The Sentimental Virtuoso: Collecting Feeling in Henry Mackenzie’s The Man of Feeling

This article explains the ambiguities in Henry Mackenzie’s quasi-ironic sentimental novel, The Man of Feeling, by examining its debt to an earlier, formative literary tradition: the seventeenth-century character collection that features the caricatured antiquarian virtuoso. Character collections, exemplified by Samuel Butler’s Characters (mainly written between 1667 and 1669), constitute catalogues of ridiculed social and psychological types, prominent among whom are collector-characters derogated for antisocial self-absorption, arrogance, scopophilia, impotence, and credulity. As a sentimental novel, written in an era that highly valued sociability, The Man of Feeling reveals how this satiric inheritance complicates the praise of feeling. It reworks the structure and types of the character tradition and the figure of the antiquarian virtuoso by means of narrative frames that distance readers from the sentimental incidents; an episodic form that fractures sequential narrative; and rhetoric, themes, and characters that play on the opposition between materiality, idea, and feeling that informs the caricature of the antiquarian virtuoso. These features help to explain the ambiguity of the “man of feeling”: the sentimental virtuoso who both objectifies and personalizes a world of collectible experiences

Collecting Trouble: Sir Hans Sloane’s Literary Reputation in Eighteenth-Century Britain [pre-print]

This article argues that the shifts in the reputation of Sir Hans Sloane, the foremost British collector of the eighteenth century, reflect the changing reputation of collecting itself from the Restoration to the Regency. By examining the literary representations of Sloane in genres ranging from poetry to memoirs, it traces Sloane’s reputation in literary culture from that of a model physician and benefactor, to a charlatan, to a toyman, and finally, to an entrepreneur. These shifts reflect the challenges that collecting presented to culture: on the one hand, it threatened conventional valuations, and on the other, offered rich opportunities both for both self-advancement and the advancement of learning. Writers show that Sloane’s activities recast the natural world as a storehouse stuffed with collectibles and collecting as an ambiguous but national practice of imperialistic acquisition. At the same time, they find in Sloane and the fashion for collecting several dangers: it reflected the increasing power of objects to oust abstract concepts as the subjects of literary description, presented new modes of self-definition and sociability, and, above all, led to a transition from an idea of nature as full of wonders to one in which nature is a treasure-house of loot and knowledge. Whereas the Restoration had embraced the new definition of a scholar-collector as a gentleman who contributed to the public good, by the midcentury, collectors seemed self-absorbed and deluded. Yet, by the end of the century, collecting was considered laudable self-advancement. Things had changed, so that on 15 January 1759, when the British Museum opened for “study and public inspection,” Sloane, formerly a charlatan and a toyman, stood as the noble exemplar of the collector and the father of a new British identity

Interferometric Astrometry of the Low-mass Binary Gl 791.2 (= HU Del) Using Hubble Space Telescope Fine Guidance Sensor 3: Parallax and Component Masses

With fourteen epochs of fringe tracking data spanning 1.7y from Fine Guidance Sensor 3 we have obtained a parallax (pi_abs=113.1 +- 0.3 mas) and perturbation orbit for Gl 791.2A. Contemporaneous fringe scanning observations yield only three clear detections of the secondary on both interferometer axes. They provide a mean component magnitude difference, Delta V = 3.27 +- 0.10. The period (P = 1.4731 yr) from the perturbation orbit and the semi-major axis (a = 0.963 +- 0.007 AU) from the measured component separations with our parallax provide a total system mass M_A + M_B = 0.412 +- 0.009 M_sun. Component masses are M_A=0.286 +- 0.006 M_sun and M_B = 0.126 +- 0.003 M_sun. Gl 791.2A and B are placed in a sparsely populated region of the lower main sequence mass-luminosity relation where they help define the relation because the masses have been determined to high accuracy, with errors of only 2%.Comment: 19 pages, 5 figures. The paper is to appear in August 2000 A

Modeling Multi-Wavelength Stellar Astrometry. I. SIM Lite Observations of Interacting Binaries

Interacting binaries consist of a secondary star which fills or is very close to filling its Roche lobe, resulting in accretion onto the primary star, which is often, but not always, a compact object. In many cases, the primary star, secondary star, and the accretion disk can all be significant sources of luminosity. SIM Lite will only measure the photocenter of an astrometric target, and thus determining the true astrometric orbits of such systems will be difficult. We have modified the Eclipsing Light Curve code (Orosz & Hauschildt 2000) to allow us to model the flux-weighted reflex motions of interacting binaries, in a code we call REFLUX. This code gives us sufficient flexibility to investigate nearly every configuration of interacting binary. We find that SIM Lite will be able to determine astrometric orbits for all sufficiently bright interacting binaries where the primary or secondary star dominates the luminosity. For systems where there are multiple components that comprise the spectrum in the optical bandpass accessible to SIM Lite, we find it is possible to obtain absolute masses for both components, although multi-wavelength photometry will be required to disentangle the multiple components. In all cases, SIM Lite will at least yield accurate inclinations, and provide valuable information that will allow us to begin to understand the complex evolution of mass-transferring binaries. It is critical that SIM Lite maintains a multi-wavelength capability to allow for the proper deconvolution of the astrometric orbits in multi-component systems.Comment: 12 pages, 6 figures, 6 tables. Accepted for publication in the Astrophysical Journa

HST Fine Guidance Sensor Astrometric Parallaxes for Three Dwarf Novae: SS Aurigae, SS Cygni, and U Geminorum

We report astrometric parallaxes for three well known dwarf novae obtained using the Fine Guidance Sensors on the Hubble Space Telescope. We found a parallax for SS Aurigae of Pi = 5.00 +/- 0.64 mas, for SS Cygni we found Pi = 6.02 +/- 0.46 mas, and for U Geminorum we obtained Pi = 10.37 +/- 0.50 mas. These represent the first true trigonometric parallaxes of any dwarf novae. We briefly compare these results with previous distance estimates. This program demonstrates that with a very modest amount of HST observing time, the Fine Guidance Sensors can deliver parallaxes of unrivaled precision.Comment: 15 pages, 2 Table

The Extrasolar Planet epsilon Eridani b - Orbit and Mass

Hubble Space Telescope observations of the nearby (3.22 pc), K2 V star epsilon Eridani have been combined with ground-based astrometric and radial velocity data to determine the mass of its known companion. We model the astrometric and radial velocity measurements simultaneously to obtain the parallax, proper motion, perturbation period, perturbation inclination, and perturbation size. Because of the long period of the companion, \eps b, we extend our astrometric coverage to a total of 14.94 years (including the three year span of the \HST data) by including lower-precision ground-based astrometry from the Allegheny Multichannel Astrometric Photometer. Radial velocities now span 1980.8 -- 2006.3. We obtain a perturbation period, P = 6.85 +/- 0.03 yr, semi-major axis, alpha =1.88 +/- 0.20 mas, and inclination i = 30.1 +/- 3.8 degrees. This inclination is consistent with a previously measured dust disk inclination, suggesting coplanarity. Assuming a primary mass M_* = 0.83 M_{\sun}, we obtain a companion mass M = 1.55 +/- 0.24 M_{Jup}. Given the relatively young age of epsilon Eri (~800 Myr), this accurate exoplanet mass and orbit can usefully inform future direct imaging attempts. We predict the next periastron at 2007.3 with a total separation, rho = 0.3 arcsec at position angle, p.a. = -27 degrees. Orbit orientation and geometry dictate that epsilon Eri b will appear brightest in reflected light very nearly at periastron. Radial velocities spanning over 25 years indicate an acceleration consistent with a Jupiter-mass object with a period in excess of 50 years, possibly responsible for one feature of the dust morphology, the inner cavity