Temporal evolution of the periodic GeV signal from 4FGL J1913.2+0512 and analysis of the SS 433 / W50 lobes
6 affiliations
- 1Institute of Space Sciences (ICE-CSIC) , Campus UAB, Carrer de Can Magrans s/n, Barcelona 08193 ,
- 2Institut d’Estudis Espacials de Catalunya (IEEC) , Barcelona 08860 ,
- 3Institució Catalana de Recerca i Estudis Avançats (ICREA) , Barcelona ,
- 4University of Science and Technology of China (USTC) CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, , Hefei 230026 ,
- 5School of Astronomy and Space Science, University of Science and Technology of China (USTC) , Hefei 230026 ,
- 6Space Science Division, Naval Research Laboratory , Washington DC 20375 ,
Abstract
SS 433 is a microquasar whose relativistic jets precess every ∼162 days, providing a laboratory for jet-interstellar medium interactions. We present a comprehensive analysis of 16 years of Fermi Large Area Telescope data (August 2008–September 2024) of the SS 433 / W50 field, using events in the 0.3 − 300 GeV range and employing pulsar gating to mitigate contamination from the bright nearby pulsar PSR J1907+0602. We detect the GeV source 4FGL J1913.2+0512 (TS = 45, where TS denotes the likelihood-ratio Test Statistic) with a power-law spectrum (photon index 2.61 ± 0.08) and confirm a GeV excess at the western lobe (TS = 17). The eastern lobe of SS 433 is hinted at with lower significance. One additional GeV excess, Fermi J1909.6+0552 (TS = 20; TS = 28 over 0.1 − 300 GeV), located outside the SS 433 / W50 system, is revealed after gating. Exposure-corrected Lomb-Scargle periodograms and precessional phase-folded light curves show a ∼162-day modulation in 4FGL J1913.2+0512. The phase-folded emission is mainly confined to the first half of the precessional cycle, while the source is not significantly detected in the second half. This periodic signal is mainly concentrated in the 5–10 yr interval, remains visible in the cumulative 0–10 yr dataset, and is not recovered in the subsequent 10–16 yr interval. Over the full 16-year dataset, the modulation remains detectable but with reduced significance, consistent with dilution by the later non-modulated epoch. These results indicate that the efficiency and/or geometry of gamma-ray production in the SS 433 environment evolves on multi-year timescales.
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BibTeX
@article{coban2026temporal,
title = {{Temporal evolution of the periodic GeV signal from 4FGL J1913.2+0512 and analysis of the SS 433 / W50 lobes}},
author = {Ömer Faruk Çoban and D F Torres and J Li and D Hadasch and A De Sarkar and M Kerr},
journal = {Monthly Notices of the Royal Astronomical Society},
year = {2026},
month = oct,
doi = {10.1093/mnras/stag2007},
url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2007/8994294},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Temporal evolution of the periodic GeV signal from 4FGL J1913.2+0512 and analysis of the SS 433 / W50 lobes
AU - Ömer Faruk Çoban
AU - D F Torres
AU - J Li
AU - D Hadasch
AU - A De Sarkar
AU - M Kerr
PY - 2026
DA - 2026/10/23
JO - Monthly Notices of the Royal Astronomical Society
DO - 10.1093/mnras/stag2007
UR - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2007/8994294
AB - SS 433 is a microquasar whose relativistic jets precess every ∼162 days, providing a laboratory for jet-interstellar medium interactions. We present a comprehensive analysis of 16 years of Fermi Large Area Telescope data (August 2008–September 2024) of the SS 433 / W50 field, using events in the 0.3 − 300 GeV range and employing pulsar gating to mitigate contamination from the bright nearby pulsar PSR J1907+0602. We detect the GeV source 4FGL J1913.2+0512 (TS = 45, where TS denotes the likelihood-ratio Test Statistic) with a power-law spectrum (photon index 2.61 ± 0.08) and confirm a GeV excess at the western lobe (TS = 17). The eastern lobe of SS 433 is hinted at with lower significance. One additional GeV excess, Fermi J1909.6+0552 (TS = 20; TS = 28 over 0.1 − 300 GeV), located outside the SS 433 / W50 system, is revealed after gating. Exposure-corrected Lomb-Scargle periodograms and precessional phase-folded light curves show a ∼162-day modulation in 4FGL J1913.2+0512. The phase-folded emission is mainly confined to the first half of the precessional cycle, while the source is not significantly detected in the second half. This periodic signal is mainly concentrated in the 5–10 yr interval, remains visible in the cumulative 0–10 yr dataset, and is not recovered in the subsequent 10–16 yr interval. Over the full 16-year dataset, the modulation remains detectable but with reduced significance, consistent with dilution by the later non-modulated epoch. These results indicate that the efficiency and/or geometry of gamma-ray production in the SS 433 environment evolves on multi-year timescales.
SN - 0035-8711
SN - 1365-2966
ER -