FAI NVO DC TAPivo://fai.kz/tapFesenkov Astrophysical InstituteFAI NVO Teamhttps://dachs.fai.kz/favicon.png2026-03-29T07:57:59ZFAI NVO Team

Observatory 23, 050020 Almaty, Kazakhstan

vo@fai.kzvirtual-observatoriescatalogsThe FAI archives's TAP end point. The Table Access Protocol (TAP) lets you execute queries against our database tables, inspect various metadata, and upload your own data. It is thus the VO's premier way to access public data holdings. Tables exposed through this endpoint include: main from the asteroids_obs_tab schema, main from the fai_agn schema, main from the gcvs_gaia_tess schema, main from the geomagnetic_field schema, main from the grb_photometry schema, obscore from the ivoa schema, main from the maksutov_50_telescope schema, main from the mesa_bin_6_4_002 schema, main from the neutrons schema, main from the pn_spec_res_table schema, main from the pulsars schema, alt_identifier, authorities, capability, g_num_stat, interface, intf_param, registries, relationship, res_date, res_detail, res_role, res_schema, res_subject, res_table, resource, stc_spatial, stc_spectral, stc_temporal, subject_uat, table_column, tap_table, validation from the rr schema, main from the schmidt_telescope_lc schema, main from the solar_flux schema, main from the specphot_stand_cat schema, data from the spectra_agn_archive schema, data from the spectra_pn_archive schema, columns, groups, key_columns, keys, schemas, tables from the tap_schema schema, main from the wr_wc_wo_sequence schema, main from the wr_wn_sequence schema.https://dachs.fai.kz/__system__/tap/run/infoIsServiceForFAI archives Obscore TableGAVO RegTAP Servicehttps://dachs.fai.kz/tapObscore-1.1Registry 1.2ADQL2.02.1The Astronomical Data Query Language is the standard IVOA dialect of SQL; it contains a very general SELECT statement as well as some extensions for spherical geometry and higher mathematics.

gavo_getauthority(ivoid TEXT) -> TEXT

returns the authority part of an ivoid (or, more generally a URI). So, ivo://org.gavo.dc/foo/bar#baz becomes org.gavo.dc. The behaviour for anything that's not a full URI is undefined.

gavo_ipix(long REAL, lat REAL) -> BIGINT

gavo_ipix returns the q3c ipix for a long/lat pair (it simply wraps the 13c_ang2ipix function). This is probably only relevant when you play tricks with indices or PPMXL ids.

gavo_match(pattern TEXT, string TEXT) -> INTEGER

gavo_match returns 1 if the POSIX regular expression pattern matches anything in string, 0 otherwise.

gavo_mocintersect(moc1 MOC, moc2 MOC) -> MOC

returns the intersection of two MOCs.

gavo_mocunion(moc1 MOC, moc2 MOC) -> MOC

returns the union of two MOCs.

gavo_specconv(expr DOUBLE PRECISION, dest_unit TEXT) -> DOUBLE PRECISION

returns the spectral value expr converted to dest_unit. expr has to be in either energy, wavelength, or frequency, and dest_unit must be a VOUnit giving another spectral unit (e.g., MHz, keV, nm, or Angstrom). This is intended to let users express spectral constraints in their preferred unit independently of the choice of unit in the database. Examples:: gavo_specconv(obscore.em_min, "keV") > 300 gavo_specconv(obscore.em_max, "MHz") > 30 gavo_specconv(spectral_start, "Angstrom") > 4000 There is a variant of gavo_specconv accepting expr's unit in a third argument.

gavo_specconv(expr NUMERIC, expr_unit TEXT, dest_unit TEXT) -> NUMERIC

returns expr assumed to be in expr_unit expressed in dest_unit. This is a variant of the two-argument gavo_specconv for when the unit of expr is not known to the ADQL translator, either because it because it is a literal or because it does not look like a spectral unit. Examples:: gavo_specconv(656, 'nm', 'J') BETWEEN spectral_start AND spectral_end gavo_specconv(arccos(phi)*incidence, 'Hz', 'eV') Clearly, overriding known units is likely to yield bad results; the translator therefore warns if an existing unit is overridden with a different unit.

gavo_vocmatch(vocname TEXT, term TEXT, matchagainst TEXT) -> INTEGER

returns 1 if matchagainst is term or narrower in the IVOA vocabulary vocname, 0 otherwise. This is intended for semantic querying. For instance, gavo_vocmatch('datalink/core', 'calibration', semantics) would be 1 if semantics is any of calibration, bias, dark, or flat. For RDF-flavoured vocabularies (strict trees), term will expand to the entire branch rooted in term. For SKOS-flavoured vocabularies (where narrower is not transitive), only directly narrower terms will be included. Both the term and the vocabulary name must be string literals (i.e., constants). matchagainst can be any string-valued expression.

ivo_geom_transform(from_sys TEXT, to_sys TEXT, geo GEOMETRY) -> GEOMETRY

The function transforms ADQL geometries between various reference systems. geo can be a POINT, a CIRCLE, or a POLYGON, and the function will return a geometry of the same type. In the current implementation, from_sys and to_sys must be literal strings (i.e., they cannot be computed through expressions or be taken from database columns). All transforms are just simple rotations, which is only a rough approximation to the actual relationships between reference systems (in particular between FK4 and ICRS-based ones). Note that, in particular, the epoch is not changed (i.e., no proper motions are applied). We currently support the following reference frames: ICRS, FK5 (which is treated as ICRS), FK4 (for B1950. without epoch-dependent corrections), GALACTIC. Reference frame names are case-sensitive.

ivo_hashlist_has(hashlist TEXT, item TEXT) -> INTEGER

The function takes two strings; the first is a list of words not containing the hash sign (#), concatenated by hash signs, the second is a word not containing the hash sign. It returns 1 if, compared case-insensitively, the second argument is in the list of words coded in the first argument. The behaviour in case the the second argument contains a hash sign is unspecified.

ivo_hasword(haystack TEXT, needle TEXT) -> INTEGER

gavo_hasword returns 1 if needle shows up in haystack, 0 otherwise. This is for "google-like"-searches in text-like fields. In word, you can actually employ a fairly complex query language; see https://www.postgresql.org/docs/current/textsearch.html for details.

ivo_healpix_center(hpxOrder INTEGER, hpxIndex BIGINT) -> POINT

returns a POINT corresponding to the center of the healpix with the given index at the given order.

ivo_healpix_index(order INTEGER, ra DOUBLE PRECISION, dec DOUBLE PRECISION) -> BIGINT

Returns the index of the (nest) healpix with order containing the spherical point (ra, dec). An alternative, 2-argument form ivo_healpix_index(order INTEGER, p POINT) -> BIGINT is also available.

ivo_histogram(val REAL, lower REAL, upper REAL, nbins INTEGER) -> INTEGER[]

The aggregate function returns a histogram of val with nbins+2 elements. Assuming 0-based arrays, result[0] contains the number of underflows (i.e., val<lower), result[nbins+1] the number of overflows. Elements 1..nbins are the counts in nbins bins of width (upper-lower)/nbins. Clients will have to convert back to physical units using some external communication, there currently is no (meta-) data as lower and upper in the TAP response.

ivo_interval_has(val NUMERIC, iv INTERVAL) -> INTEGER

The function returns 1 if the interval iv contains val, 0 otherwise. The lower limit is always included in iv, behaviour on the upper limit is column-specific.

ivo_interval_overlaps(l1 NUMERIC, h1 NUMERIC, l2 NUMERIC, h2 NUMERIC) -> INTEGER

The function returns 1 if the interval [l1...h1] overlaps with the interval [l2...h2]. For the purposes of this function, the case l1=h2 or l2=h1 is treated as overlap. The function returns 0 for non-overlapping intervals.

ivo_nocasematch(value TEXT, pattern TEXT) -> INTEGER

ivo_nocasematch returns 1 if pattern matches value, 0 otherwise. pattern is defined as for the SQL LIKE operator, but the match is performed case-insensitively. This function in effect provides a surrogate for the ILIKE SQL operator that is missing from ADQL. On this site, this is actually implemented using python's and SQL's LOWER, so for everything except ASCII, your mileage will vary.

ivo_normal_random(mu REAL, sigma REAL) -> REAL

The function returns a random number drawn from a normal distribution with mean mu and width sigma. Implementation note: Right now, the Gaussian is approximated by summing up and scaling ten calls to random. This, hence, is not very precise or fast. It might work for some use cases, and we will provide a better implementation if this proves inadequate.

ivo_simbadpoint(identifier TEXT) -> POINT

gavo_simbadpoint queries simbad for an identifier and returns the corresponding point. Note that identifier can only be a literal, i.e., as simple string rather than a column name. This is because our database cannot query simbad, and we probably wouldn't want to fire off millions of simbad queries anyway; use simbad's own TAP service for this kind of application.

ivo_string_agg(expression TEXT, delimiter TEXT) -> TEXT

An aggregate function returning all values of expression within a GROUP contcatenated with delimiter

ivo_to_jd(d TIMESTAMP) -> DOUBLE PRECISION

The function converts a postgres timestamp to julian date. This is naive; no corrections for timezones, let alone time scales or the like are done; you can thus not expect this to be good to second-precision unless you are careful in the construction of the timestamp.

ivo_to_mjd(d TIMESTAMP) -> DOUBLE PRECISION

The function converts a postgres timestamp to modified julian date. This is naive; no corrections for timezones, let alone time scales or the like are done; you can thus not expect this to be good to second-precision unless you are careful in the construction of the timestamp.

BOX

POINT

CIRCLE

POLYGON

REGION

CENTROID

COORD1

COORD2

DISTANCE

CONTAINS

INTERSECTS

AREA

COALESCE

LOWER

ILIKE

UPPER

OFFSET

CAST

IN_UNIT

WITH

TABLESAMPLE

Written after a table reference, TABLESAMPLE(10) will make the database only use 10% of the rows; these are `somewhat random' in that the system will use random blocks. This should be good enough when just testing queries (and much better than using TOP n).

MOC

A geometry function creating MOCs. It either takes a string argument with an ASCII MOC ('4/13 17-18 8/3002'), or an order and another geometry.

VECTORMATH

You can compute with vectors here. See https://wiki.ivoa.net/twiki/bin/view/IVOA/ADQLVectorMath for an overview of the functions and operators available.

CASE

The SQL92 CASE expression

UNION

EXCEPT

INTERSECT

text/tab-separated-valuestsvtext/plaintxttext/csvcsv_baretext/csv;header=presentcsvapplication/jsonjsonapplication/geo+jsongeojsonapplication/x-votable+xmlvotableapplication/x-votable+xml;serialization=BINARY2votable/b2votableb2application/x-votable+xml;serialization=TABLEDATAtext/xmlvotable/tdvotabletdapplication/x-votable+xml;serialization=TABLEDATA;version=1.1text/xmlvotabletd1.1application/x-votable+xml;version=1.1text/xmlvotable1.1application/x-votable+xml;serialization=TABLEDATA;version=1.2text/xmlvotabletd1.2application/x-votable+xml;serialization=TABLEDATA;version=1.6vodmlapplication/x-votable+xml;version=1.6vodmlbtext/htmlhtmlapplication/fitsfits172800602000020000000500000https://dachs.fai.kz/__system__/tap/run/capabilitieshttps://dachs.fai.kz/__system__/tap/run/availabilityhttps://dachs.fai.kz/__system__/tap/run/tableMetadataivoaDefinition and support code for the ObsCore data model and table.ivoa.obscoreThe IVOA-defined obscore table, containing generic metadata for datasets within this data centre.ivo://ivoa.net/std/obscore#table-1.13120dataproduct_typeHigh level scientific classification of the data product, taken from an enumerationmeta.code.classobscore:obsdataset.dataproducttypecharnullabledataproduct_subtypeData product specific typemeta.code.classobscore:obsdataset.dataproductsubtypecharnullablecalib_levelAmount of data processing that has been applied to the datameta.code;obs.calibobscore:obsdataset.caliblevelshortobs_collectionName of a data collection (e.g., project name) this data belongs tometa.idobscore:dataid.collectioncharnullableobs_idUnique identifier for an observationmeta.idobscore:DataID.observationIDcharnullableobs_titleFree-from title of the data setmeta.title;obsobscore:dataid.titlecharnullableobs_publisher_didDataset identifier assigned by the publisher.meta.ref.ivoidobscore:curation.publisherdidcharindexednullableobs_creator_didDataset identifier assigned by the creator.meta.idobscore:dataid.creatordidcharnullableaccess_urlThe URL at which to obtain the data set.meta.ref.urlobscore:access.referencecharnullableaccess_formatMIME type of the resource at access_urlmeta.code.mimeobscore:access.formatcharnullableaccess_estsizeEstimated size of data productkbytephys.size;meta.fileobscore:access.sizelongnullabletarget_nameObject a targeted observation targetedmeta.id;srcobscore:Target.Namecharnullabletarget_classClass of the target object (star, QSO, ...)src.classobscore:target.classcharnullables_raRA of (center of) observation, ICRSdegpos.eq.raobscore:char.spatialaxis.coverage.location.coord.position2d.value2.c1doubleindexednullables_decDec of (center of) observation, ICRSdegpos.eq.decobscore:char.spatialaxis.coverage.location.coord.position2d.value2.c2doubleindexednullables_fovApproximate spatial extent for the region covered by the observationdegphys.angSize;instr.fovobscore:char.spatialaxis.coverage.bounds.extent.diameterfloatnullables_regionRegion covered by the observation, as a polygonpos.outline;obs.fieldobscore:char.spatialaxis.coverage.support.areacharnullables_resolutionBest spatial resolution within the data setarcsecpos.angResolutionobscore:Char.SpatialAxis.Resolution.refval.valuefloatnullablet_minLower bound of times represented in the data setdtime.start;obs.exposureobscore:char.timeaxis.coverage.bounds.limits.starttimedoublenullablet_maxUpper bound of times represented in the data setdtime.end;obs.exposureobscore:char.timeaxis.coverage.bounds.limits.stoptimedoublenullablet_exptimeTotal exposure timestime.duration;obs.exposureobscore:char.timeaxis.coverage.support.extentfloatnullablet_resolutionMinimal significant time interval along the time axisstime.resolutionobscore:char.timeaxis.resolution.refval.valuefloatnullableem_minMinimal wavelength represented within the data setmem.wl;stat.minobscore:char.spectralaxis.coverage.bounds.limits.lolimitfloatnullableem_maxMaximal wavelength represented within the data setmem.wl;stat.maxobscore:char.spectralaxis.coverage.bounds.limits.hilimitfloatnullableem_res_powerSpectral resolving power lambda/delta lambdaspect.resolutionobscore:char.spectralaxis.resolution.resolpower.refvalfloatnullableo_ucdUCD for the product's observablemeta.ucdobscore:char.observableaxis.ucdcharnullablepol_statesList of polarization states in the data setmeta.code;phys.polarizationobscore:Char.PolarizationAxis.stateListcharnullablefacility_nameName of the facility at which data was takenmeta.id;instr.telobscore:Provenance.ObsConfig.facility.namecharnullableinstrument_nameName of the instrument that produced the datameta.id;instrobscore:Provenance.ObsConfig.instrument.namecharnullables_xel1Number of elements (typically pixels) along the first spatial axis.meta.numberobscore:Char.SpatialAxis.numBins1intnullables_xel2Number of elements (typically pixels) along the second spatial axis.meta.numberobscore:Char.SpatialAxis.numBins2intnullablet_xelNumber of elements (typically pixels) along the time axis.meta.numberobscore:Char.TimeAxis.numBinsintnullableem_xelNumber of elements (typically pixels) along the spectral axis.meta.numberobscore:Char.SpectralAxis.numBinsintnullablepol_xelNumber of elements (typically pixels) along the polarization axis.meta.numberobscore:Char.PolarizationAxis.numBinsintnullables_pixel_scaleSampling period in world coordinate units along the spatial axisarcsecphys.angSize;instr.pixelobscore:Char.SpatialAxis.Sampling.RefVal.SamplingPeriodfloatnullableem_ucdNature of the product's spectral axis (typically, em.freq, em.wl, or em.energy)meta.ucdobscore:Char.SpectralAxis.ucdcharnullablepreviewURL of a preview (low-resolution, quick-to-retrieve representation) of the data.meta.ref.url;meta.previewcharnullablesource_tableName of a TAP-queriable table this data originates from. This source table usually provides more information on the the data than what is given in obscore. See the TAP_SCHEMA of the originating TAP server for details.meta.id;meta.tablecharnullabletap_schema FAI archives's Table Access Protocol (TAP) service with table metadata.tap_schema.tablesTables available for ADQL querying.schema_nameFully qualified schema namecharnullabletable_nameFully qualified table namecharindexedprimarytable_typeOne of: table, viewcharnullabledescriptionBrief description of the tableunicodeCharnullableutypeutype if the table corresponds to a data modelcharnullabletable_indexSuggested position this table should take in a sorted list of tables from this data centerintnullablesourcerdId of the originating rd (local information)charnullablenrowsThe approximate size of the table in rowslongnullabletap_schema.schemasschema_nameschema_nametap_schema.columnsColumns in tables available for ADQL querying.table_nameFully qualified table namecharindexedprimarycolumn_nameColumn namecharindexedprimarydescriptionBrief description of columnunicodeCharnullableunitUnit in VO standard formatcharnullableucdUCD of column if anycharnullableutypeUtype of column if anycharnullabledatatypeADQL datatypecharnullablearraysizeArraysize in VOTable notationcharnullablextypeVOTable extended type information (for special interpretation of data content, e.g., timestamps or points)charnullable"size"Legacy length (ignore if you can).intnullableprincipalIs column principal?intindexedIs there an index on this column?intstdIs this a standard column?intsourcerdId of the originating rd (local information)charnullablecolumn_index1-based index of the column in database order.shortnullabletap_schema.tablestable_nametable_nametap_schema.schemasSchemas containing tables available for ADQL querying.schema_nameFully qualified schema namecharindexedprimarydescriptionBrief description of the schemaunicodeCharnullableutypeutype if schema corresponds to a data modelcharnullableschema_indexSuggested position this schema should take in a sorted list of schemas from this data center.intnullabletap_schema.keysForeign key relationships between tables available for ADQL querying.key_idUnique key identifiercharindexedprimaryfrom_tableFully qualified table namecharnullabletarget_tableFully qualified table namecharnullabledescriptionDescription of this keyunicodeCharnullableutypeUtype of this keycharnullablesourcerdId of the originating rd (local information)charnullabletap_schema.tablesfrom_tabletable_nametap_schema.tablestarget_tabletable_nametap_schema.key_columnsColumns participating in foreign key relationships between tables available for ADQL querying.key_idKey identifier from TAP_SCHEMA.keyscharnullablefrom_columnKey column name in the from tablecharnullabletarget_columnKey column in the target tablecharnullablesourcerdId of the originating rd (local information)charnullabletap_schema.keyskey_idkey_idtap_schema.groupsColumns that are part of groups within tables available for ADQL querying.table_nameFully qualified table namecharnullablecolumn_nameName of a column belonging to the groupcharnullablecolumn_utypeutype the column within the groupcharnullablegroup_nameName of the groupcharnullablegroup_utypeutype of the groupcharnullablesourcerdId of the originating rd (local information)charnullabletap_schema.tablestable_nametable_namerr Tables containing the information in the IVOA Registry. To query these tables, use `our TAP service`_. For more information and example queries, see the `RegTAP specification`_. .. _our TAP service: /__system__/tap/run/info .. _RegTAP specification: http://www.ivoa.net/documents/RegTAP/ivo://ivoa.net/std/regtap#1.2rr.resource The resources (like services, data collections, organizations) present in this registry.xpath:/ivoidUnambiguous reference to the resource conforming to the IVOA standard for identifiers.xpath:identifiercharindexedprimaryres_typeResource type (something like vg:authority, vs:catalogservice, etc).xpath:@xsi:typecharnullablecreatedThe UTC date and time this resource metadata description was created.xpath:@createdcharnullableshort_nameA short name or abbreviation given to something, for presentation in space-constrained fields (up to 16 characters).xpath:shortNamecharindexednullableres_titleThe full name given to the resource.xpath:titleunicodeCharindexednullableupdatedThe UTC date this resource metadata description was last updated.xpath:@updatedcharnullablecontent_levelA hash-separated list of content levels specifying the intended audience.xpath:content/contentLevelcharnullableres_descriptionAn account of the nature of the resource.xpath:content/descriptionunicodeCharindexednullablereference_urlURL pointing to a human-readable document describing this resource.xpath:content/referenceURLcharnullablecreator_seqThe creator(s) of the resource in the order given by the resource record author, separated by semicolons.xpath:curation/creator/nameunicodeCharindexednullablecontent_typeA hash-separated list of natures or genres of the content of the resource.xpath:content/typecharnullablesource_formatThe format of source_value. This, in particular, can be ``bibcode''.xpath:content/source/@formatcharnullablesource_valueA bibliographic reference from which the present resource is derived or extracted.xpath:content/sourceunicodeCharnullableres_versionLabel associated with creation or availablilty of a version of a resource.xpath:curation/versioncharnullableregion_of_regardA single numeric value representing the angle, given in decimal degrees, by which a positional query against this resource should be ``blurred'' in order to get an appropriate match.degxpath:coverage/regionOfRegardfloatnullablewavebandA hash-separated list of regions of the electro-magnetic spectrum that the resource's spectral coverage overlaps with.xpath:coverage/wavebandcharnullablerightsA statement of usage conditions (license, attribution, embargo, etc).xpath:/rightscharnullablerights_uriA URI identifying a license the data is made available under.xpath:/rights/@rightsURIcharnullableharvested_fromIVOID of the registry this record came from.charnullablerr.registriesharvested_fromivoidrr.capability Pieces of behaviour of a resource.xpath:/capability/ivoidThe parent resource.xpath:/identifiercharindexedprimarycap_indexAn arbitrary identifier of this capability within the resource.shortindexedprimarycap_typeThe type of capability covered here. If looking for endpoints implementing a certain standard, you should not use this column but rather match against standard_id.xpath:@xsi:typecharnullablecap_descriptionA human-readable description of what this capability provides as part of the over-all service.xpath:descriptionunicodeCharnullablestandard_idA URI for a standard this capability conforms to.xpath:@standardIDcharnullablerr.resourceivoidivoidrr.tap_table TAP-queriable tables.ivo://ivoa.net/std/regtap#1.2residIVOA identifier of the resource this table was taken from (where there is a dedicated resource containing this table in its tableset, that resource is preferred over a TAP service).charindexednullablesvcidIVOA identifier of the TAP service making this table queriable.charindexednullabletable_nameThe fully qualified name of the table. As per VODataService, this includes all catalog or schema prefixes needed to distinguish it in a query, and it comes with SQL delimiters where necessary.xpath:namecharindexednullabletable_titleA descriptive, human-interpretable name for the table.xpath:titleunicodeCharindexednullabletable_descriptionA free-text description of the table's contents.xpath:descriptionunicodeCharindexednullabletable_utypeAn identifier for a concept in a data model that the data in this table as a whole represent.xpath:utypecharnullablerr.stc_spatial The spatial coverage of resources. This table associates footprints (ADQL geometries) with ivoids. The footprints are intended for resource discovery; a reasonable expectation for the resolution thus is something like a degree.xpath:/coverage/spatialivoidThe parent resource.xpath:/identifiercharindexednullablecoverageA geometry representing the area a resource contains data for; this should be tight at least with a resolution of degrees.posxpath:.charnullableref_system_nameThe reference frame coverage is written in. This is currently reserved and fixed to NULL. Clients should always add a constraint to NULL for this to avoid matching non-celestial resources later.pos.framexpath:@framecharnullablerr.resourceivoidivoidrr.stc_temporal The temporal coverage of resources, given as one or more intervals. The total coverage is (a subset of) the union of all intervals given for a resource. All times are understood as MJD for TDB at the solar system barycenter.xpath:/coverage/temporalivoidThe parent resource.xpath:/identifiercharindexednullabletime_startLower limit of a time interval covered by the resource in MJD.dxpath:.floattime_endUpper limit of a time interval covered by the resource in MJD.dxpath:.floatrr.resourceivoidivoidrr.stc_spectral The spectral coverage of resources, given as one or more intervals. The total coverage is (a subset of) the union of all intervals given for a resource. The spectral values are given as messenger energy.xpath:/coverage/spectralivoidThe parent resource.xpath:/identifiercharindexednullablespectral_startLower limit (in Joules) of messenger energy interval covered by the resource (for the solar system barycenter).Jxpath:.floatspectral_endUpper limit (in Joules) of messenger energy interval covered by the resource (for the solar system barycenter).Jxpath:.floatrr.resourceivoidivoidrr.registries Administrative table: publishing registries we harvest, together with the dates of last full and incremental harvests.ivo://ivoa.net/std/regtap#1.2ivoidIVOID of the registry.charindexedprimaryaccessurlURL of the registry's OAI-PMH endpoint.charnullabletitleName of the registry.unicodeCharnullablelast_full_harvestDate and time of the last full harvest of the registry.charnullablelast_inc_harvestDate and time of the last incremental harvest of the registry.charnullablerr.authorities A mapping between the registries and the authorities they claim to manage.ivo://ivoa.net/std/regtap#1.2ivoidIVOID of the registry.charnullablemanaged_authorityAn authority this registry claims to serve.charindexedprimaryrr.registriesivoidivoidrr.res_role Entities (persons or organizations) operating on resources: creators, contacts, publishers, contributors.ivo://ivoa.net/std/regtap#1.2ivoidThe parent resource.xpath:/identifiercharindexednullablerole_nameThe real-world name or title of a person or organization.unicodeCharindexednullablerole_ivoidAn IVOA identifier of a person or organization.charnullablestreet_addressA mailing address for a person or organization.unicodeCharnullableemailAn email address the entity can be reached at.charnullabletelephoneA telephone number the entity can be reached at.charnullablelogoURL pointing to a graphical logo, which may be used to help identify the entity.charnullablebase_roleThe role played by this entity; this is one of contact, publisher, contributor, or creator.charindexednullablealt_identifierA non-IVOA identifier for the entity, for instance an ORCID or a ROR id. See the RegTAP document for the notations for the various identifier types.charindexednullablerr.resourceivoidivoidrr.res_subject Topics, object types, or other descriptive keywords about the resource.xpath:/content/ivoidThe parent resource.xpath:/identifiercharindexednullableres_subjectTopics, object types, or other descriptive keywords about the resource.xpath:subjectcharindexednullablerr.resourceivoidivoidrr.subject_uat res_subject mapped to the UAT. This is based on a manual mapping of keywords found in 2020, where subjects not mappable were dropped. This is a non-standard, local extension. Don't base your procedures on it, we will tear it down once there is sufficient takeup of the UAT in the VO.ivo://ivoa.net/std/regtap#1.2ivoidThe parent resource.xpath:/identifiercharindexednullableuat_conceptTerm from http://www.ivoa.net/rdf/uat; most of these resulted from mapping non-UAT designations.charindexednullablerr.resourceivoidivoidrr.res_schema Sets of tables related to resources.xpath:/tableset/schema/ivoidThe parent resource.xpath:/identifiercharindexedprimaryschema_indexAn arbitrary identifier for the res_schema rows belonging to a resource.shortindexedprimaryschema_descriptionA free text description of the tableset explaining in general how all of the tables are related.xpath:descriptionunicodeCharnullableschema_nameA name for the set of tables.xpath:name charnullableschema_titleA descriptive, human-interpretable name for the table set.xpath:titleunicodeCharnullableschema_utypeAn identifier for a concept in a data model that the data in this schema as a whole represent.xpath:utypecharnullablerr.resourceivoidivoidrr.res_table (Relational) tables that are part of schemata or resources.xpath:/(tableset/schema/|)table/ivoidThe parent resource.xpath:/identifiercharindexedprimaryschema_indexIndex of the schema this table belongs to, if it belongs to a schema (otherwise NULL).shortnullabletable_descriptionA free-text description of the table's contents.xpath:descriptionunicodeCharnullabletable_nameThe fully qualified name of the table. As per VODataService, this includes all catalog or schema prefixes needed to distinguish it in a query, and it comes with SQL delimiters where necessary.xpath:namecharnullabletable_indexAn arbitrary identifier for the tables belonging to a resource.shortindexedprimarytable_titleA descriptive, human-interpretable name for the table.xpath:titleunicodeCharnullabletable_typeA name for the role this table plays. Recognized values include "output", indicating this table is output from a query; "base_table", indicating a table whose records represent the main subjects of its schema; and "view", indicating that the table represents a useful combination or subset of other tables. Other values are allowed.xpath:@typecharnullabletable_utypeAn identifier for a concept in a data model that the data in this table as a whole represent.xpath:utypecharnullablenrowsAn estimate for the number of rows in the table.xpath:nrowslongnullablerr.resourceivoidivoidrr.table_column Metadata on columns of a resource's tables.xpath:/(tableset/schema/|)/table/column/ivoidThe parent resource.xpath:/identifiercharindexednullabletable_indexIndex of the table this column belongs to.shortnameThe name of the column.xpath:namecharindexednullableucdA unified content descriptor that describes the scientific content of the column.xpath:ucdcharindexednullableunitThe unit associated with all values in the column.xpath:unitcharnullableutypeAn identifier for a role in a data model that the data in this column represents.xpath:utypecharnullablestdIf 1, the meaning and use of this column is reserved and defined by a standard model. If 0, it represents a database-specific column that effectively extends beyond the standard.xpath:@stdshortnullabledatatypeThe type of the data contained in the column.xpath:dataTypecharnullableextended_schemaAn identifier for the schema that the value given by the extended attribute is drawn from.xpath:dataType/@extendedSchemacharnullableextended_typeA custom type for the values this column contains.xpath:dataType/@extendedTypecharnullablearraysizeThe shape of the array that constitutes the value, e.g., 4, *, 4*, 5x4, or 5x*, as specified by VOTable.xpath:dataType/@arraysizecharnullabledelimThe string that is used to delimit elements of an array value when arraysize is not '1'.xpath:dataType/@delimcharnullabletype_systemThe type system used, as a QName with a canonical prefix; this will ususally be one of vs:simpledatatype, vs:votabletype, and vs:taptype.xpath:dataType/@xsi:typecharnullableflagHash-separated keywords representing traits of the column. Recognized values include "indexed", "primary", and "nullable".xpath:flagcharnullablecolumn_descriptionA free-text description of the column's contents.xpath:descriptionunicodeCharindexednullablerr.res_tableivoidivoidtable_indextable_indexrr.g_num_stat An experimental table containing advanced statistics for numeric table columns. This is only available for very few tables at this point. Note that the values reported here may be estimates based on a subeset of the table rows.ivo://ivoa.net/std/regtap#1.2ivoidThe parent resource.xpath:/identifiercharnullabletable_indexIndex of the table this column belongs to.shortnameName of the column (see rr.table_column for more metadata).charindexednullablefill_factorAn estimate for the ratio of non-NULL values in this column to the number of rows in the table.floatnullablemin_valueThe largest value found in the column.floatnullablepercentile03An estimate for the value in the 3rd percentile of the column's distribution (for a Gaussian, roughly the lower limit of a 2σ interval).floatindexednullablemedianAn estimate for the median value (or 50th percentile) of the column's distributionfloatindexednullablepercentile97An estimate for the value in the 97th percentile of the column's distribution (for a Gaussian, roughly the upper limit of a 2σ interval).floatindexednullablemax_valueThe largest value found in the column.floatnullablerr.res_tableivoidivoidtable_indextable_indexrr.res_detail XPath-value pairs for members of resource or capability and their derivations that are less used and/or from VOResource extensions. The pairs refer to a resource if cap_index is NULL, to the referenced capability otherwise.ivo://ivoa.net/std/regtap#1.2ivoidThe parent resource.xpath:/identifiercharindexednullablecap_indexThe index of the parent capability; if NULL the xpath-value pair describes a member of the entire resource.shortnullabledetail_xpathThe xpath of the data item.charnullabledetail_value(Atomic) value of the member.unicodeCharnullablerr.resourceivoidivoidrr.interface Information on access modes of a capability.xpath:/capability/interface/ivoidThe parent resource.xpath:/identifiercharindexedprimarycap_indexThe index of the parent capability.shortindexedintf_indexAn arbitrary identifier for the interfaces of a resource.shortindexedprimaryintf_typeThe type of the interface (vr:webbrowser, vs:paramhttp, etc).xpath:@xsi:typecharnullableintf_roleAn identifier for the role the interface plays in the particular capability. If the value is equal to "std" or begins with "std:", then the interface refers to a standard interface defined by the standard referred to by the capability's standardID attribute.xpath:@rolecharnullablestd_versionThe version of a standard interface specification that this interface complies with. When the interface is provided in the context of a Capability element, then the standard being refered to is the one identified by the Capability's standardID element.xpath:@versioncharnullablequery_typeHash-joined list of expected HTTP method (get or post) supported by the service.xpath:queryTypecharnullableresult_typeThe MIME type of a document returned in the HTTP response.xpath:resultTypecharnullablewsdl_urlThe location of the WSDL that describes this Web Service. If NULL, the location can be assumed to be the accessURL with '?wsdl' appended.xpath:wsdlURLcharnullableurl_useA flag indicating whether this should be interpreted as a base URL ('base'), a full URL ('full'), or a URL to a directory that will produce a listing of files ('dir').xpath:accessURL/@usecharnullableaccess_urlThe URL at which the interface is found.xpath:accessURLcharnullablemirror_urlSecondary access URLs of this interface, separated by hash characters.xpath:mirrorURLcharnullableauthenticated_onlyA flag for whether an interface is available for anonymous use (=0) or only authenticated clients are served (=1).shortsecurity_method_idThis column was mentioned in drafts of RegTAP 1.1 but was abandoned before RegTAP 1.1 REC. Do not use any more. This is just here to avoid a flag day for clients that experimentally used this column. This is always NULL here.not mappedcharnullablerr.capabilityivoidivoidcap_indexcap_indexrr.relationship Relationships between resources (like mirroring, derivation, serving a data collection).xpath:/content/relationship/ivoidThe parent resource.xpath:/identifiercharindexednullablerelationship_typeThe type of the relationship; these terms are drawn from a controlled vocabulary and are DataCite-compatible.xpath:relationshipTypecharnullablerelated_idThe IVOA identifier for the resource referred to.xpath:relatedResource/@ivo-idcharnullablerelated_nameThe name of resource that this resource is related to.xpath:relatedResourcecharnullablerelated_alt_identifierA non-IVOA identifier for the related resource. This will typically be a DOI in URI form ('doi:10...')xpath:relatedResource/@altIdentifiercharnullablerr.resourceivoidivoidrr.intf_param Input parameters for services.xpath:/capability/interface/param/ivoidThe parent resource.xpath:/identifiercharindexednullableintf_indexThe index of the interface this parameter belongs to.shortnameThe name of the parameter.xpath:namecharnullableucdA unified content descriptor that describes the scientific content of the parameter.xpath:ucdcharnullableunitThe unit associated with all values in the parameter.xpath:unitcharnullableutypeAn identifier for a role in a data model that the data in this parameter represents.xpath:utypecharnullablestdIf 1, the meaning and use of this parameter is reserved and defined by a standard model. If 0, it represents a database-specific parameter that effectively extends beyond the standard.xpath:@stdshortnullabledatatypeThe type of the data contained in the parameter.xpath:dataTypecharnullableextended_schemaAn identifier for the schema that the value given by the extended attribute is drawn from.xpath:dataType/@extendedSchemacharnullableextended_typeA custom type for the values this parameter contains.xpath:dataType/@extendedTypecharnullablearraysizeThe shape of the array that constitutes the value, e.g., 4, *, 4*, 5x4, or 5x*, as specified by VOTable.xpath:dataType/@arraysizecharnullabledelimThe string that is used to delimit elements of an array value when arraysize is not '1'.xpath:dataType/@delimcharnullableparam_useAn indication of whether this parameter is required to be provided for the application or service to work properly (one of required, optional, ignored, or NULL).xpath:@usecharnullableparam_descriptionA free-text description of the parameter's contents.xpath:descriptionunicodeCharnullablerr.interfaceivoidivoidintf_indexintf_indexrr.validationValidation levels for resources and capabilities.xpath:/(capability/|)validationLevelivoidThe parent resource.xpath:/identifiercharindexednullablevalidated_byThe IVOA ID of the registry or organisation that assigned the validation level.xpath:validationLevel/@validatedBycharnullableval_levelA numeric grade describing the quality of the resource description, when applicable, to be used to indicate the confidence an end-user can put in the resource as part of a VO application or research study.xpath:validationLevelshortnullablecap_indexIf non-NULL, the validation only refers to the capability referenced here.shortnullablerr.resourceivoidivoidrr.resourceivoidivoidrr.res_date A date associated with an event in the life cycle of the resource. This could be creation or update. The role column can be used to clarify.xpath:/curation/ivoidThe parent resource.xpath:/identifiercharindexednullabledate_valueA date associated with an event in the life cycle of the resource.xpath:datecharnullablevalue_roleA string indicating what the date refers to, e.g., created, availability, updated. This value is generally drawn from a controlled vocabulary.xpath:date/@rolecharnullablerr.resourceivoidivoidrr.alt_identifier An alternate identifier associated with this record. This can be a resiource identifier like a DOI (in URI form, e.g., doi:10.1016/j.epsl.2011.11.037).xpath:/(curation/creator/|)altIdentifierivoidThe parent resource.xpath:/identifiercharindexednullablealt_identifierAn identifier for the resource or an entity related to the resource in URI form.charindexednullablerr.resourceivoidivoidasteroids_obs_tab This table is a preview catalog of asteroid observations carried out by the Fesenkov Astrophysical Institute (FAI) as part of our ongoing contribution to planetary defense and space situational awareness. The observations are regularly reported to the Minor Planet Center (https://minorplanetcenter.net/). The dataset includes the following fields: - **obs_date**: Date of observation (format: yyyy-mm-dd). - **target**: Asteroid designation from MPC. - **bin**: CCD binning mode (N×N pixels). - **filter**: Photometric filter used (CL means clear). - **exptime**: Exposure time in seconds. - **nframes**: Number of CCD frames obtained. - **reference**: Link to MPC circular or MPS telegram. - **page**: Page number referencing N42 telescope observations. - **notes**: Additional remarks. This is an overview table. For more details about our space situational awareness activities, please visit our SSA portal: https://ssa.fai.kz/. For questions or data reuse requests, please contact us at vo[at]fai.kz.asteroids_obs_tab.main This table is a preview catalog of asteroid observations carried out by the Fesenkov Astrophysical Institute (FAI) as part of our ongoing contribution to planetary defense and space situational awareness. The observations are regularly reported to the Minor Planet Center (https://minorplanetcenter.net/). The dataset includes the following fields: - **obs_date**: Date of observation (format: yyyy-mm-dd). - **target**: Asteroid designation from MPC. - **bin**: CCD binning mode (N×N pixels). - **filter**: Photometric filter used (CL means clear). - **exptime**: Exposure time in seconds. - **nframes**: Number of CCD frames obtained. - **reference**: Link to MPC circular or MPS telegram. - **page**: Page number referencing N42 telescope observations. - **notes**: Additional remarks. This is an overview table. For more details about our space situational awareness activities, please visit our SSA portal: https://ssa.fai.kz/. For questions or data reuse requests, please contact us at vo[at]fai.kz.obs_dateObservation date (ISO format DD-MM-YYYY)time.date;obschartargetAsteroid designation or provisional IDmeta.id;srccharbinDetector binninginstr.detector.binintfilterFilter used during observationinstr.filtercharexptimeExposure time in secondsstime.duration;obs.exposureintnframesNumber of frames per objectmeta.number;obsintreferenceURL to Minor Planet Center report PDFmeta.ref.urlcharnullablepagePage number in MPC PDFcharnullablenotesAdditional commentscharnullablefai_agn The database of Active Galactic Nuclea (AGN) photometrical observations obtained on defferent telescopes at Fesenkov Astrophysical Institute, Almaty, Kazakhstan since 2016. Observations were carried out in the optical range.fai_agn.main The database of Active Galactic Nuclea (AGN) photometrical observations obtained on defferent telescopes at Fesenkov Astrophysical Institute, Almaty, Kazakhstan since 2016. Observations were carried out in the optical range.accrefAccess key for the datameta.ref.urlAccess.ReferencecharindexednullableownerOwner of the datacharnullableembargoDate the data will become/became publicyrcharnullablemimeMIME type of the file servedmeta.code.mimeAccess.FormatcharnullableaccsizeSize of the data in bytesbyteVOX:Image_FileSizeAccess.SizelongnullablecenteralphaApproximate center of image, RAdegpos.eq.radoubleindexednullablecenterdeltaApproximate center of image, Decdegpos.eq.decdoubleindexednullableimagetitleSynthetic name of the imagemeta.titlecharnullableinstidIdentifier of the originating instrumentmeta.id;instrcharnullabledateobsEpoch at midpoint of observationdtime;obs.exposuredoublenullablenaxesNumber of axes in datapos.wcs.naxesintnullablepixelsizeNumber of pixels along each of the axespixelpos.wcs.naxisintnullablepixelscaleThe pixel scale on each image axisdeg/pixelpos.wcs.scalefloatnullablerefframeCoordinate system reference framepos.framecharnullablewcs_equinoxEquinox of the given coordinatesyrtime.equinoxfloatnullablewcs_projectionFITS WCS projection typepos.wcs.ctypecharnullablewcs_refpixelWCS reference pixelpixelpos.wcs.crpixfloatnullablewcs_refvaluesWorld coordinates at WCS reference pixeldegpos.wcs.crvaldoublenullablewcs_cdmatrixFITS WCS CDij matrixdeg/pixelpos.wcs.cdmatrixfloatnullablebandpassidFree-form name of the bandpass usedinstr.bandpasscharnullablebandpassunitUnit of bandpass specifications (always m).charnullablebandpassrefvalCharacteristic quantity for the bandpass of the imageminstr.bandpass;stat.medianfloatnullablebandpasshiUpper limit of the bandpass (in BandPass_Unit units)minstr.bandpass;stat.maxfloatnullablebandpassloLower limit of the bandpass (in BandPass_Unit units)minstr.bandpass;stat.minfloatnullablepixflagsFlags specifying the processing done (C-original; F-resampled; Z-fluxes valid; X-not resampled; V-for display onlymeta.codecharnullablecoverageField covered by the imagedegdoubleindexednullableobjectObject namemeta.id;srccharnullabletarget_raRight ascension of an object.degpos.eq.ra;meta.mainfloatnullabletarget_decDeclination of an object.degpos.eq.dec;meta.mainfloatnullableexptimeExposure time.stime.duration;obs.exposurefloatnullabletelescopeTelescope.instr.telcharnullableobservatObservatory where data was obtained.meta.id;instr.obstycharnullablereadoutmReadout mode of imagemeta.notecharnullablebinBinning factormeta.number;instr.pixelintairmassRelative optical path length through atmosphereobs.airMassfloatnullablepub_didpublisherDID of this datasetmeta.ref.ivoidcharnullablegcvs_gaia_tess This catalog combines photometric and astrometric data from three major sources: the General Catalogue of Variable Stars (GCVS, 2017ARep...61...80S), Gaia DR3, and TESS. It provides detailed information on variable stars, including their coordinates, magnitudes, variability periods, parallaxes, proper motions, spectral classifications, and other physical characteristics. Additionally, the catalog includes computed parameters such as galactocentric distances and model-predicted values for spectral types and variability types for stars with incomplete observational data. The catalog aims to facilitate studies of stellar variability, galactic structure, and stellar evolution.gcvs_gaia_tess.main This catalog combines photometric and astrometric data from three major sources: the General Catalogue of Variable Stars (GCVS, 2017ARep...61...80S), Gaia DR3, and TESS. It provides detailed information on variable stars, including their coordinates, magnitudes, variability periods, parallaxes, proper motions, spectral classifications, and other physical characteristics. Additionally, the catalog includes computed parameters such as galactocentric distances and model-predicted values for spectral types and variability types for stars with incomplete observational data. The catalog aims to facilitate studies of stellar variability, galactic structure, and stellar evolution.name_gcvsStar name in the General Catalogue of Variable Stars (GCVS)meta.idcharnullablera_gcvsRight Ascension (J2000) from GCVSdegpos.eq.ra;meta.maindoubleindexednullabledec_gcvsDeclination (J2000) from GCVSdegpos.eq.dec;meta.maindoubleindexednullablemin_mag_gcvsMinimum recorded magnitude (GCVS)magphot.mag;stat.mindoublenullablemax_mag_gcvsMaximum recorded magnitude (GCVS)magphot.mag;stat.maxdoublenullableperiod_gcvsVariability period (days) from GCVSdtime.perioddoublenullablevar_star_num_gcvsVariable star number assigned in GCVSmeta.idintnullablevar_star_cpt_gcvsComponent of a variable star system in GCVSmeta.idcharnullablesource_id_gaiaUnique Gaia DR3 source identifiermeta.id;meta.mainlongnullableparallax_gaiaStellar parallax in milliarcseconds (Gaia DR3)maspos.parallaxdoublenullablepmra_gaiaProper motion in Right Ascension (mas/yr, Gaia DR3)mas/yrpos.pm;pos.eq.radoublenullablepmdec_gaiaProper motion in Declination (mas/yr, Gaia DR3)mas/yrpos.pm;pos.eq.decdoublenullablephot_g_mag_gaiaMean magnitude in Gaia G-bandmagphot.mag;em.optdoublenullabletess_idTESS Input Catalog identifiermeta.idlongnullableteff_tessEffective temperature (Kelvin) from TESSKphys.temperature.effectivedoublenullablelogg_tessSurface gravity (log g) from TESScm/s2phys.gravitydoublenullablemass_tessStellar mass in solar masses (TESS)solMassphys.massdoublenullabled_tessDistance to the star in parsecs (TESS)pcpos.distancedoublenullabler_gal_calcGalactocentric distance of the star (calculated)kpcpos.distance.galacticdoublenullablespt_sourceSource of spectral type (GCVS, Gaia, or machine learning prediction)meta.codecharnullablefinal_spect_typeFinal assigned spectral type (observed or predicted)src.spTypecharnullablevar_sourceSource of variability type (GCVS, Gaia, or machine learning prediction)meta.codecharnullablefinal_var_typeFinal assigned variability type (observed or predicted)src.varTypecharnullablegeomagnetic_field The Alma-Ata Geomagnetic Observatory provides continuous monitoring of Earth's geomagnetic field. Located at 1300 meters above sea level in the foothills of the Tien Shan Mountains, approximately 10 km from Almaty, Kazakhstan, the observatory operates state-of-the-art equipment certified by INTERMAGNET, including the fluxgate magnetometer LEMI-008 and the proton Overhauser magnetometer POS-1. The data service includes: * **Observables**: Three components of the geomagnetic field vector (X, Y, Z) and the total field amplitude (F), measured in nanoteslas (nT). * **Data Resolution**: - XYZ components measured at a 1-second frequency. - F component measured at a 5-second frequency. - Derived minute averages for XYZF components available in real time. - Absolute measurements performed two to three times per week. The service provides open access to minute- and hour-resolution data (XYZF components and the geomagnetic K-index) from 2003 onward via the Institute of Ionosphere’s website (https://ionos.kz/). Minute-resolution variation data since 2004 are also available through the INTERMAGNET network. Data prior to 2003 are available upon request. The dataset is maintained by the Institute of Ionosphere and is additionally accessible through the Kazakhstan Space Weather Portal (https://ssa.fai.kz/, registration required), which also offers interactive plots and visualizations.geomagnetic_field.main The Alma-Ata Geomagnetic Observatory provides continuous monitoring of Earth's geomagnetic field. Located at 1300 meters above sea level in the foothills of the Tien Shan Mountains, approximately 10 km from Almaty, Kazakhstan, the observatory operates state-of-the-art equipment certified by INTERMAGNET, including the fluxgate magnetometer LEMI-008 and the proton Overhauser magnetometer POS-1. The data service includes: * **Observables**: Three components of the geomagnetic field vector (X, Y, Z) and the total field amplitude (F), measured in nanoteslas (nT). * **Data Resolution**: - XYZ components measured at a 1-second frequency. - F component measured at a 5-second frequency. - Derived minute averages for XYZF components available in real time. - Absolute measurements performed two to three times per week. The service provides open access to minute- and hour-resolution data (XYZF components and the geomagnetic K-index) from 2003 onward via the Institute of Ionosphere’s website (https://ionos.kz/). Minute-resolution variation data since 2004 are also available through the INTERMAGNET network. Data prior to 2003 are available upon request. The dataset is maintained by the Institute of Ionosphere and is additionally accessible through the Kazakhstan Space Weather Portal (https://ssa.fai.kz/, registration required), which also offers interactive plots and visualizations.1600000obs_timeTime of observation in UTC (yyyy-mm-ddThh:mm:ssZ).time.epochcharindexednullableobs_mjdTime of the observation at the detector as MJD.dtime.epochdoublenullableb_xMagnetic field component in the X direction.nTphys.magField;pos.cartesian.xdoublenullableb_yMagnetic field component in the Y direction.nTphys.magField;pos.cartesian.ydoublenullableb_zMagnetic field component in the Z direction.nTphys.magField;pos.cartesian.zdoublenullableb_totalTotal magnetic field strength.nTphys.magFielddoubleindexednullablesource_pathFile this row was parsed from.meta.id;meta.filecharindexednullablegrb_photometry The database of Gamma Ray Burst (GRB) photometrical observations obtained on defferent telescopes at Fesenkov Astrophysical Institute, Almaty, Kazakhstan. Observations were carried out in the optical range.grb_photometry.main The database of Gamma Ray Burst (GRB) photometrical observations obtained on defferent telescopes at Fesenkov Astrophysical Institute, Almaty, Kazakhstan. Observations were carried out in the optical range.accrefAccess key for the datameta.ref.urlAccess.ReferencecharindexednullableownerOwner of the datacharnullableembargoDate the data will become/became publicyrcharnullablemimeMIME type of the file servedmeta.code.mimeAccess.FormatcharnullableaccsizeSize of the data in bytesbyteVOX:Image_FileSizeAccess.SizelongnullablecenteralphaApproximate center of image, RAdegpos.eq.radoubleindexednullablecenterdeltaApproximate center of image, Decdegpos.eq.decdoubleindexednullableimagetitleSynthetic name of the imagemeta.titlecharnullableinstidIdentifier of the originating instrumentmeta.id;instrcharnullabledateobsEpoch at midpoint of observationdtime;obs.exposuredoublenullablenaxesNumber of axes in datapos.wcs.naxesintnullablepixelsizeNumber of pixels along each of the axespixelpos.wcs.naxisintnullablepixelscaleThe pixel scale on each image axisdeg/pixelpos.wcs.scalefloatnullablerefframeCoordinate system reference framepos.framecharnullablewcs_equinoxEquinox of the given coordinatesyrtime.equinoxfloatnullablewcs_projectionFITS WCS projection typepos.wcs.ctypecharnullablewcs_refpixelWCS reference pixelpixelpos.wcs.crpixfloatnullablewcs_refvaluesWorld coordinates at WCS reference pixeldegpos.wcs.crvaldoublenullablewcs_cdmatrixFITS WCS CDij matrixdeg/pixelpos.wcs.cdmatrixfloatnullablebandpassidFree-form name of the bandpass usedinstr.bandpasscharnullablebandpassunitUnit of bandpass specifications (always m).charnullablebandpassrefvalCharacteristic quantity for the bandpass of the imageminstr.bandpass;stat.medianfloatnullablebandpasshiUpper limit of the bandpass (in BandPass_Unit units)minstr.bandpass;stat.maxfloatnullablebandpassloLower limit of the bandpass (in BandPass_Unit units)minstr.bandpass;stat.minfloatnullablepixflagsFlags specifying the processing done (C-original; F-resampled; Z-fluxes valid; X-not resampled; V-for display onlymeta.codecharnullablecoverageField covered by the imagedegdoubleindexednullableobjectObject namemeta.id;srccharnullabletarget_raRight ascension of an object.degpos.eq.ra;meta.mainfloatnullabletarget_decDeclination of an object.degpos.eq.dec;meta.mainfloatnullableexptimeExposure time.stime.duration;obs.exposurefloatnullabletelescopeTelescope.instr.telcharnullableobservatObservatory where data was obtained.instr.telcharnullablereadoutmReadout mode of imagemeta.notecharnullablebinBinning factormeta.number;instr.pixelintairmassRelative optical path length through atmosphereobs.airMassfloatnullablepub_didpublisherDID of this datasetmeta.ref.ivoidcharnullablemaksutov_50_telescope The archive of digitized plates obtained on Wide aperture Maksutov meniscus telescope with main mirror 50 cm at the Fesenkov Astrophysical Institute (FAI), Almaty, Kazakhstan. They represent the results of photometric observations of stars, comets, nebulae etc. for 50 years - from 1950 to 2000. Observations were carried out in the optical range. Telescope specifications: diameter of main mirror D = 500 mm, focal length F = 1200 mm.maksutov_50_telescope.main The archive of digitized plates obtained on Wide aperture Maksutov meniscus telescope with main mirror 50 cm at the Fesenkov Astrophysical Institute (FAI), Almaty, Kazakhstan. They represent the results of photometric observations of stars, comets, nebulae etc. for 50 years - from 1950 to 2000. Observations were carried out in the optical range. Telescope specifications: diameter of main mirror D = 500 mm, focal length F = 1200 mm.1715accrefAccess key for the datameta.ref.urlAccess.ReferencecharindexednullableownerOwner of the datacharnullableembargoDate the data will become/became publicyrcharnullablemimeMIME type of the file servedmeta.code.mimeAccess.FormatcharnullableaccsizeSize of the data in bytesbyteVOX:Image_FileSizeAccess.SizelongnullablecenteralphaApproximate center of image, RAdegpos.eq.radoubleindexednullablecenterdeltaApproximate center of image, Decdegpos.eq.decdoubleindexednullableimagetitleSynthetic name of the imagemeta.titlecharnullableinstidIdentifier of the originating instrumentmeta.id;instrcharnullabledateobsThe date of observation from observational log. (Y-M-D .. Y-M-D)dtime;obs.exposuredoublenullablenaxesNumber of axes in datapos.wcs.naxesintnullablepixelsizeNumber of pixels along each of the axespixelpos.wcs.naxisintnullablepixelscaleThe pixel scale on each image axisdeg/pixelpos.wcs.scalefloatnullablerefframeCoordinate system reference framepos.framecharnullablewcs_equinoxEquinox of the given coordinatesyrtime.equinoxfloatnullablewcs_projectionFITS WCS projection typepos.wcs.ctypecharnullablewcs_refpixelWCS reference pixelpixelpos.wcs.crpixfloatnullablewcs_refvaluesWorld coordinates at WCS reference pixeldegpos.wcs.crvaldoublenullablewcs_cdmatrixFITS WCS CDij matrixdeg/pixelpos.wcs.cdmatrixfloatnullablebandpassidFree-form name of the bandpass usedinstr.bandpasscharnullablebandpassunitUnit of bandpass specifications (always m).charnullablebandpassrefvalCharacteristic quantity for the bandpass of the imageminstr.bandpass;stat.medianfloatnullablebandpasshiUpper limit of the bandpass (in BandPass_Unit units)minstr.bandpass;stat.maxfloatnullablebandpassloLower limit of the bandpass (in BandPass_Unit units)minstr.bandpass;stat.minfloatnullablepixflagsFlags specifying the processing done (C-original; F-resampled; Z-fluxes valid; X-not resampled; V-for display onlymeta.codecharnullablecoverageField covered by the imagedegdoubleindexednullableobjectName of object from the observation log.meta.id;srccharnullablefilenameName of .fit file (object_date_exp_id.fit).meta.id;srccharnullabletarget_raRight ascension of object from observation log.degpos.eq.ra;meta.mainfloatnullabletarget_decDeclination of object from observation log.degpos.eq.dec;meta.mainfloatnullableexptimeExposure time from observation log.stime.duration;obs.exposurefloatnullabletelescopeTelescope from observation log.instr.telcharnullablemesa_bin_6_4_002 Grid of Close-Binary Evolution Models This dataset contains a grid of close-binary evolution models computed with the **MESA** (Modules for Experiments in Stellar Astrophysics) code, version `r24.08.1`. The primary objective is to investigate the dependence of binary interaction on the initial orbital period. **Model Configuration:** * **Donor Star (M1):** Fixed initial mass of 6.0 M_sun. The evolution is followed self-consistently. * **Companion (M2):** Represented as a point mass of 4.0 M_sun. * **Orbit:** Initially circular; the grid is constructed by varying the initial orbital period. **Physics and Assumptions:** * **Mass Transfer:** Implemented via the *Ritter prescription* for Roche-lobe overflow (RLOF). * **Efficiency:** Fully conservative mass transfer is assumed. * **Angular Momentum:** Includes losses due to gravitational radiation, magnetic braking, and systemic mass loss. * **Tides:** Tidal synchronization of the donor star is accounted for. * **Exclusions:** Wind mass transfer and irradiation effects are not included. **Termination Criteria:** Calculations are terminated if: 1. Roche-lobe overflow occurs at the very first timestep. 2. The system undergoes overflow through the outer Lagrangian point (L2). The setup is designed to isolate the role of the initial orbital period in determining the onset of mass transfer and the subsequent evolutionary regime.mesa_bin_6_4_002.main Grid of Close-Binary Evolution Models This dataset contains a grid of close-binary evolution models computed with the **MESA** (Modules for Experiments in Stellar Astrophysics) code, version `r24.08.1`. The primary objective is to investigate the dependence of binary interaction on the initial orbital period. **Model Configuration:** * **Donor Star (M1):** Fixed initial mass of 6.0 M_sun. The evolution is followed self-consistently. * **Companion (M2):** Represented as a point mass of 4.0 M_sun. * **Orbit:** Initially circular; the grid is constructed by varying the initial orbital period. **Physics and Assumptions:** * **Mass Transfer:** Implemented via the *Ritter prescription* for Roche-lobe overflow (RLOF). * **Efficiency:** Fully conservative mass transfer is assumed. * **Angular Momentum:** Includes losses due to gravitational radiation, magnetic braking, and systemic mass loss. * **Tides:** Tidal synchronization of the donor star is accounted for. * **Exclusions:** Wind mass transfer and irradiation effects are not included. **Termination Criteria:** Calculations are terminated if: 1. Roche-lobe overflow occurs at the very first timestep. 2. The system undergoes overflow through the outer Lagrangian point (L2). The setup is designed to isolate the role of the initial orbital period in determining the onset of mass transfer and the subsequent evolutionary regime.14accrefDownload FITS modelmeta.ref.urlcharindexednullableownerOwner of the datacharnullableembargoDate the data will become/became publicyrcharnullablemimeMIME type of the file servedmeta.code.mimeAccess.FormatcharnullableaccsizeSize of the data in bytesbyteVOX:Image_FileSizeAccess.SizelongnullablepreviewfloatnullablenameModel identifier (e.g., p_0.90)meta.id;meta.maincharnullablem1Fixed initial mass of the donor starsolMassphys.massfloatnullablem2Fixed initial mass of the point-mass companionsolMassphys.massfloatnullablepInitial orbital perioddtime.periodfloatnullablezFixed initial metallicityphys.abund.Zfloatnullableneutrons The Alma-Ata Cosmic Ray Station operates the 18NM-64 neutron supermonitor at an altitude of 3340 meters above sea level, with a geomagnetic cutoff rigidity of 6.7 GeV. The station provides real-time, minute-level measurements of cosmic ray intensity, contributing to the international NMDB network. These data support the study of cosmic ray variations and space weather phenomena. The provided dataset consists of daily tables, where each table corresponds to a single observation day. The data includes two columns: - **Obs_time**: The time of observation at the detector (UTC). - **Count [ct/s]**: The recorded cosmic ray intensity in counts per second. The data are collected and provided by the Institute of Ionosphere, (https://ionos.kz/) and are also available through the Kazakhstan Space Weather Portal (https://ssa.fai.kz/, registration required), which additionally offers interactive visualizations and graphs.neutrons.main The Alma-Ata Cosmic Ray Station operates the 18NM-64 neutron supermonitor at an altitude of 3340 meters above sea level, with a geomagnetic cutoff rigidity of 6.7 GeV. The station provides real-time, minute-level measurements of cosmic ray intensity, contributing to the international NMDB network. These data support the study of cosmic ray variations and space weather phenomena. The provided dataset consists of daily tables, where each table corresponds to a single observation day. The data includes two columns: - **Obs_time**: The time of observation at the detector (UTC). - **Count [ct/s]**: The recorded cosmic ray intensity in counts per second. The data are collected and provided by the Institute of Ionosphere, (https://ionos.kz/) and are also available through the Kazakhstan Space Weather Portal (https://ssa.fai.kz/, registration required), which additionally offers interactive visualizations and graphs.1600000obs_timeTime of observation in UTC (yyyy-mm-ddThh:mm:ssZ).time.epochcharindexednullableobs_mjdTime of observation in MJD.dtime.epochdoubleindexednullablecountsAverage neutron counts per second, derived from one-minute measurements.ct/sarith.rate;phys.particle.neutrondoubleindexednullablesource_pathFile this row was parsed from.meta.id;meta.filecharindexednullablepn_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.bibcodecharnullablepulsars This catalog contains data on the Galactic population of 82 confirmed X-ray pulsars in high-mass X-ray binary (HMXB) systems, classified into 18 persistent and 64 transient sources. Key parameters include spin periods, spin evolution (local and global trends), orbital periods, X-ray luminosities, magnetic fields, distances, and detailed companion star characteristics. The data have been compiled through cross-matching with recent HMXB catalogs and databases such as Fortin et al. (2023), Neumann et al. (2023), and Krivonos et al. (2022), supplemented with literature and SIMBAD database analysis. The catalog aims to support studies on stellar evolution, accretion processes, and binary dynamics.pulsars.main This catalog contains data on the Galactic population of 82 confirmed X-ray pulsars in high-mass X-ray binary (HMXB) systems, classified into 18 persistent and 64 transient sources. Key parameters include spin periods, spin evolution (local and global trends), orbital periods, X-ray luminosities, magnetic fields, distances, and detailed companion star characteristics. The data have been compiled through cross-matching with recent HMXB catalogs and databases such as Fortin et al. (2023), Neumann et al. (2023), and Krivonos et al. (2022), supplemented with literature and SIMBAD database analysis. The catalog aims to support studies on stellar evolution, accretion processes, and binary dynamics.81numberCatalog number of the objectmeta.id;meta.mainintnameName of the objectmeta.idcharnullableraThe pulsar's ICRS right ascension from SIMBADdegpos.eq.ra;meta.maindoubleindexednullabledecThe pulsar's ICRS declenation from SIMBADdegpos.eq.dec;meta.maindoubleindexednullablepsSpin period of the pulsarstime.period.rotationdoublenullablee_psError in spin periodsstat.error;time.period.rotationdoublenullablepsyrYear of spin period measurementyrtime.epochintnullabler_psReference for spin periodmeta.bib.bibcodecharnullableplocspdownLocal spin-down periodstime.perioddoublenullablee_plocspdownError in local spin-down periodsstat.error;time.perioddoublenullableplocspdownstartStart date of local spin-down period measurement in MJDdtime.start;obsdoublenullableplocspdownstopEnd date of local spin-down period measurement in MJDdtime.end;obsdoublenullabler_plocspdownReference for local spin-down periodmeta.bib.bibcodecharnullableplocspupsignSign of local spin-up periodmeta.codecharnullableplocspupLocal spin-up periodstime.perioddoublenullablee_plocspupError in local spin-up periodsstat.error;time.perioddoublenullableplocspupstartStart date of local spin-up period measurement in MJDdtime.start;obsdoublenullableplocspupstopEnd date of local spin-up period measurement in MJDdtime.end;obsdoublenullabler_plocspupReference for local spin-up periodmeta.bib.bibcodecharnullablepglospdownGlobal spin-down periodstime.perioddoublenullablee_pglospdownError in global spin-down periodsstat.error;time.perioddoublenullablepglospdownstartStart date of global spin-down period measurement in MJDdtime.start;obsdoublenullablepglospdownstopEnd date of global spin-down period measurement in MJDdtime.end;obsdoublenullabler_pglospdownReference for global spin-down periodmeta.bib.bibcodecharnullablepglospupsignSign of global spin-up periodmeta.codecharnullablepglospupGlobal spin-up period in secondsstime.perioddoublenullablee_pglospupError in global spin-up periodsstat.error;time.perioddoublenullablepglospupstartStart date of global spin-up period measurement in MJDdtime.start;obsdoublenullablepglospupstopEnd date of global spin-up period measurement in MJDdtime.end;obsdoublenullabler_pglospupReference for global spin-up periodmeta.bib.bibcodecharnullableporbsignSign of orbital periodmeta.codecharnullableporblowerLower limit of orbital perioddtime.perioddoublenullableporbupperUpper limit of orbital perioddtime.perioddoublenullableporberrError in orbital perioddstat.error;time.perioddoublenullableporbrefReference for orbital periodmeta.bib.bibcodecharnullablelxlowerLower limit of X-ray luminosityerg/sphys.luminosity;em.x-raydoublenullablelxupperUpper limit of X-ray luminosityerg/sphys.luminosity;em.x-raydoublenullablelxrangeRange of X-ray luminositymeta.codecharnullablelxrefReference for X-ray luminositymeta.bib.bibcodecharnullablebsignSign of magnetic field strengthmeta.codecharnullableblowerLower limit of magnetic field strength in GaussGphys.magfielddoublenullablebupperUpper limit of magnetic field strength in GaussGphys.magfielddoublenullableberrError in magnetic field strength in GaussGstat.error;phys.magfielddoublenullablebrefReference for magnetic field strengthmeta.bib.bibcodecharnullabledistsignSign of distance measurementmeta.codecharnullabledistlowerLower limit of distance in parsecspcpos.distance;stat.mindoublenullabledistupperUpper limit of distance in parsecspcpos.distance;stat.maxdoublenullabledisterrorError in distance measurement in parsecspcstat.error;pos.distancedoublenullabledistrefReference for distance measurementmeta.bib.bibcodecharnullablecompnameName of the companion objectmeta.id;srccharnullablecompnameclassClassification of the companion objectsrc.classcharnullablecompnamerefReference for companion object namemeta.bib.bibcodecharnullablecompbmagCompanion B-band magnitudemagphot.mag;em.opt.bdoublenullablee_compbmagError in companion B-band magnitudemagstat.error;phot.magdoublenullablecompvmagCompanion V-band magnitudemagphot.mag;em.opt.vdoublenullablee_compvmagError in companion V-band magnitudemagstat.error;phot.magdoublenullablecomprmagCompanion R-band magnitudemagphot.mag;em.opt.rdoublenullablee_comprmagError in companion R-band magnitudemagstat.error;phot.magdoublenullablecompimagCompanion I-band magnitudemagphot.mag;em.opt.idoublenullablee_compimagError in companion I-band magnitudemagstat.error;phot.magdoublenullablecompbvrimagrefReference for companion B, V, R, I magnitudesmeta.bib.bibcodecharnullablecompjmagCompanion J-band magnitudemagphot.mag;em.ir.jdoublenullablee_compjmagError in companion J-band magnitudemagstat.error;phot.magdoublenullablecomphmagCompanion H-band magnitudemagphot.mag;em.ir.hdoublenullablee_comphmagError in companion H-band magnitudemagstat.error;phot.magdoublenullablecompkmagCompanion K-band magnitudemagphot.mag;em.ir.kdoublenullablee_compkmagError in companion K-band magnitudemagstat.error;phot.magdoublenullablecompjhkmagrefReference for companion J, H, K magnitudesmeta.bib.bibcodecharnullableextbminusvColor excess E(B−V)magphot.colordoublenullablee_extbminusvError in color excess E(B−V)magstat.error;phot.colordoublenullabler_extbminusvReference for color excess E(B−V)meta.bib.bibcodecharnullablepersistentFlag indicating the type of pulsar: 1 for persistent pulsars, 0 for transient pulsarsmeta.code.qualshortschmidt_telescope_lc The archive of digitized plates obtained on Schmidt telescope (large camera) at the Fesenkov Astrophysical Institute (FAI), Almaty, Kazakhstan. They represent the results of photometric observations of stars, comets, nebulae etc. for 50 years - from 1950 to 2000. Observations were carried out in the optical range. Telescope specifications: diameter of main mirror D = 397 mm, focal length F = 773 mm.schmidt_telescope_lc.main The archive of digitized plates obtained on Schmidt telescope (large camera) at the Fesenkov Astrophysical Institute (FAI), Almaty, Kazakhstan. They represent the results of photometric observations of stars, comets, nebulae etc. for 50 years - from 1950 to 2000. Observations were carried out in the optical range. Telescope specifications: diameter of main mirror D = 397 mm, focal length F = 773 mm.1216accrefAccess key for the datameta.ref.urlAccess.ReferencecharindexednullableownerOwner of the datacharnullableembargoDate the data will become/became publicyrcharnullablemimeMIME type of the file servedmeta.code.mimeAccess.FormatcharnullableaccsizeSize of the data in bytesbyteVOX:Image_FileSizeAccess.SizelongnullablecenteralphaApproximate center of image, RAdegpos.eq.radoubleindexednullablecenterdeltaApproximate center of image, Decdegpos.eq.decdoubleindexednullableimagetitleSynthetic name of the imagemeta.titlecharnullableinstidIdentifier of the originating instrumentmeta.id;instrcharnullabledateobsThe date of observation from observational log. (Y-M-D .. Y-M-D)dtime;obs.exposuredoublenullablenaxesNumber of axes in datapos.wcs.naxesintnullablepixelsizeNumber of pixels along each of the axespixelpos.wcs.naxisintnullablepixelscaleThe pixel scale on each image axisdeg/pixelpos.wcs.scalefloatnullablerefframeCoordinate system reference framepos.framecharnullablewcs_equinoxEquinox of the given coordinatesyrtime.equinoxfloatnullablewcs_projectionFITS WCS projection typepos.wcs.ctypecharnullablewcs_refpixelWCS reference pixelpixelpos.wcs.crpixfloatnullablewcs_refvaluesWorld coordinates at WCS reference pixeldegpos.wcs.crvaldoublenullablewcs_cdmatrixFITS WCS CDij matrixdeg/pixelpos.wcs.cdmatrixfloatnullablebandpassidFree-form name of the bandpass usedinstr.bandpasscharnullablebandpassunitUnit of bandpass specifications (always m).charnullablebandpassrefvalCharacteristic quantity for the bandpass of the imageminstr.bandpass;stat.medianfloatnullablebandpasshiUpper limit of the bandpass (in BandPass_Unit units)minstr.bandpass;stat.maxfloatnullablebandpassloLower limit of the bandpass (in BandPass_Unit units)minstr.bandpass;stat.minfloatnullablepixflagsFlags specifying the processing done (C-original; F-resampled; Z-fluxes valid; X-not resampled; V-for display onlymeta.codecharnullablecoverageField covered by the imagedegdoubleindexednullableobjectName of object from the observation log.meta.id;srccharnullablefilenameName of .fit file (object_date_exp_id.fit).meta.id;srccharnullabletarget_raRight ascension of object from observation log.degpos.eq.ra;meta.mainfloatnullabletarget_decDeclination of object from observation log.degpos.eq.dec;meta.mainfloatnullableexptimeExposure time from observation log.stime.duration;obs.exposurefloatnullabletelescopeTelescope from observation log.instr.telcharnullablesolar_flux The “Orbita” Radio Polygon at an altitude of 2750 meters conducts solar radio emission observations using state-of-the-art equipment. This includes instruments for monitoring solar radio flux at frequencies of 1 GHz and 2.8 GHz, as well as the Callisto solar radio spectrograph, which is part of the international e-Callisto network. These tools enable the detection of solar radio bursts of types II, III, IV, and V, and provide valuable insights for forecasting the geo-effectiveness of solar flare activity. The provided dataset consists of daily tables, where each table corresponds to a single observation day. The data includes two columns: - **Obs_time**: The time of observation at the detector (UTC). - **Flux [SFU]**: The solar flux unit measurement, representing the intensity of solar radio emission in SFU (Solar Flux Units). The data are collected and provided by the Institute of Ionosphere, (https://ionos.kz/) and are also available through the Kazakhstan Space Weather Portal (https://ssa.fai.kz/, registration required), which additionally offers interactive visualizations and graphs.solar_flux.main The “Orbita” Radio Polygon at an altitude of 2750 meters conducts solar radio emission observations using state-of-the-art equipment. This includes instruments for monitoring solar radio flux at frequencies of 1 GHz and 2.8 GHz, as well as the Callisto solar radio spectrograph, which is part of the international e-Callisto network. These tools enable the detection of solar radio bursts of types II, III, IV, and V, and provide valuable insights for forecasting the geo-effectiveness of solar flare activity. The provided dataset consists of daily tables, where each table corresponds to a single observation day. The data includes two columns: - **Obs_time**: The time of observation at the detector (UTC). - **Flux [SFU]**: The solar flux unit measurement, representing the intensity of solar radio emission in SFU (Solar Flux Units). The data are collected and provided by the Institute of Ionosphere, (https://ionos.kz/) and are also available through the Kazakhstan Space Weather Portal (https://ssa.fai.kz/, registration required), which additionally offers interactive visualizations and graphs.9300000obs_timeTime of observation in UTC (yyyy-mm-ddThh:mm:ssZ).time.epochcharindexednullableobs_mjdTime of observation in MJD.dtime.epochdoubleindexednullablefluxSolar radio flux density measured in Solar Flux Units (SFU).SFUphot.flux.density;em.radiodoubleindexednullablesource_pathFile this row was parsed from.meta.id;meta.filecharindexednullablespecphot_stand_cat The **Spectrophotometric Catalogue of Stars** (A.V. Kharitonov, V.M. Tereshenko, L.N. Knyazeva, 2011) provides calibrated monochromatic irradiances for bright northern-hemisphere stars and is intended for absolute/relative flux calibration of spectra and photometry. **Content (one row per star):** * Identifiers: sequential catalogue number, common name (if any), **BS** and **HD** numbers. * Astrometry: J2000.0 right ascension and declination (also given in decimal degrees as *raj2000*, *dej2000*). * Photometry and classification: visual magnitude **V**, colour index **B−V**, spectral type, trigonometric parallax (when available). * Notes/flags: *st_ds* (short classification/remarks), *n* (mantissa exponent; see below). * Spectrophotometry: monochromatic irradiances **F_λ** at fixed wavelengths from **3225 Å to 7575 Å** in **50 Å** steps (columns *f3225*, *f3275*, …, *f7575*). Values are given as **mantissae**; the full physical value is *F_λ = mantissa × 10^{-6}* in units of **W·m⁻²·m⁻¹**. **Intended use:** * Absolute/relative flux calibration of long-slit and fiber spectra. * Cross-checks of instrumental response and atmospheric extinction curves. * Educational and research tasks in stellar astrophysics. **Coverage:** * Wavelength grid: 3225–7575 Å, Δλ = 50 Å, continuous per star. * Typical targets: bright standards of spectral classes **O–M**, luminosity classes **I–V**.specphot_stand_cat.main The **Spectrophotometric Catalogue of Stars** (A.V. Kharitonov, V.M. Tereshenko, L.N. Knyazeva, 2011) provides calibrated monochromatic irradiances for bright northern-hemisphere stars and is intended for absolute/relative flux calibration of spectra and photometry. **Content (one row per star):** * Identifiers: sequential catalogue number, common name (if any), **BS** and **HD** numbers. * Astrometry: J2000.0 right ascension and declination (also given in decimal degrees as *raj2000*, *dej2000*). * Photometry and classification: visual magnitude **V**, colour index **B−V**, spectral type, trigonometric parallax (when available). * Notes/flags: *st_ds* (short classification/remarks), *n* (mantissa exponent; see below). * Spectrophotometry: monochromatic irradiances **F_λ** at fixed wavelengths from **3225 Å to 7575 Å** in **50 Å** steps (columns *f3225*, *f3275*, …, *f7575*). Values are given as **mantissae**; the full physical value is *F_λ = mantissa × 10^{-6}* in units of **W·m⁻²·m⁻¹**. **Intended use:** * Absolute/relative flux calibration of long-slit and fiber spectra. * Cross-checks of instrumental response and atmospheric extinction curves. * Educational and research tasks in stellar astrophysics. **Coverage:** * Wavelength grid: 3225–7575 Å, Δλ = 50 Å, continuous per star. * Typical targets: bright standards of spectral classes **O–M**, luminosity classes **I–V**.numberSequential number in the catalogmeta.idintnullablenameStar namemeta.id;meta.maincharnullablebsBright Star (BS) catalog numbermeta.idcharnullablehdHenry Draper (HD) catalog number (primary)meta.id;meta.maincharnullableraj2000Right Ascension J2000degpos.eq.ra;meta.maindoublenullabledej2000Declination J2000degpos.eq.dec;meta.maindoublenullablevmagV magnitudemagphot.magdoublenullableb_vB−V color indexmagphot.colordoublenullableparallaxParallaxmaspos.parallaxintnullablesp_typeSpectral typesrc.spTypecharnullablest_dsStandard-star mark. β Ari - A, γ Ori - R, β Tau - T, α Leo - L, η UMa - U, α Lyr - Y, α Aql - Q, α Peg - P, HD221525 - Hmeta.codecharnullablenOrder of magnitude factor for monochromatic illuminances; given in table header as 10^(-n), to be applied to flux mantissasarith.factorcharnullablef3225Mantissa of monochromatic irradiance F_lambda at 3225 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3275Mantissa of monochromatic irradiance F_lambda at 3275 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3325Mantissa of monochromatic irradiance F_lambda at 3325 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3375Mantissa of monochromatic irradiance F_lambda at 3375 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3425Mantissa of monochromatic irradiance F_lambda at 3425 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3475Mantissa of monochromatic irradiance F_lambda at 3475 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3525Mantissa of monochromatic irradiance F_lambda at 3525 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3575Mantissa of monochromatic irradiance F_lambda at 3575 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3625Mantissa of monochromatic irradiance F_lambda at 3625 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3675Mantissa of monochromatic irradiance F_lambda at 3675 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3725Mantissa of monochromatic irradiance F_lambda at 3725 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3775Mantissa of monochromatic irradiance F_lambda at 3775 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3825Mantissa of monochromatic irradiance F_lambda at 3825 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3875Mantissa of monochromatic irradiance F_lambda at 3875 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3925Mantissa of monochromatic irradiance F_lambda at 3925 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef3975Mantissa of monochromatic irradiance F_lambda at 3975 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4025Mantissa of monochromatic irradiance F_lambda at 4025 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4075Mantissa of monochromatic irradiance F_lambda at 4075 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4125Mantissa of monochromatic irradiance F_lambda at 4125 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4175Mantissa of monochromatic irradiance F_lambda at 4175 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4225Mantissa of monochromatic irradiance F_lambda at 4225 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4275Mantissa of monochromatic irradiance F_lambda at 4275 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4325Mantissa of monochromatic irradiance F_lambda at 4325 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4375Mantissa of monochromatic irradiance F_lambda at 4375 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4425Mantissa of monochromatic irradiance F_lambda at 4425 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4475Mantissa of monochromatic irradiance F_lambda at 4475 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4525Mantissa of monochromatic irradiance F_lambda at 4525 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4575Mantissa of monochromatic irradiance F_lambda at 4575 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4625Mantissa of monochromatic irradiance F_lambda at 4625 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4675Mantissa of monochromatic irradiance F_lambda at 4675 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4725Mantissa of monochromatic irradiance F_lambda at 4725 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4775Mantissa of monochromatic irradiance F_lambda at 4775 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4825Mantissa of monochromatic irradiance F_lambda at 4825 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4875Mantissa of monochromatic irradiance F_lambda at 4875 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4925Mantissa of monochromatic irradiance F_lambda at 4925 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef4975Mantissa of monochromatic irradiance F_lambda at 4975 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5025Mantissa of monochromatic irradiance F_lambda at 5025 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5075Mantissa of monochromatic irradiance F_lambda at 5075 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5125Mantissa of monochromatic irradiance F_lambda at 5125 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5175Mantissa of monochromatic irradiance F_lambda at 5175 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5225Mantissa of monochromatic irradiance F_lambda at 5225 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5275Mantissa of monochromatic irradiance F_lambda at 5275 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5325Mantissa of monochromatic irradiance F_lambda at 5325 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5375Mantissa of monochromatic irradiance F_lambda at 5375 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5425Mantissa of monochromatic irradiance F_lambda at 5425 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5475Mantissa of monochromatic irradiance F_lambda at 5475 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5525Mantissa of monochromatic irradiance F_lambda at 5525 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5575Mantissa of monochromatic irradiance F_lambda at 5575 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5625Mantissa of monochromatic irradiance F_lambda at 5625 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5675Mantissa of monochromatic irradiance F_lambda at 5675 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5725Mantissa of monochromatic irradiance F_lambda at 5725 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5775Mantissa of monochromatic irradiance F_lambda at 5775 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5825Mantissa of monochromatic irradiance F_lambda at 5825 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5875Mantissa of monochromatic irradiance F_lambda at 5875 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5925Mantissa of monochromatic irradiance F_lambda at 5925 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef5975Mantissa of monochromatic irradiance F_lambda at 5975 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6025Mantissa of monochromatic irradiance F_lambda at 6025 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6075Mantissa of monochromatic irradiance F_lambda at 6075 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6125Mantissa of monochromatic irradiance F_lambda at 6125 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6175Mantissa of monochromatic irradiance F_lambda at 6175 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6225Mantissa of monochromatic irradiance F_lambda at 6225 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6275Mantissa of monochromatic irradiance F_lambda at 6275 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6325Mantissa of monochromatic irradiance F_lambda at 6325 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6375Mantissa of monochromatic irradiance F_lambda at 6375 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6425Mantissa of monochromatic irradiance F_lambda at 6425 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6475Mantissa of monochromatic irradiance F_lambda at 6475 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6525Mantissa of monochromatic irradiance F_lambda at 6525 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6575Mantissa of monochromatic irradiance F_lambda at 6575 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6625Mantissa of monochromatic irradiance F_lambda at 6625 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6675Mantissa of monochromatic irradiance F_lambda at 6675 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6725Mantissa of monochromatic irradiance F_lambda at 6725 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6775Mantissa of monochromatic irradiance F_lambda at 6775 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6825Mantissa of monochromatic irradiance F_lambda at 6825 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6875Mantissa of monochromatic irradiance F_lambda at 6875 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6925Mantissa of monochromatic irradiance F_lambda at 6925 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef6975Mantissa of monochromatic irradiance F_lambda at 6975 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7025Mantissa of monochromatic irradiance F_lambda at 7025 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7075Mantissa of monochromatic irradiance F_lambda at 7075 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7125Mantissa of monochromatic irradiance F_lambda at 7125 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7175Mantissa of monochromatic irradiance F_lambda at 7175 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7225Mantissa of monochromatic irradiance F_lambda at 7225 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7275Mantissa of monochromatic irradiance F_lambda at 7275 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7325Mantissa of monochromatic irradiance F_lambda at 7325 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7375Mantissa of monochromatic irradiance F_lambda at 7375 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7425Mantissa of monochromatic irradiance F_lambda at 7425 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7475Mantissa of monochromatic irradiance F_lambda at 7475 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7525Mantissa of monochromatic irradiance F_lambda at 7525 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablef7575Mantissa of monochromatic irradiance F_lambda at 7575 Å; multiply by 10^{-6}.W m-2 m-1phot.flux.density;em.wldoublenullablespectra_agn_archive The archive of AGN spectral observations is obtained on AZT-8 telescope at the Fesenkov Astrophysical Institute (FAI), Almaty, Kazakhstan. It represents the result of observations for abot 25 years - from 1970 to 1995. All observations were carried out at AZT-8 (D = 700 mm, F[main] = 2800 mm, F[Cassegrain] = 11000 mm) with a high-power spectrograph. In 1967-68, on the basis of the image intensifier (https://doi.org/10.1080/1055679031000084795a) developed and assembled the spectrograph of the original design in the workshops of the FAI.spectra_agn_archive.data The archive of AGN spectral observations is obtained on AZT-8 telescope at the Fesenkov Astrophysical Institute (FAI), Almaty, Kazakhstan. It represents the result of observations for abot 25 years - from 1970 to 1995. All observations were carried out at AZT-8 (D = 700 mm, F[main] = 2800 mm, F[Cassegrain] = 11000 mm) with a high-power spectrograph. In 1967-68, on the basis of the image intensifier (https://doi.org/10.1080/1055679031000084795a) developed and assembled the spectrograph of the original design in the workshops of the FAI.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_dstitleDataset titlemeta.titlecharnullablessa_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_targnameTarget namemeta.id;srccharnullablessa_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_dateobsThe date of observation from observational log in JDdtime.epochdoublenullablessa_timeextExposure timestime.duration;obs.exposuredoublenullablessa_specmidMidpoint of region covered in this datasetminstr.bandpassssa:Char.SpectralAxis.Coverage.Location.Valuefloatnullablessa_specextWidth of the spectrumminstr.bandwidthssa:Char.SpectralAxis.Coverage.Bounds.Extentfloatnullablessa_specstartStart wavelengthAngstromem.wl;stat.mindoublenullablessa_specendEnd wavelengthAngstromem.wl;stat.maxdoublenullablessa_lengthNumber of spectral pointsmeta.numberintssa_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_specresWavelength step (sampling)Angstromem.wldoublenullablessa_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 link to a datalink document for this spectrum.meta.ref.urlcharnullableobjectsName of galaxymeta.id;srccharnullableraThe AGN's ICRS right ascension from SIMBAD (J2000)degpos.eq.ra;meta.maindoublenullabledecThe AGN's ICRS delination from SIMBAD (J2000)degpos.eq.dec;meta.maindoublenullableexp_timeExposure timestime.duration;obs.exposuredoublenullablespec_lineThe spectral line observed, such as H-alpha or H-beta.em.linedoublenullablespectra_pn_archive Spectra of planetary nebulae obtained at the AZT-8 telescope (0.7-m, Fesenkov Astrophysical Institute, Kamenskoe Plato, Almaty, Kazakhstan) during 1970–1998. Observations were carried out with a diffraction spectrograph equipped with the UM-92 image tube, in the 4000–8000 Å range, recorded on A-600 and A-600U photographic plates.spectra_pn_archive.data Spectra of planetary nebulae obtained at the AZT-8 telescope (0.7-m, Fesenkov Astrophysical Institute, Kamenskoe Plato, Almaty, Kazakhstan) during 1970–1998. Observations were carried out with a diffraction spectrograph equipped with the UM-92 image tube, in the 4000–8000 Å range, recorded on A-600 and A-600U photographic plates.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_dateobsThe date of observation from observational log in JDdtime.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 link to a datalink document for this spectrum.meta.ref.urlcharnullableobjectsPlanetary nebula identifiermeta.idcharnullableraICRS right ascension (J2000)degpos.eq.ra;meta.maindoublenullabledecICRS declination (J2000)degpos.eq.dec;meta.maindoublenullableexp_timeTotal exposure time (seconds)sobs.exposuredoublenullablewr_wc_wo_sequence This catalogue contains results of **photometric and spectral observations** of seven Galactic **Wolf–Rayet stars** of the **WC and WO sequences**, obtained in 2021–2022 at the *Fesenkov Astrophysical Institute (FAI), Kazakhstan*. The observing programme included moderately bright stars (mostly fainter than *V = 10m*) observed in **B**, **V**, and **Rc** photometric filters, as well as **medium-resolution spectra** for measuring absolute fluxes in prominent emission lines. For each object, the table provides: * identifiers (WR catalogue number, alternative name), * spectral subtype, * equatorial coordinates (J2000), * literature photometry (B_cat, V_cat) and reference codes, * date of observation and Julian Date (JD−2400000), * measured **B**, **V**, **Rc** magnitudes with their errors, * and absolute fluxes and equivalent widths for a set of emission lines, including **C III λ4650**, **He II λ4686**, **C IV λ5017**, **He II λ5411**, **He II + C IV λ6560**, **C III λ6744**, **C IV λ7065**, and **C II λ7234**. These data were **first published** in the paper *“Photometric and Spectral Studies of a Group of Galactic Wolf–Rayet Stars. II. WC and WO Sequences”*, *Astrophysics*, **Vol. 67, No. 1 (February 2024)**, by *L.N. Kondratyeva, I.V. Reva, E.K. Denisyuk, S.A. Shomshekova, A.K. Aimanova*. DOI: `10.54503/0002-3051-2024.77.1-13`wr_wc_wo_sequence.main This catalogue contains results of **photometric and spectral observations** of seven Galactic **Wolf–Rayet stars** of the **WC and WO sequences**, obtained in 2021–2022 at the *Fesenkov Astrophysical Institute (FAI), Kazakhstan*. The observing programme included moderately bright stars (mostly fainter than *V = 10m*) observed in **B**, **V**, and **Rc** photometric filters, as well as **medium-resolution spectra** for measuring absolute fluxes in prominent emission lines. For each object, the table provides: * identifiers (WR catalogue number, alternative name), * spectral subtype, * equatorial coordinates (J2000), * literature photometry (B_cat, V_cat) and reference codes, * date of observation and Julian Date (JD−2400000), * measured **B**, **V**, **Rc** magnitudes with their errors, * and absolute fluxes and equivalent widths for a set of emission lines, including **C III λ4650**, **He II λ4686**, **C IV λ5017**, **He II λ5411**, **He II + C IV λ6560**, **C III λ6744**, **C IV λ7065**, and **C II λ7234**. These data were **first published** in the paper *“Photometric and Spectral Studies of a Group of Galactic Wolf–Rayet Stars. II. WC and WO Sequences”*, *Astrophysics*, **Vol. 67, No. 1 (February 2024)**, by *L.N. Kondratyeva, I.V. Reva, E.K. Denisyuk, S.A. Shomshekova, A.K. Aimanova*. DOI: `10.54503/0002-3051-2024.77.1-13`objectWR catalogue number of the star.meta.id;srccharnullablealt_nameAlternative identifier of the star (e.g., HD, BD number).meta.id;srccharnullablespSpectral type of the star.src.spTypecharnullableraRight Ascension (J2000) of the star in decimal degrees.degpos.eq.ra;meta.maindoublenullabledecDeclination (J2000) of the star in decimal degrees.degpos.eq.dec;meta.maindoublenullableb_catCatalogue B magnitude from literature.magphot.mag;em.opt.Bfloatnullablev_catCatalogue V magnitude from literature.magphot.mag;em.opt.Vfloatnullablemag_refReference code for the catalogue magnitudes.meta.bibcharnullabledate_obsUTC date of the observation.time.epochcharnullableb_magMeasured B magnitude from observations.magphot.mag;em.opt.Bfloatnullableb_mag_errUncertainty in the measured B magnitude.magstat.error;phot.mag;em.opt.Bfloatnullablev_magMeasured V magnitude from observations.magphot.mag;em.opt.Vfloatnullablev_mag_errUncertainty in the measured V magnitude.magstat.error;phot.mag;em.opt.Vfloatnullablerc_magMeasured Cousins R magnitude from observations.magphot.mag;em.opt.Rfloatnullablerc_mag_errUncertainty in the measured Cousins R magnitude.magstat.error;phot.mag;em.opt.Rfloatnullableheii_civ_4340_fabsAbsolute flux of HeII and CIV λ4340 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_civ_4340_ewEquivalent width of HeII and CIV λ4340 blend.Angstromspect.line.eqWidthfloatnullableciii_civ_4444_fabsAbsolute flux of CIII and CIV λ4444 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_civ_4444_ewEquivalent width of CIII and CIV λ4444 blend.Angstromspect.line.eqWidthfloatnullableciii_heii_4515_4540_fabsAbsolute flux of CIII and HeII λ4515 and 4540 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_heii_4515_4540_ewEquivalent width of CIII and HeII λ4515 and 4540 blend.Angstromspect.line.eqWidthfloatnullableheii_4540_fabsAbsolute flux of HeII III λ4540 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_4540_ewEquivalent width of HeII λ4540 emission line.Angstromspect.line.eqWidthfloatnullableciii_4619_fabsAbsolute flux of CIII λ4619 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_4619_ewEquivalent width of CIII λ4619 emission line.Angstromspect.line.eqWidthfloatnullableciv_heii_4650_4686_fabsAbsolute flux of CIV and HeII λ4650 and 4686 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_heii_4650_4686_ewEquivalent width of CIV and HeII λ4650–4686 blend.Angstromspect.line.eqWidthfloatnullableciv_heii_4650_fabsAbsolute flux of CIV and HeII λ4650 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_heii_4650_ewEquivalent width of CIV and HeII λ4650 blend.Angstromspect.line.eqWidthfloatnullableciv_4656_fabsAbsolute flux of CIV λ4656 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_4656_ewEquivalent width of CIV λ4656 emission line.Angstromspect.line.eqWidthfloatnullableciii_civ_4656_fabsAbsolute flux of CII and CIV λ4656 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_civ_4656_ewEquivalent width of CIII and CIV λ4656 blend.Angstromspect.line.eqWidthfloatnullableciv_heii_4660_fabsAbsolute flux of CIV and HeII λ4660 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_heii_4660_ewEquivalent width of CIV and HeII λ4660 blend.Angstromspect.line.eqWidthfloatnullableciv_4660_fabsAbsolute flux of CIV λ4660 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_4660_ewEquivalent width of CIV λ4660 emission line.Angstromspect.line.eqWidthfloatnullableciv_heii_4686_fabsAbsolute flux of CIV λ4686 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_heii_4686_ewEquivalent width of CIV and HeII λ4686 blend.Angstromspect.line.eqWidthfloatnullableheii_4686_fabsAbsolute flux of HeII λ4686 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_4686_ewEquivalent width of HeII λ4686 emission line.Angstromspect.line.eqWidthfloatnullableoiv_civ_4780_fabsAbsolute flux of OIV and CIV λ4945 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableoiv_civ_4780_ewEquivalent width of OIV and CIV λ4945 blend.Angstromspect.line.eqWidthfloatnullablecii_4780_fabsAbsolute flux of СII λ4780 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_4780_ewEquivalent width of СII λ4780 emission line.Angstromspect.line.eqWidthfloatnullableheii_4860_fabsAbsolute flux of HeII λ4860 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_4860_ewEquivalent width of HeII λ4860 emission line.Angstromspect.line.eqWidthfloatnullableciv_heii_4860_fabsAbsolute flux of CIV and HeII λ4860 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_heii_4860_ewEquivalent width of CIV and HeII λ4860 blend.Angstromspect.line.eqWidthfloatnullableciv_heii_4861_fabsAbsolute flux of CIV and HeII λ4861 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_heii_4861_ewEquivalent width of CIV and HeII λ4861 blend.Angstromspect.line.eqWidthfloatnullablehei_4921_fabsAbsolute flux of HeI λ4921 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablehei_4921_ewEquivalent width of HeI λ4921 emission line.Angstromspect.line.eqWidthfloatnullableheii_4921_fabsAbsolute flux of HeII λ4921 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_4921_ewEquivalent width of HeII λ4921 emission line.Angstromspect.line.eqWidthfloatnullableov_4930_fabsAbsolute flux of OV λ4930 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableov_4930_ewEquivalent width of OV λ4930 emission line.Angstromspect.line.eqWidthfloatnullableov_4940_fabsAbsolute flux of OV λ4940 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableov_4940_ewEquivalent width of OV λ4940 emission line.Angstromspect.line.eqWidthfloatnullableheii_4940_fabsAbsolute flux of HeII λ4940 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_4940_ewEquivalent width of HeII λ4940 emission line.Angstromspect.line.eqWidthfloatnullableciv_5016_fabsAbsolute flux of CIV λ5016 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_5016_ewEquivalent width of CIV λ5016 emission line.Angstromspect.line.eqWidthfloatnullableciv_hei_5016_fabsAbsolute flux of CIV and HeI λ5016 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_hei_5016_ewEquivalent width of CIV and HeI λ5016 blend.Angstromspect.line.eqWidthfloatnullableciv_5017_fabsAbsolute flux of CIV λ5017 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_5017_ewEquivalent width of CIV λ5017 emission line.Angstromspect.line.eqWidthfloatnullableciv_hei_5017_fabsAbsolute flux of CIV and HeI λ5017 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_hei_5017_ewEquivalent width of CIV and HeI λ5017 blend.Angstromspect.line.eqWidthfloatnullablecii_ciii_5141_fabsAbsolute flux of CII and CIII λ5141 blend.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_ciii_5141_ewEquivalent width of CII and CIII λ5141 blend.Angstromspect.line.eqWidthfloatnullableciii_5250_5270_fabsAbsolute flux of CIII λ5250 and 5270 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_5250_5270_ewEquivalent width of CIII λ5250 and 5270 emission line.Angstromspect.line.eqWidthfloatnullableciii_5250_5305_fabsAbsolute flux of CIII λ5250+5305 emission blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_5250_5305_ewEquivalent width of CIII λ5250+5305 emission blend.Angstromspect.line.eqWidthfloatnullableciii_oiv_5260_fabsAbsolute flux of CIII + OIV λ5260 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_oiv_5260_ewEquivalent width of CIII + OIV λ5260 emission line.Angstromspect.line.eqWidthfloatnullableovi_5280_fabsAbsolute flux of OVI λ5280 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableovi_5280_ewEquivalent width of OVI λ5280 emission line.Angstromspect.line.eqWidthfloatnullableciii_5305_fabsAbsolute flux of CIII λ5305 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_5305_ewEquivalent width of CIII λ5305 emission line.Angstromspect.line.eqWidthfloatnullableheii_5411_fabsAbsolute flux of HeII λ5411 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_5411_ewEquivalent width of HeII λ5411 emission line.Angstromspect.line.eqWidthfloatnullableheii_civ_5411_fabsAbsolute flux of HeII + CIV λ5411 emission blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_civ_5411_ewEquivalent width of HeII + CIV λ5411 emission blend.Angstromspect.line.eqWidthfloatnullableheii_ciii_5411_5470_fabsAbsolute flux of HeII + CIII λ5411–5470 emission feature.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_ciii_5411_5470_ewEquivalent width of HeII + CIII λ5411–5470 emission feature.Angstromspect.line.eqWidthfloatnullablecvi_5440_fabsAbsolute flux of CVI λ5440 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecvi_5440_ewEquivalent width of CVI λ5440 emission line.Angstromspect.line.eqWidthfloatnullableciv_5460_fabsAbsolute flux of CIV λ5460 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_5460_ewEquivalent width of CIV λ5460 emission line.Angstromspect.line.eqWidthfloatnullableciv_5469_fabsAbsolute flux of CIV λ5469 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_5469_ewEquivalent width of CIV λ5469 emission line.Angstromspect.line.eqWidthfloatnullableciv_5471_fabsAbsolute flux of CIV λ5471 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_5471_ewEquivalent width of CIV λ5471 emission line.Angstromspect.line.eqWidthfloatnullableheii_civ_5595_fabsAbsolute flux of HeII + CIV λ5595 emission blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_civ_5595_ewEquivalent width of HeII + CIV λ5595 emission blend.Angstromspect.line.eqWidthfloatnullableheii_civ_6560_fabsAbsolute flux of HeII + CIV λ6560 emission blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_civ_6560_ewEquivalent width of HeII + CIV λ6560 emission blend.Angstromspect.line.eqWidthfloatnullableheii_6560_fabsAbsolute flux of HeII λ6560 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableheii_6560_ewEquivalent width of HeII λ6560 emission line.Angstromspect.line.eqWidthfloatnullablecii_heii_6580_fabsAbsolute flux of blended CII + HeII λ6580 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_heii_6580_ewEquivalent width of blended CII + HeII λ6580 emission line.Angstromspect.line.eqWidthfloatnullablehei_6678_fabsAbsolute flux of HeI λ6678 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablehei_6678_ewEquivalent width of HeI λ6678 emission line.Angstromspect.line.eqWidthfloatnullablecii_ciii_6732_fabsAbsolute flux of CII + CIII λ6732 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_ciii_6732_ewEquivalent width of CII + CIII λ6732 emission line.Angstromspect.line.eqWidthfloatnullableciii_6740_fabsAbsolute flux of CIII λ6740 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_6740_ewEquivalent width of CIII λ6740 emission line.Angstromspect.line.eqWidthfloatnullableciii_cii_6744_fabsAbsolute flux of CIII + CII λ6744 emission blend.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_cii_6744_ewEquivalent width of CIII + CII λ6744 emission blend.Angstromspect.line.eqWidthfloatnullableciii_civ_6748_fabsAbsolute flux of CIII + CIV λ6748 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_civ_6748_ewEquivalent width of CIII + CIV λ6748 emission line.Angstromspect.line.eqWidthfloatnullableci_ciii_6748_fabsAbsolute flux of CI + CIII λ6748 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableci_ciii_6748_ewEquivalent width of CI + CIII λ6748 emission line.Angstromspect.line.eqWidthfloatnullablecii_ciii_6780_fabsAbsolute flux of CII + CIII λ6780 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_ciii_6780_ewEquivalent width of CII + CIII λ6780 emission line.Angstromspect.line.eqWidthfloatnullableciii_7037_fabsAbsolute flux of CIII λ7037 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciii_7037_ewEquivalent width of CIII λ7037 emission line.Angstromspect.line.eqWidthfloatnullableciv_7060_fabsAbsolute flux of CIV λ7060 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_7060_ewEquivalent width of CIV λ7060 emission line.Angstromspect.line.eqWidthfloatnullableciv_hei_7060_fabsAbsolute flux of blended CIV + HeI λ7060 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_hei_7060_ewEquivalent width of blended CIV + HeI λ7060 emission line.Angstromspect.line.eqWidthfloatnullableciv_hei_7065_fabsAbsolute flux of blended CIV + HeI λ7065 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_hei_7065_ewEquivalent width of blended CIV + HeI λ7065 emission line.Angstromspect.line.eqWidthfloatnullablecii_hei_7065_fabsAbsolute flux of blended CII + HeI λ7065 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_hei_7065_ewEquivalent width of blended CII + HeI λ7065 emission line.Angstromspect.line.eqWidthfloatnullableciv_cii_7065_fabsAbsolute flux of blended CIV + CII λ7065 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableciv_cii_7065_ewEquivalent width of blended CIV + CII λ7065 emission line.Angstromspect.line.eqWidthfloatnullablehei_7065_fabsAbsolute flux of HeI λ7065 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablehei_7065_ewEquivalent width of HeI λ7065 emission line.Angstromspect.line.eqWidthfloatnullablecii_7122_fabsAbsolute flux of CII λ7122 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_7122_ewEquivalent width of CII λ7122 emission line.Angstromspect.line.eqWidthfloatnullablecii_7207_7258_fabsAbsolute flux of CII λ7207–7258 emission feature.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_7207_7258_ewEquivalent width of CII λ7207–7258 emission feature.Angstromspect.line.eqWidthfloatnullablecii_7234_fabsAbsolute flux of CII λ7234 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_7234_ewEquivalent width of CII λ7234 emission line.Angstromspect.line.eqWidthfloatnullableunknown_7254_fabsAbsolute flux of λ7254 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullableunknown_7254_ewEquivalent width of λ7254 emission line.Angstromspect.line.eqWidthfloatnullablecii_7260_fabsAbsolute flux of CII λ7260 emission line.10**-15 W m**(-2)phot.flux;em.linefloatnullablecii_7260_ewEquivalent width of CII λ7260 emission line.Angstromspect.line.eqWidthfloatnullable