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: Upper limit on the number density of SMBHBs in the local universe as a function of GW frequency. Different curves correspond to binaries with different chirp mass values. Note that as expected, we can place more stringent limits on the number density of systems with higher masses. The density is measured in terms of comoving volume.
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: Bolometric light curves using the FRDM nuclear model (left) and the HFB model (right) assuming an ejecta mass of 0.005 M ⊙. For each nuclear model, three sets of heating rates are used: only Z < 90 elements (solid gray), only Z < 104 elements (dotted colors), and all elements (solid colors). The paucity of superheavy elements produced in the FRDM simulation explains why the green solid (“Z = all”) and light-blue dotted (“Z < 104”) curves appear identical; there is effectively no difference between these models.
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: Nucleosynthesis network mass fraction yields of the heaviest elements at 7.5 hr post-merger for three nuclear mass model and fission barrier combinations. Under the same astrophysical conditions, there can be over 3 orders of magnitude difference in the mass fractions of superheavy elements that are synthesized, arising solely from what nuclear models are adopted.
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: Heating rates over time for two extremes of nuclear variations showing the contribution by all elements (thick, solid lines), only up to the actinides (shaded), and excluding the actinides and superheavy elements (thin, solid lines). The dashed line is a simple model in which the heating rate evolves scales with time by 10−1.3 (see, e.g., Metzger 2019). The divergence between the shaded region and the thick lines (e.g., at about 10−2–101 days for HFB) indicates heating uniquely from the superheavy elements.
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: Bolometric light curves for the HFB model with ejecta renormalized such that the heating rates at 1 day are equal for all models. Three sets of heating rates: only Z < 90 elements (gray), only Z < 104 elements (dashed pink), and all elements (dark pink).
Paper: Templates for Fitting Photometry of Ultra-high-redshift Galaxies
Authors: Charles L. Steinhardt, Vasily Kokorev, Vadim Rusakov, Ethan Garcia, Albert Sneppen
Figure caption: Expected change in inferred stellar masses using the IMFs in this work relative to Galactic IMF as a function of T  g . The dashed black line indicates the average shift based on the analytical integral while holding all other parameters fixed, which is a close match for the observed differences in fitting the three z > 12 candidates under the same conditions. The actual shift in stellar mass will combine this effect, the difference between Kroupa and Chabrier choices of Galactic IMF, and changes in stellar age and nebular emission lines, and it will typically exceed the analytical integral shown here.
Paper: Templates for Fitting Photometry of Ultra-high-redshift Galaxies
Authors: Charles L. Steinhardt, Vasily Kokorev, Vadim Rusakov, Ethan Garcia, Albert Sneppen
Figure caption: A switch from the standard template basis to the ones developed in this work reduces the best-fit stellar masses. Using stellar masses derived by Labbe et al. (2023) from modified T  g  = 20 K EAZY templates (black), Boylan-Kolchin (2023) find that z = 10 galaxies are too massive to have been produced with a ΛCDM cosmology (this figure is reproduced from Figure 2 in Boylan-Kolchin 2023). However, the lower masses from templates optimized for high-redshift galaxies (red) can still be consistent with halo formation under the standard cosmological paradigm, even with a similar stellar baryon fraction to the local Universe.
Paper: Templates for Fitting Photometry of Ultra-high-redshift Galaxies
Authors: Charles L. Steinhardt, Vasily Kokorev, Vadim Rusakov, Ethan Garcia, Albert Sneppen
Figure caption: Best-fit reconstructed spectra (left) and redshift probability functions (right) for three galaxies in SMACS0723. The fits were performed with the standard EAZY Chabrier IMF at T  g  = 20 K (blue) and with the Kroupa IMF at T  g  = 60 K (maroon), with the latter fit expected to be a better description of galaxies at z > 12.
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: Geometry of the binary and jets. The axes x and y are in the binary plane, and +z gives the direction along the binary vector,  e  orb (away from the observer, given the observed clockwise rotation). The observer is at an angle, i orb, with respect to  e  orb, and ϕ is the orbital phase; ϕ = 0 and π correspond to the superior and inferior conjunction, respectively. The binary rotation follows the increasing ϕ. The shown configuration is close to the latter. Then, θ BH is the inclination of the BH spin vector,  e  BH, and the counterjet with respect to  e  orb; ϕ BH is its azimuthal angle; and h is the distance of the radio source from the BH center. The counterjet emission is neglected in our model. The distance from the radio source measured along the direction toward the observer is l. The distances of the point at l measured from the centers of the BH and the donor are s (not shown for clarity) and r, respectively.
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: The MCMC results for the case of b = 0.5. The panels show the histograms of the one-dimensional posterior distributions for the model parameters and the two-parameter correlations. The median results for the fitted quantities are shown by the middle vertical dashed lines in the distribution panels. The surrounding vertical dashed lines correspond to the 90% uncertainty. The parameters obtained are given above the posterior distributions.
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: Observed orbital modulations fitted by our model (solid curves). The left and right panels assume that 100% (b = 0) and 50% (b = 0.5) of the total flux is modulated, respectively. (a) 15 GHz, (b) 8.3 GHz, (c) 2.25 GHz, (d) 15 GHz, (e) 8.3 GHz, (f) 2.25 GHz. For clarity, two cycles are shown.
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: Savage-Dickey Bayes factors for the CW+CURN model vs. the CURN model as a function of frequency (black). Also shown are Bayes factors when excluding PSR J1713+0747 (red, only computed for f GW > 24 nHz) and Bayes factors based on a resampled posterior that takes into account the presence of HD correlations in the common red noise process, i.e., CW+HD vs. HD (orange, only computed for 2.1 nHz < f GW < 5.9 nHz). Shaded regions show the 1σ uncertainties.
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: The 95% lower limits on the luminosity distance to an individual SMBHB. The blue line shows the effective luminosity distance radius corresponding to the exclusion volume. The blue shaded region shows the range of distance limits over 12 equal-area sky pixels. The red line shows the all-sky distance limit calculated from the all-sky strain upper limit. Note that this is dominated by the worst sky location at every frequency.
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: Map of the 95% lower limit on the distance to individual SMBHBs with ﹩{ \mathcal M }={10}^{9}{M}_{\odot }﹩ and f GW = 27 nHz. White diamonds indicate the positions of known SMBHB candidates, and white squares show the location of large galaxy clusters that could contain an SMBHB. Black dots mark the location of quasars with periodic variability. We show the all-sky limit (dotted white) and R eff (solid white) on the color scale.
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: All-sky CW strain 95% upper limits compared to previous data sets. We see the most significant improvements at low frequencies where marginalizing over the common red noise allows us to set more constraining upper limits.
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: Noise-marginalized MCOS S/N distributions of different spatially correlated processes with (bottom panel) and without (top panel) the binary signal removed. Solid vertical lines show the maximum-likelihood values, while dashed lines indicate the mean of each distribution. Removing the binary candidate around 4 nHz is able to shift the distribution for both processes so that they become consistent with zero.
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: Map of CW strain 95% upper limits at 6 nHz, the most sensitive frequency (see Figure 5). Red stars indicate the location of pulsars included in the data set. Note that the upper limit is almost an order of magnitude lower toward the galactic center, toward which most of the pulsars are located. The white line on the color scale indicates the upper limit we find when marginalizing over sky location.