We present the preliminary light curve of SN 2009ig. The brightness have not still reached maximum. We also derived the magnitude of comparison stars. We performed the imaging of the standard stars from Landolt star catalogue (Landolt 1992). , when the photometric standard was in as high airmass as the object.
We updated J- and H-band light curves on Aug. 30. Decline trends are continue in both bands.
We performed near-infrared photometry of V5583 Sgr. As can be seen in the figure, our preliminary results shows that the nova faded rapidly from the maximum brightness. The decline rate in J is slightly smaller than that in H band. This would be explained by the contribution of the prominent Pa-beta emission in J band.
■ [blazar] QSO 0133+476 : faded
The figure shows the light curve of the object and the temporal variation of polarization degree in V band. The object was faded and the amplitude was about 1.4 . The polarization degree has been high.
The object has brightened since JD 2455050, and reached the maximum of V~14.3. We will continue to observe this object.
We update spectra of V5583 Sgr. Bluer components in the H-alpha & the H-beta have weakened with time.
We updated near-infrared spectra of V2672 Oph. The last spectra (blue line) was obtained on 24 Aug. 2009. The rapid change of line profiles in the Pa-beta and the Pa-gamma are seen in our spectra. These spectra indicate that gas density of the nova would be rapidly changing in the expanding ejecta.
We have started the B,V,Rc,Ic-band photometry of SN 2099ig in NGC 1015 (z=0.01) since Aug. 22 (UT). SN 2009ig was discovered on Aug. 20.5. Therefore, the object was classified as very young Type Ia supernova by Navasardyan et al.(2009). The blueshifted line velocity of SiII6355 reached 24,000km/s. Our preliminary multicolor photometric results indicated that the luminosity increased >0.5 mag in a day and the color rapidly become blue. These phenomena would be consistent with the characteristics of a young Type Ia SN. We encourage the spectroscopic and photometric observations for this exciting object!
The upper figure shows our preliminary spectra of V2672 Oph(= Nova Oph 2009) observed by HSspec. The object rapidly declined within a week. On 22 August, our observation detected only the H-alpha emission because of the low S/N ratio. The profile of the H-alpha emission have significantly changed. Three components of the H-alpha emission was also reported in the 1999 outburst of U Sco (e.g. Iijima 2002, A&A, 387, 1013).
The lower figure shows near-infrared spectra of the nova by TRISPEC. The Pa-beta(1.2818 um) emission profile is similar to that of the H-alpha. Three components are observed at the Pa-beta. Howver, the profile of the Pa-gamma would not be similar to Pa-beta or H-alpha. The He I emission might be blended in Pa-gamma.
We show optical spectra of V5583 Sgr obtained by KANATA/HSspec in the figure. Balmer and Fe II emissions are strong. The nova is still bright and the spectral feature indicates that the nova is a Fe II-type nova. The development of H-alpha and H-beta is interesting. Bluer components weaken with time compared with redder ones. The FWHM of balmar line is about 2600 km/s.
We performed an optical spectroscopic observation of Nova Oph 2009 (CBET 1910, CBET 1919, CBET 1912) on Aug. 18. The left panel shows our spectrum with a range of 4300-6800A. The H-alpha emission line shows a complex and asymmetric structure. The H-beta emission is also seen in our spectrum. The right panel shows the H-alpha emission in the velocity form (centered by 6563A). We found five peaks of H-alpha in the spectrum. The most blue- and red-shifted components are peaked at -3000 km/s and 3300 km/s from the H-alpha center, respectively. The intensity of the red components is stronger than that of the blue component. A Similar profile is found in the emission of the Pa-beta (see the previous report). Our spectrum indicates that nova ejecta asymmetrically distributed in Nova Oph 2009.
The figure shows the NIR spectrum of Nova Oph 2009 on Aug.18. The nova shows strong and broad emission lines at Pa-beta and Pa-gamma. Br series emission lines are not strong yet. Our rough estimation of the FWHM of Pa-beta gives about 6400 km/s assuming a single gaussian prifile.
We started near-infrared spectroscopic observation of V5583 Sgr on 2009 Aug. 7. The figure shows our preliminary NIR spectra. On Aug. 7, the object shows a strong blue continuum emission from a pseudo-photosphere. After a week, the photospheric component decayed and strong hydrogen lines (Pa and Br series) become strong. On Aug. 17, the spectrum is similar to that on Aug. 14.
The figure shows our optical spectra of V5583 Sgr(IAUC 9061). The spectra obtained on Aug. 14 shows double-peaked and flat-topped profiles at H-apha and H-beta emissions, respectively. Until Aug. 17, some Fe II emission lines and blue components of H-alpha and H-beta emissions significantly weaken. The FWHM of H-alpha emission is about 2900 km/s on Aug. 17.
We performed optical spectroscopic observation of Nova Sgr 2009 #3 (CBET 1899) on 07 Aug using KANATA/High Speed Spectrograph. The spectrum is shown in the figure. The H-a emission line showed an asymmetric profile. The FWHM of the Ha emission line was about 2100 km/s. The FeII emission and possible NaD absorption lines were seen.