ner_tags: O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O B-Formula I-Formula I-Formula O O O O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O B-Wavelength O O O O O O B-Citation O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O B-Wavelength O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation O B-Citation O B-Citation O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O B-CelestialObject I-CelestialObject O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O B-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O B-Citation O B-Citation O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O B-Citation O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O B-Wavelength O O B-Wavelength O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O
tokens: cooling break signature does not appear in the spectrum. Since some young PWNe have a soft injection spectrum of p 2 ∼ −3.0, we also study such PWNe. Figure 2 shows model spectra for the small magnetic field cases ( B , p 2 ) = (3 μ G, −3.0). The braking index is different for the left ( n = 3) and the right ( n = 2) panels, and then we search for the value of γ b for the calculated X-ray flux to be close to F O11 . In both cases, a large TeV γ -ray flux is predicted when compared with Figure 1 without increasing the energy density of the ISRF ( u IR , u OPT ). 4. DISCUSSION AND CONCLUSIONS Considering the plasma outflows from the magnetar, we build a broadband emission model of MWNe based on the one-zone model of young PWNe around RPPs ( TT10 , TT11 , TT13b ). The model is simplified for application to MWNe that have less observational information than PWNe. We apply the model to the MWN around 1E 1547.0-5408, which is the most promising object for detecting MWNe among all the known magnetars because of its large L spin and its small distance to the Earth. Because of poor current observational constraints on the MWN around 1E 1547.0-5408, various combinations of parameters are allowed. However, here, we compare Models 1 and 2 based on past studies of young PWNe, especially focusing on Kes 75 around PSR J1846-0258, which is the only HBP showing a magnetar-like behavior (Gavriil et al. 2008 ). Model 1 has η and γ b similar to Kes 75, while Model 2 has a similar magnetic field strength B . It is known that the mean magnetic field B is very different for each young PWN 3 ≲ B ≲ 80 μ G (e.g., TT13b ; Torres et al. 2014 ). On the other hand , TT11 and TT13b showed that η ∼ 10 −3 is common among young PWNe, except for Kes 75, by using almost the same model as this study, i.e., adopting ( α R , α B ) = (1.0, −1.5) in Equations ( 7 ), ( 8 ), and ( 10 ). Kes 75 has an exceptionally small η compared to other young PWNe for our model and also for other models, although the values of η are different among models (Bucciantini et al. 2011 ; Torres et al. 2014 ). We favor Model 1 over Model 2 because we expect that magnetars have the wind property η and γ b similar to HBPs, where γ b is related to the bulk Lorentz factor of the wind just upstream the termination shock (e.g., Kennel Coroniti 1984 ; Bucciantini et al. 2011 ). Models 3 and 4 are cases for the soft injection spectrum p 2 = −3 and the large break Lorentz factor ( γ b ≫ 10 6 ), although such γ b and p 2 are not typical among young PWNe ( TT13b ). Both models are interesting because they predict a larger TeV γ -ray flux than Model 1 without increasing the local ISRF ( u IR , u OPT ). For example, the γ -ray flux increases if the photons from the nearby star-forming region contribute to the local ISRF ( Torres et al. 2014 ). Model 3 is brighter than Model 2 in TeV γ -rays because the injection of the high energy particles is an increasing function of γ b . Model 4 predicts larger TeV γ -ray flux