adsabs/AstroCLIMB huggingface dataset:
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Ratio of the visibility of each satellite for each X-ray transient over the full search time range.
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Visibility of each satellite to the X-ray transient at trigger time. Percentage represents how much of all X-ray transient sources are visible. Shaded areas represent visibility.
Paper: Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT
Authors: Yan-Qiu Zhang, Wang-Chen Xue, Jin-Peng Zhang, Ce Cai, Shao-Lin Xiong, Cheng-Kui Li, Yuan Liu, Chen-Wei Wang, Hao-Xuan Guo, Shuo Xiao, Wen-Jun Tan, Chao Zheng, Jia-Cong Liu, Sheng-Lun Xie, Peng Zhang, Wen-Long Zhang, Yue Wang, Zheng-Hang Yu, Yang-Zhao Ren, Ping Wang, Yue Huang, Xiao-Bo Li, Xiao-Yun Zhao, Shi-Jie Zheng, Zhen Zhang, Shu-Xu Yi, Li-Ming Song, Shuang-Nan Zhang
Figure caption: Property comparison of gamma-ray counterparts with X-ray transients.
Paper: Spectropolarimetry of a Nuclear Transient AT2023clx: Revealing the Geometrical Alignment between the Transient Outflow and the Nuclear Dusty Region
Authors: Kohki Uno, Keiichi Maeda, Takashi Nagao, Giorgos Leloudas, Panos Charalampopoulos, Seppo Mattila, Kentaro Aoki, Kenta Taguchi, Miho Kawabata, Javier Moldon, Miguel Pérez-Torres, Miika Pursiainen, Thomas Reynolds
Figure caption: Left (panel (a)): time evolution of the spectra of AT2023clx from +4 days to +121 days after its first detection. Additionally, the preoutburst spectrum at the position of AT2023clx taken by the Sloan Digital Sky Survey (SDSS) is presented by a gray line. All the spectra are shown in the rest wavelength, corrected for their redshift (z = 0.01107). The vertical dashed lines in red, blue, green, and gray correspond to the rest wavelengths of hydrogen, helium, nitrogen, and sodium lines, respectively. The gray-shaded regions are affected by the telluric absorption. In the early phases, the spectra displayed a blue continuum and broad hydrogen lines. In the later phases, the broad features became weaker. The overall spectral features on +121 days closely resembled the preoutburst spectrum. Right (panel (b)): time evolution of the Hα profile, plotted in velocity space. The rest wavelengths are indicated on the top horizontal axis. The dashed lines show the rest wavelengths of hydrogen and helium lines. The dotted lines show the same atomic lines but with an additional blueshift of 10,000 km s−1. The gray-shaded region shows the wavelength range affected by the telluric absorption. The high-velocity component was diminishing toward later phases.
Paper: Spectropolarimetry of a Nuclear Transient AT2023clx: Revealing the Geometrical Alignment between the Transient Outflow and the Nuclear Dusty Region
Authors: Kohki Uno, Keiichi Maeda, Takashi Nagao, Giorgos Leloudas, Panos Charalampopoulos, Seppo Mattila, Kentaro Aoki, Kenta Taguchi, Miho Kawabata, Javier Moldon, Miguel Pérez-Torres, Miika Pursiainen, Thomas Reynolds
Figure caption: Preoutburst image of the host galaxy of AT2023clx (NGC 3799), created by combining g-, i-, and y-band images from the Pan-STARRS1 survey (N. Kaiser et al. 2002). The inset panel (bottom right) shows an enlarged view of a postoutburst image, as obtained by combining the g-, r-, and i-band images taken by Seimei/TriCCS, showing AT2023clx on the core of NGC 3799. NGC 3799 is in an interacting system with NGC 3800 (another galaxy seen in the top left corner).
Paper: Thermonuclear Superburst of MAXI J1752−457 Observed with NinjaSat and MAXI
Authors: Amira Aoyama, Teruaki Enoto, Takuya Takahashi, Sota Watanabe, Tomoshi Takeda, Wataru Iwakiri, Kaede Yamasaki, Satoko Iwata, Naoyuki Ota, Arata Jujo, Toru Tamagawa, Tatehiro Mihara, Chin-Ping Hu, Akira Dohi, Nobuya Nishimura, Motoko Serino, Motoki Nakajima, Takao Kitaguchi, Yo Kato, Nobuyuki Kawai
Figure caption: The MAXI/GSC 2.0–10.0 keV image obtained between MJD 60623.5 and 60624.0 after being smoothed with a Gaussian filter of its Gaussian kernel of 2 pixel (9﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩0). The color map is shown in a unit of integrated X-ray counts at each 4﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5 × 4﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5 pixel. The positions of MAXI J1752−457 reported by MAXI and EP240809a by Swift are shown as the red cross and blue square markers, respectively (H. Y. Liu et al. 2024; M. Serino et al. 2024). The MAXI 1σ error region is shown as the dashed red circle, whereas the reported EP240809a (Swift) error circle is invisibly small in this plot. The NinjaSat GMC boresight direction and the 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1 FOV are shown in the orange cross and orange dashed circle, respectively. The nearby X-ray sources H 1735−444 and IGR J17361−4441 (green diamonds) are outside of the NinjaSat FOV.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: Top left panel: the muon number obtained by direct measurements at Auger (A. Aab et al. 2020a, 2021) compared to the predictions with and without the application of ΔXmax. Note that in case of the SIBYLL 2.3d model, only the predictions at energy 1019 eV were at our disposal. Top right panel: the ratio of the muon signal in the data and the signal predicted from air-shower simulations with (filled markers) and without (open markers) application of ΔXmax. The results from A. Abdul Halim et al. (2024a) are displayed by triangles. Bottom panels: the Xmax distribution of Auger data (A. Aab et al. 2014a) compared to the prediction for the heavy-metal scenario (Gauss × exp.) using QGSJET II-04 + ΔXmax (left) and SIBYLL 2.3d + ΔXmax (right) in the energy bin 1018.0−18.5 eV. For visualization purposes, the fits to the tail of the predicted Xmax distributions (Λη), corrected for detector acceptance, are shown.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: Top panel: possible directions of an extragalactic dipole in the arrival directions of cosmic rays above 8 EeV, compatible at the 1σ (blue area) and 2σ (blue contour) levels with the Auger measurement (A. Aab et al. 2017b), for the UF23 models of the GMF, shown in Galactic coordinates. The mass composition scenario obtained for SIBYLL 2.3d + ΔXmax is used. Middle panel: the distribution of backtracked directions at the edge of the Galaxy for the 100 most energetic Auger events (A. Abdul Halim et al. 2023a), shown in Galactic coordinates. Bottom panel: distribution of the backtracked directions at the edge of the Galaxy for isotropically distributed arrival directions of iron nuclei on Earth, shown in Galactic coordinates and accounting for the Auger geometrical exposure.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: Top panel: the normalized distribution of the extragalactic amplitudes of the identified solutions from the top panel of Figure 5 for the individual models of the UF23 model of the GMF. Middle panel: possible extragalactic directions of a dipole, compatible at the 1σ (dashed lines) and 2σ (solid lines) levels with the Auger measurement for the eight individual UF23 models of the GMF, shown in Galactic coordinates, using the mass composition obtained for model SIBYLL 2.3d + ΔXmax. Bottom panel: possible extragalactic directions of a dipole at the 2σ level for the UF23 base model of the GMF and three different coherence lengths, shown in Galactic coordinates, using the mass composition obtained for the model SIBYLL 2.3d + ΔXmax.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: Test of beam purity for iron nuclei (left) and silicon nuclei (right) above the energy Emin using the Auger DNN data (A. Abdul Halim et al. 2025a). The p-values of the χ2 test for a constant elongation rate of a single primary type above Emin (in red) and for Xmax fluctuations consistent with pure nuclei above Emin (in black).
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: The ratio of the 100 most energetic backtracked Auger events to the expectation for backtracked isotropically distributed arrival directions on Earth, smoothed with a 25° top-hat function, shown in Galactic coordinates. The supergalactic plane is depicted by dashed–dotted lines with indicated directions of selected groups of galaxies.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: Distributions of Xmax obtained from fits in each energy bin using the model SIBYLL 2.3d + ΔXmax. The plot shows the total fit (sum) alongside the individual contributions of particle species. The p-value of the fit and the energy bin for which the fit is performed are indicated in each panel.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: Same as Figure 7 but for model QGSJET II-04 + ΔXmax.
Paper: Spectropolarimetry of a Nuclear Transient AT2023clx: Revealing the Geometrical Alignment between the Transient Outflow and the Nuclear Dusty Region
Authors: Kohki Uno, Keiichi Maeda, Takashi Nagao, Giorgos Leloudas, Panos Charalampopoulos, Seppo Mattila, Kentaro Aoki, Kenta Taguchi, Miho Kawabata, Javier Moldon, Miguel Pérez-Torres, Miika Pursiainen, Thomas Reynolds
Figure caption: Left (panel (a)): time evolution of the polarization in the Q–U diagram, including the measurements from the imaging polarimetry. To estimate the host dilution factor, we adopt the aperture size of 2″ (see Appendix B). The color of each point corresponds to its wavelength, as indicated by the bottom colorbars; the viridis bar corresponds to the data on Day 5, while the rainbow bar corresponds to the data on Day 52. The black star symbol indicates the background polarization estimated from the averaged data on Day 121. Furthermore, the blue and red contours in the QU plane show the two-dimensional density distributions of the polarization data points on Days 5 and 52, respectively. The contours correspond to enclosed probability levels of 30% (dotted), 50% (dashed), and 80% (solid), based on Gaussian kernel density estimation. The polarization angle flipped by ∼90° from Day 5 to 52 with respect to the background polarization. Right (panel (b)): the Q–U diagram shown across the Hα profile on Day 5. The gray crosses are all the data points, and the color points are the data points for the Hα, color-coded by the Hα velocity. The black star symbol indicates the background polarization estimated from the averaged data at Day 121. These figures show that the polarization degrees and angles at the wavelengths corresponding to the Hα deviate from the continuum region of the Day 5 data, indicating the line depolarization effect. The Q–U position of the Hα is intermediate between the Day 5 continuum and the Day 121 data point, overlapping with the latter; this behavior supports our interstellar polarization estimation.
Paper: Spectropolarimetry of a Nuclear Transient AT2023clx: Revealing the Geometrical Alignment between the Transient Outflow and the Nuclear Dusty Region
Authors: Kohki Uno, Keiichi Maeda, Takashi Nagao, Giorgos Leloudas, Panos Charalampopoulos, Seppo Mattila, Kentaro Aoki, Kenta Taguchi, Miho Kawabata, Javier Moldon, Miguel Pérez-Torres, Miika Pursiainen, Thomas Reynolds
Figure caption: Evolution of spectropolarimetric properties of AT2023clx. Panel (a) shows the Stokes parameters of Q (top panel) and U (second panel), the polarization degree P (third panel), and the polarization angle θ (bottom panel) on Day 5. The blue data point represents polarization values binned with 20 pixels, corresponding to ∼26.8 Å. The error bars show the photon shot noise per bin. The underlying gray spectrum in each plot is the unbinned flux spectrum at the same epoch. AT2023clx exhibited the polarization degree of ∼0.6% with a constant angle of 122﹩\mathop{.}\limits^{\unicode{x000b0}}﹩0  ±  8﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1 at the continuum component, without significant wavelength dependence. Panel (b) is the same as panel (a), but for the data taken on Day 52. The polarization values are binned with 40 pixels, corresponding to ∼53.6 Å. AT2023clx showed a wavelength-dependent polarization degree (0%–2%, increasing toward the blue) with a constant angle of 32﹩\mathop{.}\limits^{\unicode{x000b0}}﹩0  ±  5﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4. The polarization data presented in panels (a) and (b) have been corrected for the host dilution effects (see Appendix B). Panel (c) is the same as panel (a), but for the data taken on Day 121. The data are binned with 75 pixels, corresponding to ∼100.5 Å. The wavelength-averaged polarization degree and angle, as represented by the orange lines, showed a constant degree of ∼0.5% and a constant angle of 37﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7 ±  9﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1; this is interpreted to originate from the background component (i.e., the static host component).
Paper: Spectropolarimetry of a Nuclear Transient AT2023clx: Revealing the Geometrical Alignment between the Transient Outflow and the Nuclear Dusty Region
Authors: Kohki Uno, Keiichi Maeda, Takashi Nagao, Giorgos Leloudas, Panos Charalampopoulos, Seppo Mattila, Kentaro Aoki, Kenta Taguchi, Miho Kawabata, Javier Moldon, Miguel Pérez-Torres, Miika Pursiainen, Thomas Reynolds
Figure caption: Polarized fluxes of AT2023clx on Day 52. The polarized flux is calculated by Q[%] × , U[%] × , and P[%] ×  flux obtained on Day 52, where the flux is normalized by the mean flux over the spectral wavelengths. The underlying gray spectrum in each panel is the unbinned spectrum on Day 5. The polarized fluxes correlated with the spectrum on Day 5 demonstrate that the polarization on Day 52 originates from light echoes.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: Energy evolution of the primary fractions (top panels) and evolution of differential fluxes of individual primary species as functions of energy (middle panels) and rigidity (bottom panels) using QGSJET II-04 + ΔXmax (left panels) and SIBYLL 2.3d + ΔXmax (right panels). The primary fractions were obtained by fitting the Auger Xmax distributions (A. Aab et al. 2014a), while the total differential flux of cosmic rays was taken from A. Aab et al. (2020b). The two types of parameterized energy evolution of the primary fractions, see Section 3, are represented using dashed and solid lines in the panels.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: The relation between the interpreted moments of ﹩\mathrm{ln}A﹩ with (filled markers) and without (open markers) the application of ΔXmax to the model predictions using Auger DNN data (A. Abdul Halim et al. 2025a). The dashed and solid lines correspond to the systematic uncertainties. The range of possible combinations for p, He, N, and Fe nuclei is limited by the black lines forming the umbrella. The resulting value of ﹩{\sigma }^{2}(\mathrm{ln}A)﹩ inferred from the correlation coefficient rG between the ground signal and Xmax (A. Aab et al. 2016b) for 3–10 EeV is shown by the gray band, with the darker and narrower band indicating the respective energy range of the points for ΔXmax.
Paper: A Heavy-metal Scenario of Ultra-high-energy Cosmic Rays
Authors: Jakub Vícha, Alena Bakalová, Ana L. Müller, Olena Tkachenko, Maximilian K. Stadelmaier
Figure caption: Left panel: the energy evolution of the mean and standard deviation of Xmax for data (C. J. Todero Peixoto 2019; A. Yushkov 2019; A. Abdul Halim et al. 2025a) measured by the Pierre Auger Observatory (black), including the systematic uncertainty in the case of Auger DNN (brackets). The original model predictions for four primary species are depicted by thin lines and the adjusted predictions by thick lines. Right panel: the energy evolution of the two lowest moments of ﹩\mathrm{ln}A﹩, interpreted from the Auger DNN data shown in the left panel, using the adjusted (filled markers) and original (open markers) model predictions.
Paper: Thermonuclear Superburst of MAXI J1752−457 Observed with NinjaSat and MAXI
Authors: Amira Aoyama, Teruaki Enoto, Takuya Takahashi, Sota Watanabe, Tomoshi Takeda, Wataru Iwakiri, Kaede Yamasaki, Satoko Iwata, Naoyuki Ota, Arata Jujo, Toru Tamagawa, Tatehiro Mihara, Chin-Ping Hu, Akira Dohi, Nobuya Nishimura, Motoko Serino, Motoki Nakajima, Takao Kitaguchi, Yo Kato, Nobuyuki Kawai
Figure caption: (a) The 2–10 keV light curves of MAXI J1752−457 observed with NinjaSat/GMC (red circles), MAXI/GSC (black squares), and NuSTAR/XRT (blue diamonds; S. Pike et al. 2024) presented in the mCrab unit between MJD 60235 (November 11) and 60632 (November 18). NuSTAR fluxes were taken from S. Pike et al. (2024). The NinjaSat/GMC data are shown with the bin size of 1.5 hr on MJD 60624.6–60626.5, 3.0 hr on MJD 60626.5–60627.4, and 6.0 hr after MJD 60626.5. The X-ray intensities with MAXI and NinjaSat are converted to the Crab unit and then to the flux unit (see details in the main text). Each time span for spectral fittings is indicated in the upper part of the figure. (b) The ratio of data to the best-fit curve (Equation (2)) of panel (a) (see the main text). (c) The blackbody temperature. (d) The blackbody radius of the blackbody model at the assumed distance of 8 kpc (Table 1).
Paper: Thermonuclear Superburst of MAXI J1752−457 Observed with NinjaSat and MAXI
Authors: Amira Aoyama, Teruaki Enoto, Takuya Takahashi, Sota Watanabe, Tomoshi Takeda, Wataru Iwakiri, Kaede Yamasaki, Satoko Iwata, Naoyuki Ota, Arata Jujo, Toru Tamagawa, Tatehiro Mihara, Chin-Ping Hu, Akira Dohi, Nobuya Nishimura, Motoko Serino, Motoki Nakajima, Takao Kitaguchi, Yo Kato, Nobuyuki Kawai
Figure caption: (a) Evolution of the bolometric blackbody flux at the NS surface assuming the source distance of MAXI J1752−457 at 8 kpc in the log-log format. The blackbody parameters are obtained by the 2–10 keV fitting (Figure 3 and Table 1). The observed data are shown in red and black marks, corresponding to the assumptions of the burst onset time at Δt0 = 0.00 hr (i.e., the first MAXI scan of the detection) and Δt0 = 1.44 hr, respectively. The analytical models are overlaid at the best-fit parameters in Equation (3) of E17 = 2.0 and y12 = 2.8 for the Δt0 = 0.00 hr (red marks), whereas E17 = 5.1 and y12 = 1.8 for the Δt0 = 1.44 hr (black marks). Each reduced χ2 is 3.16 (d.o.f. = 6) and 3.50 (d.o.f. = 6), respectively. (b) Comparison of the observed burst energy E17 and column depth y12 of MAXI J1752−457 (red symbol) with previously reported long-duration bursts (black symbols) (M. Serino et al. 2016). In the same way as M. Serino et al. (2016), each data point of MAXI J1752−457 corresponds to the different assumptions of the burst onset at Δt0 = 0.00, 0.24, 0.48, 0.72, 0.96, 1.20, and 1.44 hr.
Paper: Thermonuclear Superburst of MAXI J1752−457 Observed with NinjaSat and MAXI
Authors: Amira Aoyama, Teruaki Enoto, Takuya Takahashi, Sota Watanabe, Tomoshi Takeda, Wataru Iwakiri, Kaede Yamasaki, Satoko Iwata, Naoyuki Ota, Arata Jujo, Toru Tamagawa, Tatehiro Mihara, Chin-Ping Hu, Akira Dohi, Nobuya Nishimura, Motoko Serino, Motoki Nakajima, Takao Kitaguchi, Yo Kato, Nobuyuki Kawai
Figure caption: The fitted X-ray spectra of MAXI/GSC and NinjaSat/GMC using the absorbed blackbody model. The time spans A, B, and C correspond to MAXI/GSC, with no markers. The time spans D, F, and H correspond to NinjaSat/GMC, represented by circular markers. The time spans are shown in Figure 2(a). The upper panel displays the unfolded spectrum, while the lower panel shows the ratio of the data to the best-fitting model (see Table 1).
Paper: 3D Simulations Demonstrate Propagating Thermohaline Convection for Polluted White Dwarfs
Authors: Imogen G. Cresswell, Adrian E. Fraser, Evan B. Bauer, Evan H. Anders, Benjamin P. Brown
Figure caption: Initial nondimensionalized (as described in the text) composition (black line) and temperature (red line) profiles (left) and 3D visualization of the initial composition field (right). The purple dashed line shows the initial location of the front at z = 100, above which the system is thermohaline-unstable.
Paper: 3D Simulations Demonstrate Propagating Thermohaline Convection for Polluted White Dwarfs
Authors: Imogen G. Cresswell, Adrian E. Fraser, Evan B. Bauer, Evan H. Anders, Benjamin P. Brown
Figure caption: Composition (left) and vertical velocity (right) are visualized for Pr = 0.05, τ = 0.05 at different times. The top right plot shows the depth of the front (the boundary between thermohaline-stable and -unstable regions) as a function of time, with this depth also indicated by the dashed line on the 3D renderings. The bottom right plot shows a 2D slice of the vertical velocity, zoomed in to the front location to highlight that dynamics extend past the front in an overshoot region.
Paper: The First Detection of Molecular Activity in the Largest Known Oort Cloud Comet: ALMA Imaging of C/2014 UN271 (Bernardinelli–Bernstein) at 16.6 au from the Sun
Authors: Nathan X. Roth, Stefanie N. Milam, Martin A. Cordiner, Dominique Bockelée-Morvan, Nicolas Biver, Michael S. P. Kelley, Anthony J. Remijan, Steven B. Charnley, Carrie E. Holt, Kiernan D. Foster, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tim Lister, Helen Usher
Figure caption: (A) Spectrally integrated flux map for CO on 2024 March 8. Contour intervals are in 1σ increments of the rms noise, with the lowest contour being 3σ. Sizes and orientations of the synthesized beam (Table B1) are indicated in the lower left corner. The comet’s illumination phase (ϕ ∼ 3°), as well as the direction of the Sun and dust trail, are indicated in the lower right. The black cross indicates the peak continuum position. σ gives the rms noise, and δcont gives the separation between the location of the peak continuum and peak gas emission. A spectral line profile taken at the continuum peak in a 10″ diameter aperture is shown. (B) Continuum flux map with contours for the spectrally integrated red and blue CO components overlaid separately. The extracted spectral line profile shows the integration region for the blue and red maps across the line. (C) Comparison of autocorrelation and interferometric CO spectra. (D) Continuum flux map in UN271. Contours are in 5σ increments of the rms noise, with the lowest contour being 5σ.