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FAI archives TAP service
The 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 fai_agn schema, main from the grb_photometry schema, obscore from the ivoa schema, main from the maksutov_50_telescope schema, main from the pulsars schema, main from the schmidt_telescope_lc schema, data from the spectra_agn_archive schema, columns, groups, key_columns, keys, schemas, tables from the tap_schema schema.
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KazVO RegTAP Service
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/
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AGN observations obtained at FAI
Service Info
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.
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Alma-Ata Geomagnetic Observatory Data Service
Service Info
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.
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Alma-Ata Station Neutron Monitor Data Service
Service Info
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.
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ArXSP: Archive Spectrum Processing Tool
Service Info
ArXSP is a Python-based desktop application for the reduction and
analysis of digitized archival spectra obtained at the Fesenkov
Astrophysical Institute. The software provides geometric correction
tools (cropping and alignment of spectral images), extraction of
characteristic curves, s-distortion correction, and conversion from
optical density to relative intensity. Installers for Linux, Windows,
and macOS are available on the FAI VO portal
(https://vo.fai.kz/software.php).
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Archival of Planetary Nebulae Spectral Observation
Service Info
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.
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Archive of AGN spectral observations
Service Info
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.
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Archive of the FAI 50 cm Meniskus Maksutov telescope
Service Info
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.
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Archive of the FAI Schmidt telescope (large camera)
Service Info
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.
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Astronomical Calendar: Sun and Moon Ephemerides and Twilight
Calculator
Service Info
The Astronomical Calendar is a software package for automated
calculations of the celestial coordinates (ephemerides) of the Sun and
Moon. It computes the times of sunrise and sunset, the boundaries of
civil, nautical, and astronomical twilight, and lunar phases, based on
the geographic coordinates of the observing site and its time zone. A
web-based implementation is hosted at the Fesenkov Astrophysical
Institute and is available in Kazakh, Russian, and English. The
service allows users to obtain ephemerides for any location on Earth
and export results as tables (including PDF output).
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FAI Asteroid Observation Log
Service Info
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.
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FAI CCD Photometric Image Service
Service Info
Reduced, astrometrically calibrated CCD images obtained with
telescopes operated by the Fesenkov Astrophysical Institute. The
initial release contains observations from the Zeiss-1000 East
telescope at the Tian Shan Astronomical Observatory; further FAI
telescopes will be added as their reduced data become available.
Discovery metadata remain public during proprietary periods. Before
the RELEASE date, downloads contain the original FITS headers but
zero-valued data arrays; afterwards the original FITS product is
delivered.
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Galactic X-ray Pulsars
Service Info
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.
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MESA Grid: Binary Evolution (M1=6.0, M2=4.0, Z=0.02)
Service Info
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.
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ML-Enhanced GCVS: Variable Stars with Gaia DR3 and TESS
Service Info
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.
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Order Computational and Storage Resources at FAI
Service Info
Via this service, it is possible to order computations with FAI
computer cluster.
Fesenkov Astrophysical Institute operates a computer cluster that
consists of several· high-performance computing nodes equipped with
high-end multi-core CPUs and GPU cards. The theoretical single
precision performance of the cluster currently peaks at 68 TFLOPS for
CPU operations (784 cores / 1 568 threads) and 1235 TFLOPS for GPU
(286 208 CUDA cores). In addition, it has redundant data storage of
300 terabytes in volume. Cluster has 10 gigabit interlink and operates
under Linux based OS. Task scheduling is organized using SLURM
workload manager. For external users, computation and data storage
operations on the FAI cluster can be arranged via online task
submission that once approved results in an SSH account to the master
node with agreed permissions.
To order simulations, please, Log In on VO web-page
(https://vo.fai.kz/) and press the button "Order Simulations" into
your account or go to https://vo.fai.kz/comput_sub.php.
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Order Observations at FAI Telescopes
Service Info
Via this service, it is possible to request astronomical observations
with telescopes operated by the Fesenkov Astrophysical Institute.
The Academician Omarov Assy-Turgen Observatory is located on the
Assy-Turgen plateau at an altitude of 2750 m, approximately 85 km east
of Almaty. Observations have been conducted since 1981. In 2017, the
largest telescope in Kazakhstan (AZT-20) began regular operations. The
site is characterized by high atmospheric transparency, minimal light
pollution, and low turbulence.
Available telescopes include: AZT-20, Zeiss-1000, RC-500, WFOS-40.
To request observations, please log in to the VO web portal
(https://vo.fai.kz/) and select "Order Observations" in your account,
or use the page: https://vo.fai.kz/observatory_descrip.php
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Photometric and Spectral Data of Galactic Wolf-Rayet Stars (WC and WO
sequence)
Service Info
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`
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Photometric and Spectral Data of Galactic Wolf-Rayet Stars (WN
sequence)
Service Info
This catalogue contains results of **photometric and spectral observations**
of eleven Galactic **Wolf–Rayet stars** of the **WN sequence**,
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 measurement of 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
**He II λ4540**, **N III λ4619**, **He II λ4685**, **He II + H I λ4859**,
**N V λ4945**, **He II λ5411**, **He II λ6560**, **He II λ6583**, and **N IV λ7109**.
These data were **first published** in the paper
*“Photometric and Spectral Studies of a Group of Galactic Wolf–Rayet Stars. I. WN Sequence”*,
*Astrophysics*, **Vol. 66, No. 4 (November 2023)**,
by *L.N. Kondratyeva, I.V. Reva, E.K. Denisyuk, S.A. Shomshekova, A.K. Aimanova*.
DOI: `10.54503/0002-3051-2023.76.4-521`
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Photometrical observations of GRB
Service Info
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.
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Planetary Nebulae: results of abs spectroscopy
Service Info
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.
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Solar Radio Emission Observations at “Orbita” Radio Polygon
Service Info
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.
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Spectrophotometric Standard Stars Catalog
Service Info
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**.
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Wavelength Calibration Tool
Service Info
The Wavelength Calibration Tool converts pixel coordinates of a
one-dimensional calibration-lamp spectrum into a physical wavelength
scale. Calibration requires a corresponding reference lamp spectrum
with an already known wavelength axis, supplied by the user or
selected from the built-in reference data. The service uses Dynamic
Time Warping (DTW) to match emission peaks and RANSAC to reject
incorrect matches and construct a robust polynomial dispersion
solution. Users can inspect diagnostic plots and residual errors, then
export the calibrated spectrum and calibration solution.
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