J/A+A/675/A86ivo://CDS.VizieR/J/A+A/675/A86doi:10.26093/cds/vizier.36750086CDSKristensen L.E.Godard B.Guillard P.Gusdorf A.Pineau des Forets G.2026-07-01T14:00:45Z2023-07-05T08:15:59ZCDS support team

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

cds-question@unistra.frastronomical-modelsinterstellar-mediumMolecular hydrogen, H_2_, is the most abundant molecule in the Universe. Thanks to its widely spaced energy levels, it predominantly lights up in warm gas, T>100K, such as shocked regions externally irradiated or not by interstellar UV photons, and it is one of the prime targets of James Webb Space Telescope (JWST) observations. These may include shocks from protostellar outflows, supernova remnants impinging on molecular clouds, all the way up to starburst galaxies and active galactic nuclei. Sophisticated shock models are able to simulate H_2_ emission from such shocked regions. We aim to explore H_2_ excitation using shock models, and to test over which parameter space distinct signatures are produced in H_2_ emission. We here present simulated H_2_ emission using the Paris-Durham shock code over an extensive grid of ~14000 plane-parallel stationary shock models, a large subset of which are exposed to a semi-isotropic external UV radiation field. The grid samples six input parameters: the preshock density, shock velocity, transverse magnetic field strength, UV radiation field strength, the cosmic-ray-ionization rate, and the abundance of polycyclic aromatic hydrocarbons, PAHs. Physical quantities resulting from our self-consistent calculations, such as temperature, density, and width, have been extracted along with H_2_ integrated line intensities. These simulations and results are publicly available on the Interstellar Medium Services platform. The strength of the transverse magnetic field, as quantified by the magnetic scaling factor, b, plays a key role in the excitation of H_2_. At low values of b (<0.3, J-type shocks), H_2_ excitation is dominated by vibrationally excited lines; whereas, at higher values (b>1, C-type shocks), rotational lines dominate the spectrum for shocks with an external radiation field comparable to (or lower than) the solar neighborhood. Shocks with b>1 can potentially be spatially resolved with JWST for nearby objects. H_2_ is typically the dominant coolant at lower densities (<10^4^cm^-3^); at higher densities, other molecules such as CO, OH, and H_2_O take over at velocities <20km/s and atoms, for example, H, O, and S, dominate at higher velocities. Together, the velocity and density set the input kinetic energy flux. When this increases, the excitation and integrated intensity of H_2_ increases similarly. An external UV field mainly serves to increase the excitation, particularly for shocks where the input radiation energy is comparable to the input kinetic energy flux. These results provide an overview of the energetic reprocessing of input kinetic energy flux and the resulting H_2_ line emission.2023A&A...675A..86Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A86CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/675/A86https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/675/A86http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/675/A86https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/675/A86https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/675/A86http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/675/A86GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/675/A86/physgridPhysical results of the shock simulations (table B1)XPAHPAH abundancephys.abundfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAllDisplay data in all tablesmeta.ref.urlcharnHPreshock densitycm**-3phys.densitydoubleVsShock velocitykm/sphys.velocfloatbMagnetic field scaling factorarith.factorfloatG0Strength of UV fieldspect.line.widthfloatzetaCosmic-ray-ionization rates**-1phot.count;em.X-rayfloatTypeShock type (0J-1C-2Cs-3CJ)meta.notefloatTgas-iniInitial gas temperatureKphys.temperaturefloatTgas-maxMaximum neutral gas temperatureKphys.temperaturedoubleDelta-zShock widthAUsrc.morph.paramdoubleDelta-tShock ageyrtime.agedoubleNHShock column densitycm**-2phys.columnDensitydoublenHmaxMaximum densitycm**-3phys.densitydoubleJ/A+A/675/A86/coldensColumn densities of select ions (table B2)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAllDisplay data in all tablesmeta.ref.urlcharnHPreshock densitycm**-3phys.densitydoubleVsShock velocitykm/sphys.velocfloatbMagnetic field scaling factorarith.factorfloatG0Strength of UV fieldspect.line.widthfloatzetaCosmic-ray-ionization rates**-1phot.count;em.X-rayfloatXPAHPAH abundancephys.abundfloatTypeShock type (0J-1C-2Cs-3CJ)meta.notefloatNHH column densitycm**-2phys.columnDensitydoubleNH2H2 column densitycm**-2phys.columnDensitydoubleNOO column densitycm**-2phys.columnDensitydoubleNOHOH column densitycm**-2phys.columnDensitydoubleNH2OH2O column densitycm**-2phys.columnDensitydoubleNCpC+ column densitycm**-2phys.columnDensitydoubleNCC column densitycm**-2phys.columnDensitydoubleNCOCO column densitycm**-2phys.columnDensitydoubleJ/A+A/675/A86/h2excH2 excitation diagrams (table B3)v2-J2Column density of v2_J2cm**-2phys.columnDensityfloatrecnoRecord number assigned by the VizieR team. 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Eup_v0_J22Kphys.energy;phys.atmol.leveldoublev5-J9Column density of v5_J9cm**-2phys.columnDensityfloatEup-v5-J9Upper level energy Eup_v5_J9Kphys.energy;phys.atmol.leveldoublev6-J4Column density of v6_J4cm**-2phys.columnDensityfloatEup-v6-J4Upper level energy Eup_v6_J4Kphys.energy;phys.atmol.leveldoublev1-J20Column density of v1_J20cm**-2phys.columnDensityfloatEup-v1-J20Upper level energy Eup_v1_J20Kphys.energy;phys.atmol.leveldoublev2-J18Column density of v2_J18cm**-2phys.columnDensityfloatEup-v2-J18Upper level energy Eup_v2_J18Kphys.energy;phys.atmol.leveldoublev6-J5Column density of v6_J5cm**-2phys.columnDensityfloatEup-v6-J5Upper level energy Eup_v6_J5Kphys.energy;phys.atmol.leveldoublev4-J13Column density of v4_J13cm**-2phys.columnDensityfloatEup-v4-J13Upper level energy Eup_v4_J13Kphys.energy;phys.atmol.leveldoublev5-J10Column density of v5_J10cm**-2phys.columnDensityfloatEup-v5-J10Upper level energy Eup_v5_J10Kphys.energy;phys.atmol.leveldoublev3-J16Column density of v3_J16cm**-2phys.columnDensityfloatEup-v3-J16Upper level energy Eup_v3_J16Kphys.energy;phys.atmol.leveldoublev6-J6Column density of v6_J6cm**-2phys.columnDensityfloatEup-v6-J6Upper level energy Eup_v6_J6Kphys.energy;phys.atmol.leveldoublev0-J23Column density of v0_J23cm**-2phys.columnDensityfloatEup-v0-J23Upper level energy Eup_v0_J23Kphys.energy;phys.atmol.leveldoublev1-J21Column density of v1_J21cm**-2phys.columnDensityfloatEup-v1-J21Upper level energy Eup_v1_J21Kphys.energy;phys.atmol.leveldoublev6-J7Column density of v6_J7cm**-2phys.columnDensityfloatEup-v6-J7Upper level energy Eup_v6_J7Kphys.energy;phys.atmol.leveldoublev5-J11Column density of v5_J11cm**-2phys.columnDensityfloatEup-v5-J11Upper level energy Eup_v5_J11Kphys.energy;phys.atmol.leveldoublev4-J14Column density of v4_J14cm**-2phys.columnDensityfloatEup-v4-J14Upper level energy Eup_v4_J14Kphys.energy;phys.atmol.leveldoublev2-J19Column density of v2_J19cm**-2phys.columnDensityfloatEup-v2-J19Upper level energy Eup_v2_J19Kphys.energy;phys.atmol.leveldoublev7-J0Column density of v7_J0cm**-2phys.columnDensityfloatEup-v7-J0Upper level energy Eup_v7_J0Kphys.energy;phys.atmol.leveldoublev3-J17Column density of v3_J17cm**-2phys.columnDensityfloatEup-v3-J17Upper level energy Eup_v3_J17Kphys.energy;phys.atmol.leveldoublev6-J8Column density of v6_J8cm**-2phys.columnDensityfloatEup-v6-J8Upper level energy Eup_v6_J8Kphys.energy;phys.atmol.leveldoublev7-J1Column density of v7_J1cm**-2phys.columnDensityfloatEup-v7-J1Upper level energy Eup_v7_J1Kphys.energy;phys.atmol.leveldoublev7-J2Column density of v7_J2cm**-2phys.columnDensityfloatEup-v7-J2Upper level energy Eup_v7_J2Kphys.energy;phys.atmol.leveldoublev5-J12Column density of v5_J12cm**-2phys.columnDensityfloatEup-v5-J12Upper level energy Eup_v5_J12Kphys.energy;phys.atmol.leveldoublev7-J3Column density of v7_J3cm**-2phys.columnDensityfloatEup-v7-J3Upper level energy Eup_v7_J3Kphys.energy;phys.atmol.leveldoublev4-J15Column density of v4_J15cm**-2phys.columnDensityfloatEup-v4-J15Upper level energy Eup_v4_J15Kphys.energy;phys.atmol.leveldoublev6-J9Column density of v6_J9cm**-2phys.columnDensityfloatEup-v6-J9Upper level energy Eup_v6_J9Kphys.energy;phys.atmol.leveldoublev7-J4Column density of v7_J4cm**-2phys.columnDensityfloatEup-v7-J4Upper level energy Eup_v7_J4Kphys.energy;phys.atmol.leveldoublev1-J22Column density of v1_J22cm**-2phys.columnDensityfloatEup-v1-J22Upper level energy Eup_v1_J22Kphys.energy;phys.atmol.leveldoublev0-J24Column density of v0_J24cm**-2phys.columnDensityfloatEup-v0-J24Upper level energy Eup_v0_J24Kphys.energy;phys.atmol.leveldoublev2-J20Column density of v2_J20cm**-2phys.columnDensityfloatEup-v2-J20Upper level energy Eup_v2_J20Kphys.energy;phys.atmol.leveldoublev7-J5Column density of v7_J5cm**-2phys.columnDensityfloatEup-v7-J5Upper level energy Eup_v7_J5Kphys.energy;phys.atmol.leveldoublev3-J18Column density of v3_J18cm**-2phys.columnDensityfloatEup-v3-J18Upper level energy Eup_v3_J18Kphys.energy;phys.atmol.leveldoublev5-J13Column density of v5_J13cm**-2phys.columnDensityfloatEup-v5-J13Upper level energy Eup_v5_J13Kphys.energy;phys.atmol.leveldoublev6-J10Column density of v6_J10cm**-2phys.columnDensityfloatEup-v6-J10Upper level energy Eup_v6_J10Kphys.energy;phys.atmol.leveldoublev7-J6Column density of v7_J6cm**-2phys.columnDensityfloatEup-v7-J6Upper level energy Eup_v7_J6Kphys.energy;phys.atmol.leveldoublev4-J16Column density of v4_J16cm**-2phys.columnDensityfloatEup-v4-J16Upper level energy Eup_v4_J16Kphys.energy;phys.atmol.leveldoublev7-J7Column density of v7_J7cm**-2phys.columnDensityfloatEup-v7-J7Upper level energy Eup_v7_J7Kphys.energy;phys.atmol.leveldoublev6-J11Column density of v6_J11cm**-2phys.columnDensityfloatEup-v6-J11Upper level energy Eup_v6_J11Kphys.energy;phys.atmol.leveldoublev1-J23Column density of v1_J23cm**-2phys.columnDensityfloatEup-v1-J23Upper level energy Eup_v1_J23Kphys.energy;phys.atmol.leveldoublev5-J14Column density of v5_J14cm**-2phys.columnDensityfloatEup-v5-J14Upper level energy Eup_v5_J14Kphys.energy;phys.atmol.leveldoublev2-J21Column density of v2_J21cm**-2phys.columnDensityfloatEup-v2-J21Upper level energy Eup_v2_J21Kphys.energy;phys.atmol.leveldoublev0-J25Column density of v0_J25cm**-2phys.columnDensityfloatEup-v0-J25Upper level energy Eup_v0_J25Kphys.energy;phys.atmol.leveldoublev3-J19Column density of v3_J19cm**-2phys.columnDensityfloatEup-v3-J19Upper level energy Eup_v3_J19Kphys.energy;phys.atmol.leveldoublev8-J0Column density of v8_J0cm**-2phys.columnDensityfloatEup-v8-J0Upper level energy Eup_v8_J0Kphys.energy;phys.atmol.leveldoublev8-J1Column density of v8_J1cm**-2phys.columnDensityfloatEup-v8-J1Upper level energy Eup_v8_J1Kphys.energy;phys.atmol.leveldoublev7-J8Column density of v7_J8cm**-2phys.columnDensityfloatEup-v7-J8Upper level energy Eup_v7_J8Kphys.energy;phys.atmol.leveldoublev4-J17Column density of v4_J17cm**-2phys.columnDensityfloatEup-v4-J17Upper level energy Eup_v4_J17Kphys.energy;phys.atmol.leveldoublev8-J2Column density of v8_J2cm**-2phys.columnDensityfloatEup-v8-J2Upper level energy Eup_v8_J2Kphys.energy;phys.atmol.leveldoublev8-J3Column density of v8_J3cm**-2phys.columnDensityfloatEup-v8-J3Upper level energy Eup_v8_J3Kphys.energy;phys.atmol.leveldoubleAllDisplay data in all tablesmeta.ref.urlcharJ/A+A/675/A86/h2int*H2 intensities (table B4)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAllDisplay data in all tablesmeta.ref.urlcharnHPreshock densitycm**-3phys.densitydoubleVsShock velocitykm.s**-1phys.velocfloatbMagnetic field scaling factorarith.factorfloatG0Strength of UV fieldspect.line.widthfloatzetaCosmic-ray-ionization rates**-1phot.count;em.X-rayfloatXPAHPAH abundancephys.abundfloatTypeShock type (0J-1C-2Cs-3CJ)meta.notefloatJ/A+A/675/A86/h2widthWidths of H2-emitting regions (table B5)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAllDisplay data in all tablesmeta.ref.urlcharnHPreshock densitycm**-3phys.densitydoubleVsShock velocitykm/sphys.velocfloatbMagnetic field scaling factorarith.factorfloatG0Strength of UV fieldspect.line.widthfloatzetaCosmic-ray-ionization rates**-1phot.count;em.X-rayfloatXPAHPAH abundancephys.abundfloatTypeShock type (0J-1C-2Cs-3CJ)meta.notefloatv0-J3-v0-J1Width of v=0-0 S(1) emitting regionAUspect.line.widthdoublev1-J3-v0-J1Width of v=1-0 S(1) emitting regionAUspect.line.widthdoublev0-J11-v0-J9Width of v=0-0 S(9) emitting regionAUspect.line.widthdoublev1-J3-v0-J5Width of v=1-0 O(5) emitting regionAUspect.line.widthdoublev2-J3-v1-J1Width of v=2-1 S(1) emitting regionAUspect.line.widthdoubleJ/A+A/675/A86/h2oprH2 o/p ratios (table B6)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAllDisplay data in all tablesmeta.ref.urlcharnHPreshock densitycm**-3phys.densitydoubleVsShock velocitykm/sphys.velocfloatbMagnetic field scaling factorarith.factorfloatG0Strength of UV fieldspect.line.widthfloatzetaCosmic-ray-ionization rates**-1phot.count;em.X-rayfloatXPAHPAH abundancephys.abundfloatTypeShock type (0J-1C-2Cs-3CJ)meta.notefloatopr-initInitial o/p ratiospect.line.intensity;arith.ratiofloatopr-maxMaximum local o/p ratiospect.line.intensity;arith.ratiofloatopr-Ntoto/p ratio from N_o/N_pspect.line.intensity;arith.ratiofloatopr-Nroto/p ratio from N_o(rot)/N_p(rot)spect.line.intensity;arith.ratiofloatopr-Nvibo/p ratio from N_o(vib)/N_p(vib)spect.line.intensity;arith.ratiofloat