Testing EMRI models for Quasi-Periodic Eruptions with 3.5 years of monitoring eRO-QPE1
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arXiv
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| Natura: | Preprint |
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2024
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| author | Chakraborty, Joheen Arcodia, Riccardo Kara, Erin Miniutti, Giovanni Giustini, Margherita Tetarenko, Alexandra J. Rhodes, Lauren Franchini, Alessia Bonetti, Matteo Burdge, Kevin B. Goodwin, Adelle J. Maccarone, Thomas J. Merloni, Andrea Ponti, Gabriele Remillard, Ronald A. Saxton, Richard D. |
| author_facet | Chakraborty, Joheen Arcodia, Riccardo Kara, Erin Miniutti, Giovanni Giustini, Margherita Tetarenko, Alexandra J. Rhodes, Lauren Franchini, Alessia Bonetti, Matteo Burdge, Kevin B. Goodwin, Adelle J. Maccarone, Thomas J. Merloni, Andrea Ponti, Gabriele Remillard, Ronald A. Saxton, Richard D. |
| contents | Quasi-Periodic Eruptions (QPEs) are luminous X-ray outbursts recurring on hour timescales, observed from the nuclei of a growing handful of nearby low-mass galaxies. Their physical origin is still debated, and usually modeled as (a) accretion disk instabilities or (b) interaction of a supermassive black hole (SMBH) with a lower mass companion in an extreme mass-ratio inspiral (EMRI). EMRI models can be tested with several predictions related to the short- and long-term behavior of QPEs. In this study, we report on the ongoing 3.5-year NICER and XMM-Newton monitoring campaign of eRO-QPE1, which is known to exhibit erratic QPEs that have been challenging for the simplest EMRI models to explain. We report 1) complex, non-monotonic evolution in the long-term trends of QPE energy output and inferred emitting area; 2) the disappearance of the QPEs (within NICER detectability) in October 2023, then reappearance by January 2024 at a luminosity $\sim$100x fainter (and temperature $\sim$3x cooler) than initial discovery; 3) radio non-detections with MeerKAT and VLA observations partly contemporaneous with our NICER campaign (though not during outbursts); and 4) the presence of a possible $\sim$6-day modulation of the QPE timing residuals, which aligns with the expected nodal precession timescale of the underlying accretion disk. Our results tentatively support EMRI-disk collision models powering the QPEs, and we demonstrate that the timing modulation of QPEs may be used to jointly constrain the SMBH spin and disk density profile. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2402_08722 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Testing EMRI models for Quasi-Periodic Eruptions with 3.5 years of monitoring eRO-QPE1 Chakraborty, Joheen Arcodia, Riccardo Kara, Erin Miniutti, Giovanni Giustini, Margherita Tetarenko, Alexandra J. Rhodes, Lauren Franchini, Alessia Bonetti, Matteo Burdge, Kevin B. Goodwin, Adelle J. Maccarone, Thomas J. Merloni, Andrea Ponti, Gabriele Remillard, Ronald A. Saxton, Richard D. High Energy Astrophysical Phenomena Quasi-Periodic Eruptions (QPEs) are luminous X-ray outbursts recurring on hour timescales, observed from the nuclei of a growing handful of nearby low-mass galaxies. Their physical origin is still debated, and usually modeled as (a) accretion disk instabilities or (b) interaction of a supermassive black hole (SMBH) with a lower mass companion in an extreme mass-ratio inspiral (EMRI). EMRI models can be tested with several predictions related to the short- and long-term behavior of QPEs. In this study, we report on the ongoing 3.5-year NICER and XMM-Newton monitoring campaign of eRO-QPE1, which is known to exhibit erratic QPEs that have been challenging for the simplest EMRI models to explain. We report 1) complex, non-monotonic evolution in the long-term trends of QPE energy output and inferred emitting area; 2) the disappearance of the QPEs (within NICER detectability) in October 2023, then reappearance by January 2024 at a luminosity $\sim$100x fainter (and temperature $\sim$3x cooler) than initial discovery; 3) radio non-detections with MeerKAT and VLA observations partly contemporaneous with our NICER campaign (though not during outbursts); and 4) the presence of a possible $\sim$6-day modulation of the QPE timing residuals, which aligns with the expected nodal precession timescale of the underlying accretion disk. Our results tentatively support EMRI-disk collision models powering the QPEs, and we demonstrate that the timing modulation of QPEs may be used to jointly constrain the SMBH spin and disk density profile. |
| title | Testing EMRI models for Quasi-Periodic Eruptions with 3.5 years of monitoring eRO-QPE1 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2402.08722 |