adsabs/AstroCLIMB huggingface dataset:
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: Global properties of the four models mentioned in the bottom right, namely, the maximum density (panel (a)), outflow mass fluxes through the sphere at r = 104  km and mass fluxes into the central BH once formed (panel (b)), ratio of the total neutrino luminosities to the volume-integrated viscous heating rate (panel (c)), masses of the NS and torus (panel (d)), angular momenta of the NS and torus (panel (e)), radii of the NS surface in the equatorial and polar directions (panel (f)), luminosities of electron-type neutrinos (panel (g)) and heavy-lepton neutrinos (panel (h)), neutrino mean energies (computed as the ratio of energy-to-number fluxes; panel (i)), mass-averaged radius of the torus (∫rdm/∫dm; panel (j)), and mass average of the torus electron fraction (∫Y  e  dm/∫dm) and its equilibrium value ﹩{Y}_{e}^{\mathrm{eq}}﹩ (panel (k)). The torus is defined as all material below r = 104  km having ρ < 1012  g cm−3, and the NS is defined as all material with ρ > 1012  g cm−3. All neutrino-related quantities are measured in the lab frame at r = 500  km by an observer at infinity. The neutrino fluxes vanish initially (at t pm ≲ t map = 10  ms) because the plot shows only data from the postmerger simulations (which are initialized at t map with vanishing neutrino fluxes).
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: Snapshots of model sym-n1-a6 at different postmerger times, t pm. Panels (a)–(d) show the density ρ, radial velocity v  r , electron fraction Y  e , and entropy per baryon s, as well as velocity arrows (left side) and contours of temperature T (right side). Panel (e) shows the mass fractions of lanthanides plus actinides, X LA, and of elements in the first, second, and third r-process peaks, overlaid with green lines denoting the time-dependent location of the radial photosphere (computed as in Just et al. 2022). Panel (f) shows a map color-coding the three main ejecta components, the opacity κ, and the effective radioactive heating rate Q heat. Panels (a)–(d) show data from both hemispheres, and panels (e) and (f) show data from just the northern hemisphere assuming equatorial symmetry.
Paper: Evidence for a Black Hole Spin–Orbit Misalignment in the X-Ray Binary Cyg X-1
Authors: Andrzej A. Zdziarski, Alexandra Veledina, Michał Szanecki, David A. Green, Joe S. Bright, David R. A. Williams
Figure caption: Image of the jet obtained with the VLBA/VLA observation (Stirling et al. 2001) on 1998 August 10 at 8.4 GHz. We show the projected position vectors of the orbit and the spin of the BH.
Paper: The Origin of Universality in the Inner Edges of Planetary Systems
Authors: Konstantin Batygin, Fred C. Adams, Juliette Becker
Figure caption: Census of well-characterized extrasolar planets (circles) and moons of gas (squares) and ice (triangles) giants of the solar system. The mass ratio of the planet or satellite to the central body (m/M) is shown as a function of the orbital period. The points are color-coded by the spectral type of the host (with P denoting a planetary central body). The top panel shows a histogram of the orbital period of the innermost planet or satellite in each system, similarly color-coded by the spectral type of the host star. A peak in the P ∼ 2–12 days range is evident within the distribution. A complementary view of the orbital distribution is provided in Figure A1.
Paper: The Origin of Universality in the Inner Edges of Planetary Systems
Authors: Konstantin Batygin, Fred C. Adams, Juliette Becker
Figure caption: Distribution of innermost orbital periods, sorted by host type. Unlike in Figure 1, here we do not restrict the dataset to systems with measured masses, yielding a somewhat distinct view of the galactic planetary census. The orbital periods of Jupiter’s moon Io and Saturn’s moon Titan are also shown for comparison. It is important to note that both bodies have experienced some degree of outward tidal migration. In the case of Titan, the work of Lainey et al. (2020) suggests that long-range tidal migration might have occurred. The distributions for M-, K-, G-, and F-type hosts appear quite similar. For A- and B-type hosts, there is a slight preference for lower periods. However, it is worth noting the planetary sample for these types of stars is different: while the fractions of planets with radii smaller than 4 Earth radii are 56%, 66%, 69%, and 45% for M-, K-, G-, and F-type stars, respectively, it is 14% and 0% for A- and B-type stars, illustrating the sample disparity.
Paper: The Origin of Universality in the Inner Edges of Planetary Systems
Authors: Konstantin Batygin, Fred C. Adams, Juliette Becker
Figure caption: A schematic diagram of the physical processes considered in this work. A central body of mass M ⋆ is encircled by a disk, which accretes at a rate ﹩\dot{M}﹩. Convective energy transport within the body drives gravitational contraction of its radius, R ⋆, as well as dynamo action, which generates a field, B ⋆, that is regulated by the bolometric flux, q. Magnetospheric interactions between the central body and the disk generate a cavity with an edge that corresponds to an orbital frequency, Ω.
Paper: TOI-1859b: A 64 Day Warm Jupiter on an Eccentric and Misaligned Orbit
Authors: Jiayin Dong, Songhu Wang, Malena Rice, George Zhou, Chelsea X. Huang, Rebekah I. Dawson, Gudmundur K. Stefánsson, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Sarah E. Logsdon, Ryan C. Terrien, Karen A. Collins, Gregor Srdoc, Ramotholo Sefako, Didier Laloum, David W. Latham, Allyson Bieryla, Paul A. Dalba, Diana Dragomir, Steven Villanueva, Steve B. Howell, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Avi Shporer, David Rapetti
Figure caption: TESS SPOC PDC_SAP light curves and ground-based transits of TOI-1859b. TOI-1859b transits are labeled in blue on TESS light curves in the left two panels. The median of the fitted transit model is plotted in blue on the two right panels. Two ground-based transits are shown in the lower right panel.
Paper: TOI-1859b: A 64 Day Warm Jupiter on an Eccentric and Misaligned Orbit
Authors: Jiayin Dong, Songhu Wang, Malena Rice, George Zhou, Chelsea X. Huang, Rebekah I. Dawson, Gudmundur K. Stefánsson, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Sarah E. Logsdon, Ryan C. Terrien, Karen A. Collins, Gregor Srdoc, Ramotholo Sefako, Didier Laloum, David W. Latham, Allyson Bieryla, Paul A. Dalba, Diana Dragomir, Steven Villanueva, Steve B. Howell, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Avi Shporer, David Rapetti
Figure caption: NEID spectra are reduced by three different data reduction techniques. Inferred projected stellar obliquities are consistent. (a) and (b) In-transit RV measurements of the TOI-1859 system using the NEID spectra. The blue dots and black bars are NEID RVs and their corresponding uncertainties. Using the RM effect, the projected stellar obliquity is constrained. (c) The Doppler Tomography signal of the TOI-1859 system during TOI-1859b’s transit. The left, middle, and right panels are data extracted from the NEID spectra, best-fit model, and the residual of the data after subtracting the best-fit model. The color scale presents the flux variation of the velocity channel.
Paper: TOI-1859b: A 64 Day Warm Jupiter on an Eccentric and Misaligned Orbit
Authors: Jiayin Dong, Songhu Wang, Malena Rice, George Zhou, Chelsea X. Huang, Rebekah I. Dawson, Gudmundur K. Stefánsson, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Sarah E. Logsdon, Ryan C. Terrien, Karen A. Collins, Gregor Srdoc, Ramotholo Sefako, Didier Laloum, David W. Latham, Allyson Bieryla, Paul A. Dalba, Diana Dragomir, Steven Villanueva, Steve B. Howell, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Avi Shporer, David Rapetti
Figure caption: Sky-projected stellar obliquity vs. the semimajor axis of all measured giant planets colored by their eccentricities. Eccentric orbits with median e > 0.2 are colored in orange, and circular orbits with e ≤ 0.2 are colored in blue. Literature data are extracted from Table A1 in Albrecht et al. (2022).
Paper: TOI-1859b: A 64 Day Warm Jupiter on an Eccentric and Misaligned Orbit
Authors: Jiayin Dong, Songhu Wang, Malena Rice, George Zhou, Chelsea X. Huang, Rebekah I. Dawson, Gudmundur K. Stefánsson, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Sarah E. Logsdon, Ryan C. Terrien, Karen A. Collins, Gregor Srdoc, Ramotholo Sefako, Didier Laloum, David W. Latham, Allyson Bieryla, Paul A. Dalba, Diana Dragomir, Steven Villanueva, Steve B. Howell, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Avi Shporer, David Rapetti
Figure caption: The SED analysis of TOI-1859. Each blue point corresponds to a photometric filter, and the x-axis error bar corresponds to the passband of the filter. The best-fitted SED model is shown in gray. The orange diamond shows the combined synthetic flux over each passband. The SED residuals normalized by the photometric uncertainties are shown in the lower panel.
Paper: TOI-1859b: A 64 Day Warm Jupiter on an Eccentric and Misaligned Orbit
Authors: Jiayin Dong, Songhu Wang, Malena Rice, George Zhou, Chelsea X. Huang, Rebekah I. Dawson, Gudmundur K. Stefánsson, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Sarah E. Logsdon, Ryan C. Terrien, Karen A. Collins, Gregor Srdoc, Ramotholo Sefako, Didier Laloum, David W. Latham, Allyson Bieryla, Paul A. Dalba, Diana Dragomir, Steven Villanueva, Steve B. Howell, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Avi Shporer, David Rapetti
Figure caption: Speckle imaging of TOI-1859 taken by the Gemini-North `Alopeke. Angular separations from 0.″1 to 1″ correspond to physical distances from 22.4 to 224 au. Companions are ruled out to a contrast of 6.36 mag at 0.″5 separation (or a physical distance of 112 au) in the 832 nm band (red curve and the inset image) and a contrast of 4.31 mag at 0.″5 separation in the 562 nm band (blue curve).
Paper: Investigating Possible Binarity for GJ 229B
Authors: Alex R. Howe, Avi M. Mandell, Michael W. McElwain
Figure caption: Comparison of the observed spectrum of GJ 229B (black) with best-fit binary spectra from the S-B model grid (blue) and our APOLLO forward model grid (gold), in the 71 M  J  case. Residuals for each fit are plotted on the same scale below the x-axis in green and red, respectively.
Paper: TOI-1859b: A 64 Day Warm Jupiter on an Eccentric and Misaligned Orbit
Authors: Jiayin Dong, Songhu Wang, Malena Rice, George Zhou, Chelsea X. Huang, Rebekah I. Dawson, Gudmundur K. Stefánsson, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Sarah E. Logsdon, Ryan C. Terrien, Karen A. Collins, Gregor Srdoc, Ramotholo Sefako, Didier Laloum, David W. Latham, Allyson Bieryla, Paul A. Dalba, Diana Dragomir, Steven Villanueva, Steve B. Howell, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Avi Shporer, David Rapetti
Figure caption: Individual TESS transits of TOI-1859b. The medians and 3σ uncertainties of the fitted transit model are plotted in blue lines and light blue contours, respectively.
Paper: TOI-1859b: A 64 Day Warm Jupiter on an Eccentric and Misaligned Orbit
Authors: Jiayin Dong, Songhu Wang, Malena Rice, George Zhou, Chelsea X. Huang, Rebekah I. Dawson, Gudmundur K. Stefánsson, Samuel Halverson, Shubham Kanodia, Suvrath Mahadevan, Michael W. McElwain, Jaime A. Alvarado-Montes, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Sarah E. Logsdon, Ryan C. Terrien, Karen A. Collins, Gregor Srdoc, Ramotholo Sefako, Didier Laloum, David W. Latham, Allyson Bieryla, Paul A. Dalba, Diana Dragomir, Steven Villanueva, Steve B. Howell, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Avi Shporer, David Rapetti
Figure caption: Corner plots of the posteriors of the inferred orbital parameters from the NEID-DRP RVs in black, SERVAL RVs in blue, and Doppler Tomography in orange.
Paper: The NANOGrav 15 yr Data Set: Observations and Timing of 68 Millisecond Pulsars
Authors: Gabriella Agazie, Md Faisal Alam, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Victoria Bonidie, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, Christopher Chapman, 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, 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, Ross J. Jennings, Cody Jessup, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Anastasia Kuske, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Ye Lin, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Kaleb Maraccini, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Elisa Panciu, Timothy T. Pennucci, Benetge B. P. Perera, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Laura Salo, Shashwat C. Sardesai, Carl Schmiedekamp, Ann 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, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Epochs of all TOAs in the data set. The observatory and observing frequency are indicated by color: Arecibo observations are red (327 MHz), orange (430 MHz), light blue (1.4 GHz), and purple (2.1 GHz); GBT observations are green (800 MHz) and dark blue (1.4 GHz); and VLA observations are brown (1.4 GHz) and pink (3 GHz). The Arecibo and GBT data acquisition systems are indicated by symbols: open circles are ASP or GASP, and closed circles are PUPPI or GUPPI. Only a single back end (YUPPI) was used at the VLA.
Paper: The NANOGrav 15 yr Data Set: Observations and Timing of 68 Millisecond Pulsars
Authors: Gabriella Agazie, Md Faisal Alam, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Victoria Bonidie, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, Christopher Chapman, 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, 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, Ross J. Jennings, Cody Jessup, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Anastasia Kuske, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Ye Lin, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Kaleb Maraccini, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Elisa Panciu, Timothy T. Pennucci, Benetge B. P. Perera, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Laura Salo, Shashwat C. Sardesai, Carl Schmiedekamp, Ann 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, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Grid of χ 2 as a function of inclination i and longitude of the ascending node Ω for PSR J1713+0747, computed with PINT. All other parameters were fit at each grid point. The values are in the DT92 (Damour & Taylor 1992) convention (see Appendix D). The color scale and contours are the logarithm of difference of χ 2 compared to the best-fit value, with an inset zooming in to the best-fit region. The magenta diamond is the value from the 12.5 yr data release (Alam et al. 2021a) converted from the IAU convention to DT92; these parameters will be slightly shifted owing to the choice of timing model. The cyan pentagon shows the value from Splaver et al. (2005) converted from the IAU convention to DT92 and additionally converted from equatorial to ecliptic coordinates. The green hexagon is the best fit when using equatorial coordinates, converted to ecliptic. The black square is the best fit when using ecliptic coordinates directly. Finally, the blue star is the minimum point in the χ 2 grid.
Paper: The NANOGrav 15 yr Data Set: Observations and Timing of 68 Millisecond Pulsars
Authors: Gabriella Agazie, Md Faisal Alam, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Victoria Bonidie, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, Christopher Chapman, 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, 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, Ross J. Jennings, Cody Jessup, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Anastasia Kuske, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Ye Lin, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Kaleb Maraccini, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Elisa Panciu, Timothy T. Pennucci, Benetge B. P. Perera, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Laura Salo, Shashwat C. Sardesai, Carl Schmiedekamp, Ann 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, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Comparisons of the two RN parameters (the spectral index γ red and log10 amplitude, ﹩{\mathrm{log}}_{10}{A}_{\mathrm{red}}﹩) between NG15 and NG12. Left: ﹩{\mathrm{log}}_{10}{A}_{\mathrm{red}}﹩ vs. γ red for NG15 (blue) and NG12 (orange) without error bars. Filled squares are values for pulsars whose RN was found to be significant and is included in the timing model. Crosses are the measured RN parameters for pulsars without significant RN. Middle and right panels: same as the left panel, but split into the NG15 values (middle) and NG12 values (right), including the 1σ confidence interval error bars. For crosses (insignificant RN) appearing in the “high-A red” group of points, the RN priors are the only information constraining those measurements, that is, the data provide no information about the RN content of those MSPs.
Paper: The NANOGrav 15 yr Data Set: Observations and Timing of 68 Millisecond Pulsars
Authors: Gabriella Agazie, Md Faisal Alam, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Laura Blecha, Victoria Bonidie, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Bence Bécsy, Christopher Chapman, 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, 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, Ross J. Jennings, Cody Jessup, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Anastasia Kuske, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Natalia Lewandowska, Ye Lin, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Kaleb Maraccini, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Elisa Panciu, Timothy T. Pennucci, Benetge B. P. Perera, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Laura Salo, Shashwat C. Sardesai, Carl Schmiedekamp, Ann 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, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, Olivia Young
Figure caption: Posterior probability distributions for pulsar mass m  p  for each NG15 binary with well-constrained traditional Shapiro delay parameters. Solid lines within the pdf curves indicate the median mass value, while the two dotted lines represent the 68.3% confidence interval. Orange curves were derived using NG12 measurements; blue curves are from the updated NG15 data set. Of the 14 Shapiro delay measurements common to NG12 and NG15, seven of the mean masses decreased, while seven either increased or did not appreciably change.