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The MOVE Fire

This is a personal recollection on the Move fire on May 13, 1985 Philadelphia police fired thousands of rounds at the MOVE house, city officials approved dropping an explosive device on the roof, the resulting fire was allowed to burn, 11 people—including five children—died, and 61 homes were destroyed. Philadelphia City Council later called it a “brutal attack carried out by the City of Philadelphia on its own citizens” and acknowledged that no individual faced criminal consequences for the bombing. One timeline correction worth preserving for the BHP record: the major previous MOVE-police confrontation was August 8, 1978, about seven years before the bombing, not a year or two earlier. Officer James Ramp was killed, other police and firefighters were wounded, nine MOVE members were later convicted, and television cameras recorded police beating Delbert Africa during his arrest. The 1985 MOVE Commission later specifically criticized city planners for failing to adequately use lessons from that 1978 confrontation. And that actually strengthens the point you’re making: 1985 did not happen without precedent or institutional memory. There had already been a deadly confrontation with MOVE, years of conflict, negotiations and police involvement before Osage Avenue.

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BLACK FACTS
The Truths They Never Taught You...

Shirley Chisholm — Unbought and Unbossed

In 1968 Shirley Chisholm became the first Black woman elected to the United States Congress. In 1972 she launched a campaign for the Democratic presidential nomination, breaking another political barrier.

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Wikipedia

HITRAN

HITRAN logo, representing archiving of molecular transitions.

HITRAN (an acronym for High Resolution Transmission) molecular spectroscopic database is a compilation of spectroscopic parameters used to simulate and analyze the transmission and emission of light in gaseous media, with an emphasis on planetary atmospheres. The knowledge of spectroscopic parameters for transitions between energy levels in molecules (and atoms) is essential for interpreting and modeling the interaction of radiation (light) within different media.

For half a century, HITRAN has been considered to be an international standard which provides the user a recommended value of parameters for millions of transitions for different molecules.[citation needed] HITRAN includes both experimental and theoretical data which are gathered from a worldwide network of contributors as well as from articles, books, proceedings, databases, theses, reports, presentations, unpublished data, papers in-preparation and private communications. A major effort is then dedicated to evaluating and processing the spectroscopic data. A single transition in HITRAN has many parameters, including a default 160-byte fixed-width format used since HITRAN2004.[1] Wherever possible, the retrieved data are validated against accurate laboratory data.[2]

The original version of HITRAN was compiled by the US Air Force Cambridge Research Laboratories (1960s) in order to enable surveillance of military aircraft detected through the terrestrial atmosphere.[2] One of the early applications of HITRAN was a program called Atmospheric Radiation Measurement (ARM) for the US Department of Energy.[2] In this program spectral atmospheric measurements were made around the globe in order to better understand the balance between the radiant energy that reaches Earth from the sun and the energy that flows from Earth back out to space.[2] The US Department of Transportation also utilized HITRAN in its early days for monitoring the gas emissions (NO, SO2, NO2) of super-sonic transports flying at high altitude.[2] HITRAN was first made publicly available in 1973[3] and today there are a multitude of ongoing and future NASA satellite missions which incorporate HITRAN.[2] One of the NASA missions currently utilizing HITRAN is the Orbiting Carbon Observatory (OCO) which measures the sources and sinks of CO2 in the global atmosphere.[2] HITRAN is a free resource and is currently maintained and developed at the Center for Astrophysics | Harvard & Smithsonian, Cambridge MA, USA.[4]

This image represents light being gathered via a prism onto an archival medium, in this case the "rosetta" stone (an abstraction of HITRAN) with an imprint of spectra, parameters etc.

HITRAN is the worldwide standard for calculating or simulating atmospheric molecular transmission and radiance from the microwave through ultraviolet region of the spectrum.[5] The HITRAN database is officially released on a quadrennial basis, with updates posted in the intervening years on HITRANonline.[6]There is a new journal article published in conjunction with the most recent release of the HITRAN database, and users are strongly encouraged to use the most recent edition.[6] Throughout HITRAN's history, there have been around 50,000 unique users of the database and in recent years there are over 40,000 users registered on HITRANonline. There are YouTube tutorials on the HITRANonline webpage to answer frequently asked questions by users.[2]

Calculated transmission spectra through four sample cells containing one atmosphere of each molecule at 296 K with the corresponding path length. Spectra have been calculated using the HITRAN2016 database and HAPI Python libraries. Credit: HITRAN Team
Data Available from HITRAN
Line-by-Line Transitions
Absorption Cross Sections
Collision Induced Absorption
MT_CKD Water Vapor Continuum
Aerosol Refractive Indices
HITEMP
HAPI
Supplemental data for radiative-transfer calculations[5]

Line-by-Line

[edit]

The current version of the database, HITRAN2024[6], contains 61 molecules in the line-by-line portion of HITRAN along with some of their most significant isotopologues (156 isotopologues in total).[6] These data are archived as a multitude of high-resolution line transitions, each containing many spectral parameters required for high-resolution simulations.

This image depicts the number of line-by-line transitions within HITRAN per year. AFGL values are atmospheric absorption line parameters. AFGL is an acronym for the Air Force Geophysical Laboratory Catalog, which was the predecessor of HITRAN. Credit: HITRAN Team

Absorption Cross-Sections

[edit]

In addition to the traditional line-by-line spectroscopic absorption parameters, the HITRAN database contains information on absorption cross-sections where the line-by-line parameters are absent or incomplete. Typically HITRAN includes absorption cross-sections for heavy polyatomic molecules (with low-lying vibrational modes) which are difficult for detailed analysis due to the high density of the spectral bands/lines, broadening effects, isomerization, and overall modeling complexity.[6][7] There are 644 molecular species in the current edition of the database provided as cross-section files. The cross-section files are provided in the HITRAN format described on the official HITRAN website.

Collision-Induced Absorption

[edit]

The HITRAN compilation also provides collision-induced absorption (CIA)[8][9] that was first introduced into HITRAN in the 2012 edition.[10] CIA refers to absorption by transient electric dipoles induced by the interaction between colliding molecules. Instructions for accessing the CIA data files can be found on HITRAN/CIA.[11]

MT_CKD Water Vapor Continuum

[edit]

The MT_CKD (Mlawer-Tobin-Clough-Kneizys-Davies) Water Vapor Continuum Model [12][13][14] provides water vapor absorption coefficients that should be added to the local contributions of water vapor transitions, such as those available in the HITRAN line-by-line section, in order to obtain the total absorption due to water vapor. Compared to line absorption, the continuum absorption varies more slowly across the spectrum.

The MT_CKD Water Vapor Continuum provides absorption coefficients for both the self continuum (arising from interactions between water molecules) and the foreign continuum (arising from interactions between water vapor and other atmospheric gases). These coefficients are distributed in a netCDF file at a reference density corresponding to a pressure of 1013 mbar and temperature of 296 K for both the self and foreign continuum. This file also contains the temperature-dependence coefficients for the self continuum, allowing users to adjust the reference values for temperatures other than 296 K. The accompanying code performs the appropriate scaling and interpolation to compute the continuum absorption coefficients at arbitrary pressures, temperatures, and wavenumbers.

The MT_CKD Water Vapor Continuum Model is constrained to remain consistent with high-quality analyses of atmospheric and laboratory measurements. Keeping the MT_CKD continuum consistent with current observational studies requires periodic updates to the continuum coefficients. A record of revisions to the MT_CKD Water Vapor Continuum Model can be found on the model's GitHub page.

The associated code and data are available through the HITRAN website at hitran.org/mtckd and at the AER GitHub site at github.com/AER-RC/MT_CKD_H2O.

Aerosol Refractive Indices

[edit]

HITRAN2024 also has an aerosols refractive indices section, with data in the visible, infrared, and millimeter spectral ranges of many types of cloud and aerosol particles. Knowledge of the refractive indices of the aerosols and cloud particles and their size distributions is necessary in order to specify their optical properties.[15]

HITEMP

[edit]

HITEMP is the molecular spectroscopic database analogous to HITRAN for high-temperature modeling of the spectra of molecules in the gas phase.[16] HITEMP encompasses many more bands and transitions than HITRAN for eight absorbers: H2O, CO2, N2O, CO, CH4, NO, NO2 and OH.[16][17][18] Due to the extremely large number of transitions required for high-temperature simulations, it was necessary to provide the HITEMP data as separate files to that of HITRAN. The HITEMP line lists retain the same 160-character format that was used for earlier editions of HITRAN.[16][1] There are numerous applications for HITEMP data, some examples include the thermometry of high-temperature environments,[19] analysis of combustion processes,[20] and modeling spectra of atmospheres in the Solar System,[21] exoplanets,[22] brown dwarfs,[23] and stars.[24]

HAPI

[edit]

A Python library HAPI (HITRAN Application Programming Interface) has been developed which serves as a tool for absorption and transmission calculations as well as comparisons of spectroscopic data sets.[25] HAPI extends the functionality of the main site, in particular, for the calculation of spectra using several types of line shape calculations, including the flexible HT (Hartmann-Tran) profile. This HT line shape can also be reduced to a number of conventional line profiles such as Gaussian (Doppler), Lorentzian, Voigt, Rautian, Speed-Dependent Voigt and Speed-Dependent Rautian. In addition to accounting for pressure, temperature and optical path length, the user can include a number of instrumental functions to simulate experimental spectra. HAPI is able to account for broadening of lines due to mixtures of gases as well as make use of all broadening parameters supplied by HITRAN. This includes the traditional broadeners (air, self) as well as additional parameters for CO2, H2O, H2 and He broadening.[26][27] The following spectral functions can be calculated in the current version #1 of HAPI:[25]

  • absorption coefficient
  • absorption spectrum
  • transmittance spectrum
  • radiance spectrum[25]

HAPIEST (an acronym for HITRAN Application Programming Interface and Efficient Spectroscopic Tools) is a graphical user interface allowing users to access some of the functionality provided by HAPI without any knowledge of Python programming, including downloading data from HITRAN, and plotting of spectra and cross-sections. The source code for HAPIEST is available on GitHub (HAPIEST), along with binary distributions for Mac and PC.[28]

See also

[edit]

References

[edit]
  1. ^ a b Rothman, Laurence S.; Jacquemart, D.; Barbe, A.; Chris Benner, D.; Birk, M.; Brown, L.R.; Carleer, M.R.; Chackerian, C.; Chance, K.; Coudert, L.H.; Dana, V.; Devi, V.M.; Flaud, J.-M.; Gamache, R.R.; Goldman, A.; Hartmann, J.-M.; Jucks, K.W.; Maki, A.G.; Mandin, J.-Y.; Massie, S.T.; Orphal, J.; Perrin, A.; Rinsland, C.P.; Smith, M.A.H.; Tennyson, J.; Tolchenov, R.N.; Toth, R.A.; Vander Auwera, J.; Varanasi, P.; Wagner, G. (2005). "The HITRAN 2004 molecular spectroscopic database". Journal of Quantitative Spectroscopy and Radiative Transfer. 96 (2): 139–204. Bibcode:2005JQSRT..96..139R. doi:10.1016/j.jqsrt.2004.10.008.
  2. ^ a b c d e f g h Rothman, Laurence S. (2021). "History of the HITRAN Database". Nature Reviews Physics. 3 (5): 302–304. Bibcode:2021NatRP...3..302R. doi:10.1038/s42254-021-00309-2. S2CID 233527113.
  3. ^ McClatchey R. A., Benedict W. S., Clough S. A., et al, "AFCRL Atmospheric Absorption Line Parameters Compilation", AFCRL-TR-73-0096, Environmental Research Papers, No. 434, Optical Physics Laboratory, Air Force Cambridge Research Laboratories (1973).
  4. ^ "HITRAN and HITEMP Database | Center for Astrophysics | Harvard & Smithsonian". www.cfa.harvard.edu. Retrieved 26 November 2025.
  5. ^ a b "HITRANonline data: Supplemental". hitran.org. Retrieved 2025-11-25.
  6. ^ a b c d e Gordon, I.E.; Rothman, L.S.; Hargreaves, R.J.; Gomez, F.M.; Bertin, T.; Hill, C.; Kochanov, R.V.; Tan, Y.; Wcisło, P.; Makhnev, V.Yu.; Bernath, P.F.; Birk, M.; Boudon, V.; Campargue, A.; Coustenis, A.; Drouin, B.J.; Gamache, R.R.; Hodges, J.T.; Jacquemart, D.; Mlawer, E.J.; Nikitin, A.V.; Perevalov, V.I.; Rotger, M.; Robert, S.; Tennyson, J.; Toon, G.C.; Tran, H.; Tyuterev, V.G.; Adkins, E.M.; Barbe, A.; Bailey, D.M.; Bielska, K.; Bizzocchi, L.; Blake, T.A.; Bowesman, C.A.; Cacciani, P.; Čermák, P.; Császár, A.G.; Denis, L.; et al. (2026). "The HITRAN2024 molecular spectroscopic database". Journal of Quantitative Spectroscopy and Radiative Transfer. 353 109807. Bibcode:2026JQSRT.35309807G. doi:10.1016/j.jqsrt.2026.109807.
  7. ^ Gordon, I.E.; Rothman, L.S.; Hill, C.; Kochanov, R.V.; Tan, Y.; Bernath, P.F.; Birk, M.; Boudon, V.; Campargue, A.; Chance, K.V.; Drouin, B.J.; Flaud, J.-M.; Gamache, R.R.; Hodges, J.T.; Jacquemart, D.; Perevalov, V.I.; Perrin, A.; Shine, K.P.; Smith, M.-A.H.; Tennyson, J.; Toon, G.C.; Tran, H.; Tyuterev, V.G.; Barbe, A.; Császár, A.G.; Devi, V.M.; Furtenbacher, T.; Harrison, J.J.; Hartmann, J.-M.; et al. (2017). "The HITRAN2016 molecular spectroscopic database". Journal of Quantitative Spectroscopy and Radiative Transfer. 203: 3–69. Bibcode:2017JQSRT.203....3G. doi:10.1016/j.jqsrt.2017.06.038. hdl:2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/263338.
  8. ^ Terragni, J. (2025). "Collision induced absorption in HITRAN2024: Enhanced and improved data for atmospheric and planetary studies". Journal of Quantitative Spectroscopy and Radiative Transfer. 347 109631. Bibcode:2025JQSRT.34709631T. doi:10.1016/j.jqsrt.2025.109631.
  9. ^ Karman, Tijs; Gordon, Iouli E.; Van Der Avoird, Ad; Baranov, Yury I.; Boulet, Christian; Drouin, Brian J.; Groenenboom, Gerrit C.; Gustafsson, Magnus; Hartmann, Jean-Michel; Kurucz, Robert L.; Rothman, Laurence S.; Sun, Kang; Sung, Keeyoon; Thalman, Ryan; Tran, Ha; Wishnow, Edward H.; Wordsworth, Robin; Vigasin, Andrey A.; Volkamer, Rainer; Van Der Zande, Wim J. (2019). "Update of the HITRAN collision-induced absorption section". Icarus. 328: 160–175. Bibcode:2019Icar..328..160K. doi:10.1016/J.ICARUS.2019.02.034. hdl:2066/204360. S2CID 111387566.
  10. ^ Richard, C.; Gordon, I.E.; Rothman, L.S.; Abel, M.; Frommhold, L.; Gustafsson, M.; Hartmann, J.-M.; Hermans, C.; Lafferty, W.J.; Orton, G.S.; Smith, K.M.; Tran, H. (2012). "New section of the HITRAN database: Collision-induced absorption (CIA)". Journal of Quantitative Spectroscopy and Radiative Transfer. 113 (11): 1276–1285. Bibcode:2012JQSRT.113.1276R. doi:10.1016/j.jqsrt.2011.11.004.
  11. ^ Terragni, J. (2025). "Collision induced absorption in HITRAN2024: Enhanced and improved data for atmospheric and planetary studies". Journal of Quantitative Spectroscopy and Radiative Transfer. 347 109631. Bibcode:2025JQSRT.34709631T. doi:10.1016/j.jqsrt.2025.109631.
  12. ^ Mlawer, E.J.; Payne, V.H.; Moncet, J.-L.; Delamere, J.S.; Alvarado, M.J.; Tobin, D.D. (2012). "Development and recent evaluation of the MT_CKD model of continuum absorption". Philosophical Transactions of the Royal Society A. 370: 1–37. doi:10.1098/rsta.2011.0295.
  13. ^ Mlawer, E.J.; Turner, D.D.; Paine, S.N.; Palchetti, L.; Bianchini, B.; Payne, V.H.; Cady-Pereira, K.E.; Pernak, R.L.; Alvarado, M.J.; Gombos, D.; Delamere, J.S.; Mlynczak, M.G.; Mast, J.C. (2019). "Analysis of Water Vapor Absorption in the Far-Infrared and Submillimeter Regions Using Surface Radiometric Measurements From Extremely Dry Locations". Journal of Geophysical Research: Atmospheres. 124: 8134–8160. doi:10.1029/2018JD029508.
  14. ^ Mlawer, E.J.; Cady-Pereira, K.E.; Mascio, J.; Gordon, I.E. (2023). "The inclusion of the MT_CKD water vapor continuum model in the HITRAN molecular spectroscopic database". Journal of Quantitative Spectroscopy and Radiative Transfer. 306 108645. doi:10.1016/j.jqsrt.2023.108645.
  15. ^ Rothman, L.S.; Gordon, I.E.; Babikov, Y.; Barbe, A.; Chris Benner, D.; Bernath, P.F.; Birk, M.; Bizzocchi, L.; Boudon, V.; Brown, L.R.; Campargue, A.; Chance, K.; Cohen, E.A.; Coudert, L.H.; Devi, V.M.; Drouin, B.J.; Fayt, A.; Flaud, J.-M.; Gamache, R.R.; Harrison, J.J.; Hartmann, J.-M.; Hill, C.; Hodges, J.T.; Jacquemart, D.; Jolly, A.; Lamouroux, J.; Le Roy, R.J.; Li, G.; Long, D.A.; et al. (2013). "The HITRAN2012 molecular spectroscopic database". Journal of Quantitative Spectroscopy and Radiative Transfer. 130: 4–50. Bibcode:2013JQSRT.130....4R. doi:10.1016/j.jqsrt.2013.07.002.
  16. ^ a b c Rothman, L.S.; Gordon, I.E.; Barber, R.J.; Dothe, H.; Gamache, R.R.; Goldman, A.; Perevalov, V.I.; Tashkun, S.A.; Tennyson, J. (2010). "HITEMP, the high-temperature molecular spectroscopic database". Journal of Quantitative Spectroscopy and Radiative Transfer. 111 (15): 2139–2150. Bibcode:2010JQSRT.111.2139R. doi:10.1016/j.jqsrt.2010.05.001.
  17. ^ Hargreaves, Robert J.; Gordon, Iouli E.; Rey, Michael; Nikitin, Andrei V.; Tyuterev, Vladimir G.; Kochanov, Roman V.; Rothman, Laurence S. (2020). "An Accurate, Extensive, and Practical Line List of Methane for the HITEMP Database". The Astrophysical Journal Supplement Series. 247 (2): 55. arXiv:2001.05037. Bibcode:2020ApJS..247...55H. doi:10.3847/1538-4365/ab7a1a. S2CID 210718603.
  18. ^ Hargreaves, Robert J.; Gordon, Iouli E.; Rothman, Laurence S.; Tashkun, Sergey A.; Perevalov, Valery I.; Lukashevskaya, Anastasiya A.; Yurchenko, Sergey N.; Tennyson, Jonathan; Müller, Holger S.P. (2019). "Spectroscopic line parameters of NO, NO2, and N2O for the HITEMP database". Journal of Quantitative Spectroscopy and Radiative Transfer. 232: 35–53. arXiv:1904.02636. Bibcode:2019JQSRT.232...35H. doi:10.1016/j.jqsrt.2019.04.040. S2CID 102353423.
  19. ^ Pinkowski, Nicolas H.; Biswas, Pujan; Shao, Jiankun; Strand, Christopher L.; Hanson, Ronald K. (2021). "Thermometry and speciation for high-temperature and -pressure methane pyrolysis using shock tubes and dual-comb spectroscopy". Measurement Science and Technology. 32 (12): 125502. Bibcode:2021MeScT..32l5502P. doi:10.1088/1361-6501/ac22ef. S2CID 238246785.
  20. ^ Spearrin, R. M.; Goldenstein, C. S.; Jeffries, J. B.; Hanson, R. K. (2013). "Fiber-coupled 2.7 µm laser absorption sensor for CO2 in harsh combustion environments". Measurement Science and Technology. 24 (5) 055107. Bibcode:2013MeScT..24e5107S. doi:10.1088/0957-0233/24/5/055107. S2CID 99625680.
  21. ^ Haus, R.; Kappel, D.; Arnold, G. (2013). "Self-consistent retrieval of temperature profiles and cloud structure in the northern hemisphere of Venus using VIRTIS/VEX and PMV/VENERA-15 radiation measurements". Planetary and Space Science. 89: 77–101. Bibcode:2013P&SS...89...77H. doi:10.1016/j.pss.2013.09.020.
  22. ^ Giacobbe, Paolo; Brogi, Matteo; Gandhi, Siddharth; Cubillos, Patricio E.; Bonomo, Aldo S.; Sozzetti, Alessandro; Fossati, Luca; Guilluy, Gloria; Carleo, Ilaria; Rainer, Monica; Harutyunyan, Avet; Borsa, Francesco; Pino, Lorenzo; Nascimbeni, Valerio; Benatti, Serena; Biazzo, Katia; Bignamini, Andrea; Chubb, Katy L.; Claudi, Riccardo; Cosentino, Rosario; Covino, Elvira; Damasso, Mario; Desidera, Silvano; Fiorenzano, Aldo F.~M.; Ghedina, Adriano; Lanza, Antonino F.; Leto, Giuseppe; Maggio, Antonio; Malavolta, Luca; et al. (2021). "Five carbon- and nitrogen-bearing species in a hot giant planet's atmosphere". Nature. 592 (7853): 205–208. arXiv:2104.03352. Bibcode:2021Natur.592..205G. doi:10.1038/s41586-021-03381-x. PMID 33828321. S2CID 233181895.
  23. ^ Bailey, Jeremy; Kedziora-Chudczer, Lucyna (2012). "Modelling the spectra of planets, brown dwarfs and stars using VSTAR". Monthly Notices of the Royal Astronomical Society. 419 (3): 1913–1929. arXiv:1109.3748. Bibcode:2012MNRAS.419.1913B. doi:10.1111/j.1365-2966.2011.19845.x. S2CID 118601237.
  24. ^ Pavlenko, Yakiv V.; Yurchenko, Sergei N.; Tennyson, Jonathan (2020). "Analysis of the first overtone bands of isotopologues of CO and SiO in stellar spectra". Astronomy & Astrophysics. 633: A52. arXiv:1911.12326. Bibcode:2020A&A...633A..52P. doi:10.1051/0004-6361/201936811. S2CID 208310051.
  25. ^ a b c Kochanov, R.V.; Gordon, I.E.; Rothman, L.S.; Wcisło, P.; Hill, C.; Wilzewski, J.S. (2016). "HITRAN Application Programming Interface (HAPI): A comprehensive approach to working with spectroscopic data". Journal of Quantitative Spectroscopy and Radiative Transfer. 177: 15–30. Bibcode:2016JQSRT.177...15K. doi:10.1016/j.jqsrt.2016.03.005.
  26. ^ Tan, Y. (2022). "H2, He, and CO2 Pressure-induced Parameters for the HITRAN Database. II. Line Lists of CO2, N2O, CO, SO2, OH, OCS, H2CO, HCN, PH3, H2S, and GeH4". The Astrophysical Journal Supplement Series. 262. doi:10.3847/1538-4365/ac83a (inactive 14 February 2026).{{cite journal}}: CS1 maint: DOI inactive as of February 2026 (link)
  27. ^ Wilzewski, Jonas S.; Gordon, Iouli E.; Kochanov, Roman V.; Hill, Christian; Rothman, Laurence S. (2016). "H2, He, and CO2 line-broadening coefficients, pressure shifts and temperature-dependence exponents for the HITRAN database. Part 1: SO2, NH3, HF, HCL, OCS and C2H2". Journal of Quantitative Spectroscopy and Radiative Transfer. 168: 193–206. Bibcode:2016JQSRT.168..193W. doi:10.1016/j.jqsrt.2015.09.003.
  28. ^ "hitranonline/hapiest". GitHub. 10 June 2025. Retrieved 26 November 2025.

Further reading

[edit]
[edit]

Source: Wikipedia. Article content is retrieved live through the MediaWiki API.

Wikipedia

HITRAN

HITRAN (an acronym for High Resolution Transmission) molecular spectroscopic database is a compilation of spectroscopic parameters used to simulate and analyze the transmission and emission of light in gaseous media, with an emphasis on planetary atmospheres. The knowledge of spectroscopic parameters for transitions between energy levels in molecules (and atoms) is essential for interpreting and modeling the interaction of radiation (light) within different media. For half a century, HITRAN has been considered to be an international standard which provides the user a recommended value of parameters for millions of transitions for different molecules. HITRAN includes both experimental and theoretical data which are gathered from a worldwide network of contributors as well as from articles, books, proceedings, databases, theses, reports, presentations, unpublished data, papers in-preparation and private communications. A major effort is then dedicated to evaluating and processing the spectroscopic data. A single transition in HITRAN has many parameters, including a default 160-byte fixed-width format used since HITRAN2004. Wherever possible, the retrieved data are validated against accurate laboratory data. The original version of HITRAN was compiled by the US Air Force Cambridge Research Laboratories (1960s) in order to enable surveillance of military aircraft detected through the terrestrial atmosphere. One of the early applications of HITRAN was a program called Atmospheric Radiation Measurement (ARM) for the US Department of Energy. In this program spectral atmospheric measurements were made around the globe in order to better understand the balance between the radiant energy that reaches Earth from the sun and the energy that flows from Earth back out to space. The US Department of Transportation also utilized HITRAN in its early days for monitoring the gas emissions (NO, SO2, NO2) of super-sonic transports flying at high altitude. HITRAN was first made publicly available in 1973 and today there are a multitude of ongoing and future NASA satellite missions which incorporate HITRAN. One of the NASA missions currently utilizing HITRAN is the Orbiting Carbon Observatory (OCO) which measures the sources and sinks of CO2 in the global atmosphere. HITRAN is a free resource and is currently maintained and developed at the Center for Astrophysics | Harvard & Smithsonian, Cambridge MA, USA. HITRAN is the worldwide standard for calculating or simulating atmospheric molecular transmission and radiance from the microwave through ultraviolet region of the spectrum. The HITRAN database is officially released on a quadrennial basis, with updates posted in the intervening years on HITRANonline.There is a new journal article published in conjunction with the most recent release of the HITRAN database, and users are strongly encouraged to use the most recent edition. Throughout HITRAN's history, there have been around 50,000 unique users of the database and in recent years there are over 40,000 users registered on HITRANonline. There are YouTube tutorials on the HITRANonline webpage to answer frequently asked questions by users.

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Wikipedia

HITRANS

The Highlands and Islands Transport Partnership (HITRANS) is the statutory regional transport partnership for Na h-Eileanan Siar, Highland, Moray, Orkney Islands and Argyll and Bute (less the Helensburgh and Lomond area, which is covered by the Strathclyde Partnership for Transport). It was created by Transport Scotland under the Transport (Scotland) Act 2005, along with six similar groups covering other areas of Scotland. HITRANS covers the largest area of any such partnership in Scotland, covering over 50% of the country's total landmass.

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Wikipedia

Johannes Orphal

Johannes Orphal (born 11 July 1966, in Magdeburg) is a German physicist. He is Head of Division 4 "Natural and Built Environment" and Full Professor of Physics at the Karlsruhe Institute of Technology (KIT). From 2009 to 2020 he was Director of the Institute of Meteorology and Climate Research (IMK) at KIT. Until 2009, he was Professor at the University of Paris-Est in Créteil and research scientist at the CNRS. In 2005, Orphal served as Secretary of the Organizing Committee for the Opening Ceremonies of the World Year of Physics at UNESCO headquarters in Paris. His main scientific contributions are in the field of molecular spectroscopy applied to the Earth's atmosphere: laboratory measurements of unstable and reactive molecules and radicals, data evaluation for international databases e.g. HITRAN, preparation and use of remote-sensing satellite missions (GOME, SCIAMACHY, MIPAS, MetOp, MTG ...) to observe stratospheric chemistry, tropospheric air quality and processes of relevance for climate, as well as the development of sensitive in-situ measurements techniques such as IBBCEAS. In 2017, he was awarded the Gentner-Kastler Prize of the French and German Physical Societies (SFP and DPG) and the Gay-Lussac Humboldt Prize of the Académie des sciences in Paris.

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Wikipedia

FUTBOLIN

FUTBOLIN (FUll Transfer By Optimized LINe-by-line methods) is a radiative transfer model for the calculation of line-by-line atmospheric emission/transmission spectra in planetary atmospheres. It has been developed by Javier Martín-Torres. It allows generating high-resolution synthetic spectra in the 0.3-1000 micrometre spectral range. The code can handle spherical or plane-parallel atmospheres. It reads spectral lines in HITRAN or GEISA format and can handle CO2 line mixing and continuum absorption from H2O, O2, N2 and CO2. It also takes into account the Non Local Thermodynamic Equilibrium (NLTE) effects on the rotational, electronic and vibrational populations of the atmospheric species and allows to specify any combinations of clouds, coverage and spectral albedo. It has been used to model the Earth's atmosphere, and the atmospheres of Mars, Venus, and Titan. The code can calculate reflection, transmission, absorption, infrared cooling rate, and flux spectra.

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TOPIC OF THE DAY

Greenwood / Black Wall Street

Before the 1921 destruction of Tulsa’s Greenwood District, Black residents had created a remarkable center of business and community life. The district included stores, professional offices, entertainment venues and homes owned by Black citizens. Understanding Greenwood means learning what was built—not only what was burned.

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TRIVIA QUESTION OF THE DAY

Which Supreme Court case ruled state-sponsored public-school segregation unconstitutional?

Brown v. Board of Education in 1954.