Peremennye Zvezdy (Variable Stars) 34, No. 2, 2014 Received 15 May; accepted 20 May.

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Photometric observations of type II Supernovae 2009af and 2009ay

D. Yu. Tsvetkov

Lomonosov Moscow University, Sternberg Astronomical Institute, University Ave. 13, 119992 Moscow, Russia; e-mail: tsvetkov@sai.msu.su

1. Introduction

Supernovae (SNe) of type II are characterized by the presence of hydrogen in their spectra and large diversity of photometric properties. Barbon et al. (1979) suggested division of SNe II into two sub-classes: SNe II-P, which show a long-duration plateau in their photometric evolution, and SNe II-L, which have "linear" declining light curves. The physical reasons for this division and the degree of separation of the sub-classes are still a subject of investigations (cf., e.g., Anderson et al. 2014).

Continuing the long-term program of SN observations at Sternberg Astronomical Institute, we carried out photometry of SNe II 2009af and 2009ay.

SN 2009af was discovered by Cortini (2009) on February 16.75 UT at magnitude 15.0 during the supernova search with a 0.35-m telescope at Monte Maggiore Observatory. The SN is located at (equinox 2000.0), which is west and north of the center of the galaxy UGC 1551. Ciroi et al. (2009) report that a spectrogram (range 370-720 nm, resolution 1 nm) of SN 2009af, obtained on Feb. 18.76 UT at Asiago Observatory with the Galileo 1.22-m telescope shows it to be a type II supernova about 2-3 weeks after explosion. The spectrum of SN 2009af was obtained at the Kanata Observatory¹on February 21, it is typical of SNe II and shows similarity to the spectrum of SN 1993J near maximum light.

SN 2009ay was discovered by Puckett and Peoples (2009) at magnitude 16.4 on unfiltered CCD images taken with a 0.35-m reflector at Ellijay on Mar. 20.41 UT in the course of the Puckett Observatory Supernova Search. The new object was located at (equinox 2000.0), which is east and north of the center of NGC 6479.

Challis (2009) reports that a spectrum (range 360-800 nm) of 2009ay, obtained on Mar. 25 UT by W. Brown with the F.L. Whipple Observatory 1.5-m telescope, shows it to be a type II supernova. The spectrum shows featureless continuum with hints of broad H and H features. Soderberg and Brown (2009) observed SN 2009ay with the MMT/Blue Channel Spectrograph on Mar. 28.5 UT. They report that the spectrum clearly shows broad P Cygni hydrogen Balmer features superposed on a nearly featureless blue continuum, confirming the earlier report by Challis (2009). From the absorption minimum of the H line, they infer an expansion velocity of 9800 km/s after accounting for the recession velocity of the host galaxy. They further note that the spectrum resembles those of luminous and peculiar type II supernovae 2008es and 2005ap.

2. Observations and Light Curves

We carried out observations of SN 2009af and 2009ay with the following telescopes and CCD cameras: the 60-cm reflector of Crimean Observatory of Sternberg Astronomical Institute (C60), equipped with an Apogee AP-47 CCD camera; the 50/70-cm Maksutov telescope of Crimean Observatory (C50) with a Meade Pictor 416XT camera; the 70-cm reflector in Moscow (M70) with an Apogee AP-7p camera. The images of SN 2009af were obtained also with the 2-m Faulkes North telescope (F200). The standard image reductions and photometry were made using IRAF.² Photometric measurements of the SNe were made relative to local standard stars using PSF fitting with IRAF DAOPHOT package. Subtraction of host galaxy background was applied for the images of SN 2009af taken in September and November, 2009. The images used for subtraction were downloaded from the CASU archive³. All the images for SN 2009ay were corrected for the host galaxy background; we used the images obtained at the 1-m telescope of the Special Astrophysical Observatory (Russian Academy of Sciences) (SAO RAS) a year after the SN outburst for subtraction.

The magnitudes of local standards were calibrated on photometric nights, when photometric standards were observed at different air masses. They are reported in Table 1. Images of the SNe with marked local standards are shown in Figs. 1, 2. The results of photometry of the supernovae are presented in Tables 2, 3.

The light curves of SN 2009af are presented in Fig. 3. According to Ciroi et al. (2009), the most probable date of explosion is January 31 (JD 2454862). The first set of our observations started on February 19 and continued till March 14. The second set covered the period from September 1 to November 21. The maximum light is not traced by our observations, and the small length of the first set and the large gap in the observations do not allow us to perform a complete analysis of the light curves. We may conclude that the early decline after maximum was very fast, the rates (in mag/day) in the bands being 0.08 in , 0.027 in , 0.021 in . After the gap in observations, the rates are: 0.0093 in , 0.013 in , and 0.015 in . The fast early decline allows us to suppose that SN 2009af belongs to the type II-L. Indeed, the light curves of typical SNe II-L 1979C, 1980K, 1998S (Balinskaya et al. 1980; Buta 1982; Fassia et al. 2000) are a good match for the early part of the light curves of SN 2009af. However, the drop of brightness for the first 200 days past maximum is only 1.6 in the band, 2.0 in , and 3.1