adsabs/AstroCLIMB huggingface dataset:
Paper: The NANOGrav 12.5 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Harsha Blumer, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Siyuan Chen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Megan E. DeCesar, Paul B. Demorest, Timothy Dolch, Brendan Drachler, Justin A. Ellis, E. C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nathan Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Joey Shapiro 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, Dustin R. Madison, Alexander McEwen, Maura A. McLaughlin, Chiara M. F. Mingarelli, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena Siwek, Renée Spiewak, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Joseph K. Swiggum, Jessica Sydnor, Stephen R. Taylor, Jacob E. Turner, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Gregory Walsh, Caitlin A. Witt, Olivia Young
Figure caption: Savage–Dickey Bayes factors for a CW at each GW frequency. At low frequencies, inclusion of a CRN in the model (filled red) is necessary to avoid a false CW detection as in the CW-only model (open purple). Squares indicate a frequency where the initial analysis returned an undefined Savage–Dickey Bayes Factor, meaning that the zoom-in analysis was necessary to calculate an accurate Bayes factor. With these methods, we found that no CWs are detected in the 12.5 yr data set. Key frequencies are marked by vertical lines, including f yr (blue solid), ﹩{f}_{\max ,\mathrm{RN}}=30/{T}_{\mathrm{obs}}﹩ (black dotted), and ﹩{f}_{\max ,\mathrm{CRN}}=5/{T}_{\mathrm{obs}}﹩ (red dashed).
Paper: The NANOGrav 12.5 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Harsha Blumer, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Siyuan Chen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Megan E. DeCesar, Paul B. Demorest, Timothy Dolch, Brendan Drachler, Justin A. Ellis, E. C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nathan Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Joey Shapiro 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, Dustin R. Madison, Alexander McEwen, Maura A. McLaughlin, Chiara M. F. Mingarelli, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena Siwek, Renée Spiewak, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Joseph K. Swiggum, Jessica Sydnor, Stephen R. Taylor, Jacob E. Turner, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Gregory Walsh, Caitlin A. Witt, Olivia Young
Figure caption: The difference in strain upper limits for an equatorial slice of the sky map shown in Figure 5 plotted against ϕ (or RA). The results for the real data (red points) are well within the range of values encompassed by the standard deviation of 10 realizations simulated (blue), with near-identical mean values of Δh 95 (horizontal red and blue lines). Therefore, we conclude that the overall increase in upper limit across much of the sky at our most sensitive frequency is due to the 12.5 yr data set’s sensitivity to the CRN.
Paper: The NANOGrav 12.5 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Harsha Blumer, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Siyuan Chen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Megan E. DeCesar, Paul B. Demorest, Timothy Dolch, Brendan Drachler, Justin A. Ellis, E. C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nathan Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Joey Shapiro 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, Dustin R. Madison, Alexander McEwen, Maura A. McLaughlin, Chiara M. F. Mingarelli, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena Siwek, Renée Spiewak, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Joseph K. Swiggum, Jessica Sydnor, Stephen R. Taylor, Jacob E. Turner, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Gregory Walsh, Caitlin A. Witt, Olivia Young
Figure caption: The upper limits on CW strain are continuing to decrease. The 12.5 yr data set (red curve and error region) is more sensitive than the 11, 9, and 5 yr data sets (blue, orange, and green curves, respectively) at high frequencies. At the most sensitive frequency of f GW = 7.65 × 10−9 Hz, the CRN is impeding further sensitivity improvements, and upper limits are comparable between the 12.5 and 11 yr data sets. At frequencies greater than f yr, NANOGrav’s sensitivity has improved by a factor of 1.40 since the 11 yr data set.
Paper: The NANOGrav 12.5 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Harsha Blumer, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Siyuan Chen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Megan E. DeCesar, Paul B. Demorest, Timothy Dolch, Brendan Drachler, Justin A. Ellis, E. C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nathan Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Joey Shapiro 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, Dustin R. Madison, Alexander McEwen, Maura A. McLaughlin, Chiara M. F. Mingarelli, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena Siwek, Renée Spiewak, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Joseph K. Swiggum, Jessica Sydnor, Stephen R. Taylor, Jacob E. Turner, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Gregory Walsh, Caitlin A. Witt, Olivia Young
Figure caption: Difference in strain 95% upper limits for the 12.5 yr data set vs. the 11 yr data set at our most sensitive frequency. Blue pixels indicate a decrease in upper limit, while red pixels indicate an increase. The overall increase in upper limit across much of the sky at the most sensitive frequency was found to be due to the presence of the CRN and is consistent with the all-sky limit shown in Figure 3.
Paper: The NANOGrav 12.5 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Harsha Blumer, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Siyuan Chen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Megan E. DeCesar, Paul B. Demorest, Timothy Dolch, Brendan Drachler, Justin A. Ellis, E. C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nathan Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Joey Shapiro 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, Dustin R. Madison, Alexander McEwen, Maura A. McLaughlin, Chiara M. F. Mingarelli, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena Siwek, Renée Spiewak, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Joseph K. Swiggum, Jessica Sydnor, Stephen R. Taylor, Jacob E. Turner, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Gregory Walsh, Caitlin A. Witt, Olivia Young
Figure caption: All-sky CW strain 95% upper limits and associated error regions, with (red) and without (purple) a CRN included in the model. At low frequencies, modeling the CRN is necessary to avoid overestimating our strain upper limits. We are the least sensitive to CWs at f GW = 1/(1 yr) owing to Earth’s orbit, creating the large feature seen in this and other figures.
Paper: The NANOGrav 12.5 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Authors: Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Harsha Blumer, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Siyuan Chen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Megan E. DeCesar, Paul B. Demorest, Timothy Dolch, Brendan Drachler, Justin A. Ellis, E. C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nathan Garver-Daniels, Peter A. Gentile, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Joey Shapiro 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, Dustin R. Madison, Alexander McEwen, Maura A. McLaughlin, Chiara M. F. Mingarelli, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Nihan S. Pol, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena Siwek, Renée Spiewak, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Joseph K. Swiggum, Jessica Sydnor, Stephen R. Taylor, Jacob E. Turner, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Gregory Walsh, Caitlin A. Witt, Olivia Young
Figure caption: Map of CW strain 95% upper limits at f GW = 7.65 × 10−9 Hz, the most sensitive frequency searched, for the 12.5 yr data set. Pulsar locations are shown as white stars, with new pulsars added from the 12.5 yr data set outlined in red. The most sensitive pixel is marked with a red circle and is located at an R.A. of 19h07m30s and a decl. of ﹩-30^\circ 00^{\prime} 00^{\prime\prime} ﹩. In this region, where our best-timed pulsars lie, our upper limits are nearly an order of magnitude more sensitive than the least sensitive pixel.
Paper: Rejuvenating Star Formation Activity in an Early-type Dwarf Galaxy, LEDA 1915372, with Accreted H I Gas
Authors: Sanjaya Paudel, Suk-Jin Yoon, Omkar Bait, Chandreyee Sengupta, Woong-Bae G. Zee, Daya Nidhi Chhatkuli, Binod Adhikari, Binil Aryal
Figure caption: The HI velocity field from the GMRT low-resolution cube. The black contour traces the lowest column density contour of the low-resolution integrated HI image (N(HI) = 0.5 × 1020 cm−2). The white contours trace the optical g-band light at the surface brightness levels of 26 mag arsec−2. The solid blue line represents the position of the P–V slice (see Figure 8). The inset shows the integrated HI spectrum of LEDA 1915372 and MRK 0689. The vertical dashed line represents their respective optical velocities.
Paper: Rejuvenating Star Formation Activity in an Early-type Dwarf Galaxy, LEDA 1915372, with Accreted H I Gas
Authors: Sanjaya Paudel, Suk-Jin Yoon, Omkar Bait, Chandreyee Sengupta, Woong-Bae G. Zee, Daya Nidhi Chhatkuli, Binod Adhikari, Binil Aryal
Figure caption: P–V diagram along a line crossing the HI bridge and the two galaxies (see Figure 7) with a width of the slice of 56″. We produced the P–V diagram using CARTA v3.0.0.
Paper: Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, George B. Hobbs, Matthew Bailes, Valentina Di Marco, Agastya Kapur, Axl F. Rogers, Eric Thrane, Jacob Askew, N. D. Ramesh Bhat, Andrew Cameron, Małgorzata Curyło, William A. Coles, Shi Dai, Boris Goncharov, Matthew Kerr, Atharva Kulkarni, Yuri Levin, Marcus E. Lower, Richard N. Manchester, Rami Mandow, Matthew T. Miles, Rowina S. Nathan, Stefan Osłowski, Christopher J. Russell, Renée Spiewak, Songbo Zhang, Xing-Jiang Zhu
Figure caption: Posterior probability density violins for the uncorrelated common-spectrum noise amplitude as a function of time, using a 6 yr (top) and 9 yr (bottom) sliding window (slices) over the data set. The spectral index is fixed at −13/3. Slices with unconstrained (log) amplitude posteriors have been reweighted to have linear priors in ﹩{A}_{13/3}^{\mathrm{CRN}}﹩ (orange), and the 95% confidence upper limits are denoted with vertical arrows. Slices with constrained measurements of ﹩{\mathrm{log}}_{10}{A}_{13/3}^{\mathrm{CRN}}﹩ are colored in blue. For reference, the dashed horizontal line indicates the 1.2 × 10−15 upper limit set by our first 9 yr slice. The solid horizontal line and gray band indicate the measured ﹩{\mathrm{log}}_{10}{A}_{13/3}^{\mathrm{CRN}}﹩ of −14.69 and its 68% credible interval from our full PPTA-DR3 analysis. Here and elsewhere, the violins represent the probability density of a parameter, with broader segments of a violin corresponding to higher probability density.
Paper: Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, George B. Hobbs, Matthew Bailes, Valentina Di Marco, Agastya Kapur, Axl F. Rogers, Eric Thrane, Jacob Askew, N. D. Ramesh Bhat, Andrew Cameron, Małgorzata Curyło, William A. Coles, Shi Dai, Boris Goncharov, Matthew Kerr, Atharva Kulkarni, Yuri Levin, Marcus E. Lower, Richard N. Manchester, Rami Mandow, Matthew T. Miles, Rowina S. Nathan, Stefan Osłowski, Christopher J. Russell, Renée Spiewak, Songbo Zhang, Xing-Jiang Zhu
Figure caption: Statistics assessing the support for a noise process with γ = 13/3 for each pulsar in PPTA-DR3. Top: posterior probability density ratio for a γ = 13/3 process, at ﹩{\mathrm{log}}_{10}{A}_{13/3}=-14.69﹩, relative to ﹩{\mathrm{log}}_{10}{A}_{13/3}\lt -16.5﹩ (where the data are insensitive to a γ = 13/3 process) in blue, and the prior density in orange. Bottom: Savage–Dickey Bayes factor ﹩{ \mathcal B }﹩ for a γ = 13/3 process at any amplitude, which is also the ratio of the orange to blue points in the top panel. Filled and hollow circles correspond to prior range lower bounds on ﹩{\mathrm{log}}_{10}{A}_{13/3}﹩ of −20 and −18, respectively.
Paper: Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, George B. Hobbs, Matthew Bailes, Valentina Di Marco, Agastya Kapur, Axl F. Rogers, Eric Thrane, Jacob Askew, N. D. Ramesh Bhat, Andrew Cameron, Małgorzata Curyło, William A. Coles, Shi Dai, Boris Goncharov, Matthew Kerr, Atharva Kulkarni, Yuri Levin, Marcus E. Lower, Richard N. Manchester, Rami Mandow, Matthew T. Miles, Rowina S. Nathan, Stefan Osłowski, Christopher J. Russell, Renée Spiewak, Songbo Zhang, Xing-Jiang Zhu
Figure caption: Factorized-likelihood analysis on the ﹩{\mathrm{log}}_{10}{A}_{13/3}﹩ from the PPTA-DR3 pulsars. We highlight the three pulsars showing the highest (PSRs J1909−3744, J0437−4715, and J2145−0750) and lowest (PSRs J1744−1134, J1603−7202, and J1713+0747) consistency with the inferred common process with colored histograms. Other pulsars are presented as light-gray histograms. The prior density is shown with the green dashed line, and the total factorized-likelihood constraint for ﹩{\mathrm{log}}_{10}{A}_{13/3}^{\mathrm{CRN}}﹩ (the product of all other histograms) is shown by the black line.
Paper: Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, George B. Hobbs, Matthew Bailes, Valentina Di Marco, Agastya Kapur, Axl F. Rogers, Eric Thrane, Jacob Askew, N. D. Ramesh Bhat, Andrew Cameron, Małgorzata Curyło, William A. Coles, Shi Dai, Boris Goncharov, Matthew Kerr, Atharva Kulkarni, Yuri Levin, Marcus E. Lower, Richard N. Manchester, Rami Mandow, Matthew T. Miles, Rowina S. Nathan, Stefan Osłowski, Christopher J. Russell, Renée Spiewak, Songbo Zhang, Xing-Jiang Zhu
Figure caption: Free-spectrum common-noise inference for the PPTA-DR3. The violins show the probability density of the power spectral density for the free spectrum of a common-noise process (the width of the violin represents the probability density, with a linear scale). Solid green violins are from a factorized-likelihood analysis using the achromatic noise in single pulsars. Black violins are from a common free-spectrum inference assuming no cross correlations. Gold violins show the free spectrum of a common-noise process with Hellings–Downs cross correlations.
Paper: Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, George B. Hobbs, Matthew Bailes, Valentina Di Marco, Agastya Kapur, Axl F. Rogers, Eric Thrane, Jacob Askew, N. D. Ramesh Bhat, Andrew Cameron, Małgorzata Curyło, William A. Coles, Shi Dai, Boris Goncharov, Matthew Kerr, Atharva Kulkarni, Yuri Levin, Marcus E. Lower, Richard N. Manchester, Rami Mandow, Matthew T. Miles, Rowina S. Nathan, Stefan Osłowski, Christopher J. Russell, Renée Spiewak, Songbo Zhang, Xing-Jiang Zhu
Figure caption: Marginal posterior probability distributions for the measured logarithmic amplitude and spectral index (γ) of a common uncorrelated process assuming different solar system ephemerides (SSE). Using DE440 (green) we measure γ = 3.87 ± 0.36 and ﹩{\mathrm{log}}_{10}{A}^{\mathrm{CRN}}=-{14.50}_{-0.16}^{+0.14}﹩ (median and 68% credible interval; shaded regions in one-dimensional histograms). The contours on the two-dimensional marginal distribution show the 1σ, 2σ, and 3σ credible intervals for each of the SSEs.
Paper: Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array
Authors: Daniel J. Reardon, Andrew Zic, Ryan M. Shannon, George B. Hobbs, Matthew Bailes, Valentina Di Marco, Agastya Kapur, Axl F. Rogers, Eric Thrane, Jacob Askew, N. D. Ramesh Bhat, Andrew Cameron, Małgorzata Curyło, William A. Coles, Shi Dai, Boris Goncharov, Matthew Kerr, Atharva Kulkarni, Yuri Levin, Marcus E. Lower, Richard N. Manchester, Rami Mandow, Matthew T. Miles, Rowina S. Nathan, Stefan Osłowski, Christopher J. Russell, Renée Spiewak, Songbo Zhang, Xing-Jiang Zhu
Figure caption: Marginal posterior probability distributions for the logarithmic amplitude and spectral index (γ) of a common uncorrelated process, under our tailored single-pulsar priors (blue) and broader equal priors (orange).
Paper: The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background
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, Rand Burnette, Robin Case, Maria Charisi, Shami Chatterjee, Katerina Chatziioannou, Belinda D. Cheeseboro, Siyuan Chen, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Curt J. Cutler, Megan E. DeCesar, Dallas DeGan, Paul B. Demorest, Heling Deng, Timothy Dolch, Brendan Drachler, Justin A. Ellis, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Kristina Islo, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Tonia C. Klein, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Tyson B. Littenberg, Tingting Liu, Andrea Lommen, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Margaret A. Mattson, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Priyamvada Natarajan, 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, Levi Schult, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Jerry P. Sun, 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, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Empirical background distribution of HD  γ -to-CURN  γ  Bayes factor (left; see Section 3) and noise-marginalized optimal statistic (right; see Section 4), as computed by the phase-shift technique (Taylor et al. 2017) to remove interpulsar correlations. We only compute 5000 Bayesian phase shifts, compared to 400,000 optimal statistic phase shifts, because of the huge computational resources needed to perform the Bayesian analyses. For the optimal statistic, we also compute the background distribution using 27,000 simulations (orange line) and compare to an analytic calculation (green line). Dotted lines indicate Gaussian-equivalent 2σ, 3σ, and 4σ thresholds. The dashed vertical lines indicate the values of the detection statistics for the unshifted data sets. For the Bayesian analyses, we find p = 10−3 (≈3σ); for the optimal statistic analyses, we find p = 5 × 10−5 to 1.9 × 10−4 (≈3.5σ–4σ).