Figure 7 from The ODYSSEUS Survey. Motivation and First Results: Accretion, Ejection, and Disk Irradiation of CVSO 109

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The ODYSSEUS Survey. Motivation and First Results: Accretion, Ejection, and Disk Irradiation of CVSO 109

Authors: C. C. Espaillat, G. J. Herczeg, T. Thanathibodee, C. Pittman, N. Calvet, N. Arulanantham, K. France, Javier Serna, J. Hernández, Á. Kóspál, F. M. Walter, A. Frasca, W. J. Fischer, C. M. Johns-Krull, P. C. Schneider, C. Robinson, Suzan Edwards, P. Ábrahám, Min Fang, J. Erkal, C. F. Manara, J. M. Alcalá, E. Alecian, R. D. Alexander, J. Alonso-Santiago, Simone Antoniucci, David R. Ardila, Andrea Banzatti, M. Benisty, Edwin A. Bergin, Katia Biazzo, César Briceño, Justyn Campbell-White, L. Ilsedore Cleeves, Deirdre Coffey, Jochen Eislöffel, Stefano Facchini, D. Fedele, Eleonora Fiorellino, Dirk Froebrich, Manuele Gangi, Teresa Giannini, K. Grankin, Hans Moritz Günther, Zhen Guo, Lee Hartmann, Lynne A. Hillenbrand, P. C. Hinton, Joel H. Kastner, Chris Koen, K. Maucó, I. Mendigutía, B. Nisini, Neelam Panwar, D. A. Principe, Massimo Robberto, A. Sicilia-Aguilar, Jeff A. Valenti, J. Wendeborn, Jonathan P. Williams, Ziyan Xu, and R. K. Yadav

2022 The Astronomical Journal 163 114.

Provider: AAS Journals

Caption: Figure 7.

Profile of the C IV 1549 line in the CVSO 109A spectrum. The observed profile (blue) has been boxcar smoothed by 3 pixels. The upper panel shows the model line profile emitted by the postshock regions of columns with energy flux log ﹩{ \mathcal F }=10﹩ (red), 11 (green), and 12 (brown), weighted by the filling factors that explain the NUV–NIR continuum (Figure 6). The total model line profile is shown in orange. The lower panel shows again the observed profile and the total postshock emission. A Gaussian with mean RV of +80 km s⁻¹ and width 100 km s⁻¹ (dark green) added to the total postshock emission can approximately explain the observed profile (light green).

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