DES16C2nm: A superluminous supernova at z=2.0

Studying the Ultraviolet Spectrum of the First Spectroscopically Confirmed Supernova at redshift two

M. Smith Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK M. Sullivan Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK R. C. Nichol Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK L. Galbany PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA C. B. D’Andrea Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA C. Inserra Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK C. Lidman ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) Australian Astronomical Observatory, North Ryde, NSW 2113, Australia A. Rest Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA M. Schirmer Gemini Observatory, Casilla 603, La Serena, Chile A. V. Filippenko Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA Miller Senior Fellow, Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA W. Zheng Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA S. Bradley Cenko NASA/Goddard Space Flight Center C. R. Angus Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK P. J. Brown Department of Physics and Astronomy,4242 TAMU, College Station, TX 77843, USA George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy T. M. Davis ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) School of Mathematics and Physics, University of Queensland, QLD 4072, Australia D. A. Finley Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA S. González-Gaitán Centro de Modelamiento Matemático, Universidad de Chile, Beauchef 851, Piso 7, Santiago, Chile CENTRA, Instituto Superior Técnico - Universidade de Lisboa, Portugal C. P. Gutiérrez Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK R. Kessler Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA S. Kuhlmann Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA J. Marriner Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA A. Möller ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) The Research School of Astronomy and Astrophysics, Australian National University, ACT 2601, Australia P. E. Nugent Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA S. Prajs Department of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK R. Thomas Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA R. Wolf Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA A. Zenteno Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile T. M. C. Abbott Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile F. B. Abdalla Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown, 6140, South Africa S. Allam Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA J. Annis Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA K. Bechtol LSST, 933 North Cherry Avenue, Tucson, AZ 85721, USA A. Benoit-Lévy CNRS, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France E. Bertin CNRS, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France D. Brooks Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK D. L. Burke Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA A. Carnero Rosell Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil M. Carrasco Kind Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA J. Carretero Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona) Spain F. J. Castander Institute of Space Sciences, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain M. Crocce Institute of Space Sciences, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain C. E. Cunha Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA L. N. da Costa Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil C. Davis Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA S. Desai Department of Physics, IIT Hyderabad, Kandi, Telangana 502285, India H. T. Diehl Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA P. Doel Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK T. F. Eifler Department of Physics, California Institute of Technology, Pasadena, CA 91125, USA Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA B. Flaugher Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA P. Fosalba Institute of Space Sciences, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain J. Frieman Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA J. García-Bellido Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, 28049 Madrid, Spain E. Gaztanaga Institute of Space Sciences, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain D. W. Gerdes Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA D. A. Goldstein Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA D. Gruen Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA R. A. Gruendl Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA J. Gschwend Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil G. Gutierrez Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA K. Honscheid Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA Department of Physics, The Ohio State University, Columbus, OH 43210, USA D. J. James Astronomy Department, University of Washington, Box 351580, Seattle, WA 98195, USA M. W. G. Johnson National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA K. Kuehn Australian Astronomical Observatory, North Ryde, NSW 2113, Australia N. Kuropatkin Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA T. S. Li Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA M. Lima Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, São Paulo, SP, 05314-970, Brazil Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil M. A. G. Maia Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil J. L. Marshall Department of Physics and Astronomy,4242 TAMU, College Station, TX 77843, USA George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy P. Martini Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA F. Menanteau Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA C. J. Miller Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA R. Miquel Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona) Spain R. L. C. Ogando Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil D. Petravick National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA A. A. Plazas Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA A. K. Romer Department of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton, BN1 9QH, UK E. S. Rykoff Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA M. Sako Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA E. Sanchez Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain V. Scarpine Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA R. Schindler SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA M. Schubnell Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA I. Sevilla-Noarbe Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain R. C. Smith Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile M. Soares-Santos Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA F. Sobreira Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, 13083-859, Campinas, SP, Brazil Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil E. Suchyta Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831 M. E. C. Swanson National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA G. Tarle Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA A. R. Walker Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile mat.smith@soton.ac.uk
Abstract

We present observations of DES16C2nm, the first spectroscopically confirmed hydrogen-free superluminous supernova (SLSN-I) at redshift . DES16C2nm was discovered by the Dark Energy Survey (DES) Supernova Program, with follow-up photometric data from the Hubble Space Telescope, Gemini, and the European Southern Observatory Very Large Telescope supplementing the DES data. Spectroscopic observations confirm DES16C2nm to be at , and spectroscopically similar to Gaia16apd (a SLSN-I at ), with a peak absolute magnitude of . The high redshift of DES16C2nm provides a unique opportunity to study the ultraviolet (UV) properties of SLSNe-I. Combining DES16C2nm with ten similar events from the literature, we show that there exists a homogeneous class of SLSNe-I in the UV ( Å), with peak luminosities in the (rest-frame) band, and increasing absorption to shorter wavelengths. There is no evidence that the mean photometric and spectroscopic properties of SLSNe-I differ between low () and high redshift (), but there is clear evidence of diversity in the spectrum at  Å, possibly caused by the variations in temperature between events. No significant correlations are observed between spectral line velocities and photometric luminosity. Using these data, we estimate that SLSNe-I can be discovered to by DES. While SLSNe-I are typically identified from their blue observed colors at low redshift (), we highlight that at these events appear optically red, peaking in the observer-frame -band. Such characteristics are critical to identify these objects with future facilities such as the Large Synoptic Survey Telescope, Euclid, and the Wide-Field Infrared Survey Telescope, which should detect such SLSNe-I to , 3.7, and 6.6, respectively.

supernovae: general, supernovae: individual (DES16C2nm), surveys, distance scale
\collaboration

(The DES Collaboration) \noaffiliation

1 Introduction

Superluminous supernovae (SLSNe) are extremely bright, but rare, supernova-like events, peaking at luminosities in excess of  mag, around a hundred times greater than classical core-collapse events. While at least two classes of SLSNe have been observationally identified (see Gal-Yam, 2012; Quimby et al., 2011; Inserra et al., 2016), the most common are known as SLSNe-I, or SLSNe-Ic, as they are hydrogen poor (Quimby et al., 2011; Inserra et al., 2013) and spectroscopically similar to Type Ic supernovae. The power source of SLSNe-I remains unclear, but it is unlikely to be the radioactive decay of Ni that powers the light curves of normal SNe (see Chatzopoulos et al., 2009; Chomiuk et al., 2011; Inserra et al., 2013; Papadopoulos et al., 2015). Alternative mechanisms could be the spin down of a rapidly-rotating magnetar (e.g., Kasen & Bildsten, 2010; Woosley, 2010; Bersten et al., 2016), a pair-instability SN explosion (e.g., Langer et al., 2007; Kasen et al., 2011; Kozyreva et al., 2017), the interaction of SN ejecta with circumstellar material (e.g., Woosley et al., 2007; Chevalier & Irwin, 2011; Chatzopoulos et al., 2012, 2013), or the fallback of accreted material onto a compact remnant (Dexter & Kasen, 2013).

Beyond the puzzle of their astrophysical nature, SLSNe are ideal probes of the high-redshift universe because of their high luminosity and long-lived (time-dilated) light curves. With the peak of their energy output in the ultraviolet (UV), redshifted into the optical at high redshift, studies (e.g., Cooke et al., 2012; Berger et al., 2012; Howell et al., 2013; Pan et al., 2017) have detected a few SLSN candidates at , and suggest that the SLSN rate at such redshifts is a factor of higher than at low redshifts, possibly tracking the cosmic star-formation rate (Prajs et al., 2017). Therefore, there is significant potential for detecting many more SLSNe to and beyond with forthcoming facilities like the Large Synoptic Survey Telescope (LSST; Scovacricchi et al., 2016), Euclid (Inserra et al., 2017), and the Wide-Field Infrared Survey Telescope (WFIRST; Yan et al., 2017).

High-redshift observations of SLSNe-I can provide additional constraints on the physical processes that drive these events. A typical spectrum of a SLSN-I around maximum light can be well described by a hot, black-body continuum with broad absorption lines produced by C, O, Si, Mg, and Fe with characteristic velocities of to km s (Quimby et al., 2011; Inserra et al., 2013). These lines are especially prominent in the UV spectra of SLSNe-I, with a characteristic turnover at  Å where strong line-blanketing from iron-group elements suppresses the black-body flux. These features provide information on the synthesized material and intrinsic metal abundance of the progenitor star, necessary to constrain the physical processes that govern SLSNe-I.

Yan et al. (2017), using a Hubble Space Telescope (HST) spectrum of Gaia16apd at , showed that SLSNe-I exhibit significantly less line blanketing in the UV than any classical-luminosity SN, and hence are likely metal-poor in the outer ejecta. However, given the scarsity of low-redshift SLSNe-I and difficulties of observing in the observer-frame UV, Gaia16apd and the recently discovered SN 2017egm (Dong et al., 2017; Bose et al., 2017) are the only SLSNe-I in the local Universe () with rest-frame UV spectral information. At , observations at optical wavelengths probe the rest-frame UV, presenting an avenue to determine the diversity of SLSNe-I in the UV, and thus provide constraints on progenitor scenarios.

In this paper we present DES16C2nm, a new SLSN-I discovered by the Dark Energy Survey (DES) Supernova Program (DES-SN; Bernstein et al., 2012). At , DES16C2nm is the highest-redshift spectroscopically confirmed SN (of any type) to date. The two SLSN candidates of Cooke et al. (2012) found in Canada-France-Hawaii Telescope Legacy Survey data were not spectroscopically confirmed in real time, but their redshifts ( and 3.90) were measured from host-galaxy spectra. DES16C2nm also supersedes the highest-redshift spectroscopically confirmed Type Ia supernovae (SNe Ia). For example, Rodney et al. (2012) provide strong evidence for a spectroscopically confirmed SN Ia at (“SN Primo”) detected as part of the HST CANDELS project. Classifications of higher-redshift SNe Ia rely on other information, such as model fits to the photometric light-curve data and/or prior knowledge of the host-galaxy redshift; thus, they do not possess independent spectroscopic confirmations (e.g., Riess et al., 2001; Jones et al., 2013; Rodney et al., 2014, 2016; Rubin et al., 2017).

In Section 2, we provide the observational data used to detect and classify DES16C2nm, while in Section 3 we analyze the UV properties of this SLSN, and compare it to the literature. Section 4 discusses the consequences of this discovery for ongoing and future searches of SLSNe. We summarize our conclusions in Section 5. Throughout, we assume H km s Mpc and a flat CDM cosmology with .

2 Observations

DES16C2nm was discovered at and (J2000) in the first DECam (Flaugher et al., 2015) images of the fourth season (Y4) of DES-SN (Bernstein et al., 2012). It was detected with the difference imaging pipeline (Kessler et al., 2015) in all passbands () taken on 2016 August 22 (all dates herein are UTC) and was not detected in the last DES-SN images taken in the previous season (Y3) on 2016 February 08. DES16C2nm did, however, have a marginal detection at (point source) in -band DECam images taken as part of SUDSS111“Search Using DECam for Superluminous Supernovae” (PI: Sullivan) on 2016 March 9, but was not detected in any other SUDSS image taken at that time. DES16C2nm was first designated a transient on 2016 August 27 and monitored in all passbands () on an average 7 day cadence by DES-SN until the end of January 2017, when it fell below the detection limit of the single-epoch DES-SN images. Further details of the DES-SN observing strategy and spectroscopic follow-up programs can be found in D’Andrea et al. (in prep.). Information on the DES-SN difference-imaging search pipeline and machine-learning algorithms to identify transient objects can be found in Kessler et al. (2015) and Goldstein et al. (2015).

Photometric measurements were made using the pipeline discussed by Papadopoulos et al. (2015) and Smith et al. (2016), which has also been extensively used in the literature (e.g., Firth et al., 2015, and references therein). This pipeline subtracts a deep template image from each individual SN image to remove the host-galaxy light using a point-spread-function (PSF) matching routine. SN photometry is then measured from the difference image using a PSF fitting technique. Figure 1 shows the full light curve of DES16C2nm averaged with a 14-day window for clarity.

The time of maximum light, which varies with wavelength, can be best constrained from our -band data. A third order polynomial fit to the observer-frame fluxes indicates that DES16C2nm reached a peak magnitude in the band of (after correcting for foreground extinction using  mag; Schlegel et al., 1998) on MJD 5763914. DES16C2nm peaked 3321 days earlier at in the band, and 97 days later at in the band. The uncertainties on the time of maximum light are driven by the slow photometric evolution of DES16C2nm. In the band, most of our detections have low signal-to-noise ratio (S/N). Based on the available data, we estimate the -band peak magnitude to be prior to the start of DES Y4 (MJD = 57623.4). The individual photometric measurements are listed in Table 1 and are also available from the WISeREP archive222http://wiserep.weizmann.ac.il/ (Yaron & Gal-Yam, 2012).

Figure 1: The photometric data of DES16C2nm from DES (filled circles), SUDSS band (open circle), Gemini/Flamingoes-2 (stars), HST (black filled circle), VLT/FORS2 and VLT/HAWKI (crosses). The DES data have been averaged with a 14-day window for clarity. 3 upper limits are shown as downward arrows, and the various epochs of spectroscopy are shown as black upward arrows. The best-fit magnetar model evaluated at (Section 3.2) is shown as dashed lines, with the model of Piro (2015) at early times (Section 3.3) plotted as dash-dotted lines. The colors correspond to different passbands. The phases presented are relative to peak luminosity in the observer-frame DES band (MJD = 57639) as highlighted by a black dot-dashed line.

DES16C2nm was prioritized for follow-up spectroscopy based on its slowly evolving light curve (in both brightness and color). The first spectrum was obtained on 2016 October 09 (Galbany et al., 2016, when the object was  mag) at the Magellan-Clay Telescope at the Las Campanas Observatory, using the Low Dispersion Survey Spectrograph (LDSS-3). The spectrum was reduced using standard IRAF routines333Image Reduction and Analysis Facility, distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the U.S. National Science Foundation., and has an effective wavelength coverage of 4500 to  Å (observer frame). This spectrum showed evidence of the Mg ii absorption doublet (2796 Å and 2804 Å rest frame) from the host galaxy at 8387 Å and 8403 Å, but at low S/N.

DES16C2nm was then spectroscopically reobserved at the European Southern Observatory (ESO) Very Large Telescope (VLT) using the X-SHOOTER instrument on 2016 October 24 and 25, as well as the Keck-II telescope using the DEep Imaging Multi-Object Spectrograph (DEIMOS; Faber et al., 2003) instrument on 2016 October 25. These spectra unambiguously confirmed the presence of the Mg ii doublet at 8382 Å and 8402 Å, as well as additional absorption features produced by Fe ii (2344, 2383, 2587, 2600 Å rest frame). These features confirmed the redshift of DES16C2nm as , where the uncertainty is the observed scatter in the redshift estimates obtained from the individual absorption features. Figure 2 shows the observer-frame optical spectral series of DES16C2nm including an additional spectrum taken at the VLT on 2016 November 22, once the high redshift of DES16C2nm was known.

Figure 2: The spectral series of DES16C2nm, with rest-frame phase information (relative to peak luminosity in the observer-frame band (MJD = 57639)). The spectra have been smoothed (to 10 Å, 8 Å, 8 Å, and 12 Å, respectively), adjusted to match the colors from the nearest epoch of photometry, and are offset for clarity. Prominent host-galaxy absorption features are labeled in red.

Figure 3 shows the Keck spectrum of DES16C2nm 15 rest-frame days after maximum light in -band, highlighting the galaxy absorption features used to determine the redshift. For comparison, we also show the spectrum of iPTF13ajg (a SLSN-I at Vreeswijk et al., 2014) at approximately the same phase (9 days after maximum light) in the light curve. The broad absorption features at 2200 Å, 2450 Å, and 2700 Å (rest frame) are common in SLSN-I spectra around maximum light (Quimby et al., 2011; Vreeswijk et al., 2014; Mazzali et al., 2016) and spectroscopically classify DES16C2nm as a SLSN-I at .

To constrain the rest-frame optical properties of DES16C2nm, a near-infrared (NIR) spectrum using WFC3/G141 on HST was obtained on 2016 December 20. Information about all spectra can be found in Table 2. The spectra are also available from WISeREP.

Figure 3: The rest-frame optical spectrum of DES16C2nm obtained at Keck-II on 2016 October 25. Prominent galaxy absorption features due to Mg ii and Fe ii are labeled in red. Also shown is a spectrum of iPTF13ajg (; Vreeswijk et al., 2014) at a similar phase in the light curve. A velocity shift of 3,000 km s has been applied to the iPTF13ajg spectrum as discussed in Section 3.5. Key spectral features from the SN identified by Mazzali et al. (2016) and discussed in Section 3.5 are highlighted with downward arrows.

Once the high redshift of DES16C2nm was established, further follow-up observations, including NIR imaging from HST, Gemini/Flamingos-2, and VLT/HAWK-I and optical imaging from VLT/FORS2 (detailed in Table 3), were obtained. Reductions of the HST, VLT/HAWK-I, and VLT/FORS2 data were performed using the standard pipelines provided by the various observatories, with the Gemini/Flamingos-2 data reduced using the THELI pipeline (Erben et al., 2005; Schirmer, 2013), following standard procedures outlined by Schirmer (2013). Magnitudes were estimated using SEXTRACTOR (Bertin & Arnouts, 1996). These ancillary photometric data are shown in Figure 1.

The host galaxy of DES16C2nm is detected in stacked images from DES Science Verification (SV) that contain no SN light. Using SEXTRACTOR, we measure host-galaxy AB magnitudes (MAG_AUTO) of , , , = , , , and , respectively (after correcting for Galactic extinction). Using the Z-PEG photometric-redshift software (Le Borgne & Rocca-Volmerange, 2002), we estimate the stellar mass of the host galaxy to be and a star-formation rate (SFR) of , assuming a Kroupa (2001) initial mass function and fixing the redshift at . The host galaxy of DES16C2nm is not detected in any existing NIR catalogues, necessary to reliably constrain the continuum flux and metallicity at . Despite this, these host-galaxy properties are consistent with the properties of other, lower-redshift SLSN-I host galaxies as seen in DES (Papadopoulos et al., 2015; Smith et al., 2016; Pan et al., 2017) and in the literature (e.g., Neill et al., 2011; Lunnan et al., 2014; Leloudas et al., 2015; Perley et al., 2016; Angus et al., 2016; Chen et al., 2017).

3 Analysis

The high redshift of DES16C2nm provides an opportunity to study the rest-frame UV properties of SLSNe-I, and, by comparing to literature events, to study their diversity and possible evolution with redshift. We first consider the photometric properties of DES16C2nm compared with other SLSNe-I in the literature. Phases given are relative to peak luminosity in the observer-frame band (MJD = 57639).

3.1 Rest-Frame UV Light Curve

We use a standard -correction procedure to estimate the rest-frame light curve of DES16C2nm. Figure 4 shows the rest-frame wavelength range covered by our data collected on DES16C2nm, compared to the rest-frame () Swift (Gehrels et al., 2004; Roming et al., 2005; Poole et al., 2008; Breeveld et al., 2011) and Johnson (Bessell, 1990) filters. This figure illustrates that the rest-frame ( Å), (2255 Å), (2615 Å), (3605 Å), (4413 Å), and (5512 Å) passbands roughly correspond to the observer-frame , , , , , and passbands (respectively) for DES16C2nm. As our VLT and HST spectra have limited wavelength coverage and do not overlap, we use the spectra of Gaia16apd (Yan et al., 2017) at maximum light for -corrections to the light curve of DES16C2nm. This spectrum is similar to that of DES16C2nm and is the only available spectrum of a SLSN-I that covers the full spectral range probed by the photometry of DES16C2nm (1200 to 8700 Å; Figure 4). To test the validity of this approach, we measure the scatter in the inferred absolute magnitude of DES16C2nm when using the maximum-light spectrum of Gaia16apd compared to the spectra of DES16C2nm, PS1-11bam (Berger et al., 2012), iPTF13ajg (Vreeswijk et al., 2014), SNLS06-D4eu (Howell et al., 2013), SCP06F6 (Barbary et al., 2009), and Gaia16apd (Yan et al., 2017) after maximum light. These are the only literature SLSNe-I with spectra extending below 2000 Åin the rest-frame. We find standard deviations of 0.39 (in the filter), 0.08 (), 0.16 (), 0.15 (), 0.01 (), and 0.14 () mag between the -corrections determined using the spectrum of Gaia16apd at peak and the available literature spectra. No evidence of increased scatter is seen as a function of phase. These -correction uncertainties are added in quadrature to the measured uncertainties of the rest-frame light curve of DES16C2nm and comparison literature events. Early-phase data ( days pre-peak) are -corrected using a black body of  K, as discussed in Section 3.3.

At each epoch in the main light curve, we adjust the spectrum of Gaia16apd so that its synthetic photometry matches the observed photometry of DES16C2nm at and calculate the cross-filter -correction required to determine the rest-frame magnitudes in the filters listed above. We fit a polynomial function to the resulting rest-frame light curves, shown in Figure 5, and determine peak absolute magnitudes of , , and (AB). DES16C2nm is most luminous (in integrated flux) in the rest-frame band, and is one of the brightest SLSNe-I (at peak) discovered so far; only iPTF13ajg (Vreeswijk et al., 2014) is brighter at peak ( mag) using the same methodology. The phase of maximum light is statistically consistent for all three filters. We do not have sufficiently high-quality data around maximum light in the rest-frame and bands to make similar measurements.

Figure 4: The rest-frame wavelength coverage for our observations of DES16C2nm. Our observed , , , , , , and filters are shown as dashed lines but shifted back to the rest frame assuming . The solid lines are the rest-frame Swift , , , and Johnson , , filters. Our VLT and HST spectra of DES16C2nm (at +15 d and +34 d, respectively) are shown in black with the composite spectrum of Gaia16apd (at maximum light) shown in orange. The filter pairs used for the cross-filter -corrections (e.g., the DES band ) are plotted in the same color. The DES band is used to correct to rest-frame owing to the larger dataset around maximum light.
Figure 5: The rest-frame (, , , , , ) light curves of DES16C2nm. Magnitudes are estimated with a standard -correction procedure, using the spectrum of Gaia16apd for the main light curve and a black body of 27,000 K for the early-time data (see Sections 3.1 and 3.3). Uncertainties are determined from the observer-frame light curve and include a filter-dependent -correction uncertainty (see Section 3.1) added in quadrature. 3 upper limits are denoted with arrows. For clarity, the and data points have been offset by and +1 day, respectively. The best-fit magnetar model (Section 3.2) is shown as dashed lines, with the model of Piro (2015) at early times (Section 3.3) plotted as a dash-dotted line.

3.2 Physical Modeling

The light curves of SLSNe-I are well described by the spin-down of a rapidly rotating magnetar (Inserra et al., 2013; Papadopoulos et al., 2015; Smith et al., 2016). We fit this model (as described in Appendix D of Inserra et al., 2013) to the observer-frame fluxes of DES16C2nm around maximum light ( phase days), fitting all filters simultaneously and show the best-fitting magnetar model in Figures 1 and 5. The best-fit model has an initial spin period of  ms, an initial magnetic field strength of  G, and a diffusion timescale of  days assuming an opacity of and an explosion energy of erg. From these parameter values, we infer an ejecta mass of . The best fitting model has , suggesting that while the model is a good match to the light-curve and color evolution of DES16C2nm  it does not capture the full variation, potentially due to the strong UV absorption observed in the spectral series of DES16C2nm (Figure 2). These inferred parameters are consistent with the modeling of other SLSNe-I in the literature, such as SN2011kf (e.g. Nicholl et al., 2017).

3.3 Early-Time Data

DES16C2nm was first observed with a significance of 3.3 in SUDSS -band imaging and 2.7 in -band imaging on 2016 March 9, 61 rest-frame days prior to maximum light. No other 3 detections are found in the previous 2 yr of DES imaging. While this detection is at low significance, it is consistent in phase with the precursor peaks observed in other SLSNe (Smith et al., 2016; Nicholl et al., 2015; Leloudas et al., 2012). In particular, LSQ14bdq (Nicholl et al., 2015) showed a bright and relatively fast precursor peak, 60 rest-frame days prior to the peak of the main SLSN. These precursors have peak temperatures of  K and cool rapidly, with typical timescales of 15 rest-frame days (Smith et al., 2016), and are well modeled as shock cooling from extended material around the progenitor star (Ofek et al., 2010; Piro, 2015).

Considering a black body, the observer-frame and -band fluxes of the precursor detection are best fit by a temperature and radius of  K and  cm, respectively, consistent with values determined from other literature events (Smith et al., 2016; Nicholl et al., 2015) and when all available photometric measurements (, , , and band) are considered. Finally, in Figure 5, we compare the rest-frame luminosity of this epoch with a shock-cooling model from Piro (2015) with parameters consistent with those obtained for the light curve of LSQ14bdq (Smith et al., 2016). For this epoch, -corrections are determined using the best-fitting black body with  K. The precursor epoch has a peak luminosity comparable to the main light curve in ( Å) and is consistent with the Piro (2015) model of shock cooling from extended material (dash-dotted line).

3.4 Comparison to Literature Events

In Figures 6 and 7, we compare the rest-frame UV light curves of DES16C2nm to SLSNe-I in the literature. Figure 6 compares the rest-frame Swift light curve of DES16C2nm to SLSNe-I at low () and high () redshift. All SLSNe-I have been -corrected with the procedure described for DES16C2nm using the observed filter having an effective wavelength closest to 2615 Å (the central wavelength of Swift ). Uncertainties due to our -correction procedure are included for all events.

While the number of low-redshift SLSNe-I is small owing to the low intrinsic rate of these events and the limited volume probed, there is evidence of a homogeneous sample of SLSNe-I with similar peak luminosity distributions and evolution. The UV luminosity (at  Å) of DES16C2nm is consistent with other SLSNe-I in the literature, including Gaia16apd at . The exceptions are PTF11rks, which is known to be underluminous in all filters (Inserra et al., 2013), and SN 2015bn, which has been shown to evolve more slowly (photometrically and spectroscopically) than other events (Nicholl et al., 2016). The remaining objects exhibit a scatter of  mag at peak.

There is some evidence that the light curve of DES16C2nm is broader than other literature events, but this may be caused by uncertainties in the estimate of maximum light (4 rest-frame days; Section 2), as the light curve shows little evolution around maximum light at these wavelengths. Further, with observations preferentially in the rest-frame optical, the time of maximum light for low-redshift SLSNe-I is typically estimated in the rest-frame band. DES16C2nm peaks 147 days after our fiducial estimate of maximum light in -band. At high redshift (), the scatter in the luminosity distribution of the SLSNe-I is larger, but all events have  mag at peak (i.e., a scatter of  mag). This includes the photometrically classified SN2213-1745 (Cooke et al., 2012), which has a host-galaxy spectroscopic redshift of 2.05. No evidence of a difference in the mean peak luminosity of SLSNe-I at high and low redshifts is observed, with and  mag, respectively.

Figure 7 shows the rest-frame Swift color evolution of SLSNe-I at low () and high () redshifts. In this analysis, we follow the procedure described above, obtaining -corrections for and from different observed filters. In all cases, SLSNe-I show little scatter in their rest-frame UV color near maximum light, with a scatter of  mag, and they exhibit little evidence of significant color evolution ( mag) around maximum light ( days). At all redshifts, the majority of SLSNe-I have  mag at maximum light. From this analysis, there is no indication that SLSNe-I at high redshift exhibit different colors, or evolve differently, from those at lower redshifts.

Figure 6: The light curve of DES16C2nm compared to literature events at low (; top panel) and high (; lower panel) redshifts. -corrections have been determined using the spectrum of Gaia16apd around maximum light as discussed in the text. An average of the available light curves is overplotted in black. Data for the literature objects are from various sources (Chomiuk et al., 2011; Berger et al., 2012; Cooke et al., 2012; Inserra et al., 2013; Howell et al., 2013; Vreeswijk et al., 2014; Nicholl et al., 2016; Yan et al., 2017; Pan et al., 2017).
Figure 7: The rest-frame color evolution of DES16C2nm compared to literature events at low (; top panel) and high (; lower panel) redshifts. The color is determined by requiring observations in two distinct filters, as discussed in the text. Data for the literature objects are from various sources (Chomiuk et al., 2011; Berger et al., 2012; Cooke et al., 2012; Inserra et al., 2013; Howell et al., 2013; Nicholl et al., 2016; Yan et al., 2017; Pan et al., 2017).

3.5 Rest-Frame UV Spectral Evolution

We now consider the spectral diversity and evolution of SLSNe-I compared to DES16C2nm. Figure 8 shows a temporal series of UV spectra of DES16C2nm compared to other UV spectral data from the literature. As optical observations at probe the rest-frame UV spectrum, the vast majority of SLSNe-I with available rest-frame UV data around maximum light are at , and in particular . At , only Gaia16apd has rest-frame spectral data below 1800 Å.

At  Å, the vast majority of SLSNe-I exhibit strong absorption features at  Å (identified as a blend of C iii, C ii, and Ti iii by Mazzali et al., 2016), at  Å (identified as C ii, Ti iii, and Si ii), and at  Å (identified as Mg ii and C ii). These features are ubiquitous to all SLSNe-I, with the exception of SNLS-06D4eu and DES15E2mlf, which only exhibit absorption at  Å. These spectra are modeled by Mazzali et al. (2016) to have higher temperatures ( K) than canonical events (such as iPTF13ajg, with  K). At these temperatures, in the Mazzali et al. (2016) model, C ii and Mg ii are ionised to C iii and Mg iii, respectively. The absence of C ii and Mg ii reduces absorption at  Å and  Å, but the presence of C iii preserves the absorption feature at  Å. The higher intrinsic temperature of these SLSNe results in higher expansion velocities, resulting in the observed absorption features being blueshifted relative to other events. With higher intrinsic temperatures, the black bodies for these events peak at bluer wavelengths than for lower-temperature SLSNe, such as iPTF13ajg.

For events where absorption at  Å,  Å, and  Å is seen, there is no evidence of evolution or significant diversity in the strength of these lines around maximum light, consistent with the luminosity distribution determined in Figure 6. The spectra of DES16C2nm are consistent with those of literature SLSNe-I, with some evidence of a lower strength in the  Å absorption feature. However, Figure 8 suggests diversity in the observed velocity distribution of SLSNe-I. Liu et al. (2017) measured the photospheric velocity evolution of SLSNe-I, from the Fe ii 5169 Å feature. They show that SLSNe velocities range from to km s around maximum light, before falling linearly at phases greater than 10 days after peak. This result is consistent with that found by Chomiuk et al. (2011) and Inserra et al. (2013), and matches the dispersion observed in Figure 8. At comparable phases, DES16C2nm shows a lower velocity than Gaia16apd and reveals no evidence of velocity evolution in the  Å feature (see also Figure 2), but is consistent with the velocity evolution of other events, such as iPTF13ajg. Considering all available spectra, we find no evidence of a correlation between line velocity and far-UV (FUV) luminosity or color (see Section 3.4).

Below  Å all events exhibit absorption at  Å, determined to be a blend of Fe iii and Co iii, and an additional feature at  Å, tentatively identified as Al iii and Si iii by Mazzali et al. (2016). For SLSNe-I with higher intrinsic temperatures, such as SNLS-06D4eu and DES15E2mlf, the black body peaks in this wavelength range. There is no evidence of varying absorption at 2000 Å  so the diversity in this wavelength range is primarily driven by differences in the underlying temperature distribution.

Figure 8: The FUV spectroscopic evolution of SLSNe-I. A rest-frame UV spectral time series of DES16C2nm and compiled literature SLSNe-I as a function of phase from maximum light. Low-redshift () SLSNe-I are plotted with dashes, while high-redshift () events are shown as solid lines. The spectra have been smoothed and offset for clarity. Key spectral features from the SNe identified by Mazzali et al. (2016) and discussed in Section 3.5 at 267, 240, and 220 nm are highlighted with vertical lines. Swift filter responses are also shown to highlight the effective wavelength coverage probed by these spectra compared to the photometric analysis in Figures 6 and  7. Data for the literature objects are from various sources (Barbary et al., 2009; Berger et al., 2012; Howell et al., 2013; Vreeswijk et al., 2014; Yan et al., 2017; Pan et al., 2017).

4 Discussion

4.1 Rest-Frame UV: Implications for High-Redshift Searches

The discovery and spectroscopic confirmation of SLSNe-I at provides unique insights into how to identify such events at higher redshifts. With lower metallicities and younger stellar populations at , these studies are key to distinguishing whether SLSNe-I show diversity with respect to the metallicity, mass, or age of the stellar population, thereby constraining progenitor scenarios. Observations of SLSNe-I at open an avenue to measuring the interstellar medium (ISM; Berger et al., 2012) in distant galaxies, measuring cosmological parameters beyond the reach of SNe Ia (Inserra & Smartt, 2014), and finding the explosions of Population III stars (Cooke et al., 2012).

At low redshift, SLSNe-I are typically identified by their blue color, driven by their spectral energy distribution (SED) peaking in the rest-frame band, and by their long-duration light curves. However, as discussed in Section 3.5, at higher redshifts, the -band flux is redshifted toward redder filters, and the rest-frame UV and FUV become prominent in the selection. At , the rest-frame -band flux is no longer visible in optical filters (Figure 4), and only the UV flux is observed in optical searches. Figure 5 characterizes the UV properties of DES16C2nm, highlighting that in the UV, significant absorption and a turnover in the black body result in reduced flux in the FUV, compared to the optical, with decreasing 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.

To identify 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  Å. 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 and passbands. Figure 9 shows the evolution in luminosity and color for these spectra, along with other events in the literature. Where required, -corrections have been determined from the spectrum of Gaia16apd. The single-epoch 5 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; Scolnic, 2017). These limits suggest that in a single epoch, DES can detect SLSNe-I that are spectroscopically similar to Gaia16apd and DES16C2nm, to in -band observations of its deep fields or for objects that are spectroscopically similar to DES15E2mlf. For the LSST deep-drilling fields, the maximum redshifts in the band are 3.5 for the DES16C2nm spectrum and 4.3 when considering the DES15E2mlf spectrum.

This analysis can be extended to the observer-frame NIR, where surveys such as Euclid (with 5 limiting magnitude per visit in the deep fields and an irregular cadence of 10 visits to each of two fields in a 6-month observing window for 5 yr; Inserra et al., 2017) and WFIRST (limiting magnitude per exposure, , 24.6, and 26.2, and a regular cadence of 5 days; Hounsell et al., 2017) will search for high-redshift SLSNe-I. An object spectrally similar to DES16C2nm can be detected to with Euclid and , 4.4, and 6.6 in the WFIRST shallow, medium, and deep surveys, respectively.

From the lower panel of Figure 9, SLSNe-I in the literature are usually characterized as being observationally blue at low redshift, with all but one event having  mag at . This is well matched by the optical and NIR spectrum of Gaia16apd. At intermediate redshifts (), where the band probes the peak of the black-body emission in the rest-frame band, and the band probes the absorption triplet at  Å, SLSNe-I in the literature are red with  mag. The sole exception is the intrinsically hot, and therefore bluer, DES15E2mlf, which still has  mag.

The lower panel of Figure 9 provides a diagnostic to identify SLSNe-I at . In this redshift range, the available spectra, which are warped to be consistent with available photometry, all indicate that SLSNe-I have  mag at maximum light, with increasing color as a function of redshift. This observation is in good agreement with DES16C2nm and the photometrically classified SN2213-1745 at (Cooke et al., 2012).

At , SLSNe-I will have characteristic observer-frame timescales of months, with little luminosity evolution over this time. This, combined with the magnitude and color evolution described above, will enable the robust identification of these events from existing datasets, such as DES, HSC, PS1, SNLS, and SDSS, and upcoming facilities such as LSST, Euclid, and WFIRST. Given the slow evolution of SLSNe-I and time-dilation effects at high redshift, these estimates are conservative. Current and upcoming surveys will be able to combine single-epoch images over month-long timescales to obtain deep stacks with which to identify SLSNe-I to .

Figure 9: The observer-frame evolution of SLSNe-I. Upper panel: The apparent -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. -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 band. Third panel: The -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 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.

5 Conclusions

The first confirmation of a SLSN-I at provides new insights into these ultraluminous events. The spectroscopic similarity between DES16C2nm at , iPTF13ajg at , and Gaia16apd at highlights that these events exist at all redshifts, and show little evolution with cosmic time. Comparing the UV luminosity and color evolution of SLSNe-I at a range of redshifts, we find no evidence of a difference in mean luminosity or color between SLSNe-I at high and low redshift. After maximum light, these events show similar spectroscopic features in the UV in the range 2000–3000 Å.

The enormous luminosity of these events means that it is theoretically possible to discover and monitor them to . However, at identifying these objects requires an understanding of the FUV spectra of SLSNe-I, for which only a handful of objects exist. In its first 4 yr of operations, DES has discovered and spectroscopically confirmed the two highest-redshift SLSNe-I to date. These objects show differing levels of absorption in the rest-frame UV at  Å, but the implications from both events are clear: SLSNe-I are identified by their blue intrinsic colors at low redshift, while at the highest redshifts () these events are observationally red. The next challenges for surveys such as DES, HSC, LSST, Euclid, and WFIRST is to discover and spectroscopically confirm these objects to .

Acknowledgements

This paper has gone through internal review by the DES collaboration. It has Fermilab Preprint number PUB17380AE.

We acknowledge support from EU/FP7-ERC grant 615929. R.C.N. would like to acknowledge support from STFC grant ST/N000688/1 and the Faculty of Technology at the University of Portsmouth. L.G. was supported in part by the U.S. National Science Foundation (NSF) under grant AST-1311862. P.J.B.’s work on SLSNe is supported by the Swift GI program through grant NNX15AR41G. A.V.F.’s group is grateful for financial assistance from the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (U.C. Berkeley). We also thank the anonymous referee for comments.

Based in part on data obtained from the ESO Science Archive Facility under programs 298.D-5010 and 198.A-0915. Based in part on observations obtained at the Gemini Observatory, under program GS-2016B-DD-6, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the NSF (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). Based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program GO-14899.

Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the NSF. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W.M. Keck Foundation. We also acknowledge the help of T. G. Brink in obtaining the Keck spectrum.

This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.

Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. NSF, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey.

The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium.

The DES data management system is supported by the U.S. NSF under grants AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.

This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.

\facilities

Blanco (DECAM), VLT:Kueyen (X-SHOOTER), Keck:II (DEIMOS), Magellan:Clay (LDSS-3), Gemini:South (Flamingoes-2), HST (WFC3), VLT:Antu (FORS2), VLT:Antu (HAWK-I)

References

  • Angus et al. (2016) Angus, C. R., Levan, A. J., Perley, D. A., et al. 2016, MNRAS, 458, 84
  • Barbary et al. (2009) Barbary, K., Dawson, K. S., Tokita, K., et al. 2009, ApJ, 690, 1358
  • Berger et al. (2012) Berger, E., Chornock, R., Lunnan, R., et al. 2012, ApJ, 755, L29
  • Bernstein et al. (2012) Bernstein, J. P., Kessler, R., Kuhlmann, S., et al. 2012, ApJ, 753, 152
  • Bersten et al. (2016) Bersten, M. C., Benvenuto, O. G., Orellana, M., & Nomoto, K. 2016, ApJ, 817, L8
  • Bertin & Arnouts (1996) Bertin, E., & Arnouts, S. 1996, A&AS, 117, 393
  • Bessell (1990) Bessell, M. S. 1990, PASP, 102, 1181
  • Bose et al. (2017) Bose, S., Dong, S., Pastorello, A., et al. 2017, ArXiv e-prints, arXiv:1708.00864
  • Breeveld et al. (2011) Breeveld, A. A., Landsman, W., Holland, S. T., et al. 2011, in American Institute of Physics Conference Series, Vol. 1358, American Institute of Physics Conference Series, ed. J. E. McEnery, J. L. Racusin, & N. Gehrels, 373–376
  • Chatzopoulos et al. (2009) Chatzopoulos, E., Wheeler, J. C., & Vinko, J. 2009, ApJ, 704, 1251
  • Chatzopoulos et al. (2012) —. 2012, ApJ, 746, 121
  • Chatzopoulos et al. (2013) Chatzopoulos, E., Wheeler, J. C., Vinko, J., Horvath, Z. L., & Nagy, A. 2013, ApJ, 773, 76
  • Chen et al. (2017) Chen, T.-W., Smartt, S. J., Yates, R. M., et al. 2017, MNRAS, 470, 3566
  • Chevalier & Irwin (2011) Chevalier, R. A., & Irwin, C. M. 2011, ApJ, 729, L6
  • Chomiuk et al. (2011) Chomiuk, L., Chornock, R., Soderberg, A. M., et al. 2011, ApJ, 743, 114
  • Cooke et al. (2012) Cooke, J., Sullivan, M., Gal-Yam, A., et al. 2012, Nature, 491, 228
  • D’Andrea et al. (in prep.) D’Andrea, C., et al. 2018, in prep.
  • Dexter & Kasen (2013) Dexter, J., & Kasen, D. 2013, ApJ, 772, 30
  • Dong et al. (2017) Dong, S., Bose, S., Chen, P., et al. 2017, The Astronomer’s Telegram, 10498
  • Erben et al. (2005) Erben, T., Schirmer, M., Dietrich, J. P., et al. 2005, Astronomische Nachrichten, 326, 432
  • Faber et al. (2003) Faber, S. M., Phillips, A. C., Kibrick, R. I., et al. 2003, in Proc. SPIE, Vol. 4841, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, ed. M. Iye & A. F. M. Moorwood, 1657–1669
  • Firth et al. (2015) Firth, R. E., Sullivan, M., Gal-Yam, A., et al. 2015, MNRAS, 446, 3895
  • Flaugher et al. (2015) Flaugher, B., Diehl, H. T., Honscheid, K., et al. 2015, AJ, 150, 150
  • Gal-Yam (2012) Gal-Yam, A. 2012, Science, 337, 927
  • Galbany et al. (2016) Galbany, L., D’Andrea, C., Prajs, S., et al. 2016, The Astronomer’s Telegram, 9700
  • Gehrels et al. (2004) Gehrels, N., Chincarini, G., Giommi, P., et al. 2004, ApJ, 611, 1005
  • Goldstein et al. (2015) Goldstein, D. A., D’Andrea, C. B., Fischer, J. A., et al. 2015, AJ, 150, 82
  • Hounsell et al. (2017) Hounsell, R., Scolnic, D., Foley, R. J., et al. 2017, ArXiv e-prints, arXiv:1702.01747
  • Howell et al. (2013) Howell, D. A., Kasen, D., Lidman, C., et al. 2013, ApJ, 779, 98
  • Inserra & Smartt (2014) Inserra, C., & Smartt, S. J. 2014, ApJ, 796, 87
  • Inserra et al. (2013) Inserra, C., Smartt, S. J., Jerkstrand, A., et al. 2013, ApJ, 770, 128
  • Inserra et al. (2016) Inserra, C., Smartt, S. J., Gall, E. E. E., et al. 2016, ArXiv e-prints, arXiv:1604.01226
  • Inserra et al. (2017) Inserra, C., Nichol, R. C., Scovacricchi, D., et al. 2017, ArXiv e-prints, arXiv:1710.09585
  • Jones et al. (2013) Jones, D. O., Rodney, S. A., Riess, A. G., et al. 2013, ApJ, 768, 166
  • Kasen & Bildsten (2010) Kasen, D., & Bildsten, L. 2010, ApJ, 717, 245
  • Kasen et al. (2011) Kasen, D., Woosley, S. E., & Heger, A. 2011, ApJ, 734, 102
  • Kessler et al. (2015) Kessler, R., Marriner, J., Childress, M., et al. 2015, AJ, 150, 172
  • Kozyreva et al. (2017) Kozyreva, A., Gilmer, M., Hirschi, R., et al. 2017, MNRAS, 464, 2854
  • Kroupa (2001) Kroupa, P. 2001, MNRAS, 322, 231
  • Langer et al. (2007) Langer, N., Norman, C. A., de Koter, A., et al. 2007, A&A, 475, L19
  • Le Borgne & Rocca-Volmerange (2002) Le Borgne, D., & Rocca-Volmerange, B. 2002, A&A, 386, 446
  • Leloudas et al. (2012) Leloudas, G., Chatzopoulos, E., Dilday, B., et al. 2012, A&A, 541, A129
  • Leloudas et al. (2015) Leloudas, G., Schulze, S., Krühler, T., et al. 2015, MNRAS, 449, 917
  • Liu et al. (2017) Liu, Y.-Q., Modjaz, M., & Bianco, F. B. 2017, ApJ, 845, 85
  • Lunnan et al. (2014) Lunnan, R., Chornock, R., Berger, E., et al. 2014, ApJ, 787, 138
  • Mazzali et al. (2016) Mazzali, P. A., Sullivan, M., Pian, E., Greiner, J., & Kann, D. A. 2016, MNRAS, 458, 3455
  • Neill et al. (2011) Neill, J. D., Sullivan, M., Gal-Yam, A., et al. 2011, ApJ, 727, 15
  • Nicholl et al. (2017) Nicholl, M., Guillochon, J., & Berger, E. 2017, ApJ, 850, 55
  • Nicholl et al. (2015) Nicholl, M., Smartt, S. J., Jerkstrand, A., et al. 2015, ApJ, 807, L18
  • Nicholl et al. (2016) Nicholl, M., Berger, E., Smartt, S. J., et al. 2016, ApJ, 826, 39
  • Ofek et al. (2010) Ofek, E. O., Rabinak, I., Neill, J. D., et al. 2010, ApJ, 724, 1396
  • Pan et al. (2017) Pan, Y.-C., Foley, R. J., Smith, M., et al. 2017, MNRAS, 470, 4241
  • Papadopoulos et al. (2015) Papadopoulos, A., D’Andrea, C. B., Sullivan, M., et al. 2015, MNRAS, 449, 1215
  • Perley et al. (2016) Perley, D. A., Quimby, R. M., Yan, L., et al. 2016, ApJ, 830, 13
  • Piro (2015) Piro, A. L. 2015, ApJ, 808, L51
  • Poole et al. (2008) Poole, T. S., Breeveld, A. A., Page, M. J., et al. 2008, MNRAS, 383, 627
  • Prajs et al. (2017) Prajs, S., Sullivan, M., Smith, M., et al. 2017, MNRAS, 464, 3568
  • Quimby et al. (2011) Quimby, R. M., Kulkarni, S. R., Kasliwal, M. M., et al. 2011, Nature, 474, 487
  • Riess et al. (2001) Riess, A. G., Nugent, P. E., Gilliland, R. L., et al. 2001, ApJ, 560, 49
  • Rodney et al. (2012) Rodney, S. A., Riess, A. G., Dahlen, T., et al. 2012, ApJ, 746, 5
  • Rodney et al. (2014) Rodney, S. A., Riess, A. G., Strolger, L.-G., et al. 2014, AJ, 148, 13
  • Rodney et al. (2016) Rodney, S. A., Riess, A. G., Scolnic, D. M., et al. 2016, AJ, 151, 47
  • Roming et al. (2005) Roming, P. W. A., Kennedy, T. E., Mason, K. O., et al. 2005, Space Sci. Rev., 120, 95
  • Rubin et al. (2017) Rubin, D., Hayden, B., Huang, X., et al. 2017, ArXiv e-prints, arXiv:1707.04606
  • Schirmer (2013) Schirmer, M. 2013, ApJS, 209, 21
  • Schlegel et al. (1998) Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525
  • Scolnic (2017) Scolnic, D. 2017, Private communication
  • Scovacricchi et al. (2016) Scovacricchi, D., Nichol, R. C., Bacon, D., Sullivan, M., & Prajs, S. 2016, MNRAS, 456, 1700
  • Smith et al. (2016) Smith, M., Sullivan, M., D’Andrea, C. B., et al. 2016, ApJ, 818, L8
  • Vreeswijk et al. (2014) Vreeswijk, P. M., Savaglio, S., Gal-Yam, A., et al. 2014, ApJ, 797, 24
  • Woosley (2010) Woosley, S. E. 2010, ApJ, 719, L204
  • Woosley et al. (2007) Woosley, S. E., Blinnikov, S., & Heger, A. 2007, Nature, 450, 390
  • Yan et al. (2017) Yan, L., Quimby, R., Gal-Yam, A., et al. 2017, ApJ, 840, 57
  • Yaron & Gal-Yam (2012) Yaron, O., & Gal-Yam, A. 2012, PASP, 124, 668
UTC Date MJD Phase
(days)aaPhase is in the rest frame and relative to maximum light in the DES band (MJD = 57639.2) (counts)bbFluxes in each filter are given in counts. A zeropoint of 31.0 converts counts into AB magnitudes. No correction for Galactic extinction has been applied. (counts) (counts) (counts)
14-01-2016
21-01-2016
08-02-2016
09-03-2016
23-08-2016
27-08-2016
02-09-2016
06-09-2016
12-09-2016
13-09-2016
14-09-2016
22-09-2016
29-09-2016
06-10-2016
12-10-2016
19-10-2016
20-10-2016
22-10-2016
25-10-2016
02-11-2016
09-11-2016
10-11-2016
16-11-2016
17-11-2016
22-11-2016
26-11-2016
28-11-2016
03-12-2016
04-12-2016
08-12-2016
18-12-2016
20-12-2016
25-12-2016
29-12-2016
03-01-2017
08-01-2017
17-01-2017
25-01-2017
31-01-2017
04-02-2017
07-02-2017
08-02-2017
16-02-2017
Table 1: DES and SUDSS Light-Curve Data for DES16C2nm
UTC Date MJD Phase Telescope Instrument Observed Range Exp. time Rest Range
Date (days)aaPhase is in the rest frame and relative to maximum light in the DES band (MJD = 57639.2). (Å) (s) (Å)
09-10-2016 10.3 Magellan LDSS3 4500-10000 1800 2250-5000
24-10-2016 14.9 VLT XSHOOTER 3500-9800 9900 1750-4900
25-10-2016 15.3 Keck-II DEIMOS 4900-9600 6000 2250-4800
22-11-2016 24.6 VLT XSHOOTER 3500-9800 6300 1750-4900
20-12-2016 34.4 HST WFC3/G141 11000-17000 2400 5500-8500
Table 2: Details of the Spectral Data Obtained for DES16C2nm
UTC Date MJD Phase
(days)aaPhase is in the rest frame and relative to maximum light in the DES band (MJD = 57639.2). (counts)bbFluxes in each filter are given in counts. A zeropoint of 31.0 converts counts into AB magnitudes. No correction for Galactic extinction has been applied. (counts) (counts) (counts) (counts) (counts) (counts)
09-11-2016
10-11-2016
04-12-2016
20-12-2016
25-12-2016
03-01-2017
04-02-2017
08-02-2017
Table 3: Ancilliary Light-Curve Data for DES16C2nm
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