adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Dependence of the orbital and superhumps waveform on the accretion disk precession phase for all deeply eclipsing light curves containing negative superhumps. For each light curve the left frame contains, from bottom to top, the average orbital waveform in equally spaced phase intervals of the disk precession phase, starting from phase zero. The upper curve repeats the lower one to complete the precession cycle. In general, the zero-point of the precession phase is taken to be the brightness minimum of the supraorbital variations. For exceptions to this rule, see the text. Similarly, the right frames contain the superhump waveform as a function of the disk precession phase.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Eclipse amplitude as a function of out-of-eclipse flux for those systems and light curves where the slope α of this relationship decreases above a given threshold. The red (blue) lines are linear least-squares fits to all data below (above) the threshold, extrapolated as dashed lines to higher (lower) flux values.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Brightness variations, O − C curve of eclipse epochs, and eclipse width (EW) as a function of time (left), together with their respective power spectra (right) for all light curves of deeply eclipsing systems which contain negative superhumps. The original light curve is drawn in gray, while the red dots are averages over one orbital period (after masking eclipses). The broken vertical lines indicate the fundamental frequencies (red), and their first (green) and second (blue) overtones, of the beat between the orbital and superhump variations.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: The same as Figure 6 for light curves exhibiting positive superhumps.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: The same as Figure 4 for light curves with positive superhumps. The turquoise vertical line in the power spectra of BH Lyn (LC#2) indicates the beat frequency between the simultaneously present positive and negative superhumps in this system.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Slope α of the flux–amplitude relation as a function of the orbital inclination for all systems and light-curve sections listed in Table 6.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Orbital waveforms (part 4; for details, see the text).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Orbital waveforms (part 1; for details, see the text).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Power spectra (eclipses masked) of LC#1 and LC#2 of BH Lyn in the low-frequency range (left) and in the range around the orbital and superhump frequencies (right). Peaks at the orbital (Ω), positive (Σ+), and negative (Σ−) superhump frequencies and linear combinations thereof are marked.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Orbital waveforms (part 2; for details, see the text).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: TESS light curve of GS Pav (eclipses masked; top) and power spectra of narrow frequency ranges around, from top to bottom, the orbital frequency and its first two overtones. The left-hand frames contain the “conventional” power spectra, the right-hand ones the time-resolved spectra, calculated using a sliding window with a width of 4 days.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Top: light curve LC#2 of DO Leo. Middle: difference between the observed and calculated eclipse minimum epochs as a function of time, assuming a constant orbital period. Bottom: eclipse width as a function of time.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: ASAS-SN light curve (eclipses masked) of the 2019 observing season (left) and power spectrum of the entire 10 yr ASAS-SN light curve of GS Pav (right).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Low-frequency part of the power spectrum of WX Ari calculated using the entire TESS light curve (left) and the individual sectorial light curves (right).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Orbital waveforms (part 3; for details, see the text).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 1).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Left: light curve LC#1 of ASASSN-14ix, and the O − C diagram of eclipse epochs. The horizontal broken red line in the upper frame indicates the time intervals when the system exhibits negative superhumps (Paper III). Right: the corresponding power spectra. The broken vertical lines indicate the frequency of the beat between the orbital and negative superhump variations. The power spectrum of the light curve was calculated after subtracting variations on longer timescales (i.e., the brightening).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: The two TESS light curves of J0518 (top), the O − C diagrams of the eclipse epochs with respect to the linear ephemeris (middle), and the eclipse widths as a function of time (bottom).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Maximum accretion disk radius in a CV (in units of the component separation a) for total eclipse at the lower conjunction of the secondary star as a function of the mass ratio for different values of the orbital inclination.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: TESS light curve LC#2 of 1RXS J0644 (top) and the simultaneous g-band ASAS-SN light curve (bottom). Eclipses are masked in both light curves.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Power spectrum of SDSS J1206 with a strong peak at twice the orbital frequency.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Upper frame: ASAS-SN long-term light curve of HS 1813. Blue and red dots refer to V-band and g-band observations, respectively. Middle and lower frames: light curves of four observing seasons during which HS 1813 displayed series of low-scale stunted outbursts, drawn on the same time and magnitude scale.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: ASAS-SN light curve (eclipses masked) of the 2019 observing season (left) and power spectrum of the entire 9 yr ASAS-SN light curve of ASASSN-14ix (right).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves LC#1 and LC#2 of V347 Pup (top and bottom, respectively), together with the eclipse width as a function of time for both light curves and the O − C curve of the eclipse epochs for LC#2.
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 10).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 7).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 9).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 4).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 2).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 3).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 6).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 8).
Paper: TESS Light Curves of Cataclysmic Variables. IV. A Synoptic View of Eclipsing Old Novae and Novalike Variables
Authors: Albert Bruch
Figure caption: Light curves of NLs used in this study (part 5).
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Visual representation of a typical turbulent magnetic field (left panels) and current density field (right panels) as generated by BxC. Top row: 3D plot of the norm of the fields. Middle row: 2D cuts of isocontours for different levels (∣ B ∣, ∣ j ∣ = 0.1, 0.2, 0.3, 0.5, 0.7, 0.8). Bottom row: magnetic field streamlines (left) and current density isocontours (right) for ∣ j ∣ = 0.6.
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Schematic representation of a turbulent power spectrum and its characteristic features. k  i , P  i  (blue lines) are the wavenumber and spectral power coordinates of the injection scale; k  d , P  d  (red lines) are the wavenumber and spectral power coordinates of the dissipation scale; and ﹩{k}_{\max },{P}_{\max }﹩ (yellow lines) are the wavenumber and spectral power coordinates of the maximum point. The slope in the inertial range (ζ) is indicated in green.
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Top panel: fit performed to find a quantitative relation between h  B  and P  i , which is a secondary effect of varying h  B . Middle panel: 3D norm of  B  generated for h  B  = 1. Bottom panel: comparison between PDF of increments in  B  for h  B  = 1 (pink scale) and h  B  = 2 (gray scale) for different lags.
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Background magnetic field structures implemented in the model and their turbulent realizations for different intensities of turbulence. Top row: uniform magnetic field; middle row: arcade with shear (Terradas et al. 2015); bottom row: cylindrical flux tube with a force-free Gold–Hoyle model (Vandas & Romashets 2017). Left column: background structures; middle column: lightly turbulent realizations; right column: highly turbulent realizations.
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Effects of varying the L  R  parameter on k  i . Top panel: power spectrum for each value of L  R ; dashed vertical lines correspond to the (variable) injection scale. Bottom panel: fit performed that shows a linear relation between L  R  and k  i .
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Effects of varying the L  R  parameter on k  c . Top panel: autocorrelation function for each value of L  R . Bottom panel: fit performed that shows a Gaussian relation between L  R  and k  c .
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Results for varying the η  B  parameter. Top panel: power spectrum for each value of η  B ; dashed vertical lines correspond to the (variable) dissipation scale. Bottom panel: fit performed to find a quantitative relation between η  B  and k  d . Both plots are colored according to the values of the parameter.
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Results for varying the h  B  parameter. Top panel: power spectrum for each value of h  B ; dashed lines indicate the slope given by the minimum and maximum spectral index. Bottom panel: fit performed to find a quantitative relation between h  B  and ζ. Both plots are colored according to the values of the parameter.
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Results for varying the L  B  parameter. Top panel: power spectrum for each value of L  B ; dashed horizontal lines correspond to the (variable) injection spectral power. Bottom panel: fits performed to find a quantitative relation between L  B  and P  i .
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Fits performed to find quantitative relations for the secondary effects of changing η  B . Top panel: relation between η  B  and ζ. Bottom panel: relation between η  B  and P  i .
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Fitting curves describing the relation between h  B  and ζ for different values of η  B .
Paper:  BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields
Authors: Daniela Maci, Rony Keppens, Fabio Bacchini
Figure caption: Results of anisotropy study in terms of 1D power spectra (left column), 2D power spectra (middle column), and current density isocontours for ∣ j ∣ = 0.35 (right column). First row: isotropic case; second row: σ  z  = 10; third row: L  R  = [0.4, 0.4, 0.01]; fourth row: L  R  = [0.01, 0.01, 0.4].
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: Optical spectra of 15 of the literature sample of 91T-like SNe obtained from −12 to +4 days. Missing from this figure are SNF20070803-005 and SNF20080723-012 whose spectra are not publicly available but are reproduced in Scalzo et al. (2012). Spectra of SN 1991T at five phases covering this range are plotted in black for comparison. All of the spectra have been corrected for Galactic reddening. Identifications of the strongest features at premaximum and postmaximum phases are included.
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: (Left) Comparison of velocity measurements of the Si II, Si III, S II, Fe III, and O I ions for SNe 1991T and 2011fe. The measurements correspond to the absorption minima of each line. The gray shaded band displays the rms dispersion of CN SNe Ia from Folatelli et al. (2013). (Right) Same plot comparing velocity measurements for SNe 1999aa and 2011fe.
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: Expansion velocity measurements of the Si II λ6355, Si III λ4560, S II λλ5449, 5622, and Fe III λ4404 absorption features for all of the 91T-like SNe in the literature and CSP-II samples. Where ≥3 measurements for the same SN could be made, these are joined by solid lines. Velocities for the same features in the spectra of SN 1991T are plotted for comparison. Error bars are not shown in order to keep the plot uncluttered, but typically are ±500 km s−1 or less. The gray shaded bands display the rms dispersion of CN SNe Ia from Folatelli et al. (2013).
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: (Left) NIR spectra of four 91T-like SNe observed in the course of the CSP-II. Included for comparison is the spectrum of SN 1991T published by Meikle et al. (1996). Phases with respect to ﹩t({B}_{\max })﹩ are indicated for each spectrum. The spectra have been corrected for telluric absorption; wavelength regions of the strongest telluric features are shaded in gray and indicated by the Earth symbol. (Right) Similar plot of the NIR spectra of three 99aa-like SNe observed by the CSP-II. Some of the more notable absorption and emission features are labeled by their major contributors.
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: Nebular spectra of SN 1991T, the 91T-like SNF20080723-012, SN 1999aa, and the Branch CN SN 2011fe. Phases with respect to the time of maximum light in the B band are indicated, as are identifications of the strongest emission features. References for the spectra are: SN 1991T (Gómez & López 1998), SNF20080723-012 (Taubenberger et al. 2013), SN 1999aa (Silverman et al. 2012), and SN 2011fe (K. Zhang et al. 2016).
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: Expansion velocity measurements of Si II λ6355 and O I λ7774 plotted vs. each other for a sample of SNe Ia observed by the CSP-I. Velocities for Si II λ6355 correspond to maximum light and are taken from Folatelli et al. (2013) and Morrell et al. (2024). The velocities for O I λ7774 were measured from spectra taken within ±4 days of maximum. Measurements for two 99aa-like (2013hh and ASASSN-15as) and three 91T-like SNe (LSQ12gdj, 2013U, and 2014eg) from the CSP-II sample are included in the plot, as are points for SN 1991T and SN 1999aa. The dotted line is for comparison, and indicates a one-to-one trend.
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: Series of optical spectra of SN 1991T showing the time evolution of the Si III λ4560 (left) and Si II λ6355 (right) absorption features. The blue dashed lines illustrate the approximate velocity evolution of both lines.
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: Profiles of the Si II λ6355 absorption in SN 1991T, SN 1999aa, and SN 2011fe at premaximum epochs (top), as well as near maximum (bottom). Pseudocontinuum points to the blue and red were used to define a continuum that has been subtracted from the spectra.
Paper: 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Peter J. Brown, L. Galbany, M. A. Tucker, Christopher R. Burns, Carlos Contreras, P. Hoeflich, E. Y. Hsiao, S. Kumar, Nidia Morrell, Syed A. Uddin, E. Baron, Wendy L. Freedman, Kevin Krisciunas, S. E. Persson, Anthony L. Piro, B. J. Shappee, Maximilian Stritzinger, Nicholas B. Suntzeff, Sudeshna Chakraborty, R. P. Kirshner, J. Lu, G. H. Marion, Abigail Polin, M. Shahbandeh
Figure caption: (a) BVri light curves of 12 of the literature sample of 91T-like SNe. K-corrections have been applied using the Hsiao et al. (2007) spectral template. The light curves in each filter were then shifted vertically to the same magnitude at maximum light after correction for time dilation. Decline rates, Δm 15(B), for each SN are given in parentheses. (b) Same as (a), but for BVri light curves of the 10 91T-like SNe observed by the CSP-II.