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Occurrence rates of small planets from HARPS: Focus on the Galactic context

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Dolev Bashi, Shay Zucker, Vardan Adibekyan, Nuno C. Santos, Lev Tal-Or, Trifon Trifonov, Tsevi Mazeh

Earth and Planetary Astrophysics · Submitted 7 Oct 2020

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We find the occurrence rates of these planets in the thin and thick disks to be comparable.

how it is stated · asserted 1.00 read the record →

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arXiv ID2010.03237 (version 2)
Pith IDT3CL2MD5, Pith's permanent record of this paper and its review
CitationDolev Bashi, Lev Tal-Or, Nuno C. Santos, Shay Zucker, Trifon Trifonov, Tsevi Mazeh, Vardan Adibekyan. "Occurrence rates of small planets from HARPS: Focus on the Galactic context." arXiv:2010.03237 (2020). https://pith.science/paper/T3CL2MD5
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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 10,748 input tokens.

What the abstract itself states, as probabilities: claims first 0.78 · states limitation 0.41 · human participants 0.02 · controlled comparison 0.81 · randomized assignment 0.01 · states quantitative result 0.22 · compares with prior results 0.96 · mentions code or data availability 0.03.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

Context. The stars in the Milky Way thin and thick disks can be distinguished by several properties such as metallicity and kinematics. It is not clear whether the two populations also differ in the properties of planets orbiting the stars. In order to study this, a careful analysis of both the chemical composition and mass detection limits is required for a sufficiently large sample. Currently, this information is still limited only to large radial-velocity (RV) programs. Based on the recently published archival database of the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph, we present a first analysis of low-mass (small) planet occurrence rates in a sample of thin- and thick-disk stars. Aims. We aim to assess the effects of stellar properties on planet occurrence rates and to obtain first estimates of planet occurrence rates in the thin and thick disks of the Galaxy. As a baseline for comparison, we also aim to provide an updated value for the small close-in planet occurrence rate and compare it to results of previous RV and transit ($\textit{Kepler}$) works. Methods. We used archival HARPS RV datasets to calculate detection limits of a sample of stars that were previously analysed for their elemental abundances. For stars with known planets we first subtracted the Keplerian orbit. We then used this information to calculate planet occurrence rates according to a simplified Bayesian model in different regimes of stellar and planet properties. Results. Our results suggest that metal-poor stars and more massive stars host fewer low-mass close-in planets. We find the occurrence rates of these planets in the thin and thick disks to be comparable. In the iron-poor regimes, we find these occurrence rates to be significantly larger at the high-$\alpha$ region (thick-disk stars) as compared with the low-$\alpha$ region (thin-disk stars). In general, we find the...

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 Context. background 1.00 0.02 0.01 unclear 1.00
s1 The stars in the Milky Way thin and thick disks can be distinguished by several properties such as metallicity and kinematics. background 1.00 0.05 0.02 asserted 1.00
s2 It is not clear whether the two populations also differ in the properties of planets orbiting the stars. gap 0.97 0.04 0.02 unclear 0.62
s3 In order to study this, a careful analysis of both the chemical composition and mass detection limits is required for a sufficiently large sample. background 0.51 0.06 0.02 asserted 0.93
s4 Currently, this information is still limited only to large radial-velocity (RV) programs. gap 0.94 0.05 0.01 asserted 1.00
s5 Based on the recently published archival database of the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph, we present a first analysis of low-mass (small) planet occurrence rates in a sample of thin- and thick-disk stars. Aims. contribution 1.00 0.90 0.03 asserted 0.99
s6 We aim to assess the effects of stellar properties on planet occurrence rates and to obtain first estimates of planet occurrence rates in the thin and thick disks of the Galaxy. contribution 0.89 0.21 0.04 unclear 0.62
s7 As a baseline for comparison, we also aim to provide an updated value for the small close-in planet occurrence rate and compare it to results of previous RV and transit ($\textit{Kepler}$) works. Methods. contribution 0.89 0.41 0.02 unclear 0.66
s8 We used archival HARPS RV datasets to calculate detection limits of a sample of stars that were previously analysed for their elemental abundances. method 1.00 0.96 0.02 asserted 0.99
s9 For stars with known planets we first subtracted the Keplerian orbit. method 1.00 0.94 0.01 asserted 0.96
s10 We then used this information to calculate planet occurrence rates according to a simplified Bayesian model in different regimes of stellar and planet properties. Results. method 0.98 0.94 0.03 asserted 0.83
s11 Our results suggest that metal-poor stars and more massive stars host fewer low-mass close-in planets. result 0.98 0.93 0.43 hedged possibility 1.00
s12 We find the occurrence rates of these planets in the thin and thick disks to be comparable. result 1.00 0.96 0.38 asserted 1.00
s13 In the iron-poor regimes, we find these occurrence rates to be significantly larger at the high-$\alpha$ region (thick-disk stars) as compared with the low-$\alpha$ region (thin-disk stars). result 1.00 0.96 0.20 asserted 1.00
s14 In general, we find the... result 0.99 0.77 0.07 unclear 0.89

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from analysis of existing data 1.00.

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sources read
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not examined
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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

Context. The stars in the Milky Way thin and thick disks can be distinguished by several properties such as metallicity and kinematics. It is not clear whether the two populations also differ in the properties of planets orbiting the stars. In order to study this, a careful analysis of both the chemical composition and mass detection limits is required for a sufficiently large sample. Currently, this information is still limited only to large radial-velocity (RV) programs. Based on the recently published archival database of the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph, we present a first analysis of low-mass (small) planet occurrence rates in a sample of thin- and thick-disk stars. Aims. We aim to assess the effects of stellar properties on planet occurrence rates and to obtain first estimates of planet occurrence rates in the thin and thick disks of the Galaxy. As a baseline for comparison, we also aim to provide an updated value for the small close-in planet occurrence rate and compare it to results of previous RV and transit ($\textit{Kepler}$) works. Methods. We used archival HARPS RV datasets to calculate detection limits of a sample of stars that were previously analysed for their elemental abundances. For stars with known planets we first subtracted the Keplerian orbit. We then used this information to calculate planet occurrence rates according to a simplified Bayesian model in different regimes of stellar and planet properties. Results. Our results suggest that metal-poor stars and more massive stars host fewer low-mass close-in planets. We find the occurrence rates of these planets in the thin and thick disks to be comparable. In the iron-poor regimes, we find these occurrence rates to be significantly larger at the high-$\alpha$ region (thick-disk stars) as compared with the low-$\alpha$ region (thin-disk stars). In general, we find the...

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