{"id":"56d004f2-7897-440f-88b5-bf8714ec8f3b","arxiv_id":"astro-ph/0003365","paper_version":2,"verdict":"CONDITIONAL","confidence":"HIGH","novelty_score":6.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":0,"one_line_summary":"Ultra-light scalar dark matter at m ~ 10^-22 eV, behaving as a coherent wave, suppresses small-scale structure and forms kpc-scale cores, potentially solving the cusp-core and missing-satellite problems of cold dark matter.","lead":"The paper proposes that dark matter made of ultra-light particles (about 10^-22 eV) would have wave properties that smooth out the small-scale problems of cold dark matter: cuspy halo cores and too many dwarf galaxies. It gives the analytic scaling, a linear power-spectrum cutoff, and one-dimensional simulations as a first test.","discovery_kind":"new_application","skeptic_critique":{"model":"selfhosted/deepseek-v4.1-flash","headline":"The load-bearing soft spot is the single-mass coincidence: one m ~ 10^-22 eV must give both kpc cores and the dwarf-abundance cutoff, yet Eq. (6) is used outside its stated regime for M <~ 10^10 M_sun, and cited numbers imply a factor ~2-10 tension in the required mass.","rationale":"The paper is the founding statement of fuzzy/wave dark matter, and its analytic core — the Jeans scale as the geometric mean of dynamical and Compton scales, Eq. (4), properly attributed to Khlopov-Malomed-Zel'dovich (1985) and Sin (1994) — is sound. The genuinely new content is the specific mass window, the linear transfer function Eq. (8), and the 1D Schrödinger-Poisson simulations. The reader's verdict of CONDITIONAL at HIGH confidence is appropriate. I agree partially with the reader's weakest_assumption: the transfer fit is a real soft spot, but it is not the most load-bearing one, because the qualitative sharp cutoff follows analytically from k_Jeq and survives order-unity changes in the fit. The more load-bearing concern is the coincidence claim: the abstract promises that one m solves both the core and abundance problems, and the paper's own numbers and cited comparisons (Kamionkowski-Liddle 4.5 h/Mpc; White-Croft 2 h/Mpc) imply required masses that differ by factors of a few to ~10 from the value that gives kpc cores. The paper acknowledges that 'whether the required masses actually coincide in detail can only be addressed by simulations,' and that 3D simulations are required; these are honest limitations, and I do not present them as new findings. What remains unresolved is the unquantified 'mild effect' of the Eq. (6) regime violation in the dwarf regime, and the size of the coincidence tension. Neither is fatal to the proposal, which is appropriately hedged ('might be solved'), and neither moves the verdict. One metadata anomaly: the manuscript header reads 'Revised November 26, 2024' on an arXiv v2 dated 26 Mar 2000; this does not affect the physics but is worth noting as an inserted passage.","tokens_in":8488,"tokens_out":11757,"duration_ms":222289,"concrete_test":"Compute the pair (r_core at M = 10^9 M_sun, k_1/2) as a function of m_22 and check whether a single m_22 in [0.3, 3] lands both in the observed windows. For r_core, solve r_J(r) = r self-consistently with the full NFW enclosed mass (Eq. 5), without the r^-1 approximation, and compare to Eq. (6). For k_1/2, integrate the GDM equations numerically with the Eq. (7) sound speed, using both the sharp matching and a smooth interpolation, and compare to Eq. (9). If the self-consistent r_core at M = 10^9 M_sun differs from Eq. (6) by more than ~50%, or if k_1/2 shifts enough to move the required m_22 by more than a factor ~2, the single-mass coincidence claim weakens.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The abstract's plural claim — 'these problems might be solved' — requires a single m ~ 10^-22 eV to deliver both kpc-scale cores and the linear cutoff that suppresses dwarf abundances. The core prediction is Eq. (6), derived by setting r_J(r) = r with the NFW enclosed density under the assumption r_Jh << r_v/c. The paper concedes this 'is technically violated for M10 <~ 1' — i.e., for M <~ 10^10 M_sun, precisely the dwarf-spheroidal regime where the cusp problem is most acute — and asserts 'only a mild effect' without quantifying it. The abundance side, Eq. (9), gives k_1/2 = 4.5 m_22^{4/9} Mpc^-1. Matching Kamionkowski-Liddle's suggested 4.5 h/Mpc (~2.9 Mpc^-1) requires m_22 ~ 0.4; matching White-Croft's 2 h/Mpc requires m_22 ~ 0.06; whereas kpc cores at M ~ 10^8-10^9 M_sun want m_22 of several. The required masses therefore do not obviously coincide, and the paper's own cited comparisons point to tension rather than agreement. This is not a fatal flaw — the qualitative suppression of cusps survives any order-unity shift — but the quantitative coincidence is the paper's distinctive claim and its least secure link. The reader's focus on the transfer fit (Eq. 8) is related but secondary: the fit's accuracy moves k_1/2 at the order-unity level, which is exactly the level at which the coincidence is already strained. The authors do acknowledge that 'whether the required masses actually coincide in detail can only be addressed by simulations,' so this is a gap they flag; the concern is that the gap is wider than the text implies.","agreement_with_reader":"partial"},"referee_report":{"model":"selfhosted/deepseek-v4.1-flash","summary":"The manuscript proposes fuzzy cold dark matter (FCDM): ultra-light scalar particles (m ~ 10^-22 eV) in a Bose-Einstein condensate, whose wave nature supplies a Jeans/de Broglie scale that stabilizes gravitational collapse on small scales. The authors derive the Jeans scale as the geometric mean of the dynamical and Compton scales (Eq. 4), estimate the halo core radius from the NFW profile (Eq. 6), compute the linear transfer function with a sharp cutoff at k_1/2 ~ 4.5 Mpc^-1 (Eqs. 8-9), discuss implications for dwarf-galaxy abundance, first objects, and reionization, and present 1D simulations (Fig. 1) showing cores rather than cusps. The central claim is that a single m ~ 10^-22 eV can address both the cusp and the dwarf-abundance problems without invoking new dark matter interactions.","tokens_in":8893,"tokens_out":17434,"duration_ms":318589,"significance":"If correct, this is an elegant and influential proposal: it addresses the small-scale shortcomings of CDM with free particles only, and it makes falsifiable predictions. The analytic Jeans scale (Eq. 4) is clean and correct, and the rho^{-1/4} density dependence gives a testable relation between core radii in objects of different characteristic density. The sharp linear cutoff (Eq. 9) is a distinctive prediction, and the paper is appropriately explicit that 3D simulations are needed. The proposal has been widely taken up. The main open question is whether one mass really delivers both the kpc cores and the dwarf-abundance cutoff.","major_comments":[{"comment":"The intermediate expression k_1/2 ~ 12 k_Jeq m_22^{-1/18} is inconsistent with the final result 4.5 m_22^{4/9} Mpc^-1. With k_Jeq = 9 m_22^{1/2} Mpc^-1 as stated two sentences earlier, 12 k_Jeq = 108 m_22^{4/9} Mpc^-1, a factor of 24 larger than 4.5. Evaluating the fit T_F = cos(x^3)/(1+x^8) at half power gives x ~ 0.78, i.e. k_1/2 ~ 0.5 k_Jeq m_22^{-1/18} ~ 4.4 m_22^{4/9} Mpc^-1, so the final number is right and the coefficient '12' should be about 0.5. Please correct the intermediate expression, since Eq. (9) is the number compared to the dwarf-abundance requirement.","section":"Linear Perturbations, Eq. (9)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The derivation assumes r_Jh << r_v/c, and the text concedes this 'is technically violated for M10 <~ 1' -- precisely the dwarf-spheroidal regime where the cusp problem is most acute -- while asserting 'only a mild effect' without quantification. Please provide a quantitative estimate of the correction for M ~ 10^8-10^9 M_sun, or state the domain of validity of Eq. (6) explicitly and carry the caveat into the abstract-level claim.","section":"Jeans / de Broglie Scale, Eq. (6)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The paper compares its k_1/2 ~ 4.5 Mpc^-1 to Kamionkowski-Liddle's 4.5h Mpc^-1 and White-Croft's 2h Mpc^-1 without noting the h factor; for h ~ 0.7 these are ~3.2 and ~1.4 Mpc^-1, implying m_22 ~ 0.5 and ~0.07 respectively, whereas kpc cores at M ~ 10^8-10^9 M_sun want m_22 of a few. The paper says the abundance problem 'may' be solved 'as well' and defers to simulations, but the quantitative coincidence is the distinctive claim and the cited numbers point to a factor of a few to an order of magnitude tension. Please state this tension explicitly rather than leaving it implicit.","section":"Low Mass Halos, comparison to [2] and [16]","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The matching of the effective sound speed in Eq. (7) is asserted to have a negligible effect ('We have verified...') but the verification is not displayed, and the transfer function Eq. (8) is a numerical fit with no stated accuracy. Since k_1/2 is the number that matters for the abundance comparison, please show the verification or state the fit's accuracy. In addition, the form cos(x^3)/(1+x^8) produces zeros in T_F (e.g. at x^3 = pi/2); please state whether these zeros are physical or an artifact of the fitting form.","section":"Linear Perturbations, Eqs. (7)-(8)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The nonlinear claim that FCDM produces cores rather than cusps rests on 1D simulations with idealized initial conditions (a single sine mode, real psi, psi=0 boundaries). The authors are explicit that 3D simulations are required, but the abstract's 'providing halo cores' is stronger than the 1D evidence supports. Please qualify the abstract and discussion accordingly, or add a 2D/3D check if feasible.","section":"Live Halos, Fig. 1","authors_acknowledge":null,"authors_acknowledge_p":null}],"minor_comments":[{"comment":"There are spacing artifacts from typesetting (e.g. 'structur e', 'sol ved', 'interact ions', 'co vari ant', 'feature s', 'teste d', 'gravi tating'); please proofread the final version.","section":"Throughout","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"Reference [4] lists Peebles' preprint as astro-ph/9911103, the same identifier given for [2] Kamionkowski & Liddle; the correct Peebles identifier is likely astro-ph/0002495. Please check.","section":"References [2] and [4]","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"Reference [22] is missing a period after 'Lett', and [24] reads 'Astrophs' for 'Astrophys'. Please correct.","section":"References [22] and [24]","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The header 'Revised November 26, 2024' is inconsistent with the arXiv v2 date of 26 Mar 2000; please correct or explain.","section":"Header","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"'initially in a (cold) Bose-Einstein condensate' -- please clarify whether the BEC assumption is essential to the proposal or merely a convenient description, and whether the field is assumed to be in the ground state.","section":"Abstract","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"Fig. 1 shows only two snapshots (t/t_dyn = 99 and 100); the claim of continuous evolution on t_dyn would be better supported by a time sequence or by a quantitative measure of the variability.","section":"Fig. 1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The hydrogen-atom analogy is loose: atomic stability is a kinetic-energy/uncertainty tradeoff, not literally the same mechanism as the Jeans-scale stabilization; please soften or qualify.","section":"Introduction","authors_acknowledge":null,"authors_acknowledge_p":null}],"recommendation":"minor_revision","confidential_remarks":"The paper is a Letter and appropriately hedged; the referee should not demand the 3D simulations the authors already say are needed. The main request is to make the single-mass tension explicit and to fix the Eq. (9) coefficient, not to resolve the coincidence here. The duplicate arXiv identifier in Ref. [4] should be caught in proof."},"author_rebuttal":null,"desk_editor":{"model":"selfhosted/deepseek-v4.1-flash","letter":"Short version: this is the paper that started wave/fuzzy dark matter, and most of it holds up. The one thing to watch is arithmetic the authors half-acknowledge — their own scaling relations want two different particle masses for the two problems they claim to solve at once. That is the real soft spot, not the transfer-function fit the reader flagged first (that one is order-unity and secondary). The stress-test note has this right, and I'd weight it more heavily than the Pith report does. Note also that the report's 'limitations the authors state: none found' is wrong; the paper states several, including that 3D simulations are required and that Eq. (6) is used outside its stated regime for M <~ 10^10 M_sun. Credit them for saying so, then push on whether the gap is as small as they imply. Run the numbers: Eq. (9) gives k_1/2 = 4.5 m_22^{4/9} Mpc^-1, so matching Kamionkowski-Liddle's ~2.9 Mpc^-1 needs m_22 ~ 0.4, and White-Croft's ~1.3 Mpc^-1 needs m_22 ~ 0.06. Meanwhile Eq. (6) at M ~ 10^9 M_sun gives a kpc core only for m_22 of several. Those are not the same mass, and the mismatch is a factor of ten to twenty, not a detail. The qualitative claim — that wave pressure suppresses cusps and cuts small-scale power — survives any order-unity shift, so this is a quantitative-coincidence problem, not a fatal one. What is genuinely new and well done: the specific 10^-22 eV window, the geometric-mean/de Broglie reading of the Jeans scale (cleanly derived, and correctly attributed to Khlopov-Malomed-Zel'dovich 1985 and Sin 1994), the generalized-dark-matter mapping with c_eff^2 = k^2/4a^2m^2 in Eq. (7) — that is a reusable trick the field still uses — the transfer fit in Eq. (8), and the 1D Schrodinger-Poisson runs showing cores and interference. The 1D simulations are crude but they are real evidence, and the paper is honest about their limits. Minor: the matching verification in Eq. (7) is asserted, not shown; the dateline 'Revised November 26, 2024' on a 2000 v2 is inconsistent and worth a query to the authors. Who should read it: anyone working on small-scale CDM problems or light dark matter; it is the reference you cite for the mass window. Yes, send it to referees — it is a well-posed proposal with a checkable numerical tension, which is exactly what referee time is for.","headline":"The founding fuzzy-dark-matter paper, and the analytic core holds up — but the authors' own Eqs. (6) and (9) pull the required particle mass apart by roughly an order of magnitude, and the text treats that as a detail for future simulations.","tokens_in":9561,"tokens_out":2432,"would_cite":true,"duration_ms":41503,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"pith_extraction":{"msc":[],"pacs":["95.35.+d"],"model":"selfhosted/deepseek-v4.1-flash","headline":"Ultra-light dark matter, with a mass around $10^{-22}$ eV, would behave as a wave on galactic scales, and that wave behaviour alone could remove the small-scale failures of cold dark matter without any new particle interactions.","keywords":["fuzzy dark matter","ultra-light scalar field","Bose-Einstein condensate","Jeans scale","de Broglie wavelength","cusp-core problem","dwarf galaxies","linear power spectrum cutoff"],"falsifier":"A measurement of the linear power-spectrum cutoff, from high-redshift galaxy counts or the Lyman-$\\alpha$ forest, that sits well away from $k_{1/2} ≈ 4.5$ Mpc$^{-1}$, or high-resolution rotation curves showing core radii that do not scale with characteristic density as $ρ^{-1/4}$, would settle the proposal against it.","tokens_in":9830,"feed_emoji":"🌌","tokens_out":3374,"duration_ms":67364,"temperature":0.7,"pith_summary":"Cold dark matter reproduces the large-scale universe well but predicts more small-scale structure than observers see: density cusps at the centres of halos and a larger population of low-mass halos than the dwarf galaxies of the Local Group suggest. Hu, Barkana and Gruzinov ask whether both problems can be cured by making the dark matter particle extraordinarily light, around $10^{-22}$ eV, so that its de Broglie wavelength is of order a kiloparsec. In that regime the dark matter is a classical scalar field in a Bose-Einstein condensate, and its wave nature resists compression below a Jeans scale for the same reason the uncertainty principle keeps an electron from falling into a nucleus. The authors show analytically that this scale lands near the core radii inferred for dwarf galaxies, and that the same field produces a sharp cut in the linear power spectrum near $k=4.5$ Mpc$^{-1}$, close to the cutoff others had argued is needed to thin out low-mass halos. The appeal is economy: the successes of cold dark matter are retained and the failures are addressed by one parameter, the particle mass, with no self-interactions and no new forces.","feed_headline":"Wave-like dark matter could erase cold dark matter's small-scale flaws","feed_subtitle":"Particles of 10^-22 eV would blur kpc-scale cusps and thin out the dwarf galaxy population.","key_machinery":"The load-bearing object is the Jeans scale of a self-gravitating scalar field, obtained by balancing the gravitational growth rate $γ^2 = 4πGρ$ against the free-field oscillation rate $(k^2/2m)^2$, which gives $r_J = π^{3/4}(Gρ)^{-1/4}m^{-1/2}$. The authors then re-express the scalar field as a relativistic imperfect fluid with an effective sound speed $c_eff^2 = 1$ at early times (while the field is slowly rolling, $a ≤ k/2m$) and $c_eff^2 = k^2/4a^2m^2$ afterwards, solve the standard linear theory with radiation and baryons, and fit the resulting suppression as $P_FCDM(k) = T_F^2(k)P_CDM(k)$ with $T_F ≈ cos(x^3)/(1+x^8)$ and $x = 1.61 m_{22}^{-1/18}k/k_Jeq$. That transfer function is what converts the microscopic wave picture into a falsifiable statement about the linear power spectrum and hence about halo abundance.","core_discovery":"The paper's central claim is that a dark matter particle of mass $m$ around $10^{-22}$ eV, treated as a self-gravitating classical scalar field obeying the nonlinear Schrödinger equation, has a Jeans scale $r_J = 3.6 m_{22}^{-1/2}(Gρ)^{-1/4}$-type scaling, explicitly $r_J = π^{3/4}(Gρ)^{-1/4}m^{-1/2} ≈ 55 m_{22}^{-1/2}(ρ/ρ_b)^{-1/4}(Ω_m h^2)^{-1/4}$ kpc, below which gravitational collapse is stabilised. Because this scale is the geometric mean of the dynamical scale and the Compton wavelength, it is the de Broglie wavelength of the ground state of a particle in the potential well, so the stabilisation is the uncertainty principle at work rather than any new force. The authors argue that for $m ≈ 10^{-22}$ eV the scale falls near the kiloparsec cores where cold dark matter simulations predict cusps, and that the same field suppresses linear power sharply, by a factor of two at $k_{1/2} ≈ 4.5 m_{22}^{4/9}$ Mpc$^{-1}$, which is roughly the scale others had argued would reduce the excess abundance of low-mass halos. They support the picture with one-dimensional simulations in which a bound halo forms without the cusp seen in the cold dark matter comparison run, while the density shows interference features that evolve on the dynamical time.","pith_inferences":["The proposal's real test is a joint one: a single mass must simultaneously reproduce the core sizes of dwarf spheroidals and the cutoff in the halo mass function. Either success alone is weak; the coincidence of the two is the claim worth checking.","Because the cutoff in linear power is sharp and nearly scale-independent in comoving coordinates, high-redshift galaxy counts or the Lyman-alpha forest can constrain $m$ independently of any rotation-curve measurement, giving two handles on one number.","The interference-driven time variation of the potential is a channel for transferring energy to baryons; it could plausibly puff up gas in dwarfs and push the field toward its ground state, which connects this proposal to the same core and satellite problems that motivate it.","The posted text carries a revision date decades after the original preprint, so the numerical coefficients quoted here, particularly the transfer-function fit and the half-power wavenumber, are worth checking against the original version before being used as fixed targets."],"forward_implications":["Halo density profiles should turn over at the Jeans scale instead of continuing as $r^{-1}$ cusps down to the resolution limit, with the turnover radius scaling as $ρ^{-1/4}$ across objects of different characteristic density.","The abundance of low-mass halos should be sharply reduced relative to cold dark matter, with consequences for the dwarf galaxy luminosity function in the Local Group.","Star formation at high redshift should shift to more massive objects, potentially delaying reionization and reducing the number of galaxies detectable before it by a factor of a few.","Density profiles on scales near the Jeans length should be non-universal and should evolve continuously on the dynamical time through interference, while rotation curves, which respond to the smoother gravitational potential, stay comparatively steady.","Choosing the particle mass to match the core radius of one class of dark-matter-dominated objects fixes the core radius of another class, given the ratio of their densities, which is a relation that can be checked against data."],"supporting_citations":[{"why":"Earlier derivation of the Jeans scale for a scalar-field dark matter component, which the paper recovers in a simpler form.","marker":"[10]"},{"why":"Supplies the Navarro-Frenk-White halo profile whose $r^{-1}$ cusp the Jeans scale is claimed to remove.","marker":"[11]"},{"why":"Provides the generalized dark matter fluid mapping used to evolve the scalar field linearly inside and outside the horizon.","marker":"[12]"},{"why":"Argues that a sharp cutoff near $k = 4.5h$ Mpc$^{-1}$ in the initial power spectrum could solve the low-mass halo abundance problem, the coincidence the paper leans on.","marker":"[2]"},{"why":"Simulations of cold dark matter with a smooth power-spectrum cutoff, used to calibrate how much reduction in low-mass halos a given cutoff produces.","marker":"[16]"},{"why":"Earlier treatment of halo dark matter as stationary energy states of an ultra-light field, background for the ground-state interpretation of the Jeans scale.","marker":"[8]"},{"why":"The self-interacting dark matter alternative whose extra interactions this proposal aims to avoid.","marker":"[1]"},{"why":"Warm dark matter free-streaming alternative, the baseline small-scale suppression mechanism the paper compares against.","marker":"[3]"}],"fun_headline_variants":["Ultralight scalar dark matter cores replace cold dark matter cusps","10^-22 eV dark matter blurs kpc cusps in 1D simulations","Bose-Einstein condensate dark matter suppresses small-scale power","Uncertainty principle stabilizes dark matter halos, no new force","Fuzzy dark matter matches dwarf cores without particle interactions"],"cache_read_input_tokens":0,"weakest_assumption_plain":"The claim depends on the effective sound-speed matching and the fitted transfer function placing the linear cutoff at the right scale, and the paper says the matching details were checked but does not show that check.","fun_headline_variants_meta":{"raw":{"variants":["Ultralight scalar dark matter cores replace cold dark matter cusps","10^-22 eV dark matter blurs kpc cusps in 1D simulations","Bose-Einstein condensate dark matter suppresses small-scale power","Uncertainty principle stabilizes dark matter halos, no new force","Fuzzy dark matter matches dwarf cores without particle interactions"]},"model":"selfhosted/deepseek-v4.1-flash","effort":"low","attempts":1,"cost_usd":0.0,"raw_usage":{"total_tokens":2210,"prompt_tokens":942,"completion_tokens":1268,"prompt_tokens_details":null,"completion_tokens_details":{"reasoning_tokens":1186}},"tokens_in":942,"tokens_out":1268,"duration_ms":25868,"image_pages":[],"temperature":1.0,"reasoning_budget":50,"reasoning_tokens":1186,"transport_provider":"selfhosted","cache_read_input_tokens":0,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-10-29T18:14:13.544398+00:00","model_set":{"reader":"selfhosted/deepseek-v4.1-flash"},"falsifier":"A measurement of the linear power-spectrum cutoff, from high-redshift galaxy counts or the Lyman-$\\alpha$ forest, that sits well away from $k_{1/2} ≈ 4.5$ Mpc$^{-1}$, or high-resolution rotation curves showing core radii that do not scale with characteristic density as $ρ^{-1/4}$, would settle the proposal against it.","supporting_citations":[{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Earlier derivation of the Jeans scale for a scalar-field dark matter component, which the paper recovers in a simpler form."},{"cited_title":"Astrophys. J. 490, 493","cited_arxiv_id":null,"evidence_quote":"Supplies the Navarro-Frenk-White halo profile whose $r^{-1}$ cusp the Jeans scale is claimed to remove."},{"cited_title":"Astrophys. J. 506, 485","cited_arxiv_id":null,"evidence_quote":"Provides the generalized dark matter fluid mapping used to evolve the scalar field linearly inside and outside the horizon."},{"cited_title":"Suppressing Linear Power on Dwarf Galaxy Halo Scales","cited_arxiv_id":"astro-ph/0001247","evidence_quote":"Simulations of cold dark matter with a smooth power-spectrum cutoff, used to calibrate how much reduction in low-mass halos a given cutoff produces."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Earlier treatment of halo dark matter as stationary energy states of an ultra-light field, background for the ground-state interpretation of the Jeans scale."},{"cited_title":"Observational evidence for self-interacting cold dark matter","cited_arxiv_id":"astro-ph/9909386","evidence_quote":"The self-interacting dark matter alternative whose extra interactions this proposal aims to avoid."},{"cited_title":"New Dark Matter Physics: Clues from Halo Structure","cited_arxiv_id":"astro-ph/0002330","evidence_quote":"Warm dark matter free-streaming alternative, the baseline small-scale suppression mechanism the paper compares against."}],"review_version":1}