adsabs/AstroCLIMB huggingface dataset:
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Structure velocity dispersion against radius for all leaves (blue) and branches (orange), but this time for unextrapolated quantities (points). We additionally use levelprops traces as in Figure 8 to show the change of velocity dispersion and size as the contour level is raised in 0.1 K intensity steps. The traces are plotted in gray where they contain fewer pixels than half the beam size. Three linear least-squares fits are shown, with their slopes in km s−1 pc−1: to the unextrapolated points (solid line; uncertainty is standard error), all points including traces (dashed line; uncertainty is standard error), and the mean of fits to individual traces (dotted line; uncertainty is standard deviation). The estimated 50% completeness limits (Section 3.3) are demarcated by the hatched boundaries.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Exploring the impact of dendrogram parameter choices on the resulting mass, radius, and velocity dispersion distribution functions. The canonical parameters are set to min_value = 2.5σ, min_delta = 3σ, and min_npix = 4Ω, where σ represents the characteristic noise of 0.4 K and Ω the beam solid angle in pixels (see Section 3.1). In the top row (red) we vary min_value while keeping the other two parameters constant; in the middle (purple) we vary min_delta; and in the bottom (green) we vary min_npix.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Structure aspect ratio against the logarithm of size for leaves (blue) and branches (orange) in our catalog. A least-squares fit, shown in red, returns a slope of −0.1  ±  0.1 pc−1.
Paper: The Hierarchical Dynamical State of Molecular Gas from 3 to 300 pc in NGC 253
Authors: Elias K. Oakes, Christopher M. Faesi, Erik Rosolowsky, Adam K. Leroy, Simon C. O. Glover, Annie Hughes, Sharon E. Meidt, Eva Schinnerer, Jiayi Sun, Amirnezam Amiri, Ashley T. Barnes, Zein Bazzi, Ivana Bešlić, Frank Bigiel, Guillermo A. Blanc, Charlie Burton, Ryan Chown, Enrico Congiu, Daniel A. Dale, Simthembile Dlamini, Hao He, Eric W. Koch, Fu-Heng Liang, Jérôme Pety, Miguel Querejeta, Sumit K. Sarbadhicary, Sophia K. Stuber, Antonio Usero, Thomas G. Williams
Figure caption: Logarithm of the virial parameter against structure radius for all structures in the dendrogram, colored by aspect ratio. The horizontal lines and hatched region are as in Figure 4.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: Total accretion rates ﹩\dot{M}={\dot{M}}_{1}+{\dot{M}}_{2}﹩ of retrograde binaries for the viscosities noted in the top right of each panel. The inspiral is initiated at ﹩t=1000\,[2\pi {{\rm{\Omega }}}_{0}^{-1}]﹩ orbits, at which time the time series cadence is also increased. The dashed gray lines correspond to the times at which the density snapshots are taken in Figure 1 (i.e., ab = [100rG, 67rG, 24rG, 11rG]) in all panels. The accretion rate is normalized to unity in each panel, with ﹩{\dot{M}}_{{\rm{i}}}\gt 3\pi \nu {{\rm{\Sigma }}}_{0}﹩ (this overshoot is discussed in M. Clyburn & J. Zrake 2024 and attributed to an artifact of the outer boundary). The dashed blue lines represent the “weakening-torque effect” from J. Zrake et al. (2025).
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: A logarithmic plot of the cavity semimajor axis ac as a function of the binary semimajor axis ab throughout the inspiral (early times to the left, later times to the right). The dashed and solid lines represent prograde and retrograde disk configurations, respectively, while the different colors represent different kinematic viscosities. The vertical faded lines denote the predicted decoupling semimajor axis from Equation (10) with ξ = 0.5, while the black overlay line traces the cavity evolution during the coupled-phase of binary-disk evolution.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: The normalized accretion rate (top), disk surface density (middle), and vortensity (bottom) during a phase of bridge instability (gray band) for ﹩\tilde{\nu }=1{0}^{-4}﹩. The arrows illustrate the velocity profile of the disk, while the white circles represent the component sinks. The vortensity can be either aligned (red) or misaligned (blue) with the binary angular momentum vector. The white vectors illustrate the local gas velocity while the binary moves counterclockwise. The time in each panel is expressed in units of the initial orbital period ﹩{P}_{0}=2\pi {{\rm{\Omega }}}_{0}^{-1}﹩.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: Zero-velocity curves for different values of the Jacobi constant CJ. The critical value ﹩{C}_{J}^{* }﹩ (solid black line) is the minimum value that separates the binary (black dots) from the outer regions of the disk. For ﹩{C}_{J}\lt {C}_{J}^{* }﹩ (red dashed line), a particle can cross through L2 or L3 to travel between the inner and outer regions of the disk. The Roche-bound region (dashed black line) is described by an isocontour ﹩{C}_{J}^{R}﹩ and describes test particles that are bound to one of the binary components.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: Zoom in on one of the binary components. The arrows represent the direction of fluid velocity in the frame corotating with the binary, and the colormap is the logarithmic surface density. Regions (i) and (ii) experience significant deflections by the binary and collide, forming a shock behind each binary component.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: Subcritical (gray), supercritical (orange), and Roche-bound (beige) values of the Jacobi constant for prograde (top) and retrograde (bottom) Keplerian disks. The solid, dashed, and dotted lines are tracks of test particles in the corotating frame, initialized on circular Keplerian orbits at radii r/a0 = 1.2, 1.6, 2. The black and white arrows denote the particle's initial and final positions, respectively.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: The ratio of averaged gravitational torques to averaged accretion torques taken over fixed time intervals of ﹩\delta t=12\pi {{\rm{\Omega }}}_{0}^{-1}﹩. The dashed gray lines at ﹩t=1000\,[2\pi {{\rm{\Omega }}}_{0}^{-1}]﹩ denote the start of the orbital inspiral.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: Two stable minidisk configurations for γsink = 1 Ω0, corresponding to different values of the softening radius, rsoft = 0.03a0 (left) and rsoft = 0.05a0 (right) in otherwise identical simulations. These density snapshots are taken at ﹩t=200[2\pi {{\rm{\Omega }}}_{0}^{-1}]﹩ with the large white arrows depicting the direction of motion of the binary.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: The torque exerted on the disk by the binary (blue) is normalized by the magnitude of the steady-state value determined during the burn-in phase ﹩| {{ \mathcal T }}_{i}| ﹩. A negative torque means that the disk is losing angular momentum to the binary. The black line denotes the binned means of the torque, while the light blue line denotes (minus) the binary semimajor axis −ab(t)/a0. Similar to the accretion rates, less viscous disks (top) exhibit strong variability in their torque profiles, while larger viscosities (bottom) correspond to more regular profiles.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 H2 0–0 S(1) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 [Ne II]12.814μm emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 H2 0–0 S(3) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 H2 0–0 S(4) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 H2 0–0 S(2) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 H2 0–0 S(8) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 H2 0–0 S(5) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 H2 0–0 S(6) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 H2 0–0 S(7) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: Chandra ACIS-S image of N132D in the energy band 1.2–7.0 keV produced from the LP data (Epoch B). The white arc regions (labeled S1–S8 along the southern rim and N1–N6 along the northern boundary) indicate the regions used for the expansion measurement and the spectral analysis. The bin size of the image is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩492. The units of the color bar are counts.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The raw measured expansion of the S1–S8 (labeled sequentially from left to right) and N1–N6 regions (“raw shifts” in Table 5), with the fitted average expansion (blue solid line) from the S1–S8 regions.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: As in Figure 6, but for the final expansion estimates. The expansion of each region (“corrected shifts” in Table 5) is based on the raw shifts shown in Figure 6, corrected for the PSF bias and COE bias. The blue solid line shows the average expansion of the S1–S8 regions.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The expansion of N132D along selected regions around the rim. The arrows point in the direction of the orientation of the regions (see Table 5), and their lengths are proportional to the estimated expansion velocities. The COE (white cross) is estimated assuming that the regions along the southern rim (S1–S8) lie on a circular rim, and their orientations closely follow the azimuthal locations of the rim (for comparison, the COE of the optical knots is also shown as the cyan cross; J. Banovetz et al. 2023; and the blue plus J. A. Morse et al. 1995). The orientations of the regions along the northern rim (N1–N6) are substantially different from their azimuthal locations relative to the COE.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: Point sources used in the registration are shown as labeled red circles on a merged Epoch B image. The circle labels are the point-source IDs (see Table 2). The image is binned to two ACIS sky pixels (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩964), and the energy band is 1.2–7.0 keV; the image is shown in logarithmic gray scale.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The C-stat variation with position shift for region S1. The green and blue data points are the C-stat calculated from the 2020 profile and shifted 2006 profile at the shift positions. The blue data points are included in the quadratic fitting for the shift estimate. The red solid line is the fitted quadratic function. The vertical dashed lines show the 1σ error range of the estimated shifts.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The cumulative radial enclosed counts fraction (ECF) in the two epochs for point source 2 (from Figure 2) in energy band 1.2–7.0 keV. The x-axis is the radius in ACIS “sky” pixels (“physical coordinates”). The narrower (blue) distribution, showing error bars at ECF intervals of 0.025, are for the merged Epoch A observations after registration. The broader (red) line and error bars are for the merged Epoch B observations after registration.