Near-infrared monitoring of the accretion outburst in the massive young stellar object S255-NIRS3

Abstract We followed up the massive young stellar object S255-NIRS3 (= S255-IRS1b) during its recent accretion outburst event in the $K_{\rm s}$ band with Kanata/HONIR for four years after its burst and obtained a long-term light curve. This is the most complete near-infrared light curve of the S255...

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Veröffentlicht in:Publications of the Astronomical Society of Japan 2020-02, Vol.72 (1)
Hauptverfasser: Uchiyama, Mizuho, Yamashita, Takuya, Sugiyama, Koichiro, Nakaoka, Tatsuya, Kawabata, Miho, Itoh, Ryosuke, Yamanaka, Masayuki, Akitaya, Hiroshi, Kawabata, Koji, Yonekura, Yoshinori, Saito, Yu, Motogi, Kazuhito, Fujisawa, Kenta
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Sprache:eng
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Zusammenfassung:Abstract We followed up the massive young stellar object S255-NIRS3 (= S255-IRS1b) during its recent accretion outburst event in the $K_{\rm s}$ band with Kanata/HONIR for four years after its burst and obtained a long-term light curve. This is the most complete near-infrared light curve of the S255-NIRS3 burst event that has ever been presented. The light curve showed a steep increase reaching a peak flux that was 3.4 mag brighter than the quiescent phase and then a relatively moderate year-scale fading until the last observation, similar to that of the accretion burst events such as EXors found in lower-mass young stellar objects. The behavior of the $K_{\rm s}$-band light curve is similar to that observed in 6.7 GHz class II methanol maser emission, with a sudden increase followed by moderate year-scale fading. However, the maser emission peaks appear 30–50 d earlier than that of the $K_{\rm s}$ band emission. The similarities confirmed that the origins of the maser emission and the $K_{\rm s}$-band continuum emission are common, as previously shown from other infrared and radio observations by Stecklum et al. (2016, Astronomer’s Telegram, 8732), Caratti o Garatti et al. (2017b, Nature Phys., 13, 276), and Moscadelli et al. (2017, A&A, 600, L8). However, the differences in energy transfer paths, such as the exciting/emitting/scattering structures, may cause the delay in the flux-peak dates.
ISSN:0004-6264
2053-051X
DOI:10.1093/pasj/psz122