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The 2006 Canadian Arctic ACE (Atmospheric Chemistry Experiment) Validation Campaign collected measurements at the Polar Environment Atmospheric Research Laboratory (PEARL, 80.05◦ N, 86.42◦ W, 610 m above sea level) at Eureka, Canada from 17 February to 31 March 2006. Two of the ten instruments involved in the campaign, 5 both Fourier transform spectrometers (FTSs), were operated simultaneously, recording atmospheric solar absorption spectra. The first instrument was an ABB Bomem DA8 high-resolution infrared FTS. The second instrument was the Portable Atmospheric Research Interferometric Spectrometer for the Infrared (PARIS-IR), the ground-based version of the satellite-borne FTS on the ACE satellite (ACE-FTS). From the mea10 surements collected by these two ground-based instruments, total column densities of seven stratospheric trace gases (O3, HNO3, NO2, HCl, HF, NO, and ClONO2) were retrieved using the optimal estimation method and these results were compared. Since the two instruments sampled the same portions of atmosphere by synchronizing observations during the campaign, the biases in retrieved columns from the two spectrom15 eters represent the instrumental differences. These differences were consistent with those seen in previous FTS intercomparison studies. Partial column results from the ground-based spectrometers were also compared with partial columns derived from ACE-FTS version 2.2 (including updates for O3, HDO and N2O5) profiles and the differences found were consistent with the other validation comparison studies for the 20 ACE-FTS version 2.2 data products. Column densities of O3, HCl, ClONO2, and HNO3 from the three FTSs were normalized with respect to HF and used to probe the time evolution of the chemical constituents in the atmosphere over Eureka during spring 2006.


Introduction
Validating data products from satellite-borne infrared Fourier transform spectrometers (FTSs) can be challenging because of the wide range of atmospheric species that are measured.Ground-based FTSs, such as those that are part of the Network for the Detection of Atmospheric Composition Change (NDACC, http://www.ndsc.ncep.noaa.gov/), contribute significantly to these efforts, because they cover a similar spectral range with high spectral resolution, and are thus a key part of the validation program for a limb-sounding satellite FTS (e.g., Vigouroux et al., 2007;Cortesi et al., 2007;Wetzel et al., 2007).Some information on the altitude distribution of the atmospheric trace gases can be retrieved from the shapes of the spectral lines obtained from these ground-based FTSs (e.g., Pougatchev et al., 1995;Rinsland et al., 1998).This allows partial column densities to be calculated from the ground-based measurements and it is these quantities that are compared with partial columns derived from the satellite observations.In order to make these comparisons, it is necessary to understand the differences between ground-based instruments that are used in satellite validation studies and this is the focus of this paper.
The Atmospheric Chemistry Experiment (ACE), also known as SCISAT, is a Canadian-led satellite mission for remote sensing of the Earth's atmosphere from a circular, low Earth orbit (altitude 650 km, inclination 74 • ).An infrared Fourier transform spectrometer (ACE-FTS; Bernath et al., 2005) together with a dual, ultraviolet(UV)visible-near-infrared spectrophotometer named Measurement of Aerosol Extinction in the Stratosphere and Troposphere Retrieved by Occultation (ACE-MAESTRO; McElroy et al., 2007), are the scientific instruments onboard the satellite.The ACE mission studies primarily the upper troposphere and stratosphere.It measures the concentrations of more than 30 chemical constituents that influence the distribution of stratospheric ozone, a major chemical species that absorbs the Sun's biologically-damaging ultraviolet radiation (Bernath et al., 2005;Bernath, 2006).
The 2006 Canadian Arctic ACE Validation Campaign was the third in a series of campaigns held in Eureka, as part of the calibration and validation program for the ACE mission (Kerzenmacher et al., 2005;Walker et al., 2005;Manney et al., 2008;Sung et al., 2007;Fraser et al., 2007).The campaign took place at the Polar Environment Atmospheric Research Laboratory (PEARL, 80.05  Fu et al., 2007) and ACE-MAESTRO (MAESTRO-G; Kerzenmacher et al., 2005;McElroy et al., 2007) together with a DIfferential Absorption Lidar (Bird et al., 1996), a high resolution FTS (DA8 FTS; Donovan et al., 1997;Wiacek et al, 2006;Farahani et al., 2007), ozonesondes (Davies et al., 2000;Tarasick et al., 2005), a ground-based SunPhotoSpectrometer (McElroy, 1995), two Brewer spectrophotometers (Savastiouk and McElroy, 2005), the University of Toronto ground-based ultravioletvisible spectrometer (Bassford et al., 2005;Melo et al., 2004), and a SAOZ (Syst ème Analyse par Observations Z énithales; Pommereau and Goutail, 1988).These instruments were used to derive total columns, partial columns, and vertical profiles for most of the ACE target species, as well as temperature and pressure.Throughout this paper, the term "total column" is used to indicate that the column amount was calculated from the full altitude range of the ground-based measurement (typically from the ground to 100 km) whereas the term "partial column" is used for results obtained over a narrower altitude range.Depending on the type of ground-based measurement, the total column retrieved may be more sensitive to one region of the atmosphere than another (for example, NO 2 retrievals from FTSs are only sensitive to the stratospheric part of the total column; Sussmann et al., 2005).This work will describe observations made by PARIS-IR and the Environment Canada (EC) DA8 FTS and will discuss comparisons both between the ground-based instruments and with the ACE-FTS results.The results will focus on trace gas species that play an important role in ozone depletion processes that occur each spring in the polar vortex, including O 3 , the chlorine and nitrogen reservoir species (HCl, ClONO 2 5309 and HNO 3 ), NO x (NO and NO 2 ), and a stratospheric tracer (HF) (e.g.Solomon, 1999).PEARL is located in a region of large stratospheric variability in the Arctic (Harvey and Hitchman, 1996), where there is a good chance of making measurements both inside and outside the polar vortex.Although PARIS-IR was deployed at Eureka in 2004 and 2005 (Sung et al., 2007;Sung et al. 1 ), there were major instrument changes and improvements for the 2006 campaign.In addition, optical parts in PARIS-IR were realigned in mid-2005.PARIS-IR's performance in 2006 is expected to be different from the performance in the 2004 and 2005 campaigns.The EC DA8 FTS has been operating at Eureka since 1993 and was compared to the portable FTS from National Physical Laboratory (NPL) (Murphy et al., 2001).Hence, one of the goals of the campaign is to investigate the differences between the retrieved columns obtained by PARIS-IR, which is a relatively "new" campaign instrument, and the DA8 FTS, which is a permanently installed instrument and has been making long term observations at PEARL since 1993.
To focus on the differences in the vertical columns that arise from the instrument performance, PARIS-IR and the DA8 FTS were configured to measure atmospheric absorption spectra simultaneously.This measurement strategy differs from that used in the 2004 and 2005 Canadian Arctic ACE Validation Campaigns, when PARIS-IR and the DA8 FTS recorded spectra alternately.Details on the configuration of the two ground-based FTSs in the 2006 campaign will be illustrated in Sect. 2. Making simultaneous measurements ensured that PARIS-IR and the DA8 FTS were sampling the same atmosphere and thus removed any differences in vertical columns due to temporal and spatial variations.The ground-based FTS retrieval method and measurement characterization are described in Sect.3. The ACE-FTS measurements and retrievals are described in Sect. 4. In Sect.5, total columns, partial columns and column ratios obtained from simultaneous atmospheric remote sensing measurements 1 Sung, K., Strong, K., Mittermeier, R. L., Walker, K. A., et al.: Partial and total column SFIT2 retrievals from Eureka DA8 spectra in spring 2004 and 2005, including comparisons with the PARIS-IR and ACE Satellite measurements, to be submitted to Atmos.Chem.Phys., 2008.
using PARIS-IR and the DA8 FTS at Eureka are reported.The results are used to compare measurements from PARIS-IR and the DA8 FTS, to investigate the quality of ACE occultation measurements, and to probe the time evolution of the chemical constituents in the atmosphere over the Canadian high Arctic during spring 2006.

Ground-based instrumentation and observations
PARIS-IR is a portable FTS built for atmospheric remote sensing from the ground and airborne platforms such as high-altitude balloon gondolas.It was constructed as a terrestrial version of the ACE-FTS using a similar design and incorporating flight-spare optical components from the satellite instrument.Hence, PARIS-IR can achieve the same spectral resolution (maximum optical path difference (MOPD) of ±25 cm; maximum spectral resolution of 0.02 cm −1 ) and spectral coverage (750-4400 cm −1 ) as the ACE-FTS.Its maximum scanning speed is 2.5 cm/s, which makes PARIS-IR capable of recording one double-sided interferogram at MOPD every 20 s.A sandwich-type detector, which consists of mercury cadmium telluride (MCT) and indium antimonide (InSb) elements, is used in PARIS-IR to record spectra over its entire spectral range in a single scan (Fu et al., 2007).
An ABB Bomem DA8 FTS, a high-spectral-resolution (MOPD of 250 cm; maximum spectral resolution of 0.002 cm −1 ) Michelson interferometer using dynamic alignment techniques, was installed at PEARL in February 1993 (Donovan et al., 1997;Farahani et al., 2007).Two independent detectors, MCT and InSb, are used to cover the spectral range from 700 to 5100 cm −1 .DA8 FTS measurements are made using a sequence of nine optical filters to improve the Signal-to-Noise Ratio (SNR).For this study, we used spectra recorded with the following filters: S1 (3950-4300 cm −1 ), S3 (2400-3300 cm −1 ), S5 (1800-2050 cm −1 ) and S6 (700-1300 cm −1 ).The MCT detector was used with filter S6 and for the rest of the filters, the spectra were recorded with the InSb detector.
A sun-tracking mirror system, permanently mounted on the roof of PEARL, was used 5311 to direct the solar beam into the FTS laboratory.To observe the atmosphere simultaneously using the two spectrometers, the solar beam (diameter ∼14 cm) was split into two parts.One third of the solar beam was directed through the input window of PARIS-IR using a flat pickoff mirror.The rest of the solar beam was directed into the DA8 FTS.The SNR and retrieved total column densities from several spectra recorded in shared beam mode and in whole beam mode were compared at the beginning of the campaign.Differences in total column densities between the two modes were found to be small, generally of the order of 1%.PARIS-IR has a shorter acquisition time per spectrum (20 s) than the DA8 FTS (about 190 s).A single measurement from the DA8 FTS consists of four co-added spectra and requires about 13 min to collect.To further ensure simultaneity, all of the individual spectra (∼40) collected by PARIS-IR during each 13-min DA8 measurement interval were co-added.
The campaign was carried out in two phases: the intensive and extended phases.The intensive phase took place from 17 February to 8 March 2006.During this time, measurements were made by all of the campaign instruments, including PARIS-IR and the DA8 FTS, when weather conditions allowed.The ground-based FTS measurements started on 21 February when the Sun became visible above the horizon.Also, balloon-borne ozonesondes were launched daily from the nearby Eureka Weather Station.After the intensive phase, PARIS-IR was shipped back to its home station, the Waterloo Atmospheric Observatory.The extended phase continued from 9 to 31 March 2006, with measurements by the DA8 FTS and several of the UV-visible grating spectrometers and weekly EC ozonesonde flights.

Spectral analysis and retrievals for ground-based FTSs
The spectra measured by PARIS-IR and the DA8 FTS were analyzed in a consistent manner using the same retrieval program, spectroscopic parameters, spectral ranges and a priori information.This was done in order to eliminate, as much as possible, any differences due to the retrieval process.The analyses were performed using SFIT2 (version 3.91) (Pougatchev et al., 1995;Rinsland et al., 1998).SFIT2 makes use of the Optimal Estimation Method (OEM) (Rodgers, 1976(Rodgers, , 1990(Rodgers, , 2000) ) to include a priori volume mixing ratio (VMR) profiles of atmospheric constituents as a function of altitude in the retrievals.The spectral ranges, called microwindows (MWs), used in the PARIS-IR and DA8 FTS retrievals are listed in Table 1.All of the spectroscopic line parameters and cross sections used in these retrievals are taken from the HIgh resolution TRANsmission molecular absorption database (HITRAN) 2004 (Rothman et al., 2004).
A model atmosphere is used in the SFIT2 program to simulate spectra.A forward model, named FSCATM (Gallery et al., 1983;Meier et al., 2004a), was applied to generate the model atmospheres using a priori VMR estimates, and pressure and temperature profiles.FSCATM carries out refractive ray tracing and a calculation of the air mass distribution, which is the number of molecules as a function of altitude, for each model atmosphere.The a priori estimates of VMR profiles were adapted from the a priori profiles constructed by A. Meier in 1998 for the NDACC station at Kiruna (Meier et al., 2004b).To adapt this set of VMR profiles for use with measurements from Eureka, the VMR profiles for O 3 , HNO 3 , HCl, HF, ClONO 2 , NO, NO 2 , HDO, H 2 O, CH 4 , and N 2 O, which are the target trace gases for this work or major interfering species in the spectral regions used in the retrievals, have been updated using results from: the HALogen Occultation Experiment (HALOE) v. 19 data set between 1991 to 2005 (Russell et al., 1994;Grooß and Russell, 2005 and references therein), the 2002-2004 Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) version 3.0 profiles produced with the Institut f ür Meteorologie und Klimaforschung scientific processor (H öpfner et al., 2006), the Stratospheric Processes And their Role in Climate 2000 climatology (SPARC2000) (Randel et al., 2002), and Eureka ozonesonde archive (Tarasick et al., 2005).The procedure used to update the VMR profiles is presented in detail in Sung et al. 2 .Pressure and temperature profiles were produced 2 Sung, K., Strong, K., Mittermeier, R. L., Walker, K. A., et al.: Partial and total column SFIT2 retrievals from Eureka DA8 spectra in spring 2004 and 2005, including comparisons with the 5313 using data from three sources: the daily radiosondes from the Eureka Weather Station (launched daily at 11:15 and 23:15 UT), the National Centers for Environmental Prediction (NCEP)/National Center for Atmospheric Research (NCAR) analyses provided by the NASA Goddard Space Flight Centre automailer (obtained from the Goddard Automailer science@hyperion.gsfc.nasa.gov)(McPherson et al., 1979;Kalnay et al., 1996), and the Mass-Spectrometer-Incoherent-Scatter model (MSIS-2000) (Picone et al., 2002).From the surface to about 38 km, the radiosonde measurements were used.Above that, the NCEP/NCAR analyses extend the profile from 38 to 50 km and the output from MSIS was used from 50 to 100 km.
Instrument parameters, including the apodization and instrument lineshape functions, are required to simulate the absorption spectra used in the SFIT2 retrieval process.This is the area where the retrievals differed for the two FTSs.For the apodization function, the DA8 FTS used a Hamming function and PARIS-IR used a boxcar function.In earlier comparisons, it was demonstrated that it is necessary to have a wellcharacterized instrument line shape (ILS) in order to retrieve accurate total columns of stratospheric gases from PARIS-IR spectra (Wunch et al., 2007).In this current work, we used the LINEFIT program (Hase et al., 1999, version 11) to retrieve ILS information for the two FTSs from N 2 O features between 2400 and 2800 cm −1 .These spectra were measured using a blackbody source and a 10-cm-long, 5.0-cm-diameter cell that was filled with 14.7 hPa of N 2 O.The ILS results obtained were consistent with earlier measurements for the DA8 FTS and PARIS-IR (Wunch et al., 2007; Sung et al.  3 ).In the SFIT2 retrieval, the ILS parameters obtained from the cell measurements were used as a priori inputs and values were retrieved from the atmospheric spectra as part of the state vector.A 29-layer grid was used to retrieve profiles from the PARIS-IR and DA8 FTS spectra.
In addition to the profiles, integrated vertical column densities are produced for each of the layers.These were used to calculate the total column densities and partial column densities used in this work.The fitting residuals from the SFIT2 retrievals were used to evaluate the quality of the results for the DA8 FTS and PARIS-IR.Using the data from the entire campaign, the mean and the 1σ standard deviation of the root mean square (RMS) fitting residual were calculated for each MW and each FTS.Only those retrievals whose RMS fitting residuals were within one standard deviation of the mean were included in this study.For the DA8, this technique excluded at most 3-4 measurements out of ∼60 recorded for each filter band during the campaign.OEM, the method used in the SFIT2 spectral retrieval program, provides a method to compute the major uncertainties in the retrievals of vertical columns such as smoothing error, retrieval noise error and model parameter error (Rodgers, 2000;Rodgers and Connor, 2003).Smoothing error, also known as null space error in the Rodger's OEM formalism, arises from the limited altitude resolution of the observing system.Retrieval noise error is due to measurement noise in the spectra.The forward model parameters such as spectral background, slope and instrumental line shape also generate uncertainties in the retrievals and these contributions are grouped together as model parameter error.Table 2 summarizes these errors in the total column densities obtained from the PARIS-IR and DA8 FTS observations and the root-sum-square of these errors was used to provide a total error estimate.
The spectral resolution of a measurement affects the amount of vertical information obtained from the spectral line shape of a measured species (Rodgers, 2000).With higher spectral resolution, more precise vertical information can be obtained.As shown in Table 2, the results from the DA8 FTS typically have higher values of Degrees Of Freedom for Signal (DOFS), which are the number of independent quantities obtained from the observations (the vertical partial columns in a specified altitude range, in this case), than those from PARIS-IR since the DA8 FTS has a spectral resolution 10 times higher than that of PARIS-IR.The DOFS can be improved by choosing high quality microwindows, i.e. spectral segments which contain many absorption lines of the 5315 investigated species with few (and ideally weak) absorption features from interfering species.The microwindows used in this work have generally improved the retrievals of O 3 and HCl compared to those carried out in an instrument comparison campaign at University of Toronto (Wunch et al., 2007) in terms of DOFS.
According to the Rodger's OEM theory, the averaging kernel is the derivative of a derived parameter with respect to its a priori state value, i.e., when this normalized derivative is small (nearly 0) all of the information comes from the a priori and when it is large (near 1) then the information in the retrieval comes mainly from the measured spectra (Rodgers, 1976(Rodgers, , 1990(Rodgers, , 2000)).The typical averaging kernel profiles of seven investigated species are shown in Fig. 1.For all of the seven species investigated, the retrievals show good performance since the averaging kernel values are close to 1 in the altitude ranges where most of the molecules are located.For example, the averaging kernel values from the O 3 retrievals using spectral segments near 1120 cm −1 (MW1120) are close to 1 from 10 to 60 km for both FTSs.More than 80% of the total ozone resides in the altitude range from 10 to 60 km.

ACE-FTS satellite observations and analyses
The ACE-FTS instrument performs up to 30 solar occultation measurements each day.Its spectral resolution (0.02 cm −1 ) and spectral range (750-4400 cm −1 ) match those of PARIS-IR.The ACE-FTS instrument records one measurement every 2 seconds.The result of this sampling rate is that the typical vertical spacing of measurements within an occultation is 3-4 km, neglecting the effects of refraction that compress the spacing at low altitudes.The actual vertical resolution of the ACE-FTS measurements is limited to about 3-4 km, due to the extent of the instrument field-of-view (1.25 mrad) and the orbit altitude of the satellite (650 km).
The spectra measured by the ACE-FTS are analysed using a nonlinear least squares global fitting approach to obtain VMR profiles of trace gases in the Earth's atmosphere, along with pressure and temperature profiles (Boone et al., 2005).The retrieved pro-files have a vertical resolution of 3-4 km and extend from the cloud tops (or 5 km under clear conditions) to about 100 km.The current ACE-FTS data set, version 2.2 with updates for O 3 , N 2 O 5 , and HDO, contains VMR profiles for more than 30 atmospheric constituents.Validation results for the primary molecules measured with ACE can be found in this Special Issue (for example, the O 3 validation paper by Dupuy et al., 2008).
Partial column densities were calculated using atmospheric densities derived from the ACE-FTS measurements.Uncertainties in the partial column densities were calculated using the statistical fitting errors reported for the ACE-FTS VMR profiles.
During the campaign, ACE-FTS made thirteen occultation measurements within 500 km of PEARL.The location for each ACE occultation is given as the latitude, longitude and time of the 30-km tangent point (calculated geometrically), and it is this value that was used in determining coincidences between observations.The ACE satellite measurements were made between 22 February and 13 March 2006.

Results and discussion
The spectra recorded with PARIS-IR, the DA8 FTS, and ACE-FTS during the campaign were analyzed using the methods described in Sections 3 and 4. The results for seven primarily stratospheric trace gases (O 3 , HNO 3 , HCl, ClONO 2 , NO 2 , NO, and HF) are discussed here.In Sect.5.1, comparisons of results between PARIS-IR and the DA8 FTS are described.In Section 5.2, results from the ground-based observations are compared to the ACE-FTS occultation measurements.Finally, in Section 5.3, results from the three FTSs will be used to examine the time evolution of chemical constituents in the atmosphere over the Canadian high Arctic during spring 2006.In these sections, total column and partial column densities will be used.The altitude range used for the partial columns was chosen to match the common range covered by all of the ACE-FTS measurements.
When comparing satellite and ground-based measurements, pairs of collocated measurements are identified using criteria based on the difference in distance and time 5317 between the measurements.Typically, the distance between the observatory housing the instrument and the tangent point of a specific altitude in the satellite profile is used to determine the spatial coincidence.For high-latitude stations where the solar elevation is relatively small, the location of the observatory does not necessarily give a good estimate of the location of the measured airmass because of the long slant path through the atmosphere.The tangent point of the atmospheric layer where the measurement is most sensitive can be located up to several hundred km away from the observatory.To better understand the region of the atmosphere that is being sounded in the DA8 FTS and PARIS-IR observations during the campaign, we have used a geometric calculation to estimate the tangent point locations of several altitudes along the slant path of the solar radiation.Refraction effects have been neglected.In the calculation, the distance between the observatory and the tangent point is calculated using the solar zenith angle and the hour angle (the difference between the measurement local solar time and solar noon).Then, these are used with the location of PEARL and the haversine equation (Sinnott, 1984) used to determine the latitude and longitude of the tangent point.This method was used to estimate the locations of the 18-km tangent point in the PARIS-IR and DA8 FTS measurements on 4 March 2006 and these points are shown in Fig. 2.This altitude was chosen because it is near the peak in number density for O 3 , HCl, HNO 3 , and other species of interest in this study during polar spring.Also, in this figure, the locations of the ACE-FTS occultations on 4 and first week of the campaign, the measurements were limited because the Sun is only visible for a short period of time around noon, and that is further limited by topography and cloud.The length of each day increases rapidly at the beginning of the campaign (increasing from ∼2 h on 21 February to ∼6 h on 28 February, values calculated from the sunrise and sunset times provided by the Astronomical Application Department of U.S. Naval Observatory; http://aa.usno.navy.mil/).Often the measurements on the first days have large fitting residuals and thus very few are included in the comparisons.It should also be noted that the solar zenith angles for the measurements between 21 and 26 February range between ∼89 and 90 • .The weather conditions were poor during the middle of the intensive phase: no ground-based FTS measurements were made from 27 February to 3 March 2006 because of clouds and snow at PEARL.There were good observing conditions at the end of the intensive phase, from 4 to 7 March 2006.
Figure 3 shows the time series of the individual (panel a) and the daily mean (panel b) ozone total column densities from the DA8 FTS and PARIS-IR obtained using the MWs near 1120 cm −1 (MW1120).Also included in these plots are the total columns estimated from the ozonesonde flights made during the campaign.These estimates were made by extrapolating the ozonesonde profile above the highest measured altitude and integrating to obtain a total column density (Tarasick et al., 2005).It can be seen that there are fewer DA8 FTS ozone measurements than PARIS-IR measurements in the early part of the campaign due to the sequence in which the filters are used for the observations.When the observing time during a day is less than ∼6-7 h, the DA8 FTS cannot measure a full series of spectra (obtained by recording spectra with each filter twice) and thus not all of the target species have been measured every day by both ground-based FTSs.In contrast, PARIS-IR does not use filters and, therefore, can provide column densities for all of the trace gases of interest from each observation.
Results from PARIS-IR provide information with higher temporal resolution than those from the DA8 FTS.For example, on 4 March 2006, ten observations were made using PARIS-IR and the DA8 FTS simultaneously.Vertical column densities of ozone are available from all ten observations made using PARIS-IR on that day.However only 5319 two measurements were recorded by the DA8 FTS with the S6 filter (700-1300 cm −1 ) and thus only two ozone column results are available from MW1120.As indicated in Fig. 2, for the rest of that day, the DA8 FTS recorded atmospheric absorption spectra in spectral ranges other than the one covered by the S6 filter.Because of this, the spatial and temporal coverage of the PARIS-IR ozone measurements is much wider than that of the DA8 FTS.The impact of this difference in sampling is seen in panel c of To investigate this further, we calculated the differences between the PARIS-IR and DA8 FTS total column densities for the six species (O 3 , HNO 3 , HCl, NO 2 , ClONO 2 , and HF) and these are shown in Table 3 (note that PARIS-IR did not measure NO).
The comparisons were performed in two ways, one approach using daily mean values and the other approach using individual measurements.For the former method, daily mean total column densities were calculated for a given species retrieved by both FTSs, and percentage differences were calculated for each measurement day using where, CP x and CDx are the daily mean values of observed total columns of the given species x (x can be O 3 , HNO 3 , HCl, NO 2 , ClONO 2 , or HF) observed by PARIS-IR and the DA8 FTS, respectively.All of the percentage differences were then averaged to obtain the results shown in the third column of Table 3 together with the 1σ standard deviation of the differences in parentheses.In the second comparison method, differences between individual measurements were calculated using where, C P x and C Dx are the individual values of simultaneously observed total columns.All of these differences between individual measurements were then averaged to obtain the results shown in the fourth column of Table 3 (along with the 1σ standard deviation of the mean).For all six of the species investigated, the comparisons using daily mean values show larger differences (by up to 13%) between two FTSs than those using the individual observations recorded simultaneously.Variation in the measured total column densities during each observation day, as shown in Figs. 3, 4, and 5, arises from the temporal and spatial differences in Arctic atmospheric composition.This variation has to be taken into consideration when making comparisons between ground-based instruments measuring at high latitudes and when choosing coincidence criteria for satellite comparison studies.
The differences between the simultaneous measurements made by the DA8 FTS and PARIS-IR can be compared to results from earlier intercomparison campaigns.In 1999, an instrument comparison campaign was held at Eureka and the retrieved vertical columns from the portable NPL FTS (a Bruker 120M) were compared with those from the DA8 FTS at PEARL (Murphy et al., 2001).These comparisons show that the differences between the NPL FTS and the DA8 FTS have a consistent systematic bias of about 3% for HCl, HNO 3 and O 3 , and 7% for HF, with the DA8 FTS reporting higher column amounts than the NPL FTS for all comparisons.The large difference 5321 between instruments for HF was attributed to an instrument lineshape problem and a zero level problem (when the atmosphere has 100% absorption the signal should be zero).In addition, the non-linearity of the MCT detector was found to be causing a major portion of the differences in retrieved HNO 3 columns between the NPL FTS and the DA8 FTS.The mean individual differences obtained from the 2006 Canadian Arctic ACE Validation Campaign are generally similar to or smaller than those reported in the 1999 comparison and these differences show systematically lower column values for five species (HNO 3 , HCl, NO 2 , ClONO 2 , and HF) and higher column values for O 3 from PARIS-IR than from the DA8 FTS.For all species except O 3 , the results from the current work are consistent with the earlier NPL intercomparison study.
The different spectral resolutions of the instruments could also contribute to the differences between the PARIS-IR and DA8 FTS.This was investigated during comparisons between PARIS-IR and two FTSs with higher spectral resolutions that were carried out in summer 2005 at the University of Toronto (Wunch et al., 2007).One of these FTSs was the Toronto Atmospheric Observatory Fourier Transform Spectrometer (TAO-FTS), an ABB Bomem DA8 FTS with the same specifications as the Eureka DA8 FTS.Total column differences for O 3 and HCl between PARIS-IR and the TAO-FTS were found to be about ±1% to +4%, respectively, consistent in magnitude with the agreement between PARIS-IR and the Eureka DA8 FTS in this work.However, it should be noted that the MW regions for HCl and O 3 used in the two studies were different and this may contribute to the difference.

Partial column comparisons between ACE-FTS measurements and groundbased FTS observations
The concentration profiles of trace gases retrieved from ground-based observations provide limited vertical resolution (DOFS about 1 to 4 over the altitude range from the ground to 100 km, as shown in Table 2), much coarser than the vertical resolution (about 3-4 km) of observations from ACE-FTS.Because of this, the present comparisons are restricted to partial column abundances rather than profiles.As shown in Sung et al. (2007), the comparisons of partial columns from ground-based instruments with ACE-FTS results poses difficulties for molecules with maximum VMR in the troposphere (such as N 2 O or CH 4 ), particularly for an FTS with the resolution of PARIS-IR.Thus, we restrict our comparisons to molecules where the VMR peaks in the stratosphere.
There were 13 occultation measurements within 500 km of PEARL during the campaign.Coincident ground-based measurements occurred on eight days for the DA8 FTS and seven days for PARIS-IR, with multiple coincidences on some days for each instrument.The partial columns, C x , of the seven trace gases were calculated for ACE-FTS using where x stands for O 3 , HCl, ClONO 2 , HF, HNO 3 , NO 2 , or NO.; ρ(i ) (in molecules/cm 3 ), VMR x (i ), and Z(i ) (in cm) are the number density of air, the volume mixing ratio of the species x in the i th layer, and the thickness of the i th layer.The occultation measurements made by the ACE-FTS usually have different altitude ranges due to factors such as clouds limiting how low in altitude the measurements extend.Therefore, common altitude ranges were used for the partial columns calculated from the ACE-FTS profiles.These results are shown in Table 4 together with their altitude ranges, measurement dates, and occultation names.In addition, the uncertainty in each partial column density, as determined from the root-sum-square of the spectral fitting error from the corresponding ACE-FTS profile, is given.
For the two species where retrievals for the DA8 FTS and PARIS-IR were performed using two different MWs, only one was chosen for the comparisons with ACE-FTS based on the reasoning given below.The ACE-FTS version 2.2 update retrievals use a wide spectral region near 1120 cm −1 containing a high density of O 3 absorption lines.
During the development of the version 2.2 O 3 update, it was found that retrievals made using lines near 1100 cm −1 and those near 2775 cm −1 differed by ∼5% due to the 5323 spectroscopic parameters.To avoid this known inconsistency, O 3 column densities from MW2775 were not included in this section.For HNO 3 , both MW868 and MW872 results were available from the PARIS-IR and the DA8 FTS and, as shown in the previous section, are in good agreement (within 2%) in the total column density.The results from MW868 were used in the comparison with ACE-FTS since there was slightly better agreement between two ground-based FTSs for this MW than for MW872.When comparing measurements made at high latitudes, an additional coincidence criterion is often needed: this is the location relative to the polar vortex.The ACE-FTS partial column densities described above can be used to demonstrate this additional consideration.For example, three sunset measurements named ss13778, ss13793 and ss13794 were made within 500 km of PEARL by the ACE-FTS on 4 and 5 March 2006 (Fig. 2).The observation times for ss13778, ss13793 and ss13794 were 20:56:26 UT (4 March), 21:22:04 UT (5 March) and 22:59:47 UT (5 March), respectively.The partial columns for ss13793 and ss13794 (given in Table 4) show percentage differences of −8.11%, −6.79%, −38.06%, −12.32%, −14.88%, 1.96%, and 7.67% for O 3 , HCl, ClONO 2 , HF, HNO 3 , NO 2 , and NO, respectively.For O 3 , HCl, NO 2 and NO, these percentage differences are approximately within the combined estimated uncertainty of the partial column densities.However, for the other three species, the differences are larger than the uncertainty estimates.For ss13778 and ss13793, which differ in space by ∼30 km and time by ∼24 h, the observed partial columns show percentage differences of −18.14%, −16.83%, −71.18%, −40.51%, −37.45%, 11.14%, and −3.21%, for O 3 , HCl, ClONO 2 , HF, HNO 3 , NO 2 , and NO, respectively.These differences are much larger than the combined uncertainty estimates for all species except for NO.To determine if the same air mass was being sampled by these pairs of ACE-FTS measurements, the location of the polar vortex was investigated using scaled Potential Vorticity (sPV in units of 10 −4 s −1 ) calculated from the Goddard Earth Observing System version 4.03 (GEOS-4) analyses (Bloom et al., 2005).These results were obtained from the Derived Meteorological Products (DMPs) provided for the ACE-FTS occultation measurements (Manney et al., in press).sPV is the scaled (Dunkerton and Delisi, 1986;Manney et al., 1994) Rossby-Ertel potential vorticity (PV), which can be used to describe the intensity and extent of the polar vortex.In the stratosphere, the vortex edge region is typically at sPV values of about 1.2 to 1.6×10 −4 s −1 .For these three occultations, the sPV values at two altitudes (potential temperature levels) along the slant path were compared: 18.5 km (∼465 K) and 30.5 km (∼760 K) were chosen because they are near the peak in number density for O 3 , HCl, ClONO 2 , HF, and HNO 3 , and NO 2 and NO, respectively.At 18.5 km, the sPV values for ss13778, ss13794 and ss13793 are 1.07×10 −4 s −1 , 1.24×10 −4 s −1 and 1.37×10 −4 s −1 , respectively, corresponding to the measurement location moving from outside of the polar vortex into the vortex edge region.For the 30.5 km level, the values are 1.94×10 −4 s −1 , 2.22×10 −4 s −1 , and 2.26×10 −4 s −1 for ss13778, ss13794 and ss13793, respectively, which are all within the vortex.The change in the column densities of O 3 , HCl, ClONO 2 , HF and HNO 3 for ss13778, ss13794 and ss13793 is mirrored in the change in sPV at 18.5 km, which is the approximate altitude of the peak in number density for these species.Similarly, at 30.5 km, the change in sPV has the same behaviour as the change in NO 2 column density.Because of the magnitude of the uncertainty, no comment can be made about the trend in NO column density.This shows that considering sPV, in addition to spatial and temporal coincidence criteria, can assist in determining if similar air masses are being compared.It should be noted that during the campaign, the polar vortex in the lower stratosphere was rather poorly defined (see Manney et al., 2008 and detailed discussion in Sect.5.3).Because the vortex was weak with a lot of mixing with extravortex air, there is likely to be more dayto-day and measurement-to-measurement variability seen in these results than can be accounted for using a "strict" sPV vortex edge criterion.
To compare the partial column densities calculated from the ACE-FTS measurements with those from PARIS-IR and the DA8 FTS, the difference in the vertical resolution between the measurements has to be taken into account.This was done by smoothing the VMR profiles from the ACE-FTS using the averaging kernels from PARIS-IR and DA8 FTS retrievals (Rodgers and Connor, 2003).The VMR profiles from 5325 ACE-FTS were interpolated on to the 29-layer grid used for the ground-based FTSs.These profiles were extended below the lowest retrieved altitude using information from the ground-based FTS a priori profiles.Then these composite profiles were smoothed using the DA8 FTS and PARIS-IR averaging kernels and a priori profile.The vertical partial columns were recalculated using the smoothed ACE-FTS profiles in place of VMR x (i ) in Eq. ( 3).These smoothed ACE-FTS partial column densities were divided by the partial column results from the DA8 FTS and PARIS-IR (calculated over the same altitude range) to obtain the ratios in Table 5.Also, the mean percentage differences ({[ACE-FTS] -[ground-based FTS]}/[ground-based FTS]) and the 1σ standard deviation of the differences were calculated.As mentioned earlier, in order to make valid comparisons, the altitude ranges for the PARIS-IR and DA8 FTS partial columns were chosen to match those used for ACE-FTS.Over these altitude ranges, the PARIS-IR and DA8 FTS retrievals have averaging kernel values generally larger than 0.5 (as shown in Fig. 1), which indicates that retrieved columns of the investigated species are primarily obtained from observations rather than a priori information.All ACE-FTS measurements within 500 km of PEARL were used for this comparison.For PARIS-IR, the partial column densities of individual ground-based observations that were closest in time to the ACE-FTS observation were used.For the DA8 FTS, the daily mean of the partial column densities was used.Typically, two measurements were taken sequentially with each filter on each day with up to four sequential measurements on some days.
In Table 5, with the exception of the HNO 3 comparisons for PARIS-IR, the mean differences in the partial column densities between the ground-based FTSs and ACE-FTS are negative.However, for all of the species, the mean ratios and mean percentage differences are smaller than the total errors for the DA8 FTS and PARIS-IR reported in Table 2.The largest variation in the ratios is for ClONO 2 for which the standard deviations of the mean difference are 28.3% and 14.2% for DA8 FTS and PARIS-IR, respectively.To some degree, this reflects the challenge in retrieving this molecule from the ground-based spectra.In general, the results from PARIS-IR show better agreement with ACE-FTS than the DA8 FTS results.This is most likely due to better temporal coincidences.The temporal and spatial differences between the ACE-FTS and ground-based instruments are shown in Table 6 for PARIS-IR and Tables 7-10 for the DA8 FTS (each table corresponds to the group of molecules measured in each filter region).The PARIS-IR measurements are taken up to ∼4 h before the ACE-FTS occultation, with an average difference of ∼2 h.For the DA8-FTS, the maximum temporal differences are between ∼5 and ∼8.5 h and the average differences are ∼3.5 to ∼7 h.All of the ACE-FTS measurements were selected because they occurred within 500 km of PEARL.However, this does not necessarily reflect the distance between the ACE-FTS occultation and the ground-based FTS measurement.This was calculated using the method described above and the distances between the ACE-FTS occultation location and the ground-based measurement (using the 18-km altitude tangent point as representative of the region of the atmosphere being sampled) are given in Tables 6-10.The spatial differences between the ACE-FTS and PARIS-IR observations are on average 400 km with a maximum of 700 km.For the DA8 FTS and ACE-FTS comparisons, the maximum spatial differences are ∼500-600 km and the average values are between 300 and 400 km.Because these distances between the measurements can be larger than the stated distance coincidence criterion, it is important to ensure that the comparisons are considering similar air masses using sPV.This is given in Tables 6 through 10 for the ∼18 km and ∼30 km altitudes for each of the measurements.
Based on the values at ∼18 km, these measurements are primarily sampling outside or on the edge of the vortex (sPV<1.4×10−4 s −1 ) with the exception of 13 March 2006 where both are inside (sPV ∼1.8×10 −4 s −1 ).At ∼30 km, all sPV values are greater than 1.6×10 −4 s −1 indicating that the measurements are sampling inside the vortex.At both levels, there are no obvious mismatches (one measurement inside and the other outside) which could contribute to the differences seen between the ACE-FTS and ground-based measurements.
As part of the validation of the ACE-FTS version 2.2 (plus updates) data products, comparisons of partial column densities have been made between measurements by 5327 ACE-FTS and high-resolution ground-based FTSs.The same smoothing and partial column calculation techniques were used for all of the studies.However, these results differ in some respects from the current study because wider time ranges were used (typically February 2004 through December 2006, rather than only during spring 2006) and, in some cases, broader coincidence criteria were used (up to 1000 km; ±24 h).Despite these differences, our results are in reasonable agreement for all species.For example, Dupuy et al. (2008) found percentage differences between −10 and +7% for their O 3 comparisons and the DA8 FTS and PARIS-IR results (−5.9% and −5.2%, respectively) fall within this range.Comparisons for HCl and HF, done by Mahieu et al. (2008), show average agreement between the ground-based FTS and ACE-FTS partial column densities of approximately +6% and +8%, respectively.Here the differences for HCl and HF are −4.6% and −4.7%, for PARIS-IR, and −8.5% and −0.9% for the DA8 FTS, respectively.The differences found for ClONO 2 by Wolff et al. (2008) covered a wide range from −34% to +56% with a large standard deviation for the mean difference of ±35%.The mean differences and standard deviation of the differences found in this study are consistent with the work of Wolff and coworkers.For HNO 3 , the percentage differences found by Wolff et al. (2008) ranged from -13% to +6% and are consistent with the results obtained here which were differences of −6.6% with the DA8 FTS and +5.7% with PARIS-IR.Finally for NO 2 and NO, Kerzenmacher et al. (2008) reported differences between ground-based FTSs and ACE-FTS between −9% and +21% for NO 2 and the current results for the DA8 FTS and PARIS-IR fall within this range (−4.6% and −5.2%, respectively).During the campaign, only the DA8 FTS was able to provide NO results and these partial columns differed from ACE-FTS by −9.9%.This difference is smaller in magnitude than that found by Kerzenmacher et al., who reported differences between −14.5% and −67.5%.
Figure 6 shows scatter plots of the ACE-FTS partial column densities versus the ground-based FTS partial column densities for O 3 , HCl, and HF.The PARIS-IR and DA8 FTS results are both included on each plot.The plots show good correlation between the satellite and ground-based data sets.For the regression fits (shown in dotted black line), both the DA8 and PARIS-IR results were fitted together and the intercepts were set to zero because of the limited number of data points available.The fitted slopes are slightly smaller than one in all cases.

Time evolution of trace gases during the 2006 Canadian Arctic ACE validation Campaign
The satellite observations together with meteorological analyses have previously been used to study the Arctic vortex, temperature and trace gas evolution over Eureka during the 2003-2004, 2004-2005and 2005-2006winters (Manney et al., 2008)).The 2005-2006 winter had a very strong, prolonged major "stratospheric sudden warming" (SSW) beginning in early to mid January 2006 that ended in the mid-to late February 2006.After the SSW, a pole-centred strong vortex redeveloped quickly in the lower mesosphere.Throughout the campaign, the vortex was recovering and strengthening in the upper stratosphere.Figures 1 to 3 of Manney et al. (2008) show the relative position of PEARL and the polar vortex using maps of sPV on the 1700 K, 850 K and 490 K potential temperature surfaces.In the lower stratosphere (490 K), the vortex did not recover significantly from the SSW so during the 2006 campaign it was fairly weak and poorly defined.This picture is shown in terms of sPV in Fig. 10 of Manney et al. (2008) and consistent with the time series of sPV values for the measurements made by ACE-FTS and the ground-based FTSs during the campaign.The campaign time series is shown in panel e of Fig. 7 for altitudes of 18 km, 26 km, and 36 km along the slant paths of the DA8 FTS and ACE-FTS observations from 21 February to 31 March 2006.For ACE-FTS, the 18.5 km, 26.5 km and 36.5 km levels were used for this plot.At 36 km, the sPV values are larger than 2×10 −4 s −1 during the entire campaign which is consistent with the Arctic vortex strongly reforming after the SSW.In the middle stratosphere (26 km), the sPV values tend to be larger than 1.6×10 −4 s −1 and are generally increasing throughout the measurement period.This is consistent with the vortex strengthening and reforming over Eureka during this time.In the lower stratosphere (18 km), the 5329 sPV values vary between about 1×10 −4 s −1 and 1.4×10 −4 s −1 (with a few days having sPV values of greater than 1.6×10 −4 s −1 ).Therefore, the measurements at this altitude are primarily made outside or in the vortex edge region.When investigating changes in trace gas species with time, it is useful to be able to separate chemical and dynamical effects.Previous studies have used long-lived tracers such as HF, to normalize the column densities of stratospheric species in order to remove most of the dynamical effects such as diabatic descent (Toon et al., 1999;Mellqvist et al., 2002).This technique works well because the O 3 , ClONO 2 , HCl, HNO 3 , and HF atmospheric profiles have similar shapes with peak values in the stratosphere.For this study, the total columns of O 3 , HCl, ClONO 2 , and HNO 3 from PARIS-IR and the DA8 FTS were normalized by taking ratios with the total columns of HF and the results are shown in panels a-d of Fig. 8, respectively.Because the DA8 FTS cannot measure ClONO 2 , HCl, HNO 3 , and O 3 simultaneously with HF (the MWs are not in the same filter band), the daily mean total column densities were used for this investigation.For PARIS-IR, individual simultaneous measurements were used to compute the ratios and these ratios were then averaged to obtain the daily mean column ratios of For the three days where there are measurements from both instruments, PARIS-IR and the DA8 FTS are in reasonable agreement and have similar trends.The same normalization procedure was also applied to the ACE-FTS partial column densities of O 3 , ClONO 2 , HCl, HNO 3 and HF.
For each species, the altitude range for the partial column ratio was chosen to match the range where retrievals were available for both the molecule and HF.The ACE-FTS partial column density ratios are expected to have an offset from those obtained from the ground-based FTSs because the satellite profiles were truncated in the lowermost stratosphere due to the altitude range available for the ACE-FTS HF data.The results for ACE-FTS and the ground-based spectrometers appear to have similar trends.
The time evolution of the ratios, [HCl]/[HF], [ClONO 2 ]/[HF], [HNO 3 ]/ [HF], and [O 3 ]/[HF], is consistent with the region of the polar vortex that is sampled by these measurements.For this discussion, we will use the sPV values at 18 km because the maximum number density of all of these species is near this altitude (for the Arctic at this time of year).Based on sPV at 18 km, the ground-based campaign measurements can be divided between those primarily inside the vortex (13-16 March and 28-31 March) and those primarily near the edge or outside of the vortex .This classification corresponds to air masses having sPV values greater or less than 1.6×10 −4 s −1 .For HCl, HNO 3 and O 3 , the ratios inside the vortex are slightly lower than those outside and on the edge of the vortex as is expected in polar springtime.The ClONO 2 ratio values obtained for the inside and outside/edge regions are more similar.To look at the correlation more closely, the ratio of The partitioning of chlorine during the 2006 Arctic vortex has been investigated using measurements from two satellite instruments, the Microwave Limb Sounder (MLS) on Aura and ACE-FTS on SCISAT, and the SLIMCAT three-dimensional chemical transport model (Santee et al., in press). Tey found that the SSW in mid-January essentially caused chemical processing in the vortex to end and chlorine deactivation to begin. Tis can be seen in Fig. 6 of Santee et al. which shows the time series of vortex average HCl, ClONO 2 , and ClO at the 520 K potential temperature level for four 5 •wide equivalent latitude bands from 65 • to 80 • .By the beginning of the ground-based FTS measurements in late February, chlorine deactivation within the vortex was nearly complete and there were thus no rapid or significant changes in HCl and ClONO 2 VMRs observed at Eureka throughout the six weeks of the campaign.For the inside the vortex measurements, this relatively constant behaviour is what was seen in the ground-based FTS ratios of HCl and ClONO 2 with HF from PEARL (Fig. 7).Similarly, within the vortex, there was no rapid change in O 3 VMR, and the HNO 3 VMR was observed to decline slowly by MLS and ACE-FTS from late February to the end of March (e.g., Fig. 7 in Santee et al., in press).This behaviour can be seen in the PARIS-IR and DA8 FTS O 3 in-vortex results.However, it is difficult to discern a trend in HNO 3 5331 from the relatively few points obtained within the vortex from the ground-based FTS measurements.For those ground-based FTS measurements taken within or near the edge of the vortex, there appears to be a small decrease in the ratios of O 3 , HNO 3 and HCl over the campaign period whereas the ClONO 2 does not show as significant a change.

Summary and conclusions
The 2006 Canadian Arctic ACE Validation Campaign made measurements for the Atmospheric Chemistry Experiment (ACE) satellite mission at PEARL, Eureka from 17 February until 31 March in 2006.The DA8 FTS and PARIS-IR observations were performed simultaneously so that instrument performance could be compared directly.
The solar beam was shared between the two FTSs and spectral co-additions were performed over the same time intervals to ensure simultaneity.From these spectra, vertical total columns and partial columns of O 3 , ClONO 2 , HCl, HNO 3 , NO, NO 2 , and HF were retrieved using the SFIT2 program (version 3.91).Mean differences in total column densities of O 3 , HNO 3 , NO 2 , HCl, HF, and ClONO 2 from the observations between PARIS-IR and the DA8 FTS are 2.84%, −1.94%, −0.08%, −3.22%, −1.45% and −4.28%, respectively.These differences are comparable to those seen in earlier intercomparison studies for both instruments.By using the same analysis program, spectroscopic parameters, spectral regions, and a priori information to analyze the spectra recorded by PARIS-IR and the DA8 FTS, these differences can be taken to be due to instrumental differences such as spectral resolution.
The ground-based observations using the DA8 FTS and PARIS-IR were compared with the version 2.2 (plus updates) results from the ACE-FTS satellite instrument using partial column densities.The results from PARIS-IR in general agree better with the ACE-FTS than those from the DA8 FTS for all of the investigated species.This has been attributed to better temporal coincidence with ACE-FTS observations for PARIS-IR than for the DA8 FTS measurements.Ground-based partial column results agree with the ACE-FTS partial column results to within the uncertainty estimated for the DA8 FTS and PARIS-IR and the results are consistent with those found in the other ACE-FTS version 2.2 validation studies.To verify that the air masses measured by each of the instruments in these comparisons were similar, the tangent points of the altitudes with the maximum number density for the species of interest were calculated geometrically and the scaled potential vorticity at these levels were compared.This method provided an additional verification that the comparisons were valid.
The results from the three FTSs (ACE-FTS, PARIS-IR, and the DA8 FTS) were used to probe the time evolution of chemical constituents in the atmosphere over Eureka during spring 2006.For this investigation, the effects of subsidence were removed by normalizing the column densities using the long-lived tracer HF.There were no significant changes observed in O 3 , HCl, ClONO 2 , and HNO 3 amounts recorded inside the polar vortex during the campaign.These observations are generally consistent with the results of Santee et al. (in press), who showed that chemical processing within the polar vortex in spring 2006 had nearly ceased by the beginning of the campaign at Eureka..5-84.5 11.5-47.5 14.5-30.5 13.5-44.5 10.5-31.5 17.5-35.5∆ is distance from ACE-FTS occultation measurement to PEARL.d ACE-FTS partial column error was calculated from the spectral fitting error for each measurement.This value is given in parentheses.3.For the measurements using ozonesondes, the total columns were estimated by extrapolating above the highest measured altitude and the uncertainty given is ±6% (taken from Tarasick et al., 2005).2. Red dashed lines and blue dashed lines indicate the daily mean total column densities measured by the DA8 FTS (red squares) and PARIS-IR (blue diamonds), respectively.
Fig. 3. Here, the individual PARIS-IR and DA8 FTS MW1120 ozone observations from 4 March 2006 are shown and the daily mean value is indicated.When the measurements from the two FTSs were made simultaneously, there was good agreement within the respective uncertainties.However, because the ozone column densities retrieved by PARIS-IR differed throughout the day as the measurement location and time changed, the daily mean values for the DA8 FTS and PARIS-IR do not agree as well as the simultaneous measurements.These differences observed between the daily mean comparisons and individual comparisons vary with day and with species.Panel d of Fig.3shows the ozone total column density results for PARIS-IR and the DA8 FTS on 5 March 2006.Here the daily mean results are in better agreement.Figures4 and 5provide similar comparisons for HCl, ClONO 2 , HNO 3 , HF, and NO 2 total column densities on 5 March and 7 March 2006, respectively.The daily mean and individual comparisons for these days generally agree within the uncertainties.
from ACE-FTS occultation measurement to PARIS-IR observation.d ∆ 3 is the difference in time between the ACE-FTS occultation measurement and the DA8 FTS observation.e The scaled Potential Vorticity (sPV) at altitudes of 18.5 km and 18.0 km along the optical paths of the ACE-FTS and PARIS-IR, respectively.f The scaled Potential Vorticity (sPV) at altitudes of 30.5 km and 30.0 km along the optical paths of the ACE-FTS and PARIS-IR, respectively.

d∆ 3
is the difference in time between the ACE-FTS occultation measurement and the DA8 FTS observation.e The scaled Potential Vorticity (sPV) at altitudes of 18.5 km and 18.0 km along the optical paths of the ACE-FTS and DA8 FTS, respectively.f The scaled Potential Vorticity (sPV) at altitudes of 30.5 km and 30.0 km along the optical paths of the ACE-FTS and DA8 FTS, respectively.

c∆ 2
is distance from ACE-FTS occultation measurement to DA8 FTS observation.d ∆ 3 is the difference in time between the ACE-FTS occultation measurement and the DA8 FTS observation.e The scaled Potential Vorticity (sPV) at altitudes of 18.5 km and 18.0 km along the optical paths of the ACE-FTS and DA8 FTS, respectively.f The scaled Potential Vorticity (sPV) at altitudes of 30.5 km and 30.0 km along the optical paths of the ACE-FTS and DA8 FTS, respectively.

Fig. 3 .
Fig. 3. O 3 total vertical column densities obtained from the spectra near MW 1120 cm −1 (MW1120) recorded using PARIS-IR (blue diamonds) and the DA8 FTS (red squares) during the 2006 Canadian Arctic ACE Validation Campaign are shown together with total columns calculated from ozonesonde measurements (black circles).Panels (a) and (b) show the individual and the daily mean column densities for the entire campaign period, respectively.Enlarged views of daily observations and uncertainties of total column densities on 4 and 5 March 2006 are shown in panels (c) and (d), respectively.Red and blue dashed lines indicate the daily mean vertical column densities for the DA8 FTS and PARIS-IR, respectively.The errors for DA8 and PARIS-IR are the total percent errors given in Table3.For the measurements using ozonesondes, the total columns were estimated by extrapolating above the highest measured altitude and the uncertainty given is ±6% (taken fromTarasick et al., 2005).

Fig. 4 .
Fig. 4. Total vertical column densities of HCl (a), ClONO 2 (b), HNO 3 (MW 868) (c), HF (d), and NO 2 (e) retrieved from spectra obtained with PARIS-IR and the DA8 FTS at PEARL on 5 March 2006.Error bars indicate the DA8 FTS and PARIS-IR total percentage errors given in Table2.Red dashed lines and blue dashed lines indicate the daily mean total column densities measured by the DA8 FTS (red squares) and PARIS-IR (blue diamonds), respectively.
W, 610 m above sea level) in Eureka, Nunavut, Canada, from 17 February to 31 March 2006.A combination of ten scientific instruments was used for the campaign, including terrestrial versions of ACE-FTS (Portable Atmospheric Research Interferometric Spectrometer for the Infrared, PARIS-IR; • N, 86.42  •

Table 1 .
Species, spectral ranges of microwindows, interfering species, and filters used in ground-based observations.Filters were placed in front of the entrance aperture of the DA8 FTS to improve the SNR of the measurements.See text for the spectral ranges of filters used in observations.c Several spectral ranges from individual spectra were used in the retrievals simultaneously; also known as "multi-microwindow" fitting.d PARIS-IR has no results for NO from the 2006 Canadian Arctic ACE Validation Campaign.5341 a Microwindow region.b

Table 2 .
Degrees of freedom for signal and uncertainties in the retrievals of total vertical column densities obtained from measurements by the DA8 FTS and PARIS-IR.

Table 3 .
Comparisons of total columns observed by the DA8 FTS and PARIS-IR from 21 February to 8 March 2006.See Table 1 for spectral ranges of microwindows.bSee text for calculation method description.Uncertainty given is the 1σ standard deviation of the mean difference.5343 a

Table 4 .
Partial columns calculated from ACE-FTS measurements taken during the 2006 Canadian Arctic ACE Validation Campaign.

Table 6 .
The spatial and temporal differences between PARIS-IR and ACE-FTS observations a Universal time of observation.b∆1 is distance from ACE-FTS occultation measurement to PEARL.

Table 7 .
The spatial and temporal differences between DA8 and ACE-FTS observations for O 3 , HNO 3 , and ClONO 2 during the 2006 Canadian Arctic ACE Validation Campaign.∆ 3 is the difference in time btween the ACE-FTS occultation measurement and the DA8 FTS observation.e The scaled Potential Vorticity (sPV) at altitudes of 18.5 km and 18.0 km along the optical paths of the ACE-FTS and DA8 FTS, respectively.5347 a Universal time of observation.b ∆ 1 is distance from ACE-FTS occultation measurement to PEARL.c ∆ 2 is distance from ACE-FTS occultation measurement to DA8 FTS observation.d

Table 8 .
The spatial and temporal differences between DA8 and ACE-FTS for HCl and NO 2 during the 2006 Canadian Arctic ACE Validation Campaign.
b∆ 1 is distance from ACE-FTS occultation measurement to PEARL.c ∆ 2 is distance from ACE-FTS occultation measurement to DA8 FTS observation.

Table 9 .
The spatial and temporal differences between DA8 and ACE-FTS for HF during the 2006 Canadian Arctic ACE Validation Campaign.∆ 1 is distance from ACE-FTS occultation measurement to PEARL.c ∆ 2 is distance from ACE-FTS occultation measurement to DA8 FTS observation.d ∆ 3 is the difference in time between the ACE-FTS occultation measurement and the DA8 FTS observation.e The scaled Potential Vorticity (sPV) at altitudes of 18.5 km and 18.0 km along the optical paths of the ACE-FTS and DA8 FTS, respectively.5349 a Universal time of observation.b

Table 10 .
The spatial and temporal differences between DA8 and ACE-FTS for NO during the 2006 Canadian Arctic ACE Validation Campaign.
a Universal time of observation.b ∆ 1 is distance from ACE-FTS occultation measurement to PEARL.