The GAPS programme at TNG. XLVI. Deep search for low-mass planets in late-dwarf systems hosting cold Jupiters
M. Pinamonti, D. Barbato, A. Sozzetti, L. Affer, S. Benatti, K. Biazzo, A. Bignamini, F. Borsa, M. Damasso, S. Desidera, A. F. Lanza, J. Maldonado, L. Mancini, … 展开作者
M. Pinamonti, D. Barbato, A. Sozzetti, L. Affer, S. Benatti, K. Biazzo, A. Bignamini, F. Borsa, M. Damasso, S. Desidera, A. F. Lanza, J. Maldonado, L. Mancini, L. Naponiello, D. Nardiello, M. Rainer, L. Cabona, C. Knapic, G. Andreuzzi, R. Cosentino, A. Fiorenzano, A. Ghedina, A. Harutyunyan, V. Lorenzi, M. Pedani, R. Claudi, E. Covino, A. Maggio, G. Micela, E. Molinari, I. Pagano, G. Piotto, E. Poretti
我们展示了对3颗 hosting well-measured orbits 的 long-period giants 的 late-type dwarf stars 进行 high-cadence 和 high-precision radial velocity (RV) monitoring 的结果，以 search for short-period sub-Neptunes (SN, $M \sin i < 30$ M$_\oplus$)。Building on the results and expertise of our previous studies, 我们 carry out combined fits of our HARPS-N data with literature RVs, using MCMC analyses 和 Gaussian Process regression。然后，我们使用 survey 的结果来 estimate sub-Neptunes 在 hosting cold-Jupiters 的系统中的 frequency, $f(SN|CJ)$, 并将其与 field M-dwarfs 周围的 frequency $f(SN)$ 进行比较。我们识别出一颗 orbiting GJ 328 的 new short-period low-mass planet, GJ 328\\,c, 其 $P_c = 241.8^{+1.3}_{-1.7}$ d 和 $M_c \sin i = 21.4^{+ 3.4}_{- 3.2}$ M$_\oplus$。此外，我们还识别并 model 了 GJ 649 和 GJ 849 的 chromospheric activity signals 和 rotation periods，在这两颗星周围未找到 additional planet。然后，taking into account also planetary system around the previosuly-analyzed low-mass star BD-11 4672, 我们 derive 了对此类系统中 inner planets frequencies 的 estimate。特别是对于 mini-Neptunes ($10$ M$_\oplus < M \sin i < 30$ M$_\oplus$, $P < 150$ d), $f(SN|CJ) = 0.25^{+0.58}_{-0.07}$, marginally larger than $f(SN)$。对于 lower-mass planets ($M \sin i < 10$ M$_\oplus$), 则 $f(SN|CJ) <0.69$, compatible with $f(SN)$。鉴于 newly detected mini-Neptune, 我们发现了此类 planets 与 inner low-mass planets 存在 positive correlation 的 tentative evidence, $f(SN|CJ) > f(SN)$。这可能表明 cold Jupiters 对 late-type dwarfs 周围 inner sub-Neptunes 的 formation 产生的影响与其对 solar-type counterparts 的影响相反，是 boosting mini-Neptunes 的 formation 而非 impeding it。
英文摘要：
We present the results of a high-cadence and high-precision radial velocity (RV) monitoring of 3 late-type dwarf stars hosting long-period giants with well-measured orbits, in order to search for short-period sub-Neptunes (SN, $M \sin i < 30$ M$_\oplus$). Building on the results and expertise of our previous studies, we carry out combined fits of our HARPS-N data with literature RVs, using MCMC analyses and Gaussian Process regression. We then use the results of our survey to estimate the frequency of sub-Neptunes in systems hosting cold-Jupiters, $f(SN|CJ)$, and compare it with the frequency around field M-dwarfs, $f(SN)$. We identify a new short-period low-mass planet orbiting GJ 328, GJ 328\,c, with $P_c = 241.8^{+1.3}_{-1.7}$ d and $M_c \sin i = 21.4^{+ 3.4}_{- 3.2}$ M$_\oplus$. We moreover identify and model the chromospheric activity signals and rotation periods of GJ 649 and GJ 849, around which no additional planet is found. Then, taking into account also planetary system around the previosuly-analyzed low-mass star BD-11 4672, we derive an estimate of the frequencies of inner planets in such systems. In particular $f(SN|CJ) = 0.25^{+0.58}_{-0.07}$ for mini-Neptunes ($10$ M$_\oplus < M \sin i < 30$ M$_\oplus$, $P < 150$ d), marginally larger than $f(SN)$. For lower-mass planets ($M \sin i < 10$ M$_\oplus$) instead $f(SN|CJ) <0.69$, compatible with $f(SN)$. In light of the newly detected mini-Neptune, we find tentative evidence of a positive correlation between the presence of those planets and that of inner low-mass planets, $f(SN|CJ) > f(SN)$. This might indicate that cold Jupiters have an opposite influence in the formation of inner sub-Neptunes around late-type dwarfs as opposed to their solar-type counterparts, boosting the formation of mini-Neptunes instead of impeding it.
The GAPS Programme at TNG XXXIX -- Multiple molecular species in the atmosphere of the warm giant planet WASP-80 b unveiled at high resolution with GIANO-B
The GAPS Programme with HARPS-N at TNG. XIII. The orbital obliquity of three close-in massive planets hosted by dwarf K-type stars: WASP-43, HAT-P-20 and Qatar-2
The GAPS Programme at TNG. LXXX. Characterisation of the 400 Myr old multi-planet system K2-233
University of Palermo（巴勒莫大学）；INAF – Osservatorio Astronomico di Palermo（意大利国家天体物理研究所–巴勒莫天文台）；University of Michigan（密歇根大学）；University of Warwick（华威大学）；ESO - European Southern Observatory（欧洲南方天文台）；INAF – Osservatorio Astronomico di Roma（意大利国家天体物理研究所–罗马天文台）
The GAPS Programme at TNG. LXXIII. Confirmation of the hot sub-Neptune TOI-4602 b (HD 25295 b), a key target for future atmospheric characterization
INAF – Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；ESO - European Southern Observatory（欧洲南方天文台）；INAF-Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；INAF – Osservatorio Astrofisico di Catania（意大利国家天体物理研究所卡塔尼亚天文台）；Institute for Particle Physics and Astrophysics, ETH Zürich（苏黎世联邦理工学院粒子物理与天体物理研究所）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）
The GAPS Programme with HARPS-N at TNG VIII: Observations of the Rossiter-McLaughlin effect and characterisation of the transiting planetary systems HAT-P-36 and WASP-11/HAT-P-10
The HADES RV Programme with HARPS-N@TNG VIII. Gl15A: A multiple wide planetary system sculpted by binary interaction
我们提出了20年的径向速度（RV）测量的M1矮G115 A，结合5年的密集RV监测与HARPS-N摄谱仪与15年的档案HIRES/凯克RV数据。我们进行MCMC为基础的RV时间序列的分析，包括高斯过程（GP）的方法来描述恒星活动引起的RV变化。我们的分析证实了开普勒性质，并改进了11.44天周期的超级地球Gl 15 A\，b的轨道解，将其振幅减小到$1.68^{+0.17}_{-0.18}$ m s $^{-1}$（$M \sin i = 3.03^{+0.46}_{-0.44}$ M $_\oplus$），并成功地模拟了组合RV数据集中的长期趋势，其依据的是具有大约7600天的周期和$2.5^{+1.3}_{-1.0}$ m s $^{-1}$的幅度的开普勒轨道，对应于超海王星质量（$M \sin i = 36^{+25}_{-18}$ M $_\oplus$）行星伴星。通过详细的数值模拟，我们还讨论了G1 15 A行星系与大分离伴星G1 15 B之间Lidov-Kozai相互作用的可能结果，并讨论了G1 15 A的轨道构型.为了改善动力学分析的结果，我们推导出一个新的轨道解的双星系统，结合我们的RV测量和天体测量数据从WDS目录。Lidov-Kozai偏心率分析表明，Gl 15 B对Gl 15 A行星系有很强的影响，它可以产生与观测到的$75^\circ$和$90^\circ$…
The GAPS Programme at TNG LXXIV. A reanalysis of the planetary systems TOI-1272 and TOI-1694 with HARPS-N and retraction of the planetary interpretation of TOI-1272 c
University of Rome “Tor Vergata”（罗马托尔维加塔大学）；INAF – Turin Astrophysical Observatory（意大利国家天体物理研究所都灵天文台）；INAF – Astronomical Observatory of Rome（意大利国家天体物理研究所罗马天文台）；INAF – Astrophysical Observatory of Catania（意大利国家天体物理研究所卡塔尼亚天文台）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CSIC-INTA））；Fundacion Galileo Galilei（伽利略基金会）；INAF – Astronomical Observatory of Trieste（意大利国家天体物理研究所的里雅斯特天文台）
The GAPS Programme with HARPS-N at TNG XVI: Measurement of the Rossiter-McLaughlin effect of the transiting planetary systems HAT-P-3, HAT-P-12, HAT-P-22, WASP-39 and WASP-60
The GAPS programme at TNG LXXVIII. Phase-resolved detection of multiple atomic species in the atmosphere of KELT-20b/MASCARA-2b
INAF – Osservatorio Astronomico di Brera（INAF - 布里拉天文台）；Dipartimento di Scienza e Alta Tecnologia, Università degli Studi dell’Insubria（因苏布里亚大学科学与技术高等学院）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；INAF – Osservatorio Astronomico di Palermo（INAF - 巴勒莫天文台）；INAF – Osservatorio Astrofisico di Torino（INAF - 都灵天文台）；INAF – Osservatorio Astronomico di Padova（INAF - 帕多瓦天文台）；Dipartimento di Fisica e Astronomia, Università degli Studi di Padova（帕多瓦大学物理与天文学系）；INAF – Osservatorio Astrofisico di Catania（INAF - 卡塔尼亚天文台）
The GAPS Programme at TNG: XXXVI. Measurement of the Rossiter-McLaughlin effect and revising the physical and orbital parameters of the HAT-P-15, HAT-P-17, HAT-P-21, HAT-P-26, HAT-P-29 eccentric planetary systems
The GAPS Programme with HARPS-N@TNG IX. The multi-planet system KELT-6: detection of the planet KELT-6 c and measurement of the Rossiter-McLaughlin effect for KELT-6 b
HADES RV Programme with HARPS-N at TNG. VII. Rotation and activity of M-Dwarfs from time-series high-resolution spectroscopy of chromospheric indicators
HADES RV programme with HARPS-N at TNG XIV. A candidate super-Earth orbiting the M-dwarf GJ 9689 with a period close to half the stellar rotation period
The GAPS Programme at TNG LXVII. Detection of water and preliminary characterisation of the atmospheres of the two hot Jupiters KELT-8 b and KELT-23 Ab
The GAPS programme at TNG LX Atmospheric characterisation of KELT-9 b via single-line analysis: Detection of six H I Balmer lines, Na I, Ca I, Ca II, Fe I, Fe II, Mg I, Ti II, Sc II, and Cr II
The GAPS Programme with HARPS-N at TNG LXXVII. Occurrence rates of small close-in planets in the presence of cold Jupiters
INAF, Astrophysical Observatory of Catania（意大利国家天体物理研究所，卡塔尼亚天文台）；INAF, Astrophysical Observatory of Padova（意大利国家天体物理研究所，帕多瓦天文台）；INAF, Astrophysical Observatory of Turin（意大利国家天体物理研究所，都灵天文台）；INAF, Astronomical Observatory of Palermo（意大利国家天体物理研究所，巴勒莫天文台）；INAF, Astronomical Observatory of Rome（意大利国家天体物理研究所，罗马天文台）
The GAPS programme at TNG LXX. HD 128717 B/Gaia-6 B: a long-period eccentric low-mass brown dwarf from astrometry and radial velocities
INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；INAF - Osservatorio Astrofisico di Catania（意大利国家天体物理研究所卡塔尼亚天文台）；INAF - Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；Department of Astronomy and Steward Observatory, The University of Arizona（亚利桑那大学天文学系和斯图尔德天文台）；Fundación Galileo Galilei - INAF（伽利略基金会-意大利国家天体物理研究所）；School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Department of Physics, University of Turin（都灵大学物理系）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
HADES RV Programme with HARPS-N at TNG XV. Planetary occurrence rates around early-M dwarfs
我们提出了完整的贝叶斯统计分析的HARPS-N红矮星系外行星调查（HADES），监测径向速度的大样本M矮星与HARPS-N在TNG，在过去的6年。这些目标是在从M0到M3的狭窄光谱类型范围内选择的，$0.3$ M $_\odot < M_\star < 0.71$ M $_\odot$，目的是研究围绕一个定义明确的宿主恒星的行星群。我们利用贝叶斯统计，得出一个准确的估计的可检测性功能的调查。我们的分析还包括高斯过程方法的应用，以考虑恒星活动引起的径向速度变化，并提高检测限，周围的最观测和最活跃的目标。马尔可夫链蒙特卡罗和高斯过程技术，我们在这项分析中应用已被证明是非常有效的M-矮行星系统的研究，帮助大多数的HADES行星的检测。从可探测性函数中，我们可以计算出早期M矮星周围小质量行星的出现率，或者只考虑11颗已经发表的HADES行星，或者加上在这次分析中发现的5颗新的行星候选者，并将它们与之前对M矮星或太阳型恒星周围行星出现率的估计进行比较：仅考虑已确认的行星，我们发现低质量行星的频率最高（$1$ M $_\oplus < m_p \sin i < 10$ M $_\oplus$），周期为$10$ d $ < P < 100$ d，$f_\text{occ} = 85^{+5}_{-19}\%$，而对于短周期行星（$1$ d $ < P < 10$ d），我们发现频率为$f_\te…
