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Chen, P., Gal-Yam, A., Sollerman, J., Schulze, S., Post, R. S., Liu, C., . . . Yan, L. (2024). A 12.4-day periodicity in a close binary system after a supernova. Nature, 625(7994), 253-258
Öppna denna publikation i ny flik eller fönster >>A 12.4-day periodicity in a close binary system after a supernova
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2024 (Engelska)Ingår i: Nature, ISSN 0028-0836, E-ISSN 1476-4687, Vol. 625, nr 7994, s. 253-258Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

Neutron stars and stellar-mass black holes are the remnants of massive star explosions1. Most massive stars reside in close binary systems2, and the interplay between the companion star and the newly formed compact object has been theoretically explored3, but signatures for binarity or evidence for the formation of a compact object during a supernova explosion are still lacking. Here we report a stripped-envelope supernova, SN 2022jli, which shows 12.4-day periodic undulations during the declining light curve. Narrow Hα emission is detected in late-time spectra with concordant periodic velocity shifts, probably arising from hydrogen gas stripped from a companion and accreted onto the compact remnant. A new Fermi-LAT γ-ray source is temporally and positionally consistent with SN 2022jli. The observed properties of SN 2022jli, including periodic undulations in the optical light curve, coherent Hα emission shifting and evidence for association with a γ-ray source, point to the explosion of a massive star in a binary system leaving behind a bound compact remnant. Mass accretion from the companion star onto the compact object powers the light curve of the supernova and generates the γ-ray emission.

Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-226987 (URN)10.1038/s41586-023-06787-x (DOI)001143579000018 ()38200292 (PubMedID)2-s2.0-85181900770 (Scopus ID)
Tillgänglig från: 2024-03-04 Skapad: 2024-03-04 Senast uppdaterad: 2024-03-04Bibliografiskt granskad
Srinivasaragavan, G. P., Swain, V., O'Connor, B., Anand, S., Ahumada, T., Perley, D., . . . Wold, A. (2024). Characterizing the Ordinary Broad-line Type Ic SN 2023pel from the Energetic GRB 230812B. Astrophysical Journal Letters, 960(2), Article ID L18.
Öppna denna publikation i ny flik eller fönster >>Characterizing the Ordinary Broad-line Type Ic SN 2023pel from the Energetic GRB 230812B
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2024 (Engelska)Ingår i: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 960, nr 2, artikel-id L18Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

We report observations of the optical counterpart of the long gamma-ray burst (GRB) GRB 230812B and its associated supernova (SN) SN 2023pel. The proximity (z = 0.36) and high energy (Eγ,iso ∼ 1053 erg) make it an important event to study as a probe of the connection between massive star core collapse and relativistic jet formation. With a phenomenological power-law model for the optical afterglow, we find a late-time flattening consistent with the presence of an associated SN. SN 2023pel has an absolute peak r-band magnitude of Mr = −19.46 ± 0.18 mag (about as bright as SN 1998bw) and evolves on quicker timescales. Using a radioactive heating model, we derive a nickel mass powering the SN of MNi = 0.38 ± 0.01 M and a peak bolometric luminosity of Lbol ∼ 1.3 × 1043 erg s−1. We confirm SN 2023pel's classification as a broad-line Type Ic SN with a spectrum taken 15.5 days after its peak in the r band and derive a photospheric expansion velocity of vph = 11,300 ± 1600 km s−1 at that phase. Extrapolating this velocity to the time of maximum light, we derive the ejecta mass Mej = 1.0 ± 0.6 M and kinetic energy EKE = 1.3 +3.3/-1.2 x 1051 erg. We find that GRB 230812B/SN 2023pel has SN properties that are mostly consistent with the overall GRB-SN population. The lack of correlations found in the GRB-SN population between SN brightness and Eγ,iso for their associated GRBs across a broad range of 7 orders of magnitude provides further evidence that the central engine powering the relativistic ejecta is not coupled to the SN powering mechanism in GRB-SN systems.

Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-226049 (URN)10.3847/2041-8213/ad16e7 (DOI)001138589900001 ()2-s2.0-85182349337 (Scopus ID)
Tillgänglig från: 2024-02-12 Skapad: 2024-02-12 Senast uppdaterad: 2024-02-12Bibliografiskt granskad
Anand, S., Barnes, J., Yang, S., Kasliwal, M. M., Coughlin, M. W., Sollerman, J., . . . Zhang, C. (2024). Collapsars as Sites of r-process Nucleosynthesis: Systematic Photometric Near-infrared Follow-up of Type Ic-BL Supernovae. Astrophysical Journal, 962(1), Article ID 68.
Öppna denna publikation i ny flik eller fönster >>Collapsars as Sites of r-process Nucleosynthesis: Systematic Photometric Near-infrared Follow-up of Type Ic-BL Supernovae
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2024 (Engelska)Ingår i: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 962, nr 1, artikel-id 68Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

One of the open questions following the discovery of GW170817 is whether neutron star (NS) mergers are the only astrophysical sites capable of producing r-process elements. Simulations have shown that 0.01–0.1 M of r-process material could be generated in the outflows originating from the accretion disk surrounding the rapidly rotating black hole that forms as a remnant to both NS mergers and collapsing massive stars associated with long-duration gamma-ray bursts (collapsars). The hallmark signature of r-process nucleosynthesis in the binary NS merger GW170817 was its long-lasting near-infrared (NIR) emission, thus motivating a systematic photometric study of the light curves of broad-lined stripped-envelope (Ic-BL) supernovae (SNe) associated with collapsars. We present the first systematic study of 25 SNe Ic-BL—including 18 observed with the Zwicky Transient Facility and 7 from the literature—in the optical/NIR bands to determine what quantity of r-process material, if any, is synthesized in these explosions. Using semi-analytic models designed to account for r-process production in SNe Ic-BL, we perform light curve fitting to derive constraints on the r-process mass for these SNe. We also perform independent light curve fits to models without the r-process. We find that the r-process-free models are a better fit to the light curves of the objects in our sample. Thus, we find no compelling evidence of r-process enrichment in any of our objects. Further high-cadence infrared photometric studies and nebular spectroscopic analysis would be sensitive to smaller quantities of r-process ejecta mass or indicate whether all collapsars are completely devoid of r-process nucleosynthesis.

Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-226991 (URN)10.3847/1538-4357/ad11df (DOI)001159107900001 ()2-s2.0-85184922589 (Scopus ID)
Tillgänglig från: 2024-03-04 Skapad: 2024-03-04 Senast uppdaterad: 2024-03-04Bibliografiskt granskad
Strotjohann, N. L., Ofek, E. O., Gal-Yam, A., Sollerman, J., Chen, P., Yaron, O., . . . Purdum, J. (2024). Search for Supernova Progenitor Stars with ZTF and LSST. Astrophysical Journal, 960(1), Article ID 72.
Öppna denna publikation i ny flik eller fönster >>Search for Supernova Progenitor Stars with ZTF and LSST
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2024 (Engelska)Ingår i: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 960, nr 1, artikel-id 72Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

The direct detection of core-collapse supernova (SN) progenitor stars is a powerful way of probing the last stages of stellar evolution. However, detections in archival Hubble Space Telescope images are limited to about one detection per year. Here, we explore whether we can increase the detection rate by using data from ground-based wide-field surveys. Due to crowding and atmospheric blurring, progenitor stars can typically not be identified in preexplosion images alone. Instead, we combine many pre-SN and late-time images to search for the disappearance of the progenitor star. As a proof of concept, we implement our search of ZTF data. For a few hundred images, we achieve limiting magnitudes of ∼23 mag in the g and r bands. However, no progenitor stars or long-lived outbursts are detected for 29 SNe within z ≤ 0.01, and the ZTF limits are typically several magnitudes less constraining than detected progenitors in the literature. Next, we estimate progenitor detection rates for the Legacy Survey of Space and Time (LSST) with the Vera C. Rubin telescope by simulating a population of nearby SNe. The background from bright host galaxies reduces the nominal LSST sensitivity by, on average, 0.4 mag. Over the 10 yr survey, we expect the detection of ∼50 red supergiant progenitors and several yellow and blue supergiants. The progenitors of Type Ib and Ic SNe will be detectable if they are brighter than −4.7 or −4.0 mag in the LSST i band, respectively. In addition, we expect the detection of hundreds of pre-SN outbursts depending on their brightness and duration.

Nyckelord
Core-collapse supernovae, Massive stars, Red supergiant stars, Sky surveys
Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-225381 (URN)10.3847/1538-4357/ad06b6 (DOI)001132042000001 ()2-s2.0-85181149974 (Scopus ID)
Tillgänglig från: 2024-01-19 Skapad: 2024-01-19 Senast uppdaterad: 2024-01-19Bibliografiskt granskad
Irani, I., Chen, P., Morag, J., Schulze, S., Gal-Yam, A., Strotjohann, N. L., . . . Medford, M. S. (2024). SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material. Astrophysical Journal, 962(2), Article ID 109.
Öppna denna publikation i ny flik eller fönster >>SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material
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2024 (Engelska)Ingår i: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 962, nr 2, artikel-id 109Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected <1 day after the explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early-time spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high ionization C and O absorption features at velocities of 4000 km s−1, while its photospheric radius expands at 20,000 km s−1, indicating a pre-existing distribution of expanding C/O material. After ∼2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of ∼10,000 km s−1, in agreement with the evolution of the photospheric radius. The optical light curves reach a second peak at t ≈ 15 days. By t = 60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong Ca ii and [Ca ii] emission with no detectable [O i], marking this event as Ca-rich. The early behavior can be explained by 10−3M of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf–Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by both the interaction of the ejecta with the optically thin CSM and shock cooling (in the massive star scenario). The observations can be explained by CSM that is optically thick to X-ray photons, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from downscattered X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.

Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-226985 (URN)10.3847/1538-4357/ad04d7 (DOI)001159919400001 ()2-s2.0-85184936369 (Scopus ID)
Tillgänglig från: 2024-03-05 Skapad: 2024-03-05 Senast uppdaterad: 2024-03-05Bibliografiskt granskad
Coughlin, M. W., Sollerman, J. & Sharma, V. (2023). A Data Science Platform to Enable Time-domain Astronomy. Astrophysical Journal Supplement Series, 267(2), Article ID 31.
Öppna denna publikation i ny flik eller fönster >>A Data Science Platform to Enable Time-domain Astronomy
2023 (Engelska)Ingår i: Astrophysical Journal Supplement Series, ISSN 0067-0049, E-ISSN 1538-4365, Vol. 267, nr 2, artikel-id 31Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

SkyPortal is an open-source software package designed to discover interesting transients efficiently, manage follow-up, perform characterization, and visualize the results. By enabling fast access to archival and catalog data, crossmatching heterogeneous data streams, and the triggering and monitoring of on-demand observations for further characterization, a SkyPortal-based platform has been operating at scale for >2 yr for the Zwicky Transient Facility Phase II community, with hundreds of users, containing tens of millions of time-domain sources, interacting with dozens of telescopes, and enabling community reporting. While SkyPortal emphasizes rich user experiences across common front-end workflows, recognizing that scientific inquiry is increasingly performed programmatically, SkyPortal also surfaces an extensive and well-documented application programming interface system. From back-end and front-end software to data science analysis tools and visualization frameworks, the SkyPortal design emphasizes the reuse and leveraging of best-in-class approaches, with a strong extensibility ethos. For instance, SkyPortal now leverages ChatGPT large language models to generate and surface source-level human-readable summaries automatically. With the imminent restart of the next generation of gravitational-wave detectors, SkyPortal now also includes dedicated multimessenger features addressing the requirements of rapid multimessenger follow-up: multitelescope management, team/group organizing interfaces, and crossmatching of multimessenger data streams with time-domain optical surveys, with interfaces sufficiently intuitive for newcomers to the field. This paper focuses on the detailed implementations, capabilities, and early science results that establish SkyPortal as a community software package ready to take on the data science challenges and opportunities presented by this next chapter in the multimessenger era.

Nyckelord
Open source software, Astronomy software, Time domain astronomy
Nationell ämneskategori
Astronomi, astrofysik och kosmologi Datavetenskap (datalogi)
Identifikatorer
urn:nbn:se:su:diva-223401 (URN)10.3847/1538-4365/acdee1 (DOI)001041591800001 ()2-s2.0-85169024658 (Scopus ID)
Tillgänglig från: 2023-11-02 Skapad: 2023-11-02 Senast uppdaterad: 2023-11-02Bibliografiskt granskad
Levan, A. J., Malesani, D. B., Gompertz, B. P., Nugent, A. E., Nicholl, M., Oates, S. R., . . . Tanvir, N. R. (2023). A long-duration gamma-ray burst of dynamical origin from the nucleus of an ancient galaxy. Nature Astronomy, 7(8), 976-985
Öppna denna publikation i ny flik eller fönster >>A long-duration gamma-ray burst of dynamical origin from the nucleus of an ancient galaxy
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2023 (Engelska)Ingår i: Nature Astronomy, E-ISSN 2397-3366, Vol. 7, nr 8, s. 976-985Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

The majority of long-duration (>2 s) gamma-ray bursts (GRBs) arise from the collapse of massive stars, with a small proportion created from the merger of compact objects. Most of these systems form via standard stellar evolution pathways. However, a fraction of GRBs may result from dynamical interactions in dense environments. These channels could also contribute substantially to the samples of compact object mergers detected as gravitational wave sources. Here we report the case of GRB 191019A, a long GRB (a duration of T90 = 64.4 ± 4.5 s), which we pinpoint close (⪅100 pc projected) to the nucleus of an ancient (>1 Gyr old) host galaxy at z = 0.248. The lack of evidence for star formation and deep limits on any supernova emission disfavour a massive star origin. The most likely route for progenitor formation is via dynamical interactions in the dense nucleus of the host. The progenitor, in this case, could be a compact object merger. These may form in dense nuclear clusters or originate in a gaseous disc around the supermassive black hole. Identifying, to the best of our knowledge, a first example of a dynamically produced GRB demonstrates the role that such bursts may have in probing dense environments and constraining dynamical fractions in gravitational wave populations.

Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-221078 (URN)10.1038/s41550-023-01998-8 (DOI)001019740000004 ()2-s2.0-85162673864 (Scopus ID)
Tillgänglig från: 2023-09-25 Skapad: 2023-09-25 Senast uppdaterad: 2023-09-25Bibliografiskt granskad
Karamehmetoglu, E., Sollerman, J., Taddia, F., Barbarino, C., Feindt, U., Fremling, C., . . . Zapartas, E. (2023). A population of Type Ibc supernovae with massive progenitors Broad lightcurves not uncommon in (i)PTF. Astronomy and Astrophysics, 678, Article ID A87.
Öppna denna publikation i ny flik eller fönster >>A population of Type Ibc supernovae with massive progenitors Broad lightcurves not uncommon in (i)PTF
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2023 (Engelska)Ingår i: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 678, artikel-id A87Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

If high-mass stars (≳20 − 25 M) are the progenitors of stripped-envelope (SE) supernovae (SNe), their massive ejecta should lead to broad, long-duration lightcurves. Instead, literature samples of SE SNe have reported relatively narrow lightcurves corresponding to ejecta masses between 1 − 4 M that favor intermediate-mass progenitors (≲20 − 25 M). Working with an untargeted sample from a single telescope to better constrain their rates, we searched the Palomar Transient Factory (PTF) and intermediate-PTF (iPTF) sample of SNe for SE SNe with broad lightcurves. Using a simple observational marker of g- or r-band lightcurve stretch compared to a template to measure broadness, we identified eight significantly broader Type Ibc SNe after applying quantitative sample selection criteria. The lightcurves, broad-band colors, and spectra of these SNe are found to evolve more slowly relative to typical Type Ibc SNe, proportional with the stretch parameter. Bolometric lightcurve modeling and their nebular spectra indicate high ejecta masses and nickel masses, assuming radioactive decay powering. Additionally, these objects are preferentially located in low-metallicity host galaxies with high star formation rates, which may account for their massive progenitors, as well as their relative absence from the literature. Our study thus supports the link between broad lightcurves (as measured by stretch) and high-mass progenitor stars in SE SNe with independent evidence from bolometric lightcurve modeling, nebular spectra, host environment properties, and photometric evolution. In the first systematic search of its kind using an untargeted sample, we used the stretch distribution to identify a higher than previously appreciated fraction of SE SNe with broad lightcurves (∼13%). Correcting for Malmquist and lightcurve duration observational biases, we conservatively estimate that a minimum of ∼6% of SE SNe are consistent with high-mass progenitors. This result has implications for the progenitor channels of SE SNe, including late stages of massive stellar evolution, the origin of the observed oxygen fraction in the universe, and formation channels for stellar-mass black holes.

Nyckelord
supernovae: general, methods: statistical, surveys, methods: data analysis, techniques: photometric
Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-223850 (URN)10.1051/0004-6361/202245231 (DOI)001084587200004 ()2-s2.0-85175010454 (Scopus ID)
Tillgänglig från: 2023-11-20 Skapad: 2023-11-20 Senast uppdaterad: 2023-11-20Bibliografiskt granskad
Kool, E. C., Pearson Johansson, J., Sollerman, J., Moldón, J., Moriya, T. J., Mattila, S., . . . Stern, D. (2023). A radio-detected type Ia supernova with helium-rich circumstellar material. Nature, 617(7961), 477-482
Öppna denna publikation i ny flik eller fönster >>A radio-detected type Ia supernova with helium-rich circumstellar material
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2023 (Engelska)Ingår i: Nature, ISSN 0028-0836, E-ISSN 1476-4687, Vol. 617, nr 7961, s. 477-482Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

Type Ia supernovae (SNe Ia) are thermonuclear explosions of degenerate white dwarf stars destabilized by mass accretion from a companion star1, but the nature of their progenitors remains poorly understood. A way to discriminate between progenitor systems is through radio observations; a non-degenerate companion star is expected to lose material through winds2 or binary interaction3 before explosion, and the supernova ejecta crashing into this nearby circumstellar material should result in radio synchrotron emission. However, despite extensive efforts, no type Ia supernova (SN Ia) has ever been detected at radio wavelengths, which suggests a clean environment and a companion star that is itself a degenerate white dwarf star4,5. Here we report on the study of SN 2020eyj, a SN Ia showing helium-rich circumstellar material, as demonstrated by its spectral features, infrared emission and, for the first time in a SN Ia to our knowledge, a radio counterpart. On the basis of our modelling, we conclude that the circumstellar material probably originates from a single-degenerate binary system in which a white dwarf accretes material from a helium donor star, an often proposed formation channel for SNe Ia (refs. 6,7). We describe how comprehensive radio follow-up of SN 2020eyj-like SNe Ia can improve the constraints on their progenitor systems.

Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-223960 (URN)10.1038/s41586-023-05916-w (DOI)001078324200011 ()37198310 (PubMedID)2-s2.0-85159611552 (Scopus ID)
Tillgänglig från: 2023-11-24 Skapad: 2023-11-24 Senast uppdaterad: 2023-11-24Bibliografiskt granskad
Ho, A. Y. Q., Perley, D. A., Gal-Yam, A., Lunnan, R., Sollerman, J., Schulze, S., . . . Winters, J. M. (2023). A Search for Extragalactic Fast Blue Optical Transients in ZTF and the Rate of AT2018cow-like Transients. Astrophysical Journal, 949(2), Article ID 120.
Öppna denna publikation i ny flik eller fönster >>A Search for Extragalactic Fast Blue Optical Transients in ZTF and the Rate of AT2018cow-like Transients
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2023 (Engelska)Ingår i: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 949, nr 2, artikel-id 120Artikel i tidskrift (Refereegranskat) Published
Abstract [en]

We present a search for extragalactic fast blue optical transients (FBOTs) during Phase I of the Zwicky Transient Facility (ZTF). We identify 38 candidates with durations above half-maximum light 1 day < t (1/2) < 12 days, of which 28 have blue (g - r less than or similar to -0.2 mag) colors at peak light. Of the 38 transients (28 FBOTs), 19 (13) can be spectroscopically classified as core-collapse supernovae (SNe): 11 (8) H- or He-rich (Type II/IIb/Ib) SNe, 6 (4) interacting (Type IIn/Ibn) SNe, and 2 (1) H&He-poor (Type Ic/Ic-BL) SNe. Two FBOTs (published previously) had predominantly featureless spectra and luminous radio emission: AT2018lug (The Koala) and AT2020xnd (The Camel). Seven (five) did not have a definitive classification: AT 2020bdh showed tentative broad H alpha in emission, and AT 2020bot showed unidentified broad features and was 10 kpc offset from the center of an early-type galaxy. Ten (eight) have no spectroscopic observations or redshift measurements. We present multiwavelength (radio, millimeter, and/or X-ray) observations for five FBOTs (three Type Ibn, one Type IIn/Ibn, one Type IIb). Additionally, we search radio-survey (VLA and ASKAP) data to set limits on the presence of radio emission for 24 of the transients. All X-ray and radio observations resulted in nondetections; we rule out AT2018cow-like X-ray and radio behavior for five FBOTs and more luminous emission (such as that seen in the Camel) for four additional FBOTs. We conclude that exotic transients similar to AT2018cow, the Koala, and the Camel represent a rare subset of FBOTs and use ZTF's SN classification experiments to measure the rate to be at most 0.1% of the local core-collapse SN rate.

Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
urn:nbn:se:su:diva-218369 (URN)10.3847/1538-4357/acc533 (DOI)001001445700001 ()2-s2.0-85161632715 (Scopus ID)
Tillgänglig från: 2023-06-27 Skapad: 2023-06-27 Senast uppdaterad: 2023-06-27Bibliografiskt granskad
Organisationer
Identifikatorer
ORCID-id: ORCID iD iconorcid.org/0000-0003-1546-6615

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