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: (a) The X-ray flare energy in the 0.2–12 keV range (EX) vs. flare total duration (ttotal) from Table 7. The three large remarkable flares (Flares 11, 15, and 23), which are analyzed in Sections 4.1 and 4.2, are highlighted with the red circle, blue triangle, and black square. (b) Same as (a), but the data points are plotted with Neupert classifications in T23 (also listed in Table 7). (c) The X-ray flare energy in 0.2–12 keV range (EX) vs. the UVW2-band NUV flare energy EUVW2 from Table 7. The data points are plotted with the Neupert classifications as in (b). The line showing EX = EUVW2 is plotted for reference (dashed line). (d) The flare X-ray average temperature (Tave) vs. the flare total emission measure (EMtot). As in (a), Flares 11, 15, and 23 are highlighted with the red circle, blue triangle, and black square. The gray dashed lines correspond to Equation (6) with n0 = 1011.5 cm−3 and B = 15 G, 50 G, 150 G, 500 G, and 1.5 kG. The green dashed–dotted lines correspond to Equation (7) with n0 = 1011.5 cm−3 and L = 108, 1010, and 1012 cm.
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 9, but for Obs-ID 0822740401 (see Figure 3).
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 30, but for Obs-ID 0822740601 (see Figure 5).
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: The equivalent width (E.W.) lightcurves of Hα, Hβ, He I D3 5876 Å, Na I D1 and D2, and Ca II 8542 Å lines from the CHIRON data, as normalized with the peak and preflare values of Flare 65 on 2018 October 24. The peak Hα and Hβ E.W. values of Flare 65 are 4.96 Å and 7.33 Å, while the preflare values are 2.44 Å and 1.43 Å, respectively (see Figure 22). The peak He I D3 5876 Å E.W. value of Flare 65 is 0.52 Å, while the preflare value is 0.03 Å (see Figure 22). As for the Na I D1 and D2, and Ca II 8542 Å lines, the E.W. values are measured as the excess equivalent widths as done for Flare 23 in Section 4.1. The peak Na I D1 and D2, and Ca II 8542 Å excess E.W. values are 1.59 Å and 0.41 Å, respectively (see Figure 22).
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: (a) The red and black points are the PN spectra of the potential dimming phase (i) and preflare phase around Flares 35 and 36, shown in Figure 18. The blue solid and green dashed lines are model fitting results to these two, respectively. Different from the other figures of PN spectra in this paper, the y-axis of this figure is plotted in the linear scale, following Figure 2 of A. M. Veronig et al. (2021). (b) Same as (a), but for MOS1 data. (c) and (d) Same as (a) and (b), but for the dimming phase (ii) data. (e) Emission measure (EM) distribution from the model fitting to the potential dimming phase (i) and preflare phase. (f) Same as (e) but for the dimming phase (ii). Statistical 90% confidence region errors are shown in (e) and (f).
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: The PN and MOS1 spectra and best-fit model result for the Phases No. 1–No. 4 (see Figure 13) of Flare 23. The data and fit results are plotted in the same way as in Figure 11.
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 10 but for Obs-ID 0822740601.
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 10 but for Obs-ID 0822740401.
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 9, but for Obs-ID 0822740501 (see Figure 4).
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 10 but for Obs-ID 0822740501.
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: (a) Time evolution of Tave and Etot of Flare 23 (see Figure 13 and Table 5). The gray dashed lines and green dashed–dotted lines are plotted in the same way as in Figure 25(d). The phase numbers (e.g., “P.1,” “P.2”) plotted in this figure correspond to those in Figure 13(e). (b) The trend of Tave vs. the square root of volume emission measure (VEM) derived from each spectrum, for Flare 23, along with a determination of the slope ζ, given by the red solid line. (c) and (d) Same as (a) and (b), but for Flare 11 (see Figure 17 and Table 6). (e) and (f) Same as (a) and (b), but for Flare 15 (see Figure 17 and Table 6). The slope ζ is not determined for Flare 15 since the flare decay phase is not observed.
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: The black data points and gray downward triangles show VLA detections and 3σ upper limits of optically overluminous TDEs. In comparison, we show radio (∼6 GHz) light curves of on-axis jetted TDEs (red lines) and other TDEs with high-cadence radio observations in the literature. We also plot 6 GHz light curves from a jet with the same properties as found for the best-fit model of Sw J1644 (P. Beniamini et al. 2023), but at different θobs (see Section 4.2). References: ASASSN-15oi (A. Horesh et al. 2021; A. Hajela et al. 2025), iPTF16fnl (K. D. Alexander et al. 2020; A. Horesh et al. 2021; Y. Cendes et al. 2024), AT2018hyz (Y. Cendes et al. 2022, 2024), AT2019azh (A. J. Goodwin et al. 2022), AT2019dsg (Y. Cendes et al. 2021, 2024), AT2020opy (A. J. Goodwin et al. 2023b), AT2020vwl (A. J. Goodwin et al. 2023a, 2025b), eRASSt J234402.9-52640 (also AT2020wjw) (A. J. Goodwin et al. 2024); Sw J1644+57 (B. A. Zauderer et al. 2011, 2013; T. Eftekhari et al. 2018), Sw J2058+05 (S. B. Cenko et al. 2012; D. R. Pasham et al. 2015; G. C. Brown et al. 2017), Sw J1112-82 (G. C. Brown et al. 2017), and AT2022cmc (I. Andreoni et al. 2022; L. Rhodes et al. 2025). We also show two overluminous TDE candidates with radio observations reported in the literature: ASASSN-15lh (Mg,peak ∼ −23.4 mag; E. C. Kool et al. 2015; G. Leloudas et al. 2016; R. Margutti et al. 2017) and eRASSt J2344 (Mg,peak ∼ −21.8 mag; D. Homan et al. 2023; A. J. Goodwin et al. 2024).
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 43, the He I D3 5876 Å, Na D1 and D2, and Ca II 8542 lines.
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: ZTF r-band light curves of our sample. We assume that disruption occurs at the first-light epoch (tfl). To guide the eye in tracking the light curve evolution, we fit the data using a combination of functional forms and Gaussian process smoothing, following procedures described in Appendix B.4 of Y. Yao et al. (2020). The best-fit models are shown as solid lines, with the 68% confidence intervals displayed in transparent colors. Absolute magnitude is computed using ﹩M=m-5\,{{\rm{log}}}_{10}[{D}_{L}/(10\,{\rm{pc}})]+2.5\,{{\rm{log}}}_{10}(1+z)﹩, where the last term is a rough estimation of the K-correction.
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: Cumulative optical TDE rate (upper panel) and rest-frame g-band (νrest = 6.3 × 1014 Hz) luminosity function (bottom panel; Y. Yao et al. 2023). The vertical lines mark the peak Lg of two on-axis jetted TDEs (D. R. Pasham et al. 2015; I. Andreoni et al. 2022; Y. Yao et al. 2024).
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: The same sample as in Figure 2, but in the galaxy color–mass diagram. TDEs selected for Very Large Array observations are hosted by higher-mass galaxies.
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: ZTF-selected TDEs (2019.0–2022.3) on the diagram of redshift vs. peak rest-frame g-band absolute magnitude. Overluminous TDEs selected for Very Large Array (VLA) observations are annotated.
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 SEDs of AT2022hvp and AT2021aeou, overplotted with the best-fit broken power-law models.
Paper: A Mechanism for Electrostatic Solitary Waves Observed in Ganymede’s Magnetopause
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: Panels (a) and (b) depict the electric and magnetic field power spectra. Panel (c) shows the ratio E/cB vs. frequency and time. E/cB ∼ 1 indicates electromagnetic emissions, while E/cB ≫ 1 indicates electrostatic or quasi-electrostatic emissions. (d) Electric field observed at the outbound magnetopause crossing. Closing up on the waveform, one notices the existence of ESWs. (e) 15 ms duration burst-mode electric field waveform with a running average over 10 sample points removed. Region 1 corresponds to Ganymede’s wake. Regions 2 and 3 are two distinct regions within the magnetosphere. (Figure reproduced from W. S. Kurth et al. 2022 (AGU Publishing) under a Creative Commons License.)
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 of threshold voids with δv,g = −0.7 detected in the Abacus lightcone in a redshift bin of z ∈ [1.54, 1.895] in various fiducial cosmologies, as listed in the legend. Upper panel: the error bars show the VSF measured assuming various fiducial cosmologies (also listed in the legend), the uncertainty is Poissonian. The colored circles connected with a dashed line of the same color show the VSF measured in fiducial cosmologies, different from the true one and corrected using AP. The blue stars connected with a blue line show the VSF measured in the true cosmology and forwarded to the fiducial cosmologies. To avoid overpopulating the plot, we only show here the two most extreme cases, ﹩{{\rm{\Omega }}}_{{\rm{M}}}^{\mathrm{fid.}}={{\rm{\Omega }}}_{{\rm{M}}}^{\mathrm{true}}\pm 32 \% ﹩. Lower panel: ratio between the AP corrected VSF in the fiducial cosmologies and the one in the true cosmology (circles); ratio between the VSF in the true cosmology forwarded to the fiducial with AP with respect to the ones measured in the corresponding fiducial cosmology (stars). The ratios are shown in units of the Poissonian uncertainty, which corresponds to the cosmic variance. The vertical dashed, dashed–dotted, and dotted lines correspond to 1, 2, and 3 times the mean galaxy separation, respectively.
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 are depicted, related to the slow ion-acoustic mode, corresponding to the parameters of Set 3, with the normalized parameters: ni,1,0 = 0.2, nb,1,0 = 0.1, nb,2,0 = 0.2, σi,1 = 0.2, σi,2 = 0.1, σb,1 = 0.2, σb,2 = 0.01, vb,1,0 = 0.1, and vb,2,0 = −0.05. 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 Mach number 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: 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 w0waCDM model, obtained from the VSF (blue) and VGCF (orange), and combining the two statistics (dark gray). The plot is organized as in Figure 10.
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 dispersion of the relative difference between the volume of the Voronoi cells in the true cosmology and different fiducial cosmologies corrected with the AP factor. The histograms are normalized with respect to the maximum, and refer to Voronoi cells of galaxies with redshift z ∈ [1.53.1. 895]. Each panel shows a different fiducial cosmology. The histograms of different color show the results for Voronoi cells with different normalized density, ρ/[〈ρ〉(z)]. The color, from blue to dark red, refers to the following normalized density binning: (0, 0.049,0.15, 0.49, 1.5, 4.8, 15).
Paper: A Mechanism for Electrostatic Solitary Waves Observed in Ganymede’s Magnetopause
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: Fast ion-acoustic mode corresponding to the parameters of Set 3 (same as Figure 3). The variation of (a) pseudopotential, S(ϕ) with ϕ, (b) electrostatic potential ϕ with ξ, (c) electric field with ξ, and (d) the FFT of the electric power spectra for varied Mach number 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 variation of the angular frequency ω with the wavenumber k is depicted, for Set 3. The curves corresponding to ω4 and Ω5 represent the slow ion-acoustic mode, while ω3 and ω6 represent the fast ion-acoustic mode. The curves represented by ω1, ω2, ω7, and ω8 correspond to the electron-acoustic mode.
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 of VIDE  voids detected in the Abacus lightcone in a redshift bin of z ∈ [1.54, 1.895] in various fiducial cosmologies, as listed in the legend. The plot is organized as in Figure 13.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Distribution of S4G barred galaxies from S. Díaz-García et al. (2016) in the plane defined by the maximum H I circular velocity, Vmax, and stellar mass, M*. The top and right panels draw the histograms of M* and Vmax, respectively. The blue star symbol marks the location of the Milky Way, while the red squares with error bars indicate the mean and standard deviation within each of the four stellar mass bins.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Temporal changes of the bar strength A2/A0 for all models in (a) Group 1, (b) Group 2, (c) Group 3, and (d) Group 4. The shaded vertical bands in (c) and (d) 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: Contours of the normalized cross-correlation of the perturbed surface density in the radius-frequency plane for the snapshots shown in Figure 6. Various curves draw instantaneous Ω (solid) and Ω ± κ/2 (dashed) at a given time.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Left: evolution of the maximum wavenumber pmax that maximizes the Fourier amplitude ∣A(2, p)∣, as defined in Equation (7), for the m = 2 logarithmic spirals in model G3A29, along with the corresponding maximum amplitude Amax = ∣A(2, pmax)∣. The shaded regions labeled (a) and (c) indicate the time intervals of swing amplification, while those labeled (b) and (d) correspond to the feedback stage. Right: surface density maps of the m = 2 mode at the final times in the corresponding shaded regions. Rotation is counterclockwise in the disk.
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: The left and middle panels are similar to the column corresponding to Cetus in Figure 3, except the integration period is extended back to 10 Gyr ago. The right panel shows the distribution of distances at pericenter (rperi) relative to the MW and M31 in the orbits where one exists. Close passages (i.e., within the virial radius of the MW or M31) are more common if Cetus is a backsplash galaxy of M31.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Logarithm of the disk surface density Σ at selected times for models G1A40, G2A36, G3A35, and G4A60, from left to right. The time, t, is given in Gyr, and the color bars at the top label ﹩\mathrm{log}{\rm{\Sigma }}/({M}_{\odot }\,{\,\rm{pc}\,}^{-2})﹩.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Radial distributions of (a) the Toomre stability parameter QT, (b) the dimensionless azimuthal wavelength X, and (c) frequencies Ω (solid) and Ω − κ/2 (dashed) at t = 0. In (a), a small dot marks the location of the minimum QT for each model.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Initial distributions of the circular velocity vrot as a function of radius, shown as solid lines for the models in (a) Group 1, (b) Group 2, (c) Group 3, and (d) Group 4. The dashed line in each panel indicates the contribution from the disk component.
Paper: Very Bright, Very Blue, and Very Red: JWST CAPERS Analysis of Highly Luminous Galaxies with Extreme Ultraviolet Slopes at z = 10
Authors: Callum T. Donnan, Mark Dickinson, Anthony J. Taylor, Pablo Arrabal Haro, Steven L. Finkelstein, Thomas M. Stanton, Intae Jung, Casey Papovich, Hollis B. Akins, Anton M. Koekemoer, Derek J. McLeod, Lorenzo Napolitano, Ricardo O. Amorín, Ryan Begley, Denis Burgarella, Adam C. Carnall, Caitlin M. Casey, Antonello Calabrò, Fergus Cullen, James S. Dunlop, Richard S. Ellis, Vital Fernández, Mauro Giavalisco, Michaela Hirschmann, Weida Hu, Garth Illingworth, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Ho-Hin Leung, Ray A. Lucas, Alexa M. Morales, Ross McLure, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Struan Stevenson, Jonathan R. Trump, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: The β–z relation (left) and the β–MUV relation (right) from F. Cullen et al. (2024; red line) in comparison to COSMOS-52185 (green), COSMOS-300001 (purple), and EGS-25297 (red). The gray data points show other measurements from spectroscopically confirmed galaxies at z > 9 (same references as Figure 4). The blue horizontal region shows the steepest UV slopes possible assuming a contribution from both stellar and nebular continua assuming no escape of Lyman continuum.