Doubling the Number of Blue Large-Amplitude Pulsators: Final Results of Searches for BLAPs in the OGLE Inner Galactic Bulge Fields
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arXiv
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| Autori principali: | , , , , , , , , , , , , , , , |
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| Natura: | Preprint |
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2025
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| author | Borowicz, J. Pietrukowicz, P. Skowron, J. Mróz, M. J. Udalski, A. Szymański, M. K. Soszyński, I. Ulaczyk, K. Poleski, R. Kozłowski, S. Mróz, P. Skowron, D. M. Rybicki, K. Iwanek, P. Wrona, M. Gromadzki, M. |
| author_facet | Borowicz, J. Pietrukowicz, P. Skowron, J. Mróz, M. J. Udalski, A. Szymański, M. K. Soszyński, I. Ulaczyk, K. Poleski, R. Kozłowski, S. Mróz, P. Skowron, D. M. Rybicki, K. Iwanek, P. Wrona, M. Gromadzki, M. |
| contents | Blue Large-Amplitude Pulsators (BLAPs) are rare short-period ($\lesssim$80 min) pulsating variable stars exhibiting large-amplitude brightness variations (typically between 0.1 and 0.4 mag). As a recently discovered class of radial-mode pulsators, the origin and nature of these variables remain the subject of ongoing investigations. Here, we present a comprehensive summary of all BLAPs identified in the data of the Optical Gravitational Lensing Experiment (OGLE), including the discovery of 88 new BLAPs in the inner Galactic bulge fields. We performed a systematic search for periodic signals in the $I$-band light curves of more than 400 million stars with magnitudes down to $I = 21$. Our search effectively doubles the number of these variables to almost 200. The detected BLAPs exhibit pulsation periods between roughly 5 and 76 minutes. The analyzed dataset covers a timespan from 2001 to 2024, with some stars observed up to 20,000 times, providing the temporal coverage needed to study period and amplitude variations. We report on three objects that show enormous period changes, at a rate of $10^{-5}$ yr$^{-1}$, which could provide important clues to the evolutionary status of BLAPs. Full dataset is incorporated into the publicly available OGLE Collection of Variable Stars (OCVS), enabling future studies of these enigmatic objects. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_20823 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Doubling the Number of Blue Large-Amplitude Pulsators: Final Results of Searches for BLAPs in the OGLE Inner Galactic Bulge Fields Borowicz, J. Pietrukowicz, P. Skowron, J. Mróz, M. J. Udalski, A. Szymański, M. K. Soszyński, I. Ulaczyk, K. Poleski, R. Kozłowski, S. Mróz, P. Skowron, D. M. Rybicki, K. Iwanek, P. Wrona, M. Gromadzki, M. Solar and Stellar Astrophysics Blue Large-Amplitude Pulsators (BLAPs) are rare short-period ($\lesssim$80 min) pulsating variable stars exhibiting large-amplitude brightness variations (typically between 0.1 and 0.4 mag). As a recently discovered class of radial-mode pulsators, the origin and nature of these variables remain the subject of ongoing investigations. Here, we present a comprehensive summary of all BLAPs identified in the data of the Optical Gravitational Lensing Experiment (OGLE), including the discovery of 88 new BLAPs in the inner Galactic bulge fields. We performed a systematic search for periodic signals in the $I$-band light curves of more than 400 million stars with magnitudes down to $I = 21$. Our search effectively doubles the number of these variables to almost 200. The detected BLAPs exhibit pulsation periods between roughly 5 and 76 minutes. The analyzed dataset covers a timespan from 2001 to 2024, with some stars observed up to 20,000 times, providing the temporal coverage needed to study period and amplitude variations. We report on three objects that show enormous period changes, at a rate of $10^{-5}$ yr$^{-1}$, which could provide important clues to the evolutionary status of BLAPs. Full dataset is incorporated into the publicly available OGLE Collection of Variable Stars (OCVS), enabling future studies of these enigmatic objects. |
| title | Doubling the Number of Blue Large-Amplitude Pulsators: Final Results of Searches for BLAPs in the OGLE Inner Galactic Bulge Fields |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2510.20823 |