<?xml version="1.0" encoding="UTF-8"?> <!DOCTYPE article PUBLIC "-//NLM//DTD Journal Publishing with OASIS Tables v3.0 20080202//EN" "https://jats.nlm.nih.gov/nlm-dtd/publishing/3.0/journalpub-oasis3.dtd"> <article xmlns:xlink="http://www.w3.org/1999/xlink" xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:oasis="http://docs.oasis-open.org/ns/oasis-exchange/table" xml:lang="en" dtd-version="3.0" article-type="research-article"> <front> <journal-meta><journal-id journal-id-type="publisher">ACP</journal-id><journal-title-group> <journal-title>Atmospheric Chemistry and Physics</journal-title> <abbrev-journal-title abbrev-type="publisher">ACP</abbrev-journal-title><abbrev-journal-title abbrev-type="nlm-ta">Atmos. Chem. Phys.</abbrev-journal-title> </journal-title-group><issn pub-type="epub">1680-7324</issn><publisher> <publisher-name>Copernicus Publications</publisher-name> <publisher-loc>Göttingen, Germany</publisher-loc> </publisher></journal-meta> <article-meta> <article-id pub-id-type="doi">10.5194/acp-24-12925-2024</article-id><title-group><article-title>Upper-stratospheric temperature trends: new results from the Optical Spectrograph and InfraRed Imager System (OSIRIS)</article-title><alt-title>Upper-stratospheric temperature trends</alt-title> </title-group> <contrib-group> <contrib contrib-type="author" corresp="yes" rid="aff1"> <name><surname>Dubé</surname><given-names>Kimberlee</given-names></name> <email>kimberlee.dube@usask.ca</email> <ext-link>https://orcid.org/0000-0001-6103-5918</ext-link></contrib> <contrib contrib-type="author" corresp="no" rid="aff1"> <name><surname>Tegtmeier</surname><given-names>Susann</given-names></name> <ext-link>https://orcid.org/0000-0001-9206-3161</ext-link></contrib> <contrib contrib-type="author" corresp="no" rid="aff1"> <name><surname>Bourassa</surname><given-names>Adam</given-names></name> </contrib> <contrib contrib-type="author" corresp="no" rid="aff1"> <name><surname>Zawada</surname><given-names>Daniel</given-names></name> </contrib> <contrib contrib-type="author" corresp="no" rid="aff1"> <name><surname>Degenstein</surname><given-names>Douglas</given-names></name> </contrib> <contrib contrib-type="author" corresp="no" rid="aff2"> <name><surname>Randel</surname><given-names>William</given-names></name> <ext-link>https://orcid.org/0000-0002-5999-7162</ext-link></contrib> <contrib contrib-type="author" corresp="no" rid="aff3"> <name><surname>Davis</surname><given-names>Sean</given-names></name> <ext-link>https://orcid.org/0000-0001-9276-6158</ext-link></contrib> <contrib contrib-type="author" corresp="no" rid="aff4"> <name><surname>Schwartz</surname><given-names>Michael</given-names></name> <ext-link>https://orcid.org/0000-0001-6169-5094</ext-link></contrib> <contrib contrib-type="author" corresp="no" rid="aff4"> <name><surname>Livesey</surname><given-names>Nathaniel</given-names></name> </contrib> <contrib contrib-type="author" corresp="no" rid="aff2"> <name><surname>Smith</surname><given-names>Anne</given-names></name> <ext-link>https://orcid.org/0000-0003-2384-5033</ext-link></contrib> <aff id="aff1"><label>1</label><institution>Institute of Space and Atmospheric Studies, University of Saskatchewan, Saskatoon, SK, Canada</institution> </aff> <aff id="aff2"><label>2</label><institution>NSF National Center for Atmospheric Research, Boulder, CO, USA</institution> </aff> <aff id="aff3"><label>3</label><institution>NOAA Chemical Sciences Laboratory, Boulder, CO, USA</institution> </aff> <aff id="aff4"><label>4</label><institution>Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA</institution> </aff> </contrib-group> <author-notes><corresp id="corr1">Kimberlee Dubé (kimberlee.dube@usask.ca)</corresp></author-notes><pub-date><day>21</day><month>November</month><year>2024</year></pub-date> <volume>24</volume> <issue>22</issue> <fpage>12925</fpage><lpage>12941</lpage> <history> <date date-type="received"><day>26</day><month>April</month><year>2024</year></date> <date date-type="rev-request"><day>2</day><month>May</month><year>2024</year></date> <date date-type="rev-recd"><day>12</day><month>September</month><year>2024</year></date> <date date-type="accepted"><day>3</day><month>October</month><year>2024</year></date> </history> <permissions> <copyright-statement>Copyright: © 2024 Kimberlee Dubé et al.</copyright-statement> <copyright-year>2024</copyright-year> <license license-type="open-access"><license-p>This work is licensed under the Creative Commons Attribution 4.0 International License. To view a copy of this licence, visit <ext-link ext-link-type="uri" xlink:href="https://creativecommons.org/licenses/by/4.0/">https://creativecommons.org/licenses/by/4.0/</ext-link></license-p></license></permissions><self-uri xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024.html">This article is available from https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024.html</self-uri><self-uri xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024.pdf">The full text article is available as a PDF file from https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024.pdf</self-uri> <abstract><title>Abstract</title> <p id="d2e184">Temperature trends in the upper stratosphere, particularly above <inline-formula><mml:math id="M1" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 45 km, are difficult to quantify due to a lack of observational data with high vertical resolution in this region that span multiple decades. The recent v7.3 upper-stratospheric (35–60 km) temperature data product from the Optical Spectrograph and InfraRed Imager System (OSIRIS) includes over 22 years of observations that can be used to estimate temperature trends. The trends in OSIRIS temperatures over 2005–2021 are compared to those from two other satellite limb instruments: Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) and Microwave Limb Sounder (MLS). We find that the upper stratosphere cooled by <inline-formula><mml:math id="M2" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 0.5 to 1 K per decade during this period. Results from the three instruments are generally in agreement. By merging the OSIRIS observations with those from channel 3 of the Stratospheric Sounding Unit (SSU), we find that the stratosphere cooled at a rate of approximately <inline-formula><mml:math id="M3" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>0.6 K per decade between 1979 and 2021 near 45 km, in agreement with earlier results based on SSU and MLS. The similarity between OSIRIS temperature trends and those from other records improves confidence in observed upper-stratospheric temperature changes over the last several decades.</p> </abstract> <funding-group> <award-group id="gs1"> <funding-source>Canadian Space Agency</funding-source> <award-id>21SUASULSO</award-id> </award-group> <award-group id="gs2"> <funding-source>National Aeronautics and Space Administration</funding-source> <award-id>80NM0018D004</award-id> </award-group> <award-group id="gs3"> <funding-source>National Aeronautics and Space Administration</funding-source> <award-id>80NSSC20K0928</award-id> </award-group> </funding-group> </article-meta> </front> <body> <sec id="Ch1.S1" sec-type="intro"> <label>1</label><title>Introduction</title> <p id="d2e217">A consequence of increasing anthropogenic greenhouse gas emissions is an altered thermal structure in the atmosphere, consisting of tropospheric warming and stratospheric cooling (e.g. <xref ref-type="bibr" rid="bib1.bibx24 bib1.bibx12" id="altparen.1"/>). Temperatures in the troposphere and lower stratosphere (below <inline-formula><mml:math id="M4" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 35 km) have been monitored for several decades by radiosondes <xref ref-type="bibr" rid="bib1.bibx13" id="paren.2"/> and satellites <xref ref-type="bibr" rid="bib1.bibx18 bib1.bibx26" id="paren.3"/>, and temperature changes in this region are well defined <xref ref-type="bibr" rid="bib1.bibx20 bib1.bibx12" id="paren.4"/>. At higher altitudes, above <inline-formula><mml:math id="M5" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 35 km, temperature observations are more limited, so there is uncertainty in the magnitude of the middle- and upper-stratospheric cooling rate <xref ref-type="bibr" rid="bib1.bibx12" id="paren.5"/>. New and updated temperature observations in the middle and upper stratosphere are necessary for better understanding the multidecadal cooling rate (cooling trend) and to more accurately quantify the impact of humanity on the climate. Considering middle- and upper-stratospheric cooling rather than just tropospheric warming increases the confidence that observed atmospheric temperatures are a direct result of human activities and not due to natural variability <xref ref-type="bibr" rid="bib1.bibx40" id="paren.6"/>.</p> <p id="d2e253">Most knowledge about temperatures above <inline-formula><mml:math id="M6" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 35 km comes from a series of nadir sounders that have operated on various National Oceanic and Atmospheric Administration (NOAA) satellites since late 1978 <xref ref-type="bibr" rid="bib1.bibx36 bib1.bibx33" id="paren.7"/>. Measurements are taken by three different instruments: the Stratospheric Sounding Unit (SSU), the Microwave Sounding Unit (MSU), and the Advanced Microwave Sounding Unit (AMSU-A). These instruments all have limited vertical resolution as temperatures are measured in different channels covering altitude ranges determined by their weighting functions <xref ref-type="bibr" rid="bib1.bibx33" id="paren.8"/>. Channels 2 and 3 of SSU and channels 13 and 14 of AMSU-A cover the range between <inline-formula><mml:math id="M7" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 35 and <inline-formula><mml:math id="M8" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 45 km, while MSU only has tropospheric and lower-stratospheric channels. Each individual SSU and AMSU-A data record is quite short, and it is necessary to merge measurements from multiple instruments before calculating multidecadal trends <xref ref-type="bibr" rid="bib1.bibx55" id="paren.9"/>. It is also necessary to merge the SSU observations with those from AMSU-A (or another instrument) when considering temperature trends over the full 4 decades from 1979 to the present: the last SSU instrument ceased operations in 2006, and the first AMSU-A instrument began operating in 1998 <xref ref-type="bibr" rid="bib1.bibx54" id="paren.10"/>.</p> <p id="d2e290">Satellite limb instruments are the best option available for retrieving temperature profiles that have a high (1–4 km) vertical resolution and extend into the upper stratosphere. Limb observations have been available since the end of the 20th century from an assortment of instruments. Datasets from a single instrument that extend for multiple decades, such as the Atmospheric Chemistry Experiment – Fourier transform spectrometer <xref ref-type="bibr" rid="bib1.bibx1 bib1.bibx2" id="paren.11"><named-content content-type="pre">ACE-FTS, Feb 2004–ongoing;</named-content></xref>, the Microwave Limb Sounder <xref ref-type="bibr" rid="bib1.bibx49 bib1.bibx43" id="paren.12"><named-content content-type="pre">MLS, Aug 2004–ongoing;</named-content></xref>, and the Sounding of the Atmosphere using Broadband Emission Radiometry instrument <xref ref-type="bibr" rid="bib1.bibx38 bib1.bibx37" id="paren.13"><named-content content-type="pre">SABER, Sept 2002–ongoing;</named-content></xref>, are best when considering atmospheric trends. <xref ref-type="bibr" rid="bib1.bibx34" id="text.14"/> also created a merged SSU+MLS data record covering 1979 to the present; however its vertical resolution is limited to that of the three SSU channels.</p> <p id="d2e311">Global mean temperature trends in merged SSU+AMSU-A and SSU+MLS datasets for the ozone recovery period (after <inline-formula><mml:math id="M9" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 1998) range from <inline-formula><mml:math id="M10" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>0.19 to <inline-formula><mml:math id="M11" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>0.5 K per decade (SSU channel 2) and from <inline-formula><mml:math id="M12" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>0.28 to <inline-formula><mml:math id="M13" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>0.6 K per decade (SSU channel 3) <xref ref-type="bibr" rid="bib1.bibx34 bib1.bibx35 bib1.bibx25 bib1.bibx45" id="paren.15"/>. The disparate time periods and latitude regions that were used make it difficult to compare the cooling rates from different studies directly, but in general the cooling rate is greater at higher altitudes, and including more recent years in the analysis (e.g. <xref ref-type="bibr" rid="bib1.bibx45" id="altparen.16"/>) results in a greater stratospheric temperature decrease per decade compared to older studies (e.g. <xref ref-type="bibr" rid="bib1.bibx35" id="altparen.17"/>).</p> <p id="d2e360">Here we focus on results from a new temperature retrieval in the middle and upper stratosphere (35–60 km) that was recently developed for the Optical Spectrograph and InfraRed Imaged System <xref ref-type="bibr" rid="bib1.bibx22 bib1.bibx52" id="paren.18"><named-content content-type="pre">OSIRIS;</named-content></xref>. OSIRIS has been in orbit on Odin since 2001, and the more than 22-year data record provides an excellent opportunity to study long-term cooling in the middle and upper stratosphere. In the first part of this work, OSIRIS temperature trends are compared to those from SABER and MLS. The observation-based temperature trends are also compared to temperature trends from several reanalyses and a climate model in order to assess the ability of models and data assimilation products to represent upper-stratospheric cooling. The second main goal of this work is to create a merged SSU+OSIRIS temperature product to complement the existing SSU+MLS and SSU+AMSU-A datasets <xref ref-type="bibr" rid="bib1.bibx34 bib1.bibx54" id="paren.19"/>. By merging more recent observations with those from SSU, which operated from 1979 to 2006, it is possible to look at changes in stratospheric temperatures over more than 4 decades. Considering each of the OSIRIS, MLS, and AMSU-A observations for the last 20 years of the record provides increased confidence in observed temperature trends during the 21st century.</p> </sec> <sec id="Ch1.S2"> <label>2</label><title>Data and models</title> <sec id="Ch1.S2.SS1"> <label>2.1</label><title>Satellite observations</title> <sec id="Ch1.S2.SS1.SSS1"> <label>2.1.1</label><title>OSIRIS</title> <p id="d2e393">The optical spectrograph component of OSIRIS measures limb-scattered sunlight between 280 and 810 nm, with a spectral resolution of approximately 1 nm. Each scan takes about 90 s, and there are 15 orbits per day, resulting in 100–400 vertical solar radiance profile measurements each day, depending on the time of year and the scanning mode.</p> <p id="d2e396">Temperature profiles are retrieved in a multi-stage fashion where the signals at 310 and 350 nm are used to estimate the Rayleigh scattering background number density, which can then be converted to temperature using hydrostatic balance and the ideal gas law. Similar techniques have been applied to measurements from the Global Ozone Monitoring by Occultation of Stars (GOMOS) instrument <xref ref-type="bibr" rid="bib1.bibx14" id="paren.20"/> and from the Ozone Mapping and Profiler Suite – Limb Profiler (OMPS-LP) <xref ref-type="bibr" rid="bib1.bibx4" id="paren.21"/>, among others. Limb scatter measurements can offer high signal levels with good vertical resolution; however the temperature inversion is subject to several biases partially from complexities in modelling the scattered signal. A detailed discussion of the technique, specifics of the OSIRIS v7.3 temperature data product, and expected biases are given in <xref ref-type="bibr" rid="bib1.bibx52" id="text.22"/>. The vertical resolution of the temperature profiles is 3.0–3.5 km, and the retrieval precision is 1–4 K.</p> <p id="d2e408">One notable source of bias in the OSIRIS temperature retrieval is stratospheric aerosol contamination of the measured radiances, limiting the useful range of the retrieved data product to <inline-formula><mml:math id="M14" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 35 km and higher. A second source of bias is the need of an external reference temperature near 65 km to initialize the hydrostatic balance integration. Two versions of the OSIRIS temperature product were developed in order to quantify this second source of bias: one that uses a value from the Modern-Era Retrospective analysis for Research and Applications, Version 2 <xref ref-type="bibr" rid="bib1.bibx8" id="paren.23"><named-content content-type="pre">MERRA-2;</named-content></xref>, interpolated to the OSIRIS profile as a reference temperature at 65 km, and one that uses climatological values from the NRLMSISE-00 model <xref ref-type="bibr" rid="bib1.bibx30" id="paren.24"/> as the reference temperature. The choice of reference temperature introduces a bias of up to 5 K at 65 km that decreases exponentially with decreasing altitude. This is the main source of uncertainty in the OSIRIS retrieval above 45 km <xref ref-type="bibr" rid="bib1.bibx52" id="paren.25"/>. The MERRA-2 version of the retrieval is more physically realistic as the climatology forces a trend of 0 K per decade at 65 km, so the MERRA-2-based OSIRIS retrieval is used as the default. The effect of the reference temperature choice on the OSIRIS temperature trends is discussed further in Sect. <xref ref-type="sec" rid="Ch1.S4"/>.</p> <p id="d2e431">Only the OSIRIS descending node profiles are used due to a drift in Odin's orbit that has resulted in a loss of ascending node measurements over the course of the mission. The descending node observations occur near a local solar time (LST) of 06:30. The data are further filtered by removing scans with a solar zenith angle greater than 85°. Monthly zonal means are then calculated for months with more than 15 measurements in a given 10° latitude and 1 km altitude bin. Months with fewer profiles typically occur when OSIRIS resumes taking measurements after being in darkness (i.e. following the winter at mid- and high latitudes).</p> </sec> <sec id="Ch1.S2.SS1.SSS2"> <label>2.1.2</label><title>MLS</title> <p id="d2e442">MLS has been operating from the Aura satellite since August 2004 <xref ref-type="bibr" rid="bib1.bibx49" id="paren.26"/>. MLS observes microwave limb emissions, measuring <inline-formula><mml:math id="M15" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 3500 vertical profiles each day. Temperatures are retrieved near the O₂ spectral lines at 118 and 239 GHz <xref ref-type="bibr" rid="bib1.bibx21" id="paren.27"/>. The vertical resolution of the temperature profiles is 3 km at 30 hPa (<inline-formula><mml:math id="M17" display="inline"><mml:mo lspace="0mm">∼</mml:mo></mml:math></inline-formula> 25 km), and it decreases to 9 km at 0.1 hPa (<inline-formula><mml:math id="M18" display="inline"><mml:mo lspace="0mm">∼</mml:mo></mml:math></inline-formula> 65 km) <xref ref-type="bibr" rid="bib1.bibx43" id="paren.28"/>. Temperatures from version 5 of the MLS retrieval are used here. All profiles are filtered per the guidelines provided in <xref ref-type="bibr" rid="bib1.bibx21" id="text.29"/>. As MLS is retrieved on a native pressure grid, the profiles must be converted to a vertical altitude grid before comparison with OSIRIS. This is done using the geopotential height (GPH) profiles that are retrieved along with each MLS temperature profile to calculate the geometric height of each pressure level and then interpolating to the 1 km OSIRIS altitude grid.</p> </sec> <sec id="Ch1.S2.SS1.SSS3"> <label>2.1.3</label><title>SABER</title> <p id="d2e496">SABER measures infrared CO₂ emissions from its platform on board the Thermosphere, Ionosphere, Mesosphere Energetics and Dynamics (TIMED) satellite. It has been in orbit since December 2001. Temperatures are retrieved between 10 and 100 km, with a vertical resolution of 2 km <xref ref-type="bibr" rid="bib1.bibx37" id="paren.30"/>. Profiles from version 2.0 of the SABER retrieval are used here. The SABER viewing mode is such that continuous coverage is only available from 52° S to 52° N, with higher latitudes observed for 60–63 d periods that alternate between the hemispheres <xref ref-type="bibr" rid="bib1.bibx37" id="paren.31"/>. To avoid any bias that this might introduce in the trends, we only use SABER observations from 50° S–50° N.</p> <p id="d2e514">Due to the sampling pattern, the SABER measurement time changes with each scan rather than observing near a fixed LST like OSIRIS and MLS. It takes approximately 60 d for SABER to observe the full 24 h cycle. This could introduce a bias when considering monthly mean temperatures as only half of the LSTs will be sampled. We tried accounting for this by using 30 d on either side of the 15th day of each month to calculate the monthly zonal means such that the full range of LSTs was included in the mean, as suggested by <xref ref-type="bibr" rid="bib1.bibx53" id="text.32"/>. It was found that the temperature trends were nearly the same whether regular monthly means (averaging from the first to last day of a month) or this more complicated technique was used, so only results for the regular monthly means are shown in Sect. <xref ref-type="sec" rid="Ch1.S4"/>.</p> </sec> <sec id="Ch1.S2.SS1.SSS4"> <label>2.1.4</label><title>SSU and AMSU-A</title> <p id="d2e530">The SSU and AMSU-A instruments were designed to be used for weather forecasting, but the global coverage and extensive length of the data record allows their observations to be used for climate-length trend studies. SSU is a three-channel radiometer that measures infrared CO₂ emissions <xref ref-type="bibr" rid="bib1.bibx27" id="paren.33"/>. The weighting functions of the channels peak near 30, 39, and 45 km and have vertical resolutions (calculated as the full width at half maximum) of 19, 17, and 15 km, respectively. SSU instruments were flown on numerous NOAA satellites between November 1978 and April 2006. We use the NOAA version 2 SSU temperature dataset developed by <xref ref-type="bibr" rid="bib1.bibx55" id="text.34"/>. This version of the data uses reprocessed temperatures retrieved from recalibrated radiances, which improved agreement between SSU observations taken from different spacecraft.</p> <p id="d2e548">AMSU-A measures molecular oxygen emissions between 50 and 58 GHz <xref ref-type="bibr" rid="bib1.bibx54" id="paren.35"/>. AMSU-A has higher vertical resolution than SSU. There are 15 channels, with channels 9–14 dedicated to measuring temperatures at approximately 18, 20, 25, 30, 35, and 40 km. Channels 13 and 14 each have a vertical resolution of around 12 km. Various iterations of AMSU-A have flown on NOAA, NASA, and MetOp spacecrafts since 1998. The process for combining these observations into a single record is described in <xref ref-type="bibr" rid="bib1.bibx47" id="text.36"/>.</p> <p id="d2e557">We also consider two merged stratospheric temperature datasets that use the SSU measurements. The SSU+AMSU-A dataset created by <xref ref-type="bibr" rid="bib1.bibx54" id="text.37"/> uses a merging process that combines information from multiple AMSU-A channels to weight the higher-resolution AMSU-A observations such that they match the three SSU channels. <xref ref-type="bibr" rid="bib1.bibx34" id="text.38"/> combined the SSU temperature observations with temperature retrieved from MLS. The much higher vertical resolution of MLS compared to SSU means that the MLS profiles can simply be weighted with the SSU weighting functions before using the overlap period to combine the datasets. <xref ref-type="bibr" rid="bib1.bibx34" id="text.39"/> and <xref ref-type="bibr" rid="bib1.bibx45" id="text.40"/> found that trends in the SSU+MLS record agreed with trends in SSU+AMSU-A temperatures within the regression uncertainties.</p> </sec> </sec> <sec id="Ch1.S2.SS2"> <label>2.2</label><title>Reanalyses and climate model</title> <p id="d2e581">The observed temperature trends are compared to reanalysis and model results to evaluate the ability of these systems to accurately represent changes in upper-stratospheric temperatures. The lack of temperature observations above 45 km (prior to <inline-formula><mml:math id="M21" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 2004) makes it particularly difficult to evaluate model simulations in this region.</p> <p id="d2e591">The three most up-to-date reanalyses are considered: MERRA-2, ERA5, and the Japanese 55-year Reanalysis (JRA-55). MERRA-2 is the latest reanalysis from the NASA Global Modelling and Assimilation Office (GMAO), based on the Goddard Earth Observing System (GEOS) model <xref ref-type="bibr" rid="bib1.bibx8" id="paren.41"/>. JRA-55 is produced by the Japan Meteorological Agency (JMA) <xref ref-type="bibr" rid="bib1.bibx19" id="paren.42"/>. ERA5 is the fifth generation reanalysis from the European Centre for Medium Range Weather Forecasting (ECMWF) <xref ref-type="bibr" rid="bib1.bibx15" id="paren.43"/>. ERA5, JRA-55, and MERRA-2 all assimilate radiances from SSU, MSU, and AMSU, as well as bending angles from GNSS-RO instruments <xref ref-type="bibr" rid="bib1.bibx8 bib1.bibx15 bib1.bibx19" id="paren.44"/>. MERRA-2 also assimilates MLS temperatures, which are included above 5 hPa beginning in August 2004 <xref ref-type="bibr" rid="bib1.bibx8" id="paren.45"/>. It should be noted that despite including many of the same observations, each reanalysis deals with the transitions between satellites and instruments in a different way. These transitions, along with changes in the reanalysis production streams, can create discontinuities that occur at different times in each reanalysis <xref ref-type="bibr" rid="bib1.bibx23 bib1.bibx7" id="paren.46"/>.</p> <p id="d2e613">A cold bias in the stratosphere exists in ERA5 between 2000 and 2006 <xref ref-type="bibr" rid="bib1.bibx44" id="paren.47"/>. This motivated the development of a corrected reanalysis for those years, called ERA5.1. For simplicity, when we refer to ERA5, we are actually referring to the combined ERA5 and ERA5.1 dataset. It should be noted that while ERA5.1 is generally an improvement, <xref ref-type="bibr" rid="bib1.bibx44" id="text.48"/> found that the combination of ERA5 and ERA5.1 does not perform as well as the previous generation reanalysis, ERA-Interim, with regards to upper-stratospheric temperatures for years prior to <inline-formula><mml:math id="M22" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 2010.</p> <p id="d2e629">The OSIRIS temperatures are retrieved on an altitude grid with 1 km spacing, so the reanalysis results must be converted to this same grid before doing any comparisons. First, reanalysis temperatures are interpolated to the latitude, longitude, and time of each OSIRIS profile. In the case of MERRA-2 we start with the 3-hourly temperature profiles on pressure levels and use the corresponding geopotential height to compute the geometric altitude corresponding to each pressure level for each profile. This relationship is then used to interpolate the temperature profiles to the OSIRIS altitude grid. For ERA5 we start with the hourly model-level results and calculate the geopotential height of each model level from the surface pressure, before computing the geometric altitude of each level and interpolating to the OSIRIS grid. For JRA-55 we use 6-hourly model-level results. The geopotential height on each model level is provided, so we only have to calculate the geometric altitude and interpolate to the OSIRIS profiles' locations and times. The same process is repeated for ERA5, JRA-55, and MERRA-2 but interpolated to the MLS profile locations and times so that we can determine the impact of the OSIRIS sampling on the resulting trends.</p> <p id="d2e633">In addition to the three reanalyses, we also consider temperature trends from simulations using the Whole Atmosphere Community Climate Model (WACCM) version 6 <xref ref-type="bibr" rid="bib1.bibx9" id="paren.49"/>. WACCM version 6 has 70 vertical levels extending from the surface to 140 km and a horizontal resolution of 0.95° latitude by 1.25° longitude. We consider four ensemble members from the free-running version of the model, covering the period 1960–2018 and following the REFD1 scenario. This scenario includes forcing from observed sea surface temperatures, greenhouse gases, ozone-depleting substances, and volcanic aerosol <xref ref-type="bibr" rid="bib1.bibx31" id="paren.50"/>. The quasi-biennial oscillation <xref ref-type="bibr" rid="bib1.bibx46" id="paren.51"><named-content content-type="pre">QBO;</named-content></xref> was nudged to match observations.</p> </sec> </sec> <sec id="Ch1.S3"> <label>3</label><title>Regression analysis</title> <p id="d2e656">A multiple linear regression (MLR) model is applied to monthly zonal mean observations in 10° latitude and 1 km altitude bins to study the long-term trends and variability in upper-stratospheric temperatures. The MLR model is defined as <disp-formula id="Ch1.E1" content-type="numbered"><label>1</label><mml:math id="M23" display="block"><mml:mtable rowspacing="0.2ex" class="split" displaystyle="true" columnalign="right left"><mml:mtr><mml:mtd><mml:mrow><mml:mi>T</mml:mi><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:mtd><mml:mtd><mml:mrow><mml:mspace linebreak="nobreak" width="0.25em"/><mml:mo>=</mml:mo><mml:mi mathvariant="italic">β</mml:mi><mml:mo>+</mml:mo><mml:msub><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">trend</mml:mi></mml:msub><mml:mo>×</mml:mo><mml:mtext>linear</mml:mtext><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo><mml:mo>+</mml:mo><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qboa</mml:mi><mml:mrow><mml:mo>(</mml:mo><mml:mn mathvariant="normal">2</mml:mn><mml:mo>)</mml:mo></mml:mrow></mml:msubsup><mml:mo>×</mml:mo><mml:msub><mml:mtext>QBO</mml:mtext><mml:mi>a</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:mtd></mml:mtr><mml:mtr><mml:mtd/><mml:mtd><mml:mrow><mml:mspace width="0.25em" linebreak="nobreak"/><mml:mo>+</mml:mo><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qbob</mml:mi><mml:mrow><mml:mo>(</mml:mo><mml:mn mathvariant="normal">2</mml:mn><mml:mo>)</mml:mo></mml:mrow></mml:msubsup><mml:mo>×</mml:mo><mml:msub><mml:mtext>QBO</mml:mtext><mml:mi>b</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo><mml:mo>+</mml:mo><mml:msub><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">solar</mml:mi></mml:msub><mml:mo>×</mml:mo><mml:msub><mml:mi>F</mml:mi><mml:mn mathvariant="normal">10.7</mml:mn></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo><mml:mo>+</mml:mo><mml:mi>R</mml:mi><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo><mml:mspace width="0.125em" linebreak="nobreak"/><mml:mo>,</mml:mo></mml:mrow></mml:mtd></mml:mtr></mml:mtable></mml:math></disp-formula> where each <inline-formula><mml:math id="M24" display="inline"><mml:mrow><mml:msub><mml:mi mathvariant="italic">β</mml:mi><mml:mi>i</mml:mi></mml:msub></mml:mrow></mml:math></inline-formula> defines a regression coefficient. The superscripts in Eq. (<xref ref-type="disp-formula" rid="Ch1.E1"/>) define the highest-order seasonal harmonic included for a term. Thus, the coefficient for the QBO<inline-formula><mml:math id="M25" display="inline"><mml:mrow><mml:msub><mml:mi/><mml:mi>a</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula> term is <disp-formula id="Ch1.E2" content-type="numbered"><label>2</label><mml:math id="M26" display="block"><mml:mtable rowspacing="0.2ex" class="split" displaystyle="true" columnalign="right left"><mml:mtr><mml:mtd><mml:mrow><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qboA</mml:mi><mml:mrow><mml:mo>(</mml:mo><mml:mn mathvariant="normal">2</mml:mn><mml:mo>)</mml:mo></mml:mrow></mml:msubsup></mml:mrow></mml:mtd><mml:mtd><mml:mrow><mml:mspace width="0.25em" linebreak="nobreak"/><mml:mo>=</mml:mo><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qboA</mml:mi><mml:mn mathvariant="normal">0</mml:mn></mml:msubsup><mml:mo>+</mml:mo><mml:munderover><mml:mo movablelimits="false">∑</mml:mo><mml:mrow><mml:mi>k</mml:mi><mml:mo>=</mml:mo><mml:mn mathvariant="normal">1</mml:mn></mml:mrow><mml:mn mathvariant="normal">2</mml:mn></mml:munderover></mml:mrow></mml:mtd></mml:mtr><mml:mtr><mml:mtd/><mml:mtd><mml:mrow><mml:mspace linebreak="nobreak" width="0.25em"/><mml:mfenced open="(" close=")"><mml:mrow><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qboA</mml:mi><mml:mrow><mml:mn mathvariant="normal">2</mml:mn><mml:mi>k</mml:mi><mml:mo>-</mml:mo><mml:mn mathvariant="normal">1</mml:mn></mml:mrow></mml:msubsup><mml:mi>sin⁡</mml:mi><mml:mspace width="0.125em" linebreak="nobreak"/><mml:mstyle displaystyle="true"><mml:mfrac style="display"><mml:mrow><mml:mn mathvariant="normal">2</mml:mn><mml:mi mathvariant="italic">π</mml:mi></mml:mrow><mml:mn mathvariant="normal">365.25</mml:mn></mml:mfrac></mml:mstyle><mml:mi>k</mml:mi><mml:mi>t</mml:mi><mml:mo>+</mml:mo><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qboA</mml:mi><mml:mrow><mml:mn mathvariant="normal">2</mml:mn><mml:mi>k</mml:mi></mml:mrow></mml:msubsup><mml:mi>cos⁡</mml:mi><mml:mspace width="0.125em" linebreak="nobreak"/><mml:mstyle displaystyle="true"><mml:mfrac style="display"><mml:mrow><mml:mn mathvariant="normal">2</mml:mn><mml:mi mathvariant="italic">π</mml:mi></mml:mrow><mml:mn mathvariant="normal">365.25</mml:mn></mml:mfrac></mml:mstyle><mml:mi>k</mml:mi><mml:mi>t</mml:mi></mml:mrow></mml:mfenced><mml:mspace width="0.125em" linebreak="nobreak"/><mml:mo>.</mml:mo></mml:mrow></mml:mtd></mml:mtr></mml:mtable></mml:math></disp-formula> <inline-formula><mml:math id="M27" display="inline"><mml:mrow><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qboB</mml:mi><mml:mrow><mml:mo>(</mml:mo><mml:mn mathvariant="normal">2</mml:mn><mml:mo>)</mml:mo></mml:mrow></mml:msubsup></mml:mrow></mml:math></inline-formula> is also expanded in the same way. There are 13 regression coefficients in total: three corresponding to the constant, trend, and <inline-formula><mml:math id="M28" display="inline"><mml:mrow><mml:msub><mml:mi>F</mml:mi><mml:mn mathvariant="normal">10.7</mml:mn></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula> terms in Eq. (<xref ref-type="disp-formula" rid="Ch1.E1"/>) and five coefficients from each of the QBO<inline-formula><mml:math id="M29" display="inline"><mml:mrow><mml:msub><mml:mi/><mml:mi>a</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula> and QBO<inline-formula><mml:math id="M30" display="inline"><mml:mrow><mml:msub><mml:mi/><mml:mi>b</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula> terms. The data are deseasonalized prior to applying the regression model, so there is no need to include regression terms for annual oscillations. The deseasonalization is done to monthly zonal mean data by subtracting the mean temperature of a given month from all values for that month for a specified latitude and altitude bin. Seasonal harmonics are nonetheless included for the QBO predictors, QBO<inline-formula><mml:math id="M31" display="inline"><mml:mrow><mml:msub><mml:mi/><mml:mi>a</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula> and QBO<inline-formula><mml:math id="M32" display="inline"><mml:mrow><mml:msub><mml:mi/><mml:mi>b</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula>, to account for coupling between the QBO and the seasonal cycle. It was found by <xref ref-type="bibr" rid="bib1.bibx6" id="text.52"/> that the MLR does not capture the full QBO signal in the mid-stratosphere when the seasonal harmonics are not included, even if the data have been deseasonalized, because the extratropical QBO signal is modulated by the annual cycle (e.g. <xref ref-type="bibr" rid="bib1.bibx11 bib1.bibx32" id="altparen.53"/>).</p> <p id="d2e1048">In Eq. (<xref ref-type="disp-formula" rid="Ch1.E1"/>), <inline-formula><mml:math id="M33" display="inline"><mml:mrow><mml:msub><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">trend</mml:mi></mml:msub></mml:mrow></mml:math></inline-formula> is the temperature trend in units of kelvin per decade, and <inline-formula><mml:math id="M34" display="inline"><mml:mrow><mml:msub><mml:mi>F</mml:mi><mml:mn mathvariant="normal">10.7</mml:mn></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula> is the solar flux at 10.7 cm. QBO<inline-formula><mml:math id="M35" display="inline"><mml:mrow><mml:msub><mml:mi/><mml:mi>a</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula> and QBO<inline-formula><mml:math id="M36" display="inline"><mml:mrow><mml:msub><mml:mi/><mml:mi>b</mml:mi></mml:msub><mml:mo>(</mml:mo><mml:mi>t</mml:mi><mml:mo>)</mml:mo></mml:mrow></mml:math></inline-formula> are the first two principal components of the monthly mean zonal winds between 300 and 10 hPa measured in Singapore. The MLR was also tested with terms representing the El Niño–Southern Oscillation and the aerosol optical depth; however these were found to play a negligible role in explaining the temperature variability between 35 and 60 km. Further details on the regression model, as well as the proxy data sources, are described in <xref ref-type="bibr" rid="bib1.bibx5" id="text.54"/>.</p> <p id="d2e1117">We only consider temperatures to the end of 2021 when calculating trends to avoid the influence of the Hunga Tonga–Hunga Ha'apai (HTHH) volcanic eruption, which significantly altered stratospheric temperatures throughout 2022 <xref ref-type="bibr" rid="bib1.bibx48 bib1.bibx50" id="paren.55"/>. As this occurred near the end of our dataset, it could skew the trend values by altering the end point. Including an aerosol optical depth proxy in the MLR is not adequate to account for the effects of HTHH as water vapour played a significant role in altering the dynamics and composition of the stratosphere following the eruption.</p> <p id="d2e1123">OSIRIS measures limb-scattered sunlight, so there are only observations available during daylight. This means that there are no data available when the measurement time of the descending node (local time of approximately 06:30) occurs during the night, i.e. at higher latitudes in the winter. In more recent years there are also some gaps in the monthly mean observations because the aging OSIRIS instrument does not have power for as much of each orbit as it used to. These months without OSIRIS measurements, which are different for each latitude bin, are removed from the MLS and SABER observations before applying the MLR in order to most directly compare trends in all three datasets. The effect on the trends of removing these points, as well as of the overall OSIRIS sampling pattern, is discussed in Sect. <xref ref-type="sec" rid="Ch1.S4"/>.</p> </sec> <sec id="Ch1.S4"> <label>4</label><title>Results</title> <sec id="Ch1.S4.SS1"> <label>4.1</label><title>Vertically resolved temperature trends</title> <p id="d2e1143">An initial validation of the OSIRIS temperature observations is provided in <xref ref-type="bibr" rid="bib1.bibx52" id="text.56"/>. MLS and OSIRIS temperatures were shown to agree within <inline-formula><mml:math id="M37" display="inline"><mml:mrow><mml:mo>±</mml:mo><mml:mn mathvariant="normal">5</mml:mn></mml:mrow></mml:math></inline-formula> K between 35 and 55 km, with some of the bias caused by differences in the measurement time of day. The OSIRIS and MLS time series also agree very well: Fig. <xref ref-type="fig" rid="Ch1.F1"/> shows the deseasonalized temperature anomalies for OSIRIS, MLS, and SABER in four example latitude and altitude bins. The variability is similar across all three datasets, and the correlations are greater than 0.5 in all bins and greater than 0.8 in most bins below 45 km (Appendix A, Fig. <xref ref-type="fig" rid="App1.Ch1.S1.F9"/>). MLS and SABER are more similar to one another than either is to OSIRIS: much of this difference is likely due to the sparser OSIRIS sampling pattern.</p> <fig id="Ch1.F1" specific-use="star"><label>Figure 1</label><caption><p id="d2e1165">Deseasonalized monthly zonal mean anomaly of OSIRIS, SABER, and MLS temperatures in four representative 10° latitude and 1 km altitude bins. Results are shown only for months when data from all three instruments are available.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f01.png"/> </fig> <p id="d2e1174">In the tropics the largest source of variability up to <inline-formula><mml:math id="M38" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 45 km is the QBO (Fig. <xref ref-type="fig" rid="Ch1.F1"/>b). At latitudes greater than <inline-formula><mml:math id="M39" display="inline"><mml:mrow><mml:mo>±</mml:mo><mml:mn mathvariant="normal">40</mml:mn></mml:mrow></mml:math></inline-formula>° the magnitude of the temperature anomalies peaks in the winter and lasts to the spring. Only the tail ends of these peaks, in September, are visible in Fig. <xref ref-type="fig" rid="Ch1.F1"/>c due to the lack of OSIRIS observations in the winter at 50° S. At this time of year there is significant interannual variability in the temperatures that does not get removed when deseasonalizing the data.</p> <p id="d2e1199">The MLR described in Sect. <xref ref-type="sec" rid="Ch1.S3"/> is used to determine temperature trends over 2005–2021 (2005 is the first full year when all three instruments were operating). Trends are calculated independently at each altitude (every 1 km from 34.5 to 59.5 km). The trends are shown in Fig. <xref ref-type="fig" rid="Ch1.F2"/>. Observations from each of MLS, SABER, and OSIRIS show stratospheric cooling during 2005–2021, ranging from about <inline-formula><mml:math id="M40" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>0.5 to <inline-formula><mml:math id="M41" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>1.5 K per decade. OSIRIS observations have the greatest cooling in the Southern Hemisphere (SH) and tropics, while SABER observations show the greatest cooling in the Northern Hemisphere (NH). Despite this difference, the OSIRIS and SABER temperature trend profiles (Fig. <xref ref-type="fig" rid="Ch1.F2"/>d to h) have a similar vertical structure, particularly in the tropics (Fig. <xref ref-type="fig" rid="Ch1.F2"/>f). When considering the larger latitude bins, OSIRIS and SABER temperature trends agree within the regression uncertainty everywhere except at 50 km and above 56 km in the 30–10° S bin.</p> <fig id="Ch1.F2" specific-use="star"><label>Figure 2</label><caption><p id="d2e1227">Temperature trends for 2005–2021. Trends are shown for <bold>(a)</bold> MLS, <bold>(b)</bold> SABER, and <bold>(c)</bold> OSIRIS. Hatching denotes statistically insignificant trends at the 2<inline-formula><mml:math id="M42" display="inline"><mml:mi mathvariant="italic">σ</mml:mi></mml:math></inline-formula> level. The bottom row, panels <bold>(d)</bold> to <bold>(h)</bold>, shows vertical profiles comparing the same trends from the three instruments in 20° latitude bins. The shaded regions denote the 2<inline-formula><mml:math id="M43" display="inline"><mml:mi mathvariant="italic">σ</mml:mi></mml:math></inline-formula> uncertainty in the MLR.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f02.png"/> </fig> <p id="d2e1266">The MLS temperature trends agree with those from OSIRIS and SABER in the tropics, but at higher latitudes the MLS trends oscillate in altitude (Fig. <xref ref-type="fig" rid="Ch1.F2"/>d and h): at the stratopause (48–50 km) the MLS cooling rate is <inline-formula><mml:math id="M44" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> <inline-formula><mml:math id="M45" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>1.5 K per decade, but the trend quickly drops to nearly 0 K per decade at 45 km before going back to <inline-formula><mml:math id="M46" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> <inline-formula><mml:math id="M47" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>1 K per decade at 40 km. The effect is more pronounced in the SH compared to the NH. The OSIRIS and SABER trends change very little between 40 and 50 km in either hemisphere. More work is required to determine if the vertical structure in the MLS trends is physical.</p> <p id="d2e1299">The MLR used to compute the temperature trends also includes terms for the QBO and the solar cycle. The regression coefficients corresponding to these terms for OSIRIS, SABER, and MLS are provided in Fig. <xref ref-type="fig" rid="App1.Ch1.S1.F10"/> in Appendix A. The QBO coefficients that are shown are the zeroth-order terms, <inline-formula><mml:math id="M48" display="inline"><mml:mrow><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qboA</mml:mi><mml:mn mathvariant="normal">0</mml:mn></mml:msubsup></mml:mrow></mml:math></inline-formula> and <inline-formula><mml:math id="M49" display="inline"><mml:mrow><mml:msubsup><mml:mi mathvariant="italic">β</mml:mi><mml:mi mathvariant="normal">qboB</mml:mi><mml:mn mathvariant="normal">0</mml:mn></mml:msubsup></mml:mrow></mml:math></inline-formula>. The coefficients are very similar for all three datasets. The solar cycle, represented by the <inline-formula><mml:math id="M50" display="inline"><mml:mrow><mml:msub><mml:mi>F</mml:mi><mml:mn mathvariant="normal">10.7</mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> solar flux proxy, has a positive impact on the temperature throughout the upper stratosphere as expected, as higher levels of solar irradiance lead to greater warming. The high values for the QBO coefficients in the SH are caused by the OSIRIS sampling pattern and not by a real physical phenomenon. OSIRIS only measures at higher latitudes in the SH for a few months of the year. When months without OSIRIS observations are not removed from MLS and SABER, the SH QBO coefficients for these two datasets look more similar to their NH counterparts (not shown here)</p> <p id="d2e1341">There are two main factors that introduce uncertainties into the OSIRIS temperature trends: the choice of the reference temperature used in the retrieval and the spatial and temporal sampling pattern. We quantify how the choice of reference temperature influences the trends by comparing the trends in OSIRIS temperatures retrieved using MERRA-2 to the trends in temperatures retrieved using NRLMSISE-00 reference temperatures. NRLMSISE-00 is a climatology, and there is no trend (0 K per decade trend) in the temperatures at the reference altitude of 65 km, even after interpolating to the OSIRIS profiles locations and times. Therefore the difference in the trends for the two OSIRIS retrieval versions shows how much MERRA-2 is contributing to the resulting OSIRIS temperature trend at each latitude and altitude (Fig. <xref ref-type="fig" rid="Ch1.F3"/>). The influence of the reference temperature on the retrieved temperatures decreases exponentially downward in altitude, becoming small below <inline-formula><mml:math id="M51" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 45 km <xref ref-type="bibr" rid="bib1.bibx52" id="paren.57"/>. Similarly, the effect of the reference temperature on the temperature trends is greatest at 60 km and negligible below <inline-formula><mml:math id="M52" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 45 km. The reference temperature does not have the same impact on the OSIRIS trends at all latitudes. This is because the trend in MERRA-2 at the reference altitude is more negative in the SH compared to the NH, resulting in an OSIRIS trend that is further away from the climatological 0 K per decade trend in the SH. Overall, the effect of the reference temperature on the trends is less than 0.3 K per decade below 50 km in the NH and tropics and at almost all levels in the SH. It is important to note that the effect of the reference temperature trend does not correspond directly to an error in the retrieved OSIRIS trends: MERRA-2 assimilates MLS observations, so the temperatures are more physically realistic than those from a climatology. Comparing the temperature trends from the two versions of the OSIRIS retrieval only tells us how much of an effect the reference temperature choice can have on the trends.</p> <fig id="Ch1.F3"><label>Figure 3</label><caption><p id="d2e1366">The difference between temperature trends from OSIRIS retrieved with a MERRA-2 reference temperature and OSIRIS retrieved with a climatological (NRLMSISE-00) reference temperature. Trends are calculated over 2005–2021.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f03.png"/> </fig> <p id="d2e1375">To evaluate the impact of the OSIRIS sampling pattern on the temperature trends, we compare trends in reanalysis temperatures that are sampled like OSIRIS and that are sampled like MLS. The OSIRIS temperature trends and the trends in each of MERRA-2, ERA5, and JRA-55 sampled to the OSIRIS profiles are shown in the top row of Fig. <xref ref-type="fig" rid="Ch1.F4"/>. The middle row of the figure shows the MLS temperature trends and trends in the same three reanalyses but sampled like MLS. The MLS trends are slightly different from those in Fig. <xref ref-type="fig" rid="Ch1.F2"/>, as months when OSIRIS does not have any observations were removed from MLS before calculating the trends in Fig. <xref ref-type="fig" rid="Ch1.F2"/>. The differences in the reanalysis trends with MLS sampling compared to OSIRIS sampling are in the bottom row of Fig. <xref ref-type="fig" rid="Ch1.F4"/>. This direct comparison shows that the effect of the OSIRIS sampling pattern on the trends is largest at latitudes greater than <inline-formula><mml:math id="M53" display="inline"><mml:mrow><mml:mo>±</mml:mo><mml:mn mathvariant="normal">30</mml:mn></mml:mrow></mml:math></inline-formula>°. The effect of sampling is also slightly greater in the SH compared to the NH. As OSIRIS can only measure the sunlit portion of the atmosphere, there are regularly gaps in the data record at middle–high latitudes, depending on the season, so it is logical for the sampling pattern to affect the trends more at these latitudes. The OSIRIS orbit is also such that there are more observations in the NH compared to the SH, resulting in the greater impact of sampling on the SH trends. As with the reference temperature, it is not possible to relate these sampling biases directly to an error in the OSIRIS trends, and we can only conclude that caution should be taken when considering latitudes greater than <inline-formula><mml:math id="M54" display="inline"><mml:mrow><mml:mo>±</mml:mo><mml:mn mathvariant="normal">30</mml:mn></mml:mrow></mml:math></inline-formula>°, particularly above 50 km.</p> <fig id="Ch1.F4" specific-use="star"><label>Figure 4</label><caption><p id="d2e1409">Temperature trends for 2005–2021. Trends are shown for <bold>(a)</bold> OSIRIS and <bold>(e)</bold> MLS, along with MERRA-2, ERA5, and JRA-55 sampled like OSIRIS <bold>(b, c, d)</bold> and sampled like MLS <bold>(f, g, h)</bold>. Panels <bold>(i)</bold>, <bold>(j)</bold>, and <bold>(k)</bold> show the difference between trends with the two types of sampling for each reanalysis. The black contour lines mark differences of <inline-formula><mml:math id="M55" display="inline"><mml:mo>-</mml:mo></mml:math></inline-formula>0.5 (dashed) and <inline-formula><mml:math id="M56" display="inline"><mml:mo>+</mml:mo></mml:math></inline-formula>0.5 K per decade (solid). In all panels hatching denotes statistically insignificant trends at the 2<inline-formula><mml:math id="M57" display="inline"><mml:mi mathvariant="italic">σ</mml:mi></mml:math></inline-formula> level.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f04.png"/> </fig> <p id="d2e1461">In addition to their use for discussing the OSIRIS sampling issues, the reanalysis temperature trends are also worth considering on their own. Reanalyses are often taken to be the best measure of the truth when validating and tuning climate models, but they are limited by the data that are assimilated and often have discontinuities whenever there are changes in the observational records that are assimilated <xref ref-type="bibr" rid="bib1.bibx23" id="paren.58"/>. MERRA-2 is the only reanalysis that assimilates temperatures above <inline-formula><mml:math id="M58" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 45 km, corresponding to the upper limit of SSU and AMSU-A observations. MLS temperatures are assimilated above <inline-formula><mml:math id="M59" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 30 km, and the result is that the MERRA-2 temperature trends are similar to the MLS temperature trends. The ERA5 temperature trends look similar to those in OSIRIS and MLS in the tropics below 45 km where there are data assimilated, but the cooling rate at higher altitudes is more than twice what is seen in observations. JRA-55 also does not assimilate MLS, but the JRA-55 temperature trends above 45 km are nonetheless more similar to MERRA-2 and the observations than they are to ERA5. This suggests that the problem with ERA5 is not solely because of the lack of assimilated observations at higher altitudes. There are discontinuities in the ERA5 temperature time series at the higher altitudes that contribute to the more negative trends. Further work is needed to determine the origin of these discontinuities in ERA5 as they are not obviously related to changes in the processing or in the assimilated observations.</p> <p id="d2e1481">Finally, we consider temperature trends in four ensemble members from the WACCM REFD1 scenario (Appendix A, Fig. <xref ref-type="fig" rid="App1.Ch1.S1.F11"/>). The WACCM results are only available to the end of 2018, so these trends cannot be compared directly with the results from observations and reanalyses. The key point here is rather that the temperature trends from each WACCM ensemble member have substantial variability – up to 2 K per decade in some latitude and pressure bins. Since the emissions and radiative calculations are identical in each ensemble member, this suggests that upper-stratospheric temperature trends are significantly affected by internal variability (over the relatively short period of 2005–2021).</p> </sec> <sec id="Ch1.S4.SS2"> <label>4.2</label><title>Merging with SSU and trends in SSU channel 3</title> <p id="d2e1494">It is necessary to combine observations from multiple instruments to study upper-stratospheric temperature trends prior to the 21st century. The most consistent data source available to use is SSU, which operated from 1979 to 2006. As discussed in Sect. <xref ref-type="sec" rid="Ch1.S2"/>, SSU temperatures have been previously merged with those from MLS and AMSU-A. We now create a third merged dataset using OSIRIS temperatures.</p> <p id="d2e1499">Before they can be merged with SSU temperatures, it is necessary to weight the OSIRIS temperature profiles using the SSU weighting functions. We only consider SSU channel 3, as it is the channel that best matches the OSIRIS altitude range: 82 % of the channel 3 weighting function falls between 35 and 60 km (Fig. <xref ref-type="fig" rid="Ch1.F5"/>). As another point of comparison, we also weight the OSIRIS temperature profiles using the narrower AMSU-A channel 14 weighting function, 92 % of which falls within the OSIRIS altitude range.</p> <fig id="Ch1.F5"><label>Figure 5</label><caption><p id="d2e1506">Weighting functions for SSU channels 2 and 3 and AMSU-A channels 13 and 14. The yellow shaded region denotes the altitude range of the OSIRIS temperature product.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f05.png"/> </fig> <fig id="Ch1.F6" specific-use="star"><label>Figure 6</label><caption><p id="d2e1518"><bold>(a)</bold> Bias between OSIRIS and SSU and OSIRIS and AMSU-A temperature for the overlap periods. OSIRIS is weighted separately to match SSU channel (Ch.) 3 and AMSU-A Ch. 14. The error bars are the standard deviation of the mean bias. <bold>(b, c, d)</bold> SSU Ch. 3 temperatures and OSIRIS temperature weighted like SSU Ch. 3 for three latitude bands. <bold>(e, f, g)</bold> AMSU-A Ch. 14 temperatures and OSIRIS temperature weighted like AMSU-A Ch. 14 for three latitude bands.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f06.png"/> </fig> <p id="d2e1535">Each OSIRIS profile is individually weighted by the weighting functions before calculating the monthly zonal means. Figure <xref ref-type="fig" rid="Ch1.F6"/>a shows the mean bias between monthly zonal mean temperatures from SSU channel 3 with OSIRIS and between temperatures from AMSU-A channel 14 and OSIRIS. In both cases the bias is slightly higher in the tropics compared to other latitudes. OSIRIS and SSU agree within 6–7 K, while OSIRIS and AMSU-A agree within 1–2 K. Figure <xref ref-type="fig" rid="Ch1.F6"/>b–d compare the OSIRIS and SSU time series at northern and southern mid-latitudes and in the tropics. While the monthly variability is similar, OSIRIS is consistently biased high. Figure <xref ref-type="fig" rid="Ch1.F6"/>e–g show the same comparison for AMSU-A and OSIRIS. The datasets are extremely similar, and there are no changes in the bias with time, which provides confidence that the various AMSU-A datasets were merged correctly. It is likely that OSIRIS agrees better with AMSU-A than with SSU because AMSU-A has narrower weighting functions, and AMSU-A channel 14 aligns better with the OSIRIS retrieval range than SSU channel 3. While AMSU-A is not particularly useful for extending the OSIRIS observations as the measurement periods are nearly the same, the similarity between OSIRIS and AMSU-A provides further confidence in the accuracy of the OSIRIS temperature retrieval, at least below 45 km.</p> <fig id="Ch1.F7" specific-use="star"><label>Figure 7</label><caption><p id="d2e1546">Merged SSU+AMSU-A, SSU+MLS, and SSU+OSIRIS temperature anomalies for five latitude bands. All datasets are weighted like SSU Ch. 3.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f07.png"/> </fig> <p id="d2e1555">After weighting the OSIRIS profiles with the SSU channel 3 weighting function, the merging process is the same as the one used to merge OSIRIS <inline-formula><mml:math id="M60" display="inline"><mml:mrow class="chem"><mml:msub><mml:mi mathvariant="normal">O</mml:mi><mml:mn mathvariant="normal">3</mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> and <inline-formula><mml:math id="M61" display="inline"><mml:mrow class="chem"><mml:msub><mml:mi mathvariant="normal">NO</mml:mi><mml:mn mathvariant="normal">2</mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> with observations from the Stratospheric Aerosol and Gas Experiment II <xref ref-type="bibr" rid="bib1.bibx3 bib1.bibx6" id="paren.59"/>. First, the bias between the OSIRIS and SSU temperatures is removed by subtracting the bias from OSIRIS in each latitude bin. The bias is calculated by grouping the observations by month and finding the mean difference for each month when both instruments have observations and then taking the average of these monthly values. Then the datasets are deseasonalized individually to account for differences in their sampling patterns that could affect the seasonal cycle. Finally, the OSIRIS and SSU temperatures are merged by taking the mean in months when both instruments have observations. The resulting time series, for several 10° latitude bins, are shown in Fig. <xref ref-type="fig" rid="Ch1.F7"/>. While the OSIRIS sampling affects the results somewhat, the SSU+OSIRIS temperatures are extremely similar to both the SSU+MLS and SSU+AMSU-A temperatures at all latitudes.</p> <p id="d2e1585">Trends in each of the merged datasets are calculated using the MLR described in Sect. <xref ref-type="sec" rid="Ch1.S3"/>. Figure <xref ref-type="fig" rid="Ch1.F8"/>a shows the temperature trends as a function of latitude between 1979 and 2021. The trends from all three merged datasets are nearly identical. At this level, near 45 km, the stratosphere cooled by <inline-formula><mml:math id="M62" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 0.6 K per decade during the 42 years considered. The cooling rate is slightly greater in the NH than in the SH. For just the OSIRIS period, from 2002–2021, the merged temperature records are mainly based on the other instrument, rather than SSU, so we are comparing MLS, AMSU-A, and OSIRIS trends only. These temperature trends agree within the regression error at all latitudes (Fig. <xref ref-type="fig" rid="Ch1.F8"/>b). At all latitudes the cooling rate is about 0.5 K per decade. The SSU+OSIRIS temperature trends are more variable than those from SSU+AMSU-A and SSU+MLS because of the less regular OSIRIS sampling pattern.</p> <fig id="Ch1.F8" specific-use="star"><label>Figure 8</label><caption><p id="d2e1604">Trends in temperatures from merged SSU+AMSU-A, SSU+MLS, and SSU+OSIRIS in 10° latitude bins. Trends are shown for <bold>(a)</bold> 1979–2021 and <bold>(b)</bold> 2002–2021. Error bars are the 2<inline-formula><mml:math id="M63" display="inline"><mml:mi mathvariant="italic">σ</mml:mi></mml:math></inline-formula> uncertainty in the MLR.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f08.png"/> </fig> </sec> </sec> <sec id="Ch1.S5" sec-type="conclusions"> <label>5</label><title>Conclusions</title> <p id="d2e1636">Upper-stratospheric temperature trends have historically been difficult to quantify due to a deficit of observations with high vertical resolution above 35 km. Using the new OSIRIS v7.3 temperature product, we find that the upper stratosphere, between 35 and 60 km, cooled by 0.5–1 K per decade during 2005–2021. The two main sources of uncertainty in the OSIRIS temperature trends are due to sampling biases and the choice of the reference temperatures used in the OSIRIS retrieval. These factors somewhat limit our confidence in the OSIRIS temperature trends at latitudes greater than <inline-formula><mml:math id="M64" display="inline"><mml:mrow><mml:mo>±</mml:mo><mml:mn mathvariant="normal">30</mml:mn></mml:mrow></mml:math></inline-formula>° and at altitudes above 50 km. Despite this, the OSIRIS temperature trends agree with trends from SABER and MLS within the regression uncertainties at most latitudes and altitudes between <inline-formula><mml:math id="M65" display="inline"><mml:mrow><mml:mo>±</mml:mo><mml:mn mathvariant="normal">50</mml:mn></mml:mrow></mml:math></inline-formula>° and 35–60 km. By having a third temperature record in the upper stratosphere, where previously there were only MLS and SABER, we increase confidence in the stratospheric cooling rate. We are also able to observe a possible issue with MLS temperatures at latitudes outside <inline-formula><mml:math id="M66" display="inline"><mml:mrow><mml:mo>±</mml:mo><mml:mn mathvariant="normal">30</mml:mn></mml:mrow></mml:math></inline-formula>°. At these latitudes the MLS temperature trends oscillate in altitude, with trends becoming significantly more negative than those from SABER and OSIRIS near 50 km.</p> <p id="d2e1669">We also compared the OSIRIS and MLS temperature trends to temperature trends from reanalyses and a climate model. The modelled temperature trends from four WACCM ensemble members are generally within the range of those from the observational datasets, but internal variability alters the trends by up to 2 K per decade, highlighting trend uncertainties in short data records. The reanalysis trends agree reasonably well with the observations below 45 km, where SSU and AMSU-A observations are assimilated, but are highly variable at higher altitudes. MERRA-2 is the only reanalysis that assimilates temperatures (from MLS) above 45 km, and it is clear from the large trend differences with ERA5 and JRA-55 that this constraint is important. However, this is not the only factor affecting the reanalysis temperature trends above 45 km. JRA-55 trends are at most <inline-formula><mml:math id="M67" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula>1 K per decade too low, while ERA5 trends in some bins are more than 3 K per decade lower than the trends in observations. This suggests that there is some issue with the ERA5 temperatures at these altitudes, apart from the lack of assimilated observations. The ERA5 temperature time series has discontinuities above <inline-formula><mml:math id="M68" display="inline"><mml:mo>∼</mml:mo></mml:math></inline-formula> 54 km that contribute to the more negative trends. Further work is needed to understand these discontinuities as they cannot be clearly attributed to changes in the production stream or to changes in the input observations.</p> <p id="d2e1686">For the comparison of OSIRIS temperature observations to those from the nadir sounders SSU and AMSU-A, the OSIRIS profiles were weighted to match either channel 3 of SSU or channel 14 of AMSU-A. OSIRIS and AMSU-A temperatures agree extremely well, with OSIRIS biased high by at most 2 K. The bias between OSIRIS and SSU channel 3 is greater: OSIRIS is warmer by 6–7 K.</p> <p id="d2e1689">By merging the OSIRIS observations with SSU we determined temperature trends over the 42 years from 1979–2021. The cooling rate for this extended period is about 0.6 K per decade. This is in agreement with the cooling rate in temperatures from SSU merged with MLS and from SSU merged with AMSU-A. The temperature trends in the merged SSU+OSIRIS, SSU+MLS, and SSU+AMSU-A also all agree for 2002–2021. During this period the trends are mainly based on the data records that are merged with SSU, as SSU ceased operations in 2006.</p> <p id="d2e1693">In summary, our results show that the upper stratosphere, from 35–60 km, cooled at a rate of 0.5–1 K per decade between 1979 and 2021. The consistent trends across all observations from OSIRIS, MLS, SABER, SSU, and AMSU-A provide confidence that these cooling trends are accurate. Initial comparisons with reanalysis and model trends highlight the need for further model development in order to accurately represent upper-stratospheric temperature changes. The significant stratospheric cooling rate is yet another sign that anthropogenic activities are altering the climate, and it is necessary to model this cooling correctly in order to understand the effects of climate change on the whole atmosphere.</p> </sec> </body> <back><app-group> <app id="App1.Ch1.S1"> <label>Appendix A</label><title>Extra figures</title> <fig id="App1.Ch1.S1.F9"><label>Figure A1</label><caption><p id="d2e1709">Correlation coefficient for deseasonalized monthly mean anomalies during 2005–2021 in 10° latitude and 1 km altitude bins. Only months when OSIRIS has observations are considered.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f09.png"/> </fig> <fig id="App1.Ch1.S1.F10"><label>Figure A2</label><caption><p id="d2e1723">Regression coefficients for the solar <inline-formula><mml:math id="M69" display="inline"><mml:mrow><mml:msub><mml:mi>F</mml:mi><mml:mn mathvariant="normal">10.7</mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> flux and the first two principal components of the QBO. Coefficients are shown for each of MLS, SABER, and OSIRIS temperatures over 2005–2021. Only months when OSIRIS has observations are considered.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f10.png"/> </fig> <fig id="App1.Ch1.S1.F11"><label>Figure A3</label><caption><p id="d2e1748">Temperature trends for 2005–2018 for four WACCM ensemble members. The shaded regions denote the 2<inline-formula><mml:math id="M70" display="inline"><mml:mi mathvariant="italic">σ</mml:mi></mml:math></inline-formula> uncertainty in the MLR.</p></caption> <graphic xlink:href="https://acp.copernicus.org/articles/24/12925/2024/acp-24-12925-2024-f11.png"/> </fig> </app> </app-group><notes notes-type="codedataavailability"><title>Code and data availability</title> <p id="d2e1772"><list list-type="bullet"> <list-item> <p id="d2e1777">OSIRIS v7.3 temperature profiles are available at <uri>https://doi.org/10.5281/zenodo.8271140</uri> <xref ref-type="bibr" rid="bib1.bibx51" id="paren.60"/>.</p> </list-item> <list-item> <p id="d2e1789">MLS v5 temperature profiles are available at <uri>https://doi.org/10.5067/Aura/MLS/DATA2520</uri> <xref ref-type="bibr" rid="bib1.bibx42" id="paren.61"/>.</p> </list-item> <list-item> <p id="d2e1801">MLS v5 geopotential heights are available at <uri>https://doi.org/10.5067/Aura/MLS/DATA2507</uri> <xref ref-type="bibr" rid="bib1.bibx41" id="paren.62"/>.</p> </list-item> <list-item> <p id="d2e1813">SABER v2 temperature profiles are available at <uri>https://data.gats-inc.com/saber/custom/Temp_O3_H2O/v2.0/</uri> <xref ref-type="bibr" rid="bib1.bibx39" id="paren.63"/>.</p> </list-item> <list-item> <p id="d2e1825">The SSU v2 temperatures and weighting functions, the AMSU-A v2 temperatures and weighting functions, and the merged v3 SSU+AMSU-A temperatures are all available at <uri>https://www.star.nesdis.noaa.gov/smcd/emb/mscat/products.php</uri> <xref ref-type="bibr" rid="bib1.bibx28" id="paren.64"/>.</p> </list-item> <list-item> <p id="d2e1838">SSU+MLS temperatures are available upon request from William Randel (randel@ucar.edu) (<uri>https://doi.org/10.1175/JCLI-D-15-0629.1</uri>; <xref ref-type="bibr" rid="bib1.bibx34" id="altparen.65"/>).</p> </list-item> <list-item> <p id="d2e1850">MERRA-2 temperatures are available at <uri>https://doi.org/10.5067/WWQSXQ8IVFW8</uri> <xref ref-type="bibr" rid="bib1.bibx10" id="paren.66"/>.</p> </list-item> <list-item> <p id="d2e1862">ERA5 temperatures are available at <uri>https://doi.org/10.24381/cds.adbb2d47</uri> <xref ref-type="bibr" rid="bib1.bibx16" id="paren.67"/>.</p> </list-item> <list-item> <p id="d2e1874">JRA-55 temperatures are available at <uri>https://doi.org/10.5065/D6HH6H41</uri> <xref ref-type="bibr" rid="bib1.bibx17" id="paren.68"/>.</p> </list-item> <list-item> <p id="d2e1886">The WACCM results are available at <uri>ftp://odin-osiris.usask.ca/Models</uri> <xref ref-type="bibr" rid="bib1.bibx29" id="paren.69"/>. Instructions for downloading the WACCM files are at <uri>https://research-groups.usask.ca/osiris/data-products.php#Download</uri> (last access: 20 August 2022).</p> </list-item> <list-item> <p id="d2e1901">The LOTUS regression code and documentation are available at <uri>https://github.com/usask-arg/lotus-regression</uri> <xref ref-type="bibr" rid="bib1.bibx5" id="paren.70"/>.</p> </list-item> </list></p> </notes><notes notes-type="authorcontribution"><title>Author contributions</title> <p id="d2e1915">KD performed the analysis and prepared the manuscript. DZ developed the OSIRIS retrieval. WR provided the WACCM results and the merged SSU+MLS data. ST, AB, DZ, DD, and WR provided input on the method and analysis. ST, AB, and DD supervised the project. SD provided the ERA5 results interpolated to the OSIRIS and MLS profiles. All authors provided significant feedback on the manuscript.</p> </notes><notes notes-type="competinginterests"><title>Competing interests</title> <p id="d2e1921">The contact author has declared that none of the authors has any competing interests.</p> </notes><notes notes-type="disclaimer"><title>Disclaimer</title> <p id="d2e1927">Publisher's note: Copernicus Publications remains neutral with regard to jurisdictional claims made in the text, published maps, institutional affiliations, or any other geographical representation in this paper. While Copernicus Publications makes every effort to include appropriate place names, the final responsibility lies with the authors.</p> </notes><ack><title>Acknowledgements</title><p id="d2e1933">This research was supported by the Canadian Space Agency (grant no. 21SUASULSO). The authors thank the Swedish National Space Agency and the Canadian Space Agency for the continued operation and support of Odin and OSIRIS. The National Center for Atmospheric Research is sponsored by the US National Science Foundation. This work was partly supported by the NASA Aura Science Team under grant no. 80NSSC20K0928. Work at the Jet Propulsion Laboratory, California Institute of Technology, was carried out under contract with NASA (grant no. 80NM0018D004).</p></ack><notes notes-type="financialsupport"><title>Financial support</title> <p id="d2e1938">This research has been supported by the Canadian Space Agency (grant no. 21SUASULSO), the National Aeronautics and Space Administration (grant no. 80NM0018D004), and the National Aeronautics and Space Administration (grant no. 80NSSC20K0928).</p> </notes><notes notes-type="reviewstatement"><title>Review statement</title> <p id="d2e1944">This paper was edited by John Plane and reviewed by two anonymous referees.</p> </notes><ref-list> <title>References</title> <ref id="bib1.bibx1"><label>Bernath et al.(2005)</label><mixed-citation>Bernath, P. F., McElroy, C. 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