Articles | Volume 15, issue 8
Atmos. Meas. Tech., 15, 2361–2376, 2022
https://doi.org/10.5194/amt-15-2361-2022
Atmos. Meas. Tech., 15, 2361–2376, 2022
https://doi.org/10.5194/amt-15-2361-2022
Research article
20 Apr 2022
Research article | 20 Apr 2022

Ground-based Ku-band microwave observations of ozone in the polar middle atmosphere

Ground-based Ku-band microwave observations of ozone in the polar middle atmosphere
David A. Newnham1, Mark A. Clilverd1, William D. J. Clark1, Michael Kosch2,3,4, Pekka T. Verronen5,6, and Alan E. E. Rogers7 David A. Newnham et al.
  • 1British Antarctic Survey, High Cross, Madingley Road, Cambridge, CB3 0ET, UK
  • 2Physics Department, Lancaster University, Lancaster, LA1 4YB, UK
  • 3South African National Space Agency (SANSA), Hospital Street, Hermanus 7200, South Africa
  • 4Department of Physics and Astronomy, University of the Western Cape, Robert Sobukwe Road, Bellville, 7535, South Africa
  • 5Sodankylä Geophysical Observatory, University of Oulu, Tähteläntie 62, 99600 Sodankylä, Finland
  • 6Space and Earth Observation Centre, Finnish Meteorological Institute, P.O. Box 503, 00101, Helsinki, Finland
  • 7MIT Haystack Observatory, Route 40, Westford, MA 01886, USA

Correspondence: David A. Newnham (dawn@bas.ac.uk)

Abstract

Ground-based observations of 11.072 GHz atmospheric ozone (O3) emission have been made using the Ny-Ålesund Ozone in the Mesosphere Instrument (NAOMI) at the UK Arctic Research Station (latitude 78550′′ N, longitude 115559′′ E), Spitsbergen. Seasonally averaged O3 vertical profiles in the Arctic polar mesosphere–lower thermosphere region for night-time and twilight conditions in the period 15 August 2017 to 15 March 2020 have been retrieved over the altitude range 62–98 km. NAOMI measurements are compared with corresponding, overlapping observations by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) satellite instrument. The NAOMI and SABER version 2.0 data are binned according to the SABER instrument 60 d yaw cycles into nominal 3-month “winter” (15 December–15 March), “autumn” (15 August–15 November), and “summer” (15 April–15 July) periods. The NAOMI observations show the same year-to-year and seasonal variabilities as the SABER 9.6 µm O3 data. The winter night-time (solar zenith angle, SZA  110) and twilight (75 SZA  110) NAOMI and SABER 9.6 µm O3 volume mixing ratio (VMR) profiles agree to within the measurement uncertainties. However, for autumn twilight conditions the SABER 9.6 µm O3 secondary maximum VMR values are higher than NAOMI over altitudes 88–97 km by 47 % and 59 %, respectively in 2017 and 2018. Comparing the two SABER channels which measure O3 at different wavelengths and use different processing schemes, the 9.6 µm O3 autumn twilight VMR data for the three years 2017–2019 are higher than the corresponding 1.27 µm measurements with the largest difference (58 %) in the 65–95 km altitude range similar to the NAOMI observation. The SABER 9.6 µm O3 summer daytime (SZA < 75) mesospheric O3 VMR is also consistently higher than the 1.27 µm measurement, confirming previously reported differences between the SABER 9.6 µm channel and measurements of mesospheric O3 by other satellite instruments.

1 Introduction

1.1 Background information

Ozone (O3) is an important trace species in the mesosphere and lower thermosphere, affecting atmospheric heating rates and the chemical and radiative budgets of the middle atmosphere (Brasseur and Solomon, 2005; Sinnhuber et al., 2012; Palmroth et al., 2021). The secondary O3 maximum (Hays and Roble, 1973) near the mesopause at  90–95 km arises from downward transport and recombination of atomic oxygen (O) produced by far-UV (FUV) dissociation of molecular oxygen (O2) in the lower thermosphere. The diurnal cycle in odd oxygen (Ox) leads to rapid interconversion at twilight between daytime O and O3 at night. In the summer mesosphere, the abundance of odd hydrogen (HOx) from FUV photo-dissociation of water vapour leads to a deep minimum in O3 abundance. However, a seasonal tertiary O3 layer forms at altitudes  70–75 km in mid-latitude to high latitudes when H2O is no longer efficiently dissociated into HOx due to high optical depths in the FUV (Marsh et al., 2001). The tertiary O3 peak in the middle mesosphere is observed from early autumn until late spring between 30 latitude and the equatorward edge of the polar-night terminator (Hartogh et al., 2004). The spatial and temporal structure of the tertiary O3 layer in the polar winter mesosphere, and its night-time variability, has been reported (Smith et al., 2015, 2018; Sofieva et al., 2009). Mesospheric O3 is also strongly affected by space weather processes which increase energetic particle precipitation (EPP) into the atmosphere (Baker et al., 2018). D-region ionisation due to EPP increases mesospheric HOx and odd nitrogen (NOx) which impact on O3 abundances (e.g. Daae et al., 2012; Andersson et al., 2014; Verronen and Lehmann, 2015; Zawedde et al., 2019). Atmospheric dynamical processes including meridional circulation, vertical diffusion, planetary and gravity wave activity, atmospheric tides, polar mesospheric cloud occurrences, and sudden stratospheric warming events also modify O3 distributions in the middle atmosphere (e.g. Pancheva et al., 2014; Limpasuvan et al., 2016; Siskind et al., 2018; Smith-Johnsen et al., 2018).

1.2 Previous ozone measurements

O3 vertical profiles in the upper mesosphere (70–100 km) from observations by nine satellite instruments have been reviewed and compared by Smith et al. (2013). More recently, O3 profiles have been reported up to  105 km during dark conditions and  95 km during sunlit periods from measurements using the middle atmosphere modes of the Michelson Interferometer for Passive Atmospheric Sounding (MIPAS). Validation of the 10-year satellite dataset (López-Puertas et al., 2018) shows that MIPAS O3 has a positive bias of  10 % at 50–75 km and agrees with other instruments over 75–90 km to within 10 % at night-time and 10 %–20 % for daytime. Above 90 km, MIPAS daytime O3 agrees with other instruments to 10 %, but at night the positive bias increases from 10 % at 90 km to 20 % at 95–100 km. Daytime mesospheric O3 profiles derived from OSIRIS Infrared Imager observations of the 1.27 µm oxygen airglow band were found to have positive biases of up to 25 % below 75 km and up to 50 % at higher altitudes, compared to other instruments on the Odin satellite (Li et al., 2020).

O3 vertical profiles are derived from the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) infrared 9.6 µm emission and 1.27 µm daytime airglow channels. However, daytime O3 volume mixing ratio (VMR) from SABER 9.6 µm measurements is  20 %–50 % higher than other satellite instruments over the altitude range 60–80 km although night-time observations show better agreement with <10 % difference (Smith et al., 2013). Applying updated, lower night-time atomic O values to the SABER processing scheme confirms that SABER 9.6 µm daytime O3 is too large, with implications for inferred atomic hydrogen abundances (Mlynczak et al., 2018; Kulikov et al., 2019).

Ground-based millimetre-wave radiometry in the 110–250 GHz frequency range provides continuous measurements of O3 (e.g. Hartogh et al., 2004; Daae et al., 2014; Ryan et al., 2016) over the altitude range  20–75 km. Ground-based millimetre-wave measurements are of limited vertical resolution, typically  8 km at best, but can be compared with more highly resolved O3 profiles from overlapping balloon-borne ozonesonde observations and satellite measurements by considering the retrieval diagnostics (Ryan et al., 2016). At lower, microwave frequencies the 40,431,3 rotational transition of 16O3 (using the notation JKa,KcJKa′′,Kc′′′′ where J, Ka′, and Kc′ are the upper state rotational quantum numbers and J′′, Ka′′, and Kc′′ are the lower state rotational quantum numbers) gives rise to a weak atmospheric line centred at 11.072 GHz. The emission line is within the 10.70–12.75 GHz frequency range of Ku-band downlinks used for direct broadcast satellite services in Europe. This has allowed ground-based microwave radiometers operating at 11.072 GHz to be developed using commercially available Ku-band low-noise block (LNB) downconverters developed for satellite receivers (Rogers et al., 2009; Tenneti and Rogers, 2009). The atmosphere in the Ku-band (12–18 GHz) region is much less opaque than at 110–250 GHz, and Doppler broadening for the 11.072 GHz line is 10–23 times smaller, allowing O3 to be retrieved at altitudes above 75 km including the secondary O3 layer (Newnham et al., 2019). Low-cost radiometer instruments have been constructed and operated as part of “The Mesospheric Ozone System for Atmospheric Investigations in the Classroom” (MOSAIC) educational project. O3 partial columns for the lower mesosphere ( 50–80 km) and the upper mesosphere/lower thermosphere ( 80–100 km) have been determined using MOSAIC observations from mid-latitude sites and used to estimate seasonal O3 variability near the mesopause (Rogers et al., 2012).

1.3 This work

In this work we report new, ground-based 11.072 GHz microwave radiometer measurements of the polar mesosphere and lower thermosphere from a high-latitude location at Ny-Ålesund over 3 years, from 2017 to 2020. O3 vertical profiles are determined using established retrieval techniques and measurement uncertainties estimated. Seasonally averaged O3 profiles for night-time and twilight conditions are compared with the corresponding 9.6 µm SABER observations to investigate uncertainties and biases in the mesospheric O3 satellite dataset. Daytime mesospheric O3 abundances are too low to be measured using the Ku-band microwave technique. Instead, overlapping daytime and twilight SABER 9.6 and 1.27 µm satellite observations are compared to confirm previously reported differences between O3 derived from the two satellite infrared channels.

2 Methodology

The following sections describe the ground-based microwave radiometer configuration for observations of the Arctic polar atmosphere, the O3 profile retrieval, and the method used for selecting overlapping SABER data.

2.1 Ground-based ozone measurements

2.1.1 Instrument configuration

The Ny-Ålesund Ozone in the Mesosphere Instrument (NAOMI) is a development of the original MOSAIC 11.072 GHz O3 radiometer configuration of Rogers et al. (2009). For NAOMI, input signals in the frequency band 10.7–11.7 GHz are collected by a 60 cm diameter satellite TV reflector dish (Primesat “Easy Fit” EF60) and down-converted to the 950–1950 MHz output range using a dual LNB feedhorn (LNBF, Star Com Communications Ku-band twin model SR-3602). An antenna beam efficiency of 0.74 is incorporated in the O3 VMR retrieval. The beamwidth of the parabolic antenna, where microwave power is half (3 dB) of the maximum value, is estimated to be 3.2 at the target frequency of 11.072 GHz. The LNBF outputs are filtered (Mini-Circuits VHF-740 high-pass filter, typical passband 780–2800 MHz), to minimise out-of-band interference, and attenuated. Two software defined radio (SDR) receivers (Type RTL2832U with R820T) capture a 2.5 MHz bandwidth from each linear polarisation of the LNBF. Measuring both horizontal and vertical polarisation outputs of the LNBF gives a 2 improvement in signal-to-noise compared to measurements of a single polarisation. Frequency-switched spectra of the 11.072 GHz O3 line are acquired every 60 s using an Intel® Next Unit of Computing (NUC) minicomputer. The spectral data are comprised of 256 channels, each of width 2.44 kHz, giving a total frequency bandwidth of 0.625 MHz. Frequency calibration is performed by measuring the frequency harmonic at 11.070 GHz generated by a 10 MHz oven crystal oscillator.

2.1.2 NAOMI observations

Ground-based atmospheric observations using NAOMI are made from the UK Arctic Research Station (latitude 78550′′ N, longitude 115559′′ E) at Ny-Ålesund, Spitsbergen, which is part of the Svalbard archipelago. NAOMI observations have been made from this site since 4 July 2017. The antenna assembly is mounted on the external wall of a building at a height approximately 2 ma.g. A clear, unobscured sky view is obtained with the antenna pointing at 11 elevation and azimuthal angle of 345, with the line-of-sight NAOMI view shown in Fig. 1. Transformation of local azimuth-elevation-range (AER) spherical coordinates for NAOMI to geodetic coordinates, specified by latitude, longitude, and altitude, used the World Geodetic System 1984 (WGS 84) reference ellipsoid. Pointing the instrument towards the north minimises pickup of interfering signals from geostationary satellites at low to mid-latitudes. Detected microwave signals from non-atmospheric sources such as satellites could lead to errors in the O3 retrieval or, in a worst case, obscure the 11.072 GHz emission line.

https://amt.copernicus.org/articles/15/2361/2022/amt-15-2361-2022-f01

Figure 1Map of Svalbard and the Arctic region poleward of geographic latitude 76 N and from 30 W to 40 E. The black circle shows the NAOMI ground-based location (78550′′ N, 115559′′ E). The black line is the projection of the line-of-sight view of NAOMI at elevation angle 11 and azimuth 345. The dashed purple box shows the region ± 20 longitude and ± 5 latitude of the NAOMI intercept at altitude 90 km (821657′′ N, 5650′′ E) used for selecting overlapping SABER observations. The filled, coloured circles show the locations and SZAs of SABER observations within the dashed purple box during night-time conditions (SZA at altitude 90 km> 110) in the 2017–2018 winter (i.e. 29 December 2017–16 February 2018).

NAOMI data were binned according to the local solar zenith angle (SZA) at 90 km into night-time (SZA > 110), twilight (75 SZA  110), and daytime (SZA < 75) observations. Binned O3 records between 15 August 2017 and 15 March 2020 were averaged for the following three periods: 15 December–15 March, 15 April–15 July, and 15 August–15 November. The 3-month periods, hereafter identified as “winter”, “summer”, and “autumn”, respectively, were chosen to overlap the SABER 60 d yaw cycles rather than matching meteorological definitions of the seasons. In all cases the NAOMI measurements selected for averaging occurred within 3 h of the selected SABER observation times (see Sect. 2.2), as well as meeting the SZA criteria at 90 km. NAOMI data were not recorded from 26 September to 14 November 2019 due to a temporary instrument fault. Averaging a smaller subset of valid observations between 29 August and 25 September 2019 produces an O3 spectrum with poorer signal to noise compared to a complete autumn dataset but is included in the analysis for completeness.

Differing seasonal meteorology has been assessed (Newnham et al., 2019) to have little impact on Ku-band microwave observations such as those made by NAOMI in polar conditions, even when viewing the atmosphere at shallow angles such as 11 elevation. Therefore, we do not expect varying tropospheric water vapour content to significantly affect the measurements and averaging process. Heavy precipitation during poor weather conditions could potentially affect the measurements and attenuate the mesospheric O3 emission signal through microwave absorption and scattering. In future, screening for such weather events and removal of affected microwave data could yield improvements in the data quality.

2.1.3 NAOMI ozone retrieval

Mesospheric O3 profiles were retrieved from the NAOMI observations using version 2.2.58 of the Atmospheric Radiative Transfer Simulator (ARTS) (available at http://www.radiativetransfer.org/, last access: 8 August 2016) (Buehler et al., 2005, 2018; Eriksson et al., 2011) and the Qpack2 (a part of atmlab v2.2.0) software package (Eriksson et al., 2005) using the optimal estimation method (OEM) (Rodgers, 2000). The configuration of ARTS/Qpack2 for optimal estimation retrieval in the Ku-band region was described in Newnham et al. (2019), and specific details of the O3 retrieval from NAOMI observations are given here. Adjusted parameters were O3 VMR, frequency shift, and baseline slope. The Planck formalism was used for calculating brightness temperatures and atmospheric transmittance. Spectroscopic line parameters for ozone (O3), hydroxyl radical (OH), water vapour (H2O), molecular nitrogen (N2), molecular oxygen (O2), and carbon dioxide (CO2) were taken from the high-resolution transmission (HITRAN) molecular absorption database (Gordon et al., 2017). For all molecules except OH the Kuntz approximation (Kuntz, 1997) to the Voigt line shape with a Van Vleck–Huber prefactor (Van Vleck and Huber, 1977) and a line cut-off of 750 GHz was used, which is valid for the pressures considered. The water vapour continuum parameterisation used the Mlawer–Tobin Clough–Kneizys–Davies (MT-CKD) model (version 2.5.2), which includes both foreign and self-broadening components (Mlawer et al., 2012). Collision-induced absorption (CIA) is the main contribution to the dry continua in the microwave range, and therefore the CIA parameterisations from the MT-CKD model (Clough et al., 2005) (version 2.5.2 for N2 and CO2 and version 1.0 for O2) were applied. Diagonal elements in the covariance of the O3 VMR profiles were fixed to 1.5 ppmv. The off-diagonal elements of the covariance linearly decrease with a correlation length of a fifth of a pressure decade (approximately 3 km).

Vertical profiles of O3 VMR were calculated using a 10-year dataset from WACCM-D (Verronen et al., 2016) covering 2000–2009. WACCM-D is a 3-D global atmospheric model that incorporates a detailed representation of D-region chemistry in the specified dynamics (SD) version of the Whole Atmosphere Community Climate Model (WACCM 4) (Marsh et al., 2013). The WACCM-D data at 78.632 N and 12.500 E, the model grid point closest to Ny-Ålesund, were used. Water vapour (H2O) VMR profiles were a combination of 6 hourly, model level Modern-Era Retrospective analysis for Research and Applications, Version 2 (MERRA-2) data (download date: 18 April 2020) and WACCM-D data. MERRA-2 H2O data were selected at pressure levels below 10−2hPa overlapping NAOMI observations, for the reanalysis grid point at latitude 79.000 N and longitude 11.875 E closest to the instrument location and combined with WACCM-D data for higher altitudes (i.e. at pressures below 10−2hPa). Similarly, temperature profiles were constructed by combining MERRA-2 data at atmospheric levels below 10−2hPa, SABER version 2.0 data (downloaded from http://data.gats-inc.com/saber/custom/Temp_O3_H2O/v2.0/, last access: 30 April 2020) between 10−2 and 10−4hPa, and WACCM-D data at pressures below 10−4hPa. The inclusion of SABER data provides more realistic mesospheric temperatures than WACCM-D averages, in particular following the sudden stratospheric warmings of 12 February 2018 and 2 January 2019 when mesospheric temperatures decreased by up to 40 K.

2.2 SABER ozone data

SABER version 2.0 temperature, O3 VMR, and water vapour VMR profiles (downloaded from ftp://saber.gats-inc.com/custom/Temp_O3_H2O/v2.0/, last update: 30 April 2020) were used in the analysis. SABER profiles were selected where the tangent point at 90 km is within ± 20 longitude and ± 5 latitude of the calculated NAOMI measurement co-ordinates (8216'57′′ N, 56'50′′ E). The 90 km altitude is chosen as it is the approximate mesopause height and below the secondary O3 VMR maximum. The locations of night-time SABER profiles for the 2017–2018 winter are shown in Fig. 1. The SABER observations overlap the NAOMI line-of-sight path and are more tightly clustered towards the northerly extent of 83.5 N. The SABER observations in the defined region were then binned and averaged into night-time, twilight, and daytime datasets within the defined winter, summer, and autumn periods, as was done for the NAOMI data (Sect. 2.1.2). The SZAs at 90 km for the binned regions, plotted in Fig. 2, show that daytime SABER observations are restricted to the summer periods and the start of autumn, whereas night-time measurements occur at the end of autumn and during winter.

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Figure 2SZA of SABER observations at 90 km altitude with spatial overlap of the NAOMI measurements. The plotted SABER observations, covering the period from 27 March 2017 to 5 April 2020, are a subset of the full SABER dataset. SABER observations during night-time (SZA at altitude 90 km> 110), twilight (75 SZA at altitude 90 km 110), and daytime conditions (SZA at altitude 90 km< 75) are shown by blue “+” symbols, purple triangles, and red circles, respectively. Red, orange, and blue shaded regions indicate nominal summer (15 April–15 July), autumn (15 August–15 November), and winter (15 December–15 March) periods, respectively. The grey horizontal bars show the periods when NAOMI observations were made.

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3 Results

The NAOMI O3 vertical profile retrieval and estimated uncertainties are presented and discussed in Sect. 3.1, using the 2017–2018 winter night-time case as an example. The NAOMI and SABER 9.6 µm O3 vertical profiles for winter night-time, winter twilight, and autumn twilight periods are compared in Sect. 3.2. SABER 9.6 and 1.27 µm observations overlap in the region of the NAOMI measurements during summer daytime and twilight conditions in summer and autumn, and the selected portions of the satellite datasets during 2017, 2018, and 2019 are compared in Sect. 3.3.

https://amt.copernicus.org/articles/15/2361/2022/amt-15-2361-2022-f03

Figure 3Ozone (O3) retrieval for NAOMI observations during 2017–2018 winter night-time (29 December 2017–16 February 2018, SZA at altitude 90 km> 110) conditions. The seasonal mean O3 spectrum and retrieval fit is shown in (a), and the residual differences are shown in (b). The a priori and retrieved O3 volume mixing ratio (VMR) profiles are shown in (c), where the green shading represents the a priori uncertainty (± 1.5 ppmv). The medium blue and light blue shading show the profiles of O3 VMR ± measurement uncertainty (σobs) and O3 VMR ± total uncertainty (σtot), respectively. In (d) every sixth averaging kernel is shown and in (e) the measurement response (MR), with the vertical grey dashed line showing the cut-off for MR  0.8. Panel (f) shows the full-width half maxima of each averaging kernel (AVK FWHM). The measurement uncertainty (σobs) and total uncertainty (σtot) are shown in (g) and (h), respectively. The grey shaded regions and thicker sections of the plotted curves in (c–h) indicate the pressure and altitude ranges where MR  0.8.

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3.1 Ozone retrieval

Ozone retrievals were performed for the winter and autumn night-time, and autumn twilight, periods where mesospheric O3 abundances were higher than during sunlit conditions. The retrieval results for the seasonally averaged 2017–2018 winter night-time NAOMI spectrum are shown in Fig. 3. Figure 3a compares the final retrieval fit (red line) with the measured O3 spectrum (black line), with the root mean square (rms) noise of the residual differences having the same value (2.4 mK) as the RMS baseline noise level of the seasonally averaged NAOMI spectrum. Figure 3c shows the retrieved (red line) and a priori (dashed green line) O3 VMR profiles, the a priori uncertainty (green shading), the measurement uncertainty (medium blue shading), and the total uncertainty (light blue shading). The retrieval altitude range, where information is obtained from the observations, is indicated by the thicker solid lines and shaded grey areas and is determined as described in the next paragraph. Outside of the retrieved altitude range the O3 VMRs approach the a priori values.

The averaging kernels (AVKs) for every sixth retrieved altitude are shown in Fig. 3c. The AVKs describe the relationship between the true, a priori, and retrieved atmospheric states (Rodgers, 2000) and can be used to indicate the altitudes over which O3 is observed and the height resolution. The sum of the AVKs at each altitude is the measurement (or total) response (MR), which represents the contribution of the measurement to the retrieval solution compared to the a priori influence at that altitude (Christensen and Eriksson, 2013). The altitude range where the retrieved O3 profile has a high degree of independence from the a priori is identified by MR values higher than 0.8. The retrieval pressure (altitude) range where the MR 0.8 criterion is met is 9 × 10−4–0.13 hPa ( 97–62 km), shown by the thicker sections of the lines and the shaded grey areas in Fig. 3b–g. Outside of these altitudes (i.e. below 62 km and above 97 km) MR is < 0.8 and O3 values should be interpreted with caution as the information from the a priori becomes important. In the ideal case the AVKs would be delta functions, but in practice they are peaked functions with finite widths dependent on the spatial resolution of the observing system. The full-width half-maximum (FWHM) widths of the kernels provide a measure of the vertical resolution of the retrieved profile. The FWHM values shown in Fig. 3e indicate the altitude resolution is worst at 18.0 km at  90 km and improves with decreasing altitude to 10.9 km at 62 km in the lower mesosphere. The altitude resolution can also be estimated from the degrees of freedom for signal (DOFS) for the inversion, given by the trace of the AVK matrix (Rodgers, 2000; Ryan and Walker, 2015). Dividing the retrieved altitude range ( 35 km) by the DOFS ( 2.9) over the same range gives an altitude resolution of 12.1 km, within the range of AVK FWHM values.

Observation errors (σobs) and total retrieval (observation plus smoothing) errors (σtot) from the OEM retrievals provide further estimates of the retrieved profile uncertainty. The observation errors describe how the retrieved profiles are affected by measurement noise and are shown in Fig. 3f, with mean value 0.32 ppmv. Observation errors decrease above and below the AVK peaks as the retrieval tends towards the a priori and the measurement contribution is small in these regions. The total retrieval errors shown in Fig. 3g are in the range 1.09–1.33 ppmv, with mean value 1.17 ppmv, and tend towards the a priori uncertainty of 1.5 ppmv outside the range of AVK peaks.

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Figure 4Jacobian matrix describing the NAOMI ozone (O3) retrieval, normalised by the layer thickness of the retrieval grid. The data are for observations during 2017–2018 winter night-time (29 December 2017–16 February 2018, SZA at altitude 90 km> 110). Rows of the Jacobian matrix for selected altitude levels are plotted in (a). The grey scale in (b) indicates the values of the Jacobian matrix.

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The values of the Jacobian matrix of the O3 forward model, normalised by the layer thickness of the retrieval grid, are shown in Fig. 4. Normalised Jacobian values close to the centre of the 11.072 GHz emission line are in the range 0.4–0.5 mK(ppmv)-1km-1 at mesospheric altitudes 60–90 km. At higher altitudes, above 90 km, the gain response is weaker and spread over a narrow range of frequencies due to negligible pressure broadening of the emission line.

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Figure 5Estimated uncertainties in the ozone (O3) retrieval for NAOMI observations during winter 2017–2018 night-time (29 December 2017–16 February 2018, SZA at altitude 90 km> 110). Absolute O3 VMR uncertainties are shown in (a) and relative (%) uncertainties in (b). The grey shaded regions indicate the pressure and altitude ranges where MR  0.8.

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Contributions to uncertainties in the O3 retrieval were determined by comparing the night-time, 2017–2018 winter profiles from separate runs where input parameters were perturbed from their nominal values in turn. The adjusted parameters were brightness temperature calibration (Tb ± 10 % for all observed frequencies), air broadening coefficient of the O3 line (γair± 5 %), O3 line intensity (S± 2 %), and observation zenith angle (nominal ZA ± 2). A priori O3 VMR values were scaled by 0.5 and 2.0 at all pressure levels, and the temperature profile perturbed by ± 5 K. The differences between the retrieved O3 profiles from the perturbed and nominal runs are shown in Fig. 5a and b as absolute VMR (ppmv) and percentage uncertainties, respectively. The uncertainty contributions are within the envelope of total retrieval uncertainty, shown by the red shading, over the range of retrieved altitudes. The largest absolute error of ± 0.80 ppmv at  90–95 km is from the estimated 10 % radiometric calibration error, followed by zenith angle and O3 a priori uncertainties above 80 km. The largest percentage uncertainties, exceeding 94 %, are at  62 and 80 km where the VMR is close to zero.

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Figure 6Mean ozone vertical profiles from NAOMI and SABER 9.6 µm observations during winter night-time (within 15 December–15 March, SZA at altitude 90 km> 110) in 2017–2018 (a–d), 2018–2019 (e–h), and 2019–2020 (i–l). The second and third columns give the absolute and relative (%) differences (NAOMI minus SABER 9.6 µm). The red, blue, and purple shading are the estimated uncertainties of the plotted parameters. The grey shaded regions and thicker sections of the plotted curves indicate the pressure and altitude ranges where MR  0.8.

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https://amt.copernicus.org/articles/15/2361/2022/amt-15-2361-2022-f07

Figure 7Mean ozone vertical profiles from NAOMI and SABER 9.6 µm observations during winter twilight (within 15 December–15 March, 75 SZA at altitude 90 km 110) in 2017–2018 (a–d), 2018–2019 (e–h), and 2019–2020 (i–l). The second and third columns give the absolute and relative (%) differences (NAOMI minus SABER 9.6 µm). The red, blue, and purple shading are the estimated uncertainties of the plotted parameters. The grey shaded regions and thicker sections of the plotted curves indicate the pressure and altitude ranges where MR  0.8.

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https://amt.copernicus.org/articles/15/2361/2022/amt-15-2361-2022-f08

Figure 8Mean ozone vertical profiles from NAOMI and SABER 9.6 µm observations during autumn twilight (within 15 September–15 November, 75 SZA at altitude 90 km 110) conditions in 2017 (a–d), 2018 (e–h), and 2019 (i–l). The second and third columns give the absolute and relative (%) differences (NAOMI minus SABER 9.6 µm). The red, blue, and purple shading are the estimated uncertainties of the plotted parameters. The grey shaded regions and thicker sections of the plotted curves indicate the pressure and altitude ranges where MR  0.8.

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Figure 9Mean ozone partial columns at 62–80 km (a–c), 80–98 km (d–f), and 62–98 km (g–i) from NAOMI and SABER 9.6 µm observations during night-time winter (left column), winter twilight (centre column), and autumn twilight (right column) conditions in 2017–2020. The error bars are the estimated uncertainties of the plotted parameters. Note that the partial column scales for the upper (a–c), middle (d–f), and lower (g–i) panel plots differ.

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3.2 Comparison of NAOMI and SABER mesospheric ozone profiles

The O3 vertical profiles for winter night-time, winter twilight, and autumn twilight periods where the NAOMI and SABER 9.6 µm datasets overlap are shown in Figs. 6–8, respectively. The seasonal mean SABER profiles were smoothed using the NAOMI AVK's for direct comparison with the ground-based observations, and absolute VMR and percentage differences calculated. O3 number densities were calculated from the NAOMI and SABER 9.6 µm O3 VMR profiles using pressures and temperatures from the combined MERRA-2, SABER, and WACCM-D profiles constructed for the NAOMI retrievals. The number densities were integrated to determine the O3 partial columns over altitudes 62–80, 80–98 km, and the full NAOMI retrieval range of 62–98 km as shown in Fig. 9.

Table 1Secondary and tertiary ozone peak VMR and altitudes from NAOMI and SABER 9.6 µm observations during winter night-time (within 15 December–15 March, SZA at altitude 90 km> 110) for 2017–2018, 2018–2019, and 2019–2020. ± figures after the VMR values are uncertainties.

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The night-time O3 VMR profiles for the 2017–2018, 2018–2019, and 2019–2020 winters are compared in Fig. 6 and Table 1. For NAOMI the uncertainties are total error (σtot) from the O3 retrievals at the peak altitude and for SABER the estimated uncertainties are 20 % of the peak VMR. For both NAOMI and SABER data, the secondary O3 peak VMR values are higher in the 2017–2018 and 2019–2020 winters than in 2018–2019. For NAOMI, the highest secondary maximum is 10.7 ± 1.3 ppmv for the 2019–2020 winter compared to 8.3(13) ppmv for the previous, 2018–2019 winter. The tertiary maxima are similar for each of the three winters, but the tertiary O3 layers from NAOMI are narrower than those measured by SABER and more sharply peaked with maximum VMR 31 %–52 % higher. The tertiary and secondary maxima in the NAOMI VMR profiles are at 69–70 and 93–94 km, respectively, 1–2 km lower in altitude than SABER. The largest percentage differences occur at  64 and 80 km due to very low (< 0.2 ppmv) O3 VMR at these altitudes.

Table 2Secondary and tertiary ozone peak VMR and altitudes from NAOMI and SABER 9.6 µm observations during winter twilight (within 15 December–15 March, 75 SZA at altitude 90 km 110) for 2017–2018, 2018–2019, and 2019–2020. ± figures after the VMR values are uncertainties.

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Table 3Secondary and tertiary ozone peak VMR and altitudes from NAOMI and SABER 9.6 µm observations during autumn twilight (within 15 September–15 November, 75 SZA at altitude 90 km 110) in 2017 and 2018. ± figures after the VMR values are uncertainties.

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The average O3 profiles for the three twilight winters, presented in Fig. 7 and Table 2, show a similar pattern to the night-time winters with secondary O3 peak VMR values higher in the 2017–2018 and 2019–2020 winters than in 2018–2019. However, the secondary maximum VMRs for winter twilight are 6 %–26 % smaller, apart from the SABER 2018–2019 twilight peak, which is 8 % larger than the corresponding night-time value. The most significant differences between NAOMI and SABER observations are found in the autumn twilight O3 profiles (Fig. 8 and Table 3) at secondary layer altitudes in the range 88–97 km. For the two years 2017 and 2018, where the most complete autumn twilight measurements are available, the NAOMI secondary maximum VMRs are 47 % and 59 % of the SABER peak values, respectively. The largest differences are at altitudes above 88 km, in the secondary O3 layer, whereas below 88 km the NAOMI and SABER profiles agree to within the measurement uncertainties. The 2019 autumn twilight profiles show even larger differences with no secondary O3 peak in the NAOMI profile. The differences for the 2019 dataset may be due to the shorter period (29 August–25 September) of NAOMI measurements compared to the previous 2 years (2 September–3 November 2017 and 31 August–1 November 2018). As well as lower signal to noise in the integrated NAOMI spectra affecting the O3 retrieval, during the earlier autumn 2019 period more of the NAOMI observations would have occurred in sunlit conditions (mean SZA 88.6 at 90 km) compared to SABER (mean SZA 90.3 at 90 km), potentially affecting mesospheric O3 abundances.

The differences between NAOMI and SABER appear more distinct in the higher O3 number densities below  80 km. NAOMI number density profiles show a distinct tertiary peak at  70 km, whereas the SABER densities increase more uniformly with decreasing altitude from 78 to 62 km. However, the differences between NAOMI and SABER largely disappear when the number densities over 62–80 km are integrated to produce partial columns, suggesting that the limited height resolution ( 11–13 km) of the NAOMI retrieval is a significant factor in the profile shape over this 18 km altitude range.

https://amt.copernicus.org/articles/15/2361/2022/amt-15-2361-2022-f10

Figure 10Mean ozone vertical profiles from SABER 9.6 and 1.27 µm observations during (a–d) summer daytime (within 15 April–15 July, SZA at altitude 90 km< 75), (e–h) summer twilight (within 15 April–15 July, 75 SZA at altitude 90 km 110), and (i–l) autumn twilight (within 15 September–15 November, 75 SZA at altitude 90 km 110). The second and third columns give the absolute and relative (%) differences (SABER 9.6 µm minus SABER 1.27 µm).

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Table 4Secondary ozone peak VMR and altitudes from SABER 9.6 and 1.27 µm observations during summer daytime (15 April–15 July, SZA at altitude 90 km< 75), summer twilight (15 April–15 July, 75 SZA at altitude 90 km 110), and autumn twilight (15 September–15 November, 75 SZA at altitude 90 km 110). ± figures after the VMR values are uncertainties.

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The NAOMI and SABER O3 partial columns are shown in Fig. 9 for winter night and autumn night and twilight conditions in the different years. The columns over 62–80 km (Fig. 9a–c) are up to an order of magnitude higher than over 80–98 km (Fig. 9d–f) and are generally higher in the winter night and twilight cases (Fig. 9a–b, d–e and g–h) than in autumn twilight (Fig. 9c, f and i) where lower SZA conditions and correspondingly higher solar irradiance decrease middle atmospheric O3 abundance. Observations by the two instruments show a similar pattern of variability from year to year, with the highest O3 columns in the 2019–2020 winter. The columns measured by the two instruments agree to within the measurement uncertainties shown by the vertical error bars, apart from the 2018–2019 and 2019–2020 winter nights at 80–98 km and for the 2017 autumn twilight at 62–80 km. Over the full retrieved altitude range (62–98 km), the NAOMI column for the 2017 autumn twilight is 51 % smaller than the corresponding SABER measurement. The largest contribution to the difference is at 62–80 km (Fig. 9c), whereas the smaller columns over 80–98 km (Fig. 9f) are in good agreement as are the 2018 data (Fig. 9c, f, and i). The large discrepancy between the autumn 2017 NAOMI and SABER observations could be due to a significant spectrum baseline ripple during the initial months of NAOMI operation. This possible cause is also indicated by the larger deviation of NAOMI O3 number density, which is integrated to produce partial columns, from the smoothed SABER profile for 2017 (Fig. 8d) compared to 2018 (Fig. 8h). As indicated by the retrieval Jacobians (Fig. 4), smoothly varying offsets and distortions over the 0.625 MHz NAOMI spectral bandwidth will affect O3 retrieval for the lower mesosphere, whereas the narrow-band Gaussian signal corresponding to O3 emission above  80 km will be less affected.

3.3 SABER 9.6 µm and 1.27 µm ozone profiles

The overlapping O3 profile data from SABER 9.6 and 1.27 µm observations during daytime in summer and twilight in summer and autumn are compared in Fig. 10 and Table 4. The secondary O3 maximum from both SABER channels show a similar pattern, with larger peak VMR for all three cases in 2019 compared to the two previous years. However, SABER 9.6 µm O3 VMR consistently exceeds SABER 1.27 µm over 65–95 km with the largest difference (up to 58 %) during autumn twilight. On the other hand, SABER 9.6 µm O3 VMR over 48–65 km is consistently lower than SABER 1.27 µm in summer and autumn twilight and by as much as 50 % lower at  56 km in autumn twilight. The altitude of the secondary O3 maximum in O3 mixing ratio is 90–92 km during day and 95 km at night. The secondary maximum in VMR in the SABER 9.6 µm measurements is at 96–97 km,  1–2 km lower than the corresponding SABER 1.27 µm data.

4 Conclusions

Seasonal O3 vertical profiles in the Arctic polar mesosphere and lower thermosphere (MLT) region (altitude range 62–98 km) have been retrieved from ground-based Ku-band microwave (NAOMI) atmospheric observations from Ny-Ålesund during 2017–2020. The NAOMI observations show broadly the same year-to-year and seasonal O3 variabilities as overlapping satellite data (version 2.0) from the SABER 9.6 µm channel during night-time and twilight conditions. The winter night-time and twilight NAOMI and SABER 9.6 µm O3 VMR profiles agree, but differences in the secondary O3 region at 88–97 km during autumn twilight exceed the measurement uncertainties. The SABER secondary maximum VMR values are higher by 47 % and 59 %, respectively compared to NAOMI for the 2 years, 2017 and 2018, where autumn twilight measurements were made. Considering the two SABER infrared channels which measure O3 at different wavelengths and use different processing schemes, the autumn twilight SABER 9.6 µm O3 VMRs for the 3 years 2017–2019 are higher than the corresponding overlapping 1.27 µm measurements, with the largest difference of 58 % over the altitude range 65–95 km similar to that between SABER 9.6 µm O3 and the NAOMI observation. The SABER 9.6 µm O3 summer daytime mesospheric O3 VMR is also consistently higher than the 1.27 µm measurement. Our intercomparison between ground-based microwave observations and the two SABER O3 channels builds on a previous study (Smith et al., 2013) where SABER 9.6 µm mesospheric O3 showed good relative agreement with other satellite measurements (< 10 % difference), but daytime O3 over the altitude range 60–80 km was biased 20 %–50 % higher. Our new analysis of ground-based (NAOMI) observations and SABER datasets confirms the previously reported level of agreement between night-time SABER 9.6 µm mesospheric O3 and other satellite datasets but show that under twilight conditions the 9.6 µm observations of secondary O3 peak VMR are  50 % higher than both the SABER 1.27 µm and NAOMI measurements.

Possible reasons for the differences between mesospheric O3 measured by the SABER 9.6 µm channel and other satellite datasets have been discussed by Smith et al. (2013). Here, we consider these reasons and other potential causes for observational differences in the context of our NAOMI ground-based measurements and comparisons between the SABER 9.6 and 1.27 µm data products. The differences between observations can be categorised as those that occur due to systematic and random differences in coincident retrieved profiles and those caused by the different sampling by each instrument.

Our work uses the latest publicly available SABER v2.0 data products, whereas Smith et al. (2013) used the earlier v1.07 dataset. The v2.0 processing includes improved Level 1 radiance profile calibration and improvements to the Level 2 procedures used to retrieve mesospheric temperatures in non-local thermodynamic equilibrium conditions as well as updated atomic oxygen, atomic hydrogen, and chemical heating algorithms. More information on the SABER data processing and retrieval schemes can be found on the instrument website: http://saber.gats-inc.com (last access: 30 April 2020). The changes in the SABER v2.0 datasets should have improved the O3, water vapour, and temperature profiles used in our analysis. However, we observe similar differences in O3 above  60 km as the earlier study (Smith et al., 2013) using v1.07 data, suggesting that significant uncertainties remain in SABER mesospheric O3.

The SABER O3 processing schemes are complex and, despite recent improvements, the retrievals are highly dependent on knowledge of numerous photochemical and quenching rates. For the 9.6 µm O3 emission scheme, the SABER model includes spontaneous emission by over 340 radiative transitions, chemical pumping, collisional excitation, and quenching processes. The 1.27 µm measurement is known to be prone to errors when O3 concentration is changing rapidly, including during sunrise and sunset (Zhu et al., 2007). O3 abundances in the upper mesosphere are also sensitive to temperature and atomic oxygen transport, which can vary rapidly and locally due to sunlight and tidal effects and may amplify sampling differences between different observations. Smith et al. (2013) show that sampling differences between instruments can lead to substantially different vertical profile structures and seasonal variations even when coincident comparisons indicate good agreement. In our work, we have matched up co-located NAOMI and SABER observations in terms of overlapping geographic location, SZA, and local observation time. However, sampling differences between the ground-based and satellite instruments inevitably remain and contribute to the observed O3 differences. Continuous atmospheric measurements from ground-based instruments such as NAOMI offer a complementary approach to satellite data analysis. Further work is needed to investigate and minimise instrument sampling differences, in particular local time and location effects that may be sensitive to the diurnal cycle in SZA. Studies focusing on O3 profiles during twilight and summer daytime conditions, when observations show large differences, are needed to address current uncertainties in mesospheric O3.

Data availability

The processed NAOMI and SABER datasets (Newnham et al., 2022) used in this study are available from the UK Polar Data Centre (https://www.bas.ac.uk/data/uk-pdc/, last access: 22 March 2022; NERC, 2022). SABER data used in this study can be downloaded from http://data.gats-inc.com/saber/Version2_0/Level2A/ (last access: 30 April 2020; GATS, 2022). The presented data can be downloaded from https://doi.org/10.5285/19845e8e-d6ef-4f95-8961-4da60f8294d3 (last access: 2 February 2022; Newnham et al., 2022).

Author contributions

DAN performed the SABER and NAOMI data processing, O3 retrieval calculations, and co-ordinated the study. PTV provided atmospheric model data (WACCM-D) for the retrievals. WDJC and MAC assembled and tested the 11.072 GHz O3 spectrometer (NAOMI), deployed the instrument at Ny-Ålesund, and provided technical details. MK is a principal investigator for the Ny-Ålesund MOSAIC project and carried out instrument tests. AEER provided MOSAIC data acquisition code and instrument development support.

Competing interests

The contact author has declared that neither they nor their co-authors have any competing interests.

Disclaimer

Publisher's note: Copernicus Publications remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

Acknowledgements

The authors thank the ARTS and Qpack development teams and Peter J. Kirsch at BAS for assistance configuring and running the code. The SABER and GATS teams are acknowledged for making the satellite datasets available and the NASA Global Modeling and Assimilation Office for MERRA-2.

Financial support

This work has been supported by the UK's Natural Environment Research Council (NERC) Technologies Proof-of-Concept project “Satellite TV-based Ozone and OH Observations using Radiometric Measurements (STO3RM)” (grant no. NE/P003478/1) awarded to David A. Newnham. NAOMI testing and deployment was supported by the Royal Society Newton Fund project “The Effect of High-Energy Particle Precipitation from Space on the Earth’s Atmosphere” (grant no. NI150103) awarded to Michael Kosch and Mark A. Clilverd. Pekka T. Verronen was supported by Academy of Finland project “ICT-Solutions to Understand Variability of Arctic Climate (ICT-SUNVAC)” (grant no. 335555).

Review statement

This paper was edited by Jörg Gumbel and reviewed by two anonymous referees.

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Short summary
Ozone (O3) is an important trace gas in the mesosphere and lower thermosphere (MLT), affecting heating rates and chemistry. O3 profiles measured by the Ny-Ålesund Ozone in the Mesosphere Instrument agree with Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) for winter night-time, but autumn twilight SABER abundances are up to 50 % higher. O3 abundances in the MLT from two different SABER channels also show significant differences for both autumn twilight and summer daytime.