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GalPaK3D: A BAYESIAN PARAMETRIC TOOL FOR EXTRACTING MORPHOKINEMATICS OF GALAXIES FROM 3D DATA

  • Authors: N. Bouché, H. Carfantan, I. Schroetter, L. Michel-Dansac, and T. Contini

2015 The Astronomical Journal 150 92.

  • Provider: AAS Journals

Caption: Figure 2.

Example of the algorithm application on a disk model simulated with a seeing of 1.″0 (FWHM), a flux of 10−16 erg s−1 cm−2, and an S/N pixel−1 of ∼4 at the brightest pixel. The top, middle, and bottom rows show the flux map, the velocity map, and the apparent velocity profile Vz(r) across the major axis, respectively. From left to right, the panel columns show the data, the convolved model, the modeled disk (free from the PSF), and the high-S/N, high-resolution reference data (PSF = 0.″15 and S/N = 100). In the bottom panels, the solid red curves correspond to the reference case, the triangles represent the apparent rotation curve, and the dotted lines show the apparent ﹩{V}_{\mathrm{max}}\;\mathrm{sin}i﹩. One sees that the velocity profile from the modeled disk (third column) is in good agreement with the reference data.

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