Pith. sign in

REVIEW 3 major objections 7 minor 280 references

Reviewed by Pith at T0; open to challenge.

T0 means a machine referee read the full paper against a public rubric. The mark states how deep the mechanical check went, never who wrote it. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · glm-5.2

Lensed kilonovae from neutron star mergers detectable ~once per year

2026-07-09 19:40 UTC pith:NTXXIEKW

load-bearing objection Solid forward-modeling pipeline for lensed BNS multi-messenger rates; quantitative predictions are order-of-magnitude estimates with unquantified EOS and opacity systematics, plus a missing duty-cycle correction in Table 1. the 3 major comments →

arxiv 2607.07120 v1 pith:NTXXIEKW submitted 2026-07-08 astro-ph.HE astro-ph.GA

Prospect for Detection of Strongly Lensed Multi-messenger Signals of Binary Neutron Star Mergers

Zhiwei Chen , Youjun Lu , Changwen Zeng This is my paper
classification astro-ph.HE astro-ph.GA
keywords lensedafterglowsdetectkilonovaeeventsmergersapproximatelybands
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper estimates how often the various electromagnetic signals from binary neutron star mergers—short gamma-ray bursts, kilonovae, and afterglows—would be seen in gravitationally lensed form by next-generation gravitational-wave detectors and their electromagnetic follow-up telescopes. The central mechanism is a pointed observation strategy: rather than scanning the entire gravitational-wave localization region, astronomers would target pre-identified galaxy-scale lens candidates within that region, cross-matching the gravitational-wave trigger against existing lens catalogs. The paper finds that lensed kilonovae are the most promising signal, detectable at roughly half an event per year with a Roman-Space-Telescope-like infrared facility, while lensed short gamma-ray bursts remain rare even with substantially improved gamma-ray sensitivity, and lensed afterglows are detectable mainly in X-rays at a rate of perhaps one event every few years with a future facility like ATHENA. The rates depend on a population synthesis model for binary neutron star component masses and merger rate evolution, which sets the distribution of ejecta masses, jet energies, and thus the luminosities of the electromagnetic counterparts.

Core claim

The paper's central result is a set of detection-rate estimates for lensed electromagnetic counterparts of binary neutron star mergers, showing that kilonovae are the most accessible signal (approximately 0.45–0.55 detections per year in near-infrared bands with a pointed lens-targeting strategy), while sGRBs and afterglows are substantially harder—sGRBs requiring gamma-ray sensitivity more than ten times beyond current instruments for even one detection per decade, and afterglows being detectable primarily in X-rays at 0.5–5 events per decade. The pointed strategy targeting pre-identified galaxy-scale lens candidates yields an identifiable lensed-host fraction of 0.15–0.30, which the paper取

What carries the argument

The rate estimation chain runs from a binary population synthesis model (alpha10.kb_beta0.9) generating 10^7 mock BNS mergers with component masses and redshifts, through calibrated fits to numerical relativity simulations mapping those masses to ejecta masses and remnant disk masses, through a Blandford-Znajek jet-launching model setting sGRB and afterglow energies, through an elliptical power-law density lensing model (EPL with external shear) producing multiple images with magnification factors and time delays, to a Bayesian framework for identifying lensed host galaxies within gravitational-wave localization regions. Detection criteria combine gravitational-wave signal-to-noise ratios,电磁

Load-bearing premise

The entire rate estimation depends on a binary population synthesis model correctly predicting the distribution of neutron star masses, mass ratios, and merger rate evolution out to redshifts of about 2. If the true binary neutron star population at high redshift differs—for instance, having a different mass distribution or merger rate evolution—the predicted electromagnetic counterpart rates could shift by factors of several.

What would settle it

If next-generation gravitational-wave detectors observe that the binary neutron star mass distribution or merger rate density evolution at high redshift differs substantially from the alpha10.kb_beta0.9 model predictions, the ejecta mass and jet energy distributions—and thus the kilonova and afterglow luminosity functions—would shift, potentially changing the predicted lensed detection rates by factors of several in either direction.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If the predicted kilonova detection rate of ~0.5/yr holds, a decade of operation with CE+ET and an RST-like facility could accumulate 5–15 lensed kilonova events, enabling time-delay cosmography with gravitational-wave sources as independent distance indicators.
  • The pointed lens-candidate strategy could be validated even before CE/ET operations begin by testing it on simulated or real O4-era lensed GW candidates, measuring the fraction of lensed hosts recoverable with current survey depths.
  • If supramassive neutron star remnants inject additional energy into kilonovae (as the paper notes but does not model), the kilonova detection rates could increase by a factor of two or more, making the infrared channel even more dominant.
  • The rarity of lensed sGRB detections (~0.1/yr even with 10x Fermi-GBM sensitivity) implies that gamma-ray follow-up of lensed BNS events is not a viable primary detection channel and should be treated as a bonus rather than a baseline strategy.

Where Pith is reading between the lines

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

  • The pointed strategy's dependence on pre-existing lens catalogs means its effectiveness scales with survey completeness; Euclid, CSST, and Roman's wide-field lens surveys become enabling infrastructure for lensed multi-messenger astronomy, not just for their primary cosmology missions.
  • If the BNS mass distribution at high redshift differs systematically from the population synthesis model—say, due to metallicity-dependent evolution or a different channel contribution—the ejecta mass and jet energy distributions shift, and the kilonova rate could move by factors of several in either direction, making early high-redshift BNS detections critical for calibrating the model.
  • The dominance of double-image cases over triples and quadruples in the detection rates suggests that Einstein ring and cross configurations, while visually striking, contribute negligibly to the lensed multi-messenger event budget.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 7 minor

Summary. This manuscript estimates detection rates of strongly lensed electromagnetic counterparts (sGRBs, kilonovae, afterglows) associated with lensed binary neutron star (BNS) gravitational-wave events detectable by third-generation detectors (Cosmic Explorer and Einstein Telescope). The authors extend prior work (Ma et al. 2023) by using a binary population synthesis model to generate diverse BNS parameters rather than fixing all systems to GW170817-like values. Ejecta masses and jet energies are derived from component masses via fitted numerical-relation formulas, kilonova light curves are modeled with an anisotropic multi-component model, and afterglows are computed with AfterglowPy. A complementary pointed follow-up strategy targeting pre-identified galaxy-scale lens candidates is introduced. The main findings are: (1) lensed sGRBs are rare (~0.1/yr even with 10x Fermi-GBM sensitivity); (2) the identifiable lensed-host fraction is 0.15–0.30; (3) RST-like infrared facilities could detect lensed kilonovae at ~0.45–0.55/yr; (4) lensed afterglows are detectable mainly in X-rays with ATHENA (~0.5–5 events per decade). The methodology is internally consistent and validated against Colombo et al. (2022) and Yu et al. (2021).

Significance. The paper provides a timely and detailed forecast for lensed multi-messenger BNS science in the third-generation GW era. The use of a population synthesis model to sample BNS component masses—rather than assuming all systems resemble GW170817—is a genuine improvement over Ma et al. (2023) and makes the predicted kilonova and afterglow luminosity functions more representative. The pointed follow-up strategy targeting pre-identified lens candidates is a practical and well-motivated complement to wide-field ToO searches. The falsifiable, quantitative rate predictions for specific telescope/detector combinations (Table 1, Figures 4 and 8) are useful for observational planning. The validation against independent published rates (Colombo et al. 2022; Yu et al. 2021) lends credibility to the pipeline.

major comments (3)
  1. Section 2.1 discusses a duty-cycle correction of ~20–30% for GW detector downtime but this correction does not appear to be applied to the rates in Table 1. The note to Table 1 lists duty cycle as an 'additional uncertainty' rather than a correction already incorporated. If the quoted rates in Table 1 and the abstract do not include this factor, they are systematically overestimated by ~20–30%. The authors should clarify whether the duty-cycle correction is included in all quoted rates, and if not, either apply it or state explicitly that rates are upper limits assuming 100% duty cycle.
  2. Section 2.2 and Appendix A.1: The kilonova luminosity function depends on ejecta masses computed via the Krüger & Foucart (2020) fits (Eqs. A1–A3), which require NS compactness derived from the SLy EOS (M_TOV = 2.06 M⊙). This is a single EOS choice. Alternative EOSs (e.g., APR4, DD2) would yield different compactness for the same component masses, shifting ejecta masses and thus f_KN and the final detection rates. The paper does not quantify this sensitivity. The authors should at minimum provide an estimate of how much f_KN or the kilonova detection rate changes under a different EOS choice, or discuss the range of uncertainty this introduces.
  3. Section 2.2: The opacity and energy normalization parameters (κ_low = 44.7, κ_high = 0.43, κ_wind = 33.5, κ_vis = 47.8, ε₀ = 183.4×10¹⁸) are fixed to GW170817-fitted values and assumed universal across the BNS population. Given that the authors themselves note GW170817 'likely ranks among the most luminous kilonovae,' fixing these parameters to GW170817 may bias the luminosity function. The authors should discuss whether these parameters are expected to vary with ejecta composition (which depends on mass ratio and remnant lifetime) and how sensitive the final rates are to this assumption.
minor comments (7)
  1. Section 2.2: The text lists 'κ_low = 44.7 cm²/g' and then 'κ_low = 0.43 cm²/g' for high-elevation opacity. The second should be κ_high. This is a typo.
  2. Figure 1 caption: The x-axis label reads 'mF158' but the figure shows distributions for three bands (F106, F158, F213). The label should be generic (e.g., 'm_AB') or the caption should clarify that the x-axis applies to all three bands.
  3. Section 2.3, Eq. (12): The variable 'a' is defined as a(θ, θ_v) but the subscript notation is inconsistent with Eq. (13) where 'a' appears without arguments. Minor notational cleanup needed.
  4. Table 1: The 'Relative fraction' column header could be more explicit (e.g., 'Lensed fraction among all detectable lensed BNS GW events'). The current phrasing is slightly ambiguous.
  5. Section 4.5: The Vega-to-AB conversion (Eq. 18) uses 1090 Jy as the Vega flux in F158. A reference or derivation for this zero-point value would be helpful for reproducibility.
  6. Section 2.4: The 10-hour response time is justified but the statement that a 1-hour response would enhance rates by a factor of ~2–3 is stated without derivation. A brief justification or reference would strengthen this claim.
  7. The abstract states rates as '~0.45^{+0.81}_{-0.34}' etc. The large asymmetric error bars (upper errors nearly 2x the central value) suggest a highly skewed posterior from the merger rate uncertainty. A brief note in the abstract or at first mention in Section 4.4 explaining the source of this asymmetry would aid interpretation.

Circularity Check

0 steps flagged

No significant circularity; forward-modeling pipeline with external calibrations throughout

full rationale

The paper is a forward-modeling prediction study. The detection rates are computed by propagating a mock BNS population (from Chu et al. 2022, rescaled to GWTC-4) through ejecta-mass fitting formulas (Krüger & Foucart 2020; Dietrich & Ujevic 2017), kilonova light-curve models calibrated to AT2017gfo (Breschi et al. 2021; Villar et al. 2017), afterglow models fitted to GW170817 data (Makhathini et al. 2021), and lensing magnification from an EPL profile with SLACS-survey parameters (Koopmans et al. 2009). No step feeds the target detection rate back into the inputs. The self-citations (Chen et al. 2022b for the host-galaxy Bayesian formalism, Chen et al. 2025a/b for discussion points) are not load-bearing: Eq. 15 is standard Bayes' theorem, and the host identification criteria come from Collett (2015). The consistency check in Section 2.4 validates the afterglow pipeline against Colombo et al. (2022) rates, providing an external benchmark. The systematic uncertainties flagged by the reader (single EOS choice, GW170817-fixed opacities, population model evolution) are legitimate correctness/modeling risks but do not constitute circularity — they are external assumptions with stated limitations, not definitions that make the output equivalent to the input by construction.

Axiom & Free-Parameter Ledger

7 free parameters · 5 axioms · 0 invented entities

No new physical entities, particles, or forces are introduced. The paper combines existing models (population synthesis, lensing, kilonova/afterglow radiation) in a forward-modeling pipeline. The free parameters are either fitted to GW170817/AT2017gfo data or taken from external observational constraints.

free parameters (7)
  • R0 (local BNS merger rate density) = 89 Gpc^-3 yr^-1
    Rescaled from GWTC-4 observation; central value from LIGO-Virgo-KAGRA 2025. Large uncertainty (+159/-67) propagated to final rates.
  • eta_gamma (jet-to-radiation conversion efficiency) = uniform in [0.1, 0.3]
    Section A.2; chosen to match GW170817 but authors note observed sGRB values range from 0.0066 to 0.97, introducing factor-of-5+ uncertainty in sGRB/afterglow rates.
  • ISM parameters (n_e,0, p, epsilon_e, epsilon_B) = fitted to GW170817 afterglow
    Appendix B; Table 2 gives posterior values from emcee fitting of GW170817 multi-band data. Assumed universal across all BNS mergers.
  • kappa_low, kappa_high, kappa_wind, kappa_vis (opacities) = 44.7, 0.43, 33.5, 47.8 cm^2/g
    Section 2.2; fitted to AT2017gfo light curves from Villar et al. 2017 and assumed constant for all mock mergers.
  • epsilon_0 (r-process energy normalization) = 183.4e18 erg/g/s
    Section 2.2; fixed from AT2017gfo fitting, assumed universal.
  • f_Host (identifiable lensed host fraction) = 0.15-0.30
    Section 4.2; derived from P(H|GW) plateau values and assumed sky-availability factor of 0.5. Linearly scalable for shallower surveys.
  • 10-hour response time = 10 hours
    Section 2.4; adopted as representative baseline from O3/O4 latency observations. Authors note 1-hour response would enhance rates by factor ~2-3.
axioms (5)
  • domain assumption The alpha10.kb_beta0.9 binary population synthesis model accurately predicts BNS mass distribution and merger rate evolution out to z~5
    Section 2; the entire mock BNS population is generated from this model. The model is calibrated to Galactic BNS observations and local GW rates but its high-redshift predictions are unverified.
  • domain assumption The SLy equation of state (M_TOV = 2.06 M_sun) correctly describes neutron star structure for computing compactness and ejecta masses
    Section 2; NS radii r1, r2 are computed from SLy EOS, which directly affects ejecta mass via Eq. A1-A3. Different EOS choices would change the mass-radius relation and thus the kilonova luminosities.
  • domain assumption Only HMNS/BH remnants can launch BZ jets; SMNS remnants cannot
    Section A.2; the condition m_rem > 1.2*M_TOV determines whether a jet is produced. Authors note in Section 5 that recent simulations (Bamber et al. 2024) show SMNS remnants can also form jets, which would increase afterglow rates.
  • domain assumption Galaxy strong lensing is dominated by elliptical early-type galaxies modeled as EPL+external shear
    Section 2; late-type galaxy lensing is noted as potentially contributing but is excluded. The EPL parameters (lambda mean=2, scatter=0.2) are from SLACS survey.
  • domain assumption The BNS merger rate traces stellar mass in host galaxies
    Section 2.5; mock host galaxies are populated with mergers proportional to stellar mass M*, reflecting massive-binary evolution origin.

pith-pipeline@v1.1.0-glm · 33227 in / 3439 out tokens · 409823 ms · 2026-07-09T19:40:50.421419+00:00 · methodology

0 comments
read the original abstract

The gravitational lensing of multi-messenger signals from binary neutron star mergers (BNSs), including gravitational waves (GWs), short Gamma-Ray bursts (sGRBs), kilonovae, and afterglows, can serve as a unique probe to constrain the mass of the graviton and cosmological parameters. In this paper, we estimate the detection rates of lensed electromagnetic counterparts associated with lensed BNS GW events detected by Cosmic Explorer and Einstein Telescope. For kilonovae and afterglows, we further consider a complementary pointed follow-up strategy targeting pre-identified galaxy-scale lens candidates within the GW localization region. By utilizing both numerical and observational constraints on BNS mergers, we find that: (1) Future $\gamma$-ray telescopes, even with a sensitivity more than ten times better than that of Fermi-GBM, may only detect lensed sGRB prompt emission at a rate $\sim 0.1$ yr$^{-1}$, corresponding to $\sim 2\times 10^{-3}$ of detectable lensed BNS GW events. (2) For the known-lens pointed strategy, the identifiable lensed-host fraction is approximately $0.15-0.30$ for the fiducial deep lens-catalog case considered, suggesting a possible gain in per-lens sensitivity for faint kilonovae and afterglows. (3) An RST-like near-infrared facility could detect lensed kilonovae at rates of approximately $\sim 0.45^{+0.81}_{-0.34}$, $0.55^{+0.98}_{-0.41}$, and $0.078^{+0.139}_{-0.059}$ yr$^{-1}$ in the F106, F158, and F213 bands, respectively. (4) Lensed afterglows remain difficult to detect in the optical and radio bands, while ATHENA-like X-ray observations may detect $0.5-5$ events over ten years.

Figures

Figures reproduced from arXiv: 2607.07120 by Changwen Zeng, Youjun Lu, Zhiwei Chen.

Figure 1
Figure 1. Figure 1: The normalized probability distribution of the apparent magnitudes for the kilonova signals from the mock BNS mergers, calculated one day post-merger over the red￾shift range of [0, 5), if observed by F106 (blue), F158 (or￾ange), and F213 (green) bands of RST, respectively. where F peak ν denotes the kilonova’s flux in the observer frame after applying the K-correction (by redshifting the spectral models a… view at source ↗
Figure 3
Figure 3. Figure 3: The normalized distribution of the peak flux of afterglow signals after 10 h within the redshift range of [0, 5), in the infrared F158 (left), radio 8.4 GHz (mid), and X-ray 5 keV (right) bands, respectively. The deeper color region in each panel shows the population below the detection threshold of RST, Chandra and SKA respectively. where “H” and “GW” denote host galaxies with iden￾tifiable lensing images… view at source ↗
Figure 4
Figure 4. Figure 4: The total joint detection rate of lensed GW and sGRB signals per year by third generation GW detectors and Fermi-GBM. The blue, orange and green solid lines show the results of ET, CE and their network respectively. In the top panel, the detection threshold for sGRBs is fixed as Fγ,0 = 2×10−7 erg cm−2 , which is the detection threshold of Fermi￾GBM. In the bottom panel, the detection S/N threshold of GW si… view at source ↗
Figure 5
Figure 5. Figure 5: Steps for searching lensed multi-messenger sig￾nals of BNS mergers. In this paper, the joint detection rate is estimated us￾ing the search strategy shown in [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: The probability of a lensed BNS GW event that has lensing signatures of its host galaxy (the conditional probability P(H|GW)) identifiable by a (survey) telescope with the limiting magnitude of mlim for different third gen￾eration GW detectors and their network. its host galaxy (the conditional probability P(H|GW)) identifiable by a survey is related to the physical prop￾erties of the BNS merger and its ho… view at source ↗
Figure 7
Figure 7. Figure 7: The dependence of the fraction of those lensed EM counterparts can be observed, i.e., fKN and fAG for kilonova (top) and afterglow (bottom) respectively. In the top panels, the left, mid and right panel represent the results of fKN for F106, F158, F213 band of RST, while in the bottom panels, the left, mid and right panel represent fAG for F158, radio at 8.4 GHz and X-ray at 5KeV, respectively. In each pan… view at source ↗
Figure 8
Figure 8. Figure 8: The total joint detection rate per year of the lensed GW associated with detectable lensed kilonova (top panels) and afterglow signals (bottom panels), i.e., N˙ ℓ GW+KN and N˙ ℓ GW+AG. In the top panels, the left, mid and right panel represent the results of N˙ ℓ GW+KN for F106, F158, F213 band of RST, while in the bottom panels, the left, mid and right panel represent N˙ ℓ GW+AG for F158, radio at 8.4GHz … view at source ↗
Figure 9
Figure 9. Figure 9: Multiband light curves of afterglow of GW170817 and the best model fit. The green, blue and purple symbols with error bar represent the data points transferred into X-ray (5 keV), optical (590 nm) and radio (6 GHz) band. The corresponding solid lines show the best-fit results [PITH_FULL_IMAGE:figures/full_fig_p021_9.png] view at source ↗

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

280 extracted references · 280 canonical work pages · 208 internal anchors

  1. [1]

    The Swift X-ray Telescope

    The Swift X-Ray Telescope. , keywords =. doi:10.1007/s11214-005-5097-2 , archivePrefix =. astro-ph/0508071 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-005-5097-2

  2. [2]

    International Journal of Modern Physics D , keywords =

    The SVOM mission. International Journal of Modern Physics D , keywords =. doi:10.1142/S0218271822300087 , archivePrefix =. 2203.10962 , primaryClass =

    work page doi:10.1142/s0218271822300087

  3. [3]

    Handbook of X-ray and Gamma-ray Astrophysics , year = 2022, editor =

    The Einstein Probe Mission. Handbook of X-ray and Gamma-ray Astrophysics , year = 2022, editor =. doi:10.1007/978-981-16-4544-0_151-1 , adsurl =

    work page doi:10.1007/978-981-16-4544-0_151-1 2022

  4. [4]

    Light Curves of the Neutron Star Merger GW170817/SSS17a: Implications for R-Process Nucleosynthesis

    Light curves of the neutron star merger GW170817/SSS17a: Implications for r-process nucleosynthesis. Science , keywords =. doi:10.1126/science.aaq0049 , archivePrefix =. 1710.05443 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.aaq0049

  5. [5]

    The Unprecedented Properties of the First Electromagnetic Counterpart to a Gravitational Wave Source

    The Unprecedented Properties of the First Electromagnetic Counterpart to a Gravitational-wave Source. , keywords =. doi:10.3847/2041-8213/aa905e , archivePrefix =. 1710.05440 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aa905e 2041

  6. [6]

    Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report

    Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report. arXiv e-prints , keywords =. doi:10.48550/arXiv.1503.03757 , archivePrefix =. 1503.03757 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1503.03757 2015

  7. [7]

    GWTC-4.0: Population Properties of Merging Compact Binaries

    GWTC-4.0: Population Properties of Merging Compact Binaries. arXiv e-prints , keywords =. doi:10.48550/arXiv.2508.18083 , archivePrefix =. 2508.18083 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2508.18083

  8. [8]

    Detection of the Gravitational Lens Magnifying a Type Ia Supernova

    Detection of the Gravitational Lens Magnifying a Type Ia Supernova. Science , keywords =. doi:10.1126/science.1250903 , archivePrefix =. 1404.6014 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.1250903

  9. [9]

    iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova

    iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova. Science , keywords =. doi:10.1126/science.aal2729 , archivePrefix =. 1611.00014 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.aal2729

  10. [10]

    On the detection and precise localisation of merging black holes events through strong gravitational lensing

    On the detection and precise localization of merging black holes events through strong gravitational lensing. , keywords =. doi:10.1093/mnras/stae1023 , archivePrefix =. 2204.08732 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stae1023

  11. [11]

    Philosophical Transactions of the Royal Society of London Series A , keywords =

    Finding black holes: an unconventional multi-messenger. Philosophical Transactions of the Royal Society of London Series A , keywords =. doi:10.1098/rsta.2024.0152 , archivePrefix =. 2406.14257 , primaryClass =

    work page doi:10.1098/rsta.2024.0152 2024

  12. [12]

    Astroparticle Physics , keywords =

    Enabling kilonova science with Nancy Grace Roman Space Telescope. Astroparticle Physics , keywords =. doi:10.1016/j.astropartphys.2023.102904 , archivePrefix =. 2307.09511 , primaryClass =

    work page doi:10.1016/j.astropartphys.2023.102904 2023

  13. [13]

    The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VII. Properties of the Host Galaxy and Constraints on the Merger Timescale. , keywords =. doi:10.3847/2041-8213/aa9055 , archivePrefix =. 1710.05458 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aa9055 2041

  14. [14]

    Rubin ToO 2024: Envisioning the Vera C. Rubin Observatory LSST Target of Opportunity program

    Rubin ToO 2024: Envisioning the Vera C. Rubin Observatory LSST Target of Opportunity program. arXiv e-prints , keywords =. doi:10.48550/arXiv.2411.04793 , archivePrefix =. 2411.04793 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2411.04793 2024

  15. [15]

    Science objectives of the Einstein Probe mission

    Science objectives of the Einstein Probe mission. Science China Physics, Mechanics, and Astronomy , keywords =. doi:10.1007/s11433-024-2600-3 , archivePrefix =. 2501.07362 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11433-024-2600-3

  16. [16]

    The Gravitational-wave Optical Transient Observer (GOTO)

    The Gravitational-wave Optical Transient Observer (GOTO). Ground-based and Airborne Telescopes X , year = 2024, editor =. doi:10.1117/12.3018305 , archivePrefix =. 2407.17176 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1117/12.3018305 2024

  17. [17]

    Searching for gravitational wave optical counterparts with the Zwicky Transient Facility: summary of O4a

    Searching for Gravitational Wave Optical Counterparts with the Zwicky Transient Facility: Summary of O4a. , keywords =. doi:10.1088/1538-3873/ad8265 , archivePrefix =. 2405.12403 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/ad8265

  18. [18]

    Identifying strongly lensed gravitational wave signals from binary black hole mergers

    Identifying strongly lensed gravitational wave signals from binary black hole mergers. arXiv e-prints , keywords =. doi:10.48550/arXiv.1807.07062 , archivePrefix =. 1807.07062 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1807.07062

  19. [19]

    Searching for Electromagnetic Counterparts to Gravitational-wave Merger Events with the Prototype Gravitational-wave Optical Transient Observer (GOTO-4)

    Searching for electromagnetic counterparts to gravitational-wave merger events with the prototype Gravitational-Wave Optical Transient Observer (GOTO-4). , keywords =. doi:10.1093/mnras/staa1845 , archivePrefix =. 2004.00025 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa1845 2004

  20. [20]

    Lensing or luck? False alarm probabilities for gravitational lensing of gravitational waves

    Lensing or luck? False alarm probabilities for gravitational lensing of gravitational waves. , keywords =. doi:10.1103/PhysRevD.107.063023 , archivePrefix =. 2201.04619 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.107.063023

  21. [21]

    Eccentric Black Hole Mergers in Active Galactic Nuclei

    Eccentric Black Hole Mergers in Active Galactic Nuclei. , keywords =. doi:10.3847/2041-8213/abd4d3 , archivePrefix =. 2010.10526 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/abd4d3 2041

  22. [22]

    The mass spectrum of compact remnants from the PARSEC stellar evolution tracks

    The mass spectrum of compact remnants from the PARSEC stellar evolution tracks. , keywords =. doi:10.1093/mnras/stv1161 , archivePrefix =. 1505.05201 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1161

  23. [23]

    arXiv e-prints , keywords =

    Blackhole Mergers Through Evection Resonances. arXiv e-prints , keywords =

    work page

  24. [24]

    , year = 2022, month = mar, volume =

    AGN as potential factories for eccentric black hole mergers. , year = 2022, month = mar, volume =. doi:10.1038/s41586-021-04333-1 , adsurl =

    work page doi:10.1038/s41586-021-04333-1 2022

  25. [25]

    The Eccentric and Accelerating Stellar Binary Black Hole Mergers in Galactic Nuclei: Observing in Ground and Space Gravitational Wave Observatories

    The Eccentric and Accelerating Stellar Binary Black Hole Mergers in Galactic Nuclei: Observing in Ground and Space Gravitational-wave Observatories. , keywords =. doi:10.3847/1538-4357/ac2c07 , archivePrefix =. 2109.14842 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac2c07

  26. [26]

    Gravitational-wave merging events from the dynamics of stellar mass binary black holes around the massive black hole in a galactic nucleus

    Gravitational-wave Merging Events from the Dynamics of Stellar-mass Binary Black Holes around the Massive Black Hole in a Galactic Nucleus. , keywords =. doi:10.3847/1538-4357/ab1b28 , archivePrefix =. 1903.02685 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1b28 1903

  27. [27]

    Precision cosmology from future lensed gravitational wave and electromagnetic signals

    Precision cosmology from future lensed gravitational wave and electromagnetic signals. Nature Communications , keywords =. doi:10.1038/s41467-017-01152-9 , archivePrefix =. 1703.04151 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41467-017-01152-9

  28. [28]

    H0LiCOW IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology

    H0LiCOW - IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology. , keywords =. doi:10.1093/mnras/stw3077 , archivePrefix =. 1607.01403 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw3077

  29. [29]

    Constraining cosmological parameters in FLRW metric with lensed GW+EM signals

    Constraining Cosmological Parameters in the FLRW Metric with Lensed GW+EM Signals. , keywords =. doi:10.3847/1538-4357/ab037e , archivePrefix =. 1901.10638 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab037e 1901

  30. [30]

    Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology

    Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology. , keywords =. doi:10.1103/PhysRevD.97.064031 , archivePrefix =. 1710.05325 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.97.064031

  31. [31]

    doi:10.1007/978-3-662-03758-4 , adsurl =

    Gravitational Lenses. doi:10.1007/978-3-662-03758-4 , adsurl =

    work page doi:10.1007/978-3-662-03758-4

  32. [33]

    , keywords =

    Isothermal elliptical gravitational lens models. , keywords =

    work page

  33. [34]

    Strong lensing as a giant telescope to localize the host galaxy of gravitational wave event

    Strong lensing as a giant telescope to localize the host galaxy of gravitational wave event. , keywords =. doi:10.1093/mnras/staa1952 , archivePrefix =. 2007.00828 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa1952 2007

  34. [35]

    Gravitational lensing of gravitational waves: A statistical perspective

    Gravitational lensing of gravitational waves: a statistical perspective. , keywords =. doi:10.1093/mnras/sty411 , archivePrefix =. 1802.05089 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty411

  35. [36]

    GW150914: Implications for the stochastic gravitational wave background from binary black holes

    GW150914: Implications for the Stochastic Gravitational-Wave Background from Binary Black Holes. , keywords =. doi:10.1103/PhysRevLett.116.131102 , archivePrefix =. 1602.03847 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.116.131102

  36. [37]

    Survey of Gravitationally lensed Objects in HSC Imaging (SuGOHI) -- VII. Discovery and Confirmation of Three Strongly Lensed Quasars

    Survey of Gravitationally Lensed Objects in HSC Imaging (SuGOHI) - VII. Discovery and confirmation of three strongly lensed quasars. , keywords =. doi:10.1093/mnras/stab145 , archivePrefix =. 2006.16584 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab145 2006

  37. [38]

    Detecting Lensing-Induced Diffraction in Astrophysical Gravitational Waves

    Detecting lensing-induced diffraction in astrophysical gravitational waves. , keywords =. doi:10.1103/PhysRevD.98.104029 , archivePrefix =. 1810.00003 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.98.104029

  38. [39]

    , year = 1998, month = feb, volume =

    Gravitational Lensing of Gravitational Waves from Inspiraling Binaries by a Point Mass Lens. , year = 1998, month = feb, volume =. doi:10.1103/PhysRevLett.80.1138 , adsurl =

    work page doi:10.1103/physrevlett.80.1138 1998

  39. [40]

    Gravitational Lensing of Gravitational Waves from Merging Neutron Star Binaries

    Gravitational Lensing of Gravitational Waves from Merging Neutron Star Binaries. , keywords =. doi:10.1103/PhysRevLett.77.2875 , archivePrefix =. astro-ph/9605140 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.77.2875

  40. [41]

    Strong gravitational lensing of gravitational waves from double compact binaries - perspectives for the Einstein Telescope

    Strong gravitational lensing of gravitational waves from double compact binaries perspectives for the Einstein Telescope. JCAP , keywords =. doi:10.1088/1475-7516/2014/10/080 , archivePrefix =. 1409.8360 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2014/10/080 2014

  41. [42]

    GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

    GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs. Physical Review X , keywords =. doi:10.1103/PhysRevX.9.031040 , archivePrefix =. 1811.12907 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevx.9.031040

  42. [43]

    arXiv e-prints , keywords =

    GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run. arXiv e-prints , keywords =

    work page

  43. [44]

    Candidate Electromagnetic Counterpart to the Binary Black Hole Merger Gravitational Wave Event S190521g

    Candidate Electromagnetic Counterpart to the Binary Black Hole Merger Gravitational-Wave Event S190521g ^ *. , keywords =. doi:10.1103/PhysRevLett.124.251102 , archivePrefix =. 2006.14122 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.124.251102 2006

  44. [45]

    Multi-messenger Observations of a Binary Neutron Star Merger

    Multi-messenger Observations of a Binary Neutron Star Merger. , keywords =. doi:10.3847/2041-8213/aa91c9 , archivePrefix =. 1710.05833 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aa91c9 2041

  45. [46]

    , year = 1995, month = may, volume =

    Book Review: Gravitational lenses / Springer-Verlag, 1993. , year = 1995, month = may, volume =

    work page 1993

  46. [47]

    A concise reference to (projected) Sersic R^{1/n} quantities, including Concentration, Profile Slopes, Petrosian indices, and Kron Magnitudes

    A Concise Reference to (Projected) S \'e rsic R ^ 1/n Quantities, Including Concentration, Profile Slopes, Petrosian Indices, and Kron Magnitudes. PASP , keywords =. doi:10.1071/AS05001 , archivePrefix =. astro-ph/0503176 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1071/as05001

  47. [49]

    and Akrami, Y

    Aghanim, N. and Akrami, Y. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Ballardini, M. and Banday, A. J. and Barreiro, R. B. and Bartolo, N. and et al. , year=. Planck 2018 results , volume=. doi:10.1051/0004-6361/201833910 , journal=

    work page doi:10.1051/0004-6361/201833910 2018

  48. [50]

    Dynamical Formation of the GW150914 Binary Black Hole

    Dynamical Formation of the GW150914 Binary Black Hole. , keywords =. doi:10.3847/2041-8205/824/1/L8 , archivePrefix =. 1604.04254 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8205/824/1/l8 2041

  49. [51]

    The first gravitational-wave source from the isolated evolution of two 40-100 Msun stars

    The first gravitational-wave source from the isolated evolution of two stars in the 40-100 solar mass range. , keywords =. doi:10.1038/nature18322 , archivePrefix =. 1602.04531 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature18322

  50. [52]

    R., et al

    Intermediate mass black holes in AGN discs - I. Production and growth. , keywords =. doi:10.1111/j.1365-2966.2012.21486.x , archivePrefix =. 1206.2309 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21486.x 2012

  51. [53]

    Nauchnye Informatsii , year = 1973, month = jan, volume =

    Evolution of massive close binaries. Nauchnye Informatsii , year = 1973, month = jan, volume =

    work page 1973

  52. [54]

    , keywords =

    Erratum: The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks. , keywords =. doi:10.1093/mnras/stz892 , adsurl =

    work page doi:10.1093/mnras/stz892

  53. [55]

    The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks

    The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks. , keywords =. doi:10.1093/mnras/sty1999 , archivePrefix =. 1806.00001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1999

  54. [56]

    , keywords =

    Primordial black holes in globular clusters. , keywords =. doi:10.1038/364423a0 , adsurl =

    work page doi:10.1038/364423a0

  55. [57]

    Black hole mergers in the universe

    Black Hole Mergers in the Universe. , keywords =. doi:10.1086/312422 , archivePrefix =. astro-ph/9910061 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/312422

  56. [58]

    Rapid and Bright Stellar-mass Binary Black Hole Mergers in Active Galactic Nuclei

    Rapid and Bright Stellar-mass Binary Black Hole Mergers in Active Galactic Nuclei. , keywords =. doi:10.3847/1538-4357/835/2/165 , archivePrefix =. 1602.03831 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/835/2/165

  57. [59]

    Assisted Inspirals of Stellar Mass Black Holes Embedded in AGN Disks: Solving the "Final AU Problem"

    Assisted inspirals of stellar mass black holes embedded in AGN discs: solving the `final au problem'. , keywords =. doi:10.1093/mnras/stw2260 , archivePrefix =. 1602.04226 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2260

  58. [60]

    Systematic errors in strong gravitational lensing reconstructions, a numerical simulation perspective , volume=

    Enzi, Wolfgang and Vegetti, Simona and Despali, Giulia and Hsueh, Jen-Wei and Benton Metcalf, R , year=. Systematic errors in strong gravitational lensing reconstructions, a numerical simulation perspective , volume=. , publisher=. doi:10.1093/mnras/staa1224 , number=

    work page doi:10.1093/mnras/staa1224

  59. [61]

    2021 , eprint=

    Lensing magnification: gravitational waves from coalescing stellar-mass binary black holes , author=. 2021 , eprint=

    work page 2021

  60. [62]

    Redshifts and lens profile for the double quasar QJ 0158-4325

    Redshifts and lens profile for the double quasar QJ 0158-4325. , keywords =. doi:10.1051/0004-6361:200810277 , archivePrefix =. 0812.1308 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:200810277

  61. [63]

    The Sloan Lens ACS Survey. I. A Large Spectroscopically Selected Sample of Massive Early-Type Lens Galaxies. , keywords =. doi:10.1086/498884 , archivePrefix =. astro-ph/0511453 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/498884

  62. [64]

    SDSS J1640+1932: a spectacular galaxy-quasar strong lens system

    SDSS J1640+1932: a spectacular galaxy-quasar strong lens system. , keywords =. doi:10.1093/mnras/stx733 , archivePrefix =. 1703.07495 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx733 1932

  63. [65]

    HOLISMOKES. IV. Efficient mass modeling of strong lenses through deep learning. , keywords =. doi:10.1051/0004-6361/202039574 , archivePrefix =. 2010.00602 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039574 2010

  64. [66]

    Discovery of two Einstein crosses from massive post--blue nugget galaxies at z>1 in KiDS

    Discovery of Two Einstein Crosses from Massive Post-blue Nugget Galaxies at z > 1 in KiDS. , keywords =. doi:10.3847/2041-8213/abc95b , archivePrefix =. 2011.09150 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/abc95b 2041

  65. [67]

    Night-time measurements of astronomical seeing at Dome A in Antarctica

    Night-time measurements of astronomical seeing at Dome A in Antarctica. , keywords =. doi:10.1038/s41586-020-2489-0 , archivePrefix =. 2007.15365 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-020-2489-0 2007

  66. [68]

    Internal and Collective Properties of Galaxies in the Sloan Digital Sky Survey

    Internal and Collective Properties of Galaxies in the Sloan Digital Sky Survey. , keywords =. doi:10.1086/511060 , archivePrefix =. astro-ph/0611607 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/511060

  67. [69]

    Strong gravitational lensing of gravitational waves in Einstein Telescope

    Pi\'orkowska, Aleksandra and Biesiada, Marek and Zhu, Zong-Hong. Strong gravitational lensing of gravitational waves in Einstein Telescope. JCAP. 2013. doi:10.1088/1475-7516/2013/10/022. arXiv:1309.5731

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2013/10/022 2013

  68. [70]

    Dynamics of the NGC 4636 Globular Cluster System - An extremely dark matter dominated galaxy?

    Schuberth, Ylva and Richtler, T. and Dirsch, B. and Hilker, M. and Larsen, S. S. and Kissler-Patig, M. and Mebold, U. Dynamics of the NGC 4636 Globular Cluster System: An extremely dark matter dominated galaxy?. Astron. Astrophys. 2006. doi:10.1051/0004-6361:20053134. arXiv:astro-ph/0604309

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20053134 2006

  69. [71]

    R., et al

    A deep, wide-field study of Holmberg II with Suprime-Cam: evidence for ram pressure stripping. , keywords =. doi:10.1111/j.1365-2966.2012.22025.x , archivePrefix =. 1208.4808 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.22025.x 2012

  70. [72]

    Luminosity functions of globular clusters in five nearby spiral galaxies using HST/ACS images

    Luminosity functions of globular clusters in five nearby spiral galaxies using HST/ACS images. , keywords =. doi:10.1093/mnras/stab2890 , archivePrefix =. 2110.00703 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab2890

  71. [75]

    Host galaxy properties of mergers of stellar binary black holes and their implications for advanced LIGO gravitational wave sources , volume=

    Cao, Liang and Lu, Youjun and Zhao, Yuetong , year=. Host galaxy properties of mergers of stellar binary black holes and their implications for advanced LIGO gravitational wave sources , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1093/mnras/stx3087 , number=

    work page doi:10.1093/mnras/stx3087

  72. [76]

    Stochastic Gravitational Wave Background and Eccentric Stellar Compact Binaries

    Stochastic gravitational wave background and eccentric stellar compact binaries. , keywords =. doi:10.1093/mnras/staa2707 , archivePrefix =. 2009.01436 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa2707 2009

  73. [77]

    Localizing merging black holes with sub-arcsecond precision using gravitational-wave lensing

    Localizing merging black holes with sub-arcsecond precision using gravitational-wave lensing. , keywords =. doi:10.1093/mnras/staa2577 , archivePrefix =. 2004.13811 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa2577 2004

  74. [78]

    Event rate predictions of strongly lensed gravitational waves with detector networks and more realistic templates

    Event rate predictions of strongly lensed gravitational waves with detector networks and more realistic templates. , keywords =. doi:10.1093/mnras/stab3298 , archivePrefix =. 2105.07011 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab3298

  75. [79]

    Resolving the Stellar Outskirts of M81: Evidence for a Faint, Extended Structural Component

    Resolving the Stellar Outskirts of M81: Evidence for a Faint, Extended Structural Component. , keywords =. doi:10.1088/0004-6256/138/5/1469 , archivePrefix =. 0909.1430 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/138/5/1469

  76. [80]

    The ACS Virgo Cluster Survey. XV. The Formation Efficiencies of Globular Clusters in Early-Type Galaxies: The Effects of Mass and Environment. , keywords =. doi:10.1086/587951 , archivePrefix =. 0803.0330 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/587951

  77. [81]

    Diffuse Tidal Structures in the Halos of Virgo Ellipticals

    Diffuse Tidal Structures in the Halos of Virgo Ellipticals. , keywords =. doi:10.1088/0004-637X/715/2/972 , archivePrefix =. 1004.1473 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/715/2/972

  78. [82]

    First results from the Dragonfly Telephoto Array: the apparent lack of a stellar halo in the massive spiral galaxy M101

    First Results from the Dragonfly Telephoto Array: The Apparent Lack of a Stellar Halo in the Massive Spiral Galaxy M101. , keywords =. doi:10.1088/2041-8205/782/2/L24 , archivePrefix =. 1401.5467 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/782/2/l24 2041

  79. [83]

    An Atlas of Galaxy Spectral Energy Distributions from the Ultraviolet to the Mid-Infrared

    An Atlas of Galaxy Spectral Energy Distributions from the Ultraviolet to the Mid-infrared. , keywords =. doi:10.1088/0067-0049/212/2/18 , archivePrefix =. 1312.3029 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/212/2/18

  80. [84]

    Introducing the LBT Imaging of Galactic Halos and Tidal Structures (LIGHTS) survey. A preview of the low surface brightness Universe to be unveiled by LSST

    Introducing the LBT Imaging of Galactic Halos and Tidal Structures (LIGHTS) survey. A preview of the low surface brightness Universe to be unveiled by LSST. , keywords =. doi:10.1051/0004-6361/202141603 , archivePrefix =. 2109.07478 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202141603

Showing first 80 references.