The NANOGrav 15 yr Data Set: Chromatic Gaussian Process Noise Models for Six Pulsars
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2024
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| author | Larsen, Bjorn Mingarelli, Chiara M. F. Hazboun, Jeffrey S. Chalumeau, Aurelien Good, Deborah C. Simon, Joseph Agazie, Gabriella Anumarlapudi, Akash Archibald, Anne M. Arzoumanian, Zaven Baker, Paul T. Brook, Paul R. Cromartie, H. Thankful Crowter, Kathryn DeCesar, Megan E. Demorest, Paul B. Dolch, Timothy Ferrara, Elizabeth C. Fiore, William Fonseca, Emmanuel Freedman, Gabriel E. Garver-Daniels, Nate Gentile, Peter A. Glaser, Joseph Jennings, Ross J. Jones, Megan L. Kaplan, David L. Kerr, Matthew Lam, Michael T. Lorimer, Duncan R. Luo, Jing Lynch, Ryan S. McEwen, Alexander McLaughlin, Maura A. McMann, Natasha Meyers, Bradley W. Ng, Cherry Nice, David J. Pennucci, Timothy T. Perera, Benetge B. P. Pol, Nihan S. Radovan, Henri A. Ransom, Scott M. Ray, Paul S. Schmiedekamp, Ann Schmiedekamp, Carl Shapiro-Albert, Brent J. Stairs, Ingrid H. Stovall, Kevin Susobhanan, Abhimanyu Swiggum, Joseph K. Wahl, Haley M. Champion, David J. Cognard, Ismael Guillemot, Lucas Hu, Huanchen Keith, Michael J. Liu, Kuo McKee, James W. Parthasarathy, Aditya Perrodin, Delphine Possenti, Andrea Shaifullah, Golam M. Theureau, Gilles |
| author_facet | Larsen, Bjorn Mingarelli, Chiara M. F. Hazboun, Jeffrey S. Chalumeau, Aurelien Good, Deborah C. Simon, Joseph Agazie, Gabriella Anumarlapudi, Akash Archibald, Anne M. Arzoumanian, Zaven Baker, Paul T. Brook, Paul R. Cromartie, H. Thankful Crowter, Kathryn DeCesar, Megan E. Demorest, Paul B. Dolch, Timothy Ferrara, Elizabeth C. Fiore, William Fonseca, Emmanuel Freedman, Gabriel E. Garver-Daniels, Nate Gentile, Peter A. Glaser, Joseph Jennings, Ross J. Jones, Megan L. Kaplan, David L. Kerr, Matthew Lam, Michael T. Lorimer, Duncan R. Luo, Jing Lynch, Ryan S. McEwen, Alexander McLaughlin, Maura A. McMann, Natasha Meyers, Bradley W. Ng, Cherry Nice, David J. Pennucci, Timothy T. Perera, Benetge B. P. Pol, Nihan S. Radovan, Henri A. Ransom, Scott M. Ray, Paul S. Schmiedekamp, Ann Schmiedekamp, Carl Shapiro-Albert, Brent J. Stairs, Ingrid H. Stovall, Kevin Susobhanan, Abhimanyu Swiggum, Joseph K. Wahl, Haley M. Champion, David J. Cognard, Ismael Guillemot, Lucas Hu, Huanchen Keith, Michael J. Liu, Kuo McKee, James W. Parthasarathy, Aditya Perrodin, Delphine Possenti, Andrea Shaifullah, Golam M. Theureau, Gilles |
| contents | Pulsar timing arrays (PTAs) are designed to detect low-frequency gravitational waves (GWs). GWs induce achromatic signals in PTA data, meaning that the timing delays do not depend on radio-frequency. However, pulse arrival times are also affected by radio-frequency dependent "chromatic" noise from sources such as dispersion measure (DM) and scattering delay variations. Furthermore, the characterization of GW signals may be influenced by the choice of chromatic noise model for each pulsar. To better understand this effect, we assess if and how different chromatic noise models affect achromatic noise properties in each pulsar. The models we compare include existing DM models used by NANOGrav and noise models used for the European PTA Data Release 2 (EPTA DR2). We perform this comparison using a subsample of six pulsars from the NANOGrav 15 yr data set, selecting the same six pulsars as from the EPTA DR2 six-pulsar dataset. We find that the choice of chromatic noise model noticeably affects the achromatic noise properties of several pulsars. This is most dramatic for PSR J1713+0747, where the amplitude of its achromatic red noise lowers from $\log_{10}A_{\text{RN}} = -14.1^{+0.1}_{-0.1}$ to $-14.7^{+0.3}_{-0.5}$, and the spectral index broadens from $γ_{\text{RN}} = 2.6^{+0.5}_{-0.4}$ to $γ_{\text{RN}} = 3.5^{+1.2}_{-0.9}$. We also compare each pulsar's noise properties with those inferred from the EPTA DR2, using the same models. From the discrepancies, we identify potential areas where the noise models could be improved. These results highlight the potential for custom chromatic noise models to improve PTA sensitivity to GWs. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_14941 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The NANOGrav 15 yr Data Set: Chromatic Gaussian Process Noise Models for Six Pulsars Larsen, Bjorn Mingarelli, Chiara M. F. Hazboun, Jeffrey S. Chalumeau, Aurelien Good, Deborah C. Simon, Joseph Agazie, Gabriella Anumarlapudi, Akash Archibald, Anne M. Arzoumanian, Zaven Baker, Paul T. Brook, Paul R. Cromartie, H. Thankful Crowter, Kathryn DeCesar, Megan E. Demorest, Paul B. Dolch, Timothy Ferrara, Elizabeth C. Fiore, William Fonseca, Emmanuel Freedman, Gabriel E. Garver-Daniels, Nate Gentile, Peter A. Glaser, Joseph Jennings, Ross J. Jones, Megan L. Kaplan, David L. Kerr, Matthew Lam, Michael T. Lorimer, Duncan R. Luo, Jing Lynch, Ryan S. McEwen, Alexander McLaughlin, Maura A. McMann, Natasha Meyers, Bradley W. Ng, Cherry Nice, David J. Pennucci, Timothy T. Perera, Benetge B. P. Pol, Nihan S. Radovan, Henri A. Ransom, Scott M. Ray, Paul S. Schmiedekamp, Ann Schmiedekamp, Carl Shapiro-Albert, Brent J. Stairs, Ingrid H. Stovall, Kevin Susobhanan, Abhimanyu Swiggum, Joseph K. Wahl, Haley M. Champion, David J. Cognard, Ismael Guillemot, Lucas Hu, Huanchen Keith, Michael J. Liu, Kuo McKee, James W. Parthasarathy, Aditya Perrodin, Delphine Possenti, Andrea Shaifullah, Golam M. Theureau, Gilles High Energy Astrophysical Phenomena Astrophysics of Galaxies Instrumentation and Methods for Astrophysics Pulsar timing arrays (PTAs) are designed to detect low-frequency gravitational waves (GWs). GWs induce achromatic signals in PTA data, meaning that the timing delays do not depend on radio-frequency. However, pulse arrival times are also affected by radio-frequency dependent "chromatic" noise from sources such as dispersion measure (DM) and scattering delay variations. Furthermore, the characterization of GW signals may be influenced by the choice of chromatic noise model for each pulsar. To better understand this effect, we assess if and how different chromatic noise models affect achromatic noise properties in each pulsar. The models we compare include existing DM models used by NANOGrav and noise models used for the European PTA Data Release 2 (EPTA DR2). We perform this comparison using a subsample of six pulsars from the NANOGrav 15 yr data set, selecting the same six pulsars as from the EPTA DR2 six-pulsar dataset. We find that the choice of chromatic noise model noticeably affects the achromatic noise properties of several pulsars. This is most dramatic for PSR J1713+0747, where the amplitude of its achromatic red noise lowers from $\log_{10}A_{\text{RN}} = -14.1^{+0.1}_{-0.1}$ to $-14.7^{+0.3}_{-0.5}$, and the spectral index broadens from $γ_{\text{RN}} = 2.6^{+0.5}_{-0.4}$ to $γ_{\text{RN}} = 3.5^{+1.2}_{-0.9}$. We also compare each pulsar's noise properties with those inferred from the EPTA DR2, using the same models. From the discrepancies, we identify potential areas where the noise models could be improved. These results highlight the potential for custom chromatic noise models to improve PTA sensitivity to GWs. |
| title | The NANOGrav 15 yr Data Set: Chromatic Gaussian Process Noise Models for Six Pulsars |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2405.14941 |