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Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Portions of the Palomar/DBSP optical spectrum of LkHα 225 South (magenta) compared to other young stellar objects with rare spectral signatures. Left panel highlights absorption in LkHα 225 South throughout the blue spectral range, with comparison made to the FU Ori stars V1057 Cyg and V2493 Cyg (PTF 10qpf; HBC 722). Right panel highlights the prominent TiO emission in the red, with comparison made to the bright states of PTF 10nvg (Covey et al. 2011) and VV CrA (Herczeg & Hillenbrand 2014); an example field M dwarf with TiO in absorption is also shown.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Left panel: 2003 Gemini/Near-Infrared Imager image in H2 2.12 μm. The ridge of nebulosity extending southward from LkHα 225 North, which is apparent in optical images, is present in the near-infrared, as well. Also familiar is the compact nebulosity just northeast of LkHα 225 South, which was seen in our 1999 optical image (Figure 2). Several additional extended nebulosities appear in H2 that are not seen in the optical. Right panels: spectra taken in 2003 of LkHα 225 North (labeled V1318 Cyg North) and LkHα 225 South (labeled V1318 Cyg South), during the faint state of the latter. The 1–4 μm data show a red continuum in both components of LkHα 225. Lower plots in each case highlight the K-band spectral region.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Top: ZTF r-band light curve with linear detrending performed separately for the 2018, 2019, and 2020 seasons. Color scale shows a progression of hues from earlier to later cycles. Bottom: phased light curve for a period of 43.4 days, repeated twice so as to more readily discern the full-phase shape. Larger red points are the seven data points from Magakian et al. (2019).
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: IRTF/SpeX data comparing the 2019 outburst spectrum (upper, magenta) with a version of the 2003 faint-state spectrum (lower, purple) that has been scaled (by a factor of 50) and shifted (individually in each panel). In the faint state, LkHα 225 South exhibited relatively weak atomic emission features but strong molecular emission from H2 (labeled as 2-1 or 1-0) and CO bands. During the brightening from 2003 to 2019, the LkHα 225 South infrared continuum has become bluer though it is still extremely red on an absolute scale. The line-to-continuum ratio of the weak atomic emission has increased, while the line-to-continuum of the previously prominent H2 lines has become weaker; the CO line-to-continuum appears relatively unchanged.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Left panels: comparison of LkHα 225 South (magenta) and V1057 Cyg (green) at infrared wavelengths. These sources are a reasonable match in terms of their absorption features at blue optical wavelengths in low- (Figure 6) and high- (Figure 14) spectral-resolution data. This is also true at red optical wavelengths (top panel), including the TiO emission shared by both sources. At >9000 Å, however, the spectral match is less good, with LkHα 225 South lacking the strong molecular H2O, as well as the TiO, VO, and CO absorption that is seen in V1057 Cyg at these longer wavelengths. The redward side of the J band and the H band does indicate some weak H2O, however. In addition, rather than CO absorption, LkHα 225 South has strong CO emission, as well as other atomic emission lines that are more reminiscent of other types of young-star outbursting sources. Right panels: the same LkHα 225 South spectrum as in the left panels (magenta) now compared to V2492 Cyg (blue) and Gaia 19ajj (brown). LkHα 225 South shares the weak H2O absorption in the J band and H band with Gaia 19ajj, though the TiO and VO patterns differ slightly. The CO emission of LkHα 225 South is more similar to V2492 Cyg than Gaia 19ajj, and the atomic emission-line patterns better match this source, as well. The only atomic absorption in LkHα 225 South is from Sr II (see also Figure 13), which is also seen in both V1057 Cyg and Gaia 19ajj.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Portions of the 2019 August Keck/HIRES spectrum illustrating the strong wind of LkHα 225 South via blueshifted absorption features. In the lower-right panel, the narrower Ca I absorption line validates the wavelength scale and thus our heliocentric correction to the stellar rest velocity. The Hα profile (upper-right panel) has a clear P Cygni nature, with the absorption against the emission profile extending to about −210 km s−1 on the blue side, though the emission wing continues to about −325 km s−1. The red-side emission peaks at +85 km s−1 and extends to +275 km s−1. Broad blueshifted absorption is also seen in Li I (lower-right panel), and the K I doublet, the O I triplet, the Na I D doublet lines, the Mg I b triplet lines, and among the wind-sensitive Fe II lines. The typical terminal velocity in the metal lines is −150 km s−1.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: The optical ionized calcium lines in LkHα 225 South. Top and middle panels show the permitted transitions of Ca II as seen in the Palomar/DBSP spectrum, while the bottom panel shows the forbidden transitions of [Ca II] as seen in the Keck/HIRES spectra (with uncorrected telluric absorption contamination still present in the data).
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Keck/NIRSPEC line profiles for LkHα 225 South in He I 10830 Å, H I Paγ, and Sr II. The magenta spectrum is from 2019 June while the green spectrum is from September 2020. In the He I panel, the marked Si I line at 10827 Å is unlikely to be a contributor to the observed profile, given the absence of comparable-strength Si I lines at 10844 and 10870 Å. Similarly, in the Sr II panel, the marked Mg II line at 10914 Å is unlikely to be a contributor to the observed profile, given the absence of a comparable-strength line at 10952 Å. The narrow absorption features in the Paγ and Sr II panels are uncorrected telluric lines. While the He I profile shows no change, the H I line has evolved from a P Cygni profile to pure absorption. The Sr II profile has evolved similarly. These line profiles can be compared to those exhibited by the cooler optical wind lines of Figure 11.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Portions of the 2019 August HIRES spectrum highlighting the spectral similarity of LkHα 225 South (magenta) to other outbursting sources. The absorption component in LkHα 225 South bears resemblance at shorter wavelengths (e.g., top panel) to that of the FU Ori stars V1515 Cyg, V1057 Cyg, and V2493 Cyg (PTF 10qpf, HBC 722). At longer wavelengths (e.g., bottom panel) the absorption component is less obvious, but still present in the stronger lines. Note in particular the presence of Ba II, which is atypical in nonoutbursting T Tauri or Herbig Ae/Be stars, but generally is seen in FU Ori objects. In addition to the weakening absorption component toward longer wavelengths, there is increasingly weak emission, which can be appreciated by comparison with another recent outbursting source, Gaia 19ajj. Like LkHα 225 South, this source has a mixed spectrum of absorption and emission lines in neutral metals, with overall stronger emission and weaker absorption relative to LkHα 225 South.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: Resulting peak heights from a cross-correlation of LkHα 225 South Keck/HIRES spectrum with a grid of spectral templates from the ELODIE spectral library, plotted as a function of spectral type. Right panel shows dwarf (circles) templates and left panel shows giant (squares) and supergiant (triangles) templates. Blue points are from the 4485–4600 Å region, green 5200–5285 Å, and red 6220–6275 Å. For all wavelength ranges, the best correlations are for stars in the A3–A6 spectral type range, with no clear surface gravity preference. The 5200 Å spectral range has a broad plateau of good correlation strength that extends throughout the FG and early-K spectral types.
Paper: LkHα 225 (V1318 Cyg) South in Outburst
Authors: Lynne A. Hillenbrand, Howard Isaacson, Antonio C. Rodriguez, Michael Connelley, Bo Reipurth, Michael A. Kuhn, Tracy Beck, and Diego Rodriguez Perez
Figure caption: “Corner plot” output from the Markov Chain Monte Carlo fitting procedure applied to the spectral energy distribution of LkHα 225 South that is shown in Figure 5. The preferred parameter values are given above the boxes and shown as red lines, with formal uncertainties indicated as vertical dashed lines. The units in the panels are ﹩{M}_{\odot }^{2}\,{\,\mathrm{yr}}^{-1}﹩, R⊙, and magnitudes, along the diagonal.
Paper: 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
Figure caption: TESS light curves of CVSO 109 from the 2018 (sector 6) and 2020 (sector 32) observing seasons, showing magnitude changes relative to the mean brightness in each season.
Paper: 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
Figure caption: SEDs of CVSO 109A and CVSO 109B. We show HST/STIS spectra and NIR photometry derived from X-shooter and magnitude ratios from Tokovinin et al. (2020). For comparison, we plot a combined STIS+X-Shooter WTTS spectrum used in Section 6.1.1. The spectrum is smoothed for clarity.
Paper: 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
Figure caption: Left: optical light curves of CVSO 109. Data from Konkoly Observatory, AAVSOnet, OACt, and ASAS-SN are denoted with circles, squares, triangles, and stars. Vertical dashed and dotted lines mark the epochs of HST and VLT observations. In the bottom panel, the black curve displays the TESS data. Upper right: color–magnitude diagram for CVSO 109. Lower right: color–color diagram for CVSO 109. In the right panels, lines fitted to the data points are also plotted. The short lines in the upper-right panel indicate how an increase of 0.2 mag in AV would change the colors for R = 3.1 (solid lines) or for R = 5 (dotted lines).
Paper: 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
Figure caption: An Hα profile and two residual profiles from the three CHIRON spectra obtained on a daily cadence. These were obtained approximately 12 hr before, 12 hr after, and 36 hr after the HST spectra. We refer to these as days −1, 0, and +1, respectively. The black spectrum is the continuum-subtracted profile of Hα on day 1, 1.5 days after the HST observations (day 1). This profile is symmetric; we use it as a reference. This line flux peaks at 6.3 in these units (7.3 continuum units). The other spectra are normalized to the continua, and the reference spectrum is subtracted. The residual spectrum taken before the HST observations (day –1, in blue) shows a modest flux increase near line center and an inverse P Cygni profile, suggestive of infalling gas. Twelve hours after the HST observations (day 0, magenta), the residual spectrum is brighter and broadened to the red. Figure 5 shows that the Hα emission was brighter during the UVES spectrum, obtained closer to the time of the HST spectrum. These velocities are heliocentric and are not corrected for the stellar RV, which is insignificant on this scale.
Paper: 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
Figure caption: Hα EW derived from the color index measured at OACt (dots) over one month (top) and zoomed into a 15 day interval (bounded by the blue lines on the top plot) to highlight the epoch of HST observations. The scale of the color index is shown in the right vertical axis. The Hα EW measured on X-shooter, UVES, CHIRON, and McDonald spectra are overplotted with different symbols as indicated in the legend. A zoom around the HST observations (cyan hatched area) is displayed in the lower box.
Paper: 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
Figure caption: 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.
Paper: 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
Figure caption: 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).
Paper: 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
Figure caption: The extended accretion flow model fit to CHIRON spectrum of CVSO 109 in Hα (left) and Hβ (right) observed on MJD = 59181.70. The observation is shown in blue. The template photosphere and chromosphere, shown as dashed orange lines, are from UVES observation of the M0 WTTS TWA 25. The light gray lines are 100 best fits, and the red lines and the dashed–dotted black lines are the average magnetospheric profiles and the total magnetosphere + chromosphere + photosphere model profiles, respectively.