Abstract
Although experimental efforts have been active for about 30 years, a direct laboratory observation of vacuum magnetic birefringence, due to vacuum fluctuations, still needs confirmation: the predicted birefringence of vacuum is \(\Delta n = 4.0\times 10^{24}\) @ 1 T. Key ingredients of a polarimeter for detecting such a small birefringence are a long optical path within the magnetic field and a time dependent effect. To lengthen the optical path a Fabry–Perot is generally used with a finesse ranging from \({{\mathscr {F}}} \approx 10^4\) to \({{\mathscr {F}}} \approx 7\times 10^5\). Interestingly, there is a difficulty in reaching the predicted shot noise limit of such polarimeters. We have measured the ellipticity and rotation noises along with CottonMouton and Faraday effects as a function of the finesse of the cavity of the PVLAS polarimeter. The observations are consistent with the idea that the cavity mirrors generate a birefringencedominated noise whose ellipticity is amplified by the cavity itself. The optical path difference sensitivity at \(10\;\hbox {Hz}\) is \(S_{\Delta {{\mathscr {D}}}}=6\times 10^{19}\;\hbox {m}/\sqrt{\mathrm{Hz}}\), a value which we believe is consistent with an intrinsic thermal noise in the mirror coatings. Our findings prove that the continuous efforts to increase the finesse of the cavity to improve the sensitivity has reached a limit.
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1 Introduction
The development of extremely sensitive polarimeters has been driven in recent years by attempts to measure directly vacuum magnetic birefringence, a non linear quantum electrodynamic effect in vacuum closely related to lightbylight elastic scattering. Non linear electrodynamic effects in vacuum were first predicted in 1935 by the Euler–Kockel perturbative effective Lagrangian density [1,2,3,4,5,6,7,8,9,10,11,12],
which takes into account vacuum fluctuations with the creation of electronpositron pairs. As of today, \({{\mathscr {L}}}_{\mathrm{EK}}\) still needs direct experimental confirmation at low energies. This Lagrangian density is valid for field intensities much lower than the critical values: \(B \ll B_{\mathrm{crit}}={m_e^{2}c^{2}}/{e \hbar }=4.4\times 10^{9}~\hbox {T}\), \(E \ll E_{\mathrm{crit}}={m_e^{2}c^{3}}/{e \hbar }=1.3\times 10^{18}~\hbox {V}/\hbox {m}\). Here
describes the entity of the quantum correction to Classical Electrodynamics. The Lagrangian density (1) predicts that vacuum becomes birefringent in the presence of either an external electric or magnetic field [8,9,10,11,12]. In the case of an external magnetic field the unitary birefringence, to order \(\alpha ^2\), is expected to be,
In the presence of an external electric field, \(B^2\) is replaced by \(\left( E/c\right) ^2\).
Due to this birefringence, a linearly polarised beam of light propagating perpendicularly to the external magnetic field acquires an ellipticity \(\psi \),
where \(\psi _0\) is the ellipticity amplitude, \(\lambda \) is the wavelength of the light, L is the length of the magnetic field and \(\vartheta \) is the angle between the magnetic field and the polarisation direction. With the parameters of the PVLAS experiment [13], \(B = 2.5\;\hbox {T}\), \(L = 1.64\;\hbox {m}\) and \(\lambda = 1064\;\hbox {nm}\), the induced ellipticity is \(\psi = 1.2\times 10^{17}\), an extremely small value. As we will see in the following section, one way to enhance the induced ellipticity is to increase the effective length of the magnetic field region using a Fabry–Perot cavity with finesse \({{\mathscr {F}}}\). Such a cavity enhances an ellipticity (or a rotation) by a factor \(N = 2{{\mathscr {F}}}/\pi \) [14,15,16,17] which, today, can be as high as \(N = 4.5\times 10^5\) [18].
Several experiments are underway, of which the most sensitive at present are based on polarimeters with such very high finesse Fabry–Perot cavities [19,20,21,22]. Furthermore all of these experiments use variable magnetic fields in order to induce a time dependent effect hence further increasing their sensitivities. This time dependence can be obtained either by varying the magnetic field intensity, in which case \(\Delta n = \Delta n(t)\), or by rotating the field direction in a plane perpendicular to the propagation direction such that \(\vartheta = \vartheta (t)\). In this second case, adopted by the PVLAS experiment [19] with \(N = 4.5\times 10^5\), the signal to be measured is,
At present the lowest measured value for \(\Delta n/B^2\) is [23],
The experimental uncertainty on this value is a factor of about seven above the predicted QED value in Eq. (3).
2 Polarimetry: state of the art
A scheme of the PVLAS polarimeter is shown in Fig. 1. A beam first passes through a polariser and then enters the Fabry–Perot cavity composed of two highreflectance mirrors placed at a distance \(D = 3.303\;\hbox {m}\) apart. Between the mirrors is a magnetic field of length L which, in the case of the PVLAS experiment, is generated by two identical rotating permanent magnets characterised by the total parameter \(\int _0^L{B^2 dl} = 10.25\;\hbox {T}^2\hbox {m}\) resulting in an average field \(B = 2.5\;\hbox {T}\) over a length \(L = 1.64\;\hbox {m}\). These two magnets have been rotated up to a frequency \(\nu _{B} = 23\;\hbox {Hz}\). Given the dependence of the induced ellipticity \(\psi (t)\) with \(2\vartheta (t)\), the ellipticity signal due to magnetic birefringence has a frequency component at \(2\nu _{B}\). Since the magnetic field could in principle also generate rotations \(\phi (t)\) due to a magnetic dichroism (for example from axionlike particles [24]) in Fig. 1 the total effect is indicated with a complex number \(\xi = \phi + i\psi \). Indeed one can assign an absolute phase to the electric field of the light such that a rotation is described by a pure real number whereas an ellipticity is a pure imaginary quantity. After the output mirror, an ellipticity modulator adds a known ellipticity of amplitude \(\eta _0\ll 1\) to the polarisation at a frequency \(\nu _{m}\gg \nu _B\). The beam of power \(I_0\) then passes through an analyser (a polariser set to extinction) which divides the light into two polarisation components: parallel and perpendicular to the input polariser, \(I_\parallel \) and \(I_\perp \) respectively. These beams are collected by the two photodiodes PDT and PDE with efficiencies \(q = 0.7\;\hbox {A}/\hbox {W}\).
If all ellipticities (and rotations) are small these add algebraically. In the presence of both a rotation \(\Phi (t)=N\phi (t)\) and an ellipticity \(\Psi (t) = N\psi (t)\) (\(\Phi ,\Psi \ll 1\)) and without the presence of the quarterwave plate shown in Fig. 1, the power reaching PDE is
As can be seen, only the ellipticity \(\Psi (t)\) beats with the effect of the modulator \(\eta (t)\). The modulation amplitude \(\eta _0\) must be chosen such that the term \(\eta _0^2/2\) is well above the noise in the PDE signal: generally \(\Phi (t), \Psi (t) \ll \eta _0\). If \(\eta (t)\) and \(\Psi (t)\) are sinusoidal functions at frequencies \(\nu _m\) and \(\nu \) respectively (having chosen \(\nu _m\approx 50\;\hbox {kHz}\)), the product \(2\eta (t)\Psi (t)\) generates Fourier components at \(\nu _m\pm \nu \).
By demodulating the current signal from PDE \(i^{\mathrm{ell}}_\perp (t) = qI^{\mathrm{ell}}_\perp (t)\) at the frequencies \(\nu _{m}\) and \(2\nu _{m}\), one obtains the inphase Fourier components,
from which one can extract the amplitude (with relative sign) for \(\Psi _0\):
By inserting the quarterwave plate with one of its axes aligned with the polarisation, the ellipticity generated by the magnetic field becomes a rotation and viceversa [25]. In this case, the power reaching PDE is,
where the signs depend on whether the polarisation is aligned with the fast or the slow axis of the \(\lambda /4\) wave plate. Again the value of \(\Phi _0(\nu )\) can be extracted using the same expressions in Eq. (9). We explicitly note that Eqs. (7), (9) and (10) hold for both an ellipticity/rotation signal and for an ellipticity/rotation noise.
In the spectra obtained from Eq. (9), an ellipticity generated by a magnetic birefringence or a rotation generated by a magnetic dichroism will appear at \(\nu = 2\nu _{B}\) whereas a rotation due to a time dependent Faraday effect at \(\nu _F\) will appear at \(\nu = \nu _{F}\).
Given the scheme in Fig. 1, one can determine the expected peak ellipticity sensitivity \(S_\Psi (\nu )\) of the polarimeter in the presence of various noise sources (see Fig. 2). All noise contributions will be expressed as electric currents. In general the rms noise measured at the output of the demodulator at a frequency \(\nu \) is the incoherent sum of the rms noise densities \(S_{+}\) and \(S_{}\) respectively at the frequencies \(\nu _m+\nu \) and \(\nu _m\nu \). Generally \(S_{+}=S_{}=S_{\nu }\). Using Eq. (9) one finds,
The ultimate peak sensitivity \(S_\Psi \) of such a polarimeter is given by the shotnoise limit. The rms current spectral density \(i^{\mathrm{shot}}\) at PDE due to an incident d.c. light power \(I_\perp {\mathrm{(dc)}}\) is,
constant over the whole spectrum. Equation (11) then leads to,
where we have introduced the extinction ratio of the polarisers \(\sigma ^2\) and we have introduced \(I_\parallel \) as a measurement of \(I_0\). If the modulation term is \(\eta _0^2/2\gg \sigma ^2\), the above expression simplifies to,
Typical working values for the extinction ratio \(\sigma ^2\) and the modulation amplitude \(\eta _0\) are \(\sigma ^2 \lesssim 10^{7}\) and \(\eta _0\approx 10^{2}\). The extinction ratio reported is with the cavity and the modulator crystal inserted. It does not change significantly when the QWP is also inserted. As will be discussed below, the value of the power \(I_0\approx I_\parallel \) at the output of the cavity used in the PVLAS setup during the measurements presented in this work is \(I_\parallel = 0.7\;\hbox {mW}\) from which one obtains a shot noise peak sensitivity of,
With the effect to be measured \(\Psi =5.4\times 10^{11}\) and with the above shot noise the measurement time for a unitary signaltonoise ratio should be \(T = \left( {S^{\mathrm{shot}} _\Psi }/{\Psi }\right) ^2 = 1.1\times 10^5\;\hbox {s}\), in principle a reasonable integration time.
Considering other known noise sources such as the Johnson noise, \(i^{\mathrm{JN}}\), the diode dark current noise \(i^{\mathrm{DN}}\) and the laser’s relative intensity noise \(i^{\mathrm{RIN}}\) one obtains the curves shown in Fig. 2 for the sensitivity as a function of the modulation amplitude \(\eta _0\) [19]. As can be seen there is a region in the modulation amplitude around \(\eta _0\approx 2\times 10^{2}\) which should in principle allow shot noise sensitivity.
The outofphase quadrature signal \(i^{\mathrm{qu}}_{\nu _{m}}(\nu )\) at the output of the demodulator can be used as a good measurement of noise contributions uncorrelated to ellipticity noise. In principle, if \(S_\Psi (\nu )\) was limited by one of the wide band noises reported in Fig. 2 then \(i_{\nu _{m}}(\nu ) = i^{\mathrm{qu}}_{\nu _{m}}(\nu )\). Unfortunately this is not the case and the measured sensitivity of the PVLAS polarimeter when measuring ellipticities with \(N = 4.5\times 10^5\) is significantly worse than the values in Fig. 2: \(S_\Psi ^{\mathrm{PVLAS}} \sim 35\times 10^{7}/\sqrt{\mathrm{Hz}}\) for frequencies \(\nu \sim 10\)–20 Hz and \(\eta _0 = 10^{2}\).
To better understand the actual sensitivity reached by the PVLAS experiment one should consider, rather than the ellipticity, the sensitivity in optical path difference \(\Delta {{\mathscr {D}}} =\int \nolimits _{path}{\Delta n\; dl}\):
between 10 and 20 Hz. This value can be compared to the ones for gravitational wave detection using interferometer techniques [26]. Indeed the quantities to be compared are,
where \(l_{\mathrm{arm}}\) is the arm length of the gravitational wave interferometer and \(h_{\mathrm{sens}}\) is its sensitivity in strain [26]. For example in Advanced LIGO (Figure 2 of Ref. [27]) with \(l_{\mathrm{arm}} = 4000\;\hbox {m}\) and \(h_{\mathrm{sens}} \approx 1.5\times 10^{22}/\sqrt{\mathrm{Hz }} \,@ 20\hbox { Hz}\), one finds \(S_{\Delta {{\mathscr {D}}}} \approx 10^{18}\;\hbox {m}/\sqrt{\mathrm{Hz}}\), a value slightly above the one of the PVLAS experiment. It must also be noted that gravitational wave interferometers are not shot noise limited at these frequencies but are limited by technical noises [27].
Interestingly, all of the past and present experimental efforts also have been limited by a yet to be understood wide band noise. In Fig. 3 we report the optical path difference sensitivities of past and present experiments dedicated to measuring vacuum magnetic birefringence with optical techniques. These sensitivities are plotted as a function of the frequencies at which each experiment typically works/worked at. Although each experiment is characterised by a different finesse of the cavity and uses different detection schemes (heterodyne, homodyne), the sensitivities lie on a common power law \(\propto \nu ^{x}\) with \(x = 0.78\pm 0.03\). The only experiment significantly above this common curve is BFRT [28]. This is the oldest effort and used a multipass cavity with separate optical benches rather than a Fabry–Perot. The mirrors were also of different fabrication. Furthermore all of these sensitivities are well above their expected shot noise limit with the exception of the OVAL experiment which uses a very low power of \(10\;\upmu \hbox {W}\) at the output of the cavity and whose sensitivity coincides with its expected one [22].
Finally, without the presence of the Fabry–Perot cavity the PVLAS polarimeter reaches shotnoise sensitivity above \(\nu \sim 10\;\hbox {Hz}\). Below this frequency the noise is due to pointing fluctuations of the laser beam coupled to birefringence gradients present in all optical elements.
A possibile interpretation of the general behaviour shown in Fig. 3 is that there is an intrinsic birefringence noise being generated in the mirror reflective coatings. Given the order of magnitude of the sensitivities in Fig. 3 we believe that we have reached a thermal intrinsic noise in birefringence, not induced by the laser power, but due to the mirrors in thermal equilibrium at \(T \approx 300\hbox { K}\).
To verify whether the excess noise present in the PVLAS experiment is indeed a birefringence noise originating from the reflective coatings of the mirrors we performed a series of measurements both in ellipticity and in rotation as a function of the finesse of our cavity. The measurements were performed with a pure birefringence signal due to Argon gas at a pressure \(P\approx 0.85\;\hbox {mbar}\) and with an external solenoid generating a Faraday rotation on the input mirror of the cavity. In this paper the results of these measurements are presented showing that indeed the excess noise is dominated by birefringence noise and that the ellipticity noise is proportional to the finesse of the cavity.
3 Method
The basic scheme of our polarimeter was described above but to fully understand the measurements we are going to present, we must here include some extra details.
3.1 Mirror birefringence
The most important point is that the mirrors of Fabry–Perot cavities always present an intrinsic structured birefringence [32] over the reflecting surface. The composition of the birefringence of the two mirrors can be treated as a single birefringent element [33] inside a perfect non birefringent cavity. If \(\alpha _1\) and \(\alpha _2\) are the phase retardations upon reflection on each mirror for two polarisations parallel and perpendicular to their slow axis and if we take as a reference angle the slow axis of the first mirror then, per round trip, the two mirrors are equivalent to a single birefringent element with a total retardation \(\alpha _{\mathrm{EQ}}\) at an angle \(\vartheta _{\mathrm{EQ}}\) with respect to the first mirror’s slow axis [33]:
where \(\vartheta _{\mathrm{WP}}\) is the angular position of the slow axis of the second mirror. Typical values for \(\alpha _{1,2}\) are \(\sim \,10^{7} \,\mathrm{to}\, 10^{5}\;\)rad. This leads to a high finesse cavity having two non degenerate resonances slightly separated in frequency by,
where \(\nu _{fsr} = \frac{c}{2D}\) is the cavity’s free spectral range. This separation is to be compared with each resonance’s FWHM \(\Delta \nu _{\mathrm{cav}} = \nu _{fsr}/{{\mathscr {F}}}\).
To reach a good extinction, necessary to have a good sensitivity, the input polarisation must be aligned to one of the axes of the cavity’s equivalent birefringence. In this way no component perpendicular to \(E_\parallel \) will be generated by the cavity itself. The reflected light used to lock the laser to the cavity has a polarisation parallel to the input polariser. For this reason the laser is locked to only one of the two resonances whereas the ellipticity (or rotation) signal will respond to the resonance shifted by \(\Delta \nu _{\mathrm{sep}}\).
As discussed in Refs. [17, 19] the ratio \(\Delta \nu _\mathrm{sep}/\Delta \nu _\mathrm{cav} = {{\mathscr {F}}}\frac{\alpha _\mathrm{EQ}}{2\pi }= \frac{1}{2}\frac{N\alpha _\mathrm{EQ}}{2}\) leads to an extra phase between the two perpendicular polarisation states and to a reduction of the signal. Assuming the presence of only an ellipticity \(\Psi _0\) the resulting expression for \(E_\perp (t)\) is:
where,
The expression for \(E_\perp (t)\) is actually only valid in the limit of low frequencies with \(\nu \ll \Delta \nu _\mathrm{cav}\), as will be discussed in Sect. 3.2. Apart from a reduction of the accumulated ellipticity \(\Psi _0\) by a factor \(k(\alpha _\mathrm{EQ})\), \(E_\perp (t)\) is no longer a pure imaginary number but also has a real component corresponding to a rotation \(\frac{N\alpha _\mathrm{EQ}}{2}k(\alpha _\mathrm{EQ})\Psi _0\). The result of this modification of \(E_\perp (t)\) is therefore a mixing of an ellipticity and a rotation by a factor \(\frac{N\alpha _\mathrm{EQ}}{2}\). The same mixing occurs in the presence of a pure rotation.
In the presence of both an accumulated rotation \(\Phi _0 = N\phi _0\) and an accumulated ellipticity \(\Psi _0 = N\psi _0\) the measured ellipticity \(\Psi _{\nu \rightarrow 0}^\mathrm{meas}\) and the measured rotation \(\Phi _{\nu \rightarrow 0}^\mathrm{meas}\) can therefore be determined from (\(\nu \ll \Delta \nu _\mathrm{cav}\)),
Measuring \(\alpha _\mathrm{EQ}\) is thus fundamental to disentangle ellipticities and rotations.
Having measured the finesse of the cavity and considering the presence of a pure ellipticity only \((\Phi _0 = 0)\) one finds that (\(\nu \ll \Delta \nu _\mathrm{cav}\)),
gives a direct value for \(\alpha _\mathrm{EQ}\). The same is true in the presence of a pure rotation \((\Psi _0 = 0)\) in which case,
The determination of \(\alpha _\mathrm{EQ}\) can therefore be easily done either by measuring a CottonMouton signal or a Faraday effect, in either case with and without the quarterwave plate inserted. In the next sections we will see how these must be modified to determine \(\alpha _\mathrm{EQ}\) also for frequencies \(\nu \gtrsim \nu _\mathrm{cut}\).
As we will see below, the mixing of an ellipticity with a rotation will also help us understand the origin of the excess noise typically observed in polarimeters based on high finesse cavities.
3.2 Frequency response
In the previous paragraph we introduced the mixing between ellipticities and rotations due to the cavity birefringence in the low frequency limit. Due to the relatively narrow cavity width \(\Delta \nu _\mathrm{cav}\sim 65\;\hbox {Hz}\) with respect to the frequencies of our signals it is important to take into account the frequency response of the system.
An ideal Fabry–Perot behaves as a first order low pass filter with a frequency cutoff \(\nu _\mathrm{cut}\) determined by the cavity line width \(\Delta \nu _\mathrm{cav}\):
Therefore in the presence of a non birefringent cavity the measurement of an ellipticity signal generated by a time dependent birefringence at a frequency \(\nu \) will be filtered according to [31],
With a finesse \({{\mathscr {F}}} = 7\times 10^5\) and a Fabry–Perot length \(D = 3.303\;\hbox {m}\), as is the case in the PVLAS experiment, the frequency cutoff is \(\nu _\mathrm{cut} = 32\;\hbox {Hz}\).
3.2.1 The case for \(N\alpha _\mathrm{EQ}\ll 1\)
Considering now a birefringent cavity, it can be shown [34] that for \(N\alpha _\mathrm{EQ}\ll 1\) the frequency response of the measured rotation signal in the presence of a time dependent pure birefringence (or viceversa the ellipticity signal in the presence of an effect generating a pure rotation) is well approximated by,
The expressions given in Eqs. (23) and (24) therefore become,
Significant filtering is therefore present already for frequencies \(\nu \simeq \nu _\mathrm{cut}\). Furthermore the two mixing quantities have different frequency responses.
3.2.2 The case for \(N\alpha _\mathrm{EQ}\lesssim 1\)
If \(N\alpha _\mathrm{EQ}\lesssim 1\), as is the case under consideration as we will see below, the first and second order filters of the Fabry–Perot, \(h_0(\nu )\) and \(H_0(\nu )\), deviate significantly from the standard curves given in Eqs. (28) and (29), respectively. Remembering that \(\Psi _0= N\psi _0\) and that similarly \(\Phi _0 = N\phi _0\), the multiplicative factors \(Nk(\alpha _\mathrm{EQ})h_0(\nu )\) and \(Nk(\alpha _\mathrm{EQ})H_0(\nu )\frac{N\alpha _\mathrm{EQ}}{2}\) in Eqs. (30) and (31) must be substituted with the more complicated expressions [34]:
where \(\delta = \frac{2\pi }{\nu _{fsr}}\nu \) and R is the reflectance of the mirrors (assumed to be equal). In the limits for \(\alpha _\mathrm{EQ}\ll 1\) and \(\delta \ll 1\), the righthand sides of these expressions correctly reduce to their lefthand sides.
Although these expressions are rather bulky separately, it can be shown that the ratio of the righthand sides of Eqs. (33)–(32) reduces to the same expression as in the case \(N\alpha _\mathrm{EQ}\ll 1\):
Even for \(N\alpha _\mathrm{EQ}/2\sim 1\) this ratio is proportional to a simple first order filter \(h_0(\nu )\). We will therefore define a modified first order filter function \(h_{\alpha _\mathrm{EQ}}(\nu )\) from,
and in Eqs. (30) and (31) we can therefore make the substitutions,
In Fig. 4 we report the comparison of \(h_0(\nu )\) with \(h_{\alpha _\mathrm{EQ}}(\nu )\) for two different values of \(\frac{N\alpha _\mathrm{EQ}}{2}\): 0.50 and 0.17. Given that our values of \(N\alpha _\mathrm{EQ}/2\), as we will see below, are close to the values reported in the Fig. 4, to correctly interpret our noise spectra the more general expression of \(h_{\alpha _\mathrm{EQ}}(\nu )\) must be used.
With all these considerations the measured values for \(\Psi ^\mathrm{meas}\) and \(\Phi ^\mathrm{meas}\) as a function of \(\Psi _0\), \(\Phi _0\) and \(\alpha _\mathrm{EQ}\) are finally,
where the ratio,
gives a direct value for \(\alpha _\mathrm{EQ}\). The same is true in the presence of an effect generating a pure rotation \((\Psi _0 = 0)\) in which case,
These last four Eqs. (38)–(41) will be used when analysing our data in what follows.
3.3 Noise studies
By studying the noise spectra in ellipticity and rotation and the CottonMouton and Faraday signals one can understand whether the noises \(S_\Psi (\nu )\) and \(S_\Phi (\nu )\) are proportional to N or not and therefore if they originate from inside or outside of the cavity. Moreover by comparing the measured ellipticity noise \(S_{\Psi ^\mathrm{meas}}(\nu )\) with the measured rotation noise \(S_{\Phi ^\mathrm{meas}}(\nu )\) one can determine whether they are dominated by an ellipticity noise \(S_\Psi (\nu )\) or a rotation noise \(S_\Phi (\nu )\).
Since the measured noise both in ellipticity and in rotation is significantly greater than the expected noise, we assume independent contributions by both ellipticity and/or rotation noises, \(S_{\Psi ^\mathrm{meas}}(\nu )\) and \(S_{\Phi ^\mathrm{meas}}(\nu )\), generated and amplified inside the cavity. Hence we use, for the noise densities, the same expressions (38) and (39) used for the signals. We therefore model the measured spectral noise densities as,
where \(S_\Psi (\nu )=Ns_\psi (\nu )\) and \(S_\Phi (\nu )=Ns_\phi (\nu )\) are respectively the ellipticity and the rotation spectral densities and where we have added white noise contributions \(S_r\) and \(S_e\) to \(S_{\Phi ^\mathrm{meas}}(\nu )\) and \(S_{\Psi ^\mathrm{meas}}(\nu )\) respectively.
4 Measurements
Let us remind the reader that the aim of the present work is to study the signaltonoise ratio in the PVLAS apparatus as a function of the finesse of the Fabry–Perot cavity. To reduce the finesse of the cavity we have introduced controlled extra losses p to the Fabry–Perot cavity. Given the transmittance T and the intrinsic losses \(p_0\) of the mirrors, p will cause the finesse \({{\mathscr {F}}}\) and the output intensity \(I_0\) to change according to,
In the case of the PVLAS cavity, the best finesse measured was \({{\mathscr {F}}} \approx 7.7\times 10^5\) with a 25% transmission [18], corresponding to \(p_0 = (1.7\pm 0.2)\;\hbox {ppm}\) and a transmittance of each mirror (assumed to be equal) \(T = 2.4\pm 0.2\;\hbox {ppm}\). Therefore an extra loss \(p\approx 0\div 10~\hbox {ppm}\) will change the finesse from \({{\mathscr {F}}} = 7.7\times 10^5\) to \({{\mathscr {F}}} =2.5 \times 10^5\).
To introduce these extra losses we have used one of the manual vacuum gate valves present in front of the output mirror to clip the Gaussian mode between the mirrors. With a width \(r_0\) of the intensity profile of the Gaussian mode and therefore \(\sigma = \frac{r_0}{2}\), clipping at \((4.55) \sigma \) level is sufficient to achieve the desired losses p. An estimate can be made considering a circular aperture of radius a. The power loss per pass of the beam inside the cavity is,
With a ratio \(x = a/\sigma = 4.8\) the resulting extra losses are \(p = 10\;\hbox {ppm}\). Given the relatively large value of x, these extra power losses are therefore obtained without significantly altering the Gaussian beam profile. It is also true, though, that very small position variations of the gate valve with respect to the beam generate significant variations of the finesse. We have observed that, with the valve inserted, the stability of the finesse is of the order of 1%. In our measurements this is the dominant uncertainty factor.
Note also that even if the noise is generated within the whole thickness of the reflecting layers, the physical structures of the multilayer dielectric mirrors corresponding to the highest and the lowest finesses used would differ by no more than a pair of dielectric layers [35]; this justifies the use of an extra loss located outside the mirrors as a means to study the intrinsic birefringence noise of the mirrors as a function of the finesse.
Since a reduction by a factor 3 of the finesse results in a factor 9 reduction at the output of the cavity and given that the output power is \(I_\parallel = T I_\mathrm{cav}\) this also means a factor 9 reduction of the power on the mirrors. We therefore chose to change the input power to the cavity so that at each finesse the output power was the same during all measurements: we chose \(I_0 = 0.7\;\hbox {mW}\).
The theoretical sensitivity for \(I_0 = 0.7\;\hbox {mW}\) was already shown in Fig. 2. Superimposed is also the measured sensitivity between 10 and 20 Hz with a modulation \(\eta _0 = 10^{2}\). This measured sensitivity does not change by increasing or decreasing the output power by a factor ten.
During our measurements the magnets were kept in rotation at two different frequencies, \(\nu _\alpha = 4\;\hbox {Hz}\) and \(\nu _\beta =5\;\hbox {Hz}\) generating CottonMouton peaks at twice these frequencies due to the presence of Argon gas at \(850\;\upmu \hbox {bar}\). The frequency of the Faraday rotation signal induced on the input mirror using an external solenoid was chosen to be \(\nu _F = 19\;\hbox {Hz}\).
Six different values of the finesse were chosen for the measurements, each separated by approximately 20%. For each finesse value we first measured in the ellipticity configuration and then in the rotation configuration by inserting the quarterwave plate. The finesse was determined by measuring the intensity decay exiting the cavity after unlocking the laser at the end of each series of measurements.
The intensity decay graphs for the six positions of the gate valve, resulting in the six finesse values used during the measurements, are shown in Fig. 5. These correspond respectively to,
with a 1% uncertainty.
The main goal of the present work is to show whether the noise present in the two configurations of the polarimeter is dominated by an ellipticity noise generated by a fluctuating birefringence inside the cavity, i.e. whether it is multiplied by the gain factor N of the Fabry–Perot. To accomplish this, for each finesse value we first determined the value of \(\alpha _\mathrm{EQ}\) from Eqs. (40) and (41) for both the Faraday and the CottonMouton measurements. The dependence of both the CottonMouton and Faraday signals are expected to follow the relations given in Eqs. (38) and (39). We have then studied the signaltonoise ratios of the various signals both in the rotation and in the ellipticity configurations to study their behaviour as a function of the finesse.
5 Results and discussion
Typical raw ellipticity (top) and rotation (bottom) spectra measured in a time \(t = 512\;\hbox {s}\) at the highest finesse of \({{\mathscr {F}}}_1 = 6.88\times 10^5\) are shown in Fig. 6. Data sampling was performed at 256 Hz resulting in spectra with a frequency resolution of \(\Delta \nu _\mathrm{res} = 1.5\times 10^{5}\;\hbox {Hz}\). In both the ellipticity and rotation channels the Argon CottonMouton signals at \(2\nu _{\alpha } = 8\;\hbox {Hz}\) and \(2\nu _{\beta } = 10\;\hbox {Hz}\) are clearly visible, with equal amplitudes due to identical magnets, along with the Faraday rotation signal at \(\nu _F = 19\;\hbox {Hz}\) induced in the input mirror of the cavity. The small sidebands around \(2\nu _{\alpha ,\beta }\) are due to small oscillations of the rotation frequency of the magnets generated by the driving system of the magnets. The amplitude error on the main peaks due to these sidebands is less than . In both panels of the Fig. 6 one can also distinguish two peaks at \(\nu _{\alpha } = 4\;\hbox {Hz}\) and \(\nu _{\beta } = 5\;\hbox {Hz}\) due to a small component of the magnetic field along the beam direction generated by a small non orthogonality of the magnetic field with respect to the beam propagation direction. This small component of the magnetic field generates a Faraday rotation in the gas inside the cavity. Indeed these peaks are higher in the rotation spectrum. A small Faraday effect is also generated in the mirrors due to the stray field but this rotation is negligible with respect to the rotation generated in the gas.
Notice how in the rotation spectrum the integrated noise and the two CottonMouton signals are smaller with respect to the ellipticity spectra whereas the Faraday signals are larger.
In Fig. 6 we have also reported (in black) the quadrature demodulation spectra integrated over the same time t. This integrated noise corresponds to a peak spectral density of \(S_{\mathrm{quad}} = 1.6\times 10^{8}/\sqrt{\mathrm{Hz}}\), in agreement with the sensitivity, shown in Fig. 2, due to noise sources independent of ellipticity such as shotnoise, Johnson noise, diode dark current noise and laser relative intensity noise considering \(I_0 = 0.7\;\hbox {mW}\) and \(\eta _0 = 10^{2}\). This noise is the same in both the ellipticity and the rotation spectra. The inphase noise is clearly of a different origin. Small peaks, less than 1% of the inphase peaks, are present in the quadrature channel which are consistent with a phase error in the demodulation of about \(1^\circ \).
5.1 Determination of \(\alpha _{EQ}\)
For each value of the finesse we have first determined the value of \(\alpha _{EQ}\), necessary to evaluate the true ellipticities and rotations due to the CottonMouton and Faraday effects, according to Eqs. (40) and (41). In Fig. 7 we have plotted the values of the ratios,
at 8 and 10 Hz as a function of the number of passes \(N = \frac{2{{\mathscr {F}}}}{\pi }\) and
Since \(\alpha _\mathrm{EQ}\) is a property of the mirror coatings it is independent of N, as expected. The average value for \(\alpha _\mathrm{EQ}\) at 8 and 10 Hz is
where \(\sigma _{\alpha _\mathrm{EQ}}\) is the standard deviation obtained from the plotted data. This value is consistent with the statistical error of each single measurement.
The same can be done by considering the measured rotation and ellipticity peaks at \(\nu = 19\;\hbox {Hz}\):
Here the standard deviation \(\sigma _{\alpha _\mathrm{EQ}}_{\nu = 19\;{\mathrm{Hz}}}\) obtained from the plotted data is significantly larger than the statistical error of each data point due to the significantly smaller value of \(\alpha _\mathrm{EQ}\) at \(N = 161000\) with respect to the other data points. Furthermore the average value of \(\alpha _\mathrm{EQ}\) for the data at the higher finesses is significantly larger than the average value obtained using the CottonMouton effect. There is clearly a small systematic effect when using the Faraday effect by applying a magnetic field on the mirrors which at the moment is not well understood but may be due to the substrate of the mirror. The weighted average of the two values considering the standard deviations reported in (50) and (51), which we will use in the following, is \(\alpha _\mathrm{EQ}=2.305\times 10^{6}\;\)rad with standard deviation \(\sigma _{\alpha _\mathrm{EQ}} = 2\times 10^{8}\;\)rad.
5.2 CottonMouton and Faraday signals in the ellipticity channel versus N
In Fig. 8 we have plotted the peak amplitudes \(\Psi ^\mathrm{meas}\) of the ellipticity signals at 8 and 10 Hz as a function of N. In the same figure we have also plotted the values of \(\Psi _0\) obtained from Eq. (38) taking into account the frequency dependence \(h_{\alpha _\mathrm{EQ}}(\nu )\) of the signals and the amplitude reduction due to \(k(\alpha _\mathrm{EQ})\). As expected these lie on a line passing through the origin indicating that indeed the signal is \(\Psi _0 = N\psi _0\). The slope of the lines give the value of the ellipticity per pass \(\psi _0 = (7.20\pm 0.04)\times 10^{11}\) acquired by the light resulting in a CottonMouton constant [36] \(\Delta n_u = {\Delta n}/{B^2} = (5.63\pm 0.14)\times 10^{15}\;\hbox {T}^{2}\, @ 1064\hbox { nm}\) with \(P_\mathrm{Ar} = (850\pm 20)\;\upmu \hbox {bar}\).
In Fig. 9 we have plotted the values of \(\Psi ^\mathrm{meas}\) of the ellipticity at 19 Hz. This signal is due to the Faraday rotation being transformed into ellipticity because of the birefringence of the cavity. In the same figure we have also plotted the values of \(N^2\frac{\alpha _\mathrm{EQ}}{2}\phi _0\), obtained having normalised the values \(\Psi ^\mathrm{meas}\) for the response of the polarimeter, as a function of N according to the expression deduced from Eq. (38) having set \(\Psi _0 = 0\):
As expected from this last equation these values lie on a parabolic curve allowing the determination of the rotation per pass \(\phi _0 = (1.96\pm 0.04)\times 10^{11}\;\)rad/pass. It is estimated that the contribution of the substrate is less than 1%, compatible with the parabola passing through the origin within the errors.
5.3 Ellipticity noise versus N
In Fig. 10 one can see the ellipticity rms spectra at the six different finesse values, where the raw spectra have been rebinned in 0.5 Hz frequency bins.
These spectra have not been normalised for the amplification factor N and frequency response \(k(\alpha _\mathrm{EQ})h_{\alpha _\mathrm{EQ}}(\nu )\) given by Eq. (32). As can be seen not only do the CottonMouton ellipticity signals and the peaks at \(\nu _F = 19\;\hbox {Hz}\) decrease with decreasing N, as already discussed, but so does the noise. By normalising each spectrum with the cavity response given by Eq. (38) and assuming the noise to be dominated by the intracavity ellipticity noise \(s_\psi \) (\(s_\phi =0\) and \(S_e=0\)) in Eq. (42), one finds the plot shown in Fig. 11. In this figure, all the noise components of the spectra lie on a common curve (except for a small broad structure between 5 and 10 Hz at the lower finesse values). The CottonMouton peaks also indicate a common value whereas the signal at \(\nu _F\) does not, as expected.
Instead, by normalising the noise spectra assuming an intracavity rotation noise \(s_\phi \) (\(s_\psi =0\) and \(S_e=0\)) in equation (42), one obtains the plots in Fig. 12. In this case the peaks at \(\nu _F\), which have an origin from a Faraday effect, overlap whereas the noise and the CottonMouton peaks do not. It is also apparent that the noise does not behave as an intracavity rotation noise \(s_\phi \).
In Fig. 13 we report the signaltonoise ratios for both the CottonMouton signals at \(2\nu _\alpha = 8\;\hbox {Hz}\) (purple) and \(2\nu _\beta =10\;\hbox {Hz}\) (green) extracted from Fig. 10. On the same plot we have also reported the ratio of the CottonMouton signal at \(2\nu _\beta =10\;\hbox {Hz}\) with respect to the noise at 20, 30, 40 and 90 Hz to see whether indeed the noise is independent of the finesse also at higher frequencies. The value of the noise at 8 and 10 Hz is determined as the average of the noise on either side of the peaks in a frequency range of 0.5 Hz. For the other frequencies the noise is determined as the average over a 0.5 Hz frequency range.
As can be seen, the ratios at 8 and 10 Hz are indeed independent of the finesse. The apparent increase of the signaltonoise ratio with N at higher noise frequencies is actually only due to the different frequency response of the cavity at the frequency of the signal and at the frequency of the noise.
Following the hypothesis that the noise in the polarimeter is dominated by an ellipticity noise per pass \(s_\psi \) we have fitted the different signaltonoise ratios with the expression,
obtaining the superimposed fits.
Considering the more complicated expression (42) in which one fixes a common ellipticity noise per pass \(s_\psi \), a common rotation noise per pass \(s_\phi \) for each value of N and a flat baseline noise contribution \(S_e\) according to the expression,
does not improve the quality of the fitted data estimated using \(\chi ^2_{\mathrm{ndf}}\). A global fit considering all the data in Fig. 13 gives the following limits: \(s_\phi /s_\psi < 0.4\) and \(S_e< 2\times 10^{8}\;1/\sqrt{\mathrm{Hz}}\).
The noise therefore behaves as an ellipticity noise \(s_{\psi }\) generated within the cavity and multiplied by a factor N, just like the CottonMouton signals: the total noise \(S_\Psi = Ns_\psi \) is proportional to the number of passes N. We therefore conclude that the dominating noise source at frequencies up to \(\nu = 90\;\hbox {Hz}\) is due to a pure ellipticity noise generated in the dielectric coatings of the cavity mirrors.
By rescaling Fig. 11 to obtain an optical path difference sensitivity one finds the graph in Fig. 14.
5.4 Ellipticity noise versus rotation noise
In the previous section we have discussed the ellipticity spectra for the six finesse values. In Fig. 15 we report the respective rotation spectra.
Two facts are apparent: the rotation noise is smaller than the ellipticity noise at all frequencies for corresponding finesse values; the noise spectra in rotation flatten above about 40 Hz at the lower finesse values. This noise floor results to be \(S_r = 3.2\times 10^{8}/\sqrt{\mathrm{Hz}}\) with a dispersion around \(S_r\) of \(\sigma _{S_r} = 0.2\times 10^{8}/\sqrt{\mathrm{Hz}}\). This noise is slightly above the quadrature noise which corresponds to the intrinsic rotation noise of the polarimeter.
To further confirm that the dominant noise source originates from a birefringence fluctuation we have considered the ratios of the noise spectrum in ellipticity with respect to the noise spectrum in rotation for the six different finesse values. These spectra have been fitted with the expressions (42) and (43),
where we have used a frequency dependence of \(s_\psi (\nu ) = \sqrt{(a\nu ^{1})^2+(b\nu ^{0.25})^2}\) as a result of fitting Fig. 11, from 10 to 90 Hz, and we have assumed that the ratio \(s_\phi /s_\psi \) is independent of frequency. The fit of the ratio of the noises using Eq. (55) has been performed from 20 to 90 Hz and the frequencies at which a peak is present have been excluded. With these assumptions we obtain the global fits shown in Fig. 16 in which the free parameters are the ratio \(s_\phi /s_\psi \) and \(S_e\) and the fixed value of \(S_r = 3.2\times 10^{8}/\sqrt{\mathrm{Hz}}\) was used as deduced from Fig. 15 above 40 Hz. The fits indicate a ratio \(s_\phi /s_\psi =(0.21\pm 0.01)\) and \(S_e \le 3 \times 10^{8}/\sqrt{\mathrm{Hz}}\) compatible with the shot noise limit shown in Fig. 2. On the same graphs we have also plotted the two cases for \(s_\phi /s_\psi = 0\) (dashed green) and \(s_\phi /s_\psi = 1\) (dashed blue) keeping the values for \(S_e\) as obtained from the global fit and \(S_r = 3\times 10^{8}\).
These results confirm our interpretation of the noise measurements: the observed noise is dominated by an ellipticity noise generated by a birefringence inside the cavity. Rotation noise plays only a minor role.
5.5 Consequences of results
A first important consequence of the findings presented in this section is that the signaltonoise ratio in a Fabry–Perot based polarimeter with a calculated optical path difference sensitivity equal to or better than the sensitivity shown in Fig. 14 will not improve by increasing the finesse of the cavity. Assuming a predicted shot noise sensitivity given by Eq. (14), the maximum useful finesse up to which one gains in signal to noise ratio is determined by,
where \(S_{\Delta {{\mathscr {D}}}}\) can be read off Fig. 14. For the experimental configuration presented in this paper, where \(S_{\Delta {{\mathscr {D}}}} \approx 6\times 10^{19}\;\hbox {m}/\sqrt{\mathrm{Hz}}\, @ 10~\hbox {Hz}\), one finds \({{\mathscr {F}}}_\mathrm{max} = 1.6\times 10^4\).
The second important fact resulting from these measurements is that the dominant source of noise is indeed due to a birefringence fluctuation in the cavity mirror coatings.
6 Noise origin
Polarimetric measurements using a Fabry–Perot cavity to increase the effective optical path length have reached an intrinsic limit due to the coatings of the cavity mirrors. Our measurements show that this noise is due to birefringence fluctuations in the coatings which we believe are of thermal origin.
As mentioned in Sect. 3.1 cavity mirrors always present an intrinsic birefringence. There could therefore be two principal causes for these birefringence fluctuations: a fluctuation of the intrinsic birefringence; a fluctuation of the birefringence independent of the intrinsic value. As was shown in Fig. 3, there is a very strong correlation in the optical path difference noise between completely different experiments with very different values of \({{\mathscr {F}}}\). This seems to indicate that the source of the intrinsic birefringence noise is independent of the intrinsic mirror birefringence inducing the retardations \(\alpha _{1,2}\). This hypothesis seems confirmed by the estimation of the thermorefractive noise in Sect. 6.1.
We also note that any polarization effect intrinsic to the cavity, be it static or dynamical, is generated in the first reflecting layers encountered by the light from inside the cavity. With a transmittance of the mirrors \(T=2.4\times 10^{6}\), as is the case of the PVLAS experiment [18], the electric field inside the reflective coatings has an exponential decay with,
where \(N_{\mathrm{LP}}\approx 20\) is the total number of high refractive index  low refractive index pairs composing the reflective coating and \(\lambda _{\mathrm{LP}}\) represents the number of coating pairs after which the electric field (as opposed to the intensity) has decreased to 1 / e of the incident field. One finds \(\lambda _{\mathrm{LP}} = 3.0\). Most of the ellipticity (signal and noise) is therefore accumulated in the first \(\lambda _{\mathrm{LP}}\) pairs of dielectric coatings for each reflection. This corresponds to a geometrical thickness \(d_{\mathrm{LP}} \simeq 1\;\upmu \hbox {m}\). These considerations further justify the use of an extra loss located outside the mirrors as a means to study the intrinsic birefringence noise of the mirrors.
There are three possible causes for birefringence thermal noise in a medium: direct temperature dependence of the index of refraction (thermorefractive effect); indirect temperature dependence of the index of refraction due to a linear expansion coefficient coupled to a stress optic coefficient; volume fluctuations due to Brownian motion. Here we will only discuss the first two effects.
A lot of literature (see for example [38,39,40,41] exists which deals with the phase noise induced in interferometric gravitational wave antennas by thermal fluctuations of mirrors (coating, substrate). Indeed the main concern in their case are length variations in the incident direction. Very little (if none) exists for what concerns the effect of fluctuations in the plane of the mirror surface causing birefringence. In the following we will try to estimate this effect.
6.1 Thermorefractive effect
Let us consider the indeces of refraction of the mirror coatings along the natural axes of a mirror as \(n_\parallel \) and \(n_\perp \) resulting in a birefringence \(\Delta n = n_\parallel  n_\perp \). The optical path through the coating of a mirror per reflection for light polarised parallel and perpendicularly to the slow axis (here considered to be the \(\parallel \) direction) will be,
where the factor 2 is intended to take into account the round trip inside the coating. The intrinsic optical path difference of a mirror coating per reflection will therefore be,
By considering the thermorefractive effect due to a temperature dependence of \(n = n({\mathrm{T}})\), the optical path difference temperature dependence will be,
Hence \({d\Delta {{\mathscr {D}}}({\mathrm{T}})}/{d{\mathrm{T}}}\ne 0\) only if \(d n_\parallel /d{\mathrm{T}}\ne d n_\perp /d{\mathrm{T}}\). In this case the optical path difference spectral density \(S_{\Delta {{\mathscr {D}}}}(\nu )\) due to the thermorefractive effect will be,
where \(S_{\mathrm{T}}(\nu )\) is the temperature noise spectral density.
An estimate of \(\Delta {{\mathscr {D}}}\) due to the intrinsic mirror birefringence can be obtained from the value of \(\alpha _\mathrm{EQ} = 2.3\times 10^{6}\;\)rad, resulting in,
A rough value for \(\frac{1}{\Delta n}\frac{d\Delta n}{d{\mathrm{T}}} \sim 10^{5}\;\hbox {K}^{1}\) for fused silica can be deduced from the expressions reported in [37] considering \(n_\parallel \simeq n_\perp \). Therefore,
Following Ref. [38] the temperature fluctuations averaged over a volume \(\pi r_0^2 d_{\mathrm{LP}}/2\) occupied by the Gaussian power profile of waist \(r_0\) being reflected using a weight function \(q(\mathbf {r})\),
results in a temperature noise spectral density \(S_{\mathrm{T}}(\nu )\) [38],
where \(\kappa _B\) is the Boltzmann constant, \(\rho \) is the density, \(C_{\mathrm{T}}\) is the specific heat capacity, \(\lambda _{\mathrm{T}}\) is the thermal conductivity and,
is the characteristic diffuse heat transfer length (\(d_{\mathrm{LP}}\ll r_{\mathrm{T}}\ll r_0\)). In Eq. (66) the ratio \({r_{\mathrm{T}}^2}/{r_0^2}\) represents the inverse of the number of unit spheres of radius \(r_{\mathrm{T}}\) covering the beam of radius \(r_0\) thereby averaging out the temperature fluctuations. Considering fused silica (FS), for which \(\rho = 2200\;\hbox {kg}/\hbox {m}^3\), \(C_{\mathrm{T}} = 670\;\hbox {J}/(\hbox {kg}\hbox { K})\) and \(\lambda _{\mathrm{T}} = 1.4\;\hbox {W}/(\hbox {m}\hbox { K})\) this results in,
having set the beam diameter \(r_0 \approx 0.5\;\hbox {mm}\). Considering tantala, \(\hbox {Ta}_2\hbox {O}_5\), (TA) instead (we are assuming this is the material used for the highindex layer in the mirror coating), for which \(\rho = 8200\;\hbox {kg}/\hbox {m}^3\), \(C_{\mathrm{T}} = 300\;\hbox {J}/(\hbox {kg}\hbox { K})\) and \(\lambda _{\mathrm{T}} = \left[ 0.026 \div 15\right] \;\hbox {W}/(\hbox {m }\hbox {K})\) (for a film) [42], one finds,
With the above values the thermorefractive noise spectral density in optical path difference \(S^{\mathrm{TR}}_{\Delta {{\mathscr {D}}}}({\nu })\) can be estimated to be of the order,
well below the measured values reported in Figs. 3 and 14. We therefore believe that the source of noise in the PVLAS polarimeter is not due to a thermorefractive effect.
6.2 Stress induced birefringence
Local length fluctuations will generate stress fluctuations leading to birefringence through the stress optic coefficient. Indeed given a stress optical coefficient \(C_\mathrm{SO}\) and a Young’s modulus Y the induced variation in the index of refraction due to stress is given by,
where \({\delta l_{\parallel ,\perp }}/{l}\) is a relative length variation along two perpendicular directions \(\parallel \) and \(\perp \) over a length l. Again following the considerations in Ref. [38] an order of magnitude estimate of the induced birefringence noise spectral density \(S_{\Delta n}(\nu )\) over the spot size of the reflected beam due to temperature fluctuations related to stress can be made.
The average relative length fluctuations of \(\frac{{\delta r_{\mathrm{T}}}}{r_{\mathrm{T}}}\) over the spot surface, indicated by the brackets \(\langle \rangle _{\parallel ,\perp }\) where \(\parallel \) and \(\perp \) indicate two perpendicular directions, will be,
where \(\alpha _{\mathrm{T}}\) is the linear expansion coefficient. This will generate a birefringence noise spectral density,
A very rough estimate of the optical path difference spectral density noise \(S_{\Delta {{\mathscr {D}}}}=2\int _{d_{\mathrm{LP}}}{S_{\Delta n} \;dl}\) accumulated in a reflection results in,
For fused silica for which \(\alpha _{\mathrm{T}} = 5\times 10^{7}\;\hbox {K}^{1}\), \(Y = 70\;\hbox {GPa}\) and \(C_\mathrm{SO} = 3\times 10^{12}\;\hbox {Pa}^{1}\) one finds,
whereas for tantala,
where the values for tantala are \(Y= 150\;\hbox {GPa}\) and \(\alpha _{\mathrm{T}} = 8\times 10^{6}\;\hbox {K}^{1}\) and we have use \(C_{\mathrm{SO}} = 3\times 10^{12}\;\hbox {Pa}^{1}\) for fused silica not having found a value for tantala in the literature. Generally it is found in literature that \(C_{\mathrm{SO}}\) is \(\sim (10^{12}\div 10^{11})\;\hbox {Pa}^{1}\) with a particularly large value for \(\hbox {Nb}_2\hbox {O}_5\) with \(C_{\mathrm{SO}} = 95\times 10^{12}\;\hbox {Pa}^{1}\) [43]. These values justify our approximation.
The value for \(S^\mathrm{TA}_{\Delta {{\mathscr {D}}}}\) in the case of tantala is quite close to the measured values especially at higher frequencies. The exact expression for \(S_{\Delta {{\mathscr {D}}}}\) is beyond the scope of this paper but indeed a stress mechanism could generate a birefringence noise of the same order of magnitude as the one measured.
This stress will be present both in the substrate and in the mirror coatings. As discussed above, given that the electric field within the coating is strongest in the first \(\lambda _{\mathrm{LP}}\) layers encountered by the light in the cavity, the induced \(S_{\Delta {{\mathscr {D}}}}\) will be dominated by these first layers and in particular by the tantala layers.
7 Conclusions
Birefringence noise of the Fabry–Perot cavity limits the sensitivity of precision measurements in polarimeters like those designed to detect the birefringence of vacuum due to magnetic fields. We have measured the noise present in the PVLAS polarimeter in both ellipticity and rotation modes along with CottonMouton and Faraday signals as a function of the finesse of the Fabry–Perot cavity. We have shown that the signaltonoise ratio of the CottonMouton ellipticity signals is independent of the finesse of the cavity as is the ellipticity noise. We have shown that for the rotation noise this is not the case. We have also studied the ellipticity noise to rotation noise ratios which confirm that the dominant noise source in the polarimeter is a fluctuating birefringence inside the Fabry–Perot cavity.
We note that the noise is generated in the first few layers of the mirror coatings and we infer that, with an order of magnitude estimation, the origin could be due to thermally induced stress fluctuations namely due to a thermoelastic effect.
It is therefore apparent that the continuous search to improve the sensitivity in optical path difference \(S_{\Delta {{\mathscr {D}}}}\) by increasing the finesse of the Fabry–Perot cavity has reached a limit.
The quest to measure vacuum magnetic birefringence using optical techniques must therefore,

reduce the optical path difference noise by cooling the mirrors and/or by finding new materials for the coatings with a lower stress optic coefficient and/or lower linear expansion coefficient;

decrease the number of reflections (finesse) and increase the cavity and magnetic field lengths to preserve the optical path length.

increase the vacuum magnetic birefringence signal using high, long, static superconducting fields and inducing the necessary signal modulating for improved sensitivity by varying the polarisation [44, 45].
Finally let us note that if the intrinsic total retardation \(\frac{N\alpha _\mathrm{EQ}}{2}\) can be kept low in such a way that the mixing between ellipticity and rotation is also small, then increasing the finesse during rotation measurements is advantageous. Indeed given that the dominant source of ellipticity noise is due to birefringence fluctuations, rotation sensitivity may not be limited by an intrinsic thermal source. This could lead to improved laboratory experimental limits on the existence of axion like particles [19, 23, 24, 46].
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Zavattini, G., Della Valle, F., Ejlli, A. et al. Intrinsic mirror noise in Fabry–Perot based polarimeters: the case for the measurement of vacuum magnetic birefringence. Eur. Phys. J. C 78, 585 (2018). https://doi.org/10.1140/epjc/s100520186063y
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DOI: https://doi.org/10.1140/epjc/s100520186063y