adsabs/AstroCLIMB huggingface dataset:
Paper: The Kick Velocity Distribution of Isolated Neutron Stars
Authors: Paul Disberg, Ilya Mandel
Figure caption: CDFs of the distributions fitted to our data set: our lognormal fiducial kick distribution (Equation (5); black), a Maxwellian distribution (Equation (7); light teal), a double-Maxwellian distribution (Equation (9); teal), and a Weibull distribution (Equation (E1); purple), together with the distributions of A. P. Igoshev (2020; red), F. Verbunt et al. (2017; blue), and G. Hobbs et al. (2005; green). The orange line is our median bootstrapped distribution, and the light-orange region corresponds to the 95% confidence region (Figure 1). All distributions are normalized between 0 and 1000 km s−1.
Paper: The Kick Velocity Distribution of Isolated Neutron Stars
Authors: Paul Disberg, Ilya Mandel
Figure caption: Individual velocity distributions for each (parallax) pulsar in our sample, for the present-day velocity distributions (τc ≤ 10 Myr; top panel) and the kinematically constrained velocity distributions (τc > 10 Myr; bottom panel), shown in histograms with bins of 0.1. The distributions are rescaled based on their mode (i.e., vpeak). The dotted light-purple lines show the median 68% intervals for these two methods. The dashed purple lines show the impact of the isotropic projection to estimate line-of-sight velocity (see Equations (3) and (4)).
Paper: Waiting Time Distribution of Supra-arcade Downflows
Authors: Zichao Yang, Rui Liu
Figure caption: WTDs derived from the start time of SADs. The histograms are normalized to show the probability density and fitted with the MLE method for power-law (red), log-normal (green), and exponential (blue) functions. The fitting parameters are shown in Table 2.
Paper: The Kick Velocity Distribution of Isolated Neutron Stars
Authors: Paul Disberg, Ilya Mandel
Figure caption: Spin properties and ages of the pulsars in our sample, for pulsars that have parallax distance estimates (brown) and pulsars that only have a DM distance estimate (teal). Panel (a) shows the derivative of the spin period (﹩\dot{P}﹩) vs. the actual spin period (P), together with the “death line” (Equation (A1), dashed light-teal line). Panel (b) shows the distributions of the characteristic ages ﹩{\tau }_{\,{\rm{c}}\,}=1/2\cdot P/\dot{P}﹩. Both panels include lines that indicate values of τc equal to 3, 10, and 40 Myr (light-brown lines).
Paper: The Kick Velocity Distribution of Isolated Neutron Stars
Authors: Paul Disberg, Ilya Mandel
Figure caption: Distances and velocities of the pulsars in our sample, for parallax distances (brown), DM distances for pulsars with existing parallax estimates (i.e., DMπ; dashed teal), and DM distances for all pulsars (dotted purple), and for both young pulsars (dark) and all ages (light). Panels (a), (b), and (c) show the distributions of distances, observer-frame transverse velocities, and three-dimensional velocities, respectively.
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: Left: the neutrino flux from 106 M⊙ supermassive DSs that can seed SMBHs for different DM annihilation channels considering DM mass mχ = 100 GeV (dashed line) and 10 TeV (solid line), for reference cross section 〈σv〉 = 3 × 10−26. Measurements of atmospheric neutrino flux by Super-Kamiokande (E. Richard et al. 2016; circles) and IceCube (M. G. Aartsen et al. 2015, 2016; triangles) for electron neutrinos (gray) and muon neutrinos (black) are shown. The predicted combined muon and electron neutrino atmospheric flux from M. Honda et al. (2011; solid gray line) is also displayed. Right: DM annihilation cross sections for which the DS neutrino flux peak exceeds that of the atmospheric background for a selection of fSMSD and fν = 1/3. Line colors indicate where Super-Kamiokande (green) and IceCube (magenta) have leading sensitivity. The steep DS collapse model (thick lines) and gradual DS collapse model (thin lines), consistent with JWST candidate events, are shown. We assume that DSs grow to 1% of their host halo mass in Mh = 106–109 M⊙ halos, to an upper mass limit of MDS = 106 M⊙. Overlaid (shaded regions) are existing bounds from indirect DM detection searches in IceCube (R. Abbasi et al. 2023), Super-Kamiokande (K. Abe et al. 2020), and ANTARES (S. R. Gozzini 2021) derived assuming fν = 1. The thermal relic DM annihilation cross section (G. Steigman et al. 2012; gray dashed line) is displayed for reference.
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: Evolution of DS luminosity for different DM masses and annihilation channels. We assume a baryonic accretion rate of 0.1 M⊙ yr−1 in a 108 M⊙ halo until the DS reaches a mass of ∼106 M⊙. We consider that baryonic accretion stalls when the DS reaches approximately ∼1% of the host halo mass, resulting in a plateau corresponding to DS mass and luminosity being approximately constant until DM annihilation becomes inefficient and DS collapses.
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: Halo formation rate density d2n/dMhdt integrated over halo mass range. Shown are the integrated halo formation rate density we consider as a reference (green line), results extended to lighter halos (yellow line), and results extended to more massive halos (lavender line). Press–Schechter (P-S; solid lines) and Sheth–Tormen (S-T; dashed lines) halo formation are indicated.
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: Comparison of the DSNB and DS neutrino fluxes for 1 and 10 GeV DM annihilating to ﹩\nu \bar{\nu }﹩.
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: Differential neutrino spectra normalized to one neutrino for a range of DM masses from mχ = 10 GeV to 10 TeV for different DM annihilation channels. Spectra are taken from P. Ciafaloni et al. (2011) and M. Cirelli et al. (2011)
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: DS photosphere radius for DM annihilation channel ﹩\nu \bar{\nu }﹩ for different masses considering that the fraction of DM mass mχ converted to neutrino energy is fν = 1/3.
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: Same as Figure 2, but considering the gradual DS collapse model with fsur given by Equation (B2).
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: Extragalactic neutrino flux from 10 TeV DM annihilating in DSs (pink/solid) assuming that DSs reach 1% of their host halo mass, which is in the range Mh = 106–109 M⊙ compared to the expected neutrino flux from conventional DM halos (purple/dashed) from C. A. Argüelles et al. (2021).
Paper: Diffuse Neutrino Signals from Dark Stars Seeding Supermassive Black Holes
Authors: Thomas Schwemberger, Volodymyr Takhistov
Figure caption: Same as Figure 2, but for DM annihilation to W+W− (top left), ﹩b\bar{b}﹩ (top right), and μ+μ− (bottom). Existing bounds from indirect DM detection searches by HAWC (A. Albert et al. 2023), Fermi-LAT (M. Ackermann et al. 2015), AMS (M. Aguilar et al. 2014; L. Accardo et al. 2014), Planck (N. Aghanim et al. 2020), and HESS (H. Abdallah et al. 2016) are shown as shaded regions.
Paper: James Webb Space Telescope Observations of the Nearby and Precisely Localized FRB 20250316A: A Potential Near-IR Counterpart and Implications for the Progenitors of Fast Radio Bursts
Authors: Peter K. Blanchard, Edo Berger, Shion E. Andrew, Aswin Suresh, Kohki Uno, Charles D. Kilpatrick, Brian D. Metzger, Harsh Kumar, Navin Sridhar, Amanda M. Cook, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Wen-fai Fong, Walter W. Golay, Daichi Hiramatsu, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Kenzie Nimmo, Aaron B. Pearlman, Vishwangi Shah, Kaitlyn Shin, Sunil Simha
Figure caption: CMD of stellar sources within a radius of 3″ (570 pc) of the location of FRB 20250316A. The data points are sized by projected distance to FRB 20250316A (larger for closer sources). Stars that appear spatially coincident with the nearby H II region are shown as orange points. Left: comparison to MIST evolutionary tracks for several initial masses: 1, 5, 10, 20 M⊙. On each track, thick gray shading indicates the RGB; thick orange shading on the 20 M⊙ track indicates the main sequence. The location of NIR-1 on the CMD is shown as the horizontal blue bar and is consistent with a ∼1–10 M⊙ red giant, a ∼1–5 M⊙ post-AGB star, or a massive ≳20 M⊙ main-sequence star. Right: comparison to isochrones for several stellar population ages: 0.01, 0.1, 1, 10 Gyr. We find that the stellar population near the location of FRB 20250316A contains both young (∼10–100 Myr) and old (∼1–10 Gyr) stars. If the actual FRB counterpart (e.g., isolated magnetar) remains undetected in our JWST data, it is possible that it originated in the younger population, which is dominated by stars in the nearby H II region. We note that NIR-2 is also consistent with this young population and may indicate that the young population overlaps the location of FRB 20250316A.
Paper: James Webb Space Telescope Observations of the Nearby and Precisely Localized FRB 20250316A: A Potential Near-IR Counterpart and Implications for the Progenitors of Fast Radio Bursts
Authors: Peter K. Blanchard, Edo Berger, Shion E. Andrew, Aswin Suresh, Kohki Uno, Charles D. Kilpatrick, Brian D. Metzger, Harsh Kumar, Navin Sridhar, Amanda M. Cook, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Wen-fai Fong, Walter W. Golay, Daichi Hiramatsu, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Kenzie Nimmo, Aaron B. Pearlman, Vishwangi Shah, Kaitlyn Shin, Sunil Simha
Figure caption: Top left: our JWST/NIRCam F150W2 image of NGC 4141, the host galaxy of FRB 20250316A, zoomed in to highlight the large-scale structure of the galaxy. Top right: zoomed-in region corresponding to the box in the top left panel showing the 1σ, 2σ, and 3σ localization regions of FRB 20250316A in relation to the surrounding resolved stellar population, including a nearby H II region, which is resolved into individual stars and a faint diffuse background. Bottom: further zoom-in on the location of FRB 20250316A, revealing a single faint source, NIR-1, near the center of the FRB localization region in the F150W2 image (left); the only other detected sources are on the edge of the 3σ region (marked NIR-2 to NIR-5). NIR-1 is not clearly identified in the lower-resolution F322W2 image (right). The images are aligned with north up and east to the left.
Paper: James Webb Space Telescope Observations of the Nearby and Precisely Localized FRB 20250316A: A Potential Near-IR Counterpart and Implications for the Progenitors of Fast Radio Bursts
Authors: Peter K. Blanchard, Edo Berger, Shion E. Andrew, Aswin Suresh, Kohki Uno, Charles D. Kilpatrick, Brian D. Metzger, Harsh Kumar, Navin Sridhar, Amanda M. Cook, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Wen-fai Fong, Walter W. Golay, Daichi Hiramatsu, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Kenzie Nimmo, Aaron B. Pearlman, Vishwangi Shah, Kaitlyn Shin, Sunil Simha
Figure caption: K-band luminosity distributions of GCs (blue) and young clusters (green) in M31, as well as the approximate luminosity ranges of RSGs (red); stars on the RGB (orange), including the RGB “tip” and “clump”; and main-sequence O stars (cyan). The F150W2 absolute magnitude of NIR-1 (dashed vertical line) indicates that it is not a stellar cluster or an RSG and is instead consistent with the luminosities of red giants near the clump or the massive end of main-sequence O stars.
Paper: James Webb Space Telescope Observations of the Nearby and Precisely Localized FRB 20250316A: A Potential Near-IR Counterpart and Implications for the Progenitors of Fast Radio Bursts
Authors: Peter K. Blanchard, Edo Berger, Shion E. Andrew, Aswin Suresh, Kohki Uno, Charles D. Kilpatrick, Brian D. Metzger, Harsh Kumar, Navin Sridhar, Amanda M. Cook, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Wen-fai Fong, Walter W. Golay, Daichi Hiramatsu, Ronniy C. Joseph, Victoria M. Kaspi, Mattias Lazda, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Kenzie Nimmo, Aaron B. Pearlman, Vishwangi Shah, Kaitlyn Shin, Sunil Simha
Figure caption: H-R diagram of companion stars in binary systems with mass transfer onto a compact object, based on binary population synthesis models, color-coded by volumetric rate (K. Uno et al. 2025, in preparation). The main panel shows the entire population, while the top panels separate the population into stable mass-transfer (left; RLOF) and unstable mass-transfer (right; CE) systems. In the main panel we highlight the locations of NIR-1 (solid contour) and NIR-2 (dashed contour); dotted lines show fixed blackbody radii. The blue shading marks the region ruled out, as it leads to counterparts brighter than NIR-1.
Paper: The Kick Velocity Distribution of Isolated Neutron Stars
Authors: Paul Disberg, Ilya Mandel
Figure caption: Kick estimates for our pulsar sample, for parallax distances (left column) and DM distances (right column). The top row shows the distributions of the most likely present-day velocities (vpd) of all pulsars younger than 3 Myr (light brown) and younger than 10 Myr (dark brown), in histograms with bins of 50 km s−1. The dashed black line in all panels is the fiducial kick distribution resulting from a lognormal fit (Equation (5), μ = 5.60 and σ = 0.68) to the vpd distribution based on parallax distances for τc ≤ 10 Myr. The middle row shows a histogram of the most likely values of the kinematically constrained kicks vkc for pulsars with ages between 10 and 40 Myr (dark teal) and pulsars older than 40 Myr (light teal). In all panels, the dotted lines show the lognormal fits listed in Table 1, where the black dotted line corresponds to the fit for τc ≤ 40 Myr. The top two rows also display the number of pulsars in each subsample (N). The bottom row shows CDFs of the (median) vpd empirical distribution for τc ≤ 10 Myr (brown line) and the (median) vkc distribution for 10 < τc/Myr ≤ 40 (teal line). We estimated the 95% confidence intervals of these distributions by bootstrapping them (light-brown area and light-teal lines, respectively). The CDFs in the bottom panels are normalized between 0 and 1000 km s−1.
Paper: The Kick Velocity Distribution of Isolated Neutron Stars
Authors: Paul Disberg, Ilya Mandel
Figure caption: Velocity distributions for the pulsar samples of A. P. Igoshev (2020), F. Verbunt et al. (2017), and G. Hobbs et al. (2005). Panels (a), (b), and (c) show the total velocity distributions for ages below 3 Myr (light colors) and 10 Myr (dark colors), in histograms with bins of 50 km s−1. The dashed black lines show our fiducial kick distribution (Equation (6)). The dotted light-red, light-blue, and pink lines show the kick distributions of A. P. Igoshev (2020; for τc ≤ 3 Myr), F. Verbunt et al. (2017; for τc ≤ 10 Myr), and G. Hobbs et al. (2005; for τc ≤ 3 Myr), respectively. These panels also list the sample sizes (i.e., N) for the different samples. Panel (d) shows median CDFs of the velocity distributions for pulsars with τc ≤ 10 Myr (dark lines), as well as their 95% confidence intervals (light areas and lines), our fiducial kick distribution (black dashed line), and our fit for τc ≤ 40 Myr (black dotted line). The distributions in panel (d) are normalized between 0 and 1000 km s−1.
Paper: The Kick Velocity Distribution of Isolated Neutron Stars
Authors: Paul Disberg, Ilya Mandel
Figure caption: Analysis of the young (i.e., τc ≤ 3 Myr) pulsar sample of G. Hobbs et al. (2005). Panel (a) contains a histogram of the logarithms of (observer-frame) transverse velocities (﹩{\mathrm{log}}\,{v}_{t}﹩) in uniform logarithmic bins. This histogram is identical to the one of G. Hobbs et al. (2005, see their Figure 4(b)). Panel (b) shows our three-dimensional velocity estimates for the pulsars in their young sample, determined by assuming GC isotropy (Equation (3)), in a purple histogram with bins of 50 km s−1. The dashed black line shows our fiducial kick distribution, and the dotted light-purple line shows the Maxwellian fit of G. Hobbs et al. (2005) with σ = 265 km s−1.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: Localization of the active black hole. Left panel: comparison of the spatial profile of the [Ne III] line and the continuum emission along the LRIS slit. The [Ne III] line is unresolved at the LRIS resolution and coincides with the compact ∞ cen region in Figure 1. Middle panel: VLA 3 GHz map, with an FWHM beam of ﹩0\mathop{.}\limits^{^{\prime\prime} }77﹩. The strong radio source coincides with ∞ cen to ﹩\lesssim 0\mathop{.}\limits^{^{\prime\prime} }1﹩. Right panel: the object is also a strong X-ray source, with LX ≈ 1.5 × 1044 erg s−1. The number of detected photons is shown in the lower left corner of each Chandra pixel. The pixel containing the ∞ cen region has the highest number of photons. For clarity, pixels with ≤2 counts are not shown.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: EW map of the Hα + [N II] + [S II] line emission in the NIRCAM F150W filter, overplotted on the F277W (rest-frame J) image. The scale bar indicates the strength of the line emission, expressed as a fraction of the F150W continuum. The rest-frame EW is approximately EWrest ≈ f × 1350 Å, with f the continuum fraction. The strong emission line source associated with the black hole is embedded in an elongated ionized gas distribution with a roughly constant EW that is in between the two nuclei.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: The ∞ galaxy is interpreted as the aftermath of a nearly head-on collision between two face-on disk galaxies with massive, compact bulges. The bulges survived the collision, and the inner disk stars were swept up in outwardly expanding collisional rings around the bulges. The nearby galaxy II Hz 4 is the prototype for this kind of binary ring formation (R. Lynds & A. Toomre 1976). Compression and shocks in the colliding gas likely produced a dense gaseous remnant in between the nuclei, as has been observed in the bullet cluster on much larger scales. It is proposed that the black hole formed within this gas.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: The ∞ galaxy was observed three times with Keck/LRIS, with three different slit angles (see inset). The radial velocity of the low-ionization [O II] doublet is shown as a function of position along the slit, with the positive x-direction indicated by the arrows in the inset. There is a gradient of ±100 km s−1 that is symmetric with respect to the velocity of the highly ionized lines from the SMBH’s narrow-line region. Note that the velocity profile is heavily smoothed by the 1″ seeing of the observations. The intrinsic profile could be a step function, with each side moving at a constant velocity.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: Top: stellar population fit, using the eazy code, for ∞ NW. The implied stellar mass is 8 × 1010 M⊙. Note that the galaxy has strong 8 μm PAH emission, sampled in the F1800W MIRI band. Bottom: fit for ∞ SE. This galaxy has a mass of 1.8 × 1011 M⊙ and is mostly composed of evolved stellar populations. Both galaxies are dusty, with AV ∼ 2.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: The ∞ galaxy in the rest-frame ultraviolet. From left to right, images at progressively shorter wavelengths are shown. For reference, the inset shows the JWST F277W image (λrest = 1.3 μm). The location of the blue compact object that we associate with the black hole is indicated with a cross. It is bright in the Subaru B and CFHT u bands and likely dominates the GALEX NUV band.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: Main panel: possible geometry of the ∞ galaxy along the line of sight. Measured properties are indicated in red and derived properties in black. The orientation is set by the axis ratio of the rings, b/a ∼ 0.77. Top panel: projection onto the sky. The rings appear to be overlapping but are actually ∼15 kpc apart.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: Combined Keck/LRIS spectrum of the ∞ galaxy. The top panel shows the entire wavelength range, with a logarithmic y-axis to capture the large dynamic range of the emission lines. Zoomed views are on a linear scale. Black lines are observations, gray lines indicate the errors, and red lines are Gaussian emission line fits redshifted to z = 1.1403. For [Ne III] and Hγ, a second component was fit to model the outflow and broad component, respectively. The spectrum shows a high degree of ionization and resembles that of a narrow-line AGN.
Paper: The ∞ Galaxy: A Candidate Direct-collapse Supermassive Black Hole between Two Massive, Ringed Nuclei
Authors: Pieter van Dokkum, Gabriel Brammer, Josephine F. W. Baggen, Michael A. Keim, Priyamvada Natarajan, Imad Pasha
Figure caption: Left: JWST F150W image, containing both continuum and the Hα, N II, and S II emission lines. Second from left: continuum image, created by interpolating the F090W and F200W images. Second from right: emission line map, created by subtracting the continuum image from the F150W image. Right: EW map, a division of the emission line map by the continuum image.
Paper: CHIME/Fast Radio Burst Discovery of an Unusual Circularly Polarized Long-period Radio Transient with an Accelerating Spin Period
Authors: Fengqiu Adam Dong, Kaitlyn Shin, Casey Law, Mason Ng, Ingrid Stairs, Geoffrey Bower, Alyssa Cassity, Emmanuel Fonseca, B. M. Gaensler, Jason W. T. Hessels, Victoria M. Kaspi, Bikash Kharel, Calvin Leung, Robert A. Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Obinna Modilim, Ayush Pandhi, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick Smith
Figure caption: Residuals for a 841 s period. The error bars are 1σ. The right panel shows a zoomed-in image of the densest portion of TOAs when all instruments were observing CHIME J1634+44. The arrows show offsets possibly due to timing noise between burst as discussed in the text.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)