The supernova impostor PSN J09132750+7627410 and its progenitor

We report the results of our follow-up campaign of the supernova impostor PSN J09132750+7627410, based on optical data covering $\sim250\,\rm{d}$. From the beginning, the transient shows prominent narrow Balmer lines with P-Cygni profiles, with a blue-shifted absorption component becoming more prominent with time. Along the $\sim3\,\rm{months}$ of the spectroscopic monitoring, broad components are never detected in the hydrogen lines, suggesting that these features are produced in slowly expanding material. The transient reaches an absolute magnitude $M_r=-13.60\pm0.19\,\rm{mag}$ at maximum, a typical luminosity for supernova impostors. Amateur astronomers provided $\sim4\,\rm{years}$ of archival observations of the host galaxy, NGC 2748. The detection of the quiescent progenitor star in archival images obtained with the Hubble Space Telescope suggests it to be an $18-20$\msun white-yellow supergiant.Comment: 7 pages, 4 figures, supplemental material available in the source file. Accepted for publication on Astrophysical Journal Letter

SN 2013df, a double-peaked IIb supernova from a compact progenitor and an extended H envelope

Optical observations of the type IIb SN 2013df from a few days to about 250 days after explosion are presented. These observations are complemented with UV photometry taken by \textit{SWIFT} up to 60 days post-explosion. The double-peak optical light curve is similar to those of SNe 1993J and 2011fu although with different decline and rise rates. From the modelling of the bolometric light curve, we have estimated that the total mass of synthesised $^{56}$Ni in the explosion is $\sim0.1$ M$_{\odot}$, while the ejecta mass is $0.8-1.4$ M$_{\odot}$ and the explosion energy $0.4-1.2 \times 10^{51}$erg. In addition, we have estimated a lower limit to the progenitor radius ranging from $64-169$ $R_{\odot}$. The spectral evolution indicates that SN 2013df had a hydrogen envelope similar to SN 1993J ($\sim 0.2$ M$_{\odot}$). The line profiles in nebular spectra suggest that the explosion was asymmetric with the presence of clumps in the ejecta, while the [O\,{\sc i}] $\lambda$$\lambda$$6300$, $6364$ luminosities, may indicate that the progenitor of SN 2013df was a relatively low mass star ( $\sim 12-13$ M$_{\odot}$).Comment: 18 pages, 11 figures, 9 tables, accepted for publication in MNRA

Depresión en adultos mayores y su relación con la actividad física y sedentarismo en Talca, Chile

The population is aging rapidly and Talca is not immune to this demographic phenomenon. Aging leads to a progressive deterioration of all systems such as cardiovascular, osteo-articular, muscular and nervous. The objective of this work is to relate depression with physical activity and other sociodemographic variables. This study is correlational and cross-sectional. Self-employed adults aged 65 years and over were recruited from the urban sector of the city of Talca. Face-to-face interviews were conducted to obtain sociodemographic data and apply the GDS questionnaires for depression and the IPAQ for physical activity. The statistical package SPSS version 25.0 was used. The sample is made up of 100 AM (N = 100), with a mean age of 73.2 years. A depression prevalence of 21% (N = 21) was found, in both men and women, which is related to physical activity (r = -0.229 and p = 0.004), and educational level (p = 0.035). Our results are consistent with previous studies. It is concluded that vigorous physical activity is related to low levels of depression and vice versa, as well, older adults with a low educational level tend to present more depression than those with a higher educational level.La población envejece rápidamente y Talca no escapa a este fenómeno demográfico. El envejecimiento conlleva un deterioro progresivo de todos los sistemas como cardiovascular, osteo-articular, muscular y nervioso. El objetivo de este trabajo es relacionar la depresión con la actividad física y otras variables sociodemográficas. Este estudio es de tipo correlacional y de corte transversal. Se reclutaron adultos mayores de 65 años y más, autovalentes del sector urbano de la ciudad de Talca. Se realizaron entrevistas cara a cara para obetner datos sociodemográficos y aplicar los cuestionarios GDS para depresión y el IPAQ para actividad física. Se utilizó el paquete estadístico SPSS versión 25.0. La muestra la conforman 100 AM (N=100), con una media de edad de 73,2 años. Se encontró una prevalencia de depresión de 21% (N=21), tanto en hombres como en mujeres, que se relaciona con la actividad física (r=-0,229 y p=0,004), y el nivel educacional (p=0,035). Nuestros resultados son coincidentes con estudios previos. Se concluye que una actividad física vigorosa se relaciona con bajos niveles de depresión y viceversa, así también, adultos mayores con bajo nivel educacional tienden a presentar más depresión que aquellos con nivel educacional más alto

Massive stars exploding in a He-rich circumstellar medium - VIII. PSN J07285387+3349106, a highly reddened supernova Ibn

We present spectroscopic and photometric observations for the Type Ibn supernova (SN) dubbed PSN J07285387+3349106. Using data provided by amateur astronomers, we monitored the photometric rise of the SN to maximum light, occurred on 2015 February 18.8 UT (JD(max,V) = 2457072.0 +- 0.8). PSN J07285387+3349106 exploded in the inner region of an infrared luminous galaxy, and is the most reddened SN Ibn discovered so far. We apply multiple methods to derive the total reddening to the SN, and determine a total colour excess E(B-V)(tot) = 0.99 +- 0.48 mag. Accounting for the reddening correction, which is affected by a large uncertainty, we estimate a peak absolute magnitude of M(V) = -20.30 +- 1.50. The spectra are dominated by continuum emission at early phases, and He I lines with narrow P-Cygni profiles are detected. We also identify weak Fe III and N II features. All these lines show an absorption component which is blue-shifted by about 900-1000 km/s. The spectra also show relatively broad He I line wings with low contrast, which extend to above 3000 km/s. From about 2 weeks past maximum, broad lines of O I, Mg II and the Ca II near-infrared triplet are identified. The composition and the expansion velocity of the circumstellar material, and the presence of He I and alpha-elements in the SN ejecta indicate that PSN J07285387+3349106 was produced by the core-collapse of a stripped-envelope star. We suggest that the precursor was WNE-type Wolf-Rayet star in its dense, He-rich circumstellar cocoon.Comment: 12 pages, 7 figures, 2 tables. Accepted for publication in MNRA

Mixotrophic ciliate dynamics in two zones of a temperate and highly turbid estuary in South America, Argentina

La mixotrofía es una estrategia de alimentación por medio de la cual un organismo combina la autotrofia y la heterotrofia. La dinámica estacional de cinco ciliados mixótrofos comúnmente presentes en las aguas superficiales de la zona interna y media del estuario de Bahía Blanca, Argentina, rico en nutrientes, somero y con alta turbidez, se estudió mensualmente desde enero a diciembre de 2009. Se registraron los valores de temperatura, salinidad, turbidez y clorofila a, así como también la abundancia y biomasa de Strombidium capitatum, Strombidium acutum, Cyrtostrombidium sp., Lohmanniella oviformis y Tontonia appendiculariformis. La abundancia más alta de los mixótrofos se registró en el invierno en la zona interna, mientras que en la zona media del estuario la presencia de estos ciliados fue casi nula. La contribución más alta de clorofila proveniente de los mixótrofos a la clorofila a total fue 6% en la zona interna y 23% en la zona media (ambas estimaciones registradas en otoño). La baja abundancia de mixótrofos en la zona media del estuario durante el invierno, como usualmente es observado en otros sistemas costeros, podría ser explicada por una presión de pastoreo elevada en esta zona (control de tipo “top-down”) por parte de mesozooplancton (e.g., copépodos), en comparación con la zona interna. La floración secundaria del fitoplancton observada durante los últimos veranos, dominada por diatomeas de pequeño tamaño y fitoflagelados del nanoplancton, podría haber sustentado la alta abundancia de ciliados mixótrofos que se registró en la zona media en otoño y verano.Mixotrophy is a feeding strategy by which some organisms combine autrotrophic and heterotrophic activities. The seasonal dynamics of the five most common mixotrophic ciliates were studied monthly in surface layers of the inner and middle zone of the Bahía Blanca estuary, a nutrient-rich, shallow and highly turbid environment in Argentina, from January to December 2009. Temperature, salinity, turbidity and chlorophyll a were recorded, as well as the abundance and biomass of Strombidium capitatum, Strombidium acutum, Cyrtostrombidium sp., Lohmanniella oviformis and Tontonia appendiculariformis. The highest mixotrophic ciliate abundance was recorded during the austral winter (June-July) in the inner zone, meanwhile in the middle zone of the estuary the presence of these ciliates was almost null. The highest chlorophyll contribution derived from mixotrophic ciliates to total chlorophyll a ranged from 6% in the inner zone to 23% in the middle zone, both registered in autumn. The low abundance of mixotrophs in the middle zone of the estuary during the winter, as is usually observed in other coastal ecosystems, could be explained through a higher grazing pressure in this zone (top-down control) by mesozooplankton (e.g., copepods) in comparison to the inner zone. The secondary bloom of phytoplankton consistently observed during the last summers dominated by small sized diatoms and nanoplankton phytoflagelates, could have sustained the high abundance of mixotrophic ciliates registered in the middle zone in autumn and summer

Optical and near infrared observations of SN 2014ck: an outlier among the Type Iax supernovae

We present a comprehensive set of optical and near-infrared photometric and spectroscopic observations for SN 2014ck, extending from pre-maximum to six months later. These data indicate that SN 2014ck is photometrically nearly identical to SN 2002cx, which is the prototype of the class of peculiar transients named SNe Iax. Similar to SN 2002cx, SN 2014ck reached a peak brightness $M_B=-17.37 \pm 0.15$ mag, with a post-maximum decline-rate $\Delta m_{15} (B) = 1.76 \pm 0.15$ mag. However, the spectroscopic sequence shows similarities with SN 2008ha, which was three magnitudes fainter and faster declining. In particular, SN 2014ck exhibits extremely low ejecta velocities, $\sim 3000$ km s$^{-1}$ at maximum, which are close to the value measured for SN 2008ha and half the value inferred for SN 2002cx. The bolometric light curve of SN 2014ck is consistent with the production of $0.10^{+0.04}_{-0.03} M_{\odot}$ of $^{56}$Ni. The spectral identification of several iron-peak features, in particular Co II lines in the NIR, provides a clear link to SNe Ia. Also, the detection of narrow Si, S and C features in the pre-maximum spectra suggests a thermonuclear explosion mechanism. The late-phase spectra show a complex overlap of both permitted and forbidden Fe, Ca and Co lines. The appearance of strong [Ca~II] $\lambda\lambda$7292, 7324 again mirrors the late-time spectra of SN 2008ha and SN 2002cx. The photometric resemblance to SN 2002cx and the spectral similarities to SN 2008ha highlight the peculiarity of SN 2014ck, and the complexity and heterogeneity of the SNe Iax class.Comment: MNRAS Accepted 2016 March 22. Received 2016 March

The multi-faceted Type II-L supernova 2014G from pre-maximum to nebular phase

We present multi-band ultraviolet, optical, and near-infrared photometry, along with visual-wavelength spectroscopy, of supernova (SN) 2014G in the nearby galaxy NGC 3448 (25 Mpc). The early-phase spectra show strong emission lines of the high ionisation species He II/N IV/C IV during the first 2-3 d after explosion, traces of a metal-rich CSM probably due to pre-explosion mass loss events. These disappear by day 9 and the spectral evolution then continues matching that of normal Type II SNe. The post-maximum light curve declines at a rate typical of Type II-L class. The extensive photometric coverage tracks the drop from the photospheric stage and constrains the radioactive tail, with a steeper decline rate than that expected from the $^{56}$Co decay if $\gamma$-rays are fully trapped by the ejecta. We report the appearance of an unusual feature on the blue-side of H$\alpha$ after 100 d, which evolves to appear as a flat spectral feature linking H$\alpha$ and the O I doublet. This may be due to interaction of the ejecta with a strongly asymmetric, and possibly bipolar CSM. Finally, we report two deep spectra at ~190 and 340 d after explosion, the latter being arguably one of the latest spectra for a Type II-L SN. By modelling the spectral region around the Ca II, we find a supersolar Ni/Fe production. The strength of the O I $\lambda\lambda$6300,6363 doublet, compared with synthetic nebular spectra, suggests a progenitor with a zero-age main-sequence mass between 15 and 19 M$_\odot$.Comment: 24 pages, 14 figure