{"id":"a371c243-8063-4a8e-9ca8-77ab127f3e57","arxiv_id":"2501.05342","paper_version":3,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":6.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":0,"one_line_summary":"Zero-modes of spherical bosonic stars under axisymmetric perturbations explain the bifurcations into chain, ring, and gyroscope-like bosonic star families.","lead":"The authors solve the linear perturbation equations for spherical bosonic stars and show that the known chain and ring shaped bosonic star families branch off exactly where a zero-mode appears. They also report a new mixed 'gyroscope-like' family and chains with up to seven components.","discovery_kind":"new_method","skeptic_critique":{"model":"deepseek-v4-flash","headline":"The perturbation ansatz (4.2) imposes δg_tt/g_tt = δg_rr/g_rr, but the nonlinear ABS metric (2.7) used to build the chains/rings instead ties δg_rr/g_rr to δg_θθ/g_θθ and leaves δg_tt/g_tt independent; no gauge argument justifies this truncation, so the computed zero-modes may not be the tangent…","rationale":"The central claim is that the zero-modes computed from Eq. (4.2) are the bifurcation points of the chain/ring ABS families. For this to be true, the perturbation subspace must contain the actual tangent vector of those families. I find the weakest link precisely where the reader placed it: Eq. (4.2) is asserted without a completeness or gauge-fixing argument. The sharpest version of the problem is the mismatch with the nonlinear metric ansatz (2.7): linearizing (2.7) enforces δg_rr/g_rr = δg_θθ/g_θθ (H=K in Eq. (4.2)), whereas (4.2) instead enforces δg_tt/g_tt = δg_rr/g_rr (same H for both) and leaves K independent. Since the standard Regge-Wheeler gauge leaves H0, H2, K independent (static, even-parity, m=0), the restriction H0=H2 is a genuine truncation of the perturbation space, not a gauge freedom. If the actual tangent has H0 ≠ H2 and/or H ≠ K, the computed zero-modes solve a different linear problem. The agreement with the known bifurcation frequencies (Table 1, Fig. 2) is suggestive but does not by itself validate the ansatz: the frequencies are computed from the same truncated ODEs, while the nonlinear families are solved independently. The l=4 result, based on a single delicate numerical search, inherits the same issue. This is addressable: one can linearize (2.7) directly and test whether zero modes persist, or extract tangent vectors from nearby nonlinear solutions. Because the paper already provides multiple independent nonlinear constructions matching the predicted frequencies, the appropriate verdict remains CONDITIONAL pending this consistency check, not REJECT.","tokens_in":22722,"tokens_out":20537,"duration_ms":197044,"concrete_test":"Re-derive the linearized perturbation equations by linearizing the exact ABS metric ansatz (2.7) around the spherical background, so that the tangent satisfies δg_rr/g_rr = δg_θθ/g_θθ with δg_tt/g_tt independent; solve these zero-mode equations for the same backgrounds and compare the resulting frequencies with Table 1 and the l=4 point. If the frequencies shift, or if the solution requires δg_tt/g_tt ≠ δg_rr/g_rr, then the ansatz (4.2) is not the tangent space of the reported ABS families and the central identification fails.","verdict_should_be":"UNCHANGED","load_bearing_attack":"Section 4.2's Eq. (4.2) parameterizes the metric perturbation with a single function H(r) multiplying both δg_tt/g_tt and δg_rr/g_rr, and a single K(r) multiplying δg_θθ/g_θθ and δg_φφ/g_φφ. But the ABS solutions whose bifurcations are being explained are constructed with the ansatz (2.7), g_rr = e^{2F1}, g_θθ = r^2 e^{2F1}. Linearizing (2.7) around the spherical background gives δg_rr/g_rr = 2δF1 = δg_θθ/g_θθ, i.e., H=K in (4.2), while δg_tt/g_tt = 2δF0 is an independent function. Thus the tangent space of the nonlinear family is (H0, H, K=H), not (H, H, K) with H and K independent. In the standard Regge-Wheeler gauge for even-parity perturbations of a spherical background, H0, H2, K are independent after gauge fixing, so setting H0=H2 is not a gauge choice. The paper neither derives (4.2) from (2.7) nor shows that the zero-mode it finds satisfies H=K and H0=H; without this, the frequency agreement in Table 1 could be an artifact of a truncated problem, and the l=4 gyroscope claim inherits the same gap.","agreement_with_reader":"agree"},"referee_report":{"model":"deepseek-v4-flash","summary":"The manuscript studies bifurcations of spherical bosonic stars (SBSs) into axisymmetric bosonic stars (ABSs). It constructs scalar and Proca SBSs, then solves linearized axisymmetric perturbation equations (4.3)-(4.4) by a multi-parameter shooting method, looking for zero-modes under \\ell=2 and \\ell=4 perturbations. It claims that the resulting zero-mode frequencies coincide with the bifurcation points of previously constructed chain-like and ring-like ABS families, that this identifies those bifurcation points with the critical points of stability against \\ell=2 (and, for one case, \\ell=4) axisymmetric perturbations, and that the \\ell=4 zero-mode leads to a new 'gyroscope-like' ABS family. It also reports the construction of scalar chains with up to seven constituents and their associated ring-like counterparts, as well as the empirical relation N_S=(N_A-1)/2 between the SBS node number and the ABS constituent number.","tokens_in":23043,"tokens_out":11350,"duration_ms":102414,"significance":"If the central claim is correct, the paper would provide a linearized explanation for the observed branching of chain/ring ABSs from spherical branches and would add a qualitatively new \\ell=4 perturbation channel leading to gyroscope-like configurations. The internal agreement between the zero-mode calculation and known nonlinear bifurcation points is a genuine check rather than an input, and the construction of seven-constituent chains extends the known solution space. However, the load-bearing perturbation ansatz is not shown to be tangent to the nonlinear ABS families used for comparison, and the reduction to the simplified ODEs is not presented; these gaps currently prevent the results from being interpreted as a proof of the bifurcation mechanism.","major_comments":[{"comment":"The perturbation ansatz (4.2) is not derived from, and is not the linearization of, the nonlinear ansatz (2.7) used to construct the ABS families. In (2.7) the three functions F0, F1, F2 are independent, so the tangent space around a spherical background contains \\delta g_tt/g_tt = 2\\delta F0, \\delta g_rr/g_rr = \\delta g_\\theta\\theta/g_\\theta\\theta = 2\\delta F1, and \\delta g_\\phi\\phi/g_\\phi\\phi = 2\\delta F2 as independent perturbations. Equation (4.2), by contrast, identifies \\delta g_tt/g_tt (up to sign) with \\delta g_rr/g_rr through the single function H and identifies \\delta g_\\theta\\theta/g_\\theta\\theta with \\delta g_\\phi\\phi/g_\\phi\\phi through K. Linearizing (2.7) would impose H=K and would leave \\delta F0 and \\delta F2 independent, neither of which is justified in (4.2). The manuscript gives no gauge-fixing argument showing that every even-parity axisymmetric zero-mode of the full system can be brought to this form, nor does it show that off-diagonal perturbations such as \\delta g_{r\\theta} decouple. Without this, the zero-mode found by shooting may not be the tangent direction of the chain/ring/gyroscope branches, and the agreement with Table 1 is insufficient to establish the central claim of Section 5.1. A concrete check would be to linearize the full PDE system (2.10)-(2.13) around the spherical background at the claimed bifurcation frequency and compare the zero-mode subspace with the tangent direction obtained from the nonlinear ABS branches.","section":"Section 4.2, Eq. (4.2); Section 2.1, Eq. (2.7)"},{"comment":"The reduction from the linearized Einstein-matter system to the simplified ODEs (4.3)-(4.4) is not shown. The text states that K, K', and K'' are eliminated using the (r,r), (r,\\theta), and (\\theta,\\theta) Einstein equations, but it does not present the elimination, does not state which residual equations are used, and does not discuss possible degeneracies of the algebraic equation (4.6) at zeros of \\omega^2-\\mu^2\\sigma^2 N. The coefficient functions in (4.7)-(4.8) are long and are written with \\kappa=4\\pi G set to 1 only after the equations; no derivation or code is provided. Since the zero-mode frequencies are the central quantitative output, the reduction should be made available, at least as supplementary material, so the reader can verify that no spurious modes are introduced by the elimination procedure.","section":"Section 4.2, Eqs. (4.3)-(4.5)"},{"comment":"The claimed quantitative agreement between the zero-mode frequencies and the nonlinear bifurcation points is never tabulated. Table 1 lists the background SBS parameters (\\omega, M, Q) at the bifurcation points of the nonlinear families, and Figure 3 shows the zero-mode background profiles, but the paper does not list the independently obtained zero-mode frequencies, masses, or charges, nor their differences from the Table 1 values. The sentence 'After comparing the relevant parameters, we can confirm the consistency' is the only explicit statement. This agreement is the key evidence for the central claim in Section 5.1, so an explicit comparison table with numerical precision is required.","section":"Section 5.1, Table 1"},{"comment":"For the new \\ell=4 gyroscope-like family, the evidence is only qualitative. The text reports one \\ell=4 zero-mode in scalar SBSs with N_S=3 and shows the perturbation profiles in Figure 7, but it does not give the zero-mode frequency, nor a numerical comparison with the nonlinear branch point marked in Figure 6. Table 4 displays energy-density surfaces, but there is no quantitative match between the perturbation tangent and the constructed nonlinear solutions. Since the abstract elevates the \\ell=4 gyroscope-like ABSs to a headline result, this case needs the same level of numerical evidence as the \\ell=2 case.","section":"Section 5.2, Fig. 6 and Table 4"}],"minor_comments":[{"comment":"The term for \\bar H_2 appears to be written as A_2(r) P_\\ell(\\cos\\theta)/d\\theta, which is almost certainly intended to be A_2(r) dP_\\ell(\\cos\\theta)/d\\theta; please correct the notation.","section":"Eq. (4.2)"},{"comment":"The boundary conditions in (3.1) and (3.2) contain apparent typos: (3.2) repeats m(0)=0 and \\sigma(r)=\\sigma_0 from the origin conditions, whereas the intended conditions at infinity should presumably be m(\\infty) finite and \\sigma(\\infty)=1.","section":"Section 3.1, Eqs. (3.1)-(3.2)"},{"comment":"There are several grammatical and typographical errors: 'red and pueple curves' should be 'red and purple curves', and 'We discovered that exhibit zero-modes' is missing a grammatical subject.","section":"Section 5.2 and Conclusions"},{"comment":"The text mentions 'black dashed lines' in connection with Figure 2, but the figure caption and the visible markers refer to 'black points' for bifurcations; please reconcile the description.","section":"Figure 2 and surrounding text"},{"comment":"In Eq. (3.13), the right-hand side depends on \\theta through \\cos^2\\theta, while the left-hand side M_2 is a spacetime quadrupole moment and should be \\theta-independent; please check the formula and the definitions of B_0 and \\nu_2.","section":"Eq. (3.13)"},{"comment":"The empirical relation N_S=(N_A-1)/2 is stated without derivation or a statement of its domain of validity; since it is used to select the constructed cases, a brief explanation or at least a caveat would help.","section":"Section 4.1, Eq. (4.1)"}],"recommendation":"major_revision","confidential_remarks":"The manuscript is potentially interesting, but the central perturbation analysis needs substantial work before it can support the claimed bifurcation mechanism. The referees should particularly weigh whether the zero-mode ansatz (4.2) is tangent to the nonlinear ABS family (2.7); without that, the main explanatory claim is not established. I would be willing to review a revised version that provides the full reduction, a gauge/tangent-space justification, and explicit numerical comparisons."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"The paper explains the known chain and ring bifurcations of spherical bosonic stars as l=2 zero-modes of the linearized Einstein-matter system, and adds a new l=4 gyroscope-like family plus 7-constituent chains. The core numerical result is strong: the computed zero-mode frequencies match the nonlinear bifurcation points in Table 1 for three scalar cases and one Proca case. That agreement is the paper's best evidence, and it holds up.\n\nWhat is actually new: the l=2 zero-mode calculation itself, the first l=4 zero-mode and the corresponding gyroscope-like solutions, and the 7-component chains. The paper is candid about not performing a systematic stability analysis and about the numerical difficulty of finding more l=4 cases. The citation pattern is fine; the earlier chain and ring constructions are the authors' own, and they use them as comparison data, not assumptions.\n\nThe soft spots are real but not fatal. Section 4.2's perturbation ansatz (4.2) is not derived by linearizing the nonlinear ABS ansatz (2.7). In (2.7), g_rr and g_theta theta share the same conformal factor, so the tangent space of the nonlinear family has delta g_rr/g_rr = delta g_theta theta/g_theta theta; in (4.2) those two are independent (H and K). The stress-test note is right to flag this. The authors eliminate K via the Einstein constraints and solve for H and the matter perturbations, but they never show that the resulting K equals H for the zero-mode solutions. Without that check, the modes could be zero modes of a broader problem rather than of the actual family. The counterargument is empirical: if the ansatz were spurious, hitting the same four bifurcation frequencies would be an unlikely coincidence. So I think the result is very likely correct, but the paper needs to square the two ansatze, or at least report K(r) versus H(r) at the zero modes.\n\nAlso missing: the reduction from the Einstein equations to the simplified ODEs (4.3)-(4.4) is stated without derivation, and no code or data is shipped. The l=4 search has no resolution study, and the perturbation functions there are large, so a grid-convergence statement would help. These are addressable in revision.\n\nWho this is for: people working on bosonic stars, solitons in GR, and bifurcation or stability of compact objects. It deserves a serious referee. I would send it to review with a request to address the ansatz consistency and to report the K-H relation. The central claim is likely right; the loose ends are technical.","headline":"Solid numerical work explaining known bosonic-star bifurcations as zero-modes; the l=4 gyroscope family is genuinely new, and the ansatz-consistency gap is technical and addressable.","tokens_in":47,"tokens_out":4234,"would_cite":true,"duration_ms":100469,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"Spherical bosonic stars have perturbative zero modes at the exact points where chain-like, ring-like, and gyroscope-like axisymmetric families branch off.","keywords":["bosonic stars","axisymmetric perturbations","zero modes","bifurcation","chain-like configurations","ring-like configurations","Proca stars","gyroscope-like stars"],"falsifier":"A direct check would be to solve the full linearized Einstein-matter equations for axisymmetric perturbations without imposing the restricted diagonal ansatz of Eq. (4.2), allowing for example an off-diagonal $g_{r\\theta}$ perturbation, and ask whether a zero mode with all fields regular and decaying at infinity still occurs at the same frequencies reported here (about $\\omega=0.8583$, $0.8553$, $0.8634$ for scalar stars with NS=1,2,3; $\\omega=0.8713$ for the Proca star; and the l=4 scalar NS=3 zero mode of Section 5.2). If the unrestricted problem has no such mode at those frequencies, the bifurcating branches would not be explained; if it has modes at different frequencies, additional ABS families should exist there. A complementary nonlinear test is to start from the spherical solution and follow the l=4 perturbation branch numerically to confirm that the gyroscope-like family persists away from linear order.","tokens_in":22481,"feed_emoji":"🪐","tokens_out":8877,"duration_ms":82922,"temperature":0.7,"pith_summary":"This paper aims to explain previously observed bifurcations of spherical bosonic stars into axisymmetric chain and ring configurations as the zero modes of a specific class of axisymmetric linear perturbations. The authors solve the first-order perturbation equations on scalar and Proca spherical bosonic-star backgrounds and find that at the same frequencies where the axisymmetric families attach, the perturbation functions can be made to vanish at infinity, the signature of a marginal mode. At l=2, the sign of the perturbation parameter selects whether matter collects along the axis, forming chains, or in the equatorial plane, forming rings, for excited scalar stars with one, two, and three nodes and for the first excited Proca star. At l=4, a scalar star with three nodes has a second zero mode, and the paper constructs the corresponding family, whose matter distribution mixes chain and ring features and is called gyroscope-like. If correct, this gives a perturbation-theoretic explanation for the branching of the reported axisymmetric bosonic star families from spherical solutions, and it extends the scalar chain family to seven constituents.","feed_headline":"Zero modes split bosonic stars into chains, rings, gyroscopes","feed_subtitle":"Excited spherical stars bifurcate under l=2 and l=4 perturbations, producing chain, ring, and gyroscope-like families.","key_machinery":"The central object is the linearized, time-independent axisymmetric perturbation ansatz of Eq. (4.2): the spherical metric functions get perturbations $H(r)P_\\ell(\\cos\\theta)$ and $K(r)P_\\ell(\\cos\\theta)$ on the diagonal, with $P_\\ell$ the Legendre polynomial, together with matter perturbations $\\psi_1(r)P_\\ell(\\cos\\theta)$ for scalar stars and $A_0,A_1,A_2$ for Proca stars. Substituting into the Einstein-matter equations, keeping first order in the small parameter $\\epsilon$, and using three Einstein equations to eliminate $K(r)$ and its derivatives reduces the system to two coupled second-order linear ODEs for the scalar case and three for the Proca case, Eqs. (4.3)-(4.4). The zero modes are found by a multi-parameter shooting method that requires all perturbation functions to vanish at infinity; the spherical backgrounds at which such solutions exist are exactly the bifurcation points. The sign of $\\epsilon$ in the perturbed metric and matter fields acts as the branching selector, with opposite signs corresponding to the two distinct axisymmetric branches.","core_discovery":"The paper's central discovery is that spherical bosonic stars of the complex scalar and Proca fields, in excited states, possess static axisymmetric zero modes at discrete frequencies, and that each such zero mode is the tangent direction of a branch of static axisymmetric bosonic stars that splits off from the spherical trunk. For l=2 perturbations, each studied spherical background, scalar with node number NS=1,2,3 and Proca with NS=1, admits exactly one zero mode; the two signs of the perturbation amplitude reproduce the two known bifurcation branches, the chain-like ABSs with NA=2NS+1 constituents, where matter is concentrated on the axis, and the ring-like ABSs, where matter is concentrated near the equatorial plane. For l=4, the scalar NS=3 background admits another zero mode, and the paper constructs the corresponding new family of ABSs, called gyroscope-like, whose constant-energy-density surfaces simultaneously exhibit chain-like and ring-like features. The paper also constructs, for the first time, scalar bosonic-star chains with seven constituents and their ring counterparts. The physical quantities of the spherical and axisymmetric solutions coincide at the bifurcation points, and the quadrupole moment changes sign according to whether matter is drawn toward the axis or the equator.","pith_inferences":["If the restricted ansatz is complete, the same method should predict an infinite sequence of higher-multipole bifurcations: scalar stars with more nodes should have l=4, l=6, and higher zero modes at distinct frequencies, so searching for zero modes on NS>=4 backgrounds would test the ladder structure beyond the single l=4 example.","The gyroscope-like morphology is likely the l=4 member of a broader pattern of mixed multipole matter distributions; extrapolating from l=2, which separates chains and rings, l=6 modes might create matter accumulation at intermediate angular locations, giving a sequence of increasingly complex ABS matter configurations.","The sign reversal between the scalar and Proca cases suggests that the branch morphology is fixed by the angular profile of the background energy density rather than by the sign of the perturbation parameter alone, so a more model-independent criterion could be derived by studying which sign of $\\epsilon$ lowers the energy for a given field spin.","The zero-mode technique could be exported to other soliton-gravity systems, such as Q-balls in flat spacetime or hairy black holes, as a way to locate bifurcation points from perturbation equations before constructing full nonlinear solutions."],"forward_implications":["Every reported static axisymmetric bosonic star family can be traced to a spherical bosonic star through a zero mode: at l=2, the sign of the perturbation parameter chooses chains versus rings, verified for scalar stars with one, two, and three nodes and for the first excited Proca star.","A single spherical background can host more than one bifurcation: the three-node scalar star has both the l=2 zero mode, giving chains and rings, and an l=4 zero mode, giving the new gyroscope-like family with mixed chain and ring morphology.","The empirical relation between the scalar star's node number NS and the chain constituent number NA, $N_S=(N_A-1)/2$, directly connects higher excited spherical states to longer chains, so constructing larger chains should correspond to probing higher excited spherical backgrounds.","The quadrupole moment acts as a clean order parameter for these bifurcations: it vanishes at the spherical background, becomes positive for scalar chain-like branches and negative for scalar ring-like branches, and is always negative for the gyroscope-like family, reflecting its equatorial dominance.","If a sufficiently strong quartic self-interaction is added, the zero modes may be removed at a threshold coupling, which would eliminate the bifurcations; the paper explicitly speculates that such a threshold exists."],"supporting_citations":[{"why":"Supplies the original scalar boson-star model and solution family whose excited states are the spherical backgrounds studied here.","marker":"[27]"},{"why":"Introduces the Proca-star model used for the s=1 bifurcation analysis.","marker":"[28]"},{"why":"Provides the chain-like scalar ABS solutions and the three-constituent branches whose bifurcation points the l=2 zero modes reproduce.","marker":"[24]"},{"why":"Reports the chain-like and ring-like ABS families that the paper matches to the perturbation zero modes.","marker":"[25]"},{"why":"Gives the quadrupolar Proca-star family and the ABS framework that the paper extends to seven-constituent chains.","marker":"[26]"},{"why":"Defines the discrete-symmetry and hybrid multipolar constructions whose boundary conditions and nomenclature connect to the new ABSs.","marker":"[36]"},{"why":"Provides the asymptotic multipole expansion used to compute the quadrupole moments that distinguish chain-like from ring-like and gyroscope-like ABSs.","marker":"[79]"},{"why":"The numerical PDE solver package used to construct the axisymmetric solutions, including the new seven-constituent chains and gyroscope-like stars.","marker":"[82–84]"}],"fun_headline_variants":["Zero modes spawn chains, rings, and gyroscope stars","Bosonic stars fork into chains, rings, gyroscopes","Spherical stars turn into chains and rings via zero modes","New bosonic star families: chains, rings, and gyroscopes","Bifurcation of bosonic stars into chain and ring shapes"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The argument assumes that the simple perturbation pattern the authors write down, two parts of the spherical gravitational field deformed by a single angular function plus matching changes in the matter field, catches every possible even, symmetric way the star can start to become axisymmetric; if some other independent pattern exists that this ansatz misses, the computed bifurcation points could be wrong or incomplete.","fun_headline_variants_meta":{"raw":{"variants":["Zero modes spawn chains, rings, and gyroscope stars","Bosonic stars fork into chains, rings, gyroscopes","Spherical stars turn into chains and rings via zero modes","New bosonic star families: chains, rings, and gyroscopes","Bifurcation of bosonic stars into chain and ring shapes"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000849,"raw_usage":{"total_tokens":3715,"prompt_tokens":987,"completion_tokens":2728,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":603,"completion_tokens_details":{"reasoning_tokens":2640}},"tokens_in":603,"tokens_out":2728,"duration_ms":18652,"temperature":1.0,"reasoning_tokens":2640,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-10T21:14:31.068144+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"A direct check would be to solve the full linearized Einstein-matter equations for axisymmetric perturbations without imposing the restricted diagonal ansatz of Eq. (4.2), allowing for example an off-diagonal $g_{r\\theta}$ perturbation, and ask whether a zero mode with all fields regular and decaying at infinity still occurs at the same frequencies reported here (about $\\omega=0.8583$, $0.8553$, $0.8634$ for scalar stars with NS=1,2,3; $\\omega=0.8713$ for the Proca star; and the l=4 scalar NS=3 zero mode of Section 5.2). If the unrestricted problem has no such mode at those frequencies, the bifurcating branches would not be explained; if it has modes at different frequencies, additional ABS families should exist there. A complementary nonlinear test is to start from the spherical solution and follow the l=4 perturbation branch numerically to confirm that the gyroscope-like family persists away from linear order.","supporting_citations":[{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Gives the quadrupolar Proca-star family and the ABS framework that the paper extends to seven-constituent chains."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Defines the discrete-symmetry and hybrid multipolar constructions whose boundary conditions and nomenclature connect to the new ABSs."}],"review_version":1}