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NO EVIDENCE OF INTRINSIC OPTICAL/NEAR-INFRARED LINEAR POLARIZATION FOR V404 CYGNI DURING ITS BRIGHT OUTBURST IN 2015: BROADBAND MODELING AND CONSTRAINT ON JET PARAMETERS

  • Authors: Y. T. Tanaka, R. Itoh, M. Uemura, Y. Inoue, C. C. Cheung, M. Watanabe, K. S. Kawabata, Y. Fukazawa, Y. Yatsu, T. Yoshii, Y. Tachibana, T. Fujiwara, Y. Saito, N. Kawai, M. Kimura, K. Isogai, T. Kato, H. Akitaya, M. Kawabata, T. Nakaoka, K. Shiki, K. Takaki, M. Yoshida, M. Imai, S. Gouda, Y. Gouda, H. Akimoto, S. Honda, K. Hosoya, A. Ikebe, K. Morihana, T. Ohshima, Y. Takagi, J. Takahashi, K. Watanabe, D. Kuroda, T. Morokuma, K. Murata, T. Nagayama, D. Nogami, Y. Oasa, and K. Sekiguchi

2016 The Astrophysical Journal 823 35.

  • Provider: AAS Journals

Caption: Figure 1.

Top: V-band light curve of V404 Cyg during the most active phase in 2015 June (taken from Kimura et al. 2016). Horizontal dashed line indicates the quiescent flux level of V = 18.6 (Wagner et al. 1991). The hatched orange rectangles indicate the Kanata/HONIR observation periods shown in detail in the bottom multipanel plots. Bottom left panels: Kanata/HONIR and Pirka/MSI polarimetric observations in MJD 57193. Note that the R-band magnitudes shown in the first panel are offset by 3.0 mag for illustrative purposes (i.e., the actual R-band magnitudes are 3.0 mag fainter). The two black arrows and gray rectangle in the first panel indicate the time ranges when Kanata/HONIR ﹩{{VRIJHK}}_{s}﹩ and Swift/XRT X-ray spectra were constructed, respectively (see also left panels in Figures 5 and 6). Bottom right panels: same as bottom left panels, but for the data in MJD 57194. A black horizontal arrow indicates the period when Kanata/HONIR multiband polarimetric observations were performed (see also Figure 4 and right panels of Figures 5 and 6).

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