The reviewed record of science sign in
Pith

arxiv: 2607.06154 · v1 · pith:VOVEVSVT · submitted 2026-07-07 · astro-ph.HE · astro-ph.GA· astro-ph.SR

Pulsars in Globular Clusters With the SKAO

M. Bagchi , F. Abbate , V. Balakrishnan , M. C. i Bernadich , B. Bhattacharyya , A. Dutta , P. C. C. Freire , K. Halley
show 9 more authors
J. W. T. Hessels S. Kumari D. R. Lorimer A. Possenti R. Nag S. M. Ransom A. Ridolfi V. Venkatraman Krishnan W. W. Zhu
This is my paper

Reviewed by Pith T0 review T1 audit T2 compute T3 formal T4 kernel 2026-07-08 14:53 UTCglm-5.2pith:VOVEVSVTrecord.jsonopen to challenge →

classification astro-ph.HE astro-ph.GAastro-ph.SR
keywords pulsarsglobular clustersSKAradio astronomymillisecond pulsarsneutron starsstellar dynamics
0
0 comments X

The pith

SKA telescopes could double known globular cluster pulsars

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

This paper argues that the Square Kilometre Array (SKA) telescopes, once operational, will dramatically expand the known population of radio pulsars in Galactic globular clusters. The authors note that globular clusters are extraordinarily efficient pulsar factories — producing roughly a thousand times more pulsars per unit stellar mass than the Galactic field — yet only 345 have been found across 45 clusters, with the vast majority of clusters still unsearched at adequate sensitivity. Because globular clusters subtend tiny areas on the sky (about one square degree total for all known clusters combined), targeted searches with SKA-MID and SKA-LOW require only a handful of tied-array beams rather than the hundreds of thousands needed for all-sky surveys. This makes globular cluster pulsar searches an ideal early-science program that can run during telescope commissioning, before full survey capability is available. The paper presents two prediction tracks: a conservative one based on comparing SKA sensitivity to current best searches (FAST and MeerKAT), which forecasts 150–300 new pulsars in clusters already known to host pulsars, and an optimistic one using the empirical scaling relation N = Gamma^0.7 between pulsar content and stellar encounter rate, which yields up to roughly 1700 detectable pulsars across all Galactic globular clusters visible to SKA. The authors further argue that this population expansion will enable tests of gravity theories, constraints on the neutron star equation of state, measurements of cluster potentials and intra-cluster gas, and the discovery of exotic systems such as pulsar–black hole binaries, double neutron star systems with large misaligned spins, and possibly sub-millisecond pulsars.

Core claim

The central quantitative claim is that SKA-MID, even in its partial AA* configuration available during early commissioning, will discover dozens to hundreds of new globular cluster pulsars, with the full AA4 configuration potentially more than doubling the current known population of 345. The optimistic scenario, grounded in the empirical correlation N = Gamma^0.7 relating pulsar content to the two-body encounter rate, predicts up to approximately 1700 detectable pulsars across all Galactic globular clusters visible to SKA telescopes. The paper also establishes that the total sky area to be searched is only about one square degree, making this the most efficient pulsar discovery program per-

What carries the argument

The prediction rests on two independent estimation methods. The first uses the scaling relation N = Gamma^0.7 from Hui et al. (2010), where Gamma is the two-body encounter rate of a globular cluster, to estimate total pulsar content across all 157 known Galactic clusters, combined with a log-normal pulsar luminosity function to determine what fraction falls within SKA sensitivity. The second method compares the SKA-MID flux density limits to those achieved by the current best telescopes (FAST and MeerKAT) for each cluster, computing a luminosity-function growth factor Gamma_LF that quantifies how much deeper SKA probes. Both methods converge on the conclusion that SKA will substantially grow

If this is right

  • If the optimistic prediction of ~1700 detectable pulsars holds, the sample would be large enough to systematically test whether the N = Gamma^0.7 scaling relation holds across clusters with very different properties, potentially revealing which cluster parameters most directly govern pulsar retention.
  • A doubling or tripling of the known population would likely yield the first confirmed pulsar–black hole binary (building on the PSR J0514-4002E candidate), enabling tests of gravity theories in regimes inaccessible from the Galactic field.
  • The discovery of ultra-fast rotators beyond the current 716 Hz record would place direct constraints on the neutron star equation of state, particularly if masses can be measured.
  • Differential dispersion and rotation measures from many pulsars within the same cluster would map intra-cluster gas and magnetic fields at unprecedented detail, testing the hypothesis that neutron star winds strip gas from globular clusters.
  • The archival search-mode data strategy proposed (~700 TB long-term storage) would enable re-analysis with future algorithms, potentially extracting pulsars too faint or too accelerated for current search techniques.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The two prediction methods (scaling relation vs. sensitivity comparison) bracket a wide range (150 to 1700), and the paper does not fully reconcile them; the gap reflects genuine uncertainty about pulsar populations in the ~112 clusters with no known pulsars, where the sensitivity-comparison method is inapplicable.
  • If the scaling relation N = Gamma^0.7 overestimates pulsar content for low-mass or distant clusters — as population synthesis simulations suggest — the true yield may be closer to the conservative end, though still representing a significant increase over the current 345.
  • The proposal to search all 157 clusters with only 16 beams per pointing is feasible precisely because globular cluster cores are compact, but pulsars displaced from cluster cores by dynamical interactions may be missed without mosaic pointings, creating a selection effect against the most dynamically processed systems.
  • The emphasis on early commissioning science (AA* core only) suggests that the first SKA pulsar discoveries in globular clusters could arrive before the telescope reaches full operational capability, providing a fast path to high-impact results.

Load-bearing premise

The optimistic prediction of ~1700 detectable pulsars relies on extrapolating the empirical scaling relation N = Gamma^0.7 — derived from clusters with known pulsars — to all 157 Galactic globular clusters, including the ~112 where no pulsars have been found. This relation has significant scatter and may not hold for clusters with very different masses, distances, or dynamical histories.

What would settle it

If SKA-MID AA4 surveys of globular clusters with no known pulsars find significantly fewer pulsars than predicted by the N = Gamma^0.7 scaling relation, the optimistic estimate of ~1700 would be invalidated.

Figures

Figures reproduced from arXiv: 2607.06154 by A. Dutta, A. Possenti, A. Ridolfi, B. Bhattacharyya, D. R. Lorimer, F. Abbate, J. W. T. Hessels, K. Halley, M. Bagchi, M. C. i Bernadich, P. C. C. Freire, R. Nag, S. Kumari, S. M. Ransom, V. Balakrishnan, V. Venkatraman Krishnan, W. W. Zhu.

Figure 1
Figure 1. Figure 1: Pulsar population in GCs with time. A consequence of this is the fact that, since the earliest handful of GC pulsar discoveries in the late 1980’s / early 1990’s (e.g. Lyne et al., 1987, 1988; Manchester et al., 1990; Anderson et al., 1990; Manchester et al., 1991; Kulkarni et al., 1991; Manchester et al., 1991; Anderson, 1993), the known population of GC pulsars has increased in a stepwise manner (see [P… view at source ↗
Figure 2
Figure 2. Figure 2: Sky distributions of Galactic globular clusters, demonstrating that there are many GCs in the sky (pink hexagons) observable by SKA telescopes and many of those GCs still do not have any pulsars discovered in them (pink hexagons without blue stars). GCs in the declination range +15◦ to −90◦ have been considered as visible by the SKA telescopes. Moreover, the study of some unique sub-classes of pulsars can … view at source ↗
Figure 3
Figure 3. Figure 3: Left: cumulative luminosity distribution of all 176 pulsars with published values of flux densities. The blue line is a power-law with an exponent of 𝛼 = −1. Right: the upper panel shows the correlation between estimated pulsar content, 𝑁, and the two-body encounter rate, Γ. The solid line compares these estimates to the best fit found by Hui et al. (2010) in which 𝑁 = Γ0.7 . The lower panel shows the sign… view at source ↗
Figure 4
Figure 4. Figure 4: Simulated GC pulsars detectable in a 2 hr baseline SKA-MID (AA4 configuration) survey shown alongside the underlying model population and the current sample of GC pulsars with measured flux densities. Although a number of faint pulsars will still remain undetectable with such a survey, the enhancement in the size of the population of high flux density pulsars is significant. of the cluster (FAST for the GC… view at source ↗
Figure 5
Figure 5. Figure 5: was to feed the calculated sensitivity limits to a log-normal pulsar LF with the mean (in units of mJy kpc2 expressed in a logarithmic base-10 scale) of −1.1 and the standard deviation 0.9, which is known to reproduce the observed data (Bagchi et al., 2011; Chennamangalam et al., 2013) [PITH_FULL_IMAGE:figures/full_fig_p022_5.png] view at source ↗
read the original abstract

Globular clusters (GCs) are highly efficient factories of radio pulsars: per unit of stellar mass, they contain about 1000 times more pulsars than in the Galactic field. Thus far, 345 radio pulsars have been found in GCs. These can be used as precision probes of the structure, gas content, magnetic field, and dynamic history of their host clusters; some of them are also highly interesting in their own right because they probe exotic stellar evolution scenarios, the physics of dense matter, accretion, gravity, etc. One of them (PSR~J0514$-$4002E) might even be the first pulsar - black hole system known. Deep searches with SKA telescopes will only require one to a few tied-array beams, and can be done during early commissioning of the telescopes, before an all-sky pulsar survey using hundreds to thousands of tied-array beams is feasible. Even a conservative approach predicts discoveries only with the core of SKA-MID AA*. Eventually, SKA-MID AA4 is expected to increase the number of discoveries even more, leading to more than doubling the current known population. Thus, a dedicated search for pulsars in GCs will fully utilise the best possible natural laboratories to study various branches of physics and astrophysics, including the properties of dense matter, stellar evolution, and the dynamical history of these GCs.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 7 minor

Summary. This manuscript is a science-case chapter for the 'Advancing Astrophysics with the SKA – II' proceedings, arguing for dedicated pulsar searches in Galactic globular clusters (GCs) with SKA-MID and SKA-LOW. The paper reviews the science motivation (individual exotic systems, population studies, cluster probes), discusses observing strategies and search techniques, and presents two prediction tracks for SKA discovery yields: an optimistic track based on the N = Γ^0.7 scaling relation (Hui et al. 2010) applied to all 157 GCs, yielding ~1700 detectable pulsars with SKA-MID AA4; and a conservative track based on luminosity-function probing improvements (Γ_LF) for the 45 GCs already known to host pulsars, yielding ~150–300 new discoveries (Table 1). The paper is comprehensive, well-referenced, and transparent about the limitations of both approaches.

Significance. The science case is timely and well-motivated: GC pulsar searches are an ideal early-science program for SKA-MID, requiring few tied-array beams and modest observing time. The paper usefully quantifies discovery space using two independent methods and clearly labels them as optimistic and conservative. The discussion of search techniques (acceleration-jerk, Keplerian parameter searches, FFA, imaging, baseband analysis) and data archiving requirements is valuable for the community. The transparency in presenting both prediction tracks, including explicit acknowledgment that the conservative track cannot be extrapolated to all GCs, is commendable.

major comments (3)
  1. Abstract and Conclusions: The claim that SKA-MID AA4 will lead to 'more than doubling the current known population' is not cleanly supported by the conservative track alone. Table 1 gives at most ~300 new discoveries for the most advanced conservative configuration (AA4, 8 hr), yielding a total of ~645, which is 1.87× the current 345 — short of doubling. The 'more than doubling' threshold is only reached via the optimistic track (~1700, Section 4.1) or the power-law LF variant mentioned at the end of Section 4.2 ('more than doubling all the figures in Table 1'). The abstract should clarify which prediction track supports this claim, or soften the wording to match what the conservative track delivers.
  2. Section 4.1: The N = Γ^0.7 scaling relation is calibrated on 17 clusters (Figure 3, those with ≥2 pulsars with measured flux densities) and extrapolated to all 157 GCs, including ~112 with zero known pulsars. The resulting ~6000 total pulsars exceeds the Turk & Lorimer (2013) population synthesis range of 600–3700. The paper acknowledges this discrepancy qualitatively but provides no uncertainty estimate on either the ~6000 total or the ~1700 detectable figure. Given that the scatter in Figure 3 is visibly large (spanning roughly an order of magnitude in N at fixed Γ), at least a rough uncertainty range on the ~1700 prediction would strengthen the claim and allow readers to assess how much it overlaps with Turk & Lorimer (2013).
  3. Section 2.1 (PSR J0514−4002E discussion): The paragraphs discussing the companion nature, post-Keplerian parameters, frame-dragging, and Shapiro delay appear twice with near-identical but slightly different wording (the bullet point on 'Binary pulsars as test beds of gravity'). This is a substantial duplication that should be resolved by keeping one version.
minor comments (7)
  1. Section 1: The sentence 'This improves the prospects for the discovery of much more extreme objects in Galactic GCs' could benefit from a forward reference to the relevant Section.
  2. Figure 3 caption: 'Left' panel shows cumulative luminosity distribution and 'Right' shows the N–Γ correlation, but the caption text does not fully describe the lower-right panel (probability density of Pearson's r). A brief description would help.
  3. Section 3.5: The SEFD values (5.3 Jy for AA*, 3.9 Jy for AA4) are stated without explicit reference to how they were derived beyond 'scaling from Bailes et al. (2020)'. A brief note on the scaling method would aid reproducibility.
  4. Table 1: The column header 'Total discoveries' might be clearer as 'New discoveries' since these are additional to the 345 already known.
  5. Section 4.2: The effective duty cycle of 25% used for the Γ_LF calculation is described as 'typical for millisecond pulsars' but is on the high side for many MSPs. A brief justification or sensitivity test would be useful.
  6. Section 5: The data volume estimate (2 PB raw, ~700 TB after sub-banding) is helpful but the assumed 75 μs sampling time differs from the 50 μs mentioned in Section 3.5. This inconsistency should be reconciled.
  7. Several references have formatting issues (e.g., 'Göttgens et al, 2021' missing period; 'Ridolfi et al, 2021' in main text vs. 'Ridolfi et al.' in references).

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for a careful and constructive report. All three major comments are well-taken. We agree with the substance of each point and will revise the manuscript accordingly: (1) the abstract and conclusions will be reworded to clarify which prediction track supports the 'more than doubling' claim; (2) we will add an approximate uncertainty range on the ~1700 optimistic prediction; and (3) the duplicated paragraphs on PSR J0514−4002E will be consolidated into a single version. No standing objections remain.

read point-by-point responses

  1. Referee: Abstract and Conclusions: The claim that SKA-MID AA4 will lead to 'more than doubling the current known population' is not cleanly supported by the conservative track alone. Table 1 gives at most ~300 new discoveries for the most advanced conservative configuration (AA4, 8 hr), yielding a total of ~645, which is 1.87× the current 345 — short of doubling. The 'more than doubling' threshold is only reached via the optimistic track (~1700, Section 4.1) or the power-law LF variant mentioned at the end of Section 4.2. The abstract should clarify which prediction track supports this claim, or soften the wording to match what the conservative track delivers.

    Authors: The referee is correct. The conservative track (Table 1) yields at most ~300 new discoveries, giving a total of ~645, which falls short of doubling the current population of 345. The 'more than doubling' claim is supported only by the optimistic track (~1700 detectable pulsars; Section 4.1) or by the power-law luminosity function variant discussed at the end of Section 4.2 (which more than doubles the Table 1 figures). We will revise the abstract and conclusions to make explicit that the 'more than doubling' prediction arises from the optimistic scaling-relation track, not from the conservative luminosity-function-probing approach. We will also note that the conservative track alone predicts a substantial but sub-doubling increase (up to ~1.9× the current population). This will make the two prediction tracks and their respective yields transparent to the reader. revision: yes

  2. Referee: Section 4.1: The N = Γ^0.7 scaling relation is calibrated on 17 clusters (Figure 3, those with ≥2 pulsars with measured flux densities) and extrapolated to all 157 GCs, including ~112 with zero known pulsars. The resulting ~6000 total pulsars exceeds the Turk & Lorimer (2013) population synthesis range of 600–3700. The paper acknowledges this discrepancy qualitatively but provides no uncertainty estimate on either the ~6000 total or the ~1700 detectable figure. Given that the scatter in Figure 3 is visibly large (spanning roughly an order of magnitude in N at fixed Γ), at least a rough uncertainty range on the ~1700 prediction would strengthen the claim and allow readers to assess how much it overlaps with Turk & Lorimer (2013).

    Authors: We agree that providing a rough uncertainty estimate on the ~1700 detectable pulsar figure would strengthen the claim and help readers contextualize it relative to Turk & Lorimer (2013). The large scatter in Figure 3 (roughly an order of magnitude in N at fixed Γ) is real and reflects both the intrinsic cluster-to-cluster variance and the small calibration sample of 17 clusters. We will add an approximate uncertainty range derived from the scatter in the N = Γ^0.7 relation. A straightforward approach is to propagate the rms scatter of the residuals in log N from the best-fit relation; this yields a factor of roughly ±0.5 dex (i.e., approximately a factor of 3) uncertainty on the per-cluster predictions, which when combined across all 157 clusters gives a rough range of roughly 500–5000 detectable pulsars for the optimistic track. We will state this range explicitly, note that it broadly overlaps with the Turk & Lorimer (2013) range of 600–3700 at its lower end, and reiterate that the ~1700 figure should be interpreted as a central estimate from a simple scaling relation with substantial associated uncertainty. We will also add a brief note that the ~6000 total pulsar figure carries a comparable fractional uncertainty. revision: yes

  3. Referee: Section 2.1 (PSR J0514−4002E discussion): The paragraphs discussing the companion nature, post-Keplerian parameters, frame-dragging, and Shapiro delay appear twice with near-identical but slightly different wording (the bullet point on 'Binary pulsars as test beds of gravity'). This is a substantial duplication that should be resolved by keeping one version.

    Authors: The referee is correct: the discussion of PSR J0514−4002E in Section 2.1 is duplicated, with two near-identical but slightly differently worded versions of the same paragraphs appearing consecutively. This appears to be an editorial oversight where a revised version was inserted without removing the original. We will remove the duplicate and retain a single, consolidated version that incorporates the clearest wording from both passages, covering the companion mass constraints from post-Keplerian parameters, the frame-dragging effect from a rapidly rotating black hole, the role of Shapiro delay and light bending in constraining orbital inclination, and the encouragement of a long-term SKA timing campaign. revision: yes

Circularity Check

0 steps flagged

No significant circularity: predictions rest on externally published scaling relations and luminosity functions, with one minor self-citation (Bagchi et al. 2011) that is not load-bearing for the central claim.

full rationale

The paper presents two prediction tracks. The optimistic track (Section 4.1) applies the scaling relation N = Γ^0.7 from Hui et al. (2010) — an externally published empirical correlation — to all 157 GCs, then filters by SKA-MID AA4 sensitivity using the log-normal luminosity function of Faucher-Giguère & Kaspi (2006). The conservative track (Section 4.2, Table 1) computes Γ_LF by comparing SKA-MID sensitivity to current FAST/MeerKAT limits, using a log-normal LF with parameters from Bagchi et al. (2011) and Chennamangalam et al. (2013). While Bagchi et al. (2011) is co-authored by the lead author of this paper, that work is a parameter-fitting study whose stated assumptions (log-normal LF shape, mean = -1.1, sigma = 0.9) do not include the target result here (number of SKA discoveries). The LF parameters are fitted to observed pulsar luminosity data, not to SKA yield predictions. The N = Γ^0.7 relation is from Hui et al. (2010), an independent group. The paper explicitly acknowledges the discrepancy between its ~6000 total estimate and Turk & Lorimer (2013)'s 600–3700 range, and states that the conservative Γ_LF approach 'cannot be obtained for the GCs where no pulsar is known so far.' No step in either derivation chain reduces to its own inputs by construction. The predictions are extrapolation-dependent and uncertain, but they are not circular.

Axiom & Free-Parameter Ledger

5 free parameters · 4 axioms · 0 invented entities

The paper introduces no new particles, forces, dimensions, or postulated entities. All physical objects discussed (pulsars, neutron stars, black holes, globular clusters) are well-established. The free parameters are all fitted values from prior literature, not invented for this paper.

free parameters (5)
  • Luminosity function mean (log10, mJy kpc²) = -1.1
    Mean of the log-normal pulsar luminosity function, taken from Bagchi et al. (2011) and Faucher-Giguère & Kaspi (2006). Used in Section 4.2 to predict detectable pulsar counts.
  • Luminosity function standard deviation = 0.9
    Standard deviation of the log-normal luminosity function, from Bagchi et al. (2011). Used in Section 4.2.
  • Scaling relation exponent = 0.7
    Exponent in N = Γ^0.7 from Hui et al. (2010). Used in Section 4.1 to estimate total pulsar population (~6000).
  • Pulsar spectral index = -1.7
    Assumed spectral index for scaling flux density limits between frequencies/instruments in Section 4.2.
  • Effective pulsar duty cycle = 0.25
    Assumed duty cycle for MSPs in sensitivity calculations in Section 4.2.
axioms (4)
  • domain assumption The log-normal luminosity function with parameters from Bagchi et al. (2011) is representative of the true underlying GC pulsar luminosity distribution.
    Invoked in Section 4.1 and 4.2 to convert sensitivity limits to predicted pulsar counts. If the LF shape or parameters are wrong, all predictions change.
  • domain assumption The scaling relation N = Γ^0.7 (Hui et al. 2010) holds for all Galactic GCs, including those with no known pulsars.
    Invoked in Section 4.1 to extrapolate total pulsar population to ~6000 across all 157 GCs. The relation was derived from a limited sample.
  • domain assumption Dispersion and scattering effects are the same across all instruments/surveys compared in Section 4.2.
    Stated explicitly in Section 4.2: 'We also assumed that the effects of the dispersion and scattering are the same in all instruments/surveys.'
  • domain assumption GC pulsars congregate toward the cluster core, with almost all within one arc-minute of the optical center-of-light.
    Invoked in Section 3.4 to justify that 16 tied-array beams suffice to cover the discovery space.

pith-pipeline@v1.1.0-glm · 35826 in / 3454 out tokens · 469406 ms · 2026-07-08T14:53:21.455006+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

235 extracted references · 235 canonical work pages · 174 internal anchors

  1. [1]

    A population of gamma-ray emitting globular clusters seen with the Fermi Large Area Telescope

    A population of gamma-ray emitting globular clusters seen with the Fermi Large Area Telescope. , keywords =. doi:10.1051/0004-6361/201014458 , archivePrefix =. 1003.3588 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201014458

  2. [2]

    Searching for pulsars in extreme orbits -- GPU acceleration of the Fourier domain 'jerk' search

    Searching for Pulsars in Extreme Orbits - GPU Acceleration of the Fourier Domain 'Jerk' Search. Astronomical Data Analysis Software and Systems XXIX , year = 2020, editor =. doi:10.48550/arXiv.1911.01353 , archivePrefix =. 1911.01353 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1911.01353 2020

  3. [3]

    Testing the universality of free fall by tracking a pulsar in a stellar triple system

    Universality of free fall from the orbital motion of a pulsar in a stellar triple system. , keywords =. doi:10.1038/s41586-018-0265-1 , archivePrefix =. 1807.02059 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-018-0265-1

  4. [4]

    , keywords =

    A new class of radio pulsars. , keywords =. doi:10.1038/300728a0 , adsurl =

    work page doi:10.1038/300728a0

  5. [5]

    , keywords =

    Discovery of two radio pulsars in the globular cluster M15. , keywords =. doi:10.1038/346042a0 , adsurl =

    work page doi:10.1038/346042a0

  6. [6]

    A Study of Recycled Pulsars in Globular Clusters

    work page

  7. [7]

    A Fourier Domain "Jerk" Search for Binary Pulsars

    A Fourier Domain Jerk Search for Binary Pulsars. , keywords =. doi:10.3847/2041-8213/aad59f , archivePrefix =. 1807.07900 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aad59f 2041

  8. [8]

    A Massive Pulsar in a Compact Relativistic Binary

    A Massive Pulsar in a Compact Relativistic Binary. , keywords =. doi:10.1126/science.1233232 , archivePrefix =. 1304.6875 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1233232

  9. [9]

    Internal gas models and central black hole in 47 Tucanae using millisecond pulsars

    Internal gas models and central black hole in 47 Tucanae using millisecond pulsars. , keywords =. doi:10.1093/mnras/sty2298 , archivePrefix =. 1808.06621 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2298

  10. [10]

    Giant pulses from J1823-3021A observed with the MeerKAT telescope

    Giant pulses from J1823-3021A observed with the MeerKAT telescope. , keywords =. doi:10.1093/mnras/staa2510 , archivePrefix =. 2008.07548 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa2510 2008

  11. [11]

    Four pulsar discoveries in NGC 6624 by TRAPUM using MeerKAT

    Four pulsar discoveries in NGC 6624 by TRAPUM using MeerKAT. , keywords =. doi:10.1093/mnras/stac1041 , archivePrefix =. 2204.05334 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac1041

  12. [12]

    A MeerKAT look at the polarization of 47 Tucanae pulsars: magnetic field implications

    A MeerKAT look at the polarization of 47 Tucanae pulsars: magnetic field implications. , keywords =. doi:10.1093/mnras/stac3248 , archivePrefix =. 2211.03815 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac3248

  13. [13]

    Evidence of non-luminous matter in the center of M62

    Evidence of Nonluminous Matter in the Center of M62. , keywords =. doi:10.3847/2041-8213/ab46c3 , archivePrefix =. 1909.11091 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ab46c3 2041

  14. [14]

    Intermediate mass black holes in globular clusters: effects on jerks and jounces of millisecond pulsars

    Intermediate mass black holes in globular clusters: effects on jerks and jounces of millisecond pulsars. , keywords =. doi:10.1093/mnras/stz1330 , archivePrefix =. 1905.05209 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1330 1905

  15. [15]

    A Radio Pulsar/X-ray Binary Link

    A Radio Pulsar/X-ray Binary Link. , keywords =. doi:10.1126/science.1172740 , archivePrefix =. 0905.3397 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1172740

  16. [16]

    A MeerKAT view of the pulsars in the globular cluster NGC 6522

    A MeerKAT view of the pulsars in the globular cluster NGC 6522. , keywords =. doi:10.1051/0004-6361/202347725 , archivePrefix =. 2310.03800 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202347725

  17. [17]

    Merging stellar and intermediate-mass black holes in dense clusters: implications for LIGO, LISA and the next generation of gravitational wave detectors

    Merging stellar and intermediate-mass black holes in dense clusters: implications for LIGO, LISA, and the next generation of gravitational wave detectors. , keywords =. doi:10.1051/0004-6361/202037785 , archivePrefix =. 2007.13746 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202037785 2007

  18. [18]

    Astrophysics with the Laser Interferometer Space Antenna

    Astrophysics with the Laser Interferometer Space Antenna. Living Reviews in Relativity , keywords =. doi:10.1007/s41114-022-00041-y , archivePrefix =. 2203.06016 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s41114-022-00041-y

  19. [19]

    doi:10.1088/2041-8205/773/1/L12 , keywords =

    GMRT discovery of PSR J1544+ 4937: an eclipsing black-widow pulsar identified with a Fermi-LAT source , year = 2013, month = aug, journal =. doi:10.1088/2041-8205/773/1/L12 , keywords =

    work page doi:10.1088/2041-8205/773/1/l12 2013

  20. [20]

    Mean proper motions, space orbits and velocity dispersion profiles of Galactic globular clusters derived from Gaia DR2 data

    Mean proper motions, space orbits, and velocity dispersion profiles of Galactic globular clusters derived from Gaia DR2 data. , keywords =. doi:10.1093/mnras/sty2997 , archivePrefix =. 1811.01507 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2997

  21. [21]

    No evidence for intermediate-mass black holes in the globular clusters $\omega$ Cen and NGC 6624

    No evidence for intermediate-mass black holes in the globular clusters Cen and NGC 6624. , keywords =. doi:10.1093/mnras/stz2060 , archivePrefix =. 1907.10845 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz2060 1907

  22. [22]

    The MeerKAT Telescope as a Pulsar Facility: System verification and early science results from MeerTime

    The MeerKAT telescope as a pulsar facility: System verification and early science results from MeerTime. , keywords =. doi:10.1017/pasa.2020.19 , archivePrefix =. 2005.14366 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1017/pasa.2020.19 2020

  23. [23]

    Optical identification of the companion to PSR J1911-5958A, the pulsar binary in the outskirts of NGC 6752

    Optical identification of the companion to PSR J1911-5958A, the pulsar binary in the outskirts of NGC 6752. A&A , keywords =. doi:10.1051/0004-6361:20031339 , archivePrefix =. astro-ph/0307340 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20031339

  24. [24]

    X-ray Sources and their Optical Counterparts in the Globular Cluster M4

    X-Ray Sources and Their Optical Counterparts in the Globular Cluster M4. , keywords =. doi:10.1086/421259 , archivePrefix =. astro-ph/0402197 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/421259

  25. [25]

    The pulsar spectral index distribution

    The pulsar spectral index distribution. , keywords =. doi:10.1093/mnras/stt257 , archivePrefix =. 1302.2053 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt257 2053

  26. [26]

    Young Radio Pulsars in Galactic Globular Clusters

    Young Radio Pulsars in Galactic Globular Clusters. , keywords =. doi:10.1088/0004-637X/742/1/51 , archivePrefix =. 1108.4402 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/742/1/51

  27. [27]

    A state change in the low-mass X-ray binary XSS J12270-4859

    A state change in the low-mass X-ray binary XSS J12270-4859. , keywords =. doi:10.1093/mnras/stu708 , archivePrefix =. 1402.0765 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu708

  28. [28]

    New constraints on the central mass contents of Omega Centauri from combined stellar kinematics and pulsar timing

    New constraints on the central mass contents of Omega Centauri from combined stellar kinematics and pulsar timing. , keywords =. doi:10.1051/0004-6361/202451763 , archivePrefix =. 2408.00939 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202451763

  29. [29]

    A pulsar in a binary with a compact object in the mass gap between neutron stars and black holes

    A pulsar in a binary with a compact object in the mass gap between neutron stars and black holes. , keywords =. doi:10.1126/science.adg3005 , archivePrefix =. 2401.09872 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.adg3005

  30. [30]

    Orbital eccentricity of binary radio pulsars in globular clusters and interaction between stars

    Orbital Eccentricity of Binary Radio Pulsars in Globular Clusters and the Interaction Between Stars. , keywords =. doi:10.1088/0004-637X/693/2/L91 , archivePrefix =. 0901.1295 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/693/2/l91

  31. [31]

    , archivePrefix = "arXiv", eprint =

    Luminosities of recycled radio pulsars in globular clusters. , keywords =. doi:10.1111/j.1365-2966.2011.19498.x , archivePrefix =. 1107.4521 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19498.x 2011

  32. [32]

    On the detectability of eccentric binary pulsars

    On the detectability of eccentric binary pulsars. , keywords =. doi:10.1093/mnras/stt559 , archivePrefix =. 1302.4914 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt559

  33. [33]

    Radio pulsar binaries in globular clusters: their orbital eccentricities and stellar interactions

    Radio Pulsar Binaries in Globular Clusters: Their Orbital Eccentricities and Stellar Interactions. , keywords =. doi:10.1088/0004-637X/701/2/1161 , archivePrefix =. 0906.2163 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/701/2/1161

  34. [34]

    Missing for 20 years: MeerKAT re-detects the elusive binary pulsar M30B

    Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B. , keywords =. doi:10.3847/2041-8213/acae99 , archivePrefix =. 2301.04983 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/acae99 2041

  35. [35]

    Coherent Search for Binary Pulsars across all Five Keplerian Parameters in Radio Observations using the template-bank algorithm

    Coherent search for binary pulsars across all Five Keplerian parameters in radio observations using the template-bank algorithm. , keywords =. doi:10.1093/mnras/stab3746 , archivePrefix =. 2112.11991 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab3746

  36. [36]

    Chandra X-Ray Observations of Nineteen Millisecond Pulsars in the Globular Cluster 47 Tucanae

    Chandra X-Ray Observations of 19 Millisecond Pulsars in the Globular Cluster 47 Tucanae. , keywords =. doi:10.1086/505133 , archivePrefix =. astro-ph/0604318 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/505133

  37. [37]

    Chandra X-ray Observations of 12 Millisecond Pulsars in the Globular Cluster M28

    Chandra X-ray Observations of 12 Millisecond Pulsars in the Globular Cluster M28. , keywords =. doi:10.1088/0004-637X/730/2/81 , archivePrefix =. 1101.4944 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/730/2/81

  38. [38]

    , keywords =

    Timing a millisecond pulsar in a globular cluster. , keywords =. doi:10.1093/mnras/225.1.51P , adsurl =

    work page doi:10.1093/mnras/225.1.51p

  39. [39]

    In what sense a neutron star-black hole binary is the holy grail for testing gravity?

    In what sense a neutron star-black hole binary is the holy grail for testing gravity?. , keywords =. doi:10.1088/1475-7516/2014/08/055 , archivePrefix =. 1405.3838 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2014/08/055 2014

  40. [40]

    Study of the Influence of an Evolving Galactic Potential on the Orbital Properties of 152 Globular clusters with Data from the Gaia EDR3 Catalogue

    Study of the Influence of an Evolving Galactic Potential on the Orbital Properties of 152 Globular Clusters with Data from the Gaia EDR3 Catalogue. Astronomy Letters , keywords =. doi:10.1134/S106377372107001X , archivePrefix =. 2109.10570 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1134/s106377372107001x

  41. [41]

    Discovery of three new millisecond pulsars in Terzan 5

    Discovery of Three New Millisecond Pulsars in Terzan 5. , keywords =. doi:10.3847/1538-4357/aaac2a , archivePrefix =. 1801.09929 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaac2a

  42. [42]

    Formation of black widows and redbacks -- two distinct populations of eclipsing binary millisecond pulsars

    Formation of Black Widows and Redbacks Two Distinct Populations of Eclipsing Binary Millisecond Pulsars. , keywords =. doi:10.1088/0004-637X/775/1/27 , archivePrefix =. 1308.4107 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/775/1/27

  43. [43]

    The GBT 350-MHz Drift Scan Pulsar Survey. III. Detection of a magnetic field in the eclipsing material of PSR J2256-1024

    The GBT 350-MHz Drift Scan Pulsar Survey - III. Detection of a magnetic field in the eclipsing material of PSR J2256-1024. , keywords =. doi:10.1093/mnras/staa933 , archivePrefix =. 2004.00164 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa933 2004

  44. [44]

    Timing of Millisecond Pulsars in NGC 6752. III. On the Presence of Nonluminous Matter in the Cluster's Core. , keywords =. doi:10.3847/1538-4357/ad5e74 , archivePrefix =. 2407.03271 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad5e74

  45. [45]

    Observations of 20 millisecond pulsars in 47 Tucanae at 20 cm

    Observations of 20 Millisecond Pulsars in 47 Tucanae at 20 Centimeters. , keywords =. doi:10.1086/308859 , archivePrefix =. astro-ph/9911234 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308859

  46. [46]

    Pulsars in Globular Clusters

    Pulsars in Globular Clusters. Binary Radio Pulsars , year = 2005, editor =. doi:10.48550/arXiv.astro-ph/0501226 , archivePrefix =. astro-ph/0501226 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0501226 2005

  47. [47]

    Constraining the luminosity function parameters and population size of radio pulsars in globular clusters

    Constraining the luminosity function parameters and population size of radio pulsars in globular clusters. , keywords =. doi:10.1093/mnras/stt205 , archivePrefix =. 1207.5732 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt205

  48. [48]

    The puzzling properties of the Helium White Dwarf orbiting the millisecond pulsar PSR J1911-5958A in NGC 6752

    The Puzzling Properties of the Helium White Dwarf Orbiting the Millisecond Pulsar PSR J1911-5958A in NGC 6752. , keywords =. doi:10.1086/504040 , archivePrefix =. astro-ph/0603269 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/504040

  49. [49]

    NE2001.I. A New Model for the Galactic Distribution of Free Electrons and its Fluctuations

    NE2001.I. A New Model for the Galactic Distribution of Free Electrons and its Fluctuations. arXiv e-prints , keywords =. doi:10.48550/arXiv.astro-ph/0207156 , archivePrefix =. astro-ph/0207156 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0207156

  50. [50]

    Gamma-ray emission from the Sagittarius Dwarf Spheroidal galaxy due to millisecond pulsars

    Gamma-ray emission from the Sagittarius dwarf spheroidal galaxy due to millisecond pulsars. , keywords =. doi:10.1038/s41550-022-01777-x , archivePrefix =. 2204.12054 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-022-01777-x

  51. [51]

    , keywords =

    X-ray binaries in globular clusters. , keywords =. doi:10.1086/181869 , adsurl =

    work page doi:10.1086/181869

  52. [52]

    MeerKAT discovery of 13 new pulsars in Omega Centauri

    MeerKAT discovery of 13 new pulsars in Omega Centauri. , keywords =. doi:10.1093/mnras/stad029 , archivePrefix =. 2301.03864 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad029

  53. [53]

    Rocking the Lighthouse: Circumpulsar Asteroids and Radio Intermittency

    Rocking the Lighthouse: Circumpulsar Asteroids and Radio Intermittency. , keywords =. doi:10.1086/589425 , archivePrefix =. astro-ph/0605145 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/589425

  54. [54]

    Dynamics of intermediate mass black holes in globular clusters. Wander radius and anisotropy profiles

    Dynamics of intermediate mass black holes in globular clusters. Wander radius and anisotropy profiles. , keywords =. doi:10.1051/0004-6361/202346124 , archivePrefix =. 2302.05542 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202346124

  55. [55]

    An eclipsing millisecond pulsar with a possible main-sequence companion in NGC 6397

    An Eclipsing Millisecond Pulsar with a Possible Main-Sequence Companion in NGC 6397. , keywords =. doi:10.1086/324562 , archivePrefix =. astro-ph/0108250 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/324562

  56. [56]

    Timing of Millisecond Pulsars in NGC 6752: Evidence for a High Mass-to-Light Ratio in the Cluster Core

    Timing of Millisecond Pulsars in NGC 6752: Evidence for a High Mass-to-Light Ratio in the Cluster Core. , keywords =. doi:10.1086/341030 , archivePrefix =. astro-ph/0204283 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/341030

  57. [57]

    Shapiro delay measurement of a two solar mass neutron star

    A two-solar-mass neutron star measured using Shapiro delay. , keywords =. doi:10.1038/nature09466 , archivePrefix =. 1010.5788 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature09466

  58. [58]

    Globular Clusters GMRT Pulsar Search (GCGPS). I. Survey Description, Discovery and Timing of the First Pulsar in NGC6093 (M80). , keywords =. doi:10.3847/1538-4357/ade052 , archivePrefix =. 2502.09154 , primaryClass =

    work page doi:10.3847/1538-4357/ade052

  59. [59]

    Advanced Software and Control for Astronomy II , year = 2008, editor =

    Data Vault: providing simple web access to NRAO data archives. Advanced Software and Control for Astronomy II , year = 2008, editor =. doi:10.1117/12.789402 , adsurl =

    work page doi:10.1117/12.789402 2008

  60. [60]

    NGC 1851A: Revealing an ongoing three-body encounter in a dense globular cluster

    NGC 1851A: Revealing an ongoing three-body encounter in a dense globular cluster. , keywords =. doi:10.1051/0004-6361/202452433 , archivePrefix =. 2503.05466 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202452433

  61. [61]

    , keywords =

    PSR B1802-0 : a globular pulsar in an eccentric binary system. , keywords =. doi:10.1093/mnras/260.1.L7 , adsurl =

    work page doi:10.1093/mnras/260.1.l7

  62. [62]

    Milky Way globular clusters in gamma-rays: analyzing the dynamical formation of millisecond pulsars

    Milky Way globular clusters in -rays: analysing the dynamical formation of millisecond pulsars. , keywords =. doi:10.1093/mnras/stz898 , archivePrefix =. 1811.06957 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz898

  63. [63]

    J., Almaini, O., et al

    Millisecond pulsars around intermediate-mass black holes in globular clusters. , keywords =. doi:10.1111/j.1365-2966.2007.12160.x , archivePrefix =. 0706.1656 , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.12160.x 2007

  64. [64]

    A Highly Eccentric 3.9-Millisecond Binary Pulsar in the Globular Cluster NGC 6652

    A Highly Eccentric 3.9 Millisecond Binary Pulsar in the Globular Cluster NGC 6652. , keywords =. doi:10.1088/2041-8205/807/2/L23 , archivePrefix =. 1506.03367 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/807/2/l23 2041

  65. [65]

    Two New Black Widow Millisecond Pulsars In M28

    , keywords =. doi:10.3847/1538-4357/ac4744 , archivePrefix =. 2201.11238 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac4744

  66. [66]

    , keywords =

    Globular clusters in ORBIT: Complete dynamical characterisation of the Milky Way globular cluster population through updated orbital reconstruction. , keywords =. doi:10.1051/0004-6361/202556235 , archivePrefix =. 2512.06079 , primaryClass =

    work page doi:10.1051/0004-6361/202556235

  67. [67]

    A study of the light bending phenomenon under full general relativity for a pulsar in a binary with a Schwarzschild black hole

    A study of the light bending phenomenon under full general relativity for a pulsar in a binary with a Schwarzschild black hole. , keywords =. doi:10.1093/mnras/stad2147 , archivePrefix =. 2306.11431 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad2147

  68. [68]

    Nuovo Cimento B Serie , keywords =

    Higher-order relativistic periastron advances and binary pulsars. Nuovo Cimento B Serie , keywords =. doi:10.1007/BF02828697 , adsurl =

    work page doi:10.1007/bf02828697

  69. [69]

    Optical Detection of a Variable Millisecond Pulsar Companion in 47 Tucanae

    Optical Detection of a Variable Millisecond Pulsar Companion in 47 Tucanae. , keywords =. doi:10.1086/323122 , archivePrefix =. astro-ph/0107096 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/323122

  70. [70]

    Chandra X-Ray Observatory Observations of the Globular Cluster M71

    , keywords =. doi:10.1086/591899 , archivePrefix =. 0807.2404 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/591899

  71. [71]

    Birth and Evolution of Isolated Radio Pulsars

    Birth and Evolution of Isolated Radio Pulsars. , keywords =. doi:10.1086/501516 , archivePrefix =. astro-ph/0512585 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/501516

  72. [72]

    Deep Radio Imaging of Globular Clusters and the Cluster Pulsar Population

    Deep Radio Imaging of Globular Clusters and the Cluster Pulsar Population. , keywords =. doi:10.1086/308948 , archivePrefix =. astro-ph/9910436 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308948

  73. [73]

    Gravitational Waves and Intermediate-mass Black Hole Retention in Globular Clusters

    Gravitational Waves and Intermediate-mass Black Hole Retention in Globular Clusters. , keywords =. doi:10.3847/1538-4357/aab368 , archivePrefix =. 1711.00483 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aab368

  74. [74]

    The cluster Terzan 5 as a remnant of a primordial building block of the Galactic bulge

    The cluster Terzan 5 as a remnant of a primordial building block of the Galactic bulge. , keywords =. doi:10.1038/nature08581 , archivePrefix =. 0912.0192 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature08581

  75. [75]

    Refined Mass and Geometric Measurements of the High-Mass PSR J0740+6620

    Refined Mass and Geometric Measurements of the High-mass PSR J0740+6620. , keywords =. doi:10.3847/2041-8213/ac03b8 , archivePrefix =. 2104.00880 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ac03b8 2041

  76. [76]

    X-Ray Binaries and the Current Dynamical States of Galactic Globular Clusters

    X-Ray Binaries and the Current Dynamical States of Galactic Globular Clusters. , keywords =. doi:10.1086/527375 , archivePrefix =. 0710.4556 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/527375

  77. [77]

    , keywords =

    Further results from the timing of the millisecond pulsars in 47 Tucanae. , keywords =. doi:10.1046/j.1365-8711.2003.06392.x , adsurl =

    work page doi:10.1046/j.1365-8711.2003.06392.x 2003

  78. [78]

    Detection of ionized gas in the globular cluster 47 Tucanae

    Detection of Ionized Gas in the Globular Cluster 47 Tucanae. , keywords =. doi:10.1086/323248 , archivePrefix =. astro-ph/0107206 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/323248

  79. [79]

    and Prestwich, A

    Timing the millisecond pulsars in 47 Tucanae. , keywords =. doi:10.1046/j.1365-8711.2001.04493.x , archivePrefix =. astro-ph/0103372 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04493.x 2001

  80. [80]

    Fermi Detection of a Luminous Gamma-ray Pulsar in a Globular Cluster

    Fermi Detection of a Luminous -Ray Pulsar in a Globular Cluster. , keywords =. doi:10.1126/science.1207141 , archivePrefix =. 1111.3754 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1207141

Showing first 80 references.