Microquasars, the local siblings of extragalactic quasars, are binary systems comprising a compact object and a companion star. By accreting matter from their companions, microquasars launch powerful winds and jets, influencing the interstellar environment around them. Steady gamma-ray emission is expected to rise from their central objects, or from interactions between their outflows and the surrounding medium. The latter prediction was recently confirmed with the detection of SS 433 at high (TeV) energies1. In this report, we analyse more than ten years of gigaelectronvolt gamma-ray data from the Fermi Gamma-ray Space Telescope on this source. Detailed scrutiny of the data reveal emission in the vicinity of SS 433, co-spatial with a gas enhancement, and hints of emission possibly associated with a terminal lobe of one of the jets. Both gamma-ray excesses are relatively far from the central binary, and the former shows evidence of a periodic variation at the precessional period of SS 433, linking it with the microquasar. This result challenges obvious interpretations and is unexpected from previously published theoretical models. It provides us with a chance to unveil the particle transport from SS 433 and to probe the structure of the magnetic field in its vicinity.
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The datasets generated and/or analysed during the current study are available from the corresponding author on reasonable request.
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The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work was performed in part under DOE Contract DE-AC02-76SF00515. J.L. acknowledges support from the Alexander von Humboldt Foundation and the National Natural Science Foundation of China via grant numbers NSFC-11673013 and NSFC-11733009. The work of D.F.T. was supported by grant numbers PGC2018-095512-B-I00, SGR2017-1383 and AYA2017-92402-EXP. J.L. and D.F.T. acknowledge discussions with the international team on ‘Understanding and unifying the gamma rays emitting scenarios in high mass and low mass X-ray binaries’ of the ISSI (International Space Science Institute), Beijing, as well as the support of the COST Action PHAROS (CA16214). E.d.O.W. acknowledges support from the Alexander von Humboldt Foundation. Work at the NRL is supported by NASA. We thank R. Bühler, F. Acero, J. Ballet, P. Bruel, S. Digel, G. Jóhannesson, D. J. Thompson and J. L. Racusin for their comments and suggestions. We thank P. Zhang for help with the weighted wavelet Z-transform. This publication uses data from the GALFA H i survey dataset obtained with ALFA on the Arecibo 305 m telescope. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968) and in alliance with Ana G. Méndez-Universidad Metropolitana and the Universities Space Research Association. The GALFA H i surveys were funded by the NSF through grants to Columbia University, the University of Wisconsin and the University of California.
The authors declare no competing interests.
Peer review information Nature Astronomy thanks Pol Bordas and the other, anonymous, reviewer(s) for their contribution to the peer review of this work.
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a, 100 MeV – 300 GeV counts map of the Fermi-LAT field of the SS 433 region. The microquasar itself is noted with a bold cross. The fitted position of Fermi J1913+0515 and west excess are shown with green crosses. The regions used to produce pulse profiles are shown with dotted circles. b, Folded pulse profile of PSR J1907+0602 above 300 MeV with an ROI of 0.6∘. Two rotational pulse periods are shown, with a resolution of 100 phase bins per period. The Bayesian block decomposition is shown by red lines. The off-peak interval (ϕ=0.697–1.136) is defined by black dotted lines. c, Folded pulse profile of the photons centered on SS 433 with a radius of 0.6∘ above 100 MeV, using the ephemeris of PSR J1907+0602. Two rotational pulse periods are shown, with a resolution of 25 phase bins per period. The vertical error bar in (b) and (c) indicates the 68% credible interval.
a, b, Fermi-LAT spectra of Fermi J1913+0515 (a) and the west excess (b).The maximum likelihood model (power law) fitted with gtlike is shown with a dashed line. The vertical error bar indicates the 68% credible interval and the upper limits are at the 99% confidence level.
Exposure-corrected Lomb-Scargle power spectra constructed from the 1–300 GeV weighted light curve of Fermi J1913+0515 covering the entire period range of the observation data (top panel, 0–700 days; bottom panel, 700–3800 days). The red dashed line indicates false alarm probability of 5% level corresponding to the full period range power spectra.
Precessional phase light curve of Fermi J1913+0515 flux (top panel) and TS values (bottom panel) in 1-300 GeV with a binning of 0.1. The vertical error bar indicates the 68% credible interval and the upper limits are at the 95% confidence level.
a, cumulative likelihood analysis during precession phase 0.0–0.5 and 0.5–1.0. The TS of Fermi J1913+0515 in precession phase 0.0-0.5 and 0.5-1.0 are shown with blue squares and red triangles. The ΔTS of the flux deviation from a constant are shown with black dots. The TS of the flux difference between two precessional phase bins are shown with green stars. b, 2D plane contour plotting for the WWZ power spectrum.
a, the contributions to 10 GeV cosmic rays at different distances from the injection point of 100 individual injection events, compared to the Galactic cosmic-ray sea (the black horizontal line). Each symbol/color represents a different distance (30, 35, 40, 45 and 50 pc) from injection to the interaction point. b, the cosmic-ray density at all energies. The green lines represent individual injection event (corresponding to 10, 20, 30... 100 in the x-axis of (a)), whereas the violet line shows the sum of the contribution of all injection events. c, the hadronic gamma-ray emission at 1 GeV at different distances. Symbol/color representations are the same with (a).
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Li, J., Torres, D.F., Liu, RY. et al. Gamma-ray heartbeat powered by the microquasar SS 433. Nat Astron 4, 1177–1184 (2020). https://doi.org/10.1038/s41550-020-1164-6
Nature Astronomy (2020)