A HAWAII-2RG infrared camera operated under fast readout mode for solar polarimetry

Polarimetry is a crucial method to investigate solar magnetic fields. From the viewpoint of space weather, the magnetic field in solar filaments, which occasionally erupt and develop into interplanetary flux ropes, is of particular interest. To measure the magnetic field in filaments, high-performance polarimetry in the near-infrared wavelengths employing a high-speed, large-format detector is required; however, so far, this has been difficult to be realized. Thus, the development of a new infrared camera for advanced solar polarimetry has been started, employing a HAWAII-2RG (H2RG) array by Teledyne, which has 2048×2048\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$2048~\times 2048$$\end{document} pixels, focusing on the wavelengths in the range of 1.0-1.6μm\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$1.0\;{-}\;1.6\;~\mu {\text{m}} $$\end{document}. We solved the problem of the difficult operation of the H2RGs under “fast readout mode” synchronizing with high-speed polarization modulation by introducing a “MACIE” (Markury ASIC Control and Interface Electronics) interface card and new assembly codes provided by Markury Scientific. This enables polarization measurements with high frame-rates, such as 29–117 frames per seconds, using a H2RG. We conducted experimental observations of the Sun and confirmed the high polarimetric performance of the camera.


Introduction
Solar polarimetry is indispensable to determine solar magnetic fields governing a variety of phenomena in the solar atmosphere. Eruptive events occurring on the solar surface occasionally result in a harmful effect to the Earth, and thus, the investigation of such phenomena and the magnetic field information on the Sun is crucially important. From the viewpoint of space weather, to obtain accurate magnetic field information, the realization of advanced solar polarimetry, employing a highspeed, large-format detector covering near-infrared wavelengths is required.
Near-infrared polarimetry provides a new insight into the solar magnetic field study. Therefore, many attempts have been performed particularly in the past two decades with such instruments as the Tenerife Infrared Polarimeter (TIP; Mártinez Pillet et al. 1999) and TIP II (Collados et al. 2007) at the German Vacuum Tower Telescope of the Observatorio del Teide, the GREGOR Infrared Spectrograph (Collados et al. 2012) at the GREGOR telescope also of the Observatorio del Teide, and the Facility Infrared Spectropolarimeter (Jaeggli et al. 2010) installed at the Dunn Solar Telescope at Sacramento Peak.
One of the reasons of the advantage of the near-infrared observations is that there are a number of rather informative absorption lines in the near-infrared range. One of these is the He I 1083.0-nm line, which is formed in the chromosphere (e.g., Lagg 2007;Penn 2014). In addition to the information on the chromosphere, the He I 1083.0-nm line provides information on the magnetic field in solar filaments (e.g., Hanaoka and Sakurai 2017). Filaments occasionally erupt and become part of coronal mass ejections (CMEs), and the magnetic field in the filaments is the source of the magnetic field in the CME interplanetary flux ropes. From the viewpoint of space weather, the information on the magnetic field in the flux ropes arriving at the Earth is crucially important, because the orientation of the magnetic field in the flux ropes affects the severity of the resulting geomagnetic Open Access *Correspondence: yoichiro.hanaoka@nao.ac.jp 1 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Japan Full list of author information is available at the end of the article storms. To determine the magnetic field orientation in the interplanetary flux ropes in advance, the information on the magnetic field in the filaments before their eruption is an important factor. So far, pieces of indirect information, such as fine structures in filaments seen in H α , have been used to estimate the magnetic field in filaments; however, the direct measurements of the magnetic field in filaments using the He I 1083.0-nm line provide essential contributions to the prediction of the magnetic field of interplanetary flux ropes.
Another advantage of the He I 1083.0-nm line is that a close photospheric line, Si I 1082.7 nm, can be detected simultaneously with it in spectroscopic observations. Observations using these two lines provide both photospheric and chromospheric magnetic field information. In addition, the Fe I 1564.8-nm line is also an important target in near-infrared wavelengths (see Hall 1975 andalso Penn 2014). Although it is a photospheric line, it shows a particularly large Zeeman splitting, which provides us a different method to investigate the magnetic field from other lines.
Besides the selection of target absorption lines, the performance of detectors is also important to realize advanced solar polarimetry. High speed is one of the key specifications required for detectors, because it contributes to the reduction of noise level. The polarization of the solar light is generally weak; thus, the typical required noise level is as low as 10 −3 -10 −4 (see e.g., Lagg et al. 2017). This results in the requirement of rapid polarization modulation. The polarization modulation produces a variation in the light intensity reaching the detector depending on the polarization state of the incident light. In solar polarimetry with ground-based telescopes, the image distortion due to the seeing effect during the polarization modulation produces unwanted variation in the light intensity. To reduce this seeing-induced error, fast polarization modulation and high frame rate are required. Their combination enables complete image acquisition before the image distortion becomes substantially large. The noise level 10 −3 -10 −4 indicates that photoelectrons at least in the range of 10 6 -10 8 e − need to be accumulated. To realize this, many images need to be integrated; however, due to the extremely high brightness of the Sun, this can be performed within a short time with a high frame rate. The shortness of the data acquisition time enables a high-cadence observation, which is necessary to acquire data before the structure of the observing targets changes substantially.
In addition, large-format detectors are required to realize efficient data acquisition. Small-format cameras have already been successfully used for solar polarimetry. For example, the solar group of the National Astronomical Observatory of Japan (NAOJ) has been operating regular full-disk, full-Stokes polarimetry observations of the Sun at wavelengths including He I 1083.0 nm and Fe I 1564.8 nm with XEVA cameras by Xenics, equipped with a 640 × 480-pixel InGaAs detector (Sakurai et al. 2018). The instruments used at the Observatorio del Teide and Sacramento Peak mentioned above also use detectors with up to 1024 × 1024 pixels. However, the efficiency of observations with small-format cameras is not sufficiently high to track the evolution of the magnetic field.
Therefore, for solar polarimetry, a high-speed, largeformat infrared detector is required. The HAWAII-xRG focal plane arrays by Teledyne Imaging Sensors are largeformat, low-noise HgCdTe detectors for near-infrared wavelengths, and they can be operated with high frame rates. Among them, the HAWAII-2RG (H2RG) detector (Blank et al. 2012) has been used most commonly in astronomical observations. A H2RG has 2048 × 2048 pixels with a pixel size of 18 × 18 µm , and its full-well capacity is ∼100, 000 e − . In night-time astronomical observations, it is used in the slow readout mode (readout speed of 100 kHz) where the readout noise is as low as ∼ 15 e − . Nevertheless, a fast readout mode (5 MHz) is also available, and with this mode, the frame rate can be as high as 33 frames per second (fps), with 32-channel simultaneous readouts. In the fast readout mode, the noise level increases to a certain extent ( ∼ 70 e − ) and the depth of analog-to-digital (A/D) conversion is lowered to 12 bits from 16 bits in the slow readout mode. Nevertheless, this high frame rate is suitable to observe photon-rich targets such as the Sun. Therefore, the H2RG is expected to meet the requirements of a high-speed, large-format infrared detector for solar polarimetry.
However, it has been difficult to employ a H2RG for solar polarimetry. For the efficient and precise solar polarimetry, many images should be taken continuously synchronizing with the polarization modulation. However, a H2RG and its peripheral electronics were not necessarily designed for such an operation. Even in the fast readout mode, they are basically optimized for a single image acquisition, and it is difficult to carry out stable, uninterrupted continuous image acquisitions. Furthermore, there is no function to synchronize the exposure timing and an external device like a polarization modulator very precisely. On the other hand, some small-format cameras have a function to be synchronized with external signals under the stable continuous image-acquisition mode, and it is the reason why they have been used for solar polarimetry.
Our aim was to develop a mechanism for the synchronization, to realize a large-format, low-noise infrared camera for advanced solar polarimetry using a H2RG detector. To realize the synchronization in the fast readout mode of the H2RG, in cooperation with Kyoto University, we introduced a "MACIE" (Markury ASIC Control and Interface Electronics) card (Loose et al. 2018) manufactured by Markury Scientific. Finally, we realized the synchronization of the polarization modulation and image acquisition with a H2RG under the fast readout mode, as briefly reported by Hanaoka et al. (2019). We adopted a H2RG device with the cut-off wavelength of 1.7 µm , because we focused on the wavelengths in the range of 1.0−1.6 µm . In principle, our development had an experimental purpose; therefore, we chose an engineering model of H2RG (serial number #17087). Nevertheless, such a development can realize efficient polarimetry with future advanced telescopes.
We present an overview of the camera system and an example of experimental polarimetric observations of the Sun in the following two sections and summarize our results in the conclusion section.

Overview of the system and the principle of the synchronous operation
The configuration of the camera system is shown in Fig. 1. We adopted a rotating waveplate driven by a stepper motor for the polarization modulator. The incident light goes through the rotating waveplate and an "analyzer" (a linear polarizer) and reaches the H2RG detector. As described before, in polarimetry the synchronization between the polarization modulation and image acquisition is crucially important.
We employed a MACIE card for the interface between a "SIDECAR" (System for Image Digitization, Enhancement, Control And Retrieval; Chen et al. 2014) application-specific integrated circuit (ASIC) focal plane electronics (which outputs A/D-converted signals) and a personal computer (PC). Typically a "SAM" (SIDECAR Acquisition Module) card by Teledyne (Blank et al. 2012) is used for the interface; however, it is difficult to synchronize the polarization modulation and image acquisition using a SAM card. Nevertheless, the MACIE card has a function to send and receive timing signals. The synchronization with the polarization modulator becomes possible using these signals. New assembly codes (firmwares) developed by Markury Scientific have been installed into the SIDECAR to realize the synchronizing operation.
The synchronization is managed by a timing controller. The timing controller functions are implemented by a Complex Programmable Logic Device (CPLD), which receives the "row clock" (line sync signal) from the MACIE card and provides motor drive pulses to the polarization modulator. It also produces trigger signals to start the image readouts synchronizing with the rotation of the waveplate and sends the signals to the MACIE card. Figure 2 shows the timing relations among various signals and data readouts in detail. Using the 32-channel readout in fast readout mode, a H2RG and a SIDECAR run under the row clock of ∼ 70 kHz . One cycle of the row clock corresponds to the processing time of each row of the detector. Specifically, a H2RG/SIDECAR processes approximately 70,000 rows in a second in fast readout mode. The row clock is an internal signal produced by the SIDECAR; therefore, it can be used as the base clock to control the overall timing of the system.
When the MACIE card receives an external trigger signal, it starts the data readout of a frame by the SIDECAR. To drain out the photoelectrons, a reset of the detector is implemented at the row clock after the subsequent one of the readout at each row. An exposure starts after the reset signal and ends at the readout. The exposure needs to be longer than the time needed to read the data of all the rows, i.e., 2048 row clocks (and a margin) for a full frame. As the dead time between a "read" and a "reset" is only two row clocks, it is virtually negligible (the duty ratio, the ratio of the exposure time to the exposure interval, is > 99% ). Hence, this is a rather effective system, where most of the photons coming into the detector are used to produce images.
Nevertheless, such a "reset-read" operation has some shortcomings. The noise level in the "reset-read" operation is generally higher than that in the "reset-readread" operation (correlated double sampling, CDS), and therefore, the CDS is commonly used in night-time astronomical observations. In fast readout mode, the CDS also lowers the noise level to a certain extent; however, it is not very effective (Blank et al. 2012). Nevertheless, the CDS lowers the frame rate and increases the dead time. Another shortcoming is the residual image or persistency due to the residual photoelectrons, which  Fig. 1 Diagram of the camera system. The incident light travels through a polarization modulator and an analyzer. It is detected by a H2RG, and analog-to-digital conversion is carried out by a SIDECAR. They are installed in a cryogenic dewar. The digitized data are transferred from the SIDECAR to a PC relayed by a MACIE card via CameraLink. A timing controller receives the row clock from the MACIE card and controls the synchronous actions among polarization modulation, image acquisition, and data transfer remain after the reset operation (e.g., Mosby et al. 2016), and which are also among the sources of noise on images.
It is known that a single reset operation cannot completely drain out the photoelectrons accumulated during the exposure. Repeated reset operations are effective to reduce the residual electrons, and the CDS is also useful. However, these operations result in a reduction of the frame rate. Therefore, there is a trade-off relation between the noise and the frame rate. The effectiveness of the introduction of the CDS and/or multiple resets will be analyzed in future studies. The polarization can be fully expressed by four Stokes parameters (I, Q, U, and V), and to determine them, typically 16 images are taken during one rotation of the waveplate of a polarization modulator. In our case, one rotation of the waveplate is completed by 400 drive pulses for the stepper motor, and thus, the frame time to take an image corresponds to 25 drive pulses. In the case of a full-frame image (2048 rows), we typically set the frame time to be 2400 row clocks including a margin. It means that the exposure time starting at a "reset" and ending at a "read" (see Fig. 2) is 2398 ( = 2400 − 2 clocks of dead time) row clocks. The timing controller divides 2400 row clocks to 25 drive pulses in this case.
The rotating waveplate unit is equipped with an origin sensor. The waveplate hits the origin sensor once in  Fig. 2 Timing chart of the synchronous system including the timing controller, the polarization modulator, and the SIDECAR/MACIE with the H2RG every rotation, and the timing controller receives the origin signal. Then, the timing controller starts to send out the external trigger signals to start the image readout by the H2RG/SIDECAR every 25 drive pulses. The actual number of drive pulses between two origin signals, which needs to be 400, is constantly monitored to detect any step-outs of the motor. In this manner, the external trigger signals are issued at the same phase angles in every rotation, and thus realizing the synchronization. The data acquired by the MACIE card are transferred to the PC. The PC receives the origin signal via the timing controller, and uses it as the trigger to start to record the transferred data.
As mentioned above, we typically set the number of clocks to be 2400 for a full-frame image. The number of row clocks of 2400 per frame corresponds to a frame rate of 29 fps and a waveplate rotation of 1.8 rps. The new assembly codes for the SIDECAR enable vertical windowing. By decreasing the width of the window from 2048, the frame rate increases. For instance, a 1024-row window (1200 row clocks per frame) enables 59 fps with a rotation of 3.7 rps, and a 512-row window (600 row clocks per frame) enables 117 fps with 7.3 rps.
The drive pulse frequency for all rotation speeds mentioned above is higher than the maximum pull-in pulse rate of the stepper motor. Therefore, the motor starts to rotate with low-frequency pulses produced by the timing controller, and then it is accelerated to a target speed such as 1.8 rps for the full-frame readout. After reaching the target speed, the drive clock is gradually switched to that produced from the row clock. Thus, the synchronization between the waveplate rotation and the row clock is established. In this way, using the H2RG, we realized polarimetry with high frame rates such as 29-117 fps.
As shown in Fig. 2, the exposure of each row starts progressively. Such an operation corresponds to the rolling shutter, and each row undergoes different polarization modulations. To demonstrate the synchronization and the progressive readout, Fig. 3 shows measurement results of completely polarized artificial light. The incident polarized light (linear polarizations of Stokes Q/I = 1 and U /I = 1 ) traveled through the rotating waveplate and the analyzer, and the light intensity reaching the detector varied sinusoidally due to the polarization modulation. We set the window of 512 rows ( 2048 × 512 pixels), and the waveplate completed one rotation with 9600 row clocks (600 row clocks × 16 images). The x-axis in Fig. 3 represents one rotation of the waveplate. At row clock 1, row 1 of the first image was read, and at row clock 512, row 512 of the first image was read. At row clocks 601-1112, the second image was read and at row clocks 9001-9512, the last (16th) image was read. In Fig. 3, the measured light intensities averaged every row are plotted at the row clock corresponding to their readout timings. Each segment of the curves (one of which is marked by an orange circle in Fig. 3) is comprised of 511 data points (row 1 contains dummy data) in an image, and as a whole, the measurement results for both Stokes inputs Q/I and U/I show sinusoidal variations as expected. In Fig. 3, the measurement results of 16 continuous rotations are overplotted. All data points of 16 rotations look like to fall on a single curve. The fluctuation of the measured signal during the 16 rotations is about 4 × 10 −4 , even including the possible brightness fluctuation of the light source. This result indicates that the quality of the synchronization of the data readout and the polarization modulation is very high.

Experimental observation and the verification of the performance
To verify the performance of the camera system, experiments for the polarization measurement of the Sun were carried out using the Domeless Solar Telescope (DST; Nakai and Hattori 1984) of the Hida Observatory, Kyoto University in November 2018 and in November 2019.
The camera system and its experimental arrangement are shown in Fig. 4. The H2RG and the SIDECAR were installed in a dewar (manufactured by OptCraft). A cryocooler (a helium Stirling cooler by Twinbird) cooled the H2RG down to − 130 • C to reduce thermal noise. As the frame rate is high and the cut-off wavelength is as short To prevent rapid temperature changes, which can result in a failure of the H2RG, the control input of the cryocooler was gradually increased and decreased by a microcomputer. In addition, aluminum blocks were attached to the back plate of the H2RG to increase the heat capacity of the H2RG unit to compensate for any problem due to the rapid change of the cryocooler temperature. The DST is a vacuum solar telescope with a 60-cm primary mirror. We installed the camera into the vertical spectrograph of the DST as shown in Fig. 4. The solar light from the telescope arrives from above at a slit located at the top of the spectrograph. The incident light travels downward into the spectrograph and the reflected outgoing spectrum exits upwardly. We positioned the dewar containing the H2RG at the exit focal plane of the spectrograph. The length of the spectrograph slit is 5 cm, which corresponds to the field angle of 5 ′ . Therefore, the H2RG, with an area of 37 mm × 37 mm , covers a field of view of 3 ′ .7 along the slit with a spatial sampling of 0 ′′ .11 pixel −1 . The dispersion is 0.039 nm mm −1 ( 0.7 pm pixel −1 ) at 1083.0 nm (using the second order of the dispersion grating) and 0.1 nm mm −1 ( 1.8 pm pixel −1 ) at 1564.8 nm (first order). The polarization modulator is a rotating waveplate with 1/4-retardation at 1.6 µm and with a retardation of approximately 1/3at 1083.0 nm. Although the waveplate could be rotated rapidly (Hanaoka 2012), the rotation rate of the waveplate was set as 1.8 rps to accumulate a sufficient amount photoelectrons during the exposure. As 16 exposures were made during every rotation, the frame rate was ∼ 29 fps as mentioned in the previous section. As an analyzer, a linear polarizer was installed in front of the slit behind the polarization modulator. This polarimeter had a single-beam configuration using only one of the orthogonal linear polarizations.
Using this arrangement, experimental studies with the polarimeter were successfully performed in the He I 1083.0-nm and Fe I 1564.8-nm wavelengths in 2018 and in 2019. These years were in the solar minimum phase, and there were no sunspots or conspicuous filaments in any of these years during our observational periods. Therefore, in this paper, we show a polarimetry result of a weak plage region (known as NOAA 12727) without sunspots using the wavelengths including Si I 1082.7-nm and He I 1083.0-nm lines. Figures 5a, b show an example of the Stokes I spectra and a corresponding Stokes V/I spectrum, respectively. The Si I 1082.7-nm line providing photospheric magnetic field information and the He I 1083.0-nm line providing chromospheric magnetic field information can be found in the spectra. A total of 480 images (16 exposures × 30 rotations) were obtained at one slit position during 17 s. The data were integrated into 8 images corresponding to a cycle of the polarization modulation, and they were converted to a set of images presenting Stokes signals. Even though the data were taken with insufficient light intensity, the noise level of the Stokes signals is as low as 3 × 10 −3 ; because the signal-to-noise ratio is mainly limited by the photon statistics, a lower noise level is expected with a sufficient number of photons. In the Stokes V/I spectrum (Fig. 5b), remarkable Zeeman polarization signals in the Si I 1082.7-nm line and weak Zeeman signals both in the blue (1082.91 nm) and red (1083.03 nm) components of the He I 1083.0-nm line can be seen. We acquired such spectral data at 26 slit positions separated at every 2 ′′ ; as a result, we obtained polarization data of a two-dimensional field of view of 3 ′ .7 × 52 ′′ . Figure 5c shows a Stokes V/I map of Si I 1082.7 nm of this field of view, which represents the photospheric longitudinal magnetic field of the weak plage region. The black and white patterns correspond to a bipolar magnetic polarity distribution (negative and positive polarities, respectively) in the plage region. Figure 5d shows a longitudinal magnetogram obtained by the Helioseismic and Magnetic Imager (HMI; Scherrer et al. 2012) of the Solar Dynamics Observatory (SDO; Pesnell et al. 2012) including the same area. The HMI uses photospheric magnetic field data based on the Fe I 617.3-nm line. It is confirmed that results from the HMI magnetic field map and the Stokes V/I map recorded with the infrared camera are in good agreement.
The result of this experiment confirms the high polarimetric performance of the new infrared camera. Nevertheless, certain problems, such as the degradation of the image quality due to the noise from the cryocooler, have been revealed. This noise is a kind of electromagnetic interferences, which increases in proportion to the output of the cryocooler (the data shown in Fig. 5 were taken while the cryocooler was turned off ). Now we are improving the grounding and the isolation to cope with this noise. After addressing these problems, the camera will be introduced to regular observations.

Conclusions
We successfully constructed a polarimeter system with a H2RG array by Teledyne, which is a large-format, highspeed, near-infrared detector suitable for solar polarimetry. Although it has been difficult to synchronize H2RGs under fast readout mode with external devices, such as a polarization modulator, we solved this problem by introducing a MACIE card and relevant assembly codes provided by Markury Scientific. With this development, advanced solar polarimetry is realized, which will enable the tracking of the evolution of the magnetic field in solar filaments, which occasionally erupt and develop into CMEs.
The synchronous operation of the SIDECAR/H2RG with an external device under fast readout mode can be realized using an existing SIDECAR/H2RG without preparing a new, dedicated camera system. Only the addition of a set of a MACIE card and assembly codes is required.