Figure 6 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 6.

Fitting the NUV–NIR continuum of CVSO 109A. We show the HST and X-shooter spectra (black) along with the photospheric template (dark blue), which is scaled using optical veiling derived by X-shooter. The parameters of the best-fitting model (red solid line) are listed in Table 4. The best-fit model is a combination of the accretion shock model (consisting of the three columns with energy fluxes of 1 × 10¹⁰, 1 × 10¹¹, and 1 × 10¹² erg s⁻¹ cm⁻², each with filling factors shown in parentheses in the legend; cyan, sea-green, and brown solid lines, respectively) and the D’Alessio et al. Irradiated Accretion Disk (DIAD) model (consisting of the emission from the inner wall; dashed line). Emission lines and regions strongly affected by telluric absorption were excluded from the fit. The gaps in the NIR spectra are the telluric regions, which are omitted from the plot to improve the readability of the figure.

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