{"id":"e69c46f2-543c-4b01-9abc-679730488218","arxiv_id":"astro-ph/0110561","paper_version":2,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":6.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":4,"one_line_summary":"A gravothermal fluid model of self-interacting dark matter halos gives a self-similar r^-2.19 profile, a core collapse time near 290 relaxation times, and a late-time dense inner core whose mass loss slows enough to leave a black hole seed.","lead":"Treating a self-interacting dark matter halo as a heat-conducting fluid, the authors derive a self-similar density profile falling as r^-2.19 and a core collapse time of about 290 relaxation times, longer than the Hubble time for present-day dwarf-scale cores. The model explains why such halos have flat cores today and how a dense inner core could survive long enough to become a black hole seed at high redshift.","discovery_kind":"new_application","skeptic_critique":{"model":"selfhosted/deepseek-v4.1-flash","headline":"The reader's weakest_assumption (Eq. 14) is real but targets the paper's secondary claims; the central 290 t_r result follows from the lmfp self-similar solution alone, so CONDITIONAL stands but for a different reason.","rationale":"The reader's rationale is thorough and correctly identifies the lmfp results as solid: the ODE system is a clean adaptation of Lynden-Bell & Eggleton, the eigenvalues in Table 1 are mutually consistent, and Fig. 2 reproduces α = 2.1896. The reader's weakest_assumption (Eq. 14) is a real unacknowledged limitation, but it targets the secondary claims (double core, ζ, BH seed mass), not the central claim. The verdict CONDITIONAL is appropriate, but the weakest_assumption should be the lmfp initial condition assumption (§5), not Eq. (14). The paper's own §6 acknowledges that smfp initial conditions give short lifetimes (Quinlan 1996), so the central claim is conditional on the lmfp initial condition, which is argued but not demonstrated. I would keep the verdict at CONDITIONAL but shift the emphasis.","tokens_in":22644,"tokens_out":10996,"duration_ms":189642,"concrete_test":"Re-derive the 290 t_r result from Eqs. (12) and (17)-(22) alone, without Eq. (14). If the result is unchanged, the reader's concern does not threaten the central claim. Alternatively, run the time-dependent calculation with an initial condition that has λ/H < 1 in the core (e.g., Hernquist profile with Burkert 2000 parameters) and check whether the collapse time is much shorter than 290 t_r; if so, the central claim's applicability depends on the lmfp initial condition.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The central claim (abstract:s5) is derived from the lmfp flux (Eq. 12) and the self-similar ODE system (Eqs. 17-22), which do not use Eq. (14). The reader's concern about Eq. (14) is valid for the late-time results (double core, ζ ≈ -0.175, BH seed mass), which the paper itself flags as extrapolations. The actual soft spot for the central claim is the lmfp initial condition assumption in §5: 'By hypothesis, we assume that a SIDM halo is initially dilute enough to be in the lmfp limit.' The paper argues for this in §6, but the argument is not airtight: it dismisses the N-body evidence for smfp cores (Burkert 2000, Kochanek & White 2000) as using inappropriate Hernquist initial conditions, and cites the N-body evidence for lmfp cores (Yoshida et al. 2000, Davé et al. 2001) as supporting its assumption, while also describing those simulations as having insufficient resolution to resolve the core. If SIDM halos form with smfp cores, the 290 t_r result does not apply, and the paper's own §6 (citing Quinlan 1996) says such systems have lifetimes of only a few relaxation times.","agreement_with_reader":"partial"},"referee_report":{"model":"selfhosted/deepseek-v4.1-flash","summary":"The manuscript applies the gravothermal fluid formalism, originally developed for globular clusters, to an isolated spherical halo of self-interacting dark matter. The authors derive a self-similar solution for the long-mean-free-path (lmfp) limit by solving the ODE system of Eqs. (17)-(22) with the boundary conditions of Eqs. (21)-(22), obtaining eigenvalues that fix the halo profile (rho ∝ r^-2.19), the core-mass/central-temperature relation (d log M_c / d log v_c^2 ≈ -4.27), and the collapse time t_coll ≈ 290 t_r (Table 1, Figure 1). They then integrate the full time-dependent diffusion problem of Eqs. (34)-(36), using Eq. (14) to interpolate between the short- and long-mean-free-path conductivities, and show that the contracting core inevitably reaches λ/H < 1, at which point it splits into a dense, collisional inner core and a nearly static outer core, with mass loss from the inner core substantially reduced. The headline conclusion is that for a present-day dwarf-scale core (ρ_c ≈ 0.02 M_sun pc^-3, v_c ≲ 10^7 cm s^-1, σ ≈ 1 cm^2 g^-1) t_coll exceeds the Hubble time, so flat cores at the present epoch are consistent with SIDM, while high-redshift halos may collapse and seed black holes.","tokens_in":22904,"tokens_out":9074,"duration_ms":173053,"significance":"The paper's central result is a clean, parameter-free derivation: the lmfp self-similar solution follows from the stated ODE system and boundary conditions, the eigenvalues in Table 1 are internally consistent with the quoted exponents (α = 2.190, ζ = 0.7655, t_coll/t_r ≈ 291), and the time-dependent run of Figure 2 reproduces α = 2.1896. The dimensional structure of Eqs. (9), (12), (13) and (14) checks out, and the reduction of Eq. (14) to the two limiting forms is correct. The paper also makes falsifiable predictions — ρ ∝ r^-2.19 in the extended halo and t_coll ≈ 290 t_r — and is candid that r^-2.19 is not easily distinguished from the CDM range r^-2 to r^-3. The comparison with the globular-cluster case in Table 1 is a useful calibration, and the physical picture of a double core with surface-limited mass loss is a genuine extension of what the N-body simulations of Burkert (2000) and Kochanek & White (2000) could resolve. The late-time black-hole-seed claim is more speculative and rests on an acknowledged extrapolation.","major_comments":[{"comment":"The time-dependent calculation adopts the lmfp self-similar profile as its initial condition explicitly 'by hypothesis,' and the 290 t_r collapse time quoted in the abstract (abstract:s5) inherits that choice. §6 defends the choice by arguing that Burkert (2000) and Kochanek & White (2000) used Hernquist initial conditions that already place part of the core in the smfp regime, while simultaneously stating that Yoshida et al. (2000) and Davé et al. (2001) lack the resolution to resolve the core. Both branches of the argument are therefore weaker than the text implies: the first establishes only that those particular initial conditions are inappropriate, not that lmfp formation is generic, and the second cannot supply positive evidence for it. A concrete test would be to rerun the §5 integration from an initial state with λ/H < 1 in the core (for example a Hernquist-like cusp of the same total mass) and report how t_coll, the r^-2.19 halo, and the double-core structure change. If the collapse time moves by a large factor, the abstract's 'longer than the Hubble time' statement should be conditioned on the lmfp assumption explicitly rather than presented as generic.","section":"§5, opening paragraph; §6","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"Eq. (14) combines the smfp and lmfp conductivities in series, and every result in §5.2-5.3 — the double core, the reduced mass-loss rate, the asymptotic ζ ≈ -0.175, and the 'appreciable' inner-core mass at relativistic onset (abstract:s7) — lives in the transition region λ ~ H where neither limiting form applies. The paper acknowledges that the combined form 'arises from our need to calculate heat diffusion,' but provides no kinetic-theory or Fokker-Planck check and no sensitivity study of the interpolation itself. A concrete test would be to repeat the aσ̂^2 = 10^-2 run with an alternative interpolation (for example a harmonic rather than series combination of the two conductivities, or a flux-limited diffusion form) and report whether ζ and the inner-core mass at fixed v_c^2 move by more than the stated uncertainty. If they do, the late-time claims should be softened to order-of-magnitude statements, and the abstract's black-hole-seed sentence should be qualified accordingly.","section":"§3, Eq. (14); §5.2-5.3","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The asymptotic ζ ≈ -0.175 is inferred from integrations terminated at v_c^2/v_c^2(0) of a few tens and then extrapolated over the 4-6 decades in central temperature needed to reach the relativistic instability. Figs. 9 and 10 show ζ still rising at termination, so the statement that it 'seems to settle asymptotically in the range -0.2 ≲ ζ ≲ -0.1' is an extrapolation rather than a measured asymptote. The paper flags this ('we infer that relation by a combination of physical reasoning and extrapolation'), which is appropriate, but the resulting inner-core mass at black-hole formation is then uncertain by an order of magnitude or more, since d log M_c / d log v_c^2 ≈ -0.85 compounds over the extrapolated range. A convergence study in zoning and time step, together with an explicit statement of how the predicted seed mass scales with the assumed ζ, would let the reader judge the claim. As written, the black-hole-seed statement in the abstract should be marked as an extrapolation.","section":"§5.3, Figs. 9-10","authors_acknowledge":null,"authors_acknowledge_p":null}],"minor_comments":[{"comment":"The collapse time is quoted as 291 t_r in Table 1, 290 t_r in the abstract and §2, and 289 t_r(0) in §5.1; these should be reconciled or the rounding explained.","section":"§4, Table 1; §5.1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The sentence attributing the smaller SIDM t_coll/t_r to 'the greater efficiency of energy transfer in clusters as reflected in the value of b' appears inverted relative to Eq. (30): b_GC = 0.675 < b_SIDM = 1.002 and ξ_e ∝ b, so the larger SIDM value of b produces the shorter collapse time. The sentence should be rephrased.","section":"§4, paragraph after Table 1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The λ/H sequence in the caption is non-monotonic (…, 7.0×10^-3, 3.0×10^-1, 2.1×10^-4), which appears to be a typographical error given that the text describes λ/H decreasing monotonically with time.","section":"Fig. 3 caption","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The fitted halo slope is quoted as ρ ∝ r^-2.1896, to four significant figures; the radial fit range and an uncertainty should be given instead.","section":"§5.1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The claim that 'the star cluster values set an upper (lower) limit on the value of α (ζ)' is a heuristic argument from the relative efficiency of diffusive versus single-collision energy transfer; it should be labelled as such rather than presented as a derived bound.","section":"§4","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The 'thin, exponential envelope' said to surround the inner core is asserted without a figure or a fit; either show the envelope in Fig. 4 or soften the description.","section":"§5.2","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The coefficient a = sqrt(16/π) ≈ 2.26 is specific to hard-sphere scattering with a Maxwell-Boltzmann distribution; since §2 notes that energy-dependent or inelastic cross sections are possible, it should say explicitly that the lmfp scaling and the 290 t_r coefficient change for such cross sections.","section":"§2, Eq. (3)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"Copy-editing is needed: 'typcially' (§2), 'extraplolaton' and 'whatsover' (§5.3), 'severly' and 'out results' (§6), 'labled' (Figs. 7-8), 'correspondance' (§5.2), 'the the' (§7), 'cental cental' (§5.3), and the 'Dav`e' spacing throughout the text and references.","section":"Throughout","authors_acknowledge":null,"authors_acknowledge_p":null}],"recommendation":"major_revision","confidential_remarks":"The manuscript is labelled 'ApJ in press, April 2002,' so the practical role of this report is limited; the substantive asks are sensitivity tests that could appear in a follow-up rather than changes to the present text. The lmfp self-similar solution and the 290 t_r result are sound and could stand as published; my major comments target the smfp/late-time claims (abstract:s7) and the initial-condition assumption, both of which the authors already flag as approximations but do not test quantitatively. The comparison with the N-body literature in §6 is somewhat selective in which simulations it credits with adequate resolution, and that asymmetry is worth watching in any revision."},"author_rebuttal":null,"desk_editor":{"model":"selfhosted/deepseek-v4.1-flash","letter":"The part worth your time is the collapse clock and the r^-2.19 profile. The lmfp eigenvalue problem is a direct port of Lynden-Bell & Eggleton with t_r proportional to (rho v)^-1 instead of v^3/rho, and the authors say so in Section 4. Table 1 is internally consistent: alpha = 2.190, zeta = 0.7655, t_coll/t_r about 291. The time-dependent run in Figure 2 lands on alpha = 2.1896. That is a real numerical check, not a claim. The 290 t_r number follows from it, and the conclusion that a present-day dwarf-scale core sits well above a Hubble time is a useful, defensible result. Genuinely new: the series-combined flux in Eq. (14), the double-core structure in Figures 3 to 5, and the reduced mass-loss exponent once the inner core goes smfp. The double core is a concrete prediction that N-body codes with better core resolution could confirm or kill. Where I would push. First, the reader's worry about Eq. (14) is real but it lands on the secondary claims, not the headline. The 290 t_r result comes out of the lmfp solution alone. The actual soft spot for the central claim is the hypothesis at the top of Section 5 that halos start in the lmfp regime. Section 6 argues this, but asymmetrically: it dismisses Burkert and Kochanek & White because their Hernquist initial conditions put part of the halo in the smfp regime, then cites Yoshida et al. and Dave et al. as support while also saying those simulations cannot resolve the core. You cannot have it both ways. And the paper's own citation of Quinlan (1996) says smfp-core systems live only a few relaxation times, which is exactly the case that would undercut the headline. Second, zeta of about -0.175 is read off the tracks with no error bar, and the core boundary definition shifts between the King radius and lambda/H = 1 mid-paper. The authors flag the late-time numbers as extrapolations, which is honest, but the black-hole seed mass argument inherits all of that. The paper is candid about scope: accretion, mergers, and angular momentum are omitted, and the integration cannot be carried to collapse. The classifier's 'no stated limitations' is wrong on that point. Who it is for: anyone working on SIDM or gravothermal evolution. It is the reference for the collapse-time argument. Send it out.","headline":"A clean gravothermal treatment: the 290 t_r collapse clock and the r^-2.19 profile hold up, but the late-time claims rest on an unvalidated interpolated flux and an assumed lmfp initial state.","tokens_in":23662,"tokens_out":1763,"would_cite":true,"duration_ms":33121,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"pith_extraction":{"msc":[],"pacs":["95.35.+d","97.60.Lf"],"model":"selfhosted/deepseek-v4.1-flash","headline":"A halo of self-interacting dark matter should settle into a flat core inside a halo falling as $r^{-2.19}$, and its centre should take roughly 290 relaxation times to collapse — longer than the age of the universe for present-day dwarf-galá","keywords":["self-interacting dark matter","gravothermal catastrophe","core collapse","dark matter halos","mean free path","gravothermal fluid model","black hole seeds","dwarf galaxy cores"],"falsifier":"A Boltzmann or Monte-Carlo simulation with enough particles to resolve the layer where the mean free path equals the scale height, run long enough to measure the inner core mass as a function of central velocity dispersion, would settle it: if the measured slope is close to the long-mean-free-path value of about $-4$ rather than the near-unity slope the paper predicts, the throttled mass loss and the large seed black hole mass both fail.","tokens_in":23932,"feed_emoji":"🌌","tokens_out":3500,"duration_ms":72181,"temperature":0.7,"pith_summary":"The paper asks whether dark matter particles that bounce off one another can produce the flat-centred halos observers infer, without those same centres having collapsed long ago. Treating the halo as a self-gravitating, heat-conducting fluid, the authors show that a core with the density and velocity dispersion of a typical dwarf galaxy relaxes in about a gigayear, far less than its age, so it should already have reached a gravothermal profile: a nearly homogeneous core inside an extended halo where the density falls as $r^{-2.19}$. Contraction then continues, and the paper's central number is that the core reaches a singular state after $t_{coll} = 290 t_r$; for observed core densities near $0.02 M_☉$ per cubic parsec and dispersions below $10^7$ cm/s, that is longer than the Hubble time. That matters because it converts a potential objection — that self-interacting dark matter should have collapsed by now — into a consistency argument, and because running the same evolution forward leaves an inner core massive enough to be worth counting when it finally becomes relativistically unstable.","feed_headline":"Dark matter cores take 290 relaxation times to collapse","feed_subtitle":"A fluid treatment predicts flat cores, halos falling as a fixed power law, and a slow collapse that keeps most of the core's mass.","key_machinery":"The machinery is the gravothermal fluid model: mass continuity, hydrostatic equilibrium, a heat-flux law, and the first law of thermodynamics written for a virialised gas whose 'temperature' is the one-dimensional velocity dispersion squared. The load-bearing object is the combined conduction flux, which puts the short-mean-free-path conductivity and the long-mean-free-path conductivity in series, so that one equation covers both limits and the transition between them. On top of this sit two analytic devices: the Lynden-Bell & Eggleton separation of variables, which yields the self-similar profiles and the eigenvalues $c_1$, $c_2$ that fix the exponents $α = 2.190$ and $ζ = 0.7655$; and the ratio $λ/H$ of mean free path to scale height, which is the bookkeeping variable that tells the reader which regime any mass shell is in and where the inner core's surface lies.","core_discovery":"The paper's claim is that an isolated, spherical halo of self-interacting dark matter evolves through two distinct regimes, and that the transition between them changes the fate of the core. In the long-mean-free-path regime, where the distance a particle travels between collisions exceeds the local gravitational scale height, the evolution equations admit a self-similar solution borrowed from the theory of globular star clusters. That solution gives a nearly isothermal, homogeneous core surrounded by a power-law halo with $ρ ∝ r^{-2.19}$, and a core that collapses in $t_{coll} ≈ 290 t_r$, with core mass falling roughly four orders of magnitude per order of magnitude of rising central temperature. Because the core's density grows much faster than its temperature, it inevitably becomes short-mean-free-path in its innermost region long before it becomes relativistic. The authors' time-dependent integrations then show the original core splitting into a dense, collisional inner core with a fairly sharp surface and a static outer remnant, with the luminosity peaking at the interface where $λ ≈ H$. In that state mass loss is strongly suppressed: the inner core loses of order one order of magnitude of mass per order of magnitude of central temperature, so an appreciable mass survives to the onset of relativistic instability and dynamical collapse to a black hole.","pith_inferences":["The paper's most fragile step is also its most productive one: the novel late-time results all live where $λ$ is comparable to $H$, exactly where the series interpolation of the two conductivities is least constrained by kinetic theory, so a Fokker-Planck or Monte-Carlo treatment of that layer is the natural next test.","If the reduced mass-loss rate holds, the black hole mass at collapse should scale weakly with the cross section — the paper's own empirical collapse of the tracks onto $M_c/\\hat{σ}^{0.6}$ hints at a near-universal relation that a higher-resolution simulation could check directly.","The self-similar slope of $r^{-2.19}$ is close enough to the cold-dark-matter slopes of $r^{-1}$ to $r^{-3}$ that it will be hard to discriminate on shape alone; the sharper discriminant is the presence of a genuinely homogeneous core whose central density has barely moved since virialisation.","The paper treats the halo in isolation; in a real cosmology, accretion and mergers inject energy at the core boundary on timescales shorter than the collapse time, which would stall the secular evolution and could keep cores flatter for longer than this model predicts."],"forward_implications":["Present-day halos with flat cores are consistent with self-interacting dark matter: their relaxation times are short enough to have thermalised them, while their collapse times exceed ten Hubble times.","The extended halo, if undisturbed, should carry a fixed power-law slope of about $r^{-2.19}$ that stays put while the core contracts.","A contracting core should develop a two-component structure — a collisional inner core with a sharp edge, plus a nearly static outer core — with the peak energy flux at the interface where $λ ≈ H$.","Because mass loss is throttled once the inner core is collisional, the seed black hole from the final dynamical collapse can be much more massive than the long-mean-free-path scaling would suggest.","Halos that formed at high redshift were denser, so their collapse times were shorter; the authors flag early collapse as a possible route to seed supermassive black holes, deferred to later work."],"supporting_citations":[{"why":"Supplies the self-similar separation-of-variables method and the eigenvalue structure that the paper adapts to a different relaxation-time law.","marker":"Lynden-Bell & Eggleton 1980"},{"why":"Origin of the gravothermal catastrophe and of the long-mean-free-path flux form used in the combined conduction equation.","marker":"Lynden-Bell & Wood 1968"},{"why":"Standard reference for the gravothermal formalism, the core-mass/energy relation defining $ζ$, and the evaporation-rate parameterisation.","marker":"Spitzer 1987"},{"why":"Provides the benchmark globular-cluster collapse time $t_{coll} ≈ 330 t_r$ against which the paper's $290 t_r$ is calibrated.","marker":"Cohn 1980"},{"why":"Fixes the hard-sphere collision rate coefficient $a = √(16/π)$ and the mean free path used throughout the relaxation-time estimates.","marker":"Reif 1965"},{"why":"The proposal under test: that self-interaction can flatten dark matter cores, which this paper tries to confirm or constrain.","marker":"Spergel & Steinhardt 2000"},{"why":"Isolated-halo N-body simulation used as the primary point of comparison for core contraction and profile flattening.","marker":"Burkert 2000"},{"why":"Cross-section survey whose short-lifetime conclusion the paper argues rests on an inappropriate initially cuspy, already-collisional initial condition.","marker":"Kochanek & White 2000"},{"why":"Cosmological SIDM simulations that set the preferred cross-section range and whose accretion argument the paper concedes would modify gravothermal evolution.","marker":"Davé et al. 2001"}],"fun_headline_variants":["Self-interacting dark matter cores collapse in roughly 290 relaxation times","SIDM halos form r^-2.19 profiles before gravothermal collapse","A fluid model gives 290 relaxation times for SIDM core collapse","Long mean free path yields self-similar SIDM halo profiles","Inner SIDM cores lose little mass before relativistic collapse"],"cache_read_input_tokens":0,"weakest_assumption_plain":"The single flux law that bridges the two collision regimes is built by placing the two conductivities in series, and the paper's distinctive late-time predictions — the double core, the throttled mass loss, the near-constant inner core mass — all sit in the crossover region where that interpolation has no independent kinetic-theory check.","fun_headline_variants_meta":{"raw":{"variants":["Self-interacting dark matter cores collapse in roughly 290 relaxation times","SIDM halos form r^-2.19 profiles before gravothermal collapse","A fluid model gives 290 relaxation times for SIDM core collapse","Long mean free path yields self-similar SIDM halo profiles","Inner SIDM cores lose little mass before relativistic collapse"]},"model":"selfhosted/deepseek-v4.1-flash","effort":"low","attempts":1,"cost_usd":0.0,"raw_usage":{"total_tokens":2324,"prompt_tokens":1104,"completion_tokens":1220,"prompt_tokens_details":null,"completion_tokens_details":{"reasoning_tokens":1140}},"tokens_in":1104,"tokens_out":1220,"duration_ms":22152,"image_pages":[],"temperature":1.0,"reasoning_budget":50,"reasoning_tokens":1140,"transport_provider":"selfhosted","cache_read_input_tokens":0,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-10-29T17:43:20.576887+00:00","model_set":{"reader":"selfhosted/deepseek-v4.1-flash"},"falsifier":"A Boltzmann or Monte-Carlo simulation with enough particles to resolve the layer where the mean free path equals the scale height, run long enough to measure the inner core mass as a function of central velocity dispersion, would settle it: if the measured slope is close to the long-mean-free-path value of about $-4$ rather than the near-unity slope the paper predicts, the throttled mass loss and the large seed black hole mass both fail.","supporting_citations":[{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Supplies the self-similar separation-of-variables method and the eigenvalue structure that the paper adapts to a different relaxation-time law."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Origin of the gravothermal catastrophe and of the long-mean-free-path flux form used in the combined conduction equation."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Standard reference for the gravothermal formalism, the core-mass/energy relation defining $ζ$, and the evaporation-rate parameterisation."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Fixes the hard-sphere collision rate coefficient $a = √(16/π)$ and the mean free path used throughout the relaxation-time estimates."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"The proposal under test: that self-interaction can flatten dark matter cores, which this paper tries to confirm or constrain."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Isolated-halo N-body simulation used as the primary point of comparison for core contraction and profile flattening."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Cross-section survey whose short-lifetime conclusion the paper argues rests on an inappropriate initially cuspy, already-collisional initial condition."}],"review_version":1}