Issue 
A&A
Volume 625, May 2019



Article Number  A38  
Number of page(s)  12  
Section  Astronomical instrumentation  
DOI  https://doi.org/10.1051/00046361/201935043  
Published online  07 May 2019 
Modeling the eAPD SAPHIRA/CRED ONE camera at low flux level
An attempt to count photons in the nearinfrared with the MIRCX interferometric combiner
^{1}
Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
email: cyprien.lanthermann@univgrenoblealpes.fr
^{2}
University of Exeter, School of Physics and Astronomy, Stocker Road, Exeter, EX4 4QL, UK
^{3}
University of Michigan, Department of Astronomy, 1085 S. University Ave, West Hall 323, Ann Arbor, MI 48109, USA
Received:
10
January
2019
Accepted:
15
March
2019
Context. We implement an electron avalanche photodiode (eAPD) in the MIRCX instrument, which is an upgrade of the sixtelescope nearinfrared imager MIRC, at the CHARA array. This technology should improve the sensitivity of nearinfrared interferometry.
Aims. We aim to characterize a nearinfrared CRED ONE camera from First Light Imaging (FLI) using an eAPD from Leonardo (previously SELEX).
Methods. We first used the classical meanvariance analysis to measure the system gain and the amplification gain. We then developed a physical model of the statistical distribution of the camera output signal. This model is based on multiple convolutions of the Poisson statistic, the intrinsic avalanche gain distribution, and the observed distribution of the background signal. At low flux level, this model independently constrains the incident illumination level, the total gain, and the excess noise factor of the amplification.
Results. We measure a total transmission of 48 ± 3% including the cold filter and the Quantum Efficiency. We measure a system gain of 0.49 ADU/e, a readout noise of 10 ADU, and amplification gains as high as 200. These results are consistent between the two methods and therefore validate our modeling approach. The measured excess noise factor based on the modeling is 1.47 ± 0.03, with no obvious dependency with flux level or amplification gain.
Conclusions. The presented model allows the characteristics of the eAPD array to be measured at low flux level independently of a preexisting calibration. With < 0.3 electron equivalent readout noise at kilohertz frame rates, we confirm the revolutionary performances of the camera with respect to the PICNIC or HAWAII technologies. However, the measured excess noise factor is significantly higher than what is claimed in the literature (< 1.25), and explains why counting multiple photons remains challenging with this camera.
Key words: instrumentation: detectors / techniques: high angular resolution / methods: data analysis / infrared: general
© C. Lanthermann et al. 2019
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
1. Introduction
Optical long baseline interferometry allows for imaging at higher angular resolution than classical monolithic telescopes for a given wavelength. For instance, the gain in resolution is about a factor 3 (resp., 8) between a diffractionlimited 40 m singledish telescope and the Very Large Telescope Interferometer (VLTI, Haguenauer et al. 2012) (resp., the CHARA array; Gies et al. 2018). As it is a natural tradeoff between the damaging effect of atmospheric turbulence at shorter wavelengths and the increased sky brightness at longer wavelengths, many interferometric instruments operate in the nearinfrared (NIR), like PIONIER and GRAVITY at the VLTI (Le Bouquin et al. 2011; GRAVITY Collaboration 2017): CLIMB, CLASSIC, JouFLU, and MIRCX at CHARA (Monnier et al. 2006a; ten Brummelaar et al. 2012; Scott et al. 2014). As a typical example, singlemode optical interferometry in the Hband (1.6 μm) requires individual exposure times of about 10 ms. In this spectral range, to cope with atmospheric effects and to stabilize the interferometric fringe patterns implies measurement and servocontrol of the fringe positions during a fraction of the coherence time, that is, during less than a few milliseconds. Fringe tracking in the NIR thus needs fast detectors working at kilohertz speed and allows for the instrument sensitivity to be increased by allowing minutelong exposures to be done on the scientific detector (GRAVITY Collaboration 2017).
In addition, in the Hband, the total instrument and sky background is about ten photons per exposure per telescope. Considering that at least 100 × 10 pixels are commonly needed to encode the spectrally dispersed fringe signal, the background noise is much lower than one photon per pixel and per exposure. Typical readout noise of PICNIC or HAWAII detectors for such a frame rate and format are approximately eight electrons per exposure and per pixel (Pedretti et al. 2004; Beckmann et al. 2014). Consequently, the detector readout noise has remained the limiting factor for decades.
The situation changed in the 2000s with the development of matrices of electron Avalanche PhotoDiodes (eAPD) in the NIR. These detectors promised to deliver subelectron readout noise thanks to amplification of the signal before the readout. On the one hand, a French collaboration of industrial (SOFRADIR, CEALETI) and academic (IPAG, LAM, ONERA) partners designed and built several prototypes of the socalled RAPID detector (Feautrier et al. 2014; Guieu et al. 2014). On the another hand, the Leonardo company (former SELEX) in collaboration with the ESO developed the SAPHIRA detectors to use them in the wavefront sensors and the fringe tracker of the GRAVITY instrument (Finger et al. 2016; GRAVITY Collaboration 2017). This detector was made available as a commercial product, called CRED ONE, by the First Light Imaging company (Greffe et al. 2016).
Within the framework of the installation of adaptive optics on the CHARA array (ten Brummelaar et al. 2016) and with the aim of increasing the sensitivity of highangularresolution imaging in the NIR, we purchased the first two CRED ONE cameras in 2017. The first one was used to upgrade the Hband sixtelescope combiner MIRC, now called MIRCX (Monnier et al. 2012; Kraus et al. 2018), at the focus of the CHARA optical interferometer since mid2017. The second one will be used in the Kband copy of this instrument, called MYSTIC, and is expected to be installed in 2019 at CHARA (Monnier et al. 2018).
The goal of this paper is to measure the characteristics of the eAPD detector of MIRCX at our typical low flux level and to determine whether or not photoncounting is achievable in realistic operational conditions.
After this introduction, the second section describes the CRED ONE camera and the eAPD technology. In the third section, we present a classical characterization of the detector noise and amplification of the camera, based on the meanvariance method. In the fourth section, we introduce an innovative model of the signal distribution which allows us to extract the excess noise factor and the gain. The fifth section discusses the obtained results and compares them with the literature, especially the significant discrepancy of the excess noise factor. The paper ends with a brief summary and conclusion.
2. The CRED ONE camera
2.1. eAPD technology
The eAPD technology consists in applying a bias voltage in a lower layer of the pixel. The electron generated by the incident photon in the absorption region migrates to the bottom of the pixel. When the electron travels through the multiplication region, it is accelerated by the bias voltage. At some point, the kinetic energy is high enough to ionize an atom of the substrate by a collision. The two electrons are accelerated again, generating new electrons by collision. This avalanche process is explained in more detail in Finger et al. (2010) and Finger et al. (2012).
The avalanche process is a stochastic process. An incident photon can lead to different numbers of final electrons with a given probability distribution. In this paper, we refer to this probability distribution as the avalanche gain distributionM. From this amplification gain distribution, we can derive two principal characteristics of the system: the mean avalanche gain and the excess noise factor. The mean avalanche gain is defined by
The excess noise factor (ENF) is defined by
The ENF is the additional noise brought by the avalanche process on the output signal compared to the photon noise obtained without the avalanche process. In the following, we also make use of the mean total gain, defined as
where G_{sys} is the system gain in ADU/e.
2.2. Camera readout
Our CRED ONE cameras (Fig. 1left) use SAPHIRA MCT SWIR Mark13 eAPD 320 × 256 pixels detectors whose overall characteristics are summarized in Table 1.
Fig. 1.
Left: photograph of the MIRCX CRED ONE. Right: scheme of the experimental setup. 1: H band singlemode fiber fed by a whitelight source; 2: dispersion prism; 3: camera cold stop and baffle; 4: low pass cold filter; 5: detector. 

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Characteristics of the SAPHIRA MCT SWIR Mark13 detector used in our CRED ONE camera, as specified by the manufacturer.
The camera offers various readout modes. Our custom readout is inspired from the PICNIC camera from the IOTA observatory (Monnier et al. 2006b). First, it consists of multiple consecutive reads of the same pixel (NREADS) before moving to the next pixel on the row. A row is then read multiple times (NLOOPS) before moving to the next row. Those multiple NREADS and NLOOPS are then averaged. It reduces the readout noise and extends the integration time while keeping a somewhat simultaneous integration window for the various pixels of the same row. In the following, we use frame to refer to the process of reading the entire array once, with this combination of NREADS and NLOOPS. Finally, the array is read multiple times nondestructively (NFRAMES_PER_RESET) before the detector is reset and the process starts again. We note that it is possible to read subwindows of the full pixel array. Cropping is possible in the row and column directions and this increases the frame rate.
In most implementations of the ontheramp mode, the set of NFRAMES_PER_RESET along the ramp is collapsed into a single value of flux per pixel by the mean of a linear fit. This is not the case in interferometric instruments where a fast frame rate is necessary (Pedretti et al. 2004; Le Bouquin et al. 2011). Instead, we individually analyze the flux of each frame in the ramp by subtracting the measurement of the previous frame.
A typical setup used for onsky observations consists of reading a window of 320 × 17 pixels, with NREADS = 12 and NLOOPS = 8. It provides a frame rate of ≈355 Hz. The detector is generally reset every 100 frames only. In the experiments of this paper, we used NREADS = 8 and NLOOPS = 2 in order to increase the frame rate to ≈1916 Hz. This was necessary to lower the background signal per pixel and per frame. Each data set has a total of 2000 frames.
Before being analyzed, we correct the RAW data from a parasitic electronic signal from the pulse tube, which appears as a nearly sinusoidal additive signal; the process is explained in Lanthermann et al. (2018). We then compute the flux per frame, in ADU, by taking the difference between two consecutive frames.
2.3. Cold optics
The CRED ONE camera is delivered in a standalone cryostat, operating at 80 K thanks to a pulsetube. It has a cold aperture of f/4 at about 35 mm from the detector and 15 mm from the external surface of the cryostat window (e.g., where the last warm optics can be located). Our MIRCX camera holds four lowpass cold filters to remove the thermal background; two have a cutoff wavelength at 1.739 μm, and two at 2.471 μm. The latter is mandatory to increase the rejection at wavelengths longer than 3 μm. The theoretical amount of electrons due to the thermal background flux seen by a pixel in a single frame can be computed as follows.
where B(λ, 300 K) is the blackbody emission at 300 K, A = (24 μm)^{2} is the surface of a pixel, Ω = π/64 str is the solid angle corresponding to the cold aperture, T(λ) is the combined transmission of the filters, QE(λ) is the quantum efficiency, and f = 1916 Hz is the frame rate. We measured the combined transmission and quantum efficiency of the camera at 1.55 μm by the mean of a NISTtraceable calibrated diode. The result is 48 ± 3%. This value is somewhat in agreement with the theoretical specifications of 55% at this wavelength. Using the theoretical transmission and quantum efficiency values gives an incident background on the detector of F_{BKGthermal} = 0.042 e frame^{−1} pixel^{−1}.
2.4. Warm optics setup
The data set used for the model presented in this paper have been taken with the optical configuration used for onsky observations, but with the instrument fed by an internal thermal whitelight source (Fig. 1right). In summary, the light is injected into a fiber whose output acts as the entrance slit of a simple spectrograph. A prism disperses the light over 12 pixels across the Hband. The image on the detector therefore consists of 3 × 12 illuminated pixels. The neighboring pixels are not illuminated by the flux coming from the fiber. In the following, we used only the value of a single pixel of the spectrum, which receives the flux from a sharp spectral band of approximately 0.05 μm centered on 1.55 μm.
3. Detector characterization
3.1. Meanvariance analysis
The meanvariance method is a very common way of measuring the gain and the readout noise of a detector (Bohndiek et al. 2008). It is based on the fact that the temporal variance of a photometrically stable signal is proportional to the flux signal. The proportionality coefficient is the total gain multiplied by the excess noise factor. The interception of the fit with the yaxis gives the readout noise. To measure the system gain of our detector, we perform a meanvariance curve at an avalanche gain of 1 (i.e., without avalanche process).
We measure (Fig. 2) a system gain G_{sys} = 0.49 ADU/e. We note that this is somewhat different from the expected system gain of 0.59 ADU/e provided on the data sheet from FLI. We dig into the calibration data of the manufacturer. Depending on the portion of the curve that we fit, the gain can vary from 0.42 to 0.61. These differences may be explained by the nonlinearity of the detector at different flux levels. We do not study the effects of the nonlinearity in this paper because we focus on the lowlightlevel regime.
Fig. 2.
Meanvariance curve at avalanche gain = 1 (no avalanche process). The horizontal axis shows the mean flux in ADU/frame/pixel while the vertical axis gives the temporal variance. The blue dots are the data points. The black line is the fit of a linear function on the data points. 

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The meanvariance analysis also allows for the detector readout noise to be estimated as the floor noise obtained without illumination. The readout noise is ≈17 ADU RMS, derived from the variance of 293 ADU^{2} from the fit. Using the system gain, this corresponds to ≈35 e, which is comparable to the 45 e measured with no APD gain by Finger et al. (2016) on a similar device and with a similar method.
We have identified that this detector noise is in fact partially correlated between the pixels. When using proper filtering (Lanthermann et al. 2018), we typically achieve detector noise as low as ≈12 ADU RMS.
3.2. Avalanche gain
The avalanche gain is the mean value of electrons at the end of the avalanche process for one incident photoelectron. It represents the amplification of the incoming signal before the readout. To calibrate the avalanche gain, we measure the flux registered by the camera at different requested avalanche gains and divide it by the flux measured with no avalanche gain for the same incident flux. At the wavelength of 1.55 μm, the quantum efficiency of the camera is constant with the avalanche gain as shown in Fig. 6 of Finger et al. (2016). We double checked the temporal stability of the flux using a calibrated diode. Over the course of the experiment, the calibrated photometry of our light source was stable within a few percent.
Figure 3 displays the measured avalanche gain compared to the manufacturer calibration. The unity gain is used as a reference to compute the avalanche gain and therefore lies on the red curve by definition. Our measured avalanche gain is consistently 0.93 times the avalanche gain calibrated by the manufacturer. Although not presented in Fig. 3, we have verified that this relation applies for avalanche gain up to 150.
Fig. 3.
Derived avalanche gain as a function of the avalanche gain provided by the manufacturer. The red line is the 1:1 relation. The black line is a linear fit, excluding the unity gain. 

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The calibration from the manufacturer is based on a different method; it is a meanvariance analysis for each amplification gain. Our independent measurement confirms this calibration. The remaining discrepancy of few percent on the absolute gain is not an issue in our operational scenario. Neither the realtime fringetracking algorithms nor the instrument datareduction algorithms rely on our absolute knowledge of the gain.
3.3. Attempt of photon counting
For a total gain of 50 ADU/e or higher, the signal of incoming individual photons should overwhelm the readout noise of 12 ADU and therefore allows photon counting. This is especially true since the expected excess noise factor (ENF) is small (1.25). The ENF is the noise added by the avalanche process of the eAPD. The lower it is, the lower the add noise of the avalanche process. It has a limit of one for a noiseless avalanche process. The effect of the ENF on the photon counting was to spread the signal distribution of one photon. To explore this possibility of individual photon counting, we compute the histograms of the temporal sequences of the values of a single illuminated pixel. Typical histograms are shown in Fig. 4. We interpret the histogram of the background as the sum of (1) a Gaussian distribution of RMS 12 ADU corresponding to the detector readout noise; and (2) a small tail toward positive values corresponding to the few frames with a background photon (approximately 1 over 23 frames). The histogram measured in the lowflux regime shows a break at 25 ADU. We interpret this break as the transition between the zerophoton events and the one or more photon events. This means that we can derive the proportion of zerophoton events, hence the incoming flux. In the highflux regime, the fraction of zerophoton events becomes negligible. The clear transition between the zerophoton events and events with one or more photons is no longer noticeable. Therefore, it appears that performing discretized photoncounting is not possible with this camera. In the following, we develop a simple model that reproduces these histograms and allows us to measure the excess noise factor.
Fig. 4.
Histograms of counts measured on a single pixel, with a lowflux illumination (< 1 e frame^{−1} pixel^{−1}, darker blue) and with a high flux illumination (< 3 e frame^{−1} pixel^{−1}, lighter blue). The total gain is 50 ADU/e. The histogram without illumination is shown in green and represents the intrinsic statistic of the zerophoton events. 

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4. Modeling the photonic signal
We record histograms for various illuminations and various gains. Because of the very low flux levels we are interested in, it was unfortunately impossible to build an absolute calibration of the illumination.
4.1. Model
In the following, we use F to refer to the mean flux reaching the considered pixel and coming from the internal source, in e/frame/pixel. This is an unknown parameter. F = 0 is by definition the mean of the histogram of the background counts (in green in Fig. 4). We developed a simple model with the goal being to reproduce the observed distributions H(ADU) as a function of the parameters G (gain in ADU/photon), the F (flux in photon/frame/pixel), and the ENF (excess noise factor). Our model is described by the following equation.
where the asterisk represents convolution, BKG(ADU, G) is the measured distribution without illumination, P(p, F) is the Poisson probability of a pphoton event given a mean flux Flux, and
is the iterative selfconvolution of the gain distribution because each avalanche generates its own avalanche gain distribution. This model is based on the following realistic assumptions and follows these steps:

1.
The amplification gains of the individual photons summed up in a frame with pphoton are not correlated. Therefore the distribution of the pphoton frames is represented by p − 1 convolutions of the gain distribution M.

2.
These pphoton frames are uncorrelated, therefore the combined distribution is a weighted sum according to the Poisson distribution for the desired flux.

3.
The background flux is additive and uncorrelated with the illumination flux. Therefore the distribution given by the previous steps is convoluted by the distribution measured on the background.
The key physical ingredient of this model is the gain distribution M.
4.2. Prescription for the gain distribution
The mean gain G and the ENF are intrinsic properties of M. A Gaussian distribution (Kardynał et al. 2008) truncated over ℝ^{+} can only model low ENF values (< 1.2). This is because the fraction of nonphysical “negative amplifications” becomes numerically significant at larger ENF values. A decreasing exponential distribution truncated over ℝ^{+} (Tsujino et al. 2009) has a fixed ENF of 2.0. It is unsuited to reproduce the expected ENF of 1.25 of our camera.
The Gamma distribution is classically used to model the photon distribution in EMCCD cameras (Hirsch et al. 2013). It describes the process of multiplication of a single electron inside the pixel. The Gamma distribution is an intrinsically asymmetric function defined and normalized over ℝ^{+}. It is defined by two positive parameters, k and θ (see Appendix A). The former parameter describes the shape of the function, while the latter describes its scale. These two parameters can be directly linked to the ENF and the mean gain by
and
The Gamma distribution allows spanning the entire range of ENF values between 1 and +∞. Figure A.1 displays four examples of the Gamma distribution. Interestingly, the exponential distribution and the Gaussian distribution are special cases of the Gamma distribution. Therefore these two situations are included in our parameter space.
4.3. Fit strategy
Our model uses three free parameters (G, ENF, and the mean photonic flux F) in order to reproduce the observed distribution H(ADU). The background distribution BKG(ADU) is measured by turning off the internal source.
We first run a bruteforce minimization by computing the reduced chisquared between the data and the model for each point in the cube (G, ENF, F). At the end of the brute force method, we run a classical gradient descent toward the bestfit parameters with the minimum position in the cube as the starting point. The whole process on the 25 data files takes ∼3 h with 25 points on the grid for each parameter. We checked that this sampling is enough to sample the degeneracy by processing some data sets with 50 and 100 points on the grid for each parameter.
5. Results and discussion
5.1. Bestfit quality
Figure 5 shows the results of the minimization for a data set with a low flux level. The overall shape of the data is convincingly reproduced by the bestfit solution. The solution has no degeneracy and there is only one minimum for each parameter. This is because the fraction of zerophoton events is well constrained by the “bump” at zero. Knowing the flux, the mean on the histogram constrains the gain. Finally, the ENF is constrained by the shape of the histogram tail.
Fig. 5.
Example of minimization result. This example is from data with Gman = 76.7, the expected gain from the manufacturer calibration. The parameters that minimize the are F = 0.46, G = 52.2, and ENF = 1.38. Diagonal: minimum as a function of ENF (top left), G (middle), and F (bottom right), the two other parameters being free. Lower left: maps of minimum . Upper right: histogram for the data with illumination in blue, histogram of the background in light green, and histogram obtained with the parameters that minimize the in orange. 

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Appendix C shows all the results. The bestfit models convincingly reproduce the data for all flux and gain. This confirms that the Gamma distribution is an adequate model of the amplification process. As expected, for F > 3 e frame^{−1} pixel^{−1}, the degeneracy of the model increased significantly, as shown in Figs. C.3–C.5. This is due to the fact that the proportion of zerophoton events is no longer significant enough to constrain the flux with the data histograms. The maps show that we have only a lower limit to F. As a consequence, we only have a higher limit for G, and ENF is poorly constrained.
5.2. Gain
Figure 6 displays the bestfit gain versus the expected gain as calibrated by the manufacturer. The results obtained with different flux levels and gains are selfconsistent: our bestfit gain (G) is consistent with 0.71 times the expected gain from the manufacturer calibration (G_{man}). We notice that the higher the flux level, the larger the uncertainties. This is due to the degeneracy at high flux levels. Interestingly, the bestfit gains for those highflux data are still consistent with the ones at low flux.
Fig. 6.
Bestfit gain as a function of the expected gain from the manufacturer calibration. The black line is a linear fit, while the red line is the expected 1:1 relation. The different colors of the data points show the different flux estimated by the modelfitting. 

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We analyzed several pixels in order to check the uniformity of the results in the matrix (see Appendix B). The results are consistent over the pixels and show a mean gain G = 0.70 ± 0.04 × G_{man}. This is in overall agreement with the fully independent calibrations presented in Sect. 3. With these more classical methods, we obtained a ratio of G_{sys measured}/G_{sys man} × G_{ava ratio} = 0.49/0.59 × 0.93 = 0.77 for the total gain, compared to the manufactured calibration. This also confirms that our simple model adequately captures the statistics of the amplification process.
5.3. Excess noise factor
Figure 7 shows the measured ENF as a function of the manufacturer gain. The median value of all the measured ENF is 1.49 ± 0.12. As expected, the uncertainty increases for measurements at higher flux but the error bars all remain compatible with the median value. As for the gain, we performed the same study on several pixels. The results are summarized in Appendix B. The mean ENF over the pixels is 1.47 ± 0.03.
Fig. 7.
Bestfit ENF as a function of the manufacturer gain. Colors represent the flux estimated by the bestfit. The black line is the median value of measurements. The red line is the value from the manufacturer. 

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The discrepancy between our measured ENF and the value reported in the literature is striking. Finger et al. (2016) measure an ENF of 1.3 at a temperature of 90 K and 1.1 at 40 K. Their method to measure the ENF is independent of a gain distribution model. They control the illumination by using a blackbody source located in front of the detector. They compare the noise on the detector with the photon noise expected for the controlled flux. Based on this calibration, the value expected by the manufacturer for our camera is 1.25 for an operating temperature of 80 K.
The detailed study of a MARK13 SAPHIRA presented by Atkinson et al. (2018) gives interesting clues on the ENF. Their Fig. 6 shows a histogram of the detector signal with very low illumination (about 0.1 photon frame^{−1} pixel^{−1}). The histogram has a peak at the position of the zerophoton events whose shape is similar to the histogram without illumination, and a tail for the events with one or more photons. As in our measurements, there is no separation between those two distributions. We run our model on the data extracted from Fig. 6 of Atkinson et al. (2018). The results are presented in Fig. C.6. The model reproduces adequately the shape of the observed histogram. The best fit ENF = 1.45 is consistent with the results obtained on our own data.
The first possibility is the somewhat arbitrary choice of the gain distribution model M in our study. We also tried a Gaussian model defined over ℝ^{+}. The resulting ENF were not significantly different.
Another possibility is that the illumination contains photons at higher wavelengths. These photons are absorbed deeper in the pixel, possibly inside the multiplication region. This would create a less amplified signal, spreading the gain distribution. But our optical setup disperses the spectrum of the whitelight source. Based on the spectral calibration of the instrument, we are sure that the pixels considered for this study only receive photons between 1.55 and 1.6 μm coming from the whitelight source. We remind the reader that the photons of the warm background are already taken into account in the background histogram.
Another hypothesis is that the signal of individual photon is temporally smeared. In Finger et al. (2016), the detector response time is of the order of 1 ms. As the measurement of the ENF in the same paper is made at 1 kHz, the signal would not be smeared. In our experiment, we took data at 1900 Hz, which is faster than the detector response time. But the claim is that the detector response time is dominated by the electron migration in the substrate and not by the avalanche process (Finger et al. 2016). Hence, it would delay the signal, not smear it. Another smearing occurs due to our specific readout mode, for photons arriving between consecutive readout that are averaged together into a single frame. We read an entire row several times before reading the others, and average these measurements. As we read 20 rows, it means that only 5% of the photons are smeared this way. This is too low to explain the difference between our value and the ones in the literature. Moreover, such an effect skews the distribution of gain toward the lower values (negative skewness), not toward the higher values (positive skewness) as seen in Fig. 6 of Atkinson et al. (2018) and across this paper.
The last possibility is that the results existing in the literature have been obtained for relatively high flux (several tens of photons per frame and per pixel), while our study and that of Atkinson focus on very low flux levels (less than 5 photons per frame and per pixel, and more typically less than 1 photon per frame and per pixel). We suspect that the physics of the detector is not the same when there is one or several electrons migrating in the amplification zone.
5.4. Consequences for photoncounting
As shown in Sect. 3.3, photon counting by fully separating the distributions of zero, single, or multiple photon events is not possible with our camera. This is due to the unexpected ENF of 1.47. However, Fig. 4 shows that we do see two different distributions at low flux: the one of the zerophoton events, and the one of the events with one or more photon. Therefore, one could define a threshold that would separate the frames with and without photons, with some statistical uncertainties. Computing this optimal threshold for each gain and each frame rate is out of the scope of this paper.
Although disentangling the zerophoton events from those with one or more photons may appear attractive, we did not implement this in the datareduction pipeline of the instrument. Indeed, when dealing with a significant fraction of events with more than or equal to two photons, such a threshold dramatically complicates the unbiasing of the fringe bispectrum. A detailed discussion on the impact of the measurement statistics on the fringe bispectrum can be found in Basden & Haniff (2004), Gordon & Buscher (2012), and Garcia et al. (2016). We are currently upgrading the bispectrum debiasing algorithm in the MIRCX pipeline based on our new understanding of the signal statistic presented in this study.
5.5. Consequences on instrument performance
We simulate the S/N of the MIRCX instrument for two realistic situations. First, we simulate a flux of 0.1 e pixel^{−1} ms^{−1} which is typically obtained on faint objects, such as young stellar objects (YSOs). These are the primary science goals of MIRCX. The fringe visibility is often high (close to 1) because the objects are unresolved. Secondly, we simulate a flux of 100 e pixel^{−1} ms^{−1} which is typical of bright objects, such as fully resolved stellar surfaces. These targets have very low visibility (e.g., 0.01). We estimate the detector and background noise by using actual measurements in background exposures obtained with the former PICNIC camera and with the CRED ONE at an avalanche gain of 60 (best compromise between readout noise and tunneling noise; Lanthermann et al. 2018). We used the measured ENF = 1.47 for the CRED ONE camera, and ENF = 1 for the PICNIC camera that does not have additional noise from an avalanche process. For both cameras, the fringe signal is encoded into 100 pixels. Results are shown in Fig. 8.
Fig. 8.
Simulation of the S/N as a function of the coherent integration time in two operational conditions of flux and fringe visibility, for the previous PICNIC camera of MIRC and the new CRED ONE camera of MIRCX. 

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The operational limit for fringe detection is defined by S/N > 3. In the lowflux regime, the simulation shows an improvement of one decade in terms of necessary integration time between the former PICNIC camera and the new CRED ONE. This corresponds to a gain in sensitivity of 2.5 mag. In the highflux regime, the PICNIC camera is more efficient but the difference is relatively small in terms of limiting magnitude. For the specific case of averaging many exposures on bright targets with the goal being to reach a high S/N, the PICNIC camera remains theoretically advantageous because it does not suffer from the ENF. However, this is not true in practice because other effects quickly become dominant such as the piston noise or the calibration accuracy.
This simulation compares realistically with the results obtained on sky so far. The typical limiting magnitude of the instrument with the former PICNIC camera was H ≈ 5.5. Since the upgrade, it has been possible to observe several YSOs and massive stars at magnitudes of H ≈ 7.5. Overall, in terms of scientific productivity for MIRCX, the sensitivity boost obtained in the lowflux regime largely overcomes the possible sensitivity losses in the highflux regime.
6. Conclusions
We have characterized the first NIR CRED ONE camera manufactured by the First Light Imaging company. This SAPHIRA electron avalanche photodiode camera is now part of the MIRCX instrument operating in the H band and installed at the combined focus of the CHARA array.
We have presented the characterization of this CRED ONE camera in the operational scenario of the MIRCX instrument (multiple readouts, kHz frame rate and low flux illumination). We first performed a classical analysis based on the meanvariance curve and mean flux level in order to determine the system gain and amplification gain. We then presented a simple but innovative modeling of the signal distribution from the camera at low flux level enabling us to estimate both the total gain and the excess noise factor brought by the amplification process. The model adequately reproduces the observed distributions of photon events for a large range of flux and gains. We also applied our model to existing literature data to confirm our measurements.
We measured a system gain and total gain slightly lower than those provided by the manufacturer. This result is observed consistently when using the meanvariance method and our model based on the signal distribution. Our modeling also revealed that the ENF (1.47) is significantly higher than the values in the literature for this type of detector (1.25). The reason for such a discrepancy could not be determined. After reviewing various possibilities, we proposed that the amplification process could behave differently in the lowflux and highflux regimes.
From Sect. 5.5, we show that the CRED ONE in the MIRCX instrument brings a theoretical improvement in sensitivity of 2.5 mag in the H band for faint objects, when its performances are comparable to the former PICNIC camera for bright objects. More generally, with an equivalent readout noise of < 0.3 electrons at kilohertz frame rates computed from the background histograms (Fig. 4), we confirm the revolutionary performances of the camera with respect to the PICNIC or HAWAII technologies for highframerate applications. In current operation, the camera has improved the limiting magnitude of our MIRCX instrument by up to two magnitudes, the exact value depending on the atmospheric coherence time and the setup of the spectrograph. However, the observed higher excess noise factor is consistent with the fact that we cannot separate the events with different numbers of photons in the observed signal distribution.
Acknowledgments
We would like to thanks MarcAntoine Martinod, Johan Rothman, and Romain Laugier for their interest in this work and the fruitful discussions that lead to the choice of the Gamma distribution for the gain distribution. We thank also FLI for their collaboration in the characterization and the comprehension of the camera. We also thank the University of Michigan for welcoming us and making this collaboration work possible. We finally thank CHARA and all the people that allowed us to collect data and observe. This work has been partially supported by the LabEx FOCUS ANR11LABX0013. The research leading to these results has received funding from the European Unions Horizon 2020 research and innovation programme under Grant Agreement 730890 (OPTICON) and Grant Agreement No. 639889 (ERC Starting Grant “ImagePlanetFormDiscs”). This work has been supported by a grant from Labex OSUG@2020 (Investissements d’avenir ANR10 LABX56). This work was supported by the Programme National de Physique Stellaire (PNPS) of CNRS/INSU cofunded by CEA and CNES. This work was supported by the Action Spécifique Haute Résolution Angulaire (ASHRA) of CNRS/INSU cofunded by CNES.
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Appendix A: Gamma distribution
Figure A.1 shows four examples of the Gamma distribution for different values of avalanche gain and ENF. In the upperleft corner, we see a Gaussian distribution. In the lowerleft corner, we are in the regime of an exponential distribution. The probability density function of the Gamma distribution is defined by
Fig. A.1.
Different examples of gain distribution modeled with the Gamma distribution. Upperleft corner: ENF = 1.05 and G = 40. Upperright corner: ENF = 1.3 and G = 40. Lowerleft corner: ENF = 1.9 and G = 40. Lowerright corner: ENF = 1.3 and G = 80. 

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for x > 0 and k, θ > 0, and where Γ(k) is the gamma function. For this distribution, the k parameter describes the shape of the distribution and θ parameter describes the scale of the distribution.
Appendix B: Results from different pixels
Table B.1 summarizes the results obtained for five different pixels, in order to quickly assess the homogeneity of the result across the detector.
Results of gain and ENF for five different pixels.
The coordinates are measured within the 320 × 20 pixel window. The gain factor is computed with the linear fit of the gain of the bestfit model as a function of the manufacturer gain (Fig. 6). The ENF is obtained with the median of the different ENF measured by the model for various fluxes (Fig. 7). The plots shown in the main sections of the paper were for pixel (66; 9). Table B.1 shows that we obtain similar values for other pixels.
Appendix C: Different minimization results
This appendix presents the results of minimizations for different typical configurations. Figure C.1 is for a lowflux and lowgain configuration. Figure C.2 is for a lowflux and highgain configuration. Figure C.3 is for a highflux and lowgain configuration. Figure C.4 is for a highflux and highgain configuration. Figure C.5 is for a high flux at the maximum gain used for this study. Figure C.6 is for the data from Fig. 6 of Atkinson et al. (2018).
Fig. C.1.
minimization result example for low flux, low gain. 

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Fig. C.2.
minimization result example for low flux, high gain. 

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Fig. C.3.
minimization result example for high flux, low gain. 

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Fig. C.4.
minimization result example for high flux, high gain. 

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Fig. C.5.
minimization result example for high flux, highest gain. 

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Fig. C.6.
minimization result for Atkinson et al. (2018) data. 

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All Tables
Characteristics of the SAPHIRA MCT SWIR Mark13 detector used in our CRED ONE camera, as specified by the manufacturer.
All Figures
Fig. 1.
Left: photograph of the MIRCX CRED ONE. Right: scheme of the experimental setup. 1: H band singlemode fiber fed by a whitelight source; 2: dispersion prism; 3: camera cold stop and baffle; 4: low pass cold filter; 5: detector. 

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In the text 
Fig. 2.
Meanvariance curve at avalanche gain = 1 (no avalanche process). The horizontal axis shows the mean flux in ADU/frame/pixel while the vertical axis gives the temporal variance. The blue dots are the data points. The black line is the fit of a linear function on the data points. 

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In the text 
Fig. 3.
Derived avalanche gain as a function of the avalanche gain provided by the manufacturer. The red line is the 1:1 relation. The black line is a linear fit, excluding the unity gain. 

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In the text 
Fig. 4.
Histograms of counts measured on a single pixel, with a lowflux illumination (< 1 e frame^{−1} pixel^{−1}, darker blue) and with a high flux illumination (< 3 e frame^{−1} pixel^{−1}, lighter blue). The total gain is 50 ADU/e. The histogram without illumination is shown in green and represents the intrinsic statistic of the zerophoton events. 

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In the text 
Fig. 5.
Example of minimization result. This example is from data with Gman = 76.7, the expected gain from the manufacturer calibration. The parameters that minimize the are F = 0.46, G = 52.2, and ENF = 1.38. Diagonal: minimum as a function of ENF (top left), G (middle), and F (bottom right), the two other parameters being free. Lower left: maps of minimum . Upper right: histogram for the data with illumination in blue, histogram of the background in light green, and histogram obtained with the parameters that minimize the in orange. 

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In the text 
Fig. 6.
Bestfit gain as a function of the expected gain from the manufacturer calibration. The black line is a linear fit, while the red line is the expected 1:1 relation. The different colors of the data points show the different flux estimated by the modelfitting. 

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In the text 
Fig. 7.
Bestfit ENF as a function of the manufacturer gain. Colors represent the flux estimated by the bestfit. The black line is the median value of measurements. The red line is the value from the manufacturer. 

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In the text 
Fig. 8.
Simulation of the S/N as a function of the coherent integration time in two operational conditions of flux and fringe visibility, for the previous PICNIC camera of MIRC and the new CRED ONE camera of MIRCX. 

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In the text 
Fig. A.1.
Different examples of gain distribution modeled with the Gamma distribution. Upperleft corner: ENF = 1.05 and G = 40. Upperright corner: ENF = 1.3 and G = 40. Lowerleft corner: ENF = 1.9 and G = 40. Lowerright corner: ENF = 1.3 and G = 80. 

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In the text 
Fig. C.1.
minimization result example for low flux, low gain. 

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In the text 
Fig. C.2.
minimization result example for low flux, high gain. 

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In the text 
Fig. C.3.
minimization result example for high flux, low gain. 

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In the text 
Fig. C.4.
minimization result example for high flux, high gain. 

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In the text 
Fig. C.5.
minimization result example for high flux, highest gain. 

Open with DEXTER  
In the text 
Fig. C.6.
minimization result for Atkinson et al. (2018) data. 

Open with DEXTER  
In the text 
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