## 1 Introduction

Spectral phase interferometry for direct electric-field reconstruction (SPIDER)^{[1, 2]} is one of the major methods to measure and retrieve the electric-field information of ultrashort laser pulses. Compared to another major method, frequency-resolved optical gating (FROG)^{[3]}, which iteratively reconstructs light field from the measured two-dimensional spectrograms, SPIDER allows one to retrieve directly the spectral phase from one-dimensional spectrograms and thus supports real-time display in much higher frame rate. Recently, in order to improve the ability of SPIDER to measure the laser pulses with complex fields, considerable attention has been paid to broaden measured spectral range and to improve the spectral resolution. In original version of SPIDER, two ultrashort test pulse replicas are obtained by a Michelson interferometer (MI) which introduces dispersions and affects its application for ultra-broadband pulses. A method called zero-additional phase (ZAP) SPIDER^{[4]}, which uses one fundamental (FH) test pulse instead of two FH test pulse replicas, can avoid dispersive distortion by the unbalanced pulse replicator, and broaden the measuring spectral range of SPIDER to hundreds of nanometers.

Promoting the spectral resolution is much more challenging for SPIDER that bases shear spectral interferometry. One of the causes is that spectral interferometry encodes the differential spectral phase into the interval of interferential fringes, so SPIDER should operate at a high spectral sampling rate typically 5–10 times of the Nyquist limit^{[5]}. Wavelet transform has been suggested as a substitute of Fourier transform for phase retrieval^{[6]}, and proven to increase the detection window and thus the minimum of the required sampling rate by 20%. However, wavelet transform has lower computational efficiency compared to Fourier transform. Moreover, this method is also based on the traditional measurement and limited by the case mentioned above. To realize 100% sampling of differential spectral phase, another dimension is required to resolve the interferential fringes. It can be either space (e.g., SEA-SPIDER^{[5, 7]}) or time (2D-SI SPIDER^{[8, 9]}), however, needs inevitably more complex structures and expensive devices, e.g., imaging spectrograph for SEA-SPIDER, motor-controlled element for 2D-SI SPIDER. Moreover, the recorded 2D data means much longer time required to process than the usual 1D data.

A more important factor that affects the reconstructed resolution is to promote the measured signal-to-noise ratio (SNR). From SPIDER measurement, what we get directly from the interferogram is the differential phase. The spectral phase is recovered by concatenating the differential phase with a spectral interval of
$\unicode[STIX]{x1D6FA}$
, the spectral shear, which usually plays a very important role in the sampling interval or spectral resolution of SPIDER. The choice of
$\unicode[STIX]{x1D6FA}$
depends strongly on the measured SNR. If
$\unicode[STIX]{x1D6FA}$
is chosen too small, the differential phase becomes unmeasurably small due to the detection noise^{[10]}. Moreover, this noise is also accumulated in the course of the phase concatenations. Small
$\unicode[STIX]{x1D6FA}$
leads to large concatenation number, and at the wavelengths far away from the central wavelength, the recovered phase noise becomes very large^{[11]}. For the finite SNR, SPIDERs usually work at relative shear
$\unicode[STIX]{x1D6FA}/\unicode[STIX]{x0394}\unicode[STIX]{x1D714}=4.6\%{-}20\%$
^{[1, 2, 6–8, 10]}, where
$\unicode[STIX]{x0394}\unicode[STIX]{x1D714}$
is the spectral bandwidth. A method called multiple-shearing spectral interferometry combines the phase information obtained with multi-shears^{[11]}. However, this method is relatively complex which involves shear changing in the measurements. It also asks for relatively high consistency of the multi-shear data.

Previously, we have successfully combined two-step phase-shifting (TSPS) into SPIDER^{[12]}, called T-SPIDER here, where two spectral interferograms with
$\unicode[STIX]{x1D70B}$
phase-shifting are recorded to remove experimentally the effect of the dc portion occurring in traditional SPIDER method. T-SPIDER can effectively avoid the disturbances from the time delay (
$\unicode[STIX]{x1D70F}$
) between the test pulse replicas and the temporal filtering in the traditional SPIDER method. What is more, the subtraction of one spectral interferogram from the other, to some extent, is equivalent to a balanced detection where the balanced output is the difference between the two signals recorded by two similar receivers, and thereby can cancel the intensity noise somewhat^{[13]}. However, that design is based on traditional configuration which limits its applying to ultra-broadband pulses. Furthermore, in this setup, TSPS measurement is not available for the reference interferogram without changing any elements.

In this paper, we present a complete TSPS prism-based SPIDER, or CTP-SPIDER, which can implement TSPS in both reference spectra and test spectra. Here, complete TSPS acts as a balanced detection which can not only remove the effect of the dc term of the interferogram, but also reduce measurement noises. To improve the stability of the device and suppress the noise further, some prisms are used to replace some sensitive optical components, especially reflective optics. To improve its performance in ultra-broadband laser pulse, the SPIDER is designed based on ZAP geometry. Our experiments show our SPIDER can work at the spectral shear as low as 0.1 nm (0.2 THz), corresponding to 1.5% of the pulse bandwidth. Our SPIDER is suitable (but not limited) for laser pulses with ultra-broad bandwidth and fine spectral structure.

Figure 1. (a) SPIDER setup; (b) prism-based chirped-pulse-replicas generator (CG); (c) prism-based light path delayer (DL); (d) prism-based beam combiner (BC). BS1-BS3: beam splitters,
$\unicode[STIX]{x1D706}/2$
: half-wave plate, OPM: off-axis parabolic mirror, SP: spectrograph, RP1 and RP2: right-angle prism pair, CR1-CR4: prism-mirrors corner reflectors, PMR1-PMR4: prism-mirrors reflectors, L: lens.

## 3 Results and discussions

For a traditional SPIDER, the recorded spectral interferogram from two SF-pulses with spectral shear
$\unicode[STIX]{x1D6FA}$
and time interval
$\unicode[STIX]{x1D70F}$
can be expressed by

where
$\unicode[STIX]{x1D714}$
is the angular frequency, while
$\unicode[STIX]{x1D703}(\unicode[STIX]{x1D714})=\unicode[STIX]{x1D711}(\unicode[STIX]{x1D714})-\unicode[STIX]{x1D711}(\unicode[STIX]{x1D714}-\unicode[STIX]{x1D6FA})$
is the differential phase between two pulses. To extract
$\unicode[STIX]{x1D703}(\unicode[STIX]{x1D714})$
, some Fourier transforms and temporal filtering are usually applied to
$D(\unicode[STIX]{x1D714})$
. Correspondingly, the temporal function
$\tilde{D}(t)$
, the Fourier transform of
$D(\unicode[STIX]{x1D714})$
, includes three components. One is called dc portion from
$|E(\unicode[STIX]{x1D714}-\unicode[STIX]{x1D6FA})|^{2}+|E(\unicode[STIX]{x1D714})|^{2}$
centered at
$t=0$
while the other two, ac components from
$|E(\unicode[STIX]{x1D714}-\unicode[STIX]{x1D6FA})E(\unicode[STIX]{x1D714})|\cos [\unicode[STIX]{x1D70F}\unicode[STIX]{x1D714}+\unicode[STIX]{x1D703}(\unicode[STIX]{x1D714})]$
, are situated at
$t=\pm \unicode[STIX]{x1D70F}$
, respectively. In traditional SPIDER algorithms, proper
$\unicode[STIX]{x1D70F}$
is required in order that all the three components separate well in time. For a test pulse with narrow bandwidth or with complex spectral structures, larger
$\unicode[STIX]{x1D70F}$
should be required, which leads to higher noise level for less sampling points per fringe.

We have first applied the TSPS method to SPIDER in Ref. [12] (T-SPIDER), where a quarter-wave plate (equivalent to a half-wave plate when the light passes twice) is set in one of the MI arms to induce
$\unicode[STIX]{x1D70B}$
phase-shifting by aligning the polarization respectively along the fast axis or the slow axis of the wave plate at twice. When aligning the polarization along the fast axis, we record an interferogram as expressed by Equation (1), and then by rotating the wave plate by
$90^{\circ }$
, we can record another interferogram with
$\unicode[STIX]{x1D70B}$
phase-shifting expressed by

where
$\unicode[STIX]{x1D6FC}$
expresses a small phase deviation from
$\unicode[STIX]{x1D70B}$
due to the dispersion of the wave plate. Subtracting Equation (2) from (1), we can get TSPS interferogram without the dc term by

Equation (3) shows that, TSPS method still takes effect in eliminating the dc term even though the phase-shifting deviates from
$\unicode[STIX]{x1D70B}$
. When the deviation
$\unicode[STIX]{x1D6FC}\approx 0$
,
$\cos (\unicode[STIX]{x1D6FC}/2)\approx 1$
, the TSPS interferogram has the maximal amplitude, twice the ac portion that in Equation (2). This scheme can be realized conveniently by inducing a wave plate to a traditional SPIDER. However, when the test pulses have few-cycle duration or supercontinuum spectrum, optical dispersion and
$\unicode[STIX]{x1D714}$
-dependent residual phase (
$\unicode[STIX]{x1D6FC}=\unicode[STIX]{x1D6FC}(\unicode[STIX]{x1D714})$
) induced by the wave plate will be too strong to be ignored, which can degrade the recover results. In our scheme, CTP-SPIDER, as shown in Figure 1, we set a half-wave plate for
$\unicode[STIX]{x1D70B}$
phase-shift of one of the chirped pulse replicas. Because only very small part of the chirped spectral components (quasi-monochromatic slice) can interact with the test pulse, no broad bandwidth is required for the half-wave plate in spite that the test pulse has very wide bandwidth.

In SPIDER measurement, to recover
$\unicode[STIX]{x1D711}(\unicode[STIX]{x1D714})$
correctly, it is very important to calibrate
$\unicode[STIX]{x1D714}\unicode[STIX]{x1D70F}$
accurately, or else the residual of
$\unicode[STIX]{x1D714}\unicode[STIX]{x1D70F}$
added to
$\unicode[STIX]{x1D703}(\unicode[STIX]{x1D714})$
will accumulate to a nonnegligible level in the course of the phase concatenations^{[9]}. A significant advantage of CTP-SPIDER is that we can conveniently apply TSPS to record the reference interferograms to calibrate the linear phase
$\unicode[STIX]{x1D714}\unicode[STIX]{x1D70F}$
more accurately, only by setting the time delay of CG to synchronize two chirped pulses (
$\unicode[STIX]{x1D6FA}=0$
) without changing any other optics in the setup. The corresponding spectral phase is
$\unicode[STIX]{x1D714}\unicode[STIX]{x1D70F}+\unicode[STIX]{x1D711}(\unicode[STIX]{x1D714})-\unicode[STIX]{x1D711}(\unicode[STIX]{x1D714}-0)=\unicode[STIX]{x1D714}\unicode[STIX]{x1D70F}$
. In the adjustment procedure, the delay
$\unicode[STIX]{x1D70F}$
never changes, because the moments of two SF pulse replicas generated in the nonlinear crystal are not determined by the two chirped pulses but the test short pulse. For T-SPIDER based on traditional geometry, the parameters
$\unicode[STIX]{x1D6FA}$
and
$\unicode[STIX]{x1D70F}$
are not independent with each other, and the reference interferogram cannot be realized by setting
$\unicode[STIX]{x1D6FA}=0$
. A common calibration method is to record the interferogram between two self-frequency-doubling pulses of the test pulse replicas as mentioned in Ref. [1]. Can we realize TSPS by inducing
$\unicode[STIX]{x1D70B}$
-phase-shifting to one of the FH test pulses? It cannot be done directly, because when the phase of the pulse changes
$\unicode[STIX]{x1D70B}$
, the phase of its frequency-doubling pulse will change
$2\unicode[STIX]{x1D70B}$
. We may set a noncommercial eighth-wave plate instead of the quarter-wave plate to realize TSPS for the reference interferograms, however, which will change the dispersion of the SPIDER. Nevertheless, T-SPIDER is effective compared to traditional SPIDER^{[12]}, because in the reference interferogram, the ac components are usually separated much better with the dc, thereby filtered out more easily than in the shear interferogram. Anyway, CTP-SPIDER can work better with TSPS than T-SPIDER.

For its complete TSPS capacity, we can easily extract the ac term of the spectral data of CTP-SPIDER by choosing the data in the positive (or negative) axis of
$\tilde{D}^{\text{TSPS}}(t)$
, the Fourier transform of
$D^{\text{TSPS}}(\unicode[STIX]{x1D714})$
, without the need of an appropriately selective filtering window required in traditional SPIDER algorithms. Although T-SPIDER does not need window-filtering to the sheared spectra, it should be also applied to the reference spectrum. Figure 2(a) shows the reconstructed spectral phases by CTP-SPIDER (black line) and T-SPIDER using different filtering windows with widths
$t_{\text{win}}=0.5$
, 0.7 and 0.9 ps (red, blue and green lines) for the reference spectrum, for
$\unicode[STIX]{x1D6FA}=0.5$
nm (0.95 THz) and
$\unicode[STIX]{x1D70F}=0.47$
ps. Figure 2(b) is the corresponding temporal shapes and phases. The pulse width is 72 fs. The spectral phases reconstructed by T-SPIDER at
$t_{\text{win}}=0.5$
ps and 0.7 ps agree well with that by CTP-SPIDER. However, when the filtering width increases to 0.9 ps, approximately to twice of
$\unicode[STIX]{x1D70F}$
, an obvious modulation appears in the recovered spectral phase (green line in Figure 2(a)) and its value has great deviation away from the spectrum width range. The corresponding temporal characters also deviate with others. This means that, T-SPIDER is also restricted by the filtering width although its choice is looser than traditional SPIDER.

Figure 2. (a) The reconstructed spectral phases by CTP-SPIDER (black line) and T-SPIDER using different filtering windows with width twin of 0.5, 0.7 and 0.9 ps (red, blue and green lines) for the reference spectrum. (b) The temporal shapes and phases corresponding to (a).

When we decrease the delay
$\unicode[STIX]{x1D70F}$
between the pulse replicas, the interval of the spectral fringes
$1/\unicode[STIX]{x1D70F}$
becomes wider, and the sampling number per fringe increases, which can suppress the effects of uncorrelated noises inversely proportional to the square root of the sampling point number^{[12]}, or reduce the requirement for the resolution of the spectrograph. As mentioned above, CTP-SPIDER can apply TSPS in both test spectra and the reference spectra, relaxing greatly the limitation of
$\unicode[STIX]{x1D70F}$
. Figure 3 shows the recovered temporal intensity and phases for different pulse delays
$\unicode[STIX]{x1D70F}=0.125$
, 0.19, 0.40, 0.47 and 0.69 ps by our CTP-SPIDER. The corresponding shear
$\unicode[STIX]{x1D6FA}=0.5$
nm (0.95 THz) and the measured pulse width is 67 fs. It shows that even when
$\unicode[STIX]{x1D70F}=0.125$
ps, the recovered result also agrees with others at larger delays. The inset of Figure 3 shows the amplitudes of
$\tilde{D}(t)$
(black line) and
$\tilde{D}^{\text{TSPS}}(t)$
(red line) for
$\unicode[STIX]{x1D70F}=0.125$
ps. In the black line in the inset, the dc terms centered at 0 ps overlap greatly with the ac terms centered at
$\pm 0.125$
ps, from which the differential phase is unable to be extracted by both traditional and T-SPIDER. As shown by the red line, we can realize ac terms separation at the absence of the dc by applying TSPS technology, and CTP-SPIDER operates well. T-SPIDER, which is subjected to the overlap between the dc and ac terms for its non-TSPS reference interferogram, also cannot deal with such situation. Moreover, for non-ZAP SPIDER, small
$\unicode[STIX]{x1D70F}$
will lead to small shear
$\unicode[STIX]{x1D6FA}$
, which means that T-SPIDER is not suitable for operating with too small
$\unicode[STIX]{x1D70F}$
.

As we mentioned, a SPIDER should retain its sampling number no less than five times of the Nyquist limit, to guarantee the accuracy of phase reconstruction. When we use SPIDER to measure laser pulses complex spectral phase modulation, the resolution of the spectrograph becomes critical. CTP-SPIDER allows the device to operate in much lower
$\unicode[STIX]{x1D70F}$
to increase the width of the fringe, which reduces the requirement for fine resolution of the spectrograph. We rotate the grating in the compressor of the Ti:sapphire laser amplifier to induce a moderate third-order modulation to the spectral phase, which is measured by CTP-SPIDER for
$\unicode[STIX]{x1D70F}=1$
and 0.3 ps by using a spectrograph with sampling rate of 0.03 nm, as shown by the black lines in Figures 4(a) and 4(b), respectively. To estimate the complexity of the phase, we change the width of filtering window in Fourier domain, and find that
$t_{\text{win}}$
should be no less than 0.3 ps, from which the modulation fineness
$\unicode[STIX]{x0394}\unicode[STIX]{x1D706}_{M}$
of the differential phase
$\unicode[STIX]{x1D703}(\unicode[STIX]{x1D714})$
can be estimated as
${\sim}3$
THz (1.6 nm around 400 nm wavelength). We numerically resample the measured interferogram with different resolutions, and the reconstructed phases are shown by the colored lines in Figures 4(a) and 4(b) for
$\unicode[STIX]{x1D70F}=1$
and 0.3 ps. For
$\unicode[STIX]{x1D70F}=1$
ps, the phase curve agrees well with the original one (black line) when sampling rate
$\unicode[STIX]{x0394}\unicode[STIX]{x1D706}_{s}=0.1$
nm (0.19 THz), and deviates slightly when
$\unicode[STIX]{x0394}\unicode[STIX]{x1D706}_{s}=0.2$
nm (0.38 THz). When
$\unicode[STIX]{x0394}\unicode[STIX]{x1D706}_{s}=0.3$
nm (0.57 THz) the phase curve gives a complete wrong result. This is to say, to measure such laser pulses correctly, the resolution of the employed spectrograph should be no larger than 0.2 nm, corresponding to
$1/8$
of the modulation fineness
$\unicode[STIX]{x0394}\unicode[STIX]{x1D706}_{M}$
. For
$\unicode[STIX]{x1D70F}=0.3$
ps, the maximal available sampling rate will increase to 0.6 nm (1.14 THz) as shown in Figure 4(b), corresponding to
$1/2.7$
of
$\unicode[STIX]{x0394}\unicode[STIX]{x1D706}_{M}$
.

Figure 4. Restore spectral phases by using different sampling resolutions of the interferograms for (a)
$\unicode[STIX]{x1D70F}=1$
ps and (b) 0.3 ps when
$\unicode[STIX]{x1D6FA}=0.5$
nm (0.95 THz).

We usually use a cover over the SPIDER to avoid the perturbation by the airflow. Here, to check the improvement of the SNR, we measure laser pulses by T-SPIDER and CTP-SPIDER without the cover at shear
$\unicode[STIX]{x1D6FA}=0.5$
nm (0.95 THz) and delay
$\unicode[STIX]{x1D70F}=1$
ps, and the recovered phase error is shown by the blue (T-SPIDER) and red lines (CTP-SPIDER) in Figure 5, respectively. By T-SPIDER, as shown by the blue line, the error is retained at a level of 0.1 rad within 23-THz-bandwidth range (
$365{-}388$
THz), where the corresponding spectral intensity is higher than 10% of its peak. For CTP-SPIDER, this range can extend to 31 THz (
$362{-}393$
THz), even at the frequencies where the intensity is lower than 1% of the peak. This means CTP-SPIDER has much better capability to extract the spectral phase from weak spectral domain at the two wings of the pulse. To compare the phase retrieval around the center of the pulse, we calculate the weighted average values
$\unicode[STIX]{x0394}\unicode[STIX]{x1D711}_{\text{avg}}$
of the phase errors within the range of full width at half maximum (FWHM) of the pulse for both SPIDERs:
$\unicode[STIX]{x0394}\unicode[STIX]{x1D711}_{\text{avg}}=\int _{\text{(FWHM)}}\unicode[STIX]{x0394}\unicode[STIX]{x1D711}(\unicode[STIX]{x1D714})I(\unicode[STIX]{x1D714})\,\text{d}\unicode[STIX]{x1D714}/\int _{\text{(FWHM)}}I(\unicode[STIX]{x1D714})\,\text{d}\unicode[STIX]{x1D714}$
, where
$\unicode[STIX]{x0394}\unicode[STIX]{x1D711}(\unicode[STIX]{x1D714})$
is the spectral phase error and
$I(\unicode[STIX]{x1D714})$
is the spectral intensity. The results show that, by using new method, the phase retrieval error
$\unicode[STIX]{x0394}\unicode[STIX]{x1D711}_{\text{avg}}$
improves from 74.2 mrad (T-SPIDER) to 19.3 mrad (CTP-SPIDER) around the center of the pulse, with a factor of
${\sim}4$
. The measured error by CTP-SPIDER is also better than those by previous reports^{[6, 15, 16]}, where the measured phases were presented with similar level to T-SPIDER. We attribute this superior measured SNR to two factors. The first one is our TSPS measurement which can eliminate the effect of the dc term of the signals, like that in balanced detection. For T-SPIDER, the TSPS method is only applied to measuring the sheared interference spectrum but not to the reference spectrum, so it cannot take full advantage of TSPS to suppress the noise. The second factor is our prism-based design, including the prism-based chirped-pulse-replicas generator, light path delayer and BC where the prisms fix directly on brawny metal posts to replace the mirrors. SPIDER is a spectral interferometry, which is very sensitive to the external conditions, such as vibration and temperature. Mirrors installed on adjustable mounts are easily affected by the environmental perturbation. In CTP-SPIDER, the prism-based design can improve the stability as well as the measured SNR of the system.

Figure 5. The measured phase errors by T-SPIDER (blue line) and CTP-SPIDER (red line).

Figure 6. (a) The recovered spectral phases and (b) the temporal characteristics of the laser pulses for different shears from 0.1 to 1.0 nm at
$\unicode[STIX]{x1D70F}=0.43$
ps.

Figure 7. The measured pulses by three kinds of SPIDER in small shear: (a) 0.1 nm, (b) 0.25 nm, and (c) 0.35 nm.

Figure 6(a) shows the recovered spectral phases of the laser pulse by CTP-SPIDER for different shears
$\unicode[STIX]{x1D6FA}$
from 0.1 nm to 1.0 nm (
$0.19{-}1.90$
THz) while Figure 6(b) shows the corresponding temporal shapes and phases of the pulses. The laser pulse is centered at 367.5 THz (796 nm) with a spectral width of 12.7 THz (26.8 nm), and the corresponding Fourier-limited pulse width is 35 fs. The curves coincide well within the range of
$\unicode[STIX]{x1D6FA}$
from 0.25 to 1.0 nm, corresponding to
$\unicode[STIX]{x1D6FA}/\unicode[STIX]{x0394}\unicode[STIX]{x1D714}=3.7\%{-}15\%$
, as away from this range, the curves begin to separate from others due to the accumulated noise. Fortunately, within the spectral width there gathers the majority of the energy of the spectra, so the shapes and the phases of the pulses agree with others well, as shown in Figure 6(b). The measured pulse width is about 69 fs. The curve of
$\unicode[STIX]{x1D6FA}=0.1$
nm (
$\unicode[STIX]{x1D6FA}/\unicode[STIX]{x0394}\unicode[STIX]{x1D714}=1.5\%$
) with pulse width of 74 fs in Figure 6(b) deviates slightly with other curves, which can also reflect the basic feature of the pulse. The shear of 0.1 nm corresponds to three times of the sampling rate or two times of the resolution of the spectrograph we used. Our SPIDER, with a ZAP structure, can operate at
$\unicode[STIX]{x1D6FA}/\unicode[STIX]{x0394}\unicode[STIX]{x1D714}=3.7\%$
(even 1.5%), which reveals that CTP-SPIDER can control the random phase noise very well. We also compare CTP-SPIDER with traditional and T-SPIDER at small shears, as shown in Figures 7(a)–7(c). For
$\unicode[STIX]{x1D6FA}=0.35$
nm, all the curves coincide, which means that the three kinds of SPIDER can operate well under this shear. When we decrease the shear to 0.25 nm, CTP-SPIDER operates well as mentioned above, but the results by traditional and T-SPIDER deviate the curves by CTP-SPIDER as shown in Figure 7. For
$\unicode[STIX]{x1D6FA}=0.1$
nm, this deviation becomes more obvious. This means that our CTP-SPIDER has very low measured noise that can support a very small shear which needs large phase-connected number. In our opinion, this can be attributed to the prism-based structure and the TSPS measurement that eliminate the dc term of the signals, like that in balanced detection.

We use a 6-mm-thick BK7 glass as the Kerr medium to modulate the spectrum; the sheared interferential spectrum is shown in the inset of Figure 8(a) for
$\unicode[STIX]{x1D70F}=0.6$
ps. In the Fourier domain, the dc and ac terms of
$\tilde{D}(t)$
, both with complex structures, overlap partly with each other, as shown by the gray line in Figure 8. Even so, after applying TSPS, the
$+$
dc term can be easily filtered (red line). The recovered spectral and temporal characters are shown in Figures 8(b) and 8(c). The measurement can keep available when
$\unicode[STIX]{x1D70F}$
decreases to 0.4 ps, corresponding to
$N_{f}=44$
, where
$N_{f}$
is the sampling points per interferential fringe. When we use a traditional design, the experiments show that
$\unicode[STIX]{x1D70F}$
should be no less than 1.3 ps, corresponding to
$N_{f}=13$
. This means that CTP-SPIDER with larger
$N_{f}$
can suppress the random noise (
${\sim}N_{f}^{1/2}$
) more effectively, or, it has higher capability to measure the pulses that have complex spectral structures.

Figure 8. Measured results of complex spectra by inducing Kerr effect.