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Contents
Contents
The homogeneous Ariel stellar catalogue currently includes the following parameters:
Identification parameters
Photometric properties
Kinematics properties (galactic positions, velocities, parallaxes)
Effective temperature, surface gravity and [Fe/H]
vsin(i), vmicro
Mass*, Radius, age
Abundances of C, N, O for 181 stars
*Notes: the stellar mass is always updated for all the stars anytime a release is done. This means that, for instance, following the constant development of the code (Bossini et al, in prep.) stellar masses for the targets initially included in Magrini et al, 2022 have been updated (with respect to the values reported in the paper).
The catalogue can be downloaded in .csv file here.
Details for the columns in the file can be found here.
Foreseen updates
Foreseen updates
Homogeneous:
stellar ages for 353 stars (Bossini et al) ;
logR'HK for 200+ stars (Wizani et al) ;
parameters for 18 very hot stars (Ramler et al.)
limb darkening coefficients for 353 stars (both claret-4; power2 laws)
How to compute the stellar elemental abundance ratio ?
How to compute the stellar elemental abundance ratio ?
In the table we are providing the elemental abundances over hydrogen (by number), in the usual from A(El)=12+log(n(El)/N(H)) where n(El) is number density of the element El (i.e., the number of atoms of that element per unit volume) and n(H) is the number density of H .
To compute their ratio on the solar scale you have to:
[El/H]=A(El)−A(El)_Sun
To compute the abundance ratio over Fe on the solar scale:
[El/Fe]=A(El)-[Fe/H] - A(El)_Sun=[El/H]-[Fe/H]
To compute the abundance ratio (on a logarithmic scale) of two elements (without normalisation to the Sun):
log(El1/El2)=A(El1)- A(El2)
e.g. log(N/O)=A(N)-A(O)
This is particularly relevant when you want to normalise the planetary abundances, to its own stellar ones, to check for chemical enrichment of the planet and infer the planetary location formation within the context of its own planetary system.
The adopted solar abundances for C, N and O are:
A(C)_Sun = 8.43
A(N)_Sun = 7.83
A(O)_Sun = 8.69
Kiel diagram
Kiel diagram
Kiel diagram for the Ariel Stellar Catalogue sample as a function of PARSEC isochrones at solar metallicity (Z = 0.013, in purple) and at super-solar metallicity (Z = 0.06, in red)
(Tsantaki et al., in press)
Toomre diagram
Toomre diagram
The separation of the Ariel sample in the Galactic disc based on their kinematics. Stars within the blue circle belong to the thin disc, stars within the red annulus are transitioning between thin and thick, and stars within the purple belong to the thick disc.
(Tsantaki et al., in press)
Galactic planetary population
Galactic planetary population
Cumulative distribution functions for the three planetary mass populations hosted by the stars in the Ariel Stellar Catalogue. The gray dashed line shows the limit of 0.2 Mj to separate between low mass and giant planets. In the currently analysed Ariel sample of transiting planets, the smallest planets orbit mostly thick disc stars.
(Tsantaki et al., in press)
Acknowledgments
Acknowledgments
for publications
for publications
When using this catalogue, please acknowledge this web site and include the following statement into your manuscript:
"This work made use of the Ariel Stellar Catalogue developed by the Stellar Characterisation WG in preparation of the ESA Ariel space mission"
Depending on whether your are using atmospheric parameters, elemental abundances, etc, please make sure to include the references to the team relevant publications (here).
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