adsabs/AstroCLIMB huggingface dataset:
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Zoom-ins of the eastern (left) and western (right) NAT sources on the adaptively smoothed X-ray image. Overlaid are the 1.4 GHz VLA FIRST (green) and 150 MHz TGSS (cyan) radio contours.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Excess emission in the 0.7–7 keV energy range after the subtraction of a 2D beta-model. The residual image was smoothed using a σ = 15″ Gaussian.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Gaussian-smoothed (top left; see the left panel of Figure 1) and adaptively smoothed (top right; see the right panel of Figure 1) X-ray images and projected temperature map (bottom left) showing the regions defined for extracting the radial profiles (labeled CF1, CF2, and SF1; see Section 5). The solid blue (cold fronts) and red (shock) lines mark the locations of the brightness edges identified from the fits to the radial profiles. In order to aid visualization, included is a cartoon schematic (bottom right) showing the merger shock and a possible scenario of the CF regions connecting to form a sloshing spiral structure. Overlaid on all panels are the 1.4 GHz (green) and 150 MHz (blue) radio contours of the two NAT sources.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Radial profiles of X-ray surface brightness, projected temperature, deprojected density, and pressure for the regions discussed in Section 5 and shown in Figure 9. The surface brightness profiles include the best-fit model (red line) and the 3D density profile (inset) obtained from the fit. The dashed lines in all panels denote the best-fit edge radius and the shaded regions are the 1σ errors on the fitted radius.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: GGM-filtered (0.7–7 keV) image with σ = 40 pixels (1 pixel = 0.″492). The brightest regions correspond to the steepest changes in X-ray surface brightness. Overlaid are the 1.4 GHz (green) and 150 MHz (cyan) radio contours. Some notable features are highlighted.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Radial profiles of (a) surface brightness, (b) deprojected density, (c) deprojected pressure, (d) projected temperature, and (e) projected abundance for the global cluster emission.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Radial profile across the eastern NAT source used to calculate the velocities in Section 6.2. The dashed lines denote the radial extent of the bins, containing the NAT host galaxy, from which the pressure and density are estimated.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: A cluster merger simulation that qualitatively matches our preferred scenario for A119. Left: gradient-filtered X-ray surface brightness (0.5–7.0 keV band). Right: projected spectroscopic-like (Mazzotta et al. 2004) gas temperature. We include an inset of the cartoon schematic from Figure 9 to aid in comparison of the features observed in A119 with the simulation results.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Radial profile across the western NAT source used to calculate the velocities in Section 6.2. The dashed lines denote the radial extent of the bins, containing the NAT host galaxy, from which the pressure and density are estimated.
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Adaptively smoothed X-ray image showing locations of three optical subclusters reported in previous studies (Fabricant et al. 1993; Kriessler & Beers 1997; Ramella et al. 2007; Lee et al. 2016).
Paper: CHANDRA X-Ray Observations of A119: Cold Fronts and a Shock in an Evolved Off-axis Merger
Authors: Courtney B. Watson, Elizabeth L. Blanton, Scott W. Randall, Craig L. Sarazin, Arnab Sarkar, John A. ZuHone, E. M. Douglass
Figure caption: Temperature map of A119, overlaid with 1.4 GHz (green) and 150 MHz (blue) radio contours. The white contours are from the smoothed X-ray image (see Figure 1).
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Example of calculating the maxima and minima of NSHs and an example of slope and amplitude variations. Top panel: Example of slope variation from the magenta rectangular box in Figure 2(g). Middle panel: The red and blue circles represent the maxima and minima, respectively, and the solid magenta line is a linear superposition Gaussian fit with a fitted width of 0.5 NSHs phase; the light curve corresponds to the magenta rectangular in box in Figure 2(b). Bottom panel: Partial amplitude variation and sine fit from the magenta rectangular box in Figure 6.
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Results of the analysis of the s52 light curve. The interpretation of each plate is consistent with Figure 2, except that the light curve is replaced with s52.
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Frequency–amplitude plots of the NSH amplitude, maxima O − C, and slope variation. The four plots on the left are from the analysis of the TESS s25 data, and the right is from s52. From top to bottom, NSHs amplitude, rising slope, declining slope, and O − C period analysis are shown.
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Frequency–amplitude spectrum of the s25 light curve at different stages. The meanings of the different curves are shown in the legend, and the letters correspond to the individual stages in Figure 2(a).
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Validation plot of the amplitude periodic variation in NSHs. The top panel is consistent with Figure 2(d), and the solid green line is the LOESS fit; the bottom panel shows the residuals of the LOESS fit, and the solid red line is the sine fit.
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Frequency–amplitude spectrum of AH Her. The black and red solid lines correspond to the analysis results of s25 and s52, and the blue and magenta dashed vertical lines correspond to 0.24497(1) days and 0.25824(3)/2 days, respectively.
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Analysis of QPOs at the top of long outbursts in TESS s25. The solid blue line in the top panel is the LOESS fit; the bottom panel is the residuals of the LOESS fit, and the solid red line is the sine fit.
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Frequency–amplitude plots for the analysis of QPOs. The top and bottom panels analyze the top detrended light curves for c25 and c52 long outbursts, respectively.
Paper: Evolution of Negative Superhumps, Quasiperiodic Oscillations, and Outbursts in the Z Cam-type Dwarf Nova AH Her
Authors: Qi-Bin Sun, Sheng-Bang Qian, Min-Yu Li
Figure caption: Analysis of QPOs at the top of outbursts in TESS s52.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Left: Column densities summed over 0.6 pc for the Rot-M1.5-B10P model at 0.3 Myr (top) and Col-M1.5-B10P model at 0.2 Myr (bottom) with the same realization of the input turbulence. The black lines show the average velocity field projected onto the plane. The position of the most massive dense core is indicated with a black circle. Right: Momentum structure around the most massive dense core corresponding to the left panel. Purple lines show the average momentum around the x-axis: ﹩{\int }_{S}\rho ({v}_{x}-{v}_{x,\mathrm{core}}){dydz}/{\int }_{S}{dydz}﹩, where ﹩{v}_{x,\mathrm{core}}﹩ is the x-component of the center of mass velocity of the core, and ﹩S=\{(y,z)| {\left[{\left(y-{y}_{\mathrm{core}\ }\right)}^{2}+{\left(z-{z}_{\mathrm{core}\ }\right)}^{2}\right]}^{1/2}\leqslant 0.05\mathrm{pc}\}﹩. The horizontal axis corresponds to ﹩x-{x}_{\mathrm{core}\ }﹩. Similarly, the green and blue lines represent the average momentum around the y-axis and z-axis, respectively. Momentum around the core is isotropic in the Col-M1.5-B10P model, while the y-component is dominant in the Rot-M1.5-B10P model.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Histograms of the cosine of the relative angle between ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩ and Ω col for fast collision models with θ 0 = 45°. The black line shows the expected distribution for an isotropic orientation of ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩. In the legends, the orientation parameter ﹩{S}_{B,{\rm{\Omega }}}=(3\langle {\cos }^{2}\measuredangle [{{\boldsymbol{B}}}_{\mathrm{core}},{{\boldsymbol{\Omega }}}_{\mathrm{col}}]\rangle -1)/2﹩ for each model is shown, and values with ﹩{S}_{L,{B}_{0}}\gt 0.25﹩ are indicated in bold. In models with weak magnetic fields (indicated by solid lines), the strong alignment of ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩ with Ω col is observed. Furthermore, in the weak magnetic field model, S  B,Ω is higher than ﹩{S}_{B,{B}_{0}}﹩, indicating that the direction of ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩ is determined not by the direction of the initial magnetic field, but rather by the direction of the collision axis.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Total angular momentum of clump gas in the z-direction, L z, as a function of time. The top and middle panels display the time evolution of gas above density 104 and 105 cm−3, respectively. The bottom panel illustrates the time evolution of the total gas mass above density 105 cm−3 for comparison. We are comparing models with the same realization of the input turbulence for weak turbulence ﹩{ \mathcal M }=1.5﹩ and θ 0 = ﹩{0}^{\circ }﹩, where Ω 0 (Ω col) is parallel to the z-axis. As the angular momentum of the clump is approximately conserved, L z with n > 104 cm−3 is nearly constant. On the other hand, L z with n > 105 cm−3(> n clump = 1.2 × 104 cm−3) increases as dense regions form.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Slice plots of the gas density in a plane through the center of the simulation box at t = 0.2 Myr in Col-M1.5-B10P and Col-M1.5-B10D models. Black lines show the magnetic field direction ( B  0 is parallel to the z-axis). The length of lines corresponds to the magnetic field strength. White arrows indicate the collision axis. The magnetic field is amplified and aligned along the shocked layer.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Same as Figure 4 except for Collision Setup models. Fast collision velocity cases with θ 0 = 0° are shown in the top panel and those of θ 0 = 45° are shown in the middle panel. Slow collision velocity cases are shown in the bottom panel.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Same as Figure 5 except for Collision Setup models. Fast collision velocity cases are shown in the top panel, and slow collision velocity cases are shown in the bottom panel. The Collision Setup model has a higher degree of alignment for ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩ compared to Rotation Setup and w/o Setup models. Especially when B 0 is weak, the field aligns along the shocked layer, resulting in a significantly higher degree of alignment for ﹩{{\boldsymbol{B}}}_{\mathrm{core}}﹩.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Velocity dispersion in z-direction, σ z, as a function of time. The top and bottom panels display the time evolution of gas above density 104 and 105 cm−3, respectively. We are comparing models with the same realization of the input turbulence for weak turbulence ﹩{ \mathcal M }=1.5﹩and θ 0 = ﹩{0}^{\circ }﹩. Increasing the initial collision velocity leads to a higher increase in σ z.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Same as Figure 6 except for Collision Setup models. Fast collision velocity cases with θ 0 = 0° are shown in the top panel and those of θ 0 = 45° are shown in the middle panel. Slow collision velocity cases are shown in the bottom panel. In most models, they suggest random distributions of ﹩\measuredangle [{{\boldsymbol{L}}}_{\mathrm{core}},{{\boldsymbol{B}}}_{\mathrm{core}}]﹩.
Paper: Unveiling the Dynamics of Dense Cores in Cluster-forming Clumps: A 3D Magnetohydrodynamics Simulation Study of Angular Momentum and Magnetic Field Properties
Authors: Shinichi. W. Kinoshita, Fumitaka Nakamura
Figure caption: Same as Figure 3 except for Collision Setup models. Fast collision velocity cases are shown in the top panel, and slow collision velocity cases are shown in the bottom panel. Regardless of the models, ﹩\cos ,{\theta }_{L,L}﹩ is close to 0.5 for most separation ranges, which suggests that the direction of ﹩{{\boldsymbol{L}}}_{\mathrm{core}}﹩ is randomly distributed.
Paper: Entrapment of Hypervolatiles in Interstellar and Cometary H2O and CO2 Ice Analogs
Authors: Alexia Simon, Mahesh Rajappan, Karin I. Öberg
Figure caption: (a) 3D sketch of the complete setup used in this study except for the pump stations and frame. (b) Zoom-in sketch of the sample substrate holder present at the center of the chamber. (c) Photograph of the experimental setup. (d) 3D sketch of the gas mixing line connected to the chamber.
Paper: Entrapment of Hypervolatiles in Interstellar and Cometary H2O and CO2 Ice Analogs
Authors: Alexia Simon, Mahesh Rajappan, Karin I. Öberg
Figure caption: Histograms showing the percentage of entrapment in CO2 and H2O ice matrices for the experiments listed in Table 3. The bars are color-coded by hypervolatile, while a solid bar indicates a CO2 matrix and a patterned bar an H2O matrix. Top panels: comparison of entrapment efficiencies between different experimental conditions for each hypervolatile. Bottom panels: comparison of entrapment efficiencies between the four hypervolatiles for each experimental condition.
Paper: Entrapment of Hypervolatiles in Interstellar and Cometary H2O and CO2 Ice Analogs
Authors: Alexia Simon, Mahesh Rajappan, Karin I. Öberg
Figure caption: TPD curves of H2O:13CO (upper panel) and CO2:13CO (lower panel) ice mixtures. In both panels the orange solid or dashed curve traces m/z = 29, i.e., 13CO. In the upper panel the solid purple curve is m/z = 18, i.e., H2O, and in the lower panel the dashed purple line traces m/z = 44, i.e., CO2. The 13CO peak in the rectangular boxes is the quantity considered as trapped.
Paper: Entrapment of Hypervolatiles in Interstellar and Cometary H2O and CO2 Ice Analogs
Authors: Alexia Simon, Mahesh Rajappan, Karin I. Öberg
Figure caption: TPD data for the experiments listed in Table 3 organized by ice matrix (H2O top and CO2O bottom panels), and ice thickness and ice mixing ratio (left to right). Within each panel, orange is for 13CO, crimson for 12CH4, purple for 15N2, and black for Ar.
Paper: Entrapment of Hypervolatiles in Interstellar and Cometary H2O and CO2 Ice Analogs
Authors: Alexia Simon, Mahesh Rajappan, Karin I. Öberg
Figure caption: Comparison of CO2 and H2O ice matrices for each experiment. Each panel shows the comparisons of one compound at the different combination of parameters.
Paper: Entrapment of Hypervolatiles in Interstellar and Cometary H2O and CO2 Ice Analogs
Authors: Alexia Simon, Mahesh Rajappan, Karin I. Öberg
Figure caption: TPD profiles of 50 ML CO2:13CO and H2O:13CO mixtures in ratios of 3:1 and 10:1 used to determine of entrapment uncertainties.
Paper: Entrapment of Hypervolatiles in Interstellar and Cometary H2O and CO2 Ice Analogs
Authors: Alexia Simon, Mahesh Rajappan, Karin I. Öberg
Figure caption: Infrared spectra of H2O:13CO (upper panel) and CO2:13CO (lower panel) ice mixtures at ∼50 ML at 3:1 ratio. The 13CO peak is zoomed-in in the rectangular boxes to show its structure.
Paper: Entrapment of Hypervolatiles in Interstellar and Cometary H2O and CO2 Ice Analogs
Authors: Alexia Simon, Mahesh Rajappan, Karin I. Öberg
Figure caption: Comparison of entrapment in CO2 and H2O ice matrices for each hypervolatile, ice thickness, and mixing ratio.
Paper: A Light Redback Companion of PSR J1622–0315 and Irradiation Power in Spider Systems
Authors: Y. X. Jane Yap, Albert K. H. Kong, Kwan-Lok Li
Figure caption: The folded light curve of PSR J1622–0315 companion in ﹩r^{\prime} ﹩(top) and ﹩g^{\prime} ﹩(bottom) band. Phase 0 corresponds to the inferior conjunction of the companion. The black solid line is the best-fit model from PHOEBE. The most recent data set (2021 July 4) is not included in the fit. The gray solid line demonstrates the effect of irradiation on the companion star surface due to heating from the pulsar; the effect is most obvious at the companion superior conjunction where most of the extra irradiation is seen.
Paper: A Light Redback Companion of PSR J1622–0315 and Irradiation Power in Spider Systems
Authors: Y. X. Jane Yap, Albert K. H. Kong, Kwan-Lok Li
Figure caption: Corner plot of the posterior distributions for the fitted parameters. The median values are displayed with the respective 1σ uncertainties, indicated by dotted lines. Degeneracy is observed in the following parameters: (i) q binary and i binary, (ii) T eff,secondary and A V, and (iii) R secondary and d. Given the data quality, we were unable to constrain the extinction parameter, A V.
Paper: A Light Redback Companion of PSR J1622–0315 and Irradiation Power in Spider Systems
Authors: Y. X. Jane Yap, Albert K. H. Kong, Kwan-Lok Li
Figure caption: Propagated distribution of parameters M primary (NS) and M secondary (companion). The median values are displayed with the respective 1σ uncertainties.
Paper: A Light Redback Companion of PSR J1622–0315 and Irradiation Power in Spider Systems
Authors: Y. X. Jane Yap, Albert K. H. Kong, Kwan-Lok Li
Figure caption: Projected view of the companion star across different orbital phases, including its effective temperature distribution. This model corresponds to the parameter values reported in Table 3.
Paper: A Light Redback Companion of PSR J1622–0315 and Irradiation Power in Spider Systems
Authors: Y. X. Jane Yap, Albert K. H. Kong, Kwan-Lok Li
Figure caption: Lomb–Scargle periodogram of the combined light curves taken in 2019 for PSR J1622–0315. The peak with the strongest amplitude is located at a frequency that corresponds to a period of 0.162(2) days, indicating the orbital period of the system. Our result is consistent with the previously reported orbital period obtained using radio timing, which is indicated by a dotted line.
Paper: Excitation and Ionization Properties of Star-forming Galaxies at z = 2.0–9.3 with JWST/NIRSpec
Authors: Ryan L. Sanders, Alice E. Shapley, Michael W. Topping, Naveen A. Reddy, Gabriel B. Brammer
Figure caption: SFR vs. M * for samples at z = 2.0–6.5. Filled circles with error bars display SFR(Hα), while hollow squares present SFR(SED). In each panel, the dashed line displays the star-forming main sequence from the parameterization of Speagle et al. (2014), calculated at the median redshift of the galaxies in each bin. The gray two-dimensional histogram displays the distribution of z ∼ 0 star-forming galaxies from SDSS, for which the orange line shows the median trend.
Paper: Excitation and Ionization Properties of Star-forming Galaxies at z = 2.0–9.3 with JWST/NIRSpec
Authors: Ryan L. Sanders, Alice E. Shapley, Michael W. Topping, Naveen A. Reddy, Gabriel B. Brammer
Figure caption: Composite spectra of samples in each redshift interval, constructed as described in Section 2.6. Each spectrum has been normalized to the measured Hβ intensity and offset vertically for display purposes. The inset panel zooms in on the weak red rest-optical lines for the z < 6.5 composites on the same scale, vertically offset for clarity. The measured line ratios and uncertainties are reported in Table 1.
Paper: Effects of Barnett Magnetic Dipole–Dipole Interaction on Grain Growth and Destruction
Authors: Thiem Hoang, Bao Truong
Figure caption: The enhancement of collision rate by Barnett dipole–dipole interaction with respect to the envelope radius, assuming the radiation field and gas properties of O-rich AGB stars (i.e., IK Tau, see Tram et al. 2020). Under intense stellar radiation, the collision rate of SPM grains with a high level of iron inclusions could be significantly increased with ﹩{({b}_{\max }/a)}^{2}\gt 100﹩. The collision rate decreases with increasing gas and dust temperature toward the central star. For comparison, rotational disruption by RAT-D is also shown for two values of tensile strength.