20 research outputs found
Dieta e dispersão de sementes por Cerdocyon thous (Linnaeus) (CarnÃvora, Canidae), em um fragmento florestal no Paraná, Brasil Diet and seed dispersal by Cerdocyon thous (Linnaeus) in a forest fragment in Paraná (Carnivora, Canidae)
Embora o cachorro-do-mato, Cerdocyon thous (Linnaeus, 1706), seja um Canidae relativamente comum, não há muita informação sobre sua dieta e seu papel como dispersor de sementes nos diferentes habitats onde ocorre. O objetivo deste trabalho foi o de reportar a dieta de C. thous e sua importância como dispersor e/ou predador de sementes, e ainda testar a taxa de germinação de sementes após passar pelo trato digestório do animal. O estudo foi realizado em um fragmento (680 ha) de Floresta Estacional Semidecidual, o Parque Estadual Mata dos Godoy, localizado na cidade de Londrina, Paraná, sul do Brasil. A metodologia consistiu de coletas de fezes de C. thous, as quais foram analisadas em laboratório para identificar os itens consumidos. Nos testes de germinação, as sementes foram dispostas para germinar em placas de Petri com algodão umedecido em água. Noventa e três amostras fecais com 219 itens de origem vegetal e animal foram registradas, sendo 36,52% contendo restos de pequenos roedores, 24,19% de gramÃneas, 13,24% de aves, 10,47% de insetos, 6,39% de Syagrus romanzoffiana (Cham.) Glassm., 4,6% de outros itens de origem animal e 4,54% de outros itens de origem vegetal. Ainda, C. thous dispersou nove espécies de plantas, com relevante importância para a germinação de algumas sementes que passaram pelo trato digestório do animal, exceto para S. romanzoffiana, cujas sementes não germinaram nas condições de laboratório. Conclui-se que, C. thous apresentou uma dieta generalista e oportunista, sobrevivendo em áreas degradadas e antrópicas, e agindo como dispersor de sementes nestes locais.<br>Although the crab eating fox, Cerdocyon thous (Linnaeus, 1706), is a relatively common Canidae, there isn't much information about its diet and its role as a seed disperser in the different habitats where it occurs. The aim of this work was to report the diet of the C. thous and its importance as a seed disperser and / or a seed predator and to test the rate of germination of the seeds after passing through the digestive tract of the animal. The work was carried out in a 680 ha fragment of the Semidecidual Seasonal Forest in the Parque Estadual Mata dos Godoy, located in the city of Londrina-Paraná, south of Brazil. The methodology consisted of the collection of excrement of C. thous which were analyzed in laboratory for identification of consumed items and seeds. In germination tests, the seeds were placed to germinate in Petri dishes with wet cotton. Ninety-three animal feces samples, with 219 animal and vegetable items were registered, being 36.52% remaining portions of small rodents, 24.19% of grasses, 13.24% of birds, 10.47% of insects, 6.39% of Syagrus romanzoffiana (Cham.) Glassm., 4.6% of other items of animal origin and 4.54% of items vegetable origin. In addition, C. thous dispersed nine species of plants, with relevant importance to the germination of some seeds, which passed through the digestive tract, except for the most consumed of fruit, S. romanzoffiana, whith no seed germination at all in lab conditions. In conclusion, C. thous has a generalistc and opportunistc diet, surviving in degraded and anthropic areas and being able to act as a seed disperser
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Constraining the Progenitor System of the Type Ia Supernova 2021aefx
We present high-cadence optical and ultraviolet light curves of the normal Type Ia supernova (SN) 2021aefx, which shows an early bump during the first two days of observation. This bump may be a signature of interaction between the exploding white dwarf and a nondegenerate binary companion, or it may be intrinsic to the white dwarf explosion mechanism. In the case of the former, the short duration of the bump implies a relatively compact main-sequence companion star, although this conclusion is viewing-angle dependent. Our best-fit companion-shocking and double-detonation models both overpredict the UV luminosity during the bump, and existing nickel-shell models do not match the strength and timescale of the bump. We also present nebular spectra of SN 2021aefx, which do not show the hydrogen or helium emission expected from a nondegenerate companion, as well as a radio nondetection that rules out all symbiotic progenitor systems and most accretion disk winds. Our analysis places strong but conflicting constraints on the progenitor of SN 2021aefx; no current model can explain all of our observations. © 2022. The Author(s). Published by the American Astronomical Society.Open access journalThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]
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Shock Cooling and Possible Precursor Emission in the Early Light Curve of the Type II SN 2023ixf
We present the densely sampled early light curve of the Type II supernova (SN) 2023ixf, first observed within hours of explosion in the nearby Pinwheel Galaxy (Messier 101; 6.7 Mpc). Comparing these data to recently updated models of shock-cooling emission, we find that the progenitor likely had a radius of 410 ± 10 R ⊙. Our estimate is model dependent but consistent with a red supergiant. These models provide a good fit to the data starting about 1 day after the explosion, despite the fact that the classification spectrum shows signatures of circumstellar material around SN 2023ixf during that time. Photometry during the first day after the explosion, provided almost entirely by amateur astronomers, does not agree with the shock-cooling models or a simple power-law rise fit to data after 1 day. We consider the possible causes of this discrepancy, including precursor activity from the progenitor star, circumstellar interaction, and emission from the shock before or after it breaks out of the stellar surface. The very low luminosity (−11 mag > M > −14 mag) and short duration of the initial excess lead us to prefer a scenario related to prolonged emission from the SN shock traveling through the progenitor system. © 2023. The Author(s). Published by the American Astronomical Society.Open access journalThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]
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Evidence of Weak Circumstellar Medium Interaction in the Type II SN 2023axu
We present high-cadence photometric and spectroscopic observations of SN 2023axu, a classical Type II supernova with an absolute V-band peak magnitude of -17.2 ± 0.1 mag. SN 2023axu was discovered by the Distance Less Than 40 Mpc (DLT40) survey within 1 day of the last nondetection in the nearby galaxy NGC 2283 at 13.7 Mpc. We modeled the early light curve using a recently updated shock cooling model that includes the effects of line blanketing and found the explosion epoch to be MJD 59971.48 ± 0.03 and the probable progenitor to be a red supergiant. The shock cooling model underpredicts the overall UV data, which point to a possible interaction with circumstellar material. This interpretation is further supported by spectral behavior. We see a ledge feature around 4600 Å in the very early spectra (+1.1 and +1.5 days after the explosion), which can be a sign of circumstellar interaction. The signs of circumstellar material are further bolstered by the presence of absorption features blueward of Hα and Hβ at day >40, which is also generally attributed to circumstellar interaction. Our analysis shows the need for high-cadence early photometric and spectroscopic data to decipher the mass-loss history of the progenitor. © 2024. The Author(s). Published by the American Astronomical Society.Open access journalThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]
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The Early Light Curve of SN 2023bee: Constraining Type Ia Supernova Progenitors the Apian Way
We present very early photometric and spectroscopic observations of the Type Ia supernova (SN Ia) 2023bee, starting about 8 hr after the explosion, which reveal a strong excess in the optical and nearest UV (U and UVW1) bands during the first several days of explosion. This data set allows us to probe the nature of the binary companion of the exploding white dwarf and the conditions leading to its ignition. We find a good match to the Kasen model in which a main-sequence companion star stings the ejecta with a shock as they buzz past. Models of double detonations, shells of radioactive nickel near the surface, interaction with circumstellar material, and pulsational delayed detonations do not provide good matches to our light curves. We also observe signatures of unburned material, in the form of carbon absorption, in our earliest spectra. Our radio nondetections place a limit on the mass-loss rate from the putative companion that rules out a red giant but allows a main-sequence star. We discuss our results in the context of other similar SNe Ia in the literature. © 2023. The Author(s). Published by the American Astronomical Society.Open access journalThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]
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SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova
We present five far- and near-ultraviolet spectra of the Type II plateau supernova, SN 2022acko, obtained 5, 6, 7, 19, and 21 days after explosion, all observed with the Hubble Space Telescope/Space Telescope Imaging Spectrograph. The first three epochs are earlier than any Type II plateau supernova has been observed in the far-ultraviolet revealing unprecedented characteristics. These three spectra are dominated by strong lines, primarily from metals, which contrasts with the featureless early optical spectra. The flux decreases over the initial time series as the ejecta cool and line blanketing takes effect. We model this unique data set with the non-local thermodynamic equilibrium radiation transport code CMFGEN, finding a good match to the explosion of a low-mass red supergiant with energy E kin = 6 × 1050 erg. With these models we identify, for the first time, the ions that dominate the early ultraviolet spectra. We present optical photometry and spectroscopy, showing that SN 2022acko has a peak absolute magnitude of V = − 15.4 mag and plateau length of ∼115 days. The spectra closely resemble those of SN 2005cs and SN 2012A. Using the combined optical and ultraviolet spectra, we report the fraction of flux as a function of bluest wavelength on days 5, 7, and 19. We create a spectral time-series of Type II supernovae in the ultraviolet, demonstrating the rapid decline of flux over the first few weeks of evolution. Future observations of Type II supernovae are required to map out the landscape of exploding red supergiants, with and without circumstellar material, which is best revealed in high-quality ultraviolet spectra. © 2023. The Author(s). Published by the American Astronomical Society.Open access journalThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]