adsabs/AstroCLIMB huggingface dataset:
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Measured pattern speeds for rotations lasting ≥ 1 h −1 Gyr for DM-only and DM+B runs of TNG50. The histograms are fit by log-normal distributions with a mean of 0.254 ± 0.005 h km s−1 kpc−1 for the DM-only simulation and 0.289 ± 0.007 h km s−1 kpc−1 for the mixed-phase DM+baryonic run. Predicted counts for our DM-only halos using the distributions measured by Bailin & Steinmetz (2004) and Bryan & Cress (2007) are shown. There is very good agreement between our results and those of Bryan & Cress (2007) in TNG50 DM-only halos, but we observe a slight shift to higher pattern speeds in the TNG50 DM+B halos on the order of ∼14%.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Normalized 2D histograms of rotation axis orientations for mixed DM+B runs (top left) and DM-only (top right) TNG50 runs. Bottom row shows scatter plot of the same halos. The halo minor axis is along the z direction (θ = 90°), and the major axis is along the x direction (θ, ϕ = 0°). DM-only and DM+B simulations show qualitatively similar results, with a majority halos having their rotation axes aligned with the halo minor axis or major axis. Rotation axes that are aligned with no principal axis are present in both types of simulations.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Left: Fraction of figure rotation axes within 20° of the halo minor axis against the duration of the rotation. Right: Cumulative distribution of the rotation axis polar angle, binned in rotation duration. A higher cumulative fraction of rotation axes within a given angular distance indicates stronger alignment between the figure rotation axis and the halo minor axis. In both DM-only and DM+B TNG50 realizations, longer-lived rotations show a higher degree of alignment between the rotation axis and the halo minor axis. In the presence of baryons, rotation axes are better aligned with the halo minor axis at all rotation durations.
Paper: Figure Rotation of IllustrisTNG Halos
Authors: Neil Ash, Monica Valluri
Figure caption: Observed figure rotation pattern speeds are independent of the halo virial mass. Left: Scatter plot of measured pattern speeds against the halo virial mass at z = 0 for both DM-only (blue) and DM+B (orange) runs of TNG50. Right: Medians of log-normal distributions fit in four different mass bins spanning 1010 h −1–1012 h −1 M ⊙ using bootstrap fitting with 500 samples per mass bin. The shaded region shows the upper and lower bounds of these bootstrap samples. Dashed lines indicate the full population medians. Results of the bootstrap analysis are consistent with pattern speeds that are independent of halo mass.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: BH mass M BH as a function of galaxy stellar mass M * for a sample of low-mass IMBHs from Filippenko & Ho (2003), Barth et al. (2004), van den Bosch & de Zeeuw (2010), Reines et al. (2013), Baldassare et al. (2015), Baldassare et al. (2016), Nguyen et al. (2018, 2019), and Baldassare et al. (2020). We also include the M *–M BH relation for dwarf galaxies from Reines & Volonteri (2015) and a sample of dwarf galaxies from Ward et al. (2022), scaled to the Reines & Volonteri (2015) relation. In blue, we show the best-fit M * for the Ia-TDE candidates and place them with upper limits on the mass of the BH of 105 M ⊙.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: Separation between transients and their host galaxy as a function of the normalized host separation R  n . The nuclear Ia-TDE candidates, shown as stars, appear to be a better match to the Ia-TDE models from M16 than the best off-nuclear candidates, shown as diamonds. The relative size of each data point corresponds to 1/χ 2 and represents the goodness of fit to the M16 light-curve models.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: In color, we show spectra of the four classified nuclear Ia-TDE candidates. The gray spectra are examples of SNe Ia rejected as Ia-TDE candidates in Section 3. The pink spectrum is the normal Type Ia SN 2011fe. The black dot marks the trough of the Si II λ6355 line for each transient, showing the velocity difference between normal SNe Ia and the Ia-TDE candidates. Compare to Figure 9 of M16.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: Spectrum of the most likely Ia-TDE candidate, SN 2020lrt from Dahiwale & Fremling (2020b), and a spectrum of SN 2020bpf, classified as a SN Ib by Dahiwale & Fremling (2020a). For comparison, we show the best-fit spectral model from M16 to the spectrum of SN 2020lrt, and a comparison SN Iax spectrum from Blondin et al. (2012). We mark common elements with vertical lines.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: Photometry of the host galaxies of the nuclear Ia-TDE candidates. The blue line represents the best-fit Prospector model, and the blue squares are the corresponding model photometry points, with the observed photometry in red. The best-fit stellar mass for each galaxy is shown in Table 1.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: The g − r color measured during peak compared to the time it takes a transient to rise from discovery to peak for the 1838 nuclear transients. We also show where the best Ia-TDE candidates lie in this parameter space.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: The same as Figure 4, but for the off-nuclear transients. 2021xpf and 2020xmo do not have a spectroscopic classification.
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: The optical spectrum of Gaia17bpp using the APO 3.5 m KOSMOS spectrograph using the high-red grating. The uncorrected telluric lines have been marked with gray solid lines. We compare the Gaia17bpp spectrum to HD 19305 (M0V) and HD 213893 (M0IIIb) standards (Rayner et al. 2009).
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Historical optical-to-near-IR light curve of Gaia17bpp. We correct the PS1r and PS1g to match the average magnitude baseline of the ZTF light curves. The data in the bottom panel are provided in machine-readable form in the online journal.(The data used to create this figure are available.)
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: SED fit (black synthetic PHOENIX spectrum) to the obtained broadband photometry outside the Gaia17bpp dimming event. We also include a simple blackbody fit to the photometry accounting for the effects of extinction at the line of sight. The bottom panel represents the residual levels from the PHOENIX model. We note that the SED fitting model does not extend to the W3 detection and W4 upper limit.
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Color evolution of Gaia17bpp in the infrared and infrared-to-optical photometry. We highlight in gray the primary region of the dimming event and in red the egress of the dimming event. In each panel, the underlying solid black line model was produced from a generalized Gaussian distribution described in Section 4.
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Corner plot of the posterior distribution from the nested Monte Carlo sampling using Ariadne. The dashed lines are the median and 2σ  confidence interval of each distribution.
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Color−magnitude diagram (in gray) for the nearby Gaia DR3 sample (Gaia Collaboration et al. 2023) shaded by the number of stars per bin. We overplot the position of Gaia17bpp on the color−magnitude diagram from the most recent BP/RP fluxes and Gaia G estimates using GPSA.
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: MIST isochrone mass posterior distribution histogram including a KDE (black line).
Paper: Gaia17bpp: A Giant Star with the Deepest and Longest Known Dimming Event
Authors: Anastasios Tzanidakis, James R. A. Davenport, Eric C. Bellm, Yuankun Wang
Figure caption: Gaia17bpp issued alert light curve in Gaia G. The red line indicates the issued alert epoch.
Paper: Using Tianwen-1 Differential One-way Range Signals to Probe Corotating Interaction Regions: Case Studies
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: In situ measurements of solar wind plasma by STEREO-A from 2021 February 7 to 11 (a)–(d) and near the Earth from 2021 February 11 to 15 (e)–(h). From top to bottom, the plots show the solar wind density, speed, temperature, and total magnetic field, respectively. The red dashed lines indicate the times of the solar wind speed maxima within the CIRs of interest.
Paper: Using Tianwen-1 Differential One-way Range Signals to Probe Corotating Interaction Regions: Case Studies
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: Simulation results of the CIRs passing through the DOR signal path. (a) Constructed CIR structure on 2021 February 11 using the solar wind density data measured by STEREO-A. (b) The relative changes in the differential phase delay and TEC on 2021 February 11. (c) Constructed CIR structure on 2021 February 17 using the solar wind density data measured by STEREO-A. (d) The relative changes in the differential phase delay and TEC on 2021 February 17, 18, and 19.
Paper: Using Tianwen-1 Differential One-way Range Signals to Probe Corotating Interaction Regions: Case Studies
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: In situ measurements of solar wind plasma by STEREO-A from 2021 February 13 to 20 (a)–(d) and near the Earth from 2021 February 17 to 24 (e)–(h). From top to bottom, the plots show the solar wind density, speed, temperature, and total magnetic field, respectively. The red dashed lines indicate the times of the solar wind speed maxima within the CIRs of interest.
Paper: Probing Ultralate Reionization: Direct Measurements of the Mean Free Path over 5 < z < 6
Authors: Yongda Zhu, George D. Becker, Holly M. Christenson, Anson D'Aloisio, Sarah E. I. Bosman, Tom Bakx, Valentina D'Odorico, Manuela Bischetti, Christopher Cain, Frederick B. Davies, Rebecca L. Davies, Anna-Christina Eilers, Xiaohui Fan, Prakash Gaikwad, Martin G. Haehnelt, Laura C. Keating, Girish Kulkarni, Samuel Lai, Hai-Xia Ma, Andrei Mesinger, Yuxiang Qin, Sindhu Satyavolu, Tsutomu T. Takeuchi, Hideki Umehata, Jinyi Yang
Figure caption: (a) Direct measurements of λ mfp from this work (orange–red squares) compared to the predictions from recent models (Cain et al. 2021; Garaldi et al. 2022; Lewis et al. 2022). (b) Our measurements compared with indirect constraints based on Lyα opacities (Gaikwad et al. 2023; F. B. Davies et al. 2023, in preparation; Y. Qin et al. 2023, in preparation). Open circles correspond to marginal constraints and arrows correspond to 2σ limits for F. B. Davies et al. (2023, in preparation). The shaded region shows the posterior from Y. Qin et al. (2023, in preparation) at the 68% confidence level. In both panels, for comparison, we also show the direct λ mfp measurements in B21 and Worseck et al. (2014), as well as the lower-limit constraint in Bosman (2021). Symbols are displaced in redshift for display.
Paper: Probing Ultralate Reionization: Direct Measurements of the Mean Free Path over 5 < z < 6
Authors: Yongda Zhu, George D. Becker, Holly M. Christenson, Anson D'Aloisio, Sarah E. I. Bosman, Tom Bakx, Valentina D'Odorico, Manuela Bischetti, Christopher Cain, Frederick B. Davies, Rebecca L. Davies, Anna-Christina Eilers, Xiaohui Fan, Prakash Gaikwad, Martin G. Haehnelt, Laura C. Keating, Girish Kulkarni, Samuel Lai, Hai-Xia Ma, Andrei Mesinger, Yuxiang Qin, Sindhu Satyavolu, Tsutomu T. Takeuchi, Hideki Umehata, Jinyi Yang
Figure caption: Composite QSO spectra for each redshift bin (left-hand panel) and fits to the LyC transmission (right-hand panel). Black curves show observed flux normalized by the median flux over 1270–1380 Å in the rest frame. The red curve shows our best-fit model. Thin orange curves show the fits from bootstrap realization (only 1000 curves are plotted here for display).
Paper: Probing Ultralate Reionization: Direct Measurements of the Mean Free Path over 5 < z < 6
Authors: Yongda Zhu, George D. Becker, Holly M. Christenson, Anson D'Aloisio, Sarah E. I. Bosman, Tom Bakx, Valentina D'Odorico, Manuela Bischetti, Christopher Cain, Frederick B. Davies, Rebecca L. Davies, Anna-Christina Eilers, Xiaohui Fan, Prakash Gaikwad, Martin G. Haehnelt, Laura C. Keating, Girish Kulkarni, Samuel Lai, Hai-Xia Ma, Andrei Mesinger, Yuxiang Qin, Sindhu Satyavolu, Tsutomu T. Takeuchi, Hideki Umehata, Jinyi Yang
Figure caption: (a) Dependence of the λ mfp measurements on Γbg at different redshifts. Nominal values and uncertainties of Γbg we adopt from Gaikwad et al. (2023) are shown with horizontal error bars. (b) Measured λ mfp based on fixed ξ values of 0.33, 0.67, and 1.00. Symbols are displaced in redshift for display.
Paper: Probing Ultralate Reionization: Direct Measurements of the Mean Free Path over 5 < z < 6
Authors: Yongda Zhu, George D. Becker, Holly M. Christenson, Anson D'Aloisio, Sarah E. I. Bosman, Tom Bakx, Valentina D'Odorico, Manuela Bischetti, Christopher Cain, Frederick B. Davies, Rebecca L. Davies, Anna-Christina Eilers, Xiaohui Fan, Prakash Gaikwad, Martin G. Haehnelt, Laura C. Keating, Girish Kulkarni, Samuel Lai, Hai-Xia Ma, Andrei Mesinger, Yuxiang Qin, Sindhu Satyavolu, Tsutomu T. Takeuchi, Hideki Umehata, Jinyi Yang
Figure caption: Direct measurements of λ mfp from this work (orange–red squares) and from the literature (Prochaska et al. 2009; Fumagalli et al. 2013; O’Meara et al. 2013; Worseck et al. 2014; Lusso et al. 2018; B21). Error bars show 68% limits. The dashed line shows the power-law extrapolation of λ mfp from measurements at z < 5.16 (Worseck et al. 2014). The blue arrow shows the lower-limit constraint on λ mfp at z = 6 from Bosman (2021). Symbols are displaced in redshift for display.
Paper: Probing Ultralate Reionization: Direct Measurements of the Mean Free Path over 5 < z < 6
Authors: Yongda Zhu, George D. Becker, Holly M. Christenson, Anson D'Aloisio, Sarah E. I. Bosman, Tom Bakx, Valentina D'Odorico, Manuela Bischetti, Christopher Cain, Frederick B. Davies, Rebecca L. Davies, Anna-Christina Eilers, Xiaohui Fan, Prakash Gaikwad, Martin G. Haehnelt, Laura C. Keating, Girish Kulkarni, Samuel Lai, Hai-Xia Ma, Andrei Mesinger, Yuxiang Qin, Sindhu Satyavolu, Tsutomu T. Takeuchi, Hideki Umehata, Jinyi Yang
Figure caption: [C II] 158 μm emission maps and spectra of QSOs with our new Keck/ESI observations. Contours show (2σ, 3σ, 4σ, 6σ, 8σ, 10σ) levels. Measured redshifts are labeled for each QSO and red curves show the best Gaussian fits. The observed frequency and FWHM of the [C II] emission are also provided for reference.
Paper: Probing Ultralate Reionization: Direct Measurements of the Mean Free Path over 5 < z < 6
Authors: Yongda Zhu, George D. Becker, Holly M. Christenson, Anson D'Aloisio, Sarah E. I. Bosman, Tom Bakx, Valentina D'Odorico, Manuela Bischetti, Christopher Cain, Frederick B. Davies, Rebecca L. Davies, Anna-Christina Eilers, Xiaohui Fan, Prakash Gaikwad, Martin G. Haehnelt, Laura C. Keating, Girish Kulkarni, Samuel Lai, Hai-Xia Ma, Andrei Mesinger, Yuxiang Qin, Sindhu Satyavolu, Tsutomu T. Takeuchi, Hideki Umehata, Jinyi Yang
Figure caption: New Keck/ESI QSO spectra obtained for this work. Orange–red and gray curves plot the flux and zero flux, respectively. J0056+2241 and J1236+4657 (labeled with *) are not included in our sample of λ mfp measurements (see text for details). The spectra are rebinned to 2 Å for display.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: The Sun at 04:00 UT on 2022 September 5 as seen by the different remote-sensing instruments on board Solar Orbiter. Panel (a) shows the line-of-sight magnetic field observed by PHI/FDT, saturated at ±50 G; panel (b) shows the low corona observed using the EUI/FSI 174 Å passband and processed using the multiscale Gaussian normalization technique of Morgan & Druckmüller (2014), with the inset showing a close-up of the source active region (AR). Blue arrows show the AR filament above the internal polarity inversion line. Panel (c) shows the SPICE Ne VIII raster summed across the spectral window, with the solid and dashed squares corresponding to the blue and red spectra respectively shown in Figure 6. The blue squares in panels (a) and (b) show the SPICE field of view, with the red arrow indicating the source AR. Panel (d) shows the location of Solar Orbiter and Parker Solar Probe during the period studied here.
Paper: The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies
Authors: Alessia Moretti, Paolo Serra, Cecilia Bacchini, Rosita Paladino, Mpati Ramatsoku, Bianca M. Poggianti, Benedetta Vulcani, Tirna Deb, Marco Gullieuszik, Jacopo Fritz, Anna Wolter
Figure caption: Molecular gas fraction ﹩{f}_{{{\rm{H}}}_{2}}(={M}_{{{\rm{H}}}_{2}}/{M}_{\star }﹩) as a function of the galaxy stellar mass: the blue line shows the mean scaling relation found in the xCOLD GASS survey by Saintonge et al. (2017) for field galaxies on the main sequence, with its dispersion as the blue shaded region, while orange lines refer to spiral galaxies from the EDGE-CALIFA survey (Bolatto et al. 2017). Gray circles are Virgo galaxies from Brown et al. (2021). Red squares are GASP jellyfish galaxies from Moretti et al. (2020b), with measured ALMA fluxes. Green and magenta symbols show the APEX measurements for galaxies with and without a star-forming tail, with transparent triangles showing the low-S/N detections (and the upper limit for the A3376_S84 source). Symbols enclosed in squares are jellyfish galaxies, from either GASP (black) or Vertico (gray). Galaxies having a MUSE counterpart (Table 1) are labeled with the GASP ID.
Paper: The Eruption of a Magnetic Flux Rope Observed by Solar Orbiter and Parker Solar Probe
Authors: David M. Long, Lucie M. Green, Francesco Pecora, David H. Brooks, Hanna Strecker, David Orozco-Suárez, Laura A. Hayes, Emma E. Davies, Ute V. Amerstorfer, Marilena Mierla, David Lario, David Berghmans, Andrei N. Zhukov, Hannah T. Rüdisser
Figure caption: The filament channel seen using the 193 Å passband on SDO/AIA on August 24 (panel (a)), and line-of-sight photospheric magnetic field observed by SDO/HMI on August 25 (panel (b)) and Solar Orbiter/PHI on September 5 (panel (c)). The cyan arrows in panel (a) show the direction of the plumes associated with the filament channel, indicating a sinistral configuration (see text for details). The cyan lines in panels (b) and (c) show the path of the plasma flow identified using EUI/FSI on September 5 as shown in Figure 3. Both magnetograms have been saturated at ±50 G.
Paper: The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies
Authors: Alessia Moretti, Paolo Serra, Cecilia Bacchini, Rosita Paladino, Mpati Ramatsoku, Bianca M. Poggianti, Benedetta Vulcani, Tirna Deb, Marco Gullieuszik, Jacopo Fritz, Anna Wolter
Figure caption: Phase-space diagram (i.e., galaxy projected velocities normalized to the cluster velocity dispersion (Δ V /σ cl) against the galaxy distances from the central BCG normalized to each cluster r 200) of the three cluster members (A85, A3558, A3376) from OmegaWINGS (grayscale contours, from Moretti et al. 2017), superimposed with the galaxies discussed in this paper (circles) and the four GASP galaxies in Moretti et al. (2020b; squares). Galaxies are color-coded according to their H2 deficiency (top panel) and to their H I deficiency (bottom panel), with green symbols being gas deficient and purple being gas rich. Black triangles in the top panel show low-S/N detections, while black circles in the bottom panel indicate a no detection in MeerKAT (JW108) and missing data (JO60, JO49).
Paper: The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies
Authors: Alessia Moretti, Paolo Serra, Cecilia Bacchini, Rosita Paladino, Mpati Ramatsoku, Bianca M. Poggianti, Benedetta Vulcani, Tirna Deb, Marco Gullieuszik, Jacopo Fritz, Anna Wolter
Figure caption: Correlation between the H I and H2 deficiencies. Crosses show the galaxies in the Virgo cluster from Zabel et al. (2022), while the APEX sample is shown by the colored stars and points, depending on whether the galaxy has star formation in the tail or not. Each symbol is colored according to the classification proposed by Yoon et al. (2017) based on the H I morphology and the H I and H2 content (see text).
Paper: The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies
Authors: Alessia Moretti, Paolo Serra, Cecilia Bacchini, Rosita Paladino, Mpati Ramatsoku, Bianca M. Poggianti, Benedetta Vulcani, Tirna Deb, Marco Gullieuszik, Jacopo Fritz, Anna Wolter
Figure caption: Total cold gas fraction (including both the atomic phase and the molecular phase) against the galaxy stellar mass for the APEX galaxy sample here described (colors and symbols are as in Figure 5) and the XGASS sample (gray circles) from Wang et al. (2020) and Catinella et al. (2018).
Paper: The Evolution of the Cold Gas Fraction in Nearby Clusters’ Ram-pressure-stripped Galaxies
Authors: Alessia Moretti, Paolo Serra, Cecilia Bacchini, Rosita Paladino, Mpati Ramatsoku, Bianca M. Poggianti, Benedetta Vulcani, Tirna Deb, Marco Gullieuszik, Jacopo Fritz, Anna Wolter
Figure caption: CO (2–1) spectra normalized to the peak temperature for the tail observations with an S/N > 3 (excluding the marginal emission shown in the lower right corner, which has S/N = 2.7). The red Gaussian is the best fit. The blue solid line shows the optical velocity, while the orange dashed one shows the H I velocity. The gray shaded region is the rms of the observations in the plot range, after excluding the line emission.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Comparison of cumulative flare frequency distributions in energy. The MUSCLES FFDs are in the FUV (Loyd et al. 2018). TESS FFDs are obtained from Stelzer et al. (2022). The Tilley et al. (2019) FFD is a simulation in the U band, extrapolated from Kepler observations by Hawley et al. (2014).