Data¶
On this page you find a list of the supported data. Please give credit to the relevant references when using any of the external data in a publication. Support for other datasets can be requested by creating an issue on the GitHub page.
Atmospheric models¶
Model |
$T_\mathrm{eff}$ range |
$\lambda/\Delta\lambda$ |
Wavelength range |
Reference |
Tag |
|---|---|---|---|---|---|
\([100, 6600]\,\mathrm{K}\) |
\(2000\) |
\([0.5, 40]\,\mu\mathrm{m}\) |
Allard et al. (2001) |
ames-cond |
|
\([500, 4000]\,\mathrm{K}\) |
\(2000\) |
\([0.5, 40]\,\mu\mathrm{m}\) |
Allard et al. (2001) |
ames-dusty |
|
\([200, 3000]\,\mathrm{K}\) |
\(1000\) |
\([0.2, 2000]\,\mu\mathrm{m}\) |
Phillips et al. (2020) |
atmo |
|
\([200, 3000]\,\mathrm{K}\) |
\(2000\) |
\([0.2, 2000]\,\mu\mathrm{m}\) |
Phillips et al. (2020) |
atmo-ceq |
|
\([200, 1800]\,\mathrm{K}\) |
\(2000\) |
\([0.2, 2000]\,\mu\mathrm{m}\) |
Phillips et al. (2020) |
atmo-neq-strong |
|
\([200, 1800]\,\mathrm{K}\) |
\(2000\) |
\([0.2, 2000]\,\mu\mathrm{m}\) |
Phillips et al. (2020) |
atmo-neq-weak |
|
\([800, 3000]\,\mathrm{K}\) |
\(3000\) |
\([0.2, 30]\,\mu\mathrm{m}\) |
Petrus et al. (2023) |
atmo-petrus2023 |
|
\([800, 3000]\,\mathrm{K}\) |
\(10000\) |
\([0.2, 2.5]\,\mu\mathrm{m}\) |
Petrus et al. (2023) |
atmo-petrus2023-highres |
|
\([10, 20000]\,\mathrm{K}\) |
\(1000\) |
\([0.1, 5000]\,\mu\mathrm{m}\) |
Planck (1901) |
blackbody |
|
\([800, 4000]\,\mathrm{K}\) |
\(5000\) |
\([0.1, 100]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-cond |
|
\([2600, 4000]\,\mathrm{K}\) |
\(5000\) |
\([0.1, 100]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-cond-feh |
|
\([1000, 4000]\,\mathrm{K}\) |
\(5000\) |
\([0.1, 100]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-dusty |
|
\([2600, 30000]\,\mathrm{K}\) |
\(2000\) |
\([0.1, 5000]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-nextgen |
|
\([2600, 30000]\,\mathrm{K}\) |
\(200000\) |
\([0.1, 50]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-nextgen-highres |
|
\([2600, 30000]\,\mathrm{K}\) |
\(500000\) |
\([0.1, 1.0]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-nextgen-optical |
|
\([2600, 30000]\,\mathrm{K}\) |
\(2000\) |
\([0.1, 50]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-nextgen-subsolar |
|
\([400, 4000]\,\mathrm{K}\) |
\(2000\) |
\([0.1, 500]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-settl |
|
\([1200, 7000]\,\mathrm{K}\) |
\(10000\) |
\([0.1, 5000]\,\mu\mathrm{m}\) |
Allard et al. (2012) |
bt-settl-cifist |
|
\([1000, 3000]\,\mathrm{K}\) |
\(2000\) |
\([0.1, 500]\,\mu\mathrm{m}\) |
Helling et al. (2008) |
drift-phoenix |
|
\([400, 2000]\,\mathrm{K}\) |
\(500\) |
\([0.34, 250.0]\,\mu\mathrm{m}\) |
Charnay et al. (2018) |
exo-rem-lowres |
|
\([200, 1950]\,\mathrm{K}\) |
\(500\) |
\([0.34, 250.0]\,\mu\mathrm{m}\) |
Charnay et al. (2018) |
exo-rem-nocloud |
|
\([400, 2000]\,\mathrm{K}\) |
\(20000\) |
\([0.7, 250.0]\,\mu\mathrm{m}\) |
Charnay et al. (2018) |
exo-rem-highres |
|
\([400, 2000]\,\mathrm{K}\) |
\(20000\) |
\([0.7, 250.0]\,\mu\mathrm{m}\) |
Charnay et al. (2018) |
exo-rem-highres-isotopes |
|
\([5000, 80000]\,\mathrm{K}\) |
\(1000\) |
\([0.1, 3]\,\mu\mathrm{m}\) |
Koester (2010) |
koester-wd |
|
\([200, 600]\,\mathrm{K}\) |
\(4000\) |
\([0.4, 300]\,\mu\mathrm{m}\) |
Lacy & Burrows (2023) |
lacy2023-clear-eq |
|
\([200, 600]\,\mathrm{K}\) |
\(4000\) |
\([0.4, 300]\,\mu\mathrm{m}\) |
Lacy & Burrows (2023) |
lacy2023-clear-neq |
|
\([200, 450]\,\mathrm{K}\) |
\(4000\) |
\([0.4, 300]\,\mu\mathrm{m}\) |
Lacy & Burrows (2023) |
lacy2023-cloudy-thick-eq |
|
\([200, 450]\,\mathrm{K}\) |
\(4000\) |
\([0.4, 300]\,\mu\mathrm{m}\) |
Lacy & Burrows (2023) |
lacy2023-cloudy-thick-neq |
|
\([200, 450]\,\mathrm{K}\) |
\(4000\) |
\([0.4, 300]\,\mu\mathrm{m}\) |
Lacy & Burrows (2023) |
lacy2023-cloudy-thin-eq |
|
\([200, 450]\,\mathrm{K}\) |
\(4000\) |
\([0.4, 300]\,\mu\mathrm{m}\) |
Lacy & Burrows (2023) |
lacy2023-cloudy-thin-neq |
|
\([400, 1300]\,\mathrm{K}\) |
\(6000\) |
\([0.6, 30]\,\mu\mathrm{m}\) |
Morley et al. (2012) |
morley2012 |
|
\([500, 1000]\,\mathrm{K}\) |
\(1000\) |
\([0.1, 250]\,\mu\mathrm{m}\) |
Mollière et al. (2015) |
petitcode-cool-clear |
|
\([500, 850]\,\mathrm{K}\) |
\(1000\) |
\([0.1, 250]\,\mu\mathrm{m}\) |
Mollière et al. (2015) |
petitcode-cool-cloudy |
|
\([1000, 2000]\,\mathrm{K}\) |
\(1000\) |
\([0.1, 250]\,\mu\mathrm{m}\) |
Mollière et al. (2015) |
petitcode-hot-clear |
|
\([1000, 2000]\,\mathrm{K}\) |
\(1000\) |
\([0.1, 250]\,\mu\mathrm{m}\) |
Mollière et al. (2015) |
petitcode-hot-cloudy |
|
\([150, 1000]\,\mathrm{K}\) |
\(1000\) |
\([0.1, 250]\,\mu\mathrm{m}\) |
Linder et al. (2019) |
petitcode-linder2019-clear |
|
\([150, 1000]\,\mathrm{K}\) |
\(1000\) |
\([0.1, 250]\,\mu\mathrm{m}\) |
Linder et al. (2019) |
petitcode-linder2019-cloudy |
|
\([2300, 12000]\,\mathrm{K}\) |
\(20000\) |
\([0.09, 30]\,\mu\mathrm{m}\) |
Hauschildt et al. (2025) |
phoenix-hauschildt2025 |
|
\([2300, 12000]\,\mathrm{K}\) |
\(20000\) |
\([0.5, 5]\,\mu\mathrm{m}\) |
Husser et al. (2013) |
phoenix-husser2013 |
|
\([500, 2400]\,\mathrm{K}\) |
\(6000\) |
\([0.4, 50]\,\mu\mathrm{m}\) |
Saumon & Marley (2008) |
saumon2008-clear |
|
\([500, 2400]\,\mathrm{K}\) |
\(6000\) |
\([0.4, 50]\,\mu\mathrm{m}\) |
Saumon & Marley (2008) |
saumon2008-cloudy |
|
\([500, 1300]\,\mathrm{K}\) |
\(5000\) |
\([1, 250]\,\mu\mathrm{m}\) |
Karalidi et al. (2021) |
sonora-cholla |
|
\([200, 2400]\,\mathrm{K}\) |
\(5000\) |
\([0.4, 50]\,\mu\mathrm{m}\) |
Marley et al. (2021) |
sonora-bobcat |
|
\([200, 2400]\,\mathrm{K}\) |
\(5000\) |
\([0.4, 50]\,\mu\mathrm{m}\) |
Marley et al. (2021) |
sonora-bobcat-co |
|
\([1300, 2400]\,\mathrm{K}\) |
\(60000\) |
\([0.6, 15]\,\mu\mathrm{m}\) |
Mukherjee et al. (2023) |
sonora-elfowl-l |
|
\([575, 1200]\,\mathrm{K}\) |
\(60000\) |
\([0.6, 15]\,\mu\mathrm{m}\) |
Mukherjee et al. (2023) |
sonora-elfowl-t |
|
\([275, 550]\,\mathrm{K}\) |
\(60000\) |
\([0.6, 15]\,\mu\mathrm{m}\) |
Mukherjee et al. (2023) |
sonora-elfowl-y |
|
\([900, 2400]\,\mathrm{K}\) |
\(6000\) |
\([0.3, 250]\,\mu\mathrm{m}\) |
Morley et al. (2024) |
sonora-diamondback |
|
\([900, 2400]\,\mathrm{K}\) |
\(30000\) |
\([0.3, 250]\,\mu\mathrm{m}\) |
Morley et al. (2024) |
sonora-diamondback-highres |
|
\([2000, 4000]\,\mathrm{K}\) |
\(250\) |
\([0.1, 20]\,\mu\mathrm{m}\) |
Iyer et al. (2023) |
sphinx |
Tip
The available_models() method of the Database class can be used for printing a detailed overview of all available model grids:
from species import SpeciesInit
from species.data.database import Database
SpeciesInit()
database = Database()
database.available_models()
Tip
It is also possible to add your own custom grid of model spectra with add_custom_model().
Evolutionary models¶
Spectral libraries¶
NIR spectra of young M/L dwarfs by Allers & Liu (2013)
NIR spectra of young M/L dwarfs by Bonnefoy et al. (2014)
Photometric libraries¶
Photometry from S. Leggett
Magnitudes, stellar properties, and other parameters of directly imaged planets and brown dwarfs
Parallaxes, photometry, and spectra from the SIMPLE database
Calibration¶
Filters from the Filter Profile Service
Dust extinction¶
Extinction models from dust-extinction
Dust cross sections computed with PyMieScatt
Optical constants from Mollière et al. (2019)