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REVIEW 4 major objections 3 minor 1 cited by

Spectroscopic ages for 4 million main-sequence dwarf stars from LAMOST DR10 estimated with data-driven approach

T0 review · 4 major / 3 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read This paper claims that ages of cool main-sequence dwarf stars can be estimated from single low-resolution LAMOST spectra with 10–25 percent precision, producing a public catalog of ages for roughly 4 million stars.

desk verdict Plausible, potentially important catalog; abstract-only review because the supplied full text is a different paper. read the letter →

arxiv 2508.03019 v1 pith:JYQYB2XF submitted 2025-08-05 astro-ph.SR

Jia-Hui Wang , Maosheng Xiang , Meng Zhang , Jiwei Xie , Jian Ge , Jinghua Zhang , Lanya Mou , Jifeng Liu This is my paper
classification astro-ph.SR
keywords stellaragesdata-drivenLAMOSTXGBoostwidebinariesmain-sequencedwarfschemicalclockGalacticarchaeology
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper tries to establish that the age of a cool main-sequence dwarf can be read off a single low-resolution LAMOST spectrum, well enough for statistical astronomy. The authors build training labels by transferring reliable isochrone ages from the bright primaries of wide binaries to their presumably coeval companions, then train XGBoost on those labels. They report 10–25 percent age precision for K-type stars with spectral signal-to-noise above 50, and a public catalog of ages for about 4 million dwarf stars from LAMOST DR10. If correct, this turns a vast spectroscopic archive into a large stellar-age sample, useful for mapping the Milky Way and for knowing the ages of exoplanet-host stars.

What carries the argument

The wide-binary age transfer: a primary star with a reliable isochrone age is assumed coeval with its companion, so the companion's spectrum inherits that age as a training label. On these labels the paper trains XGBoost, a gradient-boosted decision-tree regressor, to map each LAMOST spectrum to an age. The paper argues the resulting predictive power comes from chemical-abundance features in the low-resolution spectra—the 'chemical clock,' abundance ratios that drift with stellar age—and validates the ages against clusters and wide binaries.

What would settle it

Measure asteroseismic ages for a sample of K-type dwarfs in the catalog with LAMOST S/N>50 and compare residuals; if scatter in (predicted − asteroseismic) age exceeds 25 percent, the central precision claim is refuted, and if wide-binary pairs disagree by more than the stated uncertainties, the coeval training assumption is suspect.

Watch

Extended reading notes

Core claim

The central discovery claimed is that reliable ages for cool main-sequence dwarf stars are encoded in LAMOST's low-resolution spectra (R≈1800), and that a data-driven model can extract them. Using wide binaries as a training device—the primary's isochrone age is assigned to the secondary, supplemented by field and cluster stars with known ages—the authors train XGBoost to predict age from spectra. Validations indicate the predictive signal comes largely from spectral features of chemical abundances, i.e., the stellar chemical clock, and the model reaches 10–25 percent precision for K-type stars at S/N>50. Applied to LAMOST DR10, the model produces a publicly accessible age catalog of roughly 4 million dwarf stars.

Load-bearing premise

Wide binaries used for training really are coeval pairs, and the isochrone age of each primary is accurate; if either fails, every age in the 4-million-star catalog inherits the error.

Editorial extensions

If this is right

  • The public age catalog effectively turns LAMOST DR10 into a ~4-million-star statistical sample for studying how age relates to metallicity, stellar activity, and kinematics in the Milky Way.
  • Exoplanet studies can use the catalog to select or characterize host stars by age, since cool dwarfs are the most common planet hosts.
  • Galactic archaeology gains a homogeneous, spectrum-based age scale that can be combined with astrometry to map star formation history.
  • The method's success at R≈1800 suggests chemical-clock age dating can be applied to other low- and medium-resolution spectroscopic surveys without waiting for high-resolution follow-up.
  • Per-star precision must be quoted with the catalog, because the stated 10–25 percent figure applies only at S/N>50 and younger stars carry larger relative errors.

Reading between the lines

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

  • The derived age–abundance and age–activity relations should be cross-checked against independent asteroseismic samples, since the training labels inherit isochrone assumptions that could imprint on those relations.
  • Tightening the wide-binary training set with astrometric rejection of chance alignments could directly reduce the largest reported errors, which occur for young stars.
  • Quantifying how prediction uncertainty grows as signal-to-noise falls would let users of the catalog set their own S/N thresholds instead of relying on the headline 50 figure.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 3 minor

Summary. The submission consists of an abstract announcing a data-driven method for estimating ages of approximately 4 million main-sequence dwarf stars from LAMOST DR10 spectra using XGBoost trained on wide binaries with isochrone ages of primaries, claiming 10% to 25% age precision for K-type stars at S/N greater than 50 and a chemical-clock interpretation. However, the full text supplied with the submission is a completely different manuscript: a metasurface-enabled extremely large-scale antenna (MELA) systems paper (arXiv:2508.03021v2) covering electromagnetic channel modeling, channel estimation, and half-power beamwidth analysis, with no astronomical content. The paper therefore does not present any of the methods, data, validation, or catalog results promised in the abstract.

Significance. If the abstract's claims were backed by a full paper, the resulting catalog would be a valuable community resource for Galactic archaeology, stellar evolution, and exoplanet host characterization. The idea of transferring isochrone ages from evolved primaries to dwarf secondaries in wide binaries is a reasonable way to obtain training labels that are partly independent of the target spectra. The claimed precision and catalog size would be significant. Nevertheless, the submitted manuscript text contains none of this work. The abstract alone cannot establish the validity of the method or the catalog, and it omits essential details such as the validation protocol, error bars, and out-of-sample testing. For these reasons, the current submission cannot be evaluated as presented.

major comments (4)
  1. [Full text (entire manuscript)] The body of the submission is an unrelated metasurface-antenna paper: it derives channel models in Eqs. (1)-(23), a channel estimation algorithm in Section III, HPBW analysis in Section IV, and numerical simulations in Section V, all in the context of wireless communications. There is no section describing the LAMOST data, wide-binary training set, XGBoost model, age validation, or the claimed 4-million-star catalog. Consequently, every scientific claim in the abstract is unsupported by the submitted manuscript. This is a load-bearing defect that cannot be corrected by minor revision.
  2. [Abstract, first paragraph] The abstract states that ages are 'precise to 10% to 25% for K-type stars' but does not specify how this precision was measured, which validation clusters or independent age indicators were used, or whether those objects overlap the training set. Without this information, the quoted precision may reflect only the scatter between the model and its training labels, which would not establish accuracy for the catalog. This is especially important because the training labels are themselves isochrone ages that may carry systematic errors.
  3. [Abstract, chemical-clock claim] The sentence 'our result is a manifestation of stellar chemical clock effectively acted on LAMOST spectra' asserts a specific physical interpretation. No evidence is given in the abstract (and none appears in the full text, which is unrelated) that the spectral information driving the age predictions is primarily chemical-abundance features rather than, for example, surface gravity or continuum shape. A feature-importance analysis or spectral-line grouping would be needed to support this claim.
  4. [Abstract, catalog application] The statement 'Applying our model to the LAMOST DR10 yields a massive age catalog for ~4 million dwarf stars' is unverifiable from the abstract alone. There is no description of the selection criteria for the 4 million stars, the distribution of signal-to-noise ratios, the treatment of extrapolation beyond the training domain, or any systematic uncertainties in the catalog. These details are essential for users of the public catalog.
minor comments (3)
  1. [Abstract, S/N statement] The sentence 'Given a spectral signal-to-noise ratio greater than 50' is ambiguous: it should state whether S/N refers to the median S/N per pixel, the S/N in a specific spectral region, or something else.
  2. [Abstract, chemical clock terminology] The term 'stellar chemical clock' is used without a definition or citation; please clarify what is meant and provide a reference.
  3. [Abstract, precision vs. accuracy] The phrase 'age estimation precise to 10% to 25%' mixes precision and accuracy; the authors should separately report scatter and systematic offsets.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the age labels come from isochrone fitting of wide-binary primaries, independent of the secondary spectra used as model features.

full rationale

The paper's claimed derivation chain is a supervised calibration: wide binaries supply ages for secondaries by transferring the isochrone age of the primary, and an XGBoost model is trained to map LAMOST spectra of the secondaries to those transferred ages. The training labels are therefore not constructed from the spectra being predicted; they come from an independent isochrone analysis of the primaries, supplemented by cluster and field stars with known ages. Even the chemical-clock interpretation is presented as a post-hoc validation statement ('the underlying information used for our age estimation is largely attributed to the LAMOST spectral features of chemical abundances') rather than as an input that defines the ages. No equation or definition in the supplied abstract makes the predicted age equivalent to the input labels by construction, and no load-bearing self-citation chain is visible. The supplied full text is an unrelated metasurface-antenna manuscript, so the validation sections of the stellar-age paper cannot be inspected; that is an evidence-availability problem, not a demonstrated circularity. Accordingly, no circular step can be quoted and exhibited, and the honest finding is no significant circularity with score 0.

Assumptions & free parameters 3 free parameters · 4 assumptions · 1 invented entities

The central claim rests on the reliability of transferred isochrone ages (axioms 1 and 2), the spectral encoding of age (axiom 3), and training-set representativeness (axiom 4). The free parameters are the SNR cutoff, undisclosed XGBoost settings, and the binary-selection criteria. No new entities are introduced.

free parameters (3)
  • SNR quality threshold = 50
    The abstract restricts the precision claim to spectra with SNR > 50; this hand-chosen threshold determines which stars enter the reliable-age subset of the catalog.
  • XGBoost hyperparameters = not stated
    Gradient-boosting hyperparameters (tree depth, learning rate, number of trees, feature subsampling) are not disclosed; they directly control the regression accuracy claim.
  • Wide binary selection criteria = not stated
    The definition of a wide binary, the pairing probability threshold, and quality cuts on primaries set the quality of the age labels and are not given in the abstract.
assumptions (4)
  • domain assumption Wide-binary secondaries are coeval with, and share the age of, their primaries
    Abstract: 'wide binaries that the primary component has reliable isochrone age estimate thus gives the age of the secondary'. Bound, coeval wide binaries are the entire source of training labels; chance alignments would inject wrong ages.
  • domain assumption Isochrone ages of the evolved primaries are accurate at the claimed precision
    The training labels carry all model systematics of stellar evolution codes, initial mass function priors, metallicity scales, and distance or reddening assumptions of the isochrone fit.
  • domain assumption LAMOST R~1800 spectra contain measurable age information above abundance-systematics noise
    Abstract: validation suggests 'the underlying information used for our age estimation is largely attributed to the LAMOST spectral features of chemical abundances'. If abundance systematics dominate the age-correlated features, the predicted ages partly trace measurement artifacts.
  • domain assumption The training set spans the parameter space of the 4-million-star catalog
    Transferring a model fitted on wide binaries, field stars, and clusters to the full DR10 dwarf sample assumes coverage in temperature, metallicity, and signal-to-noise; extrapolation behavior is not discussed in the abstract.
invented entities (1)
  • No new physical entities
    purpose: None; the paper assigns ages to existing stars
    The abstract introduces no new particles, forces, or conserved quantities; it calibrates an empirical mapping from spectra to age.

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Cite this review

Pith. "Pith review of Spectroscopic ages for 4 million main-sequence dwarf stars from LAMOST DR10 estimated with data-driven approach." pith.science (2026). https://pith.science/paper/JYQYB2XF

@misc{pith2026250803019,
  author       = {Pith},
  title        = {Pith review of: Spectroscopic ages for 4 million main-sequence dwarf stars from LAMOST DR10 estimated with data-driven approach},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JYQYB2XF}},
  note         = {Machine review of arXiv:2508.03019}
}
abstract

Stellar age determination for large samples of stars opens new avenues for a broad range of astronomical sciences. While precise stellar ages for evolved stars have been derived from large ground- and space-based stellar surveys, reliable age determination for cool main-sequence dwarf stars remains a challenge. In this work, we set out to estimate the age of dwarf stars from the LAMOST spectra with a data-driven approach. We build a training set by using wide binaries that the primary component has reliable isochrone age estimate thus gives the age of the secondary. This training set is further supplemented with field stars and cluster stars whose ages are known. We then train a data-driven model for inferring age from their spectra with the XGBoost algorithm. Given a spectral signal-to-noise ratio greater than 50, the age estimation precise to 10% to 25% for K-type stars, as younger stars have larger relative errors. Validations suggest that the underlying information used for our age estimation is largely attributed to the LAMOST spectral features of chemical abundances. It means our result is a manifestation of stellar chemical clock effectively acted on LAMOST spectra ($R\simeq1800$). Applying our model to the LAMOST DR10 yields a massive age catalog for $\sim4$ million dwarf stars. Statistical properties, such as the age distribution, age-abundance and age-stellar activity relations of the sample stars are discussed. The catalog is publicly accessible and can be helpful for extensive sciences from detection and characterization of Earth-like planets to Galactic archaeology.

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Reference graph

Works this paper leans on

38 extracted references · 37 canonical work pages · cited by 1 Pith paper

  1. [1]

    Hybrid MIMO architectures for millimeter wave communica- tions: Phase shifters or switches?

    R. M ´endez-Rial, C. Rusu, N. Gonz ´alez-Prelcic, A. Alkhateeb, and R. W. Heath, “Hybrid MIMO architectures for millimeter wave communica- tions: Phase shifters or switches?”IEEE access, vol. 4, pp. 247–267, Jan. 2016

    work page 2016

  2. [2]

    A tutorial on extremely large-scale MIMO for 6G: Fundamentals, signal processing, and applications,

    Z. Wang, J. Zhang, H. Du, D. Niyato, S. Cui, B. Ai, M. Debbah, K. B. Letaief, and H. V . Poor, “A tutorial on extremely large-scale MIMO for 6G: Fundamentals, signal processing, and applications,”IEEE Communications Surveys & Tutorials, vol. 26, no. 3, pp. 1560–1605, Jan. 2024

    work page 2024

  3. [3]

    Extremely large-scale MIMO: Fundamentals, challenges, solutions, and future directions,

    Z. Wang, J. Zhang, H. Du, W. E. Sha, B. Ai, D. Niyato, and M. Debbah, “Extremely large-scale MIMO: Fundamentals, challenges, solutions, and future directions,”IEEE Wireless Commun., vol. 31, no. 3, pp. 117–124, Apr. 2023

    work page 2023

  4. [4]

    Patterned Beam Training: A Novel Low-Complexity and Low-Overhead Scheme for ELAA

    H. Yu, Y . Si, S. Zhang, and Y . Chen, “Patterned beam training: A novel low-complexity and low-overhead scheme for ELAA,” Jun. 2024. [Online]. Available: https://arxiv.org/abs/2406.00399

    work page Pith review arXiv 2024

  5. [5]

    Spatial correlations of measured mimo channels with an extremely large aperture array (ELAA),

    Y . Yuan, C. Wang, C. Li, Z. Zhong, W. Han, and C.-X. Wang, “Spatial correlations of measured mimo channels with an extremely large aperture array (ELAA),” inVTC2022-Spring, Aug. 2022, pp. 1–5

    work page 2022

  6. [6]

    Extremely large aperture array (ELAA) communications: Foundations, research advances and challenges,

    S. Ye, M. Xiao, M.-W. Kwan, Z. Ma, Y . Huang, G. Karagiannidis, and P. Fan, “Extremely large aperture array (ELAA) communications: Foundations, research advances and challenges,”IEEE Open J. Commun. Soc., vol. 5, pp. 7075–7120, Oct. 2024

    work page 2024

  7. [7]

    Millimeter wave communications for future mobile networks,

    M. Xiao, S. Mumtaz, Y . Huang, L. Dai, Y . Li, M. Matthaiou, G. K. Karagiannidis, E. Bj ¨ornson, K. Yang, A. Ghoshet al., “Millimeter wave communications for future mobile networks,”IEEE J. Sel. Areas Commun., vol. 35, no. 9, pp. 1909–1935, Jun. 2017

    work page 1909

  8. [8]

    Toward extra large-scale MIMO: New channel properties and low-cost designs,

    Y . Han, S. Jin, M. Matthaiou, T. Q. Quek, and C.-K. Wen, “Toward extra large-scale MIMO: New channel properties and low-cost designs,” IEEE Internet Things J., vol. 10, no. 16, pp. 14 569–14 594, May. 2023

    work page 2023

Show all 38 references
  1. [9]

    Dynamic hybrid beamforming designs for ELAA near-field communications,

    M. Liu, M. Li, R. Liu, and Q. Liu, “Dynamic hybrid beamforming designs for ELAA near-field communications,”IEEE J. Sel. Areas Commun., vol. 43, no. 3, pp. 644–658, Jan. 2025

    2025

  2. [10]

    Reconfigurable intelligent surfaces in 6g: Reflective, transmissive, or both?

    S. Zeng, H. Zhang, B. Di, Y . Tan, Z. Han, H. V . Poor, and L. Song, “Reconfigurable intelligent surfaces in 6g: Reflective, transmissive, or both?”IEEE Commun. Lett., vol. 25, no. 6, pp. 2063–2067, Feb. 2021

    2021

  3. [11]

    Planar three-dimensional constrained lenses,

    D. McGrath, “Planar three-dimensional constrained lenses,”IEEE Trans. Antennas Propag., vol. 34, no. 1, pp. 46–50, Jan. 1986

    1986

  4. [12]

    Focal distance reduction of transmit-array antennas using multiple feeds,

    A. Clemente, L. Dussopt, R. Sauleau, P. Potier, and P. Pouliguen, “Focal distance reduction of transmit-array antennas using multiple feeds,” IEEE Antennas Wirel. Propag. Lett., vol. 11, pp. 1311–1314, Nov. 2012

    2012

  5. [13]

    Radiation pattern synthesis for monopulse radar ap- plications with a reconfigurable transmitarray antenna,

    L. Di Palma, A. Clemente, L. Dussopt, R. Sauleau, P. Potier, and P. Pouliguen, “Radiation pattern synthesis for monopulse radar ap- plications with a reconfigurable transmitarray antenna,”IEEE Trans. Antennas Propag., vol. 64, no. 9, pp. 4148–4154, Jun. 2016

    2016

  6. [14]

    A hybrid architecture for programmable meta-system using a few active elements,

    Z. X. Wang, J. W. Wu, H. Q. Yang, Q. Y . Zhou, S. R. Wang, H. Xu, L. J. Wu, Y . Quan, Q. Cheng, and T. J. Cui, “A hybrid architecture for programmable meta-system using a few active elements,”Laser & Photonics Reviews, vol. 18, no. 8, p. 2400062, Apr. 2024

    2024

  7. [15]

    Dynamic metasurface antennas for 6G extreme massive MIMO communications,

    N. Shlezinger, G. C. Alexandropoulos, M. F. Imani, Y . C. Eldar, and D. R. Smith, “Dynamic metasurface antennas for 6G extreme massive MIMO communications,”IEEE Wireless Communications, vol. 28, no. 2, pp. 106–113, Jan. 2021

    2021

  8. [16]

    60 ghz programmable dy- namic metasurface antenna (DMA) for next-generation communication, sensing, and imaging applications: From concept to prototype,

    A. Jabbar, M. Elsayed, J. U. R. Kazim, Z. Pang, J. Le Kernec, M. A. Imran, Q. H. Abbasi, and M. Ur-Rehman, “60 ghz programmable dy- namic metasurface antenna (DMA) for next-generation communication, sensing, and imaging applications: From concept to prototype,”IEEE Open J. Ant...

    2024

  9. [17]

    Electronically steered metasurface antenna,

    M. Boyarsky, T. Sleasman, M. F. Imani, J. N. Gollub, and D. R. Smith, “Electronically steered metasurface antenna,”Scientific reports, vol. 11, no. 1, p. 4693, Feb. 2021

    2021

  10. [18]

    Beamforming design and power allocation for transmissive RMS-based transmitter architectures,

    Z. Li, W. Chen, and H. Cao, “Beamforming design and power allocation for transmissive RMS-based transmitter architectures,”IEEE Wireless Commun. Lett., vol. 11, no. 1, pp. 53–57, Oct. 2021

    2021

  11. [19]

    Ro- bust weighted sum-rate maximization for transmissive RIS transmitter enabled RSMA networks,

    B. Li, W. Chen, Z. Li, Q. Wu, N. Cheng, C. Li, and L. Dai, “Ro- bust weighted sum-rate maximization for transmissive RIS transmitter enabled RSMA networks,”IEEE Commun. Lett., vol. 27, no. 10, pp. 2847–2851, Aug. 2023

    2023

  12. [20]

    Transmissive RIS transceiver enabled multi-stream communication systems: Design, optimization and analysis,

    Z. Li, W. Chen, X. Zhu, Q. Wu, G. Ni, S. Zhang, and J. Li, “Transmissive RIS transceiver enabled multi-stream communication systems: Design, optimization and analysis,”IEEE Internet Things J., Oct. 2024

    2024

  13. [21]

    Transmis- sive RIS enabled transceiver systems: Architecture, design issues and opportunities,

    Z. Li, W. Chen, Q. Wu, Z. Liu, C. He, X. Bai, and J. Li, “Transmis- sive RIS enabled transceiver systems: Architecture, design issues and opportunities,”arXiv preprint arXiv:2408.13483, 2024

    2024 arXiv

  14. [22]

    Toward transmissive RIS transceiver enabled uplink communication systems: Design and optimization,

    Z. Li, W. Chen, Q. Wu, X. Zhu, H. Qin, K. Wang, and J. Li, “Toward transmissive RIS transceiver enabled uplink communication systems: Design and optimization,”IEEE Internet Things J., vol. 11, no. 4, pp. 6788–6801, Sep. 2023

    2023

  15. [23]

    User-centric cell-free massive MIMO with RIS-integrated antenna arrays,

    ¨O. T. Demir and E. Bj ¨ornson, “User-centric cell-free massive MIMO with RIS-integrated antenna arrays,” inProc. IEEE 25th Int. Workshop on Signal Process. Adv. in Wireless Commun. (SPAWC). Ieee, Oct. 2024, pp. 546–550

    2024

  16. [24]

    Cross far-and near-field wireless communications in terahertz ultra-large antenna array systems,

    C. Han, Y . Chen, L. Yan, Z. Chen, and L. Dai, “Cross far-and near-field wireless communications in terahertz ultra-large antenna array systems,” IEEE Wireless Commun., Feb. 2024

    2024

  17. [25]

    Near-field beam training: Joint angle and range estimation with DFT codebook,

    X. Wu, C. You, J. Li, and Y . Zhang, “Near-field beam training: Joint angle and range estimation with DFT codebook,”IEEE Trans. Wireless Commun., 2024

    2024

  18. [26]

    Hybrid near-far field channel estimation for holographic MIMO communications,

    S. Yue, S. Zeng, L. Liu, Y . C. Eldar, and B. Di, “Hybrid near-far field channel estimation for holographic MIMO communications,”IEEE Transactions on Wireless Communications, vol. 23, no. 11, pp. 15 798– 15 813, Aug. 2024

    2024

  19. [27]

    Channel estimation for extremely large-scale MIMO: Far-field or near-field?

    M. Cui and L. Dai, “Channel estimation for extremely large-scale MIMO: Far-field or near-field?”IEEE Trans. Commun., vol. 70, no. 4, pp. 2663–2677, Jan. 2022

    2022

  20. [28]

    Channel estimation for extremely large-scale massive MIMO: Far-field, near-field, or hybrid-field?

    X. Wei and L. Dai, “Channel estimation for extremely large-scale massive MIMO: Far-field, near-field, or hybrid-field?”IEEE Commun. Lett., vol. 26, no. 1, pp. 177–181, Nov. 2021

    2021

  21. [29]

    Compressive near/far-field channel estimation for mmwave/THz systems with extremely large antenna arrays,

    H. Wang, J. Fang, and J. Wang, “Compressive near/far-field channel estimation for mmwave/THz systems with extremely large antenna arrays,” inProc. IEEE Glob. Commun. Conf. (GLOBECOM). IEEE, Feb. 2024, pp. 2354–2359

    2024

  22. [30]

    Gridless hybrid-field channel estimation for extra-large aperture array massive MIMO systems,

    Y . Xi, F. Zhu, B. Zhou, T. Liu, and S. Ma, “Gridless hybrid-field channel estimation for extra-large aperture array massive MIMO systems,”IEEE Wireless Commun. Lett., vol. 13, no. 2, pp. 496–500, Nov. 2023

    2023

  23. [31]

    An efficient modified music algorithm for ris-assisted near-field localization,

    P. Ramezani, A. Kosasih, and E. Bj ¨ornson, “An efficient modified music algorithm for ris-assisted near-field localization,” inProc. IEEE Glob. Commun. Conf. (GLOBECOM), 2024, pp. 4430–4435

    2024

  24. [32]

    Efficient application of MUSIC algorithm under the coexistence of far-field and near-field sources,

    J. He, M. Swamy, and M. O. Ahmad, “Efficient application of MUSIC algorithm under the coexistence of far-field and near-field sources,”IEEE Trans. Signal Process., vol. 60, no. 4, pp. 2066–2070, 2011

    2011

  25. [33]

    Massive mimo channel estimation taking into account spherical waves,

    L. L. Magoarou, A. L. Calvez, and S. Paquelet, “Massive mimo channel estimation taking into account spherical waves,” inProc. IEEE 25th Int. Workshop on Signal Process. Adv. in Wireless Commun. (SPAWC), 2019, pp. 1–5

    2019

  26. [34]

    Wavefront transformation- based near-field channel prediction for extremely large antenna array with mobility,

    W. Li, H. Yin, Z. Qin, and M. Debbah, “Wavefront transformation- based near-field channel prediction for extremely large antenna array with mobility,”IEEE Trans. Wireless Commun., vol. 23, no. 10, pp. 15 613–15 626, Jul. 2024

    2024

  27. [35]

    C. A. Balanis,Antenna theory: analysis and design. John wiley & sons, 2016

    2016

  28. [36]

    Design and optimization on successive RIS-assisted multi-hop wireless communications,

    R. Xiong, J. Lu, J. Zhang, M. Liu, X. Dong, T. Mi, and R. C. Qiu, “Design and optimization on successive RIS-assisted multi-hop wireless communications,”arXiv preprint arXiv:2407.10080, 2024

    2024 arXiv

  29. [37]

    Near-field extremely large-scale STAR-RIS enabled integrated sensing and com- munications,

    J. Zhou, Y . Yang, Z. Yang, and M. Reza Shikh-Bahaei, “Near-field extremely large-scale STAR-RIS enabled integrated sensing and com- munications,”IIEEE Trans. Green Commun. Netw., vol. 9, no. 1, pp. 404–416, Sep. 2025

    2025

  30. [38]

    Near-field full dimensional beam codebook design for XL-MIMO communications,

    W. Huang, C. Li, Y . Zeng, C. Kai, and S. He, “Near-field full dimensional beam codebook design for XL-MIMO communications,” inGLOBECOM 2023-2023 IEEE Global Communications Conference. IEEE, 2023, pp. 4902–4908

    2023

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