We performed the spectroscopic observation of a possible supernova in UGC 5189A at Nov. 11.8 UT. This supernova was discovered by Jack Newton and Tim Puckett at Nov. 11.206 UT (CBET 2532). We performed the follow up observations in order to clarify the spectroscopic type of this new object using HOWPol equipped with Kanata telescope. The spectrum exhibits the emission lines of H-alpha and H-beta at 4900 and 6600 A. These emission lines show the multiple features with broader (~18000 km/s) and narrower (<500 km/s) components. The spectra also exhibit weak emission lines of HeI at 5900 and 7100 A. These spectral porifles are well similar to those of extremely luminous Type IIn SN 2006tf (Smith et al. 2008). Similar report was done by Benetti et al. (CBET 2536). The extremely high luminosity would be not only originated from the synthesized 56Ni decay but also the interactions of the ejecta with circumstellar material (CSM). This object allow us to study a history of mass loss in its progenitor. We will continue the observations of extremely luminous Type IIn SN 2010jl.
We update the data of 3C 454.3. Figure shows a light curve and a temporal variation of polarization degree of the object in the V band. There was a bright flare during JD 245500 with the high polarization degree. The peak of the flux during the flare was delayed 1 day compared with that of polarization degree. After the peak, polarization degree fell down to 10 %.
We performed photometric observations of Type Ia PTF10ygu. Light curves indicate that the rising time may be much longer than 17 - 19 days confrimed in a typical Type Ia SN. Unfortunately, our photometric points are too poor to estimate the rising time with a higher precision. In general, a more luminos SN Ia have a longer timescale of the light curve. However, even super luminous Type Ia SN have a rising time above 20 days (Yamanaka et al. 2009, Silverman et al.2010, Scalzo et al. 2010 and so on). If, the rising time are longer than a typical value for a SN Ia, this object might be an intrinsically luminous object.
We have monitored the blazar 3C 454.3 since 2008. The object was reported to be bright in the near-infrared and gamma-ray bands (ATel #2988 and #2995). We also confirmed this flare. Figure shows the light curve and the temporal variation of the polarization degree in the V band. The amplitude of the magnitude was about 1.1 mag from JD 2455496 to 2455502. The polarization degree in JD 2455502 was about 34 %, and was higher than that in the 2009 flare during Dec. 2009 (around JD 2455180).