![Detection map of our sample (excluding system with inner giant planets). Red dots represent the known planets, including the new candidates discussed in Section 6.3. [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/The-GAPS-Programme-.png?fit=1200%2C671&ssl=1)
[astro-ph.EP] Context. The architecture of our Solar System, with inner small planets (ISPs) and outer giants, may or may not be common. Understanding whether a correlation exists between ISPs and outer cold giants is key to evaluating how common systems with a similar architecture to our own are.
Aims. This study aims to build a large, homogeneous sample of systems hosting cold Jupiters (CJs, a > 1 au, msini > 0.1 MJ) detected via radial velocities (RVs), and to assess the presence of additional ISPs (P < 400 d, 3 < msini < 31.7 M⊕), studying the correlation between these two types of objects.
Methods. We selected 137 stars known to host a CJ, including 23 which also harbor a hot Jupiter and were treated separately. Data from various instruments were compiled, including unpublished data gathered with HARPS-N within the GAPS program, and consistently fitted using PyORBIT. We derived RV detection maps and calculated occurrence rates for ISPs, cross-validating results with two independent codes. The sample was divided into subgroups to evaluate how system parameters influence planet occurrence.
Results. We confirmed the 213 already known planets in the 137 systems and also identified six new candidates. We divided them, based on mass and period, into Neptunes (10 < m sin i < 31.7 M⊕) and Super-Earths (3 < m sin i < 10 M⊕), and into hot (1 < P < 10 d), warm (10 < P < 100 d), and cool (100 < P < 400 d). We found occurrences of 5%, 13%, and 12% for hot, warm, and cool Neptunes, respectively, and 11% and 16% for hot and warm Super-Earths, respectively. Systems with dynamically stable inner regions show higher rates of small planets. These findings are consistent with previous studies showing no strong correlation between ISPs and CJs at average stellar metallicity and mass, and suggest that HJs may be more commonly associated with external giants.
A. Ruggieri, S. Desidera, M. Pinamonti, D. Barbato, A. Sozzetti, A. S. Bonomo, L. Naponiello, M. Damasso, S. Benatti, I. Carleo, R. Gratton, K. Biazzo, A. F. Lanza, G. Piccinini, N. Nari, G. Mantovan, J. Maldonado, D. Nardiello, A. Fiorenzano, A. Ghedina, A. Bignamini
Comments: 25 pages, 26 figures, accepted in A&A on 07/07/2026. V2 is language-edited
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2607.09320 [astro-ph.EP] (or arXiv:2607.09320v2 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2607.09320
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Submission history
From: Alessandro Ruggieri Dr.
[v1] Fri, 10 Jul 2026 12:02:18 UTC (5,919 KB)
[v2] Mon, 13 Jul 2026 12:25:54 UTC (5,921 KB)
https://arxiv.org/abs/2607.09320
Astrobiology, exoplanet,
