2. PHA design and image reconstruction

The MMI consists of a hexagonally allocated PHA, a MLM and a MCP (Figure 1(a)), which provide 2D spatial resolution (${\rm\Delta}x\approx 11~{\rm\mu}\text{m}$), spectral resolution ($E/{\rm\Delta}E\approx 150$) and time resolution (${\rm\Delta}t\approx 100~\text{ps}$), respectively. The given resolutions are typical values for our applications^{[Reference Nagayama, Mancini, Florido, Mayes, Tommasini, Koch, Delettrez, Regan and Smalyuk10–Reference Nagayama, Mancini, Florido, Mayes, Tommasini, Koch, Delettrez, Regan and Smalyuk12]}. The spatial resolution depends on pinhole size and object–PHA–detector distances. The spectral and temporal resolutions are determined by the specifications of the MLM and MCP, respectively. A key component for successful MMI data measurement is the PHA design, and it has to be optimized for every application. Here, we discuss necessary considerations to optimize the PHA design through the application to Ar-doped ICF experiments.

Figure 1.

(a) The MMI consists of a PHA, a MLM and a MCP. The signal collected through a pinhole is proportional to the source-to-pinhole solid angle, ${\rm\Omega}={\it\pi}D^{2}/4p^{2}$. (b) The spatial resolution is determined by the object–pinhole–detector distances. (c) The magnification is determined by the object–pinhole distance, $p$, and the object–detector distance, $L$. The optimal pinhole separation, $l$, is determined so that images of size $\mathit{FM}$ do not overlap.

Pinhole size is determined based on the expected signal levels on the detector and the desired spatial resolution. The expected signal level on the detector depends on the object radiation power, the pinhole size, the object–PHA–detector distances and the detector sensitivity. For example, when the ICF implosion core is diagnosed with signals from Ar tracer, the core radiation power needs to be estimated with a spectral model at $T_{e}$ and $n_{e}$ predicted from the hydrodynamic simulations. If the estimated signals seem too low for a given configuration, one can increase the signals on the detector by increasing the object radiation power, increasing the object solid angle to the pinhole or improving the detector sensitivity. In our application, we field the instrument with a fixed PHA–detector distance as close as possible to the object and use the x-ray framing camera available at OMEGA. This leaves us only two options for increasing the signal levels on the detector: (1) increasing the object solid angle to the pinhole by increasing the pinhole size (the blow-up in Figure 1(a)) or (2) increasing the object radiation power by increasing the Ar tracer amount. One must consider the trade-off due to these options. For example, as the pinhole size is increased, the spatial resolution deteriorates because the signals observed at every point on the detector are integrated over a larger area on the source, as illustrated in Figure 1(b). When the Ar fraction is increased, one has to consider its effects on the implosion hydrodynamics^{[Reference MacFarlane, Golovkin, Mancini, Welser, Bailey, Koch, Mehlhorn, Rochau, Wang and Woodruff13]}. The pinhole size needs to be optimized taking these details into account.

The pinholes are arranged in a hexagonal pattern because this allows the object images to fill the detector plane most efficiently. The pinhole separation, $l$, is optimized based on the target image size, $\mathit{FM}$, where $F$ is the object size and $M$ is the magnification (Figure 1(c)). The distance between adjacent image centers is $l(M+1)$, which defines the maximum image size allowed for a given $l$ and $M$. If the image size is larger than $l(M+1)$, the images start to overlap, which complicates the interpretation. Thus, $l$ is determined such that $\mathit{FM}\lesssim l(M+1)$.

Once the maximum allowed image size is defined, the appropriate tilt is determined based on the MCP strip width, $K$, so that the detector samples object spatial information most efficiently at each photon energy. In other words, the images aligned vertically across the MCP width should have a gradual horizontal shift so that, for every photon energy, they provide spatial information on a slightly different point in object space. The ideal tilt is computed by

(1)$$\begin{eqnarray}{\it\theta}=\arctan \left(\frac{\sqrt{4/3}l(M+1)}{K}\right),\end{eqnarray}$$

as discussed in Ref. [Reference Tommasini, Koch, Izumi, Welser, Mancini, Delettrez, Regan and Smalyuk6].

An example of MMI data with an appropriate PHA tilt is shown in Figure 2(a). The object-to-pinhole distance, $p$, is ${\approx}3~\text{cm}$; the object-to-detector distance, $L$, is ${\approx}28.5~\text{cm}$ ($M\approx 8.5$). The MLM consists of 300 bilayers of W and BC, where the periodic thickness is 15 Å. Hexagonally arranged implosion core images are shown with a horizontal spectral axis. Due to K-shell line emission from Ar in the implosion core, images appearing around the photon energies associated with Ar Ly-${\it\alpha}$ (${\sim}3320$ eV), He-${\it\beta}$ (${\sim}3686$ eV) and Ly-${\it\beta}$ (${\sim}3935$ eV) are brighter. The designed tilt angle based on Equation (1) was $8.95^{\circ }$ with respect to the vertical, and the data show $(8.66\pm 0.10)^{\circ }$. As designed, this image array efficiently provides spatial information at each photon energy. For example, Figure 2(b) shows an image reconstructed from one pixel column of the MMI data at the He-${\it\beta}$ line center (i.e., the orange line). Each pixel along this column is relocated into a single common image plane based on the position relative to its nearest image centers^{[Reference Nagayama, Mancini, Florido, Tommasini, Koch, Delettrez, Regan and Smalyuk9]}. This single column provides strips of object spatial information that are uniformly separated over the image plane.

Figure 2.

(a) MMI data with an appropriate PHA tilt. The dashed line is the reference vertical line (i.e., ${\it\theta}=0^{\circ }$). The red and green solid lines show the extracted ($8.66^{\circ }$) and optimal ($8.95^{\circ }$) PHA tilt angles. (b) Monochromatic image reconstructed from a single pixel column at the He-${\it\beta}$ line center. (c) Narrow-band He-${\it\beta}$ image reconstructed over its linewidth (i.e., ${\sim}60$ eV).

An example of MMI data with an inappropriate PHA tilt is shown in Figure 3(a). The MMI specification is identical to that of the previous example. While we used the same PHA design, it was misaligned in the MMI nose tip, which resulted in a significantly different tilt angle, $(5.22\pm 0.02)^{\circ }$, in the data. The one pixel column image provides strips that are not uniformly distributed across the image, and thus the spatial sampling is biased (Figure 3(b)).

Figure 3.

(a) MMI data with an inappropriate PHA tilt. The dashed line is the reference vertical line (i.e., ${\it\theta}=0^{\circ }$). The red and green solid lines show the extracted ($5.22^{\circ }$) and optimal ($8.95^{\circ }$) PHA tilt angles. (b) Monochromatic image reconstructed from a single pixel column at the He-${\it\beta}$ line center. (c) Narrow-band He-${\it\beta}$ image reconstructed over its linewidth (i.e., ${\sim}60$ eV).

For both cases, one pixel column does not reconstruct the whole image, and adjacent pixel columns are needed which are at slightly different photon energies. Thus, the largest strip separation in the one pixel column image, $w$, defines the minimum width required to reconstruct the whole image, which we call the reconstruction width or sampling width. On one hand, the appropriate case shown in Figure 2 has $w=8$ pixels. Thus, eight pixel columns are needed to fully reconstruct the image, which correspond to 15 eV for this particular dataset based on the extracted spectral axis^{[Reference Nagayama, Mancini, Florido, Tommasini, Koch, Delettrez, Regan and Smalyuk9]}. Thus, the whole image can be reconstructed with a much narrower width than the spectral linewidth, where its FWHM is approximately 60 eV. By extending the narrow bandwidth to its FWHM, one can improve the signal-to-noise ratio (S/N) and form a reliable He-${\it\beta}$ line image (Figure 2(c)). On the other hand, the inappropriate case shown in Figure 3 has $w=20$ pixels, which corresponds to 44 eV. This is still narrower than the FWHM of the He-${\it\beta}$ line. However, this means that the last pixel column added to form the whole image comes from $44/2=22$ eV away from the line center. The overall intensity from this pixel column is systematically lower than that of the line center, and the spatial information at the center of the gap, $w$, has to rely significantly on the intensity correction discussed in Equations (3) and (4) of Ref. [Reference Nagayama, Mancini, Florido, Tommasini, Koch, Delettrez, Regan and Smalyuk9]. Moreover, even after reconstructing the full image, the S/N of the large gap region is still very low. Accordingly, the reconstructed image structure becomes less reliable around the large gap region.

To summarize, the PHA needs to be tilted at an appropriate angle to achieve efficient spatial sampling and minimize the reconstruction width, $w$. Reliable MMI diagnostics further require that the spectral width corresponding to $w$ is much narrower than the FWHM of the diagnostic lines such as He-${\it\beta}$ and Ly-${\it\beta}$. Those linewidths need to be estimated from conditions predicted with hydrodynamic simulations and taken into account to optimize the PHA design. We note that, as long as the Stark linewidth is broader than the sampling width, the diagnostics should work. However, practically speaking, a Stark width of 60 eV could still have spectral structures that change rapidly within the sampling width (e.g., structures around the center of the line). Thus, for reliable image reconstruction, ${\rm\Delta}E_{\mathit{Stark}}>{\rm\Delta}E_{\mathit{instrum}}>w$ is ideal, where ${\rm\Delta}E_{\mathit{Stark}}$ and ${\rm\Delta}E_{\mathit{instrum}}$ are the Stark width of the line and the spectral resolution of the instrument, respectively.

The extracted one pixel column image such as Figures 2(b) and 3(b) gives some idea of how reliable the recorded MMI data are. However, it does not directly answer how critical it is to satisfy this criterion. To better illustrate this point, we perform a synthetic investigation in Section 4 using the spectral model discussed in Section 3.

3. Spectral model

The spectral model used in this paper computes emergent spectra at every point on the image plane, $I_{{\it\nu}}(x,y)$, and then $I_{{\it\nu}}(x,y)$ is used to compute both synthetic MMI data and expected images. The case of investigation is an OMEGA direct-drive Ar-doped $\text{D}_{2}$-filled ICF implosion because it has been one of our main applications of the MMI diagnostics^{[Reference Nagayama, Mancini, Florido, Mayes, Tommasini, Koch, Delettrez, Regan and Smalyuk10–Reference Nagayama, Mancini, Florido, Mayes, Tommasini, Koch, Delettrez, Regan and Smalyuk12]}. The ICF implosion core is the object for the synthetic data, and we define it as a sphere of uniform $T_{e}$ and $n_{e}$ to simplify the interpretation of the synthetic investigation. The capsule is initially filled with 20 atm of $\text{D}_{2}$ with 0.18% atomic concentration of Ar. The Ar photon-energy-dependent emissivity and opacity are computed for given $T_{e}$ and $n_{e}$, and emergent spectra are computed by solving the radiation transport along each chord parallel to the line of sight^{[Reference Nagayama, Mancini, Florido, Mayes, Tommasini, Koch, Delettrez, Regan and Smalyuk12]}.

To compute the Ar emissivity, ${\it\epsilon}_{{\it\nu}}$, and opacity, ${\it\kappa}_{{\it\nu}}$, necessary atomic data are computed with the Flexible Atomic Code (FAC)^{[Reference Gu14]}, and Ar level populations are solved for the given $T_{e}$ and $n_{e}$ with a collisional–radiative model, ABAKO^{[Reference Florido, Rodríguez, Gil, Rubiano, Martel, Mínguez and Mancini15]}. We used the Stewart and Pyatt model^{[Reference Stewart and Pyatt16]} for continuum lowering effects and the escape factor approximation to account for radiation transport effects on the populations^{[Reference Mancini, Joyce and Hooper17]}. The spectral emissivity and opacity are computed from the calculated populations including detailed Stark line profiles computed by MERL^{[Reference Mancini, Kilcrease, Woltz and Hooper18]}.

Emergent spectra are computed along each chord on the image plane by numerically integrating the radiation transport equation assuming parallel ray tracing^{[Reference Mihalas19]}:

(2)$$\begin{eqnarray}\frac{dI_{{\it\nu}}(x,y)}{dz}={\it\epsilon}_{{\it\nu}}(x,y,z)-I_{{\it\nu}}(x,y){\it\kappa}_{{\it\nu}}(x,y,z)\end{eqnarray}$$

where the $z$ axis is parallel to the line of sight, the $x{-}y$ plane is parallel to the image plane of the detector, $I_{{\it\nu}}(x,y)$ is the emergent intensity at $(x,y)$ on the source ($\text{erg}/\text{s}/\text{cm}^{2}/\text{sr}/\text{eV}$) and ${\it\tau}_{{\it\nu}}$ is the optical depth from point $z$ in the object to the observer side of the object surface. The quantities ${\it\epsilon}_{{\it\nu}}(x,y,z)$ and ${\it\kappa}_{{\it\nu}}(x,y,z)$ are determined with ABAKO at the given $T_{e}$ and $n_{e}$ if $(x,y,z)$ is inside the object and zero if it is outside the object.

Potential inaccuracy in the calculated emissivity and opacity does not affect the conclusions derived from the synthetic investigations performed in this paper because $I_{{\it\nu}}(x,y)$ is used to calculate both the synthetic MMI data and the expected images. What we pursue is the discrepancies produced due to the discrete nature of MMI data and the details of data processing.

The expected narrow-band images are computed by integrating $I_{{\it\nu}}(x,y)$ over any given spectral range as

(3)$$\begin{eqnarray}I_{{\rm\Delta}{\it\nu}}(x,y)=\int _{{\rm\Delta}{\it\nu}}I_{{\it\nu}}(x,y)\,d{\it\nu},\end{eqnarray}$$

where ${\rm\Delta}{\it\nu}$ is the bandwidth of interest.

Synthetic MMI data are computed from the emergent spectra, $I_{{\it\nu}}(x,y)$, assuming parallel ray tracing. When MMI data are processed as discussed in Ref. [Reference Nagayama, Mancini, Florido, Tommasini, Koch, Delettrez, Regan and Smalyuk9], each MMI pixel, $(x_{mmi},y_{mmi})$, uniquely defines its photon energy, $h{\it\nu}$, and its position on the image plane, $(x,y)$. Thus, using this pixel information provided from actual MMI data, one can compute each pixel of synthetic MMI data as $I_{{\it\nu}}(x,y){\rm\Delta}h{\it\nu}{\rm\Delta}A$ by converting every pixel $(x_{mmi},y_{mmi})$ into $(x,y)$ and $h{\it\nu}$. Here, ${\rm\Delta}h{\it\nu}$ and ${\rm\Delta}A$ are the finite spectral width and the finite area at the pixel $(x_{mmi},y_{mmi})$.

One concern is the validity of parallel ray tracing for the synthetic MMI data modeling. While photons going through pinholes are not precisely parallel, the parallel ray assumption is still valid for our applications. Based on the object size of $100~{\rm\mu}\text{m}$ and object–PHA distance of 3 cm, rays through a single pinhole deviate from parallel by less than ${\it\theta}<\arctan \;(100~{\rm\mu}\text{m}/3~\text{cm})=0.2^{\circ }$. This maximum deviation in angle can be interpreted in terms of the maximum deviation on the image plane as $(100~{\rm\mu}\text{m})\times \sin (0.2^{\circ })<0.3~{\rm\mu}\text{m}$, which is much smaller than the typical spatial resolution of the image, ${\rm\Delta}x\approx 11~{\rm\mu}\text{m}$.

Photons through different pinholes have a larger deviation from the parallel rays. In typical data, pinholes used to project images on a single MCP are separated by a maximum of ${\sim}2~\text{mm}$. Then, photons going through those pinholes could deviate from parallel by up to ${\it\theta}<\arctan \;(2~\text{mm}/3~\text{cm})=3.8^{\circ }$. Along the maximum chord length in the object, this results in a chord deviation of $(100~{\rm\mu}\text{m})\times \sin (3.8^{\circ })=6.6~{\rm\mu}\text{m}$ on the image plane. This deviation is still less than the spatial resolution of the instrument. Furthermore, this deviation is an upper bound because usually only a smaller portion of the MMI data is used in the analysis. For example, for He-${\it\beta}$ and Ly-${\it\beta}$ analysis, the most distant pinholes used in the analysis are separated by less than 1 mm, and thus the deviation on the image plane is less than $3.3~{\rm\mu}\text{m}$. Hence, parallel ray tracing is a good approximation to interpret the photon paths through the object for many MMI applications, including ours.

4. Impact of the criterion on MMI spatial sampling

The quality of the MMI data depends on whether or not $w$ is significantly narrower than the spectral linewidth. In this section, we synthetically investigate the impact of the criterion on the reliability of the extracted spatial information. This can be demonstrated by reconstructing images from the synthetic MMI data that do and do not satisfy the criterion and comparing them with the expected images.

First, MMI data with an appropriate PHA are created using a uniform sphere of $100~{\rm\mu}\text{m}$ diameter, $T_{e}=1500$ and $n_{e}=1.5\times 10^{24}~\text{cm}^{-3}$. The PHA pattern and the photon-energy axis are those from the appropriate data shown in Figure 2(a). The conditions are the values representative of Figure 2(a) based on the analysis of its space-integrated spectra. Thus, as already discussed in Section 2, $w=$ 8 pixels (i.e., ${\sim}15$ eV) and the FWHMs of the He-${\it\beta}$ and Ly-${\it\beta}$ lines are roughly 60 eV, which satisfies $w\ll$ FWHM.

Figure 4(a) shows the resultant synthetic MMI data. Because $w$ is much narrower than the FWHMs of the spectral lines, the reconstructed He-${\it\beta}$ and Ly-${\it\beta}$ images shown in Figure 4(b) agree very well with the expected images shown in Figure 4(c).

Figure 4.

(a) Synthetic MMI data with an appropriate PHA tilt and with the minimum reconstruction width, $w$, much narrower than the spectral linewidth. (b) Ar He-${\it\beta}$ and Ly-${\it\beta}$ images reconstructed from the synthetic MMI data. (c) Expected Ar He-${\it\beta}$ and Ly-${\it\beta}$ images.

We note that there are small vertical structures introduced in the Ly-${\it\beta}$ image in Figure 4(b). These structures come from the discrete nature of the MMI data. The MMI data have only a finite number of images, each of which spans slightly different photon-energy ranges. The processing tool combines the finite information from the different pinhole images together to approximate narrow-band images, and small discrepancies are unavoidable. The level of discrepancies can be quantified by series of synthetic investigations, which are beyond the scope of the paper and will be discussed elsewhere.

Next, inappropriate MMI data are synthetically created using a uniform sphere of $100~{\rm\mu}\text{m}$ diameter, $T_{e}=1000~\text{eV}$ and $n_{e}=3\times 10^{23}~\text{cm}^{-3}$. The PHA pattern and the photon-energy axis are those from the actual inappropriate MMI data shown in Figure 3(a). Thus, the minimum width required to reconstruct the image is $w=20$ pixels (i.e., 44 eV), as discussed in Section 2. One reason why Figure 3(c) still shows a reasonable image is that $w$ is still narrower than the linewidth (${\sim}60$ eV), while it is not significantly narrower. Thus, to show an extreme case, $n_{e}$ is purposely lowered so that $w$ becomes even broader than its Stark linewidth (${\sim}16{-}19$ eV).

Figure 5(a) displays the resultant synthetic MMI data, which show much narrower spectral features compared with Figure 3(a). Figure 5(b) shows the reconstructed Ar He-${\it\beta}$ and Ly-${\it\beta}$ images. Compared with the expected images (Figure 5(c)), the reconstructed images have a lot of artificial structure originating from the discrete nature of the MMI data, which is amplified due to $w>$ FWHM.

Figure 5.

(a) Synthetic MMI data with an inappropriate PHA tilt and with the minimum reconstruction width, $w$, broader than the spectral linewidth. (b) Ar He-${\it\beta}$ and Ly-${\it\beta}$ images reconstructed from the synthetic MMI data. (c) Expected Ar He-${\it\beta}$ and Ly-${\it\beta}$ images.