Precise masses for the transiting planetary system HD 106315 with HARPS

Barros, S. C. C.; Gosselin, H.; Lillo-Box, J.; Bayliss, Daniel; Delgado-Mena, E.; Brugger, B.; Santerne, A.; Armstrong, David J.; Adibekyan, V.; Armstrong, J. D.; Barrado, D.; Bento, J.; Boisse, I.; Bonomo, A. S.; Bouchy, F.; Brown, D. J. A.; Cochran, William D.; Cameron, A. Collier; Deleuil, M.; Demangeon, O.; Díaz, R. F.; Doyle, A. P.; Dumusque, X.; Ehrenreich, D.; Espinoza, N.; Faedi, F.; Faria, J. P.; Figueira, P.; Foxell, Emma; Hébrard, G.; Hojjatpanah, S.; Jackman, James A. G.; Lendl, M.; Ligi, R.; Lovis, C.; Melo, C.; Mousis, O.; Neal, J. J.; Osborn, H.; Pollacco, D.; Santos, N. C.; Sefako, Ramotholo; Shporer, Avi; Sousa, S. G.; Triaud, A. H. M. J.; Udry, S.; Vigan, A.; Wyttenbach, A.

doi:10.1051/0004-6361/201731276

Cited by 27 publications

(42 citation statements)

References 89 publications

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“…This system was further characterized with HARPS radial velocity observations by Barros et al (2017) to determine the planets' masses (M b =12.6 ± 3.2 M ⊕ and M c =15.2 ± 3.7 M ⊕ ). They concluded that HD 106315 b likely has a rocky core and decent water mass fraction whereas HD 106315 c has a substantial hydrogen-helium envelope.…”

Section: Hd 106315mentioning

confidence: 99%

“…Additional transits of HD 106315 c were observed with two ground based facilities: the Euler telescope (Lendl et al 2017) and the Cerro Tololo Inter-American Observatory (CTIO, Barros et al 2017). These measurements both improved the precision on the orbital period and the time of transit.…”

Section: Hd 106315mentioning

confidence: 99%

“…We ran a Markov-Chain Monte Carlo (MCMC) analysis to estimate parameter uncertainties, using the systematic model in addition to a transit signal which we modeled using batman (Kreidberg 2015). We fixed the period of each planet to the most recent measurements (Barros et al 2017;Rice et al 2019) and allowed the transit depth, center, orbital inclination, and semi major axis to vary. We also left the uncertainty of the data points as a free parameter, which we found converged to the RMS scatter of the raw light curve.…”

Section: Spitzer Transitsmentioning

confidence: 99%

“…We calculated updated ephemerides (Table 2) to further refine the time of conjunction and orbital period for future atmospheric follow-up and to better constrain these values in our radial velocity fits (Section 5). We fit a straight line to the transit centers obtained from each individual observation, incorporating all ground-based published transits thus far (Lendl et al 2017;Barros et al 2017). These planets will be accessible for future transmission spectroscopy observations throughout the JWST era; as an example, the transit time uncertainty in 2025 is under two hours for all five planets (GJ 9827 b: 0.1hr, GJ 9827 c: 0.5hr, GJ 9827 d: 0.1hr, HD 106315 b: 1.7hr, HD 106315 c: 0.4hr).…”

Section: Spitzer Transitsmentioning

confidence: 99%

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Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827* †

Kosiarek

Berardo

Crossfield

et al. 2020

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HD 106315 and GJ 9827 are two bright, nearby stars that host multiple super-Earths and sub-Neptunes discovered by K2 that are well suited for atmospheric characterization. We refined the planets' ephemerides through Spitzer transits, enabling accurate transit prediction required for future atmospheric characterization through transmission spectroscopy. Through a multi-year high-cadence observing campaign with Keck/HIRES and Magellan/PFS, we improved the planets' mass measurements in anticipation of HST transmission spectroscopy. For GJ 9827, we modeled activity-induced radial velocity signals with a Gaussian process informed from the Calcium II H&K lines in order to more accurately model the effect of stellar noise on our data. We found planet masses of M b =4.87±0.37 M ⊕ , M c =1.92 ± 0.49 M ⊕ , and M d =3.42 ± 0.62 M ⊕ . For HD 106315, we found that such activity-radial velocity decorrelation was not effective due to the reduced presence of spots and speculate that this may extend to other hot stars as well (T eff > 6200 K). We found planet masses of M b =10.5 ± 3.1 M ⊕ and M c =12.0 ± 3.8 M ⊕ . We investigated all of the planets' compositions through comparing their masses and radii to a range of interior models. GJ 9827 b and GJ 9827 c are both consistent with an Earth-like rocky composition, GJ 9827 d and HD 106315 b both require additional volatiles and are consistent with moderate amounts of water or hydrogen/helium, and HD 106315 c is consistent with 10% hydrogen/helium by mass.

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Section: Hd 106315mentioning

confidence: 99%

Section: Hd 106315mentioning

confidence: 99%

Section: Spitzer Transitsmentioning

confidence: 99%

Section: Spitzer Transitsmentioning

confidence: 99%

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Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827* †

Kosiarek

Berardo

Crossfield

et al. 2020

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“…Our choice for the planetary radius, R p /R N =0.6, corresponds to a density of Barnard b equal to that of Neptune and the mass for an edge-on orbit (M p =M min /sin(90 • )). According to Barros et al (2017), this mass and radius would correspond to a gaseous exoplanet. Any other orbital inclination would suggest a more massive and probably larger planet size, entailing better conditions for the planet to retain a H 2 -He atmosphere.…”

Section: Adopted True Configurationsmentioning

confidence: 99%

Directly imaged exoplanets in reflected starlight. The importance of knowing the planet radius

Carrión-González¹,

Muñoz²,

Cabrera³

et al. 2024

Preprint

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Context. The direct imaging of exoplanets in reflected starlight will represent a major advance in the study of cold and temperate exoplanet atmospheres. Understanding how basic planet and atmospheric properties may affect the measured spectra is key to their interpretation. Aims. We have investigated the information content in reflected-starlight spectra of exoplanets. We specify our analysis to Barnard's Star b candidate super-Earth, for which we assume a radius 0.6 times that of Neptune, an atmosphere dominated by H 2-He, and a CH 4 volume mixing ratio of 5•10 −3. The main conclusions of our study are however planet-independent. Methods. We set up a model of the exoplanet described by seven parameters including its radius, atmospheric methane abundance and basic properties of a cloud layer. We generate synthetic spectra at zero phase (full disk illumination) from 500 to 900 nm and spectral resolution R∼125-225. We simulate a measured spectrum with a simplified, wavelength-independent noise model at Signal-to-Noise ratio S/N=10. With an MCMC-based retrieval methodology, we analyse which planet/atmosphere parameters can be inferred from the measured spectrum and the theoretical correlations amongst them. We consider limiting cases in which the planet radius is either known or completely unknown, and intermediate cases in which the planet radius is partly constrained. Results. If the planet radius is known, we can generally discriminate between cloud-free and cloudy atmospheres, and constrain the methane abundance to within two orders of magnitude. If the planet radius is unknown, new correlations between model parameters occur and the accuracy of the retrievals decreases. Without a radius determination, it is challenging to discern whether the planet has clouds, and the estimates on methane abundance degrade. However, we find the planet radius is constrained to within a factor of two for all the cases explored. Having a priori information on the planet radius, even if approximate, helps improve the retrievals. Conclusions. Reflected-starlight measurements will open a new avenue for characterising long-period exoplanets, a population that remains poorly studied. For this task to be complete, direct-imaging observations should be accompanied by other techniques. We urge exoplanet detection efforts to extend the population of long-period planets with mass and radius determinations.

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Shallow transit follow‐up from Next‐Generation Transit Survey: Simultaneous observations of HD 106315 with 11 identical telescopes

et al. 2020

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The Next Generation Transit Survey (NGTS) is a photometric survey for transiting exoplanets, consisting of 12 identical 0.2-m telescopes. We report a measurement of the transit of HD 106315 c using a novel observing mode in which multiple NGTS telescopes observed the same target, with the aim of increasing the signal-to-noise ratio. Combining the data allows the robust detection of the transit, which has a depth less than 0.1%, rivaling the performance of much larger telescopes. We demonstrate the capability of NGTS to contribute to the follow-up of K2 and Transiting Exoplanet Survey Satellite discoveries using this observing mode. In particular, NGTS is well-suited to the measurement of shallow transits of bright targets. This is particularly important to improve orbital ephemerides of relatively long-period planets, where only a small number of transits are observed from space. K E Y W O R D S planetary systems, planets and satellites: HD 106315 c, techniques: photometricThis is an open access article under the terms of the Creative Commons Attribution-NonCommercial-NoDerivs License, which permits use and distribution in any medium, provided the original work is properly cited, the use is non-commercial and no modifications or adaptations are made.

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Precise masses for the transiting planetary system HD 106315 with HARPS

Cited by 27 publications

References 89 publications

Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827* †

Physical Parameters of the Multiplanet Systems HD 106315 and GJ 9827* †

Directly imaged exoplanets in reflected starlight. The importance of knowing the planet radius

Shallow transit follow‐up from Next‐Generation Transit Survey: Simultaneous observations of HD 106315 with 11 identical telescopes

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