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Paper: A Dwarf Galaxy Debris Stream Associated with Palomar 1 and the Anticenter Stream
Authors: Yong Yang, Jing-Kun Zhao, Xian-Hao Ye, Gang Zhao, Ke-Feng Tan
Figure caption: The left panel is a 2D histogram of stars in CMD with PMs selected and background subtracted. The blue dashed line represents the best-fit isochrone with age = 11 Gyr and [M/H] = −0.7 dex at dm = 14.8 mag. The right panel is a 2D histogram of PMs after CMD selection and background subtraction. Both of the diagrams are smoothed with a 2D Gaussian kernel of σ = 1 pixel. The red polygons represent the CMD and PM selections applied to the stream and offstream regions.
Paper: A Dwarf Galaxy Debris Stream Associated with Palomar 1 and the Anticenter Stream
Authors: Yong Yang, Jing-Kun Zhao, Xian-Hao Ye, Gang Zhao, Ke-Feng Tan
Figure caption: The left panel displays GCs (black points) and Yangtze (red circle) in angular momenta and energy space. The right panel presents projections of streams and orbits in Galactic coordinate. The red line and black lines indicate Yangtze and its best-fit orbit. The blue and purple lines represent ACS and EBS, respectively. The blue triangle denotes Pal 1.
Paper: Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE
Authors: Robert A. Fesen, Bradley E. Schaefer, Dana Patchick
Figure caption: Blowup of Pa 30's central region. A white cross marks the central star, J005311. North is up; east is to the left.
Paper: Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE
Authors: Robert A. Fesen, Bradley E. Schaefer, Dana Patchick
Figure caption: A [S II] λ λ 6716, 6731 image of Pa 30 revealing a highly filamentary and radial morphology.
Paper: Unified Picture of the Local Interstellar Magnetic Field from Voyager and IBEX
Authors: J. S. Rankin, D. J. McComas, E. J. Zirnstein, L. F. Burlaga, J. Heerikhuisen
Figure caption: Similar to Figure 1 but in the Voyager 2 direction, using observations taken from ∼2018.5 to 2021.0 (black). Voyager 2's heliopause crossing occurred at a radial distance of 119.0 au. Blue solid lines indicate pressure fronts (“pfa” and “pfb”) and shocks (“sh”) identified by Burlaga et al. (2022). The magnetic field observations are plotted using publicly available data.                    The superimposed results from Zirnstein et al. (2016)'s IBEX data-driven model (green) utilized a heliopause boundary condition of 121 ± 2 au in the Voyager 2 direction. Measurement uncertainties (dominated by systematic errors) are included in gray, as reported by the magnetometer team, with (constant) values of: err  B  r = ±0.03 nT, err  B  t = ±0.03 nT, err  B  n = ±0.03 nT, and err∣ B ∣ ±0.06 nT. For Voyager 2, all uncertainties (including err∣ B ∣) were provided with the data set.
Paper: Unified Picture of the Local Interstellar Magnetic Field from Voyager and IBEX
Authors: J. S. Rankin, D. J. McComas, E. J. Zirnstein, L. F. Burlaga, J. Heerikhuisen
Figure caption: Unfolding of the modeled ( B                    ﹩{}_{{\rm{V}}1,\mathrm{mod}}﹩,  B                    ﹩{}_{{\rm{V}}2,\mathrm{mod}}﹩) and measured ( B  V1,   B  V2) LISMF from the two Voyager directions projected onto a sky map in ecliptic J2000. Magnetic field vectors measured at any point in the VLISM must eventually undrape to the same point far from the heliosphere ( B @1000 au; magenta stars), as demonstrated by the modeled LISMF (colored circles). (Left) Data from the two Voyager spacecraft (colored cross symbols) show inconsistencies in the direction of unfolding, with   B  V1 pointing toward the starboard side of the heliosphere (away from the nose) and   B  V2 pointing toward the opposite direction. The observational trends also differ from those of the respective models. (Right) These discrepancies are resolved when modeled components of   B  r are substituted for the observed values at each spacecraft ( B  t and   B  n remain unchanged), indicating that this component is the cause (recall Figures 1 and 2).
Paper: Unified Picture of the Local Interstellar Magnetic Field from Voyager and IBEX
Authors: J. S. Rankin, D. J. McComas, E. J. Zirnstein, L. F. Burlaga, J. Heerikhuisen
Figure caption: Global perspective of the LISMF as it drapes around the heliopause from a model that fit the IBEX Ribbon ENA data (Zirnstein et al. 2016). (Left) LISMF lines (black curves) and magnetic field magnitude (background multicolored shading) inferred from the configuration of the ribbon as viewed from the meridional plane. Five isocontours of ENA energy are distinguished in color to show how each region contributes to the overall ENA production rate in the ribbon. The blue circles and gray lines illustrate the secondary ENA mechanism, for which suprathermal ions from the VLISM become neutralized by charge exchange (blue circles) and form ENAs, which travel back inward toward IBEX (gray lines). Black arrows roughly indicate vectors in Voyager 1's direction (V1), the interstellar inflow direction (ULISM), and the Voyager 2 direction (V2) that are projected onto the meridional plane. The arrow lengths were chosen for visibility but are not scaled to reflect the current locations listed for each spacecraft. (Right) Unfolding of the simulated LISMF components along the Voyager 1 (top panel), upstream (middle panel; opposite to the interstellar inflow), and Voyager 2 (bottom panel) directions from the heliopause out to 1000 au. The black lines illustrate how the angle of the magnetic field changes over radial distance with respect to the unfolded direction at 1000 au (﹩\overrightarrow{B}﹩                   LISM), while the red lines show how the magnitude of the magnetic field changes with respect to ∣B LISM∣. The vertical yellow lines highlight each spacecraft’s location during the year of 2022.
Paper: On the Gamma-Ray Emission of the Andromeda Galaxy M31
Authors: Yi Xing, Zhongxiang Wang, Dong Zheng, Jie Li
Figure caption: TS maps for the region of M31 in the energy ranges of 0.1–500 GeV (left panel) and 2–500 GeV (right panel). The image scale of each TS map is 0.°05 pixel−1, for which a color bar is drawn to indicate the TS value range. Also in each TS map, a white ellipse is plotted to show the M31 disk/halo boundary defined in Racine (1991) and green pluses to show the 4FGL-DR3 catalog sources, which include M31 (the center one in the ellipse). Left: a cyan cross and circle mark the best-fit uniform-brightness disk model given in Ackermann et al. (2017), and a black cross and circle the best-fit disk model we determined (note the black cross is fixed at the central position of M31 given in SIMBAD database; see Section 2.3). Right: a white cross and dashed circle mark the position and 2σ error circle respectively we determined for the M31 central emission, and a black dashed circle marks the 2σ error circle for the SE source. In addition, the position of M32 is marked by a green cross.
Paper: On the Gamma-Ray Emission of the Andromeda Galaxy M31
Authors: Yi Xing, Zhongxiang Wang, Dong Zheng, Jie Li
Figure caption:  γ-ray spectra of the central M31 and SE sources (black diamonds and red dots respectively), along which the flux upper limits are shown as the open symbols. The best-fit models for the two sources, the LP for the M31 central one and PL for the SE one, are shown as the black curve and red line respectively. For comparison, the model spectrum of our Galactic center source (4FGL J1745.6−2859) given in Abdollahi et al. (2022) is scaled by the distance ratio (8 kpc/780 kpc)2 and shown as a blue dashed curve.
Paper: Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE
Authors: Robert A. Fesen, Bradley E. Schaefer, Dana Patchick
Figure caption: Pair of [S II] λ λ 6716,6731 images of Pa 30 showing central (left) and west (right) slit positions, along with the resulting 2D spectra covering the region around the [S II] emission doublet with wavelength increasing from left to right. Ordinary background stars have their continuum spectra visible as horizontal black lines, with the saturated spectrum of Pa 30's central star, J005311, appearing as an especially wide horizontal black line in the center slit spectrum.
Paper: Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE
Authors: Robert A. Fesen, Bradley E. Schaefer, Dana Patchick
Figure caption: Left: blowup of the middle region of the center slit spectrum showing [S II] λ λ 6716,6731 emissions, along with measured radial velocities. Wavelength increases from left to right. Right: spectra for four of the brightest emission knots detected in the center slit covering the [S II] doublet lines.
Paper: Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE
Authors: Robert A. Fesen, Bradley E. Schaefer, Dana Patchick
Figure caption: Comparison of WISE 12 and 22 μm images with our [S II] image of Pa 30. Red circles are 85″ in radius and centered on the hot star, J005311, whose position is marked by a white cross in the upper right panel. North is up; east is to the left.
Paper: Multipoint Turbulence Analysis with HelioSwarm
Authors: Francesco Pecora, Sergio Servidio, Leonardo Primavera, Antonella Greco, Yan Yang, William H. Matthaeus
Figure caption: (Top) Structure functions (strategy III) for (a) isotropic and (b) anisotropic simulations in the parallel–perpendicular increment plane. Dashed colored lines are directions along which 1D cuts are collected. The dotted line indicates the correlation length (of the isotropic case). (Bottom) PSDs obtained from 1D cuts compared with exact PSD obtained from simulation (dashed line), for isotropic (c) and anisotropic (d) cases.
Paper: Multipoint Turbulence Analysis with HelioSwarm
Authors: Francesco Pecora, Sergio Servidio, Leonardo Primavera, Antonella Greco, Yan Yang, William H. Matthaeus
Figure caption: (inset) Nine spacecraft (red spheres) provide 36 baselines (black lines) that correspond to 36 points in lag space (panel (a), spheres). Three possible tetrahedra are highlighted in colors. (b) Tetrahedron in lag space with the Yaglom flux vectors at its vertices pointing roughly toward the origin (black dot on the left). Arrow length is ∝∣ Y ∣.
Paper: Multipoint Turbulence Analysis with HelioSwarm
Authors: Francesco Pecora, Sergio Servidio, Leonardo Primavera, Antonella Greco, Yan Yang, William H. Matthaeus
Figure caption: (a) 3D view of the simulation domain. Shaded colors are regions where the magnetic field is more intense. The black oblique lines are the virtual spacecraft trajectories. (b) Zoomed-in view of a region of very strong magnetic field, where individual spacecraft trajectories can be distinguished.
Paper: Multipoint Turbulence Analysis with HelioSwarm
Authors: Francesco Pecora, Sergio Servidio, Leonardo Primavera, Antonella Greco, Yan Yang, William H. Matthaeus
Figure caption: (a) Nominal phase HelioSwarm trajectories projected in the ecliptic plane, with Earth indicated as a blue dot. (b) Interspacecraft separations. The vertical dashed line indicates one time at which HelioSwarm separations are measured and transferred in the simulations (see text).
Paper: Unified Picture of the Local Interstellar Magnetic Field from Voyager and IBEX
Authors: J. S. Rankin, D. J. McComas, E. J. Zirnstein, L. F. Burlaga, J. Heerikhuisen
Figure caption: Magnetic field data observed by Voyager 1 (black) from ∼2011.6 to ∼2022.0 compared to independently derived results from Zirnstein et al. (2016)'s data-driven model of the IBEX Ribbon (green). The model utilized a heliopause boundary condition of 122 ± 2 au in the Voyager 1 direction but no magnetic field data from Voyager. The red vertical line indicates the location of Voyager 1's heliopause crossing, which occurred at a radial distance of 121.6 au. Blue lines indicate shocks (“sh1” and “sh2”) and pressure fronts (“pf1” and “pf2”) identified by Burlaga et al. (2022). The magnetic field observations are plotted using publicly available data.                    Measurement uncertainties (dominated by systematic errors) are included in gray, as reported by the magnetometer team, with (constant) values of: err  B  r =±0.06 nT, err  B  t = ±0.02 nT, and err  B  n = ±0.02 nT. The uncertainty in ∣ B ∣ was not provided with the Voyager 1 data set, so the value shown here was calculated via standard error propagation from the other three components, which yields a typical uncertainty of err∣ B ∣ = ±0.024 nT.
Paper: Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Galaxy and a Revised Black Hole Mass
Authors: Emily R. Liepold, Chung-Pei Ma, Jonelle L. Walsh
Figure caption: (Left and Right) Stellar kinematic portraits of M87 from Keck KCWI spectra in 461 spatial bins. The line-of-sight velocities (left) and velocity dispersions (right) of stars in M87 are shown over a 250″ by 300″ field of view centered at the galaxy’s nucleus. The systemic velocity of M87 has been removed in the left panel. North is up and east is to the left. The two orthogonal white arrows indicate the orientations of the photometric major axis (PA of −25°) and minor axis (PA of −115°), as determined from the mean position angle of the galaxy’s major axis between a radius of 50″ and 250″ in photometric data (Kormendy et al. 2009). The red and blue lines in the left panel mark the measured kinematic axis (PA of −165°) outward of 70″ (see Figure 2). (Middle) HST composite image of the central 200″ by 200″ FOV of M87, illustrating the misalignment of the photometric major axis (yellow) and kinematic axis (red-blue) beyond 50″ along with sample isophotes of the stellar light distribution (yellow contours).
Paper: Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Galaxy and a Revised Black Hole Mass
Authors: Emily R. Liepold, Chung-Pei Ma, Jonelle L. Walsh
Figure caption: Line-of-sight stellar velocities as a function of projected radius and azimuthal angle on the sky. (Left) Line-of-sight velocity as a function of azimuthal angle on the sky for 11 radial shells spanning R = 15″–130″. The velocities in each shell (red data points) are well fit (blue) by a sinusoidal function of the form ﹩V(R,{\rm{\Theta }})={V}_{1}(R)\cos \left[{\rm{\Theta }}-{{\rm{\Theta }}}_{0}(R)\right]﹩. (Upper right) The amplitude of rotation, V 1(R), increases with radius and reaches 25 km s−1 around 6 kpc. (Lower right) The phase of the velocity function, Θ0, measures the orientation of the kinematic axis and varies significantly with radius. It plateaus to −165° beyond 6 kpc, indicating a 40° misalignment between the kinematic axis and the photometric major axis (red dashed curves; Kormendy et al. 2009) in M87.
Paper: Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Galaxy and a Revised Black Hole Mass
Authors: Emily R. Liepold, Chung-Pei Ma, Jonelle L. Walsh
Figure caption: Representative KCWI spectra of M87. Sky-subtracted galaxy spectra (black curves) for ten representative spatial bins located at projected radii from 1″ to 130″ are shown. A total of 461 binned spectra are used in this work. The S/N of these coadded spectra range from about 100 to 200 per Å. The stellar template broadened by the best-fit LOSVD is overlaid (red curves) on each spectrum. Typical fitting residuals are comparable to the line widths. Shaded blue regions indicate masked spectral regions excluded from the analysis. At M87's redshift, the Mg I b region is contaminated by the 5200 Å [N I] skyline (marked). The central bins exhibit strong AGN emission lines, especially from [O III] (4959 Å and 5007 Å), [S II] (4069 Å and 4076 Å), Hβ (4861 Å), and Hγ (4330 Å).
Paper: Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Galaxy and a Revised Black Hole Mass
Authors: Emily R. Liepold, Chung-Pei Ma, Jonelle L. Walsh
Figure caption: Posterior distributions of six parameters from triaxial Schwarzschild orbit modeling of M87: black hole mass M BH, outer stellar mass-to-light ratio M*/L, dark matter fraction enclosed within 10 kpc f 10, and shape parameters T, T maj, and T min. The posterior distributions of the luminosity-averaged axis ratios u, p, and q are shown in the upper right. The three levels of purple shading bound the 1σ, 2σ, and 3σ regions (68%, 95%, and 99.7% confidence levels, respectively) of the parameters. The vertical lines in each one-dimensional distribution indicate the median and the corresponding three confidence levels.
Paper: Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Galaxy and a Revised Black Hole Mass
Authors: Emily R. Liepold, Chung-Pei Ma, Jonelle L. Walsh
Figure caption: Line-spread function of Keck KCWI with BL grating. We find the LSF of KCWI BL grating to be approximated well by a Gaussian function convolved with a top-hat function, as shown in Equation (A1). To measure the shape of the LSF, we simultaneously fit 31 lines of an FeAr lamp spectrum as described in Appendix A.2. Here, we plot a superposition of the nine most prominent of those lines. Black points mark the flux in the lamp spectrum around each line after normalizing for each line’s amplitude. Our best-fit LSF model (green) has a top-hat function of width Δ = 5.105 Å convolved with a Gaussian function of σ = 0.627 Å. A single Gaussian function, as is typically assumed, would provide a very poor fit to the KCWI LSF (red).
Paper: Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Galaxy and a Revised Black Hole Mass
Authors: Emily R. Liepold, Chung-Pei Ma, Jonelle L. Walsh
Figure caption: Radial profile of stellar velocity dispersion of M87 in the inner 10 kpc (on a linear scale; top) and out to 100 kpc (on a logarithmic scale; bottom). All 461 KCWI bins are shown (blue) but many overlap. (Top) The KCWI values within 1 kpc agree well with those from MUSE on the Very Large Telescope (Emsellem et al. 2014; Sarzi et al. 2018; yellow and orange, respectively), while the MUSE values are 10–20 km s−1 larger than KCWI between 1 and 3 kpc. At 4.5 kpc, our KCWI measurements match the single data point (red) from an independent KCWI observation (Forbes et al. 2020). The VIRUS-P values (Murphy et al. 2011; gray), which were used in the axisymmetric stellar-dynamical measurement of the M87 black hole (Gebhardt et al. 2011), are 30–50 km s−1 higher than all other measurements. Murphy et al. (2011) noted a similar offset between their values and earlier IFU measurements (Emsellem et al. 2004) in the inner 2 kpc. (Bottom) Red globular clusters have similar σ (red) as stars and appear to belong to M87's stellar halo (Zhang et al. 2015), whereas the intracluster component of planetary nebulae have sharply rising σ (Longobardi et al. 2018; green).
Paper: Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Galaxy and a Revised Black Hole Mass
Authors: Emily R. Liepold, Chung-Pei Ma, Jonelle L. Walsh
Figure caption: Radial profile of M*/L ratio used in this work. The logistic approximation (red) used in our modeling, given by Equation (1), is chosen to match the shape of the r-band M*/L (black) in Figure 11 of Sarzi et al. (2018). The inner M*/L is δ = 2.5 times the outer M*/L ratio, and the transition is centered around 10″. Our dynamical model prefers an outer V-band M*/L of ﹩{3.46}_{-0.06}^{+0.04}{M}_{\odot }/{L}_{\odot }﹩ and inner M*/L of ﹩{8.65}_{-0.15}^{+0.10}﹩                       M ⊙/L ⊙.
Paper: Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Galaxy and a Revised Black Hole Mass
Authors: Emily R. Liepold, Chung-Pei Ma, Jonelle L. Walsh
Figure caption: Radial profiles of the first eight moments of the stellar LOSVDs. The observed Keck KCWI moments (gray) are matched well by the moments predicted by the best-fit model (red) given by Table 1. The triaxial orbit models produce point-symmetric LOSVDs, so we have point-symmetrized the kinematic moments before fitting.
Paper: Gravitational Wave Source Populations: Disentangling an AGN Component
Authors: V. Gayathri, Daniel Wysocki, Y. Yang, Vera Delfavero, R. O'Shaughnessy, Z. Haiman, H. Tagawa, I. Bartos
Figure caption: The inferred merger rate vs. mass for PL+G+AGN and PL+G+ AGN model analyses. The solid, dashed, and dotted lines for AGN, G, and PL models components.
Paper: Gravitational Wave Source Populations: Disentangling an AGN Component
Authors: V. Gayathri, Daniel Wysocki, Y. Yang, Vera Delfavero, R. O'Shaughnessy, Z. Haiman, H. Tagawa, I. Bartos
Figure caption: The inferred merger rate vs. mass ratio for PL+AGN and PL+G+ AGN model analyses. The solid, dashed, and dotted lines for AGN, G, and PL models components.
Paper: Gravitational Wave Source Populations: Disentangling an AGN Component
Authors: V. Gayathri, Daniel Wysocki, Y. Yang, Vera Delfavero, R. O'Shaughnessy, Z. Haiman, H. Tagawa, I. Bartos
Figure caption: Graphical representations of the BBH population analysis in m 1 − m 2 − spin parameter. Top panel for the PL+G, the middle panel for the PL+AGN, and the bottom panel for the PL+G+AGN model.
Paper: Gravitational Wave Source Populations: Disentangling an AGN Component
Authors: V. Gayathri, Daniel Wysocki, Y. Yang, Vera Delfavero, R. O'Shaughnessy, Z. Haiman, H. Tagawa, I. Bartos
Figure caption: Parameter distributions for binary black holes formed in our AGN disk formation models; line color indicates the maximum natal BH mass. As expected, as the maximum mass increases, total (M) mass upper limits increase. Additionally, a higher BH maximum natal mass ﹩{m}_{\max }﹩ increases the relative frequency of asymmetric mergers, particularly highly asymmetric mergers with q < 1/10.
Paper: Crustal Magnetic Fields Do Not Lead to Large Magnetic-field Amplifications in Binary Neutron Star Mergers
Authors: Michail Chabanov, Samuel D. Tootle, Elias R. Most, Luciano Rezzolla
Figure caption: Left: evolution of the total magnetic energy E  B  for the HR full (blue solid line) and crust configurations (red solid line); dashed blue (red) lines refer to the LR full and crust configurations, respectively. Different shadings highlight the four stages of the evolution. The black dotted line shows a quadratic fit to full (HR) in the winding stage and is shifted downwards for better visualization. The quantity V denotes the reference volume of a sphere with a radius of 11 km. Right top row of right panel: the same as in the left panel but for t − t mer ≲ 2 ms. Right panel, bottom row: the same as the top row of the right panel but for the growth rate ﹩{\dot{E}}_{B}/{E}_{B}﹩.
Paper: Crustal Magnetic Fields Do Not Lead to Large Magnetic-field Amplifications in Binary Neutron Star Mergers
Authors: Michail Chabanov, Samuel D. Tootle, Elias R. Most, Luciano Rezzolla
Figure caption: Distributions on the (x, y) plane of the magnetic-field strength ∣B∣ from the HR simulations at four representative times. The top and bottom rows refer to the full and crust configurations, respectively.
Paper: Crustal Magnetic Fields Do Not Lead to Large Magnetic-field Amplifications in Binary Neutron Star Mergers
Authors: Michail Chabanov, Samuel D. Tootle, Elias R. Most, Luciano Rezzolla
Figure caption: Distributions on the (x, y) plane of the magnetic-field strength ∣B∣ (left column), of the density-weighted xy-component of the kinematic vorticity ﹩| \rho {\omega }_{\perp }^{{xy}}| ﹩ (middle column), and of the amplification source term s mag (right column) at t − t mer = 0.52 ms. The top and bottom rows refer to the full and crust configurations, respectively.
Paper: Crustal Magnetic Fields Do Not Lead to Large Magnetic-field Amplifications in Binary Neutron Star Mergers
Authors: Michail Chabanov, Samuel D. Tootle, Elias R. Most, Luciano Rezzolla
Figure caption: The first three columns from left are the same as in Figure 3, while the fourth column reports the characteristic length scale of the magnetic field, i.e., ∣B∣/∣J∣, when expressed in units of resolution spacing Δx.