adsabs/AstroCLIMB huggingface dataset:
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: The spectroscopic and broadband NIRCam lightcurves of GJ 3470 b. The top panels show the raw F322W2 and F444W lightcurves binned in the spectral direction into 0.015 μm wide spectral bins, with the transit of GJ 3470 b clearly visible at all wavelengths. The bottom panels show the broadband F322W2 and F444W lightcurve data without their associated error bars for visual clarity.
Paper: Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b
Authors: Thomas G. Beatty, Luis Welbanks, Everett Schlawin, Taylor J. Bell, Michael R. Line, Matthew Murphy, Isaac Edelman, Thomas P. Greene, Jonathan J. Fortney, Gregory W. Henry, Sagnick Mukherjee, Kazumasa Ohno, Vivien Parmentier, Emily Rauscher, Lindsey S. Wiser, Anastasia Triantafillides
Figure caption: Photometric monitoring of the GJ 3470 system from 2012 to 2023 shows sinusoidal brightness modulations with an amplitude of 2545 ± 130 ppm at a period of P = 21.6239 ± 0.0014 days in a Cousins R filter. The amplitude of stellar variability decreases significantly at longer wavelengths (Benneke et al. 2019a), and we expect this variability to affect our measured transit depths at <10 ppm over the F322W2 and F444W wavelength range.
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: Synthetic spectra (Appendix A.2) composed of areal (models 1–3) and particulate (models 4–8) mixtures, offset vertically for clarity. These spectral models include crystalline H2O ice (Mastrapa et al. 2009), crystalline CO2 ice (Quirico & Schmitt 1997a, 1997b), crystalline CO ice (Robert Brown, private communication), and amorphous carbon (Rouleau & Martin 1991), with grain diameters of 2, 10, 10, and 1 μm, respectively. Each model includes 10% CO ice and 0.5% amorphous carbon mixed with (1) 84.5% H2O ice and 5% CO2 ice, (2) 79.5% H2O ice and 10% CO2 ice, (3) 64.5% H2O ice and 25% CO2 ice, (4) 64.5% H2O ice and 25% CO2 ice, (5) 49.5% H2O ice and 40% CO2 ice, (6) 39.5% H2O ice and 50% CO2 ice, (7) 14.5% H2O ice and 75% CO2 ice, and (8) 14.5% H2O ice and 75% CO2 ice. Model 7 includes 25% CO2 (Quirico & Schmitt 1997a; 10 μm grains) and 50% CO2 (Gerakines & Hudson 2020; 100 μm grains). These models demonstrate that the Ariel features between 4.19 and 4.30 μm and between 4.65 and 4.80 μm, which are associated with the ν 3 modes of CO2 and CO ice, respectively, are exhibited by all eight models (dotted lines with bold text). In contrast, weak CO2 features tentatively observed on Ariel, near 3.01, 3.33, 4.84, and 4.93 μm (dotted lines, italicized text), are only exhibited by areal mixtures that include ≥10% CO2 (models 2–3) and are not observed in any of the particulate mixtures (25%–75% CO2 ice; models 4–8). The 4.90 μm band is expressed by all areal mixtures (5%–25% CO2, models 1–3) and particulate mixtures with ≥40% CO2 (models 5–8). The presence of weak CO2 ice features in the areal mixtures and their absence from the particulate models demonstrate that concentrated deposits of pure CO2 on Ariel’s surface are required for these features to be expressed (Section 4.1). None of the areal or particulate mixtures exhibit a ∼4 μm feature, suggesting that carbonates, or another component, are more likely to contribute to Ariel’s 4.02 μm band compared to CO2 ice (dashed line, italicized text).
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: (a) Comparison between a continuum-subtracted version of the 4.67 μm absorption band on Ariel’s trailing hemisphere (black) and laboratory absorbance spectra of pure CO ice and CO + CO2 ice mixtures measured in the Astrophysical Material Laboratory at temperatures between 20 and 30 K, with the CO feature persisting at temperatures up to 80 K in the mixed CO + CO2 samples (Tegler et al. 2024; Grundy et al. 2024a). Pure CO2 ice is essentially featureless in this wavelength range and omitted for clarity. The CO2:CO mixture (9:1, green, centered near 4.674 μm) provides a good match to the central wavelength of Ariel’s 4.67 μm band, whereas mixtures with comparable amounts of CO2 and CO (6:4, blue, centered near 4.672 μm) provide less ideal matches. Pure CO ice (red, 4.677 μm) is much narrower, offset to longer wavelengths, and exhibits a narrow sideband (4.667 μm), likely resulting from a longitudinal optical phonon mode, which does not match the broad short-wavelength sideband of Ariel’s 4.67 μm band. Neither the pure CO nor CO + CO2 mixtures are able to match Ariel’s long-wavelength sideband centered near 4.69 μm. (b) Comparison between a continuum-subtracted version of the 4.67 μm band on Ariel’s trailing hemisphere (black) and laboratory spectra of a sample dominated by CO ice generated via irradiation of a CO2 thin film with 100 KeV H+ protons at 25 K (light blue) and 50 K (orange), shown in optical depth units (−ln(R/R 0), where R is the reflectance of the film and gold substrate and R 0 is the reflectance of the bare gold substrate; Raut & Baragiola 2013). All spectra are normalized to 1 at their maxima. The radiolytic CO features do not provide good matches to the central position, width, or sidebands of Ariel’s 4.67 μm band.
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: Comparison between Ariel’s leading (purple) and trailing (red) hemisphere spectra (vertically offset for clarity, normalized to unity at 4.145 μm) and 1σ uncertainties, along with synthetic spectra of crystalline CO2 ice (1–3) and CO ice (4). These synthetic spectra were generated using CO2 grain diameters and optical constants from: model 1, 10 μm, Hansen (1997); model 2, 10 μm, Quirico & Schmitt (1997a, 1997b); model 3, 50 μm, Gerakines & Hudson (2020); model 4, 10 μm, Robert Brown (private communication). Models 1 and 2 were scaled to the depth of the 4.90 μm band on Ariel’s trailing side, Model 3 was scaled to the height of the 4.20 μm scattering peak on Ariel’s trailing side, and Model 4 was scaled to the depth of the 4.67 μm band on Ariel’s trailing side. All four models are offset vertically for clarity. The central wavelength of measured features (Table 1) and possible features near 3.01, 4.84, and 4.93 μm are indicated by dotted lines.
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: The e-folding photon penetration depths into a slab of CO2 ice (red: Gerakines & Hudson 2020; purple: Quirico & Schmitt 1997a, 1997b), CO ice (orange; Gerakines et al. 2023), and H2O ice (black; Mastrapa et al. 2009), and MOPL for photons into a layer of CO2 ice grains with 1 μm diameters (blue). The MOPLs for photons into layers composed of 10 and 100 μm diameter CO2 ice grains are intermediate between the blue and purple lines. The black dashed lines highlight the band centers for Ariel’s 3.33 and 4.90 μm bands, and the gray dashed lines highlight other subtle CO2 ice features that may be present in the spectrum of Ariel’s trailing hemisphere (centered near 3.01, 4.84, and 4.93 μm). This plot shows that only the strong ν 3 modes for 12CO2, 13CO2, 12CO, and 13CO should be exhibited by Ariel, if carbon oxides are well mixed with H2O on its surface. The presence of weaker CO2 ice features supports the presence of concentrated CO2 ice deposits exposed on Ariel’s surface (likely mixed with small amounts of CO and perhaps other carbon oxides).
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: Comparison between a continuum-subtracted version of Ariel’s 4.90 μm band on its trailing hemisphere and a 4.89 μm CO3 band generated via irradiation of CO2 ice thin film with 100 keV H+ protons, scaled in optical depth units (−ln(R/R 0), where R is the reflectance of the film and gold substrate and R 0 is the reflectance of the bare gold substrate; Raut & Baragiola 2013). All spectra are normalized to 1 at their maxima. The offset between the CO3 features and Ariel’s 4.90 μm band supports the interpretation that this feature results from collective oscillations across a crystalline CO2 ice lattice (Bini et al. 1991; Figure 2). It is possible that radiolytically produced CO3 contributes to the broad short-wavelength side of Ariel’s 4.90 μm band. However, additionally experiments are required to determine whether this broadening of Ariel’s 4.90 μm band results from mixing with CO3 or other variables such as the temperature of CO2 on Ariel.
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: Top: NIRSpec IFU (G395M/F290LP) reflectance spectra and 1σ uncertainties for Ariel’s leading (purple) and trailing (red) hemispheres, vertically offset for clarity and normalized to 1 at 4.145 μm. Bottom: close-up of the same spectra, focusing on the 3.8–5.1 μm wavelength region. Confirmed absorption bands and scattering peaks associated with H2O ice, CO2 ice, and CO ice are shown in bold, whereas suggested constituents are italicized and followed by a question mark. Amorphous CO2 is abbreviated to “A. CO2.” The central wavelengths (μm) for the identified features are listed vertically along each dotted line and in Table 1.
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: Comparison between NIRSpec IFU spectra and 1σ uncertainties for Ariel’s leading (purple) and trailing (red) hemispheres and the TNOs 47171 Lempo (1999 TC36) (1), 2013 LU28 (2), and 2004 XA192 (3), selected to represent members of the “bowl,” “cliff,” and “double-dip” TNO types (Pinilla-Alonso et al. 2021; de Pra et al. 2024), respectively. All spectra are normalized to 1 at 4.15 μm and offset vertically for clarity. Similar to other double-dip TNOs, 2004 XA192 exhibits strong 12CO2 and 13CO2 bands, with a CO2 scattering peak similar to Ariel’s 4.202 μm peak. However, none of the TNOs display a strong 4.252 μm peak, unlike Ariel. 2004 XA192 also exhibits a strong ∼4.07 μm band resulting from the Christiansen effect, where n = 1 and k = 0 in crystalline CO2 ice (Figure A3). This Christiansen band is notably absent from the Ariel spectra and synthetic spectra composed of large grain sizes (diameters ∼100 μm; Gerakines & Hudson 2020), generated using our Hapke–Mie approach (Appendix A.2).
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: The real “n” (blue) and imaginary “k” (red) complex refractive indices for crystalline CO2 ice measured in the laboratory at 70 K (Gerakines & Hudson 2020) compared to arbitrarily scaled spectra (1σ errors) of Ariel’s leading and trailing (offset upward for clarity) hemispheres. Dashed lines indicate spectral features identified on Ariel that result from 12CO2 and 13CO2 ice and correspond to changes in n and k as a function of wavelength. Ariel’s 12CO2 scattering peak starts close to 4.175 μm, where k substantially increases above n, and ends near 4.265 μm, where k drops off steeply and n increases above 6. The 4.30 μm 16O12C18O and 4.38 μm 13CO2 features coincide with small increases in k above zero and slight dips in n.
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: (a) Spectra of Ariel’s leading (purple) and trailing (red) hemispheres, scaled to arbitrary reflectance, fit by fourth-order polynomials simulating their continua. Dashed lines highlight the canonical central wavelength position of H2O2 measured in the laboratory (3.505 μm) and two other subtle features centered near 3.545 and 3.602 μm we have identified on Ariel's trailing hemisphere. (b) Continuum-subtracted spectra of Ariel’s leading (purple) and trailing (red, offset upward by 0.0025) hemispheres, spanning the 3.4–3.7 μm wavelength range. A two-Gaussian model (black) has been fit to the weak 3.55 and 3.60 μm features observed on Ariel’s trailing hemisphere that are not seen on its leading hemisphere. Neither spectrum exhibits a 3.505 μm band resulting from a H2O2 combination mode (Bain & Giguère 1955).
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: Carbon isotopic composition (light/heavy) of steady-state CO2 at the surface of Ariel. These results show how input values of the 12C/13C ratio from organics or carbonates (dark horizontal lines) are shifted downward by Jeans escape. For each set of lighter-colored curves, we consider a case with a surface-bound exosphere at all temperatures and T atm = T surf (dotted), a case where the exobase altitude has been increased to 2000 km while keeping T atm = T surf (dashed), and a case where the exobase altitude remains at 2000 km but the atmospheric temperature is 20 K lower than the surface temperature. The offsets for these cases are intended to be illustrative, and other values are possible.
Paper: JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior
Authors: Richard J. Cartwright, Bryan J. Holler, William M. Grundy, Stephen C. Tegler, Marc Neveu, Ujjwal Raut, Christopher R. Glein, Tom A. Nordheim, Joshua P. Emery, Julie C. Castillo-Rogez, Eric Quirico, Silvia Protopapa, Chloe B. Beddingfield, Matthew M. Hedman, Katherine de Kleer, Riley A. DeColibus, Anastasia N. Morgan, Ryan Wochner, Kevin P. Hand, Geronimo L. Villanueva, Sara Faggi, Noemi Pinilla-Alonso, David E. Trilling, Michael M. Mueller
Figure caption: Ratio between Ariel’s trailing and leading hemispheres, normalized to 1 at 4 μm. Dashed lines highlight the spectral features identified in the Ariel data (Figure 1) that show notable trailing/leading hemispherical asymmetries, including subtle features near 3.01, 3.33, 4.84, and 4.93 μm that could result from deposits of CO2 ice upward of 10 mm thick (Section 4.1, Figure 4). Candidate species are described in Appendix A.7.
Paper: Modeling Time-variable Elemental Abundances in Coronal Loop Simulations
Authors: Jeffrey W. Reep, John Unverferth, Will T. Barnes, Sherry Chhabra
Figure caption: The evolution of the electron temperature (left column), density (center column), and abundance factor (right column) for a 40 Mm coronal loop, heated with 0.01, 0.03, 0.1, and 1.0 erg s−1 cm−3 (rows), for a 20 s heating pulse. The blue lines show the case with time-variable abundances f(t), while orange lines show time-fixed photospheric abundances (f = 1), and green time-fixed coronal abundances (f = 4).✎
Paper: Modeling Time-variable Elemental Abundances in Coronal Loop Simulations
Authors: Jeffrey W. Reep, John Unverferth, Will T. Barnes, Sherry Chhabra
Figure caption: Two examples of nanoflare trains, with five heating events spaced 300 s apart, for loops of 40 and 80 Mm. The abundance factor f falls with each successive heating event.✎
Paper: Modeling Time-variable Elemental Abundances in Coronal Loop Simulations
Authors: Jeffrey W. Reep, John Unverferth, Will T. Barnes, Sherry Chhabra
Figure caption: Similar to Figure 1, showing the results for an 80 Mm loop heated impulsively for 20 s.✎
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: Plot of the difference in the height of the LE and core in the combined K-Cor and LASCO FOV and the difference between the SWAP eruption front and K-Cor core in the SWAP FOV for the CMEs on 2014 December 21 (a), 2020 November 26 (b), 2021 May 7 (c), 2021 June 10 (d), and 2022 May 24 (e). Please note that in (b), the corresponding SWAP observations were not available for this particular CME.
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: Snapshots of the CMEs occurring on 2014 December 21 (top row), 2020 November 26 (middle row), and 2021 May 7 (bottom row) for the eruption front as observed by SWAP (left column) and for the three-part-structured CMEs as seen in the K-Cor (right column) FOV.
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: Snapshots of the CMEs occurring on 2021 June 10 (top row) and 2022 May 24 (bottom row) for the eruption front as observed by SWAP (left column) and for the three-part-structured CMEs as observed in the K-Cor (right column) FOV.
Paper: Probing Velocity Dispersion Inside Coronal Mass Ejections: New Insights on Their Initiation
Authors: Satabdwa Majumdar, Elke D'Huys, Marilena Mierla, Nitin Vashishtha, Dana-Camelia Talpeanu, Dipankar Banerjee, Martin A. Reiss
Figure caption: Velocity profiles of the LE and core in the combined K-Cor and LASCO FOV for the CMEs on 2014 December 21 (a), 2020 November 26 (b), 2021 May 7 (c), and 2021 June 10 (d).
Paper: X-Ray Quasi-periodic Eruptions and Tidal Disruption Events Prefer Similar Host Galaxies
Authors: T. Wevers, K. D. French, A. I. Zabludoff, T. C. Fischer, K. Rowlands, M. Guolo, B. Dalla Barba, R. Arcodia, M. Berton, F. Bian, I. Linial, G. Miniutti, D. R. Pasham
Figure caption: Constraints on the ionizing luminosity. Every data point represents the minimum required ionizing luminosity to explain the EELR (indicated by the orange horizontal line), assuming recombination balance, for an individual spaxel. The inner regions of GSN 069 and eRO-QPE2 are actively star-forming, so they are excluded for clarity (marked by the red vertical lines).
Paper: X-Ray Quasi-periodic Eruptions and Tidal Disruption Events Prefer Similar Host Galaxies
Authors: T. Wevers, K. D. French, A. I. Zabludoff, T. C. Fischer, K. Rowlands, M. Guolo, B. Dalla Barba, R. Arcodia, M. Berton, F. Bian, I. Linial, G. Miniutti, D. R. Pasham
Figure caption: Aperture spectra of eRO-QPE2, for the regions indicated in Figure 1, with the same color-coding.
Paper: X-Ray Quasi-periodic Eruptions and Tidal Disruption Events Prefer Similar Host Galaxies
Authors: T. Wevers, K. D. French, A. I. Zabludoff, T. C. Fischer, K. Rowlands, M. Guolo, B. Dalla Barba, R. Arcodia, M. Berton, F. Bian, I. Linial, G. Miniutti, D. R. Pasham
Figure caption: Aperture spectra of RX J1301, for the regions indicated in Figure 1, with the same color-coding.