adsabs/AstroCLIMB huggingface dataset:
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 39, but for the Phases No. 8–No. 11 (see Figure 17) of Flare 15.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 39, but the Phases No. 5–No. 7 of Flare 11 (see Figure 17).
Paper: Optically Overluminous Tidal Disruption Events: Outflow Properties and Implications for Extremely Relativistic Disruptions
Authors: Yuhan Yao, Kate D. Alexander, Wenbin Lu, Jean J. Somalwar, Vikram Ravi, Ryan Chornock, Raffaella Margutti, Daniel A. Perley, James C. A. Miller-Jones, Paz Beniamini, Nayana A.J., Joshua S. Bloom, Collin T. Christy, Matthew J. Graham, Steven L. Groom, Erica Hammerstein, George Helou, Mansi M. Kasliwal, S. R. Kulkarni, Russ R. Laher, Ashish A. Mahabal, Jérémy Neveu, Reed Riddle, Roger Smith, Sjoert van Velzen
Figure caption: Upper: DBSP and LRIS spectra of AT2022hvp. Bottom: The +44 days spectrum divided by a blackbody+host model, which shows signatures of broad emission lines around O III, N III, and He II.
Paper: Optically Overluminous Tidal Disruption Events: Outflow Properties and Implications for Extremely Relativistic Disruptions
Authors: Yuhan Yao, Kate D. Alexander, Wenbin Lu, Jean J. Somalwar, Vikram Ravi, Ryan Chornock, Raffaella Margutti, Daniel A. Perley, James C. A. Miller-Jones, Paz Beniamini, Nayana A.J., Joshua S. Bloom, Collin T. Christy, Matthew J. Graham, Steven L. Groom, Erica Hammerstein, George Helou, Mansi M. Kasliwal, S. R. Kulkarni, Russ R. Laher, Ashish A. Mahabal, Jérémy Neveu, Reed Riddle, Roger Smith, Sjoert van Velzen
Figure caption: Radio luminosities at trest ∼ 1.5 yr for optically overluminous TDEs (Mg,peak < −20.8; shown in red) and a control sample of fainter TDEs (Mg,peak > −20.5; shown in blue). Considering both detections (solid circles) and upper limits (hollow downward triangles), our Bayesian analysis shows that our sample is brighter than the control sample at 2.1σ significance.
Paper: Optically Overluminous Tidal Disruption Events: Outflow Properties and Implications for Extremely Relativistic Disruptions
Authors: Yuhan Yao, Kate D. Alexander, Wenbin Lu, Jean J. Somalwar, Vikram Ravi, Ryan Chornock, Raffaella Margutti, Daniel A. Perley, James C. A. Miller-Jones, Paz Beniamini, Nayana A.J., Joshua S. Bloom, Collin T. Christy, Matthew J. Graham, Steven L. Groom, Erica Hammerstein, George Helou, Mansi M. Kasliwal, S. R. Kulkarni, Russ R. Laher, Ashish A. Mahabal, Jérémy Neveu, Reed Riddle, Roger Smith, Sjoert van Velzen
Figure caption: Upper: LRIS spectra of AT2020ysg. Bottom: The +141 days spectrum divided by a blackbody+host model, which shows signatures of broad emission lines around He II.
Paper: Optically Overluminous Tidal Disruption Events: Outflow Properties and Implications for Extremely Relativistic Disruptions
Authors: Yuhan Yao, Kate D. Alexander, Wenbin Lu, Jean J. Somalwar, Vikram Ravi, Ryan Chornock, Raffaella Margutti, Daniel A. Perley, James C. A. Miller-Jones, Paz Beniamini, Nayana A.J., Joshua S. Bloom, Collin T. Christy, Matthew J. Graham, Steven L. Groom, Erica Hammerstein, George Helou, Mansi M. Kasliwal, S. R. Kulkarni, Russ R. Laher, Ashish A. Mahabal, Jérémy Neveu, Reed Riddle, Roger Smith, Sjoert van Velzen
Figure caption: Radio light curves of AT2020ysg and AT2020qhs, overplotted with the best-fit Sedov–Taylor models.
Paper: Optically Overluminous Tidal Disruption Events: Outflow Properties and Implications for Extremely Relativistic Disruptions
Authors: Yuhan Yao, Kate D. Alexander, Wenbin Lu, Jean J. Somalwar, Vikram Ravi, Ryan Chornock, Raffaella Margutti, Daniel A. Perley, James C. A. Miller-Jones, Paz Beniamini, Nayana A.J., Joshua S. Bloom, Collin T. Christy, Matthew J. Graham, Steven L. Groom, Erica Hammerstein, George Helou, Mansi M. Kasliwal, S. R. Kulkarni, Russ R. Laher, Ashish A. Mahabal, Jérémy Neveu, Reed Riddle, Roger Smith, Sjoert van Velzen
Figure caption: ESI spectrum of the host galaxies of AT2021gje and AT2022hvp (black) and the best-fit models (red).
Paper: Optically Overluminous Tidal Disruption Events: Outflow Properties and Implications for Extremely Relativistic Disruptions
Authors: Yuhan Yao, Kate D. Alexander, Wenbin Lu, Jean J. Somalwar, Vikram Ravi, Ryan Chornock, Raffaella Margutti, Daniel A. Perley, James C. A. Miller-Jones, Paz Beniamini, Nayana A.J., Joshua S. Bloom, Collin T. Christy, Matthew J. Graham, Steven L. Groom, Erica Hammerstein, George Helou, Mansi M. Kasliwal, S. R. Kulkarni, Russ R. Laher, Ashish A. Mahabal, Jérémy Neveu, Reed Riddle, Roger Smith, Sjoert van Velzen
Figure caption: LRIS spectra of AT2021aeou.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: Histograms showing the number density of VIDE  voids as a function of the void effective radius, Reff. Each color corresponds to a different redshift bin, as listed in the legend.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: 2D marginalized posterior distributions for the moving barrier parameters in the true cosmology, Equation (5), for each redshift bin, as labeled in the legend. The shaded area shows the 68% CL, while the outer contours corresponds to 95% CL. The crosses show the maximum of the posterior distributions.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: Void-galaxy cross-correlation function in redshift space. Left: ξs(s⊥, s∥) in 2D (color scale with black contours) and best-fit model from Equations (20) and (22) (in white contours). Right: monopole (blue dots), quadrupole (orange triangles), and hexadecapole (green wedges) of ξs(s⊥, s∥) with their best-fit model (solid, dashed, dotted lines). The mean void redshift, ﹩\bar{Z}﹩, and effective radius, ﹩{\bar{R}}_{{\rm{eff}}}﹩, of each redshift bin are indicated.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: Projected void-galaxy cross-correlation function ﹩{\xi }_{p}^{{\rm{s}}}({s}_{\perp })﹩ in redshift space (green wedges, interpolated with dashed line) and its real-space counterpart ξ(r) in 3D after deprojection (orange triangles interpolated with dotted line). The redshift-space monopole ﹩{\xi }_{0}^{{\rm{s}}}(s)﹩ (blue dots) and its best-fit model based on Equations (20) and (22) are shown for comparison (solid line). Adjacent bins in redshift increase from left to right, with mean void redshift, ﹩\bar{Z}﹩, and effective radius, ﹩{\bar{R}}_{{\rm{eff}}}﹩, as indicated in each panel.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: VGCF: posterior probability distribution of the model parameters that enter in Equations (20) and (22), obtained via MCMC from the data shown on the left of Figure 7. Dark- and light-shaded areas represent the 68% and 95% CL, with a cross marking the best fit, and dashed lines indicate fiducial values of the RSD and AP parameters. The top of each column states the mean and standard deviation of the 1D marginal distributions. Adjacent bins in void redshift with mean value ﹩\bar{Z}﹩ increase from left to right, as indicated.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: Combination of the VGCF and VSF: posterior distributions of the cosmological parameters explored in the ΛCDM (left) and the wCDM model (right), obtained from the VSF (blue) and VGCF (orange), and combining the two statistics (dark gray). The filled internal region shows the 68% CL, the outer line shows the 95% CL. Black dashed lines indicate the true values and crosses correspond to the maximum of the posterior distributions.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: From left to right: VSF from the Roman reference HLSS-like mock (Z. Zhai et al. 2021), in each of the three redshift bins considered. Upper panels: black dots with error bars show the measured VSF from the postprocessed void catalog as described in Section 3.1 with δv,g = −0.7, the error bars are Poissonian; blue solid lines show the best-fit moving barrier calibrated in the true cosmology as described in Section 3.3; and blue shaded areas show 68% CL. Lower panel: blue solid lines show the relative values of the best VSF theoretical model with respect to measurements in σ units; blue shaded areas show the 68% CL; and gray hatched areas show the ±1σ interval.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: VSF: posterior distributions of the cosmological parameters explored in the optimistic scenario, for the three cosmological models explored: ΛCDM (blue), wCDM (orange), and w0waCDM (green). The filled internal region shows the 68% CL and the outer line shows the 95% CL. Black dashed lines show the true values, crosses correspond to the maximum of the posterior distribution, and the numbers in the panels along the diagonal list the parameter values corresponding to the maximum of the likelihood.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: VGCF: expected constraints on Ωm, w0, and wa for the three different cosmologies tested here. In blue we show the ΛCDM model, while orange and green correspond to wCDM and w0waCDM, respectively. Dashed lines indicate the true values. Numbers in color correspond to the estimated values for the parameters, for the different cosmological models.
Paper: Cosmology with Voids from the Nancy Grace Roman Space Telescope
Authors: Giovanni Verza, Giulia Degni, Alice Pisani, Nico Hamaus, Elena Massara, Andrew Benson, Stéphanie Escoffier, Yun Wang, Zhongxu Zhai, Olivier Doré
Figure caption: VSF: posterior distributions of the cosmological parameters explored in the pessimistic scenario, for the three explored cosmological models. The plot is organized as in Figure 4.
Paper: The Orbits of Isolated Dwarfs in the Local Group from New 3D Kinematics: Constraints on First Infall, Backsplash, and Quenching Mechanisms
Authors: Paul Bennet, Ekta Patel, Sangmo Tony Sohn, Andrés del Pino, Roeland P. van der Marel, Mark A. Fardal, Kristine Spekkens, Laura Congreve Hunter, Gurtina Besla, Laura L. Watkins, Daniel R. Weisz
Figure caption: Top: direct orbital histories for all six galaxies in our sample spanning the range of 6 Gyr into the future to 6 Gyr in the past. The present day is denoted with a dotted vertical line. The right of this vertical line represents past orbits, while the left illustrates future orbits. Orbits are computed in a joint potential accounting for the MW, M31, M33, and the LMC following the methods of B24. The left panel shows orbits relative to the MW, while the right panel shows orbits with respect to M31. Orbits are initialized with the 6D phase space coordinates reported in Table 2. The black and gray dashed lines indicate the virial radii of the MW and M31, respectively. Based on the direct orbital histories, none of the dwarfs have passed within the virial radius of the MW (261 kpc) or M31 (329 kpc) in the past 6 Gyr; however, Leo T and Cetus may make a close passage with the MW in the future, and Pisces may be categorized similarly with respect to M31. Bottom: spatial projection of the direct orbital histories provided in Figure 2 in Galactocentric coordinates. The virial extent of the MW (black) and M31’s (gray) halos is indicated by dashed circles. Similarly, the dotted lines show the orbits of the MW and M31 over the last 6 Gyr. For all dwarfs, markers indicate their present-day positions, and lines indicate their trajectories backward. All dwarfs except Pisces have remained outside the virial radii of both the MW and M31 over the past 6 Gyr.
Paper: The Orbits of Isolated Dwarfs in the Local Group from New 3D Kinematics: Constraints on First Infall, Backsplash, and Quenching Mechanisms
Authors: Paul Bennet, Ekta Patel, Sangmo Tony Sohn, Andrés del Pino, Roeland P. van der Marel, Mark A. Fardal, Kristine Spekkens, Laura Congreve Hunter, Gurtina Besla, Laura L. Watkins, Daniel R. Weisz
Figure caption: Orbital uncertainties for all dwarfs with respect to the MW (top panel) and M31 (bottom panel) are shown in gray, while the blue lines indicate direct orbital histories from Figure 2. The dashed orange lines indicate the virial radii of the MW and M31. Tables 5 and 6 quantitatively summarize the range of plausible orbital histories for all dwarfs. Leo T, Tucana, and Pisces are most statistically likely to be on their first passage through the MW’s halo. While Tucana has completed a pericenter around the MW, Leo T and Pisces have yet to reach their pericenter about the MW. Aquarius, Cetus, and Pegasus are more statistically likely to have reached both pericenter and apocenter about the MW. Still, these orbits do not typically bring the dwarfs closer than 500 kpc from the MW. Leo T, Pegasus, and Tucana are on first infall into M31’s halo. While most Pisces’ orbits indicate first infall into M31, a past interaction is possible for a small fraction of orbits. For Cetus and Aquarius, passages around M31 are statistically common. Cetus passes significantly closer to M31 than Aquarius does. Aquarius does not reach within 500 kpc of M31, while Cetus does.
Paper: The Orbits of Isolated Dwarfs in the Local Group from New 3D Kinematics: Constraints on First Infall, Backsplash, and Quenching Mechanisms
Authors: Paul Bennet, Ekta Patel, Sangmo Tony Sohn, Andrés del Pino, Roeland P. van der Marel, Mark A. Fardal, Kristine Spekkens, Laura Congreve Hunter, Gurtina Besla, Laura L. Watkins, Daniel R. Weisz
Figure caption: Three-dimensional position with respect to the MW (left panel) and M31 (middle panel) relative to the three-dimensional velocity for each dwarf as reported in Table 3. Escape velocity curves are also shown as gray lines of varying thickness for host galaxy halos with masses between 1 and 4 × 1012 M⊙ assuming NFW dark matter halos. Open circles show similar results (without error bars) for the LG periphery dwarfs published in B24. Four and six dwarfs are bound to the MW and M31, respectively, for the masses adopted in this work, which are 1 × 1012 M⊙ for the MW and 2 × 1012 M⊙ for M31. The right panel shows the dwarf data with respect to the LG barycenter, assuming a 1:2 mass ratio for the MW and M31, respectively (i.e., 3 × 1012 M⊙ together). In our assumed LG virial mass model, all six dwarfs are bound to the LG.
Paper: The Orbits of Isolated Dwarfs in the Local Group from New 3D Kinematics: Constraints on First Infall, Backsplash, and Quenching Mechanisms
Authors: Paul Bennet, Ekta Patel, Sangmo Tony Sohn, Andrés del Pino, Roeland P. van der Marel, Mark A. Fardal, Kristine Spekkens, Laura Congreve Hunter, Gurtina Besla, Laura L. Watkins, Daniel R. Weisz
Figure caption: Star formation histories for the past 10 Gyr for an illustrative subsample of our dwarfs. The y-axis shows the star formation rate in arbitrary units. Uncertainties are shown in the gray lines. Left panel: Aquarius from A. A. Cole et al. (2014), Aquarius shows relatively constant star formation between 2.5 and 7 Gyr ago, with a major burst at just beyond ∼7 Gyr ago. Center panel: Cetus from M. Monelli et al. (2010b), Cetus quenches at ∼8 Gyr, and the slight star formation around ∼4 Gyr is likely caused by blue straggler stars. Right panel: Leo T from D. R. Weisz et al. (2012), Leo T shows the relative constant star formation similar to Aquarius, but significantly more stochastic.
Paper: The Orbits of Isolated Dwarfs in the Local Group from New 3D Kinematics: Constraints on First Infall, Backsplash, and Quenching Mechanisms
Authors: Paul Bennet, Ekta Patel, Sangmo Tony Sohn, Andrés del Pino, Roeland P. van der Marel, Mark A. Fardal, Kristine Spekkens, Laura Congreve Hunter, Gurtina Besla, Laura L. Watkins, Daniel R. Weisz
Figure caption: Comparison of the absolute PM measurements for Leo T and Pegasus, the only two dwarfs in our sample with existing literature PMs. We show A. W. McConnachie & K. A. Venn (2020b) in blue diamonds, G. Battaglia et al. (2022) in red circles, B24 in green triangles and our own results as black squares. As can be seen the PMs reported in this work are consistent with, though far more precise than, previous estimates. The different values reported using Gaia DR3 data are primarily the result of the different membership selection methods used by those works.
Paper: A Mechanism for Electrostatic Solitary Waves Observed in Ganymede’s Magnetopause
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: Solitary waves associated with the electron-acoustic mode are depicted, adopting the parameters of Set 3 (same as Figure 3). The variation of (a) the pseudopotential S(ϕ) with ϕ, (b) the electrostatic potential ϕ with ξ, (c) the electric field with ξ, and (d) the FFT of the electric power spectra are shown, for different M values. In panel (d), the x-axis depicts the frequency in Hz and the y-axis shows the electric field power in units of dB [(V m−1)2/Hz].
Paper: A Mechanism for Electrostatic Solitary Waves Observed in Ganymede’s Magnetopause
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: The potential pulse ϕ is depicted vs. ξ, for different vb,1,0 values, in relation with (a) the slow ion-acoustic mode (M = 0.161), (b) the fast ion-acoustic mode (M = 0.793), and (c) the electron-acoustic mode (M = 15). The normalized parameters of Set 3 have been adopted in this graph.
Paper: A Mechanism for Electrostatic Solitary Waves Observed in Ganymede’s Magnetopause
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: Variation of ϕ with ξ for varied κ values for (a) slow ion-acoustic solitons (M = 0.162), (b) fast ion-acoustic solitons (M = 0.793), and (c) electron-acoustic solitons (M = 21).
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Distribution of the amplification factor Γ in the QT,bar–Xbar plane. Various symbols indicate the simulation outcomes: blue for bar-forming models and red for stable models. Open symbols represent models from this study, with circles, triangles, squares, and crosses corresponding to galaxies in Groups 1, 2, 3, and 4, respectively. The filled triangle and filled circle mark models C00 and L00 from D. Jang & W.-T. Kim (2023), respectively. The dashed line denotes the bar formation boundary corresponding to Γ = 10, as defined by the criterion in Equation (17).
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Contours of the logarithm of the projected disk densities at the end of the runs (t = 10 Gyr) for the fiducial models. The x- and z-axes correspond to the semimajor axis of the bar and the vertical direction, respectively. Dotted contours represent projected densities ∫ρd dy = 109.0, 108.5, 108.0, and 107.5 M⊙ kpc−2, from innermost to outermost.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Temporal evolution of the bar length Rbar (left) and RCR (right) for the bar-forming models in Group 1, Group 2, Group 3, and Group 4 from top to bottom. The thin portions of the curves for models G1A37, G1A40, G2A32, G2A34, and G2A36 indicate phases during which the bars are disrupted by outer spiral arms.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Temporal evolution of the BPS strength Ps for all bar-forming models in (a) Group 1, (b) Group 2, (c) Group 3, and (d) Group 4. In (c) and (d), the shaded vertical bands indicate the periods of buckling instability.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Temporal evolution of the ratio σz/σR of the vertical to radial velocity dispersions of the disk particles at R = 2 kpc for all bar-forming models in (a) Group 1, (b) Group 2, (c) Group 3, and (d) Group 4. In (c) and (d), the shaded vertical bands indicate the duration of the buckling instability.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Temporal evolution of the mean vertical velocity, ∣〈vz〉∣, measured in an annulus centered at R = 3 kpc for all bar-forming models in (a) Group 1, (b) Group 2, (c) Group 3, and (d) Group 4. In (c) and (d), the shaded vertical bands indicate the duration of the buckling instability.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Variations of ﹩S/{\kappa }_{0}^{2}﹩ and ∣ξ∣ as functions of dimensionless time τ = tκ0 for QT = 1.2 and X = 1.5. The shaded regions denote the period of most significant growth, during which S < 0.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Temporal evolution of the bar pattern speed Ωb for the bar-forming models in (a) Group 1, (b) Group 2, (c) Group 3, and (d) Group 4. The thin portions of the curves for models G1A37, G1A40, G2A32, G2A34, and G2A36 indicate phases during which the bars are disrupted by outer spiral arms.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Amplification factor Γ as a function of X for disks with QT = 1.2 (black solid), QT = 1.5 (red dashed), and QT = 2.0 (blue dotted).