleur, R.C., Fişek, S., Çakir, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, Toni, Pereira, C.L., Grazia, M.D., Burwitz, V., Calvo-Fernández, J.F., Carosati, D., Emilio, M., Burdanov, A.Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Waldemar Sybilski, P., Carrillo, J., Zanmar Sanchez, R., Tagliaferri, U., Gowe, B., Valvasori, A., Klemt, B., de la Cueva, I., Guido, E., Yuste-Moreno, M., Ciabattari, F., Bykowski, W., Kozhukhov, O.M., Serra-Ricart, M., Alarcon, Miguel R., Licandro, Javier, Masi, G., Bacci, Roberto, Wuensche, N., Kamoun, S., Bosch, Josep M., Behem, R., Müller, Thomas G., Gherase, R.M., Prost, J.-P., Altan, M., Zheleznyak, A.P., Montigiani, N., Foster, C.R., Mannucci, M., Burzynski, W., Ruocco, Nello, Cuevas, F., Ogloza, W., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Gazeas, K., Fafet, R., Collins, M., Pál, András, Borkowski, M., Csák, B., Gonçalves, R., Fernández-García, Emilio, Benedetti-Rossi, G., Sánchez-González, M., Curelaru, L., Vîntdevară, C.D., Danescu, C.A., de Santana, T., Gout, J.-F., Schmitz, C.J., Serrau, M., Ferreira, J.F., Sota, Alfredo, Belskaya, Irina, Rodríguez-Marco, M., Kilic, Y., Gomes-Júnior, A.R., Frappa, E., Klotz, A., Lavayssière, M., Sfair, R., Marques Oliveira, J., Ferreira, M., Dangl, G., Popescu, Marcel, Mammana, L.A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Fernández-Valenzuela, Estela, Pribulla, T., Tomko, D., Bento, M., Winter, O.C., Klös, O., Husárik, Marek, Erece, O., Eryilmaz, S., Buzzi, Luca, Gährken, B., Nardiello, D., Hornoch, Kamil, Sonbas, E., Urbaník, M., Holler, B.J., Er, H., Weber, C., Kalkan, S., Di Sora, M., Souami, Damya, Canales-Moreno, O., Meister, S., Bagiran, M.N., Tekeş, M., Marciniak, Anna, Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G.B., Isopi, G., Tsamis, V., Boutet, M., Sanchez, J., Trigo-Rodríguez, Josep M., Duffard, René, Renner, S., Rousselot, L., Margoti, G., Kubánek, J., André, P., Krugly, Yurij, Colazo, C., Spagnotto, J., Sickafoose, A.A., Hueso, R., Sánchez-Lavega, A., Fisher, R.S., Conjat, M., Lecacheux, J., Rengstorf, A.W., Perelló, C., Slyusarev, I., Vara-Lubiano, M., Dascalu, M., Castro-Tirado, Alberto J., Tigani, K., Sioulas, Nick, Lekkas, G., Bertesteanu, D.N., Bachini, M., Dumitrescu, V., Wilberger, A.J., Chiorny, V., Barnes, J.W., Fieber-Beyer, S.K., Swaney, R.L., Fuentes, C., Hudin, L., Plouvier, J.L., Mendez, R.A., Dumitru, B.D., Succi, G., Flynn, R.L., Mikuz, H., Wake, D.A., Morales, Nicolás, Maury, Alain, Fabrega, J., Ceravolo, P., Jehin, Emmanuel, Madiedo, J.M., Albanese, D., Mariey, H., Stoian, L., Bacci, P., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, Róbert, Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Anghel, R.M., Zhukov, V., Maestripieri, M., and Juravle, A.
Abstract: Context. The physical characterization of trans-Neptunian objects is essential for improving our understanding of the formation and evolution of our Solar System. Stellar occultation is a ground-based technique that can be successfully used to determine some of the TNOs’ fundamental physical properties with high precision, such as size and shape. Aims. This work is aimed at constraining the size, shape, and geometric albedo of the dwarf planet candidate (307261) 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also study the object’s topography by analyzing the obtained limb and residuals between the observed chords and the best-fit ellipse. Metods. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with between 3 and 61 positive chords. We derived the occultation light curves using differential aperture photometry, from which the star ingress and egress instants were calculated. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fit ellipse, combined with the object’s rotational information from the literature, sets constraints on the object’s size, shape, and albedo. Additionally, we developed a new method to characterize the topography features on the object’s limb. Results. The global limb has a semi-major axis of a′ = 412 ± 10 km, a semi-minor axis of b′= 385 ± 17 km, and the position angle of the minor axis is 121° ± 16°. From this instantaneous limb, we obtained 2002 MS4’s geometric albedo of pV = 0.1 ± 0.025, using HV = 3.63 ± 0.05 mag and a projected area-equivalent diameter of 796 ± 24 km. Significant deviations from the fitted ellipse in the northernmost limb were detected from multiple sites, highlighting three distinct topographic features: one 11 km depth depression, followed by a 25−5+4 k
Published: 2023

336. A dense ring of the trans-Neptunian object Quaoar outside its Roche limit

Author: Morgado, B. E. (B. E.), Sicardy, B. (B.), Braga-Ribas, F. (F.), Ortiz, J. L. (J. L.), Salo, H. (H.), Vachier, F. (F.), Desmars, J. (J.), Pereira, C. L. (C. L.), Santos-Sanz, P. (P.), Sfair, R. (R.), de Santana, T. (T.), Assafin, M. (M.), Vieira-Martins, R. (R.), Gomes-Júnior, A. R. (A. R.), Margoti, G. (G.), Dhillon, V. S. (V. S.), Fernández-Valenzuela, E. (E.), Broughton, J. (J.), Bradshaw, J. (J.), Langersek, R. (R.), Benedetti-Rossi, G. (G.), Souami, D. (D.), Holler, B. J. (B. J.), Kretlow, M. (M.), Boufleur, R. C. (R. C.), Camargo, J. I. (J. I. B.), Duffard, R. (R.), Beisker, W. (W.), Morales, N. (N.), Lecacheux, J. (J.), Rommel, F. L. (F. L.), Herald, D. (D.), Benz, W. (W.), Jehin, E. (E.), Jankowsky, F. (F.), Marsh, T. R. (T. R.), Littlefair, S. P. (S. P.), Bruno, G. (G.), Pagano, I. (I.), Brandeker, A. (A.), Collier-Cameron, A. (A.), Florén, H. G. (H. G.), Hara, N. (N.), Olofsson, G. (G.), Wilson, T. G. (T. G.), Benkhaldoun, Z. (Z.), Busuttil, R. (R.), Burdanov, A. (A.), Ferrais, M. (M.), Gault, D. (D.), Gillon, M. (M.), Hanna, W. (W.), Kerr, S. (S.), Kolb, U. (U.), Nosworthy, P. (P.), Sebastian, D. (D.), Snodgrass, C. (C.), Teng, J. P. (J. P.), de Wit, J. (J.), Morgado, B. E. (B. E.), Sicardy, B. (B.), Braga-Ribas, F. (F.), Ortiz, J. L. (J. L.), Salo, H. (H.), Vachier, F. (F.), Desmars, J. (J.), Pereira, C. L. (C. L.), Santos-Sanz, P. (P.), Sfair, R. (R.), de Santana, T. (T.), Assafin, M. (M.), Vieira-Martins, R. (R.), Gomes-Júnior, A. R. (A. R.), Margoti, G. (G.), Dhillon, V. S. (V. S.), Fernández-Valenzuela, E. (E.), Broughton, J. (J.), Bradshaw, J. (J.), Langersek, R. (R.), Benedetti-Rossi, G. (G.), Souami, D. (D.), Holler, B. J. (B. J.), Kretlow, M. (M.), Boufleur, R. C. (R. C.), Camargo, J. I. (J. I. B.), Duffard, R. (R.), Beisker, W. (W.), Morales, N. (N.), Lecacheux, J. (J.), Rommel, F. L. (F. L.), Herald, D. (D.), Benz, W. (W.), Jehin, E. (E.), Jankowsky, F. (F.), Marsh, T. R. (T. R.), Littlefair, S. P. (S. P.), Bruno, G. (G.), Pagano, I. (I.), Brandeker, A. (A.), Collier-Cameron, A. (A.), Florén, H. G. (H. G.), Hara, N. (N.), Olofsson, G. (G.), Wilson, T. G. (T. G.), Benkhaldoun, Z. (Z.), Busuttil, R. (R.), Burdanov, A. (A.), Ferrais, M. (M.), Gault, D. (D.), Gillon, M. (M.), Hanna, W. (W.), Kerr, S. (S.), Kolb, U. (U.), Nosworthy, P. (P.), Sebastian, D. (D.), Snodgrass, C. (C.), Teng, J. P. (J. P.), and de Wit, J. (J.)
Abstract: Planetary rings are observed not only around giant planets¹, but also around small bodies such as the Centaur Chariklo² and the dwarf planet Haumea³. Up to now, all known dense rings were located close enough to their parent bodies, being inside the Roche limit, where tidal forces prevent material with reasonable densities from aggregating into a satellite. Here we report observations of an inhomogeneous ring around the trans-Neptunian body (50000) Quaoar. This trans-Neptunian object has an estimated radius⁴ of 555 km and possesses a roughly 80-km satellite⁵ (Weywot) that orbits at 24 Quaoar radii⁶,⁷. The detected ring orbits at 7.4 radii from the central body, which is well outside Quaoar’s classical Roche limit, thus indicating that this limit does not always determine where ring material can survive. Our local collisional simulations show that elastic collisions, based on laboratory experiments⁸, can maintain a ring far away from the body. Moreover, Quaoar’s ring orbits close to the 1/3 spin–orbit resonance9 with Quaoar, a property shared by Chariklo’s ²,¹⁰,¹¹ and Haumea’s³ rings, suggesting that this resonance plays a key role in ring confinement for small bodies.
Published: 2023

337. Two new sub-Neptunes around M dwarf stars

Author: Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B.-o., De Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-gaxiola, S., Ghachoui, M., Gómez Maqueo Chew, Y., Günther, M. N., Mccormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-lópez, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., Zúñiga-fernández, S., Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B.-o., De Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-gaxiola, S., Ghachoui, M., Gómez Maqueo Chew, Y., Günther, M. N., Mccormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-lópez, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., and Zúñiga-fernández, S.
Published: 2023

338. Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

Author: Osborn, H. P., Nowak, G., Hébrard, G., Masseron, T., Lillo-Box, J., Pallé, E., Bekkelien, A., Florén, H. G., Guterman, P., Simon, A. E., Adibekyan, V., Bieryla, A., Borsato, L., Brandeker, A., Ciardi, D. R., Cameron, A. Collier, Collins, K. A., Egger, J. A., Gandolfi, D., Hooton, M. J., Latham, D. W., Lendl, M., Matthews, E. C., Tuson, A., Ulmer-Moll, S., Vanderburg, A., Wilson, T. G., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Arnold, L., Asquier, J., y Navascues, D. Barrado, Baumjohann, W., Beck, T., Belinski, A. A., Benz, W., Biondi, F., Boisse, I., Bonfils, X., Broeg, C., Buchhave, L. A., Bárczy, T., Barros, S. C.C., Cabrera, J., Guillen, C. Cardona, Carleo, I., Castro-González, A., Charnoz, S., Christiansen, J., Cortes-Zuleta, P., Csizmadia, S., Dalal, S., Davies, M. B., Deleuil, M., Delfosse, X., Delrez, L., Demory, B. O., Dunlavey, A. B., Ehrenreich, D., Erikson, A., Fernandes, R. B., Fortier, A., Forveille, T., Fossati, L., Fridlund, M., Gillon, M., Goeke, R. F., Goliguzova, M. V., Gonzales, E. J., Günther, M. N., Güdel, M., Heidari, N., Henze, C. E., Howell, S., Hoyer, S., Frey, J. I., Isaak, K. G., Jenkins, J. M., Kiefer, F., Kiss, L., Korth, J., Maxted, P. F.L., Laskar, J., des Etangs, A. Lecavelier, Lovis, C., Lund, M. B., Luque, R., Magrin, D., Almenara, J. M., Martioli, E., Mecina, M., Medina, J. V., Moldovan, D., Morales-Calderón, M., Morello, G., Moutou, C., Murgas, F., Jensen, E. L.N., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Demangeon, O. D.S., Smith, A. M.S., Santos, N., Scandariato, G., Seager, S., Sousa, S. G., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Walton, N., Winn, J. N., Osborn, H. P., Nowak, G., Hébrard, G., Masseron, T., Lillo-Box, J., Pallé, E., Bekkelien, A., Florén, H. G., Guterman, P., Simon, A. E., Adibekyan, V., Bieryla, A., Borsato, L., Brandeker, A., Ciardi, D. R., Cameron, A. Collier, Collins, K. A., Egger, J. A., Gandolfi, D., Hooton, M. J., Latham, D. W., Lendl, M., Matthews, E. C., Tuson, A., Ulmer-Moll, S., Vanderburg, A., Wilson, T. G., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Arnold, L., Asquier, J., y Navascues, D. Barrado, Baumjohann, W., Beck, T., Belinski, A. A., Benz, W., Biondi, F., Boisse, I., Bonfils, X., Broeg, C., Buchhave, L. A., Bárczy, T., Barros, S. C.C., Cabrera, J., Guillen, C. Cardona, Carleo, I., Castro-González, A., Charnoz, S., Christiansen, J., Cortes-Zuleta, P., Csizmadia, S., Dalal, S., Davies, M. B., Deleuil, M., Delfosse, X., Delrez, L., Demory, B. O., Dunlavey, A. B., Ehrenreich, D., Erikson, A., Fernandes, R. B., Fortier, A., Forveille, T., Fossati, L., Fridlund, M., Gillon, M., Goeke, R. F., Goliguzova, M. V., Gonzales, E. J., Günther, M. N., Güdel, M., Heidari, N., Henze, C. E., Howell, S., Hoyer, S., Frey, J. I., Isaak, K. G., Jenkins, J. M., Kiefer, F., Kiss, L., Korth, J., Maxted, P. F.L., Laskar, J., des Etangs, A. Lecavelier, Lovis, C., Lund, M. B., Luque, R., Magrin, D., Almenara, J. M., Martioli, E., Mecina, M., Medina, J. V., Moldovan, D., Morales-Calderón, M., Morello, G., Moutou, C., Murgas, F., Jensen, E. L.N., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Demangeon, O. D.S., Smith, A. M.S., Santos, N., Scandariato, G., Seager, S., Sousa, S. G., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Walton, N., and Winn, J. N.
Abstract: HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R (HIP 9618 b) and 3.343 ± 0.039 R (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+−000512M☉) orbiting at 26.0+−111900 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.
Published: 2023

339. TESS and CHEOPS discover two warm sub-Neptunes transiting the bright K-dwarf HD 15906

Author: Tuson, A., Queloz, D., Osborn, H. P., Wilson, T. G., Hooton, M. J., Beck, M., Lendl, M., Olofsson, G., Fortier, A., Bonfanti, A., Brandeker, A., Buchhave, L. A., Cameron, A. Collier, Ciardi, D. R., Collins, K. A., Gandolfi, D., Garai, Z., Giacalone, S., da Silva, J. Gomes, Howell, S. B., Patel, J. A., Persson, C. M., Serrano, L. M., Sousa, S. G., Ulmer-Moll, S., Vanderburg, A., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C.C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Cabrera, J., Charnoz, S., Conti, D. M., Csizmadia, Sz, Cubillos, P. E., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D.S., Demory, B. O., Dragomir, D., Dressing, C. D., Ehrenreich, D., Erikson, A., Essack, Z., Farinato, J., Fossati, L., Fridlund, M., Furlan, E., Gill, H., Gillon, M., Gnilka, C. L., Gonzales, E., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Law, N., des Etangs, A. Lecavelier, Curto, G. Lo, Lovis, C., Luque, R., Magrin, D., Mann, A. W., Maxted, P. F.L., Mayor, M., McDermott, S., Mecina, M., Mordasini, C., Mortier, A., Nascimbeni, V., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Pritchard, T., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Ricker, G. R., Rieder, M., Santos, N. C., Savel, A. B., Scandariato, G., Schwarz, R. P., Seager, S., Ségransan, D., Shporer, A., Simon, A. E., Smith, A. M.S., Steller, M., Stockdale, C., Szabó, Gy M., Thomas, N., Torres, G., Tronsgaard, R., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Venturini, J., Walton, N. A., Winn, J. N., Wohler, B., Tuson, A., Queloz, D., Osborn, H. P., Wilson, T. G., Hooton, M. J., Beck, M., Lendl, M., Olofsson, G., Fortier, A., Bonfanti, A., Brandeker, A., Buchhave, L. A., Cameron, A. Collier, Ciardi, D. R., Collins, K. A., Gandolfi, D., Garai, Z., Giacalone, S., da Silva, J. Gomes, Howell, S. B., Patel, J. A., Persson, C. M., Serrano, L. M., Sousa, S. G., Ulmer-Moll, S., Vanderburg, A., Ziegler, C., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C.C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Cabrera, J., Charnoz, S., Conti, D. M., Csizmadia, Sz, Cubillos, P. E., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D.S., Demory, B. O., Dragomir, D., Dressing, C. D., Ehrenreich, D., Erikson, A., Essack, Z., Farinato, J., Fossati, L., Fridlund, M., Furlan, E., Gill, H., Gillon, M., Gnilka, C. L., Gonzales, E., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Law, N., des Etangs, A. Lecavelier, Curto, G. Lo, Lovis, C., Luque, R., Magrin, D., Mann, A. W., Maxted, P. F.L., Mayor, M., McDermott, S., Mecina, M., Mordasini, C., Mortier, A., Nascimbeni, V., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Pritchard, T., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Ricker, G. R., Rieder, M., Santos, N. C., Savel, A. B., Scandariato, G., Schwarz, R. P., Seager, S., Ségransan, D., Shporer, A., Simon, A. E., Smith, A. M.S., Steller, M., Stockdale, C., Szabó, Gy M., Thomas, N., Torres, G., Tronsgaard, R., Udry, S., Ulmer, B., Van Grootel, V., Vanderspek, R., Venturini, J., Walton, N. A., Winn, J. N., and Wohler, B.
Abstract: We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by ∼ 734 d, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS, and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 ± 0.08 R and a period of 10.924709 ± 0.000032 d, whilst HD 15906 c has a radius of 2.93+−000607 R and a period of 21.583298+−00000055000052 d. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 ± 13 K and 532 ± 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm (700 K) sub-Neptune sized planets transiting a bright star (G ≤ 10 mag). It is an excellent target for detailed characterization studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution.
Published: 2023

340. Detecting life outside our solar system with a large high-contrast-imaging mission

Author: Snellen, Ignas A.G., Snik, F., Kenworthy, M., Albrecht, S., Anglada-Escudé, G., Baraffe, I., Baudoz, P., Benz, W., Beuzit, J. L., Biller, B., Birkby, J. L., Boccaletti, A., van Boekel, R., de Boer, J., Brogi, Matteo, Buchhave, L., Carone, L., Claire, M., Claudi, R., Demory, B. O., Désert, J. M., Desidera, S., Gaudi, B. S., Gratton, R., Gillon, M., Grenfell, J. L., Guyon, O., Henning, T., Hinkley, S., Huby, E., Janson, M., Helling, C., Heng, K., Kasper, M., Keller, C. U., Krause, O., Kreidberg, L., Madhusudhan, N., Lagrange, A. M., Launhardt, R., Lenton, T. M., Lopez-Puertas, M., Maire, A. L., Mayne, N., Meadows, V., Mennesson, B., Micela, G., Miguel, Y., Milli, J., Min, M., de Mooij, E., Mouillet, D., N’Diaye, M., D’Orazi, V., Palle, E., Pagano, I., Piotto, G., Queloz, D., Rauer, H., Ribas, I., Ruane, G., Selsis, F., Sozzetti, A., Stam, D., Stark, C. C., Vigan, A., de Visser, Pieter, Snellen, Ignas A.G., Snik, F., Kenworthy, M., Albrecht, S., Anglada-Escudé, G., Baraffe, I., Baudoz, P., Benz, W., Beuzit, J. L., Biller, B., Birkby, J. L., Boccaletti, A., van Boekel, R., de Boer, J., Brogi, Matteo, Buchhave, L., Carone, L., Claire, M., Claudi, R., Demory, B. O., Désert, J. M., Desidera, S., Gaudi, B. S., Gratton, R., Gillon, M., Grenfell, J. L., Guyon, O., Henning, T., Hinkley, S., Huby, E., Janson, M., Helling, C., Heng, K., Kasper, M., Keller, C. U., Krause, O., Kreidberg, L., Madhusudhan, N., Lagrange, A. M., Launhardt, R., Lenton, T. M., Lopez-Puertas, M., Maire, A. L., Mayne, N., Meadows, V., Mennesson, B., Micela, G., Miguel, Y., Milli, J., Min, M., de Mooij, E., Mouillet, D., N’Diaye, M., D’Orazi, V., Palle, E., Pagano, I., Piotto, G., Queloz, D., Rauer, H., Ribas, I., Ruane, G., Selsis, F., Sozzetti, A., Stam, D., Stark, C. C., Vigan, A., and de Visser, Pieter
Abstract: In this White Paper, which was submitted in response to the European Space Agency (ESA) Voyage 2050 Call, we recommend the ESA plays a proactive role in developing a global collaborative effort to construct a large high-contrast imaging space telescope, e.g. as currently under study by NASA. Such a mission will be needed to characterize a sizable sample of temperate Earth-like planets in the habitable zones of nearby Sun-like stars and to search for extraterrestrial biological activity. We provide an overview of relevant European expertise, and advocate ESA to start a technology development program towards detecting life outside the Solar System.
Published: 2023

341. No random transits in CHEOPS observations of HD 139139

Author: Alonso, R., Hoyer, S., Deleuil, M., Simon, A. E., Beck, M., Benz, W., Florén, H. -G., Guterman, P., Borsato, L., Brandeker, A., Gandolfi, D., Wilson, T. G., Zingales, T., Alibert, Y., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Broeg, Ch., Charnoz, S., Cameron, A. Collier, van Damme, C. Corral, Sz., Csizmadia, Cubillos, P. E., Davies, M. B., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D, Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Isaak, K. G., Kiss, L. L., Kopp, E., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Magrin, D., Maxted, P. F. L., Mordasini, Ch., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Smith, A. M. S., Sousa, S. G., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van grootel, V., Venturini, J., Verrecchia, F., Walton, N. A., Alonso, R., Hoyer, S., Deleuil, M., Simon, A. E., Beck, M., Benz, W., Florén, H. -G., Guterman, P., Borsato, L., Brandeker, A., Gandolfi, D., Wilson, T. G., Zingales, T., Alibert, Y., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Broeg, Ch., Charnoz, S., Cameron, A. Collier, van Damme, C. Corral, Sz., Csizmadia, Cubillos, P. E., Davies, M. B., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D, Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gillon, M., Güdel, M., Günther, M. N., Heitzmann, A., Helling, Ch., Isaak, K. G., Kiss, L. L., Kopp, E., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Magrin, D., Maxted, P. F. L., Mordasini, Ch., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Smith, A. M. S., Sousa, S. G., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van grootel, V., Venturini, J., Verrecchia, F., and Walton, N. A.
Abstract: HD 139139 (a.k.a. 'The Random Transiter') is a star that exhibited enigmatic transit-like features with no apparent periodicity in K2 data. The shallow depth of the events ($\sim$200 ppm -- equivalent to transiting objects with radii of $\sim$1.5 R$_\oplus$ in front of a Sun-like star), and their non-periodicity, constitutes a challenge for the photometric follow-up of this star. The goal of this study is to confirm with independent measurements the presence of shallow, non-periodic transit-like features on this object. We performed observations with CHEOPS, for a total accumulated time of 12.75 d, distributed in visits of roughly 20 h in two observing campaigns in years 2021 and 2022. The precision of the data is sufficient to detect 150 ppm features with durations longer than 1.5 h. We use the duration and times of the events seen in the K2 curve to estimate how many should have been detected in our campaigns, under the assumption that their behaviour during the CHEOPS observations would be the same as in the K2 data of 2017. We do not detect events with depths larger than 150 ppm in our data set. If the frequency, depth, and duration of the events were the same as in the K2 campaign, we estimate the probability of having missed all events due to our limited observing window would be 4.8 %. We suggest three different scenarios to explain our results: 1) Our observing window was not long enough, and the events were missed with the estimated 4.8 % probability. 2) The events recorded in the K2 observations were time critical, and the mechanism producing them was either not active in the 2021 and 2022 campaigns or created shallower events under our detectability level. 3) The enigmatic events in the K2 data are the result of an unidentified and infrequent instrumental noise in the original data set or its data treatment., Comment: 7 pages, 3 figures, accepted for publication in A&A. Language-corrected version
Published: 2023
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342. Constraining the reflective properties of WASP-178b using Cheops photometry

Author: Pagano, I., Scandariato, G., Singh, V., Lendl, M., Queloz, D., Simon, A. E., Sousa, S. G., Brandeker, A., Cameron, A. Collier, Sulis, S., Van Grootel, V., Wilson, T. G., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bruno, G., Carone, L., Charnoz, S., van Damme, C. Corral, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mordasini, C., Munari, M., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Reimers, C., Ribas, I., Rieder, M., Santos, N. C., Ségransan, D., Smith, A. M. S., Stalport, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., Walton, N. A., Pagano, I., Scandariato, G., Singh, V., Lendl, M., Queloz, D., Simon, A. E., Sousa, S. G., Brandeker, A., Cameron, A. Collier, Sulis, S., Van Grootel, V., Wilson, T. G., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bruno, G., Carone, L., Charnoz, S., van Damme, C. Corral, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Magrin, D., Maxted, P. F. L., Mordasini, C., Munari, M., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Reimers, C., Ribas, I., Rieder, M., Santos, N. C., Ségransan, D., Smith, A. M. S., Stalport, M., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., and Walton, N. A.
Abstract: Multiwavelength photometry of the secondary eclipses of extrasolar planets is able to disentangle the reflected and thermally emitted light radiated from the planetary dayside. This leads to the measurement of the planetary geometric albedo $A_g$, which is an indicator of the presence of clouds in the atmosphere, and the recirculation efficiency $\epsilon$, which quantifies the energy transport within the atmosphere. In this work we aim to measure $A_g$ and $\epsilon$ for the planet WASP-178 b, a highly irradiated giant planet with an estimated equilibrium temperature of 2450 K.} We analyzed archival spectra and the light curves collected by Cheops and Tess to characterize the host WASP-178, refine the ephemeris of the system and measure the eclipse depth in the passbands of the two respective telescopes. We measured a marginally significant eclipse depth of 70$\pm$40 ppm in the Tess passband and statistically significant depth of 70$\pm$20 ppm in the Cheops passband. Combining the eclipse depth measurement in the Cheops (lambda_eff=6300 AA) and Tess (lambda_eff=8000 AA) passbands we constrained the dayside brightness temperature of WASP-178 b in the 2250-2800 K interval. The geometric albedo 0.1<$\rm A_g$<0.35 is in general agreement with the picture of poorly reflective giant planets, while the recirculation efficiency $\epsilon>$0.7 makes WASP-178 b an interesting laboratory to test the current heat recirculation models., Comment: Accepted by Astronomy and Astrophysics on 31/08/2023
Published: 2023

343. Refining the properties of the TOI-178 system with CHEOPS and TESS

Author: Delrez, L., Leleu, A., Brandeker, A., Gillon, M., Hooton, M. J., Cameron, A. Collier, Deline, A., Fortier, A., Queloz, D., Bonfanti, A., Van Grootel, V., Wilson, T. G., Egger, J. A., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Buder, M., Cabrera, J., Cessa, V., Charnoz, S., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Güdel, M., Hasiba, J., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Etangs, A. Lecavelier des, Lendl, M., Lovis, C., Luque, R., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Santos, N. C., Scandariato, G., Seager, S., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Vanderspek, R., Venturini, J., Viotto, V., Walton, N. A., Winn, J. N., Delrez, L., Leleu, A., Brandeker, A., Gillon, M., Hooton, M. J., Cameron, A. Collier, Deline, A., Fortier, A., Queloz, D., Bonfanti, A., Van Grootel, V., Wilson, T. G., Egger, J. A., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Buder, M., Cabrera, J., Cessa, V., Charnoz, S., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Güdel, M., Hasiba, J., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kiss, L. L., Laskar, J., Latham, D. W., Etangs, A. Lecavelier des, Lendl, M., Lovis, C., Luque, R., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Ricker, G., Santos, N. C., Scandariato, G., Seager, S., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Vanderspek, R., Venturini, J., Viotto, V., Walton, N. A., and Winn, J. N.
Abstract: The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. Mass estimates derived from a preliminary radial velocity (RV) dataset suggest that the planetary densities do not decrease in a monotonic way with the orbital distance to the star, contrary to what one would expect based on simple formation and evolution models. To improve the characterisation of this key system and prepare for future studies (in particular with JWST), we perform a detailed photometric study based on 40 new CHEOPS visits, one new TESS sector, as well as previously published CHEOPS, TESS, and NGTS data. First we perform a global analysis of the 100 transits contained in our data to refine the transit parameters of the six planets and study their transit timing variations (TTVs). We then use our extensive dataset to place constraints on the radii and orbital periods of potential additional transiting planets in the system. Our analysis significantly refines the transit parameters of the six planets, most notably their radii, for which we now obtain relative precisions $\lesssim$3%, with the exception of the smallest planet $b$ for which the precision is 5.1%. Combined with the RV mass estimates, the measured TTVs allow us to constrain the eccentricities of planets $c$ to $g$, which are found to be all below 0.02, as expected from stability requirements. Taken alone, the TTVs also suggest a higher mass for planet $d$ than the one estimated from the RVs, which had been found to yield a surprisingly low density for this planet. However, the masses derived from the current TTV dataset are very prior-dependent and further observations, over a longer temporal baseline, are needed to deepen our understanding of this iconic planetary system., Comment: 20 pages, 5 figures, 9 tables. Accepted for publication in A&A
Published: 2023
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344. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS$_4$ measured from stellar occultations

Author: Rommel, F. L., Braga-Ribas, F., Ortiz, J. L., Sicardy, B., Santos-Sanz, P., Desmars, J., Camargo, J. I. B., Vieira-Martins, R., Assafin, M., Morgado, B. E., Boufleur, R. C., Benedetti-Rossi, G., Gomes-Júnior, A. R., Fernández-Valenzuela, E., Holler, B. J., Souami, D., Duffard, R., Margoti, G., Vara-Lubiano, M., Lecacheux, J., Plouvier, J. L., Morales, N., Maury, A., Fabrega, J., Ceravolo, P., Jehin, E., Albanese, D., Mariey, H., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, R., Aissa, D. Baba, Gringahcene, Z., Kashuba, V., Koshkin, N., Zhukov, V., Fişek, S., Çakır, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, T., Pereira, C. L., Emilio, M., Burdanov, A. Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Sanchez, R. Zanmar, Tagliaferri, U., Di Sora, M., Isopi, G., Krugly, Y., Slyusarev, I., Chiorny, V., Mikuž, H., Bacci, P., Maestripieri, M., Grazia, M. D., de la Cueva, I., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O. M., Serra-Ricart, M., Alarcon, M. R., Licandro, J., Masi, G., Bacci, R., Bosch, J. M., Behem, R., Prost, J. -P., Renner, S., Conjat, M., Bachini, M., Succi, G., Stoian, L., Juravle, A., Carosati, D., Gowe, B., Carrillo, J., Zheleznyak, A. P., Montigiani, N., Foster, C. R., Mannucci, M., Ruocco, N., Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Collins, M., Pál, A., Csák, B., Fernández-Garcia, E., Castro-Tirado, A. J., Hudin, L., Madiedo, J. M., Anghel, R. M., Calvo-Fernández, J. F., Valvasori, A., Guido, E., Gherase, R. M., Kamoun, S., Fafet, R., Sánchez-González, M., Curelaru, L., Vîntdevară, C. D., Danescu, C. A., Gout, J. -F., Schmitz, C. J., Sota, A., Belskaya, I., Rodríguez-Marco, M., Kilic, Y., Frappa, E., Klotz, A., Lavayssière, M., Oliveira, J. Marques, Popescu, M., Mammana, L. A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Pribulla, T., Tomko, D., Husárik, M., Erece, O., Eryilmaz, S., Buzzi, L., Gährken, B., Nardiello, D., Hornoch, K., Sonbas, E., Er, H., Burwitz, V., Sybilski, P. Waldemar, Bykowski, W., Müller, T. G., Ogloza, W., Gonçalves, R., Ferreira, J. F., Ferreira, M., Bento, M., Meister, S., Bagiran, M. N., Tekeş, M., Marciniak, A., Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G. B., Boutet, M., Sanchez, J., Klemt, B., Wuensche, N., Burzynski, W., Borkowski, M., Serrau, M., Dangl, G., Klös, O., Weber, C., Urbaník, M., Rousselot, L., Kubánek, J., André, P., Colazo, C., Spagnotto, J., Sickafoose, A. A., Hueso, R., Sánchez-Lavega, A., Fisher, R. S., Rengstorf, A. W., Perelló, C., Dascalu, M., Altan, M., Gazeas, K., de Santana, T., Sfair, R., Winter, O. C., Kalkan, S., Canales-Moreno, O., Trigo-Rodríguez, J. M., Tsamis, V., Tigani, K., Sioulas, N., Lekkas, G., Bertesteanu, D. N., Dumitrescu, V., Wilberger, A. J., Barnes, J. W., Fieber-Beyer, S. K., Swaney, R. L., Fuentes, C., Mendez, R. A., Dumitru, B. D., Flynn, R. L., Wake, D. A., Rommel, F. L., Braga-Ribas, F., Ortiz, J. L., Sicardy, B., Santos-Sanz, P., Desmars, J., Camargo, J. I. B., Vieira-Martins, R., Assafin, M., Morgado, B. E., Boufleur, R. C., Benedetti-Rossi, G., Gomes-Júnior, A. R., Fernández-Valenzuela, E., Holler, B. J., Souami, D., Duffard, R., Margoti, G., Vara-Lubiano, M., Lecacheux, J., Plouvier, J. L., Morales, N., Maury, A., Fabrega, J., Ceravolo, P., Jehin, E., Albanese, D., Mariey, H., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, R., Aissa, D. Baba, Gringahcene, Z., Kashuba, V., Koshkin, N., Zhukov, V., Fişek, S., Çakır, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, T., Pereira, C. L., Emilio, M., Burdanov, A. Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Sanchez, R. Zanmar, Tagliaferri, U., Di Sora, M., Isopi, G., Krugly, Y., Slyusarev, I., Chiorny, V., Mikuž, H., Bacci, P., Maestripieri, M., Grazia, M. D., de la Cueva, I., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O. M., Serra-Ricart, M., Alarcon, M. R., Licandro, J., Masi, G., Bacci, R., Bosch, J. M., Behem, R., Prost, J. -P., Renner, S., Conjat, M., Bachini, M., Succi, G., Stoian, L., Juravle, A., Carosati, D., Gowe, B., Carrillo, J., Zheleznyak, A. P., Montigiani, N., Foster, C. R., Mannucci, M., Ruocco, N., Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Collins, M., Pál, A., Csák, B., Fernández-Garcia, E., Castro-Tirado, A. J., Hudin, L., Madiedo, J. M., Anghel, R. M., Calvo-Fernández, J. F., Valvasori, A., Guido, E., Gherase, R. M., Kamoun, S., Fafet, R., Sánchez-González, M., Curelaru, L., Vîntdevară, C. D., Danescu, C. A., Gout, J. -F., Schmitz, C. J., Sota, A., Belskaya, I., Rodríguez-Marco, M., Kilic, Y., Frappa, E., Klotz, A., Lavayssière, M., Oliveira, J. Marques, Popescu, M., Mammana, L. A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Pribulla, T., Tomko, D., Husárik, M., Erece, O., Eryilmaz, S., Buzzi, L., Gährken, B., Nardiello, D., Hornoch, K., Sonbas, E., Er, H., Burwitz, V., Sybilski, P. Waldemar, Bykowski, W., Müller, T. G., Ogloza, W., Gonçalves, R., Ferreira, J. F., Ferreira, M., Bento, M., Meister, S., Bagiran, M. N., Tekeş, M., Marciniak, A., Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G. B., Boutet, M., Sanchez, J., Klemt, B., Wuensche, N., Burzynski, W., Borkowski, M., Serrau, M., Dangl, G., Klös, O., Weber, C., Urbaník, M., Rousselot, L., Kubánek, J., André, P., Colazo, C., Spagnotto, J., Sickafoose, A. A., Hueso, R., Sánchez-Lavega, A., Fisher, R. S., Rengstorf, A. W., Perelló, C., Dascalu, M., Altan, M., Gazeas, K., de Santana, T., Sfair, R., Winter, O. C., Kalkan, S., Canales-Moreno, O., Trigo-Rodríguez, J. M., Tsamis, V., Tigani, K., Sioulas, N., Lekkas, G., Bertesteanu, D. N., Dumitrescu, V., Wilberger, A. J., Barnes, J. W., Fieber-Beyer, S. K., Swaney, R. L., Fuentes, C., Mendez, R. A., Dumitru, B. D., Flynn, R. L., and Wake, D. A.
Abstract: This work aims at constraining the size, shape, and geometric albedo of the dwarf planet candidate 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also studied the object's topography by analyzing the obtained limb and the residuals between observed chords and the best-fitted ellipse. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with three to up to sixty-one positive chords. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fitted ellipse, combined with the object's rotational information from the literature, constrains the object's size, shape, and albedo. Additionally, we developed a new method to characterize topography features on the object's limb. The global limb has a semi-major axis of 412 $\pm$ 10 km, a semi-minor axis of 385 $\pm$ 17 km, and the position angle of the minor axis is 121 $^\circ$ $\pm$ 16$^\circ$. From this instantaneous limb, we obtained 2002 MS4's geometric albedo and the projected area-equivalent diameter. Significant deviations from the fitted ellipse in the northernmost limb are detected from multiple sites highlighting three distinct topographic features: one 11 km depth depression followed by a 25$^{+4}_{-5}$ km height elevation next to a crater-like depression with an extension of 322 $\pm$ 39 km and 45.1 $\pm$ 1.5 km deep. Our results present an object that is $\approx$138 km smaller in diameter than derived from thermal data, possibly indicating the presence of a so-far unknown satellite. However, within the error bars, the geometric albedo in the V-band agrees with the results published in the literature, even with the radiometric-derived albedo.
Published: 2023
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345. CHEOPS and TESS view of the ultra-short period super-Earth TOI-561 b

Author: Patel, J. A., Egger, J. A., Wilson, T. G., Bourrier, V., Carone, L., Beck, M., Ehrenreich, D., Sousa, S. G., Benz, W., Brandeker, A., Deline, A., Alibert, Y., Lam, K. W. F., Lendl, M., Alonso, R., Anglada, G., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Broeg, C., Busch, M. -D., Cabrera, J., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Viotto, V., Walton, N. A., Patel, J. A., Egger, J. A., Wilson, T. G., Bourrier, V., Carone, L., Beck, M., Ehrenreich, D., Sousa, S. G., Benz, W., Brandeker, A., Deline, A., Alibert, Y., Lam, K. W. F., Lendl, M., Alonso, R., Anglada, G., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, T., Billot, N., Bonfils, X., Broeg, C., Busch, M. -D., Cabrera, J., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Isaak, K. G., Kiss, L. L., Kopp, E., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Viotto, V., and Walton, N. A.
Abstract: Ultra-short period planets (USPs) are a unique class of super-Earths with an orbital period of less than a day and hence subject to intense radiation from their host star. While most of them are consistent with bare rocks, some show evidence of a heavyweight envelope, which could be a water layer or a secondary metal-rich atmosphere sustained by an outgassing surface. Much remains to be learned about the nature of USPs. The prime goal of the present work is to study the bulk planetary properties and atmosphere of TOI-561b, through the study of its transits and occultations. We obtained ultra-precise transit photometry of TOI-561b with CHEOPS and performed a joint analysis of this data with four TESS sectors. Our analysis of TOI-561b transit photometry put strong constraints on its properties, especially on its radius, Rp=1.42 +/- 0.02 R_Earth (at ~2% error). The internal structure modelling of the planet shows that the observations are consistent with negligible H/He atmosphere, however requiring other lighter materials, in addition to pure iron core and silicate mantle to explain the observed density. We find that this can be explained by the inclusion of a water layer in our model. We searched for variability in the measured Rp/R* over time to trace changes in the structure of the planetary envelope but none found within the data precision. In addition to the transit event, we tentatively detect occultation signal in the TESS data with an eclipse depth of ~27 +/- 11 ppm. Using the models of outgassed atmospheres from the literature we find that the thermal emission from the planet can mostly explain the observation. Based on this, we predict that NIR/MIR observations with JWST should be able to detect silicate species in the atmosphere of the planet. This could also reveal important clues about the planetary interior and help disentangle planet formation and evolution models., Comment: 17 pages, 10 + 3 figures, 4 tables, accepted for publication in A&A (abstract abbreviated)
Published: 2023
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346. TESS discovery of a super-Earth orbiting the M dwarf star TOI-1680

Author: Ghachoui, M., Soubkiou, A., Wells, R. D., Rackham, B. V., Triaud, A. H. M. J., Sebastian, D., Giacalone, S., Stassun, K. G., Ciardi, D. R., Collins, K. A., Liu, A., Chew, Y. Gómez Maqueo, Gillon, M., Benkhaldoun, Z., Delrez, L., Eastman, J. D., Demangeon, O., Barkaoui, K., Burdanov, A., Demory, B. -O., de Wit, J., Dransfield, G., Ducrot, E., Garcia, L., Gómez-Muñoz, M. A., Hooton, M. J., Jehin, E., Murray, C. A., Pedersen, P. P., Pozuelos, F. J., Queloz, D., Sabin, L., Schanche, N., Timmermans, M., Gonzales, E. J., Dressing, C. D., Aganze, C., Burgasser, A. J., Gerasimov, R., Hsu, C., Theissen, C. A., Charbonneau, D., Jenkins, J. M., Latham, D. W., Ricker, G., Seager, S., Shporer, A., Twicken, J. D., Vanderspek, R., Winn, J. N., Collins, K. I., Fukui, A., Gan, T., Narita, N., Schwarz, R. P., Ghachoui, M., Soubkiou, A., Wells, R. D., Rackham, B. V., Triaud, A. H. M. J., Sebastian, D., Giacalone, S., Stassun, K. G., Ciardi, D. R., Collins, K. A., Liu, A., Chew, Y. Gómez Maqueo, Gillon, M., Benkhaldoun, Z., Delrez, L., Eastman, J. D., Demangeon, O., Barkaoui, K., Burdanov, A., Demory, B. -O., de Wit, J., Dransfield, G., Ducrot, E., Garcia, L., Gómez-Muñoz, M. A., Hooton, M. J., Jehin, E., Murray, C. A., Pedersen, P. P., Pozuelos, F. J., Queloz, D., Sabin, L., Schanche, N., Timmermans, M., Gonzales, E. J., Dressing, C. D., Aganze, C., Burgasser, A. J., Gerasimov, R., Hsu, C., Theissen, C. A., Charbonneau, D., Jenkins, J. M., Latham, D. W., Ricker, G., Seager, S., Shporer, A., Twicken, J. D., Vanderspek, R., Winn, J. N., Collins, K. I., Fukui, A., Gan, T., Narita, N., and Schwarz, R. P.
Abstract: We report the discovery by the TESS mission of a super-Earth on a 4.8-d orbit around an inactive M4.5 dwarf (TOI-1680) validated by ground-based facilities. The host star is located 37.14 pc away, with a radius of 0.2100+/-0.0064 R_sun, mass of 0.1800+/-0.0044 M_sun and an effective temperature of 3211+/-100 K. We validated and characterized the planet using TESS data, ground-based multi-wavelength photometry from TRAPPIST, SPECULOOS, and LCO, as well as high-resolution AO observations from Keck/NIRC2 and Shane. Our analyses have determined the following parameters for the planet: a radius of 1.466+0.063/-0.049 R_earth and an equilibrium temperature of 404+/-14 K, assuming no albedo and perfect heat redistribution. Assuming a mass based on mass-radius relations, this planet is a promising target for atmospheric characterization with the James Webb Space Telescope (JWST)., Comment: Accepted in A&A
Published: 2023
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347. Investigating the visible phase-curve variability of 55 Cnc e

Author: Valdés, E. A. Meier, Morris, B. M., Demory, B. -O., Brandeker, A., Kitzmann, D., Benz, W., Deline, A., Florén, H. -G., Sousa, S. G., Bourrier, V., Singh, V., Heng, K., Strugarek, A., Bower, D. J., Jäggi, N., Carone, L., Lendl, M., Jones, K., Oza, A. V., Demangeon, O. D. S., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Cabrera, J., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Delrez, L., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Sarajlic, M., Scandariato, G., Ségransan, D., Sicilia, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., Walton, N. A., Wilson, T. G., Wolter, D., Valdés, E. A. Meier, Morris, B. M., Demory, B. -O., Brandeker, A., Kitzmann, D., Benz, W., Deline, A., Florén, H. -G., Sousa, S. G., Bourrier, V., Singh, V., Heng, K., Strugarek, A., Bower, D. J., Jäggi, N., Carone, L., Lendl, M., Jones, K., Oza, A. V., Demangeon, O. D. S., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Cabrera, J., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Delrez, L., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Sarajlic, M., Scandariato, G., Ségransan, D., Sicilia, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., Walton, N. A., Wilson, T. G., and Wolter, D.
Abstract: 55 Cnc e is an ultra-short period super-Earth transiting a Sun-like star. Previous observations in the optical range detected a time-variable flux modulation that is phased with the planetary orbital period, whose amplitude is too large to be explained by reflected light and thermal emission alone. The goal of the study is to investigate the origin of the variability and timescale of the phase-curve modulation in 55 Cnc e. To this end, we used the CHaracterising ExOPlanet Satellite (CHEOPS), whose exquisite photometric precision provides an opportunity to characterise minute changes in the phase curve from one orbit to the next. CHEOPS observed 29 individual visits of 55 Cnc e between March 2020 and February 2022. Based on these observations, we investigated the different processes that could be at the origin of the observed modulation. In particular, we built a toy model to assess whether a circumstellar torus of dust driven by radiation pressure and gravity might match the observed flux variability timescale. We find that the phase-curve amplitude and peak offset of 55 Cnc e do vary between visits. The sublimation timescales of selected dust species reveal that silicates expected in an Earth-like mantle would not survive long enough to explain the observed phase-curve modulation. We find that silicon carbide, quartz, and graphite are plausible candidates for the circumstellar torus composition because their sublimation timescales are long. The extensive CHEOPS observations confirm that the phase-curve amplitude and offset vary in time.We find that dust could provide the grey opacity source required to match the observations. However, the data at hand do not provide evidence that circumstellar material with a variable grain mass per unit area causes the observed variability. Future observations with the James Webb Space Telescope promise exciting insights into this iconic super-Earth., Comment: 27 pages, 22 figures. Accepted for publication on A&A
Published: 2023
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348. TOI-2084 b and TOI-4184 b: two new sub-Neptunes around M dwarf stars

Author: Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-Reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B. -O., de Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-Gaxiola, S., Ghachoui, M., Chew, Y. Gómez Maqueo, Günther, M. N., McCormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-López, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., Zúñiga-Fernández, S., Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-Reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B. -O., de Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-Gaxiola, S., Ghachoui, M., Chew, Y. Gómez Maqueo, Günther, M. N., McCormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-López, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., and Zúñiga-Fernández, S.
Abstract: We present the discovery and validation of two TESS exoplanets orbiting nearby M dwarfs: TOI-2084b, and TOI-4184b. We characterized the host stars by combining spectra from Shane/Kast and Magellan/FIRE, SED (Spectral Energy Distribution) analysis, and stellar evolutionary models. In addition, we used Gemini-South/Zorro & -North/Alopeke high-resolution imaging, archival science images, and statistical validation packages to support the planetary interpretation. We performed a global analysis of multi-colour photometric data from TESS and ground-based facilities in order to derive the stellar and planetary physical parameters for each system. We find that TOI-2084b and TOI-4184b are sub-Neptune-sized planets with radii of Rp = 2.47 +/- 0.13R_Earth and Rp = 2.43 +/- 0.21R_Earth, respectively. TOI-2084b completes an orbit around its host star every 6.08 days, has an equilibrium temperature of T_eq = 527 +/- 8K and an irradiation of S_p = 12.8 +/- 0.8 S_Earth. Its host star is a dwarf of spectral M2.0 +/- 0.5 at a distance of 114pc with an effective temperature of T_eff = 3550 +/- 50 K, and has a wide, co-moving M8 companion at a projected separation of 1400 au. TOI-4184b orbits around an M5.0 +/- 0.5 type dwarf star (Kmag = 11.87) each 4.9 days, and has an equilibrium temperature of T_eq = 412 +/- 8 K and an irradiation of S_p = 4.8 +/- 0.4 S_Earth. TOI-4184 is a metal poor star ([Fe/H] = -0.27 +/- 0.09 dex) at a distance of 69 pc with an effective temperature of T_eff = 3225 +/- 75 K. Both planets are located at the edge of the sub-Jovian desert in the radius-period plane. The combination of the small size and the large infrared brightness of their host stars make these new planets promising targets for future atmospheric exploration with JWST., Comment: Accepted for publication in A&A
Published: 2023

349. Refined parameters of the HD 22946 planetary system and the true orbital period of planet d

Author: Garai, Z., Osborn, H. P., Gandolfi, D., Brandeker, A., Sousa, S. G., Lendl, M., Bekkelien, A., Broeg, C., Cameron, A. Collier, Egger, J. A., Hooton, M. J., Alibert, Y., Delrez, L., Fossati, L., Salmon, S., Wilson, T. G., Bonfanti, A., Tuson, A., Ulmer-Moll, S., Serrano, L. M., Borsato, L., Alonso, R., Anglada, G., Asquier, J., Navascues, D. Barrado y, Barros, S. C. C., Bárczy, T., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Biondi, F., Bonfils, X., Buder, M., Cabrera, J., Cessa, V., Charnoz, S., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Van Eylen, V., Fortier, A., Fridlund, M., Gillon, M., Van Grootel, V., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Kiss, L. L., Kristiansen, M. H., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Luntzer, A., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., Walton, N., Garai, Z., Osborn, H. P., Gandolfi, D., Brandeker, A., Sousa, S. G., Lendl, M., Bekkelien, A., Broeg, C., Cameron, A. Collier, Egger, J. A., Hooton, M. J., Alibert, Y., Delrez, L., Fossati, L., Salmon, S., Wilson, T. G., Bonfanti, A., Tuson, A., Ulmer-Moll, S., Serrano, L. M., Borsato, L., Alonso, R., Anglada, G., Asquier, J., Navascues, D. Barrado y, Barros, S. C. C., Bárczy, T., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Biondi, F., Bonfils, X., Buder, M., Cabrera, J., Cessa, V., Charnoz, S., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Van Eylen, V., Fortier, A., Fridlund, M., Gillon, M., Van Grootel, V., Güdel, M., Günther, M. N., Hoyer, S., Isaak, K. G., Kiss, L. L., Kristiansen, M. H., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Luntzer, A., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Venturini, J., and Walton, N.
Abstract: Multi-planet systems are important sources of information regarding the evolution of planets. However, the long-period planets in these systems often escape detection. HD 22946 is a bright star around which 3 transiting planets were identified via TESS photometry, but the true orbital period of the outermost planet d was unknown until now. We aim to use CHEOPS to uncover the true orbital period of HD 22946d and to refine the orbital and planetary properties of the system, especially the radii of the planets. We used the available TESS photometry of HD 22946 and observed several transits of the planets b, c, and d using CHEOPS. We identified 2 transits of planet d in the TESS photometry, calculated the most probable period aliases based on these data, and then scheduled CHEOPS observations. The photometric data were supplemented with ESPRESSO radial velocity data. Finally, a combined model was fitted to the entire dataset. We successfully determined the true orbital period of the planet d to be 47.42489 $\pm$ 0.00011 d, and derived precise radii of the planets in the system, namely 1.362 $\pm$ 0.040 R$_\oplus$, 2.328 $\pm$ 0.039 R$_\oplus$, and 2.607 $\pm$ 0.060 R$_\oplus$ for planets b, c, and d, respectively. Due to the low number of radial velocities, we were only able to determine 3$\sigma$ upper limits for these respective planet masses, which are 13.71 M$_\oplus$, 9.72 M$_\oplus$, and 26.57 M$_\oplus$. We estimated that another 48 ESPRESSO radial velocities are needed to measure the predicted masses of all planets in HD 22946. Planet c appears to be a promising target for future atmospheric characterisation. We can also conclude that planet d, as a warm sub-Neptune, is very interesting because there are only a few similar confirmed exoplanets to date. Such objects are worth investigating in the near future, for example in terms of their composition and internal structure.
Published: 2023
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350. TOI-5678 b: A 48-day transiting Neptune-mass planet characterized with CHEOPS and HARPS

Author: Ulmer-Moll, S., Osborn, H. P., Tuson, A., Egger, J. A., Lendl, M., Maxted, P., Bekkelien, A., Simon, A. E., Olofsson, G., Adibekyan, V., Alibert, Y., Bonfanti, A., Bouchy, F., Brandeker, A., Fridlund, M., Gandolfi, D., Mordasini, C., Persson, C. M., Salmon, S., Serrano, L. M., Sousa, S. G., Wilson, T. G., Rieder, M., Hasiba, J., Asquier, J., Sicilia, D., Walter, I., Alonso, R., Anglada, G., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bárczy, T., Cabrera, J., Charnoz, S., Cointepas, M., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dumusque, X., Ehrenreich, D., Eisner, N. L., Erikson, A., Fortier, A., Fossati, L., Gillon, M., Grieves, N., Güdel, M., Hagelberg, J., Helled, R., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Nascimbeni, V., Otegi, J., Ottensammer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Psaridi, A., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Smith, A. M. S., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Van Grootel, V., Venturini, J., Walton, N. A., Ulmer-Moll, S., Osborn, H. P., Tuson, A., Egger, J. A., Lendl, M., Maxted, P., Bekkelien, A., Simon, A. E., Olofsson, G., Adibekyan, V., Alibert, Y., Bonfanti, A., Bouchy, F., Brandeker, A., Fridlund, M., Gandolfi, D., Mordasini, C., Persson, C. M., Salmon, S., Serrano, L. M., Sousa, S. G., Wilson, T. G., Rieder, M., Hasiba, J., Asquier, J., Sicilia, D., Walter, I., Alonso, R., Anglada, G., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Borsato, L., Broeg, C., Bárczy, T., Cabrera, J., Charnoz, S., Cointepas, M., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., Demory, B. -O., Dumusque, X., Ehrenreich, D., Eisner, N. L., Erikson, A., Fortier, A., Fossati, L., Gillon, M., Grieves, N., Güdel, M., Hagelberg, J., Helled, R., Hoyer, S., Isaak, K. G., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lovis, C., Magrin, D., Nascimbeni, V., Otegi, J., Ottensammer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Psaridi, A., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Smith, A. M. S., Steller, M., Szabó, G. M., Ségransan, D., Thomas, N., Udry, S., Van Grootel, V., Venturini, J., and Walton, N. A.
Abstract: A large sample of long-period giant planets has been discovered thanks to long-term radial velocity surveys, but only a few dozen of these planets have a precise radius measurement. Transiting gas giants are crucial targets for the study of atmospheric composition across a wide range of equilibrium temperatures and for shedding light on the formation and evolution of planetary systems. Indeed, compared to hot Jupiters, the atmospheric properties and orbital parameters of cooler gas giants are unaltered by intense stellar irradiation and tidal effects. We identify long-period planets in the Transiting Exoplanet Survey Satellite (TESS) data as duo-transit events. To solve the orbital periods of TESS duo-transit candidates, we use the CHaracterising ExOPlanet Satellite (CHEOPS) to observe the highest-probability period aliases in order to discard or confirm a transit event at a given period. We also collect spectroscopic observations with CORALIE and HARPS in order to confirm the planetary nature and measure the mass of the candidates. We report the discovery of a warm transiting Neptune-mass planet orbiting TOI-5678. After four non-detections corresponding to possible periods, CHEOPS detected a transit event matching a unique period alias. Joint modeling reveals that TOI-5678 hosts a 47.73 day period planet. TOI-5678 b has a mass of 20 (+-4) Me and a radius of 4.91 (+-0.08 Re) . Using interior structure modeling, we find that TOI-5678 b is composed of a low-mass core surrounded by a large H/He layer with a mass of 3.2 (+1.7, -1.3) Me. TOI-5678 b is part of a growing sample of well-characterized transiting gas giants receiving moderate amounts of stellar insolation (11 Se). Precise density measurement gives us insight into their interior composition, and the objects orbiting bright stars are suitable targets to study the atmospheric composition of cooler gas giants., Comment: 17 pages, 10 figures, accepted to A&A
Published: 2023
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