Plot type:
Histogram bins the data by a single field and displays count of objects per bin.
Heatmap bins the data by two fields and displays count as color.
Conditional distribution bins the data by one field and displays the distribution of a second field within that bin as a boxplot (range and quartiles).
Shows a scatterplot of a (random subset) of actual data points.

For log functionality, set the filter to enable only positive values.

For log functionality, set the filter to enable only positive values.

For log functionality, set the filter to enable only positive values.

Count:
Choose whether the object count per bin is shown in linear or log scale.
Count is shown on the Y axis.
Count is shown on the color (Z) axis.

Use "*" as wildcard

Examples:{{ bucket.key }}

Range:

{{filter.render(filter.aggs.min)}}

{{filter.render(filter.aggs.max)}}

Select field to filter

Example python code to apply the above filters and retrieve data. To use, download and install this module.

Field | Variable | Type | Units | Description |
---|---|---|---|---|

model | model | byte | ||

snapshot | snapshot | short | ||

time | time | float | ||

Mass | Mass | float | \(M_\odot\) | particle mass |

position | float | kpc | ||

x | x | float | kpc | position in x |

y | y | float | kpc | position in y |

z | z | float | kpc | position in z |

velocity | float | kpc | ||

v_x | v_x | float | km/s | velocity in x |

v_y | v_y | float | km/s | velocity in y |

v_z | v_z | float | km/s | velocity in z |

ID | ID | long | particle ID | |

J_R | J_R | float | km/s kpc | radial action |

J_phi | J_phi | float | km/s kpc | azimuthal action |

J_z | J_z | float | km/s kpc | vertical action |

Omega_R | Omega_R | float | km/s /kpc | radial frequency |

Omega_phi | Omega_phi | float | km/s /kpc | azimuthal frequency |

Omega_z | Omega_z | float | km/s /kpc | vertical frequency |

Theta_R | Theta_R | float | radians | radial angle |

Theta_phi | Theta_phi | float | radians | azimuthal angle |

Theta_z | Theta_z | float | radians | vertical angle |

R | R | float | kpc | Galactocentric radius |

phi | phi | float | radians | Galactocentric azimuth |

v_R | v_R | float | km/s | Galactocentric radial velocity |

v_phi | v_phi | float | km/s | Galactocentric azimuthal velocity |

The simulations presented here are Models D1, D2, M1 and M2 from Hunt et al. (2021). They are freely available, but please cite Hunt et al. (2021) if you use them! Currently available are the snapshots presented in the paper, but we intend to make the full time evolution available (at 9.77 Myr intervals) available shortly.

For the dark matter particles we provide x, y, z (kpc), v_x, v_y, v_z (km/s), mass (Solar mass), and particle ID. For the stellar particles, we provide as above, but also include actions, angles and frequencies derived with Agama (Vasiliev 2019): J_R, J_phi, J_z (kpc km/s), theta_R, theta_phi, theta_z (radians) and Omega_R, Omega_phi, Omega_z (km/s /kpc).

Model D1 is an isolated Milky Way like disc galaxy based on Model MWb from Widrow & Dubinski (2005). It remains stable against bar and spiral formation for several Gyr. We present snapshot 200 on Flathub for comparison with the merger model M1 as an example of the un-perturbed galaxy.

Model D2 is an isolated disc galaxy based on Model MWa from Widrow & Dubinski (2005). It forms a bar and transient spiral structure. We present snapshot 549 on Flathub for comparison with the merger model M2 as an example of the un-perturbed galaxy.

Model M1 is the merger of the L2 dwarf galaxy from Laporte et al. (2018) into Model D1. This is an excellent test case for the structure and kinematics induced by the merger, as the disc otherwise remains stable. We present step 702 on Flathub as the `present day’ snapshot, where the dwarf is closest to the location of Sgr in the Milky Way.

Model M2 is the merger of the L2 dwarf galaxy from Laporte et al. (2018) into Model D2. This is a violent merger which creates a thick disc and inner halo from the dwarf remnant. We present snapshot 557 on Flathub as the ‘final’ state of the system.

Note that these models are not intended to be accurate reproductions of the Milky Way - Sgr system, merely test cases for the dynamical processes involved in Disc-dwarf mergers. See Bennet, Bovy & Hunt (2021) for our attempts to better match observations of the Milky Way - Sagittarius dwarf galaxy merger.

More under:

model | snapshot | time |
Mass
\(M_\odot\) particle mass |
position kpc | velocity kpc | ID particle ID |
J_R
km/s kpc radial action |
J_phi
km/s kpc azimuthal action |
J_z
km/s kpc vertical action |
Omega_R
km/s /kpc radial frequency |
Omega_phi
km/s /kpc azimuthal frequency |
Omega_z
km/s /kpc vertical frequency |
Theta_R
radians radial angle |
Theta_phi
radians azimuthal angle |
Theta_z
radians vertical angle |
R
kpc Galactocentric radius |
phi
radians Galactocentric azimuth |
v_R
km/s Galactocentric radial velocity |
v_phi
km/s Galactocentric azimuthal velocity |
||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|

x kpc position in x | y kpc position in y | z kpc position in z | v_x km/s velocity in x | v_y km/s velocity in y | v_z km/s velocity in z |