A new infrared FabryPérotbased radialvelocityreference module for the SPIRou radialvelocity spectrograph
Geneva Observatory, University of Geneva, Maillettes 51, 1290 Sauverny, Switzerland
email: maria.cersullo@unige.ch
Received: 28 October 2016
Accepted: 30 January 2017
Context. The field of exoplanet research is moving towards the detection and characterization of habitable planets. These exoEarths can be easily found around lowmass stars by using either photometric transit or radialvelocity (RV) techniques. In the latter case the gain is twofold because the signal induced by the planet of a given mass is higher due to the more favourable planetstar mass ratio and because the habitable zone lies closer to the star. However, latetype stars emit mainly in the infrared (IR) wavelength range, which calls for IR instruments.
Aims. SPIRou is a stable RV IR spectrograph addressing these ambitious scientific objectives. As with any other spectrograph, calibration and drift monitoring is fundamental to achieve high precision. However, the IR domain suffers from a lack of suitable reference spectral sources. Our goal was to build, test and finally operate a FabryPérotbased RVreference module able to provide the needed spectral information over the full wavelength range of SPIRou.
Methods. We adapted the existing HARPS FabryPérot calibrator for operation in the IR domain. After manufacturing and assembly, we characterized the FP RVmodule in the laboratory before delivering it to the SPIRou integration site. In particular, we measured finesse, transmittance, and spectral flux of the system.
Results. The measured finesse value of F = 12.8 corresponds perfectly to the theoretical value. The total transmittance at peak is of the order of 0.5%, mainly limited by fibreconnectors and interfaces. Nevertheless, the provided flux is in line with the the requirements set by the SPIRou instrument. Although we could test the stability of the system, we estimated it by comparing the SPIRou FabryPérot with the already operating HARPS system and demonstrated a stability of better than 1 m s^{1} during a night.
Conclusions. Once installed on SPIRou, we will test the full spectral characteristics and stability of the RVreference module. The goal will be to prove that the line position and shape stability of all lines is better than 0.3 m s^{1} between two calibration sequences (typically 24 h), such that the RVreference module can be used to monitor instrumental drifts. In principle, the system is also intrinsically stable over longer time scales such that it can also be used for calibration purposes.
Key words: instrumentation: spectrographs / instrumentation: interferometers / techniques: radial velocities / telescopes
© ESO, 2017
1. Introduction
SPIRou is a nearinfrared (NIR) spectropolarimeter and velocimeter that is soon to be offered as a newgeneration instrument on the CanadaFranceHawaii Telescope (CFHT; Delfosse et al. 2013). Its main goals are a) the search and characterization of habitable exoplanets orbiting lowmass and verylow mass stars by using highprecision radialvelocity (RV) measurements and b) the study of the impact of magnetic fields in star and planet formation by means of spectropolarimetry. SPIRou is presently being integrated in Toulouse and will be transferred to the CFHT in 2017. Operations are planned to start end of 2017.
The radialvelocity method is employed to determine the Doppler shifts of absorption lines in the host star’s spectrum. M dwarfs present the opportunity to discover potential habitable planets due the larger radialvelocity signature induced by the planet on the lowermass star (Udry et al. 2007). Also, the habitable zone (HZ) of an M star lies much closer in than that of a solartype star, which again leads to a higher radialvelocity signal compared to a solartype star. However, because Mdwarfs emit most of their flux in the infrared wavelength domain (Reiners et al. 2010), a radialvelocity instrument has to operate at infrared wavelengths, to make best use of the stellar light.
The wavelength range, resolution and the design of SPIRou, as well as its stability, have been optimized to search for habitable planets around M stars. The expected RV amplitude induced by a two Earthmass planet in the HZ of an M5 dwarf, for instance, is of the order of 1.7 m s^{1} (Barnes et al. 2011). To achieve sufficiently significant detection, a measurement precision, and thus instrumental precision, of the order or better than 1 m s^{1} is required. It is well known that such a precision can only be achieved if both the spectral calibration and the instrumental drift are controlled to the same level. Both wavelength calibration and drift measurements, make use of spectral references that fix the necessary wavelength scale. The RVobservable corresponds to the measurement of the central wavelength of a spectral line that has to be referred to a known laboratory standard. Unlike the visible case, for which multiple wavelength calibration sources exist, such as spectral lamps, iodine cells, and lately also laser frequency combs (LFC; Ycas et al. 2012; Schwab et al. 2015) and FabryPérots étalons (Reiners et al. 2014), in the infrared wavelength domain we are lacking suitable references sources.
The precision limitations in the calibration of radial velocity measurements play a keyrole, especially when targeting the ambitious cases listed above. For these kind of investigations, an ultrastable, broadband, bright, flexible and reliable wavelength calibrator is required.
To ensure optimal accuracy and precision, the spectrum of the ideal calibrator must have the following main characteristics:

Many unresolved narrow lines.

Coverage of the full spectral range.

Known (or calibrated) line position.

Line stability.

No blending.

Homogeneous peak flux.
In recent years, we developed a FabryPérot calibration system with the aforementioned characteristics (Wildi et al. 2010) for the visible wavelength range. The first system, currently in use on the HARPS spectrograph, has performed well and has completely replaced the ThAr spectral lamp for instrumental drift measurement purposes. However, its lensbased optical design was not compatible with an infrared version. Therefore, we redesigned the system using an allreflective solution. Two systems of the new design have been manufactured and are currently in operation on the TNG/HARPSN and EULER/CORALIE spectrographs. Both systems have demonstrated stability of better than 1 m s^{1} during an observing night that allowed us to use them systematically for the simultaneous reference measurement (Pepe et al. 2004). Based on this second design, we have manufactured and tested a similar system for SPIRou. The only element that needed to be adapted was the étalon itself in terms of material and coatings.
In the next section we will describe the basic working principles of the FabryPérot based RVreference module for SPIRou. In Sect. 3 we will describe the optomechanical design and the rationale that led us to the final parameter choice. In Sect. 4, we present the laboratory measurement setup and the results obtained. In the final sections, we will also describe some of the particular aspects of RV precision and we will provide an outlook on possible future developments.
2. Theory of the planoplano FabryPérot étalons
A planoplano FabryPérot étalon (FP) consists of two flat parallel mirrors separated by an optical gap d. The inner surface of each mirror is coated with a partially reflecting coating and the outer surface has an antireflection coating. The medium between the mirrors is transparent and has a refractive index of n.
The FP is illuminated with a parallel light beam of divergence Φ. The light is partially reflected and transmitted by both mirrors producing interference in both reflection and transmission as shown in Fig. 1 (excerpt from Field guide to spectroscopy of Ball 2006). The transmission function of the étalon, taking into account the losses due to unavoidable absorption and scattering, is given by: (1)where R is the reflectivity the mirror, A the absorption and scattering losses per reflection, and δ = 4πndcosθ/λ the phase difference between successive beams. Defining the reflective finesse coefficient as and assuming A ≪ 1−R, the Eq. (1)is simplified to: (2)This function reaches a transmission maximum every time the phase is an integral multiple of π, namely, (3)The distance between two successive maxima, also called the free spectral range (FSR), is defined by: (4)Figure 2 shows the theoretical transmission function of a FabryPérot étalon with finesse F_{R} = 13 at 1540 nm wavelength and FSR of ~0.09 nm. In this example we chose normal incidence (θ = 0) and vacuum operation (n = 1). Transmission maxima are then reached for each wavelength λ_{m} = 2d/m and the free spectral range simplifies to FSR = λ^{2}/ 2d.
Fig. 1 Concept of the planoplano FP and sketch of the interfering light beams. 

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The finesse F of a FabryPérot étalon is defined as the ratio of the FSR to the fullwidth at half maximum (FWHM) of the transmission peak . The functional analysis leads to , leading to F = F_{R}.
We previously assumed a perfect étalon. In reality, any étalon will show errors such as surface errors and nonparallelism of the mirror. In order to take into account all these contributions, we can replace the reflective finesse F_{R} by an effective finesse F_{e} of the étalon, which can be expressed as: (5)where F_{R} is the reflectivity finesse, F_{D} is the defect finesse, and F_{P} is the parallelism finesse. An approximation of the divergence finesse is represented by F_{Φ}. This is produced by the finite dimension of the illuminating entrance slit, which in turn produces a beam divergence of the quasiparallel beam through the étalon. In the simulations we will present in the following sections, we replaced the divergence finesse by an integration over the field positions of the slit, to compute a realistic transmission function of the étalon in the case of a large entrance slit.
Fig. 2 Simulated curve for our FabryPérot passband. 

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Using the effective finesse and the definition of the resolving power RP, we computed: (6)
3. Infrared FabryPérot radialvelocityreference module for SPIRou
The FabryPérot RVreference module for SPIRou has the purpose of providing a large number of ultrastable lines in the wavelength range of the spectrograph, that allow to measure the instrumental drift during the night (or, in other terms, on the time scale between two calibrations). From the general characteristics of an ideal calibration source described in the introduction, we derived the requirements for the SPIRou RVreference module as follows:

The calibration source must cover the full wavelength range ofSPIRou, i.e. from 980 nm to2350 nm.

The lines must not be resolved by the SPIRou spectrograph, since otherwise information is lost, respectively we do not take full advantage of the spectral resolution of the instrument.

The line separation must be minimum two and maximum four the full width at half maximum (FWHMs) of the spectrograph instrumentalprofile (IP), in order to maximize the information content and avoid blends.

The line position and shape stability of all lines must be better than 0.3 m s^{1} during a night and on the time scale in between two calibrations (typically 24 h).

The lines must be equidistant and the position of all lines defined by a limited number of system parameters.

The relative intensity of any neighboring lines must be stable at 10% over any time scale.

The dynamic range of line intensities must be smaller than a factor 2 over one echelle order and a within a factor five over the full spectrum.
3.1. Spectral characteristics
Assuming the aforementioned hypothesis, we were able to design the FabryPérot RVreference module’s spectral characteristics. First, we took into account the resolution of the spectrograph R_{S}. To optimize the spectral content, we need to make the line spacing as small as possible but also ensure that on the blue side, where it is minimal, it remains larger than 3·FWHM. This led us to the first condition: (7)In the case of vacuum operation and perpendicular incidence, Eq. (3)simplifies to (8)Combining this equation with the inequality in Eq. (7), we obtained the condition for the étalon gap: (9)If we set the gap to exactly match the minimum FSR, we obtained the value: (10)On the other hand, the lines of the étalon, at constant finesse, are larger on the red side of the spectrum. Therefore, we had to ensure that they remain narrower than the IP in this area of the spectrum. Our choice was to underresolve the FP lines by a factor of two to three and not less, such that unnecessary flux loss is avoided. This choice drove the second condition: (11)Using the definition of the finesse F = FSR/FWHM and combining it with Eq. (11), we obtained for the finesse: (12)Choosing the lowest possible finesse and by substituting the gap d, we obtained for the finesse: (13)To summarize, the spectrograph’s spectral range and resolution, together with the general requirements for the RVmodule described in the previous section, defined the FabryPérot parameters summarized in Table 1.
SPIRou’s main parameters and derived étalon parameters.
Finesse budget and derived requirements.
To achieve a reflectivitylimited effective finesse of about F = 11, we distributed the various finesse components of Eq. (5)as shown in Table 2. As mentioned above, our starting choice was to determine the effective finesse by allocating a value of F_{R} = 13 to the reflectivity finesse. The remainder of the budget was almost completely used up by the divergence finesse, to maximize the fibre diameter and minimize the physical size of the étalon. The remaining finesse values were set much higher to keep F_{e} in budget.
Once the finesse values have been frozen, they define minimum requirements to the optomechanics of the étalon. The finite divergence forces a tradeoff between fibre size, the focal length of the collimator, and clear aperture of the étalon. In principle, at fixed divergence value, the physical dimensions of the assembly are minimized when the smallest fibre is selected. However, this implies a loss of flux inversely proportional to the fibre size if an incoherent (extended) light source is used. To maximize the flux while still using an incoherent source, we decided to go for the source with the highest possible surface brightness. The choice fell on the LaserDriven Light Source (LDLS) EQ99 FC by Energetiq that is composed of a hightemperature plasma bulb T = 10 000 K (Fig. 3, excerpt from LDLS EQ99 handbook) heated by a highpower diode laser. The light output perfectly matches that of an ordinary stepindex fibre of 200 μm that can directly be used to feed our FP assembly. The numerical aperture NA = 0.20 and the practical wish to keep the system compact, led us to fix the focal length of the collimator to 100 mm and the clear aperture of the étalon to 40 mm. The parallelism defect Δ<4.5 nm translated into 10^{6} rad or 0.2 arcsec. Finally, the value for the surface defects of δ = 6.7 nm required the mirrors to be manufactured with at least λ/ 50 in wavefront error.
Fig. 3 Spectral power produced by the LDLS. The original plot, which is an excerpt from LDLS EQ99 handbook, was manually digitized. 

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3.2. Sensitivity of finesse and radialvelocity stability to alignment and fibre diameter
Up to now we have considered the transmission function of the étalon to be given by Eq. (2). Defects, nonparallelism and finite divergence were taken into account by computing an effective finesse that was corrected for the various contributions. Although this approach is satisfactory for the defects and nonparallelism of the mirrors, it is incomplete for the finite divergence. The finite divergence (or fibre diameter) not only introduces a loss of finesse but also a shift in wavelength of the transmitted peaks. Furthermore, a nonuniform light distribution across the fibre exit produces a change in the shape of the transmitted peak. The resulting transmission function can be simply understood as the sum of the individual transmission functions from every field point (or, in other words, over each ray arising from the different points across the fibre tip) that will cross the étalon with slightly different incidence angles θ.
We simulated the transmission function for different fibre diameters and as a function of the decentring of the fibre from the optical axis, to understand how sensitive the finesse and the peak wavelength are as a function of these parameters. For the analysis, we needed to consider that the fibre is spatially extended and the deviation of each ray from the parallel beam is: (14)where x is the distance from the fibre centre and f = 100 mm is the focal length of the collimator (parabolic mirror). The angle θ by which the beam crosses the étalon depends on the position of the fibre of entrance.
To obtain the total transmittance spectrum, we need to compute the integral over the surface of the fibre. For the simulations we assume circular fibres and uniform illumination, and we perform the integral in polar coordinates. The total transmittance can then be written as: (15)where R is the radius of the fibre and δ = 4πndcosθ/λ, as defined earlier. The integral is divided by the surface A of the fibre tip to renormalize the peak transmittance.
In case of a decentring Δ of the fibre with respect to the optical axis of the system, the angle of incidence θ becomes: (16)where, without loss of generality, we have assumed the fibre to be decentred along the xaxis only.
Fig. 4 Simulated transmittance of a FabryPérot for fibre diameters of 200, 500, and 900 μm, assuming the fibre is centred on the optical axis and a focal length of the collimator f = 100 mm. 

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It is easily understood that, if the fibre has infinitely small diameter, all the the rays will cross the FabryPérot with θ = 0, such that we end up with the known Airy function. For the general case of a finite fibre diameter, we performed a numerical integral to obtain the transmission as a function of the diameter of the fibre D and Δ.
Figure 4 shows the transmittance as a function of fibre size for a system with focal length f = 100 mm. As expected, for small fibres the peak transmittance is close to 1 and the effective finesse is equal to the reflective finesse. For larger fibres, the transmission at the peak decreases and the width increases, which is equivalent to a reduction of the effective finesse. Simultaneously, the peak wavelength shifts towards a shorter wavelength, which reflects the fact that the number of rays having a incidence angle θ > 0 has increased. Interestingly, the peaks remain symmetric, even for very large fibres, which is due to the fact that we have assumed uniform illumination and a circular fibre. This assumption is justified by the fact that the primary source we are using has a larger étendue than the fibre. The fibre is overfilled by the source and uniformly illuminated. In the real system we are using an octagonal fibre that has even better scrambling properties and produces increased illumination uniformity (Chazelas et al. 2010).
Figure 5 shows the results of the simulation as a function of the fibre decentring, in which we fixed the fibre diameter to the chosen value of D = 200 μm. In this case we also observe a reduction of finesse and a blueshift of the peaks with increasing decentring. It is interesting to note, however, that when combining a finite fibre size with decentring, the peaks become asymmetric.
Fig. 5 Simulated transmittance of a FabryPérot for fibre decentering value of 20, 250, 500, and 1000 μm assuming a fixed fibre diameter of D = 200μm and a focal length of the collimator f = 100 mm. 

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The results for the finesse are summarized in Fig. 6. The plot shows the evolution of the finesse as a function of fibre diameter (left hand) and of the fibre decentring (right hand). To be more general, we have expressed both, the fibre diameter and decentring, in terms of angular values Δθ = D/f and θ = Δ /f, respectively. In the case of a small fibre diameter or small decentring, the value for the effective finesse approaches the nominal value of F_{R} = 13. It is important to note that the effective finesse remains larger than F_{Eff} = 11 for a fibre diameter up to Δθ = 0.0035 (D = 350 μm), which perfectly justifies our choice for a 200 μm. However, the plot as a function of decentring also tells us that, if we want to ensure the required effective finesse, the fibre must be centered to better that θ = 0.0015 (Δ = 150 μm) for the optical axis of the system.
Fig. 6 Finesse for a centred fibre as a function of fibre diameter (left) and as a function of fibre decentring (right) for a fixed fibre diameter D = 200 μm. The blue line marks the area we are interested in namely a small fibre diameter and an effective finesse close to the nominal value F_{R} = 13. 

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Fig. 7 Change in radial velocity for a centred fibre as a function of fibre diameter (left) and as a function of fibre decentring (right) for a fixed fibre diameter D = 200 μm. The blue line marks the limit area we are interested in. The area is small because small changes introduces shift of several hundreds or more of m s^{1} in both cases. 

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As mentioned before, the peak wavelength shifts towards the blue when increasing the fibre diameter or decentring the fibre. When the FabryPérot is used for absolute wavelength calibration, the position of the peaks must be known. Even more critical is that, when used as a RVreference (to measure the instrumental drift between two calibration sequences), we have to make sure that the transmission peaks remain stable in wavelength. Their dependence on fibre diameter and centring will set the requirements on the focus and centring stability of our optical system. For this reason, we have expressed the wavelength shift in terms of “radialvelocity” in the unit of [m s^{1}]. The conversion from wavelength to speed is obtained by the relation:(17)Figure 7 presents the shift of the transmission peak as a function of similarly to Fig. 6 fibre diameter Δθ = D/f and decentring θ = Δ /f. It can be seen that even a small change introduces shifts of several hundreds or even thousands of m s^{1}. However, there is no reason besides thermomechanical instabilities for the fibre diameter or the decentring to change with time. To better evaluate the calibration sensitivity to these parameters, we chose to presents the derivative of these curves (Fig. 8). Since the curve has a parabolic shape (as can be understood from the fact that cosθ ~ θ^{2} for small angles θ), its derivative is nothing more than a slope. The lefthand plot simply shows us that, the larger the fibre, the more sensitive the system is to a defocus, and, from the righthand plot, the same conclusion can be drawn for the decentring. Given the chosen fibre size (2 mrad), we derive that the radial velocity will change by 300 m s^{1} m rad^{1}. In physical terms for our system, this is 3 m s^{1} micron^{1} (relating to the change in fibre size). In terms of decentring, the sensitivity will approach zero if the fibre is perfectly centred and will increase to 600 m s^{1} mrad^{1} (6 m s^{1} micron^{1}) of additional decentring for a fibre decentred by 2 mrad (200 μm).
Fig. 8 Radial velocity sensitivity to fibresize change for a centred fibre (left) and to decentring for a fixed fibre size of D = 200 μm (right). The blue line marks the limit area we are interested in. For 2 mrad fibre size, the RV will change by 300 m s^{1} (3 m s^{1} micron^{1}) for a centred fibre. In the case of decentring, it changes by 600 m s^{1} (6 m s^{1} micron^{1}). 

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From this analysis we conclude that small fibres and excellent alignment are mandatory not only for optimum finesse and flux, but also to reach the highest spectral stability. Below, we use the derived sensitivities to specify the thermomechanical requirements of the SPIRou RVreference module.
3.3. Optomechanical requirements derived from stability requirements
3.3.1. Alignment precision
The analysis above shows that the RVsensitivity of the étalon to optomechanical mechanical misalignment increases with decentring. A perfectlyaligned system would not be sensitive to motions of the fibre, for example due to thermal or gravity effects, but even for slight misalignment our system could become unstable at radial velocities beyond 30 cm s^{1}. Assuming that we can align the fibre by autocollimation to better than onetwentieth of its diameter, that is to 10 μm and using the results presented in Fig. 8, we obtain a sensitivity of 30 m s^{1} mrad^{1} (0.3 m s^{1} micron^{1}). In other words, the fibre position must be stable to within one micron of the focal plane of the collimator and the angular alignment of the étalon with the collimators must not change by more than 0.01 mrad.
3.3.2. Pressure stability
For an airspaced étalon like SPIRou’s, any pressure change will induce a change in the optical gap and thus in the wavelength of the transmitted peaks. For this reason we made the choice to operate the RVreference module in a vacuum (see Fig. 9). To establish whether the system must be pumped continuously or not, we have to compute the drift of the system arising from pressure changes that have occurred since the last wavelength calibration of the spectrograph, which taking place at the start of the night. In other words, pressure changes in the FabryPérot system must not induced lineposition changes larger than the required RVprecision. Given the requirement for the RVprecision of 30 cm s^{1} during an observing night (typically 12 h) and using Eqs. (3)and (17), we computed that the refractive index Δn/n must not change by more than 10^{9} in relative terms. Using the approximation for the air index n_{air}−1 = 0.00027·p/p_{atm}, where p_{atm} is the average ambient pressure at sea level, we computed that the pressure p inside the vacuum tank must not change by more than 3.7 × 10^{3} mbar in 12 h or 7.4 × 10^{3} mbar day^{1}.
3.3.3. Operating pressure
An aspect which is frequently forgotten, is that pressure does not only depend on air leaks but on the volume of the air contained in the vacuum tank. External ambient pressure changes due to meteorological effects affect the volume of our vacuum tank due to the variation in pressure differences between outside and inside. Consequently, the index of the residual air inside the vacuum tank will vary and degrade the calibration system. The sensitivity to atmospheric pressure changes depends on the air pressure (or density) inside the vacuum tank. We must therefore understand at which (maximum) pressure we must operate the RVreference module to avoid effects larger than 30 cm s^{1}.
Bearing in mind Boyle’s law p·V = const., defining V_{0} as the initial volume, and defining p_{0} the initial pressure inside the vacuum tank, the refractive index n of the residual air can be written as: (18)where (n_{Atm}−1) ≈ 2.7 × 10^{4} corresponds to the refractive index of standard air at atmospheric pressure p_{Atm}, and p and V are the actual pressure and volume inside the vacuum tank.
The derivative of the refractive index n with respect to the change of the external pressure p_{out} can then be written as: (19)where is the relative volume change of the vacuum tank as a function of changes in external pressure (at constant internal pressure).
By means of a finite element analysis of the vacuum tank (the following sections detail the design description), we computed β ~ 10^{5} mbar^{1}. This value allows us to determine the maximum operational pressure to avoid change in the radial velocity of the RVreference module larger than the specified 30 cm s^{1}. If we consider that ambient pressure variations hardly exceed 10 mbar night^{1} at 2500 m altitude (e.g. at the La Silla and Paranal Observatories), we derive an upper limit for the operation pressure of p_{0}<30 mbar. In practical terms, and given the maximum allowed pressurerise rate of dp/dt = 7.4 × 10^{3} mbar day^{1} determined in the previous section, it is sufficient to evacuate the RVreference module once every 10 yrs in the worst case.
3.3.4. Temperature stability
We considered two effects induced by temperature variations. The first is the thermal stability of the optical gap that is essentially given by CTE of the spacers. The spacer material is from Corning ULE and thus the CTE is guaranteed to be lower than 2×10^{8} Kelvin^{1}. This translates into a radialvelocity sensitivity of about 6.7 m s^{1} K^{1}. Again applying the radialvelocity stability requirement, we derive a temperature stability requirement for the RVreference module of better than 0.05 K.
The second temperature effect may produce focallength changes of the collimator that would result in a “defocus” of the entrance fibre and an apparent increase of fibre diameter D. As we will describe in Sect. 3.4, the FabryPérot assembly of our RVreference module is made of aluminium (also Fig. 9). Considering the focal length of f = 100 mm and the coefficient of linear thermal expansion for aluminium as CTE_{Al} = 2.3 × 10^{5} K^{1}, we computed an absolute focal length change of df/dT = 2.3μm K^{1}. Because the Fnumber of the fibre exit (or collimator) is F/2.5, we obtained an increase of apparent diameter dD/dT ~ 1μm K^{1}. From the plot in Fig. 8 we can then derive that, for a fibre of 200 μm diameter, the radial velocity would change by Δv ~ 3 m/s K^{1}. In order to comply with the radialvelocity requirements, we have to keep the temperature of the system stable to 0.1 K.
From the analysis above, we conclude that it is sufficient to control the temperature of the RVreference module to a level of 0.05 K even when using aluminium for its structure. This kind of temperature stability is easily achieved with commercial components. Nevertheless, we made a particular effort to design the optomechanical system in the most symmetric and stable way, and to thermally isolate the critical parts inside the vacuum from the vacuum tank. Therefore operating in a vacuum will further improve the thermal stability.
3.4. Design of the SPIRou radialvelocityreference module
The RVreference module designed for SPIRou (Fig. 9) is derived from a concept that was successfully developed for HARPS and the visible wavelength range (Wildi et al. 2010). The design was later made more modular and adapted for the infrared wavelength range by replacing lenses with mirrors. This was successfully applied firstly to the HARPSN and CORALIE modules and was later essentially copied for SPIRou.
Fig. 9 Functional diagram of the RVreference unit. 

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The system conceptually consists of a FabryPerot étalon filter illuminated in white light to produce a set of equallyspaced (in frequency) emission lines of uniform intensity across a wide wavelength range. For the illumination we use a laserdriven light source (LDLS by Energetix) that essentially produces a blackbody emission of 10 000 K. Although at visible wavelengths the surface brightness of this sort of source is considerably higher than a standard halogen source of about 3000 K, the brightness difference at wavelengths above 1 μm is much lower and almost negligible. For our system we nevertheless decided to use an LDLS with a 200 μm fibre output that perfectly matches the étendue of the étalon. The LDLS light is fed to the RVreference module through an octagonal fluoride fibre of 300 μm core diameter and 2 m in length, whereas the RVreference module output fibre, which collects the light from the module and brings it to the spectrograph, is of 600 μm core diameter and 4 m length.
A vacuum tank contains the fibrefed FabryPérot optomechanical system (Fig. 10). The pressure is initially pumped to 10^{4} mbar or less, but eventually the valve is closed. More important than the actual pressure value is the pressure rise rate which must comply with the previously mentioned requirements. The temperature is controlled using heatingresistor foils glued around the vacuum tank. Two precise silicondiode temperature sensors (one on the vacuum tank for the control and the other close to the étalon for monitoring) and a Lakeshore 331 device close the temperaturecontrol loop to better than 5 mK rms. The whole system is isolated and packed inside a box to avoid heat exchange with the laboratory environment.
The optical system is placed in the vacuum vessel and fixed to the top flange in only 3 points, using thermally insulating material to minimize thermal conduction from outside. The collimating and focusing optics comprise identical protected silvercoated parabolas with a focal length of 100 mm. Parabolic mirrors were selected because they result in low aberrations and guarantee that the line profile stays symmetric.
Fig. 10 View of the vacuum tank (left) and the assembly in which the FabryPérot, fibres and mirrors are installed on the mechanical support structure (right). 

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The light enters the vacuum tank through an octagonal silica fibre purchased from CERAMOPTEC (OPTRAN WF). Its diameter is 200 μm in accordance to the derived finesse requirements. The octagonal shape was chosen to ensure a very uniform and thus stable illumination of the étalon (Chazelas et al. 2012). This is important to minimize possible illumination effects at the source level, such as PSF changes and variations of the illumination spot position or its angular distribution.
The connectorized fibre is mounted on a spider and illuminates, on its axis, a parabolic mirror of 50 mm clear aperture. Given the 100 mm focal length of the mirror, the F/2.5 beam of the fibre produces a collimated beam of 40 mm diameter. The backreflected beam is partially obstructed by the fibre and its spider, but we preferred to accept some light losses for the sake of symmetry. The beam crosses the étalon before being refocused by a second onaxis parabola on the output fibre, that is mounted in exactly the same way as the collimation part.
The output fibre inside the vacuum tank is circular and its diameter is 600 μm. A larger fibre was chosen in order make alignment easier, collect all the light, and eventually increase the stability of the system. Being located after the étalon, the diameter of this fibre has no influence on the resulting finesse.
The FabryPérot étalon used in SPIRou is shown in Fig. 11. Its physical diameter is of 60 mm while the clear aperture is 50 mm. The two mirrors are made of Suprasil. They were polished and coated by the company Thin Films Physics, Switzerland. The surface flatness is of the order of λ/ 100. The coating reflectivity of R = 80% + 2% over the 980−2350 nm range was designed to match the reflectivityfinesse requirements (Fig. 12). Both mirrors were antireflection (AR) coated on the external face. Nevertheless, a wedge was introduced between the two faces of each mirror to avoid possible parasitic interference with the external faces. The two mirrors are separated by a set of three highprecision Corning ULE (Ultra Low Expansion material – CTE< 2 × 10^{8} K) spacers produced by slsoptics, UK. The étalon was finally assembled using dry optical contacting by ICOS, UK.
Fig. 11 Picture of the SPIRou FabryPérot étalon. 

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Fig. 12 Transmission (left) and reflectance (right) of an étalon mirror. 

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4. Laboratory test
4.1. Test goals
We characterized the RVreference module in the laboratory with respect to its basic parameters. It turned out to be quite a demanding task to measure the highresolution transmission function because of the high spectral resolution of the étalon itself. To sufficiently sample the line profile we would have needed a spectrograph or spectrometer of resolving power R> 500 000 that only a FourierTransformSpectroscopy (FTS) can deliver. We decided to restrict ourselves to a tunable laser wavelength for this measurement. Once spectral performances are demonstrated at one wavelength, and knowing the étalon gap and the broadband reflectivity, the performances can be determined also at other wavelength. Nevertheless, we have separately determined the broadband transmittance and the flux delivered by the system. Also, we have measured the pressure and temperature stability to verify that the system complies with the technical requirements.
4.2. Measurements and results
4.2.1. Finesse
Figure 13 shows the setup used for characterizing our étalon. We used a temperaturecontrolled DFB laser diode at 1540 nm as a tunable laser. The centre wavelength has a temperature coefficient of 0.095 nm K^{1}. We used this characteristic to scan the transmittance of the FabryPérot as a function of wavelength. The source’s spectral width (FWHM = 2 MHz) is narrow enough to probe the line profile of our étalon (FWHM = 1 GHz). The flux was measured at the output of the system by an indiumgalliumarsenide (InGaAs) photodiode.
Fig. 13 Principle of our test setup. TCPS: temperature controller and laser diode power supply; LD: laser diode; FP: FabryPérot optomechanics, PD: photodiode 

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Fig. 14 Measured FabryPérot transmittance as a function of wavelength (blue dots) and fitted theoretical curve (green line). On the bottom the residuals to the fit are shown. 

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Figure 14 shows the measured transmittance curve T(λ) of the RVreference module. The finesse can be estimated by dividing the freespectral range (distance between two neighbouring peaks) by the FWHM of a single line. Alternatively, we fitted the obtained curve by a theoretical transmission function (green curve in Fig. 14) leaving the FSR and the effective finesse F_{E} as free parameters. The so obtained values are F_{E} ~ 12.76 and FSR = Δλ = λ^{2}/ 2nD ~ 0.09 nm, both perfectly in line with the design values. The finesse is actually slightly higher than expected because of an actual coating reflectivity of about 81−82% instead of the specified 80%. Finally, we would like to note the exact match of the fitted curve with the measured data, which demonstrates that we have all the effects which could influence the line symmetry, such as the divergence finesse, well under control.
4.2.2. Transmittance and flux
We measured the spectral power and transmittance of the system in the 950−1700 nm range directly with a laboratory Optical Spectrum Analyzer (OSA). Figure 15 shows the corresponding setup. Figure 16 shows the setup for the 1600−2400 nm spectral range, for which we employed a small optical bench with selectable bandpass filters to measure the optical power and transmittance in four discrete bands by means of a NIR photodiode.
The power was estimated using the internal calibrations and conversion factors of the OSA and the photodiode. The measurements should therefore not be considered to be of great accuracy but to provide a coarse estimate of the spectralpower density produced by the RVreference module as a whole. Figure 17 shows the spectral flux produced by the RVreference module as a function of wavelength. We originally observed a discrepancy of about a factor of 4.5 at 1625 nm where we have overlapping measurements on the two setups. We approximately measured the same factor when using an halogen lamp instead of the LDLS to lightfeed the module (Fig. 18). This factor can be explained by the bad match of the fibre diameter used to feed the OSA (60 μm) with the RVreference module output fibre. Not being able to correct for the coupling losses to the required precision, we decided to scale the measurements obtained with the OSA to the more accurate measurements with the silicon diode. To obtain the correct spectral flux we therefore multiplied the flux given for λ < 1600 nm in Figs. 17 and 18 by the measured factor of 4.5. We should note that even then we obtain a lower limit for the actual flux because we neglected transmission losses in the measuring system itself, namely the mirror, diffuser, and sensor coupling.
Fig. 15 Radial velocity reference module test setup for spectral flux and transmission measurements from 900 nm to 1700 nm. The setup includes an LDLS lamp, the FabryPérot system, a test fibre of 600 μm, and the optical spectral analyzer (OSA). 

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Fig. 16 Radial velocity reference module test setup for spectral power and transmission measurements from 1700 nm to 2460 nm. A small optical bench is included to analyze the light, comprising a collimator, filter wheel, focusing mirror, NIR photodiode, and voltmeter. 

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In interesting to note that the flux above 1000 nm produced by feeding the module with the two lamps (Figs. 17 and 18), the LDLS or the halogen lamp, is not significantly different despite the very different temperature of the lamps. This is expected by the blackbody emission law. For cost considerations, we therefore used a halogen lamp in the final RVreference module layout.
Fig. 17 Spectral flux of the RVreference module when used with the LDLS. Beyond 1700 nm, only three discrete measurement points are available. 

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Fig. 18 Spectral flux of the RVreference module when used with the halogen lamp. 

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The transmittance of the RVreference module was computed the ratio of the spectral powers measured at the output of the test setup with and without the RVreference module. In the latter case we simply connected together the input and output fibre of the module. The corresponding measurements for flux and transmittance in the four bands are summarized in Table 3. The last column indicates the transmission of the RVreference module at the peak T_{FPp} of the FabryPérot line, and has been computed by multiplying the average (broadband) transmittance of the system by the finesse of the FabryPérot.
Measured spectral power with P_{FP} and without P_{REF} the RVreference module, and the average T_{FPa} and peak throughput T_{FPp} of the RVreference module for four different filters of central wavelength λ_{c} and bandwidth Δλ.
4.2.3. Pressure and temperature stability
As explained in Sects. 3.3.3 and 3.3.4 the RVreference module must be operated in a vacuum well below 30 mbar and the pressure raise rate must be lower than 7.4 × 10^{3} mbar. After evacuating the vacuum tank and doing a leak test to ensure the absence of vacuum leak, we performed a pressure test as shown in Fig. 19. The residual outgassing rate is 7.2×10^{3} mbar day^{1}, just within the specification. Experience shows that outgassing decreases as a function of time to a level much better than the required value.
Fig. 19 Pressure (outgassing) as a function of time. 

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We tested the temperature stability in a similar way. Figure 20 shows the diagram of the setup for temperature monitoring.
Fig. 20 Scheme of the temperature control. 

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We used a LakeShore 331 temperature controller with a setpoint set at 25 C. The temperature control loop is closed on the sensor, which is bonded to the vacuum vessel’s inside wall. A second sensor monitors the temperature of the optomechanical structure in proximity of the FabryPérot étalon. Figure 21 shows the temperature of both sensors after turning on the temperature controller.
Fig. 21 Temperature of the RVreference module after switching on the control loop. The green curve shows the control sensor located on the vacuum tank. The blue curve represents the sensor located in proximity of the étalon. 

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The temperature of the vacuum tank stabilizes after less than one hour with a dispersion of σ_{T} = 1.2 mK, while the sensor close to the étalon reaches a stable temperature after about 40 h with a slightly higher dispersion of σ_{T} = 2.1 mK. This can be explained by the fact that the test was performed in a laboratory with no temperature control at all and thus nighttoday temperature variations of several degrees. Even under these conditions the temperature stability of our RVreference module is well within specification.
5. Radial velocity performance
5.1. Photon noise
By analogy with the HARPSN FabryPérot we know that the centroid of a single emission line featuring 100 000 e^{−} per line can be determined with a photonnoise limited precision σ of better than 2 m s^{1}. SPIRou will be using a Hawaii 4RG detector with lower dynamical range than typical CCD detector. If we assume a conservative line flux of only 25 000 e^{−} per exposure, given the fact that the present étalon will produce about 14 280 lines in the spectral range of SPIROU, we will obtain a global precision of the drift measurement of (20)This value is significantly lower than the aimed precision of 0.3 m s^{1} for SPIRou, and therefore compliant with the requirements.
5.2. Radial velocity stability
Radialvelocity stability measurements could however not be performed, because they would have required a spectral reference at least as stable as the RVreference module is supposed to be. We therefore decided to postpone these measurements until they can be performed on SPIRou itself, where it will be possible to compare our module directly with a Uranium hollowcathode lamp.
Nevertheless, we can refer to stability measurements of an identical system (besides the étalon coatings because they are optimized for the visible) made with HARPSN (Wildi et al. 2011). Doing this, we demonstrated that the shortterm RVdispersion obtained using the FabryPérot system is better than that measured using the ThAr hollowcathode lamp. Typical dispersion values are of the order of 0.1 to 0.2 m s^{1} on time scales from hours to a day. This is again perfectly in line with the specified RVstability requirement. Given the almost identical design of these two systems, we have plausible reason to expect similar performances on the SPIRou RVreference module.
5.3. Modal noise
Several studies have demonstrated that the finite number of modes in a wave guide such as a fibres, may introduce noise in excess to pure photon noise. For instance, the modal noise limits the signaltonoise ratio (S/N) (McCoy & Ramsey 2011) measured in the continuum of the measured spectrum. This modal noise increases with wavelength because of the fewer modes in the fibre and it may therefore represent a limit to the NIR radialvelocity precision budget. We therefore analyze the situation for the SPIRou RVreference module. The number of excited modes in a uniformlyilluminated fibre is inversely proportional to the wavelength and is given by the formula (McCoy & Ramsey 2011)(21)where d is the fibre core diameter, λ is the light’s wavelength, and NA is the fibre’s numerical aperture. In the wavelength domain of SPIRou and for the chosen fibre, we have M = 9941 at 980 nm and M = 1741 at 2350 nm. At first glance it appears that at short wavelengths there are enough modes for our FabryPérot system because we expect to obtain an S/N at continuum of the order of the square root of the number of modes(22)(Baudrand & Walker 2001) meaning about 100 on the blue end of the spectrum. On the red end of the spectrum the modelimited S/N ratio decreases to about 30, which is even below what we expect to be the limit to reach a precision of 1 m s^{1}.
Let us take HARPSN as the reference instrument. The FabryPérot spectrum recorded by HARPSN includes approximately 20 000 lines with average S/N = 187 pixel^{1} and global photonic error on the drift measurement σ_{RV} = 0.044 m s^{1}. In SPIRou the number of lines is approximately 14 000. Assuming a similar S/N per line, and by analogy with HARPSN, we estimate that the global photonic error on the drift measurement will be of the order of σ_{RV} = 0.062 m s^{1}.
Measured σ_{RV} for two limit cases of S/N.
Assuming an effective S/N = 100 pixel^{1} and S/N = 30 pixel^{1} at the two extreme ends of the spectral range of SPIRou, we computed the effective measurement error values (see Table 4). Given these values, we see that the modal noise contribution to the error budget is 0.38 m s^{1} even in the worst case, and for the average of the spectral range it is better than the 0.3 m s^{1} requirement of SPIRou.
The impact of modalnoisereduced S/N on the photocentre measurement of a spectral line and thus its radial velocity is not yet fully understood because the impact depends on many factors including the optical design of the spectrograph. Nevertheless we think that this question deserves further tests. We have therefore started and are currently conducting laboratory tests, such as mechanical agitation of the fibre, to understand the impact of modal noise in fibres in terms of radialvelocity measurement in general and on other systems, such as our RVreference module in particular. The detailed analysis of modal noise lies however beyond the goals of this paper. We refer to Blind et al. (in prep.) for a detailed discussion and presentation of these modalnoise tests and their results, and point towards Micheau et al. (2012) and Micheau et al. (2015) for the specific case of SPIRou, for which several solutions to the modalnoise problem have been proposed.
6. Conclusions
In this paper we present the design of a new infrared FabryPérot RVreference module for SPIRou and we describe its key properties and spectral characteristics in detail. The primary objectives were to build, test and finally operate a FabryPérotbased RVreference module able to provide the needed spectral information over the full wavelength range of SPIRou to measure instrumental drift to a precision of 30 cm s^{1}. It must be remarked that we followed a quite strict topdown approach: 1) after establishing the requirements set by SPIRou we 2) converted them into requirements for the RVreferece module; 3) verified the assumption by analysis and simulations; 4) designed and manufactured the module according to the choices we made; and finally 5) tested the key performances in the laboratory. The obtained performances, at least those which could be verified in the laboratory, are compliant with the requirements. Only the RVstability requirements had to be postponed to a later stage when the SPIRou spectrograph will be ready for system tests. Nevertheless, we know by analogy with the HARPSN RVreference module, that we can expect an RVstability well below 1 m s^{1}. In summary, we demonstrate that the SPIRou reference module can replace any cathode spectral lamp or absorption cell for drift measurements at relatively moderate costs.
Our module also provides equallyspaced spectral lines of uniform intensity over an extremely wide spectral range, which could greatly help in measuring the detector geometry. Although the étalon does not have the intrinsic accuracy provided by an atomic transition and the mirror coatings may introduce slow variations of the phase (and thus cause groupdelay dispersion, as per Wildi et al. 2011), it should be remembered that the line separation and position is perfectly smooth and continuous in wavelength. This information can be used to improve the wavelength solution, in particular to determine the higherorder terms of the polynomials used to describe the pixeltowavelength relationship, which are badly constrained by the sparse lines of hollowcathod lamps only. In the absence of commercial and affordable laserfrequency combs that cover the entire spectral range, we are currently investigating and implementing a combined use of hollowcathode lamps and FabryPérot calibration. The former provides the accuracy (or global wavelength “zero point”), whereas the latter provides the detector geometry and the pixeltopixel and intrapixel responses. In fact, we are also considering the possibility of varying the line position of the FabryPérot by changing the (low) pressure inside the vacuum tank, to “scan” and characterize the response of every detector pixel individually.
We can conclude that the presented RVreference module for SPIRou is able to measure instrumental drifts at the required precision level and can replace the performancelimited hollowcathode lamps and absorption cells with respect to this goal. Furthermore, we identify possible developments of the module and significant potential to convert it into a calibration source, which could turn the FabryPérotbased light source into a
costeffective alternative to laserfrequency combs, at least in the short and mid term.
Acknowledgments
This work was supported by the Swiss National Science Foundation (SNSF) grants Nos. 200021140649, 200020152721 and 200020166227. The authors acknowledge its financial support.
References
 Ball, D. W. 2006, Field guide to spectroscopy, SPIE field guides (Bellingham, Wash.: SPIE Press) [Google Scholar]
 Barnes, J. R., Jeffers, S. V., & Jones, H. R. A. 2011, MNRAS, 412, 1599 [NASA ADS] [CrossRef] [Google Scholar]
 Baudrand, J., & Walker, G. A. H. 2001, PASP, 113, 851 [NASA ADS] [CrossRef] [Google Scholar]
 Chazelas, B., Pepe, F., Wildi, F., et al. 2010, in Modern Technologies in Space and Groundbased Telescopes and Instrumentation, Proc. SPIE, 7739, 773947 [CrossRef] [Google Scholar]
 Chazelas, B., Pepe, F., & Wildi, F. 2012, in Modern Technologies in Space and Groundbased Telescopes and Instrumentation II, Proc. SPIE, 8450, 845013 [CrossRef] [Google Scholar]
 Delfosse, X., Donati, J.F., Kouach, D., et al. 2013, in SF2A2013: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, eds. L. Cambresy, F. Martins, E. Nuss, & A. Palacios, 497 [Google Scholar]
 McCoy, K., & Ramsey, L. 2011, in Advanced Maui Optical and Space Surveillance Technologies Conference, E69 [Google Scholar]
 Micheau, Y., Bouchy, F., Pepe, F., et al. 2012, Proc. SPIE, 8446, 84462 [CrossRef] [Google Scholar]
 Micheau, Y., Bouyé, M., Parisot, J., & Kouach, D. 2015, in Techniques and Instrumentation for Detection of Exoplanets VII, Proc. SPIE, 9605, 96051 [Google Scholar]
 Pepe, F., Mayor, M., Queloz, D., & Udry, S. 2004, in Planetary Systems in the Universe, ed. A. Penny, IAU Symp., 202, 103 [NASA ADS] [Google Scholar]
 Reiners, A., Bean, J. L., Huber, K. F., et al. 2010, ApJ, 710, 432 [NASA ADS] [CrossRef] [Google Scholar]
 Reiners, A., Banyal, R. K., & Ulbrich, R. G. 2014, A&A, 569, A77 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Schwab, C., Stürmer, J., Gurevich, Y. V., et al. 2015, PASP, 127, 880 [NASA ADS] [CrossRef] [Google Scholar]
 Udry, S., Bonfils, X., Delfosse, X., et al. 2007, A&A, 469, L43 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Wildi, F., Pepe, F., Chazelas, B., Lo Curto, G., & Lovis, C. 2010, in Groundbased and Airborne Instrumentation for Astronomy III, Proc. SPIE, 7735, 77354 [CrossRef] [Google Scholar]
 Wildi, F., Pepe, F., Chazelas, B., Lo Curto, G., & Lovis, C. 2011, in Techniques and Instrumentation for Detection of Exoplanets V, Proc. SPIE, 8151, 81511 [Google Scholar]
 Ycas, G. G., Quinlan, F., Diddams, S. A., et al. 2012, Optics Express, 20, 6631 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
Measured spectral power with P_{FP} and without P_{REF} the RVreference module, and the average T_{FPa} and peak throughput T_{FPp} of the RVreference module for four different filters of central wavelength λ_{c} and bandwidth Δλ.
All Figures
Fig. 1 Concept of the planoplano FP and sketch of the interfering light beams. 

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In the text 
Fig. 2 Simulated curve for our FabryPérot passband. 

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In the text 
Fig. 3 Spectral power produced by the LDLS. The original plot, which is an excerpt from LDLS EQ99 handbook, was manually digitized. 

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In the text 
Fig. 4 Simulated transmittance of a FabryPérot for fibre diameters of 200, 500, and 900 μm, assuming the fibre is centred on the optical axis and a focal length of the collimator f = 100 mm. 

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In the text 
Fig. 5 Simulated transmittance of a FabryPérot for fibre decentering value of 20, 250, 500, and 1000 μm assuming a fixed fibre diameter of D = 200μm and a focal length of the collimator f = 100 mm. 

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In the text 
Fig. 6 Finesse for a centred fibre as a function of fibre diameter (left) and as a function of fibre decentring (right) for a fixed fibre diameter D = 200 μm. The blue line marks the area we are interested in namely a small fibre diameter and an effective finesse close to the nominal value F_{R} = 13. 

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In the text 
Fig. 7 Change in radial velocity for a centred fibre as a function of fibre diameter (left) and as a function of fibre decentring (right) for a fixed fibre diameter D = 200 μm. The blue line marks the limit area we are interested in. The area is small because small changes introduces shift of several hundreds or more of m s^{1} in both cases. 

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In the text 
Fig. 8 Radial velocity sensitivity to fibresize change for a centred fibre (left) and to decentring for a fixed fibre size of D = 200 μm (right). The blue line marks the limit area we are interested in. For 2 mrad fibre size, the RV will change by 300 m s^{1} (3 m s^{1} micron^{1}) for a centred fibre. In the case of decentring, it changes by 600 m s^{1} (6 m s^{1} micron^{1}). 

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In the text 
Fig. 9 Functional diagram of the RVreference unit. 

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In the text 
Fig. 10 View of the vacuum tank (left) and the assembly in which the FabryPérot, fibres and mirrors are installed on the mechanical support structure (right). 

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In the text 
Fig. 11 Picture of the SPIRou FabryPérot étalon. 

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In the text 
Fig. 12 Transmission (left) and reflectance (right) of an étalon mirror. 

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In the text 
Fig. 13 Principle of our test setup. TCPS: temperature controller and laser diode power supply; LD: laser diode; FP: FabryPérot optomechanics, PD: photodiode 

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In the text 
Fig. 14 Measured FabryPérot transmittance as a function of wavelength (blue dots) and fitted theoretical curve (green line). On the bottom the residuals to the fit are shown. 

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In the text 
Fig. 15 Radial velocity reference module test setup for spectral flux and transmission measurements from 900 nm to 1700 nm. The setup includes an LDLS lamp, the FabryPérot system, a test fibre of 600 μm, and the optical spectral analyzer (OSA). 

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In the text 
Fig. 16 Radial velocity reference module test setup for spectral power and transmission measurements from 1700 nm to 2460 nm. A small optical bench is included to analyze the light, comprising a collimator, filter wheel, focusing mirror, NIR photodiode, and voltmeter. 

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In the text 
Fig. 17 Spectral flux of the RVreference module when used with the LDLS. Beyond 1700 nm, only three discrete measurement points are available. 

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In the text 
Fig. 18 Spectral flux of the RVreference module when used with the halogen lamp. 

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In the text 
Fig. 19 Pressure (outgassing) as a function of time. 

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In the text 
Fig. 20 Scheme of the temperature control. 

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In the text 
Fig. 21 Temperature of the RVreference module after switching on the control loop. The green curve shows the control sensor located on the vacuum tank. The blue curve represents the sensor located in proximity of the étalon. 

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In the text 