adsabs/AstroCLIMB huggingface dataset:
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: 2D cuts in the r-p plane at simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a) Magnetic field magnitude ∣ B ∣/B 0. The black contours represent the in-plane magnetic field lines, and the black stars represent two x-points. (b) Out-of-plane component magnetic field (B  a  − B  a,0)/B 0. The black arrows in this panel represent the in-plane magnetic vectors ( B   rp ). (c) Out-of-plane electron speed u  a,e /v A,i . The black arrows in this panel represent the in-plane electron velocity vectors ( u   rp,e /v A,i ). (d) Out-of-plane ion speed u  a,i /v A,i . The black arrows in this panel represent the in-plane ion velocity vectors ( u   rp,i ). In all panels, the black square outlines the diffusion region.
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: 2D cuts of the pressure tensor components in the r-p plane at the simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a) Electron scalar pressure p  e /p 0. Off-diagonal components of the electron pressure tensor: (b) Π ra,e /p 0, (c) Π pa,e /p 0, and (d) Π pr,e /p 0. (e) Ion scalar pressure p  i /p 0. Off-diagonal components of the ion pressure tensor: (f) Π ra,i /p 0, (g) Π pa,i /p 0, and (h) Π ra,i /p 0.
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: 2D cuts in the r-p plane at the simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a−e) Kinetic power density terms for electrons. (f−j) Thermal power density terms for electrons. All quantities are normalized to ﹩{\rm{\Delta }}{\varepsilon }_{0}={\omega }_{{pi}}{m}_{i}{v}_{{\rm{A}},i}^{2}﹩. The vertical dashed lines in panels (a)−(f) show the 1D trajectory for our 1D analysis.
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: Spatial context of the reconnection event within the simulation domain. Panel (a) shows a volume rendering of ∣ J ∣. Panel (b) shows the 3D magnetic field lines color-coded with ∣ B ∣. On the vertical cuts in panel (b), we show J  z . Panel (c) shows the magnetic field lines in the x-y plane. The black contours show in-plane magnetic field lines. The green square highlights the size and position of the region for the energy analysis.
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: 1D cuts of the power density terms along the ﹩\hat{p}﹩-direction at r = 5.58d  i  and at the simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a) Kinetic power density terms in Equation (8). (b) Thermal power density terms in Equation (11). The vertical dashed line represents the crossing of the x-point at r = 5.58d  i  and p = 6.6d  i .
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: Magnification of the region delimited by the black square in Figure 2 in the r-p plane at the simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a) Electron scalar pressure p  e . Off-diagonal components of the electron pressure tensor: (b) Π ra,e , (c) Π pa,e , and (d) Π pr,e . Panel (e) shows a sketch of the patterns of the scalar pressure emerging in 2D simulations of reconnection, and panels (f)−(h) show sketches of the off-diagonal terms of the electron pressure based on 2D Harris current sheet reconnection without a guide field (Yin et al. 2001).
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: 2D cuts in the r-p plane and isosurfaces of the pressure tensor components at the simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a) Electron scalar pressure p  e /p 0. Off-diagonal components of the electron pressure tensor: (b) Π ra,e /p 0, (c) Π pa,e /p 0, and (d) Π pr,e /p 0. (e) Ion scalar pressure p  i /p 0. Off-diagonal components of the ion pressure tensor: (f) Π ra,i /p 0, (g) Π pa,i /p 0, and (h) Π ra,i /p 0.
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: 2D cuts in the r-p plane and isosurfaces of the power density terms at the simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a−e) Kinetic power density terms for electrons. (f−j) Thermal power density terms for electrons. All quantities are normalized to ﹩{\rm{\Delta }}{\varepsilon }_{0}={\omega }_{{pi}}{m}_{i}{v}_{{\rm{A}},i}^{2}﹩.
Paper: IllustrisTNG Snapshots for 10 Gyr of Dynamical Evolution of Brightest Cluster Galaxies and Their Host Clusters
Authors: Jubee Sohn, Margaret J. Geller, Mark Vogelsberger, Josh Borrow
Figure caption: The (σ *,BCG/σ cl) − σ cl relation for clusters in three redshift snapshots (z = 0.0, 1.0, and 2.0 from top to bottom). We show the BCG stellar velocity dispersion measured within 3 kpc, 10 kpc, 50 kpc, and the half mass–radius (from left to right).
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: Damping and heating proxies at the simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a) 2D cuts in the r-p plane of the Zenitani parameter for electrons D  ze . (b) Diagonal part of the strain pressure interaction p θ  e . (c) Off-diagonal part of the strain pressure interaction Pi − D  e . (d) 1D cut of these terms as in Figure 7.
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: (a) Time evolution of the energy densities averaged over the full simulation domain (solid curves) and over the subdomain (dashed curves). The total energy density is ﹩{\varepsilon }^{T}={\varepsilon }_{e}^{k}+{\varepsilon }_{i}^{k}+{\varepsilon }_{e}^{\mathrm{th}}+{\varepsilon }_{i}^{\mathrm{th}}+{\varepsilon }^{\mathrm{em}}﹩. (b) Time evolution of the absolute values of the energy density rates Δ〈ε〉/Δt (dashed curves) and the dissipative power densities Ξ (solid curves with circles), averaged over the full simulation domain and normalized to ﹩{\varepsilon }_{\mathrm{full}}^{T}﹩.
Paper: Energy Transport during 3D Small-scale Reconnection Driven by Anisotropic Plasma Turbulence
Authors: Jeffersson A. Agudelo Rueda, Daniel Verscharen, Robert T. Wicks, Christopher J. Owen, Georgios Nicolaou, Kai Germaschewski, Andrew P. Walsh, Ioannis Zouganelis, Santiago Vargas Domínguez
Figure caption: 2D cuts in the r-p plane and isosurfaces at the simulation time ﹩t=120{\omega }_{{pi}}^{-1}﹩. (a) Kinetic power density dissipation ﹩{{\rm{\Xi }}}_{e}^{k}﹩. (b) Thermal power density dissipation ﹩{{\rm{\Xi }}}_{e}^{\mathrm{th}}﹩. All quantities are normalized to ﹩{\rm{\Delta }}{\varepsilon }_{0}={\omega }_{{pi}}{m}_{i}{v}_{{\rm{A}},i}^{2}﹩.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Outcomes of outbursts for given initial envelope mass vs. WD mass, as labeled. Red points shifted slightly to the left of their actual WD masses denote models with solar composition envelopes; blue points to the right of their WD masses are models with CO-enriched envelopes. The solid and dotted lines mark the approximate envelope mass below which thin, steady-state, thermally stable hydrostatic envelope solutions exist and outflows cease.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Mass outflow rate at the Roche radius vs. the remaining envelope mass for the 1.2 + 3 × 10−5 M ⊙ C/O-enriched envelope model. The thin line represents the evolution after the photosphere recedes to the iron opacity bump when a more accurate radiation transport calculation for the wind is needed.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Same as Figure 8, but for the C/O-enriched models.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Same as Figure 3, but for the 0.6 + 10−3 M ⊙ solar composition envelope model. Note the changes in axes and times.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Same as Figure 2, but for the 0.6 + 10−3 M ⊙ solar composition envelope model. Note the changes in axes and times.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Same as Figure 3, but for the 0.8 + 10−4 M ⊙ C/O-enriched envelope model. Note the changes in axes and times.
Paper: Binary Interaction Dominates Mass Ejection in Classical Novae
Authors: Ken J. Shen, Eliot Quataert
Figure caption: Same as Figure 2, but for the 0.8 + 10−4 M ⊙ C/O-enriched envelope model. Note the changes in axes and times.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: The optical, X-ray, and radio light curves of two new orphan afterglows, AT 2021any (top panel) and AT 2021lfa (bottom panel), together with their best-fit power laws. Data presented in this paper are shown as filled points, with different symbols for different instruments. Data obtained from GCNs (Zhu et al. 2021; Guelbenzu et al. 2021) are shown as unfilled circles. The optical data have been corrected for Milky Way extinction. X-ray data are shown with a plus sign and scaled by a factor of 30 for clarity. Radio X-band data are shown with crosses. Arrows indicate upper limits. An “S” along the top marks an epoch of spectroscopy. The best-fit t 0 is calculated as described in Section 3.2—we caution that these values are uncertain.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: The r-band light curve (corrected for Milky Way extinction) of each ZTF afterglow compared to the sample of afterglows detected in follow-up observations to Swift-BAT triggers (Kann et al. 2010) and Fermi-GBM triggers (Singer et al. 2015). The left panel shows afterglows with associated detected GRBs, and the right panel indicates afterglows with no associated detected GRB. For the orphan events, we caution that the estimated t 0 is uncertain. The shaded region corresponds to the 25–75 percentile bounds of the Swift-BAT sample (Kann et al. 2010). The crosses indicate the first detection of each Fermi-GBM afterglow in Singer et al. (2015). The horizontal gray line indicates the nominal ZTF limit of 20.5 mag. Photometry is obtained from Cenko et al. (2013, 2015), Bhalerao et al. (2017), Ho et al. (2020a), Andreoni et al. (2021), and D. Perley et al. (2022, in preparation). For ATLAS17aeu we include c-band points. For AT 2019pim we include TESS points obtained at Δt < 0.1  day. Our searches tend to find afterglows that are brighter than the bulk of the follow-up sample.
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: The duration and luminosity of optical transients. Measurements of superluminous supernovae (SLSNe), Type Ia supernovae (SNe Ia), and most core-collapse supernovae (CC SNe) are from the ZTF Bright Transient Survey (Fremling et al. 2020; Perley et al. 2020). Measurements of short-duration CC SNe and AT 2018cow-like transients are from dedicated searches for fast-evolving transients (Prentice et al. 2018; Perley et al. 2019b, 2021b; Ho et al. 2020b, 2021c; Yao et al. 2022). For reference we also show the timescale and luminosity of the optical emission from GW170817/AT 2017gfo (Coulter et al. 2017; Cowperthwaite et al. 2017; Kasliwal et al. 2017; Drout et al. 2017; Villar et al. 2017b) and of iPTF14yb (the only optically discovered afterglow prior to ZTF with a redshift measurement; Cenko et al. 2015). The afterglows discussed in this paper are the fastest and most luminous optical transients discovered and monitored in real time. Owing to the cadence of ZTF, our measurements typically represent upper limits on the duration and lower limits on the peak luminosity. Measurements are in rest-frame g band when possible, with a crude K-correction applied (Equation (1) for afterglows; see Ho et al. (2021c) for other sources).
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: 3.4 μm WISE+NEOWISE light curve of the four CL and CLB AGNs. The orange filled circles represent the obtained W1 magnitude at a given observing time. The red filled circles with error bars represent the binned W1 magnitude at each epoch. The vertical straight lines represent the observing date of the obtained SDSS spectra. The black/gray ones represent the date of the first/second-epoch spectrum, respectively. The dashed lines represent the time of the arrival of the information of the AD into the dusty torus region traced by the W1 band.
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: Top panels: the rest-frame optical spectra of the luminosity-declining AGN candidates showing a CLB between the two epochs of the SDSS observations (the blue and red lines represent the first- and second-epoch ones, respectively). The observation dates are shown with units of MJD in the legend of each panel. Bottom panels: the subtracted spectrum between the two epochs (black) overlaid with the fitting curve of the theoretical AD of f  λ  ∝ λ 2.3 (orange) (Shakura & Sunyaev 1973).
Paper: Cosmological Fast Optical Transients with the Zwicky Transient Facility: A Search for Dirty Fireballs
Authors: Anna Y. Q. Ho, Daniel A. Perley, Yuhan Yao, Dmitry Svinkin, A. de Ugarte Postigo, R. A. Perley, D. Alexander Kann, Eric Burns, Igor Andreoni, Eric C. Bellm, Elisabetta Bissaldi, Joshua S. Bloom, Thomas G. Brink, Richard Dekany, Andrew J. Drake, José Feliciano Agüí Fernández, Alexei V. Filippenko, Dmitry Frederiks, Matthew J. Graham, Boyan A. Hristov, Mansi M. Kasliwal, S. R. Kulkarni, Harsh Kumar, Russ R. Laher, Alexandra L. Lysenko, Bagrat Mailyan, Christian Malacaria, A. A. Miller, S. Poolakkil, Reed Riddle, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, Jesper Sollerman, Christina Thöne, Anastasia Tsvetkova, Mikhail Ulanov, Andreas von Kienlin
Figure caption: Optical spectra of AT 2021any (top panel; OSIRIS/GTC) and AT 2021lfa (bottom panel; GMOS-S/Gemini), two afterglows with no associated detected GRB. Vertical lines mark absorption features used to measure the redshifts of z = 2.5131 (AT 2021any) and z = 1.0624 (AT 2021lfa). Regions affected by telluric absorption are also marked. The blue line in the AT 2021any panel is the error spectrum.
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: Top: the distribution of luminosity-declining AGN candidates (blue circles) and parent sample (gray circles) in the BPT diagram (Baldwin et al. 1981). The two sequences are shown separating the AGNs and star-forming galaxies (Kewley et al. 2001; Kauffmann et al. 2003) and the horizontal line separating the AGN and the LINERs (Ho et al. 1997). Bottom panel: cumulative histogram of the line flux ratio of log([N II] λ6584/Hα).
Paper: Finding of a Population of Active Galactic Nuclei Showing a Significant Luminosity Decline in the Past ∼103–104 yr
Authors: Janek Pflugradt, Kohei Ichikawa, Masayuki Akiyama, Mitsuru Kokubo, Bovornpractch Vijarnwannaluk, Hirofumi Noda, Xiaoyang Chen
Figure caption: WISE and NEOWISE light curves at 3.4 μm of two of the luminosity-declining AGN candidates, SDSS J211636.33+110237.4 (left) and SDSS J111800.12+233651.5 (right). Both light curves show a continuous flux decrease over the 10 yr long time span with ΔW1 ∼ 0.49 mag (left) and ΔW1 ∼ 0.34 mag (right), respectively.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Exposure-corrected 0.5–7.0 keV image obtained with Chandra in 2001. The white and green lines indicate the analysis regions for proper motion and spectral studies, respectively. The arrows beside the regions indicate the filament velocities (proportional to the arrow lengths) of the filaments as described in Section 3.1.2. Their directions also correspond to the positive directions of the positions in Figures 17 and 18 in Appendix A.
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption: (Left) Face-on view of the gas density distribution in our hydrodynamic simulation. An eccentric gas cavity is seen. Spatial axes are in units of arcsecond, and the same distance to MWC 758 is adopted. (Middle) Face-on view of the dust density distribution in our hydrodynamic simulation. A thin ring of dust accumulation is seen at the cavity edge. (Right) Velocity deviations from the Keplerian rotation measured from the velocity map of our synthetic data of the hydrodynamic simulation. An open ellipse delineates the edge of the inner cavity. The velocity deviations are redshifted at all azimuthal angles around the edge of the inner cavity, which is theoretically expected.
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption: (Left) Our fitting of eccentric gas motion to the observed velocity deviations in the ALMA archival data of the 13CO emission in the MWC 758 disk at r = 0.″32, where the inner dust ring has been found to be eccentric. Only the positive observed deviations are considered in the fitting because the expected deviations from an eccentric orbit are positive. ϕ = 0° refers to the northwestern side of the minor axis. (Center) The radial profile of our derived gas eccentricity from the archival 13CO data. Data points are separated by half the beam size. (Right) The radial profile of the best-fit position angle of the pericenter of the eccentric orbit from the archival 13CO data. In the central and right panels, the gray shaded area shows the signal-to-noise ratio of the measured velocity deviations, and the gray line denotes the 3σ confidence level of the velocity deviation.
Paper: Particle Acceleration Controlled by Ambient Density in the Southwestern Rim of RCW 86
Authors: Hiromasa Suzuki, Satoru Katsuda, Takaaki Tanaka, Nobuaki Sasaki, Tsuyoshi Inoue, Federico Fraschetti
Figure caption: Exposure-corrected 2.0–7.0 keV image in 2001. The white rectangular regions are used to study the nonthermal spectral variations. The arrows beside the regions indicate the moving directions and velocities (proportional to the arrow lengths) of the filaments as described in Section 3.1.2. The arrows also correspond to the positive directions of the angular positions in Figure 9.
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption: (Left) Our fitting of the eccentric gas motion (light blue curve) to the measured velocity deviations in the synthetic data (blue data points). (Right) Comparison of the velocity deviations around the inner cavity between the observed and synthetic data, which are shown as black and blue data points, respectively. ϕ = 0° refers to the northwestern side of the minor axis of the disk.
Paper: Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu, Tze-En Chang
Figure caption: Difference between the projected velocity maps of the two best-fit Keplerian disk models with inclination fixed at 21° and with the stellar mass fixed at 2 M ☉.