Dancing trees:Ovid's Metamorphoses and the imprint of pantomime dancing

This article argues that Ovid's arborization narratives in the Metamorphoses would have been more meaningful, enjoyable, and rich for imperial readers able to visualize them off the page, against the cultural back-cloth of the contemporary stage, that is to say, the pantomime stage, where arboreal transformations were part of the routine repertoire of the star dancers. Ovid's tales of tree-metamorphosis may well have been informed, even if subliminally, by his active recollection of or subconscious familiarity with real-life, danced choreographies for pantomimic transformations into trees.</p

‘Closing Up’ on Animal Metamorphosis::Ovid's Micro-choreographies in the Metamorphoses and the Corporeal Idioms of Pantomime Dancing

This article reads Ovid's Metamorphoses through the lens of its contemporary art of pantomime dancing. With a focus restricted to narratives of animalization, it argues that the dancer's exquisite bodily expressiveness has been co-opted and re-calibrated for the demands of the poetic medium, as Ovid's sequences of animal metamorphosis have amalgamated aesthetic strategies borrowed from the pantomime stage. Far from having been shaped exclusively within the literary mainstream, Ovid's idiosyncratic look, astonishingly perceptive and concentrated on the movements, gestures as well as the minutest parts of his characters' bodies, was the product of a bold, intermedial cross-over between poetry and dance

<i>Incredvlvs odi</i>:Horace and the subliterary aesthetic of the Augustan stage

Starting from the comparative standpoint of elite hostility to nineteenth-century British melodrama, this article posits pantomime's 'melodramatic' mode of exhibitionist excess as one of the missing links in the landscape against which Horace composed his Ars poetica. It suggests that lines 182-8 of the Ars that disapprove the display of death, violence and physical impossibilities on the tragic stage may be better understood as Horace's hostile response to pantomime's increasing prominence in Roman theatrical life, more precisely to the dislocation of 'horror' and 'marvel' from the realm of the 'heard' to that of the 'seen' favoured by the pantomime genre.</p

On Taking our Sources Seriously: Servius and the Theatrical Life of Vergil's Eclogues

This article revisits a famous staple of the Vergilian tradition, Servius's heavily contested scholion on the actress Volumnia Cytheris's theatrical rendition of Vergil's sixth Eclogue. By shifting the focus of inquiry from the strictly historical question 'did it happen?' it cuts through, identifies and disentangles a nexus of prejudices which have led to the devaluing of Servius's information. The sidelining or dismissal of this piece of evidence, I argue, has more to teach us about our own culturally entrenched and discipline-inherited assumptions than about what could have happened in late Republican Rome. Scrutiny of the evidence on the stage re-mediation of high poetry suggests it is entirely plausible that Cytheris would have performed a theatricalized version of Vergil's masterpiece. Indeed at the very heart of the story lies the convergence between élite poetry and the world of professional stage artists. Moreover, Cytheris's possible performance of a repertoire that coincides with the mythological core of pantomime dancing in its artistic maturity opens pivotal questions concerning what Plutarch (Mor.748a) aptly calls the “full association and mutual entanglement” between the arts of poetry and dance. Taking Servius seriously gives us the impetus to explore more decisively dimensions of Roman life that have been messily sidelined as a result of the systematic privileging of “texts” in our surveys of Roman intellectual landscapes over the centuries. Even if Servius's extract turned out to be no more than a “myth”, an “anecdote”, as such narratives go, this is an incredibly helpful one, provided we are willing to press it into the service of larger inquiries regarding the “circulation” of cultural energy between élite and popular culture.</p

MIPS: The Multiband Imaging Photometer for SIRTF

The Multiband Imaging Photometer for SIRTF (MIPS) is to be designed to reach as closely as possible the fundamental sensitivity and angular resolution limits for SIRTF over the 3 to 700μm spectral region. It will use high performance photoconductive detectors from 3 to 200μm with integrating JFET amplifiers. From 200 to 700μm, the MIPS will use a bolometer cooled by an adiabatic demagnetization refrigerator. Over much of its operating range, the MIPS will make possible observations at and beyond the conventional Rayleigh diffraction limit of angular resolution

Circular Polarization of Water Masers in the Circumstellar Envelopes of Late Type Stars

We present circular polarization measurements of circumstellar H_2O masers. The circular polarization detected in the (6_{16}-5_{23}) rotational transition of the H_{2}O maser can be attributed to Zeeman splitting in the intermediate temperature and density regime. The magnetic fields are derived using a general, LTE Zeeman analysis as well as a full radiative transfer method (non-LTE), which includes a treatment of all hyperfine components simultaneously as well as the effects of saturation and unequal populations of the magnetic substates. The differences and relevances of these interpretations are discussed extensively. The field strengths are compared with previous detections of the magnetic field on the SiO and OH masers. We show that the magnetic pressure dominates the thermal pressure by a factor of 20 or more.Comment: 15 pages, 15 figures; accepted for publication in A&A; (Abstract Abridged

A multi-transition submillimeter water maser study of evolved stars - detection of a new line near 475 GHz

Context: Maser emission from the H2O molecule probes the warm, inner circumstellar envelopes of oxygen-rich red giant and supergiant stars. Multi-maser transition studies can be used to put constraints on the density and temperature of the emission regions. Aims: A number of known H2O maser lines were observed toward the long period variables R Leo and W Hya and the red supergiant VY CMa. A search for a new, not yet detected line near 475 GHz was conducted toward these stars. Methods: The Atacama Pathfinder Experiment telescope was used for a multi-transition observational study of submillimeter H2O lines. Results: The 5_33-4_40 transition near 475 GHz was clearly detected toward VY CMa and W Hya. Many other H2O lines were detected toward all three target stars. Relative line intensity ratios and velocity widths were found to vary significantly from star to star. Conclusions: Maser action is observed in all but one line for which it was theoretically predicted. In contrast, one of the strongest maser lines, in R Leo by far the strongest, the 437 GHz 7_53-6_60 transition, is not predicted to be inverted. Some other qualitative predictions of the model calculations are at variance with our observations. Plausible reasons for this are discussed. Based on our findings for W Hya and VY CMa, we find evidence that the H2O masers in the AGB star W Hya arise from the regular circumstellar outflow, while shock excitation in a high velocity flow seems to be required to excite masers far from the red supergiant VY CMa.Comment: 9 pages, 4 figures, Astronomy and Astrophyics (in press

Disk Evolution in OB Associations - Deep Spitzer/IRAC Observations of IC 1795

We present a deep Spitzer/IRAC survey of the OB association IC 1795 carried out to investigate the evolution of protoplanetary disks in regions of massive star formation. Combining Spitzer/IRAC data with Chandra/ACIS observations, we find 289 cluster members. An additional 340 sources with an infrared excess, but without X-ray counterpart, are classified as cluster member candidates. Both surveys are complete down to stellar masses of about 1 Msun. We present pre-main sequence isochrones computed for the first time in the Spitzer/IRAC colors. The age of the cluster, determined via the location of the Class III sources in the [3.6]-[4.5]/[3.6] color-magnitude diagram, is in the range of 3 - 5 Myr. As theoretically expected, we do not find any systematic variation in the spatial distribution of disks within 0.6 pc of either O-type star in the association. However, the disk fraction in IC 1795 does depend on the stellar mass: sources with masses >2 Msun have a disk fraction of ~20%, while lower mass objects (2-0.8 Msun) have a disk fraction of ~50%. This implies that disks around massive stars have a shorter dissipation timescale.Comment: Accepted for publication in Ap

The Luminosity and Mass Functions of Low-Mass Stars in the Galactic Disk: I. The Calibration Region

We present measurements of the luminosity and mass functions of low-mass stars constructed from a catalog of matched Sloan Digital Sky Survey (SDSS) and 2 Micron All Sky Survey (2MASS) detections. This photometric catalog contains more than 25,000 matched SDSS and 2MASS point sources spanning ~30 square degrees on the sky. We have obtained follow-up spectroscopy, complete to J=16, of more than 500 low mass dwarf candidates within a 1 square degree sub-sample, and thousands of additional dwarf candidates in the remaining 29 square degrees. This spectroscopic sample verifies that the photometric sample is complete, uncontaminated, and unbiased at the 99% level globally, and at the 95% level in each color range. We use this sample to derive the luminosity and mass functions of low-mass stars over nearly a decade in mass (0.7 M_sun > M_* > 0.1 M_sun). We find that the logarithmically binned mass function is best fit with an M_c=0.29 log-normal distribution, with a 90% confidence interval of M_c=0.20--0.50. These 90% confidence intervals correspond to linearly binned mass functions peaking between 0.27 M_sun and 0.12 M_sun, where the best fit MF turns over at 0.17 M_sun. A power law fit to the entire mass range sampled here, however, returns a best fit of alpha=1.1 (where the Salpeter slope is alpha = 2.35). These results agree well with most previous investigations, though differences in the analytic formalisms adopted to describe those mass functions can give the false impression of disagreement. Given the richness of modern-day astronomical datasets, we are entering the regime whereby stronger conclusions can be drawn by comparing the actual datapoints measured in different mass functions, rather than the results of analytic analyses that impose structure on the data a priori. (abridged)Comment: Accepted for publication in the Astronomical Journal. 21 pages, emulateapj format, 12 figures. Figures 1, 4, 11 and 12 degraded for astroph; full resolution version available for download at http://www.cfa.harvard.edu/~kcovey