The GAPS programme with HARPS-N at TNG

Desidera, S.; Sozzetti, A.; Bonomo, A. S.; Gratton, R.; Poretti, E.; Claudi, R.; Latham, David W.; Affer, L.; Cosentino, R.; Damasso, M.; Esposito, M.; Giacobbe, P.; Malavolta, L.; Nascimbeni, V.; Piotto, G.; Rainer, M.; Scardia, M.; Schmid, V. S.; Lanza, A. F.; Micela, G.; Pagano, I.; Bedin, L. R.; Biazzo, K.; Borsa, F.; Carolo, Elena; Covino, E.; Faedi, F.; Hébrard, G.; Lovis, C.; Maggio, A.; Mancini, L.; Marzari, F.; Messina, S.; Molinari, E.; Munari, U.; Pepe, F.; Santos, N. C.; Scandariato, G.; Shkolnik, Evgenya L.; Southworth, J.

doi:10.1051/0004-6361/201321155

Cited by 37 publications

(35 citation statements)

References 26 publications

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“…Our results indicate that there is no evidence for these two planetary systems. Moreover, in the latter case, we confirm the results recently published by Desidera et al (2013) and Müller et al (2013), who have shown that there is no indication of giant planets orbiting HIP 11952.…”

Section: Introductionsupporting

confidence: 92%

“…As for HIP 13044, this discovery was very controversial since according to the core-accretion model, giant planets are not expected to be formed around such metal-poor star, as we discussed above. However, based on much higher quality data taken with HARPS-N, Desidera et al (2013) recently showed that there is no planetary system around HIP 11952 and that the RVs are flat, showing a small scatter at the 7 m s −1 level, which has also been confirmed by Müller et al (2013).…”

Section: Hip11952mentioning

confidence: 85%

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No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044

Jones

Jenkins

2014

A&A

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Context. The recent discovery of three giant planets orbiting the extremely metal-poor stars HIP 11952 and HIP 13044 have challenged theoretical predictions of the core-accretion model. According to this, the metal content of the protoplanetary disk from which giant planets are formed is a key ingredient for the early formation of planetesimals prior to the runaway accretion of the surrounding gas. Aims. We reanalyzed the original FEROS data that were used to detect the planets to prove or refute their existence, employing our new reduction and analysis methods. Methods. We applied the cross-correlation technique to FEROS spectra to measure the radial velocity variation of HIP 13044 and HIP 11952. We reached a typical precision of ∼35 m s −1 for HIP 13044 and ∼25 m s −1 for HIP 11952, which is significantly superior to the uncertainties presented previously. Results. We found no evidence of the planet orbiting the metal-poor extragalactic star HIP 13044. We show that given our radial velocity precision, and considering the large number of radial velocity epochs, the probability for a non-detection of the radial velocity signal recently claimed is lower than 10 −4 . Finally, we also confirm findings that the extremely metal-poor star HIP 11952 does not contain a system of two gas giant planets. These results reaffirm the expectations from the core-accretion model of planet formation.

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Section: Introductionsupporting

confidence: 92%

Section: Hip11952mentioning

confidence: 85%

No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044

Jones

Jenkins

2014

A&A

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“…Since its installation in Spring 2012 at the Telescopio Nazionale Galileo, HARPS-N has allowed the obliquity of the transiting planet Qatar-1 b to be measured (Covino et al 2013) and has shown that the metal-poor star HIP 11952 does not harbor giant planets (Desidera et al 2013). The two new planets KOI-200 b and KOI-889 b presented here are the first to be detected and characterized with HARPS-N. Our observing program managed jointly with SOPHIE and HARPS-N shows the benefits that could be obtained for the follow-up of transiting planet candidates from coordinated observations secured with two spectrographs with different sensitivities, precisions, and accessibilities.…”

Section: Resultsmentioning

confidence: 99%

KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized withKepler, SOPHIE, and HARPS-N

Hébrard¹,

Almenara²,

Santerne³

et al. 2013

A&A

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We present the detection and characterization of the two new transiting, close-in, giant extrasolar planets KOI-200 b and KOI-889 b. They were first identified by the Kepler team as promising candidates from photometry of the Kepler satellite; we then established their planetary nature thanks to the radial velocity follow-up jointly secured with the spectrographs SOPHIE and HARPS-N. Combined analyses of the whole datasets allow the two planetary systems to be characterized. The planet KOI-200 b has mass and radius of 0.68 ± 0.09 M Jup and 1.32 ± 0.14 R Jup ; it orbits in 7.34 days a F8V host star with mass and radius of 1.40 +0.14 −0.11 M and 1.51 ± 0.14 R . The planet KOI-889 b is a massive planet with mass and radius of 9.9 ± 0.5 M Jup and 1.03 ± 0.06 R Jup ; it orbits in 8.88 days an active G8V star with a rotation period of 19.2 ± 0.3 days, and mass and radius of 0.88 ± 0.06 M and 0.88 ± 0.04 R . Both planets lie on eccentric orbits and are located just at the frontier between regimes where tides can explain circularization and where tidal effects are negligible. The two planets are among the first detected and characterized thanks to observations secured with HARPS-N, the new spectrograph recently mounted at the Telescopio Nazionale Galileo. These results illustrate the benefits that could be obtained from joint studies using two spectrographs as SOPHIE and HARPS-N.

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“…We have used five years of high-precision Doppler monitoring with the High Accuracy Radial velocity Planet Searcher for the Northern emisphere (HARPS-N) high-resolution (resolving power R ∼ 115 000) optical echelle spectrograph (Cosentino et al 2012) at the Telescopio Nazionale Galileo (TNG), combined with 15 yr of archival RVs data from the Lick-Carnegie Exoplanet Survey (LCES) HIRES/Keck Precision Radial Velocity survey (Butler et al 2017). The HARPS-N data were collected as part of the Harps-n red Dwarf Exoplanet Survey (HADES) programme, a collaboration between the Italian Global Architecture of Planetary Systems (GAPS; Covino et al 2013;Desidera et al 2013;Poretti et al 2016) Consortium 2 , the Institut de Ciències de l'Espai de Catalunya (ICE) and the Instituto de Astrofísica de Canarias (IAC). We also confirm the presence and update the amplitude of the Gl15A b RV signal, significantly reducing its minimum mass, while confirming the orbital period measured by Howard et al (2014).…”

Section: Introductionmentioning

confidence: 99%

The HADES RV Programme with HARPS-N at TNG

Pinamonti

Damasso

Marzari

et al. 2018

A&A

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We present 20 yr of radial velocity (RV) measurements of the M1 dwarf Gl15A, combining five years of intensive RV monitoring with the HARPS-N spectrograph with 15 yr of archival HIRES/Keck RV data. We have carried out an MCMC-based analysis of the RV time series, inclusive of Gaussian Process (GP) approach to the description of stellar activity induced RV variations. Our analysis confirms the Keplerian nature and refines the orbital solution for the 11.44-day period super Earth, Gl15A b, reducing its amplitude to 1.68, and successfully models a long-term trend in the combined RV dataset in terms of a Keplerian orbit with a period around 7600 days and an amplitude of 2.5, corresponding to a super-Neptune mass (M sin i = 36 +25 −18 M ⊕ ) planetary companion. We also discuss the present orbital configuration of Gl15A planetary system in terms of the possible outcomes of Lidov-Kozai interactions with the wide-separation companion Gl15B in a suite of detailed numerical simulations. In order to improve the results of the dynamical analysis, we have derived a new orbital solution for the binary system, combining our RV measurements with astrometric data from the WDS catalogue. The eccentric Lidov-Kozai analysis shows the strong influence of Gl15B on the Gl15A planetary system, which can produce orbits compatible with the observed configuration for initial inclinations of the planetary system between 75• and 90• , and can also enhance the eccentricity of the outer planet well above the observed value, even resulting in orbital instability, for inclinations around 0• and 15• −30• . The Gl15A system is the multi-planet system closest to Earth, at 3.56 pc, and hosts the longest period RV sub-Jovian mass planet discovered so far. Its orbital architecture constitutes a very important laboratory for the investigation of formation and orbital evolution scenarios for planetary systems in binary stellar systems.

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The GAPS programme with HARPS-N at TNG

Cited by 37 publications

References 26 publications

No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044

No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044

KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized withKepler, SOPHIE, and HARPS-N

The HADES RV Programme with HARPS-N at TNG

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