apis.epn_core | Table Info | EpnCore table for APIS service | Planetary aurorae are powerful emissions radiated from auroral
regions of magnetized planets by accelerated charged particles, in a
wide range of wavelengths (from radio to X-rays). The UV range in
particular is adequate to measure collisionaly excited transitions of
H and H2, the dominant species in the upper atmosphere of giant
planets, produced by precipitating auroral particles, and benefits a
good angular resolution. Auroral UV observations therefore provide a
rich source of informations on planetary atmospheres and
magnetospheres. They also offer a unique diagnostic to remotely probe
the solar wind activity throughout the heliosphere. |
basecom.epn_core | Table Info | N/A | Since 1973, the 18-cm lines of the OH radical have been
systematically observed in a number of comets with the Nançay radio
telescope. This allowed an evaluation of the cometary water production
rates and their evolution with time, as well as a study of several
physical processes: the excitation mechanisms of the OH radio lines,
the expansion of the cometary atmospheres, their anisotropy in
relation with non-gravitational forces, the Zeeman effect in relation
with the cometary magnetic field. The Nançay observations of 53
cometary apparitions between 1982 and 2009 are now organized in this
database. |
bdip.epn_core | Table Info | Planetary Images Database |
One Century of Planetary Images
-------------------------------
The database of planetary images (BDIP) comes from the digitization of photographs
collected and preserved by the Center for Photographic Documentation of the planets
held by the IAU at the Meudon Observatory in 1961 under the the curation of J.H. Focas
(IAUC, 12th General Assembly, Report 1964). A similar center was established at the
Lowell Observatory in Arizona, under the responsibility of W.A. Baum. The photographs
were duplicated between the two centers.
Approximately 8400 photographs of Mars, Venus, Mercury, Jupiter and Saturn, acquired
between 1890 and 1977, are kept at LESIA. They remain available for research on
justified request. The digitization of these planetary photographs was performed by
scanning between 1998 and 2000 by the staff of the Documentation Center (R. Boyer,
E. Neyvoz et al), in the framework of a project proposed to the Scientific Council
of the Paris Observatory by P. Drossart. Care was taken to preserve the best possible
definition and photometric linearity of photographs during the scanning procedure.
Storage was done using different image formats (JPEG, GIF and TIFF ie, lossy, lossless
and uncompressed). Improved techniques for mass storage and network distribution today
allow us to provide access to the highest definition images, thereby facilitating
research on the evolution of planets, at asecular time scale.
Scientific interest
-------------------
The scientific interest of the photographic database mainly concerns planetary
atmospheric evolution of Mars, Jupiter, Saturn and Venus. The evolution of the Martian
storms, or the polar caps on Mars, the survey of storms observed on Saturn, or features
like the Great Red Spot of Jupiter or oval white spots are among the subjects which
triggered on photographs. Such studies can be refined today thanks to digital pictures
(Sanchez-Lavega and Battaner, A and A Suppl. Ser., 64, 287, 1986). Some images of
Mercury are also available. |
bdip.observatories | Table Info | Observatory names |
One Century of Planetary Images
-------------------------------
The database of planetary images (BDIP) comes from the digitization of photographs
collected and preserved by the Center for Photographic Documentation of the planets
held by the IAU at the Meudon Observatory in 1961 under the the curation of J.H. Focas
(IAUC, 12th General Assembly, Report 1964). A similar center was established at the
Lowell Observatory in Arizona, under the responsibility of W.A. Baum. The photographs
were duplicated between the two centers.
Approximately 8400 photographs of Mars, Venus, Mercury, Jupiter and Saturn, acquired
between 1890 and 1977, are kept at LESIA. They remain available for research on
justified request. The digitization of these planetary photographs was performed by
scanning between 1998 and 2000 by the staff of the Documentation Center (R. Boyer,
E. Neyvoz et al), in the framework of a project proposed to the Scientific Council
of the Paris Observatory by P. Drossart. Care was taken to preserve the best possible
definition and photometric linearity of photographs during the scanning procedure.
Storage was done using different image formats (JPEG, GIF and TIFF ie, lossy, lossless
and uncompressed). Improved techniques for mass storage and network distribution today
allow us to provide access to the highest definition images, thereby facilitating
research on the evolution of planets, at asecular time scale.
Scientific interest
-------------------
The scientific interest of the photographic database mainly concerns planetary
atmospheric evolution of Mars, Jupiter, Saturn and Venus. The evolution of the Martian
storms, or the polar caps on Mars, the survey of storms observed on Saturn, or features
like the Great Red Spot of Jupiter or oval white spots are among the subjects which
triggered on photographs. Such studies can be refined today thanks to digital pictures
(Sanchez-Lavega and Battaner, A and A Suppl. Ser., 64, 287, 1986). Some images of
Mercury are also available. |
crism_speclib.epn_core | Table Info | N/A | This service provides access to the spectral library in support of
the CRISM experiment on Mars Reconnaissance Orbiter. This is a
redesigned version of the library once distributed by the PDS
Geosciences node, with data files provided as VOTable (the native
version was available at:
http://pds-geosciences.wustl.edu/mro/mro-m-crism-4-speclib-v1/mrocr_90xx/
Reference: Murchie et al (2007) Compact Reconnaissance Imaging
Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO).
JGR Planets, 112:E05S03 |
dynastvo.epn_core | Table Info | N/A | This database displays calculated orbital parameters for small bodies |
exoplanet.epn_core | Table Info | Encyclopedia of extrasolar planet | Encyclopedia of extrasolar planet |
hst_planeto.epn_core | Table Info | N/A | HST observations of planets, dwarf planets, and satellites, extracted
from the CADC database catalogue (with daily updates). Data are linked
to the CADC repository, with file names common to all HST archives.
Both calibrated and derived products are included. The main target is
identified. Physical ephemeris and thumbnails are provided when
available. Files and previews are not accessible during the
proprietary period. |
iks.epn_core | Table Info | N/A | Measurements of comet Halley in the spectral channel of IKS on board
the Vega-1 spacecraft. Data are retrieved from the PDS Small Bodies
Node data set (2011 reformatted version) and updated. The data set
consists in 101 tables providing the radiance spectrum of comet Halley
from various distances, plus two composite spectra. For details and
further references, see: Combes M. et al., 1988, The 2.5-12 micron
Spectrum of Comet Halley from the IKS-VEGA Experiment, Icarus, 76,
404-436 [1988Icar...76..404C] |
m4ast.epn_core | Table Info | compiled database for asteroid spectra in the visible and NIR regions | compiled database for asteroid spectra in the visible and NIR regions |
meteor_showers.epn_core | Table Info | N/A | The ephemeris were produced by simulating the ejection of meteoroids
from the sunlit hemisphere of cometary nuclei, typically from 0 to 3
au, followed by the propagation of orbits of meteoroids in the Solar
System, taking into account the gravity of the Sun, the 8 planets,
Pluto, and the Moon, as well as the radiation pressure and the
Poynting-Robertson drag. Note that asteroid parent bodies were
considered as active (i.e. comet-like bodies) even if they are not
active today. The showers are predicted when a planet enters a large
enough set of meteoroids, at a distance less than typically 0.01 au.
See Vaubaillon J., Colas F., Jorda L. 2005 A new method to predict
meteor showers. I. Description of the model, Astronomy and
Astrophysics, Volume 439/2 p.751-760, as well as: Vaubaillon J. 2017 A
confidence index for forecasting of meteor showers, Planetary and
Space Science, Volume 143 p.78-82 |
moonsprop.epn_core | Table Info | N/A | This service provides the physical and dynamical characteristics of
natural satellites in the Solar System: size, mass, rotational
properties, magnitude and albedo, orbital elements. These quantities
are taken from various publications listed under the bib_reference
parameter. These data will be updated as new values are published. |
planets.epn_core | Table Info | N/A | Main characteristics of Solar System planets. Data are included in
the table, which includes non-standard EPN-TAP parameters. Data are
retrieved from Archinal et al 2018 (IAU report 2015,
2018CeMDA.130...22A) [radii] and Cox et al 2000 (Allen's astrophysical
quantities, 2000asqu.book.....C) [masses, heliocentric distances, and
rotation periods]. |
spectro_asteroids.epn_core | Table Info | N/A | This service provides a compilation of spectra of asteroids in the
visible and NIR range. It is composed of various libraries distributed
as VizieR catalogues. Reformatted VOtable or fits versions are
provided with thumbnails. Ephemeris data are retrieved from Miriade
(IMCCE) for the reference date when possible. |
spectro_planets.epn_core | Table Info | N/A | This service provides a compilation of global spectra of planets and
satellites in the visible and NIR range, for quick reference purpose.
It is made from various libraries, including the
Tohoku-Hiroshima-Nagoya Planet Spectra Library (Lundock et al 2009)
and spectra from a USGS web site (R. Clark). Reformatted VOtable
versions are provided together with links to the original data. |
tap_schema.columns | Table Info | Columns in tables available for ADQL querying. | PADC TAP Server on voparis-tap-planeto.obspm.fr's Table Access Protocol (TAP) service with
table metadata. |
tap_schema.groups | Table Info | Columns that are part of groups within tables available for ADQL
querying. | PADC TAP Server on voparis-tap-planeto.obspm.fr's Table Access Protocol (TAP) service with
table metadata. |
tap_schema.key_columns | Table Info | Columns participating in foreign key relationships between tables
available for ADQL querying. | PADC TAP Server on voparis-tap-planeto.obspm.fr's Table Access Protocol (TAP) service with
table metadata. |
tap_schema.keys | Table Info | Foreign key relationships between tables available for ADQL querying. | PADC TAP Server on voparis-tap-planeto.obspm.fr's Table Access Protocol (TAP) service with
table metadata. |
tap_schema.schemas | Table Info | Schemas containing tables available for ADQL querying. | PADC TAP Server on voparis-tap-planeto.obspm.fr's Table Access Protocol (TAP) service with
table metadata. |
tap_schema.tables | Table Info | Tables available for ADQL querying. | PADC TAP Server on voparis-tap-planeto.obspm.fr's Table Access Protocol (TAP) service with
table metadata. |
titan_profiles.epn_core | Table Info | EPNcore table for temperature, pressure and element abundance profiles
in Titan's atmosphere. |
This database contains vertical profiles of temperature and composition in Titan's
atmosphere at several altitudes below 750 km. These profiles were retrieved from
the infrared spectra acquired by the Composite Infrared Spectrometer (CIRS) aboard
the Cassini spacecraft. The retrieval method and the description of the used dataset
are detailed by Vinatier et al. (2010), and completed in Mathé et al. (2020), and
Vinatier et al. (2020).
References
----------
- Vinatier et al. (**2010**) Analysis of Cassini/CIRS limb spectra of Titan acquired
during the nominal mission: I. Hydrocarbons, nitriles and CO2 vertical mixing ratio
profiles. *Icarus*, 206(2), 559-570. `doi:10.1016/j.icarus.2009.08.013
<https://doi.org/10.1016/j.icarus.2009.08.013>`_
- Mathé et al. (**2020**) Seasonal changes in the middle atmosphere of Titan
from Cassini/CIRS observations: Temperature and trace species abundance profiles
from 2004 to 2017. *Icarus*, 344, 113547. `doi:10.1016/j.icarus.2019.113547
<https://doi.org/10.1016/j.icarus.2019.113547>`_
- Vinatier et al. (**2020**), Temperature and chemical species distributions in the
middle atmosphere observed during Titan's late northern spring to early summer.
A&A 641, A116; `doi:10.1051/0004-6361/202038411
<https://doi.org/10.1051/0004-6361/202038411>`_ |
tnosarecool.epn_core | Table Info | N/A | This service lists TNO thermal properties as derived mostly from
Spitzer and Herschel observations. |
vims_satellites.epn_core | Table Info | N/A | The Visual and Infrared Mapping Spectrometer (VIMS) instrument
onboard the Cassini spacecraft observed the system of Saturn,
acquiring spectral cubes in the range 0.4-5.2 microns. This service
focuses on Saturn satellites, and provides access to calibrated and
ancillary data, computed as described here:
https://vims.univ-nantes.fr/info/isis-calibration. It also provides
direct links to a larger web site with previews. |
vvex.epn_core | Table Info | IR spectroscopy of Venus | VIRTIS/Venus Express demonstrator service: imaging spectroscopy of
Venus in the visible and the near infrared. ** Assessment version from
PI team database - some values currently missing ** This lists all
calibrated files for the total mission and the three channels M-vis,
M-IR and H. Files are described according to the PI team database,
with links to the PSA:
https://archives.esac.esa.int/psa/ftp/VENUS-EXPRESS/VIRTIS/VEX-V-VIRTIS-2-3-V3.0/.
See Piccioni et al, 2007, VIRTIS: The Visible and Infrared Thermal
Imaging Spectrometer, ESA SP 1295. |
Tablename | Info | Table desc. | Res desc. |