adsabs/AstroCLIMB huggingface dataset:
Paper: Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes
Authors: Floor S. Broekgaarden, Simon Stevenson, Eric Thrane
Figure caption: Same as Figure 7 but for the effective spins and mass ratios for our model with the optimistic common-envelope prescription (model K). There is an anticorrelation present in the MRR binaries (left panel), but the opposite behavior is visible in the non-MRR binaries (right panel). For each of the 28 star formation history combinations we draw 1000 samples (combined over MRR and non-MRR) that we highlight with larger markers. The other stellar evolution models are shown on GitHub. https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure_7_and_8_and_9_and_10_Discussion_2D_slices/individual_ChiEff_vs_q/ChiEff_vs_q_all_models_all_points_K.png https://github.com/FloorBroekgaarden/MRR_Project/blob/main/Figure_7_and_8_and_9_and_10_Discussion_2D_slices/Make_2D_scatter_Distributions.ipynb.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: Left panel: the recovery rate (%) of the period of the signal injected into a cluster member’s light curve. Right panel: same as the left panel, but for field stars rather than cluster members. The gradient from top to bottom demonstrates that the lower a signal’s amplitude is, the harder it is to recover. In both panels bins with a black or white (color chosen for optimal contrast) box drawn around them are the ones where over half (i.e., ≥25) of the injected signals are Kepler light curves.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: The CMD of kinematically selected M67 members. The left panel is using the Pan-STARRS DR2 photometry, and the right panel is using Gaia EDR3 photometry. In both panels orange points represent main-sequence single members (subject to a brightness cutoff at lower magnitudes), gray points represent photometric binaries, and purple points indicate stars with rotation periods reported in our results.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: The distribution of residuals after subtracting out a polynomial fit to the main sequence from each star in the catalog. The shaded region denotes the stars chosen as single stars on the main sequence. The −0.3 offset represents the approximate location of the valley between the two peaks in this distribution, while accounting for the wide spread about the binary peak centered at ∼−0.6. The vertical dotted line denotes the expected excess brightness for equal-mass binaries.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: Scatter plots and histograms of the three parameters used for cluster membership determination (proper motions, or PM, in R.A. and decl., and parallaxes). In gray, the distribution of these parameters for the noncluster stars is shown as a point of comparison. For cluster members color indicates the probability of membership, showing that the members on the “outskirts” of the distribution are less likely to be considered members of M67 (see Section 3.1 for further details).
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: Left panel: a scatter plot of the predicted vs. observed scatter of the zero-point-corrected magnitudes that are averaged together to form one epoch in our light curves. The expectation is that these points lie on the one-to-one line. Right panel: a scatter plot of the predicted vs. observed scatter of the zero-point-corrected magnitudes in our light curves; the one-to-one line is the expected lower limit. In both panels the predicted values are derived from our estimated uncertainties.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: The number of Kepler light curves used in the injection and recovery tests to establish completeness as a function of rotation period (P rot) and photometric variability (S ph). Bins with a black or white (color chosen for optimal contrast) box drawn around them are the ones where over half (i.e., ≥25) of the injected signals are Kepler light curves.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: The distribution of the percent differences between the injected and recovered period (irrespective of the FAP of the recovery). The precision on our rotation periods is set by the standard deviation of this distribution: 10%.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: A Sloan Digital Sky Survey DR9 i-band image of the M67 field, with all of our candidate M67 cluster members identified by circles. Blue circles identify the stars with reported rotation periods in Table 2. The black boxes are the MegaPrime footprint for one of the pointings in our dither pattern.
Paper: A 4 Gyr M-dwarf Gyrochrone from CFHT/MegaPrime Monitoring of the Open Cluster M67
Authors: Ryan Dungee, Jennifer van Saders, Eric Gaidos, Mark Chun, Rafael A. García, Eugene A. Magnier, Savita Mathur, Ângela R. G. Santos
Figure caption: The sample of late K and M dwarfs of Mann et al. (2015) used to derive our color–T eff relationship. We chose stars to have a metallicity within the range of literature values for M67. The T eff errors are of order 75 K and do not affect the dispersion.
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: Illustration of the continuum and emission-line fittings of the SDSS spectrum (left panel). In the middle two panels, we show a zoomed-in view of the emission-line profile fittings for the Hβ+O [III] region and the Hα+N [II] region, respectively. The SED fitting results from CIGALE are shown in the right panel.
Paper: Transient Radio Emission from Low-redshift Galaxies at z < 0.3 Revealed by the VLASS and FIRST Surveys
Authors: Fabao Zhang, Xinwen Shu, Luming Sun, Lei Yang, Ning Jiang, Liming Dou, Jianguo Wang, Tinggui Wang
Figure caption: The radio images at 888 MHz for 15 sources observed in RACS. The red circle in each panel has a radius of 25″. The image has a size of 4′ × 4′.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: Latitude vs. altitude distributions of temperature (a)–(b) and normalized temperature perturbations (c)–(d) for the first half of MY33 and MY35. The data are binned in 5° × 5° km latitude × altitude intervals.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: Mean vertical wavenumber spectra of normalized temperature perturbations divided by N4 at different local time bins, in the altitude range of 160–200 km (upper panels) and 180–220 km (bottom panels) in MY35.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: Local time vs. altitude distributions of temperature (a)–(b) and normalized temperature perturbations (c)–(d) for the first half of MY33 and MY35. The data are binned in 2 hr × 5 km (local time × altitude) intervals.
Paper: Spectral Analysis of Gravity Waves in the Martian Thermosphere during Low Solar Activity Based on MAVEN/NGIMS Observations
Authors: Qianqian Ji, Xiaoqian Zhu, Zheng Sheng, Tian Tian
Figure caption: As in Figure 8, but in MY33.
Paper: Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in ∼130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array
Authors: T. Morishita, Abdurro'uf, H. Hirashita, A. B. Newman, M. Stiavelli, M. Chiaberge
Figure caption: Left: HST’s RGB composite image of MACS 2129-0741, a cluster of galaxies at z = 0.57. The target of our ALMA observations, MRG-M2129, is located in the center of the white square box. Right: zoom-in image of MRG-M2129 (50″ × 50″). The field of view (FOV) of our ALMA Band 6 observations is shown by the central square box of 3″ × 3″ (also see Figure 2). The FOV of one of the previous Band 6 programs (2018.1.00276.S) is shown with a gray circle (r ∼ 24″) for comparison.
Paper: Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in ∼130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array
Authors: T. Morishita, Abdurro'uf, H. Hirashita, A. B. Newman, M. Stiavelli, M. Chiaberge
Figure caption: Top: multiband images of MRG-M2129 in a 3″ × 3″ cutout (same size as the white square in Figure 1)—ALMA 1.2 mm continuum created with the high-resolution setup (Section 2.1), HST F160W, F105W, F775W, and pseudo RGB images, from left to right. The continuum flux of ALMA is overlaid in each of the HST images, where the contours represent 3σ, 4σ, 5σ, 6σ, and 7σ. The beam size is shown at the bottom left of the ALMA image. Bottom: zoomed-in version of the images in the top row in a box of 1″ × 1″, corresponding to the white square box in the top panel. The position of the flux centroid measured in the F160W image (Section 3.1) is shown in the 1.2 mm image (cross symbol).
Paper: Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in ∼130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array
Authors: T. Morishita, Abdurro'uf, H. Hirashita, A. B. Newman, M. Stiavelli, M. Chiaberge
Figure caption: Distribution of quiescent galaxies at z ∼ 2 in the plane of molecular gas-to-stellar mass ratio (M H2/M *) vs. specific star formation rate (SFR/M *) plane. For those undetected, 3σ upper limits of the gas-to-stellar mass ratio are shown. It is noted that two measurements for MRG-M2129 derived in this study (red star; Table 3) and Whitaker et al. (2021a, orange star) are shown separately. The difference is attributed to two different methods of deriving gas mass (Section 3.3).
Paper: Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in ∼130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array
Authors: T. Morishita, Abdurro'uf, H. Hirashita, A. B. Newman, M. Stiavelli, M. Chiaberge
Figure caption: Top: SED of integrated fluxes of MRG-M2129. The best-fit model template is shown as a solid black line. Each component of the fitting template is shown in a different color as in the label. Data points are shown with 2σ errors (blue symbols). 2σ upper limits are shown for nondetections. Normalized residuals, (data − model)/data, are shown in the bottom panel with the same symbols as in the top panel. Bottom: posterior distributions of the parameters used in our SED fitting analysis.
Paper: Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in ∼130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array
Authors: T. Morishita, Abdurro'uf, H. Hirashita, A. B. Newman, M. Stiavelli, M. Chiaberge
Figure caption: Source-plane image of MRG-M2129, in HST F160W (left) and ALMA 1.2 mm (right). The stamp size corresponds to ∼20 kpc in the source plane. The HST (ALMA) image is smoothed with a Gaussian kernel of σ = 0.″2 (0.″04) and shown using an arcsinh (linear) stretch.
Paper: Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in ∼130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array
Authors: T. Morishita, Abdurro'uf, H. Hirashita, A. B. Newman, M. Stiavelli, M. Chiaberge
Figure caption: Velocity maps of [C I] in MRG-M2129. The velocity maps are shown at an interval of Δv = 50 km s−1 with respect to the [C I] line at the redshift of MRG-M2129. Each stamp has a size of 1.″5 × 1.″5. The contour levels shown by black solid lines represent positive fluxes at 3σ and 4σ; white dashed lines represent negative fluxes. No confident detection of the [C I] line is identified.
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: Results from our fitting analysis. Descriptions of all variants are provided in Table 1 and Section 4.1. Lines are used for visualization only. Left: Group X 2, relative standard deviation of the Hubble residual (Rel. SD), difference in weighted mean distance modulus residuals (μ dif), Δw, and ΔH 0 for Tully (2015), Lim et al. (2017), Lambert et al. (2020), and Crook et al. (2007) group-averaged redshift variants as compared with the galaxy redshift variant. We compare X 2 values with (solid points) and without (open points) an additional CF correction. In the first, second, and third panels we present values calculated by using only SNe updated as described in our group analysis (N = 174). In all panels, only SNe found in groups (N = 174) vary between points on a line with some panels showing values calculated with samples covering differing redshift ranges. The fourth and fifth panels are calculated with z < 2.2, and 0.023 < z < 0.15 respectively. Right: Comparing ΔX2, Rel. SD, μ dif, Δw, and ΔH 0 for various CF corrections applied to the individual galaxy redshifts or group-averaged heliocentric redshifts from T15, where available. Additionally plotted with open points are redshift sets with solely individual galaxy redshifts. In the first panel, the improvements in X 2 for two upper limits of redshift are shown. Each redshift range is specified in the legends.
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: In the lower panel, we show the relation between cosmological and observed redshift predicted by the Carrick et al. (2015) reconstruction along the line of sight for the supernova 2011dl. The shading about the predicted relation shows the expected scatter with 250 km s−1 of PV dispersion. The distribution of the underlying cosmological redshift can be found by integrating along the line at the observed redshift (z CMB = 0.031459); the upper panel shows the sampled posterior probability density function (PDF). As this SN is located near a predicted galaxy overdensity, the relation between predicted observed redshift and comoving distance/cosmological redshift takes on a characteristic S shape. Larger density concentrations can cause this curve to become non-monotonic, and the region becomes triply valued. A 250 km s−1 uncertainty in PV dispersion here becomes a broader 700 km s−1 uncertainty in cosmological redshift; there are many underlying cosmological redshifts potentially consistent with the observation. The PDF can be seen to be non-Gaussian where the second derivative of the relation is high, however we approximate it as Gaussian for computational reasons.
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: Binned with equal SNe per bin Rel. SD values from our CF analysis as compared to CF = None. Overplotted on the panels are the expected Rel. SD values for three different values of PV uncertainties. Left: all SNe used for CF analysis (N = 584). Right: heliocentric redshifts for SNe found in groups are updated according to T15 (N = 584 but 174 SN redshifts are group corrected as well).
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: Hubble residuals for z < 0.1 using the galaxy redshifts and T15 group-corrected redshifts of the SNe found in groups (N = 174). Corresponding X 2 and Rel. SD values are given in the legends. Binned (with Δz = 0.01) μ dif values are overplotted. Group corrections visibly reduce the diagonal scatter of these SNe.
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: Explanation of the difference between the apparent cosmological motion of galaxies due to the expansion of the universe and its relation to distance (1) vs. the observed motion of galaxies and peculiar motions (2). The corrections for motions are broken into four components in panels A–D and include: (A) relative CMB motion due to the motion of our galaxy, (B) small-scale virial motions of galaxies in a group, (C) large-scale coherent motions of halos of galaxies moving toward each other, and (D) large-scale external-field motions of all galaxies moving toward a place outside the local volume of redshift surveys. All of these motions (the final three being peculiar motions) contribute a radial component to the observed motion.
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: Comparison between v coh. from the primary sets of CF corrections. Results from an orthogonal distance regression fit are shown assuming no uncertainties in the PVs. SNe with z < 0.02 are in orange. All others are in blue. Upper: comparing 2M++ne to 2M++ C15. Upper middle: comparing Cf3 to 2M++ C15. Lower middle: comparing VGAS to 2M++ C15. Lower: comparing 2MRS to 2M++ C15.
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: Distribution of the low-z SNe (z < 0.08) in our sample across the sky. The points are color-coded by the CF corrections (in km s−1) obtained using the 2M++ density field. The ×’s correspond to those SNe we find to be in a group in any of the Tully (2015), the Lim et al. (2017), the Lambert et al. (2020), or the Crook et al. (2007) group catalogs.
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: Comparing Tully (2015), Lim et al. (2017), Lambert et al. (2020), and Crook et al. (2007) group assignments for the SNe found in groups. Left: corresponding group richnesses for the galaxies matched in our sample on a logarithmic scale. Right: histogram of the unweighted average redshifts of a group subtracted by the host galaxy’s redshift for each group catalog. Median differences (μ) and standard deviations (σ) are given in kilometers per second in the legend.
Paper: The Pantheon+ Analysis: Evaluating Peculiar Velocity Corrections in Cosmological Analyses with Nearby Type Ia Supernovae
Authors: Erik R. Peterson, W. D'Arcy Kenworthy, Daniel Scolnic, Adam G. Riess, Dillon Brout, Anthony Carr, Hélène Courtois, Tamara Davis, Arianna Dwomoh, David O. Jones, Brodie Popovic, Benjamin M. Rose, Khaled Said
Figure caption: Histogram of the number of galaxies vs. redshift, after successive assignments toward group catalogs. The full sample is shown in blue. Those that have host galaxy identifications are shown in orange. Hosts that appear in the PGC or 2MASS catalogs are in green (with 2MASS dotted). These can then be matched to the existing group catalogs in red (T15, Lim17, Lam20, and C07).
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: (a) Evolution of the pseudo-equivalent width pEW(Si II λ6355) for SS (turquoise dotted lines) and CN (black dotted lines) SNe from the Blondin et al. (2012) and Folatelli et al. (2013) spectroscopic samples. Measurements for SN 1991T, SN 1999aa, SN 1999ee, and SN 2011fe are highlighted. The spectra for SN 1991T are from Phillips et al. (1992) and Mazzali et al. (1995), those of SN 1999aa are from Garavini et al. (2004) and Blondin et al. (2012), those of SN 1999ee are from Hamuy et al. (2002) and Blondin et al. (2012), and those of SN 2011fe are from Pereira et al. (2013). Also included are measurements for the 02cx-like SN2005hk, and for the 03fg-like event SN2007if. The spectra for SN2005hk are from Phillips et al. (2007) and Blondin et al. (2012), and those for SN2007if are from Scalzo et al. (2010) and Blondin et al. (2012). (b) Evolution of the pEW of the Ca II H & K and Si II λ6355 absorption features as a function of light curve phase with respect to ﹩t({B}_{\max })﹩ for SN 1991T, SN 1999aa, SN 1999ee, and SN 2011fe. Each point in the diagram represents a spectrum, with a selection of the points labeled with the light-curve phase.