Interactions of Astrophysical Neutrinos with Dark Matter: A model building perspective

We explore the possibility that high energy astrophysical neutrinos can interact with the dark matter on their way to Earth. Keeping in mind that new physics might leave its signature at such energies, we have considered all possible topologies for effective interactions between neutrino and dark matter. Building models, that give rise to a significant flux suppression of astrophysical neutrinos at Earth, is rather difficult. We present a $Z^{\prime}$-mediated model in this context. Encompassing a large variety of models, a wide range of dark matter masses from $10^{-21}$eV up to a TeV, this study aims at highlighting the challenges one encounters in such a model building endeavour after satisfying various cosmological constraints, collider search limits and electroweak precision measurements.


I. INTRODUCTION
IceCube has been to designed to detect high energy astrophysical neutrinos of extragalactic origin. Beyond neutrino energies of ∼ 20 TeV the background of atmospheric neutrinos get diminished and the neutrinos of higher energies are attributed to extragalactic sources [1].
However, there is a paucity of high energy neutrino events observed at IceCube for neutrino energies greater than ∼ 400 TeV [2]. There are a few events around ∼ 1 PeV or higher, whose origin perhaps can be described by the decay or annihilation of very heavy new particles [3][4][5][6][7][8][9][10] or even without the help of any new physics [11][12][13]. In the framework of standard astrophysics, high energy cosmic rays of energies up to 10 20 eV have been observed, which leads to the prediction of the existence of neutrinos of such high energies as well [14][15][16]. In this context, it is worth exploring whether the flux of such neutrinos can get altered due to their interactions with DM particles. However, it is challenging to build such models given the relic abundance of dark matter. Few such attempts have been made in literature but these models also suffer from cosmological and collider constraints. Hence, in this paper, we take a model building perspective to encompass a large canvas of such interactions that can lead to appreciable flux suppression at IceCube.
In presence of neutrino-DM interaction, the flux of astrophysical neutrinos passing through isotropic DM background is attenuated by a factor ∼ exp(−nσL). Here n denotes number density of DM particles, L is the distance traversed by the neutrinos in the DM background and σ represents the cross-section of neutrino-DM interaction. The neutrino-DM interaction can produce appreciable flux suppression only when the number of interactions given by nσL is O (1). For lower masses of DM, the number density is significant. But the cross-section depends on both the structure of the neutrino-DM interaction vertex and the DM mass. The neutrino-DM cross-section might increase with DM mass for some particular interactions. Hence, it is essentially the interplay between DM number density and the nature of the neutrino-DM interaction, which determines whether a model leads to a significant flux suppression. As a pre-filter to identify such cases we impose the criteria that the interactions must lead to at least 1% suppression of the incoming neutrino flux. For the rest of the paper, a flux suppression of less than 1% has been addressed as 'not significant'. While checking an interaction against this criteria, we consider the entire energy range of the astrophysical neutrinos. If an interaction leads to 1% change in neutrino flux after considering the relevant collider and cosmological constraints in any part of this entire energy range, it passes this empirical criteria. We explore a large range of DM mass ranging from sub-eV regimes to WIMP scenarios. In the case of sub-eV DM, we investigate the ultralight scalar DM which can exist as a Bose-Einstein condensate in the present Universe.
In general, various aspects of the neutrino-DM interactions have been addressed in the literature [17][18][19][20][21][22][23][24][25]. The interaction of astrophysical neutrinos with cosmic neutrino background can lead to a change in the flux of such neutrinos as well [26][27][28][29][30][31][32][33][34]. But it is possible that the dark matter number density is quite large compared to the number density of the relic neutrinos, leading to more suppression of the astrophysical neutrino flux.
To explore large categories of models with neutrino-DM interactions, we take into account the renormalisable as well as the non-renormalisable models. In case of non-renormalisable models, we consider neutrino-DM effective interactions up to dimension-eight. However, it is noteworthy that for a wide range of DM mass the centre-of-mass energy of the neutrino-DM scattering can be such that the effective interaction scale can be considered to be as low as ∼ 10 MeV. We discuss relevant collider constraints on both the effective interactions and renormalisable models. We consider thermal DM candidates with masses ranging in MeV−TeV range as well as non-thermal ultralight DM with sub-eV masses. For the thermal DM candidates, we demonstrate the interplay between constraints from relic density, collisional damping and the effective number of light neutrinos on the respective parameter space. Only for a few types of interactions, one can obtain significant flux suppressions. For the renormalisable interaction leading to flux suppression, we present a UV-complete model taking into account anomaly cancellation, collider constraints and precision bounds.
In Sec. II we discuss the nature of the DM candidates that might lead to flux suppression of neutrinos. In Sec. III we present the non-renormalisable models, i.e., the effective neutrino-DM interactions categorised into four topologies. In Sec. IV we present three renormalisable neutrino-DM interactions and the corresponding cross-sections in case of thermal as well as non-thermal ultralight scalar DM. In Sec. V we present a UV-complete model mediated by a light Z which leads to a significant flux suppression. Finally in Sec. VI we summarise our key findings and eventually conclude.

II. DARK MATTER CANDIDATES
In this section, we systematically narrow down the set of DM candidates we are interested in considering a few cosmological and phenomenological arguments.
The Lambda cold dark matter (ΛCDM) model explains the anisotropies of cosmic microwave background (CMB) quite well. The weakly interacting massive particles (WIMP) are interesting candidates of CDM, mostly because they appear in well-motivated BSM theories of particle physics. Nevertheless, CDM with sub-GeV masses are also allowed. The most stringent lower bound on the mass of CDM comes from the effective number of neutrinos (N eff ) implied by the CMB measurements from the Planck satellite. For complex and real scalar DM as well as Dirac and Majorana fermion DM, this lower bound comes out to be ∼ 10 MeV [17,18]. Thermal DM with masses lower than ∼ 10 MeV are considered hot and warm DM candidates and are allowed to make up only a negligible fraction of the total dark matter abundance [35]. The ultralight non-thermal Bose-Einstein condensate (BEC) dark matter with mass ∼ 10 −21 − 1 eV is also a viable cold dark matter candidate [36]. In the rest of this paper, unless mentioned otherwise, by ultralight DM we refer to the non-thermal ultralight BEC DM.
Numerical simulations with the ΛCDM model show a few tensions with cosmological observations at small, i.e., galactic scales [37][38][39]. It predicts too many sub-halos of DM in the vicinity of a galactic DM halo, thus predicting the existence of many satellite galaxies which have not been observed. This is known as the missing satellite problem [40]. It also predicts a 'cusp' nature in the galactic rotational curves, i.e., a density profile that is proportional to r −1 near the centre, with r being the radial distance from the centre of a galaxy. On the contrary, the observed rotational curves show a 'core', i.e., a constant nature. This is known as the cusp/core problem [41]. Ultralight scalar DM provides an explanation to such small-scale cosmological problems. In such models, at small scales, the quantum pressure of ultralight bosons prevent the overproduction of sub-halos and dwarf satellite galaxies [42][43][44]. Also, choosing suitable boundary condition while solving the Schrödinger equation for the evolution of ultralight DM wavefunction can alleviate the cusp/core problem [42,[45][46][47], making ultralight scalar an interesting, even preferable alternative to WIMP. Ultralight DM form BEC at an early epoch and acts like a "cold" species in spite of their tiny masses [48].
Numerous searches of these kinds for DM are underway, namely ADMX [49], CARRACK [50] etc. It has been recently proposed that gravitational waves can serve as a probe of ultralight BEC DM as well [51]. But the ultralight fermionic dark matter is not a viable candidate for CDM, because it can not form such a condensate and is, therefore "hot". The case of ultralight vector dark matter also has been studied in the literature [52].
The scalar DM can transform under SU (2) L as a part of any multiplet. In the case of a We investigate the scenarios of scalar dark matter, both thermal and ultralight, as possible candidates to cause flux suppression of the high energy astrophysical neutrinos. Such a suppression depends on the length of the path the neutrino travels in the isotropic DM background and the mean free path of neutrinos, which depends on the cross-section of neutrino-DM interaction and the number density of DM particles. We take the length traversed by neutrinos to be ∼ 200 Mpc, the distance from the nearest group of quasars [56], which yields a conservative estimate for the flux suppression. Moreover, we consider the density of the isotropic DM background to be ∼ 1.2 × 10 −6 GeV cm −3 [57]. Comparably, in the case of WIMP DM, the number density is much smaller, making it interesting to investigate whether the cross-section of neutrino-DM interaction in these cases can be large enough to compensate for the smallness of DM number density. This issue will be addressed in a greater detail in Sec. IV.

III. EFFECTIVE INTERACTIONS
In order to exhaust the set of higher dimensional effective interactions contributing to the process of neutrino scattering off scalar DM particles, we consider four topologies of diagrams representing all the possibilities as depicted in fig. 1. Topology I represents a contact type of interaction. In case of topologies II, III, and IV we consider higher dimensional interaction in one of the vertices while the neutrino-DM interaction is mediated by either a vector, a scalar or a fermion, whenever appropriate.
νν DM DM effective interactions can arise from higher dimensional gauge-invariant interactions as well. In this case, the bounds on such interactions may be more restrictive than the case where the mediators are light and hence, are parts of the low energy spectrum. In general low energy neutrino-DM effective interactions need not reflect explicit gauge invariance.
We discuss the bounds on the effective interactions based on LEP monophoton searches and the measurement of the Z decay width. The details of our implementation of these two bounds are as follows: • Bounds from LEP monophoton searches GeV. To extract a conservative estimate on the interaction, we assume that the new contribution saturates the error in the measurement of the cross-section 1.71 ± 0.14 pb at 1σ [58].
By the same token, we consider only one effective interaction at a time. µ + µ − DM DM interactions can contribute to the muon decay width which is measured with an error of 10 −4 %. However, the partial decay width of the muon via µ → ν µ e −ν e DM DM channel is negligible compared to the error. Hence, these interactions are essentially unbounded from such considerations. The percentage error in the decay width for tauon is even larger and hence, the same is true for τ + τ − DM DM interactions.
• Bounds from the leptonic decay modes of the Z-boson The effective νν DM DM interactions can be constrained from the invisible decay width of the Z boson which is measured to be Γ(Z → inv) = 0.48 ± 0.0015 GeV [57]. When the gauge-invariant forms of such effective interactions are taken into account, l + l − DM DM interactions may be constrained from the experimental error in the partial decay width of the channel Z → l + l − : ∆Γ(Z → l + l − ) ∼ 0.176, 0.256, 0.276 MeV for = e, µ, τ at 1σ [57].
To extract conservative upper limits on the strength of such interactions, one can saturate this error with the partial decay width Γ(Z → l + l − DM DM).
If such interactions are mediated by some particle, say a light Z , then a stringent bound can be obtained by saturating ∆Γ(Z → l + l − ) with Γ(Z → l + l − Z ). Similar considerations hold true for Z → νν DM DM mediated by a Z . We note in passing that such constraints from Z decay measurements are particularly interesting for light DM candidates.

A. Topology I
In this subsection effective interactions up to dimension 8 have been considered which can give rise to neutrino-DM scattering. The phase space factor for the interaction of the high energy neutrinos with DM can be found in appendix A 1.

1.
A six-dimensional interaction term leading to neutrino-DM scattering can be written as, where ν is SM neutrino, Φ is the scalar DM and Λ is the effective interaction scale. Now, for this interaction, the constraint from Z invisible decay reads c The bounds from the measurements of the channel Z → l + l − are de- is one of the scenarios that leads to the effective interaction as in eq. (3.1).
2. Another six-dimensional interaction is given as: The constraint from the measurement of the decay width in the Z → inv channel reads c (2) l /Λ 2 < ∼ 1.8 × 10 −2 GeV −2 for light DM. The bounds on the gauge-invariant form of the interaction in eq. (3.2) from the measurement of Z → l + l − reads c The bound from the channel e + e − → γ + / E T reads c (2) e /Λ 2 2.6 × 10 −5 GeV −2 . Even with the value c (2) l /Λ 2 ∼ 10 −2 GeV −2 , such an effective interaction does not give rise to an appreciable flux suppression due to the structure of the vertex.
3. Another five dimensional effective Lagrangian for the neutrino-DM four-point interaction is given by: The above interaction gives rise to neutrino mass at the loop-level which is proportional to m 2 DM . This, in turn, leads to a bound on the effective interaction due to the smallness of neutrino mass, In passing, we note that the interaction can be written in a gauge-invariant manner at the tree-level only when ∆, a SU (2) L triplet with hypercharge Y = 2, is introduced.
The resulting gauge-invariant term goes as (c  4. There can also be a dimension-seven effective interaction vertex for neutrino-DM scattering: Bound on this interaction comes from invisible Z decay width and reads c There is no counterpart of such an interaction involving the charged leptons. Thus the gauge-invariant form of this vertex does not invite any tighter bounds. Such a bound dictates that this interaction does not lead to any considerable flux suppression. 5. Another seven-dimensional interaction can be given as: From invisible Z decay width the constraint on the coupling reads c 6. Another neutrino-DM interaction of dim-8 can be written as follows: The coupling c (6) l /Λ 4 of interaction given by eq. (3.7) is constrained from invisible Z decay width as c B. Topology II 1. We consider a vector mediator Z , with couplings to neutrinos and DM given by: This interaction has the same form of interaction as in eq (3.7) of Topology I. Bound on this interaction from invisible Z decay reads f l c The bound on the process For this interaction, the ΦΦ * Z vertex from eq. (3.8) takes the form, i c where p 2 and p 4 are the four-momenta of the incoming and outgoing DM respectively.
In light of the constraints from Z decay, the factor c 2. Consider a scalar mediator ∆ with a momentum-dependent coupling with DM, Here ∆ can be realised as the neutral component of a SU (2) L -triplet scalar with Y = 2.

C. Topology III
We consider the vector boson Z mediating the neutrino-DM interaction, with a renormalisable vectorlike coupling with the DM, but a non-renormalisable dipole-type interaction in the ννZ vertex. The interaction terms are given as, This interaction can be constrained from the measurement of the invisible decay width of Z.

D. Topology IV
We consider the fermionic field F L,R mediating the neutrino-DM interaction with In eq. (3.11), after the Higgs H acquires vacuum expectation value (vev), the first term reduces to the second term up to a further suppression of (v 2 /Λ 2 ). Following the discussion in Sec. IV A 1, such interactions do not lead to a significant flux suppression.  l /Λ 2 from Z decay, the relic density and thus the number density of the DM with such an interaction comes out to be quite small, leading to no significant flux suppression. The following argument holds for all effective interactions considered in this paper for neutrino interactions with thermal DM. The thermally-averaged DM annihilation cross-section is given by σv th ∝ (1/Λ 2 )(m 2 DM /Λ 2 ) d , where d = 0, 1, 2, 3 for five-, six-, seven-and eight-dimensional effective interactions respectively. In order to have sufficient number density, the DM should account for the entire relic density, i.e., σv th ∼ 3 × 10 −26 cm 3 s −1 . To comply with the measured relic density, the required values of Λ come out to be rather large leading to small cross section.

A. Description of the models
Here we have considered three cases of neutrinos interacting with scalar dark matter at the tree-level via a fermion, a vector, and a scalar mediator.

Fermion-mediated process
In this case, the Lagrangian which governs the interaction between neutrinos and DM is given by: (4.1) Here L and l R stand for SM lepton doublet and singlet respectively. . In contrary, for non-self-conjugate DM the process is mediated only via the u-channel and leads to a larger cross-section compared to the former case. In this paper, we only concentrate on the non-self-conjugate DM in this scenario.
Such interactions contribute to the anomalous magnetic moment, δa l ≡ g l − 2, of the charged SM leptons, which in turn constrains the value of the coefficients C L,R . The contribution of the interaction in eq. (4.1) to the anomalous dipole moment of SM charged lepton of flavour l is given by [65]: where m l is the mass of the corresponding charged lepton. In the limit m DM m l m F , the anomalous contribution due to new interaction reduces to, For electron and muon the bound on the ratio (C L C R /16π 2 m F ) reads 1.6 × 10 −9 GeV −1 and 2.9 × 10 −8 GeV −1 respectively. There is no such bound for the tauon.

Scalar-mediated process
The Lagrangian for the scalar-mediated neutrino-DM interaction can be written as: where L are the SM lepton doublets and ∆ is the SU (2) L -triplet with hypercharge Y = 2.
When ∆ acquires a vev v ∆ , the first term in eq. (4.4) leads to a non-zero neutrino mass For v ∆ ∼ 1 GeV and mass of the neutrino m ν 0.1 eV the constraint on the coupling f l reads f l < ∼ 10 −11 . The second term in eq. (4.4) contributes to DM mass In case the DM mass is solely generated from such a term, the upper bound on v ∆ dictated by the measurement of ρ-parameter, implies a lower bound on g ∆ . The mass term for DM might also arise from some other mechanisms, for example, by vacuum misalignment in case of ultralight DM. In such a scenario, for a particular value of m DM and v ∆ there exists an upper bound on the value of g ∆ .
The lower bound on the mass of the heavy CP-even neutral scalar arising from the SU (2)triplet is m ∆ ∼ 150 GeV for v ∆ ∼ 1 GeV [63], which comes from the theoretical criteria such as perturbativity, stability and unitarity, as well as the measurement of the ρ-parameter and h → γγ.

Light Z -mediated process
The interaction of a scalar DM with a new gauge boson Z is given by the Lagrangian, (4.5) Here, f l are the couplings of the l = e, µ, τ kind of neutrinos with the new boson Z , while g is the coupling between the dark matter and the mediator. f l can be constrained from the g − 2 measurements. Due to the same reason as in the fermion-mediated case, the coupling of Z with τ -flavoured neutrinos is not constrained from g − 2 measurements. Constraints for this case from the decay width of Z boson will be discussed in Sec V.
For the mass of the SM charged lepton, m l and the boson, m Z , the anomalous contribution to the g − 2 takes the form [65]: We have considered vector-like coupling between the Z and charged leptons. For electrons and muons we find the constraints on couplings-to-mediator mass ratio to be rather strong [57], From the measurement of N eff the lower bound on the mass of a light Z interacting with SM neutrinos at the time of nucleosynthesis reads m Z 5 MeV [66].

B. Thermal Relic Dark Matter
In this scenario, the DM is initially in thermal equilibrium with other SM particles via its interactions with the neutrinos. For models with thermal dark matter interacting with neutrinos, three key constraints come from the measurement of the relic density of DM, collisional damping and the measurement of the effective number of neutrinos. These three constraints are briefly discussed below.

• Relic density
If the DM is thermal in nature, its relic density is set by the chemical freeze-out of this particle from the rest of the primordial plasma. The observed value of DM relic density is Ω DM h 2 ∼ 0.1188 [57], which corresponds to the annihilation cross-section of the DM into neutrinos σv th ∼ 3 × 10 −26 cm 3 s −1 . In order to ensure that the DM does not overclose the Universe, we impose σv th 3 × 10 −26 cm 3 s −1 . (4.8)

• Collisional damping
Neutrino-DM scattering can change the observed CMB as well as the structure formation.
In presence of such interactions, neutrinos scatter off DM, thereby erasing small scale density perturbations, which in turn suppresses the matter power spectrum and disrupts large scale structure formation. The cross-section of such interactions are constrained by the CMB measurements from Planck and Lyman-α observations as [19,20], (4.9) • Effective number of neutrinos In standard cosmology, neutrinos are decoupled from the rest of the SM particles at a temperature T dec ∼ 2.3 MeV and the effective number of neutrinos is evaluated to be N eff = 3.045 [67]. For thermal DM in equilibrium with the neutrinos even below T dec , entropy transfer takes place from dark sector to the neutrinos, which leads to the bound m DM 10 MeV from the measurement of N eff . It can be understood as follows. In presence of n species with thermal equilibrium with neutrinos, the change in N eff is encoded as [17], where, Here, the effective number of relativistic degrees of freedom in thermal equilibrium with neutrinos is given as In eqs. (4.10) and (4.12), i = 1, .., n denotes the number of species in thermal equilibrium with neutrinos, g i = 7/8 (1) for fermions (bosons) and the functions I(m i /T ν ) and F (m i /T ν ) can be found in ref. [17]. For a DM in thermal equilibrium with neutrinos and m DM < ∼ 10 MeV, the contribution of F (m DM /T ν ) to (T ν /T γ ) is quite large, and such values of DM mass can be ruled out from N eff = 3.15 ± 0.23 [68], obtained from the CMB measurements.
We implement the above constraints in cases of the renormalisable models discussed in Sec IV. We present the thermally-averaged annihilation cross-section σv th and the crosssection for elastic neutrino-DM scattering σ el for the respective models in table I. The notations for the couplings and masses follow that of Sec IV. In the expressions of σv th , p cm can be further simplified as ∼ m DM v r where v r ∼ 10 −3 c is the virial velocity of DM in the galactic halo [18]. In the expressions of σ el , E ν represents the energy of the incoming relic neutrinos which can be roughly taken as the CMB temperature of the present Universe.
Two of the three renormalisable interactions discussed in this paper, namely the cases of fermion and vector mediators have been discussed in the literature in light of the cosmological constraints, i.e., relic density, collisional damping and N eff [18]. For a particular DM mass, the annihilation cross-section decreases with increasing mediator mass. Thus, in order for the DM to not overclose the Universe, there exists an upper bound to the mediator mass for a particular value of m DM . With mediator mass less than such an upper bound, the relic density of the DM is smaller compared to the observed relic density, leading to a smaller number density.
Fermion-mediated Scalar-mediated Vector-mediated As discussed earlier, the measurement of N eff places a lower bound on DM mass m DM Thus we conclude that the three renormalisable interactions stated above do not lead to any significant flux suppression of astrophysical neutrinos in case of cold thermal dark matter.

C. Ultralight Scalar Dark Matter
Here we consider the DM to be an ultralight BEC scalar with mass 10 −21 − 1 eV.
The centre-of-mass energy for the neutrino-DM interaction in this case always lies between sion at IceCube. The cross-section for neutrino-DM scattering through a fermionic mediator in case of ultralight scalar DM is given as

Fermion-mediated process
where m ν , E ν are the mass and energy of the incoming neutrino respectively, m DM is the mass of the ultralight DM, and m F is the mass of the heavy fermionic mediator. As the mass of the DM is quite small, at lower neutrino energies m 2 ν > m DM E ν and hence, the cross-section remains constant. As the energy increases, the m DM E ν term becomes more dominant and eventually, the cross-section increases with energy.
Such an interaction has been studied in literature in case of ultralight DM [21]. This analysis was improved with the consideration of non-zero neutrino mass in ref. [22]. For example, from fig. 6(a) it can be seen that the cross-section for m ν ∼ 10 −2 eV is larger compared to that for m ν ∼ 10 −5 eV. In fig. 6(b), with m ν ∼ 10 −2 eV, it is shown that no significant flux suppression takes place for a DM heavier than 10 −22 eV for m F ∼ 10 GeV.
However, it has been shown that the quantum pressure of the particles of mass 10 −21 eV suppresses the density fluctuations relevant at small scales ∼ 0.1 Mpc, which is disfavoured by the Lyman-α observations of the intergalactic medium [69,70]. Also, the constraint on the mass of such a mediator fermion, which couples to the Z boson with a coupling of the order of electroweak coupling, reads m F 100 GeV [64]. These facts together suggest that m DM ∼ 10 −22 eV and m F ∼ 10 GeV, as considered in ref. [22], are in tension with Lyman-α observations and LEP searches for exotic fermions respectively. If we consider m ν = 0.1 eV along with m F = 100 GeV, it leads to a larger cross-section compared to that with m ν = 0.01 eV, which is still smaller compared to the cross-section required to induce a significant flux suppression. Thus, taking into account such constraints, the interaction in eq. (4.1) does not lead to any appreciable flux suppression in case of ultralight DM.

Scalar-mediated process
As mentioned in Sec. IV A 2, the bound on the coupling of a scalar mediator ∆ with neutrinos is quite stringent, f l v ∆ 0.1 eV. Moreover, the mass of such a mediator are constrained as m ∆ 150 GeV [63]. In this case, the cross-section of neutrino-DM scattering is  In the standard cosmology neutrinos thermally decouple from electrons, and thus from photons, near T dec ∼ 1 MeV. Ultralight DM with mass m DM forms a Bose-Einstein condensate below a critical temperature T c = 4.8 × 10 −4 / (m DM (eV)) 1/3 a eV, where a is the scale factor of the particular epoch [71]. When the temperature of the Universe is T ∼ T dec , T c ∼ 480 MeV for m DM ∼ 10 −6 eV, i.e., the ultralight DM exists as a BEC. In order to check whether the benchmark scenario presented in fig. 8(a) leads to late kinetic decoupling of neutrinos, we verify if n ν (T dec ) σ ν−DM v ν < ∼ H(T dec ). Here, n ν (T ) and H(T ) are the density of relic neutrinos and the Hubble rate at temperature T respectively, n ν ∼ 0.091T 3 dec ∼ 1.14 × 10 31 cm −3 . pointed out that a strong neutrino-DM interaction can degrade the energies of neutrinos emitted from core collapse Supernovae and scatter those off by an significant amount to not be seen at the detectors [72][73][74]. This imposes the following constraint on the neutrino-DM cross-section [17,74]: It can seen from fig. 8(a) that such a constraint is comfortably satisfied in our benchmark scenario.

V. A UV-COMPLETE MODEL FOR VECTOR-MEDIATED ULTRALIGHT SCALAR DM
Here we present a UV-complete scenario which accommodates an ultralight scalar DM as well as a Z with mass ∼ O(10) MeV. The Z mediates the interaction between the DM and neutrinos.
The coupling of such a Z with the first two generations of neutrinos cannot be significant because of the stringent constraints on the couplings of the Z with electron and the muon.
Here, g Z is gauge coupling of U (1) and Y ϕ is the U (1) charge of the scalar ϕ. It is clear from eq. (5.1) that, in order to satisfy the collider search limit on the masses of exotic leptons ∼ 100 GeV, the gauge coupling of Z has to be rather small. Such a constraint can be avoided if the exotic fermions obtain masses from a scalar other than ϕ. This scalar cannot be realised as the SM Higgs, because then the effect of the heavy fourth generation fermions do not decouple in the loop-mediated processes like gg → h, h → γγ etc. To evade both these constraints we consider that the exotic fermions get mass from a second Higgs doublet. In order to avoid Higgs-mediated flavour-changing neutral current at the tree-level, it is necessary to ensure that no single type of fermion obtains mass from both the doublets Φ 1,2 .
Hence, we impose a Z 2 -symmetry to secure the above arrangement under which the fields transform as it is mentioned in table II. After electroweak symmetry breaking, the spectrum of physical states of this model will contain two neutral CP-even scalars h and H, a charged scalar H ± , and a pseudoscalar A. The Yukawa sector of this model looks like, also be realised in a Type-II 2HDM in the wrong-sign Yukawa limit [80].
The Z ττ interaction in our model leads to a new four-body decay channel of τ and threebody decay channels for Z and W ± . We consider that the effect of these new interactions must be such that their contribution to the respective decay processes must be within the errors of the measured decay widths at 1σ level. This leads to an upper bound on the allowed value of the coupling g τ which is enlisted in table III.
If we choose the new symmetry to be a SU (2) instead of U (1) , then in addition to Z we would have W ± in the spectrum. But the existence of a charged vector boson of mass ∼ O(10) MeV opens up a new two-body decay channel for τ . Such decay processes are highly constrained, thus making the coupling of Z to ν τ rather small.
The existing studies of the flux suppression of astrophysical neutrinos involve only a few types of renormalisable neutrino-DM interactions. As mentioned earlier, such studies suffer from various collider searches and precision tests. We take a rigourous approach to this problem by considering renormalisable as well as effective interactions between neutrinos and DM and mention the constraints on such interactions. Taking into account the bounds from precision tests, collider searches as well as the cosmological constraints, we investigate whether such interactions can provide the required value of cross-section of neutrino-DM scattering so that they lead to flux suppression of the astrophysical neutrinos.
In this paper we have contained our discussion to scalar dark matter. The effective neutrino-DM interactions considered in this paper can stem from different renormalisable models, at both tree and loop levels. In order to keep the analysis as general as possible, in contrary to the usual effective field theory (EFT) prescription, we do not assume any particular scale of the dynamics which lead to such effective interactions. As a result, it is not possible to a priori ensure that the effects of a particular neutrino-DM effective interaction will always be smaller than an effective interaction with a lower mass-dimension.
Thus we investigate effective interactions up to mass dimension-8. It is also worth mentioning that the flavour oscillation length of the neutrinos is much smaller than the mean interaction length with dark matter. Hence, the attenuation in the flux of one flavour of incoming neutrinos eventually gets transferred to all other flavours and leads to an overall flux suppression irrespective of the flavours. The criteria of 1% flux suppression helps to identify the neutrino-DM interactions which should be further taken into account to check potential signatures at IceCube. The flux of astrophysical neutrinos at IceCube also depend upon the specifics of the source flux and cosmic neutrino propagation. In order to find out the precise degree of flux suppression, one needs to solve an integro-differential equation consisting of both attenuation and regeneration effects [81], which is beyond the scope of the present paper and is addressed in ref. [82]. But the application of the criteria of 1% flux suppression, as well as the conclusions of the present work are independent of an assumption of a particular type of source flux or details of neutrino propagation.
In brief, we encompass a large canvas of interactions between neutrinos and dark matter, trying to find whether they can lead to flux suppression of the astrophysical neutrinos. The We consider the process of neutrinos scattering off DM particles. If the incoming neutrino has an energy E 1 , the energy of the recoiled neutrino is [83], where θ is the scattering angle of the neutrino. The relevant Mandelstam variables are, s = (p µ 1 + p µ 2 ) 2 = m 2 ν + m 2 DM + 2E 1 m DM , The energies of incoming neutrinos are such that, E 1 ∼ p 1 holds well. The scattering angle θ in the centre-of-momentum frame can take all values between 0 to π, whereas that is the case in the laboratory frame only when m ν < m DM . When m ν > m DM , there exists an upper bound on the scattering angle in the laboratory frame, θ max ∼ m DM /m ν .
The differential cross-section in the laboratory frame is given by [84]: where dΩ = sin θdθdφ.

Amplitudes of various renormalisable neutrino-DM interactions
• Fermion-mediated process With the renormalisable interaction presented in eq. (A2) Here, p 1 , p 2 , p 3 and p 4 are the four-momenta of the incoming neutrino, incoming DM, outgoing neutrino and outgoing DM respectively.
• Scalar-mediated process The amplitude squared for a scalar-mediated process governed by neutrino-DM interaction given by eq. (4.4) reads: The neutrinos are Majorana particles in this case and g ∆ has a mass dimension of unity.
• Vector-mediated process The square of the amplitude for a vector-mediated process described by eq.
c and U (1) Y (Gravity) 2 are automatically satisfied [76]. Still we need to take care of the chiral anomalies involving U (1) which lead to the following conditions [85,86]:   For DM with higher masses the cosmological constraints, i.e., relic density, collisional damping and N eff ensure that the above-mentioned interactions do not lead to any significant flux suppression. This has been discussed in Sec. III and IV B.