pn_spec_res_tablivo://fai.kz/pn_spec_res_table/q/mainFesenkov Astrophysical InstituteL.N. Kondratyeva, E.K. Denissyuk, S.A. Shomshekova, I.V. Reva, A.K. Aimanova, M.A. Krugov2025-09-17T07:31:44ZFAI NVO Team

Observatory 23, 050020 Almaty, Kazakhstan

vo@fai.kzemission-nebulaeplanetary-nebulaespectroscopyoptical-observation This resource provides a compiled dataset of Galactic planetary nebulae derived from absolute optical spectroscopy and supplemented by selected values from the literature. Based on these data, fundamental physical parameters were calculated, including sizes, densities, electron temperatures, and central star characteristics. The table includes: * Object identifiers, excitation classes, and interstellar extinction at Hβ. * Morphological and distance properties: angular diameters (Diam_arcsec), linear sizes (Diam_pc), and heliocentric distances (D_kpc). * Electron densities from [SII] 6717/6731 ratios. * Effective temperatures of central stars estimated both by the Zanstra method (T_HI) and empirical [OIII]-based calibrations (T0_[OIII], T1_[OIII]), given in units of 10**4 K. * Timescales: duration of available observations (delta_t_obs_year) and model reproduction intervals (delta_t_model_year), linked to evolutionary models by Bertolami (2016, A&A 588, A25). * Absolute emission-line fluxes for Hβ, HeII 4685, [OIII] 5007, Hα, [NII] 6583, HeI 6678, [SII] 6717/6731, HeI 7065, [ArIII] 7136, and [OI] 7324, with measurement uncertainties and (where relevant) a power-of-ten exponent. Each measurement is provided in a machine-readable format, separating values, uncertainties, and exponents into dedicated columns. This ensures precise numerical handling and interoperability with Virtual Observatory services and pipelines.2025Ap.....68...51Khttps://dachs.fai.kz/tableinfo/pn_spec_res_table.mainCatalogResearchFesenkov Astrophysical InstituteAZT-8Opticalpn_spec_res_table This resource provides a compiled dataset of Galactic planetary nebulae derived from absolute optical spectroscopy and supplemented by selected values from the literature. Based on these data, fundamental physical parameters were calculated, including sizes, densities, electron temperatures, and central star characteristics. The table includes: * Object identifiers, excitation classes, and interstellar extinction at Hβ. * Morphological and distance properties: angular diameters (Diam_arcsec), linear sizes (Diam_pc), and heliocentric distances (D_kpc). * Electron densities from [SII] 6717/6731 ratios. * Effective temperatures of central stars estimated both by the Zanstra method (T_HI) and empirical [OIII]-based calibrations (T0_[OIII], T1_[OIII]), given in units of 10**4 K. * Timescales: duration of available observations (delta_t_obs_year) and model reproduction intervals (delta_t_model_year), linked to evolutionary models by Bertolami (2016, A&A 588, A25). * Absolute emission-line fluxes for Hβ, HeII 4685, [OIII] 5007, Hα, [NII] 6583, HeI 6678, [SII] 6717/6731, HeI 7065, [ArIII] 7136, and [OI] 7324, with measurement uncertainties and (where relevant) a power-of-ten exponent. Each measurement is provided in a machine-readable format, separating values, uncertainties, and exponents into dedicated columns. This ensures precise numerical handling and interoperability with Virtual Observatory services and pipelines.pn_spec_res_table.main This resource provides a compiled dataset of Galactic planetary nebulae derived from absolute optical spectroscopy and supplemented by selected values from the literature. Based on these data, fundamental physical parameters were calculated, including sizes, densities, electron temperatures, and central star characteristics. The table includes: * Object identifiers, excitation classes, and interstellar extinction at Hβ. * Morphological and distance properties: angular diameters (Diam_arcsec), linear sizes (Diam_pc), and heliocentric distances (D_kpc). * Electron densities from [SII] 6717/6731 ratios. * Effective temperatures of central stars estimated both by the Zanstra method (T_HI) and empirical [OIII]-based calibrations (T0_[OIII], T1_[OIII]), given in units of 10**4 K. * Timescales: duration of available observations (delta_t_obs_year) and model reproduction intervals (delta_t_model_year), linked to evolutionary models by Bertolami (2016, A&A 588, A25). * Absolute emission-line fluxes for Hβ, HeII 4685, [OIII] 5007, Hα, [NII] 6583, HeI 6678, [SII] 6717/6731, HeI 7065, [ArIII] 7136, and [OI] 7324, with measurement uncertainties and (where relevant) a power-of-ten exponent. Each measurement is provided in a machine-readable format, separating values, uncertainties, and exponents into dedicated columns. This ensures precise numerical handling and interoperability with Virtual Observatory services and pipelines.objectPrimary identifier of the planetary nebula.meta.id;srccharnullablealt_nameAlternative name of the object.meta.id;srccharnullableexcitation_classExcitation class of the nebula, typically 'low' or 'high'.phys.atmol.ionStagecharnullableextinction_c_hbetaLogarithmic extinction at Hβ.phys.absorption.galdoublenullablediam_arcsecAngular diameter (2*radius) of the nebula in arcseconds. Zero means stellar like object.arcsecphys.angSize;stat.mindoublenullablediam_signQualifier for the physical radius: limit ('>', '<') or blank.meta.code.qualcharnullablediam_pcPhysical radius (2*radius) of the nebula in parsecs.pcphys.size.radiusdoublenullabledist_kpcDistance to the planetary nebula in kiloparsecs.kpcpos.distance;srcdoublenullablene_siiElectron density derived from the [SII] 6717/6731 line ratio.cm**-3phys.density.electrondoublenullablene_sii_errUncertainty in electron density from [SII] lines.cm**-3stat.error;phys.density.electrondoublenullablene_sii_powerPower of 10 to apply to Ne_[SII] value (i.e., Ne × 10^power).arith.factorintnullablet_hiEffective temperature of the central star derived using the Zanstra method (based on H I Balmer discontinuity).Kphys.temperature.effectivedoublenullablet_hi_errUncertainty in effective temperature T_HI.Kstat.error;phys.temperature.effectivedoublenullablet_hi_powerPower of 10 to apply to T_HI value.arith.factorintnullablet0_oiiiEffective temperature of the central star at the beginning of observations, derived using the empirical method based on [O III] lines.Kphys.temperature.effectivedoublenullablet0_oiii_errUncertainty in the effective temperature T0_[OIII].Kstat.error;phys.temperature.effectivedoublenullablet0_oiii_powerPower of 10 to apply to T0_[OIII] value.arith.factorintnullablet1_oiiiEffective temperature of the central star at the end of observations, derived using the empirical method based on [O III] lines.Kphys.temperature.effectivedoublenullablet1_oiii_errUncertainty in the effective temperature T1_[OIII].Kstat.error;phys.temperature.effectivedoublenullablet1_oiii_powerPower of 10 to apply to T1_[OIII] value.arith.factorintnullabledelta_t_obs_yearTime span in years between the first and last spectroscopic observations used in the analysis.yrtime.duration;obsdoublenullabledelta_t_model_yearTime interval in the photoionization model over which the observed variations are reproduced.yrtime.duration;modeldoublenullablemodel_numNumber of model from doi:10.1051/0004-6361/201526577.meta.code;modelintnullablemass_prog_starInitial mass of the progenitor star in solar masses according to the selected model.solMassphys.mass;stardoublenullableage_yearEstimated age of the planetary nebula.yrtime.agedoublenullableobs_yearYear of observation. If there is the second year, then the column means 'from' the yearyrtime.epochintnullableobs_year_2Ending year of observation (if applicable). It means 'to' the year.yrtime.epochintnullableobs_monthMonth of first observation (if known). If there is the second month, then the column means 'from' the monthtime.epochcharnullableobs_month_2Ending month of observation (if applicable). It means 'to' the monthtime.epochcharnullableobs_dayDay of observation (if known).time.epochcharnullablef_h_betaObserved H_beta flux in erg cm⁻² s⁻¹.erg cm**-2 s**-1phot.flux;em.line.Hbetadoublenullablef_h_beta_errUncertainty in the observed H_beta flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.Hbetadoublenullablef_h_beta_powerPower of 10 to apply to the Hβ flux (F × 10^power).arith.factorintnullableheii_4685Observed flux of the He II 4685 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.HeIIdoublenullableheii_4685_errUncertainty in the He II 4685 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.HeIIdoublenullableoiii_5007Observed flux of the [O III] 5007 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.OIIIdoublenullableoiii_5007_errUncertainty in the [O III] 5007 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.OIIIdoublenullableh_alpha_6563Observed flux of the Hα 6563 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.Halphadoublenullableh_alpha_6563_errUncertainty in the H_alpha 6563 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.Halphadoublenullablenii_6583Observed flux of the [N II] 6583 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.NIIdoublenullablenii_6583_errUncertainty in the [N II] 6583 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.NIIdoublenullablehei_6678Observed flux of the He I 6678 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.HeIdoublenullablehei_6678_errUncertainty in the He I 6678 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.HeIdoublenullablesii_6717Observed flux of the [S II] 6717 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.SIIdoublenullablesii_6717_errUncertainty in the [S II] 6717 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.SIIdoublenullablesii_6731Observed flux of the [S II] 6731 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.SIIdoublenullablesii_6731_errUncertainty in the [S II] 6731 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.SIIdoublenullablehei_7065Observed flux of the He I 7065 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.HeIdoublenullablehei_7065_errUncertainty in the He I 7065 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.HeIdoublenullableariii_7136Observed flux of the [Ar III] 7136 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.ArIIIdoublenullableariii_7136_errUncertainty in the [Ar III] 7136 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.ArIIIdoublenullableoi_7324Observed flux of the [O I] 7324 Angstrom line.erg cm**-2 s**-1phot.flux;em.line.OIdoublenullableoi_7324_errUncertainty in the [O I] 7324 Angstrom flux.erg cm**-2 s**-1stat.error;phot.flux;em.line.OIdoublenullablespec_refReference code for spectroscopic data source. Only provided for Hβ and related absolute line fluxes.meta.bib.bibcodecharnullable