A MULTI‐GENE ESTIMATE OF HIGHER‐LEVEL PHYLOGENETIC RELATIONSHIPS AMONG NIGHTJARS (AVES: CAPRIMULGIDAE)

ABSTRACT ∙ The higher‐level phylogenetic relationships of the nightjars and nighthawks (Caprimulgidae) have been challenging for traditional systematics due to their cryptic plumage and conservative morphology. We explored these relationships by combining two previously published molecular datasets with new data to generate a complete matrix (7,104 bp) of evolutionarily disparate sequence elements from four genes for 36 taxa. We analyzed each of the genes separately for base composition heterogeneity and heterozygosity. We analyzed the concatenated matrix in a likelihood framework using seven different partitioning schemes. As the number of subsets in a given partitioning scheme increased, tree length and likelihood score also increased; however, the branching topology was little affected by increasingly complex partitioning schemes. Our best maximum likelihood tree has increased bootstrap support at 13 of 30 ingroup nodes compared with previous analyses, a result likely due to doubling the length of the sequence data. Coalescent‐based species tree inference produced a tree congruent with all strongly supported nodes in the maximum likelihood tree. This topology agrees with previous molecular studies in identifying three small, early branching Old World genera (Eurostopodus, Lyncornis, and Gactornis) and four more speciose terminal clades, representing the New World nighthawks (genus Chordeiles) and three nightjar radiations centered in South America, Central America and the Old World, respectively. Increased node support across the tree reinforces a historical scenario with origins in the region surrounding the Indian Ocean, followed by diversification in the New World and subsequent recolonization and radiation in the Old World. Future work on this group should incorporate additional members of the genera Lyncornis and Eurostopodus, to determine which is the basal lineage of Caprimulgidae.RESUMEN ∙ Relaciones filogenéticas de más alto nivel de los atajacaminos (Aves: Caprimulgidae) en base a un análisis multigénico Las relaciones filogenéticas de más alto nivel de los atajacaminos y añaperos (Caprimulgidae) son un reto para la sistemática tradicional, debido a que el grupo posee morfología poco variable y plumajes crípticos. Exploramos relaciones filogenéticas en el grupo combinando dos conjuntos de datos moleculares ya publicados con nuevos datos. La matriz completa (7,104 bp) se generó con cuatro genes y 36 taxones, incluyendo marcadores con distintos modelos de evolución. Se examinó cada uno de los genes por separado para determinar heterocigosidad y heterogeneidad de la composición de bases. Se analizó la matriz concatenada en un marco de máxima verosimilitud utilizando siete particiones diferentes. La longitud de los árboles filogenéticos y su verosimilitud aumentaron a la par del número de subconjuntos en una partición particular; sin embargo, la topología del árbol varió poco entre particiones. En comparación con topologías publicadas, nuestro árbol de máxima verosimilitud tuvo mejor soporte para 13 de los 30 nodos internos, resultado que podría deberse al uso del doble de los datos de secuencias. El método de árboles de especies basado en coalescencia produjo una topología congruente con la obtenida por máxima verosimilitud. Esta topología concuerda con previos estudios moleculares, identificando tres pequeños géneros del Viejo Mundo como basales en la filogenia (Eurostopodus, Lyncornis y Gactornis), y cuatro clados terminales con más especies. Estos clados terminales representan los atajacaminos del Nuevo Mundo del género Chordeiles, y otras tres radiaciones de América del Sur, Central y del Viejo Mundo. Nuestros resultados sugieren un escenario histórico con orígenes del grupo en la región circundante al Océano Indico, seguido por la diversificación en las Américas y la posterior recolonización y radiación en el Viejo Mundo. Futuros estudios en este grupo deben incorporar miembros adicionales de los géneros Lyncornis y Eurostopodus, lo que permitirá estudiar cuál es el linaje basal de Caprimulgidae

Estudio comparativo de los nuevos anticoagulantes orales

El tratamiento anticoagulante con Antagonistas de la Vitamina K (AVK) es muy complejo. Los nuevos anticoagulantes orales han supuesto una alternativa a los fármacos inhibidores de la vitamina K, presentando un mayor margen terapéutico así como una menor variabilidad intrae interindividual. Por otra parte, pueden administrarse a dosis fijas sin necesidad de una monitorización tan estrecha como requieren los AVK. Los nuevos anticoagulantes orales se clasifican en dos grupos atendiendo a su mecanismo de acción: inhibidores directos del factor X activado (FXa) (rivaroxabán, apixabán y edoxabán) y un inhibidor directo de la trombina (dabigatrán). Se han finalizado con resultados positivos diversos ensayos de fase III en profilaxis del tromboembolismo venoso en cirugía ortopédica, tratamiento del tromboembolismo venoso, o prevención del ictus en pacientes con fibrilación auricular. Para establecer una dosificación adecuada de estos fármacos, dado que las pruebas de laboratorio disponibles no son precisas ni permiten conocer el grado de anticoagulación, es necesario considerar otros factores como las interacciones farmacológicas y el estado de la función renal de cada paciente. En el futuro, las preferencias del paciente y las características farmacológicas serán relevantes para optimizar el tratamiento. Por todo ello, estos nuevos fármacos representan un nuevo paradigma en el tratamiento anticoagulante, aportando grandes ventajas, pero no exentos de inconvenientes

Hubble Space Telescope imaging of η Carinae

We present new high spatial resolution observations of the material around η Carinae obtained with the Hubble Space Telescope Wide Field/Planetary Camera. The star η Carinae is one of the most massive and luminous stars in our Galaxy, and has been episodically expelling significant quantities of gas over the last few centuries. The morphology of the bright central nebulosity (the homunculus) indicates that it is a thin shell with very well defined edges, and is clumpy on 0".2 (~10^(16)cm) scales. An extension to the northeast of the star {NN/NS using Walborn's [ApJL, 204, L17 ( 1976)] nomenclature} appears to be a stellar jet and its associated bow shock. The bow shock is notable for an intriguing series of parallel linear features across its face. The S ridge and the W arc appear to be part of a "cap" of emission located to the SW and behind the star. Together, the NE jet and the SW cap suggest that the symmetry axis for the system runs NE-SW rather than SE-NW, as previously supposed. Overall, the data indicate that the material around the star may represent an oblate shell with polar blowouts, rather than a bipolar flow

Planetary camera observations of the central parsec of M32

Analysis of V band HST Planetary Camera images of the elliptical galaxy M32 shows that its nucleus is extremely dense and remains unresolved at even the HST diffraction limit. A combined approach of image deconvolution and model fitting is used to investigate the starlight distribution into limiting radii of 0".04 (0.14 pc at 700 kpc). The logarithmic slope of the brightness profile smoothly flattens from y= -1.2 at 3.4 pc to y= -0.5 at 0.34 pc; interior to this radius the profile is equally consistent with a singular µ(r)∝ r,^(-1/2) cusp or a small nonisothermal core with r_c<0.37 pc. The isophotes maintain constant ellipticity into tlle center, and there is no evidence for a central point source, disk, dust, or any other substructures. The cusp model implies central mass densities p_0 > 3 X 10^7 M_☉ pc^(-3) at the resolution limit and is consistent with a central M_• = 3 X 10^6 M_☉ black hole; the core model implies p_0≈4 X 10^6 M_☉ pc^(-3). From the viewpoint of long-term stability, we argue that a starlight cusp surrounding a central black hole is the more plausible interpretation of the observations. A core at the implied density and size without a black hole has a relaxation time of only ~7 X 10^7 yr and a short stellar oollision timescale implying wholesale stellar merging over the age of the universe. The core would be strongly vulnerable to collapse and concomitant runaway stellar merging. Collapse may lead to formation of a massive black hole in any case if it cannot be reversed by formation of a binary from high-mass merger products. Regardless of the ultimate fate of the core, however, structural evolution of the core will always be accompanied by strong evolution of the core population-the constant isophote shape and absence of a central color gradient appear to show that such evolution has not occurred. In contrast, the high velocities around a black hole imply long relaxation and stellar collision times for the cusp population compared to the age of the universe

Imaging of the gravitational lens system PG 1115+080 with the Hubble Space Telescope

This paper is the first of a series presenting observations of gravitational lenses and lens candidates, taken with the Wide Field/Planetary Camera (WFPC) of the Hubble Space Telescope (HST). We have resolved the gravitational lens system PG 1115 + 080 into four point sources and a red, extended object that is presumably the lens galaxy; we present accurate relative intensities, colors, and positions of the four images, and lower accuracy intensity and position of the lens galaxy, all at the epoch 1991.2. Comparison with earlier data shows no compelling evidence for relative intensity variations between the QSO components having so far been observed. The new data agree with earlier conclusions that the system is rather simple, and can be produced by the single observed galaxy. The absence of asymmetry in the HST images implies that the emitting region of the quasar itself has an angular radius smaller than about 10 milliarcsec (100 pc for H_0=50, q_0=0.5)

The core of the nearby S0 galaxy NGC 7457 imaged with the HST planetary camera

We have observed the nearby S0 galaxy NGC 7457 with the Planetary Camera of the Hubble Space Telescope. Spatial structure is observable at the diffraction-limited resolution of the 2.4 m HST primary despite the effects of spherical aberration. The central distribution of starlight appears consistent with a y ~ -1.0 power law for r 3 x 10^4 L_☉ pc^(-3) (V band). This is now the second densest core known after M32. From the ground, NGC 7457 resembles any number of unresolved elliptical galaxies, which suggests that compact dense cores may be common. The images of NGC 7457 demonstrate that HST can still provide unique and astrophysically interesting information on the central structure of galaxies

Ionization fronts and shocked flows - The structure of the Orion Nebula at 0".1

We present HST Wide-Field Camera images of a field in the Orion Nebula obtained in emission from [S II], Hβ, and [O II]. The morphology of the [S II] emission is markedly different from the other lines. While Hβ and [O II] are distributed fairly smoothly, [S II] is dominated by filamentary features with widths between 0".1 and 1" which sharply highlight ionization fronts moving into dense neutral material. These photoionization fronts act as probes of the structure of the cavity walls of this blister H II region. Their morphology indicates that while the surfaces into which they are moving are textured, subarcsecond clumps with high density contrast are uncommon. An exception is a bow shock-shaped ionization front seen along the face of a solar system-sized (0".6 = 270 AU) clump which is itself seen in extinction. The field contains a number of HH objects and related structures, many of which were previously recognized as such, but whose complex structure is revealed here by the resolution of HST. These include M42 HH 1, which is seen to be an intricate structure of knots and filaments with a head-tail morphology. M42 HH 2 shows structure from both the shocked cavity walls and the shocked atomic outflow. M42 HH 5-7 break into numerous condensations with an appearance reminiscent of HH 7-11. All objects with a bow shockshaped structure (i.e., M42 HH 1, 5, 7, and 10) show enhanced Hβ emission at the apex of the structure where the shock should be strongest. M42 HH 8 and 9 may be HH objects viewed face-on, or alternatively condensations photoionized by a nearby A or B star. Emission from [S II] traces shocks at the walls of an ionized jet apparently emanating from a star in a dark cloud. This cloud seen in extinction is coincident with H_2 Peak 1, which we propose is on the near side of the nebula