tco_hot_supergiaivo://fai.kz/tco_hot_supergiants/q/dataFesenkov Astrophysical InstituteDanford, S.Miroshnichenko, A.2026-06-19T07:52:07ZFAI NVO Team

Observatory 23, 050020 Almaty, Kazakhstan

vo@fai.kzstellar-spectroscopysupergiant-starsechelle-spectroscopyhot-stars Spectral Archive of Hot Galactic Supergiants (TCO Node) This resource provides a digital archive of one-dimensional (1D) optical spectra of hot galactic supergiants, obtained at the Three College Observatory (TCO). The archive is integrated into the Kazakhstan National Virtual Observatory (KazVO) data services and optimized for the IVOA Simple Spectral Access Protocol (SSAP). **Data Specification:** * Data Type: Medium-resolution optical echelle spectra. * File Format: FITS (Flexible Image Transport System). * Data Representation: 1D merged (stitched) spectra. * Flux Calibration: Relative intensity, normalized to the continuum. **Observational Setup and Instrumentation:** * Observatory: Three College Observatory (TCO), North Carolina, USA * Telescope: 0.81-m Ritchey-Chretien telescope * Instrument: Fiber-fed echelle spectrograph eShel * Spectrograph Manufacturer: Shelyak Instruments **Spectral Characteristics:** * Spectral Range: Approximately 3900 - 7800 Angstroms (precise wavelength boundaries are frame-dependent and fixed within individual FITS headers). * Spectral Resolution: R approx 12,000. * Wavelength Calibration: Executed using a Thorium-Argon (ThAr) reference lamp spectrum. **Data Reduction Pipeline:** Primary and scientific data reduction was performed within the IRAF (Image Reduction and Analysis Facility) environment using standard echelle spectroscopy packages. **Key Reduction Steps:** 1. Pre-processing: Bias frame subtraction. 2. Extraction: Localization and extraction of individual echelle orders. 3. Dispersion Relation: Wavelength calibration based on ThAr reference frames. 4. Order Merging: Stitching of discrete spectral orders into a continuous 1D array. 5. Kinematic Correction: Application of the heliocentric velocity correction (documented under the VHELIO FITS header keyword). 6. Continuum Normalization: Continuum flattening achieved via high-order polynomial fitting.https://dachs.fai.kz/tableinfo/tco_hot_supergiants.dataArchiveResearchIsServedByFAI archives ObscoreThree College ObservatoryeShel spectrographOpticalivoaDefinition and support code for the ObsCore data model and table.ivoa.obscoreThis data collection is queryable in FAI archives's obscore table.tco_hot_supergiants Spectral Archive of Hot Galactic Supergiants (TCO Node) This resource provides a digital archive of one-dimensional (1D) optical spectra of hot galactic supergiants, obtained at the Three College Observatory (TCO). The archive is integrated into the Kazakhstan National Virtual Observatory (KazVO) data services and optimized for the IVOA Simple Spectral Access Protocol (SSAP). **Data Specification:** * Data Type: Medium-resolution optical echelle spectra. * File Format: FITS (Flexible Image Transport System). * Data Representation: 1D merged (stitched) spectra. * Flux Calibration: Relative intensity, normalized to the continuum. **Observational Setup and Instrumentation:** * Observatory: Three College Observatory (TCO), North Carolina, USA * Telescope: 0.81-m Ritchey-Chretien telescope * Instrument: Fiber-fed echelle spectrograph eShel * Spectrograph Manufacturer: Shelyak Instruments **Spectral Characteristics:** * Spectral Range: Approximately 3900 - 7800 Angstroms (precise wavelength boundaries are frame-dependent and fixed within individual FITS headers). * Spectral Resolution: R approx 12,000. * Wavelength Calibration: Executed using a Thorium-Argon (ThAr) reference lamp spectrum. **Data Reduction Pipeline:** Primary and scientific data reduction was performed within the IRAF (Image Reduction and Analysis Facility) environment using standard echelle spectroscopy packages. **Key Reduction Steps:** 1. Pre-processing: Bias frame subtraction. 2. Extraction: Localization and extraction of individual echelle orders. 3. Dispersion Relation: Wavelength calibration based on ThAr reference frames. 4. Order Merging: Stitching of discrete spectral orders into a continuous 1D array. 5. Kinematic Correction: Application of the heliocentric velocity correction (documented under the VHELIO FITS header keyword). 6. Continuum Normalization: Continuum flattening achieved via high-order polynomial fitting.tco_hot_supergiants.data Spectral Archive of Hot Galactic Supergiants (TCO Node) This resource provides a digital archive of one-dimensional (1D) optical spectra of hot galactic supergiants, obtained at the Three College Observatory (TCO). The archive is integrated into the Kazakhstan National Virtual Observatory (KazVO) data services and optimized for the IVOA Simple Spectral Access Protocol (SSAP). **Data Specification:** * Data Type: Medium-resolution optical echelle spectra. * File Format: FITS (Flexible Image Transport System). * Data Representation: 1D merged (stitched) spectra. * Flux Calibration: Relative intensity, normalized to the continuum. **Observational Setup and Instrumentation:** * Observatory: Three College Observatory (TCO), North Carolina, USA * Telescope: 0.81-m Ritchey-Chretien telescope * Instrument: Fiber-fed echelle spectrograph eShel * Spectrograph Manufacturer: Shelyak Instruments **Spectral Characteristics:** * Spectral Range: Approximately 3900 - 7800 Angstroms (precise wavelength boundaries are frame-dependent and fixed within individual FITS headers). * Spectral Resolution: R approx 12,000. * Wavelength Calibration: Executed using a Thorium-Argon (ThAr) reference lamp spectrum. **Data Reduction Pipeline:** Primary and scientific data reduction was performed within the IRAF (Image Reduction and Analysis Facility) environment using standard echelle spectroscopy packages. **Key Reduction Steps:** 1. Pre-processing: Bias frame subtraction. 2. Extraction: Localization and extraction of individual echelle orders. 3. Dispersion Relation: Wavelength calibration based on ThAr reference frames. 4. Order Merging: Stitching of discrete spectral orders into a continuous 1D array. 5. Kinematic Correction: Application of the heliocentric velocity correction (documented under the VHELIO FITS header keyword). 6. Continuum Normalization: Continuum flattening achieved via high-order polynomial fitting.accrefAccess key for the datameta.ref.url;meta.datasetssa:Access.ReferencecharindexednullableownerOwner of the datacharnullableembargoDate the data will become/became publicyrcharnullablemimeMIME type of the file servedmeta.code.mimessa:Access.FormatcharnullableaccsizeSize of the data in bytesbytessa:Access.Sizelongnullablessa_dstitleA compact and descriptive designation of the dataset.meta.title;meta.datasetssa:DataID.Titlecharssa_creatordidDataset identifier assigned by the creatormeta.idssa:DataID.CreatorDIDcharnullablessa_pubdidDataset identifier assigned by the publishermeta.ref.ivoidssa:Curation.PublisherDIDcharindexednullablessa_cdateProcessing/Creation datetime;meta.datasetssa:DataID.Datecharnullablessa_pdateDate last published.ssa:Curation.Datecharnullablessa_bandpassBandpass (i.e., rough spectral location) of this dataset; this should be the most appropriate term from the vocabulary http://www.ivoa.net/rdf/messenger.instr.bandpassssa:DataID.Bandpasscharnullablessa_cversionCreator assigned version for this dataset (will be incremented when this particular item is changed).meta.version;meta.datasetssa:DataID.Versioncharnullablessa_targnameCommon name of object observed.meta.id;srcssa:Target.Namecharssa_targclassObject class (star, QSO,...; use Simbad object classification http://simbad.u-strasbg.fr/simbad/sim-display?data=otypes if at all possible)src.classssa:Target.Classcharnullablessa_redshiftRedshift of target objectsrc.redshiftssa:Target.Redshiftfloatnullablessa_targetposEquatorial (ICRS) position of the target object.pos.eq;srcssa:Target.pos.spointdoublenullablessa_snrSignal-to-noise ratio estimated for this datasetstat.snrssa:Derived.SNRfloatnullablessa_locationICRS location of aperture centerdegpos.eqssa:Char.SpatialAxis.Coverage.Location.Valuedoubleindexednullablessa_apertureAngular diameter of aperturedegphys.angSize;instr.fovssa:Char.SpatialAxis.Coverage.Bounds.Extentfloatnullablessa_dateobsMidpoint of exposure (MJD)dtime.epochssa:Char.TimeAxis.Coverage.Location.Valuedoublenullablessa_timeextExposure durationstime.durationssa:Char.TimeAxis.Coverage.Bounds.Extentfloatnullablessa_specmidMidpoint of region covered in this datasetminstr.bandpassssa:Char.SpectralAxis.Coverage.Location.Valuefloatnullablessa_specextWidth of the spectrumminstr.bandwidthssa:Char.SpectralAxis.Coverage.Bounds.Extentfloatnullablessa_specstartLower value of spectral coordinatemem.wl;stat.minssa:Char.SpectralAxis.Coverage.Bounds.Startfloatnullablessa_specendUpper value of spectral coordinatemem.wl;stat.maxssa:Char.SpectralAxis.Coverage.Bounds.Stopfloatnullablessa_lengthNumber of points in the spectrumssa:Dataset.Lengthintnullablessa_modelData model name and versionssa:Dataset.DataModelcharssa_csysnameSystem RA and Dec are given inssa:CoordSys.SpaceFrame.Namecharssa_timesiTime conversion factor in Osuna-Salgado convention.ssa:Dataset.TimeSIcharnullablessa_spectralsiSpectral conversion factor in Osuna-Salgado conventionssa:Dataset.SpectralSIcharnullablessa_spectralucdUCD of the spectral column in the spectra served; when you have wavelengths, use em.wl for vacuum wavelengths, em.wl;obs.atmos for air wavelengths.meta.ucdssa:Char.SpectralAxis.Ucdcharssa_spectralunitUnit of the spectral columnmeta.unitssa:Char.SpectralAxis.Unitcharssa_fluxsiFlux/magnitude conversion factor in Osuna-Salgado conventionssa:Dataset.FluxSIcharnullablessa_fluxucdUCD of the flux columnmeta.ucdssa:Char.FluxAxis.Ucdcharssa_fluxunitUnit of the flux columnmeta.unitssa:Char.FluxAxis.Unitcharssa_dstypeType of data (spectrum, time series, etc)ssa:Dataset.Typecharnullablessa_publisherPublisher of the datasets included here.meta.curationssa:Curation.Publishercharssa_creatorCreator of the datasets included here.ssa:DataID.CreatorunicodeCharnullablessa_collectionA short handle naming the collection this spectrum belongs to.ssa:DataID.Collectioncharnullablessa_instrumentInstrument or code used to produce these datasetsmeta.id;instrssa:DataID.Instrumentcharnullablessa_datasourceMethod of generation for the data (one of survey, pointed, theory, custom, artificial).ssa:DataID.DataSourcecharnullablessa_creationtypeProcess used to produce the data (archival, cutout, filtered, mosaic, projection, spectralExtraction, or catalogExtraction)ssa:DataID.CreationTypecharnullablessa_referenceURL or bibcode of a publication describing this data.meta.bib.bibcodessa:Curation.Referencecharnullablessa_fluxstaterrorStatistical error in fluxstat.error;phot.flux.density;emssa:Char.FluxAxis.Accuracy.StatErrorfloatnullablessa_fluxsyserrorSystematic error in fluxstat.error.sys;phot.flux.density;emssa:Char.FluxAxis.Accuracy.SysErrorfloatnullablessa_fluxcalibType of flux calibration (ABSOLUTE, CALIBRATED, RELATIVE, NORMALIZED, or UNCALIBRATED).ssa:Char.FluxAxis.Calibrationcharnullablessa_binsizeBin size in wavelengthmem.wl;spect.binSizessa:Char.SpectralAxis.Accuracy.BinSizefloatnullablessa_spectstaterrorStatistical error in wavelengthmstat.error;emssa:Char.SpectralAxis.Accuracy.StatErrorfloatnullablessa_spectsyserrorSystematic error in wavelengthmstat.error.sys;emssa:Char.SpectralAxis.Accuracy.SysErrorfloatnullablessa_speccalibType of wavelength calibrationmeta.code.qualssa:Char.SpectralAxis.Calibrationcharnullablessa_specresResolution (in meters of wavelength) on the spectral axismspect.resolution;em.wlssa:Char.SpectralAxis.Resolutionfloatnullablessa_spaceerrorStatistical error in positiondegstat.error;pos.eqssa:Char.SpatialAxis.Accuracy.StatErrorfloatnullablessa_spacecalibType of calibration in spatial coordinatesmeta.code.qualssa:Char.SpatialAxis.Calibrationcharnullablessa_spaceresSpatial resolution of datadegpos.angResolutionssa:Char.SpatialAxis.Resolutionfloatnullablessa_regionRough coverage based on location and aperture.pos.outline;obs.fielddoubleindexednullabledatalinkA DataLink document for this spectrum, providing SODA access and the original file.meta.ref.urlcharnullablewave_minMinimum wavelength covered by the spectrum.mem.wl;stat.mindoublenullablewave_maxMaximum wavelength covered by the spectrum.mem.wl;stat.maxdoublenullablespecrpSpectral resolving power lambda/dlambda.spect.resolutionfloatnullablecalib_levelObsCore-style calibration level. Merged relative flux spectra are level 2.meta.code.qualshortorigfileOriginal FITS file name before KazVO metadata enrichment.meta.idcharnullablepuborgPublishing archive or organisation.meta.curationcharnullabledataorigOrigin of the data with respect to KazVO/FAI.meta.notecharnullableobserverObserver(s) listed in the FITS header.meta.id;obs.observercharnullabletelescopeTelescope used for the observation.instr.telcharnullableinstrumentInstrument or spectrograph used for the observation.instrcharnullablecameraCamera listed in the FITS header.meta.id;instr.detcharnullabledetnamDetector name listed in the FITS header.meta.id;instr.detcharnullablebunitFlux unit from the enriched FITS header.meta.unitcharnullablenormTrue if the merged spectrum is continuum-normalized.meta.codebooleanwavecalTrue if the spectrum is wavelength calibrated.meta.codebooleanfluxcalFlux calibration status from the enriched FITS header.meta.codecharnullablebiascorTrue if bias correction was applied.meta.codebooleandarkcorTrue if dark correction was applied.meta.codebooleanbpixcorTrue if bad-pixel map correction was applied.meta.codebooleanflatcorTrue if flat-field correction was applied.meta.codebooleancosmicrCosmic ray removal method.meta.codecharnullabletellcorTrue if telluric correction was applied.meta.codebooleanhelcorTrue if heliocentric correction was applied.meta.codeboolean