adsabs/AstroCLIMB huggingface dataset:
Paper: The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster
Authors: Xiang-Lei Chen, Chao-Wei Tsai, Di Li, Pei Wang, Yi Feng, Jun-Shuo Zhang, Guo-Dong Li, Yong-Kun Zhang, Lu-Lu Bao, Mai Liao, Lu-Dan Zhang, Pei Zuo, Dong-Wei Bao, Chen-Hui Niu, Rui Luo, Wei-Wei Zhu, Hu Zou, Sui-Jian Xue, Bing Zhang
Figure caption: GTC/OSIRIS+ R500R spectrum of the FRB 20240114A host galaxy at z = 0.1306. The noise, including the sky residual, is represented by the red dashed line, and the blue shaded regions represent the masked areas in the emission line fitting due to noise and telluric absorption around 7600 Å. The lower panels show the best-fitting results of the emission lines of Hβ, [O III]λλ4959,5007 (left) and Hα, [N II]λλ6548,6583, [S II]λ6716 (right), respectively. The blue dashed lines represent the best fittings.
Paper: The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster
Authors: Xiang-Lei Chen, Chao-Wei Tsai, Di Li, Pei Wang, Yi Feng, Jun-Shuo Zhang, Guo-Dong Li, Yong-Kun Zhang, Lu-Lu Bao, Mai Liao, Lu-Dan Zhang, Pei Zuo, Dong-Wei Bao, Chen-Hui Niu, Rui Luo, Wei-Wei Zhu, Hu Zou, Sui-Jian Xue, Bing Zhang
Figure caption: Locations of FRB 20240114A (red dot) and the identified galaxy group candidate (blue dots). The black dashed circle represents the typical scale of a galaxy cluster with a radius of 1 Mpc. The remaining gray dots represent other galaxies used in the FoF algorithm analysis that are not part of the identified group. The projection of r500 for the foreground galaxy cluster is indicated by the purple dashed circle.
Paper: The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster
Authors: Xiang-Lei Chen, Chao-Wei Tsai, Di Li, Pei Wang, Yi Feng, Jun-Shuo Zhang, Guo-Dong Li, Yong-Kun Zhang, Lu-Lu Bao, Mai Liao, Lu-Dan Zhang, Pei Zuo, Dong-Wei Bao, Chen-Hui Niu, Rui Luo, Wei-Wei Zhu, Hu Zou, Sui-Jian Xue, Bing Zhang
Figure caption: Best-fit SED template model of the host galaxy of FRB 20240114A. The magenta points with error bars represent the extinction-corrected photometric data. The SED modeling uses the template of the irregular galaxy from R. J. Assef et al. (2010), as described in Section 3.3.
Paper: The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster
Authors: Xiang-Lei Chen, Chao-Wei Tsai, Di Li, Pei Wang, Yi Feng, Jun-Shuo Zhang, Guo-Dong Li, Yong-Kun Zhang, Lu-Lu Bao, Mai Liao, Lu-Dan Zhang, Pei Zuo, Dong-Wei Bao, Chen-Hui Niu, Rui Luo, Wei-Wei Zhu, Hu Zou, Sui-Jian Xue, Bing Zhang
Figure caption: Legacy Survey r-band image (DR9; A. Dey et al. 2019) of the host galaxy of FRB 20240114A. The red circle marks the FRB location with an uncertainty of r = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2.
Paper: Evidence for Variable Accretion onto PDS 70 c and Implications for Protoplanet Detections
Authors: Yifan Zhou, Brendan P. Bowler, Aniket Sanghi, Gabriel-Dominique Marleau, Shinsuke Takasao, Yuhiko Aoyama, Yasuhiro Hasegawa, Thanawuth Thanathibodee, Taichi Uyama, Jun Hashimoto, Kevin Wagner, Nuria Calvet, Dorian Demars, Ya-Lin Wu, Lauren I. Biddle, Sebastiaan Y. Haffert, Marta L. Bryan
Figure caption: Primary-subtracted images of PDS 70 in 2020 (left) and 2024 (right). North is up and east is to the left. Color scales of the two panels are identical. The expected positions of PDS 70 b and c are marked. The white dashed line marks the inner edge of PDS 70’s outer disk in infrared scattered light. PDS 70 b is detected in both epochs and demonstrates a significant orbital motion. PDS 70 c is only detected in Epoch 2024. The apparent brightness variations in PDS 70 b and c do not accurately represent the planets’ intrinsic variability, as high-contrast imaging postprocessing introduces flux loss. For a comprehensive analysis of the evidence for variability, refer to Section 3.3.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Evidence for Variable Accretion onto PDS 70 c and Implications for Protoplanet Detections
Authors: Yifan Zhou, Brendan P. Bowler, Aniket Sanghi, Gabriel-Dominique Marleau, Shinsuke Takasao, Yuhiko Aoyama, Yasuhiro Hasegawa, Thanawuth Thanathibodee, Taichi Uyama, Jun Hashimoto, Kevin Wagner, Nuria Calvet, Dorian Demars, Ya-Lin Wu, Lauren I. Biddle, Sebastiaan Y. Haffert, Marta L. Bryan
Figure caption: The variable Hα flux of PDS 70 c. Top and middle rows: forward modeling at the expected positions of PDS 70 c in the 2020 and 2024 data. Both epochs consist of data collected spanning a few months (Table 2). The three panels (from left to right) are cutout data stamps centered at the planet, best-fit forward models, and fitting residuals, respectively. PDS 70 c is not detected in Epoch 2020, and the model in the top-middle row is consistent with zero flux. Bottom row: a comparison of PDS 70 c’s Hα flux measured in different epochs. Marginal posterior distributions of HST-based measurements are shown by filled histograms (blue and orange). The VLT/MUSE measurement (f = (3.1 ± 0.3) × 10−16 erg s−1 cm−2; J. Hashimoto et al. 2020) is shown as a green solid line.
Paper: Evidence for Variable Accretion onto PDS 70 c and Implications for Protoplanet Detections
Authors: Yifan Zhou, Brendan P. Bowler, Aniket Sanghi, Gabriel-Dominique Marleau, Shinsuke Takasao, Yuhiko Aoyama, Yasuhiro Hasegawa, Thanawuth Thanathibodee, Taichi Uyama, Jun Hashimoto, Kevin Wagner, Nuria Calvet, Dorian Demars, Ya-Lin Wu, Lauren I. Biddle, Sebastiaan Y. Haffert, Marta L. Bryan
Figure caption: Estimations of the disk-scattered light emission (top panels) and the disk radial profiles (bottom panel). The top panels include a primary-subtracted image (left), the best-fitting model (middle), and the disk subtraction residuals. The primary subtraction was conducted using a relatively less aggressive strategy (nsector = 1, i.e., no subdivision within an annulus) to preserve disk flux. The Hα scattered light of the disk can be reasonably well fit by a simple geometric model. In the radial direction, the disk’s Hα scattered light peaks at 50 au, slightly closer to the star than the disk seen in infrared. The disk surface brightness is low and has negligible contaminations to the planets’ flux.
Paper: Evidence for Variable Accretion onto PDS 70 c and Implications for Protoplanet Detections
Authors: Yifan Zhou, Brendan P. Bowler, Aniket Sanghi, Gabriel-Dominique Marleau, Shinsuke Takasao, Yuhiko Aoyama, Yasuhiro Hasegawa, Thanawuth Thanathibodee, Taichi Uyama, Jun Hashimoto, Kevin Wagner, Nuria Calvet, Dorian Demars, Ya-Lin Wu, Lauren I. Biddle, Sebastiaan Y. Haffert, Marta L. Bryan
Figure caption: Comparisons of the Lacc–LHα relationships near the observed LHα of PDS 70 c. Predictions from the planetary accretion shock model (Y. Aoyama et al. 2021; blue solid line), the planetary magnetospheric model (T. Thanathibodee et al. 2019; orange solid line), and the empirical relation observed in T Tauri stars (J. M. Alcalá et al. 2017; green dashed line) are shown. The vertical gray region highlights the range of LHα observed in PDS 70 c. Empirically mapping the Lacc–LHα relationship in the PDS 70 planets will test these predictions.
Paper: Evidence for Variable Accretion onto PDS 70 c and Implications for Protoplanet Detections
Authors: Yifan Zhou, Brendan P. Bowler, Aniket Sanghi, Gabriel-Dominique Marleau, Shinsuke Takasao, Yuhiko Aoyama, Yasuhiro Hasegawa, Thanawuth Thanathibodee, Taichi Uyama, Jun Hashimoto, Kevin Wagner, Nuria Calvet, Dorian Demars, Ya-Lin Wu, Lauren I. Biddle, Sebastiaan Y. Haffert, Marta L. Bryan
Figure caption: Variable Hα flux emitted by the host star. Fluxes measured in Epoch 2020 and Epoch 2024 are shown as orange squares (left) and blue circles (right), respectively. Uncertainties are negligible (<1%) compared to the variability. Scales of absolute flux and relative changes are shown on the left and right axes, respectively. The variability is defined by the relative change over the median flux value.
Paper: Evidence for Variable Accretion onto PDS 70 c and Implications for Protoplanet Detections
Authors: Yifan Zhou, Brendan P. Bowler, Aniket Sanghi, Gabriel-Dominique Marleau, Shinsuke Takasao, Yuhiko Aoyama, Yasuhiro Hasegawa, Thanawuth Thanathibodee, Taichi Uyama, Jun Hashimoto, Kevin Wagner, Nuria Calvet, Dorian Demars, Ya-Lin Wu, Lauren I. Biddle, Sebastiaan Y. Haffert, Marta L. Bryan
Figure caption: Hα variability of PDS 70 c confirmed by injection/recovery tests. Point sources that have the same flux as PDS 70 c measured in Epoch 2024 are injected into the Epoch 2020 frames at the expected position of PDS 70 c (middle) and four different position angles. The injected planets are confidently recovered in all cases.
Paper: Einstein Probe Discovery of EP J005245.1−722843: A Rare Be–White Dwarf Binary in the Small Magellanic Cloud?
Authors: A. Marino, H. N. Yang, F. Coti Zelati, N. Rea, S. Guillot, G. K. Jaisawal, C. Maitra, J.-U. Ness, F. Haberl, E. Kuulkers, W. Yuan, H. Feng, L. Tao, C. Jin, H. Sun, W. Zhang, W. Chen, E. P. J. van den Heuvel, R. Soria, B. Zhang, S.-S. Weng, L. Ji, G. B. Zhang, X. Pan, Z. Lv, C. Zhang, Z. X. Ling, Y. Chen, S. Jia, Y. Liu, H. Q. Cheng, D. Y. Li, K. Gendreau, M. Ng, T. Strohmayer
Figure caption: EP/WXT light curves of J0052 around the epoch of the outburst detection in the soft (0.5–2 keV; top) and hard (2–4 keV; middle) energy bands. The drop in the middle of the light curve of CMOS 37 is caused by instrumental effects. The time evolution of the hardness ratio is also plotted (bottom).
Paper: MMS Observations of the Velocity-space Signature of Shock-drift Acceleration
Authors: P. Montag, G. G. Howes, D. McGinnis, A. S. Afshari, M. J. Starkey, M. I. Desai
Figure caption: Three views of the reduced ion velocity distribution at the edge of the shock foot (C), showing (a) fi(vn, v1), (b) fi(vn, v2), and (c) fi(v2, v1). Comparison of the field–particle correlation with the motional electric field ﹩{C}_{{E}_{1}}({\boldsymbol{v}})﹩ for the same three reduced views, showing the observational results in the second row ((d)–(f)) and the prediction from a Vlasov-mapping model in the third row ((g)–(i)).
Paper: MMS Observations of the Velocity-space Signature of Shock-drift Acceleration
Authors: P. Montag, G. G. Howes, D. McGinnis, A. S. Afshari, M. J. Starkey, M. I. Desai
Figure caption: (a) Magnetic field magnitude ∣B∣ (thin blue) and cross-shock electric field En (thin red), along with boxcar-averaged fields 〈∣B∣〉T (thick blue) and ﹩{\langle {E}_{n}\rangle }_{T}﹩ (thick red), vs. the normalized position along the shock normal xn/di,u. (b) The ion velocity distribution fi(vn, v1) at different positions (A–F) through the shock transition, where the white line is used to separate the reflected ions (above) from the incoming ions (below). (c) The number densities of reflected ions nrefl (red) and incoming beam ions nbeam (blue) vs. xn/di,u. (d) The rate of change of ion energy density by the motional electric field j1,iE1 vs. xn/di,u, split between the reflected ions (red) and incoming beam ions (blue).
Paper: MMS Observations of the Velocity-space Signature of Shock-drift Acceleration
Authors: P. Montag, G. G. Howes, D. McGinnis, A. S. Afshari, M. J. Starkey, M. I. Desai
Figure caption: The trajectory of a typical reflected ion in the shock-rest frame as it interacts with the shock transition (a) in physical space (xn, x1) and (b) in velocity space (vn, v1), where the colors indicate corresponding segments of the trajectory in 3D-3V space. For this perpendicular shock geometry, the upstream bulk flow velocity in the shock-rest frame is given by the upstream E × B velocity (black star), and the downstream bulk flow velocity is given by the downstream E × B velocity (green star). The red segment of the trajectory, where the particle has returned upstream after being turned around by Lorentz force of the strong downstream magnetic field, represents the segment where shock-drift acceleration by the motional electric field E1 > 0 is occurring, leading to the particle moving to a higher velocity further away from the origin. The corresponding spatial range of the red segment is 0 ≲ xn/di ≲ 2, corresponding to the shock foot and ramp region, as shown in Figure 2(a).
Paper: MMS Observations of the Velocity-space Signature of Shock-drift Acceleration
Authors: P. Montag, G. G. Howes, D. McGinnis, A. S. Afshari, M. J. Starkey, M. I. Desai
Figure caption: Magnetic field, electric field, ion bulk velocity, and ion number density during MMS3’s crossing through the shock, rotated and transformed to the shock-rest NIF.
Paper: Solar Flares Triggered by a Filament Peeling Process Revealed by High-resolution GST Hα Observations
Authors: Mia Mancuso, Ju Jing, Haimin Wang, Wenda Cao
Figure caption: (a) A GST Hα image prior to the first flare with slits S1 and S2 marked. S1 and S2 cover the erupting filament and are used to create the distance–time stackplot in panel (b). (b) Distance–time plot, with GOES SXR flux data (cyan), and normalized Hα intensity overplotted. The locations of slits S1 and S2 are shown above. S1 covers F1, and S2 covers B1, B2, and F2. The linear fits of the filament peeling movement are shown as yellow dashed lines.
Paper: Solar Flares Triggered by a Filament Peeling Process Revealed by High-resolution GST Hα Observations
Authors: Mia Mancuso, Ju Jing, Haimin Wang, Wenda Cao
Figure caption: Comparison between the NLFFF model and observations of the filaments. (Left) Magnetic field Bz, with two MFRs superimposed on it. The rectangle marks the FOV of the right-hand panels for close-up viewing. (Top right) The close-up view of the MRFs in the highlighted region. (Bottom right) The same region in Hα. Yellow dashed lines highlight the approximate locations of the corresponding filament structures.
Paper: Solar Flares Triggered by a Filament Peeling Process Revealed by High-resolution GST Hα Observations
Authors: Mia Mancuso, Ju Jing, Haimin Wang, Wenda Cao
Figure caption: Left: GST images with slits across the strands of filament that appear to be separating from the main body. Right: normalized Hα intensity profile along the slits shown to the left with a Gaussian fit. The FWHM gives an estimate of 177 km ± 13 km.
Paper: Solar Flares Triggered by a Filament Peeling Process Revealed by High-resolution GST Hα Observations
Authors: Mia Mancuso, Ju Jing, Haimin Wang, Wenda Cao
Figure caption: Top: graph of average twist at the footpoint of the lower MFR (boxed region shown in (b)–(e)). A threshold of Tw > 1 is imposed to only pick up the signature from the MFR; error bars are estimated from a quiet background region. The GOES SXR curve is overplotted, showing the evolution of the flare. Vertical lines correspond to the locations of F1, B1, B2, and F2. There is a distinct decrease in twist around the first and second flares, and a buildup of twist in between. Bottom: twist maps ((f)–(i)) calculated from the NLFFF extrapolation and the photospheric vertical current density Jz ((b)–(e)). The region shown is the same as the boxed area in Figure 4(a). Enhancement of twist is evident in the boxed region, which corresponds to the northern footpoint of the lower MFR as identified by the NLFFF extrapolation at 17:00 UT (see Figure 4). An arrow points to the conjugate footpoint of that MFR. The strongest twist values are observed just prior to F2. At the same time there is a decrease in Jz causing a splitting of the current sheet in the boxed area.
Paper: Einstein Probe Discovery of EP J005245.1−722843: A Rare Be–White Dwarf Binary in the Small Magellanic Cloud?
Authors: A. Marino, H. N. Yang, F. Coti Zelati, N. Rea, S. Guillot, G. K. Jaisawal, C. Maitra, J.-U. Ness, F. Haberl, E. Kuulkers, W. Yuan, H. Feng, L. Tao, C. Jin, H. Sun, W. Zhang, W. Chen, E. P. J. van den Heuvel, R. Soria, B. Zhang, S.-S. Weng, L. Ji, G. B. Zhang, X. Pan, Z. Lv, C. Zhang, Z. X. Ling, Y. Chen, S. Jia, Y. Liu, H. Q. Cheng, D. Y. Li, K. Gendreau, M. Ng, T. Strohmayer
Figure caption: Summary plot for the spectral analysis performed for J0052. Panel (a): single spectra divided by each instrument's effective area taken by EP/FXT (triangles), Swift/XRT (squares), and NICER (circles). The time for each spectrum is referenced from MJD 60458.23. Panel (b): best-fit unabsorbed models of selected observations. Panel (c): unfolded NICER spectrum taken during Epoch 4 along with the best-fit model (top panel). The bbodyrad component is represented by a dashed black line, while the apec component is drawn with dotted silver line. The energies of the identified edges are marked with vertical maroon lines. The unmodeled and modeled residuals are shown in the middle and bottom panel.
Paper: Einstein Probe Discovery of EP J005245.1−722843: A Rare Be–White Dwarf Binary in the Small Magellanic Cloud?
Authors: A. Marino, H. N. Yang, F. Coti Zelati, N. Rea, S. Guillot, G. K. Jaisawal, C. Maitra, J.-U. Ness, F. Haberl, E. Kuulkers, W. Yuan, H. Feng, L. Tao, C. Jin, H. Sun, W. Zhang, W. Chen, E. P. J. van den Heuvel, R. Soria, B. Zhang, S.-S. Weng, L. Ji, G. B. Zhang, X. Pan, Z. Lv, C. Zhang, Z. X. Ling, Y. Chen, S. Jia, Y. Liu, H. Q. Cheng, D. Y. Li, K. Gendreau, M. Ng, T. Strohmayer
Figure caption: Schematic evolutionary path of J0052 as described in the text. This is the lower-mass analog of the evolutionary model by G. M. H. J. Habets (1986a) for forming a Be X-ray binary, here adapted for the case in which the accreting object is a massive Ne–O WD.
Paper: Einstein Probe Discovery of EP J005245.1−722843: A Rare Be–White Dwarf Binary in the Small Magellanic Cloud?
Authors: A. Marino, H. N. Yang, F. Coti Zelati, N. Rea, S. Guillot, G. K. Jaisawal, C. Maitra, J.-U. Ness, F. Haberl, E. Kuulkers, W. Yuan, H. Feng, L. Tao, C. Jin, H. Sun, W. Zhang, W. Chen, E. P. J. van den Heuvel, R. Soria, B. Zhang, S.-S. Weng, L. Ji, G. B. Zhang, X. Pan, Z. Lv, C. Zhang, Z. X. Ling, Y. Chen, S. Jia, Y. Liu, H. Q. Cheng, D. Y. Li, K. Gendreau, M. Ng, T. Strohmayer
Figure caption: Best-fit spectral parameters obtained in this work and their evolution during the outburst. The color sequence is the same as the one used in Figure 2. See also Tables A1 and A2.
Paper: Lunar Ionosphere in the Geotail Region as Observed by Chandrayaan-2 Orbiter Using Two-way Radio Occultation Measurements
Authors: Keshav R. Tripathi, R. K. Choudhary, K. M. Ambili
Figure caption: The left panel displays the integrated TEC observed on 2022 November 8 at ∼18:00 UTC, near the north pole at 74° latitude and 84°W longitude, and the corresponding electron density profile (EDP) is shown in the right panel (black curve). The error bar in blue and red color indicate the σ and 3σ variation in electron density, respectively, with σ representing the standard deviation. The area shaded in cyan has negative electron density, which stands for noise. More details are given in the supplementary part of the manuscript. The gray-colored profile represents the lunar ionospheric model (LIM) output, and PCE stands for photochemical equilibrium. More details can be found in the main text. The middle panel of the figure shows the simulated EDP at the observation site when the Moon is inside the geotail in the absence of a crustal magnetic field.
Paper: Lunar Ionosphere in the Geotail Region as Observed by Chandrayaan-2 Orbiter Using Two-way Radio Occultation Measurements
Authors: Keshav R. Tripathi, R. K. Choudhary, K. M. Ambili
Figure caption: Simulation of Earth’s magnetopause using empirical relation, during solar minimum conditions. The X-axis is along the line joining Earth’s center to the Sun. The Y-axis represents the radial distance of the magnetosphere, ﹩\sqrt{{y}^{2}+{z}^{2}}﹩ in the GSM coordinate system. Values of Z component of interplanetary magnetic field (Bz) and solar wind dynamic pressure are taken from the OMNIWeb server (https://omniweb.gsfc.nasa.gov/form/dx1.html) for 2022 November 8. This structure of the magnetosphere is approximated for the other days. Purple dots are the location of the Moon for each day (00:00:00 UT). The estimated radial distance of a subsolar point on the magnetosphere is 9.13 Re, and Re is the radius of Earth.
Paper: Lunar Ionosphere in the Geotail Region as Observed by Chandrayaan-2 Orbiter Using Two-way Radio Occultation Measurements
Authors: Keshav R. Tripathi, R. K. Choudhary, K. M. Ambili
Figure caption: Upper panel: time variation in the frequency residual observed on 2022 November 8. The purple color represents baseline data above 40 km altitude. Additionally, the straight line in black color indicates the linear fit obtained using the baseline data points. Bottom panel: corresponding phase variation in the radio signal in orange color with 1σ error bars (estimated using data above 40 km altitudes), calculated using baseline-calibrated data from the upper panel. Blue points represent the phase shift averaged within 1 km vertical resolution. The black line passes through the zero and is parallel to the x-axis.
Paper: Lunar Ionosphere in the Geotail Region as Observed by Chandrayaan-2 Orbiter Using Two-way Radio Occultation Measurements
Authors: Keshav R. Tripathi, R. K. Choudhary, K. M. Ambili
Figure caption: Schematic diagram of the lunar ionosphere in a plane. Arrows depict the path of the radio signals passing through the concentric circular shells. n1, n2,...nn represent the electron density value in respective shells. a0, a1, ... and an represent the radial distance.
Paper: Magnetic Field Amplification during Stellar Collisions between Low-mass Stars
Authors: Taeho Ryu, Alison Sills, Ruediger Pakmor, Selma de Mink, Robert Mathieu
Figure caption: Growth of the magnetic field energy EB (line plot at the bottom) as a function of time in the collision between 0.7 M⊙ and 0.6 M⊙ stars with an impact parameter of b = 0.5. The panels above the line plot depict the distributions of the density ρ (top row), the passive scalar (middle row), and the magnetic field strength B (bottom row) at four different times. After the two stars make the first contact at t = 0 hr, they pass by (t = 5 hr). Magnetic fields start to grow due to instabilites and compression caused by the first encounter. However, they stop growing while the two stars are effectively isolated. Soon, they encounter (t ≃ 11 hr) and pass by again. The less massive star is destroyed at the third contact (t ≃ 14 hr) and mixed into the more massive star (t ≃ 16 hr), during which magnetic fields grow at the fastest rate. The amplification rate dramatically decreases while the collision product is being relaxed to recover a dynamically steady state (t ≳ 20 hr).
Paper: Discovery of the Richest Pulsating Ultramassive White Dwarf
Authors: Francisco C. De Gerónimo, Murat Uzundag, Alberto Rebassa-Mansergas, Alex Brown, Mukremin Kilic, Alejandro H. Córsico, Gracyn C. Jewett, Adam G. Moss
Figure caption: FT of the light curves obtained from HiPERCAM, with the same color scheme as in Figure 1. The horizontal black dashed line indicates the significance level corresponding to S/N = 4. The right panels display the spectral window for each light curve centered at 1000 μHz for a comparison.
Paper: Discovery of the Richest Pulsating Ultramassive White Dwarf
Authors: Francisco C. De Gerónimo, Murat Uzundag, Alberto Rebassa-Mansergas, Alex Brown, Mukremin Kilic, Alejandro H. Córsico, Gracyn C. Jewett, Adam G. Moss
Figure caption: Location of our UM ONe(CO)-core WD evolutionary tracks, depicted with solid (dashed) lines, together with the determinations for WD J0135+5722 (Teff = 12,415 ± 87 K and ﹩\mathrm{log}\,g=8.9\pm 0.007﹩) in the log g–Teff plane. We also include the spectroscopic determinations for the already known to pulsating UM WDs. The mass of WD J0135+5722 is 1.118 ± 0.002 M⊙ if its core is made of ONe and 1.135 ± 0.0035 M⊙ if the star has a CO core.
Paper: Discovery of the Richest Pulsating Ultramassive White Dwarf
Authors: Francisco C. De Gerónimo, Murat Uzundag, Alberto Rebassa-Mansergas, Alex Brown, Mukremin Kilic, Alejandro H. Córsico, Gracyn C. Jewett, Adam G. Moss
Figure caption: FT of the light curves obtained from APO on December 23 (upper panel) and on September 1 (bottom panel). The horizontal black dashed line indicates the significance level corresponding to S/N = 4. The right panels display the spectral window for each light curve centered at 1000 μHz for a comparison.