adsabs/AstroCLIMB huggingface dataset:
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Left panel: ﹩{\bar{\lambda }}_{x}-\delta {\lambda }_{\mathrm{red}}﹩ for the w2 and w1 filters as a function of (B − V)0 for a Planck function. Right panel: shift on ﹩{\bar{\lambda }}_{x}﹩ induced by reddening with ﹩{R}_{V}^{\mathrm{host}}=3.1﹩ as a function of the total reddening.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Top panel: α  S  against ﹩t-{t}_{V}^{\mathrm{peak}}﹩ for S = BVriJHK. Bottom-left panel: α  S  values shifted by δ α  S , where the solid line is a straight line fit corresponding to ﹩{{\rm{\Psi }}}_{0,{\alpha }_{S}}﹩. Bottom-right panel: inverse CDF for the ﹩{\delta }_{{\alpha }_{S}}﹩ values, where the solid line is the mean value. Dashed lines are ﹩\pm 1\,\hat{\sigma }﹩ limits, and error bars are 1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption:  V − i color curves of SNe IIb corrected for MW reddening and K-correction (top panel), and shifted by δ  V−i  (middle panel). The solid line is a quadratic fit, corresponding to Ψ0,V−i , while dashed lines indicate the ﹩\pm 2\,\hat{\sigma }﹩ limits. Bottom panel: cumulative distribution for the δ  V−i  values. Error bars are 1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption:                          ﹩{\tilde{E}}_{B-V}﹩ vs. EWNaID for SNe IIb (top-left panel), Ib (top-right panel), and Ic (bottom-left panel). Bottom-right panel: host-galaxy reddening vs. EWNaID. Solid and dashed lines are linear fits and ﹩1\,\hat{\sigma }﹩ limits, respectively. Error bars indicate ±1σ errors.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Histograms for the E  B−V  values of the SNe IIb, Ib, and Ic in our sample, and of the SNe II in the sample of Rodríguez et al. (2021). Dashed lines indicate median values, while red triangles mark the locations of the outliers.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Intrinsic B − V color curves (solid lines) estimated in this work (blue) and in Stritzinger et al. (2018a; red). Dashed lines are ﹩\pm 1\,\hat{\sigma }﹩ limits, while error bars represent the error on (B − V)0 due to the intrinsic uncertainty and ﹩{\mathrm{ZP}}_{{E}_{B-V}}﹩ error.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption:                          ﹩{M}_{r}^{\mathrm{peak}}﹩ against μ for SNe IIb, Ib, and Ic. Dashed lines correspond to r peak = 〈r peak〉, and dotted lines are the limits for the volume-limited samples.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Optical/IR spectra of SN 2011dh at −3 (top panel) and 70 days (bottom panel) from ﹩{t}_{V}^{\mathrm{peak}}﹩. Colored symbols are the monochromatic fluxes estimated with the magnitudes computed from the spectra.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Cumulative distributions for the ﹩{M}_{r}^{\mathrm{peak}}﹩ values in the volume-limited samples (thick lines) and the samples used to compute the zero-points of the reddening scales (thin lines). Numbers in parentheses are the sample sizes.
Paper: The Iron Yield of Core-collapse Supernovae
Authors: Ósmar Rodríguez, Dan Maoz, Ehud Nakar
Figure caption: Ψ0,c  curves for different colors of SNe IIb (blue solid lines), Ib (green dashed lines), and Ic (red dotted lines). Error bars indicate the ﹩\pm 1\,\hat{\sigma }﹩ limits around the curves.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the phase dispersion minimization periodogram for the HD 377 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 5 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 202917 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 1 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 35650 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 5 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 53143 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 1 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 145560 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 12 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 23484 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 31 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 202628 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 1 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 35841 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 5 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 166 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 17 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: HAWC significance map (2° × 2°) centered at the centroid of eHWC J2019+368. The eHWC J2019+368 flux extraction region is marked with a dashed circle (radius 0.°5). PSR J2021+3651 and Sh 2-104 are marked with a star and a triangle, respectively. The shaded region is the XMM spectrum extraction region of the outer nebula. The dotted line shows the extent of the outer nebula seen by VLA. The angular resolution of HAWC varies, depending on the energy and zenith angle. The approximate size of the 68% containment region at 56 TeV (radius 0.°2) is marked with a solid white circle at the top left corner. The HAWC image was obtained from the 3HWC survey public data (https://data.hawc-observatory.org/data sets/3hwc-survey/fitsmaps.php), and the VLA nebular extent was estimated from Roberts et al. (2008).
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: Chandra Obs IDs 8502 (black) and 7603 (red), XMM MOS1 (green) and MOS2 (blue), and NuSTAR FPMA (magenta) and FPMB (cyan) spectra of the inner nebula. The background is dominant outside 0.5–7 keV for Chandra, 0.5–8 keV for XMM, and 3–20 keV for NuSTAR. The source spectra were extracted from an annulus region with radii 2″–20″ for Chandra, a circular region with radius 40″ for XMM, and a circular region with radius ﹩1^{\prime} ﹩ for NuSTAR, all centered at PSR J2021+3651. The background spectra were extracted from a ﹩2^{\prime} \times 2^{\prime} ﹩ box in a source-free region. For XMM and NuSTAR, the pulsar spectra were subtracted. The best-fit models are displayed as solid lines in both plots.
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: The best-fit SED model from Naima. The model parameters are given in Table 2. SC flux (Sync), IC flux from the CMB (CMB), IR emission from the interstellar dust grains (IR), SC self-Compton component (SSC), and total flux are plotted. The SSC flux level is very low and located below the lower bound of the y-axis. Radio, X-ray, and TeV flux data points and GeV upper limits are overlaid. The residuals are plotted in terms of significance ((data−model) / (1σ uncertainty of data)).
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: Chandra Obs IDs 8502 and 7603 (the black and red crosses, respectively) spectra of PSR J2021+3651. The background is dominant outside 0.5–7 keV. The source spectra were extracted from a circular region with radius 2″ centered at the pulsar. The background spectra were extracted from an annulus region with radii 2″–4″ centered at the pulsar.
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: (a) The SED model for the Dragonfly from the dynamical model. The model parameters are given in Table 3. Radio, X-ray, and TeV flux data points are overlaid. The residuals are plotted in terms of significance ((data−model)/(1σ uncertainty of data)). (b) Time evolution of the PWN radius (Rpwn; blue solid line), SNR reverse shock radius (RRS; orange dashed line), and magnetic field inside the PWN (B field; green dotted line) over the true age from our model (16 kyr). The PWN collided with the SNR reverse shock at t RS = 12 kyr. (c) and (d) Time evolution of the radiation (c) and particle (d) spectrum of the Dragonfly.
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: XMM MOS1 and MOS2 (green and blue, respectively) spectra of the outer nebula. The source spectra were extracted from the dashed polygon in Figure 4. The line and continuum backgrounds are dominant below 2 keV and above 6 keV, respectively. The best-fit models are displayed as solid lines.
Paper: First Impressions: Early-time Classification of Supernovae Using Host-galaxy Information and Shallow Learning
Authors: Alexander Gagliano, Gabriella Contardo, Daniel Foreman-Mackey, Alex I. Malz, Patrick D. Aleo
Figure caption: Overview of our analysis pipeline, with relevant sections in this paper labeled. Data are outlined in blue, while analysis steps are given in green.
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: The mean of the continuum intensity time series for three different time intervals for each sunspot is shown for the approximately “circular” sunspot, NOAA 11366, at T  c1, T  c5, and T  c10 (upper panels) and the ‘elliptical” sunspot, NOAA 12146, at T  e1, T  e5, and T  e10 (lower panels). The color bar displays the magnitude of the mean time series for each time interval. The umbra/penumbra boundary was obtained by taking threshold levels for both sunspots and is indicated in black. The spatial scale is given in pixels (one pixel is equal to 0.″504, which is approximately 356 km on the surface of the Sun).
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: Continuum intensity images from SDO/HMI observations of two different sunspots. The sunspot location on the solar disk during the period of observation is identified with a black rectangle in the top and bottom panels for active regions NOAA 11366 and NOAA 12146, respectively. Magnified views of the NOAA 11366 circular cross section sunspot and the NOAA 12146 elliptical cross section sunspot are shown in the middle left and right panels, respectively.
Paper: X-Ray/UVOIR Frequency-resolved Time Lag Analysis of Mrk 335 Reveals Accretion Disk Reprocessing
Authors: Collin Lewin, Erin Kara, Edward M. Cackett, Dan Wilkins, Christos Panagiotou, Javier A. García, Jonathan Gelbord
Figure caption: Frequency-resolved lags expected from the standard disk reprocessing model given the mass and accretion rate of Mrk 335 (orange), which provides a poor description of the lags at low frequencies. The fit significantly improves when including a log-normal component to account for additional contribution to the lags from a distant reprocessor located at a radius set to the measured 13.9 day Hβ lag (i.e., the BLR) (blue). Fitting for the radius of the reprocessor still results in a radius consistent with the BLR, see Section 5.
Paper: X-Ray/UVOIR Frequency-resolved Time Lag Analysis of Mrk 335 Reveals Accretion Disk Reprocessing
Authors: Collin Lewin, Erin Kara, Edward M. Cackett, Dan Wilkins, Christos Panagiotou, Javier A. García, Jonathan Gelbord
Figure caption: The CCF lags computed using the original light curves (left) and the detrended light curves (middle), both fit with τ ∝ λ 4/3 relations with normalization values (τ 0) displayed (blue). For comparison, the lag–wavelength relation expected from disk reprocessing is shown (orange), whose normalization is τ 0 = 0.09 days. To illustrate detrending, the i-band light curve (right, black) and the best-fit cubic polynomial that the data will be subtracted by (orange) are shown.
Paper: X-Ray/UVOIR Frequency-resolved Time Lag Analysis of Mrk 335 Reveals Accretion Disk Reprocessing
Authors: Collin Lewin, Erin Kara, Edward M. Cackett, Dan Wilkins, Christos Panagiotou, Javier A. García, Jonathan Gelbord
Figure caption: Fraction of the total (disk+BLR) model made up from the BLR component, denoted f in Equation (1). The BLR fraction shows a local maximum in the U band near 3500 Å. As a point of visual comparison, the inlay at the bottom is Figure 9 from Korista & Goad (2019), which shows the ratio of the diffuse continuum emission to the total spectral energy distribution as a function of wavelength, with the x-axis aligned to match our plot.
Paper: Mass Transfer Theory Based Analysis of Influencing Factors on Component Gradient of Near-surface Atmosphere on Venus
Authors: Wen Gao, Xiaoning Yang, Jing Wang, Yanqiang Bi, Boying Lin, Yonghong Shang, Xinguang Cui
Figure caption: Molar fraction of N2 at different CO2 fluxes.
Paper: Mass Transfer Theory Based Analysis of Influencing Factors on Component Gradient of Near-surface Atmosphere on Venus
Authors: Wen Gao, Xiaoning Yang, Jing Wang, Yanqiang Bi, Boying Lin, Yonghong Shang, Xinguang Cui
Figure caption: The profile of potential temperature of Venus. This figure is extracted from Lebonnois & Schubert (2017).
Paper: Mass Transfer Theory Based Analysis of Influencing Factors on Component Gradient of Near-surface Atmosphere on Venus
Authors: Wen Gao, Xiaoning Yang, Jing Wang, Yanqiang Bi, Boying Lin, Yonghong Shang, Xinguang Cui
Figure caption: Differences of temperature and pressure between the data and calculation result in γ = 1.199 (a) and Molar fraction of N2 at different specific heat ratios (b).
Paper: Mass Transfer Theory Based Analysis of Influencing Factors on Component Gradient of Near-surface Atmosphere on Venus
Authors: Wen Gao, Xiaoning Yang, Jing Wang, Yanqiang Bi, Boying Lin, Yonghong Shang, Xinguang Cui
Figure caption: The Mole fraction of N2 at two boundary conditions from model without CO2 flux (x 0 = 0.1 × 10−5%, x 7 = 3.5%).
Paper: Mass Transfer Theory Based Analysis of Influencing Factors on Component Gradient of Near-surface Atmosphere on Venus
Authors: Wen Gao, Xiaoning Yang, Jing Wang, Yanqiang Bi, Boying Lin, Yonghong Shang, Xinguang Cui
Figure caption: The theoretic model for ideal binary gas in adiabatic process in a steady system based on the Maxwell–Stefan equation.
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: Top panel: light curve of V2493 Cyg in Johnson–Cousins B, V, R  C , and I  C , ZTF zg and zr, PTF ﹩g^{\prime} ﹩, and R, J, H, and K  S , and NEOWISE W1 and W2 bands showing pre-outburst, first outburst, intermediate quiescent phase, and the current outburst phase. The shaded region is our monitoring period. Middle panel shows the zoomed-in LC of V2493 Cyg, which covers our monitoring period corresponding to the time period between 2013 September 9 and 2021 January 4. We call our monitoring period phase (6). Bottom panel: V-band LC of V2493 Cyg coded with that of V − R and V − I  C  colors. The V − R color is depicted at the outer ring (annulus), while the color in the center depicts V − I  C  color. The diamonds represent the zg-band LC coded with zg − zr color. We find that all the colors are slowly becoming redder. The different phases, starting from phase (1) to phase (5), are adopted from the study of Baek et al. (2015).
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: The plot shows the evolution of V2493 Cyg in the absolute magnitude V vs. (V − I  C ) color–magnitude diagram (CMD). The model isomass curves for mass 0.3 M ⊙, A  V  = 0 mag, A  V  = 3.1 mag, and A  V  = 5 mag, and those for mass 0.6 M ⊙, A  V  = 3.1 mag, and A  V  = 10 mag are also plotted (Liu et al. 2022). The phase (6) locus of V2493 Cyg in the CMD plane shows that it currently lies above the η > 5 regime (marked by the vertical black red line), the regime where the circumstellar disk outshines the central PMS star so that all the spectral features that we observe are typical of the viscous accretion disk.