# Compression of Extreme-Ultraviolet Ultrashort Pulses by Grating Configurations

Authors: Fabio Frassetto; Paolo Miotti; Luca Poletto
Journal: Journal of Spectroscopy
 (2015)

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## Abstract

The design and realization of grating instruments to condition the spectral phase of ultrashort extreme-ultraviolet pulses are discussed. The main application of such configurations is the temporal compression of pulses by compensating the phase chirp and getting close to the Fourier limit. We discuss the two configurations useful for the realization of ultrafast grating compressors, namely, the classical diffraction mount and the off-plane one. The configuration may be applied to free-electron lasers and high-order laser harmonics.


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## Body

## 1. Introduction

The developments in laser technology over the last years lead to the generation of extreme-ultraviolet (XUV) and X-ray coherent ultrashort pulses in the femtosecond and subfemtosecond time scale (1 fs = 10−15 s) [1, 2]. While femtosecond optical lasers have offered unique insights into ultrafast dynamics, short wavelength radiation offers the capability to access and measure the structural arrangement and electronic structure; therefore, the advent of high-energy, short-pulse X-ray sources based on free-electron lasers (FELs), high-order laser harmonics (HHs), and laser plasmas is now making it possible to probe the dynamics of electrons within molecules [3, 4]. In the following, we will focus our attention on HHs generated in gas and FELs, as ultrashort sources with high brightness, high degree of coherence, and high peak intensity.The HH spectrum is described as a sequence of peaks corresponding to the odd harmonics of the fundamental laser wavelength and having an intensity distribution characterized by a vast plateau, whose extension is related to the pulse intensity and frequency. The use of advanced phase matching mechanisms and interaction geometries has made possible the generation of HHs up to the water window region (2.3–4.4 nm), while still using a table-top laser source [5–7]. The radiation generated with the scheme of the HHs using few-optical-cycles laser pulses is currently the main tool for the investigation of matter with attosecond resolution (1 as = 10−18 s) [8–11]. Both trains [12, 13] as well as isolated [14–18] bursts of attosecond pulses have been experimentally demonstrated. Recently, circularly polarized attosecond pulses have been also demonstrated [19, 20]. The physical grounds of such short pulses originate from the model of HHs generation, that is, the phase-matched emission of radiation as result of the recombination of a tunnel-ionized electron with its parent ion. Once the conditions for such recombination are realized in only one occurrence per laser pulse, an isolated ultrashort XUV pulse is generated. Both trains and isolated attosecond pulses are positively chirped, resulting from the different duration of the quantum paths that contribute to different portion of the emitted spectrum. A detailed discussion of the attosecond chirp is found in [21]. Due to the chirp, the pulse temporal duration is longer than the Fourier limit. The condition of being at the Fourier limit is equivalent to the condition of a frequency-independent spectral phase and implies that the time-bandwidth product is at its minimum and that there is no chirp. Positively chirped pulses may be temporally compressed down to the Fourier limit by introducing a system that gives a negative chirp that compensates for the intrinsic chirp of the pulse. This problem has been successfully addressed by exploiting the negative group delay dispersion (GDD) of a thin metallic filter (see [13, 15]) or broadband multilayer optics (see [16]). The introduction of a compressor tunable at different energies may add strong flexibility to the beamline when different spectral regions of operation are requested.FEL sources facilities generate spatially coherent XUV/X-ray radiation with characteristics similar to the light from optical lasers, ultrashort time duration, and an increase of 6–8 orders of magnitude on the peak brilliance with respect to 3rd generation synchrotrons, opening the way to new studies in ultrafast phenomena in different fields spanning from biology to physics of matter [22–25]. Several methodologies have been proposed for the generation of ultrashort FEL pulses in the femtosecond and subfemtosecond regime, as time slicing [26–28] or the reduction of the electron bunch charge [29], which has brought to the generation of FEL pulses as short as 3 fs [30]. Most of these methods rely on the selection of an opportunely small portion of the electron beam which undergoes FEL amplification. One of the main drawbacks common to these solutions is the reduction of the amount of charge effectively contributing to the light amplification. An alternative possibility is the optical compression of the radiation pulse generated by the whole electron beam. In this case, the electron beam is required to have a nonzero energy chirp in order to generate a chirped pulse. The FEL pulse has then to be compressed to reach the Fourier limit. As for solid-state lasers, where frequency chirping is introduced to stretch the pulse before its amplification and, then, after amplification, compensated to recover the ultrashort duration and high peak power, chirped pulse amplification may be applied also to FELs, if the seeding pulse is stretched in time before interacting with the electron beam [31–33]. Despite the necessity of an additional optical stage, namely, the FEL compressor, this solution allows the use of the whole electron beam charge obtaining a significantly higher number of photons with ultrashort duration.Indeed, for both HHs and FEL facilities, the availability of a XUV and X-ray tunable optical compressor is particularly attractive in order to increase the peak intensity and the time resolution of the source.Here, we discuss the use of gratings at grazing incidence to realize a broadband and tunable XUV compressor for chirped pulses. In the design of instruments for photon handling in the XUV ultrafast domain, some differences with respect to traditional schemes are notable [34, 35]. The first is that, to exploit the very short duration of the pulse, the study of the optical length of the rays gathered by the pupil and their equalization is mandatory. Moreover, the much extended bandwidth available from the coherent XUV sources may be exploited only if the instrument has a rather flat spectral response. Finally, an overall high throughput of the instrument is often a crucial feature to maintain high peak intensity.The use of gratings at grazing incidence to realize tunable monochromators for XUV ultrafast pulses is well established for both HHs and FELs. When using a grating for ultrafast pulses, the main problem to be faced is the pulse-front tilt that is introduced by diffraction. Two are the options in designing an ultrafast monochromator, namely, the single-grating [36] or the double-grating design [37, 38]. In the first case, being adopted as single grating, a residual pulse-front tilt has to be accepted at the output of the monochromator. In fact, each ray that is diffracted by two adjacent grooves is delayed by mλ/c, where m is the diffraction order, λ is the wavelength, and c is the speed of light in vacuum. The pulse-front tilt is given by the total difference in the optical paths of the diffracted beam; that is, ΔτG=mλN/c, where N is the number of the illuminated grooves. The aim of the design is to find a suitable grating geometry that minimizes the temporal broadening. Single-grating monochromators with response in the range of few tens of femtoseconds are presently used in HH beamlines [39–41] and FEL facilities [42]. In the second case, the design consists of a pair of gratings to compensate for the pulse-front tilt. The first grating is demanded to perform the spectral selection on an intermediate slit; the second grating compensates for the pulse-front tilt of the diffracted beam by equalizing the length of the optical paths, giving a temporal resolution much higher than the single-grating design. Double-grating instruments have been demonstrated to be very effective for HHs, with time resolution well below 10 fs [43–47]. The choice between the two options has to be performed as a trade-off between efficiency and throughput, which are maximized in the single-grating design, and temporal resolution, which is maximized in the double-grating design. Double-grating configurations, which are able to preserve the ultrafast duration of the pulse, have been also proposed as beam splitters for ultrafast intense pulses [48] and as IR-XUV beam separators for HHs [49].In this paper, we report on the use of gratings to realize XUV compressors for the conditioning of the spectral phase of chirped pulses. A brief introduction to the grating geometries that are required to realize XUV ultrafast instruments is given. The concept is applied to the realization of XUV compressors with applications to HHs and FELs. The concept may find suitable applications to ultrafast spectroscopy experiments.


## 2. Grating Geometries for Ultrashort Pulses

Grazing-incidence gratings may be used in two different geometries: the classical-diffraction mount (CDM) and the off-plane mount (OPM) [50].In the case of the CDM, the geometry is defined on a plane as shown in Figure1(a). Let us define the incidence angle α and the diffraction angle β, respectively, as the angles between the direction of the input beam and the normal beam to the grating and the direction of the diffracted beam and the normal beam to the grating, both taken with positive signs. The grating equation for the CDM is sinα-sinβ=mλσCD, where λ is the wavelength, m the diffracted order, and σCD the groove density.Reflection grating geometries: (a) classical-diffraction and (b) off-plane mount.
(a)
(b)The geometry of the OPM is shown in Figure1(b). In this case, the incident and diffracted wave vectors are almost parallel to the grating grooves [51]. The direction of the incoming rays is described by two parameters: the altitude and the azimuth. The altitude γ is defined as the angle between the direction of the incoming rays and the direction of the grooves. The azimuth μ of the incoming rays is defined to be zero if they lie in the plane perpendicular to the grating surface and parallel to the rulings. Let ν define the azimuth of the diffracted light at wavelength λ and order m. The grating equation for the OPM is sinγ(sinμ+sinν)=mλσOP, where σOP is the groove density. The OPM gives higher throughput than the classical mount, since it has been theoretically demonstrated and experimentally measured that the peak diffraction efficiency is close to the reflectivity of the coating at the altitude angle [52]. Therefore, the OPM geometry is suitable for the design of XUV grating instruments with high efficiency [53].When realizing a compressor for ultrafast pulses, then the main problem to be dealt with is the pulse-front tilt given by a single grating. This effect, although negligible for picosecond or longer pulses, is dramatic in the femtosecond or even subfemtosecond time scale and has to be corrected by a second grating in a compensated configuration. From the point of view of the ray paths, the differences in the path lengths of rays with the same wavelength within the beam aperture that are caused by the first grating have to be compensated by the second grating; that is, all the rays with the same wavelength make the same optical path. The second grating compensates also for the spectral dispersion caused by the first grating; that is, all the rays at different wavelengths within the pulse spectrum exit the second grating with parallel directions. Both of these conditions are satisfied by a scheme with two equal plane gratings mounted with opposite diffraction orders; that is, the incidence angle on the second grating is equal to the diffraction angle of the first grating. The phase chirp introduced by the system may be finally calculated as the difference in the optical path between rays at different wavelengths. This principle is used in many ultrafast devices in the visible and near infrared, as it was demonstrated that grating pairs may be arranged to realize compensators for the laser cavity dispersion, phase modulators, stretchers, and compressors for chirped pulse amplification [54–56].


## 3. Grazing-Incidence Grating Compressor

The basic version of the arrangement of a XUV grazing-incidence grating compressor consists of two identical plane gratings mounted in the compensated configuration, as shown in Figure2. Since the plane gratings have to be operated in parallel light, a XUV collimating mirror, that is, a paraboloidal or toroidal mirror, is required in front of the compressor. Therefore, the compressor consists of three optical elements, namely, the collimator and the two gratings. Due to the symmetry of the configuration, the output rays are parallel to the input rays for all the wavelengths. Indeed, in the case of the CDM, the incidence angle on G2, α2(λ), is equal to the diffraction angle from G1, β1(λ), and the diffraction angle from G2, β2, is constant with the wavelength and equal to the incidence angle on G1, β2=α1. Similarly, in the case of the OPM, the azimuth angle of incident rays on G2, μ2(λ), is equal to the azimuth angle of diffracted rays from G1, ν1(λ), and the azimuth angle of the rays diffracted from G2, ν2, is equal to the azimuth angle of the rays incident on G1, ν2=μ1.Plane double-grating compressor: (a) schematic view, including the collimating mirror (M), and the two gratings (G1 and G2); (b) classical-diffraction mount; (c) off-plane mount.
(a)
(b)
(c)Since different wavelengths are diffracted by G1 at different angles, the rays do not make the same optical paths within the compressor. Therefore, the group delay (GD), intended here as the propagation time of the rays from the input plane of G1 to the output plane of G2, is not constant with the wavelength. Aim of the compressor is to introduce suitable group-delay dispersion (GDD), which is a variation of the propagation time of the rays with different wavelengths.As usual, GD is expressed as a function ofω:
(1)GDω≡∂ϕ∂ω=OPωc,
where OPω is the optical path at frequency ω=2πc/λ and c is the speed of light in vacuum.Let us define the central pulse frequencyωc and the central wavelength λc as
(2)ωc≡ωmin⁡+ωmax⁡2=πc1λmin⁡+1λmax⁡,λc≡2πcωc,
where the bandwidth of the pulse is limited between ωmin⁡=2πc/λmax⁡ and ωmax⁡=2πc/λmin⁡.In the case of the CDM, the optical path is analytically expressed (for less than a constant term) as(3)OPCDλ=qCDcos⁡βccos⁡β1-sinαsinβ,
where α is the incidence angle on G1, β and βc are, respectively, the diffraction angles from G1 at the generic wavelength λ and, at the wavelength λc, and qCD is the G1-G2 distance. In case of a narrow-band pulse with Δλ/λ<20%, (3) results in linear λ. Expressing β=βc+Δβ and using the relation Δβ=-mσCDΔλ/cosβc, it may be expressed as
(4)OPCDλ=qCDλcmσCDcos⁡βc2λ-λc.Similarly, in the case of the OPM, the optical path is analytically expressed (for less than a constant term) as(5)OPOPλ=qOPsin2γcos⁡μcos⁡ν1+sinμsinν,
where the grating parameters have been calculated to have the wavelength λc diffracted at νc=μ; that is, 2sinγsinμ=mλcσOP. Expressing ν=νc+Δν and using the relation Δν=mσOPΔλ/(cos⁡μsinγ), (5) is linearized in λ, in case of a narrow-band pulse, as
(6)OPOPλ=qOPλcmσOPcos⁡μ2λ-λc.Note that, in both cases, the optical path is anyway increasing with the wavelength and this forces the GDD introduced by the compressor to be negative.Let us defineKω as
(7)KωCD≡qCDc2πmσCDωccos⁡βc2,KωOP≡qOPc2πmσOPωccos⁡μ2,
where KωCD and KωOP refer, respectively, to the CDM and to the OPM.The optical path can be expressed as a function ofω with the relation
(8)OPω=-cKω1-ωcω.Equation (8) is expanded in series of ω-ωc and is integrated to obtain the expression of the phase as
(9)φω=Φ0+Φ1ω-ωc+Φ2ω-ωc2+Oω-ωc4,
where the first coefficient that describes the distortion of the pulse temporal profile is
(10)Φ2=-Kω2ωc.For a narrow-band pulse, the GD is almost linear also inω and the GDD is constant and negative; GDD=-Kω/ωc. Once the required GDD to compress the pulse has been defined, the above equations define the parameters of the grating compressor in both geometries.Note that, in the CDM, the first grating is normally operated in the orderm=-1; that is, α<β, since this gives a shorter distance q, once the required GDD has been fixed, therefore, a more compact compressor. In the case of the OPM, the operations at order m=±1 are totally equivalent.Once the length of the armq has been selected, the two geometries give the same compression if KωOP=KωCD; that is, σOP/cosμ=σCD/cosβc. Since μ is typically below 20° and βc is above 80°, the groove density that would be required in the OPM is much higher than the CDM and may not be available from grating providers. Therefore, a compressor in the OPM is typically longer than the corresponding CDM as will be shown in the test case presented below.The compressor introduces a spatial chirp of the pulse; that is, rays with different wavelengths have the same output direction but they are not exactly superimposed. In the conventional design of compressors for IR pulses, the spatial chirp is canceled by making the beam pass two additional times through the same gratings, so the output spatial dispersion is zero. This cannot be realized in grazing incidence, since it would require the insertion of two additional gratings that would make the configuration too complex. The chirpSC(λ) is expressed, in case of a narrow-band pulse of bandwidth Δλ, as
(11)SCCDλ=qCDσCDcos⁡αcos⁡2βcΔλSCOPλ=qOPσOP1+3cos⁡2γsin2μcos⁡2μΔλ,
where SCCD and SCOP refer, respectively, to the CDM and to the OPM. Since the rays are parallel, the spatial chirp does not influence the quality of the final spot size if the beam is focused by a proper concave mirror.In the following, we will apply the double-grating configuration to the case of compression of FEL pulses and of attosecond pulses generated through HHs.


## 4. Grating Compressor Applied to FEL Pulses

The double-grating compressor, in which optical elements are used at grazing incidence, is very suitable for FEL pulses, since it has robust optical elements to be operated under the intense FEL radiation. Here, we assume the parameters of [57], which are reported in Table 1 and may be a test case for the application to FEL chirped pulse amplification.Table 1
Requirements for the FEL compressor.
Central wavelength,λc
13.5 nm
Bandwidth,Δλ
0.8 nm
Time stretching,Δt
310 fs
Group delay dispersion, GDD
−37 fs2The two geometries are compared using commercially available gratings with groove density as high as 2400 gr/mm. The resulting parameters of the compressor are shown in Figure3. Note that the size of the OPM compressor is much larger than the CDM one. Indeed, the length of the instrument in the CDM may be easily reduced well below 0.5 m by using a low-density grating; on the contrary, the OPM requires at least about 1.5 m, unless extremely high-density gratings, which are difficult to be manufactured, are adopted. The spatial chirp is shown in Figure 4. In the OPM case, for the G1-G2 distance being much longer, the spatial chirp is larger. The main advantage of the OPM is the higher total efficiency, which can be quantified in the 0.15–0.20 range compared to the 0.04–0.07 range of the CDM (see [53]).Parameters of the FEL grating compressor: (a) OPM and (b) CDM.
(a)
(b)Spatial chirp of the FEL grating compressor: (a) OPM; (b) CDM.
(a)
(b)It may be concluded that the XUV double-grating compressor for application to FEL radiation on a narrow-band emission requires, in case of the OPM, a definitely larger space than the CDM and gives also a larger spatial chirp. On the other side, the OPM gives higher efficiency. The choice between the two geometries depends mainly on the surrounding conditions, such as the available space on the beamline and the mechanical stability of the optical mountings, which may force the choice of the more compact CDM configuration with respect to the OPM.


## 5. XUV Attosecond Compressor

The double-grating configuration shown in Figure2 is not suitable for the compression of XUV attosecond pulses, since the distance q that is required to give the necessary GDD that compensates for the intrinsic pulse chirp is too small to be realized in practice. Therefore, the configuration has to be modified as shown in Figure 5. The design originates from the scheme of the double-grating XUV ultrafast monochromator realized to select a suitable harmonic within the broad HHs spectrum without altering the intrinsic femtosecond pulse time duration [58]. The OPM is adopted since it gives higher efficiency in a compact environment.Figure 5
Layout of the XUV attosecond compressor with gratings in the OPM.The layout consists of four grazing-incidence parabolic mirrors, indicated as P1, P2, P3, and P4, and two plane gratings operated in the OPM, indicated as G1 and G2. The compressor is divided into two equal sections, P1-G1-P2 and P3-G2-P4. Since the gratings have to be operated in parallel light, the first mirror of each of the two sections acts as the collimator and the second mirror as the condenser. The four mirrors are operated with unity magnification; that is, the input armsp of P1 and P3 are equal to the output arms p of P2 and P4. The gratings G1 and G2 have the same groove density and altitude.The use of parabolic mirrors instead of the more simple toroidal ones adopted for the design of femtosecond monochromators (see [43]) is required to reduce the aberrations to negligible levels, since any residual aberration causes a spread of the optical paths within the aperture of the instrument. The ideal collimator and condenser, completely free from aberrations in case of a point-like source, is the paraboloid. It can be shown that grazing-incidence toroidal surfaces when used as collimating and condensing elements exhibit residual aberrations that cannot be tolerated in the attosecond time scale (see [58]).In brief, the input beam is collimated by P1 and then is diffracted by G1, that is, placed at a distance S2 from P2. The latter realizes a spectrally dispersed image of the source on its focal plane, that is, the source plane for the second section. The beam is collimated by P3 and diffracted by G2, that is, placed at a distance S3 from P3. Due to the symmetry of the double-grating configuration, all the rays diffracted from G2 are parallel and are finally focused on the output focal point by P4. The two focusing mirrors placed between the gratings act as a telescopic arrangement reducing the effective path between the gratings. This makes it possible to(1) produce an effectively negative grating separation with positive GDD, differently from the compressor with plane gratings; (2) continuously tune the GDD from negative to positive values; (3) achieve the very small grating separations necessary for the compensation of the attosecond chirp.Since all the rays are collimated in the paths S1 between P1 and G1 and S4 between G2 and P4, the GD does not depend on the choice of S1 and S4 but only on the choice of S2 and S3, in particular on the sum S = S2 + S3. This is the key parameter to be properly set to introduce the required GDD. Due to the symmetry of the configuration, G1 is imaged on G2 when S = 2p. This is the condition that gives group delay constant with the wavelength; that is, GDD = 0. For S < 2p, G1 is imaged behind G2 and the resulting GDD is positive. For S > 2p, G1 is imaged before G2 and the resulting GDD is negative, as shown in Figure 6. Therefore, the quantity S-2p plays the role of q in the double-grating compressor, being capable to give also negative values for q. The tuning of the GGD is performed in a simple way by moving G2 and keeping G1 fixed. Therefore, the compressor has fixed input and output points, fixed output direction, and a single mechanical movement to finely tune the GDD.Operation of the configuration with variable GDD: (a) GDD = 0; (b) GDD > 0; (c) GDD < 0.
(a)
(b)
(c)As a test case, the design of a compressor for attosecond pulses in the 70–140 eV region is here discussed. Here, we assume the parameters of [59], which are reported in Table 2. The parameters of the compressor are reported in Table 3. The gratings have 200 gr/mm groove density and are operated at 1° altitude and 4.8° azimuth. The choice of the altitude has been done through ray-tracing calculations in order to minimize the spread of the optical paths of the rays with the same wavelengths, which states the ultimate limit of the time response at the output of the compressor, that results 12 as. The GD is shown in Figure 7. In such a large bandwidth, the GD is not linear, but it has also a quadratic term that originates third-order dispersion (TOD). It has been shown by simulation [59] that such a compressor is able to decrease the pulse duration down to ≈60 as FWHM, which is not far from the Fourier limit on the given bandwidth (35 as).Table 2
Requirements for the attosecond compressor.
Bandwidth
70–140 eV (18–9 nm)
Time stretching,Δt
0.47 fs
Group delay dispersion, GDD
−4.5 · 10−3 fs2Table 3
Parameters of the compressor for the 70–140 eV spectral region.
Mirrors arms
200 mm
Grating  groove density
200 gr/mm
Grating altitude
1°
Grating azimuth
4.8°
Distances S1, S2, and S4
50 mm
S3
378 mm
Total size of the compressor
≈1.4 mFigure 7
Group delay introduced by the XUV attosecond compressor with parameters of Table3.Note that the double-grating configuration presented in the previous paragraph would give the same GDD for a G1-G2 distance of 28 mm, which is not practically feasible.


## 6. Conclusions

The use of grazing-incidence gratings to realize XUV compressors has been discussed for applications to HHs and FELs. Two different grating geometries, OPM and CDM, have been compared to show the peculiarities of both of them. The use of compressors may decrease the time duration of the pulse close to the Fourier limit and increase its peak intensity to offer full exploitation of femtosecond and subfemtosecond regime for ultrafast spectroscopy.



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