[ { "id": "authors:92zx1-c5z17", "collection": "authors", "collection_id": "92zx1-c5z17", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220526-173312318", "type": "monograph", "title": "SN2020qlb: a hydrogen-poor superluminous supernova with well-characterized light curve undulations", "author": [ { "family_name": "West", "given_name": "S. L.", "clpid": "West-S-L" }, { "family_name": "Lunnan", "given_name": "R.", "orcid": "0000-0001-9454-4639", "clpid": "Lunnan-Ragnhild" }, { "family_name": "Omand", "given_name": "C. M. B.", "clpid": "Omand-Conor-M-B" }, { "family_name": "Kangas", "given_name": "T.", "clpid": "Kangas-T" }, { "family_name": "Schulze", "given_name": "S.", "orcid": "0000-0001-6797-1889", "clpid": "Schulze-Steve" }, { "family_name": "Strotjohann", "given_name": "N.", "orcid": "0000-0002-4667-6730", "clpid": "Strotjohann-Nora-Linn" }, { "family_name": "Yang", "given_name": "S.", "orcid": "0000-0002-2898-6532", "clpid": "Yang-Sheng" }, { "family_name": "Fransson", "given_name": "C.", "orcid": "0000-0001-8532-3594", "clpid": "Fransson-Claes" }, { "family_name": "Sollerman", "given_name": "J.", "orcid": "0000-0003-1546-6615", "clpid": "Sollerman-Jesper" }, { "family_name": "Perley", "given_name": "D.", "orcid": "0000-0001-8472-1996", "clpid": "Perley-Daniel-A" }, { "family_name": "Yan", "given_name": "L.", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" }, { "family_name": "Chen", "given_name": "T.-W.", "orcid": "0000-0002-1066-6098", "clpid": "Chen-Ting-Wan" }, { "family_name": "Chen", "given_name": "Z. H.", "clpid": "Chen-Z-H" }, { "family_name": "Taggart", "given_name": "K.", "orcid": "0000-0002-5748-4558", "clpid": "Taggart-Kirsty" }, { "family_name": "Fremling", "given_name": "C.", "orcid": "0000-0002-4223-103X", "clpid": "Fremling-Christoffer" }, { "family_name": "Bloom", "given_name": "J. S.", "orcid": "0000-0002-7777-216X", "clpid": "Bloom-Joshua-S" }, { "family_name": "Drake", "given_name": "A.", "clpid": "Drake-Andrew-J" }, { "family_name": "Graham", "given_name": "M. J.", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "family_name": "Kasliwal", "given_name": "M. M.", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Laher", "given_name": "R.", "orcid": "0000-0003-2451-5482", "clpid": "Laher-Russ-R" }, { "family_name": "Medford", "given_name": "M. S.", "orcid": "0000-0002-7226-0659", "clpid": "Medford-Michael-S" }, { "family_name": "Neill", "given_name": "J. D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-James-D" }, { "family_name": "Riddle", "given_name": "R.", "orcid": "0000-0002-0387-370X", "clpid": "Riddle-Reed-L" }, { "family_name": "Shupe", "given_name": "D.", "orcid": "0000-0003-4401-0430", "clpid": "Shupe-David-L" } ], "abstract": "SN 2020qlb (ZTF20abobpcb) is a hydrogen-poor superluminous supernova (SLSN-I) that is among the most luminous (maximum M\u2089 = \u221222.25 mag) and that has one of the longest rise times (77 days from explosion to maximum). We estimate the total radiated energy to be > 2.1 \u00d7 10\u2075\u00b9 ergs. SN 2020qlb has a well-sampled light curve that exhibits clear undulations, a phenomenon seen in other SLSNe, whose physical origin is still unknown. We discuss the potential power source of this immense explosion as well as the mechanisms behind its observed light curve undulations. We analyze photospheric spectra and compare them to other SLSNe-I. We construct the bolometric light curve using photometry from a large data set of observations from the Zwicky Transient Facility (ZTF), Liverpool Telescope (LT) and Neil Gehrels Swift Observatory and compare it with radioactive, circumstellar interaction and magnetar models. Model residuals and light curve polynomial fit residuals are analyzed to estimate the undulation timescale and amplitude. We also determine host galaxy properties based on imaging and spectroscopy data, including a detection of the [O III]\u03bb4363\u00c5, auroral line, allowing for a direct metallicity estimate. We rule out the Arnett \u2075\u2076Ni decay model for SN 2020qlb's light curve due to unphysical parameter results. Our most favored power source is the magnetic dipole spin-down energy deposition of a magnetar. Two to three near peak oscillations, intriguingly similar to those of SN 2015bn, were found in the magnetar model residuals with a timescale of 32\u00b16 days and an amplitude of 6% of peak luminosity. We rule out centrally located undulation sources due to timescale considerations; and we favor the result of ejecta interactions with circumstellar material (CSM) density fluctuations as the source of the undulations.", "doi": "10.48550/arXiv.2205.11143", "publisher": "arXiv", "publication_date": "2022-05-23" }, { "id": "authors:0bjjr-81j98", "collection": "authors", "collection_id": "0bjjr-81j98", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211213-225013740", "type": "monograph", "title": "AT2018lqh and the nature of the emerging population of day-scale duration optical transients", "author": [ { "family_name": "Ofek", "given_name": "E. O.", "orcid": "0000-0002-6786-8774", "clpid": "Ofek-Eran-O" }, { "family_name": "Adams", "given_name": "S. M.", "orcid": "0000-0001-5855-5939", "clpid": "Adams-Scott-M" }, { "family_name": "Waxman", "given_name": "E.", "orcid": "0000-0002-9038-5877", "clpid": "Waxman-Eli" }, { "family_name": "Sharon", "given_name": "A.", "clpid": "Sharon-A" }, { "family_name": "Kushnir", "given_name": "D.", "clpid": "Kushnir-D" }, { "family_name": "Horesh", "given_name": "A.", "orcid": "0000-0002-5936-1156", "clpid": "Horesh-Assaf" }, { "family_name": "Ho", "given_name": "A.", "orcid": "0000-0002-9017-3567", "clpid": "Ho-Anna-Y-Q" }, { "family_name": "Kasliwal", "given_name": "M. M.", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Yaron", "given_name": "O.", "orcid": "0000-0002-0301-8017", "clpid": "Yaron-Ofer" }, { "family_name": "Gal-Yam", "given_name": "A.", "orcid": "0000-0002-3653-5598", "clpid": "Gal-Yam-Avishay" }, { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Bellm", "given_name": "E.", "orcid": "0000-0001-8018-5348", "clpid": "Bellm-Eric-C" }, { "family_name": "Masci", "given_name": "F.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-Frank-J" }, { "family_name": "Shupe", "given_name": "D.", "orcid": "0000-0003-4401-0430", "clpid": "Shupe-David-L" }, { "family_name": "Dekany", "given_name": "R.", "orcid": "0000-0002-5884-7867", "clpid": "Dekany-Richard-G" }, { "family_name": "Graham", "given_name": "M.", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "family_name": "Riddle", "given_name": "R.", "orcid": "0000-0002-0387-370X", "clpid": "Riddle-Reed-L" }, { "family_name": "Duev", "given_name": "D.", "orcid": "0000-0001-5060-8733", "clpid": "Duev-Dmitry-A" }, { "family_name": "Andreoni", "given_name": "I.", "orcid": "0000-0002-8977-1498", "clpid": "Andreoni-Igor" }, { "family_name": "Mahabal", "given_name": "A.", "orcid": "0000-0003-2242-0244", "clpid": "Mahabal-Ashish-A" }, { "family_name": "Drake", "given_name": "A.", "clpid": "Drake-Andrew-J" } ], "abstract": "We report on the discovery of AT2018lqh (ZTF18abfzgpl) -- a rapidly-evolving extra-galactic transient in a star-forming host at 242 Mpc. The transient g-band light curve's duration above half-maximum light is about 2.1 days, where 0.4/1.7 days are spent on the rise/decay, respectively. The estimated bolometric light curve of this object peaked at about 7x10\u2074\u00b2 erg s\u207b\u00b9 -- roughly seven times brighter than AT2017gfo. We show that this event can be explained by an explosion with a fast (v~0.08 c) low-mass (~0.07 M_\u2299) ejecta, composed mostly of radioactive elements. For example, ejecta dominated by \u2075\u2076Ni with a time scale of t\u2080 = 1.6 days for the ejecta to become optically thin for \u03b3-rays fits the data well. Such a scenario requires burning at densities that are typically found in the envelopes of neutron stars or the cores of white dwarfs. A combination of circumstellar material (CSM) interaction power at early times and shock cooling at late times is consistent with the photometric observations, but the observed spectrum of the event may pose some challenges for this scenario. The observations are not consistent with a shock breakout from a stellar envelope, while a model involving a low-mass ejecta ramming into low-mass CSM cannot explain both the early- and late-time observations.", "doi": "10.48550/arXiv.2109.10931", "publisher": "arXiv", "publication_date": "2021-09-22" }, { "id": "authors:nqsp9-56181", "collection": "authors", "collection_id": "nqsp9-56181", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190618-155216867", "type": "monograph", "title": "The Death Throes of a Stripped Massive Star: An Eruptive Mass-Loss History Encoded in Pre-Explosion Emission, a Rapidly Rising Luminous Transient, and a Broad-Lined Ic Supernova SN2018gep", "author": [ { "family_name": "Ho", "given_name": "Anna Y. Q.", "orcid": "0000-0002-9017-3567", "clpid": "Ho-Anna-Y-Q" }, { "family_name": "Goldstein", "given_name": "Daniel A.", "orcid": "0000-0003-3461-8661", "clpid": "Goldstein-D-A" }, { "family_name": "Schulze", "given_name": "Steve", "orcid": "0000-0001-6797-1889", "clpid": "Schulze-S" }, { "family_name": "Khatami", "given_name": "David K.", "orcid": "0000-0003-4307-0589", "clpid": "Khatami-D-K" }, { "family_name": "Perley", "given_name": "D. A.", "orcid": "0000-0001-8472-1996", "clpid": "Perley-D-A" }, { "family_name": "Ergon", "given_name": "Mattias", "clpid": "Ergon-M" }, { "family_name": "Gal-Yam", "given_name": "Avishay", "orcid": "0000-0002-3653-5598", "clpid": "Gal-Yam-A" }, { "family_name": "Corsi", "given_name": "Alessandra", "orcid": "0000-0001-8104-3536", "clpid": "Corsi-A" }, { "family_name": "Andreoni", "given_name": "Igor", "orcid": "0000-0002-8977-1498", "clpid": "Andreoni-I" }, { "family_name": "Barbarino", "given_name": "Cristina", "orcid": "0000-0002-3821-6144", "clpid": "Barbarino-C" }, { "family_name": "Bellm", "given_name": "Eric C.", "orcid": "0000-0001-8018-5348", "clpid": "Bellm-E-C" }, { "family_name": "Blagorodnova", "given_name": "Nadejda", "orcid": "0000-0003-0901-1606", "clpid": "Blagorodnova-N" }, { "family_name": "Bright", "given_name": "Joe S.", "orcid": "0000-0002-7735-5796", "clpid": "Bright-J-S" }, { "family_name": "Burns", "given_name": "Eric", "clpid": "Burns-E" }, { "family_name": "Cenko", "given_name": "S. B.", "orcid": "0000-0003-1673-970X", "clpid": "Cenko-S-B" }, { "family_name": "Cunningham", "given_name": "Virginia", "orcid": "0000-0003-2292-0441", "clpid": "Cunningham-V" }, { "family_name": "De", "given_name": "Kishalay", "orcid": "0000-0002-8989-0542", "clpid": "De-Kishalay" }, { "family_name": "Dekany", "given_name": "Richard", "clpid": "Dekany-Richard" }, { "family_name": "Dugas", "given_name": "Alison M.", "clpid": "Dugas-A-M" }, { "family_name": "Fender", "given_name": "Rob P.", "clpid": "Fender-R-P" }, { "family_name": "Fransson", "given_name": "Claes", "orcid": "0000-0001-8532-3594", "clpid": "Fransson-C" }, { "family_name": "Fremling", "given_name": "Christoffer", "orcid": "0000-0002-4223-103X", "clpid": "Fremling-C" }, { "family_name": "Goldstein", "given_name": "Adam", "orcid": "0000-0002-0587-7042", "clpid": "Goldstein-A" }, { "family_name": "Graham", "given_name": "Matthew J.", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "family_name": "Hale", "given_name": "David", "clpid": "Hale-D" }, { "family_name": "Horesh", "given_name": "Assaf", "orcid": "0000-0002-5936-1156", "clpid": "Horesh-A" }, { "family_name": "Hung", "given_name": "Tiara", "orcid": "0000-0002-9878-7889", "clpid": "Hung-Tiara" }, { "family_name": "Kasliwal", "given_name": "Mansi M.", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Kuin", "given_name": "N. Paul M.", "orcid": "0000-0003-4650-4186", "clpid": "Kuin-N-P-M" }, { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Kupfer", "given_name": "Thomas", "orcid": "0000-0002-6540-1484", "clpid": "Kupfer-T" }, { "family_name": "Lunnan", "given_name": "Ragnhild", "orcid": "0000-0001-9454-4639", "clpid": "Lunnan-R" }, { "family_name": "Masci", "given_name": "Frank J.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-F-J" }, { "family_name": "Ngeow", "given_name": "Chow-Choong", "orcid": "0000-0001-8771-7554", "clpid": "Ngeow-Chow-Choong" }, { "family_name": "Nugent", "given_name": "Peter E.", "orcid": "0000-0002-3389-0586", "clpid": "Nugent-P-E" }, { "family_name": "Ofek", "given_name": "Eran O.", "orcid": "0000-0002-6786-8774", "clpid": "Ofek-E-O" }, { "family_name": "Patterson", "given_name": "Maria T.", "orcid": "0000-0002-4753-3387", "clpid": "Patterson-M-T" }, { "family_name": "Pettipas", "given_name": "Glen", "clpid": "Pettipas-G" }, { "family_name": "Rusholme", "given_name": "Ben", "orcid": "0000-0001-7648-4142", "clpid": "Rusholme-B" }, { "family_name": "Sai", "given_name": "Hanna", "clpid": "Sai-H" }, { "family_name": "Sfaradi", "given_name": "Itai", "clpid": "Sfaradi-I" }, { "family_name": "Shupe", "given_name": "D. L.", "orcid": "0000-0003-4401-0430", "clpid": "Shupe-David-L" }, { "family_name": "Sollerman", "given_name": "J.", "orcid": "0000-0003-1546-6615", "clpid": "Sollerman-J" }, { "family_name": "Soumagnac", "given_name": "Maayane T.", "orcid": "0000-0001-6753-1488", "clpid": "Soumagnac-M-T" }, { "family_name": "Tachibana", "given_name": "Yutaro", "orcid": "0000-0001-6584-6945", "clpid": "Tachibana-Yutaro" }, { "family_name": "Taddia", "given_name": "Francesco", "orcid": "0000-0002-2387-6801", "clpid": "Taddia-F" }, { "family_name": "Walters", "given_name": "Richard", "orcid": "0000-0002-1835-6078", "clpid": "Walters-R" }, { "family_name": "Wang", "given_name": "Xiaofeng", "orcid": "0000-0002-7334-2357", "clpid": "Wang-Xiaofeng" }, { "family_name": "Yao", "given_name": "Yuhan", "orcid": "0000-0001-6747-8509", "clpid": "Yao-Yuhan" }, { "family_name": "Zhang", "given_name": "Xinhan", "clpid": "Zhang-X" } ], "abstract": "We present detailed observations of ZTF18abukavn (SN2018gep), discovered in high-cadence data from the Zwicky Transient Facility as a rapidly rising (1.3 mag/hr) and luminous (M_(g,peak) = \u221220 mag) transient. It is spectroscopically classified as a broad-lined stripped-envelope supernova (Ic-BL SN). The rapid rise to peak bolometric luminosity and blue colors at peak (t_(rise)\u223c0.5-3 days, L_(bol)\u22733\u00d710^(44) erg sec^(\u22121), g\u2212r = \u22120.3) resemble the high-redshift Ic-BL iPTF16asu, as well as several other unclassified fast transients. The early discovery of SN2018gep (within an hour of shock breakout) enabled an intensive spectroscopic campaign, including the highest-temperature (T_(eff) \u2273 40,000K) spectra of a stripped-envelope SN. A retrospective search revealed luminous (M_g \u223c M_r \u2248 \u221214mag) emission in the days to weeks before explosion, the first definitive detection of precursor emission for a Ic-BL. We find a limit on the isotropic gamma-ray energy release E_(\u03b3,iso) < 4.9\u00d710^(48) erg, a limit on X-ray emission L_X < 10^(40) erg sec^(\u22121), and a limit on radio emission \u03bdL_\u03bd \u2272 10^(37) erg sec^(\u22121). Taken together, we find that the data are best explained by shock breakout in a massive shell of dense circumstellar material (0.02 M\u2299) at large radii (3\u00d710^(14)cm) that was ejected in eruptive pre-explosion mass-loss episodes.", "doi": "10.48550/arXiv.1904.11009", "publication_date": "2019-04-24" }, { "id": "authors:1rxer-jt836", "collection": "authors", "collection_id": "1rxer-jt836", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190528-131400152", "type": "monograph", "title": "Census of the Local Universe (CLU) Narrow-Band Survey I: Galaxy Catalogs from Preliminary Fields", "author": [ { "family_name": "Cook", "given_name": "David O.", "orcid": "0000-0002-6877-7655", "clpid": "Cook-D-O" }, { "family_name": "Kasliwal", "given_name": "Mansi M.", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Van Sistine", "given_name": "Angela", "orcid": "0000-0003-4131-173X", "clpid": "Van-Sistine-A" }, { "family_name": "Kaplan", "given_name": "David L.", "orcid": "0000-0001-6295-2881", "clpid": "Kaplan-D-L" }, { "family_name": "Sutter", "given_name": "Jessica S.", "orcid": "0000-0002-9183-8102", "clpid": "Sutter-J-S" }, { "family_name": "Kupfer", "given_name": "Thomas", "orcid": "0000-0002-6540-1484", "clpid": "Kupfer-T" }, { "family_name": "Shupe", "given_name": "David L.", "orcid": "0000-0003-4401-0430", "clpid": "Shupe-David-L" }, { "family_name": "Laher", "given_name": "Russ R.", "orcid": "0000-0003-2451-5482", "clpid": "Laher-R-R" }, { "family_name": "Masci", "given_name": "Frank J.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-F-J" }, { "family_name": "Dale", "given_name": "Daniel A.", "orcid": "0000-0002-5782-9093", "clpid": "Dale-D-A" }, { "family_name": "Sesar", "given_name": "Branimir", "orcid": "0000-0002-0834-3978", "clpid": "Sesar-B" }, { "family_name": "Brady", "given_name": "Patrick R.", "orcid": "0000-0002-4611-9387", "clpid": "Brady-P-R" }, { "family_name": "Yan", "given_name": "Lin", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" }, { "family_name": "Ofek", "given_name": "Eran O.", "orcid": "0000-0002-6786-8774", "clpid": "Ofek-E-O" }, { "family_name": "Reitze", "given_name": "David H.", "clpid": "Reitze-D-H" }, { "family_name": "Kulkarni", "given_name": "Shrinivas R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" } ], "abstract": "We present the Census of the Local Universe (CLU) narrow-band survey to search for emission-line (H\u03b1) galaxies. CLU-H\u03b1 has imaged \u22483\u03c0 of the sky (26,470 deg^2) with 4 narrow-band filters that probe a distance out to 200 Mpc. We have obtained spectroscopic follow-up for galaxy candidates in 14 preliminary fields (101.6 deg^2) to characterize the limits and completeness of the survey. In these preliminary fields, CLU can identify emission lines down to an H\u03b1 flux limit of 10^(\u221214) erg s^(\u22121) cm^(\u22122) at 90\\% completeness, and recovers 83% (67%) of the H\u03b1 flux from catalogued galaxies in our search volume at the \u03a3=2.5 (\u03a3=5) color excess levels. The contamination from galaxies with no emission lines is 61% (12%) for \u03a3=2.5 (\u03a3=5). Also, in the regions of overlap between our preliminary fields and previous emission-line surveys, we recover the majority of the galaxies found in previous surveys and identify an additional \u2248300 galaxies. In total, we find 90 galaxies with no previous distance information, several of which are interesting objects: 7 blue compact dwarfs, 1 green pea, and a Seyfert galaxy; we also identified a known planetary nebula. These objects show that the CLU-H\u03b1 survey can be a discovery machine for objects in our own Galaxy and extreme galaxies out to intermediate redshifts. However, the majority of the CLU-H\u03b1 galaxies identified in this work show properties consistent with normal star-forming galaxies. CLU-H\u03b1 galaxies with new redshifts will be added to existing galaxy catalogs to focus the search for the electromagnetic counterpart to gravitational wave events.", "doi": "10.48550/arXiv.1710.05016", "publisher": "arXiv", "publication_date": "2017-10-13" } ]