adsabs/AstroCLIMB huggingface dataset:
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The MIRI MRS channel maps corresponding to the continuum emission detected toward ST6 at (from left to right) 5.3, 8.1, 12.5, and 19.3 μm. Overlaid on each image is the circular spectral extraction aperture with a diameter of 3 × FWHMPSF,λ, where FWHMPSF,λ is the empirically derived FWHM of the MIRI MRS PSF at a given wavelength (λ; see Section 2 for details).
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The ENIIGMA fit to the MIRI MRS spectrum of ST6 in the 6.8–8.4 μm wavelength range. The ice mixtures used in the fit are listed in the legend. The name of each detected ice species is also indicated in the plot in the corresponding color.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The JWST MIRI MRS spectrum of the massive protostar ST6 in the LMC. The gas-phase emission lines (shown in gray) are masked for the ice analysis. Gas-phase absorption lines remain in the spectrum. In this work, we concentrate on the spectral region between 6.8 and 8.4 μm (indicated in purple) covering the main ice features associated with COMs. Major ice and silicate (9.7 and 18 μm) features are indicated.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The top and middle panels demonstrate, respectively, the global continuum and silicate subtraction procedure applied to the MIRI MRS spectrum of ST6. The continuum was determined by fitting a fourth-order polynomial function (shown in magenta in the top panel) to selected guiding points (indicated in purple). The silicate profile shown in blue in the middle panel is a combination of two laboratory silicate spectra (pyroxene and polivene, plotted individually in light blue). Bottom panel: the spectrum of ST6 after the global continuum and silicate subtraction, with the H2O ice model overlaid in aquamarine.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The left panel shows the local continuum subtraction procedure for the wavelength range covering NH3 and CH3OH (top) and CO2 (bottom) ice absorption bands. A second- (top left) or fourth- (bottom left) order polynomial function was fit to the guiding points indicated in the plots. The right panel shows the corresponding local-continuum-subtracted spectra. The double-peaked Gaussian function shown in the upper right panel was used to determine the NH3 ice column density toward ST6 (see Section 3.4 for details).
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: In the left panel, we show the local continuum subtraction procedure for the 6.8 μm ice feature attributed to the ammonium (NH4+) bend with the contribution from the CH3OH C–H reformation mode. A first-order polynomial function was fit to the guiding points indicated in the plot and represents the local continuum. The local-continuum-subtracted spectrum is shown in the right panel. The contribution from the CH3OH C–H reformation mode to the 6.8 μm ice band was estimated by matching the CH3OH laboratory spectrum (shown in blue; D. M. Hudgins et al. 1993) to the intensity of the CH3OH ice band at 9.74 μm. The contribution from NH4+ is shown in magenta (K. Slavicinska et al. 2025a), and the combined spectrum is shown in green.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The magenta curve in the left panel is a eighth-order polynomial function fit through the guiding points (indicated with purple dots), tracing the local continuum around the “COMs region.” The local-continuum-subtracted spectrum between 6.8 and 8.4 μm (corresponding to the “COMs region”) is shown in the right panel (black). Multiple absorption lines resembling noise are H2O gas-phase absorption lines. The underlying spectrum plotted in light violet was used for the ENIIGMA fitting (see Section 3.2 for details).
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The NIRSpec IFU 3.25–3.60 μm spectrum of ST6 covering the C–H stretching mode of CH3OH ice at 3.53 μm. The left panel illustrates the local continuum subtraction procedure. A sixth-order polynomial function was fit to the guiding points indicated in the plot. The local-continuum-subtracted spectrum is shown in the right panel. The 3.47 μm feature attributed to ammonia hydrate overlapping with CH3OH ice at 3.53 μm is represented by a simple Gaussian function (shown in magenta). The laboratory spectrum of CH3OH at 10 K is shown in blue (D. M. Hudgins et al. 1993), and the combined (CH3OH and NH3·H2O) spectrum is shown in green.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The NIRSpec IFU spectrum of ST6 covering the C≡N stretching mode of OCN− ice at 4.59 μm and the CO stretching mode of 12CO ice at 4.67 μm. The narrow absorption lines are from the R (4.3–4.7 μm) and P (4.7–5.2 μm) branches of the CO rovibrational transitions. The local-continuum-subtracted procedure is presented in the left panel. A first-order polynomial function was fit to the indicated guiding points to determine the local continuum. The local-continuum-subtracted spectrum is shown in the right panel. The OCN− ice band is described by a single Gaussian component.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The silicate-subtracted spectrum of ST6 and the local continuum guiding points (the same as in Figure B3) are compared to H2O (green; Figure B2) and NH4+ (orange; Figure E2) models to a posteriori verify the selection of guiding points.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: Individual components of the ENIIGMA fit to the MIRI MRS spectrum of ST6 in the 6.8–8.4 μm wavelength range, color-coded as in Figure 3. The combined ENIIGMA fit is shown as a dashed green line in each panel. For each component, the legend provides information on the ice mixture and temperature used to obtain the laboratory spectrum.
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: Infrared spectra of HOCH2CHO:CO (1:20) and HOCH2CHO:CO2 (1:20) at 15 K. The HOCH2CHO features are indicated with arrows and labeled with their vibrational modes following K. Leroux et al. (2021).
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: Experimental spectra of glycolaldehyde mixed with CO2 (black) and CO (red; see Table 2) ices compared (not fitted) to the spectrum of ST6 (gray). The ice features in the laboratory spectra are identified with their vibrational modes following K. Leroux et al. (2021). Panel (a) shows the 5.6–6.0 μm wavelength range covering two HOCH2CHO ice features (5.72 and 5.86 μm) and displays the laboratory spectra of other COMs for comparison. The laboratory spectra are taken from M. G. Rachid et al. (2020; CO:CH3OH:CH3COCH3), J. Terwisscha van Scheltinga et al. (2021; H2CO), S. E. Bisschop et al. (2007; HCOOH:CO, HCOOH:CO2), and J. Terwisscha van Scheltinga et al. (2018; CH3CHO:H2O, CH3CHO:CO). Panels (b)–(d) show other spectral ranges covering additional HOCH2CHO ice features. Both experimental spectra are scaled to the observed optical depth of the HOCH2CHO 5.72 μm ice band. The best-fit ENIIGMA model was subtracted from the ST6 spectrum shown in panels (b) and (c); the spectrum was smoothed to highlight the absorption features. In panel (d), the NH3 ice feature (see Figure E1) was subtracted from the spectrum (light gray) that was subsequently binned by a factor of 4 (dark gray).
Paper: Protostars at Subsolar Metallicity: First Detection of Large Solid-state Complex Organic Molecules in the Large Magellanic Cloud
Authors: Marta Sewiło, Will R. M. Rocha, Martijn van Gelder, Maria Gabriela Navarro, Steven B. Charnley, Miwha Jin, Joana M. Oliveira, Jacco Th. van Loon, Logan Francis, Jennifer Wiseman, Remy Indebetouw, C.-H. Rosie Chen, Roya Hamedani Golshan, Danna Qasim
Figure caption: The local continuum subtraction procedure for the ice bands at 5.72, 5.78, and 5.84 μm. An eighth-order polynomial function was fit to the guiding points indicated in the plot. The local-continuum-subtracted spectrum is shown in the upper panel of Figure G3. The 5.72 μm band is utilized to determine Nice(HOCH2CHO).
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Physical parameters inferred from the fits of the individual SEDs and nonrelativistic equipartition analysis (see Sections 4.1.1 and 4.1.2). The top left panel shows the temporal evolution of the equipartition radius (filled circles for the first flare; filled squares for the second flare). Best-fitting ﹩R\left(t\right)﹩ evolutions for an assumed constant expansion of outflows that were launched at ﹩{t}_{{\rm{launch}}}=8{4}_{-25}^{+6}﹩ days and 170 ± 10 days are also plotted (dotted–dashed lines). The top right panel shows the equipartition energy. The bottom panel shows the density profile for an outflow that was launched at time of optical discovery (filled blue circles for the first flare; filled blue squares for the second flare) and for an outflow that was launched 84 days after optical discovery (filled red circles for the first flare; filled red squares for the second flare). In addition, we plot the density profile for a delayed outflow for the second flare only in yellow squares. Also plotted are the density profiles inferred for other radio-bright TDEs. The best-fitting parameters at Δt ≃ 242 days are marked with a lighter shade to emphasize our uncertainty in the flux measurements of the ATA due to its larger beam.
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Results from the time-dependent model applied to the first radio flare, for tlaunch = 84 days. The top left panel shows the broadband SEDs, with models drawn from the posterior distributions obtained by using emcee. The top right panel is for the 10 GHz light curve, with lines drawn from the posterior distributions. The evolution of the broadband SED, and especially the change of the optically thin spectral slope, can be easily explained by the transition of the cooling break frequency from ∼60 GHz around Δt = 131 days to ≳100 GHz at Δt ≳ 154 days. The bottom left panel presents the temporal evolution of the synchrotron break frequencies (νm < 0.1 GHz at all times and is not displayed here). The black vertical lines represent the range of observed frequencies at each time. We note that while we do not fit for νIC, represented here in a blue region based on the best-fitted parameters and the optical/UV luminosity, our observations are consistent, within 1σ uncertainties with its temporal evolution. Finally, the bottom right panel displays the density profile around AT 2024tvd compared to other radio-bright TDEs (marked with colored diamonds). The density profile we infer for AT 2024tvd is marked with a red shaded region (marking 1σ uncertainty); a lighter shade is for the extrapolated radii.
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Physical parameters from the generalized equipartition analysis of a relativistic off-axis jet. The top panels show the results for the first radio flare, assuming tlaunch = 80 days, and the bottom panels show the results for the second radio flare for tlaunch = 190 days. The left panels show the evolution of the radius with time, the middle panels show the equipartition energy vs. proper velocity (we mark the temporal evolution with an arrow), and the right panels display the inferred density profile compared to other radio-bright TDEs. We show the results of this analysis for observer angles of θ = 30°, 45°, 60°, and 90°. For each observing angle we use the largest ϵe (up to ϵe = 0.1) that satisfies the relation νm ≤ 1.5 GHz in all of our epochs (see discussion in Section 4.1.3).
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Radio light curves of AT 2024tvd as in Figure 3 with power-law evolution for tlaunch = 80 days.
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Results from our time-dependent fit of the first radio flare assuming a prompt nonrelativistic outflow. The top panel is for the temporal evolution of the different break frequencies based on our best-fitting parameters: β0 = 0.14 ± 0.02, ﹩{\mathrm{log}}\,\left({n}_{{\rm{0}}}\,\left[{{\rm{cm}}}^{-3}\right]\right)=7.36\pm 0.07﹩, k = 6.05 ± 0.25, p = 2.05 ± 0.05, ﹩{\mathrm{log}}\,\left({\epsilon }_{e}\right)=-4.6\pm 0.5﹩, and ﹩{\mathrm{log}}\,\left({\epsilon }_{B}\right)=-3.5\pm 0.2﹩. The bottom left panel shows the post-shock energy for both the prompt and delayed outflows. Finally, the bottom right panel presents the density profiles we infer in each scenario compared to other radio-bright TDEs. Both the energetics and densities inferred in the prompt outflow scenario are extreme when compared to the other scenarios we explored in this work and other radio-bright TDEs.
Paper: Precision Measurement of Large Shear Signals
Authors: Jiarui Sun, Jun Zhang, Li Cui, Alessandro Sonnenfeld, Xin Wang
Figure caption: An example showing the behavior of the shear bias when the shear signals become large. The blue and red surfaces refer to the results of the FQ and FQN methods, respectively. The contours correspond to the values of 0.005, 0.035, 0.065, 0.095, 0.125, and 0.155 respectively.
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Broadband SED of the emission from the host galaxy nucleus. The filled circles are for radio detections obtained at Δt = 160 days, the square is for the detection obtained at Δt = 88 days, and the triangle is a 3σ upper limit obtained at Δt = 160 days. Also plotted is the best-fitting power-law (solid line) and models drawn from the posterior distribution.
Paper: Precision Measurement of Large Shear Signals
Authors: Jiarui Sun, Jun Zhang, Li Cui, Alessandro Sonnenfeld, Xin Wang
Figure caption: An example of the shear errors in regular galaxies at SNR = 40. Different colors in the plots represent different g2 (g1) input values. The dotted–dashed curves correspond to the FQ results, while the solid lines correspond to the FQN results. The black dashed line indicates the zero baseline for comparison.
Paper: Trans-Neptunian Object Colors as Evidence for a Past Close Stellar Flyby to the Solar System
Authors: Susanne Pfalzner, Frank W. Wagner, Paul Gibbon
Figure caption: Connection between TNO color and inclination. The left column illustrates the observational data of M. Marsset et al. (2019) and P. H. Bernardinelli et al. (2025), and the right column shows the numerical results from our flyby simulation. The top row displays scatter plots of the TNOs’ inclination as a function of periastron distance. The middle row shows color distributions for the high-inclination (i > 21°) and the low-inclination (5° < i < 21°) objects, respectively. The colors in panels (b) and (d) indicate the distance to the Sun in the preflyby disk as defined in Figure 1(a). The colors can also be used to convert the results to smaller initial disk sizes. The vertical lines in panel (c) correspond to the gray area in panel (d) and show the border between very red and gray TNOs in the observations and simulations. For the data of M. Marsset et al. (2019) we excluded the centaurs. (e) Observations of the fraction of infrared bright objects as a function of inclination bin for the classical TNOs in the DES survey (P. H. Bernardinelli et al. 2025). (f) Simulation results of the origin distribution for the same inclination bins. Only objects with 30 < p  < 60 au are considered.