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1. Optical follow-up of gravitational wave triggers with DECam during the first two LIGO/VIRGO observing runs

Author

R. E. Butler, D. L. Burke, F. Paz-Chinchón, Keith Bechtol, Brian Yanny, Ken Herner, William G. Hartley, M. Smith, N. P. Kuropatkin, D. W. Gerdes, Masao Sako, Eric H. Neilsen, I. Sevilla-Noarbe, G. Gutierrez, Alex Drlica-Wagner, Edo Berger, L. N. da Costa, S. Desai, H. S. Chen, Ben Farr, Marcelle Soares-Santos, James Annis, Elisabeth Krause, Huan Lin, M. Carrasco-Kind, G. Tarle, A. A. Plazas, K. Honscheid, Pablo Fosalba, Philip S. Cowperthwaite, M. A. G. Maia, Daniel E. Holz, J. Marriner, Nora Sherman, David James, Alejandro Garcia, V. Scarpine, J. De Vicente, Antonella Palmese, Douglas L. Tucker, Felipe Menanteau, Enrique Gaztanaga, Robert A. Gruendl, E. Suchyta, Tenglin Li, A. Carnero Rosell, Santiago Avila, Ramon Miquel, Peter K. G. Williams, M. Sauseda, William Wester, Kyler Kuehn, D. J. Brout, Ofer Lahav, J. Gschwend, Christopher J. Conselice, E. Buckley-Geer, Devon L. Hollowood, Juan Garcia-Bellido, E. Bertin, M. S. Schubnell, J. L. Marshall, Thomas Matheson, Peter Doel, H. T. Diehl, M. S. S. Gill, S. Everett, Daniel Scolnic, Marco A. P. Lima, Edward R. Cook, Santiago Serrano, Yanxi Zhang, Tim Eifler, Richard Kessler, Flavia Sobreira, D. A. Finley, J. Carretero, Tamara M. Davis, M. March, Sahar S. Allam, Zoheyr Doctor, N. Glaeser, Joshua A. Frieman, R. J. Foley, E. J. Sanchez, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DECam, National Science Foundation (US), Department of Energy (US), University of Illinois, Stanford University, New York State Office of Science, Technology and Academic Research, Lawrence Berkeley National Laboratory, University of Pennsylvania, The Ohio State University, University of Chicago, University of Michigan, Texas A&M University, University of Portsmouth, Science and Technology Facilities Council (UK), University College London, European Research Council, University of Nottingham, University of Sussex, German Research Foundation, Ministerio de Economía y Competitividad (España), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, and Financiadora de Estudos e Projetos (Brasil)

Subjects
cosmological model, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Cosmology, Gravitational waves, General Relativity and Quantum Cosmology, star, 0103 physical sciences, supernova, black hole, optical, Software and its engineering software infrastructure, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], LIGO, cosmic string, neutron star, dark energy, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation, Astronomy, imaging, Astronomy and Astrophysics, trigger, Computer Science Applications, Black hole, Neutron star, Supernova, electromagnetic, VIRGO, 13. Climate action, Space and Planetary Science, Grid computing, Dark energy, Astrophysics - Instrumentation and Methods for Astrophysics, signature
Abstract

Gravitational wave (GW) events detectable by LIGO and Virgo have several possible progenitors, including black hole mergers, neutron star mergers, black hole–neutron star mergers, supernovae, and cosmic string cusps. A subset of GW events is expected to produce electromagnetic (EM) emission that, once detected, will provide complementary information about their astrophysical context. To that end, the LIGO–Virgo Collaboration (LVC) sends GW candidate alerts to the astronomical community so that searches for their EM counterparts can be pursued. The DESGW group, consisting of members of the Dark Energy Survey (DES), the LVC, and other members of the astronomical community, uses the Dark Energy Camera (DECam) to perform a search and discovery program for optical signatures of LVC GW events. DESGW aims to use a sample of GW events as standard sirens for cosmology. Due to the short decay timescale of the expected EM counterparts and the need to quickly eliminate survey areas with no counterpart candidates, it is critical to complete the initial analysis of each night's images as quickly as possible. We discuss our search area determination, imaging pipeline, and candidate selection processes. We review results from the DESGW program during the first two LIGO–Virgo observing campaigns and introduce other science applications that our pipeline enables., Funding for the DES Projects has been provided by the DOE and NSF, MEC/MICINN/MINECO (Spain), STFC, HEFCE, NCSA (UIUC), KICP (U. Chicago), CCAPP (Ohio State), MIFPA (Texas A&M), CNPQ, FAPERJ, FINEP, DFG and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, ETH Zürich, Fermilab, University of Illinois, ICE (IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU München and the associated Excellence Cluster Universe, University of Michigan, NOAO, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Lab, Stanford University, University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES Data Management System is supported by the NSF under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-88861, FPA2015-68048, and Centro de Excelencia SEV-2016-0588, SEV-2016-0597 and MDM-2015-0509. Research leading to these results has received funding from the ERC under the EU’s 7th Framework Programme including grants ERC 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 research uses services or data provided by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. 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 U.S. Government retains and the publisher, by accepting the article for publication, acknowledges that the U.S. 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 U.S. Government purposes.

Published
2020
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2. Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the $Kepler$ 2 Observations

Author

Jakob Nordin, D. Bersier, Gautham Narayan, Dan Kasen, Zhihao Chen, R. S. Post, B. Cseh, J. Van Cleve, James M. DerKacy, L. Denneau, Lluís Galbany, M. Redick, A. Rest, Krisztián Sárneczky, Subhash Bose, Curtis McCully, Hanna Sai, B. C. Kaiser, E. Baron, C. A. Peterson, J. Vinicius de Miranda Cardoso, Jeffrey L. Coughlin, A. Razza, M. Packard, Steven Williams, G. Beerman, M. Muszynski, Cs. Kalup, B. Elsaesser, O. Hanyecz, G. Csörnyei, Iair Arcavi, J. Moffatt, Isobel Hook, Wenxiong Li, A. Villar, J. Kampmeier, Robert L. Mutel, César Rojas-Bravo, K. A. Larson, Liming Rui, R. Gangopadhyay, B. Csák, S. Margheim, Peter A. Milne, Cosimo Inserra, Subo Dong, Thomas W.-S. Holoien, Jennifer E. Andrews, J. Burke, Han Lin, Jun Mo, Jessie L. Dotson, Kaicheng Zhang, John C Wheeler, J. Palmerio, J. S. Brown, R. M. Larsen, Kate Maguire, H. Flewelling, Katie Auchettl, Danfeng Xiang, K. C. Chambers, Ori D. Fox, Attila Bódi, S. Holmbo, András Pál, C. McGinn, Edward J. Shaya, John L. Tonry, Xulin Zhao, Xiaojia Zhang, E. A. Magnier, M. Hanley, Yen-Chen Pan, Bernadett Ignácz, B. Stalder, R. Szabó, K. M. McCalmont-Everton, G. Zsidi, Joshua S. Reding, J. A. Muñoz, Geert Barentsen, Daichi Hiramatsu, K. Steward, Brad E. Tucker, J. Brimacombe, K. W. Smith, A. Zenteno, R. J. Foley, J. V. Shields, I. Rajmon, Jozsef Vinko, Xiaofeng Wang, Charles D. Kilpatrick, Steven Villanueva, A. Wheaton, B. Spencer, Ann Marie Cody, Peter J. Brown, T. Weschler, L. Migliorini, Xue Li, Claudia P. Gutiérrez, Fang Huang, Saurabh Jha, R. Bjella, C. Labonde, Benjamin J. Shappee, Mark Willman, D. Tallon, V. Nystrom, Tianmeng Zhang, Griffin Hosseinzadeh, S. Flynn, Long Wang, David A. Coulter, David J. Sand, Georgios Dimitriadis, D. O. Jones, J. J. Hermes, Thomas Barclay, Christopher Bilinski, H. Weiland, Réka Könyves-Tóth, Régis Cartier, Steve B. Howell, Peter M. Garnavich, Kim Griest, J. L. Prieto, S. E. Ross, Mark E. Huber, Zs. Bognár, Róbert Szakáts, R. Kloetzel, Krzysztof Z. Stanek, Christopher S. Kochanek, Stefano Valenti, Christina Hedges, G. Castillo, Todd A. Thompson, Ping Chen, C. Z. Waters, L. Kohnert, Adam G. Riess, Nathan Smith, T. B. Lowe, Anthony L. Piro, L. H. Reedy, Levente Kriskovics, Linyi Li, Maria R. Drout, Dale Andrew Howell, A. N. Heinze, A. Ordasi, Stephen J. Smartt, Patrick J. Vallely, A. S. B. Schultz, Joanna Bulger, Michael Gully-Santiago, Jujia Zhang, Ádám Sódor, D. Osborne, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
DATA RELEASE, ULTRAVIOLET, FACTORY OBSERVATIONS, FOS: Physical sciences, Astrophysics, Type (model theory), medicine.disease_cause, SN 2011FE, 01 natural sciences, Luminosity, Photometry (optics), individual (SN 2018oh) [supernovae], supernovae: general, CIRCUMSTELLAR MATERIAL, 0103 physical sciences, medicine, SPECTRA, Absorption (logic), Ejecta, 010303 astronomy & astrophysics, supernovae: individual, QC, Solar and Stellar Astrophysics (astro-ph.SR), QB, LIGHT CURVES, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, HIGH-VELOCITY FEATURES, 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Supernova, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, IMPROVED DISTANCES, WHITE-DWARF MODELS, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [supernovae], Ultraviolet
Abstract

Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically-confirmed type Ia supernova (SN Ia) observed in the $Kepler$ field. The $Kepler$ data revealed an excess emission in its early light curve, allowing to place interesting constraints on its progenitor system (Dimitriadis et al. 2018, Shappee et al. 2018b). Here, we present extensive optical, ultraviolet, and near-infrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3$\pm$0.3 days and $\Delta$m$_{15}(B)=0.96\pm$0.03 mag, but it seems to have bluer $B - V$ colors. We construct the "uvoir" bolometric light curve having peak luminosity as 1.49$\times$10$^{43}$erg s$^{-1}$, from which we derive a nickel mass as 0.55$\pm$0.04M$_{\odot}$ by fitting radiation diffusion models powered by centrally located $^{56}$Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of $^{56}$Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a non-degenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia, but is characterized by prominent and persistent carbon absorption features. The C II features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in a SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers., Comment: 48 pages, 23 figures. This paper is part of a coordinated effort between groups. Accepted for publication in ApJ

Published
2019
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3. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models

Author

P. S. Cowperthwaite, E. Berger, V. A. Villar, B. D. Metzger, M. Nicholl, R. Chornock, P. K. Blanchard, W. Fong, R. Margutti, M. Soares-Santos, K. D. Alexander, S. Allam, J. Annis, D. Brout, D. A. Brown, R. E. Butler, H.-Y. Chen, H. T. Diehl, Z. Doctor, M. R. Drout, T. Eftekhari, B. Farr, D. A. Finley, R. J. Foley, J. A. Frieman, C. L. Fryer, J. García-Bellido, M. S. S. Gill, J. Guillochon, K. Herner, D. E. Holz, D. Kasen, R. Kessler, J. Marriner, T. Matheson, E. H. Neilsen, E. Quataert, A. Palmese, A. Rest, M. Sako, D. M. Scolnic, N. Smith, D. L. Tucker, P. K. G. Williams, E. Balbinot, J. L. Carlin, E. R. Cook, F. Durret, T. S. Li, P. A. A. Lopes, A. C. C. Lourenço, J. L. Marshall, G. E. Medina, J. Muir, R. R. Muñoz, M. Sauseda, D. J. Schlegel, L. F. Secco, A. K. Vivas, W. Wester, A. Zenteno, Y. Zhang, T. M. C. Abbott, M. Banerji, K. Bechtol, A. Benoit-Lévy, E. Bertin, E. Buckley-Geer, D. L. Burke, D. Capozzi, A. Carnero Rosell, M. Carrasco Kind, F. J. Castander, M. Crocce, C. E. Cunha, C. B. D’Andrea, L. N. da Costa, C. Davis, D. L. DePoy, S. Desai, J. P. Dietrich, A. Drlica-Wagner, T. F. Eifler, A. E. Evrard, E. Fernandez, B. Flaugher, P. Fosalba, E. Gaztanaga, D. W. Gerdes, T. Giannantonio, D. A. Goldstein, D. Gruen, R. A. Gruendl, G. Gutierrez, K. Honscheid, B. Jain, D. J. James, T. Jeltema, M. W. G. Johnson, M. D. Johnson, S. Kent, E. Krause, R. Kron, K. Kuehn, N. Nuropatkin, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, M. March, P. Martini, R. G. McMahon, F. Menanteau, C. J. Miller, R. Miquel, J. J. Mohr, E. Neilsen, R. C. Nichol, R. L. C. Ogando, A. A. Plazas, N. Roe, A. K. Romer, A. Roodman, E. S. Rykoff, E. Sanchez, V. Scarpine, R. Schindler, M. Schubnell, I. Sevilla-Noarbe, M. Smith, R. C. Smith, F. Sobreira, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, R. C. Thomas, M. A. Troxel, V. Vikram, A. R. Walker, R. H. Wechsler, J. Weller, B. Yanny, J. Zuntz, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
AST-1714498, neutron star: binary, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], AST-1411763, Astrophysics, Kilonova, 7. Clean energy, 01 natural sciences, Luminosity, star, ultraviolet, site, optical, Astrophysics::Solar and Stellar Astrophysics, LIGO, dark energy, 010303 astronomy & astrophysics, QB, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, binaries: close, HEFCE, gravitational waves, radioactivity, black body, infrared, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, close [bibaries], Milky Way, Astrophysics::High Energy Astrophysical Phenomena, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometry (optics), stars: neutron, neutron [stars], bolometer, surveys, 0103 physical sciences, capture, STFC, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, velocity: expansion, gravitational radiation, RCUK, opacity, Astronomy and Astrophysics, Light curve, color, Neutron star, VIRGO, electromagnetic, 13. Climate action, Space and Planetary Science, spectral, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract

We present UV, optical, and NIR photometry of the first electromagnetic counterpart to a gravitational wave source from Advanced LIGO/Virgo, the binary neutron star merger GW170817. Our data set extends from the discovery of the optical counterpart at $0.47$ days to $18.5$ days post-merger, and includes observations with the Dark Energy Camera (DECam), Gemini-South/FLAMINGOS-2 (GS/F2), and the {\it Hubble Space Telescope} ({\it HST}). The spectral energy distribution (SED) inferred from this photometry at $0.6$ days is well described by a blackbody model with $T\approx 8300$ K, a radius of $R\approx 4.5\times 10^{14}$ cm (corresponding to an expansion velocity of $v\approx 0.3c$), and a bolometric luminosity of $L_{\rm bol}\approx 5\times10^{41}$ erg s$^{-1}$. At $1.5$ days we find a multi-component SED across the optical and NIR, and subsequently we observe rapid fading in the UV and blue optical bands and significant reddening of the optical/NIR colors. Modeling the entire data set we find that models with heating from radioactive decay of $^{56}$Ni, or those with only a single component of opacity from $r$-process elements, fail to capture the rapid optical decline and red optical/NIR colors. Instead, models with two components consistent with lanthanide-poor and lanthanide-rich ejecta provide a good fit to the data, the resulting "blue" component has $M_\mathrm{ej}^\mathrm{blue}\approx 0.01$ M$_\odot$ and $v_\mathrm{ej}^\mathrm{blue}\approx 0.3$c, and the "red" component has $M_\mathrm{ej}^\mathrm{red}\approx 0.04$ M$_\odot$ and $v_\mathrm{ej}^\mathrm{red}\approx 0.1$c. These ejecta masses are broadly consistent with the estimated $r$-process production rate required to explain the Milky Way $r$-process abundances, providing the first evidence that BNS mergers can be a dominant site of $r$-process enrichment., 13 Pages, 3 Figures, 2 Tables. ApJL, In Press. Keywords: GW170817, LVC

Published
2017
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4. A Search for Kilonovae in the Dark Energy Survey

Author

Alex Drlica-Wagner, C. B. D'Andrea, M. S. Schubnell, Zoheyr Doctor, J. Carretero, G. Tarle, H. T. Diehl, Daniel A. Goldstein, William Wester, Benjamin Farr, J. Gschwend, Kyler Kuehn, Felipe Menanteau, Joshua A. Frieman, James Annis, Jennifer L. Marshall, Flavia Sobreira, Daniel E. Holz, Marcos Lima, Elisabeth Krause, A. K. Romer, Marcio A. G. Maia, Tim Eifler, Sahar S. Allam, F. B. Abdalla, G. Gutierrez, Masao Sako, David Brooks, D. W. Gerdes, A. Benoit-Lévy, M. E. C. Swanson, Keith Bechtol, Tenglin Li, I. Sevilla-Noarbe, David James, N. P. Kuropatkin, Alistair R. Walker, M. March, Shantanu Desai, Marcelle Soares-Santos, V. Scarpine, Ramon Miquel, Eric H. Neilsen, D. L. Burke, Mathew Smith, D. A. Finley, H. S. Chen, R. J. Foley, Robert A. Gruendl, Carlos Cunha, E. J. Sanchez, Juan Garcia-Bellido, Robert Connon Smith, E. Buckley-Geer, Emmanuel Bertin, Daniel Scolnic, E. Suchyta, Brian Nord, Richard Kessler, A. Carnero Rosell, Eric Morganson, Darren L. DePoy, L. N. da Costa, A. A. Plazas, Alex G. Kim, Enrique Gaztanaga, M. Carrasco Kind, Robert C. Nichol, T. M. C. Abbott, Ofer Lahav, H. Spinka, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
Absolute magnitude, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, observational [methods], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Kilonova, Atomic, Physical Chemistry, 01 natural sciences, general [binaries], stars: neutron, neutron [stars], Particle and Plasma Physics, Affordable and Clean Energy, supernovae: general, 0103 physical sciences, data analysis [methods], Nuclear, 010303 astronomy & astrophysics, QB, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, Molecular, Astronomy and Astrophysics, Light curve, methods: data analysis, Galaxy, Supernova, Neutron star, binaries: general, 13. Climate action, Space and Planetary Science, Dark energy, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [supernovae], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

The coalescence of a binary neutron star (BNS) pair is expected to produce gravitational waves (GW) and electromagnetic (EM) radiation, both of which may be detectable with currently available instruments. We describe a search for a theoretically predicted r-process optical transient from these mergers, dubbed the kilonova (KN), using griz broadband data from the Dark Energy Survey Supernova Program (DES-SN). Some models predict KNe to be redder, shorter-lived, and dimmer than supernovae (SNe), but at present the event rate of KNe is poorly constrained. We simulate observations of KN and SN light curves with the Monte-Carlo simulation code SNANA to optimize selection requirements, determine search efficiency, and predict SN backgrounds. We also perform an analysis using fake point sources on images to account for anomalous efficiency losses from difference-imaging on bright low-redshift galaxies. Our analysis of the first two seasons of DES-SN data results in 0 events, and is consistent with our prediction of 1.1 background events based on simulations of SN. Given our simulation prediction, there is a 33 percent chance of finding 0 events in the data. Assuming no underlying galaxy flux, our search sets 90 percent upper limits on the KN volumetric rate of $1.0\times10^7$ Gpc$^{-3}$ yr$^{-1}$ for the dimmest KN model we consider (peak i-band absolute magnitude $M_i=-11.4$ mag) and $2.4\times10^4$ Gpc$^{-3}$ yr$^{-1}$ for the brightest ($M_i=-16.2$ mag). Accounting for efficiency loss from host galaxy Poisson noise, these limits are 1.1 times higher; accounting for anomalous subtraction artifacts on bright galaxies, these limits are ~3 times higher. While previous KN searches were based on triggered follow-up, this analysis is the first untriggered optical KN search and informs selection requirements and strategies for future KN searches and GW follow-up observations.

Published
2017
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5. ESC and KAIT Observations of the Transitional Type Ia SN 2004eo

Author

Valeri M. Larionov, W. P. S. Meikle, G. Blanc, Avet Harutyunyan, László L. Kiss, Enrico Cappellaro, S. Temporin, Weidong Li, Stuart D. Ryder, Andrea Pastorello, Brian P. Schmidt, N. Napoleone, John R. Lucey, Wolfgang Hillebrandt, Nancy Elias-Rosa, Paolo A. Mazzali, Maria Elena Salvo, M. Dolci, Filomena Bufano, Mohan Ganeshalingam, G. Pignata, S. Taubenberger, Aliz Derekas, Ferdinando Patat, Vallery Stanishev, Massimo Turatto, Rubina Kotak, Stefano Benetti, R. J. Foley, Arkady A. Arkharov, P. Székely, Alexei V. Filippenko, Jeffrey A. Rich, H. Navasardyan, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), and Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Solar mass, Mass distribution, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Infrared, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Spectral line, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova, 13. Climate action, Space and Planetary Science, 0103 physical sciences, 010306 general physics, Ejecta, 010303 astronomy & astrophysics
Abstract

We present optical and infrared observations of the unusual Type Ia supernova (SN) 2004eo. The light curves and spectra closely resemble those of the prototypical SN 1992A, and the luminosity at maximum (M_B = -19.08) is close to the average for a SN Ia. However, the ejected 56Ni mass derived by modelling the bolometric light curve (about 0.45 solar masses) lies near the lower limit of the 56Ni mass distribution observed in normal SNe Ia. Accordingly, SN 2004eo shows a relatively rapid post-maximum decline in the light curve (Delta m_(B) = 1.46), small expansion velocities in the ejecta, and a depth ratio Si II 5972 / Si II 6355 similar to that of SN 1992A. The physical properties of SN 2004eo cause it to fall very close to the boundary between the faint, low velocity gradient, and high velocity gradient subgroups proposed by Benetti et al. (2005). Similar behaviour is seen in a few other SNe Ia. Thus, there may in fact exist a few SNe Ia with intermediate physical properties., Comment: 28 pages, 17 figures, accepted for publication in MNRAS

Published
2007
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