Yifan Xiao’s research while affiliated with Yunnan University and other places

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Publications (4)


Multi-wavelength Non-thermal Radiative Properties of Pulsar Wind Nebulae with Ages Around 10 kyr
  • Article

May 2025

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1 Read

Publications of the Astronomical Society of the Pacific

Keyao Wu

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Yifan Xiao

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Huan Yu

With the advancement of detector technology, significant progress has been made in understanding Pulsar Wind Nebulae (PWNe) through multi-wavelength observations, particularly in the X-ray and TeV γ -ray bands. While young PWNe have been extensively studied, PWNe with ages around 10 kyr remain relatively underexplored. In this study, we investigate the radiative properties of four selected PWNe associated with the γ -ray sources HESS J1420-607, HESS J1418-609, HESS J1427-608, and HESS J1303-631 using a time-dependent electron population model. High-energy electrons and positrons are injected into the nebula, producing multi-wavelength non-thermal emission through synchrotron radiation and inverse Compton scattering. Based on comparisons with previous studies, we assume that four sources have not yet been compressed by the reverse shock, with estimated ages around 7–8 kyr. The injected particles follow a broken power-law distribution, with spectral indices consistent with previous studies. We find that the four nebulae are currently particle-dominated systems with magnetic field strengths ranging from a few μ G to 10 μ G, in agreement with theoretical expectations for PWNe at similar evolutionary stages. Our results support the scenario that all four sources originate with PWNe, as their multi-wavelength nonthermal emission can be reproduced with reasonable parameters.


Figure 1. Fermi-LAT TS map centered on the SrcX region in the 10-500 GeV range. Left panel: TS map including all sources from the 4FGL catalog. Right panel: TS map after subtracting all sources containing SrcX. The blue diamond represents the position of PSR J1849-0001. The red diamond represents the position of 4FGL-DR4 sources. The positions of 1LHAASO J1848-0001u and HESS J1849-000 are marked with cyan and green circles, respectively.
Figure 2. Light curve of SrcX of 10-500 GeV for 10 time bins. The time bin is set to the upper limits with a 95% confidence level when the TS value < 4. The gray histogram is used to mark the TS value for each time bin with a TS value > 4.
Figure 3. The Fermi-LAT spectral data analysis results (marked as black dots) of SrcX in the 10-500 GeV band. The gray histogram represents the TS value for each energy bin. A power-law spectrum with an index of 1.94 ± 0.28 for the GeV data is plotted by the blue solid line, and its 1σ statistical error is represented by the blue dashed lines. The red and green dots display the TeV γ-ray data observed by HESS (H.E.S.S. Collaboration et al. 2018a) and ASγ (Amenomori et al. 2023), respectively.
Spatial Distribution Analysis for SrcX with Two Types of Spatial Models in 10-500 GeV
Observed Energy Flux of SrcX with Fermi-LAT
Likely Detection of GeV γ-Ray Emission from Pulsar Wind Nebula G32.64+0.53 with Fermi-LAT
  • Article
  • Full-text available

August 2024

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8 Reads

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6 Citations

The Astrophysical Journal

In this study, we report the likely GeV γ -ray emissions originating from the pulsar PSR J1849-0001's pulsar wind nebula (PWN) G32.64+0.53. Our analysis covers approximately 14.7 yr of data from the Fermi Large Area Telescope Pass 8. The position of the source and its spectrum matches those in X-ray and TeV energy bands, so we propose that the GeV γ -ray source is indicative of PWN G32.64+0.53. We interpret the broadband spectral energy distribution (SED) using a time-dependent one-zone model, which assumes that the multiband nonthermal emission of the target source can be generated by synchrotron radiation and inverse Compton scattering (ICS) of the electrons/positrons. Our findings demonstrate that the model substantially elucidates the observed SED. These results lend support to the hypothesis that the γ -ray source originates from the PWN G32.64+0.53 powered by PSR J1849-0001. Furthermore, the γ -rays in TeV bands are likely generated by electrons/positrons within the nebula through ICS.

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Likely detection of GeV {\gamma}-ray emission from pulsar wind nebula G32.64+0.53 with Fermi-LAT

August 2024

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1 Read

In this study, we report the likely GeV {\gamma}-ray emissions originating from the pulsar PSR J1849-0001's pulsar wind nebula (PWN) G32.64+0.53. Our analysis covers approximately 14.7 years of data from the Fermi Large Area Telescope (Fermi-LAT) Pass 8. The position of the source and its spectrum matches those in X-ray and TeV energy bands, so we propose that the GeV {\gamma}-ray source is indicative of PWN G32.64+0.53. We interpret the broadband spectral energy distribution (SED) using a time-dependent one-zone model, which assumes that the multi-band non-thermal emission of the target source can be generated by synchrotron radiation and inverse Compton scattering (ICS) of the electrons/positrons. Our findings demonstrate that the model substantially elucidates the observed SED. These results lend support to the hypothesis that the {\gamma}-ray source originates from the PWN G32.64+0.53 powered by PSR J1849-0001. Furthermore, the {\gamma}-rays in TeV bands are likely generated by electrons/positrons within the nebula through Inverse Compton Scattering.


Analysis of γ-ray emission above 30 GeV from the LMC pulsar wind nebula N 157B with Fermi-LAT

September 2023

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19 Reads

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5 Citations

Monthly Notices of the Royal Astronomical Society

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Yifan Xiao

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Liancheng Zhou

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[...]

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N 157B located in the large Magellanic Cloud is the first pulsar wind nebula detected outside of the Galaxy in γ-rays. In this paper, we analyse the emission above 30 GeV from N 157B using ∼14.3 yr of Fermi-LAT data. The γ-ray spectrum between 30 and 500 GeV is well-described by a single power-law function with a photon index of 1.83 ± 0.26, and its integral photon flux is (4.10 ± 0.83) × 10⁻¹¹ photons cm⁻² s⁻¹. We adopt a one-zone leptonic model to investigate whether the multiband non-thermal emission of the target source can be generated by synchrotron radiation and inverse Compton scattering of the electrons/positrons. Assuming the electrons/positrons in the nebula have a broken power-law spectrum with two breaks, the model can reproduce the observed fluxes in the radio, X-ray and γ-ray bands. This result indicates that the γ-ray emission from N 157B can be explained by the leptonic process of electrons/positrons via inverse Compton scattering.

Citations (2)


... Recently, in many papers, the Fermi-LAT data have been analyzed to investigate the emission from extended teraelectronvolt halos (M. Di Mauro et al. 2021;J. Li et al. 2021;S. Abe et al. 2023;X. Guo & Y. Xin 2024;Y. Xiao et al. 2024). Fermi-LAT data analysis is very useful in exploring the gigaelectronvolt counterparts of the teraelectronvolt sources and subsequently identifying their origin. If both an SNR and pulsar are present within the teraelectronvolt halo, in some cases with the spatial position and morphology of the extended emission in the Fermi-LAT energy ...

Reference:

Unraveling the Nature of HAWC J1844–034 with Fermi-LAT Data Analysis and Multiwavelength Modeling
Likely Detection of GeV γ-Ray Emission from Pulsar Wind Nebula G32.64+0.53 with Fermi-LAT

The Astrophysical Journal