Comparación de las macroalgas epizóicas de la madreperla Pinctada mazatlanica (Hanley 1856) con las de fondos rocosos en la bahía de La Paz, Baja California Sur, México

El presente estudio describe la comunidad de macroalgas epizóicas de Pinctada mazatlanica y la compara con la del substrato rocoso. Colectamos un total de 36 muestras de la comunidad de macroalgas, 18 muestras sobre ostras y otras tantas sobre substrato rocoso en la Península San Juan Nepomuceno, bahía de La Paz, México. Las algas fueron colectadas mediante buceo SCUBA raspando las distintas superficies (25 cm2 de substrato rocoso). El tamaño de muestra fue ajustado por curva de acumulación de especies y expresado con un modelo polinomial. Comparamos las comunidades de algas con análisis multivariantes de similitud basados en el índice de Bray-Curtis, entre substratos, diferentes alturas de ostras perleras y profundidades. Encontramos 27 especies de algas epizóicas (15.4% Clorophyta, 3.8% Phaeophyta y 80.8% Rhodophyta) con una disimilitud de 71.16% con respecto al substrato rocoso. El dendrograma mostró tres agrupaciones de macroalgas en P. mazatlanica. El primero caracterizado por Chondria, Jania, Herposiphonia tenella y Gracilaria. El segundo compuesto por Jania, Polysiphonia acuminata, P. decusata y Spyridia filamentosa. El tercero constituido por Polysiphonia sp., Jania, Herposiphonia tenella, Ceramium canouii y Amphiroa sp. Estas agrupaciones y los talos filamentosos de las algas epizóicas corresponden a estados iniciales de sucesión.

NGC 7419 as a template for red supergiant clusters

Context. The open cluster NGC 7419 is known to contain five red supergiants and a very high number of Be stars. However, there are conflicting reports about its age and distance that prevent a useful comparison with other clusters. Aims. We intend to obtain more accurate parameters for NGC 7419, using techniques different from those of previous authors, so that it may be used as a calibrator for more obscured clusters. Methods. We obtained Strömgren photometry of the open cluster NGC 7419, as well as classification spectroscopy of ~20 stars in the area. We then applied standard analysis and classification techniques. Results. We find a distance of 4 ± 0.4 kpc and an age of 14 ± 2 Myr for NGC 7419. The main-sequence turn-off is found at spectral type B1, in excellent agreement. We identify 179 B-type members, implying that there are more than 1200 M⊙ in B stars at present. Extrapolating this to lower masses indicates an initial cluster mass of between 7000 and 10 000 M⊙, depending on the shape of the initial mass function. We find a very high fraction (≈40%) of Be stars around the turn-off, but very few Be stars at lower masses. We also report for the first time a strong variability in the emission characteristics of Be stars. We verified that the parameters of the red supergiant members can be used to obtain accurate cluster parameters. Conclusions. NGC 7419 is sufficiently massive to serve as a testbed for theoretical predictions and as a template to compare more obscured clusters. The distribution of stars above the main-sequence turn-off is difficult to accommodate with current evolutionary tracks. Though the presence of five red supergiants is marginally consistent with theoretical expectations, the high number of Be stars and very low number of luminous evolved B stars hint at some unknown physical factor that is not considered in current synthesis models.