TY - JOUR
T1 - Faraday tomography of the SS433 jet termination region
AU - Sakemi, Haruka
AU - Machida, Mami
AU - Ohmura, Takumi
AU - Ideguchi, Shinsuke
AU - Miyashita, Yoshimitsu
AU - Takahashi, Keitaro
AU - Akahori, Takuya
AU - Akamatsu, Hiroki
AU - Nakanishi, Hiroyuki
AU - Kurahara, Kohei
AU - Farnes, Jamie
N1 - Funding Information:
We carried out QU-fitting of the eastern region of W50, where a jet from SS433 seems to to be best-fitted with a two-Gaussian model. The southern terminal shock (region II) seems to have terminate. ATCAdataat1.3–3.0 GHz wereused for the analysis. The northern terminal shock (region I) tends to be best-fitted with a two-Gaussian model. The southern terminal shock (region II) seems to haveme cisosmiopnliccomaptoende fnetastluorcateesd. Tahroeu hnedli0carla dstrmu−ct2uarne d(r3e0g0iornad IImI) −a2n. The Gda ltahceti csoeumthisesrionn paarrotu onfd th0er afidlamm−en2t (regipoons sIiVb)lytceonrdre stpo obned sbetostt-heffiotrteedg rowuintdh oafWth5r0e.eW-Geaalussosiiadenntmifyodeemlis.sFioronmfr oomurW 5a0nwailtyhsiins, ϕw=e −1id12enti fy candidateGalact−2icemissioncomponentslocatedaround 0radm and 300 rad m. The Galactic emission around 0 radm−2possiblycorresponds to the foregroundof W50. We also identify emission component in this region. −2 from W50within φ= −112 to228rad m . Note thatwe could not identifyany emission from W50 in the soAuutthhoerrCnontterribmuitnioanls:sIhnovceskti g(arteigoni,oHn .SII.;)R.eWsoue rmcesa, Sy.I.n,eYe.Md. ahnidghJ.Fe.r; Ssoeftnwsairtei,vSit.I.yanddaYta.Mw.; Situhpewrviidsieorn,fMre.Mqu.;enc y coveraWrge to diiting—oristiginnalguish the component in thidraft,H.S.;Writing—reviewandediting,sregion. M.M.,T.O.,K.T.,T.A.,H.A.,H.N.,K.K.andJ.F. Funding: This work is financially supported in part by a Grant-in-Aid for Scientific Research (KAKENHI) from JSPS (P.I. MM:23740153, 16H03954). K.T’s work is partially supported by Grand-in-Aid from the Ministry of Education, Culture, Sports, and Science and Technology (MEXT) of Japan, No. 15H05896, 16H05999 and 17H01110, and Bilateral Joint Research Projects of JSPS. H.A acknowledges the support of NWO via a Veni grant. SRON is supported financially by NWO, The Netherlands Organization for Scientific Research.
Funding Information:
We are grateful to M. Haverkorn, and S. P. O'Sullivan for useful discussion. We thank the Cosmic Magnetism Science Working Group of the Japan SKA Consortium for supporting our research. We also thank the SOC of "The Power of Faraday Tomography" for providing the opportunity to present our study. This work is financially supported in part by a Grant-in-Aid for Scientific Research (KAKENHI) from JSPS (P.I. MM:23740153, 16H03954). K.T's work is partially supported by Grand-in-Aid from the Ministry of Education, Culture, Sports, and Science and Technology (MEXT) of Japan, No. 15H05896, 16H05999 and 17H01110, and Bilateral Joint Research Projects of JSPS. H.A acknowledges the support ofNWOvia a Veni grant. SRON is supported financially by NWO, The Netherlands Organization for Scientific Research
Publisher Copyright:
© 2018 by the authors.
PY - 2018/12/9
Y1 - 2018/12/9
N2 - A jet termination region provides us with useful information about how a jet interacts with the interstellar medium. Identifying the strength and orientation of magnetic fields at the terminal is crucially important to understanding the mechanism of cosmic-ray acceleration. In this article, we report results of our Faraday-tomography analysis of the eastern region of the radio nebula W50, where a jet from the microquasar SS433 seems to terminate. We apply QU-fitting, a method of Faraday-tomography, to data from the Australia Telescope Compact Array (ATCA) at 1.3-3.0 GHz. In the analysis, we distinguish multiple polarized sources along the line of sight. We identify Galactic emission candidates at Faraday depths around 0 rad m-2 and 300 rad m-2. The Galactic emission around 0 rad m-2 is possibly located in front of W50. We also find emission from W50 with Faraday depths between ϕ = -112 to 228 rad m-2.
AB - A jet termination region provides us with useful information about how a jet interacts with the interstellar medium. Identifying the strength and orientation of magnetic fields at the terminal is crucially important to understanding the mechanism of cosmic-ray acceleration. In this article, we report results of our Faraday-tomography analysis of the eastern region of the radio nebula W50, where a jet from the microquasar SS433 seems to terminate. We apply QU-fitting, a method of Faraday-tomography, to data from the Australia Telescope Compact Array (ATCA) at 1.3-3.0 GHz. In the analysis, we distinguish multiple polarized sources along the line of sight. We identify Galactic emission candidates at Faraday depths around 0 rad m-2 and 300 rad m-2. The Galactic emission around 0 rad m-2 is possibly located in front of W50. We also find emission from W50 with Faraday depths between ϕ = -112 to 228 rad m-2.
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U2 - 10.3390/galaxies6040137
DO - 10.3390/galaxies6040137
M3 - Article
AN - SCOPUS:85059381338
SN - 2075-4434
VL - 6
JO - Galaxies
JF - Galaxies
IS - 4
M1 - 137
ER -