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The X3D Pathway

Github repository associated with Vogt+, ApJ 818, 115 (2016) & Vogt+, PASP (2017)

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Interactive HTML with Python and X3D: YSNR 1E0102.2-7219
Created Sept.-Oct. 2016 by F.P.A.Vogt.
Questions, comments :
If you find this code useful for your research, please cite the following articles accordingly:

Vogt, Owen, Verdes-Montenegro & Borthakur, Advanced Data Visualization in Astrophysics: the X3D Pathway, ApJ 818, 115 (2016). (arXiv; ADS)
Vogt, Seitenzahl, Dopita & Ruiter, Linking to X3D pathway to integral field spectrographs: YSNR 1E 0102.2-7219 in the SMC as a case study, PASP (2017). (arXiv; ADS)

The interactive model below shows the three-dimensional (3-D) spatial distribution of the oxygen-rich ejecta in the Young Supernova Remnant (YSNR) 1E 0102.2-7219 (1E0102 in short) located in the Small Magellanic Cloud (SMC). This 3-D map was reconstructed from dedicated observations of 1E 0102 using the WiFeS integral field spectrograph mounted on the ANU 2.3m telescope at Siding Spring Observatory (NSW, Australia) in August 2016 (P.I.: Seitenzahl). The 3-D reconstruction procedure only assumes a free expansion of the ejecta since the supernova explosion 2050 yr ago, and a distance to the SMC of 62 kpc.

The 3-D map itself was generated from the WiFeS mosaic (initially in fits format) using the Mayavi Python module, and directly exported to the x3d file format, following the approach introduced in Vogt et al. (2016). For the detailed scientific analysis of this dataset, see Seitenzahl+ (in preparation). The central gap in the model (0.4 pc thick) corresponds to the spectral range 5007.816 Å → 5010.939 Å: the rest-frame [OIII] spectral range in the SMC. This area is contaminated by background [OIII] emission that fills the full spatial extent of the mosaic, and which was cropped off from this 3-D map for clarity purposes.

This interactive version of the 3-D map relies on the X3DOM (pronounced "X-Freedom") framework for its integration within HTML documents. Dedicated interaction buttons allow to select pre-set views of the model, add clip planes, take screenshots, toggle the reference spheres on or off, and "peel" the intensity layers of the O-rich ejecta. For each clip plane, the value \(\Delta d\) indicates in pc the distance between the given clip plane and the model center (i.e. the supernova explosion site), indicated with a black sphere of 1 pc in diameter. The supernova location is derived from the ejecta proper-motion and anchored to the SMC rest-frame for the depth. The two spheres of 6 pc and 12 pc in diameters (respectively) are included as spatial scale references. Finally, the red arrow points towards the Earth (located 62 kpc away), the green arrow points North, and the Blue arrow points East.

Typical loading time (dependant on connectivity speed): 5-30s.

The model below is based on WiFeS observations. To see the (improved) model based on MUSE observations of the same target, go check out this page.


Outer flux density level:3.5 \( \times10^{-17} \text{ erg s}^{-1} \text{ cm}^{-2}\ \AA^{-1}\)  

Reference spheres:


Clip planes:

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