Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems
Creators: name: Bonomo, A. S.
name: Dumusque, X.
name: Massa, A.
name: Mortier, A.
name: Bongiolatti, R.
name: Malavolta, L.
name: Sozzetti, A.
name: Buchhave, L. A.
name: Damasso, M.
name: Haywood, R. D.
name: Morbidelli, A.
name: Latham, D. W.
name: Molinari, E.
name: Pepe, F.
name: Poretti, E.
name: Udry, S.
name: Affer, L.
name: Boschin, W.
name: Charbonneau, D.
name: Cosentino, R.
name: Cretignier, M.
name: Ghedina, A.
name: Lega, E.
name: López-Morales, M.
name: Margini, M.
name: Fiorenzano, A. F. Martínez
name: Mayor, M.
name: Micela, G.
name: Pedani, M.
name: Pinamonti, M.
name: Rice, K.
name: Sasselov, D.
name: Tronsgaard, R.
name: Vanderburg, A.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The exoplanet population characterized by relatively short orbital periods ($P&lt;100$ d) around solar-type stars is dominated by super-Earths and sub-Neptunes. However, these planets are missing in our Solar System and the reason behind this absence is still unknown. Two theoretical scenarios invoke the role of Jupiter as the possible culprit: Jupiter may have acted as a dynamical barrier to the inward migration of sub-Neptunes from beyond the water iceline; alternatively, Jupiter may have reduced considerably the inward flux of material (pebbles) required to form super-Earths inside that iceline. Both scenarios predict an anti-correlation between the presence of small planets (SPs) and that of cold Jupiters (CJs) in exoplanetary systems. To test that prediction, we homogeneously analyzed the radial-velocity (RV) measurements of 38 Kepler and K2 transiting SP systems gathered over almost 10 years with the HARPS-N spectrograph, as well as publicly available RVs collected with other facilities. We detected five CJs in three systems, two in Kepler-68, two in Kepler-454, and a very eccentric one in K2-312. We derived an occurrence rate of $9.3^{+7.7}_{-2.9}\%$ for CJs with $0.3-13~M_{Jup}$ and 1-10 AU, which is lower but still compatible at $1.3σ$ with that measured from RV surveys for solar-type stars, regardless of the presence or absence of SPs. The sample is not large enough to draw a firm conclusion about the predicted anti-correlation between SPs and CJs; nevertheless, we found no evidence of previous claims of an excess of CJs in SP systems. As an important by-product of our analyses, we homogeneously determined the masses of 64 Kepler and K2 small planets, reaching a precision better than 5, 7.5 and 10$σ$ for 25, 13 and 8 planets, respectively. Finally, we release the 3661 HARPS-N radial velocities used in this work to the scientific community. [Abridged]
description: 21 pages, 10 figures, 10 tables, published in Astronomy and Astrophysics. The updated version of the article takes into account the A&amp;A language editing and guidelines. Tables 1, A.1 and full Table 2 are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A33