adsabs/AstroCLIMB huggingface dataset:
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: H2CO 30,3–20,2 channel map.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: CO 2–1 channel map.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: SO 65–54 channel map.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: SiO 5–4 channel map.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: 13CO 2–1 channel map.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: Integrated intensity maps of selected molecular transitions detected in SDC335. Red/blue contours: redshifted and blueshifted components, with velocity ranges labeled in each panel. Background: emission integrated over the systemic velocity gap between the blue- and redshifted ranges. Contours are drawn at 10 levels logarithmically spaced from 3σ to the map maximum. The typical 1σ rms in the integrated-intensity maps is 2.6 K km s−1 for the 3 mm data and 0.7 K km s−1 for the 1.3 mm data. Each panel lists the corresponding transition and upper energy level.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: (a) CO (2–1) RGB image constructed using the ACA+TM1+TM2 combined data. Blue- and redshifted components are integrated over velocities of −42 to −12 and +12 to +42 km s−1 relative to the systemic velocity, while the green channel traces emission within ±12 km s−1. The cyan line marks the jet axis. Hot cores C1–C3 and several emission knots are visible. (b) Zoom-in of the central region outlined in (a), with 3 mm continuum in colorscale and 1.3 mm contours highlighting compact sources. Continuum contours start at 21 mJy beam−1 and increase in steps of a factor of 1.618 (golden ratio). The beams of 3 mm (white) and 1.3 mm (gray) are shown in the lower-right corner.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: PVDs extracted along the jet axis of SDC335. The background color scale in each panel shows SiO emission, tracing the full spatial and velocity extent of the outflow. Overlaid contours correspond to representative transitions of other molecules, as labeled in each panel. Negative offsets indicate the southern (blueshifted) lobe, and positive offsets the northern (redshifted) lobe, with 0″ marking the C1.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: (a) PCA of molecular emission along the jet axis (data within ±2″ of C1 excluded). Molecules are separated into four quadrants reflecting dominant chemical–kinematic behavior: Quadrant I: COMs enhanced in shocked regions; Quadrant II: outflow tracers with low- and high-velocity components; Quadrant III: shock/high-velocity tracers; Quadrant IV: systemic-velocity or low S/N lines. (b) Schematic view of the physical and chemical structure of the bipolar outflow in SDC335. The main panel shows the spatial distribution of key molecular tracers associated with the hot core, warm envelope, and jet-driven outflows. The upper inset illustrates postshock low-velocity outflows heating the gas and sublimating molecules from icy mantles. The lower inset depicts strong shocks destroying dust grains, releasing ice-phase material, and driving Si atoms from grain cores into the gas phase to form SiO.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: Kendall rank correlation coefficients between integrated intensities of molecular lines, shown as a lower-triangular matrix to avoid duplication.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: (a) Identified molecular transitions in the 3 mm Band.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: Relative abundance proxies of selected molecules along the jet axis, computed as the ratio of their integrated intensities to that of 13CO at each position. Each line is normalized to its own maximum value across the spatial extent to emphasize the distribution pattern rather than the absolute abundance contrast. This highlights molecule-specific spatial differentiation along the outflow.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: Comparison between the rotational temperature (Trot) derived from H2CO and the spatial derivative of the SiO-to-13CO integrated intensity ratio along the outflow axis of SDC335. The horizontal axis represents the projected distance from the central hot core, while the two vertical axes show Trot (in K, left axis) and d(SiO/13CO)/dP, where P is position (right axis). The central light orange background indicates the extent of the hot core and its warm envelope, while the flanking light yellow regions mark areas in the outflow where some molecules do not show significant weakening relative to 13CO. Regions with elevated SiO 5–4 gradients coincide with local temperature peaks, indicating strong shock heating and enhanced molecular desorption.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: (a)–(d) Identified molecular transitions in the 1.3 mm Band. (e) The U line in Figures 4 and 5 here is marked as CH2NH﹩{}_{2}^{+* }﹩.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: Integrated intensities of selected molecular lines along the jet axis of SDC335, plotted as a function of projected distance from the central hot core (C1). All intensities are normalized to their values at +2″ to highlight relative enhancements or suppressions along the flow. Positive offsets correspond to the northern (redshifted) lobe, and negative offsets to the southern (blueshifted) lobe.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: An enlarged view of the weak-shock region (light yellow background) in Figure B2, showing that some transitions, such as H2CO 30,3–20,2 and SO 65–54, exhibit relatively little variation in intensity within this range, whereas other transitions show significant intensity changes.
Paper: Time-evolving Diagnostic of the Ionized Absorbers in NGC 4051. I. High-resolution Time-averaged Spectroscopy
Authors: Roberto Serafinelli, Fabrizio Nicastro, Alfredo Luminari, Yair Krongold, Francesco Camilloni, Elias Kammoun, Riccardo Middei, Enrico Piconcelli, Luigi Piro
Figure caption: The λ = 6–35 Å  RGS spectra analyzed in this paper. The gray spectrum is Epoch 1, while the light red spectrum is the one taken in Epoch 2. The black line is the best-fit model that includes all the absorbers detected in this paper. We also include the model without the absorbers, in blue, that also includes Gaussian emission lines, showing that there are significant residuals that strongly point to the presence of several ionized absorbers. The sharp vertical dips are instrumental gaps. For visual purposes only, the spectral data points have been rebinned at a minimum of 5 counts per wavelength bin.
Paper: Time-evolving Diagnostic of the Ionized Absorbers in NGC 4051. I. High-resolution Time-averaged Spectroscopy
Authors: Roberto Serafinelli, Fabrizio Nicastro, Alfredo Luminari, Yair Krongold, Francesco Camilloni, Elias Kammoun, Riccardo Middei, Enrico Piconcelli, Luigi Piro
Figure caption: Data-to-model ratios that highlight the contributions to the fit from the three ionized absorbers. The horizontal line in red represents the best-fit model described in Table 3. We removed one absorber at a time to highlight the difference between the best-fit model and the model that does not include the absorber. The green shaded area represents residuals obtained by removing the LIP, and the lavender area is obtained when we remove the HIP, while the brown area is obtained by removing the HVIP. The upper panel represents Epoch 1, and the lower panel represents Epoch 2. We stress that the data are not refit after removing each absorber and are just plotted for illustrative purposes. The data are also visually binned at a minimum of 20 counts per wavelength bin.
Paper: Time-evolving Diagnostic of the Ionized Absorbers in NGC 4051. I. High-resolution Time-averaged Spectroscopy
Authors: Roberto Serafinelli, Fabrizio Nicastro, Alfredo Luminari, Yair Krongold, Francesco Camilloni, Elias Kammoun, Riccardo Middei, Enrico Piconcelli, Luigi Piro
Figure caption: Upper panel: NuSTAR combined FPMA+B background-subtracted light curve in the 3–79 keV energy band. Lower panel: EPIC-pn light curves of both observations in the 2–10 keV energy band. All light curves are binned at 1 ks per time bin.
Paper: Time-evolving Diagnostic of the Ionized Absorbers in NGC 4051. I. High-resolution Time-averaged Spectroscopy
Authors: Roberto Serafinelli, Fabrizio Nicastro, Alfredo Luminari, Yair Krongold, Francesco Camilloni, Elias Kammoun, Riccardo Middei, Enrico Piconcelli, Luigi Piro
Figure caption: Examples of absorption lines for the contribution of the three absorbers. The gray points are the Epoch 1 observation, while the light red points are the Epoch 2 one. The black line represents the best-fit model listed in Table 3, while the blue one represents the model without one of the three absorbers, without refitting the model. Left panel: spectral region in λ = 21–23 Å. The blue line was drawn by removing the LIP to highlight some of its contribution, namely O IV Kα at λ = 22.76 Å and O VI Kα at λ = 22.03 Å. Middle panel: spectral region in λ = 15.3–16.8 Å. The blue line is obtained by removing the HIP, highlighting the strong contribution for O VIII Lyβ at λ = 16.01 Å. Right panel: spectral region in λ = 10–12.5 Å. The blue line is obtained by subtracting the HVIP component, contributing to the Ne X Lyα at λ = 12.14 Å and to the Fe XXII L-transition at λ = 11.57 Å.
Paper: Time-evolving Diagnostic of the Ionized Absorbers in NGC 4051. I. High-resolution Time-averaged Spectroscopy
Authors: Roberto Serafinelli, Fabrizio Nicastro, Alfredo Luminari, Yair Krongold, Francesco Camilloni, Elias Kammoun, Riccardo Middei, Enrico Piconcelli, Luigi Piro
Figure caption: Ionization versus power-law normalization of the three absorbers identified in this paper; each data point represents one epoch. The red line is obtained assuming that the lowest flux state is in equilibrium.
Paper: Time-evolving Diagnostic of the Ionized Absorbers in NGC 4051. I. High-resolution Time-averaged Spectroscopy
Authors: Roberto Serafinelli, Fabrizio Nicastro, Alfredo Luminari, Yair Krongold, Francesco Camilloni, Elias Kammoun, Riccardo Middei, Enrico Piconcelli, Luigi Piro
Figure caption: Two-dimensional confidence contours for the hydrogen number density ﹩{\mathrm{log}}({n}_{{\rm{H}}}/{{\rm{cm}}}^{-3})﹩ versus the ionization parameter ﹩{\mathrm{log}}U﹩ for the HIP absorber, obtained from the TEPID fit. Contours correspond to the 68% (1σ), 95.5% (2σ), and 99.7% (3σ) confidence levels for two parameters of interest. The black X marks the best-fit value.
Paper: On the Gravitational Collapse of Small Dust Grains in Self-gravitating Disk Structures
Authors: Hans Baehr, Ken Rice, Chao-Chin Yang, 朝欽 楊, Cassandra Hall
Figure caption: A sketch of what dust sizes might be expected to gravitationally collapse for differing levels of diffusivity and with different assumptions of the disk metallicity. The limitation at the higher dust sizes is the regime where coupling is weak and gravitational interactions between dust and the spiral arms are more consequential than drift toward the pressure maximum. Using Equation (5) and assuming ε = 100, we create diagonal dashed lines, which, for three different metallicities, limit collapse to the region below each curve. We finally separate into two regimes, depending on whether or not they can collapse around the maximum diffusivity (dotted line), set by the gas turbulent α (see Equation (22)). We indicate dust sizes where collapse is possible regardless of diffusivity with the shaded regions. The area to the left of each shaded region but still below the diagonal curves indicates particle sizes where collapse remains possible but only if the diffusivity is low enough.
Paper: On the Gravitational Collapse of Small Dust Grains in Self-gravitating Disk Structures
Authors: Hans Baehr, Ken Rice, Chao-Chin Yang, 朝欽 楊, Cassandra Hall
Figure caption: Left: the time evolution of the maximum dust surface density Σd relative to the spatial average 〈Σd〉. The approximate threshold separating the surface densities that result in dense clouds is marked with a horizontal dashed line at Σd = 100. Right: the time evolution of the maximum dust density ρd relative to the initial density maximum ρd,0. The Hill density is indicated by the horizontal dashed line.
Paper: On the Gravitational Collapse of Small Dust Grains in Self-gravitating Disk Structures
Authors: Hans Baehr, Ken Rice, Chao-Chin Yang, 朝欽 楊, Cassandra Hall
Figure caption: Snapshots of the dust surface density enhancement in three simulations with different total metallicities, at two different times: t = 65 Ω−1 (left column) and t = 90 Ω−1 (right column). The simulation shown in the top row is the case where Z = 0.01 and the dust does not gravitationally collapse within the simulation run time. The simulation shown in the middle row uses dust with metallicity Z = 0.02, while the bottom row has Z = 0.04. Dense clouds of dust above Roche surface density (Equation (21)) are indicated with red circles.
Paper: On the Gravitational Collapse of Small Dust Grains in Self-gravitating Disk Structures
Authors: Hans Baehr, Ken Rice, Chao-Chin Yang, 朝欽 楊, Cassandra Hall
Figure caption: The cumulative distribution of bound dust clumps formed in the simulations at t = 90 Ω−1. The flat part of the distributions on the left-hand side of the plot indicates that there are no clumps forming below this mass. Compared to the simulations with larger dust sizes in which clumps can form below ﹩\hat{M}﹩ (thinner, paler lines; e.g., H. Baehr et al. 2022), smaller grains require stronger local dust concentrations to overcome the dust diffusion.
Paper: On the Gravitational Collapse of Small Dust Grains in Self-gravitating Disk Structures
Authors: Hans Baehr, Ken Rice, Chao-Chin Yang, 朝欽 楊, Cassandra Hall
Figure caption: The value of Qd based on measured values of δ and ϵ for various particle sizes. The values for St ≥ 0.1 come from H. Baehr et al. (2022), and those for St = 0.01 and St = 0.001 are newly measured in this work. Increasing the metallicity for St = 0.01 leads to values of Qd, consistent with the gravitational collapse observed. In the case of St = 0.001, the value of Qd is in the range of stability, even though the dust does gravitationally collapse.
Paper: On the Gravitational Collapse of Small Dust Grains in Self-gravitating Disk Structures
Authors: Hans Baehr, Ken Rice, Chao-Chin Yang, 朝欽 楊, Cassandra Hall
Figure caption: Left: volume-averaged and midplane gas rms velocities in two simulations with different grid resolutions. The solid line shows the simulations with the nominal resolution 20/H, while the dashed line shows the same for an identical simulation with 10/H. Thinner and lighter lines show the rms velocity of the midplane layer only. Right: same as left panel but for dust rms velocities.
Paper: On the Gravitational Collapse of Small Dust Grains in Self-gravitating Disk Structures
Authors: Hans Baehr, Ken Rice, Chao-Chin Yang, 朝欽 楊, Cassandra Hall
Figure caption: Same as Figure 1, but for the simulation with St = 0.001 and Z = 0.04.
Paper: Continued Radio Observations of the Persistent Radio Source Associated with FRB 20190520B Provide Insights into Its Origin
Authors: Arvind Balasubramanian, Mohit Bhardwaj, Shriharsh P. Tendulkar
Figure caption: Spectrum of the PRS of FRB 20190520B showing the joint spectrotemporal fit using Equation (3). The color of the dashed lines represents the different epochs. The shaded blue region shows the uGMRT upper limits that suggest a break in the spectrum at frequencies <1 GHz.
Paper: Continued Radio Observations of the Persistent Radio Source Associated with FRB 20190520B Provide Insights into Its Origin
Authors: Arvind Balasubramanian, Mohit Bhardwaj, Shriharsh P. Tendulkar
Figure caption: Light curve with all the flux density measurements from Table 1 scaled to 1.5 GHz assuming a spectral index of −0.4. The fit is a linear regression showing a decreasing trend in the overall flux density over time.
Paper: Continued Radio Observations of the Persistent Radio Source Associated with FRB 20190520B Provide Insights into Its Origin
Authors: Arvind Balasubramanian, Mohit Bhardwaj, Shriharsh P. Tendulkar
Figure caption: Comparison of the image of the target PRS (top row) and the calibrator 3C286 (bottom row) on 2022 November 11 (left column) and 2022 November 29 (right column). This shows the calibration errors in the 2022 November 11 data.
Paper: Continued Radio Observations of the Persistent Radio Source Associated with FRB 20190520B Provide Insights into Its Origin
Authors: Arvind Balasubramanian, Mohit Bhardwaj, Shriharsh P. Tendulkar
Figure caption: Light curve of the FRB 20190520B PRS, showing the joint spectrotemporal fit using Equation (3). This fit gives an estimate of the age of the persistent source to be tage = 52 yr.
Paper: Ionization Rate of Interstellar Neutral Helium from New Horizons/SWAP Observations
Authors: Małgorzata Antonik, Paweł Swaczyna, David J. McComas, Heather A. Elliott, Maciej Bzowski
Figure caption: Estimated ISN helium density from SWAP (orange dots) and IBEX-Lo (blue dots) data with uncertainties. The values from IBEX-Lo are calculated by normalizing linear coefficients from Figure 1 in P. Swaczyna et al. (2022) and multiplying them by the ISN helium density of 0.015 cm−3. The ISN helium densities inferred from SWAP and IBEX-Lo observations show opposite trends over the overlapping periods.
Paper: Continued Radio Observations of the Persistent Radio Source Associated with FRB 20190520B Provide Insights into Its Origin
Authors: Arvind Balasubramanian, Mohit Bhardwaj, Shriharsh P. Tendulkar
Figure caption: Constraint on the radius of the PRS source using the projected size of the screen Rr. The figure is adapted from S. Bhandari et al. (2023), after correcting for the radius by dividing all limits by 2.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: H-R diagram for the observational data, shown as (g − i)0—log g and (GBP-GRP)0—MG, color coded by [Fe/H] shown in the color bar on the right. The BHB stars selected from the right panel are assigned a log g value of 2.5.