dataesr/scientific-paragraphs-categorization huggingface dataset:
The updates are detailed in an accompanying paper  [641]  in this HITRAN2016 special issue. Note that an error was found in Tables  1  and 2  of Ref. [641]  where the values corresponding to partition sums of the 16 O 17 O isotopologue were a factor of six too large. This has been fixed in the official release of HI-TRAN2016. The TIPS are made available to the scientific community in the form of tables and codes that rapidly recall the TIPS for any molecule, isotopologue, and temperature. There are several codes that are distributed with this edition of HITRAN: FOR-TRAN codes TIPS_2017. for and BD_TIPS_2017. for and a python code TIPS_2017. py with associated dictionaries. TIPS_2017. for is a standalone code that queries the user for a molecule, isotopologue, and temperature and returns Q(T).
BD_TIPS_2017. for is a subroutine application that users can insert into their codes to return Q(T) for a molecule/isotopologue/temperature selection. The python code uses python dictionaries to recall Q(T). The dictionaries are labeled by the molecule number and local ID number, see the TIPS article  [641]  for details. Details are given to develop custom python algorithms for particular molecule/isotopologue combinations. The TIPS python package was incorporated into the HITRAN Application Programming Interface (HAPI)  [5]  in order to seamlessly integrate into the cross-section generating process. The tables and codes are available at faculty. uml. edu/Robert_Gamache and www. hitran. org.
Conclusions The improvements, expansions and new structure in the new HITRAN database release have been elaborated upon. For the lineby-line data, improved line position, intensity, and line-shape parameters for many of the previously existing molecules and isotopologues have been introduced. Many new lines/bands have been added for different molecules and their isotopologues allowing for a more complete database (for atmospheric applications) and for the expansion of the spectral coverage of the existing line lists. Additionally, HITRAN continues evolving in terms of structure and scope. A new relational database structure has been established  [2]  that enabled significant expansion of the amount of important spectroscopic parameters provided in the database. Literally dozens of new parameters have been introduced that allow accommodation of non-Voigt line shapes  [6]  ; flexible representation of broadening parameters and their temperature dependencies; broadening and shift of spectral lines due to pressure of gases dominant in planetary atmospheres  [4]  (namely, H 2 , He and CO 2 ).
This extensive expansion of the database would have been very impractical in the old fixed-length ASCII format of previous HITRAN editions. An interface on the internet has also been established ( www. hitran. org ) that provides the diverse group of HITRAN users with much power to filter, extract, plot, and query the database. Even more power has been given to the user through the introduction of the HITRAN Application Programming Interface (HAPI)  [5]. HAPI is currently a set of Python libraries which not only allows users to download data from the database but also to carry out: 1) single-layer absorption calculations at different thermodynamic conditions, accounting for an instrument function, new line shape parametrizations, perturbing gas or gases, etc, 2) extended functionality provided by custom functions, line lists and partition sums.
Several new molecules and isotopologues have been added to the line-by-line portion of the compilation, which improve modeling of the absorption of the terrestrial atmosphere and beyond. One of the main highlights of the new edition is the monumental expansion of the cross-sectional part of the database which increased (in terms of amount of gases) about six-fold and now fea-Please cite this article as: I. E. Gordon   tures over 300 species. These cross-sections can also be accessible through www. hitran. org where they are divided into categories for easy browsing. Aerosols and collision induced absorption datasets have also been revised and extended. The compilation is free and can be accessed through www. hitran. org. We recommend citing this article when using the HI-TRAN2016 data. If an update to a certain molecule is announced on the website and is being used, then we encourage users to cite when they downloaded the data.
Future work While HITRAN continues to be an international standard for reference spectroscopy for atmospheric and planetary gases, there is still substantial room for improvement. In many subsections throughout the paper we mention the avenues for improvements for individual molecules, but they are really just the tip of the iceberg. The studies of the terrestrial atmosphere require further improvements to the existing parameters and what is more challenging: population of the dataset of the non-Voigt line-shape parameters. As was discussed above, the amount of measurements and calculations of the parameters obtained using the recommended HT profile are scarce and it will take time before a majority of HI-TRAN lines will have these parameters provided. Also, we remind experimentalists and theoreticians to take extreme care when fitting to these parameters to avoid correlations.
With an exception of a few diatomic molecules (namely NO, OH, HF, HCl, HBr, HI and H 2 ) HITRAN data are limited to temperatures encountered in the Earth atmosphere and will be deficient when modeling high-temperature environments including stellar and some planetary atmospheres. The users are encouraged to employ the HITEMP database for these applications  [278]. However, there are currently only five gases that are provided in HITEMP (H 2 O, CO 2 , CO, NO, OH) and a major update of the HITEMP database will be released in the near future. This update will include improvement of the spectroscopy of the existing HITEMP gases but also will introduce additional molecules. While a major update is featured here for the cross-sectional part of the database, we note that it is still far from complete in terms of gases.
Moreover, all of the current updates are in the IR part of the spectrum and another substantial update is needed for the UV cross-sections. A massive revision and expansion of the CIA data is planned for the near future. Structure and the tools provided with the database are also a very important part of the HITRAN database. We plan further improvements to the documentation for the HITRAN online interface and the development of video tutorials. Finally, development of an interactive interface is planned for HAPI, for which video tutorials will also be created.
generated a line list for phosphine; their room temperature line list consists of 137 million transitions among the 5. 6 Please cite this article as: I. E. Gordon et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx. doi. org/10. 1016/j. jqsrt. 2017. 06. 038.
asymmetry, and backscattering spectra of the cloud or aerosol particle. Provision is provided to generate output ASCII files of the inputs and spectra. The IDL version of HITRAN-RI provides output postscript files. Other special program features allow the user to compare two sets of refractive indices, and to calculate spectra for multiple-component aerosols. As an instructional aid, test cases can be run. PDF versions of the original reference papers are contained in a subdirectory, while the refractive indices are stored Please cite this article as: I. E. Gordon et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx. doi. org/10. 1016/j. jqsrt. 2017. 06. 038.
et al. [587] , recorded using a Fourier transform spectrometer. Data recorded for pure O 2 can be found in the O 2 -O 2 Please cite this article as: I. E. Gordon et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx. doi. org/10. 1016/j. jqsrt. 2017. 06. 038 Categorization for the molecules in the HITRAN2016 update.
et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx. doi. org/10. 1016/j. jqsrt. 2017. 06. 038 Summary for the updates for compounds already existing in HITRAN2012. Data from these sources can be found in the alternate folder. convenience, we now also provide the spectrum for O 2 -Air, obtained by combining the available O 2 -O 2 and O 2 -N 2 data. In the alternate folder, we now also include O 2 -Air data from Drouin et al.
et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & List of isotopologues whose partition sums have been updated for this edition of HITRAN. Note that there a few rare isotopologues here that are not in HITRAN. HD16O, HD18O, HD17O, D 2 16 O, D 2 18 O, D 2 17 O 2 12 C 16 O 2 , 13 C 16 O 2 , 16 O 12 C 18 O, 16 O 12 C 17 O, 16 O 13 C 18 O, 16 O 13 C 17 O, 12 C 18 O 2 , 17 O 12 C 18 O, 12 C 17 O 2 , 13 C 18 O 2 , 18 O 13 C 17 O, 13 C 17 O 2 , 14 C 16 O 2 4 14 N 2 16 O 5 12 C 16 O, 13 C 16 O, 12 C 18 O, 12 C 17 O, 13 C 18 O, 13 C 17 O, 14 C 16 O, 14 C 18 O, 14 C 17 O 6 12 CH 4 7 16 O 2 , 16 O 18 O, 16 O 17 O, 18 O 18 O, 18 O 17 O, 17 O 17 O 11 14 NH 3 , 15 NH 3 12 H 14 N 16 O 3 , H 15 N 16 O 3 O 35 Cl 2 , 12 C 16 O 35 Cl 37 Cl.
Acknowledgments The management and development of the HITRAN molecular database has been supported by  NASA   AURA program  grant  NNX14AI55G  and  NASA Planetary Atmosphere  grant  NNX13AI59G  , and  NASA PDART  grant  NNX16AG51G. Portions of the research described in this paper were performed at the  Jet Propulsion Laboratory, California Institute of Technology , under contract with the  National Aeronautics and Space Administration, Government  sponsorship acknowledged. We gratefully acknowledge the many researchers who provided data, experimental and/or theoretical:  Abdulsamee Alkadrou ,  Lorenzo Barrett ,  Emma Barton ,  Chris Benner ,  Linda Brown ,  Jeanna Buldyreva ,  John Coxon ,  Phillip Coles ,  Ludovic Daumont ,  Jolanta Domyslawska ,  Andre Fayt ,  Photos Hadjigeorgiou ,  Shuiming Hu ,  Ekaterina Karlovets ,  Samir Kassi ,  Julien Lamouroux ,  Daniel Lisak ,  Lorenzo Lodi ,  Gang Li ,  Anwen Liu ,  Didier Mondelain ,  Tatyana Petrova ,  Laurence Régalia ,  Candice Renaud ,  Cyril Richard ,  Alexander M.
et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & JID: JQSRT ARTICLE IN PRESS [m5G; August 21, 2017;14:18 ] Table 5 HITRAN2016 ozone update summary: principal isotopologue 16 O 3. Band v -v N Region (cm -1 ) S v 001-010 1781 281. 14-377. 51 1. 255 × 10 -21 100-010 619 295. 42-446. 63 2. 646 × 10 -23 030-020 2558 598. 26-804. 86 1. 942 × 10 -21 101-020 6 656. 12-725. 68 4. 937 × 10 -25 0 02-10 0 1779 899. 45-1176. 42 3. 233 × 10 -21 101-100 3604 911. 32-1215. 49 6. 100 × 10 -20 101-001 3457 921. 37-1211. 67 5. 148 × 10 -21 0 02-0 01 4379 926. 56-1193. 79 1. 651 × 10 -19 20 0-10 0 3966 940. 22-1229. 80 3. 141 × 10 -21 030-100 20 956. 13-1170. 40 1. 916 × 10 -23 20 0-0 01 2964 956. 68-1235. 44 6. 852 × 10 -21 030-001 15 957. 33-1201. 66 2. 254 × 10 -24 002-010 467 1302.
Experimental air-and self-broadening coefficients of H 2 S lines Left panel: Air-broadening coefficients. Waschull1994 stands for Ref. JID: JQSRT [m5G; August 21, 2017;14:18 ] Fig. 24. Gordon et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx. doi. org/10. 1016/j. jqsrt. 2017. 06. 038 ARTICLE IN PRESS.
112 N 2 Johnson et al. (2010) [519] 2,3-Dimethylfuran 14920-89-9 510-6500 278-323 760 0. 112 N 2 Johnson et al. (2010) [519] 2,5-Dimethylfuran 625-86-5 550-70 0 0 278-323 760 0. 112 N 2 Johnson et al. (2010) [519] 2,6-Dimethoxyphenol 91-10-1 580-6500 323 760 0. 112 N 2 Johnson et al. (2010) [519] 2-Carene 554-61-0 60 0-730 0 298-323 760 0. 112 N 2 Johnson et al. (2010) [519] 2-Ethyltoluene 611-14-3 520-6500 298-323 760 0. 112 N 2 Sharpe et al. (2004) [314] 2-Fluoroethanol 371-62-0 80-7250 293-323 760 0. 112-1. 0 N 2 Sharpe et al. (2004) [314] , Sellevag et al. (2004b) [563] ( continued on next page ) Please cite this article as: I. E. Gordon et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx. doi. org/10. 1016/j.
112 N 2 Sharpe et al. (2004) [314] Dimethyl sulfoxide 67-68-5 575-6500 298-323 760 0. 112 N 2 Sharpe et al. (2004) [314] Dimethylamine 124-40-3 550-6700 278-323 760 0. 112 N 2 Sharpe et al. (2004) [314] D-Limonene 5989-27-5 520-6500 298-323 760 0. 112 N 2 Johnson et al. (2010) [519] DL-Limonene 138-86-3 580-6500 298-323 760 0. 112 N 2 Johnson et al. (2010) [519] ( continued on next page ) Please cite this article as: I. E. Gordon et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx. doi. org/10. 1016/j. jqsrt. 2017. 06. 038ARTICLE IN PRESS.
5 air Sihra et al. (2001) [542] HFC-236fa 690-39-1 350-1500 296 700 0. 5 air Sihra et al. (2001) [542] HFC-245cb 1814-88-6 400-1550 296 700 0. 5 air Sihra et al. (2001) [542] HFC-245fa 460-73-1 640-1500 296 700 0. 5 air Sihra et al. (2001) [542] HFC-272ca 420-45-1 30 0-150 0 296 700 0. 5 air Sihra et al. (2001) [542] HFC-329p 375-17-7 50 0-40 0 0 296 700 0. 25 air Young et al. (2009b) [544] HFC-365mfc 406-58-6 60 0-20 0 0 296 700 0. 25 air Inoue et al. (2008) [573] HFC-41 593-53-3 50 0-650 0 278-323 700-760 0. 112-0. 5 N 2 , air Sharpe et al. (2004) [314] , Sihra et al. (2001) [542] * ( continued on next page ) Please cite this article as: I. E. Gordon et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx. doi.
112 N 2 Sharpe et al. (2004) [314] isoprene 78-79-5 60 0-650 0 278-323 760 0. 112 N 2 Sharpe et al. (2004) [314] Isopropylamine 75-31-0 60 0-680 0 278-323 760 0. 112 N 2 Sharpe et al. (2004) [314] Isovaleraldehyde 590-86-3 50 0-650 0 278-323 760 0. 112 N 2 Johnson et al. (2010) [519] Limonene oxide 1195-92-2 510-6500 298-323 760 0. 112 N 2 Johnson et al. (2010) [519] m-Cresol 108-39-4 570-6500 298-323 760 0. 112 N 2 Sharpe et al. (2004) [314] Menthol 89-78-1 580-6500 323 760 0. 112 N 2 Johnson et al. (2010) [519] Methyl 2-methyl butyrate 868-57-5 520-6500 298-323 760 0. 112 N 2 Johnson et al. (2010) [519] Methyl acetoacetate 105-45-3 520-6500 298-323 760 0. 112 N 2 Johnson et al. (2010) [519] ( continued on next page ) Please cite this article as: I. E. Gordon et al. , The HITRAN2016 molecular spectroscopic database, Journal of Quantitative Spectroscopy & Radiative Transfer (2017), http://dx.
Statistical methods In order to study the relationship between different parameters, we performed linear regression analysis using the least squares method and determined both the determination coefficient (R 2 ) and its significance (p value). The correlation between rainfall and drip rate was determined following the methodology described in  Mangin (1984)  and using the STOCHASTOS v3. 0 software of d'Hulst  (1994). www. hydrol-earth-syst-sci. net/21/5357/2017/ Hydrol. Earth Syst. Sci. , 21, 5357-5373, 2017   , 2002)  for Drobeta-Turnu Severin meteorological station (average 14. 07 • C, SD = 9. 14 • C), we see that temperature variability in our area was similar to the regional one (Fig. 4 ). Based on the good correlation between our site and the Drobeta meteorological station, we could use data from the latter in order to get more insight into the relative tem- At Ascunsȃ Cave, POM2 and POM A have a stable temperature regime (Fig.
Rainfall amount and drip rate variability Although the drip log is not continuous, spectral analysis can help reveal how it responds to precipitation. We performed Fourier transform analysis of average daily drip rates and daily rainfall amounts on three continuous time slices: 18 August-30 November 2014, 5 July-30 November 2015, and 1 April-30 November 2016. The results show there is a close link between them for the period 2014-2015, while during 2016 there seems to be a weaker relationship (Fig. 8 ). Cross-correlation analysis of the two datasets shows a similar picture: a very weak correlation in 2016 but a good correlation in 2014 and 2015. During the three periods analyzed, the strongest correlation is found 3 days after rainfall events. In 2014 and 2015 the r k values for a 3-day lag are similar (0.
77 ‰/-7. 70 ‰. The POM X δ 13 C values appear to be affected too by the slow drip rate and the increased kinetic fractionation that accompanies it. The values are higher than at POM2 and more variable. When compared to the available drip rate recorded at POM2, we see that two low δ 13 C values (-10. 54 and -11. 03 ‰) occur during periods with average drip rates of 33 and 43 drips min -1 , respectively (September/December 2014 and December 2014-February 2015), while a third one (-9. 65 ‰) was measured from a period with an average of 13 drips min -1 (July-August 2015). Moreover, when POM X δ 13 C values are compared with average air temperatures from Drobeta  (ECA dataset, Klein Tank et al. , 2002) , there seems to be a good correlation between the two, except for two periods: November 2012-February 2013 and August-September 2013.
Moreover, these equilibrators could be used to sample any dissolved gas for concentration or stable isotopic measurements. Studying monthly collected rain water samples at Drobeta and Isverna, we brought new isotope data from a region scarcely covered by the Global Network of Isotopes in Precipitation (GNIP). The δ 18 O monthly values varied between -15 ‰ in winter and -4 ‰ in summer, while the 2015 weighted mean was -9. 36 ‰ at Isverna and -8. 31 ‰ at Drobeta. These values are comparable to weighted annual means for this region derived from GNIP data. The local meteoric water line is similar to the global one and deuterium excess values reach up to 16 ‰, much higher than those interpolated from GNIP. Modeling of back trajectories shows that most of the air masses that were present at our site during rainy days are of Atlantic origin, with reduced input from the Mediterranean.
According to data extracted from the ECA database(Klein  Tank et al. , 2002), the annual rainfall amount at Drobeta was unusually high in 2014 (1169 mm) in comparison to the 1961-2000 average of 662 mm (Dragotȃ and Baciu, 2008). Values decreased to 674 mm in 2015 and rose to 746 mm in 2016. At Isverna we recorded similar values for 2015 (702 mm) and 2016 (725 mm).
Acknowledgements. This study was financially supported by the following grants: IFA-CEA  C4-08  (FREem,  Co-PIs Silviu Constantin  and  Dominique Blamart ), 17  SEE  ( CAVEMON-ITOR, PI Silviu Constantin ),  PCE-2016-0197  ( CARPATHEMS, PI Silviu Constantin ),  PN-II-RU-TE-2011-3-0235  ( PI Aurel Perşoiu ),  PNII-RU-TE-2014-4-1993  ( PI Aurel Perşoiu ),  790/2014  ( Co-PIs Aurel Perşoiu  and  Dominique Genty ) and 18  SEE  ( PI Cȃţȃlin-Constantin Roibu ). The authors gratefully acknowledge the  NOAA Air Resources Laboratory (ARL)  for the provision of the HYSPLIT transport and dispersion model used in Hydrol. Earth Syst. Sci. , 21,  5357-5373 , 2017 www. hydrol-earth-syst-sci. net/21/5357/2017/.
Acknowledgements The authors thank the staff of the  Titan Laser  and the  Jupiter Laser facility  for their support during the experimental preparation and execution. We thank  R. C. Cauble  and  J. R. Marquès  for fruitful discussions, and  R. Riquier  for the gas jet characterization. This work was partly done within the  LABEX Plas@Par project  and supported by Grant No. 11-IDEX-0004-02  and  ANR-17-CE30-0026-Pinnacle  from  Agence Nationale de la Recherche. It has received funding from the  European Union 's  Horizon 2020 research and innovation programme  under grant agreement no 654148  Laserlab-Europe , and was supported in part by the  Ministry of Education and Science of the Russian Federation  under Contract No. 14. Z50. 31. 0007. The use of the Jupiter Laser Facility was supported by the  U.
S. Department of Energy  by  Lawrence Livermore National Laboratory  under Contract  DE-AC52-07NA27344. This work is supported by  FRQNT  (nouveaux chercheurs, Grant No. 174726 , Team Grant  2016-PR-189974 ),  NSERC   Discovery Grant  (Grant No. 435416 ), ComputeCanada (Job: pve-323-ac,  P. Antici ). M. V. and L. O. S. were supported by the  European Research Council  ( ERC-2010-AdG  grant no. 267841 ). O. Willi acknowledges the  DFG  Programmes  GRK 1203  and  SFB/TR18. M. B. -G. , J. J. S. , and  E. d. 'H. acknowledge the funding from the project  ARIEL  ( Conseil Regional d' Aquitane ); their work was carried out in the framework of the Investments for the  Future Programme IdEn Bordeaux LAPHIA  ( ANR-10-iDEX-03-02 ). The PIC simulations were performed at  Fermi/Marconi (Italy)  through  PRACE allocation  and at the  Accelerates cluster (Lisbon, Portugal ).
Acknowledgements Work by K. G. was supported by the  U. S. Department of Energy, Office of Basic Energy Sciences, Materials Sciences, and Engineering Division  project " Actinide materials under extreme conditions ". The  NHMFL Pulsed Field Facility  is supported by the  NSF , the  U. S. D. O. E. , and the  State of Florida through NSF  cooperative grant  DMR-212 1157490. Work by N. H. and M. J. was supported by the  U. S. D. O. E. BES  project " Science at 100 Tesla ". We deeply thank the NHMFL 100 T magnet operation team:  Y. Coulter ,  D. Roybal ,  M. Gordon ,  J. Martin , and  H. Teshima. We thank  A. Shethker ,  C. D. Batista , and  J. F. Scott  for their interest in our results and insightful discussions. A. S. thanks fruitful discussions with  Céline Varvene  and  Jaejun Yu. M. B. S.
Data and methodology The following data will be used in the analysis: Composite or daily NOAA/ESRL and ECMWF reanalysis meteorological maps covering Europe and northern Africa and corresponding to periods of high ozone have been plotted for the following meteorological parameters: geopotential height, specific humidity anomaly, vertical wind velocity omega (and anomaly), vector wind speed and temperature anomaly. The examination was focused on the tropospheric pressure levels at 850, 700 and 500 hPa (for space limitations mainly the 850 hPa charts are presented). The NOAA/ESRL charts are based on grids of 2. 5 • × 2. 5 • , following the procedure of  Kalnay et al. (1996)  while the horizontal resolution of ECMWF charts is 0. 25 • × 0. 25 •.
Vertical ozone soundings: Further information about the vertical ozone distribution is obtained from the ozone soundings made from the site of Payerne, Switzerland; Uccle, Belgium; and Hohenpeissenberg, Germany. These are regularly carried out with balloon launches starting at 11:00 UTC using ECC (electrochemical mixing ratio cell) ozonesondes in Payerne and Uccle, and Brewer-Mast ozonesondes in Hohenpeissenberg. The data were downloaded from the website of the World Ozone and Ultraviolet Data Centre  (WOUDC, 2015) , uncertainties on the measured ozone-mixing ratios for ECC ozonesondes are between 5 and 10 % (R. Stübi, personal communication, 2005). 6. Regional air quality simulations: The CHIMERE model  (Menut et al. , 2013)  is a stateof-the-art model widely used for pollution and air quality studies  (Rouil et al.
Data availability. The following data sources were used: Figures1 and 13: EMEP data, http://www. nilu. no/projects/ccc/onlinedata/ozone/index. html. Figures2 and 7: NOAA/ESRL charts, https://www. esrl. noaa. gov/psd/data/composites/day/. Figures3 and 8: ECMWF data, http://www. ecmwf. int/en/forecasts/datasets. Figures4 and 9: IASI satellite data. The IASI satellite data used in this study are available from the authors upon request, (maxim. eremenko@lisa. u-pec. fr). Figures4 and 9: EEA data, http://www. eea. europa. eu/data-and-maps. Figures5 and 10: CHIMERE data, the CHIMERE data used in this study are available from the authors upon request (gilles. foret@lisa. u-pec. fr). The CHIMERE model is available at http://www. lmd. polytechnique. fr/chimere/. /ready. arl. noaa. gov/hypub-bin/trajtype.