Issue 
A&A
Volume 639, July 2020



Article Number  A69  
Number of page(s)  11  
Section  Planets and planetary systems  
DOI  https://doi.org/10.1051/00046361/202037741  
Published online  09 July 2020 
HDO and SO_{2} thermal mapping on Venus
V. Evidence for a longterm anticorrelation
^{1}
LESIA, Observatoire de Paris, PSL University, CNRS, Sorbonne Université, Université de Paris,
92195
Meudon, France
email: therese.encrenaz@obspm.fr
^{2}
SwRI,
Div. 15,
San Antonio,
TX
78228, USA
^{3}
LATMOS/IPSL, UVSQ Université ParisSaclay, Sorbonne Université, CNRS,
78280
Guyancourt, France
^{4}
Kyoto Sangyo University,
Kyoto
6038555, Japan
^{5}
LMD/IPSL, Sorbonne University, ENS, PSL University, Ecole Polytechnique, University Paris Saclay, CNRS,
75252
Paris Cedex 05, France
^{6}
Planetary Science Laboratory, University of Michigan,
Ann Arbor
MI
481092143, USA
^{7}
Zentrum fuer Astronomie und Astrophysik, Technische Universitaet Berlin,
Hardenbergstr. 36,
10623
Berlin, Germany
^{8}
Jet Propulsion Laboratory,
Pasadena,
CA
91109, USA
^{9}
Hokkaido Information University,
Hokkaido
0698585, Japan
^{10}
Department of Earth and Planetary Sciences, University of California,
Santa Cruz,
CA
95064, USA
Received:
14
February
2020
Accepted:
19
May
2020
Since January 2012, we have been monitoring the behavior of sulfur dioxide and water on Venus, using the Texas Echelon CrossEchelle Spectrograph imaging spectrometer at the NASA InfraRed Telescope Facility (IRTF, Mauna Kea Observatory). Here, we present new data recorded in February and April 2019 in the 1345 cm^{−1} (7.4 μm) spectral range, where SO_{2}, CO_{2}, and HDO (used as a proxy for H_{2}O) transitions were observed. The cloud top of Venus was probed at an altitude of about 64 km. As in our previous studies, the volume mixing ratio (vmr) of SO_{2} was estimated using the SO_{2}/CO_{2} line depth ratio of weak transitions; the H_{2}O volume mixing ratio was derived from the HDO/CO_{2} line depth ratio, assuming a D/H ratio of 200 times the Vienna standard mean ocean water. As reported in our previous analyses, the SO_{2} mixing ratio shows strong variations with time and also over the disk, showing evidence for the formation of SO_{2} plumes with a lifetime of a few hours; in contrast, the H_{2}O abundance is remarkably uniform over the disk and shows moderate variations as a function of time. We have used the 2019 data in addition to our previous dataset to study the longterm variations of SO_{2} and H_{2}O. The data reveal a longterm anticorrelation with a correlation coefficient of −0.80; this coefficient becomes −0.90 if the analysis is restricted to the 2014–2019 time period. The statistical analysis of the SO_{2} plumes as a function of local time confirms our previous result with a minimum around 10:00 and two maxima near the terminators. The dependence of the SO_{2} vmr with respect to local time shows a higher abundance at the evening terminator with respect to the morning. The dependence of the SO_{2} vmr with respect to longitude exhibits a broad maximum at 120–200° east longitudes, near the region of Aphrodite Terra. However, this trend has not been observed by other measurements and has yet to be confirmed.
Key words: planets and satellites: atmospheres / planets and satellites: terrestrial planets / infrared: planetary systems
© T. Encrenaz et al. 2020
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
1 Introduction
The atmospheric chemistry of Venus is driven by the cycles of water and sulfur dioxide (Krasnopolsky 1986, 2007, 2010; Mills et al. 2007; Zhang et al. 2012). Below the clouds, both species are present with relatively large abundances (about 30 ppmv and 130 ppmv respectively, Bézard & De Bergh 2012, Marcq et al. 2018) and, at low latitude, they are transported upward by Hadley convection. Following the SO_{2} photodissociation and the combination of SO_{3} with H_{2}O, sulfuric acid H_{2}SO_{4} is formed and condenses as the main component of the cloud deck. Above the cloud top, the volume mixing ratios of H_{2}O and SO_{2} drop drastically to about 1–3 ppmv (Fedorova et al. 2008; Belyaev et al. 2012) and 10–1000 ppbv (Zasova et al. 1993; Marcq et al. 2013, 2020; Vandaele et al. 2017a,b), respectively.
The water and sulfur dioxide cycles have been extensively monitored over several decades, using Pioneer Venus, the Venera 15 spacecraft, Venus Express, and Akatsuki by imaging and spectroscopy in the ultraviolet and infrared ranges. As a complementto these datasets, we have been using imaging spectroscopy in the thermal infrared since 2012 to map SO_{2} and H_{2}O at the cloudtop of Venus and to monitor the behavior of these two species as a function of time, both in the short term (a few hours) and the long term (years). Thirteen runs were recorded between 2012 and 2019. The results of the first 11 runs (January 2012–September 2018) have been presented in Encrenaz et al. (2012, 2013, 2016, 2019), which are referred as E12, E13, E16, and E19, hereafter. The main result of these studies is that SO_{2} and H_{2}O exhibit very different behaviors. We note that H_{2}O is always uniformly distributed over the disk and shows moderate variations in the long term. In contrast, the SO_{2} maps most often show sporadic plumes which appear and disappear within a time scale of a few hours. The diskintegrated SO_{2} abundance shows strong variations over the long term, with a contrast factor of about 10 between the minimum value observed in February 2014 and the maximum value from July 2018.
In this paper, we first describe the observations performed in February and April 2019 (Sect. 2). Then we use the whole TEXES data set (2012–2019) at 7.4 μm to study the longterm evolution of H_{2}O and SO_{2} (Sect. 3). Finally we update our statistical analysis of the SO_{2} plumes (E19), regarding their appearance as a function of latitude, longitude and local time (Sect. 4). The results are discussed in Sect. 5 and the conclusions are summarized in Sect. 6.
2 Observations
2.1 The data
TEXES (Texas Echelon Cross Echelle Spectrograph) is an imaging highresolution thermal infrared spectrometer in operation at the NASA InfraRed telescope Facility (Lacy et al. 2002), which combines high spectral capabilities (R = 80 000 at 7 μm) and spatial capabilities (around 1 arcsec). As for our previous observations, we selected the 1342–1348 cm^{−1} (7.4 μm) interval in order to optimize the number of weak and strong transitions of SO_{2}, HDO and CO_{2}. The diameter of Venus was 17 arcsec in February 2019 and 12 arcsec in April 2019. The Doppler shift, at 1345 cm^{−1}, was between −0.045 and −0.043 cm^{−1} in February 2019 and between +0.045 and +0.043 cm^{−1} in April 2019. The length and the width of the slit were 6.0 and 1.0 arcsec respectively at 7.4 μm.
As we did previously, we aligned the slit along the northsouth celestial axis and we shifted it from west to east, with a step of half the slit width and an integration time of 2 s per position to cover the planet in longitude from limb to limb, and to add a few pixels on the sky beyond each limb for sky subtraction. Since the rotation axis of Venus is close to the celestial axis, each scan corresponds to a given latitude range of about 6 arcsec. As the diameter of Venus was always larger than the slit length, we multiplied the scans to cover the full latitude range from north to south with some overlap. Table 1 summarizes the TEXES observations in February and April 2019. This table lists the maps which were obtained at 1345 cm^{−1}, with, in each case,the time of beginning and end of the observation, its midtime, and the number of scans used to build the maps. A scan at a given latitude was usually repeated at least twice. Typically, twelve scans were used to cover the whole latitude range; their number varied according tothe meteorological conditions; in some cases, some scans were removed if the terrestrial atmospheric transmission is too strong.
The TEXES data cubes were calibrated using the standard radiometric method (Lacy et al. 2002, Rohlfs & Wilson 2004). Calibration frames consisting of three measurements (black chopper blade, sky and lowemissiviy chopper blade) were systematically taken before each observing scan, and the difference (blacksky) was taken as a flat field. If the temperature of the black blade, the telescope and the sky are equal, this method corrects both telescope and atmospheric emissions. The atmospheric correction, however, is not complete for all terrestrial atmosphericlines, partly because these lines are not all formed at the same atmospheric levels, and thus have different temperatures. For these reasons, we did not try to correct the terrestrial atmospheric features and we selected SO_{2} and CO_{2} lines locatedoutside these features. In the case of HDO, it was not always possible; this is why, in some cases, HDO maps could not be retrieved (see below).
Figure 1 shows the geometrical configurations of the disk of Venus during the two runs of February and April 2019, which both correspond to the morning terminator. Figures 2 and 3 show representative diskintegrated spectra corresponding to the runs of February 2019 and April 2019, respectively. The spectral range (1344.8–1345.4 cm^{−1}) includes several weak SO_{2} transitions, two weak CO_{2} lines and one weak HDO line. As in our previous studies (see E19), we used the HDO line at 1344.90 cm^{−1}, the SO_{2} multiplet at 1345.1 cm^{−1} and the CO_{2} line at 1345.22 cm^{−1} in order to retrieve the H_{2}O and SO_{2} mixing ratios directly from the line depth ratios. For the conversion from the line depth ratios (ldr) into the volume mixing ratios (vmr), the following equations were used (E16, E19):
vmr (SO_{2})(ppbv) = ldr (SO_{2}) × 600.0
vmr (H_{2}O)(ppmv) = ldr (HDO) × 1.5.
To convert the HDO vmr into the H_{2}O vmr, we assume, above the clouds, a D/H ratio of 200 times the Vienna standard ocean water (VSMOW). We adopted this value in 2012, following Krasnopolsky (2010), as an averaged value from previous measurements (Bjoraker et al. 1992; Bertaux et al. 2007; Fedorova et al. 2008). We are aware of the uncertainty associated with this parameter (Krasnopolsky et al. 2013), but we keep the enrichment factor of 200 with respect to the terrestrial value for consistency within our analysis.
Figure 4 shows two maps of the CO_{2} line depth, corresponding to each of our two observing runs. The CO_{2} line depth gives us information on the temperature gradient just above the level which is probed in the continuum (E13, E16). As shown in Fig. 1, the 2019 data were recorded when the morning terminator was observed. As mentioned earlier, the signature of a thermal cooling at high latitude is expected at that time (see E13 and E16), so we would expect that the depth of the CO_{2} lines would be zero or even negative at high latitudes, as observed in E13. Surprisingly, this effect does not clearly appear in Fig. 4. We already mentioned in E19 that the effect of the thermal cooling near the polar collars, clearly observed in E16 (2012–2016), does not appear systematically in the forthcoming observations. The analysis of the thermal profile and its variations with time and longitude will be the topic of a forthcoming publication.
Summary of TEXES observations of February and April 2019.
Fig. 1
Geometrical configurations of the disk of Venus during the two TEXES runs of February and April 2019. The terminator is indicated with a black line and the subsolar point with a black dot. Both configurations show the morning terminator. 

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Fig. 2
Examples of diskintegrated spectra of Venus between 1344.8 and 1345.4 cm^{−1} (7.4 μm) recorded in February 2019. It can be seen that the broad terrestrial atmospheric absorption feature around 1344.95 cm^{−1} varies strongly from day to day. 

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Fig. 3
Examples of diskintegrated spectra of Venus between 1344.8 and 1345.4 cm^{−1} (7.4 μm) recorded in April 2019. Due to the strong terrestrial absorption around 1344.95 cm^{−1}, the depth of the HDO line at 1344.90 cm^{−1} could not be measured on April 21–24, 2019. 

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Fig. 4
Examples of maps of the line depth of the weak CO_{2} transition at 1345.22 cm^{−1} (7.4 μm), corresponding to the observations shown in Figs. 2 and 3. The scale is the same for the two maps. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

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Fig. 5
Examples of maps of the line depth ratio of a weak SO_{2} multiplet (around 1345.1 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded in February 2019 (one map per observing day). Diskintegrated spectra corresponding to these maps are shown in Fig. 2. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

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Fig. 6
Examples of maps of the line depth ratio of a weak SO_{2} multiplet (around 1345.1 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded in April 2019 (one map per observing day). Diskintegrated spectra corresponding to these maps are shown in Fig. 3. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

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2.2 SO_{2} maps
Figures 5 and 6 show examples of maps of the SO_{2} volume mixing ratioobtained from the data shown in Figs. 2 and 3, using the transitions mentioned above. One map per day is shown, in February 2019 (Fig. 5) and in April 2019 (Fig. 6). As in previous cases, SO_{2} variations are obvious, both locally over the Venus disk and on a time scale of 24 h.
As an illustration of the shortterm behavior of the SO_{2} plumes, Fig. 7 shows a time sequence of SO_{2} at the cloud top on April 16, 2019. The figure shows the fast depletion of a strong SO_{2} plume on a time scale of two hours. The peak intensity of the SO_{2} plume is close to its maximum value over the whole 2012–2019 period.
A surprising example of the SO_{2} distribution over the Venus disk is shown in Fig. 8. Two SO_{2} maps, recorded on April 20, 2019 and separated by about one hour, show a very high SO_{2} vmr all over the disk (near 600 ppbv, corresponding to a SO_{2} /CO_{2} line depth ratio close to 1.0), with a local maximum, higher than 1 ppmv, near the subsolar point, which decreases within a time scale of one hour. The location of the plume, near the subsolar point, is unusual, as well as the local SO_{2} maxima which might be due to some artifact. Near the limb, our retrieval method becomes very uncertain due to the large airmass factor. Previous analyses have shown that in the case of lines depths of 10 percent or less, the departure from linearity may induce an uncertainty of about 10 percent, and up to 20 percent at the limb (Encrenaz et al. 2015). In addition, the observationsof April 2019 refer to the morning terminator. We have seen that, in this case, a temperature inversion is observed near the polar collars, making the retrieval of minor species very difficult at high latitude. This is why the high latitude part of the map is not shown in the figure. In view of these uncertainties, the maps of April 18, 2019 have not been included in our statistical analysis (see below). Figure 8 illustrates the variety of behaviors shown by the SO_{2} plumes, which are discussed in Sect. 5.
Fig. 7
Maps of the line depth ratio of a weak SO_{2} multiplet (around 1345.1 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded onApril 16, 2019. The figure on the left (18:23 UT) is the same as in Fig. 6. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

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Fig. 8
Maps of the line depth ratio of a weak SO_{2} multiplet (around 1345.1 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded on April 20, 2019. The figure on the left (27:27 UT) is the same as in Fig. 6, with a different scale. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

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Fig. 9
Maps of the line depth ratio of the weak HDO transition (at 1344.90 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded during the February 2019 run. Data are the same as in Figs. 2 and 5. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

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Fig. 10
Examples of maps of the line depth ratio of the weak HDO transition (at 1344.90 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded during the April 2019 run. Data are the same as in Figs. 3 and 6. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. Data of April 21–24 are not shown because theterrestrial atmospheric absorption (see Fig. 3) is too strong for the HDO retrieval to be reliable. 

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2.3 HDO maps
Figure 9 shows examples of HDO maps recorded in February 2019, corresponding to the same data as shown in Figs. 2 and 5. Figure 10 shows examples of HDO maps corresponding to the April 2019 run, using the data shown in Figs. 3 and 6. Only six HDO maps are shown in Fig. 10 because,due to the strong telluric absorption (Fig. 3), HDO could not be reliably measured in the data of April 21–24.As observed in our previous observations, the HDO maps are homogeneous over the disk, but the diskaveraged H_{2}O volume mixing ratioshows a global decrease with time, as compared with previous data (E13, E16, E19). As shown in Fig. 10, the diskaveraged H_{2}O mixing ratio, measured at the end of the February run and during the April run, is close to 0.5 ppmv (corresponding to a HDO/CO_{2} line depth ratio around 0.3), i.e. lower than the maximum diskaveraged values of SO_{2} observed on April 16 and 20, 2019. The time variability of H_{2}O and its relationship with SO_{2} are discussed in Sect. 5.
Fig. 11
Longterm variations of the H_{2}O volume mixing ratio (top, blue points), inferred from the HDO measurements, and the SO_{2} volume mixing ratio (bottom, red points), measured at the cloud top from the TEXES data at 7.4 μm. A daily mean is shown in this figure. The black squares are the mean values of the H_{2}O and SO_{2} mixing ratios averaged over each run. In 3 cases (Dec. 2017–Jan. 2018, JulySept. 2018, Feb.–Apr. 2019), we have coadded alldata (separated by less than 3 months), in order to have a more homogeneous time sampling over the long term. 

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3 Longterm variations of the H_{2}O and SO_{2} abundances at the cloud top
Figure 11 shows the longterm variations of H_{2}O and SO_{2} since 2012. From 2012 to 2018, the data are the same as in E19, but we have chosen to show a single point per day because, as shown in E19, a SO_{2} plume is most often observed over a full day. It can be seen that SO_{2} exhibits larger and larger shortterm variations as the mean diskaveraged abundance of SO_{2} increases. In order to eliminate these shortterm variations, we have also plotted the data using a single mean abundance of H_{2}O and SO_{2} per run, and we have coadded the points separated by less than 3 months, which gives a total number of 10 points (Fig. 11). The data reveal, over the long term, an anticorrelation between H_{2}O and SO_{2}, with a correlation coefficient of −0.80. It is interesting to note that the anticorrelation is even stronger if the two first points, corresponding to 2012, are removed: indeed, if we consider only the 8 points between 2014 and 2019, the correlation coefficient is −0.90. The significance of this anticorrelation is discussed in Sect. 5.
4 A statistical study of the SO_{2} plumes
Using the whole TEXES dataset between 2012 and 2019, we have performed a statistical study of the SO_{2} plumes, with respect to their distribution as a function of latitude, longitude and local time. Then, we have extended this analysis to a study of the distribution of the SO_{2} abundance with local time and longitude.
First, weconsider the probability of SO_{2} appearance as a function of local time (LT). The advantage of this method, already used in E19, is that it is independent of the mean diskintegrated SO_{2} vmr; it thusallows us to disentangle LT variations from longterm temporal variations. Our method is the following. First, for each day of observation, we select one single map, the one showing the SO_{2} plume with the strongest vmr. The choice of a single map per day allows us to remove shortterm local variations, as it has been seen that a SO_{2} plume has typically a life time of a few hours (thus being present over several maps of a given day), but does not last until the following day. On this map, we evaluate the LT range over which the SO_{2} plume is present. We assign a probability of 1 within this range, and 0 outside this range. In parallel, we assign a probability of 1 over the whole observed LT range, i.e. a range of 12 h corresponding to the observed hemisphere of the planet. Then, for each LT, we do the summation of all maps for which this LT is observed (red curve in Figs. 13 and 18), and, separately, the summation of all maps for which a SO_{2} plume is present atthe given LT (blue curve in these two figures). Dividing the blue curve by the red curve gives us the probability for a SO_{2} plume to bepresent at a given LT. The same method is applied below to calculate the probability of SO_{2} appearance as a function of longitude (see below, Figs. 18 and 19).
Table 2 lists the new data from the February 2019 and April 2019 runs, which are a complement to the previous dataset shown in Table 2 of E19. This table gives, in sequence, for each observation, the longitude of the subEarth point (SEP), the longitude range of the observed SO_{2} plume (corresponding to a probability of 1), the longitude of the subsolar point (SSP), the LT of the SEP, the LT range and the latitude range of the SO_{2} plume (where the probability is 1), and finally the SO_{2} vmr within this plume. This last quantity is not used when we calculate the probability of SO_{2} plume appearance, but is used in the next step. We note that two dates are missing, as compared with Table 1: April 18 (because no SO_{2} maximum could be identified, as shown in Fig. 6), and April 20, because of the uncertainties mentioned above (Fig. 8).
Summary of TEXES observations obtained in 2019 and used for the analysis of the SO_{2} plumes.
4.1 Distribution of the SO_{2} plumes as a function of latitude
Figure 12 (an update of Fig. 6 of E19) shows the distribution of the SO_{2} plumes as a function of latitude. As observed previously, the distribution strongly peaks toward the equator, with most of the features appearing within the 30N–30S latitude range. This distribution is also observed in the SPICAV/Venus Express dataset, as shown in Fig. 9 of Marcq et al. (2020). In the case of TEXES, the identification of plumes at high latitude is more uncertain than around the equator, due to the peculiar shape of the thermal profile around the polar collar when the morning terminator is observed; in this case, when the thermal profile becomes close to isothermal, the retrieval of SO_{2} and HDO is no longer possible. For this reason, we limit our statistical analysis of the SO_{2} plumes within 50 degrees of the equator.
Fig. 12
Thick line: distribution of the location of the SO_{2} plumes as a function of latitude. The total number of observations is 48. Observations at high latitudes (above 50N and 50S) are not considered, due to the uncertainty on the thermal profile in the regions of the polar collars. Thin line: distribution obtained without the 2019 data (Fig. 6 of E19). 

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4.2 Distribution of the SO_{2} plumes as a function of local time
In this section, we estimate the probability of SO_{2} plume appearance as a function of local time, using the method described above and the whole dataset of 48 points (2012–2019). Figure 13 shows the summation of all local times observed by TEXES over the 2012–2019 period, as well as the summation of all local times for which a SO_{2} plume is present. It can be seen that the dayside is most observed, with a maximum around noon, while there are few observations around midnight. Figure 14 shows the probability of SO_{2} plume appearance as a function of local time. A depletion appears around 10:00, with a clear enhancement around the terminators,confirming our earlier results. Between 22:00 and 03:00, we consider that the statistics are too low for the result to be significant.
It must be reminded that the analysis described above considers only the location of the SO_{2} plumes as a function of local time, and not their intensity. As mentioned above, its main advantage is that it separates the study of the probability of SO_{2} appearance as a function of LT from the study of the longterm temporal variations: indeed all observations have the same weight, whatever the diskintegrated SO_{2} vmr is. However, this analysis does not allow us to compare our results with those of other instruments using occultation techniques like SPICAV/Venus Express, which do not have the capability of mapping the planet instantaneously.
In a second step, we try to estimate the distribution of the SO_{2} vmr as a function of LT, although we are aware that longterm variations of SO_{2} might have some incidence on our result. In order to incorporate this second parameter in our analysis, instead of using the probability of SO_{2} plume occurence, we now consider the SO_{2} vmr as a function of local time, estimated as follows. We have two observable parameters: (1) within the LT interval of the SO_{2} plume, we measure the SO_{2} vmr (SO_{2max}), equal to its maximum value (as given in Table 1 of E19 and Table 2 of this paper); (2) we measure the integrated value of the SO_{2} vmr over the observable LT interval (SO_{2moy}), as being equal to the diskaverage SO_{2} vmr, inferred from the diskintegrated spectra (Figs. 2, 3 and 11). If s is the LT fraction of the SO_{2} plume appearance (with s between 0 and 1), the mean SO_{2} vmr outside the plume (SO_{2min}) is such that
SO_{2max} × s + SO_{2min} × (1 – s) = SO_{2moy}
or
SO_{2min} = [SO_{2moy} – s × SO_{2max}] / (1 – s)
Figures 15 and 16 show the results, using both the whole dataset (2012–2019) and the 2012–2018 dataset (i.e. with the 34 points used in E19). Since the maximum SO_{2} vmr is usually not more than twice its diskintegrated value, the distribution curve of the SO_{2} vmr as a function of local time is considerably smoother than the probability curve shown in Fig. 14. A depletion is still observed on the morning side (10:00) and the two local maxima near the terminators are still present. In addition, an increase of the SO_{2} abundance is observed from the morning to the evening. In order to check the validity of this result, we also made this calculation using the median of the SO_{2} volume mixing ratio instead of its average. Using the median is a way to give less weight to possible outliers associated with isolated plumes. Calculations show that the shape of both curves is identical. These results are discussed in Sect. 5.
In order to better analyze the possible relation between the SO_{2} vmr and the local time, we used a second approach based on the longterm variations of SO_{2} at the cloud top. Figure 17 shows a plot of the diskaveraged SO_{2} vmr (same data as in Fig. 11), as a function of the diameter of the Venus disk. A diameter of 10 arcsec corresponds to the dayside fully illuminated, whereas a diameter of 60 arcsec (never observed because of the solar elongation constraint of the telescope) would correspond to the full night side. It can be seen that there is no apparent correlation nor anticorrelation between the Venus diameter and the diskintegrated SO_{2} vmr; the correlation coefficient between these two quantities (calculated over the 13 runs) is 0.0. The conclusion is that there is no evidence for a difference between the dayside and nightside distributions of SO_{2}.
We also wondered whether the diskintegrated SO_{2} vmr might be correlated with the type of the observed terminator (morning or evening, see Fig. 17). Again, the absence of correlation is apparent. To calculate the correlation coefficient, we assigned a coefficient equal to 0 for the morning terminator and 1 for the evening terminator. In this case, the correlation coefficient is very weakly positive (0.24). Although it may be too weak to be significant, we note that this result is consistent with the slight increase observed for the SO_{2} vmr around the evening terminator, as shown in Fig. 16.
Fig. 13
Red curve: summation of all local times observed by TEXES over the 2012–2019 period, using the 46 observations listed in Table 1 of E19 and Table 2 of this paper. Blue curve: summation of all local times for which a SO_{2} plume was present, using the same dataset. As in E19, the probability of SO_{2} plume appearance is equal to 1 within the local time range of the maximum SO_{2} and 0 elsewhere. Thick lines: Results with the whole dataset (2012–2019); thin lines: dataset without the 2019 data, as shown in Fig. 10 of E19. 

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Fig. 14
Probability of SO_{2} appearance as a function of local time, calculated as the ratio of the blue curve to the red curve in Fig. 13. The error bar is proportional to n^{−0.5}, where n is the number of observations for which the local time is observed (red curve in Fig. 13). Thick points: Results with the whole dataset (2012–2019); thin points: dataset without the 2019 data, as shown in Fig. 10 of E19. 

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Fig. 15
Thick red curve: summation of all LT observed by TEXES over the 2012–2019 period. This curve is the same as the red curve in Fig. 13. Thick blue curve: summation of all SO_{2} vmr distributions vs LT, using the same dataset. For each observation, the distribution of the SO_{2} vmr as a function of local time is calculated as described in the text. The sum of all SO_{2} vmrs has been divided by 400.0 ppbv; this number corresponds to a typical value of the SO_{2} vmr within the plumes over the whole period (see last column of Table 2); this normalization allows us to show both curves on the same scale. Thin lines: results using the dataset without the 2019 runs (34 points). 

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Fig. 16
Thick points: distributions of the SO_{2} vmr as a function of local time, calculated as the ratio of the blue curve to the red curve in Fig. 15. The error bar is proportional to n^{−0.5}, where n is the number of observations for which the local time is observed (red curve in Fig. 15). Thin points: results using the dataset without the 2019 runs (34 points). 

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Fig. 17
Diskintegrated SO_{2} vmr (xaxis, same data as in Fig. 11) plotted as a function of the diameter of the Venus disk (yaxis). Blue circles:morning terminator; red crosses: evening terminator. 

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4.3 Distribution of the SO_{2} plumes as a function of longitude
We have completed our analysis of the SO_{2} distribution as a function of longitude, using the same method as described in E19 and using the 48 data points available (Table 1 of E19 and Table 2 of this paper). Results are shown in Figs. 18 and 19. We have added all observable longitude ranges to obtain the longitude visibility curve corresponding to our dataset. In the same way, we have added all longitude ranges where a SO_{2} plume was present (Fig. 18). Dividing this curve by the longitude visibility curve gives us the probability of SO_{2} appearance as a function of the longitude (Fig. 19). As in our previous study, there is no clear trend in the longitudinal distribution of the probability of SO_{2} plume appearance, except a possible depletion around 300 E.
As a next step, we have determined the SO_{2} vmr distribution as a function of longitude, using the same method as described in the previous section. Results are shown in Figs. 20 and 21. It can be seen that the SO_{2} vmr distribution shows a regular curve with a maximum around 120–200 E and a minimum around 300–350 E. It can be noticed that the region of SO_{2} maximum isnear the region of Aphrodite Terra where the highest equatorial volcanoes are located. The significance of this result is discussed below (Sect. 5).
Fig. 18
Red curve: summation of all longitudes observed by TEXES over the 2012–2019 period, using the 48 observations listed in Table 2. Blue curve: summation of all longitudes where a SO_{2} plume was present, using the same dataset. 

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Fig. 19
Probability of SO_{2} appearance as a function of longitude, using the data shown in Table 1 of E19 and Table 2 of this paper. The error bar is proportional to n^{−0.5}, where n is the number of observations for which the longitude is observed (red curve in Fig. 18). Thick points: Results with the whole dataset (2012–2019); thin points: dataset without the 2019 data. 

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Fig. 20
Red curve: summation of all longitudes observed by TEXES over the 2012–2019 period. This curve is the same as the red curve in Fig. 18. Blue curve: summation of all SO_{2} vmr distributions vs longitude, using the same dataset. For each observation, the normalized distribution of the SO_{2} vmr as a function of longitude is calculated as described in the text. The sum of all SO_{2} vmrs has been divided by 400.0 ppbv. Thick points: results with the whole dataset (2012–2019); thin points: dataset without the 2019 data. 

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Fig. 21
Distribution of the SO_{2} vmr as a function of longitude calculated as the ratio of the blue curve to the red curve in Fig. 20. The error bar is proportional to n^{−0.5}, where n is the number of observations for which the longitude is observed (red curve in Fig. 20). Thick points: Results with the whole dataset (2012–2019); thin points: dataset without the 2019 data. 

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5 Discussion
5.1 Comparative evolution of SO_{2} and H_{2}O
When the TEXES campaign started in 2012, the diskintegrated SO_{2} vmr at the cloud top was 200–300 ppbv, i.e. about a fifth of the H_{2}O vmr (Fig. 11). In 2014 and 2015, the diskintegrated SO_{2} abundance decreased down to 100 ppbv or less, while the water abundance remained more or less constant. Since 2015 until now, we observe a regular decrease of H_{2}O and a longterm increase of the SO_{2} abundance, up to a diskintegrated vmr above 300 ppbv, with local plumes as high as 800 ppbv (Table 2 and Figs. 5–8). In parallel, the shortterm variations of SO_{2} observed in 2018 and 2019 tend to be stronger than in the previous years. This suggest that the longterm evolution of the SO_{2} abundance at the cloud top is associated with the shortterm activity of the SO_{2} plumes, as also observed by SPICAV aboard Venus Express (Marcq et al. 2020). It is interesting to note that the H_{2}O vmr at the cloud top remained more or less constant between 2012 and 2015, and then started to decrease. This is consistent with the observations of Venus Express in the nearinfrared range (Cottini et al. 2015, Fedorova et al. 2016) which foundno evidence for temporal variations at the cloud top during the lifetime of the Venus Express mission (2006–2015).
Using the 2018 and 2019 data, for which SO_{2} and H_{2}O exhibit comparable abundances, we can wonder why SO_{2} exhibits strong shortterm variations, both locally and as a function of time, whereas these variations are not observed in the HDO maps. Indeed, Figs. 9 and 10 confirm our previous statement about the local homogeneity of the HDO maps: the diskintegrated vmr of water vapor decreases with time, but remains remarkably constant over the Venus disk. If the SO_{2} plumes are associated with convective motions, we need to understand why the same behavior is not observed in the HDO maps. Possibly, the explanation is linked to the much larger vertical gradient of SO_{2} than that of H_{2}O within the clouds, since SO_{2} varies by a factor of 1000 and H_{2}O by only a factor of 30 between the bottom and the top of the Venus clouds (Bézard & De Bergh 2012). This difference implies that the signature of vertical transport should be more visible in the SO_{2} field than for H_{2}O. SO_{2} is also a sink for H_{2}O through the formation of H_{2} SO_{4}, so an increase in H_{2}O is not expected when a plume of SO_{2} is observed.
For the first time, our data show evidence for a longterm anticorrelation between the SO_{2} and H_{2}O abundances at the cloud top. The anticorrelation is maximum if we consider only the 2014–2019 time interval, which suggests that some longterm process is at work within the Venus atmosphere below and/or above the clouds. It is interesting to note that this anticorrelation does not appear on shortterm scales of hours or days. This is illustrated by a comparison between Figs. 5 and 9 which show daily variations of the SO_{2} and H_{2}O abundances during the February 2019 run: the H_{2}O abundance decreases regularly from Feb. 12 to 18, 2019 whereas the SO_{2} maps show two local maxima on Feb. 14 and 18. In addition, for these two dates, the H_{2}O maps remain uniform over the Venus disk, while SO_{2} maps show a high contrast driven by the emergence of SO_{2} plumes. In summary, the longterm anticorrelation observed between the SO_{2} and H_{2}O abundances seems to be disconnected from the shortterm activity of the SO_{2} plumes.
Photochemical models have been developed to model the behavior of water vapor and sulfur dioxide at the cloud top and within the clouds of Venus (Parkinson et al. 2015). Using a 1D chemistrydiffusion model (Zhang et al. 2012), Shao et al. (2020) have found that the anticorrelation of SO_{2} and H_{2}O at 64 km can be generally explained by the sulfur chemistry in the middle atmosphere (58–100 km) of Venus. Even when SO_{2} and H_{2}O vary randomly atthe middle cloud top (58 km), their model finds that the two species at 64 km are mostly anticorrelated, because SO_{2} and H_{2}O modulate each other through the sulfuric acid formation and intermediate SO_{3} reactions at 64 km. In contrast, a change of the eddy diffusivity in the middle atmosphere cannot explain the SO_{2} –H_{2}O anticorrelation. While the anticorrelation itself can be explained by the sulfur chemistry, the cause for the variations of species abundances at the middle cloud top is not understood. These variations may relate to atmospheric processes inside or below the clouds, as tracer transport (Marcq et al. 2013, Bierson & Zhang 2020) or geological processes on the surface, as volcanic eruption (Esposito 1984). The TEXESobserved longterm variations of SO_{2} and H_{2}O may thus contain additional information for mechanisms of how the two species covary deeper in the Venus atmosphere. Additional observations and modeling work will allow the processes inside and below the clouds to be unraveled.
5.2 Variations of SO_{2} as a function of local time
Using the 2019 data described in this paper, we have completed our analysis of the probability of SO_{2} plume occurence as a function of local time. Results shown in Fig. 14 confirm our previous conclusion (E19) about the two maxima around the terminators. We have performed an analysis of the SO_{2} abundance as a function of local time. Not surprisingly, the variations are significantly smoothed, simply because the maximum SO_{2} vmr within a plume is never more than twice its diskintegrated value. In contrast, the change in the shape of the curve (Fig. 16) is more surprising. The SO_{2} vmr at the evening terminator is higher than at the morning terminator by a factor of about 30 percent.
It can be seen from Fig. 16 that the agreement with the results of SPICAV (Fig. 10 of Marcq et al. 2020) is not as good as observed previously. Indeed, in E19, we pointed out the good agreement between these data and the TEXES results (Fig. 19 of E19). However, the TEXES curve was the probability of SO_{2} plume occurence, while the SPICAV data referred to the SO_{2} vmr as a function of local time. Thus, we would have expected a better agreement between the SPICAV curve and our new calculation of the SO_{2} vmr as a function of local time (Fig. 16 of this paper). This is actually not the case: the SPICAV data show a contrast by a factor 10 between the SO_{2} vmr around noon and its value at the terminators, while this contrast is less than a factor 2 in the TEXES data (Fig. 16). However, taking into account the error bars of both data sets, the two results are still consistent. The origin of thedifference might be the altitude shift in the levels probed by the two experiments, as the UV data of SPICAV probe a few kilometers above the cloud top, and also the different epochs explored by the SPICAV and TEXES data sets. Also, it can be noticed that, since the SPICAV observations refer to a single point on the Venus disk (while the TEXES data show a global map), it is more difficult, in the case of SPICAV, to disentangle the temporal variations from the local ones. Further comparison with the UV data of Akatsuki will be useful to investigate this issue.
As shown in Figs. 13 and 15, the TEXES dataset still lacks a good coverage of the nightside. We have analyzed the variations of the diskintegrated SO_{2} as a function of the diameter of Venus, in order to search for a possible correlation between the SO_{2} abundance and the illuminated fraction of the disk (Fig. 17). With a correlation factor of 0.0, this comparison shows that there is no evidence for a change of the SO_{2} abundance with respect to day or night.
5.3 Variations of SO_{2} as a function of longitude
Figure 19 shows the probability of SO_{2} plume appearance as a function of longitude. It is very similar to our previous analysis (Fig. 9 of E19A) and shows no clear dependence with longitude, except a possible minimum around 300° east longitude. In contrast, the variations of the SO_{2} vmr as a function of longitude (Fig. 21) shows a smooth curve with a distinct maximum around 120–200° east longitude, i.e. near the region of Aphrodite Terra. This figure is to be compared with the SPICAV results (Fig. 11 of Marcq et al. 2020). In this case, there is no agreement between the two datasets as, in the case of SPICAV, the SO_{2} vmr is maximum around 30–60° east longitude. In both cases, it is difficult to disentangle the spatial and temporal variations of SO_{2}. In addition, in the case of the TEXES data, we note that the SO_{2} vmr distribution (Fig. 21) and the probability of SO_{2} occurrence (Fig. 19), as a function of longitude, show very different shapes, which is not the case for the SO_{2} variations as a function of local time. In summary, our result regarding the SO_{2} distribution as a function of longitude should be considered with caution and has yet to be confirmed.
5.4 Comparison of the SO_{2} statistical analysis with our previous results
In this section, we analyze how our statistical analysis of the SO_{2} plumes is affected by the inclusion of the 2019 dataset, which adds 14 new points to our previous list of 34 observations. In the case of the analysis of the SO_{2} plumes as afunction of local time (LT), the addition of the 2019 dataset significantly improves the statistics in the morning side of the planet (LT = 03:00–12:00; Fig. 13). The probability of SO_{2} plume appearance as a function of LT is only slightly modified and the error bars are lowered (Fig. 14). Because of the limited number of observations between 23:00 and 03:00, we do not consider the probability of SO_{2} plume appearance to be significant in this time interval. In contrast with Fig. 14, the variations of the SO_{2} volume mixing ratio as a function of LT show a significant difference when the 2019 dataset is added (Fig. 16). The effect is probably due to the increase of the diskintegrated SO_{2} vmr between 2015 and 2019 (Fig. 11). This illustrates the difficulty of disentangling the longterm global variations of SO_{2} from its distribution as a function of local time. It confirms that, for this analysis, the probability of SO_{2} plume appearance is a more reliable indicator.
In the case of the statistical study of the SO_{2} plumes as a function of longitude, the addition of the 2019 dataset is uniformly distributed over all longitudes (Fig. 18). The probability of SO_{2} plume appearance (Fig. 19) has the same shape as in E19, with the error bars being reduced. The distribution of the SO_{2} vmr shows a maximum around 120–200° east longitude but, as pointed out above, this result remains to be confirmed. Figure 21 shows that this maximum is significantly reduced when the 2019 dataset is added, and, as mentioned above, the distribution of the SO_{2} vmr as afunction of longitude cannot be easily separated from longterm temporal variations.
5.5 Longterm variations of SO_{2} between 1979 and 2019
Thanks to the monitoring of the SO_{2} vmr achieved in the UV by Pioneer Venus (Esposito et al. 1997) and Venus Express (Marcq et al. 2013), and in the IR by Venera15 (Zasova et al. 1993) and later TEXES, we now have information on the longterm variations of the SO_{2} abundance at the cloud top of Venus over a 40year period. Figure 22 shows the SO_{2} longterm variations measured by the spacecraft between 1979 and 2014 (Marcq et al. 2013, 2020), completed with the diskaveraged SO_{2} abundance measured by TEXES between 2012 and 2020. As in E19 and in Marcq et al. (2020), we rescale the TEXES measurements by dividing the TEXES data by a factor 3, to account for the altitude difference between the UV observations (about 70 km) and the IR observations (about 64 km). It can be seen that, after the two maxima observed by Pioneer Venus in 1980 and by Venus Express in 2008, followed by a continuous decrease during 5–7 yr, the mean SO_{2} abundance at the cloud top has been continuously increasing since 2015, but is still about half the maximum value reached in 1980 and 2008. In addition to this longterm trend, as mentioned above, we note that, as observed by both SPICAV and TEXES, the shortterm variations observed in the SO_{2} plumes tend to increase as the diskintegrated abundance of SO_{2} increases. Future monitoring with Akatsuki and TEXES will hopefully allow us to continue this analysis in the future.
Fig. 22
Longterm variations of the SO_{2} volume mixing ratio at the cloud top of Venus between 1989 and 2020, as reported by Esposito et al. 1997, Marcq et al. (2013, 2020) and this paper (Fig. 11). The figure is adapted from Marcq et al. (2013). 

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6 Conclusions
In this paper, we have pursued our SO_{2} and HDO monitoring at the cloud top of Venus using the TEXES instrument at 7.4 μm by adding new data obtained in February and April 2019, and we have reanalyzed the whole TEXES dataset between 2012 and 2019 to study (1) the longterm behavior of H_{2}O and SO_{2}, and (2) the behaviorof SO_{2} as a function of latitude, local time and longitudinal. The main results of this study can be summarized as follows.
An anticorrelation is visible in the longterm variations of H_{2}O and SO_{2} at the cloud top, with a correlation coefficient of −0.80 (−0.90 between 2014 and 2019). On short timescales, this anticorrelation is hidden behind the shortterm variations due to the SO_{2} plumes which appear and disappear within a few hours.
Since 2015, we observe a longterm decrease of H_{2}O, associated with a longterm increase of SO_{2}. At the same time, the shortterm variations of SO_{2} due to the SO_{2} plumes become larger and larger, as shown in Fig. 11. For the first time, we observe in July 2018, a SO_{2} plume showing a local vmr of 800 ppbv, corresponding to a diskintegrated SO_{2} vmr of 600 ppbv, equal to the H_{2}O vmr derivedat the same time. However, we do not see evidence for an anticorrelation between SO_{2} and H_{2}O on shortterm (hours or days) time scales.
The new analysis of the probability of SO_{2} plume occurence as a function of local time confirms our previous results (E19) with two maxima around the terminators. The distribution of the SO_{2} vmr as a function of local time shows the same trend, with a local minimum occurring in the morning (10:00 local time). However, the maximum around the evening terminator is more pronounced than the one around the morning terminator.
As in our previous analysis, the probability of SO_{2} plume occurence as a function of longitude shows no clear feature, except a possible minimum around 300 E. In contrast, the distribution of the SO_{2} vmr as a function of longitude shows a clear maximum between 120 E and 200 E, in the volcanic region of Aphrodite Terra. However, this result is not confirmed by the SPICAV analysis (Marcq et al. 2020), and should be considered with caution. More generally, we need to insist on the complexity of the SO_{2} behavior, which exhibits both shortterm and longterm variations, and we emphasize the difficulty of disentangling the local time variations of SO_{2} from its longitude variations.
In the future, we plan to develop the comparison with past SPICAV and ongoing Akatsuki UV data to test the validity of our conclusions regarding the variations of the SO_{2} abundance, and in particular its dependence as a function of longitude. A comparative analysis of the two TEXES datasets, at 7.4 μm and 19 μm, as initiated in E13 and E16, should also allow us to better constrain the SO_{2} behavior within the H_{2} SO_{4} cloud.
Acknowledgements
T.E. and T.K.G. were visiting astronomers at the NASA Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. We wish to thank the IRTF staff for the support of TEXES observations. This work was supported by the Programme National de Planétologie (PNP) of CNRS/INSU, cofunded by CNES. T.K.G. acknowledges support of NASA Grant NNX14AG34G. T.E. and B.B. acknowledge support from CNRS. T.F. acknowledges support from UPMC. T.W. acknowledges support from the University of VersaillesSaintQuentin and the European Commission Framework Program FP7 under Grant Agreement 606798 (Project EuroVenus). WS acknowledges support from China Scholarship Council Fellowship. X.Z. and C.J.B. acknowledgesupport from NSF grant AST1740921. C.J.B. also acknowledges support from the NSF Graduate Research Fellowship under Grant No. NSF DGE 1339067. YJL has received funding from EU Horizon 2020 MSCAIF No. 841432.
References
 Belyaev, D. A., Montmessin, F., Bertaux, J.L., et al. 2012, Icarus, 217, 740 [NASA ADS] [CrossRef] [Google Scholar]
 Bertaux, J.L., Vandaele, A.C., Korablev, O., et al. 2007, Icarus, 217, 740 [Google Scholar]
 Bézard, B. & De Bergh, C., 2012, J. Geophys. Res., 112, E04S07 [Google Scholar]
 Bierson, C. J., & Zhang, X., 2020, J. Geophys. Res. Planets, submitted [Google Scholar]
 Bjoraker, G. L., Larson, H. P., Mumma, M. J., et al. 1992, BAAS, 24, 995 [Google Scholar]
 Cottini, V., Ignatiev, N. I., Piccioni, G., et al. 2015, Planet. Space Sci., 113, 219 [CrossRef] [Google Scholar]
 Encrenaz, T., Bézard, B., Greathouse, T. K., et al. 2004, Icarus, 170, 424 [NASA ADS] [CrossRef] [Google Scholar]
 Encrenaz, T., Greathouse, T. K., Roe, H., et al. 2012, A&A, 543, A153 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Encrenaz, T., Greathouse, T. K., Richter, M. J., et al. 2013, A&A, 559, A65 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Encrenaz, T., Greathouse, T. K., Lefèvre, F., et al. 2015, A&A, 578, A127 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Encrenaz, Greathouse, T. K., Richter, M. J., et al. 2016, A&A, 595, A74 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Encrenaz, Greathouse, T. K., Marcq, E., et al. 2019, A&A, 595, A70 [CrossRef] [EDP Sciences] [Google Scholar]
 Esposito, L. W. 1984, Science, 223, 1072 [NASA ADS] [CrossRef] [Google Scholar]
 Esposito, L. W., Bertaux, J.L., Krasnoposly, V., et al. 1997, in Venus II: Geology, Geophysics, Atmosphere, and Solar Wind Environment, Chemistry of lower atmosphere and clouds, eds. Bougher, S. W., Hunten, D. M., & Phillips, R. J. (Tucson, AZ : University of Arizona Press), 415 [Google Scholar]
 Fedorova, A., Korablev, O., Vandaele, A.C., et al. 2008, J. Geophys. Res., 113, E00B25 [CrossRef] [Google Scholar]
 Fedorova, A., Marcq, E., Luginin, M., et al. 2016, Icarus, 275, 143 [NASA ADS] [CrossRef] [Google Scholar]
 Krasnopolsky, V. A. 1986, Photochemistry of the atmospheres of Mars and Venus (New York: SpringerVerlag) [CrossRef] [Google Scholar]
 Krasnopolsky, V. A. 2007 Icarus, 191, 25 [NASA ADS] [CrossRef] [Google Scholar]
 Krasnopolsky, V. A. 2010, Icarus, 209, 314 [NASA ADS] [CrossRef] [Google Scholar]
 Krasnopolsky, V. A., Belyaev, D. A., Gordon, I. A., et al. 2013, Icarus, 224, 57 [CrossRef] [Google Scholar]
 Lacy, J. H., Richter, M. J., Greathouse, T. K., et al. 2002, PSAP, 114, 153 [NASA ADS] [CrossRef] [Google Scholar]
 Marcq, E., Bertaux, J.L., Montmessin, F., et al. 2013, Nat. Geosci. 6, 25 [NASA ADS] [CrossRef] [Google Scholar]
 Marcq, E., Mills, F. P., Parkinson, C. P., & Vandaele, A. C., 2018, Space Sci. Rev. 214, 10 [NASA ADS] [CrossRef] [Google Scholar]
 Marcq, E., Jessup, K. L., Baggio, L., et al. 2020, Icarus, 335, 11368 [CrossRef] [Google Scholar]
 Mills, F. P., Esposito, L. W., & Yung, Y. K. 2007, Geophys. Mongraph Ser., 176, 73 [Google Scholar]
 Parkinson, C., Gao, P., Esposito, L., et al. 2015, Planet. Space Sci., 112, 226 [NASA ADS] [CrossRef] [Google Scholar]
 Shao, W. D., Zhang, X., Bierson, C. J., et al. 2020, J. Geophys. Res. Planets, submitted [arXiv:2006.09522] [Google Scholar]
 Rohlfs, K., & Wilson, T. L. 2004 Tools for radioastronomy, 4th edn. (Berlin: Springer) [Google Scholar]
 Vandaele, A.C., Korablev, O., Belyaev, D., et al. 2017a, Icarus, 295, 16 [NASA ADS] [CrossRef] [Google Scholar]
 Vandaele, A.C., Korablev, O., Belyaev, D., et al. 2017b, Icarus, 295, 1 [CrossRef] [Google Scholar]
 Zhang, K., Liang, M. C., & Mills, F. P. 2012, Icarus, 217, 714 [NASA ADS] [CrossRef] [Google Scholar]
 Zasova, L. V., Moroz, V. I., Esposito, L. W., & Na, C. Y. 1993, Icarus, 105, 92 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
Summary of TEXES observations obtained in 2019 and used for the analysis of the SO_{2} plumes.
All Figures
Fig. 1
Geometrical configurations of the disk of Venus during the two TEXES runs of February and April 2019. The terminator is indicated with a black line and the subsolar point with a black dot. Both configurations show the morning terminator. 

Open with DEXTER  
In the text 
Fig. 2
Examples of diskintegrated spectra of Venus between 1344.8 and 1345.4 cm^{−1} (7.4 μm) recorded in February 2019. It can be seen that the broad terrestrial atmospheric absorption feature around 1344.95 cm^{−1} varies strongly from day to day. 

Open with DEXTER  
In the text 
Fig. 3
Examples of diskintegrated spectra of Venus between 1344.8 and 1345.4 cm^{−1} (7.4 μm) recorded in April 2019. Due to the strong terrestrial absorption around 1344.95 cm^{−1}, the depth of the HDO line at 1344.90 cm^{−1} could not be measured on April 21–24, 2019. 

Open with DEXTER  
In the text 
Fig. 4
Examples of maps of the line depth of the weak CO_{2} transition at 1345.22 cm^{−1} (7.4 μm), corresponding to the observations shown in Figs. 2 and 3. The scale is the same for the two maps. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

Open with DEXTER  
In the text 
Fig. 5
Examples of maps of the line depth ratio of a weak SO_{2} multiplet (around 1345.1 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded in February 2019 (one map per observing day). Diskintegrated spectra corresponding to these maps are shown in Fig. 2. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

Open with DEXTER  
In the text 
Fig. 6
Examples of maps of the line depth ratio of a weak SO_{2} multiplet (around 1345.1 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded in April 2019 (one map per observing day). Diskintegrated spectra corresponding to these maps are shown in Fig. 3. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

Open with DEXTER  
In the text 
Fig. 7
Maps of the line depth ratio of a weak SO_{2} multiplet (around 1345.1 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded onApril 16, 2019. The figure on the left (18:23 UT) is the same as in Fig. 6. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

Open with DEXTER  
In the text 
Fig. 8
Maps of the line depth ratio of a weak SO_{2} multiplet (around 1345.1 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded on April 20, 2019. The figure on the left (27:27 UT) is the same as in Fig. 6, with a different scale. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

Open with DEXTER  
In the text 
Fig. 9
Maps of the line depth ratio of the weak HDO transition (at 1344.90 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded during the February 2019 run. Data are the same as in Figs. 2 and 5. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. 

Open with DEXTER  
In the text 
Fig. 10
Examples of maps of the line depth ratio of the weak HDO transition (at 1344.90 cm^{−1}) to the CO_{2} transition at 1345.22 cm^{−1}, recorded during the April 2019 run. Data are the same as in Figs. 3 and 6. The subsolar point is shown as a white dot. Times refer to the midtimes of the observations. Data of April 21–24 are not shown because theterrestrial atmospheric absorption (see Fig. 3) is too strong for the HDO retrieval to be reliable. 

Open with DEXTER  
In the text 
Fig. 11
Longterm variations of the H_{2}O volume mixing ratio (top, blue points), inferred from the HDO measurements, and the SO_{2} volume mixing ratio (bottom, red points), measured at the cloud top from the TEXES data at 7.4 μm. A daily mean is shown in this figure. The black squares are the mean values of the H_{2}O and SO_{2} mixing ratios averaged over each run. In 3 cases (Dec. 2017–Jan. 2018, JulySept. 2018, Feb.–Apr. 2019), we have coadded alldata (separated by less than 3 months), in order to have a more homogeneous time sampling over the long term. 

Open with DEXTER  
In the text 
Fig. 12
Thick line: distribution of the location of the SO_{2} plumes as a function of latitude. The total number of observations is 48. Observations at high latitudes (above 50N and 50S) are not considered, due to the uncertainty on the thermal profile in the regions of the polar collars. Thin line: distribution obtained without the 2019 data (Fig. 6 of E19). 

Open with DEXTER  
In the text 
Fig. 13
Red curve: summation of all local times observed by TEXES over the 2012–2019 period, using the 46 observations listed in Table 1 of E19 and Table 2 of this paper. Blue curve: summation of all local times for which a SO_{2} plume was present, using the same dataset. As in E19, the probability of SO_{2} plume appearance is equal to 1 within the local time range of the maximum SO_{2} and 0 elsewhere. Thick lines: Results with the whole dataset (2012–2019); thin lines: dataset without the 2019 data, as shown in Fig. 10 of E19. 

Open with DEXTER  
In the text 
Fig. 14
Probability of SO_{2} appearance as a function of local time, calculated as the ratio of the blue curve to the red curve in Fig. 13. The error bar is proportional to n^{−0.5}, where n is the number of observations for which the local time is observed (red curve in Fig. 13). Thick points: Results with the whole dataset (2012–2019); thin points: dataset without the 2019 data, as shown in Fig. 10 of E19. 

Open with DEXTER  
In the text 
Fig. 15
Thick red curve: summation of all LT observed by TEXES over the 2012–2019 period. This curve is the same as the red curve in Fig. 13. Thick blue curve: summation of all SO_{2} vmr distributions vs LT, using the same dataset. For each observation, the distribution of the SO_{2} vmr as a function of local time is calculated as described in the text. The sum of all SO_{2} vmrs has been divided by 400.0 ppbv; this number corresponds to a typical value of the SO_{2} vmr within the plumes over the whole period (see last column of Table 2); this normalization allows us to show both curves on the same scale. Thin lines: results using the dataset without the 2019 runs (34 points). 

Open with DEXTER  
In the text 
Fig. 16
Thick points: distributions of the SO_{2} vmr as a function of local time, calculated as the ratio of the blue curve to the red curve in Fig. 15. The error bar is proportional to n^{−0.5}, where n is the number of observations for which the local time is observed (red curve in Fig. 15). Thin points: results using the dataset without the 2019 runs (34 points). 

Open with DEXTER  
In the text 
Fig. 17
Diskintegrated SO_{2} vmr (xaxis, same data as in Fig. 11) plotted as a function of the diameter of the Venus disk (yaxis). Blue circles:morning terminator; red crosses: evening terminator. 

Open with DEXTER  
In the text 
Fig. 18
Red curve: summation of all longitudes observed by TEXES over the 2012–2019 period, using the 48 observations listed in Table 2. Blue curve: summation of all longitudes where a SO_{2} plume was present, using the same dataset. 

Open with DEXTER  
In the text 
Fig. 19
Probability of SO_{2} appearance as a function of longitude, using the data shown in Table 1 of E19 and Table 2 of this paper. The error bar is proportional to n^{−0.5}, where n is the number of observations for which the longitude is observed (red curve in Fig. 18). Thick points: Results with the whole dataset (2012–2019); thin points: dataset without the 2019 data. 

Open with DEXTER  
In the text 
Fig. 20
Red curve: summation of all longitudes observed by TEXES over the 2012–2019 period. This curve is the same as the red curve in Fig. 18. Blue curve: summation of all SO_{2} vmr distributions vs longitude, using the same dataset. For each observation, the normalized distribution of the SO_{2} vmr as a function of longitude is calculated as described in the text. The sum of all SO_{2} vmrs has been divided by 400.0 ppbv. Thick points: results with the whole dataset (2012–2019); thin points: dataset without the 2019 data. 

Open with DEXTER  
In the text 
Fig. 21
Distribution of the SO_{2} vmr as a function of longitude calculated as the ratio of the blue curve to the red curve in Fig. 20. The error bar is proportional to n^{−0.5}, where n is the number of observations for which the longitude is observed (red curve in Fig. 20). Thick points: Results with the whole dataset (2012–2019); thin points: dataset without the 2019 data. 

Open with DEXTER  
In the text 
Fig. 22
Longterm variations of the SO_{2} volume mixing ratio at the cloud top of Venus between 1989 and 2020, as reported by Esposito et al. 1997, Marcq et al. (2013, 2020) and this paper (Fig. 11). The figure is adapted from Marcq et al. (2013). 

Open with DEXTER  
In the text 
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