SN 2006X in M100

Optical and Near-Infrared Observations of the Highly Reddened,
Rapidly Expanding Type Ia Supernova 2006X in M100

Xiaofeng Wang1 2 , Weidong Li1 , Alexei V. Filippenko1 , Kevin Krisciunas3 , Nicholas B. Suntzeff3 ,
Junzheng Li2 , Tianmeng Zhang4 , Jingsong Deng4 , Ryan J. Foley1 , Mohan Ganeshalingam1 ,
Tipei Li2 , YuQing Lou2 , Yulei Qiu4 , Rencheng Shang2 , Jeffrey M. Silverman1 ,
Shuangnan Zhang2 , and Youhong Zhang2
1affiliation: Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA; wangxf@astro.berkeley.edu .
2affiliation: Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, 100084, China; wang_xf@mail.tsinghua.edu.cn .
3affiliation: Physics Department, Texas A&M University, College Station, Texas, 77843
4affiliation: National Astronomical Observatories of China, Chinese Academy of Sciences, A20, Datun Road, Beijing 100012, China.
Abstract

We present extensive optical (), near-infrared () light curves and optical spectroscopy of the Type Ia supernova (SN) 2006X in the nearby galaxy NGC 4321 (M100). Our observations suggest that either SN 2006X has an intrinsically peculiar color evolution, or it is highly reddened [ mag] with , much lower than the canonical value of 3.1 for the average Galactic dust. SN 2006X also has one of the highest expansion velocities ever published for a SN Ia. Compared with the other SNe Ia we analyzed, SN 2006X has a broader light curve in the band, a more prominent bump/shoulder feature in the and bands, a more pronounced secondary maximum in the and near-infrared bands, and a remarkably smaller late-time decline rate in the band. The color evolution shows an obvious deviation from the Lira-Phillips relation at 1 to 3 months after maximum brightness. At early times, optical spectra of SN 2006X displayed strong, high-velocity features of both intermediate-mass elements (Si, Ca, and S) and iron-peak elements, while at late times they showed a relatively blue continuum, consistent with the blue and colors at similar epochs. A light echo and/or the interaction of the SN ejecta and its circumstellar material may provide a plausible explanation for its late-time photometric and spectroscopic behavior. Using the Cepheid distance of M100, we derive a Hubble constant of km s Mpc (statistical) from the normalized dereddened luminosity of SN 2006X. We briefly discuss whether abnormal dust is a universal signature for all SNe Ia, and whether the most rapidly expanding objects form a subclass with distinct photometric and spectroscopic properties.

dust, extinction – distance scale – galaxies: individual (NGC 4321) – supernovae: individual (SN 2006X)

1 Introduction

Type Ia supernovae (SNe Ia) are arguably the most accurate tools available for probing the expansion history of the Universe, as their luminosities at maximum light can be calibrated to an uncertainty of 15% via several empirical relations between their luminosity and light/color curves (Wang et al. 2006, and references therein). Based on studies of SN Ia apparent brightness as a function of redshift, Riess et al. (1998) and Perlmutter et al. (1999) were the first to propose that the expansion of the Universe is currently accelerating (for a review see, e.g., Filippenko 2005). This remarkable result, which suggests that the Universe is primarily composed of mysterious dark energy, was subsequently confirmed by more studies using SNe Ia (Barris et al. 2003; Tonry et al. 2003; Knop et al. 2003; Riess et al. 2004, 2007; Astier et al. 2006; Wood-Vasey et al. 2007), and by independent methods such as the power spectrum of fluctuations in the cosmic microwave background radiation (e.g., Spergel et al. 2003, 2007) and baryon acoustic oscillations (Eisenstein et al. 2005).

Despite the success of using SNe Ia as cosmological probes, a disconcerting fact is that details of the properties of SN Ia progenitors and their environments remain poorly understood. It is generally believed that a SN Ia is produced by a carbon-oxygen (CO) white dwarf (WD) accreting matter from a companion star in a binary system. However, the nature of the companion star in the binary system is still unclear: it could be a main-sequence star, a subgiant, or an evolved red giant (Nomoto, Iwamoto, Koshimoto 1997), or even another degenerate CO WD (Iben & Tutukov 1984; Webbink 1985).

Studying the absorption by dust toward SNe Ia may provide a unique way to peer into their local environments and hence set constraints on the properties of their progenitor system. If the dust enveloping the SNe is totally or partially produced by the progenitor evolution, the ratio of the total to selective absorption [] may differ from that of normal interstellar dust (e.g., Wang L 2005). Moreover, accurate determination of the absorption toward a SN Ia helps establish the accurate luminosity required for precision cosmology.

Several studies of global color fits to SNe Ia have suggested that the dust obscuring SNe Ia in their host galaxies may differ from the dust observed in the Milky Way Galaxy (Riess et al. 1996; Phillips et al. 1999; Altavilla et al. 2004; Reindl et al. 2005; Wang et al. 2006): the measured value of is often found to be smaller than the canonical Galactic value of 3.1. We measure an average from a compilation of published values111Methods that do not separate the intrinsic color variation and the host-galaxy reddening from the observed color would give even lower values (Tripp 1997; Astier et al. 2006; Wang L et al. 2006a).. The sample of well-observed, highly extinguished SNe Ia is small but growing, offering the opportunity to study variations of the extinction law on an object-by-object basis. In almost all cases, is found to be smaller than 3.1 (Krisciunas et al. 2006a; Elias-Rosa et al. 2006, hereafter ER06). It is interesting to investigate whether smaller than 3.1 is universal to all SNe Ia, or just applies to a few or highly reddened events.

SN 2006X is a bright, nearby, highly reddened SN Ia, and is favorable for a detailed study of reddening and dust properties. The recent report of variable, interstellar absorption Na I D lines the in high-resolution spectra of SN 2006X indicates of the presence of circumstellar material (CSM) around SN 2006X, which may be related to the stellar wind blown from the companion star (Patat et al. 2007). Here, we present extensive photometric and spectroscopic observations of SN 2006X, enabling us to study its intervening dust and other characteristics. The paper is organized as follows. The observations and data reduction are described in §2, while §3 presents the light curves, the color curves, and the extinction estimate. The spectral evolution is given in §4. We determine the distance and luminosity of the SN in §5. Our discussion and conclusions are given in §6.

2 Observations and Data Reduction

SN 2006X was discovered independently on 7.10 February 2006 (UT dates are used throughout this paper) by S. Suzuki and M. Migliardi (IAUC 8667), with J2000 coordinates = 122253.90 and = 154832.90. It is W and S of the center of the nearby galaxy NGC 4321 (M100), a grand-design Sbc galaxy in the Virgo cluster having a Cepheid distance of mag (Freedman et al. 2001). A spectrum of SN 2006X taken shortly after its discovery shows it to be an early SN Ia (Quimby et al. 2006), similar to that of SN 2002bo 1–2 weeks before maximum light (Benetti et al. 2004) but with a redder continuum.

2.1 Photometry

Our photometric observations of SN 2006X began on 2006 February 8.15, 11 days before -band maximum. Data were obtained with three telescopes: the 0.80 m THCA-NAOC Telescope (TNT) at Beijing Xinglong Observatory (BAO) in China, the 0.76 m Katzman Automatic Imaging Telescope (KAIT; Filippenko et al. 2001) at Lick Observatory in the U.S., and the 1.3 m telescope at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The TNT observations were obtained using a pixel back-illuminated charge-coupled device (CCD) with a field of view (FOV) of ( pixel), the KAIT observations were performed using an Apogee AP7 camera with a FOV of ( pixel), and the CTIO 1.3 m observations were obtained using the dual-channel optical/near-infrared (IR) camera ANDICAM having an optical FOV of ( pixel) and an IR FOV of ( pixel). Broad-band images were taken with all three telescopes, while the TNT also followed SN 2006X in the band and the CTIO 1.3 m telescope sampled the and bands.

As shown in Figure 1, SN 2006X is located between a relatively bright foreground star and the inner edge of one spiral arm of NGC 4321; thus, light contamination needs to be taken into account when measuring the SN flux. One way to do this is to apply galaxy subtraction. Template images of NGC 4321 in various bands were taken with KAIT and TNT on 2007 March 14 and 16 (respectively), roughly one year after the discovery of SN 2006X. For the CTIO 1.3 m observations, we used pre-explosion and images of NGC 4321 obtained on 24 April 2000 with the Apache Point Observatory 3.5 m telescope in New Mexico.

To perform image subtraction, the image containing SN 2006X is first geometrically registered to the corresponding template image. Next, the total fluxes of corresponding foreground stars in the SN and template images are compared, and an appropriate scale factor is applied to the SN image in order to match the template image. Also, the point-spread functions (PSFs) of the two images are convolved to match. The template is then subtracted from the SN image, leaving the SN with a background that is free from host-galaxy contamination. The final step is to perform standard PSF-fitting (or aperture) photometry to measure the instrumental magnitudes for the SN and the local standard stars with the IRAF222IRAF, the Image Reduction and Analysis Facility, is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation (NSF). DAOPHOT package (Stetson 1987). From the late-time (HST) Advanced Camera for Survey (ACS) archival images (Proposal 10991 by Arlin Crotts 2006), we speculate that SN 2006X was 22.0 mag in and 21.5 mag in about one year after maximum. This lingering light barely affects the early-time photometry but it probably results in underestimating the luminosity of SN 2006X by 3-6% when the SN becomes as faint as 18 19 mag.

The transformation from the instrumental magnitudes to the standard Johnson (1966) and Kron-Cousins (1981) systems is established by observing, during a photometric night, a series of Landolt (1992) standards covering a large range of airmasses and colors. The color terms obtained on different photometric nights show some differences, and their average values are listed in Table 1 for the filters used in the TNT, KAIT, and CTIO 1.3 m observations of SN 2006X.

A total of 10 photometric nights (2 for TNT, 3 for KAIT, and 5 for the CTIO 1.3 m) were used to calibrate 10 local standard stars in the field of SN 2006X. Table 2 lists the final calibrated magnitudes and their uncertainties, while Table 3 presents the near-IR -band and -band magnitudes. Only one photometric night was used to do the -band calibration, so the calibrated magnitudes may have larger errors. The near-IR magnitudes of Star 10 were measured on 14 nights with respect to the Persson et al. (1998) standards P9144 and LHS2397a. The measured and magnitudes are 0.07 mag brighter than the values from the 2MASS survey, which obtained = 14.793(0.025) mag and = 13.995(0.040) mag.

These local standard stars are then used to transform the instrumental magnitudes of SN 2006X to the standard system, and the final results of the photometry are listed in Table 3 and Table 4. Note that the -band data shown for CTIO 1.3 m telescope include the S-corrections (see details in §3.1) which are listed in Table 5. The estimated error shown in parentheses is a quadrature sum of uncertainties in the photometry and the calibrations. The main source of error comes from the photometry, caused by photon noise and uncertainties in the image subtraction.

2.2 Spectroscopy

Spectra of SN 2006X were primarily obtained with the 2.16 m telescope at BAO using the Cassegrain spectrograph and BAO Faint Object Spectrograph and Camera (BFOSC), and with the 3.0 m Shane telescope at Lick Observatory using the Kast double spectrograph (Miller & Stone 1993). Two very late-time spectra were also obtained at the W. M. Keck Observatory: one with the Low Resolution Imaging Spectrometer (LRIS; Oke et al. 1995) mounted on the 10 m Keck I telescope, and the other with the Deep Extragalactic Imaging Multi-Object Spectrograph (DEIMOS) mounted on the 10 m Keck II telescope. A journal of spectroscopic observations is given in Table 6.

All spectra were reduced using standard IRAF routines (e.g.,Foley et al. 2003). Extraction of the SN spectra was carefully performed to avoid contamination from the nearby star and the spiral arms of the galaxy. For the Kast observations, flatfields for the red-side spectra were taken at the position of the object to reduce near-IR fringing effects. Flux calibration of the spectra was performed by means of spectrophotometric standard stars observed at similar airmass on the same night as the SN. The spectra were corrected for continuum atmospheric extinction using mean extinction curves for BAO and Lick observatory; also telluric lines were removed from the Lick (but not BAO) data. For spectra observed at Lick and Keck, the slit was always aligned along the parallactic angle to avoid chromatic effects in the data (Filippenko 1982). This procedure was not adopted at BAO, however, and it may not significantly affect the continuum shape as the airmass was usually low (1.1) when getting these spectra for SN 2006X. In general, the relative spectrophotometry is quite good, consistent with the broadband photometry within about 5%.

3 Light Curves and Spectra

3.1 Optical and Near-IR Light Curves

The light curves of SN 2006X are presented in Figure 2. No K-corrections have been applied to any of the magnitudes due to the small redshift of SN 2006X (). For all the bands we have excellent temporal coverage, especially around maximum light. In general the optical measurements obtained with TNT, KAIT, and the CTIO 1.3 m telescope are consistent with each other within 0.05 mag, except in the band where differences are more noticeable. We find that the TNT -band magnitudes are systematically brighter than those of KAIT by mag and also brighter than those of the CTIO 1.3 m telescope, especially around the dip immediately after maximum where the discrepancy reaches 0.2 mag. This larger difference is likely caused by the different instrument response function in the band for the different systems.

Besides the usual color-term corrections, additional magnitude corrections between instrumental and standard bandpasses (S-corrections; Stritzinger et al. 2002) are sometimes required for the filters that are different from those defined by Bessell (1990). The filters amounted on TNT are standard Johnson-Cousins system, however, the filter transmission curves are unavailable. We obtained the S-corrections for observations of the CTIO 1.3 m telescope (see Table 5), except in and bands where the corrections were found to actually increase the systematic differences of the photometry obtained with different telescopes (e.g., Kriscusnias et al. 2003). We thus have chosen to let the ANDICAM and photometry stay as they are. The S-corrections for the filters closer to Bessell’s recipe are generally small in (e.g., 0.05 mag) but probably significantly larger in and (e.g., Pastorello et al. 2007). This is demonstrated by the consistency of the raw magnitudes of TNT and KAIT with the S-corrected magnitudes of the CTIO 1.3 m in and bands within their errors (see Fig.2). To account for the -band magnitude difference between the TNT, KAIT, and the CTIO 1 m telescope, we assign a systematic error of 0.10 mag for all the -band magnitudes in the following analysis.

A polynomial fit to the band light curve around maximum yields mag on JD 2,453,786.17 0.35 (2006 February 19.93). This means that our observations started from 11.27 d and extended to +116.32 d with respect to the time of maximum. Likewise, the light curve reached a peak magnitude of on JD 2,453,789.11 0.29, about 2.9 d after maximum. The fitting parameters for the maxima in the other bands are presented in Table 7, together with the late time decline rates (see below). From the and light curves we derived an observed mag333The true for SN 2006X is , taking into account the reddening effect on the light-curve shape (Phillips et al. 1999). and mag. We also measured the color at 12 d after maximum to be mag. These colors are much redder than the intrinsic values shown by other SNe Ia with similar (see more discussion in §3.3), suggesting that SN 2006X suffered significant line-of-sight reddening.

In Figures 38 we compare the light curves of SN 2006X with those of other well-observed, nearby SNe Ia having similar values, including SNe 1994D (; Richmond et al. 1995; Patat et al. 1996), 1998bu ( = 1.04; Jha et al. 1999), 2002bo ( = 1.15; Benetti et al. 2004; Krisciunas et al. 2004), 2002er ( = 1.32; Pignata et al. 2004), 2003cg ( = 1.25; ER06), and 2005cf ( = 1.12; Pastorello et al. 2007). The light curves of SN 1984A ( = 1.20; Barbon et al. 1989), though not as well observed as those of the other SNe in the comparison, are also included because SN 1984A shares many similar properties with SN 2006X, especially in the spectroscopy and late-time photometry. All the light curves have been normalized to the epoch of their -band maximum and shifted in peak magnitude to match those of SN 2006X.

Figure 3 shows that the observed -band light curve of SN 2006X is slightly broader than those of the other SNe Ia around maximum light, but is comparable to that of SN 2003cg which also suffered significant reddening. Two effects, both associated with large amounts of reddening, might explain why SNe 2003cg and 2006X are broader than other SNe in comparison. As demonstrated by Phillips et al. (1999) and Jha et al. (2007), the total-to-selective absorption ratio, , may vary with the supernova phase. For instance the true value of at 15 d past maximum is found to be smaller than that near maximum by about 0.15 (Jha et al. 2007). This would subsequently broaden the light curves of the reddened SNe by . On the other hand, the change of the overall spectral shape due to the high reddening may shift the effective bandpass at the shorter wavelengths to the longer wavelengths that are characteristic of broader light-curve peaks (see ER06 for a similar argument for SN 2003cg). This may also contribute to the broader peak in . Another possible feature of SN 2006X in the band is the late-time light curve, which despite the large error bar for each measurement, seems to be brighter and possibly declines more slowly than the other SNe.

Figure 4 shows the comparison in the band. While the light curves near maximum are similar to each other, they diverge at late times. Compared to other SNe Ia, SNe 2006X, 1984A, and 2002bo have relatively higher (by 0.30.5 mag) luminosity after  d, and their light curves decline more slowly. We measured a late-time decline rate of mag (100 d) for SN 2006X at  d, which is comparable to the radioactive decay rate of 0.98 mag (100 d) for the CoFe decay. The decline rates for SNe 1984A and 2002bo are slightly higher, mag (100 d) and mag (100 d), respectively. All these decline rates are significantly smaller than the typical value of a normal SN Ia, mag (100 d), as exhibited by the other SNe Ia in the comparison.

The -band light curve comparison is shown in Figure 5. At around maximum, SN 2006X is slightly broader, and shows a more prominent ”shoulder” feature at weeks than other SNe Ia. Part of the reason for this may be that compared to other SNe Ia, SN 2006X has higher reddening, and the effective bandpass is shifted more toward the band, which is broader than and has a prominent shoulder feature. It is also possible that there is an intrinsic scatter in the strength of the shoulder feature in the -band light curves of SNe Ia. In the same manner as the definition of , we computed mag for SN 2006X. This is similar to that of SNe 2003cg, 1998aq, and 2005cf [ mag, , and mag, respectively], but smaller than that of SNe 1994D and 2002er [ mag and mag, respectively]. At late times, SN 2006X has a similar evolution as SN 2002bo, and both are brighter than other comparison SNe Ia. There are no obvious differences in the late-time decline rates among the SNe.

As shown in Figures 6 and 7, SN 2006X exhibits a more prominent ”plateau” feature in the band and a stronger secondary maximum in the band than other SNe Ia. The and light curves of SNe Ia are similar to each other before  d, but diverge after that. There are considerable differences in , the duration of the plateau phase in the band444D measures the interval of the two inflection times, and , of the post-maximum -band light curves. The inflection time is defined as the moment when the first derivative at the transition phase S = is minimal (e.g., Elmhamdi et al. 2003). and the time when the band reaches the second maximum []: SN 2006X has  d, and  d, while SN 1994D has  d and  d. At late times, SN 2006X has an evolution similar to that of SN 2002bo in the band, and they are brighter than other SNe Ia. The two SNe, however, have different decline rates in the band, and SN 2006X is the brightest object in the comparison.

In Figure 8, the -band and -band light curves of SN 2006X are compared with those of SNe 1998bu, 2002bo, 2003cg, and 2005cf. The light curves of the well-observed SN 2001el ( mag; Krisciunas et al. 2003) are also overplotted (see the dotted curves). As in the optical bands, the overall light curves of SN 2006X in and resemble closely those of SN 2002bo. After the initial peak, both of these SNe show a stronger secondary maximum feature in the bands than other SNe Ia in the comparison. In SN 2001el, the second-peak feature is somewhat less pronounced; the light curve remains relatively flat from day +11 to +31. Note that there is marginal evidence for a third maximum (or shoulder) in the near-IR light curves of SN 2006X at 70 d after maximum. Kasen (2006) has come up with an explanation for the secondary maximum and has predicted that some SNe Ia might show a third maximum at 80 d. The variation of the secondary maximum of the near-IR light curves can be related to the abundance stratification in SNe Ia, the concentration of iron-group elements, and the progenitor metallicity (Kasen 2006).

3.2 Optical and Near-IR Color Curves

The optical color curves of SN 2006X (, , , and ) are presented in Figure 9. The colors of SN 2006X are much redder than those of the normal Ia SN 2005cf (the triangles) with negligible reddening, suggesting a significant amount of reddening toward SN 2006X. Also overplotted in these panels are the color curves of SNe 1994D, 1998bu, 2002bo, 2002er, 2003cg, all arbitrarily shifted to match the observed colors of SN 2006X at maximum.

The color (Fig. 9a) of SN 2006X does not become progressively redder in a linear fashion after maximum as the other SNe Ia do, but has a shoulder or plateau phase for about two weeks. A similar feature is observed in the heavily extinguished SN 2003cg. It is unclear whether this feature is caused by the high reddening of these two objects. After weeks, the colors of SN 2006X seem to be bluer than those of the comparison SNe Ia, but the error bars of the measurements are relatively large due to the poor -band data quality at late times.

The colors of all SNe in the plot (Fig. 9b) have a similar evolution before  d, although SN 2006X reached the bluest color a bit earlier, e.g. at 8.0 days rather than 5 days for the other comparison SNe. All the SNe Ia reach the reddest color at  d, although there are some differences in the time to reach the reddest color. The peak colors of the SNe Ia with smaller decline rates (or ) might occur later than those of the faster decliners (see also Figure 1 in Wang et al. 2005). We note that the color of SN 2003cg is redder than that of other SNe Ia by about 0.2 mag at the reddest peak according to the data from ER06. However, the photometric data based on the unpublished KAIT data of SN 2003cg do not have such a discrepancy. Compared with other SNe Ia, the most notable difference in the color evolution of SN 2006X is after  d: SN 2006X became bluer in a much faster pace, and showed an apparent difference from the Lira-Phillips relation (the dash-dotted line in the figure; see Lira 1995 and Phillips et al. 1999). Note also that the color of SN 1994D, although not well observed during this phase, suggests a faster evolution than the Lira-Phillips relation. Thus, as discussed in the more extreme case of the peculiar SN Ia 2000cx (Li et al. 2001), although the Lira-Phillips relation provides a method to estimate the extinction toward SNe Ia and may work in a statistical dataset, it should be used with caution for any individual SN Ia.

Given the relatively large differences seen in the and color evolution between SN 2006X and other SNe Ia in the comparison, it is surprising that all SNe Ia have similar color evolution except at very early times (Fig. 9c). The color of different SNe Ia reaches the bluest point at 12 d after maximum, then become progressively redder and reaches the maximum around day +31. After the peak the color curve moves gradually toward bluer colors. The similar evolution in the color is related to the closer match of the and photometry and also a smaller reddening effect.

The color curve of SN 2006X (Fig. 9d) exhibits a behavior which is very similar to those of the comparison SNe. All these SNe reached a minimum color at about 9 d after maximum. The following red peak occurred at around day +31. The only exception is SN 1994D, which showed a rapid increase in after the minima and then reached the peak value 4 d earlier than other SNe Ia.

Figure 10 shows the observed and colors of SN 2006X, along with those of SNe 1998bu, 2001el, 2002bo, 2003cg, and 2005cf (without color shift). All SNe Ia exhibit a deep minimum at –11 d, followed by a maximum at around day +32. Nevertheless the minus near- color of the comparison SNe Ia shows noticeable scatter, especially in where the magnitude contrast between the valley and peak can differ by more than 0.6 mag. The dashed curves in Fig. 10 represent the average loci of the and colors for normal SNe Ia (Krisciunas et al. 2000) that were reddened (shifted upward in Fig.10) by 1.72 mag and 1.95 mag, respectively. With respect to the average color curve, the and colors of SN 2002bo seem to better match those of SN 2006X.

In general, the overall color evolution of SN 2006X resembles most closely those of SN 2002bo and SN 2002er. Other comparison SNe Ia may match well with SN 2006X in and , but they show larger differences than SN 2006X in , . Both SN 2006X and SN 2003cg exhibited an atypical “shoulder” feature in for about two weeks immediately after maximum.

3.3 The Reddening Toward SN 2006X

The Galactic extinction toward NGC 4321/SN 2006X is mag (Schlegel et al. 1998), corresponding to a color excess of = 0.026 mag [adopting the standard reddening law of Cardelli, Clayton, & Mathis (1989)]. As suggested by the observed color curves of SN 2006X shown in Figures 9 and 10, SN 2006X may suffer a large amount of extinction within its host galaxy. In this section, we use two methods, global color-curve fitting and the method, to derive the host-galaxy reddening for SN 2006X. Both methods assume SN 2006X has colors similar to those of the other SNe Ia with either similar evolution in some colors, or comparable values. Given the somewhat unusual evolution in the (a plateau phase) and (an apparent deviation from the Lira-Phillips relation) colors, however, we caution that SN 2006X may have peculiar intrinsic colors, in which case it would be difficult to estimate the host-galaxy reddening toward SN 2006X.

From the comparison of color curves discussed in §3.2, we find that SN 2006X has a color evolution similar to that of SN 2002bo in and , and to that of SN 2002er in and . The host-galaxy reddenings of SNe 2002bo and 2002er have been determined by different groups (Reindl et al. 2005; Wang et al. 2006; Jha et al. 2007) to be mag and mag, respectively. We remove both the Galactic and the host-galaxy reddening from SNe 2002bo and 2002er and create their intrinsic color curves, and then apply different amounts of color excesses to the colors of SN 2006X and find the best global fit to these intrinsic color curves. We limit the fit to data with  d since the color of SN 2006X shows an apparently distinct evolution at late times. This procedure yields the average color excesses mag, mag, mag, mag, and mag.

Phillips et al. (1999) and Wang et al. (2005, 2006) proposed correlations between the light-curve width parameter and the intrinsic value (or ) or the color at 12 d after maximum [; or ], which can extend to other optical colors and even to the minus near- color (e.g., see Fig. 13 in Krisciunas et al. 2004). We use these two correlations to estimate the host-galaxy reddening of SN 2006X. Phillips et al. (1999) found that large reddening changes the observed , with , where and are the intrinsic and observed values, respectively, and is the total reddening toward the SN. Elias-Rosa et al. (2006) suggest that this relation works well for the high-reddening case of SN 2003cg. As we use to infer the intrinsic and , and derive the reddening toward SN 2006X, this is a loop process; we set as a free parameter, and iterate the fitting process until a convergence is achieved.

The color excesses derived from these two methods are consistent with each other within the uncertainties, and they are summarized in Table 8. The weighted average value of is mag, indicating that SN 2006X suffers heavy host-galaxy reddening.

Another independent way to estimate the reddening toward SN 2006X is to measure the equivalent width (EW) of the interstellar Na I D doublet, which is proposed to correlate with the amount of line-of-sight dust (Barbon 1990; Munari & Zwitter 1997). Due to the line blending and the low resolution, we only use the spectra at days +13, +68, and +75 to estimate the EW of Na I D. This yields an average EW 1.7 Å for SN 2006X (but see Patat et al. 2007 for measurements of high-resolution spectra and the possible variation of the Na I D EW). Using the prescription of Barbon (1990), EW (Na I D), we derive a reddening of mag toward SN 2006X. However, the prescription by Munari & Zwitter (1997), with EW (Na I D), suggests a larger reddening of mag. Both determinations are significantly smaller than that derived from the photometric method. Due to the large uncertainty in the correlation between the EW of the Na I D interstellar absorption and the reddening, we adopt the reddening derived from the photometric method in the following analysis.

3.4 The Extinction Coefficient

Assuming that the dust surrounding SN 2006X conforms with the extinction law proposed by Cardelli et al. (1989), we can set constraints on the value of . Cardelli et al. provide an analytic expression for the average extinction law, (where and are wavelength-dependent parameters), which well reproduce the average extinction curve of the Galaxy with . The value of for SN 2006X can be obtained by simultaneously matching different color excesses derived in §3.3 using our adopted of mag.

Figure 11 shows that the best fit to the mean color excesses ( minus ) is achieved with , which is much smaller than the standard value of 3.1. This gives a host-galaxy visual extinction (host) = 2.10 mag for SN 2006X. Excluding the color excesses derived from the near-IR bands in the fit yields the optimal = 1.580.15 and (host) = 2.24 mag. Allowing the best fit to vary marginally alters these results. Fitting the color excesses of SN 2006X using the standard extinction law () yields a reduced of 284.9 and 21.4 for the and the colors, respectively. This indicates that the dust surrounding SN 2006X is quite different from that observed in the Galaxy, probably of a much smaller grain size than that of typical interstellar dust. Note that the derived value is just the average value; the true value may actually show small variance with supernova phase. For comparison, we also determined the host-galaxy reddening of SN 2006X using the MLCS2k2 method (Jha et al. 2007), which gives (host) = 2.21 mag and , quite consistent with our determinations with the optical colors.

Besides SN 2006X, we note that other heavily extinguished SNe Ia also tend to suffer reddening by abnormal dust. In Table 9 we list the color excesses and derived for several SNe Ia with mag published in the literature. While the values of SNe 1995E and 2000ce are within of 3.1 given their relatively large error bars, the values of the other SNe are considerably smaller than 3.1. It is interesting to investigate whether the low derived for these highly extinguished SNe Ia is universal for all SNe Ia or an exception for a few events. Wang et al. (2006) derived an average for Hubble-flow SNe Ia. In the MLCS2k2 method, an value lower than 3.1 is often required to fit heavily reddened SNe Ia. More SNe Ia with well-observed multicolor light curves will help diagnose the properties of the dust surrounding SNe Ia. We note that although the infrared light curves themselves suffer little from the dust absorption, their color differences depend more sensitively on the ratio than the optical colors (as indicated by the difference between the two curves with different in Fig. 11), so they are particularly suitable for studying the of SNe Ia.

4 Optical Spectra

Twelve optical spectra of SN 2006X obtained at BAO and Lick Observatory, spanning to +97.8 d, are displayed in Figure 12. Two late-epoch Keck spectra, taken at days +277.0 and +307.0, are also shown in the plot. The spectral evolution generally follows that of a typical SN Ia near maximum brightness, but with more pronounced absorption features at 3700 Å due to Ca II H&K, 6020 Å due to Si II 6355, and 8100 Å due to the Ca II near-IR triplet. Other features at early times include the S II lines near 5400 Å and the blended lines of Fe II and Si II near 4500 Å. Unlike a normal SN Ia, however, the overall continuum of SN 2006X appears quite flat within the first 2 weeks after maximum because of its high reddening. We discuss the detailed spectral evolution of SN 2006X in the following sections.

4.1 Spectroscopic Evolution at Early Times

In Figures 13–15, we compare the spectra of SN 2006X with those of SNe 1984A (Barbon et al. 1989), 1994D (Filippenko 1997), 2002bo (Benetti et al. 2004), 2002er, and 2003cg (ER06) at several epochs ( d, one week, and one month past maximum). The spectra of SN 2002er are taken from our unpublished spectral library. All of the spectra have been corrected for reddening and redshift. For SN 2006X, mag and are used, while mag and are used for SN 2003cg (ER06). For the other SNe, the host galaxy reddening is taken from the literature (e.g., Reindl et al 2005, Wang et al. 2006, and Jha et al. 2007) and extinctions are corrected using the standard extinction law with . The line identifications adopted here are taken from Branch et al. (2005, 2006).

At  d, the spectra of SN 2006X are characterized by lines of the singly ionized intermediate-mass elements (IMEs): Ca II, Si II, and Mg II (Fig. 13). The width and strength of these lines are comparable to those seen in SNe 1984A and 2002bo, but significantly stronger than those of SNe 1994D, 2002er, and 2003cg. The absorption minima due to Si II 6355 is highly blueshifted to 6020 Å around maximum light, suggesting a high photospheric expansion velocity for SN 2006X. The strong Ca II H&K feature, blended with Si II 3858, is more similar to that of SNe 2002bo and 2002er than to the double-dipped feature seen in SNe 1994D and 2003cg. The presence or absence of such a double-dipped feature is probably related to the relative strength of Ca II and Si II as suggested by Lentz et al. (2000). In the 40004500 Å wavelength range, SNe 2006X, 1984A, and 2002bo share a similar feature with a strong absorption at around 4300 Å, probably owing to a blend of Mg II 4481 and Fe III 4404. The weak feature at 4400 Å as seen in SNe 1994D, 2002er, and 2003cg is probably due to the Si III 4553, 4568 blend, which is more sensitive to the temperature in the photosphere. Its absence in the spectra of SNe 2006X, 2002bo, and 1984A suggests a cool temperature. The double S II lines at 5400 Å and 5600 Å (the “W”-shaped feature) in SN 2006X are similar to those in the comparison SNe, but are less pronounced. The Si II 5972 absorption feature in SN 2006X is very weak, and its strength is difficult to measure. Nevertheless, we measured the potential luminosity indicator parameter R(Si II) (defined as the line strength ratio of Si II 5972 to Si II 6355; Nugent et al. 1995) as for SN 2006X, which is much lower than in the other SNe Ia having similar values of (Fig.3 of Benetti et al 2005).

At week (Fig. 14), the spectra of all the SNe Ia are still dominated by the Si II, Ca II, and S II lines with increasing contribution from the iron-group elements. The W-shaped S II lines have almost vanished in SNe 2006X and 1984A, and appears as an asymmetric absorption trough in SN 2002bo. The absorption at around 4400 Å is probably due to a blend of Fe III 4404, Fe II 4555, and Mg II 4481, and appears at a higher expansion velocity (shorter wavelength) in SNe 2002bo, 1984A, and 2006X than in the other SNe Ia. The Fe II and Si II features in the range 4700–5000 Å show less substructure in SNe 2006X, 2002bo, and 1984A, while their Si II 5051 line becomes apparently weaker than that of the other comparison SNe Ia. This probably relates to the high expansion velocity which may smear out the weaker features, or it suggests faster evolution of the S and Si in the high-velocity SNe Ia. By week the O I 7773 line strengthens in other SNe Ia but is still rather weak in SN 2006X.

At month (Fig. 15), numerous Fe II lines appear in the spectra of SNe Ia. The Na I D and Si II 5972 blend is progressively stronger. The Si II 6355 trough becomes severely affected by the Fe II 6238, 6248 and Fe II 6456, 6518 lines, and is barely visible in SN 2006X and SN 1984A, but is still present in the spectra of the other comparison SNe (see the small dip around 6150Å in Fig.15 ). The Ca II near-IR triplet feature is stronger, and appears at a higher expansion velocity in SNe 2002bo and 2006X than in the other SNe Ia. The O I line is comparable to that seen in other SNe Ia. It is impressive that the overall appearance and evolution of the spectra of SN 2006X are extremely similar to those of SN 1984A and SN 2002bo at all three epochs (although the spectra of SN 1984A have a limited spectral range). Nevertheless, it is worth pointing out that by month the spectral flux at 4000 Å appears relatively higher than that of the comparison SNe Ia, although the spectrum at this region had a poorer signal-to-noise ratio. The higher spectral flux below 4000Å seems to be also consistent with the bluer color inferred from the photometry at similar phase. The spectrum near maximum light does not show such a near-UV energy excess. It is unclear when this variation started to occur in SN 2006X, as our spectra taken during the first month past maximum light did not cover the near-UV wavelengths.

4.2 Expansion Velocity of the Ejecta

As the photosphere recedes into deeper and more slowly moving ejecta, the P-Cygni absorption minima of the spectral features in a SN Ia spectrum gradually shifts redward with time (see also Fig.12). Thus the location of the blueshifted minima can in principle trace the photospheric velocity. Indeed, the photospheric velocity () is best measured by the weakest lines, e.g. S II 5640 (Jeffery & Branch 1990, Mazzali et al. 1993, Patat et al. 1996), although it is usually difficult to measure these weak lines due to blending. The velocities inferred from the strong lines (e.g., Si II 6355) represent approximately the at early phase when the amount of the material above the photosphere is small, but they may not properly indicate of the real as the photosphere falls in the regions where the strong lines could form over a large velocity range due to a flatter density gradient. On account of rather weak S II lines after maximum in SN 2006X, we only examined the velocity evolution of Si II 6355 and the Fe II/Fe III lines.

The derived values from Si II 6355 of SN 2006X as a function of time are shown in Figure 16, together with those of the comparison SNe Ia. The reported for an early-epoch spectrum, taken on 8.35 February (corresponding to  d) by Quimby, Brown, & Gerardy (2006), is also included in the plot (shown as the open star). All velocities have been corrected for the redshifts of their respective host galaxies. As can be seen, SN 2006X shows the highest expansion velocities among all SNe in the comparison, with = 20,700 km s at  d and = 15,700 km s at  d, while the typical value for most SNe Ia is around 11,000 km s at maximum brightness (Filippenko 1997; see also Figure 1 in Benetti et al. 2005). The measured from Ca II H&K and S II 5640 near maximum are about 20,500 km s and 11,800 km s, respectively, which are also significantly higher than those measured for the other SNe Ia. SN 1984A and SN 2002bo showed similar, but less pronounced, high-velocity features of the IMEs (Si II, S II, and Ca II). Following Benetti et al. (2005), we calculate the velocity gradient of Si II 6355 for SN 2006X during the period from to  d as km s d, which puts SN 2006X in the group of normal SNe Ia with high velocity gradients (HVGs). Other SNe Ia in the HVG group include SNe 1984A and 2002bo discussed in this paper, SNe 1983G, 1989A, 1997bp, and 2002dj (Benetti et al. 2005), and 2004dt (Wang L et al. 2006b).

The Fe II and Fe III lines are sometimes used to measure the expansion velocities of the inner ejecta of Fe, providing additional clues to the nature of SN Ia explosions (e.g., Li et al. 2001). The values of determined from Fe II 4555 and/or Fe III 4404 lines of different SNe Ia are plotted in Figure 17. At early phases the high-excitation Fe III 4404 line is possibly contaminated by Mg II 4481 and hence may not give a reliable measurement of the . By 2–3 weeks, the Fe II 4555 line becomes stronger and gradually dominates the absorption feature near 4300–4400 Å. This absorption feature yields 10,000 km s for SN 2006X at month, which is about 3000 km s higher than that for SNe 1989B and 1994D and comparable to that for SN 2000cx (Li et al. 2001). Likewise, the Fe II lines of SNe 1984A and 2002bo display high-velocity behavior. As with Si II 6355, the Fe II feature in these high-velocity events shows more rapid evolution, with larger velocity gradients than in other comparison SNe Ia. The values of become much closer to each other when SNe Ia start entering the nebular phase.

The origin of the high-velocity features seen in these SNe Ia is hotly debated. Lentz et al. (2000) find that the strength, profile, and velocity of Si II 6355 is a function of metallicity. The blueward shift of the Si II feature is found to increase with higher metallicity. However, Benetti et al. (2004) found that increasing the normal metallicity in the C+O layer by a factor of 10 in the canonical deflagration model W7 is not adequate for explaining the large seen in SN 2002bo. It was also proposed that the high in these SNe Ia may result from delayed-detonation explosions with the transition density from a deflagration to a detonation as the controlling parameter for the internal dispersion of (Lentz et al. 2001; Benetti et al. 2004). With detailed non-LTE calculations, Lentz et al. (2001) find that some delayed-detonation models provide reasonable approximations to the very high-velocity feature of SN 1984A. The increase in density of IMEs at higher velocities is thus responsible for the larger blueshifts of the line minimum in the spectra and hence the higher measured expansion velocities.

4.3 Spectra in the Nebular Phase

Since the -band and probably -band light curves of SN 2006X declined more slowly at late times than those of the other comparison SNe Ia, it is necessary to examine its late-time spectral behavior in detail. Our collection of nebular-phase spectra of SN 2006X is presented in Figures 18 and 19, together with the spectra of some comparison SNe Ia at similar epochs. Proper corrections for the reddening and redshift have been applied to all the spectra.

In the early nebular phase, at months, the spectra in Figure 18 are quite similar to each other but have subtle differences. The spectra are dominated by various iron lines and have similar relative strengths. The Ca II near-IR triplet is still the strongest feature in the earlier nebular spectra. Although the late-time spectra of SN 2006X are rather noisy, they do show a relatively higher flux at  Å, and an overall bluer continuum than the comparison SNe. The most contrast is with SN 2002bo, in which the relative luminosity in seems to be fainter than that of SN 2006X by about 1.0 mag. The near-UV excess of SN 2006X might have also occurred in the spectrum at  d since maximum (see Fig. 15). This is consistent with the bluer and colors of SN 2006X compared with the other SNe (Fig. 9).

Two very late-phase nebular spectra, obtained with the Keck 10 m telescopes at days +277.0 and +307.0, are shown in Fig. 19. The comparison spectra of SNe 1996X and 1998bu are from the Suspect online supernova spectrum archive (contributed by Salvo et al. 2001 and Jha et al. 1999; see http://bruford.nhn.ou.edu/suspect), and the spectra of SN 2003du are from Stanishev et al. (2007). The spectra at this time are dominated by forbidden lines of singly and doubly ionized Fe and Co. The overall shape of the spectrum of SN 2006X looks similar to that of SN 1998bu, but the profiles and intensities of some features do show significant differences. The most pronounced one is the absorption feature at about 6100 Å, which is stronger in SN 2006X than in the other SNe Ia in our comparison. Other discrepancies include the absorption features near 4200 Å and 4500 Å, which are prominent in SNe 1996X, 1998bu, and 2003du but are marginally visible in SN 2006X. We note that both SN 2006X and SN 1998bu show relatively higher flux below 4500 Å at this phase. The extra flux for SN 1998bu could be caused by a light echo (Cappellaro et al. 2001; Spyromilio et al. 2004), which primarily contributes to the spectrum in the blue.

A possible explanation for the abnormal behavior of the nebular-phase spectra and light curves of SN 2006X in the blue is the presence of a light echo. As this supernova is found to suffer significant extinction, it may have occurred in an environment that is abundant with dust, so the occurrence of a light echo is potentially expected. Some of the observable effects of a light echo around a SN Ia include a bluer late-time color, broader spectral lines, and a brighter tail luminosity (Patat 2006), all of which agree with the observations of SN 2006X. The unidentified, prominent feature at 6100 Å seen in the spectrum at day +307 could be reminiscent of the earlier-epoch Si II 6355, reflected by the surrounding dust. Analysis of the light echo in SN 2006X is given in a separate paper (Wang et al. 2007), in which evidence from the late-time image and spectrum is presented. In particular, the PSF-subtracted HST image distinctly reveals prominent echo structure at away from the SN. The echo emission might exist at 0.05” from the SN site (at 2- level), as suggested by that the echo inferred from the spectrum is brighter than that resolved in the HST images. However, the exact location of the possible local echo is unknown due to the limitation of the image resolution. With the Cepheid distance to M100 15.2 Mpc, the materials illuminated by the resolved LE are found to lie at 27 pc 170 pc from the SN, and it is not clear whether they were produced from a distinct dust component, e.g. the local circumstellar dust, or from a continuous dust distribution as with the outer echo component.

5 The Distance and Luminosity of SN 2006X

The host galaxy of SN 2006X, NGC 4321 (M100), is a well-studied LINER/H II galaxy (e.g., Ho, Filippenko, & Sargent 1997). As one of the largest spiral galaxies in the Virgo cluster, it produced SNe 1901B, 1914A, 1959E, 1979C, and 2006X in roughly the last century. Ferarrese et al. (1997) reported a Cepheid distance to NGC 4321 of mag. A distance of mag was published by the HST Key Project (Freedman et al. 2001), which we adopt here in our analysis.

5.1 Absolute Magnitudes and

With the Cepheid distance and the reddening derived in the previous sections, it is straightforward to calculate the absolute magnitudes of SN 2006X. After correcting for the Galactic reddening of mag with and the host-galaxy reddening of mag with , we derive the -band and -band absolute magnitudes to be and mag, respectively. The magnitudes in other bands are listed in Table 10.

To compare with other SNe Ia, we need to normalize the derived absolute magnitudes of SN 2006X to a nominal light-curve shape, or value. Phillips et al. (1993) proposed a relation between and the peak luminosity of SNe Ia, and there are now several different versions available in the literature (e.g., Hamuy et al. 1996; Phillips et al. 1999; Altavilla et al. 2004). Based on a large sample of SNe Ia, Prieto et al. (2006) updated the relation (see their Table 3), which we adopt to normalize the luminosity of SN 2006X. An alternative luminosity correction method was proposed by Wang et al. (2005), who introduced a post-maximum color parameter which correlates well with the maximum luminosity of SNe Ia. The relevant correction coefficients are taken from Table 3 in Wang et al. (2006).

The normalized luminosities (to mag) of SN 2006X from the two methods are consistent with each other, and are listed in Table 10. The normalized luminosity of SN 2006X is consistent with those of the fiducial SN Ia in the , , , and bands, while it is fainter by 0.2–0.3 mag in the , , and bands. This may be partly due to the more pronounced spectral features in the red, such as the broader and deeper absorption trough of the Ca II near-IR triplet in SN 2006X than in other SNe Ia, as discussed in §4.1.

The measured luminosities for SN 2006X from the Cepheid distance to its host galaxy allow us to determine the Hubble constant via the formula , where is the absolute magnitude of SN 2006X and is the zero point defined by Hubble-flow SNe Ia. Using the normalized luminosities calibrated from the method and the zero point determined by Wang et al. (2006) from 73 Hubble-flow SNe Ia, we derive a Hubble constant (in units of km s Mpc) of 71.1, 73.5, 73.8, 83.9 from the , , , and bands, respectively. Excluding the large value obtained with the peculiar -band data, the average value of derived from SN 2006X is km s Mpc (statistical), which is consistent with the estimates from other Cepheid-calibrated SNe Ia (Jha et al. 1999; Riess et al. 2005; Wang et al. 2006). The statistical error quoted here consists of the uncertainty in the extinction correction and the intrinsic luminosity dispersion of SNe Ia. An analysis of the uncertainty associated with the Cepheid distances is important but is beyond the scope of this paper.

5.2 Bolometric Light Curve and Nickel Mass

To better understand the overall properties of SN 2006X, we constructed its quasi-bolometric light curve using our photometry. For this calculation, we used the normalized passband transmission curves given by Bessell (1990). The integrated flux in each band was approximated by the mean flux multiplied by the effective width of the passband. As we did not get any ultraviolet (below 3200Å) data in SN 2006X, we corrected for the contribution of flux in our calculation using the recipe given by Suntzeff (1996). Following the procedure in Contardo et al. (2000), we inferred the corrections for the passbands missing between and from those SNe Ia which have good observations in all the filters. For the flux beyond band, we used our own data555The missing -band data may not impact significantly to the construction of the quasi-bolometric light curve, as the flux contribution in inferred from the SNe Ia with good observations in near bands (e.g. SN 2001el, Kricisunas et al. 2003) is generally found to be smaller than 3% of the total flux before 80 days after maximum. up to 80 days and then applied the Suntzeff correction. The resulting quasi-bolometric light curve of SN 2006X is shown in Figure 20, together with those of the comparison SNe Ia.

The reddening-corrected quasi-bolometric luminosity of SN 2006X is ( erg s at maximum brightness, comparable to that of most comparison SNe Ia but slightly fainter than SN 1998bu. Differences in the peak luminosity are often considered to be caused by variations in the amount of Ni synthesized during the explosion. The “bump” feature at –32 d is more prominent in SN 2006X than in other comparison SNe. This is caused by the more pronounced shoulder and “second maximum” seen in the , , and near-IR bands in SN 2006X. We also note that the contrast between the peak and tail luminosities of SN 2006X is the smallest among the SNe in the comparison: it has a peak luminosity in the middle of the group, but the highest tail luminosity. Efficiency of the trapping of the gamma rays and the positrons from Co decay (Milne et al. 2001), and small-scale light echoes or ejecta-CSM interaction, may account for this difference.

The radioactive Ni synthesized during a SN Ia explosion is the primary physical parameter determining the peak luminosity, the light curve width, and the spectrosocpic/color evolution of the event (e.g., Kasen et al. 2006). One method to estimate the synthesized Ni mass is by assuming that the luminosity at maximum equals the instantaneous energy deposition rate from the radioactive decay, the so-called “Arnett law” (Arnett 1982; Arnett et al. 1985; Branch 1992). Following Stritzinger & Leibundgut (2005), the maximum luminosity produced by the radioactive Ni can be written as

(1)

where is the rise time of the light curve (e.g., the time spent by the SN from the explosion to the -band maximum), and is the Ni mass (in unit of the solar mass ). Assuming that the luminosity of a SN Ia evolves as an expanding fireball at very early phase (Goldhaber 1998), the rise time can be derived from the relation (Riess et al. 1999) :

(2)

where is the elapsed time since maximum and is the parameter describing the rising rate of the luminosity. Using very early photometric data in the band (including the earliest unfiltered data from IAU Circ. 8667), we derive the rise time to the maximum as 18.20.9 d. This is slightly shorter than the average rise time of 19.50.2 d for a normal SN Ia with = 1.1 mag (Riess et al. 1999, but see Strovink 2007 for the study of a possible dichotomy of the rise time in SNe Ia), but is consistent with that derived for SN 2002bo ( = 17.90.5 d; Benetti et al. 2004) and SN 2005cf ( = 18.60.4 d; Pastorello et al. 2007).

With the peak quasi-bolometric luminosity and the rise time derived for SN 2006X, we derive a Ni mass of  M. This is within the reasonable range of Ni masses of normal SNe Ia. The quoted error bar includes uncertainties in the rise time and bolometric luminosity.

Table 11 lists all the important parameters derived for SN 2006X in the previous sections as well as the parameters relevant to its host galaxy M100.

6 Discussion and Conclusions

In this paper we present extensive optical and near-IR photometry, as well as optical spectroscopy, of the nearby SN Ia 2006X in NGC 4321 (M100). Our observations indicate that SN 2006X is a highly reddened object with an value much smaller than the canonical 3.1 for average Galactic dust, and has the highest expansion velocity ever published for a SN Ia.

Compared with other SNe Ia included in this paper, SN 2006X has a broader light curve in the band, a more prominent “bump” feature in the band, a more pronounced shoulder in the band, and a brighter second maximum in the bands. Relative to the peak brightness, SN 2006X has a higher luminosity in the light curves during the nebular phase than other comparison SNe Ia. The -band decline rate at late times, mag (100 d), is much smaller than that of most normal SNe Ia. We note that other SNe Ia with high expansion velocities, such as SNe 1984A and 2002bo, also exhibit relatively small late-time decline rates. Thus, slow late-time decline in the blue bands may be common for rapidly expanding SNe Ia.

The most notable features in the color curves of SN 2006X are a plateau in the color after maximum, and an obvious deviation from the Lira-Phillips relation at to 90 d. After SN 2006X reached its reddest color in at  d, it became progressively bluer at a much faster pace than expected from the Lira-Phillips relation. We thus suggest that the Lira-Phillips relation should be applied with caution to any individual SN Ia.

We use a global color curve fitting method and the empirical relations between , the peak colors , and the post-maximum color to determine the reddening and extinction of SN 2006X. This yields an average estimate of the host-galaxy reddening for SN 2006X, mag. Assuming the absorption by dust follows the analytical model proposed by Cardelli et al. (1989), we obtain . The low value suggests that the dust around SN 2006X is quite different from that observed in the Milky Way Galaxy, perhaps of a different origin than normal ISM dust. This is also demonstrated by the relatively smaller EW of the interstellar Na I D absorption in the spectra. Further evidence against conventional interstellar dust for SN 2006X is that the polarized spectrum of SN 2006X is significantly different from that of extinguished Galactic stars (Wang L et al. 2006c). It is worth pointing out that most highly reddened known SNe Ia, with mag, tend to have values smaller than 3.1. This suggests that the dust affecting some SNe Ia may be quite different from that observed in the Galaxy.

We caution, however, that SN 2006X may have a peculiar (unknown) intrinsic color evolution, as suggested by the deviation from the Lira-Phillips relation in the color. If so, it would be difficult to estimate the host-galaxy reddening toward SN 2006X and to study its photometric properties.

Spectra of SN 2006X reveal high expansion velocities, based on the IMEs and the iron-group elements. SN 2006X evolves in a manner similar to that of other rapidly expanding events such as SNe 1984A and 2002bo. At early times, these high- objects have much stronger Si II 6355, Ca II H&K, and Ca II near-IR triplet lines than other SNe Ia. At late times, spectra of SN 2006X show a relatively bluer overall continuum, especially at  Å, than the comparison SNe. This is consistent with the bluer and colors of SN 2006X than the other SNe Ia at similar epochs, and suggests an additional input of energy, probably a light echo.

To explain the high-velocity features of some SNe Ia, Benetti et al. (2004) proposed a scenario in which the burning to IMEs extends farther out into the outermost layers than in normal SNe Ia. This model produces the IMEs at higher velocities, but with no additional Ni production, which provides a plausible explanation for most of the spectral features seen in SN 2006X. The above scenario should account not only for the high-velocity feature of the IMEs, but also for that of the iron-group elements at earlier phases of SN evolution.

On the other hand, we propose that SN 2006X may be produced in a progenitor environment having abundant CSM. In this scenario, the high-velocity features shown in the spectra are formed due to the density increase caused by interaction between the supernova ejecta and the surrounding material of the progenitor system, which could be an accretion disk, a filled Roche lobe, or a common envelope (Gerardy et al. 2004). The CSM dust, quite possibly associated with the CSM produced by the progenitor system (Patat et al. 2007), may be the source of a local light echo that could account for the late-time extra energy (beyond radioactive decay) seen at short wavelengths. SN 2006X-like events may actually represent a subclass of SNe Ia with distinct features of spectroscopy, photometry, polarization and even extinction, and the presence of significant CSM dust may be one of the possible explanations (Wang et al. 2007 in preparations). There is also possibility that the detection of CSM in SN 2006X is just tied to the particular viewing angle. Obviously, much further research, both observational and theoretical, is needed on this problem.

Some of the data presented here 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 the National Aeronautics and Space Administration (NASA). The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the BAO, Keck, and Lick Observatory staffs for their assistance with the observations. This research was supported by NSF grant AST–0607485, the TABASGO Foundation, and the National Natural Science Foundation of China (NSFC grant 10673007) and the Basic Research Funding at Tsinghua University (JCqn2005036). KAIT was made possible by generous donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the University of California, and the Sylvia & Jim Katzman Foundation. The CTIO 1.3 m telescope is operated by the Smart and Moderate Aperture Research Telescope System (SMARTS) Consortium. We are particularly grateful for the scheduling flexibility of SMARTS. A.V.F. thanks the Aspen Center for Physics, where he participated in the workshop on “Supernovae as Cosmological Distance Indicators” while this paper was nearing completion. We made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.

References

  • Altavilla et al. (2004) Altavilla, G., et al. 2004, MNRAS, 349, 1344
  • (Arnett 1982) Arnett, W. D., 1982, ApJ, 253, 785
  • (Arnett 1985) Arnett, W. D., Branch D., & Wheeler J. C., 1985, Nature, 314, 337
  • Astier et al. (2006) Astier, P., et al. 2006, A&A, 447, 31
  • Barbon (1989) Barbon, B., Rosino L., & Iijima, T. 1989, A&A, 220, 83
  • Barbon et al. (1990) Barbon, B., Benetti, S., Cappellaro, E., Rosino, L., Turrato, M. 1990, A&A, 237, 79
  • Benetti et al. (2005) Benetti, S., et al. 2005, ApJ, 623, 1011
  • (Bessell 1990) Bessell, M. S. 1990, PASP, 102, 1181
  • (Branch 2005) Branch D., et al. 2005, PASP, 117, 545
  • (Branch 2006) Branch D., et al. 2006, PASP, 118, 560
  • Cardelli et al. (1989) Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245
  • Cappellaro et al. (2001) Cappellaro, E., et al. 2001, ApJ, 549, L215
  • (Cousins 1981) Cousin, A. W. J. 1981, South African Astron. Obs. Circ. 6, 4
  • Eisenstein et al. (2005) Eisenstein, D. J., et al. 2005, ApJ, 633, 560
  • Elias-Rosa et al. (2006) Elias-Rosa, N., et al. 2006, MNRAS, 369, 1880
  • Elmhamdi et al. (2003) Elmhamdi, A., Chugai, N. N., & Danziger, I. J. 2003, A&A, 404, 1077
  • Ferarrese et al. (1997) Ferarrese, L., et al. 1997, ApJ, 475, 853
  • Filippenko (1982) Filippenko, A. V. 1982, PASP, 94, 715
  • Filippenko (1997) Filippenko, A. V. 1997, ARA&A, 35, 309
  • Filippenko (2005) Filippenko, A. V. 2005, in White Dwarfs: Cosmological and Galactic Probes, ed. E. M. Sion, S. Vennes, & H. L. Shipman (Dordrecht: Springer), 97
  • Filippenko et al. (2001) Filippenko, A. V., Li, W., Treffers, R. R., & Modjaz, M. 2001, in Small Telescope Astronomy on Global Scales, ed. B. Paczyński, W.-P. Chen, & C. Lemme (San Francisco: ASP), p. 121
  • Foley et al. (2003) Foley, R. J., et al. 2003, PASP, 115, 1220
  • Freedman et al. (2001) Freedman, W. L., et al. 2001, ApJ, 553, 47
  • Gerardy et al. (2004) Gerardy, C., et al. 2004, ApJ, 607, 391
  • Goldhaber (1998) Goldhaber, G. 1998, BAAS, 193, 47.13
  • Hamuy et al. (1996) Hamuy, M., Phillips, M. M., Suntzeff, N.B., Schommer, R.A., Maza, J., & Aviles, R. 1996, AJ, 112, 2398
  • Ho, Filippenko, & Sargent (1997) Ho, L. C., Filippenko, A. V., & Sargent, W. L. W. 1997, ApJS, 112, 315
  • Iben & Tutukov (1984) Iben I. Jr., & Tutukov A. 1984, ApJS, 55, 335
  • Jeffery & Branch (1990) Jeffery, D. J., & Branch, D. 1990 in Supernovae, Jerusalem Winter School for Theoretical Physics, ed. Wheeler J. C., Piran T., & Weinberg, S. (Singapore: World Scientific), p149
  • Jha (1999) Jha, S., et al. 1999, ApJS, 125, 73
  • Jha (2007) Jha, S., Riess A. G., & Kirshner, R. P. 2007, ApJ, 659, 122
  • Johnson (1966) Johnson, H. L., Iriarte, B., Mitchell, R. I., Wisniewskj, W. Z. 1966, Commun. Lunar Planet. Lab., 4, 99
  • Kasen (2006) Kasen, D. 2006, ApJ, 649, 939
  • Kasen & Woosley (2007) Kasen, D., & Woosley, S. E. 2007, ApJ, 656, 661
  • Knop et al. (2003) Knop, R. A., et al. 2003, ApJ, 598, 102
  • Krisciunas et al. (2006) Krisciunas, K., Prieto, J. L., Garnavich, P. M., Riley, Jessica-Lynn, G., Rest, A., Stubbs, C., & McMillan, R. 2006, AJ, 131, 1639
  • Krisciunas et al. (2000) Krisciunas, K., et al. 2000, ApJ, 539, 658
  • Krisciunas et al. (2003) Krisciunas, K., et al. 2003, AJ, 125, 166
  • Krisciunas et al. (2007) Krisciunas, K., et al. 2007, AJ, 133, 58
  • Lentz et al. (2000) Lentz, E. J., Baron, E., Branch, D., Hauschildt, P. H., & Nugent, P. E. 2000, ApJ, 530, 966
  • (Lira 1995) Lira, P. 1995, Masters thesis, University of Chile
  • Li, et al. (2001) Li, W., et al. 2001, PASP, 113, 1178
  • Mazalli et al. (1993) Mazzali, P. A., Lucy, L. B., Danziger, I. J., Couiffes C., Cappellaro, E., Turatto, M., 1993, A&A, 269, 423
  • Milne et al. (2001) Milne, P. A., The, L. S., & Leising, M. D. 2001, ApJ, 559, 1019
  • Miller & Stone (1993) Miller, J. S., & Stone, R. P. S. 1993, Lick Obs. Tech. Rep. No. 66
  • Nomoto et al. (1997) Nomoto, K.,Iwamoto, K., & Kishimoto, N. 1997, Science, 276, 1378
  • (Nugent et al. 1995) Nugent, P., et al. 1995, ApJ, 455, L147
  • Oke et al. (1995) Oke, J. B., et al. 1995, PASP, 107, 375
  • Parodi et al. (2000) Parodi, B. R., et al. 2000, ApJ, 540, 634
  • Pastorello et al. (2007) Pastorello, A., et al. 2007, MNRAS, 376,1301
  • Patat et al. (1996) Patat, F., Benetti, S., Cappellaro, E., Danziger, I. J., Della Valle, M., Mazzali, P. A., & Turatto, M. 1996, MNRAS, 278, 111
  • Patat et al. (2006) Patat, F. 2006, MNRAS, 369, 1949
  • Patat et al. (2007) Patat F. 2007, Science, 317, 924 (P07)
  • Perlmutter et al. (1999) Perlmutter, S., et al. 1999, ApJ, 517, 565
  • Persson et al. (1998) Persson, S. E., Murphy, D. C., Krzeminski, W., Roth, M., & Rieke, M. J. 1998, AJ, 116, 2475
  • Phillips (1993) Phillips, M. M. 1993, ApJ, 413, L105
  • Phillips (1999) Phillips, M. M., et al. 1999, AJ, 118, 1766 (P99)
  • Pignata et al. (2004) Pignata, G., et al. 2004, MNRAS, 355, 178
  • Prieto et al. (2006) Prieto, J. L., Rest, A., & Suntzeff, N. B. 2006, ApJ, 647, 501
  • Quimby et al. (2006) Quimby, R., Brown, P., & Gerardy, C. 2006, CBET, 393
  • Reindl et al. (2005) Reindl, B., Tammann, G. A., Sandage, A., & Saha, A. 2005, ApJ, 624, 532
  • Richmond et al. (1995) Richmond, M. W., et al. 1995, AJ, 109, 2121
  • Riess et al. (1996) Riess, A. G., Press, W. H., & Kirshner, R. P. 1996, ApJ, 473, 588
  • Riess et al. (1998) Riess, A. G., et al. 1998, AJ, 116, 1009
  • Riess et al. (2005) Riess, A. G., et al. 2005, ApJ, 627, 579
  • Riess et al. (2007) Riess, A. G., et al. 2007, ApJ, 659, 98
  • Salvo et al. (2001) Salvo M. E., et al. 2001, MNRAS, 321, 254
  • Schlegel et al. (1998) Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525
  • Spergel et al. (2003) Spergel, D. N., et al. 2003, ApJS, 148, 175
  • Spergel et al. (2007) Spergel, D. N., et al. 2007, ApJS, 170, 377
  • Spyromilio et al. (2004) Spyromilio, J., Gilmozzi, R., Sollerman, J., Leibundgut, B., Fransson, C., & Cuby, J. G. 2004, A&A, 426,547
  • (Stetson 1987) Stetson, P. B. 1987, PASP, 99, 191
  • Stritzinger et al. (2002) Stritzinger, M., et al. 2002, AJ, 124, 2100
  • Stritzinger & Leibundgut (2005) Stritzinger, M., & Leibundgut, B., 2005, A&A, 431, 423
  • Strovink (2007) Srovink, M. 2007, ApJ, in press (astro-ph/07050726)
  • (Suntzeff 1996) Suntzeff, N. B. 1996, in Supernova and Supernova Remnants, ed. R. McCray & Z. R. Wang (Cambridge: Cambridge Univ. Press), p. 41
  • (Suzuki & Migliardi) Suzuki S., & Migliardi M. 2006, IAU Circ. 8667
  • Tripp (1997) Tripp, R. 1997, A&A, 325, 871
  • Tonry et al. (2003) Tonry, J. L., et al. 2003, ApJ, 594, 1
  • Wang L (2005) Wang, L. 2005, ApJ, 635, L33
  • Wang L (2006a) Wang, L., et al. 2006a, ApJ, 641, 50
  • Wang L (2006b) Wang, L., et al. 2006b, ApJ, 653, 490
  • Wang L (2006c) Wang, L., Baade, D., Patat, F., & Wheeler, J. C. 2006c, CBET, 396
  • Wang et al. (2005) Wang, X., Wang, L., Zhou, X., Lou, Y., & Li, Z. 2005, ApJ, 620, L87
  • Wang et al. (2006) Wang, X., et al. 2006, ApJ, 645, 488
  • Wang et al. (2007) Wang, X., et al. 2007, ApJ, submitted.
  • Webbink (1984) Webbink, R. F. 1984, ApJ, 277, 355
  • Wood-Vasey et al. (2007) Wood-Vasey, W. M., et al. 2007, ApJ, in press (astro-ph/0701041)
Telescopes
TNT 0.1250.016 0.1630.016 0.0780.007 0.0980.011 0.0380.003
KAIT 0.0530.013 0.0360.007 0.0690.009 0.0010.007
CTIO 1.3 m 0.0500.002 0.0460.002 0.0190.004 0.0880.001
Table 1: Color Terms for Different Telescopes.
Star (J2000) (J2000)
1 122303.77 154731.6 14.91(02) 14.758(007) 14.123(003) 13.759(005) 13.393(006)
2 12:23:10.68 15:44:39.3 17.20(15) 17.069(036) 16.809(019) 16.549(027) 16.177(024)
3 12:23:05.93 15:43:51.4 16.36(08) 16.613(022) 16.082(010) 15.746(014) 15.385(012)
4 12:22:48.29 15:43:24.9 15.413(013) 14.763(013) 14.411(004) 14.083(004)
5 12:22:42.60 15:49:03.4 14.94(02) 14.753(011) 14.100(013) 13.746(014) 13.404(010)
6 12:22:50.09 15:50:47.9 16.51(09) 16.323(014) 15.675(026) 15.305(028) 14.941(023)
7 12:22:51.46 15:51:04.5 16.75(09) 16.340(020) 15.458(021) 14.945(008) 14.445(008)
8 12:22:53.40 15:52:18.7 17.92(23) 16.380(010) 15.224(022) 14.425(018) 13.715(033)
9 12:22:41.05 15:51:57.8 16.67(09) 16.665(008) 16.131(010) 15.775(013) 15.430(005)
10 12:22:53.98 15:48:40.9 18.233(017) 17.053(012) 16.309(006) 15.613(014) 14.721(006) 13.925(009)

Table 2: Magnitudes of the photometric standards in the field of SN 2006XaaSee Figure 1 for a chart of SN 2006X (in M100) and the comparison stars.
UT Date JD2,450,000 Phase**Relative to the epoch of -band maximum (JD = 2,453,786.17). Method Telescope
02/08/2006 3774.90 11.27 17.111(0.023) 15.679(0.019) 14.832(0.019) 14.745(0.020) PSF KAIT
02/08/2006 3775.33 10.84 17.576(0.048) 17.005(0.018) 15.566(0.014) 14.721(0.013) 14.489(0.017) PSF TNT
02/09/2006 3775.85 10.32 16.701(0.020) 15.421(0.019) 14.574(0.015) 14.416(0.021) PSF KAIT
02/09/2006 3776.19 9.98 17.449(0.153) 16.626(0.019) 15.320(0.014) 14.476(0.013) 14.318(0.017) PSF TNT
02/10/2006 3776.86 9.31 16.484(0.021) 15.146(0.020) APER CTI0 1.3m
02/10/2006 3776.96 9.21 16.386(0.054) 15.154(0.018) 14.327(0.021) 14.150(0.024) PSF KAIT
02/10/2006 3777.38 8.79 17.485(0.159) 16.297(0.015) 15.012(0.014) 14.207(0.012) 13.925(0.016) PSF TNT
02/11/2006 3778.38 7.79 16.644(0.106) 16.060(0.018) 14.797(0.015) 14.032(0.013) 13.731(0.017) PSF TNT
02/12/2006 3778.75 7.42 15.994(0.019) 14.813(0.018) 14.043(0.014) 13.781(0.022) PSF KAIT
02/13/2006 3779.80 6.37 15.778(0.020) 14.545(0.020) APER CTIO 1.3m
02/13/2006 3780.39 5.78 15.741(0.017) 14.469(0.015) 13.786(0.013) 13.443(0.017) PSF TNT
02/15/2006 3782.40 3.77 15.633(0.041) 14.343(0.017) 13.660(0.013) 13.300(0.019) PSF TNT
02/16/2006 3783.80 2.37 15.389(0.020) 14.166(0.020) 13.619(0.015) 13.298(0.015) APER CTIO 1.3m
02/17/2006 3784.27 1.90 15.441(0.014) 14.146(0.014) 13.552(0.013) PSF TNT
02/18/2006 3784.76 1.51 15.406(0.020) 14.178(0.020) 13.586(0.015) 13.297(0.015) APER CTIO 1.3m
02/18/2006 3785.25 0.92 16.256(0.034) 15.431(0.015) 14.094(0.014) 13.521(0.013) 13.283(0.016) PSF TNT
02/19/2006 3786.19 0.02 16.143(0.029) 15.407(0.014) 14.059(0.014) 13.499(0.012) 13.290(0.016) PSF TNT
02/21/2006 3787.78 1.61 15.418(0.028) 14.070(0.023) 13.518(0.015) 13.354(0.015) APER CTIO 1.3m
02/21/2006 3787.84 1.67 15.466(0.015) 14.068(0.017) 13.524(0.013) 13.409(0.018) PSF KAIT
02/21/2006 3788.27 2.10 16.273(0.022) 15.441(0.014) 14.024(0.014) 13.477(0.012) 13.323(0.016) PSF TNT
02/22/2006 3788.82 2.65 15.494(0.015) 14.054(0.020) 13.513(0.014) 13.412(0.022) PSF KAIT
02/22/2006 3789.25 3.08 16.333(0.024) 15.499(0.014) 14.013(0.014) 13.476(0.013) 13.338(0.016) PSF TNT
02/23/2006 3789.85 3.68 15.553(0.015) 14.063(0.017) 13.526(0.015) 13.444(0.018) PSF KAIT
02/23/2006 3790.23 4.06 16.401(0.040) 15.542(0.014) 14.025(0.014) 13.507(0.012) 13.376(0.016) PSF TNT
02/24/2006 3790.78 4.61 15.585(0.032) 14.111(0.020) 13.570(0.015) 13.468(0.015) APER CTIO 1.3m
02/24/2006 3790.83 4.66 15.618(0.015) 14.062(0.014) 13.543(0.041) 13.496(0.030) PSF KAIT
02/25/2006 3792.23 6.06 16.545(0.034) 15.685(0.014) 14.063(0.014) 13.579(0.012) 13.461(0.016) PSF TNT
02/26/2006 3793.23 7.06 16.594(0.083) 15.771(0.016) 14.085(0.014) 13.620(0.013) 13.508(0.017) PSF TNT
02/27/2006 3793.83 7.66 15.805(0.020) 14.126(0.018) 13.712(0.015) 13.645(0.015) APER CTIO 1.3m
02/28/2006 3795.34 9.17 16.794(0.036) 15.943(0.015) 14.186(0.014) 13.784(0.012) 13.643(0.016) PSF TNT
03/02/2006 3797.39 11.22 17.003(0.049) 16.136(0.015) 14.335(0.014) 13.949(0.013) 13.749(0.017) PSF TNT
03/04/2006 3799.39 13.22 17.246(0.047) 16.338(0.015) 14.428(0.014) 14.040(0.013) 13.757(0.017) PSF TNT
03/05/2006 3799.74 13.57 16.473(0.031) 14.488(0.041) 14.048(0.015) 13.938(0.023) APER CTIO 1.3m
03/05/2006 3800.32 14.15 17.379(0.079) 16.462(0.016) 14.516(0.014) 14.078(0.012) 13.742(0.016) PSF TNT
03/06/2006 3801.22 15.05 17.583(0.117) 16.562(0.016) 14.562(0.014) 14.083(0.012) 13.729(0.016) PSF TNT
03/07/2006 3802.23 16.06 16.654(0.019) 14.610(0.015) 14.082(0.013) PSF TNT
03/08/2006 2802.73 16.56 16.790(0.020) 14.682(0.017) 14.103(0.015) 13.864(0.015) APER CTIO 1.3m
03/09/2006 3803.22 17.05 16.760(0.018) 14.631(0.014) 14.084(0.013) 13.661(0.017) PSF TNT
03/11/2006 3806.16 19.99 17.240(0.045) 14.777(0.016) 14.096(0.013) 13.603(0.017) PSF TNT
03/12/2006 3806.74 20.57 17.303(0.030) 14.899(0.020) 14.138(0.015) 13.740(0.015) APER CTIO 1.3m
03/13/2006 3808.25 22.08 17.243(0.095) 14.821(0.017) 13.575(0.018) PSF TNT
03/15/2006 3810.31 24.14 17.506(0.104) 14.930(0.020) 14.135(0.015) PSF TNT
03/16/2006 3810.70 24.53 17.743(0.108) 15.045(0.018) 14.200(0.015) 13.650(0.015) APER CTIO 1.3m
03/18/2006 3813.23 27.06 18.959(0.343) 17.697(0.024) 15.120(0.014) 14.214(0.012) 13.518(0.016) PSF TNT
03/19/2006 3813.82 27.65 17.729(0.042) 15.221(0.017) 14.313(0.014) 13.603(0.018) PSF KAIT
03/20/2006 3814.71 28.54 17.945(0.054) 15.388(0.015) 14.433(0.015) 13.709(0.015) APER CTIO 1.3m
03/21/2006 3815.24 29.07 17.884(0.022) 15.245(0.014) 14.350(0.013) 13.566(0.018) PSF TNT
03/22/2006 3816.80 30.63 17.878(0.039) 15.454(0.016) 14.538(0.015) 13.792(0.025) PSF KAIT
03/22/2006 3817.19 31.02 19.017(0.212) 17.948(0.018) 15.432(0.014) 14.510(0.012) 13.741(0.016) PSF TNT
03/23/2006 3818.15 31.98 18.030(0.023) 15.509(0.014) 14.588(0.013) 13.818(0.016) PSF TNT
03/24/2006 3818.72 32.55 18.091(0.033) 15.607(0.033) 14.722(0.015) 13.976(0.015) APER CTIO 1.3m
03/25/2006 3820.17 34.00 19.087(0.226) 18.166(0.020) 15.631(0.014) 14.735(0.012) 13.976(0.016) PSF TNT
03/27/2006 3821.77 35.60 15.749(0.017) 14.871(0.030) 14.170(0.043) PSF KAIT
03/28/2006 3823.20 37.00 19.055(0.373) 18.132(0.035) 15.769(0.015) 14.884(0.013) 14.156(0.016) PSF TNT
03/29/2006 3824.16 37.99 19.334(0.326) 18.188(0.029) 15.814(0.015) 14.949(0.013) 14.215(0.016) PSF TNT
03/30/2006 3824.77 38.60 18.206(0.030) 15.923(0.042) 15.116(0.015) 14.371(0.011) APER CTIO 1.3m
03/30/2006 3825.10 38.93 18.278(0.052) 15.839(0.017) 14.987(0.013) 14.265(0.017) PSF TNT
04/01/2006 3827.18 41.01 18.306(0.043) 15.885(0.016) 15.091(0.013) 14.377(0.017) PSF TNT
04/02/2006 3828.20 42.02 19.368(0.344) 18.261(0.028) 15.922(0.015) 15.088(0.013) 14.429(0.017) PSF TNT
04/03/2006 3829.25 43.08 18.210(0.110) 15.984(0.034) 15.153(0.014) 14.475(0.018) PSF TNT
04/04/2006 3830.15 43.98 18.287(0.027) 15.997(0.015) 15.171(0.013) 14.516(0.016) PSF TNT
04/07/2006 3833.24 47.07 18.315(0.043) 16.080(0.017) 15.285(0.013) 14.651(0.017) PSF TNT
04/11/2006 3836.60 50.43 18.471(0.086) 16.288(0.025) 15.445(0.022) 14.913(0.053) APER CTIO 1.3m
04/12/2006 3838.14 51.97 15.382(0.037) 14.824(0.027) PSF TNT
04/16/2006 3841.65 55.48 18.523(0.053) 16.440(0.014) 15.689(0.013) 15.176(0.010) APER CTIO 1.3m
04/18/2006 3843.72 57.55 18.443(0.054) 16.386(0.019) 15.670(0.015) 15.173(0.028) PSF KAIT
04/19/2006 3845.13 58.86 18.487(0.023) 16.440(0.015) 15.695(0.013) 15.171(0.017) PSF TNT
04/21/2006 3846.63 60.46 18.444(0.032) 16.541(0.014) 15.771(0.013) 15.299(0.015) APER CTIO 1.3m
04/24/2006 3850.19 64.02 18.492(0.062) 16.538(0.023) 15.826(0.015) 15.300(0.022) PSF TNT
04/27/2006 3852.65 66.48 18.519(0.041) 16.699(0.019) 15.947(0.015) 15.576(0.018) APER CTIO 1.3m
04/27/2006 3852.68 66.51 18.506(0.070) 16.645(0.018) 15.949(0.013) 15.514(0.021) PSF KAIT
04/28/2006 3854.08 67.91 18.555(0.038) 16.670(0.018) 16.015(0.014) 15.561(0.018) PSF TNT
05/03/2006 3858.62 72.45 18.599(0.040) 16.868(0.033) APER CTIO 1.3m
05/03/2006 3859.04 72.87 18.598(0.064) 16.780(0.025) 16.139(0.016) 15.748(0.020) PSF TNT
05/05/2006 3864.66 78.49 18.818(0.105) 16.962(0.054) APER CTIO 1.3m
05/10/2006 3866.07 79.90 18.589(0.229) 16.931(0.053) 16.368(0.023) 15.978(0.024) PSF TNT
05/14/2006 3870.07 83.90 18.622(0.061) 17.091(0.024) 16.488(0.016) 16.096(0.020) PSF TNT
05/18/2006 3873.58 87.41 18.662(0.023) 17.249(0.011) APER CTIO 1.3m
05/23/2006 3879.16 92.99 18.719(0.147) 17.314(0.043) 16.721(0.026) 16.494(0.040) PSF TNT
05/26/2006 3881.60 95.43 18.773(0.020) 17.419(0.010) APER CTIO 1.3m
05/28/2006 3884.16 97.99 18.795(0.031) 17.467(0.020) 16.982(0.016) 16.652(0.020) PSF TNT
06/07/2006 3894.08 107.91 19.025(0.179) 17.643(0.032) 17.279(0.023) 16.878(0.041) PSF TNT
06/14/2006 3901.08 114.91 18.886(0.054) 17.789(0.029) 17.462(0.023) 17.064(0.045) PSF TNT
06/16/2006 3903.03 116.86 19.033(0.199) 17.969(0.028) 17.527(0.016) 17.383(0.021) PSF TNT
Table 3: Optical photometry of SN 2006X.
UT Date JD2,450,000 Phase**Relative to the epoch of -band maximum (JD = 2,453,786.17).
02/10/2006 3776.86 9.31 13.353(0.013) 13.178(0.038)
02/13/2006 3779.80 6.37 12.969(0.015) 12.885(0.034)
02/17/2006 3783.80 2.37 12.921(0.015) 12.881(0.030)
02/18/2006 3784.76 1.41 12.957(0.015) 12.854(0.030)
02/21/2006 3787.78 1.61 13.129(0.013) 12.912(0.045)
02/24/2006 3790.78 4.61 13.360(0.013) 13.061(0.043)
02/27/2006 3793.83 7.66 13.802(0.018) 13.229(0.058)
03/02/2006 3796.75 10.58 14.433(0.019) 13.239(0.040)
03/05/2006 3799.74 13.57 14.785(0.029)
03/08/2006 3802.73 16.56 14.526(0.017) 13.120(0.026)
03/12/2006 3806.74 20.57 14.328(0.017) 12.945(0.039)
03/16/2006 3810.70 24.53 14.071(0.016) 12.854(0.034)
03/20/2006 3814.71 28.54 13.780(0.016) 12.899(0.051)
03/24/2006 3818.72 32.55 13.909(0.018) 12.933(0.043)
03/30/2006 3824.77 38.60 14.480(0.019) 13.648(0.028)
04/11/2006 3836.60 50.43 15.282(0.027) 14.103(0.073)
04/16/2006 3841.65 55.48 15.727(0.034) 14.350(0.043)
04/21/2006 3846.63 60.46 15.943(0.036) 14.569(0.043)
04/27/2006 3852.65 66.48 16.302(0.047) 14.601(0.058)
05/03/2006 3858.62 72.45 16.521(0.128)
05/09/2006 3864.66 78.49 17.121(0.096) 15.124(0.072)
Table 4: Infrared photometry of SN 2006X.
UT Date JD2,450,000 Phase**Relative to the epoch of -band maximum (JD = 2,453,786.17). B V J K
02/10/2006 3776.86 9.31 0.046 0.004 0.038 0.003
02/13/2006 3779.80 6.37 0.043 0.001 0.046 0.005
02/17/2006 3783.80 2.37 0.043 0.010 0.059 0.019
02/18/2006 3784.76 1.41 0.044 0.012 0.062 0.022
02/21/2006 3787.78 1.61 0.044 0.017 0.067 0.034
02/24/2006 3790.78 4.61 0.043 0.021 0.036 0.057
02/27/2006 3793.83 7.66 0.039 0.023 0.007 0.054
03/02/2006 3796.75 10.58 0.018 0.043
03/05/2006 3799.74 13.57 0.024 0.026 0.043
03/08/2006 3802.73 16.56 0.014 0.027 0.066 0.018
03/12/2006 3806.74 20.57 0.003 0.029 0.091 0.004
03/16/2006 3810.70 24.53 0.019 0.032 0.076 0.010
03/20/2006 3814.71 28.54 0.066 0.036 0.057 0.016
03/24/2006 3818.72 32.55 0.069 0.039 0.09 0.007
03/30/2006 3824.77 38.60 0.066 0.041 0.119 0.005
04/11/2006 3836.60 50.43 0.056 0.030 0.131 0
04/16/2006 3841.65 55.48 0.049 0.025 0.131 0
04/21/2006 3846.63 60.46 0.041 0.026 0.131 0
04/27/2006 3852.65 66.48 0.032 0.026 0.131 0
05/03/2006 3858.62 72.45 0.032 0.025 0.131 0
05/09/2006 3864.66 78.49 0.032 0.025 0.131 0
05/18/2006 3873.58 87.41 0.032 0.025
05/26/2006 3881.60 95.43 0.032 0.025

Table 5: Optical and NIR S-corrections added to the data of CTIO 1.3 m telescope listed in Tables 3 and 4.
UT Date JD PhaseaaRelative to the maximum(JD=2453786.17) Range ResolutionbbApproximate Spectral Resolution (full width at half maximum intensity). Instrument
2,450,000 (days) Å Å
18/02/06 3785.3 0.9 3700-8500 4 BAO 2.16m Cassegrain
21/02/06 3787.7 +1.5 3300-11000 5-12 Lick Shane 3.0m Kast
21/02/06 3788.3 +2.1 4000-9000 3 BAO 2.16m BFOSC
25/02/06 3792.3 +6.1 3700-8200 4 BAO 2.16m Cassegrain
04/03/06 3799.2 +13.1 3700-8200 4 BAO 2.16m Cassegrain
21/03/06 3816.2 +30.1 4000-9000 3 BAO 2.16m BFOSC
22/03/06 3816.7 +30.6 3300-11000 5-12 Lick Shane 3.0m Kast
01/04/06 3827.2 +41.0 4500-6200 4 BAO 2.16m Cassegrain
07/04/06 3833.3 +47.1 4500-9000 3 BAO 2.16m BFOSC
28/04/06 3853.9 +67.7 3900-10500 5-12 Lick Shane 3.0m Kast
05/05/06 3860.9 +74.7 3900-10500 6-12 Lick Shane 3.0m Kast
28/05/06 3884.0 +97.8 3300-11000 5-11 Lick Shane 3.0m Kast
11/23/06 4063.2 +277.0 3100-9200 6 Keck I 10m LRIS
12/23/06 4093.2 +307.0 4500-7200 0.35 Keck II 10m DEIMOS
Table 6: Journal of spectroscopic observations of SN 2006X.
Band aaThe late-time decline rate (in units of mag (100 d)) of the light curve.
U 2453785.130.96 16.200.06
B 2453786.170.35 15.400.03 0.920.05
V 2453789.110.29 14.040.03 2.710.04
R 2453789.090.32 13.500.03 3.300.04
I 2453784.730.40 13.290.10 3.600.02
J 2453782.090.38 12.880.02 6.290.24
K 2453782.970.46 12.820.04 3.780.15
Table 7: Light-curve parameters of SN 2006X.
Method
Global color fit 1.410.06 0.610.05 1.270.12 1.760.09 1.950.09
1.230.13 1.380.07 0.540.07 1.020.13 1.710.10 2.040.09
1.450.06 0.660.06 1.330.12 1.730.11 1.850.11
Mean 1.230.13 1.420.04 0.610.03 1.220.07 1.740.06 1.960.06
Table 8: Host-galaxy reddening of SN 2006X derived from different methods.
SN Host Galaxy Colors Source
1995E NGC 4419 0.740.05 2.620.28 1,2
1996ai NGC 5005 1.690.10 2.030.12 1,2
1999cl NGC 4501 1.240.07 1.550.08 3
2000ce UGC 4195 0.600.06 2.700.30 1,2
2003cg NGC 3169 1.330.11 1.800.19 4
2006X NGC 4321 1.420.06 1.500.15 This paper

References. – (1)Wang et al. (2006); (2) Jha et al. (2007); (3) Krisciunas et al. (2006); (4) Elias-Rosa et al. (2006).

Table 9: Parameters of highly extinguished SNe Ia.
Method
Cepheid distance 19.630.25 19.100.20 19.060.17 19.020.15 18.520.18 18.370.14 18.230.14
Normalized to 19.230.26 19.180.22 19.130.21 18.620.23
Normalized to 19.920.30 19.310.23 19.220.21 18.630.21
Table 10: Absolute magnitudes of SN 2006X at maximum light.
SN 2006X photometric parameters
UT discovery date 7.15 February 2006 1
Epoch of maximum 2,453,786.170.35 2
15.400.03 2
1.360.04 2
1.420.04 2
1.480.06 2
19.100.20 2
(observed) 1.170.05 2
(true) 1.310.05 2
(observed) 1.830.05 2
(true) 0.420.06 2
Late-time decline rate 0.920.05 mag (100 d) 2
72.88.2 km s Mpc 2
L 1.020.10 erg s 2
18.20.9 day 2
M(Ni) 0.500.05 M 2
SN 2006X spectroscopic parameters
(Si II 6355) 15500 km s 2
(Ca II H&K) 20500km s 2
(S II 5460) 11800 km s 2
(Fe II 4555) 10300 km s 2
(Si II 6355) 12310 km s 2
R(Si II) 0.120.06 2
Parameters for NGC 4321
Galaxy type Sbc, LINER/ H II 3
0.026 3
30.910.14 4
1557 km s 3

References. – (1) Suzuki & Migliardi (2006); (2) this paper; (3) NASA Extragalactic Database; (4) Freedman et al. (2001)

Table 11: Relevant parameters for SN 2006X and its host galaxy.
Figure 1: SN 2006X in NGC 4321 (M100). This is a -band image taken by the 0.8 m TNT on 19.69 Feb. 2006. The supernova and 10 local reference stars (Table 2) are marked by numbers.
Figure 2: The light curves of SN 2006X. Solid dots denote the observations from TNT; open circles show the data from KAIT; open squares represent the data from the CTIO 1.3 m telescope. The , , , and data have been offset vertically by +0.5, 0.5, 2.0, and 2.5 mag, respectively.
Figure 3: Comparison of the observed -band light curves of SN 2006X with those of SNe 1984A, 1994D, 1998bu, 2002er, 2003cg, and 2005cf. All light curves are arbitrarily shifted in time and magnitude to fit the peak value of SN 2006X. The data sources are cited in the text.
Figure 4: Same as Fig. 3 but for the -band light curve.
Figure 5: Same as Fig. 3 but for the -band light curve.
Figure 6: Same as Fig. 3 but for the -band light curve.
Figure 7: Same as Fig. 3 but for the -band light curve.
Figure 8: Near-IR -band and -band light curves of SN 2006X compared with those of SNe 1998bu, 2001el, 2002bo, 2003cg, and 2005cf. The data sources are cited in the text.
Figure 9: , , , and color curves of SN 2006X compared with those of SNe 1994D, 1998bu, 2002bo, 2002er, 2003cg, and 2005cf. To show variations in the color evolution between different SNe Ia, the peak colors of all comparison SNe (except for SN 2005cf) have been artificially shifted redwards to match the observed values of SN 2006X at maximum. The dash-dotted line shows the Lira-Phillips relation plus a reddening of mag. The data sources are cited in the text.
Figure 10: The and color curves of SN 2006X, together with those of SNe 1998bu, 2001el, 2002bo, 2003cg, and 2005cf. The dashed lines are the loci of the average light curves from Krisciunas et al. (2000), which are shifted by +1.72 in and +1.95 in in the ordinate direction to minimize the reduced of the fits.
Figure 11: minus color differences between SN 2006X and the unreddened SNe Ia with similar values of . The solid curve shows the best-fit extinction curve following the analytical model of Cardelli et al. (1989). The dashed curve represents the standard extinction curve with .
Figure 12: Optical spectral evolution of SN 2006X. The spectra have been corrected for the redshift of NGC 4321 ( = 1567 km s) but not reddening, and they have been shifted vertically by arbitrary amounts for clarity. The numbers on the right-hand side mark the epochs of the spectra in days after maximum. Uncorrected telluric absorption is marked with a plus sign inside a circle.
Figure 13: The spectrum of SN 2006X near maximum brightness, overplotted with comparable-phase spectra of SNe 1984A, 1994D, 2002bo, 2002er, and 2003cg. All spectra shown here and in the subsequent figures have been corrected for reddening and redshift. For clarity of display, the spectra were arbitrarily shifted in the vertical direction.
Figure 14: Same as Fig. 13 but for spectra about one week after maximum.
Figure 15: Same as Fig. 13 but for spectra at about 4 weeks past maximum.
Figure 16: Evolution of the expansion velocity of SN 2006X as measured from the minimum of Si II 6355, compared with the values of SNe 1984A taken from Barbon et al. (1989), 1989B from Barbon et al. (1990), 2002bo from Benetti et al. (2004), 1994D from Patat et al. (1996), 2003cg from Elias-Rosa et al. (2006), 2002er from Pignata et al. (2004), and 2005cf from Garavini et al. (2007). Some of the data points in the plot are from our unpublished spectral library. The numbers in parentheses represent the values for the SNe Ia.
Figure 17: The same as Fig. 16, but for the Fe II 4555 line.
Figure 18: The early-epoch nebular spectra of SN 2006X compared with those of other SNe Ia at three months past maximum. The dashed spectra overlapping the spectra of SN 2006X at days +75 and +98 are those of SNe 1989B and 2002bo at similar epochs. The comparison spectra are from our unpublished spectral library. All the spectra have been vertically shifted for clarity. The numbers in parentheses represent the values for the SNe Ia.
Figure 19: Very late-time nebular spectrum of SN 2006X compared with those of SNe 1996X, 1998bu, and 2003du. The two vertical dotted lines refer to the Ca II 3945 and Na I 5892 absorptions.
Figure 20: The quasi-bolometric light curve of SN 2006X computed from the light curves. Error bars consist of the uncertainties in the photometry, the distance and absorption corrections. The quasi-bolometric light curves constructed from SNe 1994D, 1998bu, 2002bo, 2002er, 2003cg, and 2005cf are overplotted for comparison (see §3.1 for the data sources). The numbers in parentheses represent the values for the SNe Ia.
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
131718
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description