adsabs/AstroCLIMB huggingface dataset:
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: Left panel: simulated spectra from CHIANTI corresponding to the Be-med filter of XRT using photospheric abundances. Right panel: simulated spectra from CHIANTI corresponding to the Be-med filter of XRT using coronal abundances.
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: Evolution of the loop structures observed in the 171 Å channel of SDO/AIA.
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: The temperature response ratio for two filters of XRT (Be-med/Be-thin) with respect to the temperatures. The black line shows the ratios for photospheric abundance and the red line corresponds to coronal abundances.
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: Evolution of the loop structures observed in the 131 Å channel of SDO/AIA.
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: Full-disk DEM for 3 minute averaged data from 14:14 UT to 14:17 UT during the flare peak time.
Paper: What Is the Nature of the HESS J1731-347 Compact Object?
Authors: Violetta Sagun, Edoardo Giangrandi, Tim Dietrich, Oleksii Ivanytskyi, Rodrigo Negreiros, Constança Providência
Figure caption: Mass–radius relations obtained within the scenarios of purely hadronic NS with soft (blue solid curve) and stiff (green solid curve) EOSs, strange QS (orange solid curve), and HS (purple solid curve), while the scenario of purely hadronic NS admixed with DM is represented by dashed–dotted curves. The corresponding EOSs are mentioned in the legend. Light blue and yellow bands represent 1σ constraints on the mass of PSR J0348+0432 (Antoniadis et al. 2013) and PSR J1810+1744 (Romani et al. 2021). Orange and light blue contours show the NICER measurement of PSR J0030+0451 (Miller et al. 2019; Riley et al. 2019), while pink and brown contours depict the PSR J0740+6620 measurement (Miller et al. 2021; Riley et al. 2021). LIGO-Virgo observations of GW170817 (Abbott et al. 2018) and GW190425 (Abbott et al. 2020) binary NS mergers are shown in royal blue and green. The 1σ and 2σ contours of HESS J1731-347 (Doroshenko et al. 2022) are plotted in dark and light red. The shaded region is forbidden by the rotation of the fastest spinning pulsar PSR J1748-2446ad (Hessels et al. 2006).
Paper: What Is the Nature of the HESS J1731-347 Compact Object?
Authors: Violetta Sagun, Edoardo Giangrandi, Tim Dietrich, Oleksii Ivanytskyi, Rodrigo Negreiros, Constança Providência
Figure caption: Cooling curves for NSs (left panel) and HSs (right panel) of ﹩{0.77}_{-0.17}^{+0.20}\,{M}_{\odot }﹩ for unpaired and paired matter. ﹩{T}_{S}^{\infty }﹩ represents the surface temperature at infinity. Left panel: the red bands correspond to the unpaired NS matter, while paired n and p in the 1 S 0 channel and n in the 3 P 2 channel are shown in green. The color bands represent the mass measurement in the 1σ CI, whereas the thick and thin lines define the stars of 0.97 M ⊙ and 0.6 M ⊙, respectively. Right panel: the thermal evolution of HSs with unpaired and paired quark matter are depicted by the magenta and orange bands. The solid and dashed curves correspond to the light-elements and heavy-elements envelopes, respectively. The data for Cas A (number 0) and the rest of the points are taken from Wijngaarden et al. (2019) and Beznogov & Yakovlev (2015), respectively. An updated surface temperature for HESS J1731-347 is taken from Doroshenko et al. (2022), while its age is considered from Beznogov & Yakovlev (2015) (see details in Appendix A).
Paper: ALMA Observations of Supernova Remnant N49 in the Large Magellanic Cloud. II. Non-LTE Analysis of Shock-heated Molecular Clouds
Authors: H. Sano, Y. Yamane, J. Th. van Loon, K. Furuya, Y. Fukui, R. Z. E. Alsaberi, A. Bamba, R. Enokiya, M. D. Filipović, R. Indebetouw, T. Inoue, A. Kawamura, M. Lakićević, C. J. Law, N. Mizuno, T. Murase, T. Onishi, S. Park, P. P. Plucinsky, J. Rho, A. M. S. Richards, G. Rowell, M. Sasaki, J. Seok, P. Sharda, L. Staveley-Smith, H. Suzuki, T. Temim, K. Tokuda, K. Tsuge, K. Tachihara
Figure caption: Peak intensity maps of (a) 12CO(J = 1–0), (b) 12CO(J = 2–1), (c) 13CO(J = 2–1), and (d) 12CO(J = 3–2). (e) Intensity ratio map of 12CO(J = 2–1)/12CO(J = 1–0) (hereafter R 2−1/1−0). The velocity range of CO is from 285.5 to 287.8 km s−1. Superposed contours represent Chandra X-ray intensity in the energy band of 0.5–7.0 keV. The lowest contour level and the contour intervals are 5 × 10−7 and 3 × 10−6 photons pixel−1 s−1, respectively. The regions enclosed by dashed lines indicate the observed areas using ALMA. The CO peaks K, L, N, O–R, and T defined by Paper I are also indicated in (c). When we take the intensity ratio of R 2−1/1−0, the 12CO(J = 2–1) data were smoothed with a two-dimensional Gaussian kernel to match the effective beam size of the 12CO(J = 1–0) data. The gray shaded area in (e) represents the 12CO(J = 1–0) and/or 12CO(J = 2–1) data showing significance lower than ∼10σ.
Paper: ALMA Observations of Supernova Remnant N49 in the Large Magellanic Cloud. II. Non-LTE Analysis of Shock-heated Molecular Clouds
Authors: H. Sano, Y. Yamane, J. Th. van Loon, K. Furuya, Y. Fukui, R. Z. E. Alsaberi, A. Bamba, R. Enokiya, M. D. Filipović, R. Indebetouw, T. Inoue, A. Kawamura, M. Lakićević, C. J. Law, N. Mizuno, T. Murase, T. Onishi, S. Park, P. P. Plucinsky, J. Rho, A. M. S. Richards, G. Rowell, M. Sasaki, J. Seok, P. Sharda, L. Staveley-Smith, H. Suzuki, T. Temim, K. Tokuda, K. Tsuge, K. Tachihara
Figure caption: (a) Radial profile of the normalized X-ray intensity, centered at (α J2000, δ J2000) = (05h25m59.ˢ57, ﹩-66^\circ 04^{\prime} 56\buildrel{\rm{s}}\over{.} 4﹩) as the geometric center of the SNR. The steps with filled circles indicate averaged values of normalized X-ray intensity at each annulus. The green line indicates the three-dimensional Gaussian distribution, and the orange line represents its projected distribution given by the least-squares fitting (see the text). (b) Scatter plot of kinetic temperature T kin for each cloud as a function of the projected radial distance. The dashed horizontal line represents T kin=10 K, corresponding to the typical temperature of quiescent molecular clouds. The red and green symbols represent high- and moderate-temperature clouds, respectively.
Paper: ALMA Observations of Supernova Remnant N49 in the Large Magellanic Cloud. II. Non-LTE Analysis of Shock-heated Molecular Clouds
Authors: H. Sano, Y. Yamane, J. Th. van Loon, K. Furuya, Y. Fukui, R. Z. E. Alsaberi, A. Bamba, R. Enokiya, M. D. Filipović, R. Indebetouw, T. Inoue, A. Kawamura, M. Lakićević, C. J. Law, N. Mizuno, T. Murase, T. Onishi, S. Park, P. P. Plucinsky, J. Rho, A. M. S. Richards, G. Rowell, M. Sasaki, J. Seok, P. Sharda, L. Staveley-Smith, H. Suzuki, T. Temim, K. Tokuda, K. Tsuge, K. Tachihara
Figure caption: Top panels: large velocity gradient results on the number density of molecular hydrogen, n(H2), and the kinetic temperature, T kin, for the ambient cloud P, pre-shocked cloud R, and the post-shocked cloud L. The red lines and blue dashed-dotted lines indicate the intensity ratios of 12CO(J = 3–2)/12CO(J =2–1) and 13CO(J = 2–1)/12CO(J =3–2), respectively. The shaded areas surrounding the red and blue lines indicate the 1σ ranges of each intensity ratio. Yellow crosses represent the best-fit values of n(H2) and T kin for each cloud. The spatial positions and best-fit values for each cloud are shown in the top-right corners for each panel. Bottom panels: CO intensity profiles for clouds P, R, and L. The physical properties of each cloud are summarized in Table 1.
Paper: What Is the Nature of the HESS J1731-347 Compact Object?
Authors: Violetta Sagun, Edoardo Giangrandi, Tim Dietrich, Oleksii Ivanytskyi, Rodrigo Negreiros, Constança Providência
Figure caption: Scan over the particle’s mass m DM and fraction f DM of DM that reproduce M and R measurement of HESS J1731-347. While the color map represents the total maximum gravitational mass of DM-admixed NSs using the BigApple EOS, the contour lines represent the IST EOS configurations. Dashed–dotted and solid black curves are the contour lines showing the maximum mass obtainable with the IST EOS. The red solid line shows the limit at which both stiff and soft EOSs fulfill the 2σ constraint of HESS J1731-347. Above which, in the upper right corner of the plot, there is the allowed region where both baryonic models fulfill the HESS constraint.
Paper: ALMA Observations of Supernova Remnant N49 in the Large Magellanic Cloud. II. Non-LTE Analysis of Shock-heated Molecular Clouds
Authors: H. Sano, Y. Yamane, J. Th. van Loon, K. Furuya, Y. Fukui, R. Z. E. Alsaberi, A. Bamba, R. Enokiya, M. D. Filipović, R. Indebetouw, T. Inoue, A. Kawamura, M. Lakićević, C. J. Law, N. Mizuno, T. Murase, T. Onishi, S. Park, P. P. Plucinsky, J. Rho, A. M. S. Richards, G. Rowell, M. Sasaki, J. Seok, P. Sharda, L. Staveley-Smith, H. Suzuki, T. Temim, K. Tokuda, K. Tsuge, K. Tachihara
Figure caption: Scatter plot between T kin and n(H2). The dashed line indicates the linear regression using the least-squares method except for the CO clouds L, K, and T (see the text).
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption:  12CO(J = 2–1) and SiO(J = 5–4) integrated-intensity maps. The two black crosses in each panel correspond to the peak positions of the dust continuum sources, Sources A (east cross) and B (west cross). The primary beam at the full width at half maximum is also depicted by a dashed black circle in each panel. Left: low-velocity components of the 12CO(J = 2–1) emission. The blue and red contours represent the integrated intensity of the blue- and redshifted 12CO(J = 2–1) emission with the LSR velocity in the range from −13 to 6 km s−1and from 12 to 34 km s−1, respectively. The blue contour levels are [2, 4, 10, 15, 20, 25, 30]×1σ (1σ = 60.0 mJy beam−1). The red contour levels are [2, 4, 6, 8, 10]×1σ (1σ = 80.0 mJy beam−1). The black ellipse in the bottom left corner represents the synthesized beam size of the 12CO(J = 2–1) emission. Center: High-velocity components of the 12CO(J = 2–1) emission. The blue and red contours represent the integrated intensity of the blue- and redshifted 12CO(J = 2–1) emission in the LSR velocity ranges from −31 to −14 km s−1 and from 35 to 56 km s−1, respectively. The blue contour levels are [2, 4, 6, 8]×1σ (1σ = 68.9 mJy beam−1). The red contour levels are [2, 4, 6, 8]×1σ (1σ = 84.2 mJy beam−1). The black ellipse in the bottom left corner is the same as that in the left panel of this figure. Right: SiO(J = 5–4) emission. The blue and red contours represent the integrated intensity for the blue- and redshifted SiO(J = 5–4) emission in the LSR velocity ranges from −31 to −19 km s−1and from 40 to 45 km s−1, respectively. The green contours represent the integrated intensity of the SiO emission around the systemic velocity in the LSR velocity range from 8 to 9 km s−1. The blue contour levels are [2, 4, 6, 8, 10]×1σ (1σ = 40.0 mJy beam−1). The red contour levels are [2, 4, 6, 8, 10]×1σ (1σ = 20.0 mJy beam−1). The green contour levels are [2, 4, 6, 8, 10]×1σ (1σ = 7.0 mJy beam−1). The black ellipse in the bottom left corner represents the synthesized beam size for the SiO(J = 5–4) emission.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption: (a) Primary and secondary outflow image. The blue and red components correspond to integrated intensities of the 12CO (J = 2–1) emission that are larger than 2σ(1σ = 6.5 mJy beam−1) with the LSR velocity in the range from −13 to 6 km s−1 for the blueshifted component and from 12 to 34 km s−1 for the redshifted component. The yellow star represents the location of Ser-emb 15. The dashed white lines represent the axis of the primary outflow with P.A. = +20°, along which the blue- and redshifted CO emission is elongated from north to south, and the axis of the secondary outflow with P.A. = +110°, along which the redshifted CO emission is elongated to the east toward the center. The light blue ellipse in the bottom left corner of the panel represents the synthesized beam size of the 12CO (J = 2–1) emission. (b) 12CO (J = 2–1) line spectra in the primary outflow. The solid blue and red lines correspond to the spectrum of the emission integrated over the north and south lobes, respectively, as indicated in panel (a), with respect to Ser-emb 15. (c) 12CO (J = 2–1) line spectrum in the secondary outflow. The solid red line corresponds to the spectrum of the emission integrated over the east lobe, as indicated in panel (a), with respect to Ser-emb 15 . The dashed green line in panels (b) and (c) corresponds to the systemic velocity of 10.5 km s−1. The systemic velocity is estimated from the C18O (J = 2–1) line spectrum presented in Figure 5 of Appendix A.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption: Top: C18O (J = 2–1) channel map in the LSR velocity range from 5 to 13 km s−1. The color scale and black contours represent the C18O emission with a velocity resolution of 1.0 km s−1. The magenta cross is the peak flux position for Source A in the 1.3 mm continuum emission. The black contour levels are [2, 3, 5, 7, 10] × 1σ (1σ = 6.0 mJy beam−1). The synthesized beam for the C18O emission is denoted by the magenta ellipse in the panel in the bottom left corner. Bottom: C18O (J = 2–1) line spectrum obtained from a circular area with a radius of 0.″5 (∼218 au) centered on the peak flux position for Source A denoted by the dashed white line in the 11 km s−1 channel of the top panel. The solid blue and red lines represent the line spectrum from the C18O data with a velocity resolution of 0.1 km s−1 (rms = 30 mJy beam−1) and the results of the Gaussian fitting, respectively. The Gaussian fitting shows that the LSR velocity at the peak intensity is 10.5 km s−1.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption: Comparison of the spatial distributions between SiO(J = 5–4) and 12CO(J = 2–1) emission. The integrated intensity of the blueshifted 12CO(J = 2–1) emission is shown, with the relative velocity in the range from −4 to −23 km s−1 (blue). The integrated intensity of the redshifted 12CO(J = 2–1) emission is shown, with the relative velocity in the range from 1 to 2 km s−1 (red, and white contours). The white contour levels are [12, 14, 15, 20, 25, 30, 35] ×1σ (1σ = 6.5 mJy beam−1). The yellow contours represent the integrated intensity of the blueshifted SiO(J = 5–4) emission with the relative velocity in the range from −1 to −3 km s−1. The yellow contour levels are [5, 7, 9, 10] ×1σ (1σ = 7.5 mJy beam−1). The black square and triangle correspond to the peak positions of the dust continuum sources, Source A and Source B, respectively. The white and yellow ellipses in the bottom left corner represent the synthesized beam size of the 12CO(J = 2–1) and SiO(J = 5–4) emission, respectively.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption:  12CO(J = 2–1) channel map in the LSR velocity range from −40 to 20 km s−1. The color scale and black contours represent the CO emission. Each panel is obtained by combining the frequency channels to be in a velocity range of 5.0 km s−1 using the CASA task imrebin. The white cross is the peak flux position for Source A in the 1.3 mm continuum emission. The white contour levels are [3, 5, 7, 10, 12, 15, 17, 20, 25, 30, 35, 40, 45, 50, 55, 60]× 1σ (1σ = 3.0 mJy beam−1). The synthesized beam for the CO emission is denoted by the white ellipse in the panel in the bottom left corner. The color bar on the right side is fixed in the range from −5.0×10−3 to 0.15 Jy beam−1.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption: ALMA 12 m array 233 GHz continuum image represented in color scale and black contours. The black contour levels are [3, 5, 10, 14, 20, 30, 40, 50] ×1σ (1σ = 0.24 mJy beam−1). The white ellipse in the bottom left corner is the largest synthesized beam size of the continuum emission.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Ensemble-averaged oscillation frequency of processed A 2 after the bar-formation stage for different Q (square points). The size of the error bars corresponds to the standard deviation among realizations. The averaged radial oscillation frequencies of nearly circular orbit particles and eccentric orbit particles at the beginning are plotted in filled circles and filled triangles, respectively (see the specification of those particles in the text). The frequencies are presented in units of κ 0. The dashed line corresponds to the effective epicyclic frequency as a function of Q given by Equation (16).
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Top panel: ensemble-averaged angular frequency of the m = 2 mode computed before (triangle) and after (circle) the fully developed bar for different Q in units of Ω0. The dashed line corresponds to the disk's effective angular frequency as a function of Q from Equation (10). Bottom panel: ensemble-averaged fraction of a number of particles trapped in the resonance during the time around the first peak of A 2 for different Q. In both panels, error bars represent the standard deviation.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Time evolution of A 2 for a selected realization with Q = 1 presented in Figure 2 represented by the solid line. The dashed line represents the reprocessed A 2 prepared for Fourier analysis (see the description of the data processing in the text).
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Intrinsic velocity field superposed on the disk configuration, in face-on view, for indicated Q at indicated time. The size and direction of the arrows represent the magnitude (in arbitrary units) and the direction of locally averaged velocity. The left and middle panels depict the Q = 1 disk during and after the formation of the bar, respectively. The right panel represents the disk with Q = 1.5 during the formation of the bar.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Surface density as a function of radial distance Σ(r) for Q = 1 (top panel) and 1.5 (bottom panel) in solid line. Both profiles are taken at t = 6.31. The straight dashed lines correspond to the best-fitting exponential functions for different disk parts.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Time evolution of A 2 for disks in rigid (top panel) and live (bottom panel) halos for different Q.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Time evolution of angular momenta of the disk and halo for Q = 1.8 (top panel) and Q = 2.25 (bottom panel) in units of ﹩{L}_{0}\equiv {{MR}}_{0}^{2}{{\rm{\Omega }}}_{0}﹩.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Radial velocity dispersion as a function of radius σ  r (r) for Q = 1.8 (top panel) and 2.25 (bottom panel) at different times.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Plot of ﹩\cot i﹩ where i is the logarithmic pitch angle as a function of radius r for different Q. Plots are taken at the time around the first peak of A 2.
Paper: Kinetic-scale Topological Structures Associated with Energy Dissipation in the Turbulent Reconnection Outflow
Authors: S. Y. Huang, J. Zhang, Q. Y. Xiong, Z. G. Yuan, K. Jiang, S. B. Xu, Y. Y. Wei, R. T. Lin, L. Yu, Z. Wang
Figure caption: Conditional averages of ﹩{\boldsymbol{j}}\cdot {{\boldsymbol{E}}}^{{\prime} }﹩ on (a) six geometrical invariants, (b) −nQ  K , and (c) nQ  J  under three different conditions.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Example to illustrate our procedure to model an LAE spectrum and measure its Lyα and UV continuum properties. The red circles are photometric data points. The vertical error bars indicate the photometry errors and the horizontal bars indicate the FWHM of the narrow- and broadband filters. This LAE is at z = 3.673. Its power-law continuum is fitted with the broadband R, ﹩i^{\prime} ﹩, and ﹩z^{\prime} ﹩ photometry. After applying the IGM absorption, we calculate the scaling factor A in Equation (1) by matching the Lyα line profile with the narrowband photometry. The inset shows the region around the Lyα line.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: LAEs in the SXDS, SDF, and SDFn fields. The left panel shows LAEs at z ∼ 3.7 in SXDS and the right panel shows LAEs at z ∼ 4.8 in SDF and SDFn. In each panel, the gray regions indicate the coverage area of the Subaru Suprime-Cam images. The large circles represent the pointings of our Hectospec observations. The color-coded points represent spectroscopically confirmed LAEs.
Paper: Kinetic-scale Topological Structures Associated with Energy Dissipation in the Turbulent Reconnection Outflow
Authors: S. Y. Huang, J. Zhang, Q. Y. Xiong, Z. G. Yuan, K. Jiang, S. B. Xu, Y. Y. Wei, R. T. Lin, L. Yu, Z. Wang
Figure caption: The first and the second rows represent the joint pdf of ﹩P({{nQ}}_{{\rm{\Omega }}}^{e},-{{nQ}}_{D}^{e})﹩, the joint pdf of ﹩P({{nQ}}_{{\rm{\Omega }}}^{i},-{{nQ}}_{D}^{i})﹩, and the conditional averages of ﹩{\boldsymbol{j}}\cdot {{\boldsymbol{E}}}^{{\prime} }﹩ on six geometrical invariants. The left and right columns represent the results of method 1 and method 2, respectively.