J/MNRAS/406/1745ivo://CDS.VizieR/J/MNRAS/406/1745doi:10.26093/cds/vizier.74061745CDSFlower D.R.Pineau des Forets G.2024-07-11T20:17:04Z2011-03-04T13:37:37ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fratomic-physicsinterstellar-mediumThe dissipation of kinetic energy that occurs in interstellar shock waves is accompanied by the emission of radiation. In the case of shocks that are propagating into mainly molecular gas, the emission occurs principally in lines of the species H_2_, H, O, CO and H_2_O. The relative intensities of these emission lines are indicative of the type and speed of the shock wave and of the physical conditions in the ambient gas. We present the results of computations of the intensities of these lines, for small grids of models of C- and J-type shock waves, and compare with the results of previous calculations. Our results should serve to aid the interpretation of observations made with the Herschel and other satellites.2010MNRAS.406.1745Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/406/1745CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/406/1745https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/406/1745http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/406/1745https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/406/1745https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/406/1745http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/406/1745GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/MNRAS/406/1745/resultsH_2_O line intensities in shock wavesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintshockSimbad column added by the CDSphys.atmol.configurationcharUpperUpper level (1)phys.energy;phys.atmol.levelLowerLower level (1)phys.energy;phys.atmol.levelEupExcitation energy of the upper level of the transition, relative to the 0 0 0 ground levelKphys.atmol.excitation;stat.maxfloatnuFrequency of transitionGHzem.freq;phys.atmol.transitiondoublelambdaWavelength of transitionumem.wldoublev10n2e4Line intensity, TdV, for shock speed vs=10km/s and n_H_=2x10^4^cm^-3^ (2)K.km/sphot.flux.density;em.radiodoublev20n2e4Line intensity, TdV, for shock speed vs=20km/s and n_H_=2x10^4^cm^-3^ (2)K.km/sphot.flux.density;em.radiodoublev30n2e4Line intensity, TdV, for shock speed vs=30km/s and n_H_=2x10^4^cm^-3^ (2)K.km/sphot.flux.density;em.radiodoublev40n2e4? Line intensity, TdV, for shock speed vs=40km/s and n_H_=2x10^4^cm^-3^ (2)K.km/sphot.flux.density;em.radiodoublenullablev10n2e5Line intensity, TdV, for shock speed vs=10km/s and n_H_=2x10^5^cm^-3^ (2)K.km/sphot.flux.density;em.radiodoublev20n2e5Line intensity, TdV, for shock speed vs=20km/s and n_H_=2x10^5^cm^-3^ (2)K.km/sphot.flux.density;em.radiodoublev30n2e5Line intensity, TdV, for shock speed vs=30km/s and n_H_=2x10^5^cm^-3^ (2)K.km/sphot.flux.density;em.radiodoublev40n2e5? Line intensity, TdV, for shock speed vs=40km/s and n_H_=2x10^5^cm^-3^ (2)K.km/sphot.flux.density;em.radiodoublenullable