Abstract
The main purpose of this study is to review the Schenberg resonant antenna transfer function and to recalculate the antenna design strain sensitivity for gravitational waves. We consider the spherical antenna with six transducers in the semi dodecahedral configuration. When coupled to the antenna, the transducer-sphere system will work as a mass-spring system with three masses. The first one is the antenna effective mass for each quadrupole mode, the second one is the mass of the mechanical structure of the transducer first mechanical mode and the third one is the effective mass of the transducer membrane that makes one of the transducer microwave cavity walls. All the calculations are done for the degenerate (all the sphere quadrupole mode frequencies equal) and non-degenerate sphere cases. We have come to the conclusion that the “ultimate” sensitivity of an advanced version of Schenberg antenna (aSchenberg) is around the standard quantum limit (although the parametric transducers used could, in principle, surpass this limit). However, this sensitivity, in the frequency range where Schenberg operates, has already been achieved by the two aLIGOs in the O3 run, therefore, the only reasonable justification for remounting the Schenberg antenna and trying to place it in the sensitivity of the standard quantum limit would be to detect gravitational waves with another physical principle, different from the one used by laser interferometers. This other physical principle would be the absorption of the gravitational wave energy by a resonant mass like Schenberg.
Similar content being viewed by others
Introduction
Gravitational waves (GW) are ripples in the fabric of space-time generated by the acceleration of massive cosmic objects. These ripples move at the speed of light and can excite quadrupolar normal-modes of elastic bodies. The first detection of GWs from the inward spiral and merger of a pair of Black Holes (BH) (GW150914) has been widely discussed in the literature1,2,3,4. Furthermore, the recent simultaneous detection of the electromagnetic counterpart with GWs from a binary Neutron Star (NS) merger (GW170817) has officially begun the era of multi-messenger astronomy involving GWs5,6. Studying the universe with these two fundamentally different types of information will offer the possibility of a richer understanding of the astrophysical scenarios as well as of nuclear processes and nucleosynthesis. For the first time in the GW astronomy, it has been possible to determine the position in the sky of the source thanks to the detection, at the same time, of the three interferometers of the LIGO/Virgo collaboration5.
The Mario Schenberg Brazilian detector is based on the detection of five quadrupole modes relative to the mechanical vibrations of a spherical resonant-mass of \(M_S= 1124\) kg and radius \(R=32.33\) cm (Fig. 1). The operating frequency band is 3.15–3.26 kHz. The antenna is made of a CuAl(6%) alloy, which has a high mechanical quality factor Q \(\sim \) \(2\times 10^{6}\) at 4 K. The system is suspended by a vibration isolation system, capable of attenuating external vibrations by about 300 dB7,8. The instrument will be maintained at low temperatures (\(\sim \) 4 K) by cryogenic chambers (dewars), cooled down by a He flow9. The antenna is coupled to parametric transducers that will monitor the vibrations of the quadrupolar/monopolar normal modes of the sphere10,11,12,13,14. One of the main advantages of a GW spherical resonant antenna is its omnidirectional sensitivity, which makes it equally responsive to all wave directions and polarizations15. Spherical resonant-mass antennas have been already intensively studied16,17,18. The designed antenna transduction system consists of nine transducers fixed on the surface of the sphere, six of which follow the truncated icosahedron configuration proposed by Johnson and Merkowitz19. This configuration presents some benefits and allows the simplification of the equations of motion, the determination of the GW direction in the sky, and facilitates the interpretation of the signal. For more details on the Schenberg antenna, the reader is referred to20,21 and references therein. It is important to mention that, in addition to being a device to try to detect gravitational waves, the Schenberg antenna could also be used to test the hypothesis that the ripples in the curvature of the fabric of space-time can be scaled by a more minute “action”, whose detection requires sensitivities beyond the standard quantum limit22. On the other hand, the Schenberg detector can also be used to test alternative theories of gravitation, such as the reference23 which, having a massive graviton, has six polarization states. The plan of the paper is as follows: in section “Gravitationalwaves from NS-BH binary systems”, we consider the emission of GWs from the spiraling of a NS-BH binary system and we discuss the detectability of this system by the Schenberg antenna. Then, we discuss the interaction of GWs with matter in section “The interaction of GW with matter”. The detector model is introduced in section “The detector model”, which is followed by the calculation of the response function of the antenna. All the calculations are done for the degenerate (all the sphere quadrupole mode frequencies equal) and non-degenerate sphere cases. For the degenerate case, the degenerate frequency was chosen as the average of the five quadrupole frequencies measured at 2 K. Final considerations as well as the discussion of the results are presented in section “Discussions and conclusions”.
Gravitational waves from NS-BH binary systems
Coalescence of NS-BH binaries is one of the most promising GW sources for ground-based antennas. NS-BH systems are believed to be formed as a result of two supernovae in a massive binary system24,25. GWs from binaries involving NS represent a tool to study NS properties like the radius, compactness, and tidal deformability. Knowledge of NS properties will allow constraining the equation of state of nuclear-density matter26, giving us valuable information on nuclear physics. After the formation of the system, the orbital separation decreases gradually due to the long-term gravitational radiation reaction (i.e., two objects are in an adiabatic inspiral motion), and eventually, the two objects merge into a BH. The final fate of the binary depends primarily on the mass of the BH and the compactness of the NS. However, a detailed analysis has shown that the BH spin and the NS equation of state also play an important role in determining the final fate25. The effective-one-body (EOB) formalism was introduced27,28 as a promising approach to describe analytically the inspiral, merger, and ringdown waveforms emitted during a binary merger. Among the candidates of electromagnetic counterparts, a short-hard Gamma-Ray Burst (GRB) and its afterglow are vigorously studied both theoretically and observationally29,30. For a deeper analysis of NS-BH binaries, see25.
In this section, we discuss the GW signal produced by the coalescence of a non-spinning 1.4–3.0 \(M_{\odot }\) NS-BH binary system, disregarding finite-size effects such as tidal deformation. The narrow frequency window of the antenna constrains the BH mass to be \(\lesssim \) 3 \(M_{\odot }\). Compact binary systems emit periodic GWs, whose frequencies sweep the spectrum until they reach their maximum values when they are close to the coalescence. The characteristic amplitude and the frequency of GWs near the last orbit are given by25
where \(\omega \) is the angular velocity, M = \(M_{BH}\) + \(M_{NS}\), and r and D are the orbital separation and the distance to the source, respectively. The binary system studied may be in principle detected since the frequency of the gravitational signal \(\sim \) 1 ms before coalescing falls in the band of the Brazilian antenna. NS-BH mergers are also potential targets of interferometers GW detectors. Since these kinds of antennas are sensitive in a much broader frequency range (\(\sim \) 10–4000 Hz) they will detect the signal before the Schenberg antenna (during the inspiral phase). It is worth noting that due to the truncated icosahedron configuration the antenna is able to determine the polarization and the position of astrophysical sources of the GW31,32,33,34. There are a large number of waveform families in the literature, obtained from considerations about the type of source and approximation procedures used for the simulation (numerical relativity (NR), EOB formalism, post-Newtonian (PN) approximation, etc.). The gravitational signal for our analysis was generated using the PyCBC software package35,36. The waveform employed is one of those that are used by LIGO/Virgo, that is, the effective-one-body model tuned to numerical relativity (EOBNRv2). PN results are good as long as the velocities of the objects are not extreme relativistic. However, as the two objects orbit around each other, they lose energy through the emission of GWs, and their distance shrinks along with an increase in velocity. Consequently, PN predictions become more and more inaccurate the closer the binary gets to the merger, while the EOB approach, close to the merger, provides better accuracy by calibrating higher-order vacuum terms to NR waveforms. The EOBNRv2 waveform is believed to be sufficiently accurate to search for signals from non-spinning coalescing compact binaries in the aLIGO sensitive band. The EOB formalism has been refined several times to incorporate additional information from NR. Depending on the number of available NR waveforms as well as the modifications introduced to the EOB description, various versions of such EOBNR models have been developed37,38. It is beyond the scope of this paper to show the technical details of the EOB formalism and its extensions. Figure 2 also shows the waveform of the non-spinning NS-BH binary considered here. The waveform has also been re-sampled to be compatible with the sampling rate of the Schenberg antenna.
The coalescence rate of this type of system is very small and can be calculated indirectly. Upper limits (\(\sim \) \(10^{3}\) Gpc\(^{-3}\) year\(^{-1}\)) were given assuming that all short GRBs/kilonovae are linked with NS-BH mergers29 and from the assumption that all the r-process material were produced in NS-BH coalescences39.
There are indications that NS-BH binary has been directly observed40 and an estimated rate density of \(\sim \) 0.04 \(\times \) \(10^{3}\) Gpc\(^{-3}\) year\(^{-1}\) can also be derived from stellar evolution synthesis41,42. In the present work, to evaluate the event rate related to NS-BH mergers, we follow Li et al.43 and Abbott et al.44, who constrain the merger rate to be less than 6500 Gpc\(^{-3}\) year\(^{-1}\), assuming a population of binary systems of 1.4–3 \(M_{\odot }\). This estimate is sensitive to physical parameters, such as the equation of state of NS material and the mass/spin distribution of the BH. The upper limit of the rate decreases for BHs with larger masses. The expected rates for other transient sources are smaller and/or less reliable. In order to be detected, the amplitude of the GW signal needs to be compatible with the sensitivity of the antenna.
For an advanced version of the Schenberg antenna (aSchenberg), which would operate around the standard quantum limit (section “The detector model”), gravitational signals with amplitude h \(\sim \) 10\(^{-22}\) could be detected at the nominal frequency of the antenna. In this case, a signal could be produced in GWs whose characteristic amplitude is \(\sim \) 3 \(\times \) 10\(^{-22}\) at distances of the order of 0.1 Gpc (Fig. 2). In this volume, the event rate would be \(\sim \) 3.6 year\(^{-1}\) at a SNR \(\sim \) 1. This conclusion relies on the validity of the assumption that all observed kilonovae were associated with NS-BH coalescences. In addition, many statistical studies based on the stellar evolution synthesis and supernova rates predict the rates at which NS-BH merge in the Milky Way and the nearby universe, assuming that Milky Way-like galaxies dominate, to be 1–10% of that of NS-NS binaries (every \(\sim \) \(10^{6}\)–\(10^{7}\) years)45,46,47. If we consider the contribution of elliptic galaxies the total coalescence rate of the universe could be increased by a significant fraction48. These estimates show that the prospect for the detection of NS-BH mergers of 1.4–3.0 \(M_{\odot }\) by the Schenberg antenna can be very promising.
The interaction of GW with matter
As it is well known, a GW produces a tidal density force at time t and at position \({{\varvec{x}}}\) given by (sum over repeated indices implied)
where \(\rho \) is the mass density and \(\ddot{h}\) the second time derivative of the GW amplitude. Since the Schenberg antenna has a resonant frequency about 3 kHz, the wavelength of the GW detectable is about 100 km so we can use the value of \(h_{ij}(t)\) at the center of the sphere. Equation (3) can be written in terms of the gradient of a potential
where
where \({\varvec{n}}\) is the unit vector in the radial direction and r the magnitude. We can expand \(\Phi ({\varvec{x}},t)\) in terms of the real spherical harmonics, always used in this paper, \(Y_{\ell m}^\mathcal{R}(\vartheta ,\varphi )\), defined in terms of the traditional spherical harmonics
The spherical harmonics obey the normalization condition
From now on we will omit the superscript \(\mathcal R\) and write \(Y_{\ell m}^\mathcal{R}=Y_{\ell m}\). After the expansion we have (only terms with \(\ell =2\), quadrupolar modes, survive)
where the \(h_m\) are the expansion coefficients so called spherical amplitudes given by
The spherical amplitudes \(h_m\) for a GW coming from the direction defined by the polar and azimuthal angles \((\theta ,\phi )\) as seen from the lab frame is given by (see Appendix D):
In matrix notation and after making the rotation around the polarization angle \(\psi \), we have
which in a more compact form becomes,
Using Eq. (8) and the vector spherical harmonics (see Appendix C we obtain the expression of the GW density force
In the case where \({\varvec{f}}\) in the right hand side of Eq. (32) is only of GW origin, the overlap integral
is the effective force on each mode of the sphere and
are the eigenfunctions of the uncoupled sphere modes, Eq. (33), repeated here for convenience. After the integration over the angular part this integral reduces, in the case of Schenberg antenna, to
where
For the Schenberg antenna we have \(\chi _1=-0.6004\).
We have calculated \(\chi _1=\chi \) using the expression
Its worth mention that a similar expression is used by Maggiore49
with the difference that in49 in the definition of the spherical amplitude \(h_m\) is included the factor \(\sqrt{16\pi /15}\).
The detector model
As discussed above, the mechanical oscillations of the Schenberg antenna are monitored by a set of parametric transducers coupled on its surface. From a mathematical point of view, Johnson and Merkowitz50 proposed a model in which the output data from six transducers coupled to the antenna surface are related by decomposing them into the quadrupolar modes of the sphere. This method allows the reconstruction of the parameters that characterize the incident GW.
The movement equation for the displacement vector field \({\varvec{u}}({\varvec{x}},t)\) of a solid subjected to external forces density \({\varvec{f}}({\varvec{x}},t)\) is given by51
where \(\lambda _L\) and \(\mu _L\) are the tangential and volumetric Lamé coefficients of the material respectively. The initial conditions are \({\varvec{u}}({\varvec{x}},0)=0\) and \(\dot{\varvec{u}}({\varvec{x}},0)=0\). The solution of (26) is obtained expanding the displacement vector \({\varvec{u}}({\varvec{x}},t)\) in series of the eigenfunctions \(\varvec{\Psi }_N({\varvec{x}})\) of the equation
subjected to the boundary condition of tension free at the surface of the sphere49
The displacement vector field can be expanded as
where N is a set of indices, \(a_N(t)\) is the time-dependent mode amplitude and \(\varvec{\Psi }_N\) obeys the normalization condition
The integration is over the volume V of the sphere. After substituting (27) and (29) in (26), multiplying by \(\varvec{\Psi }_{N'}\) and integrating over the volume of the sphere using (30), we obtain
with \(\kappa _S\) being the elastic constant.
At this point it is convenient to introduce a damping term in Eq. (31)
where \(C_S=w_N/Q_N\), \(w_N\) the natural angular frequency of mode N and \(Q_N\) the mechanical quality factor Q for mode N. The values of the parameters are given in Table (1).
The uncoupled sphere
The solution of (27) subjected to the boundary condition of tension free at its surface are the natural modes of the sphere. They consist of two families of solution, the toroidal modes \(\varvec{\Psi }_{n\ell m}^T\) and the spheroidal modes \(\varvec{\Psi }_{n\ell m}\) (see52). We rewrite here this solution in terms of the vector spherical harmonics defined in Appendix C. Regarding the toroidal modes, in the case of a coupled sphere, they do not impart radial motion on the transducers, and the Schenberg detector is not sensitive to them, besides the fact that GWs do not excite these modes.
Spheroidal modes
The spheroidal modes are given by
where
The transverse wave vectors \(k_{n\ell }\), the longitudinal wave vectors \(q_{n\ell }\) and the natural angular frequencies \(w_{n\ell }=2\pi f_{n\ell }\) are the solution of the system of equations
where betas are given by
The coefficients \(c_l\) and \(c_t\) are respectively the longitudinal
and transversal
velocities of the elastic waves. We define the ratio
here \(\rho \) is the density of the sphere and \(\sigma \) the Poisson ratio. The Poisson ratio can be written in terms of the ratio of the longitudinal and transversal sound velocities
The solution of the system of Eqs. (36–38) only depends on \(c_l\) and \(c_t\), in this way using the measured values of the monopole and quadrupole frequencies we were able to determine them. The results are given in Table 1.
The relationship between the Poisson ratio and the Young modulus E with the Lamé coefficients \(\lambda _L\) and \(\mu _L\) are
Antenna parameters at 4 K
The linear thermal expansion as a function of temperature is given by53,54
where \(\alpha _0\) is a constant such that \(\alpha _\text{lin}(273.15)=1.75\times 10^{-5}\,{\text{K}}^{-1}\)55, A is the weighted average of CuAl6 atomic mass in kg, B is the bulk modulus
and \(\gamma \) is the weighted average of the CuAl6 Gruneisen coefficient. The lattice specific heat is
where \(R_G\) is the gas constant, \(\Theta _D\) is the weight average of CuAl6 Debye’s temperature. The Debye’s function is
The electrons specific heat is given by
with \(T_F\) being the weight average of CuAl6 Fermi temperature. Then the radius at 4 K will be given by
After calculating \(c_l\) and \(c_t\), based on its measured values at 300 K and 2 K and using the frequency of the monopolar mode and the mean frequency of the quadrupolar modes, we are able to calculate the radius of the sphere at 4 K. The solution must take into account that the coefficient of linear expansion depends on the Poisson’s ratio as well as the Eqs. (36–38) depends on it. With this methodology it is possible to calculate physical constants of CuAl6. The results are given in Table 1.
The antenna coupled with transducers
In order to detect GWs, six two stage transducers are coupled to the Schenberg antenna10. Each stage of the transducers has the same resonance frequency of the first quadrupole mode \(f_0=3205.94 \, \mathrm{Hz}\) (average of the five quadrupole frequencies measured at 2 K, also chosen as the degenerate frequency) and are sensitive only to the radial movement of the sphere. Transducers are devices that monitor the motion of the antenna surface. If a hypothetical GW excites the sphere quadrupolar modes, the corresponding mechanical energy will be transferred from the antenna to the transducers. Jonhson and Merkowitz19 discovered that if we use six transducers and locate each of them at the center of a pentagonal face of a truncated icosahedron projected onto one hemisphere of the sphere, then by a suitable linear combination of the output of the transducers, the so called mode channels, we can obtain a direct correspondence between the spherical amplitudes \(h_m(t)\) of the GW and the quadrupolar modes of the sphere \(a_{2m}(t)\). The angles of each of these transducers are given in Table 2. The Schenberg antenna makes use of two-modes parametric transducers. In this model the transducer motion is exclusively radial and only the m quadrupole modes are of interest. In an homogeneous sphere the modes are degenerated but in the real antenna they are not. The forces acting on the sphere (Fig. 3) are the GW force given by
the spring back reaction of the six transducers over the sphere at the positions \({\varvec{x}}_{a}\)
the damping back reaction of the resonators of the six transducers over the sphere at the positions \({\varvec{x}}_{a}\)
where \(C_{1}\) is the damping term of the first resonator. The noise coming from the interaction with the resonator 1 is
where \(x_{1a}\) is the displacement of the first resonator from its equilibrium position, \({{\varvec{e}}}_a\) is the radial unit vector at the position \({\varvec{x}}_a\) over the sphere and \(u_a\) the deformation of the sphere at \({\varvec{x}}_a\) given by (repeated here for convenience)
The equation for \(\varvec{\Psi }_m\), Eq. (33), is rewritten here with \(n=1\), \(\ell =2\), \(A_{12}(r)=\alpha (r)\) and \(B_{12}=\beta (r)\)
so that we have for \(u_a\)
In matrix notation this is
where \(\alpha =\alpha (R)\) and the bold letters are matrices in which each entry of \(\textbf{u}\) is related to a transducer and each entry of \(\textbf{a}\) is related to a mode of the sphere. The movement equation for the displacement of the sphere surface \(\textbf{u}\) is given in Appendix B.
The forces over the first resonator are the noise forces coming from the interaction of itself with the sphere, \(f_1^{n}\), and with the second resonators, \(f_2^{n}\), and the action and reaction of the restoration and damping forces of the first and second springs over it. The forces over the second resonator are the back action forces coming from the interaction with the microwave system, \(f_2^{bk}\), the interaction with the resonator 1, \(f_2^{n}\), and restoration and damping forces of the second springs over it, (Fig. 3).
The equations for the system are
where \({\varvec{f}}({\varvec{x}},t)={\varvec{f}}_1^\kappa ({\varvec{x}},t)+{\varvec{f}}_1^C({\varvec{x}},t)-{\varvec{f}}_1^{n}({\varvec{x}},t)+{\varvec{f}}^{GW}({\varvec{x}},t)\) are the surface forces over the sphere and the GW force. The transducers frequencies are tuned with the frequency of the quadrupole mode of the homogeneous sphere \(w_0\) such that
For the real antenna we take \(w_0\) as the mean value of the measured quadrupole mode frequencies \(w_m\). For the maximum energy transfer from the sphere to the resonators the masses obeys the relation57
where the effective mass of the antenna \(M_{\text{eff}}\) is calculated in the Appendix A. The integral in Eq. (64) can be written as
The first integral on the right hand side gives
Similarly the second gives
and the third
where \(q_{1a}=x_{1a}-u_a\) and \(q_{2a}=x_{2a}-x_{1a}\), the fourth is the Eq. (25). The result is
From now on we will use the column matrix
The equations in the new variables and in matrix notation are
In block matrix notation we have
These equations can be rewritten in terms of the block matrices
From now on we use sanserif boldface letters for block matrices. Here \({\textsf {\bf{q}}}\) is the displacement matrix
where \(\textbf{a}_{5\times 1}\) is the antenna’s mode amplitude, \(\textbf{q}_{1\, 6\times 1}\) and \(\textbf{q}_{2\,6\times 1}\) are vectors of the relative displacements for the first and second resonators of each transducer. The mass matrix is
where \(\textbf{B}_{5\times 6}\) is the model matrix. Let us rewrite this matrix in term of the effective mass using the mass ratios \(\mu ^2\) and \(\nu ^2\) given in Eq. (68). We have
The stiffness matrix is
and using \(\kappa _{mS}=M_Sw_m^2\), \(\kappa _1=M_1w_0^2\), \(\kappa _2=M_2w_0^2\) and the mass ratios \(\mu ^2\) and \(\nu ^2\) it reads
The damping matrix is
and using \({C_m}_S=M_S w_m/Q_m\), \(C_1=M_1w_0/Q_1\), \(C_2=M_2w_0/Q_2\) and the mass ratios \(\mu ^2\) and \(\nu ^2\) it reads
where \(Q_m\), \(Q_1\) and \(Q_2\) are respectively the quality factor of the modes of the sphere, the first and second resonators. In our case \(Q_m=Q\) where Q is the measured value of the quality factor of the sphere, but we leave at it is for generality. The movement equation then reads
We will need to diagonalize the matrix \({{{{\textsf {{{\bf M}}}}}}}^{-1}{{{{\textsf {{{\bf K}}}}}}}\), but this matrix is not symmetric. In order to symmetrize it we change the coordinates defining \({{{{\textsf {{{\bf q}}}}}}}={{{{\textsf {{{\bf N}}}}}}}{{{{\textsf {{{\bf y}}}}}}}\) where
and pre-multiply by \({{{\textsf {{{\bf N}}}}}}\)
Multiplying both sides of the equation by
and defining \(2\beta =\frac{w_0}{Q}\) we get
Let us define the variables \({{{{\textsf {{{\bf M}}}}}}}_y\), \({{{{\textsf {{{\bf K}}}}}}}_y\) and \({{{{\textsf {{{\bf P}}}}}}}_y\), where the subscript is the indicative that these matrices are of the equation for \({{{{\textsf {{{\bf y}}}}}}}\). The equation then reads
whose Fourier transform is
This can be rewritten
In case of brute force solution we invert for each w the matrix in the lhs of this equation, using \({{{\textsf {{{\bf q}}}}}}={{{\textsf {{{\bf Ny}}}}}}\) giving
where \({{{\textsf {{{\bf G}}}}}}_\text{BF}(w)\) is the brute force transfer function of the input \({{\tilde{{{{{\textsf {{{\bf f}}}}}}}}}}\)
The matrices are
where \(\gamma =\alpha \mu /\nu \) and
with \(\textbf{1}\) a matrix full of ones. The matrix \({{{{\textsf {{{\bf P}}}}}}}_y\) is
We need to solve Eq. (91), to do this we have two tracks to follow: the first one is the traditional method of finding eigenvalues and eigenvectors to diagonalize the matrix in the lhs of this equation, the other is that we call brute force, we solve this equation inverting the matrix for each value of the angular frequency w. The first one is easier to find the eigen frequencies of the system. For the sensibility calculation we have done using both methods with identical results, the relative error is of the order of \(10^{-7}\) in the degenerate case and of the order of \(10^{-3}\) in non degenerate case.
For the solution using the traditional method, we need to do some approximations in the matrix \({{{{\textsf {{{\bf K}}}}}}}_y\) and in the matrix \({{{{\textsf {{{\bf C}}}}}}}_y\). First of all they must be symmetric and according to Caughey and O’Kelley in (1965)58, the general condition to uncouple the modal equations with \(\varvec{M}\), \(\varvec{K}\) and \(\varvec{C}\) respectively as mass matrix, stiffness matrix and damping matrix is that \(\varvec{K}\varvec{M}^{-1}\varvec{C}=\varvec{C}\varvec{M}^{-1}\varvec{K}\).
One reason that we can do approximations in the damping matrix is that we often have little information about the precise form for this matrix, so we are free to choose it in a way that simplifies the analysis. For this purpose, in our case, we make the approximations: from now on we use the measured value of the quality factor \(Q=Q_m\), and given that
in the entries \({{{{\textsf {{{\bf K}}}}}}}_{y21}\) and \({{{{\textsf {{{\bf C}}}}}}}_{y21}\) we approximate \(\text{Diag}\left( \frac{w_m}{w_0}\right) =\textbf{I}\), in the entry \({{{{\textsf {{{\bf C}}}}}}}_{y11}\) we approximate \(\text{Diag}\left( \frac{w_m}{w_0}\right) =\text{Diag}\left( \frac{w_m^2}{w_0^2}\right) \) and use \(Q=Q_1=Q_2\) in the entries \({{{{\textsf {{{\bf C}}}}}}}_{y12}\), \({{{{\textsf {{{\bf C}}}}}}}_{y22}\), \({{{{\textsf {{{\bf C}}}}}}}_{y23}\), \({{{{\textsf {{{\bf C}}}}}}}_{y32}\), \({{{{\textsf {{{\bf C}}}}}}}_{y33}\). So that we end with \({{{{\textsf {{{\bf C}}}}}}}_y={{{{\textsf {{{\bf K}}}}}}}_y\). Then we can use the same modal matrix \({{{{\textsf {{{\bf U}}}}}}}\) to diagonalize both matrices.
Let the matrix \({{{{\textsf {{{\bf U}}}}}}}\) diagonalize \({{{{\textsf {{{\bf K}}}}}}}_y\) and let us define \({{{{\textsf {{{\bf y}}}}}}}={{{{\textsf {{{\bf U}}}}}}}{{{{\textsf {{{\bf z}}}}}}}\) and pre-multiply by \({{{{\textsf {{{\bf U}}}}}}}^T\), then Eq. (91) reads
As \({{{\textsf {{{\bf U}}}}}}\) diagonalize \({{{{\textsf {{{\bf K}}}}}}}_y\) and \({{{{\textsf {{{\bf D}}}}}}}\) being the diagonal matrix such that \({{{{\textsf {{{\bf D}}}}}}}={{{{\textsf {{{\bf U}}}}}}}^T{{{{\textsf {{{\bf K}}}}}}}_y{{{{\textsf {{{\bf U}}}}}}}\) this equation becomes
We omit the w dependence in some cases to leave the notation cleaner.
If we define the diagonal matrix
we get
We invert to find \(\varvec{{\tilde{z}}}\)
where
Returning to the old variables we have
The transfer functions for the input \({{\tilde{{{{{\textsf {{{\bf f}}}}}}}}}}\) will be
where the block matrix \({{{{\textsf {{{\bf G}}}}}}}\) can be written as
Then, we can write Eq. (106) as
Classical noise power spectrum matrix
In this work we will assume that the noise is an ergodic wide sense stationary stochastic process being analysed in an interval of time \(T_o\). Let x(t) with Fourier transform \({\tilde{x}}(w)\) be a process satisfying these conditions, then the Power Spectral Density (PSD) of x is calculated as (see Whalen Chap.(2)59 and Maggiore49 for details)
Our system is contaminated with forces of thermal noise \({\varvec{f}}_\text{th}\), forces of back action on the membrane \({{\varvec{f}}}_\text{bk}\), series forces \({\varvec{f}}_\text{se}\) and phase forces \({\varvec{f}}_\text{ph}\). The measured quantity is the output \(\textbf{q}_2\) (transducer membrane) of our system
We have splited the forces on the sencond resonator \({{\tilde{\textbf{f}}}}_2={{\tilde{\textbf{f}}}}'_2+{{\tilde{\textbf{f}}}}_{bk}\). The PSD of the output \(\textbf{q}_2\) is, assuming that the noise forces of different kind are non correlated and the forces \({\tilde{\textbf{f}}}\) are of thermal origin
The thermal noise power spectrum is based on the fluctuation dissipation theorem that stays that given a system with equation
the power spectrum of the fluctuation force \({{{{\textsf {{{\bf f}}}}}}}\) is given by
where is the impedance of the system given by
In our case we have
But from Eqs. (77) and (83) we have
The back action noise force acting on the membrane is60
where \({P_\text{inc}}\) is the pump oscillator power, \({S_\text{a}}\) is the amplitude noise spectral density of the pump oscillator, \({f_\text{p}}\) is the pump oscillator frequency, \({Q_\text{e}}\) is the transducer cavity electric Q, and dx is the membrane displacement.
The series noise acting directly on the output is
where \({T_\text{amp}}\) is the amplifier noise temperature, T is the thermodynamic temperature, and \({k_\text{B}}\) is the Boltzmann constant.
The phase noise also acting directly on the output is
where \({S_\text{p}}\) is the phase noise spectral density.
Standard quantum limit noise
In the following section we will derive the expression of the standard quantum noise. This will allow us to obtain the standard quantum limit of the Schenberg detector. The power signal-to-noise ratio \(\rho ^2\) for an optimum filter (matched filter) is61
where M(w) is the Fourier transform of the signal of interest and \(S_{nn}^\text{ds}(w)\) the double side power spectral density of the noise. Our signal is the vector with the spherical amplitudes \(\textbf{h}(t)\). Using the single side power spectral density matrix \(\textbf{S}_{nn}(w)\), the expression of the power signal-to-noise ratio becomes
For bursts of duration \(\tau _g\approx 1\,\mathrm ms\) the maximum bandwidth frequency is \(\Delta f_\text{max}\approx 1\,\mathrm kHz\) and \({{\tilde{\textbf{h}}}}(w)\) does not change very much from its value at the resonant frequency \(f_0\) in the band \(\Delta f\) of the detector. We can define a mean power spectral density \({\bar{S}}_{nn}\) such that this integral can be approximated by
where \(\textbf{h}(w_0)=|\textbf{h}(w_0)|{\hat{{\tilde{\textbf{h}}}}}\),
and
We can obtain \(|\textbf{h}(w_0)|\) as a function of the energy deposited by the burst on the sphere using the formula62
where f(t) is the external force acting on the harmonic oscillator and M its mass. Starting from the movement equation for the sphere modes (Eq. 31), the mass of the mode is \(M_S\) as a result of the normalization condition and the force is \(f(t)=\frac{1}{2}M_S\chi R\ddot{h}_m(t)\). The integration gives for each mode m
while the energy deposited in all modes is
The sensitivity is obtained when \(\rho ^2=1\). With this value, comparing Eq. (123) with Eq. (128) we obtain the mean power density spectrum as a function of the energy deposited in the sphere
The energy deposited in terms of the number of phonons n is \(E_s=n\hbar w_0\). The sensitivity at the quantum limit is when \(n=1\)
We can write this expression as a function of the longitudinal sound velocity and the longitudinal wave vector for the quadrupolar mode \(w_0=w_{12}=q_{12}c_{l}\)
For Schenberg at \(4\,\mathrm K\), \(f_0=f_{12}=3205.94\,\mathrm{Hz}\), \(M_S=1124\,\mathrm{kg}\), \(\chi =-0.6004\), \(R=32.214\,\mathrm{cm}\) and \(\Delta f=110\,\mathrm{Hz}\). With these values the spectral amplitude is
Sensitivity for classical noise
The spectral amplitude \(h_S(w)\) represents the input GW spectrum that would produce a signal equal to the noise spectrum observed at the output of the antenna instrumentation.
A useful way to characterize the sensitivity of a GW detector is to calculate the \(h_S(w)\) such that with optimal filtering the signal to noise ratio
is equal to 1 for each bandwidth. Here
where \(\varvec{q}_2\) are the output of the second transducer’s resonators, \(\dagger \) stands for Hermitean conjugate. The sensitivity of the detector is obtained by searching for an input GW with amplitude \(\textbf{h}\) that mimics the thermal noise at the output, with \(\rho = 1\) per bandwidth. In other words we search for an \(\textbf{h}\) such that
or
As we do not know the polarization neither the direction of the incoming wave we take the mean over all angles
Then we obtain
and the amplitude spectral density \(h_S(w)=\sqrt{{{\tilde{h}}}_+^2+{{\tilde{h}}}_\times ^2}\)
The sensitivity curves for various kind of noises for each of the six transducers of the real antenna are shown in Fig. (4) using the parameters given in Table 3. In the case of a degenerated sphere the sensitivity curves for each of the six transducers would be as in Fig. 5.
The sensitivity of the Schenberg antenna will be better than the sensitivity of each transducer. Assuming that all transducers have the same sesitivity, the sensitivity of the Schenberg antenna (\(h_S\)) would be \((1/h_S)^2 = (1/h_{T1})^2 + (1/h_{T2})^2 + (1/h_{T3})^ 2 + (1/h_{T4})^2 + (1/h_{T5})^2 + (1/h_{T6})^2 = 6 \times (1/h_T)^2\), which implies that \(h_S = h_T/ \sqrt{6}\).
Discussions and conclusions
The calculation of the Schenberg antenna design sensitivity for each of the sphere six transducers was revised in this work taking into account both the degenerate (perfect sphere) and the non-degenerate sphere (quadrupole modes with their different frequencies), due to the symmetry break caused by the machining of the holes for the fixation of the transducers and the copper rod for the sphere suspension. As usual, all noises are referenced at the “input of the sphere” where the oscillating movement of the sphere surface occurs.
The dominant noises are the Brownian and the series noise, taking into account the parameters available for this initial version of the Schenberg antenna. For an advanced version of the Schenberg antenna (aSchenberg), which would reach the standard quantum limit of it (\(3.29\times 10^{- 23} \text {Hz}^{-1/2}\)), the sensitivity at each of the six transducers would be \(\sqrt{6}\) times this or (\(\sim 8\times 10^{- 23} \text {Hz}^{-1/2}\)). To achieve this sensitivity at each niobium transducer we have to replace them with sapphire or silicon transducers, and with niobium coating in the microwave cavity region. In this way, we could reach mechanical quality factors of the order of \(10^{8}\)63. The sphere would have to undergo annealing or be replaced by another material, such as beryllium copper. Values of mechanical Qs close to \(10^{8}\) have already been reached by Frossati (1996)64 for small copper-beryllium spheres.
Series noise can be minimized by rounding the edges of the transducer microwave klystron cavities, using a niobium deposition with less than 100 parts per million impurities, to increase the already achieved 380k electrical quality factor by a factor of 10 or more. The loss \(L_\text{amp}\) in the microwave transmission line that carry the signal from the transducer to the cryogenic amplifier (the first line of amplifiers in the system) would need to be reduced by a factor of 5. This could be achieved using niobium coaxial cables. Finally, the electronics used in the cryogenic amplifiers would need to be replaced by one that would reduce the noise temperature from 10 K to 1 K, at the operating frequency of 10 GHz.
All these modifications, necessary to reach the standard quantum limit, are challenging, but not impossible to achieve for the small spherical antenna of 0.65 m in diameter. As parametric transducers are used, it would be possible to perform signal squeezing and exceeds the standard quantum limit, but this would require higher mechanical and electrical Qs and even less noisy electronics, which starts to be unfeasible or doubtful to be achieved.
Note, however, that the sensitivity achieved by aLIGO in the O3 run has already reached the standard quantum limit of this spherical antenna, therefore, the only reasonable justification for remounting the Schenberg antenna and trying to place it in the sensitivity of the standard quantum limit would be to detect gravitational waves using another physical principle, different from the one used by laser interferometers. This other physical principle would be the absorption of the gravitational wave energy by a resonant mass. The question that arises, then, is whether gravitational wave signals reach Earth with sufficient amplitude to be detected by the spherical antenna operating at the standard quantum limit. To answer this question, we are analyzing aLIGO’s O3 data in the range where the Schenberg antenna is most sensitive: 3.15 kHz to 3.26 kHz, looking for any type of signal (burst, chirp, continuous or stochastic). We look forward to providing the results of this investigation in the near future.
In addition, we would like to point out that the innovations in this work are the sensitivity calculation for the non-degenerate case, new relations for the model matrix B, and redefinition of the effective mass. Also was inovative to use the experimental values of the monopole and quadrupole mode frequencies at 2 K and 300 K in the determination of the elastic constant of the material and as a consequence the value of the transversal and longitudinal sound speed.
Data availability
this manuscript has no associated data or the data will not be deposited. All data generated during this study are contained in this published article.
References
Abbott, B. P. et al. Observation of gravitational waves from a binary black hole merger. Phys. Rev. Lett. 116, 061102 (2016) arXiv:1602.03837 [gr-qc].
Abbott, B. P. et al. Binary black hole mergers in the first advanced LIGO observing run. Phys. Rev. X 6, 041015 (2016) arXiv:1606.04856 [grqc].
Abbott, B. P. et al. Improved analysis of GW150914 using a fully spin-precessing waveform model. Phys. Rev. X 6, 041014 (2016).
Abbott, B. P. et al. Properties of the binary black hole merger GW150914. Phys. Rev. X 116, 241102 (2016) arXiv:1602.03840 [gr-qc].
Abbott, B. P. et al. GW170817: Observation of gravitational waves from a binary neutron star inspiral. Phys. Rev. Lett. 119, 161101 (2017).
Abbott, B. P. et al. Multi-messenger observations of a binary neutron star merger. Apjl 848, L12 (2017) arXiv:1710.05833 [astro-ph.HE].
Melo, J. L., Velloso, W. F. Jr. & Aguiar, O. D. Vibration isolation support design for the SCHENBERG detector. Class. Quantum Gravity 19, 1985 (2002).
da Silva Bortoli, F. et al. On the massive antenna suspension system in the Brazilian gravitational wave detector SCHENBERG. Braz. J. Phys. 46, 308 (2016) (cited By :23).
de Waard, A., Gottardi, L. & Frossati, G. MiniGRAIL progress report 2001: The first cooldown. Class. Quantum Gravity 19, 1935 (2002).
de Paula, L. A. N., Ferreira, E. C., Carvalho, N. C. & Aguiar, O. D. High sensitivity niobium parametric transducer for the Mario Schenberg gravitational wave detector. J. Instrum. 10, P03001 (2015).
Liccardo, V. et al. Study of the effect of NbN on microwave Niobium cavities for gravitational wave detectors. J. Instrum. 11, P07004 (2016).
da Silva Bortoli, F., Frajuca, C., Magalhaes, N. S., Aguiar, O. D. & de Souza, S. T. On the cabling seismic isolation for the microwave transducers of the Schenberg detector. Braz. J. Phys. 49, 133 (2019) (cited By :15).
Frajuca, C. et al. Optimization of a composite quadrupole mass at high-speed rotation. J. Braz. Soc. Mech. Sci. Eng. 40, 319 (2018).
Bortoli, F. S., Frajuca, C., Magalhaes, N. S., de Souza, S. T. & da Silva Junior, W. C. On the dilution refrigerator thermal connection for the SCHENBERG gravitational wave detector. Braz. J. Phys. 50, 541 (2020).
Forward, R. L. Multidirectional, multipolarization antennas for scalar and tensor gravitational radiation. Gen. Relativ. Gravit. 2, 149 (1971).
Coccia, E., Lobo, J. A. & Ortega, J. A. Proposed gravitational wave observatory based on solid elastic spheres. Prd 52, 3735 (1995).
Harry, G. M., Stevenson, T. R. & Paik, H. J. Detectability of gravitational wave events by spherical resonant-mass antennas. Prd 54, 2409 (1996) arXiv:gr-qc/9602018.
Lobo, J. A. Multiple mode gravitational wave detection with a spherical antenna. Mnras 316, 173 (2000) arXiv:gr-qc/0006109.
Johnson, W. W. & Merkowitz, S. M. Truncated icosahedral gravitational wave antenna. Phys. Rev. Lett. 70, 2367 (1993).
Aguiar, O. D. et al. The Brazilian gravitational wave detector Mario Schenberg: Status report. Class. Quantum Gravity 23, S239 (2006).
Aguiar, O. D. et al. Status report of the Schenberg gravitational wave antenna. J. Phys. Conf. Ser. J. Phys. Conf. Ser. 363, 012003 (2023).
Messina, J. F. Question of Planckian “Action’’ in Gravitational wave detection experiments. Prog. Phys. 11, 202 (2015).
de Paula, W. L. S., Miranda, O. D. & Marinho, R. M. Polarization states of gravitational waves with a massive graviton. Class. Quantum Gravity 21, 4595 (2004).
Lee, W. H., Ramirez-Ruiz, E. & van de Ven, G. Short gamma-ray bursts from dynamically assembled compact binaries in globular clusters: Pathways, rates, hydrodynamics, and cosmological setting. Apj 720, 953 (2010) arXiv:0909.2884 [astro-ph.HE].
Shibata, M. & Taniguchi, K. Coalescence of black hole-neutron star binaries. Living Rev. Relativ. 14, 6 (2011).
Foucart, F. et al. Neutron star-black hole mergers with a nuclear equation of state and neutrino cooling: Dependence in the binary parameters. Prd 90, 024026 (2014) arXiv:1405.1121 [astro-ph.HE].
Buonanno, A. & Damour, T. Effective one-body approach to general relativistic two-body dynamics. Prd 59, 084006 (1999) arXiv:gr-qc/9811091.
Buonanno, A. & Damour, T. Transition from inspiral to plunge in binary black hole coalescences. Prd 62, 064015 (2000) arXiv:gr-qc/0001013.
Nakar, E. Short-hard gamma-ray bursts. Physrep 442, 166 (2007) arXiv:astro-ph/0701748.
Berger, E. Short-duration gamma-ray bursts. Araa 52, 43 (2014) arXiv:1311.2603 [astro-ph.HE].
Magalhaes, N. S., Johnson, W. W., Frajuca, C. & Aguiar, O. D. Determination of astrophysical parameters from the spherical gravitational wave detector data. Mnras 274, 670 (1995).
Magalhães, N. S., Johnson, W. W., Frajuca, C. & Aguiar, O. D. A geometric method for location of gravitational wave sources. Apj 475, 462 (1997).
Lenzi, C. H. et al. Solution of the inverse problem in spherical gravitational wave detectors using a model with independent bars. Phys. Rev. D 78, 062005 (2008).
Lenzi, C. H. et al. Astrophysics from data analysis of spherical gravitational wave detectors. Gen. Relativ. Gravit. 40, 183 (2008).
Dal Canton, T. et al. Implementing a search for aligned-spin neutron star-black hole systems with advanced ground based gravitational wave detectors. Phys. Rev. D 90, 082004 (2014) arXiv:1405.6731 [gr-qc].
Usman, S. A. et al. The PyCBC search for gravitational waves from compact binary coalescence. Class. Quant. Grav. 33, 215004 (2016) arXiv:1508.02357 [gr-qc].
Damour, T. & Nagar, A. Improved analytical description of inspiralling and coalescing black-hole binaries. Prd 79, 081503 (2009) arXiv:0902.0136 [gr-qc].
Pan, Y. et al. Inspiral-merger-ringdown multipolar waveforms of nonspinning black-hole binaries using the effective-one-body formalism. Prd 84, 124052 (2011) arXiv:1106.1021 [gr-qc].
Bauswein, A., Pulpillo, R. A., Janka, H.-T. & Goriely, S. Nucleosynthesis constraints on the neutron star-black hole merger rate. Astrophys. J. Lett. 795, L9 (2014).
Abbott, B. P. et al. Observation of gravitational waves from two neutron star-black hole coalescences. Astrophys. J. Lett. 915, L5 (2021).
Abadie, J. et al. TOPICAL REVIEW: Predictions for the rates of compact binary coalescences observable by ground-based gravitational-wave detectors. Class. Quantum Gravity 27, 173001 (2010) arXiv:1003.2480 [astro-ph.HE].
Dominik, M. et al. Double compact objects III: Gravitational-wave detection rates. Apj 806, 263 (2015) arXiv:1405.7016 [astro-ph.HE].
Li, X., Hu, Y.-M., Jin, Z.-P., Fan, Y.-Z. & Wei, D.-M. Neutron star-black hole coalescence rate inferred from macronova observations. Apjl 844, L22 (2017) arXiv:1611.01760 [astroph. HE].
Abbott, B. P. et al. Upper limits on the rates of binary neutron star and neutron star-black hole mergers from advanced LIGO’s first observing run. Apjl 832, L21 (2016) arXiv:1607.07456 [astro-ph.HE].
Voss, R. & Tauris, T. M. Galactic distribution of merging neutron stars and black holes - prospects for short gamma-ray burst progenitors and LIGO/VIRGO. Mnras 342, 1169 (2003) arXiv:astro-ph/0303227.
Kalogera, V., Belczynski, K., Kim, C., O’Shaughnessy, R. & Willems, B. Formation of double compact objects. Physrep 442, 75 (2007) arXiv:astro-ph/0612144.
O’Shaughnessy, R., Kim, C., Kalogera, V. & Belczynski, K. Constraining population synthesis models via empirical binary compact object merger and supernova rates. Astrophys. J. 672, 479 (2008).
O’Shaughnessy, R., Kalogera, V. & Belczynski, K. Binary compact object coalescence rates: The role of elliptical galaxies. Astrophys. J. 716, 615 (2010).
Maggiore, M. Gravitational Waves. Theory and Experiments (Oxford, 2008).
Merkowitz, S. M. & Johnson, W. W. Techniques for detecting gravitational waves with a spherical antenna. Phys. Rev. D 56, 7513 (1997).
Landau, L. D. & Lifshitz, E. M. Theory of Elasticity 3rd ed., 6, Vol. 7 (Pergamon Press, 1986).
Lobo, J. A. What can we learn about gravitational wave physics with an elastic spherical antenna. Phys. Rev. D 52, 591 (1995).
Ashcroft, N. D. & Mermin, N. W. Solid State Physics (Harcourt College Publishers, 1976).
Reif, F. Fundamentals of Statistical and thermal Physics (McGraw Hill, 1981).
Ross, R. B. Metallic Materials Specification Handbook (Springer, 1992).
Callen, H. B. Thermodynamics (John Wiley & Sons, 1960).
Richard, J.-P. Wide-band bar detectors of gravitational radiation. Phys. Rev. Lett. 52, 165 (1984).
Caughey, T. K. Les vibrations forcées dans les systèmes non-linéaires, 393 (1965).
McDonough, R. & Whalen, A. Detection of Signals in Noise (Academic Press, 1995).
Tobar, M. E., Ivanov, E. N. & Blair, D. G. Parametric transducers for the advanced cryogenic resonant-mass gravitational wave detectors. Gen. Rel. Grav. 32, 1799 (2000).
Wainshtein, L. & Zubakov, V. Extraction of Signals from Noise: By L.A. Wainstein (and) V.D. Zubakov (Prentice-Hall, 1962).
Landau, L. D. & Lifshitz, E. M. Mechanique 2ed., 1. (MIR, 1966).
Locke, C. Towards Measurement of the Standard Quantum Limit of a Macroscopic Harmonic Oscillator, Ph.D. thesis, University of Western Australia (2001).
Frossati, G. MiniGRAIL progress report 2001: The first cooldown, in Proceedings of the First International Workshop on Omnidirectional Gravitational Radiation Observatory (World Scientific, 1997).
Macleod, D., Urban, A. L., Coughlin, S., Massinger, T., Pitkin, M., Altin, P., Areeda, J., Quintero, E., & Leinweber, K. GWpy: Python package for studying data from gravitational-wave detectors, astrophysics source code library. Record ascl:1912.016 (2019). arXiv:ascl:1912016
Bezanson, J., Karpinski, S., Shah, V. B. & Edelman, A. arXiv e-prints , arXiv:1209.5145 (2012). arXiv:1209.5145 [cs.PL].
Acknowledgements
The authors would like to acknowledge Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) for financial support under the grant numbers 1998/13468-9, 2006/56041-3, 2013/26258-4, 2017/05660-0, 2018/02026-0, and 2020/05238-9. ODA thanks the Brazilian Ministry of Science, Technology and Inovations and the Brazilian Space Agency as well. Support from the Conselho Nacional de Desenvolvimento Cientifíco e Tecnológico (CNPq) is also acknowledged under the grants number 302841/2017-2, 310087/2021-0, and 312454/2021. This research made use of GWpy, a Python package for gravitational-wave astrophysics65 and the Julia programming language (https://julialang.org)66.
Author information
Authors and Affiliations
Contributions
V.L. and C.L. wrote the main manuscript text and carried out the most of the analysis. R.M. provided some figures while the rest of the author participated to the review of the paper.
Corresponding author
Ethics declarations
Competing interests
The authors declare no competing interests.
Additional information
Publisher's note
Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.
Supplementary Information
Rights and permissions
Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/.
About this article
Cite this article
Liccardo, V., Lenzi, C.H., Marinho, R.M. et al. The design strain sensitivity of the schenberg spherical resonant antenna for gravitational waves. Sci Rep 13, 17706 (2023). https://doi.org/10.1038/s41598-023-43808-1
Received:
Accepted:
Published:
DOI: https://doi.org/10.1038/s41598-023-43808-1
Comments
By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.