■ [blazar] S5 0716+714 : rising the polarization degree
The figure shows the light curve and the temporal variation of the object in the V band. The polarization degree of the object became high, about 24 %. The polarization degree of the object has been typically low compared with other High Polarized Quasars (HPQs), less than 10 % in our dense monitoring from 2008 to 2010. However, the object was in the high polarized state during JD 2455180. In current state, the object was similar in the high polarized state.
We have performed the photometric observations of normal Type Ia SN 2010Y. We confirmed that the secondary maximum of I-band light curve had already passed.
We update the light curve of the Type Ic SN 2010ah (= PTF10bzf).
■ [Symbiotic Nova] Spectroscopy of V407 Cyg : observations start
We have started the spectroscopic observations of symbiotic nova since Mar. 18 (UT). The spectrum shows the strong emissions of the Balmer and Paschen series. The HeI, FeII and OI are also seen in this spectrum. This object is confirmed as a symbiotic star, which is consists of the white dwarf and the Mira-type star. When a nova eruption occurs in such a system, we expect to confirm the emissions line of the higher excitations level due to the interactions of nova ejecta with the circumstellar material. In the case of RS Oph, the highly excited emissions line were clearly detected in their spectra (Iijima 2009). We continue the spectroscopic observations of the symbiotic nova V407 Cyg.
We have started the photometric observations of the broad-lined Type Ic PTF10bzf (=SN 2010ah) since Mar. 11. The rapid decline of the light curve indicates that the this SN have already missed around the maximum light. We will observe this object.
V1280 Sco is the peculiar slow novae, whose early photometry in optical and near-infrared regions indicates that the dust formation have undergone just after its maximum light. After the rapidly fading in the light curve, the luminosity has slowly been increasing in 3 years and the recent apparent magnitude was reported of ~10.7 mag from AAVSO. We performed the spectroscopy for V1280 Sco at 2010 Mar. 11 (UT). The spectrum dominated the emissions of Balmer series, HeI and OI. Especially, the HeI clearly shows the P-Cyg profile. This result suggests that the expanding shell would be optically thick.