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Your search keyword '"McCully, C [0000-0001-5807-7893]"' showing total 4 results
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4 results on '"McCully, C [0000-0001-5807-7893]"'

1. The Type Ibn Supernova 2019kbj -- Indications for Diversity in Type Ibn Supernova Progenitors

Author

Ben-Ami, T, Arcavi, I, Newsome, M, Farah, J, Pellegrino, C, Terreran, G, Burke, J, Hosseinzadeh, G, McCully, C, Hiramatsu, D, Gonzalez, EP, Howell, DA, Ben-Ami, T [0000-0001-7513-6701], Arcavi, I [0000-0001-7090-4898], Pellegrino, C [0000-0002-7472-1279], Terreran, G [0000-0003-0794-5982], Burke, J [0000-0003-0035-6659], Hosseinzadeh, G [0000-0002-0832-2974], McCully, C [0000-0001-5807-7893], Hiramatsu, D [0000-0002-1125-9187], Gonzalez, EP [0000-0003-0209-9246], Howell, DA [0000-0003-4253-656X], and Apollo - University of Cambridge Repository

Subjects
5110 Synchrotrons and Accelerators, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Stem Cell Research, Astrophysics - High Energy Astrophysical Phenomena, 51 Physical Sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Type Ibn supernovae (SNe) are a rare class of stellar explosions whose progenitor systems are not yet well determined. We present and analyze observations of the Type Ibn SN 2019kbj, and model its light curve in order to constrain its progenitor and explosion parameters. SN 2019kbj shows roughly constant temperature during the first month after peak, indicating a power source (likely circumstellar material interaction) that keeps the continuum emission hot at ~15,000K. Indeed, we find that the radioactive decay of Ni56 is disfavored as the sole power source of the bolometric light curve. A radioactive decay + circumstellar-material (CSM) interaction model, on the other hand, does reproduce the bolometric emission well. The fits prefer a uniform-density CSM shell rather than CSM due to a steady mass-loss wind, similar to what is seen in other Type Ibn SNe. The uniform-density CSM shell model requires ~0.1 solar masses of Ni56 and ~1 solar mass of total ejecta to reproduce the light curve. SN 2019kbj differs in this manner from another Type Ibn SN with derived physical parameters, SN 2019uo, for which an order of magnitude lower Ni56 mass and larger ejecta mass were derived. This points towards a possible diversity in SN Ibn progenitor systems and explosions., Accepted to ApJ

Published
2022

2. Less Than 1% of Core-collapse Supernovae in the Local Universe Occur in Elliptical Galaxies

Author

Irani, I., Prentice, S. J., Schulze, S., Gal-Yam, A., Teffs, Jacob, Mazzali, Paolo, Sollerman, J., Gonzalez, E. P., Taggart, K., De, Kishalay, Fremling, Christoffer, Perley, Daniel A., Strotjohann, Nora L., Kasliwal, Mansi M., Howell, A., Dhawan, S., Tzanidakis, Anastasios, Hiramatsu, Daichi, Kool, Erik C., Anderson, J. P., Muller-Bravo, T. E., Dekany, Richard, Gromadzki, Mariusz, Carini, Roberta, Galbany, L., Drake, Andrew J., Burke, Jamison, Pellegrino, Craig, Della Valle, Massimo, Medford, Michael S., Rusholme, Ben, Young, D. R., Gutierrez, Claudia P., Inserra, Cosimo, Omer, Rafia, Shupe, David L., Chen, T. -W., Shin, Kyung Min, Yaron, Ofer, McCully, Curtis, Nicholl, Matt, Riddle, Reed, National Aeronautics and Space Administration (US), National Science Foundation (US), University of Hawaii, European Commission, David and Lucile Packard Foundation, Ministerio de Ciencia, Innovación y Universidades (España), Wenner-Gren Foundation, ITA, USA, GBR, FRA, DEU, Irani, I [0000-0002-7996-8780], Prentice, SJ [0000-0003-0486-6242], Schulze, S [0000-0001-6797-1889], Gal-Yam, A [0000-0002-3653-5598], Mazzali, P [0000-0001-6876-8284], Sollerman, J [0000-0003-1546-6615], Taggart, K [0000-0002-5748-4558], De, K [0000-0002-8989-0542], Fremling, C [0000-0002-4223-103X], Perley, DA [0000-0001-8472-1996], Strotjohann, NL [0000-0002-4667-6730], Kasliwal, MM [0000-0002-5619-4938], Dhawan, S [0000-0002-2376-6979], Tzanidakis, A [0000-0003-0484-3331], Hiramatsu, D [0000-0002-1125-9187], Kool, EC [0000-0002-7252-3877], Anderson, JP [0000-0003-0227-3451], Müller-Bravo, TE [0000-0003-3939-7167], Dekany, R [0000-0002-5884-7867], Gromadzki, M [0000-0002-1650-1518], Carini, R [0000-0003-1604-2064], Galbany, L [0000-0002-1296-6887], Burke, J [0000-0003-0035-6659], Pellegrino, C [0000-0002-7472-1279], Della Valle, M [0000-0003-3142-5020], Medford, MS [0000-0002-7226-0659], Rusholme, B [0000-0001-7648-4142], Young, DR [0000-0002-1229-2499], Gutiérrez, CP [0000-0003-2375-2064], Inserra, C [0000-0002-3968-4409], Shupe, DL [0000-0003-4401-0430], Shin, KM [0000-0002-1486-3582], Yaron, O [0000-0002-0301-8017], McCully, C [0000-0001-5807-7893], Nicholl, M [0000-0002-2555-3192], Riddle, R [0000-0002-0387-370X], and Apollo - University of Cambridge Repository

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Early-type galaxies, 5101 Astronomical Sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Core-collapse supernovae, Astrophysics - High Energy Astrophysical Phenomena, 51 Physical Sciences, QC, High-Energy Phenomena and Fundamental Physics, QB
Abstract

We present observations of three core-collapse supernovae (CCSNe) in elliptical hosts, detected by the Zwicky Transient Facility Bright Transient Survey (BTS). SN 2019ape is a SN Ic that exploded in the main body of a typical elliptical galaxy. Its properties are consistent with an explosion of a regular SN Ic progenitor. A secondary g-band light-curve peak could indicate interaction of the ejecta with circumstellar material (CSM). An Hα-emitting source at the explosion site suggests a residual local star formation origin. SN 2018fsh and SN 2020uik are SNe II which exploded in the outskirts of elliptical galaxies. SN 2020uik shows typical spectra for SNe II, while SN 2018fsh shows a boxy nebular Hα profile, a signature of CSM interaction. We combine these 3 SNe with 7 events from the literature and analyze their hosts as a sample. We present multi-wavelength photometry of the hosts, and compare this to archival photometry of all BTS hosts. Using the spectroscopically complete BTS, we conclude that 0.3%-0.1+0.3 of all CCSNe occur in elliptical galaxies. We derive star formation rates and stellar masses for the host galaxies and compare them to the properties of other SN hosts. We show that CCSNe in ellipticals have larger physical separations from their hosts compared to SNe Ia in elliptical galaxies, and discuss implications for star-forming activity in elliptical galaxies., ATLAS is primarily funded to search for near Earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; by products of the NEO search include images and catalogs from the survey area. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen's University Belfast, and the Space Telescope Science Institute. TMB was funded by the CONICYT PFCHA/DOCTORADOBECAS CHILE/2017-72180113. MN is supported by a Royal Astronomical Society Research Fellowship and by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 948381 M.M.K. acknowledges generous support from the David and Lucille Packard Foundation. This work was supported by the GROWTH Marshal (Kasliwal et al. 2019) developed as part of the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation under grant No. 1545949. M.G. is supported by the EU Horizon 2020 research and innovation program under grant agreement No 101004719. L.G. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00. T.-W.C. acknowledges the EU Funding under Marie Skłodowska-Curie grant H2020-MSCA-IF-2018-842471. E.C.K. acknowledges support from the G.R.E.A.T research environment funded by Vetenskapsrådet, the Swedish Research Council, under project number 2016-06012, and support from The Wenner-Gren Foundations. L.G. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00.

Published
2022
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3. SOAR/Goodman Spectroscopic Assessment of Candidate Counterparts of the LIGO-Virgo Event GW190814

Author

D. L. Tucker, M. P. Wiesner, S. S. Allam, M. Soares-Santos, C. R. Bom, M. Butner, A. Garcia, R. Morgan, F. Olivares E., A. Palmese, L. Santana-Silva, A. Shrivastava, J. Annis, J. García-Bellido, M. S. S. Gill, K. Herner, C. D. Kilpatrick, M. Makler, N. Sherman, A. Amara, H. Lin, M. Smith, E. Swann, I. Arcavi, T. G. Bachmann, K. Bechtol, F. Berlfein, C. Briceño, D. Brout, R. E. Butler, R. Cartier, J. Casares, H.-Y. Chen, C. Conselice, C. Contreras, E. Cook, J. Cooke, K. Dage, C. D’Andrea, T. M. Davis, R. de Carvalho, H. T. Diehl, J. P. Dietrich, Z. Doctor, A. Drlica-Wagner, M. Drout, B. Farr, D. A. Finley, M. Fishbach, R. J. Foley, F. Förster-Burón, P. Fosalba, D. Friedel, J. Frieman, C. Frohmaier, R. A. Gruendl, W. G. Hartley, D. Hiramatsu, D. E. Holz, D. A. Howell, A. Kawash, R. Kessler, N. Kuropatkin, O. Lahav, A. Lundgren, M. Lundquist, U. Malik, A. W. Mann, J. Marriner, J. L. Marshall, C. E. Martínez-Vázquez, C. McCully, F. Menanteau, N. Meza, G. Narayan, E. Neilsen, C. Nicolaou, R. Nichol, F. Paz-Chinchón, M. E. S. Pereira, J. Pineda, S. Points, J. Quirola-Vásquez, S. Rembold, A. Rest, Ó. Rodriguez, A. K. Romer, M. Sako, S. Salim, D. Scolnic, J. A. Smith, J. Strader, M. Sullivan, M. E. C. Swanson, D. Thomas, S. Valenti, T. N. Varga, A. R. Walker, J. Weller, M. L. Wood, B. Yanny, A. Zenteno, M. Aguena, F. Andrade-Oliveira, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, J. De Vicente, S. Desai, S. Everett, I. Ferrero, B. Flaugher, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, M. Lima, M. A. G. Maia, R. Miquel, R. L. C. Ogando, A. Pieres, A. A. Plazas Malagón, M. Rodriguez-Monroy, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, E. Suchyta, G. Tarle, C. To, Y. Zhang, Tucker, DL [0000-0001-7211-5729], Wiesner, MP [0000-0001-8653-7738], Allam, SS [0000-0002-7069-7857], Soares-Santos, M [0000-0001-6082-8529], Bom, CR [0000-0003-4383-2969], Garcia, A [0000-0001-9578-6322], Morgan, R [0000-0002-7016-5471], Olivares E., F [0000-0002-5115-6377], Palmese, A [0000-0002-6011-0530], Santana-Silva, L [0000-0003-3402-6164], Shrivastava, A [0000-0002-2854-6713], Annis, J [0000-0002-0609-3987], García-Bellido, J [0000-0002-9370-8360], Gill, MSS [0000-0003-2524-5154], Herner, K [0000-0001-6718-2978], Makler, M [0000-0003-2206-2651], Lin, H [0000-0002-7825-3206], Smith, M [0000-0002-3321-1432], Arcavi, I [0000-0001-7090-4898], Bechtol, K [0000-0001-8156-0429], Briceño, C [0000-0001-7124-4094], Brout, D [0000-0001-5201-8374], Butler, RE [0000-0003-2789-3817], Casares, J [0000-0001-5031-0128], Chen, H-Y [0000-0001-5403-3762], Conselice, C [0000-0003-1949-7638], Cooke, J [0000-0001-5703-2108], Dage, K [0000-0002-8532-4025], Davis, TM [0000-0002-4213-8783], Diehl, HT [0000-0002-8357-7467], Dietrich, JP [0000-0002-8134-9591], Doctor, Z [0000-0002-2077-4914], Drlica-Wagner, A [0000-0001-8251-933X], Drout, M [0000-0001-7081-0082], Finley, DA [0000-0003-3870-8445], Fishbach, M [0000-0002-1980-5293], Foley, RJ [0000-0002-2445-5275], Fosalba, P [0000-0002-1510-5214], Frieman, J [0000-0003-4079-3263], Frohmaier, C [0000-0001-9553-4723], Gruendl, RA [0000-0002-4588-6517], Hiramatsu, D [0000-0002-1125-9187], Holz, DE [0000-0002-0175-5064], Howell, DA [0000-0003-4253-656X], Kawash, A [0000-0003-0071-1622], Kessler, R [0000-0003-3221-0419], Kuropatkin, N [0000-0003-2511-0946], Lundquist, M [0000-0001-9589-3793], Mann, AW [0000-0003-3654-1602], Marriner, J [0000-0001-9359-6752], Marshall, JL [0000-0003-0710-9474], Martínez-Vázquez, CE [0000-0002-9144-7726], McCully, C [0000-0001-5807-7893], Menanteau, F [0000-0002-1372-2534], Neilsen, E [0000-0002-7357-0317], Nicolaou, C [0000-0001-7474-0544], Paz-Chinchón, F [0000-0003-1339-2683], Points, S [0000-0002-4596-1337], Rest, A [0000-0002-4410-5387], Rodriguez, Ó [0000-0001-8651-8772], Romer, AK [0000-0002-9328-879X], Sako, M [0000-0003-2764-7093], Salim, S [0000-0003-2342-7501], Smith, JA [0000-0002-6261-4601], Strader, J [0000-0002-1468-9668], Sullivan, M [0000-0001-9053-4820], Swanson, MEC [0000-0002-1488-8552], Thomas, D [0000-0002-6325-5671], Valenti, S [0000-0001-8818-0795], Walker, AR [0000-0002-7123-8943], Weller, J [0000-0002-8282-2010], Wood, ML [0000-0001-7336-7725], Yanny, B [0000-0002-9541-2678], Aguena, M [0000-0001-5679-6747], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Rosell, A Carnero [0000-0003-3044-5150], Kind, M Carrasco [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], De Vicente, J [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Ferrero, I [0000-0002-1295-1132], Flaugher, B [0000-0002-2367-5049], Gaztanaga, E [0000-0001-9632-0815], Gerdes, DW [0000-0001-6942-2736], Gruen, D [0000-0003-3270-7644], Gschwend, J [0000-0003-3023-8362], Gutierrez, G [0000-0003-0825-0517], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Honscheid, K [0000-0002-6550-2023], James, DJ [0000-0001-5160-4486], Kuehn, K [0000-0003-0120-0808], Maia, MAG [0000-0001-9856-9307], Miquel, R [0000-0002-6610-4836], Ogando, RLC [0000-0003-2120-1154], Pieres, A [0000-0001-9186-6042], Plazas Malagón, AA [0000-0002-2598-0514], Sanchez, E [0000-0002-9646-8198], Schubnell, M [0000-0001-9504-2059], Serrano, S [0000-0002-0211-2861], Sevilla-Noarbe, I [0000-0002-1831-1953], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], Apollo - University of Cambridge Repository, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Ministerio de Economía y Competitividad (España), European Research Council, A Tucker, D. L., Wiesner, M. P., Allam, S. S., Soares-Santos, M., Bom, C. R., Butner, M., Garcia, A., Morgan, R., Olivares E., F., Palmese, A., Santana-Silva, L., Shrivastava, A., Annis, J., García-Bellido, J., Gill, M. S. S., Herner, K., Kilpatrick, C. D., Makler, M., Sherman, N., Amara, A., Lin, H., Smith, M., Swann, E., Arcavi, I., Bachmann, T. G., Bechtol, K., Berlfein, F., Briceño, C., Brout, D., Butler, R. E., Cartier, R., Casares, J., Chen, H. -Y., Conselice, C., Contreras, C., Cook, E., Cooke, J., Dage, K., D'Andrea, C., Davis, T. M., de Carvalho, R., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica-Wagner, A., Drout, M., Farr, B., Finley, D. A., Fishbach, M., Foley, R. J., Förster-Burón, F., Fosalba, P., Friedel, D., Frieman, J., Frohmaier, C., Gruendl, R. A., Hartley, W. G., Hiramatsu, D., Holz, D. E., Howell, D. A., Kawash, A., Kessler, R., Kuropatkin, N., Lahav, O., Lundgren, A., Lundquist, M., Malik, U., Mann, A. W., Marriner, J., Marshall, J. L., Martínez-Vázquez, C. E., Mccully, C., Menanteau, F., Meza, N., Narayan, G., Neilsen, E., Nicolaou, C., Nichol, R., Paz-Chinchón, F., Pereira, M. E. S., Pineda, J., Points, S., Quirola-Vásquez, J., Rembold, S., Rest, A., Rodriguez, Ó., Romer, A. K., Sako, M., Salim, S., Scolnic, D., Smith, J. A., Strader, J., Sullivan, M., Swanson, M. E. C., Thomas, D., Valenti, S., Varga, T. N., Walker, A. R., Weller, J., Wood, M. L., Yanny, B., Zenteno, A., Aguena, M., Andrade-Oliveira, F., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Everett, S., Ferrero, I., Flaugher, B., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Miquel, R., Ogando, R. L. C., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla- Noarbe, I., Suchyta, E., Tarle, G., To, C., and Zhang, Y.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational waves, Spectroscopy, Neutron stars, Black holes, Neutron star, FOS: Physical sciences, Astronomy and Astrophysics, BURACOS NEGROS, Space and Planetary Science, 5101 Astronomical Sciences, Astrophysics - High Energy Astrophysical Phenomena, 51 Physical Sciences, Gravitational wave, High-Energy Phenomena and Fundamental Physics
Abstract

Tucker et al., On 2019 August 14 at 21:10:39 UTC, the LIGO/Virgo Collaboration (LVC) detected a possible neutron star–black hole merger (NSBH), the first ever identified. An extensive search for an optical counterpart of this event, designated GW190814, was undertaken using the Dark Energy Camera on the 4 m Victor M. Blanco Telescope at the Cerro Tololo Inter-American Observatory. Target of Opportunity interrupts were issued on eight separate nights to observe 11 candidates using the 4.1 m Southern Astrophysical Research (SOAR) telescope's Goodman High Throughput Spectrograph in order to assess whether any of these transients was likely to be an optical counterpart of the possible NSBH merger. Here, we describe the process of observing with SOAR, the analysis of our spectra, our spectroscopic typing methodology, and our resultant conclusion that none of the candidates corresponded to the gravitational wave merger event but were all instead other transients. Finally, we describe the lessons learned from this effort. Application of these lessons will be critical for a successful community spectroscopic follow-up program for LVC observing run 4 (O4) and beyond., Funding for the DES Projects has been provided by the DOE and NSF(USA), MEC/MICINN/MINECO (Spain), STFC (UK), HEFCE(UK). NCSA (UIUC), KICP (U. Chicago), CCAPP (Ohio State), MIFPA (Texas A&M), CNPQ, FAPERJ, FINEP (Brazil), DFG (Germany) and the Collaborating Institutions in the Dark Energy Survey. The DES Data Management System is supported by the NSF under grant Nos. 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. I.A. is a CIFAR Azrieli Global Scholar in the Gravity and the Extreme Universe Program and acknowledges support from that program, from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (grant agreement number 852097), from the Israel Science Foundation (grant number 2752/19), from the United States–Israel Binational Science Foundation (BSF), and from the Israeli Council for Higher Education Alon Fellowship.

Published
2021

4. SN 2015bn: a detailed multi-wavelength view of a nearby superluminous supernova

Author

Ting-Wan Chen, Philip S. Cowperthwaite, Iair Arcavi, Morgan Fraser, T. M. Reynolds, Stefano Valenti, Jussi Harmanen, Brian D. Metzger, Régis Cartier, Ryan Chornock, Stephen J. Smartt, Curtis McCully, V. A. Villar, Michael McDonald, Mark E. Huber, Matt Nicholl, Christopher S. Kochanek, Edo Berger, Lluís Galbany, K. W. Smith, Ragnhild Lunnan, Zhong-Yi Lin, J. Saario, Achintya Mitra, K. C. Chambers, Thomas W.-S. Holoien, H. Flewelling, Griffin Hosseinzadeh, M. Childress, Kate Maguire, Raffaella Margutti, Avishay Gal-Yam, Anders Jerkstrand, Cosimo Inserra, Dan Milisavljevic, P. K. Blanchard, Kate D. Alexander, Erkki Kankare, Christopher Waters, Eugene A. Magnier, Atish Kamble, Maria R. Drout, David Young, Dale Andrew Howell, Benjamin J. Shappee, Nicholl, M [0000-0002-2555-3192], Berger, E [0000-0002-9392-9681], Smartt, SJ [0000-0002-8229-1731], Margutti, R [0000-0003-4768-7586], Kamble, A [0000-0003-0861-5168], Alexander, KD [0000-0002-8297-2473], Inserra, C [0000-0002-3968-4409], Arcavi, I [0000-0001-7090-4898], Cowperthwaite, PS [0000-0002-2478-6939], Flewelling, HA [0000-0002-1050-4056], Fraser, M [0000-0003-2191-1674], Gal-Yam, A [0000-0002-3653-5598], Galbany, L [0000-0002-1296-6887], Howell, DA [0000-0003-4253-656X], Huber, ME [0000-0003-1059-9603], Jerkstrand, A [0000-0001-8005-4030], Kochanek, CS [0000-0001-6017-2961], Lunnan, R [0000-0001-9454-4639], McCully, C [0000-0001-5807-7893], McDonald, M [0000-0001-5226-8349], Milisavljevic, D [0000-0002-0763-3885], Waters, C [0000-0003-1989-4879], Young, DR [0000-0002-1229-2499], and Apollo - University of Cambridge Repository

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), supernovae: individual (SN 2015bn), FOS: Physical sciences, Astrophysics, Magnetar, 01 natural sciences, 7. Clean energy, Photometry (optics), supernovae: general, 0103 physical sciences, Emission spectrum, Ejecta, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Redshift, Galaxy, Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present observations of SN 2015bn (= PS15ae = CSS141223-113342+004332 = MLS150211-113342+004333), a Type I superluminous supernova (SLSN) at redshift $z=0.1136$. As well as being one of the closest SLSNe I yet discovered, it is intrinsically brighter ($M_U\approx-23.1$) and in a fainter galaxy ($M_B\approx-16.0$) than other SLSNe at $z\sim0.1$. We used this opportunity to collect the most extensive dataset for any SLSN I to date, including densely-sampled spectroscopy and photometry, from the UV to the NIR, spanning $-$50 to +250 days from optical maximum. SN 2015bn fades slowly, but exhibits surprising undulations in the light curve on a timescale of 30-50 days, especially in the UV. The spectrum shows extraordinarily slow evolution except for a rapid transformation between +7 and +20-30 days. No narrow emission lines from slow-moving material are observed at any phase. We derive physical properties including the bolometric luminosity, and find slow velocity evolution and non-monotonic temperature and radial evolution. A deep radio limit rules out a healthy off-axis gamma-ray burst, and places constraints on the pre-explosion mass loss. The data can be consistently explained by a $\gtrsim10\,{\rm M}_\odot$ stripped progenitor exploding with $\sim 10^{51}\,$erg kinetic energy, forming a magnetar with a spin-down timescale of $\sim20$ days (thus avoiding a gamma-ray burst) that reheats the ejecta and drives ionization fronts. The most likely alternative scenario -- interaction with $\sim20\,{\rm M}_\odot$ of dense, inhomogeneous circumstellar material -- can be tested with continuing radio follow-up., Slightly updated to match published version

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