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Direct, Indirect and Collider Detection of Neutralino Dark Matter In SUSY Models with Non-universal Higgs Masses

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Howard Baer, Azar Mustafayev, Stefano Profumo, Alexander Belyaev, Xerxes Tata

High Energy Physics - Phenomenology · Submitted 1 Apr 2005 · 107 references

Pith's verdict: The structural result is real and useful — NUHM1 gives two low-relic-density solutions at any tan beta and m0, NUHM2 opens new co-annihilation regions — but the detection-rate numbers are looser than the abstract implies, and the paper never shows the overlap between its VR>1 contours and the WMAP central band.

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CitationAlexander Belyaev, Azar Mustafayev, Howard Baer, Stefano Profumo, Xerxes Tata. "Direct, Indirect and Collider Detection of Neutralino Dark Matter In SUSY Models with Non-universal Higgs Masses." arXiv:hep-ph/0504001 (2005). https://pith.science/paper/62KSRFFN
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The paper

The paper claims

Letting the Higgs soft masses differ from squark masses turns two narrow dark-matter corners into broad, tunable regions, and puts neutralinos within reach of direct detection and a linear collider.

The reading

The paper asks what happens to supersymmetric dark matter when one assumption of the minimal supergravity model is dropped: that the two Higgs fields carry the same soft-breaking mass as the squarks and sleptons at the grand-unified scale. Universality among the matter scalars is kept, because that is what suppresses unwanted flavor-changing processes, but the Higgs masses are allowed to float — one extra parameter in the NUHM1 model ($m_phi$, with $m_{H_u}^2 = m_{H_d}^2 ne m_0^2$) and two in NUHM2. The payoff is that the two narrow corners where the minimal model can satisfy the WMAP cold-dark-matter density — the heavy-Higgs annihilation funnel, reachable only at large $tan beta$, and the higgsino region, reachable only at multi-TeV $m_0$ — become broad regions that can be dialed into at almost any point of the parameter space. If the authors are right, a large family of spectra the minimal model forbids is viable, and several of those spectra put the neutralino within reach of XENON-class direct detection, IceCube, and a 0.5–1 TeV linear collider.

What carries the argument

The argument runs through the renormalization-group evolution of the Higgs soft masses and the two electroweak-symmetry-breaking minimization conditions. The key relation is that a deviation of the Higgs mass from the universal value at the GUT scale survives running with its sign intact but shrinks in magnitude, $Delta m_{H_u}^2(mathrm{weak}) simeq Delta m_{H_u}^2(mathrm{GUT}), e^{-J_t}$ with $J_t = frac{3}{8pi^2} int dt, f_t^2 > 0$, so positive and negative $m_phi$ push $mu$ and $m_A$ in opposite directions through $mu^2 = frac{m_{H_d}^2 - m_{H_u}^2 tan^2beta}{tan^2beta - 1} - frac{M_Z^2}{2}$ and $m_A^2 = m_{H_u}^2 + m_{H_d}^2 + 2mu^2$. In NUHM2 a nonzero $S = m_{H_u}^2 - m_{H_d}^2$ enters the third-generation and first-generation scalar RGEs with hypercharge-weighted signs, splitting squark and slepton masses within a generation. The phenomenological filter is a $chi^2$ over three measurements — $Omega_{mathrm{CDM}} h^2 = 0.113 pm 0.009$, $BF(b to sgamma) = (3.25 pm 0.37) times 10^{-4}$ and $Delta a_mu = (27 pm 10) times 10^{-10}$ — plus the LEP2 chargino bound $m_{tilde W_1} geq 103.5$ GeV, with spectra from Isajet, relic densities from IsaReD and detection rates from DarkSUSY. Detection prospects are expressed as visibility ratios, signal over projected sensitivity, computed for two self-consistent halo models (a cored Burkert profile and an adiabatically contracted N03 profile) so that direct and indirect channels are compared on the same footing.

Extended reading notes

Core claim

The central claim is that splitting the GUT-scale Higgs soft masses from the matter-scalar mass $m_0$ changes which supersymmetric spectra are compatible with the measured relic density, and changes them in a way that is observable. In NUHM1 the authors argue that for essentially any choice of $m_0$, $m_{1/2}$ and $tan beta$ there are two values of $m_phi$ that bring $Omega_{tilde Z_1} h^2$ into the WMAP range: a large negative $m_phi$ pushes the pseudoscalar mass $m_A$ down to roughly twice the neutralino mass, opening the A-annihilation funnel at any $tan beta$ including low values; a large positive $m_phi$ drives $m_{H_u}^2$ negative faster during running, so that $|mu|$ becomes small while $m_0$ stays low, giving a higgsino-like lightest neutralino without the multi-TeV scalars of the minimal model's focus point. In NUHM2, $mu$ and $m_A$ can be taken as weak-scale inputs, so either region is reachable by choice for any $m_0$, $m_{1/2}$ and $tan beta$ that yields a valid spectrum. The paper further identifies co-annihilation regions that exist only in NUHM2: a large positive $S = m_{H_u}^2 - m_{H_d}^2$ drives the right-handed up and charm squarks very light, and a large negative $S$ makes the left sleptons and sneutrinos light, both of which suppress the relic density and, in the squark case, strongly enhance the spin-independent neutralino-proton cross section.

Load-bearing premise

The detection-rate claims assume that the neutralino makes up the full local dark matter density even at parameter points whose computed thermal relic abundance falls short of the measured value; the authors state this explicitly in Sec. 2.4, where they do not rescale the visibility ratios downward, and footnote 1 invokes unspecified non-thermal production or a cosmological enhancement to make up the difference.

Editorial extensions

If this is right

  • The relic-density constraint stops being a filter that forces either large $tan beta$ or multi-TeV scalar masses; spectra with low $tan beta$ and low $m_0$ become viable, so the WMAP measurement alone no longer points to a particular corner of the supersymmetric parameter space.
  • In the low-$mu$ higgsino region, charginos and neutralinos are light enough that a $sqrt{s} = 0.5$–1 TeV linear collider can reach beyond the LHC, because the LHC reach is set by squark and gluino masses while the collider reach is set by $mu$.
  • In the A-funnel region, $H$, $A$ and $H^pm$ can be light enough for direct production at the LHC or a linear collider, and can appear in gluino and squark cascades, at values of $tan beta$ far below where the minimal model allows this.
  • In NUHM2, very light $tilde u_R$ and $tilde c_R$ squarks or light left sleptons can supply the needed co-annihilation, giving large spin-independent direct detection rates and, for the squarks, dijet plus missing-energy signals at hadron colliders.
  • The same relic density can be reproduced by spectra with very different collider signatures, so a measurement of the dark matter density alone does not determine what the LHC or a linear collider will see.

Reading between the lines

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

  • If the thermal relic abundance is later shown to saturate the cosmic density with no non-thermal component, the parameter regions where $Omega h^2$ falls below about 0.094 would be removed, and with them much of the funnel and higgsino parameter space used here to argue for observable rates.
  • The NUHM2 squark co-annihilation window makes the spin-independent cross section a sharp function of the Higgs mass splitting, so a null result from a ton-scale direct detection experiment would translate into a constraint on $S$ at the GUT scale rather than merely on $m_0$ and $m_{1/2}$.
  • Because the funnel can open at low $tan beta$, the usual expectation that cascade decays are tau-rich in funnel points does not carry over, which changes the event selection that collider searches should optimize for dark-matter-motivated spectra.
  • The two-parameter version effectively promotes $mu$ and $m_A$ to inputs, so any future measurement of a light Higgsino and a heavy pseudoscalar (or the reverse) would already discriminate NUHM2 from the one-parameter case without a full spectrum fit.
Original abstract

In supersymmetric models with gravity-mediated SUSY breaking, universality of soft SUSY breaking sfermion masses m_0 is motivated by the need to suppress unwanted flavor changing processes. The same motivation, however, does not apply to soft breaking Higgs masses, which may in general have independent masses from matter scalars at the GUT scale. We explore phenomenological implications of both the one-parameter and two-parameter non-universal Higgs mass models (NUHM1 and NUHM2), and examine the parameter ranges compatible with Omega_CDM h^2, BF(b --> s,gamma) and (g-2)_mu constraints. In contrast to the mSUGRA model, in both NUHM1 and NUHM2 models, the dark matter A-annihilation funnel can be reached at low values of tan(beta), while the higgsino dark matter annihilation regions can be reached for low values of m_0. We show that there may be observable rates for indirect and direct detection of neutralino cold dark matter in phenomenologically aceptable ranges of parameter space. We also examine implications of the NUHM models for the Fermilab Tevatron, the CERN LHC and a Sqrt(s)=0.5-1 TeV e+e- linear collider. Novel possibilities include: very light s-top_R, s-charm_R squark and slepton_L masses as well as light charginos and neutralinos and H, A and H^+/- Higgs bosons.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,940 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.11 · human participants 0.01 · controlled comparison 0.33 · randomized assignment 0.01 · states quantitative result 0.22 · compares with prior results 0.85 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

In supersymmetric models with gravity-mediated SUSY breaking, universality of soft SUSY breaking sfermion masses m_0 is motivated by the need to suppress unwanted flavor changing processes. The same motivation, however, does not apply to soft breaking Higgs masses, which may in general have independent masses from matter scalars at the GUT scale. We explore phenomenological implications of both the one-parameter and two-parameter non-universal Higgs mass models (NUHM1 and NUHM2), and examine the parameter ranges compatible with Omega_CDM h^2, BF(b --> s,gamma) and (g-2)_mu constraints. In contrast to the mSUGRA model, in both NUHM1 and NUHM2 models, the dark matter A-annihilation funnel can be reached at low values of tan(beta), while the higgsino dark matter annihilation regions can be reached for low values of m_0. We show that there may be observable rates for indirect and direct detection of neutralino cold dark matter in phenomenologically aceptable ranges of parameter space. We also examine implications of the NUHM models for the Fermilab Tevatron, the CERN LHC and a Sqrt(s)=0.5-1 TeV e+e- linear collider. Novel possibilities include: very light s-top_R, s-charm_R squark and slepton_L masses as well as light charginos and neutralinos and H, A and H^+/- Higgs bosons.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 In supersymmetric models with gravity-mediated SUSY breaking, universality of soft SUSY breaking sfermion masses m_0 is motivated by the need to suppress unwanted flavor changing processes. background 1.00 0.05 0.02 asserted 0.97
s1 The same motivation, however, does not apply to soft breaking Higgs masses, which may in general have independent masses from matter scalars at the GUT scale. background 0.95 0.08 0.03 hedged possibility 0.91
s2 We explore phenomenological implications of both the one-parameter and two-parameter non-universal Higgs mass models (NUHM1 and NUHM2), and examine the parameter ranges compatible with Omega_CDM h^2, BF(b --> s,gamma) and (g-2)_mu constraints. contribution 0.92 0.87 0.07 asserted 0.79
s3 In contrast to the mSUGRA model, in both NUHM1 and NUHM2 models, the dark matter A-annihilation funnel can be reached at low values of tan(beta), while the higgsino dark matter annihilation regions can be reached for low values of m_0. result 1.00 0.78 0.16 asserted 0.99
s4 We show that there may be observable rates for indirect and direct detection of neutralino cold dark matter in phenomenologically aceptable ranges of parameter space. result 0.98 0.90 0.63 hedged possibility 0.89
s5 We also examine implications of the NUHM models for the Fermilab Tevatron, the CERN LHC and a Sqrt(s)=0.5-1 TeV e+e- linear collider. contribution 0.90 0.79 0.04 asserted 0.81
s6 Novel possibilities include: very light s-top_R, s-charm_R squark and slepton_L masses as well as light charginos and neutralinos and H, A and H^+/- Higgs bosons. result 0.91 0.71 0.07 hedged possibility 0.88

What kind of paper the classifier reports this is: theoretical result 0.62 · evidence from simulation or computation 0.95.

What was examined, and what was not

sources read
  • arXiv listing abstract v2
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

Figures
Figure 1. Plot of µ, mA and mZe1 vs. mφ for m0 = 300 GeV, m1/2 = 300 GeV, A0 = 0, tan β = 10 and mt = 178 GeV. We take µ > 0. To understand the behavior of the µ parameter and mA in the NUHM1 model, we first examine the renormalization group equations (RGEs) for the soft SUSY breaking Higgs squared mass parameters. Neglecting the Yukawa couplings for the first two generations, – 6 –
Figure 2. The evolution of m2 Hu and m2 Hd from Q = MGUT to Mweak for Mφ = 300 GeV (mSUGRA case), 500 GeV and -700 GeV. We also take m0 = 300 GeV, m1/2 = 300 GeV, A0 = 0, tan β = 10 and mt = 178 GeV, with µ > 0. For moderate to large values of tan β (as favored by LEP2 Higgs boson mass constraints), and |mHu | ≫ MZ, µ 2 ∼ −m2 Hu . Thus, we see that in the case of large negative mφ values, we would expect a large |µ| parameter, whereas for large positive mφ values, m2 Hu is barely driven to negative values, and we expect a small |µ| parameter. Within the same approximation, the tree level…
Figure 3. Various sparticle masses versus mφ in the NUHM1 model for m0 = 300 GeV, m1/2 = 300 GeV, A0 = 0, tan β = 10 and mt = 178 GeV. We take µ > 0. Thus, when Xt is small (for mφ < m0), the diagonal entries in the top and bottom squark mass squared matrices are not as suppressed due to top Yukawa coupling effects as in the mSUGRA case. In contrast, for large positive values of mφ, Xt is large and these soft masses are more suppressed resulting lighter third generation squarks. These expectations are indeed born out in
Figure 4. Ranges of p χ2 in a scan over tan β and mφ values in the NUHM1 model for fixed m0 = m1/2 = 300 GeV, A0 = 0, µ > 0 and mt = 178 GeV. The green region corresponds to low values of p χ2 <∼ √ 3, while the red region has p χ2 >∼ 5, with the yellow region corresponding to intermediate values. consist of, say, axions1 . Green points have low p χ2 <∼ √ 3 values, and agree well with the central values of each of these measurements. Red points have large p χ2 >∼ 5, and are excluded. Yellow points have intermediate values of p χ2. We show six frames illustrating various correlations am
Figure 5. Ranges of Ωh 2 , δaµ and BF(b → sγ) for the NUHM1 models scanned in
Figure 6. The p χ2 value in the m0 vs. m1/2 plane for A0 = 0, tan β = 10, µ > 0 and mt = 178 GeV. In frames a), b), c), and d) we take mφ/m0 = 1, −2.5, 1.1 and 1.5, respectively. The blue region is excluded by LEP2. In
Figure 7. The p χ2 value in the m0 vs. m1/2 plane for A0 = 0, tan β = 35, µ > 0 and mt = 178 GeV, with mφ = −2.5m0. The blue region is excluded by LEP2. In
Figure 8. Dark matter detection Visibility Ratios (i.e. signal-to-projected-sensitivity ratios) for various direct and indirect techniques, as a function of the GUT scale non-universal Higgs mass parameter mφ, for mSUGRA parameters tan β = 10, A0 = 0, sgnµ > 0, m0 = 300 GeV, m1/2 = 300 GeV, and setting mt = 178 GeV. We take the dark matter distribution to be given by the cored Burkert Halo profile described in the text. A Visibility Ratio larger than one means that the signal will be detectable over background. density enhancement, as envisaged in Ref. [83, 84] for quintessential cosmologies,…
Figure 10. Approximate projections for the reach of the CERN LHC (100 fb−1 ) and ILC in the NUHM1 model in the m0 vs. m1/2 plane for tan β = 10, A0 = 0, µ > 0 and mt = 178 GeV, for various choices of mφ/m0. The regions shaded in green are consistent with the WMAP constraint Ωh 2 < 0.13, while those shaded in red and blue are respectively excluded by theoretical and experimental constraints discussed in the text. While we expect a similar reach of the LHC (in terms of mq˜ and mg˜ parameters) to be found in both the mSUGRA and NUHM1 models, the detailed gluino and squark cascade decays will…
Figure 11. Variation in sparticle masses versus ∆mH in the NUHM2 model, for m0 = 300 GeV, m1/2 = 300 GeV, A0 = 0, tan β = 10, µ > 0 and mt = 178 GeV. Some aspects of NUHM2 phenomenology as a function of ∆mH are illustrated in
Figure 12. Variation in a) mA, µ and mZe1 , b) ΩZe1 h 2 , c) BF(b → sγ) and d) ∆aµ versus ∆mH ≡ (mHd − mHu )/2 in the NUHM2 model, for m0 = 300 GeV, m1/2 = 300 GeV, A0 = 0, tan β = 10, µ > 0 and mt = 178 GeV. A-funnel annihilation. For ∆mH large and positive, the relic density, shown in frame b), drops because left sleptons and sneutrinos become very light. The value of BF(b → sγ) and ∆aµ are also shown in frames c) and d). These rise for negative values of ∆mH because the charged Higgs bosons and the lighter charginos and neutralinos become very light with the -inos developing significant…
Figure 13. Variation of sparticle masses versus ∆mH defined in the text for the NUHM2 model, with m0 = 1450 GeV, m1/2 = 300 GeV, A0 = 0, tan β = 10, µ > 0 and mt = 178 GeV. the A-funnel, and on the right-most edge of parameter space, barely visible, is the higgsino region. The narrow green region at the upper boundary of parameter space corresponds to the slepton (or squark for large m0) co-annihilation region. The DM allowed regions of parameter space show up more prominently if the param￾eters m2 Hu and m2 Hd are traded for mA and µ as inputs. We display in
Figure 14. Variation in a) mA, µ and mZe1 , b) ΩZe1 h 2 , c) BF(b → sγ) and d) ∆aµ versus ∆mH ≡ (mHd − mHu )/2 in the NUHM2 model, for m0 = 1450 GeV, m1/2 = 300 GeV, A0 = 0, tan β = 10, µ > 0 and mt = 178 GeV. gion shows up as the broad band of green/yellow at low µ values, while the A-annihilation funnel shows up as the vertical band running upwards near mA ∼ 250 GeV. This plot highlights the importance of the measure of parameter space when deciding the likelihood that any particular framework satisfies some empirical (or, for that matter, theoretical) criteria: the tiny green/yellow sliver…
Figure 15. Plot of allowed parameter space in the mHu vs. mHd plane of the NUHM2 model for for m0 = m1/2 = 300 GeV, A0 = 0, tan β = 10, µ > 0 and mt = 178 GeV. In frame a), we show contours of µ and mA, while in frame b) we show values of χ 2 . The yellow region in frame a) is where so-called “GUT stability bound” is violated. The short-dashed black line denotes the parameter space of the NUHM1 model. The cross denotes the mSUGRA model, while the long-dashed line gives the model where the Higgs scalar mass parameters are split as in
Figure 16. Plot of regions of p χ2 in the µ vs. mA plane for m0 = m1/2 = 300 GeV, A0 = 0, tan β = 10 and mt = 178 GeV for µ > 0. The line labeled HS denotes the NUMH2 model where just the Higgs mass parameters are split as in
Figure 17. Ranges of ΩZe1 h 2 together with contours of BF(b → sγ) and ∆aµ in the µ vs. mA plane for m0 = m1/2 = 300 GeV, A0 = 0, tan β = 10 and mt = 178 GeV. For very large values of mA, we have the stau co-annihilation region. In frame a), we show contours for µ < 0 and in frame b) we show contours for µ > 0. µ − mA plane allowed by cosmology, independently of the halo model under consideration. The exception is the region with very large values of mA ∼ 1.8 TeV (not shown in the figure) where the relic density is in accord with the WMAP observation because the sleptons become very light. A…
Figure 18. The reach contours (i.e. the iso-VR=1 lines) for various dark matter detection tech￾niques in the (mA, µ) plane. Points lying to the bottom-left of the lines are within reach of the future experimental facilities, as described in Sec. 2.3. The black dashed line indicates the param￾eter space of the NUHM1 model in this plane, while the red cross locates the mSUGRA universal case. proton spin-independent scattering cross section σ SI Zf1p as a function of ∆mH, together with the current experimental limit and the projected sensitivity of Stage-2 and Stage-3 detectors. In both cases, σ…
Figure 19. The same as in
Figure 20. The neutralino-proton spin-independent scattering cross section σ SI Zf1p as a function of ∆mH (black solid line), at m0 = 300 GeV. The other input parameters are specified in the figure. The dotted red line indicates the current 90% CL exclusion limit on σ SI Zf1p delivered by the CDMS experiment [59], while the blue dashed lines and the green dot-dashed lines correspond to the projected 90%CL exclusion limits for Stage-2 and Stage-3 detectors, taking as benchmark experiments the next-generation CDMS-II detector and the XENON-1 ton facility. 5550 5575 5600 5625 5650 ∆mH (GeV)…
Figure 21. Same as in Fig.20, but at m0 = 1450 GeV. promising in the present setup, as they will entirely probe the WMAP-allowed region for both values of m0. In the m0 = 1450 GeV scenario (
Figure 22. The flux of muons from the Sun generated by charged current interactions of neutrinos produced in the center of the celestial body by neutralino-pair annihilations, integrated above a 1 GeV threshold (solid black line), as a function of ∆mH (black solid line), at m0 = 300 GeV, with other parameters as specified in the figure. The red dotted curves indicate the current 90% CL Super-Kamiokande limits on the muon flux from the Sun, while the dashed blue lines the expected 90% CL IceCube sensitivity. We corrected for the energy threshold mismatch in the computation of the projected…
Figure 24. The Dark Matter detection Visibility Ratios (VR) for various detection strategies, as a function of the GUT-scale Higgs mass splitting ∆mH, at m0 = 300 GeV. The other input parameters are specified in the figure. When the VR is above the “Visibility Threshold” (i.e. the VR=1 line) the corresponding model is within the reach of the corresponding dark matter search experiment. 5550 5575 5600 5625 5650 ∆mH (GeV) 10-5 10-4 10-3 10-2 10-1 100 101 102 103 104 Direct Detection, Z~ 1 p SI, on CDMS-II Direct Detection, Z~ 1 p SI, on XENON Muons f/Sun, on IceCube Antideuterons, on GAPS/Earth…
Figure 25. Same as in Fig.24, but at m0 = 1450 GeV. 3.4 NUHM2 model: Collider searches for SUSY In this section, we illustrate aspects of the NUHM2 model that lead to collider search possibilities not possible in the NUHM1 model. We illustrate our points by showing in
Figure 26. Approximate reach of the CERN LHC (100 fb−1 ) and ILC for supersymmetric matter in the NUHM2 model in the m0 vs. m1/2 plane for tan β = 10, A0 = 0, µ > 0 and mt = 178 GeV, for a) µ = 500 GeV, mA = 500 GeV and b) µ = 300 GeV, mA = 300 GeV. 4. Concluding Remarks We have examined the phenomenological implications of gravity-mediated SUSY breaking models with universal matter scalars, but with non-universal Higgs soft SUSY breaking masses. For simplicity, we assume a common GUT scale mass parameter for all matter scalars – this guarantees that phenomenological constraints from flavor…

Showing 24 of the paper's 26 figures. See all figures in the PDF ↗ Figures reproduced from arXiv:hep-ph/0504001 by the authors.

References
How later papers used it

47 later papers cite it

Evidence: some. 25 of the citing papers share no author with it, and 2 of those carry a confident label from Pith's citation classifier.

Pith read 11 of the 65 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

Uses its method or tool 1 of 4 papers with this label · 1 by the same authors

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How the literature uses it

46 arXiv papers cite this in 64 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

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