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| Formato: | Preprint |
| Publicado: |
2025
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| Materias: | |
| Acceso en línea: | https://arxiv.org/abs/2508.18126 |
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| author | Matt, Cayenne Gultekin, Kayhan Kelley, Luke Blecha, Laura Simon, Joseph Agazie, Gabriella Anumarlapudi, Akash Archibald, Anne Arzoumanian, Zaven Baier, Jeremy Baker, Paul Bécsy, Bence Brazier, Adam Brook, Paul Burke-Spolaor, Sarah Burnette, Rand Case, Robin Casey-Clyde, James Charisi, Maria Chatterjee, Shami Cohen, Tyler Cordes, James Cornish, Neil Crawford, Fronefield Cromartie, H. Thankful Crowter, Kathryn DeCesar, Megan Demorest, Paul Deng, Heling Dey, Lankeswar Dolch, Timothy Ferrara, Elizabeth Fiore, William Fonseca, Emmanuel Freedman, Gabriel Gardiner, Emiko Garver-Daniels, Nate Gentile, Peter Gersbach, Kyle Glaser, Joseph Good, Deborah Harris, C. Hazboun, Jeffrey Jennings, Ross Johnson, Aaron Jones, Megan Kaplan, David Kerr, Matthew Key, Joey Laal, Nima Lam, Michael Lamb, William Larsen, Bjorn Lazio, T. Lewandowska, Natalia Liu, Tingting Lorimer, Duncan Luo, Jing Lynch, Ryan Ma, Chung-Pei Madison, Dustin McEwen, Alexander McKee, James McLaughlin, Maura McMann, Natasha Meyers, Bradley Meyers, Patrick Mingarelli, Chiara Mitridate, Andrea Ng, Cherry Nice, David Ocker, Stella Olum, Ken Pennucci, Timothy Perera, Benetge Petrov, Polina Pol, Nihan Radovan, Henri Ransom, Scott Ray, Paul Romano, Joseph Runnoe, Jessie Saffer, Alexander Sardesai, Shashwat Schmiedekamp, A. Schmiedekamp, Carl Schmitz, Kai Shapiro-Albert, Brent Siemens, Xavier Fiscella, Sophia Sosa Stairs, Ingrid Stinebring, Daniel Stovall, Kevin Susobhanan, Abhimanyu Swiggum, Joseph Taylor, Jacob Taylor, Stephen Thompson, Mercedes Turner, Jacob Vallisneri, Michele van Haasteren, Rutger Vigeland, Sarah Wahl, Haley Wilson, Kevin Witt, Caitlin Wright, David Young, Olivia |
| author_facet | Matt, Cayenne Gultekin, Kayhan Kelley, Luke Blecha, Laura Simon, Joseph Agazie, Gabriella Anumarlapudi, Akash Archibald, Anne Arzoumanian, Zaven Baier, Jeremy Baker, Paul Bécsy, Bence Brazier, Adam Brook, Paul Burke-Spolaor, Sarah Burnette, Rand Case, Robin Casey-Clyde, James Charisi, Maria Chatterjee, Shami Cohen, Tyler Cordes, James Cornish, Neil Crawford, Fronefield Cromartie, H. Thankful Crowter, Kathryn DeCesar, Megan Demorest, Paul Deng, Heling Dey, Lankeswar Dolch, Timothy Ferrara, Elizabeth Fiore, William Fonseca, Emmanuel Freedman, Gabriel Gardiner, Emiko Garver-Daniels, Nate Gentile, Peter Gersbach, Kyle Glaser, Joseph Good, Deborah Harris, C. Hazboun, Jeffrey Jennings, Ross Johnson, Aaron Jones, Megan Kaplan, David Kerr, Matthew Key, Joey Laal, Nima Lam, Michael Lamb, William Larsen, Bjorn Lazio, T. Lewandowska, Natalia Liu, Tingting Lorimer, Duncan Luo, Jing Lynch, Ryan Ma, Chung-Pei Madison, Dustin McEwen, Alexander McKee, James McLaughlin, Maura McMann, Natasha Meyers, Bradley Meyers, Patrick Mingarelli, Chiara Mitridate, Andrea Ng, Cherry Nice, David Ocker, Stella Olum, Ken Pennucci, Timothy Perera, Benetge Petrov, Polina Pol, Nihan Radovan, Henri Ransom, Scott Ray, Paul Romano, Joseph Runnoe, Jessie Saffer, Alexander Sardesai, Shashwat Schmiedekamp, A. Schmiedekamp, Carl Schmitz, Kai Shapiro-Albert, Brent Siemens, Xavier Fiscella, Sophia Sosa Stairs, Ingrid Stinebring, Daniel Stovall, Kevin Susobhanan, Abhimanyu Swiggum, Joseph Taylor, Jacob Taylor, Stephen Thompson, Mercedes Turner, Jacob Vallisneri, Michele van Haasteren, Rutger Vigeland, Sarah Wahl, Haley Wilson, Kevin Witt, Caitlin Wright, David Young, Olivia |
| contents | We test the impact of an evolving supermassive black hole (SMBH) mass scaling relation (Mbh-Mbulge) on the predictions for the gravitational wave background (GWB). The observed GWB amplitude is 2-3 times higher than predicted by astrophysically informed models which suggests the need to revise the assumptions in those models. We compare a semi-analytic model's ability to reproduce the observed GWB spectrum with a static versus evolving-amplitude Mbh-Mbulge relation. We additionally consider the influence of the choice of galaxy stellar mass function on the modeled GWB spectra. Our models are able to reproduce the GWB amplitude with either a large number density of massive galaxies or a positively evolving Mbh-Mbulge amplitude (i.e., the Mbh / Mbulge ratio was higher in the past). If we assume that the Mbh-Mbulge amplitude does not evolve, our models require a galaxy stellar mass function that implies an undetected population of massive galaxies (Mstellar > 10^11 Msun at z > 1). When the Mbh-Mbulge amplitude is allowed to evolve, we can model the GWB spectrum with all fiducial values and an Mbh-Mbulge amplitude that evolves as alpha(z) = alpha_0 (1 + z)^(1.04 +/- 0.5). |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_18126 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Inferring Mbh-Mbulge Evolution from the Gravitational Wave Background Matt, Cayenne Gultekin, Kayhan Kelley, Luke Blecha, Laura Simon, Joseph Agazie, Gabriella Anumarlapudi, Akash Archibald, Anne Arzoumanian, Zaven Baier, Jeremy Baker, Paul Bécsy, Bence Brazier, Adam Brook, Paul Burke-Spolaor, Sarah Burnette, Rand Case, Robin Casey-Clyde, James Charisi, Maria Chatterjee, Shami Cohen, Tyler Cordes, James Cornish, Neil Crawford, Fronefield Cromartie, H. Thankful Crowter, Kathryn DeCesar, Megan Demorest, Paul Deng, Heling Dey, Lankeswar Dolch, Timothy Ferrara, Elizabeth Fiore, William Fonseca, Emmanuel Freedman, Gabriel Gardiner, Emiko Garver-Daniels, Nate Gentile, Peter Gersbach, Kyle Glaser, Joseph Good, Deborah Harris, C. Hazboun, Jeffrey Jennings, Ross Johnson, Aaron Jones, Megan Kaplan, David Kerr, Matthew Key, Joey Laal, Nima Lam, Michael Lamb, William Larsen, Bjorn Lazio, T. Lewandowska, Natalia Liu, Tingting Lorimer, Duncan Luo, Jing Lynch, Ryan Ma, Chung-Pei Madison, Dustin McEwen, Alexander McKee, James McLaughlin, Maura McMann, Natasha Meyers, Bradley Meyers, Patrick Mingarelli, Chiara Mitridate, Andrea Ng, Cherry Nice, David Ocker, Stella Olum, Ken Pennucci, Timothy Perera, Benetge Petrov, Polina Pol, Nihan Radovan, Henri Ransom, Scott Ray, Paul Romano, Joseph Runnoe, Jessie Saffer, Alexander Sardesai, Shashwat Schmiedekamp, A. Schmiedekamp, Carl Schmitz, Kai Shapiro-Albert, Brent Siemens, Xavier Fiscella, Sophia Sosa Stairs, Ingrid Stinebring, Daniel Stovall, Kevin Susobhanan, Abhimanyu Swiggum, Joseph Taylor, Jacob Taylor, Stephen Thompson, Mercedes Turner, Jacob Vallisneri, Michele van Haasteren, Rutger Vigeland, Sarah Wahl, Haley Wilson, Kevin Witt, Caitlin Wright, David Young, Olivia High Energy Astrophysical Phenomena Astrophysics of Galaxies We test the impact of an evolving supermassive black hole (SMBH) mass scaling relation (Mbh-Mbulge) on the predictions for the gravitational wave background (GWB). The observed GWB amplitude is 2-3 times higher than predicted by astrophysically informed models which suggests the need to revise the assumptions in those models. We compare a semi-analytic model's ability to reproduce the observed GWB spectrum with a static versus evolving-amplitude Mbh-Mbulge relation. We additionally consider the influence of the choice of galaxy stellar mass function on the modeled GWB spectra. Our models are able to reproduce the GWB amplitude with either a large number density of massive galaxies or a positively evolving Mbh-Mbulge amplitude (i.e., the Mbh / Mbulge ratio was higher in the past). If we assume that the Mbh-Mbulge amplitude does not evolve, our models require a galaxy stellar mass function that implies an undetected population of massive galaxies (Mstellar > 10^11 Msun at z > 1). When the Mbh-Mbulge amplitude is allowed to evolve, we can model the GWB spectrum with all fiducial values and an Mbh-Mbulge amplitude that evolves as alpha(z) = alpha_0 (1 + z)^(1.04 +/- 0.5). |
| title | Inferring Mbh-Mbulge Evolution from the Gravitational Wave Background |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2508.18126 |