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2 results for “T Tauri stars”
FitteR for Accretion ProPErties of T Tauri stars (FRAPPE): A new approach to use Class III spectra to derive stellar and accretion properties (Additional Plots)
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Data from "Large-scale CO spirals and complex kinematics associated with the T Tauri star RU Lup"
<p>Image cubes, self-calibrated visibilities, and self-calibration and imaging scripts for data from Huang et al., 2020, "Large-scale CO spirals and complex kinematics associated with the T Tauri star RU Lup," ApJ, 898, 140 (arXiv:2007.02974) </p> <p>The raw ALMA data can be found at the ALMA archive under program ID 2018.1.01201.S (PI: Jane Huang).</p> <p><strong>Scripts:</strong></p> <p>selfcal_C43-5.py, selfcal_C43-2.py, selfcal_ACA.py: self-calibration scripts for observation of RU Lup in various ALMA configurations</p> <p>imaging.py: imaging script used for all lines</p> <p>reductionutils.py can be downloaded from <a href="https://zenodo.org/record/3628656">https://zenodo.org/record/3628656</a></p> <p><strong>Measurement sets:</strong></p> <p>RULupcontinuum.ms.tgz: Continuum visibilities for "RULupallcontinuum.image.pbcor.fits" (the high-resolution ALMA continuum data can be found on the <a href="https://bulk.cv.nrao.edu/almadata/lp/DSHARP/">DSHARP</a> page)</p> <p>RULup_12CO.ms.contsub.tgz: Continuum-subtracted visibilities for the <sup>12</sup>CO J=2-1 line toward RU Lup</p> <p>RULup_12CO_nocontsub.ms.tgz: Visibilities for the <sup>12</sup>CO J=2-1 line (no continuum subtraction) toward RU Lup, used to make the 'RULup_12COpeakintensity.fits' file.</p> <p>RULup_13CO.ms.contsub.tgz: Continuum-subtracted visibilities for the <sup>13</sup>CO J=2-1 line toward RU Lup</p> <p>RULup_C18O.ms.contsub.tgz: Continuum-subtracted visibilities for the C<sup>18</sup>O J=2-1 line toward RU Lup</p> <p>RULup_DCOp.ms.contsub.tgz: Continuum-subtracted visibilities for the DCO<sup>+</sup> J=3-2 line toward RU Lup</p> <p><strong>Images: </strong></p> <p>RULup12CO.1sigcut.pbcor.mom0.fits: Integrated intensity map of <sup>12</sup>CO J=2-1 appearing in Fig. 1</p> <p>RULup12CO.pbcor.mom1.fits: <sup>12</sup>CO J=2-1 intensity-weighted velocity map appearing in Fig. 1</p> <p>RULup13CO.pbcor.mom0.fits: Integrated intensity map of <sup>13</sup>CO J=2-1 appearing in Fig. 1</p> <p>RULup13CO.pbcor.mom1.fits: <sup>13</sup>CO J=2-1 intensity-weighted velocity map appearing in Fig. 1</p> <p>RULupC18O.pbcor.mom0.fits: Integrated intensity map of C<sup>18</sup>O J=2-1 appearing in Fig. 1</p> <p>RULupC18O.pbcor.mom1.fits: C<sup>18</sup>O J=2-1 intensity-weighted velocity map appearing in Fig. 1</p> <p>RULup12CO.image.pbcor.fits: <sup>12</sup>CO J=2-1 image cube appearing in Fig. 2</p> <p>RULupC18O.image.pbcor.fits: C<sup>18</sup>O J=2-1 image cube appearing in Fig. 2</p> <p>RULup13CO.image.pbcor.fits: <sup>12</sup>CO J=2-1 image cube appearing in Fig. 3</p> <p>RULup_12COpeakintensity.fits: Peak intensity image of <sup>12</sup>CO used to make Figure 4</p> <p>RULupDCOp.pbcor.mom0.fits: Integrated intensity map of DCO<sup>+</sup> J=3-2 appearing in Fig. 10</p> <p>RULupDCOp.image.pbcor.fits: DCO<sup>+</sup> J=3-2 image cube appearing in Fig. 11</p> <p>RULupallcontinuum.image.pbcor.fits: Continuum image appearing in Fig. 12</p> <p>RULup12COinitial.mask.image.fits: <sup>12</sup>CO CLEAN mask shown in Fig. 13</p> <p> </p>
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