%0 Journal Article
%T Variable optical polarization during high state in gamma-ray loud narrow line Seyfert 1 galaxy 1H 0323+342
%A Ryosuke Itoh
%A Yasuyuki T. Tanaka
%A Hiroshi Akitaya
%A Makoto Uemura
%A Yasushi Fukazawa
%A Yoshiyuki Inoue
%A Akihiro Doi
%A Akira Arai
%A Hidekazu Hanayama
%A Osamu Hashimoto
%A Masahiko Hayashi
%A Hideyuki Izumiura
%A Yuka Kanda
%A Koji S. Kawabata
%A Kenji Kawaguchi
%A Nobuyuki Kawai
%A Kenzo Kinugasa
%A Daisuke Kuroda
%A Takeshi Miyaji
%A Ryo Miyanoshita
%A Yuki Moritani
%A Tomoki Morokuma
%A Katsuhiro L. Murata
%A Takahiro Nagayama
%A Yumiko Oasa
%A Tomohito Ohshima
%A Takashi Ohsugi
%A Yoshihiko Saito
%A Mahito Sasada
%A Kazuhiro Sekiguchi
%A Yuhei Takagi
%A Jun Takahashi
%A Katsutoshi Takaki
%A Takahiro Ui
%A Makoto Watanabe
%A Masayuki Yamanaka
%A Michitoshi Yoshida
%J Physics
%D 2014
%I arXiv
%R 10.1093/pasj/psu095
%X We present results of optical polarimetric and multi-band photometric observations for gamma-ray loud narrow-line Seyfert 1 galaxy 1H 0323+342. This object has been monitored by 1.5 m Kanata telescope since 2012 September but following a gamma-ray flux enhancement detected by Fermi-LAT on MJD 56483 (2013 July 10) dense follow-up was performed by ten 0.5-2.0 m telescopes in Japan over one week. The 2-year R_C-band light curve showed clear brightening corresponding to the gamma-ray flux increase and then decayed gradually. The high state as a whole lasted for ~20 days, during which we clearly detected optical polarization from this object. The polarization degree (PD) of the source increased from 0-1% in quiescence to ~3% at maximum and then declined to the quiescent level, with the duration of the enhancement of less than 10 days. The moderate PD around the peak allowed us to precisely measure the daily polarization angle (PA). As a result, we found that the daily PAs were almost constant and aligned to the jet axis, suggesting that the magnetic field direction at the emission region is transverse to the jet. This implies either a presence of helical/toroidal magnetic field or transverse magnetic field compressed by shock(s). We also found small-amplitude intra-night variability during the 2-hour continuous exposure on a single night. We discuss these findings based on the turbulent multi-zone model recently advocated by Marscher (2014). Optical to ultraviolet (UV) spectrum showed a rising shape in the higher frequency and the UV magnitude measured by Swift/UVOT was steady even during the flaring state, suggesting that thermal emission from accretion disk is dominant in that band.
%U http://arxiv.org/abs/1405.3731v2