Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · 2508.18126

Inferring Mbh-Mbulge Evolution from the Gravitational Wave Background

Cayenne Matt·Kayhan Gultekin·Luke Kelley·Laura Blecha·Joseph Simon·Gabriella Agazie·Akash Anumarlapudi·Anne Archibald·Zaven Arzoumanian·Jeremy Baier·Paul Baker·Bence Bécsy·Adam Brazier·Paul Brook·Sarah Burke-Spolaor·Rand Burnette·Robin Case·James Casey-Clyde·Maria Charisi·Shami Chatterjee·Tyler Cohen·James Cordes·Neil Cornish·Fronefield Crawford·H. Thankful Cromartie·Kathryn Crowter·Megan DeCesar·Paul Demorest·Heling Deng·Lankeswar Dey·Timothy Dolch·Elizabeth Ferrara·William Fiore·Emmanuel Fonseca·Gabriel Freedman·Emiko Gardiner·Nate Garver-Daniels·Peter Gentile·Kyle Gersbach·Joseph Glaser·Deborah Good·C. Harris·Jeffrey Hazboun·Ross Jennings·Aaron Johnson·Megan Jones·David Kaplan·Matthew Kerr·Joey Key·Nima Laal·Michael Lam·William Lamb·Bjorn Larsen·T. Lazio·Natalia Lewandowska·Tingting Liu·Duncan Lorimer·Jing Luo·Ryan Lynch·Chung-Pei Ma·Dustin Madison·Alexander McEwen·James McKee·Maura McLaughlin·Natasha McMann·Bradley Meyers·Patrick Meyers·Chiara Mingarelli·Andrea Mitridate·Cherry Ng·David Nice·Stella Ocker·Ken Olum·Timothy Pennucci·Benetge Perera·Polina Petrov·Nihan Pol·Henri Radovan·Scott Ransom·Paul Ray·Joseph Romano·Jessie Runnoe·Alexander Saffer·Shashwat Sardesai·A. Schmiedekamp·Carl Schmiedekamp·Kai Schmitz·Brent Shapiro-Albert·Xavier Siemens·Sophia Sosa Fiscella·Ingrid Stairs·Daniel Stinebring·Kevin Stovall·Abhimanyu Susobhanan·Joseph Swiggum·Jacob Taylor·Stephen Taylor·Mercedes Thompson·Jacob Turner·Michele Vallisneri
View original source ↗Read source document ↗Export metadata ↓

Abstract

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).

Explore related subjects

astro-ph.HEastro-ph.GA

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Cayenne Matt, Kayhan Gultekin, Luke Kelley, Laura Blecha, Joseph Simon, Gabriella Agazie, Akash Anumarlapudi, Anne Archibald, Zaven Arzoumanian, Jeremy Baier, Paul Baker, Bence Bécsy, Adam Brazier, Paul Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, James Casey-Clyde, Maria Charisi, Shami Chatterjee, Tyler Cohen, James Cordes, Neil Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Megan DeCesar, Paul Demorest, Heling Deng, Lankeswar Dey, Timothy Dolch, Elizabeth Ferrara, William Fiore, Emmanuel Fonseca, Gabriel Freedman, Emiko Gardiner, Nate Garver-Daniels, Peter Gentile, Kyle Gersbach, Joseph Glaser, Deborah Good, C. Harris, Jeffrey Hazboun, Ross Jennings, Aaron Johnson, Megan Jones, David Kaplan, Matthew Kerr, Joey Key, Nima Laal, Michael Lam, William Lamb, Bjorn Larsen, T. Lazio, Natalia Lewandowska, Tingting Liu, Duncan Lorimer, Jing Luo, Ryan Lynch, Chung-Pei Ma, Dustin Madison, Alexander McEwen, James McKee, Maura McLaughlin, Natasha McMann, Bradley Meyers, Patrick Meyers, Chiara Mingarelli, Andrea Mitridate, Cherry Ng, David Nice, Stella Ocker, Ken Olum, Timothy Pennucci, Benetge Perera, Polina Petrov, Nihan Pol, Henri Radovan, Scott Ransom, Paul Ray, Joseph Romano, Jessie Runnoe, Alexander Saffer, Shashwat Sardesai, A. Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Brent Shapiro-Albert, Xavier Siemens, Sophia Sosa Fiscella, Ingrid Stairs, Daniel Stinebring, Kevin Stovall, Abhimanyu Susobhanan, Joseph Swiggum, Jacob Taylor, Stephen Taylor, Mercedes Thompson, Jacob Turner, Michele Vallisneri. 2025-08-25. Inferring Mbh-Mbulge Evolution from the Gravitational Wave Background. https://doi.org/10.3847/1538-4357%2Fae2480

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

IceCube neutrino point-source searches in the direction of the KM3NeT ultra-high-energy event

While still under construction, the KM3NeT Astroparticle Research with Cosmics in the Abyss (ARCA) detector recorded a $\sim$200 PeV neutrino on February 13th, 2023. This event is the highest-energy neutrino reported. IceCube, a cubic kilometer neutrino detector located at the geographic South Pole, has previously detected neutrinos up to approximately 10 PeV. We search for high-energy neutrinos from the location of the KM3NeT event using 15 years of IceCube data and considering three temporal hypotheses: steady or flaring in time coincidence, or at an arbitrary time. We find no evidence for neutrino emission for any of the studies performed. Correspondingly, we set upper limits on the neutrino flux from a point source in the direction of KM3-230213A. We compare these limits to KM3NeT's estimated flux and show that an astrophysical explanation of this event is strongly constrained for a variety of spectral assumptions for a steady or transient point source with the flux inferred from the single KM3NeT ultra-high-energy event assuming a spectral index of 2.0.

astro-ph.HE↗
arXiv2026

Evidence for the binary nature of the long-period radio transient ASKAP/DART J1832-0911

Long-period transients are a class of periodic pulsed radio source repeating on the minute to hour timescale. Recently, an increasing number of them are being identified as binary systems, specifically white dwarfs with low-mass main-sequence companions. In this work we analyse the most luminous long-period transient discovered to date, ASKAP/DART J1832-0911, with two years of radio data, and propose that it, too, may be a white dwarf system, although in a far more compact orbit than the aforementioned. The pulses are composed of quasi-periodic components which evolve in a systematic way over days and months. The source is highly linearly or elliptically polarised and its brightness enabled very high signal-to-noise measurement of the time-resolved Faraday rotation measure, which was found to vary across pulse phase. The linear polarisation position angle, circular polarised fraction, and spectral index also varied systematically in ways not typical of pulsars and magnetars. We show that an ultra-compact asynchronous polar explains much of the phenomenology of ASKAP/DART J1832-0911, in particular the evolution of the pulse morphology, rotation measure variation, and periodic X-ray emission, although we cannot conclusively prove a binary nature. However, our model makes testable predictions.

astro-ph.HE↗
arXiv2026

Nonbirefringent model of orthogonal polarization modes in radio pulsars - New view on S swing and mode structure in pulsar beam

Two orthogonal polarization modes observed in radio pulsar signals have long been attributed to proper modes of wave oscillation in strongly magnetized plasma. Yet it has been shown recently that they show up readily for extended emission regions that produce incoherently-superposed polarization signal. In this paper we present a two-dimensional polarization model based on incoherent superposition of radio signals. The model involves a single proper mode, say the O mode, but leads to the appearance of two orthogonal polarization tracks and naturally produces the triple form of polarization mode segregation in averaged profiles (central mode flanked on boths sides by another mode), as well as the displacement of modes in latitude, previously inferred from beam mapping. In the case of conal emission regions, the modelled polarization tends to mimic general polarization properties of the rotating vector model (RVM). However, the reason for this is the symmetry of the emission region - not the usual projection of dipolar magnetic azimuths. Thus the emerging RVM parameters reveal geometry of the emission region, not of the dipolar magnetic field. The results strongly support the vital role of nonbirefringent modal effects in radio pulsar profiles. Two proper modes may not be needed to explain observations of two orthogonal polarization tracks.

astro-ph.HE↗