We observed V5579 Sgr on Sep. 21 in V- and H-band. The nova formed the dust just after the maximum and faded in optical bands.
Recently, the object has, gradually, recovered in V and faded in H due to decrease of the dust opacity.
The figure shows that the lightcurve and Polarization degree in V band of the object.
The figure shows that lightcurve and Polarization degree in V band of the object.
This object has been decreasing of the Polarization degree in these days.
We have been observing 3C 273 since 11 December 2008.
The figure shows that the lightcurve and polarization degree in V band of the object.
The object has a low polarization degree.
We update the data of 3C 66A.The figure shows that the lightcurve and polarization degree in V band.
The polarization of the object has decreased these days since we have been observed.
We started the optical observations of SN 2009af. SN 2009af was discovered in nearby galaxy UGC1551 by G,Cortini, Italy (CBET1697). Thereafter, the spectroscopic observations were performed by S, Ciroi et al. The spectrum showed the typical characteristics of Type II supernova. We also obtained optical several spectra using 1.5m-KANATA telescope with TRISPEC in Feb. 21 2009. We combined to the average spectrum using the "scombine" task in IRAF. The spectrum showed the strong P-Cyg profile of H-alpha. We compared the spectrum of SN 2009af with that of Type IIb SN 1993J around maximum light. The two spectra showed similar profile. SN 2009af might be striped-envelope SN, as Type Ib/Ic/IIb. We will continue the observations of SN 2009af.
We have performed photometric observations of SN 2008hy. The light curve began to show the slower decline, which means that the brightness variation would constantly evolve in Co decay phase.
We have performed optical observations of Type IIP SN 2008in in M61. The preliminary photometric results indicates that the light curve might show the anomalous behavior unlike typical Type IIP supernova. The each band light curve rapidly declines in a short time scale. Thereafter, the V,R,Ic-band light curve look like to start to evolve in the plateau phase. Especially, The R-band light curve increased slowly.
The spectroscopic absorptions of SN 2008in are narrower than those of SN 2008ij, which indicates that the expanding velocity of SN 2008in is slower than that of SN 2008ij. The P-Cyg profile of HI becomes stronger than that of before phase. which suggest that the first hydrogen diffusion phase would be still continued. We will continue the observations of SN 2008in.
We have performed the spectroscopic observations of Type IIP SN 2008ij on Feb.1 and Feb.11 2009. The spectra began to show stronger P Cyg profile of HI6563 than that of before phase. The line velocity of HI6563 declines, as the flux of emission and absorption lines becomes strong. We can confirm the Na I D line at 5800A in Feb.1 2009. The Na I D and Ca IR triplet deepened as time evolved. We will continue the observations of this object.
V5579 Sgr is a dust forming classical nova. We performed spectroscopic observations of the nova in Optical and NIR bands (0.47-2.35 micron). The figure shows our preliminary spectra on 2008 April 20, May 07 and May 14.
Our first spectrum was obtained at the pre-maximum phase (20 Apr.). The second spectrum shows strong hydrogen lines and CI lines. The prominent CI lines are also observed in past novae V2274 Cyg and V1280 Sco, which also went on to form dust (Rudy et al. 2003 and Das et al. 2008). The last spectrum was obtained on 14 May. In this epoch, the NIR continuum flux increased due to dust formation.