adsabs/AstroCLIMB huggingface dataset:
Paper: The NANOGrav 15 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Bence Bécsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Robin Case, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Megan E. DeCesar, Paul B. Demorest, Matthew C. Digman, Timothy Dolch, Brendan Drachler, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Rutger van Haasteren, Sarah J. Vigeland, Haley M. Wahl, Caitlin A. Witt, Olivia Young
Figure caption: Bayes factors between different combinations of CURN, HD, and CW models. CW here refers to an individual binary with frequencies between 4 nHz and 4.6 nHz, the frequency bin where the significance of the low-frequency candidate peaks (see Figure 1). The two different values on the diagonal correspond to two different ways of calculating that Bayes factor (going through the CURN+CW or the HD model) and serves as a consistency check.
Paper: The NANOGrav 15 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Bence Bécsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Robin Case, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Megan E. DeCesar, Paul B. Demorest, Matthew C. Digman, Timothy Dolch, Brendan Drachler, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Rutger van Haasteren, Sarah J. Vigeland, Haley M. Wahl, Caitlin A. Witt, Olivia Young
Figure caption: Distribution of model parameters for the low-frequency candidate at 4 nHz before (black) and after (orange) resampling to take HD correlations into account. Green lines show the prior distributions for each parameter. Note that after resampling, the peak in the amplitude posterior disappears and all other parameters follow their prior distributions, thus no longer showing support for the candidate signal.
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Whitened, band-averaged timing residuals for the PPTA-DR3. The 10, 20, and 40 cm wave bands are shown in blue, green, and orange, respectively. We show the weighted rms of the whitened residuals in the 20 cm band beneath each pulsar label.
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Marginal posterior probability distributions for the measured logarithmic amplitude (﹩{\mathrm{log}}_{10}{A}^{\mathrm{CRN}}﹩) and spectral index (γ) of a common uncorrelated process, along with the logarithmic amplitude of an HD-correlated fixed spectral index (γ = 13/3) common process, under basic (orange) and advanced (blue) noise models. The single-parameter marginal distributions are shown with logarithmic y-axes, to highlight the low-density tails of the distributions.
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Marginal posterior probability distributions for the measured logarithmic amplitude and spectral index of a common uncorrelated process under basic (orange) and advanced (blue) noise models. The contours on the two-dimensional distribution show the 1σ, 2σ, and 3σ credible intervals for each model.
Paper: End-to-end Kilonova Models of Neutron Star Mergers with Delayed Black Hole Formation
Authors: O. Just, V. Vijayan, Z. Xiong, S. Goriely, T. Soultanis, A. Bauswein, J. Guilet, H.-Th. Janka, G. Martínez-Pinedo
Figure caption: Mass vs. Y  e  histograms for models sym-n1-a6, sym-n10-a3, and asy-n1-a6 (panels (a)–(c)) and the corresponding mass fractions of synthesized elements vs. atomic mass number using nuclear network A (panels (d)–(f)) for each ejecta component and the total ejecta (see labels). The third row shows, for model sym-n1-a6, yields vs. atomic mass number (panel (g)) and elemental abundances (panel (h)) obtained with network B, as well as the specific radioactive heating rate for the indicated ejecta components and networks. All yields are shown for a time (typically about 100 Myr) when all elements, except the three longest-lived Th and U isotopes, have decayed into stable nuclei. Black circles in panels (d)–(h) show solar r-process yields (Goriely 1999) scaled to the predicted total yields of Sr, the only confirmed element in AT 2017gfo (Watson et al. 2019; Domoto et al. 2021; Gillanders et al. 2022). Orange triangles in panel (h) denote abundances observed for the metal-poor star HD 222925 (Roederer et al. 2022) scaled to match the solar Eu abundance. The gray dotted line in panel (i) shows the heating rate ﹩{10}^{10}\times {({t}_{\mathrm{pm}}/1\,\mathrm{days})}^{-1.3}﹩ erg g−1 s−1 for reference.
Paper: End-to-end Kilonova Models of Neutron Star Mergers with Delayed Black Hole Formation
Authors: O. Just, V. Vijayan, Z. Xiong, S. Goriely, T. Soultanis, A. Bauswein, J. Guilet, H.-Th. Janka, G. Martínez-Pinedo
Figure caption: Differential mass of lanthanides and actinides per solid angle along the polar angle (panels (a) and (b)); bolometric, isotropic-equivalent luminosity and effective (i.e., including thermalization as in Rosswog et al. 2017) heating rate (panels (c) and (d)); photospheric temperature (panels (e) and (f)); and photospheric velocities (panels (g) and (h)). The left (right) column shows plots for all models based on the symmetric (asymmetric) binary mass configuration. The bottom three rows share the same x-axis, and solid (dashed) lines denote quantities averaged over the entire sphere (over solid angles with θ < π/4), while black circles denote data observed in AT 2017gfo (from Waxman et al. 2018). The crosses in panels (c) and (d) denote peak emission properties obtained from one-zone estimates (Metzger 2019) using the mass, average velocity, and average opacity of all NS torus ejecta with Y  e  > 0.3. Nucleosynthesis-related properties were obtained from network A.
Paper: End-to-end Kilonova Models of Neutron Star Mergers with Delayed Black Hole Formation
Authors: O. Just, V. Vijayan, Z. Xiong, S. Goriely, T. Soultanis, A. Bauswein, J. Guilet, H.-Th. Janka, G. Martínez-Pinedo
Figure caption: Angular momentum (top) and specific angular momentum (bottom) as functions of postmerger time for different binary mass ratios q, normalized by the corresponding values of the q = 1 case, for simulations performed with our SPH code (left) and the ET (right). Solid lines only take into account NS material (i.e., regions where the density ρ > 1012  g cm−3), and dashed lines account for all matter in the integrals of Equation (B1a). Note that since dJ/dt < 0 at all plotted times, values of J(q)/J(q = 1) greater (smaller) than unity indicate a slower (faster) decline of J for a given q < 1 compared to the q = 1 case.
Paper: End-to-end Kilonova Models of Neutron Star Mergers with Delayed Black Hole Formation
Authors: O. Just, V. Vijayan, Z. Xiong, S. Goriely, T. Soultanis, A. Bauswein, J. Guilet, H.-Th. Janka, G. Martínez-Pinedo
Figure caption: The Y  e  histograms (top row) and nucleosynthesis yields (bottom row) of the dynamical ejecta in our end-to-end models (which combine data from 3D SPH and 2D grid simulations) compared to the corresponding properties for just the SPH simulations (black lines) for all models based on the symmetric (left column) and asymmetric (right column) binary mass configurations.
Paper: End-to-end Kilonova Models of Neutron Star Mergers with Delayed Black Hole Formation
Authors: O. Just, V. Vijayan, Z. Xiong, S. Goriely, T. Soultanis, A. Bauswein, J. Guilet, H.-Th. Janka, G. Martínez-Pinedo
Figure caption: Left panel: mass of material with radii r > 3000  km and velocities v/c > 0.1 as a function of time compared between model sym-n1-a6 and a corresponding model without neutrino pair annihilation, as well as another model where net neutrino heating is neglected entirely. Note that m(t) saturates significantly later than the time of BH formation (t BH ≈ 122  ms) because of the time needed by the ejecta material to travel from the NS surface to r = 3000  km. Right panel: mass–velocity distribution measured for the same models and ejecta at t pm = 0.4  s.
Paper: End-to-end Kilonova Models of Neutron Star Mergers with Delayed Black Hole Formation
Authors: O. Just, V. Vijayan, Z. Xiong, S. Goriely, T. Soultanis, A. Bauswein, J. Guilet, H.-Th. Janka, G. Martínez-Pinedo
Figure caption: Angular velocity Ω = v  ϕ /R as a function of cylindrical radius ﹩R=r\sin \theta ﹩ along the equator at the postmerger times, t pm, indicated in the legends for the three models sym-n1-a6, sym-n10-a3, and asy-n1-a6. For each time, dotted vertical lines indicate the location of the NS surface, i.e., the radius where ρ = 1012  g cm−3. Dashed lines indicate the slope of profiles proportional to R −3/2.
Paper: End-to-end Kilonova Models of Neutron Star Mergers with Delayed Black Hole Formation
Authors: O. Just, V. Vijayan, Z. Xiong, S. Goriely, T. Soultanis, A. Bauswein, J. Guilet, H.-Th. Janka, G. Martínez-Pinedo
Figure caption: Isotropic-equivalent luminosities (left) and mean energies (right) as functions of polar angle for electron neutrinos (solid lines) and antineutrinos (dashed lines) resulting from different grid widths Δx of the uniform Cartesian grid on which the ILEAS neutrino scheme is solved in the SPH merger simulations.
Paper: Implications of Atmospheric Nondetections for Trappist-1 Inner Planets on Atmospheric Retention Prospects for Outer Planets
Authors: Joshua Krissansen-Totton
Figure caption: Schematic of the PACMAN geochemical evolution model. The redox budget, thermal-climate evolution, and volatile budget are modeled from postaccretion magma ocean (left) through to temperate geochemical cycling (right). Oxygen fluxes are shown by green arrows, energy fluxes by black arrows, carbon fluxes by orange arrows, and water fluxes by blue arrows; the loss of hydrogen to space effectively adds oxygen to the atmosphere. During the magma ocean phase, the radius of solidification begins at the core–mantle boundary and moves toward the surface as internal heat is dissipated. The rate at which this occurs is controlled by radiogenic and tidal heat production, convective heat flow from the mantle to the surface, and heat flow from the core. During the temperate phase, outgassing, weathering, and oxidation reactions control the exchange of volatiles between the atmosphere and the interior. Internal heat flow balances the difference between outgoing longwave radiation (OLR) and absorbed stellar radiation (ASR) throughout.
Paper: Implications of Atmospheric Nondetections for Trappist-1 Inner Planets on Atmospheric Retention Prospects for Outer Planets
Authors: Joshua Krissansen-Totton
Figure caption: JWST observations of an airless Trappist-1b do not substantially change the odds of e and f being airless. Probability distribution of the total surface volatile inventories of Trappist-1e and f. Cyan distributions represent previous PACMAN predictions from KTF22. Magenta distributions show updated results applying the constraints on stellar evolution, atmospheric escape, and atmosphere–surface interactions implied by an airless Trappist-1b; here, initial volatile inventories for all Trappist-1 planets are assumed to be independent. Black distributions show the same updated results, but the initial volatile inventories of e and f are sampled from the same initial volatile distributions that ensure an airless b and c. For both these endmember cases, the distribution of final surface pressures is minimally modified from the original predictions.
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Red-noise posterior probability distributions. Each pulsar with constrained red-noise spectral properties is shown with a colored contour of the maximum likelihood 68% credibility region. Additionally, the 90% (upper, one-sided) credible interval for PSR J1713−0747 is shown. The dotted line indicates γ = 13/3, corresponding to the expected spectral index of GWs produced by an ensemble of SMBHBs.
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Leakage of low-frequency (ν ≤ 960  MHz) band noise into achromatic red noise and γ = 13/3 red noise in PSR J1713+0747. Green contours show posteriors from our single-pulsar model runs with a γ = 13/3 process. Blue contours show the posteriors assuming a fixed-amplitude γ = 13/3 process corresponding to the recovered common-spectrum noise, from a pairwise correlation analysis (Reardon et al. 2023). Orange contours show posteriors with a single-pulsar noise model including a 13/3 process, without a low-frequency band-noise term in the model.
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Mean solar wind density at 1 au (﹩{n}_{e}^{\mathrm{SW}}﹩), as a function of ecliptic latitude for each pulsar. The violins represent the posterior probability density of ﹩{n}_{e}^{\mathrm{SW}}﹩, and the violin transparency is set by the width of the distribution of ﹩{n}_{e}^{\mathrm{SW}}﹩ for the corresponding pulsar. The dashed black horizontal line shows the fiducial value of ﹩{n}_{e}^{\mathrm{SW}}=4\,{\mathrm{cm}}^{-3}﹩ used when developing the initial timing model (Edwards et al. 2006). The solid vertical line highlights zero ecliptic latitude. While it is a reasonable description for pulsars with ∣ELAT∣ ≳ 15°, we observe excess electron density for pulsars at low ecliptic latitudes, consistent with annual variations dominated by the slow component of the solar wind (e.g., Porowski et al. 2022).
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Free-spectrum inference for single-pulsar achromatic red noise, for J1909−3744 (green violins) and J1713+0747 (gold violins). The black violins show the inferred free spectral model of the common noise detailed in our GW companion paper (Reardon et al. 2023). The violins represent the probability density of the free-spectrum parameter ρ, with broader segments of a violin corresponding to higher probability density (with a linear scale). The posteriors are unconstrained at f = 1/(1 yr) = 31.7 nHz because of degeneracy with the timing model parameters for the pulsar positions.
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Band-averaged timing residuals and noise model validation for PSR J1909−3744. Residuals from observations with radio wavelengths near 10, 20, and 40 cm are shown in blue, green, and orange, respectively. The top panel shows the timing residuals with all noise processes present. The second panel shows the residuals after subtracting the maximum likelihood realization of the DM Gaussian process. The third and fourth panels show the residuals with the maximum likelihood realizations of all noise processes subtracted. Additionally, the residuals in the fourth panel have been normalized by the uncertainties. The legends of the top three panels show the weighted rms residual for each band, while the bottom panel shows the ADS.
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: DM Gaussian process posterior probability distributions. Each pulsar with constrained spectral properties for DM variations is shown with a colored contour of the maximum likelihood 68% credibility region. The dotted line indicates γ = 8/3, corresponding to a uniform IISM of Kolmogorov turbulence. To aid visual clarity, we divide the pulsars across both panels by R.A.
Paper: Superheavy Elements in Kilonovae
Authors: Erika M. Holmbeck, Jennifer Barnes, Kelsey A. Lund, Trevor M. Sprouse, G. C. McLaughlin, Matthew R. Mumpower
Figure caption: The effect of superheavy elements on broadband light curves for the full FRDM (no superheavy elements) and HFB (with superheavy elements) under similar observational conditions (lines).
Paper: The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, Valentina Di Marco, George B. Hobbs, Agastya Kapur, Marcus E. Lower, Rami Mandow, Hannah Middleton, Matthew T. Miles, Axl F. Rogers, Jacob Askew, Matthew Bailes, N. D. Ramesh Bhat, Andrew Cameron, Matthew Kerr, Atharva Kulkarni, Richard N. Manchester, Rowina S. Nathan, Christopher J. Russell, Stefan Osłowski, Xing-Jiang Zhu
Figure caption: Factorized likelihood analysis for timing offset parameters t JUMP (MJD; top) and ﹩{\mathrm{log}}_{10}{A}_{\mathrm{JUMP}}﹩ (with A JUMP in seconds; bottom). We color the marginal posteriors for pulsars with positive support for the MJD 58925 timing offset and show the marginal posteriors for other pulsars in light gray. In the bottom panel, we have filtered ﹩{\mathrm{log}}_{10}{A}_{\mathrm{JUMP}}﹩ samples that coincide with the time span with positive support for the MJD 58925 timing offset.