1. Introduction
The electromagnetic power that comes from the Sun has been proved to be an effective reference for checking the quality of dual-polarization weather radar receivers. Operational monitoring methods have been developed and implemented for determining the electromagnetic antenna pointing [
1], assessing the receiver stability [
2], and the differential reflectivity offset [
3]; results from such methods were successfully applied, at first during a period of quiet solar flux activity (in 2008), subsequently to the currently active Sun period [
4]. The ten C-band radar receivers analyzed in Finland, Switzerland, and the Netherlands were able to capture and describe the monthly variability of the Sun microwave signal [
5].
So far, the focus has been on relative calibration: C-band horizontal and vertical polarization signals have been mutually compared and evaluated
versus the reference S-band signal mainly in terms of standard deviation of the difference between radar-retrieved and reference flux values in solar flux units (SFUs), where 1 SFU is equal to 10
−22 W∙m
−2∙Hz
−1. The S-band solar flux measurements distributed by the Dominion Radio Astrophysical Observatory (DRAO) of the National Research Council of Canada provide a useful reference for weather radar receivers. Such measurements, precisely acquired three times per day, are consistent and accurate; furthermore, the same source can be observed simultaneously over a large area. A problem encountered with C-band radar receivers is the frequency conversion from 10.7 to 5.5 cm.
Section 5 of the paper by Tapping [
6] provides a simple conversion formula that allows one to overcome such a problem. In particular, we use the coefficients presented in Equation (1) of [
4], which are tailored to the Swiss frequency band (5430–5470 MHz). In this paper, we present results focusing on absolute calibration of vertical and horizontal polarization receivers. In other words, we also put emphasis on the absolute difference (bias) between the log-transformed radar-retrieved value and the reference value accurately measured by the DRAO.
Such absolute calibration results are obtained thanks to a convenient and effective method recently presented in [
7]. The method is complementary to the on-line technique that automatically detects and analyzes Sun signals stored in the polar volume radar reflectivity data acquired during the operational weather scan program [
1,
2,
3,
4]. Such a technique, which allows relative calibration and mutual inter-comparison between vertical and horizontal channels, has the great advantage of requiring no interruption of the weather surveillance. On the contrary, the method here applied and presented in [
7] tackles the absolute calibration of the receiver by pointing the antenna beam axis towards the center of the Sun; hence, it requires that the weather radar be off-line for a few minutes during such a special purpose scan. This idea has been applied many times in radio astronomy. In radar meteorology, it was developed in the late 1970s by Frush and Lewis at the National Center for Atmospheric Research, preliminarily presented in 1984 [
8] and thoroughly described by Pratte and Ferraro in 1989 [
9]. Subsequently, Pratte, Ferraro and Keeler have further extended it and eventually transferred to Nexrad (USA) where Ice and colleagues developed it for use with the WSR-88D [
10].
The method has been applied to the five weather radar receivers of the recently renewed Swiss weather radar network. As described in [
7], radar observations of the solar signal are performed only in fair weather conditions. In this way, wet-radome attenuation and attenuation along the path are avoided.
Section 2 briefly presents the operational Swiss weather radar receivers, the acquired and reference data, as well as the formula for the retrieval. Results are given in
Section 3 for the ten dual-polarization receivers of the Swiss weather radar network: a set of 27 observations by the five radar receivers is presented. A detailed discussion and interpretation of the results is presented in
Section 4. A summary, conclusions, and an outlook are provided in the last section.
2. Description of Instruments, Acquired Data, and Retrieval Formula
In recent years, MeteoSwiss has renewed its weather radar network with an innovative, state-of-the-art solution. From 2011 to 2015, five new polarimetric systems have been installed. Fully digital, antenna-mounted receivers, which are capable of simultaneously measuring vertical and horizontal linear polarization components, have been introduced. With respect to the conventional solution, where the receivers are installed next to the transmitter inside the technical room, this system architecture does not require the installation of a dual channel rotary joint, which may introduce differential errors in amplitude and phase; it also provides a significant reduction of Rx-losses. Another key aspect of the Swiss weather radar receivers is the use of a stable, white signal generated by a noise source (NS) as an absolute reference for the calibration of the radar Rx. Every 5 min, which is the time required to accomplish a full-volume in the 20-elevation Swiss scan program [
11], the NS reference signal (NS
ref, around −90 dBm) is injected into the Rx front-end (input of the LNA) and the corresponding log-transformed value in analog-to-digital-Units (ADUs) at the output of the A/D converter is read, NS
out. In this way, the factor for the transformation from dBADU to dBm of any received signal is known and updated every 5 min [
12].
The Dominion Radio Astrophysical Observatory (DRAO) is located at a site near Penticton (British Columbia, Canada), which is characterized by low interference levels at decimeter and centimeter wavelengths. Accurate observations of the daily solar flux have been performed since 1946; they are acquired three times per day at 10.7 cm, which is the wavelength where the slowly varying solar component is more significant compared to the quiet radio flux [
13]. The 10.7-cm solar flux measurements can be converted into other radio frequencies with some bias uncertainty. This is possible thanks to the remarkable stability of the spectrum of the slowly varying component of solar activity. As stated in the introduction, for the conversion from 10.7 cm to 5.5 cm, we used the formula listed in [
6] with the coefficients presented in Equation (1) of [
4]. For the set of measurements presented in this paper (a total of 17 days from 2 November 2013 until 22 March 2016), we have, on the one hand, checked that the spectral component was not distorted by contributions from flares or other events having spectra and variability with time that are a function of frequency, but, on the other hand, pointed the radar antennas toward the Sun in days close to the Sun minima. During active periods (
i.e., the last few years), in fact, the number of active regions (Sun spots) that enhance the radio emission with respect to the quiet component, as seen from the Earth, varies because of the Sun’s rotation around its axis. This result is an oscillation with an amplitude of a couple of decibels and a period of ~27 days. For instance, using the above cited Equation (1), in 2014, the min/max values (excluding solar flares) at 5.5 cm were around 21.3 and 23.5 dBsfu; in 2015, they were around 21.0 and 22.7 dBsfu. Note that, in Equation (1), the quiet Sun emission is assumed to be 113 sfu (
i.e., 20.53 dBsfu). Note also that, in this paper, we will use log-transformed values of solar flux units (spectral irradiances) coming from the Sun:
S = 10 log(
s/S
0), where S
0 = 10
−19 mW∙m
−2∙Hz
−1 and [
S] = dBsfu.
Finally, we need a way to transform the observed Sun signal at the output of the receiver A/D converter, S
out ([S
out] = dBADU), into equivalent spectral irradiance at 5.5 cm, incident on the radome and subsequently on the antenna, I
5.5, where [I
5.5] = dBsfu. This transformation is conceptually done in three steps that are thoroughly described in Section 2 of [
7]. For the sake of brevity, we only list an overall transformation formula, which results from the three equations presented in [
7]:
where G
dB is the radar antenna gain in dB; L
Rx represents the overall receiver insertion losses (including radome); λ is the wavelength in meter; and B
dBHz = 10 log(BW), where the bandwidth (BW) is in Hz. The number 193.5 dB reflects two deterministic factors and a problematic one: 193 is simply because the Sun radiation is unpolarized (3 dB) and 1 sfu = 10
−19 mW∙m
−2∙Hz
−1 (190 dB). The additional 0.5 dB is an estimate (hence characterized by some uncertainty) of the “additional losses” due to the fact the Sun is not a point source for the highly directive weather radar antennas. The apparent diameter of the radio Sun (~0.57°) is not negligible with respect to the half power beam width of the weather radar antenna (1.0°); consequently, the solar disc is not detected with a constant antenna gain so that the contribution of outer areas of the disc are underestimated, with respect to the center (see [
7] for a detailed discussion). For all five MeteoSwiss radar receivers, we used λ = 0.055 m and BW = 2.52 MHz (see [
14] for details). This means that the 5th and 7th terms on the right-hand side of Equation (1) are 64.01 dBHz and 36.18 dBm
−2, respectively. Regarding the two dimensionless terms in Equation (1)—L
Rx and G
dB—the values are listed in
Table 1 for both polarization and each Swiss radar. Antenna gain was measured at the manufacturer test range, while Rx losses were measured at the site during the site acceptance tests.
4. Discussion of the Results Including a Preliminary Attempt of Noise Subtraction
As previously stated, our radar-retrieved estimates of solar flux can be improved in two directions, which are characterized by opposite signs: (1) on the one hand, the retrieved estimates are slightly low because atmospheric attenuation is neglected; (2) on the other hand, the retrieved estimates are somewhat too high because of the contamination of receiver noise, which is not negligible compared to the solar signal.
Total clear sky atmospheric attenuation at the zenith is 0.076 (0.060) dB at an altitude of 1000 (3000) m—this by assuming a one-way attenuation value of 0.01 dB/km at sea level, and an equivalent atmospheric height of 8.5 km. For the typical angles of elevation used during sun-tracking, and assuming a flat atmosphere, this produces attenuation values between 0.12 dB and 0.18 dB for Albis and between 0.1 dB and 0.14 dB for WEI. Regarding noise subtraction, since the log-transformed ratio of sun to noise (
i.e., the measured quantity) divided by noise is of the order of 9 dB, the typical reduction of the retrieved solar flux is about 0.5 dB smaller than the one presented in
Section 3. Adding up, between these two second-order effects, noise subtraction is more influent than the atmospheric correction. Hence, we will attempt noise subtraction on the 22 observations coming from WEI,
Monte Lema, and Albis. Results are presented and discussed below.
The Swiss radar receivers operationally measure system noise every 2.5 min at angles of elevation of 35° and 40°, respectively. The noise measurements are taken between 60 and 70 km, integrating 120 range bins and 420 pulses within a 10° sector in azimuth. Each noise measurement is thus the average of 120 × 420 = 50,400 raw measurements. We then combine 20 noise measurements, keeping the median out of the 20 values as representative of the noise floor. This is done for both channels separately. In the present example, we use the observed noise value at 40° elevation, N
EL40 (namely, the last one before the Sun-tracking started), and subtract it from the observed value, S
out (both obviously in linear ADU). The observed value consists of the solar flux, plus an “unknown” noise component. In formula: S
out = S
Sun + N
unknown. Our estimate after noise subtraction, simply consists of subtracting the nearest-in-time observed value of N from the S values listed in
Section 3.
Table 7 shows that noise subtraction results in an average decrease of approximately 0.5 dB.
An important question: Does this kind of noise subtraction improve the agreement between the weather radar and DRAO? As can be seen in
Table 8, there is no improvement in terms of standard deviation of the error. However, one can also ask whether the agreement improves in terms of correlation and for this purpose.
Table 9 shows the percentage of explained variance (100 times the square of the correlation coefficient) for both polarizations of Albis, Lema, and WEI. It is worth noting that the number of samples is so small that the degrees of freedom are only 5 (Albis), 4 (
Monte Lema), and 7 (WEI). Noise subtraction increases the correlation for both channels of WEI and Albis. For
Monte Lema, the correlation slightly decreases. We conclude that the median-observed noise at angles of elevation of 40° is not always representative for the real (unknown) noise affecting the Sun signal measurement during the off-line Sun-tracking. For future sun-tracking experiments, we plan to use noise samples as close as possible to the sun signal, both in space and time.
5. Summary, Conclusions, and Outlook
An effective method for the absolute calibration of vertical and horizontal polarization radar receivers has been applied to the five dual-polarization radar receivers of Switzerland. Five observations are available for two radar receivers (La Dole and PPM); for the other three radar receivers, a total of 22 observations are available.
Regarding the absolute error, which is related to the absolute radar calibration, WEI and
Monte Lema show the best results,
La Dole and PPM show intermediate results, while Albis shows an underestimation of approximately −1.62 (−1.25) dB for the horizontal (vertical) channel (including noise subtraction but neglecting clear sky attenuation). The standard deviation of such an error in terms of stability is better than ±0.18 dB for both channels of Albis, Lema, and WEI. For
La Dole and PPM, the sample is too small to calculate the standard deviation. It is interesting to compare these results obtained during solar relative minima and Sun-tracking with those obtained by the operational, automatic method for the continuous monitoring of weather radar receivers through the comparison of daily radar-derived solar flux values with the DRAO reference [
2,
3,
4]. Using such a different technique for more than two hundred days in 2014, the standard deviation of the error of the horizontal channel of Albis (
Monte Lema) was, as expected, much larger than with this Sun-tracking method: ±0.35 (±0.48) dB (see Table 2 in [
4]). By restricting the analysis to 100 days (see Table 4 in [
5]), the standard deviation of the error results is smaller: ±0.26 (±0.34) dB for Albis (
Monte Lema), which is still considerably larger than with the Sun-tracking method. Similar results are obtained if we consider other C-band radar receivers in Europe: for the same 100-day period, the standard deviation of the error was ±0.26 dB for the Dutch Den Helder radar and ±0.36 dB for the Finnish Anjalankoski (ANJ) radar. When comparing the figures of the Swiss radar receivers with those from the Dutch and Finnish radar receivers, it is worth noting that the MeteoSwiss operational algorithm is based on the median of the strongest 21 daily hits, while the others are based on a full five-parameter linear model fit to both polarization channels separately. Not surprisingly, the 22 Swiss observations using Sun-tracking and avoiding solar relative maxima show a considerably smaller standard deviation of the error: better than ±0.16 dB for the horizontal channels of Albis, Lema, and WEI.
The correlation between radar estimates and the DRAO reference is also significant (see
Table 9 in the previous section). For Albis and WEI, it increases after the noise subtraction.
The method shows stability not only of the absolute error between the radar and the DRAO reference, but also in terms of the difference between the vertical and horizontal channels: for WEI, the average of 9 values of 10 log(H/V) is ~0.2 dB with ±0.1 dB standard deviation. For
Monte Lema (6 values), it is ~0.1 dB with ±0.08 dB standard deviation. For Albis (7 values), the standard deviation is as small as ±0.04 dB. It is interesting to compare this very small dispersion of the difference between H and V with the one obtained using the operational method [
2,
3,
4] for daily monitoring: during 220 (204) days in 2014, it was ±0.05 (±0.06) dB, as can be seen in Table 4 in [
4]; during the same set of 100 days in 2014, the dispersion of the difference between H and V was 0.06 dB for Albis and 0.08 dB for ANJ (see Table 3 in [
5]). In a recent manuscript that reviews several aspects of the monitoring of dual-polarization receiver using solar hits found in operational scans [
15], a dispersion as low as 0.02 dB was found for the Finnish ANJ and LUO radar. These figures refer to a shorter period: April 2015. During that month, the standard deviation was 0.03 (0.04) dB for the KES (KOR) radar.
In summary, the results obtained so far are promising and MeteoSwiss is planning to repeat off-line Sun-tracking observations on a regular basis. We aim at the alignment of all ten radar receivers by the end of 2016 after having acquired more samples and further evaluated the effect of noise subtraction and eventually atmospheric correction.