The Exotic Eclipsing Nucleus of the Ring Planetary Nebula SuWt 2

SuWt 2 is a planetary nebula (PN) consisting of a bright ionized thin ring seen nearly edge-on, with much fainter bipolar lobes extending perpendicularly to the ring. It has a bright (12th magnitude) central star, too cool to ionize the PN, which we discovered in the early 1990s to be an eclipsing binary. Although it was anticipated that there would also be an optically faint, hot, ionizing star in the system, a spectrum from the International Ultraviolet Explorer (IUE) did not reveal a UV source. We present extensive ground-based photometry and spectroscopy of the central binary collected over the ensuing two decades, resulting in the determination that the orbital period of the eclipsing pair is 4.9 days, and that it consists of two nearly identical A1 V stars, each of mass ~2.7 M sun. The physical parameters of the A stars, combined with evolutionary tracks, show that both are in the short-lived "blue-hook" evolutionary phase that occurs between the main sequence and the Hertzsprung gap, and that the age of the system is about 520 Myr. One puzzle is that the stars' rotational velocities are different from each other, and considerably slower than synchronous with the orbital period. It is possible that the center-of-mass velocity of the eclipsing pair is varying with time, suggesting that there is an unseen third orbiting body in the system. We propose a scenario in which the system began as a hierarchical triple, consisting of a ~2.9 M sun star orbiting the close pair of A stars. Upon reaching the asymptotic giant branch stage, the primary engulfed the pair into a common envelope, leading to a rapid contraction of the orbit and catastrophic ejection of the envelope into the orbital plane. In this picture, the exposed core of the initial primary is now a white dwarf of ~0.7 M sun, orbiting the eclipsing pair, which has already cooled below the detectability possible by IUE at our derived distance of 2.3 kpc and a reddening of E(B - V) = 0.40. The SuWt 2 system may be destined to perish as a Type Ia supernova.

Evidence for chronic morbillivirus infection in the Mediterranean striped dolphin (Stenella coeruleoalba)

In the summer of 1990 an epizootic infection caused by a morbillivirus (DMV) killed several thousand striped dolphins (Stenella coeruleoalba) in the Mediterranean Sea. In 1991 and 1992 the epizootic reached Italian and Greek waters. The infection by DMV in the acute period of the epizootic caused encephalitis, pneumonia and depletion of lymph nodes. After 1990, the systemic infection apparently disappeared from the Catalonian coast, giving way to cases of chronic infection of the CNS. Dolphins that died between 1991 and May 1994 were necropsied, and investigated for lesions due to DMV, and for the presence of morbillivirus antigen in tissues. Encephalitis occurred in 6 dolphins in which DMV antigen was demonstrated in the CNS and which were without lesions or antigen in other, non-nervous tissues. Inflammatory lesions, gliosis, and DMV antigen decreased in density and amount from cerebral grey matter, through the thalamic areas to the medulla oblongata. The cerebellum was usually spared. Lesions consisted of non-suppurative encephalitis, with diffuse gliosis and glial nodules and neuronophagia, and loss of neurons. Perivascular cuffing of lymphocytes and plasma cells was present in the cerebral cortex and the white matter beneath the cortex. Multinucleate syncytia were not detected in any of the dolphins. The haemagglutinin of DMV was detected mainly in neurons in the cerebral cortical areas. There was no clear relationship between the presence and amount of DMV antigen and the density or chronicity of lesions. Viral inclusions were seen in haematoxylin and eosin stained sections in 3/6 dolphins, principally in the nucleus and the cytoplasm of neurons. In the immunoperoxidase stained sections, dense granular deposits of chromogen, similar to viral inclusions, were evident in all 6 dolphins. The change in the distribution of lesions and of DMV antigen, from systemic to localized in the CNS, and the clustering of systemic DMV infections in the first four months of the epizootic, giving rise to sporadic occurrence of local CNS infection in the subsequent four years, as well as the chronic nature of the CNS lesions, which closely resembles subacute sclerosing panencephalitis, strongly support the existence of a chronic morbillivirus infection in the striped dolphin, as a delayed consequence of the 1990 epizootic.

The nucleus of Comet 67P/Churyumov-Gerasimenko. A new shape model and thermophysical analysis

Context. Comet 67P/Churyumov-Gerasimenko is the target of the European Space Agency Rosetta spacecraft rendez-vous mission. Detailed physical characteristation of the comet before arrival is important for mission planning as well as providing a test bed for ground-based observing and data-analysis methods. Aims: To conduct a long-term observational programme to characterize the physical properties of the nucleus of the comet, via ground-based optical photometry, and to combine our new data with all available nucleus data from the literature. Methods: We applied aperture photometry techniques on our imaging data and combined the extracted rotational lightcurves with data from the literature. Optical lightcurve inversion techniques were applied to constrain the spin state of the nucleus and its broad shape. We performed a detailed surface thermal analysis with the shape model and optical photometry by incorporating both into the new Advanced Thermophysical Model (ATPM), along with all available Spitzer 8-24 μm thermal-IR flux measurements from the literature. Results: A convex triangular-facet shape model was determined with axial ratios b/a = 1.239 and c/a = 0.819. These values can vary by as much as 7% in each axis and still result in a statistically significant fit to the observational data. Our best spin state solution has Psid = 12.76137 ± 0.00006 h, and a rotational pole orientated at Ecliptic coordinates λ = 78°(±10°), β = + 58°(±10°). The nucleus phase darkening behaviour was measured and best characterized using the IAU HG system. Best fit parameters are: G = 0.11 ± 0.12 and HR(1,1,0) = 15.31 ± 0.07. Our shape model combined with the ATPM can satisfactorily reconcile all optical and thermal-IR data, with the fit to the Spitzer 24 μm data taken in February 2004 being exceptionally good. We derive a range of mutually-consistent physical parameters for each thermal-IR data set, including effective radius, geometric albedo, surface thermal inertia and roughness fraction. Conclusions: The overall nucleus dimensions are well constrained and strongly imply a broad nucleus shape more akin to comet 9P/Tempel 1, rather than the highly elongated or "bi-lobed" nuclei seen for comets 103P/Hartley 2 or 8P/Tuttle. The derived low thermal inertia of

ESO observations of the Nucleus of Rosetta Target 67P/C-G

Rosetta is ESA's new comet orbiter mission, launched in March 2004 and currently en route to Jupiter-family comet 67P/Churyumov-Gerasimenko. The probe will rendezvous with the comet in 2014 and remain in orbit around the nucleus for on-going detailed physical and compositional analysis. Pre-encounter observations of the target are important for characterization of the heliocentric light-curve behaviour and the physical properties of the nucleus, information that is critical for mission planning. The nucleus was first characterized using HST observations in 2003 (Lamy et al. 2006) and observed directly in May 2005 by ground based telescopes (Lowry et al. 2006) when it was at 5.6 AU from the Sun. An extensive database of nucleus observations have since been acquired, not only from large ground-based telescopes like the ESO VLT (Tubiana et al. 2008 & 2011), but also from Spitzer (Kelley et al. 2006 & 2009; Lamy et al. 2008).