adsabs/AstroCLIMB huggingface dataset:
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: Left: Spectral energy distributions of the GRB 211106A afterglow from radio (circles) to X-rays (crosses) spanning from 14.18 to 117 days, together with a best-fit (highest-likelihood) forward-shock ISM model (lines) at z = 1.0, including expected contribution from interstellar scintillation (shaded bands). Triangles indicate upper limits. We have interpolated the radio observations, where necessary, to the common times for each epoch using broken power-law fits to the ALMA/ATCA 5.5 GHz light curves. Upper limits are not interpolated. The X-ray spectra have been scaled to the times of the SEDs using a broken power-law fit to the X-ray light curve. The HST upper limits require A V ≳ 2.6 mag of extinction in the host galaxy. Right: corresponding light curves with (solid) and without (dashed) a jet break. The model reproduces all observations, except for the 18 GHz detection at 62.7 days, which is masked during modeling (open circle). The turnover in the mm-band light curve and the steep decline in the cm-band light curve at ≳62.7 days require a jet break at t jet ≈ 29 days (gray, vertical line), constraining the jet opening angle to θ jet ≈ 16°.
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: SEDs of the host galaxy of GRB 211106A in the R band (triangle), F814W, and F110W (squares), together with SED models from CIGALE at three redshifts (gray lines) with the model fluxes as green circles. The red R − F814W color suggests a redshift, z ≈ 1.
Paper: Galactic Winds and Bubbles from Nuclear Starburst Rings
Authors: Dustin D. Nguyen, Todd A. Thompson
Figure caption: 2D slices of density, temperature, velocity, and entropy at 20 Myr from simulation “B0.” The top row shows the ﹩\hat{x}-\hat{y}﹩ plane slice at z = 1.875 kpc, the middle row shows the ﹩\hat{x}-\hat{z}﹩ plane slice at y = 0 kpc, and the bottom row shows the ﹩\hat{x}-\hat{y}﹩ plane slice at z = 0 kpc. The starburst ring (bottom row) produces a multiphase outflow (middle row) where the hot phase is enveloped with a cooler phase (top row). The starburst ring model quickly reaches a steady state within the first few Myr after the initial transient passes. The simulation size is 10 × 10 × 15 kpc (﹩\hat{x}\times \hat{y}\times \hat{z}﹩). Both the top and bottom rows are 10 × 10 kpc, and the middle row is 10 × 15 kpc.
Paper: Galactic Winds and Bubbles from Nuclear Starburst Rings
Authors: Dustin D. Nguyen, Todd A. Thompson
Figure caption: Temperature and velocity slices for t = 0.5, 1.0, 1.5, 2.5, and 4.5 Myr, for simulations “A ⋆.” Before the wind reaches its final time-steady form, it has a bubble-like morphology. The emergent bubble from the ring hole is fast, with peak velocities of 4000 km s−1, compared to the 2000 km s−1 shock front from the unobstructed, outer-ring flow. The asymptotic velocity of the steady-state configuration is v ∞ ≃ 1300 km s−1. The high-velocity feature depends on the density of the surrounding medium, and the peak velocities are slower for a denser medium (see Appendix D). The dynamics appear consistent with expectations of a bubble driven by constant energy injection in a uniform-density medium (see Equation (D2)). We see that by 4.5 Myr the leading bubble becomes radiative and cools faster than the shock front. This cooling fast bubble would be brighter than the surrounding shock in X-ray. The initial background at t = 0 consists of a galactic halo-like hot gaseous background that gets blown out of the simulation domain within ≃8 Myr. Each panel is a slice through the ﹩\hat{x}-\hat{z}﹩ plane and is 10 × 15 kpc.
Paper: Galactic Winds and Bubbles from Nuclear Starburst Rings
Authors: Dustin D. Nguyen, Todd A. Thompson
Figure caption: 2D slices of density, temperature, velocity, and entropy at 20 Myr from simulation “B0 ⋆.” The top row shows the ﹩\hat{x}-\hat{y}﹩ plane slice at z = 1.875 kpc, the middle row shows the ﹩\hat{x}-\hat{z}﹩ plane slice at y = 0 kpc, and the bottom row shows the ﹩\hat{x}-\hat{y}﹩ plane slice at z = 0 kpc. The ring of star clusters (bottom row) produces a multiphase outflow (middle row) where the hot phase is enveloped with a cooler phase (top row). The simulation size is 10 × 10 × 15 kpc (﹩\hat{x}\times \hat{y}\times \hat{z}﹩). Both the top and bottom rows are 10 × 10 kpc, and the middle row is 10 × 15 kpc.
Paper: Galactic Winds and Bubbles from Nuclear Starburst Rings
Authors: Dustin D. Nguyen, Todd A. Thompson
Figure caption: 1D ﹩\hat{z}﹩ skewer (red lines), 1D ﹩\hat{x}﹩ skewer (blue lines), and the analytic solutions to the shocked gas temperature and asymptotic velocity in orange. The ﹩\hat{z}﹩ and ﹩\hat{x}﹩ skewers pass through the origin at x = y = 0 and y = z = 0, respectively. The ﹩\hat{z}﹩ skewer goes along the minor axis, in the direction of the hot collimated wind.
Paper: Galactic Winds and Bubbles from Nuclear Starburst Rings
Authors: Dustin D. Nguyen, Todd A. Thompson
Figure caption: Schematic of the nuclear starburst ring model. In this model, SNe inject energy and mass into a ring geometry, leading to a steady-state flow that has an initial temperature within the ring of ∼107 K, which accelerates to high velocity as it leaves the ring volume. For high mass loading, the wind emanating from the outer ring can become radiative and quickly cool to 104 K at the cooling radius, r cool (see Section 3). Within the ring hole, along the minor axis, the flow shocks on itself, thermalizing its kinetic energy and maintaining high temperature. As the hot flow emerges from the inner ring region, it is collimated by the surrounding cooler flow.
Paper: Galactic Winds and Bubbles from Nuclear Starburst Rings
Authors: Dustin D. Nguyen, Todd A. Thompson
Figure caption: 2D slices of density, temperature, velocity, and Mach number at 40 Myr for varied energy thermalization efficiencies within the starburst ring: β = 1.1, 0.6, and 0.2 (simulations “B5,” “B0,” and “B6” respectively, see Table 1). All models have the same ring geometry of R  A  = 0.025 kpc and R  C  = 1.0 kpc.
Paper: Galactic Winds and Bubbles from Nuclear Starburst Rings
Authors: Dustin D. Nguyen, Todd A. Thompson
Figure caption: 2D temperature slices of simulations “B0,” “B2,” “B3,” and “B4.” We see that the different ring geometries produce different outflow morphologies despite equivalent energy and mass injection rates α and β.
Paper: Galactic Winds and Bubbles from Nuclear Starburst Rings
Authors: Dustin D. Nguyen, Todd A. Thompson
Figure caption: The X-ray surface brightness projected along the ﹩\hat{y}﹩-direction, which represents an ideal edge-on view of the ring system at 20 Myr for simulations “A” and “A ⋆” (from Figures 2 and 4). The simulation size is 10 × 10 × 15 kpc (﹩\hat{x}\times \hat{y}\times \hat{z}﹩).
Paper: Observation of Magnetic Reconnection in a Region of Strong Turbulence
Authors: R. E. Ergun, N. Pathak, M. E. Usanova, Y. Qi, T. Vo, J. L. Burch, S. J. Schwartz, R. B. Torbert, N. Ahmadi, F. D. Wilder, A. Chasipis, D. L. Newman, J. E. Stawarz, M. Hesse, D. L. Turner, D. Gershman
Figure caption: A turbulent magnetic reconnection region in Earth’s magnetotail. (a)  B  at 64.5 ms resolution. (b)  B  detrended by 10 s. (c)  E  at 31.25 ms resolution. (d)  V  Ion at 4.5 s resolution. (e) N  e  at 30 ms resolution. (f) Ion flux from 70 to 600 keV. (g) Differential ion energy flux from 3 eV to 25 keV. (h) Electron flux from 60 to 500 keV. (i) Differential electron energy flux from 6 eV to 25 keV.
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: (a) Comparison of the mm-band afterglow of GRB 211106A (magenta stars) with all published 3 mm light curves of SGRBs colored by redshift. Events with no known redshift are in gray. Triangles denote 3σ upper limits. After GRB 170817A, our ALMA observations of GRB 211106A are the deepest obtained for any SGRB to date. (b) Millimeter-band luminosity vs. rest-frame time for GRB 211106A at two assumed redshifts, z = 0.5 (solid line) and z = 1.0 (dotted line), compared to SGRBs with available redshifts. The colors are the same as in the plot above. (c) The 6 cm (5.5 GHz) ATCA light curve of the afterglow of GRB 211106A (magenta stars). For comparison, we show the cm-band (5–10 GHz) light curves of the nine other radio-detected SGRBs as well as GRB 170817A (circles) colored by the host-galaxy redshift from yellow (low) to purple (high). Triangles denote 3σ upper limits, and SGRBs with no known redshift are in gray. (d) Radio luminosity of the 6 cm (5.5 GHz) ATCA light curve of the afterglow of GRB 211106A vs. rest-frame time for two redshifts: z = 0.5 (solid line) and z = 1.0 (dotted line). For comparison, we show the cm-band (5–10 GHz) radio luminosity of the nine other radio-detected SGRBs as well as GRB 170817A (circles). The colors are the same as in the plot above.
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: Left: background-subtracted γ-ray light curves of GRB 211106A in a common reference frame corrected for light-travel time effects in the canonical 50–300 keV range from Swift/BAT (top) and Fermi/GBM (middle; both at 96 ms resolution) and at E ≳ 70 keV from INTEGRAL/SPI-ACS (bottom) with 50 ms resolution. Right: the location of this event in the duration–hardness plane of Fermi GRBs (Bhat et al. 2016) colored by P short indicates GRB 211106A has a high (≈92%) likelihood of belonging to the SGRB population (Section 2.1). White lines in the color bar refer to the values of P short ≈ 0.92 and P short ≈ 0.72 for GRB 211106A and GRB 170817A, respectively (Section 2.1).
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: HST images of GRB 211106A from stacking all available epochs (top row) and difference imaging between epochs (bottom row). The ALMA position is coincident with a ≈25.7 mag optical counterpart, which has no detectable variability. (a) HST/F814W stack with the Swift/XRT 90% error circle, consistent with several potential matches. (b) HST/F110W stack with the Chandra (green, registered to HST; see Appendix C) and ALMA (black) 1σ error circles. Numbers indicate probabilities of chance coincidence of objects in the image with the ALMA afterglow. (c) Zoom into the F110W stack, showing the relative offset between the most likely host galaxy and the afterglow. (d) Difference image between the two observations (ep1 and ep3) taken in the F814W filter. (e) Difference image between the first (ep1) and third (ep3) observations in the F110W filter. (f) Difference image between the second (ep2) and third (ep3) observations in the F110W filter. No residual flux is detected in any difference image. Panels (a) and (b) are 10″ on a side and panels (c)–(f) are 2″ on a side. All panels are shown with the same color scale and are centered on the ALMA position, with north up and east to the left.
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: Correlations and marginalized posterior density from multiwavelength modeling of GRB 211106A at z = 1 (including IC/KN effects), with n 0 in cm−3, E K,iso in erg, t jet in days, and the opening angle (θ jet) in degrees. θ jet is derived from E K,iso, n 0, and t jet (Sari et al. 1999) and is not an independent free parameter. The contours enclose 39.3%, 86.4%, and 98.9% of the probability mass in each correlation plot (corresponding to 1σ, 2σ, and 3σ regions for two-dimensional Gaussian distributions), while the dashed lines in the histograms indicate the 15.9%, 50% (median), and 84.1% quantiles (corresponding to ± 1σ for one-dimensional Gaussian distributions). See Table 4 for a summary.
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: The X-ray luminosity (0.3–10.0 keV; unabsorbed (i.e., corrected for galactic and intrinsic absorption), observer frame) vs. rest-frame time for GRB 211106A at z = 0.5 and z = 1, compared with that of Swift/BAT LGRBs (red density) and SGRBs (blue circles) with known redshifts. GRB 211106A exhibits one of the most luminous X-ray afterglows of the SGRB population to date.
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: Discovery images of the radio and mm-band afterglow of GRB 211106A with ATCA at 5.5 GHz (left) and 9.0 GHz (center) at ≈14.18 days, and with ALMA at 97.5 GHz at ≈12.89 days after the burst. Ellipses in the top right represent the synthesized beam. The radio afterglow is clearly detected in each image. All images have the same display stretch and color scale, indicated by the color bar (in Jy) at the bottom.
Paper: Discovery of the First Known Asteroid Confined within the Orbit of Venus
Authors: Wing-Huen Ip, Frank J. Masci, Quanzhi Ye, Emily A. Kramer, George Helou, Thomas A. Prince, S. R. Kulkarni, Richard Dekany, Andrew Drake, Matthew J. Graham, Steven Groom, Russ R. Laher, Ashish A. Mahabal, Ben Rusholme
Figure caption: Orbital diagram showing the orbits of the asteroid ‘Ayló’chaxnim, Mercury, and Venus corresponding to the JPL Small-body Database solution in Table 2. The vertical lines connect points on the orbit to their projection in the Ecliptic Plane.
Paper: Discovery of the First Known Asteroid Confined within the Orbit of Venus
Authors: Wing-Huen Ip, Frank J. Masci, Quanzhi Ye, Emily A. Kramer, George Helou, Thomas A. Prince, S. R. Kulkarni, Richard Dekany, Andrew Drake, Matthew J. Graham, Steven Groom, Russ R. Laher, Ashish A. Mahabal, Ben Rusholme
Figure caption: Screen capture of the orbital solution for ‘Ayló’chaxnim presented by the JPL Small-body Database on June 30, 2022.
Paper: Multiple Channels for the Onset of Magnetism in Isolated White Dwarfs
Authors: Stefano Bagnulo, John D. Landstreet
Figure caption: In the upper panel, the black solid line shows the intensity profile of the magnetic Ap star HD 94660, normalized to its maximum (its scale is given on the right axis). The shape of the intensity is due to the star’s spectral energy distribution convolved with the transmission function of the atmosphere + telescope optics + instrument. The red solid line shows the V/I profile (in percent units, the scale is on the left-hand axis), and the blue solid line is the null profile offset by −2.25% for display purposes. The null profile is the difference between the V/I profiles measured from two different pairs of exposures and represents an experimental estimate of the noise. Photon-noise error bars are also shown centered around −2.25% and appear as a light-blue background. Spectral regions highlighted by green bars have been used to determine the 〈B  z 〉 value from the H Balmer lines. The two bottom panels show the best fit obtained by minimizing the expression of Equation (A2) using the V/I profiles (left panel) and the null profiles (right panel). Data were obtained with FORS2 using grism 1200B.
Paper: Multiple Channels for the Onset of Magnetism in Isolated White Dwarfs
Authors: Stefano Bagnulo, John D. Landstreet
Figure caption: Age–mass diagram using data obtained for all WDs of the local 20 pc volume and most of the WDs younger than 0.6 Gyr up to 40 pc from the Sun. Stellar parameters are obtained as explained in Appendix B and given in Table 2. Empty circles represent WDs in which no magnetic field was detected. Filled dots identify MWDs with fields below 1 MG; filled dots surrounded by one circle represent MWDs with field strength between 1 and 10 MG, filled dots surrounded by two circles represent MWDs with field strength between 10 and 100 MG, and filled dots surrounded by three circles represent MWDs with field strength ≥ 100 MG. Solid curves represent the onset of core crystallization; the red line refers to thin-hydrogen-layer models and the blue line to thick-hydrogen-layer models as provided by theoretical computations (Bédard et al. 2020). The vertical dotted line marks the age limit of the 40 pc survey; the horizonal dotted lines mark the mass boundaries discussed in the text.
Paper: Multiple Channels for the Onset of Magnetism in Isolated White Dwarfs
Authors: Stefano Bagnulo, John D. Landstreet
Figure caption: Top panels: magnetic and nonmagnetic WDs in an age–mass diagram, with age expressed in a linear scale. The meaning of the symbols is the same as in Figure 2. Bottom panels: the observed ratio between MWDs and the total number of WDs with M ≤ 0.75 M ⊙. The left panels refer to the cooling age, while in the right panels the age is counted from the onset of core crystallization (at time ﹩\tau ﹩                   c), which varies from star to star according to mass. Horizontal error bars represent the age bin in consideration; vertical error bars represent the uncertainty of the frequency of the occurrence of magnetic field in all WDs deduced from the ratio MWDs/WDs measured in our volume-limited survey.
Paper: Multiple Channels for the Onset of Magnetism in Isolated White Dwarfs
Authors: Stefano Bagnulo, John D. Landstreet
Figure caption: FORS2 observations of WD 1008−242 obtained with grism 300V. The black solid line shows the noncalibrated flux, normalized to its maximum value (scale on the right y-axis), and the red solid line is the circular polarization expressed in percent (scale on the left y-axis).
Paper: Multiple Channels for the Onset of Magnetism in Isolated White Dwarfs
Authors: Stefano Bagnulo, John D. Landstreet
Figure caption: Age distribution of a magnitude-limited sample (top panel) and a volume-limited sample (bottom panel) of similar size (∼1000 WDs). Cooling age was estimated using the mass and temperature from the most recent WD catalog of Gentile Fusillo et al. (2021) assuming that all stars are H rich and interpolating the age from the table of the Montreal group (Bédard et al. 2020) using the results for thick-hydrogen-layer models.
Paper: Discovery of the First Known Asteroid Confined within the Orbit of Venus
Authors: Wing-Huen Ip, Frank J. Masci, Quanzhi Ye, Emily A. Kramer, George Helou, Thomas A. Prince, S. R. Kulkarni, Richard Dekany, Andrew Drake, Matthew J. Graham, Steven Groom, Russ R. Laher, Ashish A. Mahabal, Ben Rusholme
Figure caption: Discovery images in ZTF data of ‘Ayló’chaxnim obtained on 2020 January 4 during the TS. The object of interest is circled in each exposure, and the arrow indicates the apparent direction of motion. The times and coordinates of the asteroid in each image are given in Table 1 in the order of left to right.
Paper: Multiple Channels for the Onset of Magnetism in Isolated White Dwarfs
Authors: Stefano Bagnulo, John D. Landstreet
Figure caption: Same as for Figure 4, for the weakly magnetic star WD 0232+525 = EGGR 314, observed with the blue arm of ISIS. Note the shorter range of the x-axis, with respect to Figure 4, due to the fact that the Balmer lines of the WD are much broader than those of the main-sequence Ap star HD 94660.
Paper: Discovery of a Premerger Shock in an Intercluster Filament in Abell 98
Authors: Arnab Sarkar, Scott Randall, Yuanyuan Su, Gabriella E. Alvarez, Craig Sarazin, Paul Nulsen, Elizabeth Blanton, William Forman, Christine Jones, Esra Bulbul, John Zuhone, Felipe Andrade-Santos, Ryan E. Johnson, Priyanka Chakraborty
Figure caption: Top left: similar to Figure 1, but zoomed in to A98N and smoothed with a σ = 2″ Gaussian. Green regions used for spectral analysis. Top right: GGM image of A98N with a σ = 16″ Gaussian kernel. White dashed curve shows the southern shock front. Middle left: surface brightness profile of A98N in the south direction with 1σ error bars. Inset figure shows the 3D density profile. Middle right: projected temperature; bottom left: 3D density; bottom right: pressure profiles of A98N in the south direction.
Paper: Discovery of a Premerger Shock in an Intercluster Filament in Abell 98
Authors: Arnab Sarkar, Scott Randall, Yuanyuan Su, Gabriella E. Alvarez, Craig Sarazin, Paul Nulsen, Elizabeth Blanton, William Forman, Christine Jones, Esra Bulbul, John Zuhone, Felipe Andrade-Santos, Ryan E. Johnson, Priyanka Chakraborty
Figure caption: Left: black shows the surface brightness profile across the bridge measured using Chandra. Red indicates the sum of the surface brightness profiles of the diffuse, extended emission extracted from the Suzaku observations. Blue represents the residual filament emission. Right: projected temperature profile across the bridge, measured with a 1-T model. Red and green shaded regions indicate the hot component and cool component temperatures, respectively, measured with a 2-T model.
Paper: Discovery of a Premerger Shock in an Intercluster Filament in Abell 98
Authors: Arnab Sarkar, Scott Randall, Yuanyuan Su, Gabriella E. Alvarez, Craig Sarazin, Paul Nulsen, Elizabeth Blanton, William Forman, Christine Jones, Esra Bulbul, John Zuhone, Felipe Andrade-Santos, Ryan E. Johnson, Priyanka Chakraborty
Figure caption: Chandra exposure-corrected and background-subtracted image of A98 in the 0.5–2 keV energy band. White and cyan regions are used for the analysis of the filament emission. Centers of A98N and A98S are marked in black.