# Testing Cosmological Models with Type Ic Super Luminous Supernovae

###### Abstract

The use of type Ic Super Luminous Supernovae (SLSN Ic) to examine the cosmological expansion introduces a new standard ruler with which to test theoretical models. The sample suitable for this kind of work now includes 11 SLSNe Ic, which have thus far been used solely in tests involving CDM. In this paper, we broaden the base of support for this new, important cosmic probe by using these observations to carry out a one-on-one comparison between the and CDM cosmologies. We individually optimize the parameters in each cosmological model by minimizing the statistic. We also carry out Monte Carlo simulations based on these current SLSN Ic measurements to estimate how large the sample would have to be in order to rule out either model at a confidence level. The currently available sample indicates a likelihood of that the Universe is the correct cosmology versus for the standard model. These results are suggestive, though not yet compelling, given the current limited number of SLSNe Ic. We find that if the real cosmology is CDM, a sample of SLSNe Ic would be sufficient to rule out at this level of confidence, while SLSNe Ic would be required to rule out CDM if the real Universe is instead . This difference in required sample size reflects the greater number of free parameters available to fit the data with CDM. If such SLSNe Ic are commonly detected in the future, they could be a powerful tool for constraining the dark-energy equation of state in CDM, and differentiating between this model and the Universe.

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## 1 Introduction

A new type of luminous transient has been identified in recent years through the use of deep, wide surveys searching for supernovae in the local Universe (Quimby et al. 2005, 2007; Quimby 2006; Smith et al. 2007; Drake et al. 2009; Rau et al. 2009; Kaiser et al. 2010; Gal-Yam 2012; Baltay et al. 2013). These super-luminous supernovae (SLSN) have peak magnitudes mag and integrated burst energies erg. They are therefore much brighter than both Type Ia SNe and the majority of core-collapse events. Their unusually high peak luminosities, hot blackbody temperatures and bright rest frame ultra-violet emission (which renders their continuum easily detectable at optical and near-infrared wavelengths at high redshifts; Cooke et al. 2012) allow them to be studied in concert with possible gamma-ray burst associations (Li et al. 2014; Cano & Jakobsson 2014) and, more importantly, make them viable standardizable candles and distance indicators for use as cosmological probes (Inserra & Smartt 2014).

Inserra et al. (2013) and Nicholl et al. (2013) used the classification term SLSN Ic to refer to all the hydrogen poor SNLSe, though there appear to be at least two observational groups in this category. These are distinguished via the terms SN2005ap-like and SN2007bi-like events, since these are the prototypes with the faster and slower evolving lightcurves. SLSNe Ic have now been discovered out to redshifts (Chomiuk et al. 2011; Berger et al. 2012; Cooke et al. 2012; Howell et al. 2013), and appear to be rather homogeneous in their spectroscopic and photometric properties.

The brighter events decline more slowly, not unlike the Phillips relation for Type Ia SNe, which raises the possibility of correlating their peak magnitudes to their decline over a fixed number of days to reduce the scatter (Rust 1974; Pskovskii 1977; Phillips 1993; Hamuy et al. 1996). Without the use of such a relation, the uncorrected raw mean magnitudes show a dispersion of (e.g., Inserra & Smartt 2014). Correlating the peak magnitude to the decline over 30 days reduces the scatter in standardized peak magnitudes to mag. And apparently using a magnitude-color evolution reduces this scatter even more, to a low value somewhere between mag and mag.

It is therefore quite evident that SLSNe Ic may be useful cosmological probes, perhaps even out to redshifts much greater () than those accessible using Type Ia SNe. The currently available sample, however, is still quite small; adequate data to extract correlations between empirical, observable quantities, such as lightcurve shape, color evolution and peak luminosity, are available only for tens of events. Our focus in this paper is specifically to study whether SLSNe Ic can be used—not only to optimize the parameters in CDM (Li et al. 2014; Cano & Jakobsson 2014; Inserra & Smartt 2014), e.g., to refine the dark-energy equation of state but, also—to carry out comparative studies between competing cosmologies, such as CDM versus the Universe (Melia 2007; Melia & Abdelqader 2009; Melia & Shevchuk 2012; Melia 2013a).

Like CDM, the Universe is a Friedmann-Robertson-Walker cosmology that assumes the presence of dark energy, as well as matter and radiation. The principle difference between them is that the latter is also constrained by the equation of state , in terms of the total pressure and energy density . In recent years, this model has generated some discussion concerning its fundamental basis, including claims that it is actually a vacuum solution, even though . However, all criticisms leveled against thus far appear to be based on incorrect assumptions and theoretical errors. A full accounting of this discussion may be found in Melia (2015) and references cited therein.

In fact, the application of model selection tools in one-on-one comparisons between these two cosmologies has shown that the data tend to favor over CDM. Tests completed thus far include high- quasars (Melia 2013b, 2014), gamma ray bursts (Wei et al. 2013), the use of cosmic chronometers (Melia & Maier 2013) and, most recently, the Type Ia SNe themselves (Wei et al. 2014). In all of these tests, information criteria show that , with the important additional constraint on its equation of state, is favored over CDM with a likelihood of versus only .

Here, we broaden the comparison between and CDM by now including SLSNe Ic in this study. In § 2 we briefly describe the currently available sample and our method of analysis. Our results are presented in § 3. We will find that the current catalog of SLSNe Ic suitable for this study already confirms the tendencies discussed above, though the statistics are not yet good enough to strongly differentiate between these two competing models. We show in § 4 how large the source catalog needs to be in order to rule out one or the other expansion scenario at a 3-sigma confidence level, and we present our conclusions in § 5.

## 2 Methodology

Eleven of the SLSNe Ic identified by Inserra & Smartt (2014) are appropriate for this work, and we base our analysis on the methodology described in their paper and in Li et al. (2014). Briefly, the chosen SLSNe Ic must have well sampled light-curves around peak luminosity, and photometric coverage from several days pre-maximum to 30 days (in the rest frame) after the peak. This time delay appears to be optimal for use in the Phillips-like peak magnitude-decline relation (Inserra & Smartt 2014).

All 11 of these events appear to be similar to the well-observed SN2010gx, and these decay rapidly after peak brightness. They belong to the group of 2005ap-like events, the first such SN discovered in this category. Other SLSNe Ic could not be included simply because of lack of sufficient temporal coverage, even though their identification has been securely classified in previous work (see, e.g., Leloudas et al. 2012; Quimby et al 2011; Inserra et al. 2013; Chomiuk et al. 2011; Berger et al. 2012; Nicholl et al. 2014).

SN | Filter | Refs. | ||||||||
---|---|---|---|---|---|---|---|---|---|---|

SN2011ke | 0.143 | 0.01 | 17.70 (g) | 0.05 | -0.18 | 17.830.20 | 2.470.16 | 0.540.17 | 1, 8 | |

SN2012il | 0.175 | 0.02 | 18.00 (g) | 0.09 | -0.18 | 18.090.21 | 2.190.16 | 0.490.17 | 1, 8 | |

PTF11rks | 0.190 | 0.04 | 19.13 (g) | 0.17 | -0.19 | 19.150.20 | 2.620.14 | 0.950.14 | 1, 8 | |

SN2010gx | 0.230 | 0.04 | 18.43 (g) | 0.13 | -0.23 | 18.530.18 | 2.000.19 | 0.340.16 | 2, 8 | |

SN2011kf | 0.245 | 0.02 | 18.60 (g) | 0.09 | -0.13 | 18.640.18 | 1.490.16 | - | 1, 8 | |

LSQ12dlf | 0.255 | 0.01 | 18.78 (V) | 0.03 | -0.27 | 19.020.12 | 1.000.10 | 0.290.12 | 3, 8 | |

PTF09cnd | 0.258 | 0.03 | 18.29 (R) | 0.05 | -0.34 | 18.580.22 | 1.090.14 | - | 4, 8 | |

SN2013dg | 0.265 | 0.01 | 19.06 (g) | 0.03 | -0.30 | 19.330.20 | 2.080.20 | 0.510.17 | 3, 8 | |

PS1-10bzj | 0.650 | 0.01 | 21.23 (r) | 0.02 | -0.58 | 21.790.20 | 1.700.14 | 0.600.15 | 5, 8 | |

PS1-10ky | 0.956 | 0.03 | 21.15 (i) | 0.06 | -0.73 | 21.820.18 | 1.310.15 | 0.300.18 | 6, 8 | |

SCP-06F6 | 1.189 | 0.01 | 21.04 (z) | 0.01 | -1.35 | 22.380.20 | 0.890.15 | - | 7, 8 |

Notes: All values are from Inserra & Smartt (2014), except for , which is calculated here. The error bars are directly from Figures 5 and 6 in Inserra & Smartt (2014). Columns: SN name; measured redshift; extinction; observed peak magnitude (AB system) and filter; Galactic extinction in the observed filter; calculation of the synthetic 400nm magnitude from the observed filter; apparent magnitude mapped into the 400nm passband, and its dispersion; magnitude decrease in 30 restframe days and its dispersion; the color change between the 400nm and 520nm synthetic bands at peak and 30 days later, and its dispersion. References: (1) Inserra et al. (2013); (2) Pastorello et al. (2010); (3) Nicholl et al. (2014); (4) Quimby et al. (2011); (5) Lunnan et al. (2013); (6) Chomiuk et al. (2011); (7) Barbary et al. (2009); (8) Inserra & Smartt (2014).

The SNe listed in Table 1 were located in faint, dwarf galaxies, and were unlikely to have suffered significant extinction beyond the reddening induced by interstellar dust in our Galaxy. We here adopt the reddening corrections from Tables 1 and 2 of Inserra & Smartt (2014), who assumed a standard reddening curve with . We also adopt their -corrections and time dilation effects in order to obtain the absolute rest-frame peak magnitudes. This step is necessary due to the large () redshift coverage of the sample. These are listed in the table, along with the source names, their redshifts, apparent peak magnitudes (and filters), the magnitude decrease over 30 days, and the color change between the 400nm and 520nm synthetic (restframe) bands at peak and 30 days later.

In order to provide consistent, standarized comparative rest frame properties, the observed apparent magnitudes ( in Table 1) have been converted into defined, synthetic magnitudes. Since the SLSN Ic spectrum around 400nm is continuum dominated, Inserra & Smartt (2014) defined a synthetic passband with an effective width of 80nm, centered at wavelength 400nm, having steep wings and a flat top. In Table 1, this is referred to as the 400nm band. All of the chosen events in this table have sufficient photometric coverage to allow the -correction to uniformly map the observed filter’s wavelength range to this 400nm bandpass in the rest frame. The absolute magnitudes are then formally defined by the relation

(1) |

where is the apparent magnitude mapped into the restframe 400nm band, is the distance modulus calculated from the luminosity distance, is the AB magnitude in the observed filter (, , , , , or , as indicated in Table 1), is the Galactic extinction in the observed filter, and is the -correction from the observed filter in Table 1 to the synthetic 400nm bandpass. The values of and are listed in Table 1. Note that is a cosmology-independent apparent magnitude.

The peak magnitude-decline relation for SLSN Ic in the rest frame 400nm band is (Inserra & Smartt 2014)

(2) |

where is the slope, is the decline at 30 days, and is a constant representing the absolute peak magnitude at . Inserra & Smartt (2014) also found that appears to have a strong color dependence. Redder objects are fainter and also become redder faster. This peak magnitude-color evolution relation is given by

(3) |

where is the difference in color between the peak and 30 days later. (Note that and need not be the same in these two expressions.)

With Equations (2) and (3), an effective (standardized) apparent magnitude may be obtained as follows:

(4) |

The term represents an adjustment due to the peak magnitude-decline relation, in terms of , or the peak magnitude-color evolution relation, in terms of , as the case may be. The effective apparent magnitude may also be expressed as (Perlmutter et al. 1997,1999)

(5) |

where is the Hubble constant in units of km and is the luminosity distance in units of Mpc. Here is the “-free” 400nm absolute peak magnitude, represented in terms of the standardizable absolute magnitude , according to the definition

(6) |

(see Li et al. 2014 and references cited therein).

The apparent correlations suggest the use of two “nuisance” parameters ( and ) whose optimization along with the model parameters decreases the overall scatter in the distance modulus. For each model, we therefore find the best fit by minimizing the statistic, defined as follows:

(7) |

In CDM, the luminosity distance depends on several parameters, including and the mass fractions , , and , defined in terms of the current matter (), radiation (), and dark-energy () densities, and the critical density . Assuming zero spatial curvature, so that , the luminosity distance to redshift is given by the expression

(8) |

where is the dark-energy equation of state. The Hubble constant cancels out in Equation (7) when we multiply by , so the essential remaining parameters in flat CDM are and . If we further assume that dark energy is a cosmological constant with , then only the parameter is available to fit the data.

In the Universe (Melia 2007; Melia & Abdelqader 2009; Melia & Shevchuk 2012), the luminosity distance depends only on , but since here too the Hubble constant cancels out in the product , there are actually no free (model) parameters left to fit the SLSN Ic data. In this cosmology,

(9) |

## 3 Results

We have assumed that SLSNe Ic can be used as standardizable candles and applied the decline relation (with 11 objects) and the peak magnitude-color evolution relation (with 8 objects) to compare the standard (CDM) model with the Universe. In this section, we discuss how the fits have been optimized, first for CDM, and then for . The outcome for each model is more fully described and discussed in subsequent sections.

### 3.1 Cdm

In the most basic CDM model, the dark-energy equation of state parameter, , is exactly . The Hubble constant cancels out in Equation (7) when we multiply by , so the essential remaining parameter is . Type Ia SN measurements (see, e.g., Perlmutter et al. 1998, 1999; Riess et al. 1998; Schmidt et al. 1998), CMB anisotropy data (e.g., Hinshaw et al. 2013), and baryon acoustic oscillation (BAO) peak length scale estimates (e.g., Samushia & Ratra 2009), strongly suggest that we live in a spatially flat, dark energy-dominated universe with concordance parameter values and km .

We will therefore first attempt to fit the data with this concordance model, using prior values for all the model parameters, but not the two “nuisance” parameters and . For the decline relation (with 11 objects), the resulting constraints on and are shown in Figure 1(a). For this fit, we obtain , , and a per degree of freedom of , remembering that all of the CDM parameters are assumed to have prior values, except for the “nuisance” parameters and . (The corresponding data and best fit are shown in the top lefthand panel of Figure 4.) For the peak magnitude-color evolution relation (with 8 objects), the resulting constraints on and are shown in Figure 1(b). The best-fit parameters are , . The per degree of freedom for the concordance model with these optimized “nuisance” parameters is (see also the top righthand panel in Figure 4).

If we relax some of the priors, and allow to be a free parameter, we obtain the - constraint contours shown in the top panel of Figure 2 for the decline relation, and the bottom panel for the peak magnitude-color evolution relation. These contours show that at the level, the optimized parameter values are , , and . We find that the per degree of freedom for the optimized flat CDM model is . The bottom panel of Figure 2 shows the - constraints on , , and for the flat CDM model, using the peak magnitude-color evolution relation. The contours show that at the -level, , , but that is poorly constrained; only a lower limit of can be set at this confidence level and the best-fit is 0.59. The per degree of freedom is .

### 3.2 The Universe

The Universe has only one free parameter, , but since the Hubble constant cancels out in the product , there are actually no free (model) parameters left to fit the SLSN Ic data. The results of fitting the decline relation with this cosmology are shown in Figure 3(a). We see here that the best fit corresponds to and . With degrees of freedom, the reduced is . The results of fitting the peak magnitude-color evolution relation with this cosmology are shown in Figure 3(b). We see here that the best fit corresponds to and . With degrees of freedom, the reduced is .

To facilitate a direct comparison between CDM and , we show in Figure 4 the Hubble diagrams for SLSNe Ic. In the left panel of Figure 4, the effective magnitudes of 11 SLSN Ic are plotted as solid points, together with the best-fit theoretical curves (from top to bottom) for the concordance model (with prior values of the parameters, and with and ), for the optimized flat CDM model (with , and with , and ). and for the Universe (with and ). The Hubble diagrams derived using the peak magnitude-color evolution relation are shown in the righthand panels of Figure 4. Here, the effective magnitudes of 8 SLSN Ic are plotted as solid points, together with the best-fit theoretical curves for the concordance model (with prior values of the parameters, and with and ), for the optimized flat CDM model (with , and with , and ), and for the Universe (with and ). Strictly based on their values, the optimized CDM model and the Universe appear to fit the SLSN Ic data comparably well. However, because these models formulate their observables (such as the luminosity distances in Equations 8 and 9) differently, and because they do not have the same number of free parameters, a comparison of the likelihoods for either being closer to the ‘true’ model must be based on model selection tools.

### 3.3 Model Selection Tools

Several information criteria commonly used in cosmology (see, e.g., Melia & Maier 2013, and references cited therein) include the Akaike Information Criterion, , where is the number of free parameters (Akaike 1973; Takeuchi 2000; Liddle 2004, 2007; Tan & Biswas 2012), the Kullback Information Criterion, (Bhansali & Downnham 1977; Cavanaugh 1999, 2004), and the Bayes Information Criterion, , where is the number of data points (Schwarz 1978; Liddle et al. 2006; Liddle 2007). With characterizing model , the unnormalized confidence that this model is true is the Akaike weight . Model has likelihood

(10) |

of being the correct choice in this one-on-one comparison. The difference determines the extent to which is favoured over . For Kullback and Bayes, the likelihoods are defined analogously.

With the optimized fits we have reported in this paper, our analysis of the decline relation (with 11 objects) shows that is favoured over the flat CDM model with a likelihood of versus using AIC, versus using KIC, and versus using BIC. In our one-on-one comparison using the peak magnitude-color evolution relation (with 8 objects), the Universe is preferred over CDM with a likelihood of versus using AIC, versus using KIC, and versus using BIC.

## 4 Monte Carlo Simulations with a Mock Sample

These results are interesting, though the current sample of SLSNe Ic is clearly too small for either model to be ruled out just yet. However, this situation will change with the discovery of new SNe, particularly at redshifts . To anticipate how well the SLSN Ic catalog obeying the peak magnitude-color evolution relation may be used to constrain the dark-energy equation of state in CDM, and to differentiate between this standard model and the Universe, we will here produce mock samples of SLSNe Ic based on the current measurement accuracy. In using the model selection tools, the outcome AIC AIC (and analogously for KIC and BIC) is judged ‘positive’ in the range , ‘strong’ for , and ‘very strong’ for . In this section, we will estimate the sample size required to significantly strengthen the evidence in favour of or CDM, by conservatively seeking an outcome even beyond , i.e., we will see what is required to produce a likelihood versus , corresponding to a confidence level.

We will consider two cases: one in which the background cosmology is assumed to be CDM, and a second in which it is , and we will attempt to estimate the number of SLSNe Ic required in each case to rule out the alternative (presumably incorrect) model at a confidence level. The synthetic SLSNe Ic are each characterized by a set of parameters denoted as (, , ). We generate the synthetic sample using the following procedure:

1. Since a subclass of broad-lined Type Ic SNe are observed to be associated with Gamma-ray bursts (GRBs; Hjorth et al. 2003; Stanek et al. 2003), we simulate the z-distribution of our sample based on the observed z-distribution of GRBs. Shao et al. (2011) found that the z-distribution of GRBs appears to be asymptotic to a parameter-free probability density distribution, . The redshift of our SLSN Ic events is generated randomly from this function. Since they can be discovered out to redshifts (e.g., Chomiuk et al. 2011; Berger et al. 2012; Cooke et al. 2012; Howell et al. 2013), the range of redshifts for our analysis is . We assign the absolute peak magnitude uniformly between -23.0 and -21.0 mag, based on the current SLSN Ic measurements.

2. The synthetic apparent peak magnitude is calculated using the relation , where is the distance modulus at , for a flat CDM cosmology with and km (§ 4.1), or the Universe with km (§ 4.2).

3. With the selected and values, we first infer a from the peak magnitude-color evolution relation in a flat CDM cosmology with and km (§ 4.1), or the Universe with km (§ 4.2). And then we add scatter to this relation by assigning a dispersion to the value; i.e., we randomly map this quantity to the new value assuming a normal distribution with a center at and a dispersion mag. This value of is typical for the current (observed) peak magnitude-color evolution relation, which yields a standard deviation mag for the linear fit (Inserra & Smartt 2014). If mag, this SLSN Ic is included in our sample. Otherwise, it is excluded.

4. We next assign “observational” errors to and . We will assign a dispersion to each event , where is a random number between 0 and 1.

This sequence of steps is repeated for each new SLSN Ic in the sample, until we reach the likelihood criterion discussed above. As with the real 11-SLSN Ic sample, we optimize the model fits by minimizing the function in Equation (7).

### 4.1 Assuming CDM as the Background Cosmology

We have found that a sample of at least 240 SLSNe Ic is required in order to rule out at the confidence level. The optimized parameters corresponding to the best-fit CDM model for these simulated data are displayed in Figure 5. To allow for the greatest flexibility in this fit, we relax the assumption that dark energy is a cosmological constant with , and allow to be a free parameter, along with . Figure 5 shows the 1-D probability distribution for each parameter (, , , ), and 2-D plots of the - confidence regions for two-parameter combinations. The best-fit values for CDM using the simulated sample with 240 SNe in the CDM model are , , , and .

To gauge the impact of these constraints more clearly, we show in Figure 6 the confidence regions (shaded, with red contours) for and using these 240 simulated SLSNe Ic (the same as the bottom left-hand panel of Figure 5), and compare these to the constraint contours for the 580 Union2.1 Type Ia SN data (Suzuki et al. 2012) (represented by the blue contours in Figure 6). It is straightforward to see how effectively the SLSNe Ic could be used as a cosmological tool, because the confidence regions resulting from their analysis are smaller (and narrower for ) than those corresponding to the Type Ia events. The better constraints are mainly due to the fact that SLSNe Ic are distributed over a much wider redshift range, extending towards high-z, where tighter constraints on the model can be achieved.

In Figure 7, we show the corresponding 2-D contours in the plane for the Universe. The best-fit values for the simulated sample are and .

Since the number of data points in the sample is now much greater than one, the most appropriate information criterion to use is the BIC. The logarithmic penalty in this model selection tool strongly suppresses overfitting if is large (the situation we have here, which is deep in the asymptotic regime). With , our analysis of the simulated sample shows that the BIC would favor the CDM model over by an overwhelming likelihood of versus only (i.e., the prescribed confidence limit).

### 4.2 Assuming as the Background Cosmology

In this case, we assume that the background cosmology is the Universe, and seek the minimum sample size to rule out CDM at the confidence level. We have found that a minimum of 480 SLSNe Ic are required to achieve this goal. To allow for the greatest flexibility in the CDM fit, here too we relax the assumption of dark energy as a cosmological constant with , and allow to be a free parameter, along with . In Figure 8, we show the 1-D probability distribution for each parameter (, , , ), and 2-D plots of the - confidence regions for two-parameter combinations. The best-fit values for CDM using this simulated sample with 480 SLSNe Ic are , , , and . Note that the simulated SLSNe Ic give a good constraint on , but a weak constraint on ; only an upper limit of 0.09 can be set at the confidence level.

The corresponding 2-D contours in the plane for the Universe are shown in Figure 9. The best-fit values for the simulated sample are and . These are similar to those in the standard model, but not exactly the same, reaffirming the importance of reducing the data separately for each model being tested. With , our analysis of the simulated sample shows that in this case the BIC would favor over CDM by an overwhelming likelihood of versus only (i.e., the prescribed confidence limit).

## 5 Conclusions

It is quite evident that SLSNe Ic may be useful cosmological probes, perhaps even out to redshifts much greater () than those accessible using Type Ia SNe. The currently available sample, however, is still quite small; adequate data to extract correlations between empirical, observable quantities, such as lightcurve shape, color evolution and peak luminosity, are available only for tens of events. In this paper, we have proposed to use SLSNe Ic for an actual one-on-one comparison between competing cosmological models. This must be done because the results we have presented here already indicate a strong likelihood of being able to discriminate between models such as CDM and . Such comparisons have already been made using, e.g., cosmic chronometers (Melia & Maier 2013), Gamma-ray bursts (Wei et al. 2013), and Type Ia SNe (Wei et al. 2015).

We have individually optimized the parameters in each model by minimizing the statistic. With the optimized fits we have reported above, our analysis of the decline relation (with 11 objects) shows that is favoured over the flat CDM model with a likelihood of versus (depending on the information criterion). In our one-on-one comparison using the peak magnitude-color evolution relation (with 8 objects), the Universe is preferred over CDM with a likelihood of versus .

But though SLSN Ic observations currently tend to favor over CDM, the known sample of such measurements is still too small for us to completely rule out either model. We have therefore considered two synthetic samples with characteristics similar to those of the 8 known SLSN Ic measurements, one based on a CDM background cosmology, the other on . From the analysis of these simulated SLSNe Ic, we have estimated that a sample of about 240 such events are necessary to rule out at a confidence level if the real cosmology is in fact CDM, while a sample of at least 480 SNe would be needed to similarly rule out CDM if the background cosmology were instead . The difference in required sample size results from CDM’s greater flexibility in fitting the data, since it has a larger number of free parameters.

Our simulations have also shown that a moderate sample size of events could reach much tighter constraints on the dark-energy equation of state and on the matter density fraction than are currently available with the 580 Union2.1 Type Ia SNe. If SLSNe Ic can be commonly detected in the future, they have the potential of greatly refining the measurement of cosmological parameters, particularly the dark-energy equation of state .

Assembling samples of this size may be feasible with upcoming surveys.
For example, the planned survey SUDSS (Survey Using Decam for Super-luminous
Supernovae) using the Dark Energy Camera on the CTIO Blanco 4m telescope
Inserra & Smartt (2014), and the Subaru/Hyper Suprime-Cam deep survey
(Tanaka et al. 2012), have a goal of discovery several hundred SLSNe out
to over 3 years by imaging tens of square degrees to a limiting
magnitude every 2 weeks. These numbers are based on an estimated
production in the local universe (Quimby et al. 2013), who reported a rate of
events Gpc yr at a weighted redshift of
. This number is low () compared to that
of Type Ia SNe. McCrum et al. (2015) estimate a Type Ic SN rate
of the overall core-collapse SN rate within , though this number
could be higher at (Cooke et al. 2012) due, perhaps, to a decreasing
metallicity. Moreover, the increase in cosmic star formation rate would
boost the absolute numbers of SLSNe. As far as observations
from the ground are concerned, assembling a sample of several hundred Type Ic
SLSNe over 3 to 5 years therefore looks quite promising, particulary with
the surveying capability of LSST (see, e.g., Lien & Fields 2009), which
should cover the whole sky every 2 nights, down to a limiting magnitude
. The expected rate of discovery of core-collapse SNe with this survey
is expected to be s out to a redshift . Given
that of these are expected to be Type Ic SNe in this
redshift range, one should expect LSST to assemble a SLSN
sample in less than a year. The situation from space is even more
exciting. Detecting Type Ic SLSNe out to redshifts via their
restframe 400nm and 520nm bands is plausible with, e.g., EUCLID
(Laureijs et al. 2011), WFIRST and the James Webb Space Telescope
(specifically the NIRCam).^{1}^{1}1http://www.stsci.edu/jwst/instruments/nircam/

A major problem with this approach right now, however, is that one must rely on the use of a luminosity-limited sample of supernovae, i.e. those selected to be super-luminous with peak magnitudes mag and integrated burst energies erg (Inserra & Smartt 2014), in order to test the luminosity distances. The difficulty is that the luminosity-limited sample may turn out to be different with different background cosmologies, given that their inferred luminosities are themselves dependent on the models. This situation is unlikely to change as the sample grows, so it would be necessary to find a way of identifying these SNe, other than simply through their magnitudes. Fortunately, in the case of versus CDM, even though their luminosity distances are formulated differently, it turns out that the ensuing distance measures derived from these are quite similar all the way out to . As such, Type Ic SLSNe that make the cut for one model and not the other are the exception rather than the rule. In other words, the luminosity-limit applied to the sample examined here does not bias either model very much. But this may not be true in general, and an alternative method of selection is highly desirable.

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