# Type II Supernova Spectral Diversity. II. Spectroscopic and Photometric Correlations

Claudia Gutiérrez, Joseph Anderson, Mario Hamuy, Santiago

González-Gaitan, Lluis Galbany, Luc Dessart, Maximilian Stritzinger, Mark

Phillips, Nidia Morrell, Gastón Folatelli

► To cite this version:

Claudia Gutiérrez, Joseph Anderson, Mario Hamuy, Santiago González-Gaitan, Lluis Galbany, et al.. Type II Supernova Spectral Diversity. II. Spectroscopic and Photometric Correlations. The Astrophysical Journal, 2017, 850 (1), pp.90. 10.3847/1538-4357/aa8f42. hal-02351347

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Type II Supernova Spectral Diversity. II. Spectroscopic and Photometric Correlations*

Claudia P. Gutiérrez<sup>1,2,3,4</sup> ID, Joseph P. Anderson<sup>3</sup> ID, Mario Hamuy<sup>1,2</sup>, Santiago González-Gaitan<sup>1,5,6</sup>, Lluis Galbany<sup>7</sup> ID,
Luc Dessart<sup>8</sup> ID, Maximilian D. Stritzinger<sup>9</sup> ID, Mark M. Phillips<sup>10</sup> ID, Nidia Morrell<sup>10</sup> ID, and Gastón Folatelli<sup>11</sup>

<sup>1</sup>Millennium Institute of Astrophysics, Casilla 36-D, Santiago, Chile

<sup>2</sup>Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile

<sup>3</sup>European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile

<sup>4</sup>Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK; C.P.Gutierrez-Avendano@soton.ac.uk

<sup>5</sup>Center for Mathematical Modelling, University of Chile, Beauchef 851, Santiago, Chile

<sup>6</sup>CENTRA, Instituto Superior Tcnico—Universidade de Lisboa, Portugal

<sup>7</sup>PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA

<sup>8</sup>Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS umi 3386), Departamento de Astronomía, Universidad de Chile,
Camino El Observatorio 1515, Las Condes, Santiago, Chile

<sup>9</sup>Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

<sup>10</sup>Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile

<sup>11</sup>Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Instituto de Astrofísica de La Plata (IALP), CONICET, Paseo del Bosque SN, B1900FWA La Plata, Argentina

Received 2017 June 20; revised 2017 September 7; accepted 2017 September 9; published 2017 November 21

**Abstract**

We present an analysis of observed trends and correlations between a large range of spectral and photometric parameters of more than 100 type II supernovae (SNe II), during the photospheric phase. We define a common epoch for all SNe of 50 days post-explosion, where the majority of the sample is likely to be under similar physical conditions. Several correlation matrices are produced to search for interesting trends between more than 30 distinct light-curve and spectral properties that characterize the diversity of SNe II. Overall, SNe with higher expansion velocities are brighter, have more rapidly declining light curves, shorter plateau durations, and higher $^{56}$Ni masses. Using a larger sample than previous studies, we argue that “*Pd*”—the plateau duration from the transition of the initial to “plateau” decline rates to the end of the “plateau”—is a better indicator of the hydrogen envelope mass than the traditionally used optically thick phase duration (*OPTd*: explosion epoch to end of plateau). This argument is supported by the fact that *Pd* also correlates with $s_3$, the light-curve decline rate at late times: lower *Pd* values correlate with larger $s_3$ decline rates. Large $s_3$ decline rates are likely related to lower envelope masses, which enables gamma-ray escape. We also find a significant anticorrelation between *Pd* and $s_2$ (the plateau decline rate), confirming the long standing hypothesis that faster declining SNe II (SNe IIL) are the result of explosions with lower hydrogen envelope masses and therefore have shorter *Pd* values.

*Key words:* supernovae: general – surveys

**1. Introduction**

It is commonly accepted that Core-Collapse Supernovae (CC-SNe) are produced by the explosion of massive (>8M<sub>☉</sub>) stars. CC-SNe display a wide spectral and photometric variety, leading to the basis of their spectral classification. First order CC-SN classification is based on the presence or absence of hydrogen within SN spectra. SNe where hydrogen is clearly visible are called SNe II, while those without these features correspond to SNe Ib/c (Minkowski 1941; Filippenko 1997).

Initially, SNe II were classified according to the shape of the light curve: SNe with a faster decline rate are called SNe IIL, while SNe with almost constant luminosity for several months were called SNe IIP (Barbon et al. 1979). However, years later, two new classes of SNe II emerged: SNe IIn and SNe IIb. SNe IIn show narrow emission lines in their spectra, possibly due to steady interaction with a circumstellar medium (CSM; Schlegel 1990), while SNe IIb are thought to be transitional events between SNe II and SNe Ib (Filippenko et al. 1993).

The overall properties of SNe IIn and SNe IIb are sufficiently distinct from “normal” SNe II, that we do not include them for study, and they are no longer discussed in this paper.

With ever increasing numbers of SNe, new subclasses have appeared. Blanco et al. (1987), Menzies et al. (1987), Hamuy et al. (1988), Phillips et al. (1988), and Suntzeff et al. (1988) presented analysis of SN 1987A, an object that exhibited typical characteristics of the SN II spectra, but a peculiar light curve. With this SN, the 87A-like objects were introduced. Examples of these SNe can be found in Pastorello et al. (2005, 2012) and Taddia et al. (2013).<sup>12</sup> Later, Pastorello et al. (2004) and more recently Spiro et al. (2014) studied the properties of low luminosity SNe II, which additionally have narrow spectral lines (indicating low expansion velocities). On the other hand, Inserra et al. (2013) analyzed a group of luminous SNe II. Lately, intermediate luminosity SNe have also been studied, supporting the wide diversity in SNe II (e.g., Roy et al. 2011; Takáts et al. 2014).

Red super-giant (RSG) stars with zero-age main-sequence mass $\ge 8M_{\odot}$ have generally been assumed as the progenitors of SNe II, with hydrodynamical modeling supporting this hypothesis (Chevalier 1976). In recent years, a significant number of direct

<footnote>* This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile; and the Gemini Observatory, Cerro Pachon, Chile (Gemini Program GS-2008B-Q-56). Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile (ESO Programs 076.A-0156, 078.D-0048, 080.A-0516, and 082.A-0526).</footnote>

<footnote n="12"><sup>12</sup>As the SN 87A-like objects have different light-curve properties than “normal” SNe II, we also exclude them from our analysis.</footnote>
identifications of the progenitor stars of nearby SNe IIP (e.g., Van Dyk et al. 2003; Smartt et al. 2004, 2009; Maund & Smartt 2005; Smartt 2015) suggest that RSG stars with masses of 8–18 $M_\odot$ are their progenitors, supporting initial assumptions. There is little observational constraint on the progenitor mass range of SNe IIL because only two direct identifications have been obtained (Elias-Rosa et al. 2010, 2011, but see Maund et al. 2015); however, these do provide some evidence in favor of higher mass progenitors. Nevertheless, a recent analysis done by Valenti et al. (2016) with the light curves and spectra of 16 SNe II did not find any evidence for progenitor mass differences between SNe of different decline rates.

While direct detections of progenitors have constrained a relatively narrow mass range for SNe II, the same SNe show significant differences in their final explosive displays (e.g., SN 2004et, a normal SNe II, and SN 2008bk, a low luminosity event). It must therefore be that differences in stellar evolutionary processes leave the progenitors in different final states (e.g., the extent of the hydrogen envelope, the progenitor radius at explosion, the CSM) or explode with, e.g., different energies, in order to produce the diversity we observe.

Theoretical studies have suggested that progenitors that explode with smaller hydrogen envelope masses produce faster declining light curves (SNe IIL), together with shorter or nonexistent “plateaus” (e.g., Litvinova & Nadezhin 1983; Bartunov & Blinnikov 1992; Popov 1993; Morozova et al. 2015; Moriya et al. 2016). An alternative study presented by Kasen & Woosley (2009) shows that a change in the explosion energy leads to a range of luminosities, velocities, and light-curve durations. That is to say, higher explosion energies result in brighter events with higher expansion velocities and shorter plateaus. They also found that an increasing synthesized $^{56}$Ni mass extends the length of the plateau (see also Bersten 2013). Meanwhile, Dessart et al. (2013b) using radiative-transfer models explored the properties of SNe II changing the physical parameters of the progenitor and/or the explosion (e.g., metallicity, explosion energy, and radius). They found that the radius has an influence on the temperature/ionization/color evolution (more compact objects cool and recombine faster) and in the plateau brightness, while a variation in the explosion energy leads to a variation of the plateau brightness and the plateau duration, consistent with Kasen & Woosley (2009).

To quantify the spectral and photometric diversity, a number of statistical studies of SNe II have been published. Patat et al. (1994) characterized the properties of 57 SNe II using the maximum B-band magnitude, the color at maximum, and the ratio of emission to absorption ($e/a$) in $H_\alpha$. They showed that faster declining events are more luminous, have shallower P-Cygni profiles and are bluer than SNe IIP. The majority of more recent studies have focused on SNe IIP. Hamuy et al. (2002) analyzed 17 SNe IIP and found that SNe with brighter plateaus have higher expansion velocities (also seen in the models of Bersten 2013). Hamuy (2003) concluded that more massive SN IIP progenitors produce more energetic explosions and in turn produce more nickel. Similar results were found by Pastorello et al. (2003) and more recently by Faran et al. (2014b). The only exception to these works about SNe IIP was published by Faran et al. (2014a), who analyzed a sample of SNe IIL. They found that faster declining SNe II (SNe IIL) are brighter than slower declining events (SNe IIP), confirming previous results.

Gutiérrez et al. (2014) and Anderson et al. (2014a), using a large sample of SNe II, analyzed the dominant line in SNe II, the $H_\alpha$ P-Cygni profile. Gutiérrez et al. (2014) using a sample of 52 SNe II (a subsample of that which we present here) showed that SNe with smaller values of $a/e$ (the inverse of the ratio previously discussed by Patat et al. 1994) are brighter and have faster declining light curves. They concluded that these relationships and the diversity of $a/e$ can be understood in terms of a varying hydrogen envelope mass at explosion epoch, together with the possibility of an influence of circumstellar interaction. Meanwhile, Anderson et al. (2014a) analyzed the blueshifted offset in the emission peaks of $H_\alpha$ of 95 SNe II. Through comparison to spectral modeling (Dessart & Hillier 2005; Dessart et al. 2013a), they argue that this behavior is a natural consequence of the distinct density profiles found in SN ejecta.

Using a sample of 117 SNe II, Anderson et al. (2014b; hereafter A14) studied the V-band light curve diversity of these objects. They found that SNe II with shorter plateau duration (Pd) exhibit faster decline rates ($s_2$ in their nomenclature). They concluded that the envelope mass at the epoch of explosion is the dominant physical parameter that explains this observed diversity. Similar results were found by Sanders et al. (2015), Valenti et al. (2016), and Galbany et al. (2016). They also found that SNe IIP and SNe IIL show a continuum in their photometric properties and it is not suitable to isolate them in two distinct classes or types.

In addition to these results, A14 found relatively high radioactive decline rates ($s_3$) for a significant number of SNe. In $^{56}$Ni powered light curves at late times, full gamma-ray and positron trapping yields a decline rate $s_3$ of 0.98mag per 100 days. Higher decline rates than this value therefore suggest less efficient trapping of gamma-ray emission (or much greater explosion energies), suggesting lower mass ejecta for these SNe II.

The previous discussion shows how numerous relations between observed photometric and spectral parameters have been used to understand the SN II phenomenon. However, there are many additional parameters that have not been included in this discussion to date. Inclusion of additional parameters can aid in furthering our understanding of the underlying physics of SNe II. This motivates our current work where we study a sample of almost 1000 optical-wavelength spectra of >100 SNe II. To that aim, we have divided the analysis into two papers. In Gutiérrez et al. (2017; hereafter Paper I), we present the full description of the observations, data reduction techniques, and the spectral properties. We also discuss the spectral matching technique to estimate the explosion epochs, the analysis of the spectral line evolution and the nature of the extra absorption component on the blue side of $H_\alpha$.

Here, in Paper II, we analyze the correlations between different spectral parameters defined to explore the diversity of SNe II, together with their correlation with previously defined photometric measurements. Expansion velocities, pseudo-equivalent widths (pEWs), the ratio of absorption to emission ($a/e$) of the $H_\alpha$ P-Cygni profile, and velocity decline rates are used to search for correlations with photometric parameters and between other spectral properties. We analyze spectral correlations and determine the most important properties to compare them with the photometric parameters. Our overall aim is to search for trends between different measured parameters and
then attempt to link these to the underlying physical properties of SN II progenitors.

The paper is organized as follows. Section 2 briefly describes the data employed for this analysis. In Section 3, we describe our measurement techniques. An overall current physical understanding of our different observed parameters is presented in Section 4. The full analysis is presented in Section 5. We discuss our results in Section 6 and present our conclusions in Section 7.

## 2. Data

The data used in this analysis were published in A14 and Paper I. The details of the spectroscopic and photometric observations and reductions can be found in the mentioned studies. On average, we have seven spectra per SN, which are analyzed together with their V-band light curves. Details of these SNe are available in A14, Anderson et al. (2014a), Gutiérrez et al. (2014), Galbany et al. (2016), and Paper I.

A small number of SNe presented in Paper I are excluded from this work because they have insufficient spectral and/or photometric data to be useful (SNe 1988A, 1990E, 1992ad, 1992am, 1993A, 1999eg, 2002ew, 2003dq, 2004dy, 2005dw, 2005es, 2005K, 2005me, 2006bc, 2007Z, 2008F, and 2009W).

## 3. Measurements

The evolution of SNe II can be studied according to both spectral and photometric behavior. At early phases, the spectra exhibit the Balmer lines ($H_\alpha$, $H_\beta$, $H_\gamma$, $H_\delta$), and He I $\lambda$5876 Å. With time, the iron-group lines start to appear and to dominate the region between 4000 Å and 6000 Å. The Ca II triplet, Na I D, and O I also emerge. The light curve at the beginning shows a fast rise to peak brightness, followed by a slight decline, which is powered by the release of shock deposited energy. Around ~30 days post-explosion a plateau arises from the fact that the expansion of the ejecta at the photosphere compensates for the drop in optical depth. When the photospheric phase ends (around 80–120 days post-explosion, A14), the transition to the nebular phase starts and the brightness drops. Once this happens, the radioactive tail phase starts. This phase is powered by the radioactive decay of $^{56}$Co to $^{56}$Fe. Later than ~200 days, the spectra are dominated by forbidden lines, which are formed in the inner part of the ejecta. Much diversity is observed both in spectra and photometry, which suggests differences in the properties of the progenitor star and the explosion.

To study the diversity within SNe II, we use the spectral and photometric parameters defined in Gutiérrez et al. (2014) and A14. We also define a number of additional parameters below. These measurements are chosen to enable a full characterization of the diversity of SN II V-band light curves and optical spectra.

### 3.1. *Spectral Measurements*

Before proceeding with our spectral analysis, below we summarize the parameters we use, as defined in Paper I.

1. $v$ corresponds to the expansion velocity. It is measured from the minimum flux of the absorption component of P-Cygni line profile. In this analysis, we measure this parameter for 11 features in the photospheric phase: $H_\alpha$, $H_\beta$, Fe II $\lambda$4924, Fe II $\lambda$5018, Fe II $\lambda$5169, Sc II/Fe II $\lambda$5531, Sc II multiplet $\lambda$5663, Na I D, Ba II $\lambda$6142, Sc II

$\lambda$6247, and O I $\lambda$7774. In the case of $H_\alpha$, the velocity was also derived using the full width at half maximum (FWHM) of the emission component.

2. $\Delta v(H_\beta)$: defined as the rate of change of the expansion velocity of the $H_\beta$ feature. This parameter was measured at five distinct intervals (see Paper I); however, here we only use the interval $50 \le t \le 80$ days, as this shows the highest correlation with other parameters.

3. $\Delta v$ is defined as the velocity difference between $H_\alpha$ and Fe II $\lambda$5018, and Na I D and Fe II $\lambda$5018.

4. pEW corresponds to the absorption/emission strength of a particular line. Here, we measure the absolute value of pEW for the same features mentioned above.

5. *a/e* is defined as the flux ratio of the absorption to emission component of $H_\alpha$ P-Cygni profile. This ratio is the inverse of that presented by Patat et al. (1994). We propose *a/e* as this deals better with weak absorption values that are shown by a number of SNe II in our sample.

While measurements were performed in all epochs at which we obtained spectra, we choose to define common epochs between SNe at 30, 50, and 80 days post-explosion. An interpolation and extrapolation is used to obtain parameter values at these epochs. The values obtained by the interpolation are used when two available spectra are present $\pm$15 days around the common epoch, while the values from the extrapolation are used at $\pm$10 days. These intervals were chosen as they increase the strength of observed correlations. Using bigger intervals deteriorates the correlations because the polynomial does not produce reliable results in some cases (particularly for the pEW). At $\pm$15 and $\pm$10 days for interpolation and extrapolation, respectively, the results do not show a significant change compared to those obtained using a smaller interval. Hence, our choice of intervals is justified. To estimate the velocity at a common epoch, we do an interpolation/extrapolation using a power-law fit. For the pEW, we use a low order (first or second) polynomial fit. Power-law fits were found to produce satisfactory results in the case of velocity measurements; however, for pEWs, we found that low order polynomials were required. For this parameter, we used a low order polynomial and determined the best fit using the normalized root mean square (rms) of different orders. The errors of each measurement were obtained with the rms error fit. In summary, we are able to use spectral parameter values in 88, 84, and 59 SNe at 30, 50, and 80 days, respectively.

### 3.2. *Photometric Measurements*

Historical separation of SNe II into distinct classes was based on photometric differences in, e.g., decline rates and absolute magnitudes. Hence it is essential to include photometric parameters in our analysis for a full understanding of observed correlations and their implications for SN II physics. Here, we use the V-band photometric parameters already defined (and measured) in A14, which we now summarize.

1. $t_0$ corresponds to the explosion epoch (see Paper I for more details of their estimation).

2. $t_{\text{tran}}$ is determined as the transition between the initial decline ($s_1$) and the plateau decline ($s_2$).

3. $t_{\text{end}}$ corresponds to the end of the optically thick phase (i.e., the end of the plateau phase).

4. $t_{\text{PT}}$ is the midpoint of the transition from plateau to radioactive tail.
<table><caption>Table 1
Photometric Parameters</caption><thead><tr><th>SN</th><th>Pd<br>(days)</th><th>OPTd<br>(days)</th><th>Cd<br>(days)</th><th>M<sub>max</sub><br>(mag)</th><th>M<sub>end</sub><br>(mag)</th><th>M<sub>tail</sub><br>(mag)</th><th>s<sub>1</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th>s<sub>2</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th>s<sub>3</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th><sup>56</sup>Ni mass<br>M<sub>☉</sub></th><th>Δ(B − V)<sub>10,30</sub></th></tr></thead><tbody><tr><td>1986L</td><td>59.56 ± 0.71</td><td>93.74 ± 6.71</td><td>34.18 ± 3.08</td><td>-18.19 ± 0.20</td><td>-16.88 ± 0.20</td><td>-14.37 ± 0.20</td><td>3.26 ± 0.14</td><td>1.26 ± 0.03</td><td>...</td><td>>0.061</td><td>2.63 ± 0.42</td></tr><tr><td>1990K</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>2.39 ± 0.08</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1991al</td><td>...</td><td>...</td><td>...</td><td>-17.51 ± 0.15</td><td>-17.03 ± 0.15</td><td>-14.71 ± 0.15</td><td>...</td><td>1.45 ± 0.04</td><td>1.26 ± 0.26</td><td>0.067<sup>+0.016</sup><sub>-0.021</sub></td><td>3.69 ± 0.24</td></tr><tr><td>1992af</td><td>...</td><td>47.03 ± 6.71</td><td>...</td><td>-17.33 ± 0.12</td><td>-17.20 ± 0.12</td><td>-15.06 ± 0.12</td><td>...</td><td>0.58 ± 0.03</td><td>1.07 ± 0.08</td><td>0.079<sup>+0.018</sup><sub>-0.029</sub></td><td>1.90 ± 0.83</td></tr><tr><td>1992ba</td><td>...</td><td>106.97 ± 8.54</td><td>...</td><td>-15.34 ± 0.80</td><td>-14.75 ± 0.80</td><td>-12.34 ± 0.80</td><td>...</td><td>0.72 ± 0.02</td><td>0.86 ± 0.07</td><td>0.011<sup>+0.006</sup><sub>-0.015</sub></td><td>2.80 ± 0.21</td></tr><tr><td>1993K</td><td>...</td><td>...</td><td>...</td><td>-17.92 ± 0.23</td><td>-17.24 ± 0.23</td><td>...</td><td>...</td><td>2.36 ± 0.08</td><td>...</td><td>...</td><td>1.82 ± 0.09</td></tr><tr><td>1993S</td><td>...</td><td>...</td><td>...</td><td>-17.52 ± 0.07</td><td>-16.29 ± 0.07</td><td>...</td><td>...</td><td>2.34 ± 0.04</td><td>...</td><td>...</td><td>3.63 ± 0.51</td></tr><tr><td>1999br</td><td>...</td><td>...</td><td>...</td><td>-13.77 ± 0.40</td><td>-13.56 ± 0.40</td><td>...</td><td>...</td><td>0.14 ± 0.02</td><td>...</td><td>>0.002</td><td>3.58 ± 0.39</td></tr><tr><td>1999ca</td><td>40.54 ± 0.92</td><td>79.48 ± 7.62</td><td>38.94 ± 7.06</td><td>-17.48 ± 0.21</td><td>-16.60 ± 0.21</td><td>-13.78 ± 0.21</td><td>3.49 ± 0.16</td><td>1.65 ± 0.06</td><td>1.74 ± 0.33</td><td>>0.047</td><td>...</td></tr><tr><td>1999cr</td><td>43.55 ± 1.68</td><td>79.06 ± 7.62</td><td>35.51 ± 4.34</td><td>-16.90 ± 0.10</td><td>-16.23 ± 0.10</td><td>...</td><td>1.78 ± 0.09</td><td>0.49 ± 0.08</td><td>...</td><td>...</td><td>1.77 ± 0.38</td></tr><tr><td>1999em</td><td>67.04 ± 2.12</td><td>96.04 ± 5.83</td><td>29.00 ± 5.43</td><td>-16.76 ± 0.07</td><td>-16.37 ± 0.07</td><td>-13.93 ± 0.07</td><td>0.86 ± 0.11</td><td>0.30 ± 0.02</td><td>0.88 ± 0.05</td><td>0.050<sup>+0.008</sup><sub>-0.009</sub></td><td>3.07 ± 0.23</td></tr><tr><td>S0210</td><td>...</td><td>93.57 ± 9.49</td><td>...</td><td>-16.21 ± 0.04</td><td>-15.90 ± 0.04</td><td>...</td><td>...</td><td>2.37 ± 0.07</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2002fa</td><td>...</td><td>68.289 ± 7.62</td><td>...</td><td>-16.95 ± 0.04</td><td>-16.65 ± 0.04</td><td>...</td><td>...</td><td>1.56 ± 0.11</td><td>...</td><td>>0.066</td><td>...</td></tr><tr><td>2002gd</td><td>...</td><td>...</td><td>35.00 ± 4.09</td><td>-15.43 ± 0.28</td><td>-14.85 ± 0.28</td><td>...</td><td>1.87 ± 0.09</td><td>0.15 ± 0.04</td><td>...</td><td>...</td><td>3.21 ± 0.28</td></tr><tr><td>2002gw</td><td>...</td><td>88.33 ± 5.83</td><td>...</td><td>-15.76 ± 0.23</td><td>-15.48 ± 0.23</td><td>-13.07 ± 0.23</td><td>...</td><td>0.22 ± 0.03</td><td>0.75 ± 0.09</td><td>0.012<sup>+0.003</sup><sub>-0.004</sub></td><td>2.55 ± 0.20</td></tr><tr><td>2002hj</td><td>...</td><td>90.24 ± 7.62</td><td>...</td><td>-16.91 ± 0.10</td><td>-16.03 ± 0.10</td><td>-13.59 ± 0.10</td><td>...</td><td>1.57 ± 0.05</td><td>1.41 ± 0.01</td><td>>0.026</td><td>...</td></tr><tr><td>2002hx</td><td>...</td><td>68.03 ± 9.49</td><td>...</td><td>-17.00 ± 0.07</td><td>-16.36 ± 0.07</td><td>-14.60 ± 0.07</td><td>...</td><td>1.51 ± 0.03</td><td>1.24 ± 0.04</td><td>0.053<sup>+0.016</sup><sub>-0.023</sub></td><td>2.26 ± 0.32</td></tr><tr><td>2002ig</td><td>...</td><td>...</td><td>...</td><td>-17.66 ± 0.03</td><td>-16.76 ± 0.03</td><td>...</td><td>...</td><td>2.20 ± 0.12</td><td>...</td><td>...</td><td>2.42 ± 0.66</td></tr><tr><td>2003B</td><td>...</td><td>86.19 ± 11.40</td><td>...</td><td>-15.36 ± 0.28</td><td>-15.11 ± 0.28</td><td>-12.77 ± 0.28</td><td>...</td><td>0.65 ± 0.03</td><td>1.07 ± 0.03</td><td>0.017<sup>+0.006</sup><sub>-0.009</sub></td><td>...</td></tr><tr><td>2003bl</td><td>...</td><td>95.81 ± 4.24</td><td>...</td><td>-15.35 ± 0.14</td><td>-15.01 ± 0.14</td><td>...</td><td>...</td><td>0.35 ± 0.02</td><td>...</td><td>...</td><td>2.83 ± 0.46</td></tr><tr><td>2003bn</td><td>62.96 ± 10.51</td><td>92.97 ± 4.24</td><td>30.01 ± 10.93</td><td>-16.80 ± 0.16</td><td>-16.34 ± 0.16</td><td>-13.72 ± 0.16</td><td>1.38 ± 0.9</td><td>0.32 ± 0.03</td><td>...</td><td>>0.038</td><td>2.94 ± 0.25</td></tr><tr><td>2003ci</td><td>...</td><td>92.53 ± 8.54</td><td>...</td><td>-16.83 ± 0.07</td><td>-15.70 ± 0.07</td><td>...</td><td>...</td><td>1.91 ± 0.04</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003cn</td><td>48.86 ± 3.99</td><td>69.8 ± 5.00</td><td>20.94 ± 5.65</td><td>-16.26 ± 0.11</td><td>-15.61 ± 0.11</td><td>...</td><td>2.7 ± 1.14</td><td>1.34 ± 0.04</td><td>...</td><td>...</td><td>2.73 ± 0.45</td></tr><tr><td>2003cx</td><td>...</td><td>90.82 ± 5.83</td><td>...</td><td>-16.79 ± 0.06</td><td>-16.38 ± 0.06</td><td>-14.32 ± 0.06</td><td>...</td><td>0.61 ± 0.04</td><td>...</td><td>>0.051</td><td>1.95 ± 0.65</td></tr><tr><td>2003E</td><td>...</td><td>101.42 ± 7.62</td><td>...</td><td>-15.70 ± 0.15</td><td>-15.48 ± 0.15</td><td>...</td><td>...</td><td>-0.10 ± 0.03</td><td>...</td><td>...</td><td>1.49 ± 0.25</td></tr><tr><td>2003ef</td><td>...</td><td>92.93 ± 9.49</td><td>...</td><td>-16.72 ± 0.14</td><td>-16.15 ± 0.14</td><td>...</td><td>...</td><td>0.78 ± 0.02</td><td>...</td><td>...</td><td>2.76 ± 0.39</td></tr><tr><td>2003eg</td><td>...</td><td>...</td><td>30.87 ± 5.04</td><td>-17.81 ± 0.13</td><td>-14.57 ± 0.13</td><td>...</td><td>6.75 ± 0.18</td><td>1.73 ± 0.13</td><td>...</td><td>...</td><td>1.35 ± 0.18</td></tr><tr><td>2003ej</td><td>...</td><td>68.97 ± 5.83</td><td>...</td><td>-17.66 ± 0.12</td><td>-15.66 ± 0.12</td><td>...</td><td>...</td><td>3.29 ± 0.04</td><td>...</td><td>...</td><td>2.95 ± 0.29</td></tr><tr><td>2003fb</td><td>...</td><td>88.27 ± 6.71</td><td>...</td><td>-15.56 ± 0.12</td><td>-15.25 ± 0.12</td><td>-13.10 ± 0.12</td><td>...</td><td>0.46 ± 0.06</td><td>1.61 ± 0.39</td><td>>0.017</td><td>...</td></tr><tr><td>2003gd</td><td>...</td><td>...</td><td>...</td><td>...</td><td>-15.97 ± 0.40</td><td>-12.58 ± 0.40</td><td>...</td><td>2.22 ± 0.05</td><td>1.03 ± 0.04</td><td>0.012<sup>+0.006</sup><sub>-0.012</sub></td><td>...</td></tr><tr><td>2003hd</td><td>...</td><td>84.39 ± 5.83</td><td>...</td><td>-17.29 ± 0.06</td><td>-16.72 ± 0.06</td><td>-13.85 ± 0.06</td><td>...</td><td>0.93 ± 0.04</td><td>0.72 ± 0.68</td><td>0.029<sup>+0.007</sup><sub>-0.009</sub></td><td>2.80 ± 0.21</td></tr><tr><td>2003hg</td><td>63.98 ± 1.67</td><td>108.5 ± 5.83</td><td>44.52 ± 5.27</td><td>-16.38 ± 0.16</td><td>-15.50 ± 0.16</td><td>...</td><td>1.35 ± 0.05</td><td>0.52 ± 0.04</td><td>...</td><td>...</td><td>3.01 ± 0.47</td></tr><tr><td>2003hk</td><td>58.96 ± 2.34</td><td>87.00 ± 5.00</td><td>28.04 ± 4.63</td><td>-17.02 ± 0.10</td><td>-16.36 ± 0.10</td><td>-13.14 ± 0.10</td><td>3.09 ± 0.20</td><td>1.61 ± 0.06</td><td>0.40 ± 0.66</td><td>>0.017</td><td>...</td></tr><tr><td>2003hl</td><td>...</td><td>108.92 ± 5.83</td><td>...</td><td>-15.91 ± 0.30</td><td>-15.23 ± 0.30</td><td>...</td><td>...</td><td>0.76 ± 0.01</td><td>...</td><td>...</td><td>2.92 ± 0.31</td></tr><tr><td>2003hn</td><td>58.34 ± 1.55</td><td>90.1 ± 10.44</td><td>31.76 ± 10.12</td><td>-16.74 ± 0.10</td><td>-15.96 ± 0.10</td><td>-13.27 ± 0.10</td><td>5.69 ± 0.27</td><td>2.52 ± 0.07</td><td>1.08 ± 0.05</td><td>0.035<sup>+0.008</sup><sub>-0.011</sub></td><td>2.88 ± 0.29</td></tr><tr><td>2003ho</td><td>...</td><td>...</td><td>...</td><td>...</td><td>-14.75 ± 0.16</td><td>-12.00 ± 0.16</td><td>...</td><td>2.25 ± 0.11</td><td>1.69 ± 0.10</td><td>>0.005</td><td>...</td></tr><tr><td>2003ib</td><td>...</td><td>...</td><td>...</td><td>-17.10 ± 0.09</td><td>-16.09 ± 0.09</td><td>...</td><td>...</td><td>1.64 ± 0.03</td><td>...</td><td>...</td><td>1.16 ± 0.22</td></tr><tr><td>2003ip</td><td>...</td><td>80.74 ± 5.00</td><td>...</td><td>-17.75 ± 0.13</td><td>-16.65 ± 0.13</td><td>...</td><td>...</td><td>2.03 ± 0.03</td><td>...</td><td>...</td><td>2.31 ± 0.25</td></tr><tr><td>2003iq</td><td>...</td><td>84.91 ± 3.61</td><td>...</td><td>-16.69 ± 0.30</td><td>-16.18 ± 0.30</td><td>...</td><td>...</td><td>0.72 ± 0.01</td><td>...</td><td>...</td><td>2.42 ± 0.28</td></tr><tr><td>2003T</td><td>...</td><td>90.59 ± 10.44</td><td>...</td><td>-16.54 ± 0.08</td><td>-16.03 ± 0.08</td><td>-13.67 ± 0.08</td><td>...</td><td>0.69 ± 0.02</td><td>2.02 ± 0.14</td><td>>0.030</td><td>2.74 ± 0.82</td></tr><tr><td>2004ej</td><td>...</td><td>97.14 ± 8.54</td><td>...</td><td>-16.62 ± 0.21</td><td>-16.13 ± 0.21</td><td>-12.92 ± 0.21</td><td>...</td><td>1.04 ± 0.04</td><td>0.89 ± 0.13</td><td>0.019<sup>+0.005</sup><sub>-0.007</sub></td><td>...</td></tr><tr><td>2004er</td><td>57.27 ± 1.66</td><td>120.12 ± 5.00</td><td>62.85 ± 2.6</td><td>-16.74 ± 0.16</td><td>-15.67 ± 0.16</td><td>...</td><td>1.08 ± 0.02</td><td>0.52 ± 0.02</td><td>...</td><td>...</td><td>2.13 ± 1.53</td></tr><tr><td>2004fb</td><td>...</td><td>...</td><td>...</td><td>-16.19 ± 0.11</td><td>-15.46 ± 0.11</td><td>...</td><td>...</td><td>1.26 ± 0.07</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2004fc</td><td>68.06 ± 2.68</td><td>106.06 ± 3.16</td><td>38.00 ± 2.86</td><td>-16.21 ± 0.31</td><td>-15.41 ± 0.31</td><td>...</td><td>1.13 ± 0.03</td><td>0.50 ± 0.05</td><td>...</td><td>...</td><td>2.92 ± 0.20</td></tr><tr><td>2004fx</td><td>...</td><td>68.41 ± 5.00</td><td>...</td><td>-15.58 ± 0.24</td><td>-15.33 ± 0.24</td><td>-12.87 ± 0.24</td><td>...</td><td>0.25 ± 0.02</td><td>0.93 ± 0.08</td><td>0.014<sup>+0.004</sup><sub>-0.006</sub></td><td>1.52 ± 0.20</td></tr></tbody></table>
<table><caption>Table 1
(Continued)</caption><thead><tr><th>SN</th><th>Pd<br>(days)</th><th>OPTd<br>(days)</th><th>Cd<br>(days)</th><th>M<sub>max</sub><br>(mag)</th><th>M<sub>end</sub><br>(mag)</th><th>M<sub>tail</sub><br>(mag)</th><th>s<sub>1</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th>s<sub>2</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th>s<sub>3</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th><sup>56</sup>Ni mass<br>M<sub>☉</sub></th><th>Δ(B − V)<sub>10,30</sub></th></tr></thead><tbody><tr><td>2005af</td><td>...</td><td>107.01 ± 15.30</td><td>...</td><td>...</td><td>-14.94 ± 0.36</td><td>-13.41 ± 0.36</td><td>...</td><td>0.40 ± 0.05</td><td>1.25 ± 0.03</td><td>0.026<sup>+0.012</sup><sub>-0.021</sub></td><td>...</td></tr><tr><td>2005an</td><td>36.02 ± 0.63</td><td>74.67 ± 5.00</td><td>38.65 ± 6.03</td><td>-17.07 ± 0.18</td><td>-15.89 ± 0.18</td><td>...</td><td>3.21 ± 0.05</td><td>1.85 ± 0.05</td><td>...</td><td>...</td><td>2.89 ± 0.08</td></tr><tr><td>2005dk</td><td>38.97 ± 1.47</td><td>82.24 ± 6.71</td><td>43.27 ± 6.18</td><td>-17.52 ± 0.14</td><td>-16.74 ± 0.14</td><td>...</td><td>2.25 ± 0.09</td><td>1.10 ± 0.07</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dn</td><td>45.82 ± 3.31</td><td>78.72 ± 6.71</td><td>32.9 ± 6.85</td><td>-17.01 ± 0.24</td><td>-16.38 ± 0.24</td><td>...</td><td>2.00 ± 0.23</td><td>1.48 ± 0.04</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dt</td><td>...</td><td>112.9 ± 9.49</td><td>...</td><td>-16.39 ± 0.09</td><td>-15.84 ± 0.09</td><td>...</td><td>...</td><td>0.58 ± 0.06</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dx</td><td>...</td><td>89.98 ± 7.62</td><td>...</td><td>-16.05 ± 0.08</td><td>-15.24 ± 0.08</td><td>-12.12 ± 0.08</td><td>...</td><td>1.26 ± 0.05</td><td>...</td><td>>0.007</td><td>3.21 ± 0.31</td></tr><tr><td>2005dz</td><td>32.40 ± 2.84</td><td>81.86 ± 5.00</td><td>49.46 ± 4.91</td><td>-16.57 ± 0.12</td><td>-15.97 ± 0.12</td><td>-13.42 ± 0.12</td><td>1.09 ± 0.03</td><td>0.36 ± 0.10</td><td>...</td><td>>0.021</td><td>2.28 ± 0.25</td></tr><tr><td>2005J</td><td>53.01 ± 1.93</td><td>97.01 ± 7.62</td><td>44.00 ± 7.26</td><td>-17.28 ± 0.14</td><td>-16.35 ± 0.14</td><td>...</td><td>1.51 ± 0.03</td><td>1.04 ± 0.02</td><td>...</td><td>...</td><td>2.93 ± 0.17</td></tr><tr><td>2005lw</td><td>...</td><td>107.25 ± 10.44</td><td>...</td><td>-17.07 ± 0.08</td><td>-15.47 ± 0.08</td><td>...</td><td>...</td><td>2.04 ± 0.04</td><td>...</td><td>...</td><td>2.86 ± 0.70</td></tr><tr><td>2005Z</td><td>...</td><td>78.88 ± 6.71</td><td>...</td><td>-17.17 ± 0.11</td><td>-16.17 ± 0.11</td><td>...</td><td>...</td><td>1.76 ± 0.01</td><td>...</td><td>...</td><td>3.04 ± 0.29</td></tr><tr><td>2006ai</td><td>38.28 ± 0.46</td><td>63.26 ± 5.83</td><td>24.98 ± 5.02</td><td>-18.06 ± 0.14</td><td>-17.03 ± 0.14</td><td>-14.53 ± 0.14</td><td>4.61 ± 0.10</td><td>2.05 ± 0.04</td><td>1.78 ± 0.24</td><td>>0.050</td><td>2.02 ± 0.15</td></tr><tr><td>2006be</td><td>43.81 ± 1.32</td><td>76.2 ± 6.71</td><td>32.39 ± 9.10</td><td>-16.47 ± 0.29</td><td>-16.08 ± 0.29</td><td>...</td><td>1.19 ± 0.08</td><td>0.63 ± 0.02</td><td>...</td><td>...</td><td>3.04 ± 0.11</td></tr><tr><td>2006bl</td><td>...</td><td>...</td><td>17.3 ± 11.16</td><td>-18.23 ± 0.07</td><td>-16.52 ± 0.07</td><td>...</td><td>3.05 ± 0.54</td><td>2.41 ± 0.06</td><td>...</td><td>...</td><td>2.15 ± 0.38</td></tr><tr><td>2006ee</td><td>59.04 ± 2.95</td><td>85.15 ± 5.00</td><td>26.11 ± 4.97</td><td>-16.28 ± 0.15</td><td>-16.04 ± 0.15</td><td>...</td><td>0.98 ± 0.29</td><td>0.17 ± 0.03</td><td>...</td><td>...</td><td>2.45 ± 0.19</td></tr><tr><td>2006it</td><td>...</td><td>...</td><td>...</td><td>-16.20 ± 0.15</td><td>-15.97 ± 0.15</td><td>...</td><td>...</td><td>1.14 ± 0.10</td><td>...</td><td>...</td><td>3.98 ± 0.14</td></tr><tr><td>2006iw</td><td>...</td><td>...</td><td>...</td><td>-16.89 ± 0.07</td><td>-16.18 ± 0.07</td><td>...</td><td>...</td><td>1.00 ± 0.03</td><td>...</td><td>...</td><td>2.24 ± 0.67</td></tr><tr><td>2006ms</td><td>...</td><td>...</td><td>32.83 ± 6.62</td><td>-16.18 ± 0.15</td><td>-15.93 ± 0.15</td><td>...</td><td>1.65 ± 0.2</td><td>-0.05 ± 0.45</td><td>...</td><td>>0.056</td><td>4.12 ± 0.12</td></tr><tr><td>2006qr</td><td>...</td><td>96.85 ± 7.62</td><td>...</td><td>-15.99 ± 0.14</td><td>-14.24 ± 0.14</td><td>...</td><td>...</td><td>1.40 ± 0.02</td><td>...</td><td>...</td><td>2.88 ± 0.45</td></tr><tr><td>2006Y</td><td>24.69 ± 0.63</td><td>47.49 ± 5.00</td><td>22.8 ± 4.05</td><td>-17.97 ± 0.06</td><td>-16.98 ± 0.06</td><td>-14.26 ± 0.06</td><td>5.84 ± 0.13</td><td>2.11 ± 0.18</td><td>4.75 ± 0.34</td><td>>0.034</td><td>1.52 ± 0.25</td></tr><tr><td>2007aa</td><td>...</td><td>...</td><td>...</td><td>-16.32 ± 0.27</td><td>-16.32 ± 0.27</td><td>...</td><td>...</td><td>-0.05 ± 0.02</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007ab</td><td>...</td><td>71.66 ± 10.44</td><td>...</td><td>-16.98 ± 0.09</td><td>-16.55 ± 0.09</td><td>-14.22 ± 0.09</td><td>...</td><td>3.18 ± 0.06</td><td>2.31 ± 0.22</td><td>>0.040</td><td>...</td></tr><tr><td>2007av</td><td>...</td><td>...</td><td>...</td><td>-16.27 ± 0.22</td><td>-15.60 ± 0.22</td><td>...</td><td>...</td><td>0.92 ± 0.01</td><td>...</td><td>>0.015</td><td>2.21 ± 0.13</td></tr><tr><td>2007bf</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007hm</td><td>...</td><td>...</td><td>...</td><td>-16.47 ± 0.09</td><td>-16.00 ± 0.09</td><td>...</td><td>...</td><td>1.52 ± 0.04</td><td>...</td><td>>0.045</td><td>1.43 ± 0.28</td></tr><tr><td>2007il</td><td>68.68 ± 2.43</td><td>103.4 ± 5.00</td><td>34.72 ± 4.68</td><td>-16.78 ± 0.11</td><td>-16.59 ± 0.11</td><td>...</td><td>1.06 ± 0.34</td><td>0.12 ± 0.04</td><td>...</td><td>...</td><td>2.21 ± 0.12</td></tr><tr><td>2007it</td><td>...</td><td>...</td><td>13.95 ± 2.64</td><td>-17.55 ± 0.50</td><td>...</td><td>-14.83 ± 0.50</td><td>3.55 ± 1.06</td><td>1.33 ± 0.14</td><td>1.00 ± 0.01</td><td>0.072<sup>+0.031</sup><sub>-0.054</sub></td><td>2.67 ± 0.10</td></tr><tr><td>2007ld</td><td>...</td><td>...</td><td>...</td><td>-17.30 ± 0.09</td><td>-16.53 ± 0.09</td><td>...</td><td>...</td><td>2.62 ± 0.04</td><td>...</td><td>...</td><td>2.13 ± 0.50</td></tr><tr><td>2007oc</td><td>42.78 ± 0.59</td><td>71.62 ± 5.83</td><td>28.84 ± 3.06</td><td>-16.68 ± 0.15</td><td>-16.02 ± 0.15</td><td>...</td><td>2.87 ± 0.10</td><td>1.78 ± 0.01</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007od</td><td>...</td><td>...</td><td>19.61 ± 5.06</td><td>-17.87 ± 0.80</td><td>-16.81 ± 0.80</td><td>...</td><td>2.56 ± 0.10</td><td>1.50 ± 0.02</td><td>...</td><td>...</td><td>2.37 ± 0.12</td></tr><tr><td>2007P</td><td>61.34 ± 1.19</td><td>88.34 ± 5.83</td><td>27.00 ± 5.14</td><td>-17.96 ± 0.05</td><td>-16.75 ± 0.05</td><td>...</td><td>3.80 ± 0.16</td><td>1.40 ± 0.12</td><td>...</td><td>...</td><td>2.26 ± 0.38</td></tr><tr><td>2007sq</td><td>44.66 ± 2.39</td><td>87.66 ± 5.00</td><td>43.00 ± 6.46</td><td>-15.33 ± 0.13</td><td>-14.52 ± 0.13</td><td>...</td><td>2.52 ± 0.37</td><td>1.29 ± 0.08</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007U</td><td>...</td><td>...</td><td>...</td><td>-17.87 ± 0.08</td><td>-16.78 ± 0.08</td><td>...</td><td>...</td><td>2.27 ± 0.04</td><td>...</td><td>...</td><td>2.63 ± 0.35</td></tr><tr><td>2007W</td><td>56.71 ± 2.57</td><td>83.59 ± 7.62</td><td>26.88 ± 7.46</td><td>-15.80 ± 0.20</td><td>-15.34 ± 0.20</td><td>...</td><td>0.83 ± 0.27</td><td>0.00 ± 0.04</td><td>...</td><td>...</td><td>2.39 ± 0.28</td></tr><tr><td>2007X</td><td>53.92 ± 1.03</td><td>98.06 ± 5.83</td><td>44.14 ± 5.14</td><td>-17.84 ± 0.21</td><td>-16.70 ± 0.21</td><td>...</td><td>2.52 ± 0.07</td><td>1.37 ± 0.03</td><td>...</td><td>...</td><td>3.55 ± 0.15</td></tr><tr><td>2008ag</td><td>...</td><td>105.3 ± 6.71</td><td>...</td><td>-16.96 ± 0.15</td><td>-16.66 ± 0.15</td><td>...</td><td>...</td><td>0.12 ± 0.01</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008aw</td><td>37.91 ± 0.91</td><td>75.82 ± 10.44</td><td>37.91 ± 10.04</td><td>-17.71 ± 0.19</td><td>-16.60 ± 0.19</td><td>-14.04 ± 0.19</td><td>3.27 ± 0.08</td><td>2.10 ± 0.05</td><td>1.97 ± 0.09</td><td>>0.050</td><td>2.85 ± 0.16</td></tr><tr><td>2008bh</td><td>...</td><td>...</td><td>20.68 ± 5.34</td><td>-16.06 ± 0.14</td><td>-15.11 ± 0.14</td><td>...</td><td>2.69 ± 0.23</td><td>1.20 ± 0.04</td><td>...</td><td>...</td><td>2.17 ± 0.38</td></tr><tr><td>2008bk</td><td>...</td><td>107.22 ± 6.71</td><td>...</td><td>-14.86 ± 0.05</td><td>-14.59 ± 0.05</td><td>-11.98 ± 0.05</td><td>...</td><td>0.26 ± 0.01</td><td>1.18 ± 0.02</td><td>0.007<sup>+0.001</sup><sub>-0.001</sub></td><td>...</td></tr><tr><td>2008bm</td><td>...</td><td>87.04 ± 26.17</td><td>...</td><td>-18.12 ± 0.07</td><td>-16.32 ± 0.07</td><td>-12.67 ± 0.07</td><td>...</td><td>2.50 ± 0.03</td><td>...</td><td>>0.014</td><td>...</td></tr><tr><td>2008bp</td><td>...</td><td>58.57 ± 9.49</td><td>...</td><td>-14.00 ± 0.21</td><td>-13.13 ± 0.21</td><td>...</td><td>...</td><td>2.79 ± 0.13</td><td>...</td><td>...</td><td>1.79 ± 0.42</td></tr><tr><td>2008br</td><td>...</td><td>...</td><td>...</td><td>-15.30 ± 0.20</td><td>-14.94 ± 0.20</td><td>...</td><td>...</td><td>0.38 ± 0.04</td><td>...</td><td>>0.026</td><td>2.19 ± 0.22</td></tr><tr><td>2008bu</td><td>...</td><td>44.73 ± 7.62</td><td>...</td><td>-17.14 ± 0.10</td><td>-16.74 ± 0.10</td><td>-13.71 ± 0.10</td><td>...</td><td>2.37 ± 0.18</td><td>2.69 ± 0.52</td><td>>0.020</td><td>2.98 ± 0.37</td></tr><tr><td>2008ga</td><td>...</td><td>73.14 ± 5.00</td><td>...</td><td>-16.45 ± 0.14</td><td>-16.20 ± 0.14</td><td>...</td><td>...</td><td>1.10 ± 0.07</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008gi</td><td>...</td><td>...</td><td>...</td><td>-17.31 ± 0.09</td><td>-15.86 ± 0.09</td><td>...</td><td>...</td><td>2.63 ± 0.11</td><td>...</td><td>...</td><td>2.55 ± 1.35</td></tr><tr><td>2008gr</td><td>...</td><td>...</td><td>9.00 ± 6.17</td><td>-17.95 ± 0.10</td><td>-16.43 ± 0.10</td><td>...</td><td>2.22 ± 0.13</td><td>1.61 ± 0.03</td><td>...</td><td>...</td><td>2.46 ± 0.11</td></tr></tbody></table>
<table><caption>**Table 1**
(Continued)</caption><thead><tr><th>SN</th><th>Pd<br>(days)</th><th>OPTd<br>(days)</th><th>Cd<br>(days)</th><th>M<sub>max</sub><br>(mag)</th><th>M<sub>end</sub><br>(mag)</th><th>M<sub>tail</sub><br>(mag)</th><th>s<sub>1</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th>s<sub>2</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th>s<sub>3</sub><br>(mag.100<br>day<sup>-1</sup>)</th><th><sup>56</sup>Ni mass<br>M<sub>☉</sub></th><th>Δ(B − V)<sub>10,30</sub></th></tr></thead><tbody><tr><td>2008H</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008hg</td><td>...</td><td>...</td><td>...</td><td>-15.43 ± 0.12</td><td>-15.59 ± 0.12</td><td>...</td><td>...</td><td>-0.35 ± 0.08</td><td>...</td><td>...</td><td>3.25 ± 0.32</td></tr><tr><td>2008ho</td><td>...</td><td>...</td><td>...</td><td>-15.11 ± 0.23</td><td>-15.03 ± 0.23</td><td>...</td><td>...</td><td>0.32 ± 0.07</td><td>...</td><td>...</td><td>2.39 ± 0.19</td></tr><tr><td>2008if</td><td>51.04 ± 0.29</td><td>75.85 ± 5.83</td><td>24.81 ± 5.01</td><td>-17.94 ± 0.17</td><td>-16.79 ± 0.17</td><td>-14.46 ± 0.17</td><td>4.15 ± 0.07</td><td>1.99 ± 0.02</td><td>...</td><td>>0.063</td><td>1.76 ± 0.22</td></tr><tr><td>2008il</td><td>...</td><td>...</td><td>...</td><td>-16.61 ± 0.11</td><td>-16.22 ± 0.11</td><td>...</td><td>...</td><td>0.71 ± 0.05</td><td>...</td><td>...</td><td>2.39 ± 0.15</td></tr><tr><td>2008in</td><td>...</td><td>89.64 ± 6.71</td><td>...</td><td>-15.40 ± 0.47</td><td>-14.79 ± 0.47</td><td>...</td><td>...</td><td>0.91 ± 0.01</td><td>...</td><td>...</td><td>3.01 ± 0.13</td></tr><tr><td>2008K</td><td>...</td><td>89.32 ± 5.00</td><td>...</td><td>-17.45 ± 0.08</td><td>-16.04 ± 0.08</td><td>-13.40 ± 0.08</td><td>...</td><td>2.66 ± 0.02</td><td>2.07 ± 0.26</td><td>>0.013</td><td>2.61 ± 0.84</td></tr><tr><td>2008M</td><td>58.27 ± 0.27</td><td>75.35 ± 9.49</td><td>17.08 ± 9.00</td><td>-16.75 ± 0.28</td><td>-16.17 ± 0.28</td><td>-13.41 ± 0.28</td><td>5.15 ± 0.27</td><td>0.94 ± 0.02</td><td>1.18 ± 0.26</td><td>0.020<sup>+0.007</sup><sub>-0.010</sub></td><td>1.79 ± 0.18</td></tr><tr><td>2008W</td><td>...</td><td>85.84 ± 6.71</td><td>...</td><td>-16.60 ± 0.11</td><td>-16.05 ± 0.11</td><td>...</td><td>...</td><td>1.10 ± 0.04</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2009aj</td><td>...</td><td>...</td><td>...</td><td>-18.07 ± 0.20</td><td>-16.85 ± 0.20</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2009ao</td><td>...</td><td>41.68 ± 5.00</td><td>...</td><td>-15.79 ± 0.20</td><td>-15.78 ± 0.20</td><td>...</td><td>...</td><td>-0.01 ± 0.12</td><td>...</td><td>...</td><td>1.75 ± 0.29</td></tr><tr><td>2009au</td><td>...</td><td>...</td><td>...</td><td>-16.34 ± 0.21</td><td>-14.69 ± 0.21</td><td>...</td><td>...</td><td>3.03 ± 0.02</td><td>...</td><td>...</td><td>2.04 ± 0.31</td></tr><tr><td>2009bu</td><td>...</td><td>...</td><td>37.35 ± 8.23</td><td>-16.05 ± 0.19</td><td>-15.87 ± 0.19</td><td>...</td><td>0.91 ± 0.14</td><td>0.13 ± 0.04</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2009bz</td><td>...</td><td>...</td><td>...</td><td>-16.46 ± 0.19</td><td>-16.26 ± 0.19</td><td>...</td><td>...</td><td>0.36 ± 0.03</td><td>...</td><td>...</td><td>2.14 ± 0.15</td></tr><tr><td>2009N</td><td>66.73 ± 0.48</td><td>89.79 ± 5.83</td><td>23.06 ± 5.02</td><td>-15.25 ± 0.40</td><td>-14.90 ± 0.40</td><td>...</td><td>2.00 ± 0.29</td><td>0.22 ± 0.01</td><td>...</td><td>...</td><td>3.50 ± 0.06</td></tr></tbody></table>

**Note.** Same as Anderson et al. (2014b). In the first column, we list the SN name. Columns 2, 3, and 4 show the *Pd*, *OPTd*, and *Cd*. In columns 5, 6, and 7, we list the absolute magnitudes of $M_{max}$, $M_{end}$, and $M_{tail}$ respectively. These are followed by the decline rates: $s_1$, $s_2$, and $s_3$, in columns 8, 9, and 10, respectively. In column 11, we present the derived $^{56}$Ni masses (or lower limits), while in column 12 the color gradient is shown. As is explained in Section 3, the *Pd*, $s_1$, and $s_2$ show differences with respect to Anderson et al. (2014b).
<figure><img src="image_3.png" /><figcaption>**Figure 1.** Example of the light-curve parameters measured for each SN within the sample in the V band. Observed absolute magnitude at peak, $M_{max}$, $M_{end}$, and $M_{tail}$ are shown in blue, as applied to the dummy data points (yellow stars) of an SN II. The positions of the three measured slopes, $s_1$, $s_2$, and $s_3$, are shown in red. The cooling duration (Cd), plateau duration (Pd), and optically thick phase duration (OPTd), are indicated in green. Four time epochs are labeled: $t_0$, the explosion epoch; $t_{tran}$, the transition from $s_1$ to $s_2$; $t_{end}$, the end of the optically thick phase; and $t_{PT}$, the midpoint of the transition from plateau to radioactive tail.</figcaption></figure>

time has a relation with the radius at the time of the explosion. González-Gaitán et al. (2015) using a large sample of observed SNe II, concluded that SNe II progenitor radii are relatively small. We note, however, the recent results of Yaron et al. (2017), Morozova et al. (2017), Moriya et al. (2017), and Dessart et al. (2017). These investigations have provided evidence for and shown the effect of previously unaccounted for material close to the progenitor star. The interaction of the SN ejecta with such material may thus complicate the relation between early-time observations and progenitor radius.

In summary, we expect that the hydrogen envelope mass is directly related with Pd, $s_3$; the explosion energy with the expansion velocities (vel), and the luminosities ($M_{max}$, $M_{end}$); and the radius of the progenitor would have some influence in Cd.

## 5. Results

In this section, we investigate the spectral and photometric diversity of SNe II through correlations. Here we present the statistics of these correlations and their respective figures. As stated above, the spectral measurements were performed in the phases where the data were available; however, to characterize this diversity, the analysis is done at 30, 50, and 80 days with respect to the explosion epoch. In Table 2, we can see the average of the correlations for each parameter at 30, 50, and 80 days. The mean of these correlations shows a value of 0.323, 0.364, and 0.356 for each epoch, thus the following analysis is performed at 50 days, where more spectral measurements are available and the mean is higher. In Tables 3 and 4, the measured spectral parameters at 50 days are listed, while in Table 1 we present the photometric parameters.

### 5.1. Spectral Correlations in the Photospheric Phase

We analyze the spectral properties of SNe II, focusing on correlations between pEWs, expansion velocities, velocity

<table><caption>**Table 2**
Average of Correlations</caption><thead><tr><th>Parameter</th><th>Average at 30 Days</th><th>Average at 50 Days</th><th>Average at 80 Days</th></tr></thead><tbody><tr><td>Pd</td><td>0.370</td><td>0.410</td><td>0.425</td></tr><tr><td>OPTd</td><td>0.305</td><td>0.316</td><td>0.342</td></tr><tr><td>Cd</td><td>0.225</td><td>0.228</td><td>0.233</td></tr><tr><td>M<sub>max</sub></td><td>0.392</td><td>0.417</td><td>0.375</td></tr><tr><td>M<sub>end</sub></td><td>0.325</td><td>0.345</td><td>0.343</td></tr><tr><td>M<sub>tail</sub></td><td>0.406</td><td>0.423</td><td>0.456</td></tr><tr><td>s<sub>1</sub></td><td>0.355</td><td>0.391</td><td>0.344</td></tr><tr><td>s<sub>2</sub></td><td>0.304</td><td>0.348</td><td>0.325</td></tr><tr><td>s<sub>3</sub></td><td>0.334</td><td>0.374</td><td>0.363</td></tr><tr><td><sup>56</sup>Ni</td><td>0.449</td><td>0.520</td><td>0.550</td></tr><tr><td>Δ<sub>c</sub>(10 − 30)</td><td>0.208</td><td>0.219</td><td>0.213</td></tr><tr><td>V(H<sub>α</sub>)</td><td>0.361</td><td>0.468</td><td>0.452</td></tr><tr><td>V(H<sub>β</sub>)</td><td>0.416</td><td>0.479</td><td>0.441</td></tr><tr><td>V(Fe II 5018)</td><td>0.380</td><td>0.450</td><td>0.325</td></tr><tr><td>V(Fe II 5169)</td><td>0.415</td><td>0.477</td><td>0.393</td></tr><tr><td>V(Na I D)</td><td>0.450</td><td>0.519</td><td>0.480</td></tr><tr><td>pEW(H<sub>α</sub>)<sub>a</sub></td><td>0.279</td><td>0.270</td><td>0.287</td></tr><tr><td>pEW(H<sub>α</sub>)<sub>e</sub></td><td>0.138</td><td>0.362</td><td>0.427</td></tr><tr><td>pEW(Fe II 5018)</td><td>0.329</td><td>0.339</td><td>0.218</td></tr><tr><td>pEW(Fe II 5169)</td><td>0.167</td><td>0.209</td><td>0.189</td></tr><tr><td>pEW(Na I D)</td><td>0.238</td><td>0.242</td><td>0.354</td></tr><tr><td>a/e</td><td>0.269</td><td>0.328</td><td>0.316</td></tr><tr><td>Δvel(H<sub>α</sub>–Fe II 5018)</td><td>0.303</td><td>0.321</td><td>0.438</td></tr><tr><td>Δvel(Na I D—Fe II 5018)</td><td>0.403</td><td>0.426</td><td>0.419</td></tr><tr><td>Δv(H<sub>β</sub>)</td><td>0.248</td><td>0.228</td><td>0.207</td></tr></tbody></table>

**Note.** Average of the correlations at 30, 50, and 80 days since explosion presented for 11 photometric parameters and 14 spectroscopic ones. In the first column, the SN II parameter is listed (described in 3), while in the second, third, and fourth columns are the averages.

decline rate, and velocity differences. Figure 2 shows the correlation matrix of the velocity measurements at 50 days obtained by estimating the Pearson correlation coefficient. Correlation coefficients are displayed in color: darkest colors (green and purple) represent the highest correlation found with the Pearson correlation test (−1 and 1, respectively), while white colors (0) mean no correlation. These colors are presented in the lower triangle, while the upper triangle shows the Pearson correlation value ($\rho$). It is generally considered that correlation coefficients between 0 and 0.19 represent close to zero correlation, 0.2–0.39 weak, 0.4–0.59 moderate, 0.6–0.89 strong, and 0.8–1.0 very strong (Evans 1996), while also noting the statistical significance of these correlation coefficients in many cases. We will use these descriptions for the following discussion. As shown in Figure 2, all velocities strongly correlate positively with each other, as we would expect for an homologous expansion ($v \propto r$). Taking an average, $v(\text{Sc II/Fe II}) \lambda5531$, $v(\text{O I}) \lambda7774$, and $v(\text{Sc II}) \lambda6247$ show the highest correlations with the other parameters, with values of 0.887, 0.883, and 0.875, respectively, while Fe II $\lambda4924$ shows the lowest (0.714). The Sc II $\lambda6247$ line velocities correlate strongly with Fe II $\lambda5018$ and Sc II/Fe II $\lambda5531$, with a value of $\rho = 0.94$ and $\rho = 0.95$. It is important to note that while the velocities all correlate, they are offset. In general, the differences in the velocities are related to the optical depth for each line and the proximity of the line forming region to the photosphere. As $H_{\alpha}$ displays the highest velocities, it is mostly
<table><caption>Table 3
Velocity Values at 50 Days from Explosion</caption><thead><tr><th>SN</th><th>vel(H<sub>α</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(H<sub>β</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(H<sub>β</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(Fe<br>II λ4924)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>λ5018)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>λ5169)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>/Sc II)<br>(km s<sup>-1</sup>)</th><th>vel(Sc II<br>Mult.)<br>(km s<sup>-1</sup>)</th><th>vel(Na I D)<br>(km s<sup>-1</sup>)</th><th>vel(Ba II)<br>(km s<sup>-1</sup>)</th><th>vel(Sc II)<br>(km s<sup>-1</sup>)</th><th>vel(O I)<br>(km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td>1986L</td><td>7707 ± 710</td><td>6204 ± 476</td><td>6722 ± 434</td><td>4946 ± 245</td><td>4311 ± 672</td><td>4406 ± 411</td><td>4778 ± 456</td><td>4316 ± 336</td><td>5512 ± 486</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1990K</td><td>7841 ± 432</td><td>6958 ± 426</td><td>6563 ± 381</td><td>...</td><td>4440 ± 298</td><td>3942 ± 204</td><td>4886 ± 450</td><td>4604 ± 239</td><td>6363 ± 391</td><td>4468 ± 312</td><td>4139 ± 238</td><td>...</td></tr><tr><td>1991al</td><td>8897 ± 496</td><td>7950 ± 615</td><td>7789 ± 634</td><td>4921 ± 244</td><td>4790 ± 588</td><td>4982 ± 548</td><td>5256 ± 261</td><td>4575 ± 227</td><td>7835 ± 876</td><td>5696 ± 282</td><td>4149 ± 206</td><td>...</td></tr><tr><td>1992af</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1992ba</td><td>6276 ± 665</td><td>4559 ± 439</td><td>5100 ± 374</td><td>3160 ± 157</td><td>3388 ± 487</td><td>3464 ± 483</td><td>3479 ± 173</td><td>3322 ± 165</td><td>4325 ± 847</td><td>3042 ± 151</td><td>3060 ± 152</td><td>...</td></tr><tr><td>1993K</td><td>7099 ± 551</td><td>7151 ± 358</td><td>6326 ± 444</td><td>4903 ± 269</td><td>3536 ± 490</td><td>4390 ± 218</td><td>4479 ± 222</td><td>3767 ± 270</td><td>5488 ± 520</td><td>3998 ± 199</td><td>4053 ± 420</td><td>4500 ± 466</td></tr><tr><td>1993S</td><td>7800 ± 630</td><td>6132 ± 620</td><td>6886 ± 670</td><td>3269 ± 340</td><td>4822 ± 470</td><td>4943 ± 300</td><td>...</td><td>...</td><td>6071 ± 620</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1999br</td><td>3611 ± 588</td><td>3082 ± 265</td><td>3191 ± 243</td><td>1511 ± 258</td><td>1753 ± 223</td><td>1746 ± 305</td><td>2101 ± 272</td><td>1527 ± 443</td><td>1519 ± 759</td><td>1229 ± 61</td><td>1891 ± 94</td><td>1100 ± 100</td></tr><tr><td>1999ca</td><td>7375 ± 348</td><td>7039 ± 364</td><td>6840 ± 338</td><td>...</td><td>5618 ± 278</td><td>5191 ± 257</td><td>6103 ± 302</td><td>5727 ± 284</td><td>6825 ± 337</td><td>5833 ± 289</td><td>5043 ± 250</td><td>...</td></tr><tr><td>1999cr</td><td>5960 ± 361</td><td>5477 ± 323</td><td>4932 ± 478</td><td>...</td><td>3495 ± 195</td><td>3655 ± 212</td><td>...</td><td>3909 ± 194</td><td>4504 ± 224</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1999em</td><td>6025 ± 622</td><td>5591 ± 595</td><td>5709 ± 626</td><td>3768 ± 187</td><td>3337 ± 394</td><td>3464 ± 365</td><td>3383 ± 168</td><td>2992 ± 149</td><td>3722 ± 451</td><td>3048 ± 152</td><td>3107 ± 154</td><td>...</td></tr><tr><td>S0210</td><td>7955 ± 492</td><td>8197 ± 762</td><td>7050 ± 619</td><td>...</td><td>6846 ± 424</td><td>4998 ± 326</td><td>6276 ± 311</td><td>5374 ± 550</td><td>6810 ± 455</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2002fa</td><td>7649 ± 649</td><td>6184 ± 435</td><td>6359 ± 410</td><td>3567 ± 268</td><td>3832 ± 337</td><td>4133 ± 260</td><td>4163 ± 207</td><td>3603 ± 179</td><td>5741 ± 663</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2002gd</td><td>4138 ± 563</td><td>3717 ± 266</td><td>3414 ± 703</td><td>2257 ± 196</td><td>2730 ± 204</td><td>2448 ± 236</td><td>3165 ± 297</td><td>3005 ± 409</td><td>3406 ± 273</td><td>2105 ± 177</td><td>2414 ± 325</td><td>1870 ± 200</td></tr><tr><td>2002gw</td><td>6674 ± 474</td><td>5454 ± 487</td><td>5299 ± 518</td><td>3253 ± 329</td><td>3295 ± 494</td><td>3623 ± 357</td><td>3221 ± 345</td><td>3233 ± 247</td><td>3889 ± 304</td><td>3036 ± 211</td><td>2976 ± 185</td><td>3120 ± 325</td></tr><tr><td>2002hj</td><td>7933 ± 661</td><td>6540 ± 532</td><td>6447 ± 451</td><td>3432 ± 579</td><td>3787 ± 338</td><td>4192 ± 405</td><td>4645 ± 230</td><td>3592 ± 220</td><td>5239 ± 345</td><td>...</td><td>...</td><td>4080 ± 420</td></tr><tr><td>2002hx</td><td>8070 ± 434</td><td>5722 ± 504</td><td>6455 ± 554</td><td>3255 ± 337</td><td>3506 ± 215</td><td>3806 ± 284</td><td>3021 ± 157</td><td>3623 ± 200</td><td>5408 ± 477</td><td>2532 ± 160</td><td>3213 ± 302</td><td>...</td></tr><tr><td>2002ig</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003B</td><td>6256 ± 339</td><td>4604 ± 622</td><td>5524 ± 478</td><td>3204 ± 575</td><td>3458 ± 297</td><td>3509 ± 251</td><td>3643 ± 260</td><td>3523 ± 307</td><td>4051 ± 228</td><td>3343 ± 265</td><td>3121 ± 188</td><td>2970 ± 270</td></tr><tr><td>2003bl</td><td>3958 ± 481</td><td>3679 ± 435</td><td>3849 ± 326</td><td>4297 ± 255</td><td>2342 ± 213</td><td>2093 ± 190</td><td>2451 ± 263</td><td>2456 ± 207</td><td>2712 ± 582</td><td>2780 ± 426</td><td>2265 ± 184</td><td>...</td></tr><tr><td>2003bn</td><td>6892 ± 638</td><td>5887 ± 545</td><td>5688 ± 471</td><td>3639 ± 265</td><td>3611 ± 607</td><td>3612 ± 530</td><td>3457 ± 302</td><td>3254 ± 327</td><td>4077 ± 397</td><td>3296 ± 300</td><td>3134 ± 178</td><td>3000 ± 280</td></tr><tr><td>2003ci</td><td>7219 ± 280</td><td>5648 ± 357</td><td>5916 ± 293</td><td>3007 ± 150</td><td>3832 ± 190</td><td>3677 ± 183</td><td>4761 ± 236</td><td>4449 ± 483</td><td>5907 ± 292</td><td>3142 ± 156</td><td>4254 ± 211</td><td>...</td></tr><tr><td>2003cn</td><td>5409 ± 293</td><td>4223 ± 501</td><td>4521 ± 946</td><td>2399 ± 119</td><td>2778 ± 138</td><td>2699 ± 197</td><td>2962 ± 147</td><td>2533 ± 126</td><td>3836 ± 695</td><td>2817 ± 140</td><td>2980 ± 148</td><td>...</td></tr><tr><td>2003cx</td><td>9001 ± 870</td><td>5960 ± 600</td><td>7038 ± 720</td><td>4753 ± 460</td><td>4130 ± 400</td><td>4788 ± 420</td><td>...</td><td>...</td><td>5993 ± 610</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003E</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003ef</td><td>7703 ± 367</td><td>6416 ± 610</td><td>4261 ± 494</td><td>3930 ± 364</td><td>4121 ± 534</td><td>4116 ± 516</td><td>4044 ± 575</td><td>3738 ± 395</td><td>4316 ± 484</td><td>3582 ± 299</td><td>3638 ± 181</td><td>3750 ± 390</td></tr><tr><td>2003eg</td><td>8560 ± 725</td><td>7619 ± 675</td><td>6705 ± 418</td><td>...</td><td>4669 ± 405</td><td>4727 ± 456</td><td>4168 ± 207</td><td>4235 ± 210</td><td>6993 ± 468</td><td>3100 ± 320</td><td>3390 ± 410</td><td>...</td></tr><tr><td>2003ej</td><td>6897 ± 630</td><td>9181 ± 1000</td><td>5968 ± 600</td><td>...</td><td>4998 ± 480</td><td>4381 ± 405</td><td>...</td><td>...</td><td>6244 ± 600</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003fb</td><td>7583 ± 561</td><td>6132 ± 625</td><td>5840 ± 854</td><td>3906 ± 754</td><td>4033 ± 738</td><td>3819 ± 722</td><td>3996 ± 704</td><td>3516 ± 677</td><td>4749 ± 668</td><td>4319 ± 649</td><td>3430 ± 627</td><td>...</td></tr><tr><td>2003gd</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003hd</td><td>7850 ± 519</td><td>6809 ± 539</td><td>5960 ± 717</td><td>3864 ± 192</td><td>3956 ± 260</td><td>4025 ± 289</td><td>3779 ± 188</td><td>3393 ± 169</td><td>4725 ± 234</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003hg</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>4090 ± 420</td></tr><tr><td>2003hk</td><td>6622 ± 349</td><td>7062 ± 328</td><td>5682 ± 281</td><td>4053 ± 201</td><td>4144 ± 206</td><td>4161 ± 207</td><td>...</td><td>...</td><td>5767 ± 286</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003hl</td><td>6579 ± 738</td><td>5623 ± 462</td><td>4550 ± 439</td><td>3961 ± 382</td><td>3899 ± 287</td><td>3819 ± 402</td><td>3787 ± 329</td><td>3783 ± 283</td><td>4527 ± 318</td><td>3276 ± 252</td><td>3501 ± 244</td><td>3570 ± 368</td></tr><tr><td>2003hn</td><td>7016 ± 387</td><td>6594 ± 462</td><td>5336 ± 442</td><td>3455 ± 281</td><td>3425 ± 249</td><td>3484 ± 379</td><td>3466 ± 286</td><td>3148 ± 293</td><td>4470 ± 339</td><td>3596 ± 189</td><td>3039 ± 375</td><td>3480 ± 360</td></tr><tr><td>2003ho</td><td>8312 ± 755</td><td>7459 ± 520</td><td>6102 ± 302</td><td>3463 ± 172</td><td>3739 ± 186</td><td>3989 ± 198</td><td>4309 ± 214</td><td>3969 ± 197</td><td>5010 ± 248</td><td>...</td><td>...</td><td>3970 ± 410</td></tr><tr><td>2003ib</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003ip</td><td>8629 ± 486</td><td>8059 ± 533</td><td>6813 ± 388</td><td>...</td><td>5391 ± 341</td><td>4536 ± 309</td><td>5773 ± 286</td><td>5058 ± 251</td><td>6501 ± 413</td><td>4858 ± 241</td><td>5337 ± 264</td><td>6100 ± 600</td></tr><tr><td>2003iq</td><td>7483 ± 741</td><td>5953 ± 386</td><td>5483 ± 350</td><td>4254 ± 211</td><td>4213 ± 225</td><td>4329 ± 216</td><td>4171 ± 207</td><td>3935 ± 195</td><td>5123 ± 360</td><td>3743 ± 186</td><td>3920 ± 195</td><td>3950 ± 330</td></tr><tr><td>2003T</td><td>6954 ± 403</td><td>5994 ± 634</td><td>4039 ± 226</td><td>3967 ± 341</td><td>3807 ± 218</td><td>3896 ± 276</td><td>3777 ± 190</td><td>3390 ± 222</td><td>3996 ± 292</td><td>4223 ± 257</td><td>4039 ± 240</td><td>...</td></tr><tr><td>2004ej</td><td>635 ± 501</td><td>5522 ± 429</td><td>5389 ± 600</td><td>3535 ± 505</td><td>3440 ± 307</td><td>3301 ± 221</td><td>3556 ± 536</td><td>3291 ± 319</td><td>4005 ± 326</td><td>2880 ± 191</td><td>3178 ± 223</td><td>3380 ± 350</td></tr><tr><td>2004er</td><td>965 ± 582</td><td>8323 ± 549</td><td>7878 ± 600</td><td>6040 ± 427</td><td>5396 ± 386</td><td>5219 ± 436</td><td>5501 ± 311</td><td>3372 ± 470</td><td>5771 ± 506</td><td>5284 ± 634</td><td>5306 ± 475</td><td>5065 ± 520</td></tr><tr><td>2004fb</td><td>769 ± 636</td><td>6678 ± 444</td><td>5884 ± 435</td><td>3926 ± 283</td><td>4228 ± 425</td><td>4178 ± 300</td><td>4368 ± 217</td><td>3750 ± 186</td><td>4798 ± 340</td><td>5254 ± 261</td><td>3805 ± 410</td><td>...</td></tr><tr><td>2004fc</td><td>633 ± 645</td><td>5639 ± 976</td><td>4056 ± 329</td><td>3690 ± 236</td><td>3675 ± 291</td><td>3581 ± 256</td><td>3760 ± 270</td><td>3591 ± 261</td><td>4194 ± 541</td><td>3195 ± 229</td><td>3386 ± 266</td><td>3319 ± 325</td></tr><tr><td>2004fx</td><td>572 ± 525</td><td>4856 ± 446</td><td>4194 ± 318</td><td>2385 ± 206</td><td>2700 ± 209</td><td>2786 ± 401</td><td>3002 ± 177</td><td>3386 ± 168</td><td>2884 ± 389</td><td>3180 ± 158</td><td>2459 ± 133</td><td>2300 ± 210</td></tr><tr><td>2005af</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>Table 3
(Continued)</caption><thead><tr><th>SN</th><th>vel(H<sub>α</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(H<sub>β</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(H<sub>β</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(Fe<br>II λ4924)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>λ5018)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>λ5169)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>/Sc II)<br>(km s<sup>-1</sup>)</th><th>vel(Sc II<br>Mult.)<br>(km s<sup>-1</sup>)</th><th>vel(Na I D)<br>(km s<sup>-1</sup>)</th><th>vel(Ba II)<br>(km s<sup>-1</sup>)</th><th>vel(Sc II)<br>(km s<sup>-1</sup>)</th><th>vel(O I)<br>(km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td>2005an</td><td>7656 ± 888</td><td>8325 ± 494</td><td>5346 ± 1497</td><td>4356 ± 219</td><td>4333 ± 325</td><td>4011 ± 303</td><td>4753 ± 289</td><td>4551 ± 293</td><td>4738 ± 560</td><td>...</td><td>...</td><td>4580 ± 470</td></tr><tr><td>2005dk</td><td>7926 ± 531</td><td>6887 ± 470</td><td>6883 ± 359</td><td>4541 ± 312</td><td>4535 ± 289</td><td>4603 ± 306</td><td>4418 ± 311</td><td>3937 ± 329</td><td>6317 ± 709</td><td>5112 ± 457</td><td>4039 ± 256</td><td>4420 ± 420</td></tr><tr><td>2005dn</td><td>9500 ± 672</td><td>8420 ± 576</td><td>7613 ± 484</td><td>2360 ± 118</td><td>5750 ± 1511</td><td>4712 ± 434</td><td>...</td><td>4857 ± 241</td><td>6518 ± 627</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dt</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dx</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dz</td><td>7591 ± 595</td><td>6182 ± 434</td><td>5934 ± 430</td><td>925 ± 88</td><td>3927 ± 499</td><td>4101 ± 310</td><td>...</td><td>...</td><td>7397 ± 735</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005J</td><td>8434 ± 755</td><td>6353 ± 668</td><td>6380 ± 404</td><td>4235 ± 273</td><td>4129 ± 406</td><td>4224 ± 437</td><td>4151 ± 402</td><td>4190 ± 265</td><td>4994 ± 386</td><td>4097 ± 297</td><td>4581 ± 272</td><td>4500 ± 460</td></tr><tr><td>2005lw</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005Z</td><td>9479 ± 661</td><td>8538 ± 582</td><td>7879 ± 843</td><td>5673 ± 281</td><td>5646 ± 384</td><td>5196 ± 411</td><td>5633 ± 489</td><td>5435 ± 359</td><td>7375 ± 560</td><td>6432 ± 655</td><td>4671 ± 480</td><td>6040 ± 640</td></tr><tr><td>2006ai</td><td>7480 ± 821</td><td>6949 ± 559</td><td>6301 ± 560</td><td>4135 ± 353</td><td>4424 ± 427</td><td>4623 ± 340</td><td>4396 ± 258</td><td>3379 ± 526</td><td>6184 ± 434</td><td>...</td><td>...</td><td>6750 ± 710</td></tr><tr><td>2006be</td><td>7441 ± 474</td><td>6360 ± 625</td><td>5868 ± 755</td><td>3760 ± 742</td><td>3682 ± 738</td><td>3690 ± 722</td><td>3870 ± 694</td><td>3305 ± 677</td><td>4431 ± 668</td><td>4921 ± 620</td><td>...</td><td>...</td></tr><tr><td>2006bl</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2006ee</td><td>5209 ± 426</td><td>5370 ± 675</td><td>3020 ± 619</td><td>3213 ± 254</td><td>3125 ± 194</td><td>3024 ± 255</td><td>3101 ± 299</td><td>2708 ± 316</td><td>3239 ± 267</td><td>2734 ± 262</td><td>2738 ± 202</td><td>...</td></tr><tr><td>2006it</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2006iw</td><td>7373 ± 671</td><td>6104 ± 566</td><td>5337 ± 694</td><td>4352 ± 687</td><td>4127 ± 678</td><td>4148 ± 722</td><td>3790 ± 688</td><td>3352 ± 682</td><td>5074 ± 724</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2006ms</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2006qr</td><td>6501 ± 419</td><td>5558 ± 487</td><td>5103 ± 285</td><td>3166 ± 872</td><td>3593 ± 221</td><td>3643 ± 200</td><td>3780 ± 188</td><td>3529 ± 175</td><td>4844 ± 554</td><td>3795 ± 188</td><td>2932 ± 146</td><td>...</td></tr><tr><td>2006Y</td><td>9007 ± 619</td><td>7770 ± 589</td><td>6958 ± 464</td><td>3748 ± 186</td><td>4946 ± 731</td><td>5076 ± 546</td><td>...</td><td>...</td><td>7004 ± 613</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007aa</td><td>5985 ± 539</td><td>5102 ± 550</td><td>4264 ± 374</td><td>3148 ± 398</td><td>3179 ± 378</td><td>3148 ± 396</td><td>3099 ± 324</td><td>2880 ± 266</td><td>3864 ± 321</td><td>2697 ± 187</td><td>2907 ± 267</td><td>2650 ± 300</td></tr><tr><td>2007ab</td><td>9768 ± 505</td><td>8495 ± 600</td><td>8205 ± 405</td><td>...</td><td>7140 ± 353</td><td>4776 ± 237</td><td>6957 ± 344</td><td>6418 ± 318</td><td>7285 ± 404</td><td>6743 ± 337</td><td>5949 ± 614</td><td>...</td></tr><tr><td>2007av</td><td>7234 ± 338</td><td>6065 ± 402</td><td>5366 ± 311</td><td>3664 ± 182</td><td>3874 ± 192</td><td>3847 ± 191</td><td>3847 ± 191</td><td>3714 ± 185</td><td>3957 ± 605</td><td>3662 ± 182</td><td>3452 ± 172</td><td>3240 ± 299</td></tr><tr><td>2007bf</td><td>5498 ± 580</td><td>3830 ± 410</td><td>4110 ± 420</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007hm</td><td>8237 ± 383</td><td>6197 ± 544</td><td>6404 ± 432</td><td>4289 ± 213</td><td>4039 ± 201</td><td>4403 ± 515</td><td>4835 ± 240</td><td>3341 ± 166</td><td>5278 ± 262</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007il</td><td>8022 ± 809</td><td>7390 ± 482</td><td>5916 ± 505</td><td>4220 ± 281</td><td>4100 ± 481</td><td>4282 ± 383</td><td>4017 ± 370</td><td>4493 ± 420</td><td>4798 ± 769</td><td>5544 ± 560</td><td>2709 ± 250</td><td>...</td></tr><tr><td>2007it</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007ld</td><td>7176 ± 700</td><td>11416 ± 990</td><td>6024 ± 580</td><td>...</td><td>3695 ± 350</td><td>3589 ± 350</td><td>...</td><td>...</td><td>5922 ± 600</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007oc</td><td>6749 ± 492</td><td>7072 ± 435</td><td>5239 ± 436</td><td>2274 ± 198</td><td>3281 ± 315</td><td>3694 ± 343</td><td>4188 ± 480</td><td>3859 ± 378</td><td>5019 ± 450</td><td>2887 ± 218</td><td>3266 ± 291</td><td>4700 ± 500</td></tr><tr><td>2007od</td><td>7171 ± 655</td><td>7163 ± 428</td><td>6698 ± 545</td><td>...</td><td>5188 ± 363</td><td>3863 ± 300</td><td>...</td><td>3876 ± 193</td><td>6202 ± 427</td><td>5100 ± 525</td><td>4846 ± 240</td><td>...</td></tr><tr><td>2007P</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007sq</td><td>8298 ± 943</td><td>8409 ± 437</td><td>7410 ± 366</td><td>5270 ± 390</td><td>5249 ± 260</td><td>5350 ± 265</td><td>4978 ± 247</td><td>4135 ± 205</td><td>5662 ± 280</td><td>...</td><td>...</td><td>44780 ± 430</td></tr><tr><td>2007U</td><td>8037 ± 837</td><td>7395 ± 516</td><td>6911 ± 721</td><td>...</td><td>5541 ± 274</td><td>5439 ± 550</td><td>5923 ± 293</td><td>5429 ± 269</td><td>6480 ± 340</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007W</td><td>4754 ± 935</td><td>4125 ± 558</td><td>3203 ± 269</td><td>2343 ± 182</td><td>2612 ± 337</td><td>2437 ± 454</td><td>2543 ± 156</td><td>2505 ± 164</td><td>2618 ± 186</td><td>2086 ± 104</td><td>2485 ± 124</td><td>2000 ± 195</td></tr><tr><td>2007X</td><td>8597 ± 675</td><td>8418 ± 537</td><td>6685 ± 601</td><td>...</td><td>5466 ± 383</td><td>4619 ± 762</td><td>6339 ± 399</td><td>5555 ± 354</td><td>6170 ± 708</td><td>5160 ± 427</td><td>5021 ± 496</td><td>5980 ± 610</td></tr><tr><td>2008ag</td><td>6906 ± 463</td><td>6284 ± 426</td><td>4583 ± 473</td><td>4045 ± 292</td><td>3951 ± 324</td><td>3939 ± 311</td><td>3862 ± 326</td><td>3521 ± 283</td><td>4215 ± 426</td><td>3223 ± 230</td><td>3499 ± 233</td><td>3460 ± 330</td></tr><tr><td>2008aw</td><td>8257 ± 621</td><td>7783 ± 911</td><td>6641 ± 530</td><td>4728 ± 376</td><td>4724 ± 526</td><td>4532 ± 654</td><td>5027 ± 458</td><td>4429 ± 372</td><td>6436 ± 478</td><td>4545 ± 394</td><td>4458 ± 271</td><td>...</td></tr><tr><td>2008bh</td><td>7824 ± 688</td><td>7263 ± 430</td><td>6297 ± 375</td><td>4236 ± 210</td><td>4339 ± 232</td><td>4189 ± 637</td><td>4327 ± 215</td><td>4180 ± 207</td><td>4683 ± 378</td><td>4466 ± 222</td><td>3990 ± 198</td><td>...</td></tr><tr><td>2008bk</td><td>4115 ± 390</td><td>3313 ± 707</td><td>2401 ± 224</td><td>1867 ± 133</td><td>2256 ± 153</td><td>2910 ± 460</td><td>2266 ± 276</td><td>2437 ± 310</td><td>2019 ± 171</td><td>1846 ± 137</td><td>1998 ± 180</td><td>1780 ± 194</td></tr><tr><td>2008bm</td><td>1765 ± 56</td><td>11118 ± 88</td><td>1385 ± 69</td><td>1559 ± 78</td><td>1649 ± 82</td><td>1277 ± 64</td><td>...</td><td>...</td><td>1762 ± 88</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008bp</td><td>6795 ± 710</td><td>8613 ± 830</td><td>7497 ± 700</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008br</td><td>4070 ± 491</td><td>3682 ± 258</td><td>2484 ± 169</td><td>1665 ± 178</td><td>1832 ± 142</td><td>1633 ± 218</td><td>2161 ± 108</td><td>2547 ± 127</td><td>1922 ± 96</td><td>1386 ± 69</td><td>1670 ± 83</td><td>1420 ± 180</td></tr><tr><td>2008bu</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008ga</td><td>7313 ± 589</td><td>6400 ± 653</td><td>5357 ± 768</td><td>3307 ± 754</td><td>3390 ± 732</td><td>3253 ± 757</td><td>4665 ± 694</td><td>3179 ± 677</td><td>4785 ± 663</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008gi</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008gr</td><td>8832 ± 752</td><td>8361 ± 435</td><td>7548 ± 385</td><td>...</td><td>5412 ± 268</td><td>5013 ± 249</td><td>5918 ± 293</td><td>5572 ± 276</td><td>7487 ± 708</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008H</td><td>6608 ± 790</td><td>6734 ± 703</td><td>5355 ± 941</td><td>3863 ± 420</td><td>3791 ± 360</td><td>3738 ± 350</td><td>3821 ± 400</td><td>3678 ± 783</td><td>4669 ± 760</td><td>3390 ± 325</td><td>3430 ± 410</td><td>...</td></tr><tr><td>2008hg</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>Table 3
(Continued)</caption><thead><tr><th>SN</th><th>vel(H<sub>α</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(H<sub>β</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(H<sub>β</sub>)<br>(km s<sup>-1</sup>)</th><th>vel(Fe<br>II λ4924)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>λ5018)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>λ5169)<br>(km s<sup>-1</sup>)</th><th>vel(Fe II<br>/Sc II)<br>(km s<sup>-1</sup>)</th><th>vel(Sc II<br>Mult.)<br>(km s<sup>-1</sup>)</th><th>vel(Na I D)<br>(km s<sup>-1</sup>)</th><th>vel(Ba II)<br>(km s<sup>-1</sup>)</th><th>vel(Sc II)<br>(km s<sup>-1</sup>)</th><th>vel(O I)<br>(km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td>2008ho</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008if</td><td>8534 ± 1126</td><td>8717 ± 549</td><td>7226 ± 642</td><td>3198 ± 200</td><td>4929 ± 298</td><td>4758 ± 398</td><td>5062 ± 272</td><td>4785 ± 251</td><td>7404 ± 633</td><td>3802 ± 189</td><td>4619 ± 234</td><td>4975 ± 515</td></tr><tr><td>2008il</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008in</td><td>4283 ± 721</td><td>4422 ± 768</td><td>3234 ± 310</td><td>2768 ± 259</td><td>2839 ± 373</td><td>2831 ± 455</td><td>2679 ± 283</td><td>2680 ± 251</td><td>2917 ± 321</td><td>2378 ± 203</td><td>2574 ± 227</td><td>2430 ± 266</td></tr><tr><td>2008K</td><td>7885 ± 619</td><td>7987 ± 793</td><td>6868 ± 701</td><td>...</td><td>6197 ± 352</td><td>5359 ± 437</td><td>...</td><td>5491 ± 301</td><td>7066 ± 501</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008M</td><td>6872 ± 862</td><td>6123 ± 631</td><td>5709 ± 474</td><td>3508 ± 214</td><td>3457 ± 345</td><td>3647 ± 458</td><td>3772 ± 271</td><td>3616 ± 198</td><td>4793 ± 1056</td><td>3388 ± 217</td><td>3507 ± 275</td><td>3040 ± 290</td></tr><tr><td>2008W</td><td>7013 ± 665</td><td>6016 ± 435</td><td>5873 ± 435</td><td>3455 ± 335</td><td>3743 ± 233</td><td>3846 ± 297</td><td>3733 ± 224</td><td>3506 ± 278</td><td>5244 ± 470</td><td>3094 ± 255</td><td>3314 ± 185</td><td>3100 ± 324</td></tr><tr><td>2009aj</td><td>3112 ± 455</td><td>2800 ± 183</td><td>2814 ± 470</td><td>2090 ± 161</td><td>2431 ± 197</td><td>2849 ± 315</td><td>...</td><td>...</td><td>3026 ± 240</td><td>...</td><td>...</td><td>200 ± 80</td></tr><tr><td>2009ao</td><td>5979 ± 859</td><td>6753 ± 544</td><td>5240 ± 471</td><td>3792 ± 334</td><td>3695 ± 256</td><td>3597 ± 210</td><td>4155 ± 206</td><td>3770 ± 230</td><td>4687 ± 335</td><td>...</td><td>3416 ± 170</td><td>3120 ± 290</td></tr><tr><td>2009au</td><td>2586 ± 524</td><td>2613 ± 215</td><td>1985 ± 165</td><td>1618 ± 113</td><td>1732 ± 161</td><td>1474 ± 175</td><td>1775 ± 237</td><td>1919 ± 296</td><td>1949 ± 118</td><td>1289 ± 64</td><td>1704 ± 85</td><td>1520 ± 130</td></tr><tr><td>2009bu</td><td>7400 ± 596</td><td>6430 ± 521</td><td>5567 ± 604</td><td>3996 ± 267</td><td>3975 ± 436</td><td>4034 ± 456</td><td>4233 ± 210</td><td>3460 ± 172</td><td>4378 ± 308</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2009bz</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2009N</td><td>4514 ± 377</td><td>4069 ± 909</td><td>2815 ± 259</td><td>2527 ± 282</td><td>2651 ± 299</td><td>2600 ± 439</td><td>2549 ± 238</td><td>2500 ± 195</td><td>2705 ± 186</td><td>2299 ± 206</td><td>2397 ± 156</td><td>2190 ± 185</td></tr></tbody></table>

Note. Columns: (1) SN name; (2) velocity of Hα absorption component; (3) velocity of Hα emission component; (4) velocity of Hβ; (5) velocity of Fe II λ4924; (6) velocity of Fe II λ5018; (7) velocity of Fe II λ5169; (8) velocity of Fe II/Sc II; (9) velocity of Sc II Multiplet; (10) velocity of Na I D; (11) velocity of Ba II; (12) velocity of Sc II; and (13) velocity of O I.
<table><caption>Table 4
pEW Values at 50 Days from Explosion</caption><thead><tr><th>SN</th><th>H<sub>α</sub><br>(Å)</th><th>H<sub>β</sub><br>(Å)</th><th>H<sub>γ</sub><br>(Å)</th><th>Fe II λ4924<br>(Å)</th><th>Fe II λ5018<br>(Å)</th><th>Fe II λ5169<br>(Å)</th><th>Fe II/Sc II<br>(Å)</th><th>Sc II Mult.<br>(Å)</th><th>Na I D<br>(Å)</th><th>Ba II<br>(Å)</th><th>Sc II<br>(Å)</th><th>a/e</th></tr></thead><tbody><tr><td>1986L</td><td>32.8 ± 4.1</td><td>144.2 ± 34.2</td><td>48.2 ± 3.6</td><td>1.2 ± 0.6</td><td>14.7 ± 1.8</td><td>36.7 ± 3.8</td><td>7.6 ± 2.9</td><td>10.4 ± 2.1</td><td>29.2 ± 2.7</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.23 ± 0.08</td></tr><tr><td>1988A</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1990E</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1990K</td><td>42.7 ± 3.8</td><td>206.2 ± 27.4</td><td>71.9 ± 4.4</td><td>0.0 ± 0.0</td><td>10.9 ± 0.7</td><td>38.8 ± 2.1</td><td>8.9 ± 0.7</td><td>13.2 ± 1.6</td><td>50.3 ± 2.5</td><td>6.4 ± 0.4</td><td>5.9 ± 0.9</td><td>0.21 ± 0.05</td></tr><tr><td>1991aI</td><td>62.1 ± 5.8</td><td>214.2 ± 25.8</td><td>67.5 ± 5.2</td><td>4.8 ± 1.7</td><td>13.0 ± 1.7</td><td>27.2 ± 3.8</td><td>4.3 ± 1.9</td><td>6.5 ± 1.8</td><td>20.4 ± 1.2</td><td>6.4 ± 0.9</td><td>4.1 ± 1.2</td><td>0.29 ± 0.08</td></tr><tr><td>1992ad</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1992af</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1992am</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1992ba</td><td>61.9 ± 4.2</td><td>119.3 ± 19.7</td><td>47.0 ± 3.9</td><td>7.6 ± 2.5</td><td>20.2 ± 2.5</td><td>30.1 ± 3.9</td><td>9.9 ± 1.5</td><td>13.7 ± 1.7</td><td>34.2 ± 3.7</td><td>7.9 ± 1.1</td><td>7.1 ± 0.9</td><td>0.52 ± 0.15</td></tr><tr><td>1993A</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1993K</td><td>27.8 ± 3.8</td><td>126.1 ± 25.3</td><td>42.8 ± 2.7</td><td>6.4 ± 2.4</td><td>18.9 ± 3.8</td><td>28.7 ± 1.9</td><td>5.2 ± 1.2</td><td>7.3 ± 1.4</td><td>27.1 ± 1.9</td><td>3.8 ± 1</td><td>3.8 ± 1.1</td><td>0.22 ± 0.08</td></tr><tr><td>1993S</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1999br</td><td>56.0 ± 3.1</td><td>14.6 ± 10.6</td><td>33.8 ± 4.8</td><td>15.0 ± 1.7</td><td>25.2 ± 1.5</td><td>43.1 ± 3.1</td><td>15.1 ± 2.9</td><td>20.8 ± 2</td><td>20.7 ± 1.9</td><td>12.9 ± 1.6</td><td>14.2 ± 1.0</td><td>3.84 ± 3.06</td></tr><tr><td>1999ca</td><td>48.3 ± 2.7</td><td>169.4 ± 13.6</td><td>78.9 ± 3.9</td><td>0.0 ± 0.0</td><td>17.6 ± 1.3</td><td>64.1 ± 2.9</td><td>11.1 ± 1.1</td><td>19.6 ± 1.7</td><td>33.7 ± 2.1</td><td>5.4 ± 0.4</td><td>11.6 ± 0.8</td><td>0.29 ± 0.03</td></tr><tr><td>1999cr</td><td>31.7 ± 4.2</td><td>137.5 ± 22.9</td><td>37.6 ± 4.1</td><td>0.0 ± 0.0</td><td>12.4 ± 1.7</td><td>24.9 ± 1.8</td><td>0.0 ± 0.0</td><td>6.4 ± 1.1</td><td>9.3 ± 2.2</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.23 ± 0.12</td></tr><tr><td>1999eg</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>1999em</td><td>75.8 ± 5.1</td><td>141.2 ± 40.2</td><td>40.3 ± 5.6</td><td>9.9 ± 1.6</td><td>23.8 ± 1.8</td><td>43.6 ± 2.5</td><td>11.7 ± 1.8</td><td>13.4 ± 2</td><td>30.6 ± 1.8</td><td>6.7 ± 1.0</td><td>7.5 ± 1.2</td><td>0.54 ± 0.25</td></tr><tr><td>S0210</td><td>36 ± 3.9</td><td>287.4 ± 42.3</td><td>83.5 ± 4.9</td><td>0.0 ± 0.0</td><td>30.4 ± 2.5</td><td>70.1 ± 3.5</td><td>7.8 ± 1.2</td><td>40.4 ± 3.3</td><td>49.2 ± 3.2</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.13 ± 0.06</td></tr><tr><td>2002ew</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2002fa</td><td>45.4 ± 3.9</td><td>125.1 ± 43.6</td><td>52.4 ± 7.2</td><td>6.1 ± 1.1</td><td>15.5 ± 3.1</td><td>36.5 ± 2.4</td><td>9.7 ± 2.4</td><td>13.1 ± 2.4</td><td>42.4 ± 2.4</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.36 ± 0.21</td></tr><tr><td>2002gd</td><td>21.7 ± 3.3</td><td>106.8 ± 23.8</td><td>39.8 ± 3.3</td><td>5.8 ± 2.2</td><td>24.9 ± 3.5</td><td>59.3 ± 4.2</td><td>16.2 ± 2.8</td><td>26.9 ± 2.6</td><td>27.1 ± 5.1</td><td>3.8 ± 0.6</td><td>11.0 ± 2.1</td><td>0.20 ± 0.08</td></tr><tr><td>2002gw</td><td>61.4 ± 4.6</td><td>205.5 ± 29.5</td><td>58.4 ± 4.6</td><td>6.9 ± 1.6</td><td>18.2 ± 2.1</td><td>31.3 ± 2.7</td><td>5.5 ± 1.7</td><td>5.8 ± 2.0</td><td>13.5 ± 1.3</td><td>3.1 ± 1.1</td><td>3.8 ± 1.5</td><td>0.30 ± 0.11</td></tr><tr><td>2002hj</td><td>70.1 ± 5.3</td><td>207.5 ± 34.1</td><td>71.7 ± 5.5</td><td>2.8 ± 1.6</td><td>16.5 ± 2.9</td><td>40.8 ± 3.2</td><td>4.3 ± 2.5</td><td>10.2 ± 2.4</td><td>18.6 ± 1.9</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.34 ± 0.11</td></tr><tr><td>2002hx</td><td>88.8 ± 6.1</td><td>135.6 ± 18.1</td><td>73.8 ± 4.8</td><td>9.8 ± 2.2</td><td>20.8 ± 2.2</td><td>35.5 ± 3.0</td><td>7.5 ± 1.1</td><td>17.9 ± 1.7</td><td>53.1 ± 4.1</td><td>8.6 ± 1.2</td><td>1.3 ± 2.1</td><td>0.65 ± 0.16</td></tr><tr><td>2002ig</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>0.0 ± 0.0</td><td>...</td></tr><tr><td>2003B</td><td>60.1 ± 5.3</td><td>148.6 ± 27.6</td><td>53.0 ± 4.5</td><td>10.5 ± 1.8</td><td>23.4 ± 2.5</td><td>38.1 ± 2.3</td><td>14.2 ± 1.4</td><td>20.3 ± 2.4</td><td>28.6 ± 2.2</td><td>3.9 ± 0.9</td><td>8.8 ± 1.5</td><td>0.40 ± 0.11</td></tr><tr><td>2003bl</td><td>58.0 ± 4.3</td><td>116.5 ± 19.1</td><td>37.1 ± 2.1</td><td>15.1 ± 2.8</td><td>26.5 ± 2.5</td><td>38.3 ± 1.8</td><td>10.9 ± 2.9</td><td>17.0 ± 3.2</td><td>19.3 ± 1.6</td><td>11.7 ± 1.4</td><td>9.1 ± 1.9</td><td>0.51 ± 0.14</td></tr><tr><td>2003bn</td><td>77.7 ± 5.4</td><td>144.4 ± 66.6</td><td>55.3 ± 6.5</td><td>7.1 ± 1.9</td><td>17.3 ± 2.6</td><td>36.0 ± 1.1</td><td>8.3 ± 2.1</td><td>9.1 ± 1.4</td><td>16.1 ± 2.3</td><td>3.2 ± 1.0</td><td>2.5 ± 1.1</td><td>0.54 ± 0.36</td></tr><tr><td>2003ci</td><td>50.6 ± 2.5</td><td>166.2 ± 8.3</td><td>64.6 ± 3.2</td><td>1.3 ± 0.1</td><td>15.8 ± 0.8</td><td>46.2 ± 3.6</td><td>10.4 ± 0.5</td><td>20.7 ± 1.0</td><td>55.1 ± 1.8</td><td>7.7 ± 0.4</td><td>4.2 ± 0.2</td><td>0.31 ± 0.03</td></tr><tr><td>2003cn</td><td>43.7 ± 2.9</td><td>141.6 ± 18.4</td><td>52.9 ± 4.7</td><td>12.6 ± 2.1</td><td>21.1 ± 3.4</td><td>35.1 ± 2.9</td><td>9.2 ± 1.8</td><td>17.2 ± 1.3</td><td>18.2 ± 1.7</td><td>7.4 ± 1.5</td><td>7.1 ± 1.2</td><td>0.31 ± 0.06</td></tr><tr><td>2003cx</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003dq</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003E</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003ef</td><td>91.4 ± 7.3</td><td>130.5 ± 14.3</td><td>27.9 ± 4.2</td><td>9.8 ± 1.3</td><td>20.4 ± 1.7</td><td>28.3 ± 3.4</td><td>10.8 ± 2.9</td><td>9.4 ± 1.2</td><td>24.2 ± 1</td><td>1.9 ± 0.9</td><td>9.6 ± 1.2</td><td>0.70 ± 0.15</td></tr><tr><td>2003eg</td><td>9.4 ± 1.1</td><td>244.2 ± 24.5</td><td>60.6 ± 3.4</td><td>0.0 ± 0.0</td><td>14.4 ± 1.5</td><td>38.6 ± 1.1</td><td>10.5 ± 2.4</td><td>14.2 ± 1.7</td><td>58.4 ± 1.3</td><td>7.1 ± 1.1</td><td>6.5 ± 0.8</td><td>0.04 ± 0.01</td></tr><tr><td>2003ej</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003fb</td><td>73.7 ± 6.3</td><td>185.1 ± 13.4</td><td>55.1 ± 2.2</td><td>8.1 ± 0.8</td><td>18.1 ± 0.8</td><td>40 ± 2.3</td><td>7.9 ± 0.7</td><td>9.0 ± 1.1</td><td>25.0 ± 1.6</td><td>9.0 ± 1.8</td><td>7.1 ± 1.2</td><td>0.4 ± 0.06</td></tr><tr><td>2003gd</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003hd</td><td>78.1 ± 5.2</td><td>119.1 ± 30.9</td><td>56.8 ± 4.4</td><td>4.9 ± 1.1</td><td>16.1 ± 2.1</td><td>33.9 ± 2</td><td>4.6 ± 1.8</td><td>7.9 ± 0.7</td><td>15.4 ± 2.3</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.65 ± 0.26</td></tr><tr><td>2003hg</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003hk</td><td>32.6 ± 2.4</td><td>123.2 ± 12.4</td><td>39.2 ± 3.7</td><td>9.3 ± 2.9</td><td>17.6 ± 2.3</td><td>34.6 ± 2.6</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>44.3 ± 1.1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.26 ± 0.18</td></tr><tr><td>2003hl</td><td>50.4 ± 3.1</td><td>118.3 ± 22.1</td><td>32.6 ± 5.9</td><td>6.8 ± 2.4</td><td>22.1 ± 2.9</td><td>39.5 ± 3.1</td><td>15.4 ± 1.9</td><td>19.2 ± 2.1</td><td>35.9 ± 2.5</td><td>5.6 ± 1.6</td><td>1.1 ± 1.2</td><td>0.43 ± 0.13</td></tr><tr><td>2003hn</td><td>61.4 ± 4.0</td><td>178.7 ± 22.4</td><td>60.0 ± 4.4</td><td>7.2 ± 1.1</td><td>17.5 ± 1.5</td><td>39.1 ± 3.7</td><td>10.2 ± 0.8</td><td>13.3 ± 1.5</td><td>31.5 ± 2.6</td><td>4.3 ± 0.9</td><td>5.3 ± 0.8</td><td>0.34 ± 0.07</td></tr><tr><td>2003ho</td><td>68.4 ± 4.8</td><td>269.8 ± 54.9</td><td>69.1 ± 4.6</td><td>5.4 ± 1.3</td><td>16.9 ± 1.9</td><td>42.7 ± 3.2</td><td>7.9 ± 1.1</td><td>8.3 ± 0.7</td><td>36.1 ± 1.9</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.25 ± 0.08</td></tr><tr><td>2003ib</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2003ip</td><td>60.9 ± 4.2</td><td>191.4 ± 18.1</td><td>71.2 ± 6.8</td><td>0.0 ± 0.0</td><td>9.3 ± 2.2</td><td>43 ± 3.7</td><td>6.5 ± 1.4</td><td>12.0 ± 1.0</td><td>33.2 ± 2.6</td><td>4.9 ± 0.6</td><td>5.9 ± 1.1</td><td>0.32 ± 0.05</td></tr><tr><td>2003iq</td><td>84.2 ± 5.6</td><td>157.9 ± 14.4</td><td>46.2 ± 4.2</td><td>7.8 ± 2.1</td><td>21.3 ± 1.8</td><td>37.7 ± 3.1</td><td>10.4 ± 2.6</td><td>10.7 ± 0.9</td><td>32.3 ± 2.9</td><td>3.4 ± 1.2</td><td>6.0 ± 1.0</td><td>0.53 ± 0.13</td></tr></tbody></table>
<table><caption>Table 4
(Continued)</caption><thead><tr><th>SN</th><th>H<sub>α</sub> (Å)</th><th>H<sub>β</sub> (Å)</th><th>H<sub>γ</sub> (Å)</th><th>Fe II λ4924 (Å)</th><th>Fe II λ5018 (Å)</th><th>Fe II λ5169 (Å)</th><th>Fe II/Sc II (Å)</th><th>Sc II Mult. (Å)</th><th>Na I D (Å)</th><th>Ba II (Å)</th><th>Sc II (Å)</th><th>a/e</th></tr></thead><tbody><tr><td>2003T</td><td>58.5 ± 6</td><td>153.6 ± 29.6</td><td>27.6 ± 3.1</td><td>11.5 ± 3.7</td><td>22.9 ± 1.9</td><td>38.2 ± 3.6</td><td>14.0 ± 2.9</td><td>14.9 ± 1.3</td><td>35.1 ± 2.5</td><td>18.7 ± 6.7</td><td>10.2 ± 1.2</td><td>0.38 ± 0.21</td></tr><tr><td>2004dy</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2004ej</td><td>57.1 ± 3.8</td><td>114.6 ± 20.3</td><td>48.6 ± 4.7</td><td>9.1 ± 2.1</td><td>20.7 ± 1.7</td><td>44.0 ± 4.3</td><td>14.7 ± 2.3</td><td>21.8 ± 2.9</td><td>37.2 ± 3.1</td><td>6.4 ± 1.6</td><td>5.9 ± 1.7</td><td>0.50 ± 0.17</td></tr><tr><td>2004er</td><td>74.4 ± 5.7</td><td>154.3 ± 23.7</td><td>59.2 ± 4.7</td><td>3.2 ± 1.5</td><td>10.7 ± 2.3</td><td>34.3 ± 2.8</td><td>3.6 ± 0.7</td><td>6.4 ± 1.4</td><td>16.2 ± 2.3</td><td>0.4 ± 0.6</td><td>2.6 ± 0.7</td><td>0.48 ± 0.14</td></tr><tr><td>2004fb</td><td>70.1 ± 7.2</td><td>165.5 ± 26.1</td><td>59.1 ± 3.4</td><td>6.9 ± 0.5</td><td>18.7 ± 2.1</td><td>46.9 ± 4.4</td><td>11.6 ± 1.2</td><td>16.8 ± 2.1</td><td>41.6 ± 2.8</td><td>10.8 ± 1.0</td><td>10.4 ± 1.2</td><td>0.42 ± 0.29</td></tr><tr><td>2004fc</td><td>34.8 ± 6.2</td><td>85.6 ± 37.9</td><td>16.2 ± 4.8</td><td>7.9 ± 2.1</td><td>18.7 ± 2.8</td><td>28.2 ± 3.1</td><td>10.2 ± 1.9</td><td>14.4 ± 1.7</td><td>23.1 ± 2.3</td><td>5.0 ± 1.1</td><td>6.6 ± 1.8</td><td>0.41 ± 0.36</td></tr><tr><td>2004fx</td><td>70.6 ± 4.7</td><td>168.9 ± 35.7</td><td>55.7 ± 3.3</td><td>8.6 ± 2.3</td><td>18.6 ± 3.1</td><td>30.7 ± 2.0</td><td>7.2 ± 2.5</td><td>4.4 ± 0.6</td><td>11.3 ± 1.2</td><td>2.7 ± 1.2</td><td>4.8 ± 1.4</td><td>0.42 ± 0.15</td></tr><tr><td>2005af</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005an</td><td>51.9 ± 3.8</td><td>210.8 ± 27.1</td><td>74.4 ± 5.7</td><td>4.1 ± 0.4</td><td>15.4 ± 1.6</td><td>42.8 ± 2.9</td><td>12.1 ± 2.1</td><td>22.2 ± 2.5</td><td>18.4 ± 1.8</td><td>0.0 ± 0.0</td><td>10.5 ± 0.9</td><td>0.25 ± 0.06</td></tr><tr><td>2005dk</td><td>49.0 ± 3.3</td><td>166.6 ± 19.0</td><td>57.6 ± 3.5</td><td>5.4 ± 0.7</td><td>13.4 ± 1.2</td><td>32.7 ± 3.2</td><td>8.9 ± 2.3</td><td>11.1 ± 1.3</td><td>32.1 ± 1.6</td><td>4.2 ± 0.9</td><td>4.6 ± 0.9</td><td>0.29 ± 0.08</td></tr><tr><td>2005dn</td><td>66.6 ± 4.1</td><td>238.9 ± 54.3</td><td>77.9 ± 4.5</td><td>1.1 ± 2.2</td><td>3.9 ± 1.1</td><td>48.0 ± 3.1</td><td>0.0 ± 0.0</td><td>10.5 ± 1.2</td><td>30.7 ± 2.4</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.28 ± 0.09</td></tr><tr><td>2005dt</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dw</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dx</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005dz</td><td>77.2 ± 3.4</td><td>205 ± 41.1</td><td>50.4 ± 4.1</td><td>0.0 ± 0.0</td><td>20.3 ± 2.3</td><td>34.4 ± 2.8</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.38 ± 0.141</td></tr><tr><td>2005es</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005J</td><td>77.2 ± 5.5</td><td>133.7 ± 30.3</td><td>64.0 ± 2.5</td><td>5.5 ± 1.8</td><td>15.9 ± 2.5</td><td>36.6 ± 2.4</td><td>8.6 ± 1.8</td><td>12.2 ± 1.4</td><td>23.2 ± 1.4</td><td>4.8 ± 1.7</td><td>3.9 ± 1.3</td><td>0.58 ± 0.201</td></tr><tr><td>2005K</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005lw</td><td>45.1 ± 4.2</td><td>210.0 ± 15.2</td><td>50.1 ± 3.4</td><td>0.0 ± 0.0</td><td>9.2 ± 1.5</td><td>60.0 ± 3.1</td><td>6.1 ± 1.7</td><td>7.0 ± 0.7</td><td>26.0 ± 2.1</td><td>3.5 ± 1.2</td><td>4.9 ± 1.6</td><td>0.21 ± 0.17</td></tr><tr><td>2005me</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2005Z</td><td>65.9 ± 3.4</td><td>192.1 ± 35.7</td><td>56.8 ± 4.3</td><td>6.9 ± 1.5</td><td>12.7 ± 1.6</td><td>36.1 ± 3.7</td><td>10.4 ± 2.2</td><td>13.9 ± 1.6</td><td>49.2 ± 2.9</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.34 ± 0.118</td></tr><tr><td>2006ai</td><td>15.4 ± 2.6</td><td>173.2 ± 22.5</td><td>38.5 ± 3.4</td><td>3.2 ± 1.2</td><td>15.0 ± 2.1</td><td>36.8 ± 4.1</td><td>6.5 ± 2.5</td><td>7.8 ± 1.7</td><td>35.4 ± 2.1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.09 ± 0.038</td></tr><tr><td>2006bc</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2006be</td><td>62.2 ± 3.3</td><td>180.5 ± 7</td><td>68.1 ± 3.0</td><td>5.6 ± 1.3</td><td>15.1 ± 0.7</td><td>26.0 ± 2.1</td><td>8.0 ± 1.2</td><td>12.0 ± 1.2</td><td>20.0 ± 1.2</td><td>5.3 ± 1.0</td><td>0.0 ± 0.0</td><td>0.34 ± 0.037</td></tr><tr><td>2006bl</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2006ee</td><td>62.6 ± 6.2</td><td>122.1 ± 22.5</td><td>24.5 ± 4.5</td><td>15.2 ± 3.2</td><td>26.6 ± 2.9</td><td>42.4 ± 2.8</td><td>14.6 ± 1.5</td><td>18.1 ± 2.2</td><td>39.1 ± 2.8</td><td>13.1 ± 1.8</td><td>14.1 ± 1.2</td><td>0.51 ± 0.227</td></tr><tr><td>2006it</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2006iw</td><td>40.6 ± 4.2</td><td>94.7 ± 12.2</td><td>38.1 ± 3.3</td><td>3.5 ± 1.6</td><td>10.0 ± 0.7</td><td>16.0 ± 1.6</td><td>5.0 ± 0.8</td><td>6.7 ± 1.2</td><td>12.1 ± 2</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.43 ± 0.097</td></tr><tr><td>2006ms</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2006qr</td><td>69.7 ± 4.6</td><td>133.1 ± 15.1</td><td>61.9 ± 5.3</td><td>11.5 ± 0.6</td><td>22.1 ± 1.9</td><td>44.0 ± 4.2</td><td>16.3 ± 3.1</td><td>20.2 ± 2.6</td><td>33.6 ± 2.4</td><td>8.8 ± 1.9</td><td>12.6 ± 1.2</td><td>0.52 ± 0.214</td></tr><tr><td>2006Y</td><td>10.4 ± 2.9</td><td>123.7 ± 27.3</td><td>25.5 ± 2.8</td><td>1.6 ± 0.5</td><td>6.7 ± 1.8</td><td>16.3 ± 3.1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>15.8 ± 1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.08 ± 0.042</td></tr><tr><td>2007aa</td><td>74.5 ± 6.5</td><td>119.7 ± 11.0</td><td>52.5 ± 5.8</td><td>9.6 ± 1.1</td><td>20.7 ± 1.8</td><td>35.1 ± 2.5</td><td>10.7 ± 2.1</td><td>13.1 ± 1.5</td><td>31.8 ± 2.9</td><td>1.1 ± 0.9</td><td>5.7 ± 1.6</td><td>0.62 ± 0.145</td></tr><tr><td>2007ab</td><td>72.4 ± 5.1</td><td>232.1 ± 26.4</td><td>84.6 ± 5.4</td><td>0.0 ± 0.0</td><td>17.5 ± 3.6</td><td>77.2 ± 3.4</td><td>6.6 ± 2.6</td><td>23.0 ± 2.4</td><td>32.9 ± 2</td><td>8.0 ± 1.1</td><td>12.0 ± 2.3</td><td>0.31 ± 0.083</td></tr><tr><td>2007av</td><td>97 ± 6.6</td><td>164.9 ± 22.2</td><td>46.4 ± 3.3</td><td>8.6 ± 1.5</td><td>21.8 ± 1.4</td><td>43.9 ± 2.5</td><td>10.9 ± 2.8</td><td>12.3 ± 1.8</td><td>29.4 ± 3.2</td><td>7.6 ± 1.9</td><td>8.3 ± 1.5</td><td>0.59 ± 0.119</td></tr><tr><td>2007bf</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007hm</td><td>44.1 ± 4.3</td><td>180.7 ± 36.8</td><td>56.2 ± 5.9</td><td>8.3 ± 0.7</td><td>16.6 ± 3.3</td><td>29.1 ± 3.3</td><td>9.8 ± 1.6</td><td>14.3 ± 1.4</td><td>22.3 ± 2.2</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.24 ± 0.105</td></tr><tr><td>2007il</td><td>63.9 ± 5.4</td><td>190.2 ± 36.5</td><td>66.4 ± 4.2</td><td>2.8 ± 2.1</td><td>13.4 ± 2.5</td><td>28.2 ± 6.3</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>15.6 ± 1.1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.34 ± 0.114</td></tr><tr><td>2007it</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007ld</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007oc</td><td>35.5 ± 2.8</td><td>267.1 ± 22.4</td><td>70.1 ± 6.9</td><td>4.5 ± 1.5</td><td>8.0 ± 1.9</td><td>46.5 ± 4.6</td><td>4.3 ± 1.9</td><td>14.4 ± 1.9</td><td>43.6 ± 1.8</td><td>3.5 ± 1.5</td><td>2.9 ± 1.0</td><td>0.13 ± 0.022</td></tr><tr><td>2007od</td><td>32.9 ± 3.1</td><td>184.0 ± 22.5</td><td>65.2 ± 5.1</td><td>0.0 ± 0.0</td><td>14.7 ± 2.7</td><td>36.0 ± 3.8</td><td>0.0 ± 0.0</td><td>15.2 ± 1.7</td><td>16.4 ± 0.9</td><td>3.5 ± 0.6</td><td>5.3 ± 1.4</td><td>0.18 ± 0.039</td></tr><tr><td>2007P</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2007sq</td><td>37.5 ± 4.2</td><td>125.9 ± 36.4</td><td>48.3 ± 4</td><td>4.52 ± 1</td><td>6.8 ± 1.9</td><td>31.8 ± 3.5</td><td>5.1 ± 1.7</td><td>7.7 ± 0.9</td><td>22.4 ± 0.9</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.30 ± 0.167</td></tr><tr><td>2007U</td><td>31.1 ± 3.2</td><td>142.8 ± 32.4</td><td>54.3 ± 4.2</td><td>0.0 ± 0.0</td><td>12.0 ± 2.1</td><td>40.9 ± 2.3</td><td>10.0 ± 2.1</td><td>15.6 ± 2.1</td><td>17.1 ± 1.7</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.22 ± 0.079</td></tr><tr><td>2007W</td><td>67.2 ± 3.6</td><td>131.2 ± 21.7</td><td>38.1 ± 5.9</td><td>11.52 ± 2</td><td>21.7 ± 2.6</td><td>36.5 ± 2.8</td><td>10.2 ± 2.6</td><td>16.0 ± 1.8</td><td>13.5 ± 2.2</td><td>4.6 ± 1.3</td><td>4.1 ± 1.3</td><td>0.51 ± 0.127</td></tr><tr><td>2007X</td><td>45.2 ± 2.8</td><td>223.8 ± 32.8</td><td>77.1 ± 4.7</td><td>0.0 ± 0.0</td><td>13.9 ± 2.9</td><td>49.4 ± 2.1</td><td>10.3 ± 3.2</td><td>16.4 ± 1.6</td><td>22.9 ± 1.2</td><td>5.6 ± 0.9</td><td>9.1 ± 1.4</td><td>0.20 ± 0.06</td></tr><tr><td>2007Z</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>**Table 4**
(Continued)</caption><thead><tr><th>SN</th><th>H<sub>α</sub><br>(Å)</th><th>H<sub>β</sub><br>(Å)</th><th>H<sub>β</sub><br>(Å)</th><th>Fe II λ4924<br>(Å)</th><th>Fe II λ5018<br>(Å)</th><th>Fe II λ5169<br>(Å)</th><th>Fe II/Sc II<br>(Å)</th><th>Sc II Mult.<br>(Å)</th><th>Na I D<br>(Å)</th><th>Ba II<br>(Å)</th><th>Sc II<br>(Å)</th><th>a/e</th></tr></thead><tbody><tr><td>2008ag</td><td>60.6 ± 5.2</td><td>185.2 ± 15.8</td><td>39.3 ± 3.2</td><td>10.7 ± 2.1</td><td>22.3 ± 1.7</td><td>38.9 ± 2.6</td><td>10.1 ± 1.9</td><td>14.6 ± 1.7</td><td>38.4 ± 2.1</td><td>3.3 ± 1.8</td><td>5.5 ± 1.2</td><td>0.33 ± 0.072</td></tr><tr><td>2008aw</td><td>17.8 ± 2.3</td><td>175.8 ± 18.8</td><td>47.1 ± 4.6</td><td>3.1 ± 1.3</td><td>12.4 ± 1.4</td><td>37.8 ± 1.4</td><td>6.4 ± 1.2</td><td>8.2 ± 0.6</td><td>38.8 ± 2.9</td><td>3.6 ± 1.6</td><td>3.6 ± 1.3</td><td>0.10 ± 0.051</td></tr><tr><td>2008bh</td><td>55.8 ± 4.2</td><td>216.8 ± 41.7</td><td>54.4 ± 5.6</td><td>4.7 ± 1.3</td><td>16.2 ± 2.0</td><td>36.2 ± 1.1</td><td>8.3 ± 2.2</td><td>9.8 ± 1.0</td><td>16.7 ± 1.9</td><td>5.2 ± 0.9</td><td>5.2 ± 0.8</td><td>0.26 ± 0.101</td></tr><tr><td>2008bk</td><td>57.5 ± 4.8</td><td>94.3 ± 12.0</td><td>31.9 ± 3.9</td><td>16.3 ± 1.2</td><td>24.6 ± 2.1</td><td>43.7 ± 3.5</td><td>14.8 ± 1.7</td><td>21.8 ± 2.1</td><td>20.1 ± 1.7</td><td>11.8 ± 1.2</td><td>10.5 ± 1.1</td><td>0.61 ± 0.16</td></tr><tr><td>2008bm</td><td>4.6 ± 0.2</td><td>16.1 ± 0.8</td><td>19.2 ± 1.3</td><td>9.1 ± 0.5</td><td>11.6 ± 0.6</td><td>19.8 ± 2.1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>3.4 ± 0.6</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.29 ± 0.027</td></tr><tr><td>2008bp</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008br</td><td>15.8 ± 3.0</td><td>23.3 ± 17.9</td><td>22.3 ± 3.2</td><td>7.1 ± 1.8</td><td>7.2 ± 1.1</td><td>9.7 ± 2.8</td><td>8.8 ± 1.9</td><td>12.9 ± 1.1</td><td>12.4 ± 0.7</td><td>9.4 ± 1.1</td><td>6.7 ± 2.5</td><td>0.69 ± 0.752</td></tr><tr><td>2008bu</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008F</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008ga</td><td>85 ± 5.7</td><td>234.1 ± 13.2</td><td>60.0 ± 2.3</td><td>6.8 ± 1.5</td><td>17.0 ± 1.5</td><td>35.1 ± 2.1</td><td>7.1 ± 1.8</td><td>15.0 ± 1.7</td><td>55.0 ± 2.1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.36 ± 0.045</td></tr><tr><td>2008gi</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008gr</td><td>35.5 ± 3.5</td><td>186.4 ± 41.5</td><td>56.6 ± 3.6</td><td>0.0 ± 0.0</td><td>7.3 ± 0.9</td><td>34.1 ± 2.6</td><td>4.7 ± 1.8</td><td>7.8 ± 1.0</td><td>30.9 ± 2.5</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.19 ± 0.099</td></tr><tr><td>2008H</td><td>63.3 ± 5.1</td><td>150.2 ± 21.0</td><td>33.0 ± 3.1</td><td>10.0 ± 2.1</td><td>22.2 ± 1.7</td><td>51.0 ± 3.2</td><td>14 ± 1.9</td><td>20.0 ± 2.1</td><td>54.1 ± 3.1</td><td>15.0 ± 2.2</td><td>14.0 ± 1.8</td><td>0.42 ± 0.132</td></tr><tr><td>2008hg</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008ho</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008if</td><td>26.1 ± 2.3</td><td>239.2 ± 58.9</td><td>61.8 ± 3.7</td><td>2.4 ± 1.1</td><td>9.3 ± 1.3</td><td>30.2 ± 3.3</td><td>4.7 ± 1.2</td><td>6.9 ± 1.3</td><td>48.3 ± 3.2</td><td>1.2 ± 0.5</td><td>3.7 ± 0.9</td><td>0.11 ± 0.06</td></tr><tr><td>2008il</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2008in</td><td>54.8 ± 7.3</td><td>157.6 ± 49.6</td><td>36.6 ± 3.1</td><td>14.5 ± 3.1</td><td>26.9 ± 1.9</td><td>42.9 ± 2.7</td><td>14.7 ± 2.6</td><td>18.3 ± 1.4</td><td>38.8 ± 2.3</td><td>6.4 ± 1.4</td><td>8.3 ± 1.8</td><td>0.35 ± 0.22</td></tr><tr><td>2008K</td><td>40.5 ± 4.5</td><td>250.8 ± 44.5</td><td>80.4 ± 4.2</td><td>0.0 ± 0.0</td><td>17.4 ± 2.6</td><td>62.8 ± 1.8</td><td>0.0 ± 0.0</td><td>19.1 ± 2.1</td><td>41.5 ± 3.1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.16 ± 0.07</td></tr><tr><td>2008M</td><td>54.0 ± 5.5</td><td>208.7 ± 27.7</td><td>72.9 ± 3.8</td><td>5.3 ± 2.1</td><td>20.2 ± 3.4</td><td>34.0 ± 1.9</td><td>4.9 ± 2.1</td><td>7.5 ± 1.4</td><td>30.3 ± 2.8</td><td>2.5 ± 0.9</td><td>1.6 ± 1.1</td><td>0.26 ± 0.06</td></tr><tr><td>2008W</td><td>46.7 ± 4.2</td><td>200.2 ± 21.9</td><td>60.4 ± 3.4</td><td>5.1 ± 1.9</td><td>16.4 ± 2.9</td><td>36.9 ± 2.8</td><td>7.7 ± 1.9</td><td>12.7 ± 1.1</td><td>45.9 ± 1.7</td><td>3.5 ± 1.4</td><td>4.6 ± 1.7</td><td>0.23 ± 0.08</td></tr><tr><td>2009aj</td><td>8.1 ± 1.6</td><td>46.7 ± 6.1</td><td>13 ± 2.2</td><td>6.2 ± 1.6</td><td>8.5 ± 0.9</td><td>13.9 ± 3.1</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>1.7 ± 0.6</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.17 ± 0.06</td></tr><tr><td>2009ao</td><td>40.2 ± 3.1</td><td>148.6 ± 11</td><td>54.5 ± 3.4</td><td>5.8 ± 6.2</td><td>18.5 ± 1.4</td><td>41.8 ± 2.7</td><td>9.3 ± 1.6</td><td>19.4 ± 2.1</td><td>24.2 ± 1.6</td><td>0.0 ± 0.0</td><td>9.1 ± 1.8</td><td>0.27 ± 0.04</td></tr><tr><td>2009au</td><td>5.9 ± 1.4</td><td>34.3 ± 11.1</td><td>12.8 ± 2.7</td><td>8.8 ± 2.8</td><td>11.9 ± 1.7</td><td>17.2 ± 2.5</td><td>6.1 ± 1.8</td><td>7.3 ± 2.3</td><td>7.9 ± 0.8</td><td>3.3 ± 0.6</td><td>5.6 ± 1.3</td><td>0.17 ± 0.09</td></tr><tr><td>2009bu</td><td>84.6 ± 5.3</td><td>146.5 ± 23.3</td><td>55.9 ± 3.1</td><td>3.6 ± 1.1</td><td>14.2 ± 1.9</td><td>26.4 ± 1.8</td><td>5.7 ± 2.2</td><td>6.1 ± 2.5</td><td>15.1 ± 1.5</td><td>0.0 ± 0.0</td><td>0.0 ± 0.0</td><td>0.58 ± 0.14</td></tr><tr><td>2009bz</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>2009N</td><td>75.7 ± 3.1</td><td>118.5 ± 20.7</td><td>39.1 ± 3.9</td><td>15.2 ± 1.9</td><td>25.4 ± 1.6</td><td>34.4 ± 2.1</td><td>13.7 ± 1.1</td><td>20.8 ± 2.1</td><td>24.5 ± 1.2</td><td>10.3 ± 1.6</td><td>9.6 ± 1.1</td><td>0.64 ± 0.22</td></tr><tr><td>2009W</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>

Note. Columns: (1) SN name; (2) pEW of Hα absorption component; (3) pEW of Hα emission component; (4) pEW of Hβ; (5) pEW of Fe II λ4924; (6) pEW of Fe II λ5018; (7) pEW of Fe II λ5169; (8) pEW of Fe II/Sc II; (9) pEW of Sc II Multiplet; (10) pEW of Na I D; (11) pEW of Ba II; (12) pEW of Sc II; (13) ratio of absorption to emission (a/e) of Hα P-Cygni profile.
<figure><img src="image_4.png" /><figcaption>**Figure 2.** Correlation matrix of the individual velocity measurements at 50 days. Colors indicate the Pearson correlation coefficient $\rho$. The diagonal middle line shows the name of the parameter: $H_\alpha$ from FWHM and from the minimum absorption flux, $H_\beta$, Fe II $\lambda$4924, Fe II $\lambda$5018, Fe II $\lambda$5169, Sc II/Fe II $\lambda$5531, Sc II M $\lambda$5663, Na I D, Ba II $\lambda$6142, Sc II $\lambda$6247, and O I $\lambda$7774 velocities.</figcaption></figure>

formed in the outer shell of the ejecta and its optical depth is much larger than the Fe II lines, which are forming near to the photosphere.

Figure 3 shows the correlation matrix of the pEW measurements at 50 days. Searching for correlations of pEWs with each other, we find that Sc II/Fe II $\lambda$5531 seems to be the dominant parameter to correlate with all the other pEWs (on average 0.404), while the pEW of the $H_\alpha$ absorption component shows very weak correlations with other pEWs. The strongest correlations are displayed by the iron-group lines with each other. We can see moderate correlations between the pEW of O I $\lambda$7774 and $H_\beta$. In the case of *a/e*, we find a moderate correlation only with Fe II $\lambda$4924 ($\rho = 0.43$) and anticorrelation with pEW of $H_\alpha$ emission ($\rho = -0.43$). While $H_\beta$ shows a weak correlation with the $H_\alpha$ absorption component ($\rho = 0.3$), the correlation with the $H_\alpha$ emission component is strong, with a $\rho = 0.78$. The lack of correlation between $H_\alpha$ and $H_\beta$ absorption features could be due to (a) blending effects of Fe II, Sc II, and Ba II lines with $H_\beta$, and/or (b) the effects of Cachito (Paper I) on the profile of $H_\alpha$.

Figures 4–6, show the relations between the $H_\alpha$, Fe II $\lambda$5169, and Na I D velocities and the pEWs for the 11 features explained above at 50 days. Checking these correlations, we see that velocities correlate positively with Balmer and Na I D lines, but negatively with Fe II lines. For $H_\alpha$, we present the pEW of the absorption and emission component in the first two panels, respectively. In the three figures are shown five objects with the lowest velocities and smallest pEW values. Three of these SNe show signs of interaction (narrow emission lines) at early times (SN 2008bm, 2009au, and 2009bu, these SNe also display abnormally low velocities for their brightness). The other two SNe are SN 2008br and SN 2002gd. In those panels plotting pEWs of Fe II $\lambda$4924, Sc II/Fe II $\lambda$5531, Sc II $\lambda$5663, Ba II $\lambda$6142, and Sc II $\lambda$6247, one can see that there are many SNe with pEW = 0. In these spectra, we do not detect these lines.

<figure><img src="image_5.png" /><figcaption>**Figure 3.** Correlation matrix of the individual pEW measurements at 50 days. Colors indicate the Pearson correlation coefficient $\rho$. The diagonal middle line shows the name of the parameter: pEW($H_\alpha$) of absorption component, pEW($H_\alpha$) of emission component, pEW($H_\beta$), pEW(Fe II $\lambda$4924), pEW(Fe II $\lambda$5018), pEW(Fe II $\lambda$5169), pEW(Sc II/Fe II $\lambda$5531), pEW(Sc II M $\lambda$5663), pEW(Na I D), pEW(Ba II $\lambda$6142), pEW(Sc II $\lambda$6247), pEW(O I $\lambda$7774), and *a/e*.</figcaption></figure>

In Figure 4, we can see that the $H_\alpha$ velocities do not show correlations with pEW($H_\alpha$) of the absorption component, pEW(Fe II $\lambda$5169), pEW(Sc II/Fe II $\lambda$5531), pEW(Sc II multiplet), pEW(Na I D), pEW(Ba II $\lambda$6142), and pEW(Sc II $\lambda$6247). The strongest correlations are shown with pEW($H_\alpha$) of the emission component, $H_\beta$, and anticorrelations with Fe II $\lambda$4924 and Fe II $\lambda$5018. Figures 5 and 6 show that Fe II $\lambda$5169 and Na I D velocities present more scatter in their relations than those shown by $H_\alpha$ velocities.

The expansion velocities with $\Delta v(H_\beta)$ show anticorrelations, which are stronger at late epochs (between 50 and 80 days) than at early phases (15 to 30 days, 15 to 50 days, and 30 to 50 days). Meanwhile, $\Delta vel(H_\alpha-Fe II \lambda5018)$ and $\Delta vel(Na I D-Fe II \lambda5018)$ show correlations with the expansion velocities at 50 days (see Figure 7).

## 5.2. Spectroscopic and Photometric Properties

We now present a comparison of spectroscopic and photometric properties of SNe II. While we have defined and measured 31 spectroscopic and 13 photometric parameters, here we choose a smaller number of parameters to focus on and search for correlations between them. Thus, we employ 14 spectral and 11 photometric parameters: $v(H_\alpha)$ obtained from the FWHM of the emission component, $v(H_\beta)$, $v(Fe II 5018)$, $v(Fe II 5169)$, $v(Na I D)$, pEW($H_\alpha(\text{abs})$), pEW($H_\alpha(\text{emis})$), pEW($H_\beta$), pEW(Fe II 5018), pEW(Fe II 5169), pEW(Na I D), *a/e*, $\Delta v(H_\beta)$ in a range of $50 \le t \le 80$ d, $\Delta vel(H_\alpha-Fe II 5018)$, $\Delta vel(Na I D-Fe II 5018)$, OPTd, Pd, Cd, $M_{\text{max}}$, $M_{\text{end}}$, $M_{\text{tail}}$, $s_1$, $s_2$, $s_3$, $\Delta(B-V)$ in a range of $10 \le t \le 30$ d, and the $^{56}$Ni mass.

Figure 7 shows the correlation matrix of the spectroscopic parameters (obtained at 50 days from explosion) and photometric properties. Although photometric correlations have been shown in previous works (e.g., A14, Valenti et al. 2016), the incorporation of numerous spectral parameters can aid in furthering our understanding of the link between observed parameters and underlying SN II physics. As in the previous
<figure><img src="image_6.png" /><figcaption>H<sub>α</sub> Velocity from the FWHM of the emission component [km s<sup>-1</sup>]

Figure 4. Relations between H<sub>α</sub> velocities and the pEWs of H<sub>α</sub> of absorption and emission component, H<sub>β</sub>, Fe II λ4924, Fe II λ5018, Fe II λ5169, Sc II/Fe II λ5531, Sc II multiplet, Na I D, Ba II λ6142, Sc II λ6247, and O I λ7774. On the top left of each panel, the spectral feature name is displayed, together with the Pearson correlation value.</figcaption></figure>

matrix of correlation, darkest colors indicate higher correlation and white colors, no correlation.

Focusing on the photometric correlations, one can see that many of these are stronger than in A14. As discussed previously, this is because some parameters have been remeasured with new techniques (L. Galbany et al. 2017, in preparation). Interestingly, the number of SNe II with measured values of both *Pd* and *s*<sub>3</sub> show an increase from 4 in A14 to 8 in this work. As explained above, both parameters can give us an idea of the of hydrogen envelope mass at the moment of explosion, thus some relation is expected. Figure 8 shows an evident trend between both parameters, with a correlation coefficient of ρ = -0.857 (although we note the low number of SNe). SNe II with smaller *Pd* have higher *s*<sub>3</sub> decline rates, providing further evidence of a dominant role in defining light-curve morphology of the hydrogen envelope mass, while also providing further support for the use of *Pd* and *s*<sub>3</sub> as envelope mass indicators (given their relatively strong correlation).

From Figure 7, we can also see that *Pd* has a moderate correlation with velocities. Although we find a strong correlation between *Pd* and <sup>56</sup>Ni mass, in agreement to the theoretical predictions (e.g., Kasen & Woosley 2009), we are not in a position to support this result because the correlation is produced only with three points. However, when we include the lower limits for the <sup>56</sup>Ni mass, the correlation disappears (see the top panel in Figure 9). In general, the correlations

between the <sup>56</sup>Ni mass and all other parameters decrease when we use the lower limits. In the bottom panel of the same plot (Figure 9), it is possible to see how the scatter increases using these values. The correlation goes from ρ = -0.82 to ρ = -0.60. The fact that correlations become weaker when using lower <sup>56</sup>Ni mass limits suggests that one should be careful analyzing such masses when insufficient data are available for their estimation.

Continuing the analysis of *Pd*, we can see that it has a moderate correlation with pEW(H<sub>α</sub>) of the absorption component and strong correlation with *a/e*. The correlation coefficients are ρ = 0.45 and ρ = 0.61, respectively. In Figure 10, we present these correlations together with the best-fit line obtained using the `linmix_err`<sup>13</sup> package (Kelly 2007) and the variance with respect to the fit line. The trend shows that SNe with shorter *Pd* values are brighter, have faster declining light curves, lower pEW(H<sub>α</sub>) of the absorption component and *a/e* values, and higher velocities; however, the scatter is large. In many cases, this scatter is significantly larger than the that which could be ascribed to the errors on individual data points. This suggests that this scatter is due to differing underlying physics driving diversity in different parameters plotted on each axis. For example, while we argue here that *Pd* is a good indicator of the hydrogen envelope mass, theory also

<footnote n="13"><sup>13</sup> A Bayesian approach to linear regression with errors in both *X* and *Y*.</footnote>
<figure><img src="image_7.png" /><figcaption>Figure 5. Same as Figure 4 but for Fe II 5169 velocities.</figcaption></figure>

predicts this parameter to be influenced by the $^{56}$Ni mass (Kasen & Woosley 2009). Meanwhile, SN luminosities and velocities will be affected by both explosion energy and the ejecta/envelope mass. Interaction of the SN ejecta with CSM material at early times (e.g., Dessart et al. 2017; Moriya et al. 2017; Morozova et al. 2017) may also play a role in producing dispersion in our presented trends.

The fact that we see a significant anticorrelation between *Pd* and *s*₂ is in line with historical understanding of the nature of fast declining SNe II. If *Pd* is an indicator of the extent of the hydrogen envelope, then it follows that faster declining SNe II have a smaller hydrogen envelope at the epoch of explosion, consistent with previous theoretical predictions (e.g Litvinova & Nadezhin 1983; Bartunov & Blinnikov 1992; Popov 1993; Moriya et al. 2016).

In Figure 11, we test the correlation found by Hamuy & Pinto (2002) between the magnitude and the photospheric expansion velocity. Unlike Hamuy & Pinto (2002), who only used SNe IIP and the $M_V$ in the middle of the plateau, we use all our SN II sample (no distinction between SNe IIP and SNe IIL) and the magnitude at different phases: at maximum ($M_{max}$), at the end of the plateau ($M_{end}$), and at the radioactive tail phase ($M_{tail}$). We can see that brighter events (in all phases) display higher expansion velocities, confirming the result of Hamuy & Pinto (2002). The correlations between Fe II λ5169 velocity (a proxy of the photospheric velocity) at 50 days and luminosity during the optically thick phase are moderate

($\rho$ = -0.54 with $M_{max}$ and $\rho$ = -0.45 with $M_{end}$), and strong ($\rho$ = -0.62) in the radioactive tail phase. However, we again note the outliers in these figures, where the correlation appears much stronger when removing these events (the outliers are mainly the same SNe discussed previously that show abnormal spectral properties). Interestingly, correlations are higher between spectral velocities and $M_{max}$ than with $M_{end}$ (the Standardized Candle Method, SCM, is generally applied using a magnitude during the plateau, more similar to $M_{end}$). Analyzing the variance along the best-fit line, we find that the dispersion in velocity is larger in brighter SNe. Although the magnitudes and the expansion velocities are both directly related with the explosion energy, this scatter could suggest an extra influence by an external parameter. In the three main outliers in this plot, we observe signs of weak interaction at early times (see spectra presented in Paper I). In these three obvious cases, but also in other more “normal” SNe II, interaction could play a role in influencing both the magnitudes and velocities observed. CSM interaction is likely to produce more dispersion within brighter SNe II as it will generally increase the early-time luminosity while possibly decreasing velocities, hence pushing SNe II away from the classic magnitude-velocity relation. In addition, the unaccounted for effects of host galaxy reddening will produce additional dispersion.

The expansion velocities show a strong correlation with $^{56}$Ni mass (see Figure 12). This suggests that more energetic
<figure><img src="image_8.png" /><figcaption>**Figure 6.** Same as Figure 4 but for Na I D velocities.</figcaption></figure>

explosions produce more $^{56}$Ni. Additionally, the luminosities have a very strong correlation with the $^{56}$Ni mass, which supports the results obtained by Hamuy (2003), Pejcha & Prieto (2015a, 2015b), and more recently by Müller et al. (2017). It is possible to see that these three parameters (luminosities, velocities, and $^{56}$Ni mass) are related and they can be explained through a correlation of both parameters with explosion energy: more energetic explosions produce brighter SNe with faster velocities (as shown in the models of Dessart et al. 2010a). For those correlations that we do not plot, the reader can see the strength of correlation in Figure 7.

Figure 13 presents correlations between $M_{max}$ and the pEWs of H$\alpha$, Fe II 5018, and Na I D. We observe a weak correlation with the pEW(H$\alpha$) absorption component, a moderate ($\rho$ = 0.54) correlation with pEW(Fe II 5018), and no correlations with pEW(Na I D).

In Figure 14, we repeat the correlations presented by A14, which show that a faster declining SN at one epoch is generally also a fast decliner at other epochs. Although the correlation of $s_3$ and $M_{max}$ is moderate, it is driven by an outlier event, SN 2006Y. As A14 noted, this SN presents an atypical behavior in photometry, but here we confirm its strange behavior in the spectra. If we remove this SN from the analysis, the correlations decrease significantly. The correlations between $s_3$ and the velocities are moderate. In the last panel of Figure 14, the correlation between $s_3$ and the pEW(Fe II 5018) is presented, which, like $M_{max}$ is driven by SN 2006Y. Summarizing, $s_3$ has weak correlations with the pEWs and the magnitudes.

## 6. Discussion

Using numerous defined spectral and photometric parameters, we have searched for correlations between different observed properties of SNe II. We argue that Pd is a better parameter than OPTd for constraining the pre-SN hydrogen envelope mass. Our analysis shows a strong correlation between Pd and $s_3$, arguing that both of these parameters are strongly linked to the hydrogen envelope mass/ejecta mass. While expansion velocities and SN II magnitudes display a significant degree of correlation, they show only weak/ moderate correlations with Pd and $s_3$, suggesting that explosion energy—observed through diversity in velocities and luminosity—and hydrogen envelope mass vary somewhat independently between SNe II.

We now qualitatively compare our results with those found in previous studies, both observational and theoretical, attempting to tie these correlations to the underlying physics of SNe II.

### 6.1. The Influence of Explosion Energy

Hamuy & Pinto (2002) found that the luminosity of the SNe IIP correlates with the photospheric velocity (Fe II velocity) at 50 days from explosion. Brighter SNe II have higher ejecta expansion velocities. This correlation has enabled the use of SNe II as distance indicators. In Figure 11, we show the same relation, but in generalized form; velocities correlate with SN II brightness at all epochs. In addition, we show that this luminosity–velocity correlation is stronger at peak
<figure><img src="image_9.png" /><figcaption>**Figure 7.** Correlation matrix of the individual spectral and photometric parameters at 50 days. Colors indicate the Pearson correlation coefficient $\rho$. In the diagonal line is shown *Pd*: plateau duration; *OPTd*: optically thick duration; *Cd*: cooling duration; $M_{\text{max}}$: magnitude at maximum; $M_{\text{end}}$: magnitude at the end of the plateau; $M_{\text{tail}}$: magnitude in the radioactive tail phase; $s_1$: initial decline; $s_2$: plateau decline; $s_3$: radioactive tail decline; $^{56}\text{Ni}$ mass: nickel mass; $\Delta(B-V)_{10,30}$: color gradient between 10 and 30 days from explosion; $v(H_\alpha)$: H$\alpha$ velocity obtained from the FWHM of the emission component; $v(H_\beta)$: H$\beta$ velocity; $v(\text{FeII5})$: Fe II 5018 velocity; $v(\text{FeII6})$: Fe II 5169 velocity; $v(\text{Na})$: Na I D velocity, pEW(H$\alpha$)$_a$: pEW of H$\alpha$ absorption component; pEW(H$\alpha$)$_e$: pEW of the H$\alpha$ emission component, pEW(H$\beta$)$_e$: pEW of H$\beta$, pEW(FeII5): pEW of Fe II 5018, pEW(FeII6): pEW of Fe II 5169; pEW(Na): pEW of Na I D, *a/e*: ratio of absorption to emission component of H$\alpha$ P-Cygni profile; $\Delta\text{vel}(H_\alpha\text{FeII5})$: $\Delta\text{vel}(H_\alpha-\text{Fe II 5018})$, $\Delta\text{vel}(\text{NaFeII5})$: $\Delta\text{vel}(\text{Na I D}-\text{Fe II 5018})$; and $\Delta v(H_\beta)_{50,80}$: $\Delta v(H_\beta)$ in a range of [+50, +80] days.</figcaption></figure>

brightness ($M_{\text{max}}$) than during the plateau. Dessart et al. (2013a) has shown that more energetic explosions produce more $^{56}\text{Ni}$ mass, brighter SNe II with faster expanding velocities. This is consistent with our results, and suggests that explosion energy is indeed a primary parameter that influences SN II diversity, and that is traced through SN II brightness, velocities and $^{56}\text{Ni}$ mass.

## 6.2. The Influence of Hydrogen Envelope Mass

According to theoretical models, faster declining SNe II can be explained by the explosion of stars with low hydrogen envelope mass (e.g., Litvinova & Nadezhin 1983; Bartunov & Blinnikov 1992; Popov 1993 and Moriya et al. 2016). As discussed previously, differences in envelope mass are likely to

directly affect the length of the plateau, *Pd* (we again stress the difference between this parameter and *OPTd*, with the latter traditionally being assumed to be related to the envelope mass). This is because the plateau, *Pd*, is powered by the recombination of hydrogen in the expanding ejecta, and the lower the hydrogen envelope mass the quicker the recombination wave reaches its inner edge. The fact that *Pd* also correlates with $s_3$ (Figure 8) further supports this view, given that higher $s_3$ can be interpreted as being due to a lower ejecta mass (A14) that can trap the radioactive emission (which is powering the light curve at these late epochs). With respect to faster declining SNe II, we observe a significant trend in that SNe II with higher $s_2$ having smaller *Pd* values, implying that the former is indeed related to the hydrogen envelope mass as has been
<figure><img src="image_10.png" /><figcaption>**Figure 8.** Correlation between *Pd* vs. *s*<sub>3</sub>. On the top of the figure, *n* = number of events, *ρ* = Pearsons correlation coefficient, and *P* = probability of detecting a correlation by chance. The dashed horizontal line shows the expected decline rate on the radioactive tail, assuming full trapping of gamma-rays from <sup>56</sup>Co to <sup>56</sup>Fe decay.</figcaption></figure>

<figure><img src="image_11.png" /><figcaption>**Figure 9.** Top: correlations between *Pd* and the <sup>56</sup>Ni mass with the accurate values (left) and including the lower limits (right). Bottom: correlations between *M*<sub>max</sub> and the <sup>56</sup>Ni mass with the accurate values (left) and including the lower limits (right). The accurate values for <sup>56</sup>Ni mass are displayed in red. On the top of each figure, *n* = number of events, *ρ* = Pearsons correlation coefficient, and *P* = probability of detecting a correlation by chance. Histograms along the x- and y-axes show the distributions of the various parameters plotted on each axis. Each histogram displays the *ρ*<sub>val</sub> found using the Shapiro-Wilk normalization. When the *ρ*<sub>val</sub> > 0.05, the data set comes from a population that has a normal distribution.</figcaption></figure>

predicted and discussed for many years. Recent observational
works (e.g., A14, Valenti et al. 2016) suggested that the phase
between the explosion date and the end of the plateau

(historically known as the plateau duration, but here named
*OPTd*) is the key parameter constraining the envelope mass.
However, *Pd* shows higher degrees of correlation with other
parameters, in particular, *s*₂ and *s*₃. This suggests that *Pd* is
indeed a better tracer of envelope mass than *OPTd*. In addition,
we find that *a/e* shows strong and moderate correlation with *Pd*
and *s*₃, respectively, suggesting that this spectral parameter is
also a useful tracer of envelope mass (as already argued in
Gutiérrez et al. 2014).

From the the correlation matrix (Figure 7), we can observe
stronger relations between *Pd* and *s*<sub>2</sub>, as well as with the
expansion velocity, than between *OPTd* and the same
parameters. This is because all these parameters are measured
during the recombination phase, where they have similar
physical conditions. On the other hand, *OPTd* conveys
information on the physical parameters that dominate the early
phases of the light curve, plus the hydrogen envelope
recombination. Consequently, the correlations are weaker.

In Figure 7, we can see that <sup>56</sup>Ni mass shows a strong
correlation with *Pd*, while with *OPTd* it displays an antic-
orrelation. Analyzing these findings (Figure 15), we can see
that the relation between <sup>56</sup>Ni mass and the *Pd* is produced by
only three measurements, and therefore the probability of this
correlation being real is very small (*P* = 0.33). In the case of
the *OPTd*–<sup>56</sup>Ni mass plot, this anticorrelation is driven by a
number of outliers.

From Figure 7, we also see that *OPTd* has stronger
correlations with *Cd*, *s*₁, and *M*<sub>tail</sub> than with *Pd*. The strong
relation between *OPTd* and *Cd* is expected because the former,
by definition, includes the latter one (the same applies to *OPTd*
and *Pd*; see the *OPTd* definition in Figure 1). However, *Pd* and
*Cd* are not related, because they are most likely associated with
different physical properties of SNe II. Between *OPTd* and *s*₁
the correlation is moderate, but again, it is driven by the
physical parameters that dominate the early phases of the light
curve, which, by definition, are included in *OPTd*. One
interesting correlation is displayed between *OPTd* and *M*<sub>tail):
SNe II with larger *OPTd* values are fainter in the radioactive
tail phase. This relation may be understood given that the epoch
of the *M*<sub>tail</sub> measurement directly arises from the length of
*OPTd*. This means that, if the optically thick phase takes more
time, the *M*<sub>tail</sub> will be measured later, which in turn, implies
fainter magnitudes (for the same <sup>56</sup>Ni mass that is powering the
late-time LC). This suggests that, the correlation between
*OPTd* and *M*<sub>tail</sub> is essentially based on the total duration of the
optically thick phase, i.e., the photospheric phase.

In summary, we observe three key SN II parameters that we
believe are strongly related to the extent of the hydrogen
envelope mass at the moment of explosion: *Pd*, *s*<sub>3</sub>, and *a/e*.

6.3. *The Influence of Explosion Energy on the Strength of Spectral Lines*

Figures 4–6 display some interesting trends. While the
strength of each correlation is complicated by the obvious
outliers together with those SNe where no spectral line
detection was made, in general, it seems that expansion
velocities correlate positively with the strength of the Balmer
lines and NaI D, and negatively with the strength of metal
lines. The strength of metal lines at any given epoch is most
strongly related to the temperature of the line forming region.
We therefore conclude that more energetic explosions produce
SNe II that stay at higher temperatures for longer leading to
<figure><img src="image_12.png" /><figcaption>**Figure 10.** Correlations between *Pd* and six different parameters: $M_{max}$, $s_2$, $^{56}$Ni mass, $H_\alpha$ velocity, pEW of $H_\alpha$ absorption component, *a/e*. On the top of the figure, *n* = number of events, $\rho$ = Pearsons correlation coefficient, and *P* = probability of detecting a correlation by chance. In addition, each plot shows the corresponding best fit (linmix_err; Kelly 2007) as a solid orange line, while the orange shaded area indicates the variance with respect to the fit line. Histograms along the x- and y-axes show the distributions of the various parameters plotted on each axis. Each histogram displays the $\rho_{val}$ found using the Shapiro-Wilk normalization. When the $\rho_{val} > 0.05$, the data set comes from a population that has a normal distribution.</figcaption></figure>

lower metal-line pEWs. With respect to the Balmer lines (at least the emission component of $H_\alpha$ and the absorption component of $H_\beta$) this would then imply that more energetic explosions lead to relatively stronger line strengths. The exact physical interpretation of this is unclear. Brighter, i.e., more energetic SNe II also display weaker metal lines (Figure 7 and specifically Figure 13 bottom middle panel). Finally, we also note that differences in progenitor metallicity will also affect the strength of metal lines within spectra, as argued by Dessart et al. (2014) and Anderson et al. (2016; but probably to a lower degree, at least in the current sample).

## 6.4. $H_\alpha$ P-Cygni Diversity

A large diversity in the $H_\alpha$ P-Cygni profile had been shown by Patat et al. (1994) and Gutiérrez et al. (2014). They found that SNe II with smaller *a/e* values are brighter, and have higher velocities and steeper decline rates. With our analysis at 50 days, we confirm these results; however, the correlations

presented here are of lower strength than those in Gutiérrez et al. (2014). This is most likely due to the epoch of the measurements, where in Gutiérrez et al. (2014) measurements were made at $t_{tran}+10$ (where $t_{tran}$ is the transitional epoch between $s_1$ and $s_2$). Here we chose to use epochs with respect to explosion to measure our spectral parameters. This enables us to analyze the full range of events within our sample (in many SNe II, it is not possible to define $t_{tran}$). The difference in correlation strength therefore arises from the measurements in Gutiérrez et al. (2014) being made when SNe II are likely to be under more consistent physical conditions. Here, using an epoch of 50 days post-explosion different SNe are at different phases of their evolution.

It has previously been argued that the $H_\alpha$ P-Cygni diversity is directly related to the hydrogen envelope mass (Schlegel 1996; Gutiérrez et al. 2014). The results we present here also support this view, with the absorption component of $H_\alpha$— and in particular the absorption in relation to the emission, *a/e*—showing correlation with both *Pd* and $s_3$, parameters that we
<figure><img src="image_13.png" /><figcaption>**Figure 11.** Correlations between (Fe II λ5169) velocity and the magnitudes: $M_{max}$, $M_{end}$, and $M_{tail}$. In the top left of each plot the following values are given: *n* = number of events, *ρ* = Pearsons correlation coefficient, and *P* = probability of detecting a correlation by chance. In addition, each plot shows the corresponding best fit (linmix_err; Kelly 2007) as a solid orange line, while the orange shaded area indicates the variance with respect to the fit line. Histograms along the x- and y-axes show the distributions of the various parameters plotted on each axis. Each histogram displays the $\rho_{val}$ found using the Shapiro-Wilk normalization. When the $\rho_{val} > 0.05$, the data set comes from a population that has a normal distribution.</figcaption></figure>

<figure><img src="image_14.png" /><figcaption>**Figure 12.** Correlations between $^{56}$Ni and the expansion velocities. On the top of the figure, *n* = number of events, *ρ* = Pearsons correlation coefficient, and *P* = probability of detecting a correlation by chance. In addition, each plot shows the corresponding best fit (linmix_err; Kelly 2007) as a solid orange line, while the orange shaded area indicates the variance with respect to the fit line. Histograms along the x- and y-axes show the distributions of the various parameters plotted on each axis. Each histogram displays the $\rho_{val}$ found using the Shapiro-Wilk normalization. When the $\rho_{val} > 0.05$, the data set comes from a population that has a normal distribution.</figcaption></figure>

have already argued are direct tracers of the envelope mass. We also note, however, that the measurement of $H_\alpha$ absorption is complicated by the detection and diversity of Cachito (Paper I). It is quite possible, therefore, that the vast majority of the underlying diversity of $H_\alpha$ morphology is determined by the hydrogen envelope mass, but complications in the latter's measurement introduce much of the dispersion we see (in, e.g., Figure 10, bottom right).

## 6.5. Other Comparisons

As discussed in Patat et al. (1994), A14 and more recently Valenti et al. (2016), Galbany et al. (2016), and Rubin et al. (2016), we find that faster declining SNe II are brighter events (see Figure 10). In addition, we also find that SNe II with brighter luminosities have greater expansion velocities and produce more $^{56}$Ni. In Figures 12 and 13, we show a few examples of these correlations. Similar results were found by several authors in observational (e.g., Hamuy 2003;

Spiro et al. 2014; Valenti et al. 2016; Müller et al. 2017) and theoretical (e.g., Kasen & Woosley 2009) works.

Theoretical models show that an increase in the $^{56}$Ni mass leads to an increase in the plateau duration (e.g., Kasen & Woosley 2009 and Nakar et al. 2016). We do not find any observational evidence for such a trend. There are only three data points in the correlation between $Pd$ and $^{56}$Ni, therefore strong conclusions are not warranted. If we include lower mass $^{56}$Ni limits, we also see no evidence for correlation. This may suggest that observationally $Pd$ does not depend on the mass of $^{56}$Ni mass. However, given the inclusion of lower mass $^{56}$Ni limits, this warrants caution.

Many authors have found (e.g., Dessart & Hillier 2011) that SN II color evolution could be related with the radius of the progenitor star. Although we include the color gradient ($\Delta(B-V)$) between 10 and 30 days post-explosion in our analysis, we do not find significant correlations associated to this parameter. However, we do note low-level correlation between $\Delta(B-V)$ and the strength of Fe II λ5018 and Fe II λ5169 (Figure 7), in the direction one
<figure><img src="image_15.png" /><figcaption>Figure 13. Top panel: correlations between $M_{\text{max}}$ and the expansion velocities. Bottom panel: correlations between $M_{\text{max}}$ and the pEWs. On the top of the figure, $n$ = number of events, $\rho$ = Pearsons correlation coefficient, and $P$ = probability of detecting a correlation by chance. In addition, each plot shows the corresponding best fit (linmix_err; Kelly 2007) as a solid orange line, while the orange shaded area indicates the variance with respect to the fit line. Histograms along the x- and y-axes show the distributions of the various parameters plotted on each axis. Each histogram displays the $\rho_{\text{val}}$ found using the Shapiro-Wilk normalization. When the $\rho_{\text{val}} > 0.05$, the data set comes from a population that has a normal distribution.</figcaption></figure>

<figure><img src="image_16.png" /><figcaption>Figure 14. Correlations between $s_3$ and five different parameters: $s_1$, $s_2$, $M_{\text{max}}$, $H_\alpha$ velocity, pEW(Fe II $\lambda$ 5018). On the top of the figure, $n$ = number of events, $\rho$ = Pearsons correlation coefficient, and $P$ = probability of detecting a correlation by chance. Histograms along the x- and y-axes show the distributions of the various parameters plotted on each axis. Each histogram displays the $\rho_{\text{val}}$ found using the Shapiro-Wilk normalization. When the $\rho_{\text{val}} > 0.05$, the data set comes from a population that has a normal distribution.</figcaption></figure>

would expect: SNe II that cool more quickly (higher $\Delta(B-V)$) display stronger metal-line pEWs. Cd also does not display significant correlation with other parameters. While above we linked Cd to progenitor radius, as predicted

by, e.g., Dessart et al. (2013a), the direct influence of radius on Cd is complicated by any presence of CSM close to the progenitor and may explain the lack of correlations.
<figure><img src="image_17.png" /><figcaption>**Figure 15.** Correlations between $^{56}$Ni mass and *Pd* (on left) and *OPTd* (on right). On the top of the figure, *n* = number of events, *ρ* = Pearsons correlation coefficient, and *P* = probability of detecting a correlation by chance. Histograms along the *x*- and *y*-axes show the distributions of the various parameters plotted on each axis. Each histogram displays the *ρ*<sub>val</sub> found using the Shapiro–Wilk normalization. When the *ρ*<sub>val</sub> > 0.05, the data set comes from a population that has a normal distribution.</figcaption></figure>

Dessart et al. (2014) showed that differences in metallicity strongly influence in the SN II spectra, more precisely in the strength of the metal lines. Anderson et al. (2016) supported this result showing a correlation between the strength of Fe II λ5018 with the oxygen abundance of host H II regions. They showed that SNe II exploding in lower metallicity regions have lower iron absorption. Looking for relations with the pEW(Fe II λ5018), we find a correlation of 0.48 with the *Pd* and −0.62 with *s*₃. Assuming that the pEW(Fe II λ5018) gives an idea of the metallicity where the SN explode, this correlation would mean that higher metallicity produces SNe with longer plateaus, which is in the opposite direction of the predictions (e.g., Dessart et al. 2013a). However, when we correlate *Pd* with the oxygen abundance determined by Anderson et al. (2016), we do not find any relation. As in Anderson et al. (2016) we therefore conclude that (at least in the current sample), the strength of metal lines is dependent more on temperature than progenitor metallicity.

7. Conclusions

In this work, we have presented an analysis of correlations between a range of spectral and photometric parameters of 123 SNe II, with the purpose of understanding their diversity. To study this diversity, we use the expansion velocities and pseudo-equivalent widths for 11 features in the photospheric phase (from explosion to ~120 days): H<sub>α</sub>, H<sub>β</sub>, Fe II 4924, Fe II λ5018, Fe II λ5169, Sc II/Fe II λ5531, Sc II M, Na I D, Ba II λ6142, Sc II λ6247, and O I λ7774; the ratio absorption to emission (*a*/*e*) of the H<sub>α</sub> P-Cygni profile; the velocity decline rate of H<sub>β</sub> (Δv(H<sub>β</sub>)) and the velocity difference between H<sub>α</sub> and Fe II λ5018, and Na I D and Fe II λ5018 (Δvel). From the light curves, we employed three magnitude measurements at different epochs (M<sub>max</sub>, M<sub>end</sub>, M<sub>tail</sub>); three decline rates (s<sub>1</sub>, s<sub>2</sub>, s<sub>3</sub>); three time durations (OPTd, Pd, Cd); the <sup>56</sup>Ni mass, and the color gradient, Δ(B − V). We searched for correlations at 30, 50, and 80 days, finding that correlations are stronger at 50 days post-explosion. We suggest this happens because at 50 days SNe II are under similar physical conditions: at 30 and 80 days, not all SNe II are in the same stage, some are in the cooling (at early phases) and some are

in the transition to the nebular phase (at the end of the
plateau).

Our main results are summarized as follows.

1. We confirm previous results showing that brighter SNe II have higher expansion velocities. Here we show that this finding is true for all SN II decline rates, and also extends to magnitudes measured at maximum and during the radioactive tail. These results are most easily explained through differences in explosion energy: more energetic explosions produce brighter and higher velocity SNe II. Additionally, we find that more energetic (brighter and faster) events produce more $^{56}$Ni.

2. We highlight our different definition of the plateau duration (*Pd*) in this work as compared with the literature: from the *s*₁-*s*₂ transition to the end of the plateau, and conclude that it is a more robust parameter connected to H-rich envelope mass. Indeed, we find that *Pd* shows much stronger correlations with other parameters than the traditionally used definition (*OPTd* in our nomenclature). We conclude that *Pd*, *s*₃, and *a/e* are most directly affected by the hydrogen envelope mass at explosion epoch.

3. While we have found many different trends and correlations between different spectral and photometric parameters of SNe II, hinting at underlying physical trends driving diversity (explosion energy, hydrogen envelope mass, and $^{56}$Ni mass), we conclude there is no one parameter dominating these trends.

4. As expected, expansion velocities measured for different spectral lines correlate strongly with each other. However, velocities for different lines for individual SNe II are significantly offset, suggesting that they form at different regions at differing distances from the photosphere.

5. Brighter SNe have higher velocities, smaller pEWs, shorter *a/e*, steeper declines, and small *Pd* and *OPTd* values.

C.P.G. and S.G.G. acknowledge support by projects IC120009 “Millennium Institute of Astrophysics (MAS)” and P10-064-F “Millennium Center for Supernova Science” of the Iniciativa Científica Milenio del Ministerio Económico, Fomento y Turismo de Chile. C.P.G. acknowledges support from EU/FP7-ERC grant No. [615929]. M.D.S. is supported by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant and by a research grant (13261) from the VILLUM FONDEN. We gratefully acknowledge support of the CSP by the NSF under grants AST0306969, AST0908886, AST0607438, and AST1008343. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA).

ORCID iDs

Claudia P. Gutiérrez https://orcid.org/0000-0002-7252-4351
Joseph P. Anderson https://orcid.org/0000-0003-0227-3451
Lluis Galbany https://orcid.org/0000-0002-1296-6887
Luc Dessart https://orcid.org/0000-0003-0599-8407
Maximilian D. Stritzinger https://orcid.org/0000-0002-5571-1833

Mark M. Phillips https://orcid.org/0000-0003-2734-0796

Nidia Morrell https://orcid.org/0000-0003-2535-3091

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