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Timing of Seven Isolated Pulsars in the Globular Cluster Terzan 1

T0 review · 3 major / 6 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read Timing all seven pulsars in Terzan 1 shows they are isolated and measures their positions and spin-down; one may be only 11 million years old.

desk verdict New timing solutions for seven Terzan 1 pulsars look solid, but the young-pulsar age claim rests on an acceleration bound that contradicts the paper's own cluster model. read the letter →

arxiv 2412.11271 v1 pith:JCIRQAHN submitted 2024-12-15 astro-ph.HE astro-ph.GAastro-ph.SR

Justine Singleton , Megan DeCesar , Shi Dai , Deven Bhakta , Scott Ransom , Jay Strader , Laura Chomiuk , James Miller-Jones This is my paper · ORCID
classification astro-ph.HEastro-ph.GAastro-ph.SR
keywords pulsarsglobularclustersmillisecondpulsartimingTerzan1clusterdynamicsneutronstarformation
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper reports seven years of radio timing for the seven known pulsars in the globular cluster Terzan 1, connecting all observations into phase-coherent solutions. The result is a set of measured sky positions, spin frequencies, and observed spin-down rates for pulsars A through G, and the finding that all seven are isolated — consistent with the cluster's core-collapsed state, which is expected to ionize binaries. Because the observed spin-down mixes intrinsic pulsar spin-down with acceleration from the cluster's gravitational potential, the paper uses these measurements to estimate line-of-sight accelerations and to try to constrain the cluster's core radius and density, though a wide range of values remains possible. A secondary, explicitly hedged result is that the slowest pulsar, Ter 1 A, may have a characteristic age as low as about 11 million years, far younger than the roughly 12 billion-year-old cluster, hinting that it formed through a channel other than core-collapse supernova, such as the collapse of a white dwarf.

What carries the argument

The central object is the phase-connected timing solution: a continuous count of rotation phases that links every radio detection of a given pulsar across the seven-year baseline, enabling sub-microsecond fits to arrival times and precise measurements of position and spin parameters. The load-bearing identity is the decomposition of the observed spin-down, $(\dot{P}/P)_{\rm obs} = (\dot{P}/P)_{\rm int} + (a_{\rm GC} + a_G + a_{\rm PM} + a_{\rm NN})/c$, where the four acceleration terms come from the cluster potential, the Galactic potential, the Shklovskii effect (apparent acceleration from proper motion), and nearby stars; the paper shows the cluster term dominates. From this decomposition it defines the pseudo-acceleration $a_{\rm los} = c(\dot{P}_{\rm obs} - \dot{P}_{\rm int})/P$ and compares it with the analytic profile $a_1 = 2\pi G \rho_c r_c^2 / \sqrt{r_c^2 + R_\perp^2}$ to attempt to constrain the core radius $r_c$ and density $\rho_c$, and to place bounds on the intrinsic spin-down of pulsar A.

What would settle it

Find a pulsar in Terzan 1 with a measured $\dot{P}/P$ that implies a line-of-sight acceleration more negative than $-8.9\times10^{-16}\,\mathrm{s}^{-1}$; that single discovery would invalidate the assumption that Ter 1 B provides the maximum acceleration, so the derived maximum intrinsic spin-down for Ter 1 A — and hence its young age — would no longer follow.

Watch

Extended reading notes

Core claim

On the paper's own terms, the central result is a set of phase-connected timing solutions for all seven pulsars in Terzan 1 (A through G) over MJD 57855–60196 (roughly 2017–2023), built from Green Bank Telescope and Parkes radio observations. These solutions yield each pulsar's position, spin frequency, and observed period derivative $\dot{P}_{\rm obs}$, and they show that all seven pulsars are isolated — none has an orbital companion. The paper argues that the observed $\dot{P}$ values are dominated by a combination of intrinsic spin-down and acceleration from the cluster potential, and it uses a pseudo-acceleration $a_{\rm los} = c(\dot{P}_{\rm obs} - \dot{P}_{\rm int})/P$ to compare with an analytic acceleration profile, concluding that the current data cannot tightly constrain the cluster core radius and density. For the slowest pulsar, Ter 1 A, the paper derives an upper bound on intrinsic spin-down that corresponds to a characteristic age as low as roughly 11 Myr, much younger than the cluster's age of about 12 Gyr; the authors state explicitly that this young-age conclusion is not definitive.

Load-bearing premise

The claim that Ter 1 A is young rests on assuming that the largest measured cluster acceleration in this sample is an upper limit for any pulsar in the cluster, so a stronger unseen acceleration would raise its true spin-down and erase the age anomaly.

Editorial extensions

If this is right

  • The measured positions, spin frequencies, and observed period derivatives for Ter 1 A–G now serve as a reference epoch for future timing; extending the baseline will eventually reveal proper motions and any binary companions that current data cannot detect.
  • Because the observed spin-down rates, taken as accelerations, cannot pin down the cluster core radius and density, the paper's model predicts that additional pulsar discoveries or longer timing baselines are required to measure these dynamical quantities.
  • The all-isolated population is consistent with the expectation that core-collapsed clusters disrupt binaries, and it adds Terzan 1 to the list of clusters where alternative formation channels such as white-dwarf collapse are invoked to explain isolated pulsars.
  • If Ter 1 A is genuinely about 11 Myr old, it joins a small but growing set of globular cluster pulsars younger than their host clusters, implying that electron-capture supernovae from accretion- or merger-induced white-dwarf collapse can produce neutron stars in dense clusters.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If future timing in Terzan 1 uncovers a pulsar with a more negative observed spin-down than Ter 1 B's, the upper-bound assumption behind Ter 1 A's young age would be disproven; this is a direct, testable consequence of the paper's weakest premise.
  • Applying the same phase-connected timing to the remaining unidentified steep-spectrum radio sources in the cluster core could add more acceleration measurements and help break the degeneracy between core radius and density that currently prevents a constraint.
  • Across the Milky Way's core-collapsed globular clusters, the paper's logic predicts a sparse population of slow, isolated, apparently young pulsars; a systematic survey of such clusters would test whether electron-capture supernovae are a common production route.
  • Because the Shklovskii and Galactic-acceleration terms are small but not individually measured here, future proper-motion detections would let observers subtract these contributions and turn the current pseudo-accelerations into true cluster accelerations, sharpening the dynamical model.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. This paper reports phase-connected timing solutions for seven isolated pulsars (Terzan 1 A–G) in the globular cluster Terzan 1, using Green Bank Telescope and Parkes observations spanning MJD 57855–60196. The authors measure positions, spin frequencies, and frequency derivatives for all seven pulsars. They then interpret the observed period derivatives as the sum of intrinsic spin-down and accelerations (primarily from the cluster potential), use the inferred pseudo-accelerations to explore possible cluster core parameters, and argue that Terzan 1 A has a maximum intrinsic spin-down that makes it potentially as young as ~11 Myr, possibly formed via electron-capture supernova. The paper explicitly acknowledges the degeneracy between spin-down and acceleration and presents the age claim as provisional.

Significance. The phase-connected timing solutions themselves are a useful dataset for a core-collapsed globular cluster, especially with a seven-year baseline combining GBT and Parkes observations. The paper is appropriately cautious about the spin-down/acceleration degeneracy and does not present the derived cluster core parameters as conclusive. If the frequency-derivative measurements are robust, the observed negative Pdot values for B, C, and F are interesting and motivate further timing. However, the internal inconsistency identified below between the estimated maximum cluster acceleration and the inferred acceleration for Terzan 1 B means the acceleration-based conclusions, including the age estimate for Terzan 1 A, are not yet on solid ground.

major comments (3)
  1. [Sec. 4.1.1 and Sec. 4.3 (Tables 5–6)] The paper derives a maximum cluster acceleration of max a_GC/c ≈ 3–4×10^-17 s^-1 using Eq. (2) and Baumgardt & Hilker (2018) parameters. In Sec. 4.3, Table 5 infers alos/c = -8.0×10^-16 s^-1 for Terzan 1 B (and -8.9×10^-16 s^-1 with an assumed intrinsic spin-down of 10^-18), a factor of ~20 larger in magnitude. Since Secs. 4.1.2–4.1.4 show the Galactic, Shklovskii, and nearest-neighbor terms are all an order of magnitude smaller than the cluster term, no physically allowed combination of non-negative intrinsic spin-down and the stated maximum cluster acceleration can reproduce B's observed negative Pdot. This indicates either that B's phase-connected frequency derivative is not robust or that Eq. (2) with the adopted parameters does not describe this core-collapsed cluster. The paper does not acknowledge or reconcile this discrepancy. This is load-bearing because Table 6 uses B's alos/c = -8.9×10^-16 as the empirical upper bound for the other pulsars, which directly sets the upper limit on Pdot_int for Terzan 1 A and hence the ~11 Myr age claim. The authors should re-examine B's timing solution and/or revise the cluster acceleration estimate before using it as a bound.
  2. [Sec. 4.3 (Table 6)] The largest-magnitude inferred acceleration in Table 5, from a single pulsar (Terzan 1 B), is used without further justification as an upper bound on the acceleration experienced by all other pulsars, including Terzan 1 A. The maximum cluster acceleration depends on the projected distance from the cluster center (Eq. 2), and there is no argument that B sits at the smallest projected radius or otherwise experiences the global maximum line-of-sight acceleration. A pulsar closer to the center or at a different line-of-sight offset could experience a larger acceleration, which would permit a larger intrinsic spin-down for Terzan 1 A and weaken or eliminate the inferred age anomaly. The paper should either justify this empirical bound explicitly (e.g., by showing that B is the most centrally located pulsar and that the acceleration profile is monotonic) or present the age claim as conditional on this assumption.
  3. [Sec. 4.3 (Table 5)] The 'realistic upper limit' on the acceleration of Terzan 1 B is obtained by assuming an intrinsic spin-down rate of Pdot_int = 10^-18 s/s, described only as 'based on properties of pulsars within the known pulsar population with similar P.' No specific comparison or reference is given, and the inferred acceleration alos for B scales linearly with this choice. If B's true Pdot_int exceeds 10^-18, the inferred acceleration magnitude is larger, and the maximum allowable Pdot_int for Terzan 1 A in Table 6 increases, making the minimum characteristic age even smaller; if B's Pdot_int is smaller, the age bound moves toward the old, cluster-age solution. Since the paper's most notable new claim is the possible youth of Terzan 1 A, this assumption should be justified quantitatively against the observed Pdot distribution of isolated MSPs with similar spin periods, and the dependence of the conclusion on the assumed value should be stated.
minor comments (6)
  1. [Sec. 4.4] The sentence 'if its true intrinsic spin-down rate were max (Pdot_int) = 2×10^-16 from Table 6, then its characteristic age would be only ~11 Gyr' should read '~11 Myr', consistent with the Abstract and Conclusions.
  2. [Sec. 4.2] The word 'psuedo-acceleration' should be 'pseudo-acceleration'.
  3. [Table 3] The header 'Ter 1C' and 'Ter 1D' are missing spaces; for consistency with Tables 2 and 4, use 'Ter 1 C' and 'Ter 1 D'.
  4. [Sec. 4.1.4] In the sentence 'We use Equation 4 of Dai et al. (2023) to calculate the nearest-neighbor acceleration aNN that the Ter 1 A pulsars may experience', 'Ter 1 A pulsars' should be 'Terzan 1 pulsars' (or 'the Ter 1 pulsars'), as the calculation is for all pulsars, not just Ter 1 A.
  5. [Sec. 4.3] The phrase 'which will yield a lower limit on alos' is ambiguous because alos is negative; with Pdot_int=0 the magnitude is smaller than with positive Pdot_int. Clarify whether 'lower limit' refers to magnitude or algebraic value.
  6. [Sec. 3.2] For the readers' convenience, consider adding the rms residuals for the timing solutions to a table or figure; currently only the values in Tables 2–4 are given, and the residual for Ter 1 A (485.6 microseconds) is much larger than for the others and is not discussed.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the timing solutions are empirical fits, and the cluster/age inferences are explicitly hedged rather than forced by construction.

full rationale

The paper's primary deliverable is a set of phase-connected timing solutions (Tables 2-4). These are measured quantities obtained by fitting TOAs, not quantities derived from the paper's own assumptions, so there is no fitted-input-called-prediction step. The acceleration analysis in Sec. 4.2 uses observed pseudo-accelerations as inputs and explicitly concludes that a wide range of core radii and densities are possible, i.e., it does not present a fitted parameter as a prediction. The age claim for Ter 1 A in Sec. 4.3-4.4 is an explicit upper limit obtained by assuming that the largest inferred line-of-sight acceleration in the sample (from Ter 1 B) bounds the acceleration of A. This is an empirical assumption about a bound, not a definitional identity: the derived upper limit on A's intrinsic Pdot is algebraically tied to the assumed alos value, but the paper does not hide this and repeatedly hedges the age conclusion ('may be', 'cannot draw this conclusion definitively'). Self-citations exist (Prager et al. 2017 and Dai et al. 2023 include coauthors of this paper), but they are used for standard published formulas and are not invoked as a uniqueness theorem or as the sole justification for the central claim; they therefore are not load-bearing circularity. A related physical concern, that B's inferred alos/c ~ -8e-16 s^-1 exceeds the paper's own analytical maximum of ~3-4e-17 s^-1 from Eq. (2), is a correctness/consistency issue rather than a circularity: the derivation chain does not reduce to its own inputs by construction. Overall, no circular step meeting the evidentiary bar was found.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The central astrophysical interpretation rests on external catalog parameters, the Prager/Phinney acceleration profile, and assumed intrinsic spin-down values. No new entities are introduced. The main free parameter is the assumed intrinsic spin-down rate for Ter 1 B; core radius and density are trial model variables that the paper explicitly cannot constrain.

free parameters (2)
  • Assumed intrinsic spin-down rate for Ter 1 B = 1e-18 s/s
    Chosen as a large but feasible value from the MSP population to set an upper limit on cluster acceleration and hence bounds on other pulsars' intrinsic spin-down; drives Tables 5 and 6 and the Ter 1 A age estimate.
  • Core radius rc and core density rho_c in the acceleration profile model = Degenerate range; one example rc = 0.36 pc, rho_c = 8.5e5 Msun/pc3
    Two-parameter model from Eq 7 adjusted to encompass the seven pseudo-accelerations; the paper explicitly finds they are not constrained.
assumptions (4)
  • domain assumption Observed Pdot differences are dominated by line-of-sight acceleration in the cluster potential, with intrinsic spin-down negligible for the pseudo-acceleration upper limits.
    Stated in Sec 4.2: the authors begin by assuming the observed Pdot values are from acceleration and the effect of spin-down is negligible. This is necessary to convert Pdot measurements into accelerations and later into age bounds.
  • domain assumption The Prager/Phinney acceleration profile (Eq 7) with a constant-density spherical core describes the cluster potential acceleration for all seven pulsars.
    Borrowed from Phinney (1993) and Prager et al. (2017); assumes uniform core density rho_c and core radius rc. Used to model acceleration versus projected separation.
  • domain assumption External cluster parameters from Baumgardt and Hilker (2018) are correct.
    Distance, core radius, central density, and velocity dispersion from the catalog are used in Sections 4.1.1-4.1.4 and as comparison in 4.2. If these are wrong, the estimated Galactic and nearest-neighbor accelerations and the claimed discrepancy shift.
  • domain assumption The age of Ter 1 is about 12 Gyr.
    Used in Sec 4.4 to compare Ter 1 A's characteristic age with the cluster age. If the cluster is younger, the young-pulsar tension weakens.

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Cite this review

Pith. "Pith review of Timing of Seven Isolated Pulsars in the Globular Cluster Terzan 1." pith.science (2026). https://pith.science/paper/JCIRQAHN

@misc{pith2026241211271,
  author       = {Pith},
  title        = {Pith review of: Timing of Seven Isolated Pulsars in the Globular Cluster Terzan 1},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JCIRQAHN}},
  note         = {Machine review of arXiv:2412.11271}
}
read the original abstract

Globular clusters host large populations of millisecond pulsars (MSPs) due to their high gravitational encounter rates, producing many binary systems and thus MSPs via the recycling process. Seven pulsars with spin periods ranging from 3 ms to 134 ms have been discovered in Terzan 1, which was targeted for pulsar searches with the Green Bank Telescope after Australia Telescope Compact Array imaging revealed steep-spectrum point sources in the cluster core. We have obtained timing observations over seven years, for the first seven Green Bank Telescope (GBT) discoveries (Terzan 1 A through G), using the GBT and Murriyang, CSIRO's Parkes radio telescope. All seven pulsars are isolated, consistent with Terzan 1's classification as a core-collapsed cluster (core collapse is predicted to disrupt, or ionize, binaries). With these timing solutions, we measured the positions and observed period derivatives, dP/dt, for each pulsar. The measured dP/dt values are composed of intrinsic spin-down and accelerations experienced by the pulsars (primarily from the cluster's gravitational potential), and they can be used to infer line-of-sight accelerations. We attempted to constrain the radius and density of the cluster core using these inferred accelerations. A wide range of radii and densities are possible, pointing to the need for continued timing as well as new discoveries to better constrain these cluster properties. We additionally find that Ter 1 A may be younger than the cluster and thus may have formed via a formation channel other than a core-collapse supernova. Theoretical formation mechanisms such as electron-capture supernovae from accretion- or merger-induced collapse of white dwarfs could potentially explain these pulsars' origins. It may therefore be a member of a small but growing class of globular cluster pulsars that appear to be significantly younger than their host clusters.

Figures

Figures reproduced from arXiv: 2412.11271 by the authors.

Figure 1
Figure 1. shows several acceleration profiles to demonstrate how the radius and density parameters impact the fit. Be￾cause we are treating the pulsars’ intrinsic spin-down rates as negligible, the accelerations plotted here represent upper limits on the true accelerations. As can be seen in [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗

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Forward citations

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Works this paper leans on

26 extracted references · 4 canonical work pages · cited by 2 Pith papers

  1. [1]

    2018, MNRAS, 478, 1520, doi: 10.1093/mnras/sty1057

    Baumgardt, H., & Hilker, M. 2018, MNRAS, 478, 1520, doi: 10.1093/mnras/sty1057

    doi:10.1093/mnras/sty1057 2018

  2. [2]

    M., Kaspi, V

    Bhardwaj, M., Gaensler, B. M., Kaspi, V . M., et al. 2021, ApJL, 910, L18, doi: 10.3847/2041-8213/abeaa6

    doi:10.3847/2041-8213/abeaa6 2021

  3. [3]

    Chen, W., Freire, P. C. C., Ridolfi, A., et al. 2023, MNRAS, 520, 3847, doi: 10.1093/mnras/stad029

    doi:10.1093/mnras/stad029 2023

  4. [4]

    2023, MNRAS, 521, 2616, doi: 10.1093/mnras/stad704

    Dai, S., Johnston, S., Kerr, M., et al. 2023, MNRAS, 521, 2616, doi: 10.1093/mnras/stad704

    doi:10.1093/mnras/stad704 2023

  5. [5]

    2024, arXiv e-prints, arXiv:2410.23336, doi: 10.48550/arXiv.2410.23336

    Eftekhari, T., Dong, Y ., Fong, W., et al. 2024, arXiv e-prints, arXiv:2410.23336, doi: 10.48550/arXiv.2410.23336

    arXiv doi:10.48550/arxiv.2410.23336 2024

  6. [6]

    C., Camilo, F., Kramer, M., et al

    Freire, P. C., Camilo, F., Kramer, M., et al. 2003, MNRAS, 340, 1359, doi: 10.1046/j.1365-8711.2003.06392.x

    arXiv 2003

  7. [7]

    Freire, P. C. C., Ransom, S. M., B´egin, S., et al. 2008, ApJ, 675, 670, doi: 10.1086/526338

    doi:10.1086/526338 2008

  8. [8]

    A., Khovritchev, M

    Gontcharov, G. A., Khovritchev, M. Y ., Mosenkov, A. V ., et al. 2021, MNRAS, 508, 2688, doi: 10.1093/mnras/stab2756

    work page doi:10.1093/mnras/stab2756 2021

Show all 26 references
  1. [9]

    Fregeau, J. M. 2008, MNRAS, 386, 553, doi: 10.1111/j.1365-2966.2008.13064.x

    2008

  2. [10]

    Scholz, R. D. 2015, VizieR Online Data Catalog: Milky Way global survey of star clusters. V . (Kharchenko+, 2016), VizieR On-line Data Catalog: J/A+A/585/A101. Originally published in: 2016A&A...585A.101K, doi: 10.26093/cds/vizier.35850101

    2015 doi

  3. [11]

    Scholz, R. D. 2016, A&A, 585, A101, doi: 10.1051/0004-6361/201527292

    2016 doi

  4. [12]

    2022, Nature, 602, 585, doi: 10.1038/s41586-021-04354-w

    Kirsten, F., Marcote, B., Nimmo, K., et al. 2022, Nature, 602, 585, doi: 10.1038/s41586-021-04354-w

    2022 doi

  5. [13]

    S., Heinke, C

    Kremer, K., Ye, C. S., Heinke, C. O., et al. 2024, arXiv e-prints, arXiv:2409.07527, doi: 10.48550/arXiv.2409.07527

    2024 doi arXiv

  6. [14]

    S., Kıro˘glu, F., et al

    Kremer, K., Ye, C. S., Kıro˘glu, F., et al. 2022a, ApJL, 934, L1, doi: 10.3847/2041-8213/ac7ec4 —. 2022b, ApJL, 934, L1, doi: 10.3847/2041-8213/ac7ec4 8

    doi

  7. [15]

    S., Freire, P

    Lynch, R. S., Freire, P. C. C., Ransom, S. M., & Jacoby, B. A. 2012, ApJ, 745, 109, doi: 10.1088/0004-637X/745/2/109

    2012 doi

  8. [16]

    J., & Taylor, J

    Nice, D. J., & Taylor, J. H. 1995, ApJ, 441, 429, doi: 10.1086/175367

    1995 doi

  9. [17]

    1999, A&A, 350, 840 P´erez-Villegas, A., Rossi, L., Ortolani, S., et al

    Ortolani, S., Barbuy, B., Bica, E., et al. 1999, A&A, 350, 840 P´erez-Villegas, A., Rossi, L., Ortolani, S., et al. 2018, PASA, 35, e021, doi: 10.1017/pasa.2018.16

    1999 doi

  10. [18]

    Phinney, E. S. 1993, in Astronomical Society of the Pacific Conference Series, V ol. 50, Structure and Dynamics of Globular Clusters, ed. S. G. Djorgovski & G. Meylan, 141

    1993

  11. [19]

    J., Ransom, S

    Prager, B. J., Ransom, S. M., Freire, P. C. C., et al. 2017, ApJ, 845, 148, doi: 10.3847/1538-4357/aa7ed7

    2017 doi

  12. [20]

    J., Menten, K

    Reid, M. J., Menten, K. M., Brunthaler, A., et al. 2014, ApJ, 783, 130, doi: 10.1088/0004-637X/783/2/130

    2014 doi

  13. [21]

    Ridolfi, A., Freire, P. C. C., Gautam, T., et al. 2022, A&A, 664, A27, doi: 10.1051/0004-6361/202143006

    2022 doi

  14. [22]

    Shklovskii, I. S. 1970, Soviet Ast., 13, 562

    1970

  15. [23]

    Tudor, V ., Miller-Jones, J. C. A., Strader, J., et al. 2022, MNRAS, 513, 3818, doi: 10.1093/mnras/stac1034

    2022 doi

  16. [24]

    Valenti, E., Origlia, L., Mucciarelli, A., & Rich, R. M. 2015, A&A, 574, A80, doi: 10.1051/0004-6361/201424888

    2015 doi

  17. [25]

    Verbunt, F., & Freire, P. C. C. 2014, A&A, 561, A11, doi: 10.1051/0004-6361/201321177

    2014 doi

  18. [26]

    S., Kremer, K., Chatterjee, S., Rodriguez, C

    Ye, C. S., Kremer, K., Chatterjee, S., Rodriguez, C. L., & Rasio, F. A. 2019, ApJ, 877, 122, doi: 10.3847/1538-4357/ab1b21

    2019 doi

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