The 400 Day Rise of SN 2008iy

SN 2008iy: An Unusual Type IIn Supernova with an Enduring 400 Day Rise Time

A. A. Miller, J. M. Silverman, N. R. Butler, J. S. Bloom, R. Chornock, A. V. Filippenko, M. Ganeshalingam, C. R. Klein, W. Li, P. E. Nugent, N. Smith, and T. N. Steele.
Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA.
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA.
Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA.
E-mail: amiller@astro.berkeley.edu.Sloan Research Fellow.
Abstract

We present spectroscopic and photometric observations of the Type IIn supernova (SN) 2008iy. SN 2008iy showed an unprecedentedly long rise time of 400 days, making it the first known SN to take significantly longer than 100 days to reach peak optical luminosity. The peak absolute magnitude of SN 2008iy was mag, and the total radiated energy over the first 700 days was 2 erg. Spectroscopically, SN 2008iy is very similar to the Type IIn SN 1988Z at late times, and, like SN 1988Z, it is a luminous X-ray source (both supernovae had an X-ray luminosity erg s). SN 2008iy has a growing near-infrared excess at late times similar to several other SNe IIn. The H emission-line profile of SN 2008iy shows a narrow P Cygni absorption component, implying a pre-SN wind speed of 100 km s. We argue that the luminosity of SN 2008iy is powered via the interaction of the SN ejecta with a dense, clumpy circumstellar medium. The 400 day rise time can be understood if the number density of clumps increases with distance over a radius 1.7 cm from the progenitor. This scenario is possible if the progenitor experienced an episodic phase of enhanced mass loss 1 century prior to explosion or if the progenitor wind speed increased during the decades before core collapse. We favour the former scenario, which is reminiscent of the eruptive mass-loss episodes observed for luminous blue variable (LBV) stars. The progenitor wind speed and increased mass-loss rates serve as further evidence that at least some, and perhaps all, Type IIn supernovae experience LBV-like eruptions shortly before core collapse. We also discuss the host galaxy of SN 2008iy, a subluminous dwarf galaxy, and offer a few reasons why the recent suggestion that unusual, luminous supernovae preferentially occur in dwarf galaxies may be the result of observational biases.

keywords:
supernovae: general — supernovae: individual (SN 2008iy, SN 1988Z) — stars: mass-loss — circumstellar matter
pagerange: SN 2008iy: An Unusual Type IIn Supernova with an Enduring 400 Day Rise TimeReferencespubyear: 2009

1 Introduction

The recent development of synoptic, wide-field imaging has revealed an unexpected diversity of transient phenomena. One such example is the discovery of a new subclass of very luminous supernovae (VLSNe; e.g., Ofek et al. 2007; Smith et al. 2007; Quimby et al. 2007b). While events of this nature are rare (Miller et al., 2009a; Quimby et al., 2009), each new discovery serves to bracket our understanding of the physical origin of well-established classes of SNe and does, in principle, demand an increased clarity in our understanding of the post-main-sequence evolution of massive stars.

Yet another unusual transient was discovered by the Catalina Real-Time Transient Survey (CRTS; Drake et al. 2009a), which they announced via an ATel as CSS080928:160837+041626 on 2008 Oct. 07 UT111UT dates are used throughout this paper unless otherwise noted. (Drake et al., 2008). The transient was classified as a Type IIn SN with a spectrum taken on 2009 Mar. 27 (Mahabal et al. 2009; see Schlegel 1996 for a definition of the SN IIn subclass, and Filippenko 1997 for a review of the spectral properties of SNe). The SN was later given the IAU designation SN 2008iy (Catelan et al., 2009). Mahabal et al. (2009) noted that the transient was present on CRTS images dating back to 2007 Sep. 13; however, it went undetected by the CRTS automated transient detection software until 2008 because it was blended with a non-saturated, nearby (11 separation) star.

Here, we present our observations and analysis of SN 2008iy, which peaked around 2008 Oct. 29 (Catelan et al., 2009) and had a rise time of 400 days. This implies that SN 2008iy took longer to reach peak optical brightness than any other known SN. Type II SN rise times are typically 1 week (e.g., SNe 2004et and 2006bp, Li et al. 2005; Quimby et al. 2007a; see also Patat et al. 1993; Li et al. 2010a), and have never previously been observed to rise 100 days, let alone 400, making SN 2008iy another rare example of the possible outcomes for the end of the stellar life cycle. In addition to an extreme rise time, SN 2008iy is of great interest because the unique circumstellar medium (CSM) in which it exploded may provide a link to very long-lived SNe, such as SN 1988Z, and thus provide clues into the nature of their progenitors.

This paper is organised as follows. Section 2 presents the observations. The data are analysed in Section 3, and the results are discussed in Section 4. We give our conclusions, as well as predictions for the future behaviour of SN 2008iy, in Section 5.

2 Observations

2.1 Photometry

The field of SN 2008iy, which is located at = 160837.27, = +041626.5 (J2000), was imaged multiple times by the Palomar Quest survey, and those data have been reprocessed as part of the Deep Sky project222http://supernova.lbl.gov/nugent/deepsky.html. (DS; Nugent 2009). The best constraints on the explosion date come from DS imaging: in a coadd of two images from 2007 Jul. 05, we do not detect the SN down to a 3 limit of mag. DS images are best approximated by the Sloan Digital Sky Survey (SDSS; Adelman-McCarthy et al. 2008) -band filter. The field of SN 2008iy has well-calibrated SDSS photometry which we use to calibrate the DS images. The observed DS magnitudes are shown in Fig. 1 and summarised in Table 1.

Figure 1: Left: Apparent optical light curve of SN 2008iy showing the long rise time of the SN, including data from Deep Sky (this work), the Nickel telescope (this work), Catelan et al. (2009), and the CRTS website. Note: conservatively, we take the start time of the SN () to coincide with the first epoch where CRTS detects the source; however, the true explosion date is likely prior to 2007 Sep. 13, between the last Deep Sky non-detection and the first CRTS detection. Notice that the light curve is very broad, and almost symmetric about the peak. For comparison we show the light curve of the standard Type II-P SN 1999em (data from Leonard et al. 2002) and the Type IIn SN 1988Z, which shows many similarities to SN 2008iy at late times (see Section 3.2; SN 1988Z data from Turatto et al. 1993), as they would have appeared at the redshift of SN 2008iy. Right: Three panels with images of the field of SN 2008iy. Each image is , with north up and east to the left. Black crosshairs mark the location of the SN. The bottom image, marked (c), shows the last non-detection from the Deep Sky data. The middle (b) and top (a) images show the CRTS detections on day 0 and day 153, respectively; SN 2008iy can clearly be seen in each of them. The SN was not flagged as a transient in either the middle or top image by the CRTS software.
date mag333Observed value; not corrected for Galactic extinction. 444The calibration uncertainty dominates over the statistical uncertainty with values of 0.12 and 0.01 mag, respectively.
(MJD)
54618.35 17.37 0.12
54621.35 17.38 0.12
54623.33 17.35 0.12
54626.32 17.34 0.12
54627.36 17.37 0.12
54628.29 17.37 0.12
54629.30 17.36 0.12
54638.21 17.34 0.12
54651.20 17.28 0.12
Table 1: Deep Sky Observations of SN 2008iy.

To constrain the rise time of SN 2008iy we visually estimate the possible range of magnitudes for the SN from images on the CRTS website555http://crts.caltech.edu/. based on a comparison to SDSS images. As previously mentioned, SN 2008iy is blended with a nearby star and so the automated photometry produced by the CRTS does not detect the SN on these epochs. On 2007 Sep. 13 the SN was between 18.3 and 19.0 mag, while on 2008 Feb. 19 the SN was observed between 17.9 and 18.3 mag.

Near-infrared (NIR) observations of SN 2008iy were conducted with the 1.3-m Peters Automated Infrared Imaging Telescope (PAIRITEL; Bloom et al. 2006) starting on 2009 Apr. 13. PAIRITEL observes simultaneously in the J, H, and K bands. Observations were scheduled and executed via a robotic system, and the data were reduced by an automated pipeline (Bloom et al., 2006). The SN flux was measured via aperture photometry using SExtractor (Bertin & Arnouts, 1996), calibrated against the Two Micron All Sky Survey (2MASS Skrutskie et al., 2006). Filtered photometry of SN 2008iy is shown in Fig. 2 and summarised in Table 2.

666Midpoint between the first and last exposures in a single stacked image. mag777Observed value; not corrected for Galactic extinction. mag mag
(MJD) (Vega) (Vega) (Vega)
54934.42 16.59 0.05 16.00 0.05 14.98 0.05
54937.43 16.57 0.06 15.99 0.06 15.05 0.05
54941.43 16.57 0.05 16.04 0.08 15.06 0.08
54944.40 16.70 0.05 15.98 0.07 14.98 0.07
54948.40 16.59 0.05 15.87 0.06 14.98 0.06
54951.39 16.55 0.04 15.96 0.06 15.02 0.06
54954.35 16.70 0.04 15.88 0.05 15.00 0.08
54957.37 16.63 0.05 15.91 0.05 14.99 0.10
54959.37 16.68 0.05 15.89 0.06 14.97 0.07
54961.44 16.69 0.06 15.99 0.08 14.83 0.12
54970.30 16.77 0.08 15.98 0.12
54975.28 16.66 0.07 15.86 0.05 14.87 0.06
54981.35 16.72 0.04 15.90 0.05 14.93 0.08
54986.29 16.61 0.05 15.85 0.06 15.06 0.12
54990.30 16.68 0.08 16.00 0.11 14.59 0.07
54994.30 16.69 0.05 15.89 0.04 14.84 0.06
54998.31 16.67 0.05 15.92 0.07 14.90 0.07
55003.18 16.86 0.07 15.97 0.05 14.96 0.11
55030.20 16.92 0.19 16.01 0.15
55041.18 16.78 0.07 15.94 0.08 14.82 0.10
55091.10 17.08 0.09 15.94 0.07 14.74 0.08
Table 2: PAIRITEL Observations of SN 2008iy.

Ground-based optical observations of SN 2008iy were obtained using the 1.0-m Nickel telescope located at Lick Observatory (Mt. Hamilton, CA, USA) starting on 2009 Apr. 18.  photometry from the Nickel was measured using the DAOphot package (Stetson, 1987) in IRAF888IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation., and transformed into the Johnson–Cousins system. Calibrations for the field were obtained on ten photometric nights with the Nickel telescope. The Nickel photometry is shown in Fig. 2 and summarised in Table 3.

Table 3: Nickel Observations of SN 2008iy.
date mag999Observed value; not corrected for Galactic extinction. mag mag mag
(MJD) (Vega) (Vega) (Vega) (Vega)
54939.52 19.06 0.01 18.59 0.03 17.86 0.01 17.87 0.03
54940.46 19.09 0.03 18.56 0.02 17.86 0.02 17.89 0.03
54971.37 19.35 0.06 18.71 0.04 17.99 0.04 17.98 0.11
54975.36 19.25 0.03 18.75 0.02 17.96 0.02 17.92 0.07
54979.46 19.23 0.03 18.71 0.02 17.97 0.02
54999.35 19.36 0.05 18.79 0.03 18.07 0.03 18.12 0.08
55004.37 19.40 0.05 18.84 0.03 18.07 0.02 18.13 0.11
55007.43 19.56 0.11 18.84 0.10 18.02 0.04 18.37 0.13
55015.36 19.43 0.11 18.95 0.06 18.10 0.04 18.26 0.08
55019.30 19.58 0.09 19.02 0.06 18.19 0.03 18.21 0.07
55025.36 19.66 0.24 18.66 0.10 18.16 0.08 18.18 0.12
55034.26 19.52 0.02 19.02 0.03 18.19 0.02 18.23 0.11
55040.30 19.56 0.05 18.97 0.03 18.18 0.03 18.30 0.09
55042.24 19.60 0.07 19.11 0.06 18.21 0.03 18.31 0.11
55047.27 19.43 0.11 19.21 0.10 18.22 0.04 18.24 0.20
55071.22 19.66 0.04 19.17 0.05 18.23 0.03 18.34 0.09
55077.23 20.07 0.24 19.33 0.17 18.29 0.03 18.58 0.17
55100.15 19.75 0.07 19.25 0.08 18.35 0.03 18.49 0.06
Figure 2: Filtered photometry including  from the Nickel telescope and J, H, and K from PAIRITEL, showing the decline rate of SN 2008iy between days 560 and 715. To help guide the eye, we illustrate the linear fit to each band used to determine the photometric decline rates (see text). Note that the single epoch of UVOT and -band observations we measured, which agree to with Nickel data taken 2 days later, is not shown in this figure.

SN 2008iy was observed by the space-based Swift observatory on 2009 Apr. 15 and 16. Swift observed the SN simultaneously with both the X-ray Telescope (XRT; Burrows et al. 2005) and the Ultraviolet/Optical Telescope (UVOT; Roming et al. 2005). We downloaded the Level-2 UVOT images, and measured the , , and photometry using the recipe of Li et al. (2006). The UV filters (, , and ) were calibrated using the method of Poole et al. (2008). Our final UVOT photometry is summarised in Table 4. The XRT observed the field for a total of 10.71 ks. We extract the 0.3–10.0 keV counts from an extraction region of 64 pixels (), where we fit the point-spread function model (see Butler & Kocevski 2007) at the centroid of the X-ray emission. From the native XRT astrometry the centroid of the X-ray emission, located at = 160837.23, = +041626.7 (J2000), with a radial uncertainty of 5 (90% confidence interval), coincides with the optical position of SN 2008iy, suggesting that the X-rays are from the SN. In an astrometric fit relative to 2MASS we measure the position of the star 11 from the SN to be = 160836.98, = +041616.4 (J2000), with a root-mean square scatter of 0.19 in and 0.18 in for our astrometric solution. This star is therefore well outside the 90% confidence interval for the location of the X-ray emission. Furthermore, there is no catalogued X-ray source at the position of the SN in the ROSAT catalogue (Voges et al., 1999), also suggesting that the star located 11 from the SN is not the source of X-ray emission. We measure a background-subtracted 0.310.0 keV count rate of (19 6) counts s.

Table 4: UVOT Observations of SN 2008iy.
101010Midpoint between the first and last exposures in a single stacked image. filter mag111111Observed value; not corrected for Galactic extinction.
(MJD) (Vega)
54936.31 UVW2 19.14 0.06
54936.32 UVM2 18.95 0.08
54936.32 UVW1 18.53 0.07
54936.31 U 18.60 0.06
54937.49 UVW2 19.12 0.04
54937.85 B 19.04 0.06
54937.85 V 18.65 0.08

2.2 Spectroscopy

Spectra of SN 2008iy were obtained on 2009 Apr. 18, 2009 Apr. 25, and 2009 Jul. 23 with the Kast spectrograph on the Lick 3-m Shane telescope (Miller & Stone, 1993). An additional spectrum was obtained on 2009 Sep. 22 with the Low-Resolution Imaging Spectrometer (LRIS; Oke et al. 1995) on the 10-m Keck I telescope. To improve the spectral resolution at the location of the H emission feature from SN 2008iy, we used the 1200 lines mm grating on the red side of the double-arm (blue+red) LRIS system. The spectra were reduced and calibrated using standard procedures (e.g., Matheson et al. 2000). Clouds were present on the night of 2009 Apr. 25, and the observing setup from that night did not include any wavelength overlap between the red and blue arms of the Kast spectrograph; thus, the absolute flux calibration on this night is less certain than on the other nights. For the Kast spectra, we observed the SN with the slit placed at the parallactic angle, so the relative spectral shapes should be accurate (Filippenko, 1982). LRIS is equipped with an atmospheric dispersion corrector; nevertheless, we observed the SN at the parallactic angle on this night as well. In Fig. 3 we show the spectral sequence of SN 2008iy, and a summary of our observations is given in Table 5.

Figure 3: Spectral sequence of SN 2008iy (shown in black) and a single, late-time spectrum of SN 1988Z from our spectral database (shown in red), which was observed 504 days after discovery. To the left of the spectra we give the time since discovery, in rest-frame days, at which each spectrum was taken. Prominent spectral features of SN 2008iy are labelled at the top of the figure. The spectra show little evolution between days 560 and 711. Fe II multiplets 42, 48, and 49 can also be seen, though we have not labelled those lines. The spectra have been corrected for Galactic reddening ( mag; Schlegel, Finkbeiner & Davis 1998). We have assumed no reddening in the SN host galaxy (see Section 2.3).
Epoch121212Defined as rest-frame days relative to day 0, 2007 Sep. 13. UT Date Telescope/ Exposure
Instrument (s)
560 2009-04-18.458 Shane 3-m/Kast 1500
567 2009-04-25.479 Shane 3-m/Kast 1500
652 2009-07-23.274 Shane 3-m/Kast 1800
711 2009-09-22.236 Keck I 10-m/LRIS 600
Table 5: Log of spectroscopic observations.

2.3 Host Galaxy

There is no catalogued redshift for the host galaxy of SN 2008iy. To determine the redshift of the SN we examined the LRIS spectrum for the presence of narrow emission lines. Based on a fit to the [O III] 4959, 5007 doublet we adopt a heliocentric redshift of for SN 2008iy (not corrected for peculiar motions or Virgo infall). This corresponds to a luminosity distance of Mpc ( km sMpc, , ), which we adopt throughout the remainder of this paper.

The reddening of SN 2008iy by the host galaxy is uncertain. In our Kast spectra we do not detect any absorption from Na I D, and therefore we adopt mag.

We confirm the possible detection of the host galaxy by Catelan et al. (2009) in a stack of SDSS , , and -band images of the field. When the + + stack is calibrated to the SDSS band, we find that the host has = 22.75 0.15 0.08 mag in a 2.2 diameter aperture, where the two errors represent the statistical and calibration uncertainties, respectively.

As first noted by Catelan et al. (2009), the field of SN 2008iy was observed by the Galaxy Evolution Explorer (GALEX; Martin et al. 2005). On 2004 May 17, the field was imaged as part of the all-sky imaging survey (AIS); the host was not detected to a 5 limiting magnitude of 20.2 and 20.5 mag. The field was reimaged as part of the medium imaging survey on 2008 Jun. 05/06, and SN 2008iy was detected at mag and mag.

3 Results

3.1 Photometric Analysis

At = 0.0411, the absolute peak magnitude of SN 2008iy was a relatively modest mag. This places SN 2008iy well below the most luminous SNe IIn, such as SN 2006gy ( mag; Ofek et al. 2007; Smith et al. 2007) and SN 2008fz ( mag; Drake et al. 2009b), and more in the range of the well-studied SN IIn 1988Z ( mag; Turatto et al. 1993; Stathakis & Sadler 1991). Assuming no bolometric correction, the total integrated optical output from SN 2008iy during the first 700 days after discovery is 2 erg. Between day 550 and 720 the SN declines in the optical and the band, while it actually gets brighter in the and bands. During this time, the linear decay rates are as follows: = 0.51 mag (100 day), = 0.50 mag (100 day), = 0.34 mag (100 day), = 0.43 mag (100 day), = 0.30 mag (100 day), = 0.03 mag (100 day), and = 0.19 mag (100 day). These decline rates, all slower than the expected rate of decline for radioactive Co, 0.98 mag (100 day), strongly suggest that the SN is still being powered by CSM interaction 700 days after explosion.

For comparison purposes, in addition to the light curve of SN 2008iy, Fig. 1 shows the light curve of the standard Type II-P SN 1999em (Leonard et al., 2002) as it would have appeared at the redshift of SN 2008iy. As well as illustrating the very long rise time of SN 2008iy, this comparison shows that SN 2008iy was fairly luminous at the time of discovery. Thus, despite the sparse sampling over the first 200 days, this large luminosity suggests that the early detections are not related to a pre-SN outburst, as was observed for SN 2006jc (Foley et al., 2007; Pastorello et al., 2007). CRTS images indicate that the SN was rising over the first 400 days (Mahabal et al., 2009), which provides further evidence against a pre-SN outburst. Fig. 1 also shows the light curve of the long lived, interacting, Type IIn SN 1988Z (Turatto et al., 1993). The explosion date of SN 1988Z is not well constrained (see Section 4.3), so we shift the first epoch of detection to day 0. Notice the similarity of the decline rate of SN 2008iy and SN 1988Z around day 600; these SNe also have very similar late-time spectra (see Section 4.2).

We were unable to fit the UV through NIR spectral energy distribution (SED) of SN 2008iy to a single-temperature blackbody model. This is not surprising, as SNe II are dominated by emission lines at late times, and single-temperature blackbody models typically apply only to young SNe II (see, e.g., Filippenko 1997). Direct integration of the UVNIR SED shows that the bolometric correction, relative to the band, is a factor of 3 in luminosity, corresponding to 1.2 mag, on day 560. Some features stand out from the SED: there is a strong -band excess relative to the other optical bands, with mag and mag on day 715. The red colour relative to a blue colour can be attributed to the H emission with large equivalent width. This emission also accounts for the relatively slow decay rate in the band, as compared to the other optical bands. There is also a NIR excess relative to the -band flux. In fact, this excess increases with time, mag on day 560 and mag on day 710, which is indicative of the growing importance of dust in the emission from SN 2008iy.

A NIR excess at late times has been observed in many SNe IIn (e.g., Gerardy et al. 2002), and it is the result of either new dust formation (e.g., SN 2005ip; Smith et al. 2009; Fox et al. 2009) or the presence of a NIR light echo from preexisting dust (Dwek, 1983), or both. To distinguish between these two possibilities, which are virtually identical from photometry alone, requires well-sampled optical spectra (see Section 3.2.2) since line profiles are expected to change with time if new dust is being formed. On day 706, corresponding to our last PAIRITEL observation, the colour of SN 2008iy was 1.2 mag. Assuming that the dust radiates as a perfect blackbody, this colour corresponds to a dust temperature of K, while the -band measurement corresponds to a dust luminosity erg s, assuming no bolometric correction as we cannot constrain the emission in the mid-IR. This luminosity is very large, though upon making similar assumptions Gerardy et al. (2002) found NIR luminosities erg s for SNe 1995N and 1997ab at late times. Gerardy et al. also found that the NIR luminosity was roughly an order of magnitude greater than the X-ray emission from SN 1995N, which is also the case for SN 2008iy (see Section 3.3). The colour of SN 2008iy is bluer than those of the Gerardy et al. sample at a similar epoch, which may be a result of the long rise of SN 2008iy or a contribution to the NIR emission from the SN in addition to the dust. Future NIR observations, as the underlying SN light continues to fade, will place more stringent constraints on the dust near SN 2008iy.

3.2 Spectroscopic Analysis

Our spectra of SN 2008iy at ages 560 days are very similar to those of an unpublished spectrum, from our spectral database, of the Type IIn SN 1988Z taken at a comparable epoch, as shown in Fig. 3. The general features resemble those of several other SNe IIn (Filippenko, 1997): there are prominent Balmer and He I emission lines, most notably the dominant H emission, which primarily feature intermediate-width emission components with full width at half-maximum intensity (FWHM) 1650 km s in the case of SN 2008iy. The higher-resolution Keck spectrum reveals a number of narrow, marginally resolved (FWHM 170 km s) emission lines, including H, H, [O III] 4363, 4959, 5007, and He I 7065. The only high-ionisation line we detect is [Fe X] 6375. The relative lack of narrow forbidden lines and the low intensity ratio of [O III] 4959, 5007 to [O III] 4363 suggest a large electron density for the ejecta (Filippenko & Halpern, 1984; Filippenko, 1989; Stathakis & Sadler, 1991). The relative spectral features do not show strong evolution between days 560 and 711.

We can estimate the density of the unshocked emitting material based on the relative intensities of the three [O III] lines mentioned above. Note that [O III] 4363 is only resolved in our day 711 Keck spectrum, so the following estimate of the density is at that epoch only. Following a removal of the underlying continuum, we fit three Gaussian profiles to [O III] 4363 and [O III] 4959, 5007, and find that . As mentioned above, the strong presence of [O III] 4363 indicates a high density for the emitting material. In fact, with 1.7, the electron density, , must be cm regardless of the temperature of the emitting gas. Typically, [O III] emission comes from photoionised regions with –20,000, in which case cm (see Fig. 11 in Filippenko & Halpern 1984). Note that this high-density material is likely only present within clumps in the CSM (see Section 4.2), and that interclump portions of the CSM have a lower density.

3.2.1 The H Profile

As seen in Fig. 3, the H emission feature dominates over all the other lines. In the high-resolution Keck spectrum, we see evidence for three distinct emission features: a broad component (FWHM 4500 km s), an intermediate component (FWHM 1650 km s), and a marginally resolved, narrow P Cygni feature (FWHM 75 km s), as shown in Fig. 4. The main panel of Fig. 4 shows a fit to the H profile (red line) which includes a broad (FWHM 4500 km s) and an intermediate (FWHM 1650 km s) component. Panel (a) in Fig. 4 shows a close-up view of the narrow emission after the broad and intermediate components have been removed using a spline fit. We fit the spline to the observed H profile from km s to km s after masking the region between km s and km s. A narrow absorption minimum such as this, located at 100 km s, has been seen in a number of typical SNe IIn (e.g., SNe 1997ab, 1997eg, and 1998S, Salamanca, Terlevich & Tenorio-Tagle 2002; Salamanca 2000; Fassia et al. 2001), and it traces the outflow velocity of the progenitor wind. We note that while the narrow absorption is only marginally resolved, a P Cygni profile with characteristic speeds of 10 km s, typical of red supergiants (RSGs), would go completely unresolved in the Keck spectrum. Therefore, this P Cygni profile must be associated with an outflow velocity that is 10 km s, which will have important consequences for the progenitor (see Section 4.3).

Figure 4: Detailed view of the H profile from the Keck spectrum taken on day 711. Main panel: The black line shows the observed H profile, while the smooth red line illustrates a two-Gaussian fit (intermediate, FWHM km s; broad, FWHM km s) to the profile. Residual emission and absorption from a narrow component to the profile can easily be seen. The location of He I 6678 has been marked, and the residuals from an imperfect telluric absorption correction have been marked by the symbol. Inset (a): Close-up view of the residual, narrow P Cygni component. The smooth red line shows a fit to the feature that includes a Gaussian in emission and a Gaussian in absorption (both Gaussians have FWHM 75 km s). The absorption minimum of the narrow absorption is located at km s. Note that for this fit we removed the broad plus intermediate components using a spline fit over the region from km s to km s(see text). Inset (b): Residuals following the subtraction of the two-Gaussian broad plus intermediate fit from the observed H profile. The absorption minimum still occurs at km s, but the BVZI extends to km s, meaning the progenitor wind speed may be km s (see text).

It is interesting that the broad plus intermediate fit overestimates the H flux out to about 450 km s. In panel (b) of Fig. 4 we show the residual flux, centred on H, following the subtraction of our two-Gaussian fit to the broad plus intermediate emission. The blue velocity at zero intensity (BVZI) extends to roughly km s, which means that the true wind speed from the progenitor, as traced by the absorbing gas moving directly along the line of sight toward the SN, may be 100 km s and possibly as high as 450 km s. If this feature represents a true lack of emission, it would be evidence for a two-component CSM: one with velocity km s and the other with BVZI km s. Similar features were seen in SN 1998S (Fassia et al., 2001), which were modelled by Chugai et al. (2002) to be a slow wind accelerated to higher velocities by radiation from the SN photosphere, and in SN 2006gy, which Smith et al. (2010) argued was the result of a CSM shell that had been ejected from the progenitor in a pre-SN eruption. These two scenarios predict different behaviour as the SN evolves.

In the radiatively accelerated scenario, as shown by Chugai et al. (2002) for SN 1998S, the second, faster component to the wind has a negative velocity gradient. Observationally, this effect manifests itself as a BVZI for the second, faster CSM component that decreases with time, as observed in SN 1998S (Fassia et al., 2001). In the shell-ejection scenario, the wind exhibits a positive velocity gradient as the ejected shell is freely expanding, which is thought to be the result of an explosive ( erg) mass-loss event (see e.g., Chugai et al. 2004). This scenario leads to a BVZI that increases with time, as was observed for SN 2006gy (Smith et al., 2010). With only a single high-resolution spectrum, we are unable to probe the evolution of this feature, but we note that the velocity of a radiatively accelerated CSM is proportional to (Fransson, Lundqvist & Chevalier, 1996), so this mechanism is unlikely to be significant at late times ( a few hundred days).

Figure 5: Evolution of the H profile of SN 2008iy between day 560 and day 711. The profile remains largely unchanged, with the exception of a variable spectral feature between 200 km s and 20,000 km s, from day 652 to day 711. Similar spectral features have been observed in other interacting SNe (see text). Emission lines of He I 6678 and He I 7065 are labelled.

As does the overall continuum, the H luminosity declines over the course of our observations. In Table 6 we summarise the observed properties of the H profile from our spectra on days 560, 652, and 711. We do not include the spectrum from day 567, as it was taken under cloudy conditions and the overall flux scaling is uncertain, but we do not expect significant spectral evolution between days 560 and 567. The decline in the H luminosity is accompanied by a rise in the equivalent width over this same time period. For the narrow emission on day 711, we measure erg s, though we note that this value is likely underestimated because the blue emission wing is probably being partially absorbed. The FWHM of the intermediate component is 1650 km s at all epochs, while the FWHM of the broad component drops from 5800 km s on day 560, to 5200 km s on day 650, to 4400 km s on day 711. We attribute this change in the broad component to rapid evolution of the spectrum redward of H between days 560 and 711, as shown in Fig. 5. The nature of this feature is not currently understood: it could potentially be an absorption feature, or it could be related to a lack of emission from some unidentified species. Similar spectral evolution redward of H has been seen in the interacting SNe 2005gj and 2006gy (Prieto et al., 2007; Smith et al., 2010). We do not associate this feature with H, as the red velocity at zero intensity corresponds to velocities of 22,000 km s, and there are no other emission lines that show evidence for velocities this large.

Epoch131313Defined as rest-frame days relative to day 0, 2007 Sep. 13. Br. FWHM Int. FWHM Nar. FWHM (H)141414Uncertainty %. EW151515Uncertainty %. H/H
(km s) (km s) (km s) (erg s) (Å)
560 5774 1641 2122 9.49
652 5162 1685 2386 12.22
711 4405 1639 78 2786 12.54
Table 6: H line widths, luminosity, equivalent width, and ratio to H.

3.2.2 He I Emission

In addition to the prominent Balmer emission lines, SN 2008iy exhibits several He I lines in emission, including 3820, 4026, 4471, 5016, 5875, 6678, and 7065. None of these lines show evidence for a broad component, and the intermediate component, FWHM 1100–1400 km s, is slightly narrower than that observed for H. As previously mentioned, He I 7065 has a narrow, marginally resolved emission component in addition to the intermediate component.

A systematic, increasing blueshift in the He I profiles has been argued as evidence for dust formation in the cool, dense shell formed in the post-shock gas of the Type IIn SNe 1998S and 2005ip (Pozzo et al., 2004; Smith et al., 2009). Newly formed dust in the post-shock region absorbs light from the receding ejecta, resulting in a suppression of flux from the red side of the emission line. Using He I 7065, the strongest He line in our spectra, we searched for changes in the red wing of the profile. The Kast spectra from days 560 and 567 are very noisy, but in the higher signal-to-noise ratio spectra from days 652 and 711 we see no evidence for a change in the red wing of the emission profile. This hints that the observed NIR excess (see Section 3.1) is the result of a NIR echo, rather than newly formed dust, though we caution that with only two spectra separated by 50 days the lack of change in the He I profile does not constitute definitive evidence for this.

3.3 X-ray Analysis

To determine the X-ray luminosity of SN 2008iy we assume a thermal plasma spectrum with temperature 0.6 keV (see, e.g., Immler & Kuntz 2005), which has been absorbed by a Galactic column density of cm (Kalberla et al., 2005). Using the 0.3–10 keV XRT count rate (see Section 2.1) and PIMMS161616http://heasarc.nasa.gov/Tools/w3pimms.html., we measure the unabsorbed flux, assuming no absorption within the host, to be (6.1 1.9) 10 erg cm s. At the adopted distance of SN 2008iy this corresponds to a luminosity of erg s. Note that Fox et al. (2000) fit the late-time ( 3 yr) X-ray spectra of SN 1995N with a larger temperature of 9.1 keV, which would correspond to a flux and luminosity of (9.1 2.9) 10 erg cm s and erg s, respectively, were we to adopt this value for SN 2008iy. Similar luminosities ( erg s) are observed for other interacting SNe more than 1 year post explosion (e.g., SNe 1988Z and 1995N; Fox et al. 2000).

4 Discussion

4.1 Mass Loss in the SN 2008iy Progenitor

We assume that the continuum emission traced by the light curve of SN 2008iy is powered solely by CSM interaction. The half life of Ni is 6.0 days, much too short to power the 400 day rise of SN 2008iy, while the photometric decay rates are too slow to be powered by Co (see Sec. 3.1), implying that radioactivity contributes minimally to the light curve of SN 2008iy. Furthermore, the SN ejecta will suffer considerable adiabatic losses during the 400 day rise of the light curve, suggesting that interaction is the only viable mechanism for powering SN 2008iy over this entire time.

Following our assumption of interaction-driven luminosity, the expelled gas from the progenitor overtaken by the shock at each epoch can be written as (see Chugai & Danziger 1994)

(1)

where  is the mass-loss rate of the progenitor, is an efficiency factor describing the conversion of kinetic energy into radiation, is the luminosity of the SN, is the wind speed of the progenitor, and is the velocity of the blast wave overrunning the CSM. We adopt = 0.5, but this number is likely an overestimate given the optically thin nature of the emission (see Section 4.2). The CSM wind is only probed by our higher-resolution spectrum from day 711, so we adopt = 100 km s based on the narrow P Cygni absorption seen in H, though this may not be valid at all times between days 0 and 700 (see below). We adopt = 5000 km s based on the typical widths of the broad H emission, which should trace the speed of the blast wave. Unlike our assumption of a constant wind speed, the adoption of a constant-velocity blast wave at all times should at the very least be valid after the peak, at which point the CSM density is decreasing with increasing radius. Hydrodynamic modelling of SNe IIn demonstrates that the blast wave is quickly decelerated to a roughly constant expansion speed as the ejecta sweep up successively more CSM (see, e.g., Chugai et al. 2004). This scenario may not apply to SN 2008iy, however, because the 400 day rise time implies that the CSM density may have been increasing with radius, in which case the blast wave may have been continually decelerated during the rise.

Following the above assumptions we can use Equation 1 to determine the mass loss traced by the optical luminosity at a number of different epochs of interest. At each epoch we determine the radius, km s , and the luminosity based on the light curve shown in Fig. 1. We do not adopt the bolometric correction determined in Section 3.1 for two reasons: (i) it is unclear whether this same correction is valid at early times, and (ii) emission from a NIR echo should not be incorporated into Equation 1, as that contribution to the total luminosity is not directly the result of CSM interaction. Thus, the estimates below of the luminosity do not reflect any emission from dust. At early times, day 153, L, which corresponds to   1.3 M yr at cm, while at the time of peak L, cm, and   2.3 M yr. On day 563, coincident with our X-ray observations of SN 2008iy  the optical luminosity was L, which corresponds to cm and   1.3 M yr. On day 714, roughly coincident with our high-resolution Keck spectrum, L, cm, and   0.8 M yr.

These results are quite remarkable; they suggest that at a time 5000 km s  400 day/100 km s  55 years prior to the explosion of SN 2008iy, the progenitor underwent a period of heightened mass loss. This enhanced mass-loss period was then followed by a period of decreasing mass loss leading up to the time of the SN explosion. While the quantitative results for the mass loss discussed above are sensitive to our adopted quantities, most specifically the progenitor wind speed and the speed of the SN blast wave, the fact remains that the continuum luminosity did increase over a period of 400 days after the SN explosion. Rearrangement of Equation 1 shows that this luminosity increase is proportional to the wind-density parameter, . Thus, must have increased over a distance cm from the progenitor, regardless of the true wind speed over that distance. An increasing value of means that during roughly the century prior to the SN, there was a significant change in the wind properties of the progenitor.

Using our X-ray detection of SN 2008iy we have an alternative method to probe the mass-loss history of the progenitor on day 563. Following Immler & Kuntz (2005), the X-ray luminosity may be written as

(2)

where is the X-ray luminosity, is the mean mass per particle ( = 2.1 g for a H+He plasma), is the cooling function of a plasma heated to temperature ,  is the mass-loss rate of the progenitor, is the wind speed of the progenitor ( km s, see above), is the speed of the SN blast wave ( km s, see above), and is the time since explosion, 563 days. Assuming a temperature K, appropriate for an optically thin thermal plasma (Immler & Kuntz, 2005), the effective cooling function is erg cm s. The X-ray luminosity on day 563 was erg s. Substituting these values into Equation 2, we find   M yr, which shows agreement with the value derived from the optical continuum, M yr, given the uncertainty in a number of the assumptions we have adopted.

An additional estimate of the mass-loss rate of the progenitor comes from the narrow H emission seen in our Keck spectrum on day 711. Chugai & Danziger (2003) show that the H emission from the unshocked CSM is related to :

(3)

where is the inner radius corresponding to the position of the SN blast wave, is the outer radius related to the fast-moving forward shock, is the effective recombination coefficient for H, is the energy of an H photon, is the degree of H ionisation, is the hydrogen mass fraction, and is Avogadro’s number. We cannot constrain or , so we conservatively adopt , , and , all of which have the effect of minimising . Assuming Case B H recombination, cm s, which is appropriate assuming that the narrow emission comes from photoionised gas. Substituting the narrow H luminosity ( erg s) and cm into Equation 3, we find that g cm. With km s on day 711, this corresponds to   M yr. At a similar epoch (see above), we find   M yr based on the optical luminosity. Again, the agreement between these two methods to within a factor of 2 is reasonable given the uncertainties in our adopted parameters.

4.2 Late-Time Emission and the Similarity to SN 1988Z

To explain the late-time (i.e., post peak) emission from SN 2008iy we adopt a model that is virtually identical to that developed by Chugai & Danziger (1994) for SN 1988Z: the CSM contains optically thick clumps in addition to a rarefied wind between these clumps (see, e.g., Fig. 1 of Chugai & Danziger 1994). As the SN ejecta sweep through the CSM, they drive a fast-moving forward shock into the rarefied wind. This shocked material forms a cool dense shell between the forward and reverse shocks, and gives rise to the broad emission component seen in H (FWHM 5000 km s for SN 2008iy). At the same time a slower shock is being driven into the dense clumps, which leads to the intermediate-width emission (FWHM 1650 km s in the case of SN 2008iy) seen in the spectra. The narrow P Cygni profile results from the pre-shock photoionised wind.

The observed similarities between SN 2008iy and SN 1988Z provide further evidence that comparable models are appropriate for the two SNe. In addition to having similar spectra at late times (see Fig. 3), SNe 1988Z and 2008iy have large X-ray luminosities (both SNe have ; Fabian & Terlevich 1996, this work), and similar late-time decline rates (0.30.5 mag (100 day) in the optical; Turatto et al. 1993, this work), which in both cases are slower than the expected bolometric decline of radioactive Co. Estimates for the mass-loss rate from the progenitor of SN 1988Z vary by roughly an order of magnitude. From X-ray observations Schlegel & Petre (2006) find M yr, while Williams et al. (2002) estimate M yr based on radio observations, and the models of the optical emission by Chugai & Danziger (1994) yield M yr. While these estimates are 1–2 orders of magnitude less than those for SN 2008iy, we note that in each of the above estimates for a wind speed of 10 km s was adopted for the progenitor of SN 1988Z. If SN 1988Z had a progenitor wind speed closer to 100 km s, a very reasonable possibility given the wind speed of SN 2008iy and other similarities between the two SNe, this would result in an increase in the estimated mass-loss for the progenitor by a factor of 10, thereby bringing the estimates for the two SNe into accord.

Based on the late-time emission, SN 2008iy seems to belong to the group of SNe IIn that exhibit a slow evolution sustained by long-lived ( 1 decade) CSM interaction. In addition to SN 1988Z, other members of this group include SN 1986J (Rupen et al., 1987), SN 1995N (Fox et al., 2000; Fransson et al., 2002), and possibly also the VLSN 2003ma (Rest et al., 2009). Both SN 1986J and SN 1995N exhibit evidence for a clumpy progenitor wind, like SN 2008iy and SN 1988Z. Chugai (1993) modelled the X-ray emission from SN 1986J as the interaction between the SN ejecta and a clumpy wind (though note that Houck et al. 1998 prefer a model with a smooth CSM, but they conclude that they cannot rule out the clumpy model). The evidence for a clumpy wind from the progenitor of SN 1995N comes from both the optical spectra (Fransson et al., 2002) and the X-ray emission (Zampieri et al., 2005). Also, the optical decline of both SNe 1986J and 1995N is very slow: SN 1986J declined by 1 mag in the optical between 1994 and 2003 (Milisavljevic et al., 2008), while the -band decline of SN 1995N was only 2.2 mag between 1998 and 2003 (Zampieri et al., 2005).

The duration of the interaction means that the large mass-loss rates from the respective progenitors must have been sustained for at least yr prior to core collapse after the conservative assumption that = 1000 km s, and = 100 km s. Typically the blast wave continues to expand at 1000 km s (SN 1988Z had a broad component that remained nearly constant at 2000 km s from day 1500 to 3000; Aretxaga et al. 1999), which would make this time period 100 yr. These very long-lived SNe IIn are therefore connected in that their progenitors experienced lengthy periods with high mass-loss rates. This stands in stark contrast to the Type IIn SN 1994W, which had a light curve with an abrupt drop 100 days post explosion (Sollerman, Cumming & Lundqvist, 1998). The mass loss from the progenitor of SN 1994W has been modelled to occur in a short (1 yr), violent episode (Chugai et al., 2004), and the sudden drop in the light curve occurs because the SN ejecta have overtaken the dense CSM, thereby halting any interaction luminosity.

4.3 Origin of the 400 Day Rise Time and Implications for the Progenitor

With a model to account for the late-time emission from SN 2008iy, we are still left with the puzzle of explaining the 400 day rise time.171717We have no spectra of the SN while it was still on the rise, thus we have no way of knowing if the SN underwent significant spectral evolution prior to day 560. This rise in the optical is significantly longer than that seen in any other known SN. As previously discussed, this scenario is possible if the progenitor underwent a phase of enhanced mass loss 55 years prior to the SN explosion. The optical luminosity traces the wind-density parameter, , meaning that during the decades prior to explosion either (i) the mass-loss rate declined, or (ii) the wind speed increased, or (iii) both.

Episodic periods of enhanced mass loss, sometimes in the form of a shell ejection, have been observed for numerous LBVs (see Humphreys & Davidson 1994), though the underlying physics of these eruptions is not currently well understood (see Smith & Owocki 2006). If the progenitor of SN 2008iy had a giant eruption (similar to that of LBVs) 1 century prior to explosion, this could result in a density profile that peaks 1.7 cm from the progenitor. In the clumpy-wind scenario described in Section 4.2, this would mean that the ejecta are expanding into a wind where the number density of clumps is increasing with radius. Thus, as more and more clumps are overtaken by the ejecta, the continuum luminosity continues to rise, until after 400 days when the ejecta have reached 1.7 cm, the number density of clumps begins to decline and so does the optical luminosity. Alternatively, the long rise could result from the ejecta expanding into a nonspherical wind, such as a bipolar outflow, though this hypothesis would need to be examined with detailed hydrodynamical models.

The inferred mass-loss rate for SN 2008iy,   M yr, is similar to that for the first LBV, P Cygni, during its great eruption ( M yr during the 1600 AD eruption; Smith & Hartigan 2006). Furthermore, the terminal wind speed in the P Cygni nebula is 185 km s (Lamers et al., 1996; Najarro, Hillier & Stahl, 1997), which is similar to the observed BVZI for the narrow blue absorption seen in SN 2008iy, corresponding to –450 km s. We illustrate these comparisons to show that derived properties of the progenitor wind of SN 2008iy are similar to the giant eruption of a Galactic LBV; we are not insinuating that the great outburst from P Cygni is a direct analogue to the proposed LBV-like eruption from SN 2008iy. Such eruptions are not expected from RSGs.

Further evidence that the progenitor of SN 2008iy could not have had a RSG progenitor comes from the observed narrow P Cygni H profile. RSGs have typical wind speeds of 10 km s, with extreme RSG winds reaching 40 km s (see Smith et al. 2007). The observed 100 km s wind speed from SN 2008iy is more characteristic of LBVs (e.g., P Cygni, see above) or the escape velocity from a blue supergiant. Similar 100 km s P Cygni profiles have been seen in a number of SNe IIn, such as SNe 1997ab (Salamanca, 2000), 1997eg (Salamanca, Terlevich & Tenorio-Tagle, 2002), 1998S (Fassia et al., 2001), and 2007rt (Trundle et al., 2009), implying that the progenitors of each of these SNe may have been in a similar state shortly before core collapse.

The dense CSM and large luminosities associated with many SNe IIn have led a number of authors to suggest that at least some SNe IIn are associated with progenitors that experienced LBV-like mass loss shortly before core collapse (see e.g., Chu et al. 1999; Salamanca 2000; Chugai & Danziger 2003; Chugai et al. 2004). This possible connection was considerably strengthened following the direct identification of the progenitor of the normal Type IIn SN 2005gl on archival Hubble Space Telescope images (Gal-Yam et al., 2007; Gal-Yam & Leonard, 2009). While the diagnostics above are not ubiquitous for all SNe IIn181818Note that the low-resolution spectrographs typically employed to observe SNe lack sufficient resolution to resolve narrow (FWHM 150 km s) absorption lines., many of the signatures (high-density CSM, episodic mass loss with   M yr, and 100 km s progenitor wind speed) are shared with SN 2008iy, suggesting that it too had an LBV-like progenitor.

As mentioned above, an alternative way to generate a wind-density parameter that is increasing with distance from the progenitor is to increase the progenitor wind speed in the years leading up to the SN event. A relatively mild change in the wind speed by a factor of 3 could, in fact, explain the observed increase in luminosity. During the post-main-sequence evolution of very massive stars a slightly more extreme transition is expected as stars exit the RSG or LBV phase, with wind speeds of 10100 km s, to become Wolf-Rayet stars, with typical wind speeds of 1000 km s. As this fast wind expands into the slower wind it will sweep up a thin, dense shell at the interface of the two winds and thus create a wind-blown bubble (e.g., Dwarkadas 2005). A SN exploding in one of these bubbles will appear as a normal SN until the ejecta reach the edge of the bubble. As the ejecta overtake the thin shell the appearance of the SN will dramatically change as CSM interaction begins to provide a significant contribution to the broad-band luminosity. This is the precise scenario proposed for the Type IIn SN 1996cr, for which Bauer et al. (2008) found an optical luminosity that is clearly decreasing between 1996 and 1999, but the radio emission sharply increases in late 1997 while X-ray emission abruptly turns on some time between 1998 Mar. and 2000 Jan. The X-ray emission is especially interesting because after the abrupt initial rise, it continues to rise for at least the next seven years, a feature which had not previously been observed for any X-ray SN. A similar scenario is proposed for SN 2001em, classified as a Type Ic, but which showed unexpectedly strong radio and X-ray emission yr after explosion, as well as a FWHM 1800 km s H emission line (Soderberg, Gal-Yam & Kulkarni, 2004). Each of these late-time peculiarities can be understood if the progenitor of SN 2001em lost the remainder of its hydrogen envelope during a phase of large mass-loss (2–10) M yr, about (1–2) yr prior to core collapse (Chugai & Chevalier, 2006). After the hydrogen envelope has been lost, a fast wind from the progenitor sweeps the hydrogen into a shell. The interaction of the Type Ic ejecta with this swept-up shell give rise to the unusual late-time emission.

Can the long optical rise be the result of SN 2008iy exploding inside a wind-blown bubble? There is a somewhat sharp rise in the optical ( 2 mag brightening during the 68 days between the last DS non-detection and the first CRTS detection of the SN) followed by a slow and steady increase over the next 400 days, which may hint that the SN exploded in such a wind-driven cavity. However, we do not favour this model. In the wind-blown bubble scenario, after peak the thin shell has been overtaken by the ejecta, and the luminosity is powered by the interaction of the ejecta with the slower, older wind. To explain this, the wind on day 711 requires   10 M yr and km s, which requires LBV-like mass loss (see above). The wind-blown bubble scenario therefore seems to unnecessarily complicate the scenario discussed above, which is needed to explain the late-time observations, as it requires the transition from a LBV to a Wolf-Rayet star. Yet the addition of this transition does not clearly model any observed properties that could not otherwise be explained.

Additionally, we see no evidence for a normal SN in the years leading up to the initial detection of SN 2008iy as would be expected in the wind-blown bubble scenario. While it would be impossible to completely rule out a SN prior to the first detection of SN 2008iy on 2007 Sep. 13 (for instance, the field is virtually unobservable for 3 months each year while it is behind the Sun), DS images dating to 2004 show no evidence for such an event. These DS images have similar depths to those quoted in Section 2.1, which at the distance of the host galaxy corresponds to an absolute magnitude of mag. This detection threshold is well below the mean peak magnitude for stripped-envelope SNe: and mag for SNe Ib, Ic, and IIb, respectively (Li et al., 2010a). Stronger constraints on the presence of a stripped-envelope SN prior to 2007 Sep. 13 are based on the individual DS images. There are DS images of the field of SN 2008iy from 2004 Apr. and Jul., 2005 May, Jun., and Jul., 2006 May and Jun., and 2007 Apr., May, Jun., and Jul. Adopting the mean peak magnitudes and mean light curves for stripped-envelope SNe from Li et al. (2010a), we find that on average (note that there is a great deal of dispersion in the peak absolute magnitude and duration of stripped-envelope SNe), SNe Ib and IIb are observable for 70 days above the DS detection threshold, while SNe Ic are observable for only 45 days above the DS detection threshold. In addition to not being detected during any of the months listed above, we can also rule out SNe Ib and IIb in the 2 months prior to those listed above, while SNe Ic can be ruled out in the 1.5 months prior to those above. Therefore, in the 3.5 years prior to SN 2008iy we can rule out SNe Ib or IIb in 21 out of 42 months, while SNe Ic can be ruled out for 18 out of 42 months.

Perhaps the most intriguing points about the progenitor of SN 2008iy are the implications for the progenitors of the very long-lived SNe IIn discussed in Section 4.2, such as SN 1988Z. It is interesting that episodic, LBV-like eruptions, which we argue occurred shortly before SN 2008iy, may be applicable to SNe 1988Z, 1995N, and 1986J, each of which has relatively poor constraints on the actual date of explosion.

SN 1988Z was first observed after peak (Stathakis & Sadler, 1991), with an observational constraint on the rise time of 250 days (Turatto et al., 1993). It was argued by Turatto et al. (1993) that the rise time of SN 1988Z must have been short, in part because at the time no other known SN looked quite like SN 1988Z. SN 2008iy, which is a virtual clone of SN 1988Z at late times, does provide an example of a SN with a long rise time and a peak absolute magnitude that is brighter than the discovery magnitude of SN 1988Z. This negates the necessity of a short rise to peak for SN 1988Z. We submit that it is possible that SN 1988Z had a long rise time, though we note that with no observations during the 250 days prior to discovery, there is no way to definitely prove this claim one way or another. A long rise to peak would, however, further strengthen the similarity of SN 2008iy and SN 1988Z.

Similarly, SNe 1986J and 1995N have poor constraints on the rise time. SN 1986J was discovered in the radio, with constraints on the explosion date ranging from 1982 to 1984; constraints on the optical rise are even worse, owing in part to the large extinction in the host galaxy, 2 mag (see Rupen et al. 1987). Typically, 10 months prior to discovery is adopted as the explosion date for SN 1995N (see Fox et al. 2000). However, this age of 10 months is based on the H profile of SN 1995N, which looked similar to the H profile of SN 1993N 10 months after SN 1993N had been discovered (Benetti, Bouchet & Schwarz, 1995). We note that SNe IIn are a very heterogeneous subclass, and in our experience spectral ages of SNe IIn are not reliable, especially at times greater than a few months. Thus, poor optical constraints mean that SNe 1986J, 1988Z, and 1995N all may have had long rise times, by the standards of typical SNe II whose rise times are 1 week (Li et al., 2010a).

4.4 Similarities to Very Luminous SNe IIn

The long rise time and broad, symmetric evolution of SN 2008iy around peak optical emission is reminiscent of the Type IIn VLSNe 2006gy and 2008fz (Ofek et al., 2007; Smith et al., 2007; Drake et al., 2009b). Applying the “shell shock” model of Smith & McCray (2007), which was originally developed to explain the light curve of SN 2006gy, does not provide a physically plausible scenario for SN 2008iy because the relatively low  and large radius at peak imply that the CSM shell was not opaque. The “shell shock” model argues that the extreme luminosity of these SNe is powered via a shock running into a dense, optically thick shell. Radiation from the shock is thermalised by the optically thick gas and must diffuse out of the shell.

Nevertheless, SN 2008iy does share a few similarities with the VLSNe IIn. Like SNe 2006gy and 2006tf, SN 2008iy shows evidence for a 100 km s pre-shock CSM wind (see Smith et al. 2007, 2008a), and like SNe 2006gy, 2006tf, and 2008fz, SN 2008iy experienced a period of enhanced mass loss during the decades prior to explosion. The difference between these systems is that the mass-loss rate from SN 2008iy,   M yr, was less extreme than that from SNe 2006gy, 2006tf, 2008fz, where   M yr (e.g., Smith et al. 2010). Also, the time between the period of enhanced mass loss and the SN was longer for SN 2008iy, 55 years, than for SNe 2006gy and 2006tf, years (Smith et al., 2010, 2008a). The result of these differences is that SN 2008iy did not reach as extreme a peak luminosity and took considerably more time to reach peak optical output than the VLSNe IIn. Finally, if the late-time NIR excess is the result of an IR dust echo, this would be similar to SN 2006gy (Smith et al., 2008b; Agnoletto et al., 2009; Miller et al., 2009b). Smith et al. (2008b) and Miller et al. (2009b) argue that a giant eruption 1000 year prior to SN 2006gy could potentially create the dust shell giving rise to the echoes, and a similar shell around SN 2008iy may explain the observed NIR excess.

The connection between VLSNe and very massive stars, such as Car, was first made by Smith et al. (2007) because the large mass-loss rates needed to explain the extreme optical luminosity are reminiscent of Car during the great eruption of 1843. It is interesting to note that were Car to explode as a SN today, its appearance would be less like the VLSNe IIn discussed above and more similar to SN 2008iy. The reason for this is that with the eruption happening 150 yr ago, the ejected shell surrounding Car has had sufficient time to expand ( cm) and become clumpy (Morse et al., 1998), with an optical depth that is now near unity (Davidson et al., 2001). Thus, Car does not have the compact ( cm), very optically thick shell required to generate an extreme peak luminosity following a SN. Instead, as the SN ejecta sweep through the large shell,191919The shell around Car is much bigger than the one around SN 2008iy because the wind speeds are greater, km s (Smith, 2006), and the nebula is older, 165 yr relative to 55 yr. they will successively overtake more and more mass within the clumpy CSM. This will likely give rise to a long rise time, similar to what was seen in SN 2008iy.

4.5 The Host of SN 2008iy

At the adopted distance to SN 2008iy, our detection of the host galaxy in stacked SDSS images (see Section 2.3) means that the host has an absolute magnitude of mag. This is significantly fainter than the Small Magellanic Cloud (with mag). We do not detect narrow emission lines from the host in our SN spectra in order to make a direct measurement of the metallicity. The prospects for such a measurement in the near future are not good: if SN 2008iy continues to evolve like SN 1988Z, light from the SN may dominate over light from the host galaxy for years to come.

We can, however, estimate the metallicity based on the absolute magnitude of the host. Lee et al. (2006) use 27 dwarf irregular galaxies to determine the luminosity-metallicity relation for low-mass galaxies, and following from their Equation 1, we find , assuming . The uncertainty in this value is large, perhaps as great as 0.3 dex, based both on our assumption of mag for the host and the substantial scatter in the luminosity-metallicity relationship for faint galaxies (Lee et al. 2006 find a scatter of 0.16 dex), yet this nevertheless shows that SN 2008iy occurred in a metal-poor galaxy.

It has recently been suggested that the unusual SNe discovered by the non-targeted transient surveys, such as CRTS, preferentially occur in subluminous, possibly metal-poor host galaxies (Miller et al., 2009a; Drake et al., 2009b). SN 2008iy is yet another example of an unusual SN in a low-luminosity host. We caution, however, that a number of biases may be skewing initial impressions about the hosts of these unusual SNe. Preliminary calculations show that these VLSNe are rare (Miller et al., 2009a; Quimby et al., 2009). Both the large peak luminosity and slow evolution of SN 2008iy mean that similar SNe would be easily detectable in the galaxies of targeted SN surveys. The lack of other examples of SNe with 400 day rise times suggests that SN 2008iy is also rare. The CRTS, however, does not employ image subtraction during their search for transients; instead they use aperture photometry to find new sources, or sources with large increases in flux, and flag those as possible transients. Consequently, their survey is biased toward the discovery of intrinsically bright SNe in faint host galaxies. From the Lick Observatory Supernova Search (LOSS), we know that SNe IIn are rare, regardless of whether they are very luminous or have long rise times (Li et al., 2010b). Yet, even LOSS, which targets specific galaxies, may be biased in that it observes relatively few subluminous galaxies. New and upcoming surveys, such as the Palomar Transient Factory (Law et al., 2009; Rau et al., 2009), which employ image subtraction and survey large, non-targeted fields of view, will not suffer from the same biases discussed above, and hence will be in a better position to address whether these unusual SNe preferentially occur in subluminous host galaxies.

5 Conclusions

We have reported on observations of the Type IIn SN 2008iy, which took 400 days to reach peak optical output. There are few known SNe with optical rise times 50 days, and SN 2008iy is the first with a rise time 1 year. We argue that this long rise to peak is caused by the interaction of the SN ejecta with a dense CSM; radioactivity is unlikely to drive a 400-day rise. Furthermore, the late-time optical decay, 0.4 mag (100 days), is slower than that of Co, which provides further evidence that radioactive heating is not a dominant energy source for SN 2008iy. Spectroscopically, SN 2008iy is very similar to SN 1988Z at late times. SN 1988Z is understood to have exploded in a dense, clumpy CSM (Chugai & Danziger, 1994), which we argue was also the case for SN 2008iy. We detect SN 2008iy in X-rays with a total luminosity erg s, which is similar to that of the Type IIn SNe 1988Z and 1995N (Fox et al., 2000). Similar to other SNe IIn, SN 2008iy has a growing NIR-excess at late times. SN 2008iy had a peak absolute magnitude of mag and a total radiated energy of erg in the optical (assuming no bolometric correction).

The steady increase in optical luminosity over a 400-day period means that the wind-density parameter, , increased over a distance of 1.7 cm from the SN. We propose two possible scenarios to explain this increase in : (i) the progenitor experienced an episode of LBV-like, eruptive mass-loss 55 years prior to the SN, or (ii) the wind speed of the progenitor was increasing during the years leading up to core collapse. We prefer the former scenario, as the later adds unnecessarily complicated pieces to the puzzle without providing a unique solution. Our favoured scenario provides yet another piece of evidence that some SNe IIn are connected to LBV-like progenitors (see Gal-Yam et al. 2007, and references therein). We find that the host of SN 2008iy is a subluminous dwarf galaxy, though we caution against premature conclusions that unusual SNe, specifically those that are very luminous or have very long rise times, preferentially occur in low-mass dwarf galaxies.

Finally, we close with some predictions for the late-time behaviour of SN 2008iy. There are examples of SNe IIn whose luminosity dramatically drops after the SN ejecta overtake the dense CSM (e.g., SN 1994W; Sollerman, Cumming & Lundqvist 1998). However, the similarities to SN 1988Z suggest that SN 2008iy could continue interacting, and thus remain luminous, for several years. This would allow long-term monitoring in the radio, X-ray, and optical, like SN 1988Z (Williams et al., 2002; Schlegel & Petre, 2006; Aretxaga et al., 1999). We predict that SN 2008iy is a luminous radio source, like SN 1988Z (Van Dyk et al., 1993), though we note that at deep observations may be necessary for detection. The increasing -band luminosity from day 560 to 710 is likely due to the presence of dust, and we predict that SN 2008iy will also be luminous in the mid-IR (35 m). The data are insufficient to distinguish between newly formed dust or dust that was present prior to the SN, but future medium- to high-resolution spectroscopy could distinguish between these two cases. If new dust is being formed, it should result in a systematic blueshift in the line profiles, as the dust creates an optically thick barrier to radiation from the receding SN ejecta.


A.A.M. would like to thank D. Poznanski for useful discussions that helped improve this paper and M. Modjaz for discussions concerning the metallicity of the host. We thank Neil Gehrels for approving the Swift ToO request for SN 2008iy, which was submitted by Dave Pooley, and the Swift team for scheduling and obtaining those observations. We acknowledge the use of public data from the Swift archive. Cullen Blake, Dan Starr, and Emilo Falco assisted with the operation of PAIRITEL. We wish to thank the following Nickel observers: P. Thrasher, M. Kislak, J. Rex, J. Choi, I. Kleiser, J. Kong, M. Kandrashoff, and A. Morton. We thank the referee, Nikolai Chugai, for suggestions that helped to improve this paper.

A.A.M. is supported by the NSF Graduate Research Fellowship Program and DOE grant #DE-FC02-06ER41453. J.S.B.’s group is partially supported by NASA/Swift grant #NNX08AN84G. A.V.F.’s group is grateful for the financial assistance of NSF grant AST–0908886 and the TABASGO Foundation. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, the camera loan from the University of Virginia, and the continued support of the SAO and UC Berkeley. The PAIRITEL project is partially supported by NASA/Swift Guest Investigator Grant #NNX08AN84G. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration (NASA) and the National Science Foundation (NSF). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; it was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain.

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