tokens: flux toward the Lyman limit. The consequence of this is that at high redshift (), SLSNe-I have a characteristic red observer-frame color and long-duration light curves. The identification of SLSNe-I at requires information on the UV spectrum and evolution. As highlighted in Section 3.5 , data in this wavelength range are sparse, with only DES16C2nm, Gaia16apd, PS1-11bam, and DES15E2mlf having data that extend to . Figure 9 shows the luminosity and color evolution of SLSNe-I at maximum light inferred from these spectra as a function of redshift. The spectra have been normalized and adjusted to the peak magnitude and color of each event. These spectra are then redshifted between 0 and 4, and integrated through the DECam r and z passbands. Figure 9 shows the evolution in luminosity and color for these spectra, along with other events in the literature. Where required, K -corrections have been determined from the spectrum of Gaia16apd. The single-epoch 5 σ magnitude limits of the DES deep and shallow fields are shown along with those expected for LSST wide-field and deep-drilling fields (Scovacricchi et al. 2016 ; D. Scolnic 2017, private communication). These limits suggest that in a single epoch, DES can detect SLSNe-I that are spectroscopically similar to Gaia16apd and DES16C2nm, to z = 3.2 in z -band observations of its deep fields or z = 3.8 for objects that are spectroscopically similar to DES15E2mlf. For the LSST deep-drilling fields, the maximum redshifts in the z band are 3.5 for the DES16C2nm spectrum and 4.3 when considering the DES15E2mlf spectrum. Figure 9. Observer-frame evolution of SLSNe-I. Upper panel: the apparent r -band evolution of SLSNe-I as a function of redshift. DES16C2nm is shown as a purple star, with literature SLSNe-I in orange and the photometrically confirmed objects of Cooke et al. ( 2012 ) shown as black crosses. Values determined from the maximum-light spectrum of Gaia16apd, normalized to the peak magnitude of Gaia16apd, are shown in blue, with the corresponding DES16C2nm spectrum from VLT in red and DES15E2mlf in green. K -corrections for literature events have been determined using the Gaia16apd spectrum. The magnitude limits for the DES deep and shallow fields and LSST wide-field and deep-drilling fields are also shown. Second panel: as above, only for the z band. Third panel: the J -band evolution of SLSNe-I as a function of redshift. The magnitude limits for the Euclid and WFIRST shallow, medium, and deep surveys are also shown. Lower panel: the r − z color evolution of SLSNe-I as a function of redshift as inferred from the upper two panels. A horizontal line of mag highlights the difference between low () and high () redshift events. This analysis can be extended to the observer-frame NIR, where surveys such as Euclid (with 5 σ limiting magnitude per visit in the deep fields and an irregular cadence of 10 visits to each of the two fields in a 6-month observing window for 5 years; Inserra et al. 2018a )
ner_tags: O O O O O O O O O O O O O O B-TextGarbage O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O B-CelestialObject B-CelestialObject B-CelestialObject O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Instrument B-Wavelength O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O B-Survey O O O O O O O O O O O B-Telescope O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O B-Survey O O O O O O O O B-CelestialObject O B-CelestialObject O B-Formula I-Formula I-Formula O B-Wavelength I-Wavelength O O O O O O B-Formula I-Formula I-Formula O O O O O O O B-CelestialObject O O B-Telescope O O O O O O O B-Wavelength I-Wavelength O O O O B-CelestialObject O O O O O O B-CelestialObject O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O B-CelestialObject O O O O O O B-CelestialObject O O O O O O O B-CelestialObject O O B-Telescope O O O B-CelestialObject O O O O O O O O O O O O B-CelestialObject O O O O O O B-Survey O O O O O B-Telescope O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O B-Telescope O B-Telescope O O O O O O O O O O O B-Wavelength O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O B-TextGarbage O O B-TextGarbage O O O O O O O O O O B-Wavelength O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O