252 research outputs found
Tools: Stuff: Art
Between 1890 and 1898 Erik Satie lived at 6 rue Cortot: âin a wardrobeâ. Satie was a collector [âŠ]. After his death his wardrobe was found to contain 84 handkerchiefs besides 12 identical velvet suits and dozens of umbrellas.
Trois morceaux en forme de poire [âŠ] three pieces in the form of a pear. The title of a piano piece in seven parts by Erik Satie. Satie composed this piece in response to Debussy's criticism that his works lacked a 'sense of form'. What exactly did Debussy mean by this? Where and what actually was this scene of formlessness?
The first part of the Paper will advance some possible reasoning behind Debussy's comments. Was Debussy questioning Satie's attitude to what Heidegger [in The Origin of the Work of Art] would term the 'thingly' element of the Work of Art, or more precisely â the relationship between 'things' and the 'thing in itself'?
Heidegger's contemplation of 'Form' and his writings on 'tools', 'material' and 'art', and the section dealing with the Temple provides an interesting locus in which to discus Debussy's comments.
The second section gives some ideas of how I reinterpreted this argument to produce a series of visual works inspired by another of Satie's works, Furniture Music â Musique d' ameublement, a piece of music that was not to be listened to.
Milhaud later recounted: âIt was no use Satie shouting: âTalk for heaven's sake! Move around! Don't listen!â They kept quiet. They listened. The whole thing went wrong.
The Luminosity of SN 1999by in NGC 2841 and the Nature of `Peculiar' Type Ia Supernovae
We present UBVRIJHK photometry and optical spectroscopy of the so-called
'peculiar' Type Ia supernova 1999by in NGC 2841. The observations began one
week before visual maximum light which is well-defined by daily observations.
The light curves and spectra are similar to those of the prototypical
subluminous event SN 1991bg. We find that maximum light in B occurred on 1999
May 10.3 UT (JD 2,451,308.8 +/- 0.3) with B=13.66 +/- 0.02 mag and a color of
B_max-V_max=0.51 +/- 0.03 mag. The late-time color implies minimal dust
extinction from the host galaxy. Our photometry, when combined with the recent
Cepheid distance to NGC 2841 (Macri et al. 2001), gives a peak absolute
magnitude of M_B=-17.15 +/- 0.23 mag, making SN 1999by one of the least
luminous Type Ia events ever observed. We estimate a decline rate parameter of
dm15(B)=1.90 mag, versus 1.93 for SN 1991bg, where 1.10 is typical for
so-called 'normal' events. We compare SN 1999by with other subluminous events
and find that the B_max-V_max color correlates strongly with the decline rate
and may be a more sensitive indicator of luminosity than the fading rate for
these objects. We find a good correlation between luminosity and the depth of
the spectral feature at 580 nm, which had been attributed solely to Si II. We
show that in cooler photospheres the 580 nm feature is dominated by Ti II,
which provides a simple physical explanation for the correlation. Using only
subluminous Type Ia supernovae we derive a Hubble parameter of H_0=75 +12 -11
km/s Mpc, consistent with values found from brighter events.Comment: 36 preprint pages including 18 figures. Near-IR photometry of the SN
has been added to the paper. Scheduled to appear in ApJ vol. 613 (September
2004). High-resolution version available from
http://www.nd.edu/~pgarnavi/sn99by/sn99by.p
Mapping High-velocity H-alpha and Lyman-alpha Emission from Supernova 1987A
We present new {\it Hubble Space Telescope} images of high-velocity
H- and Lyman- emission in the outer debris of SN~1987A. The
H- images are dominated by emission from hydrogen atoms crossing the
reverse shock. For the first time we observe emission from the reverse shock
surface well above and below the equatorial ring, suggesting a bipolar or
conical structure perpendicular to the ring plane. Using the H imaging,
we measure the mass flux of hydrogen atoms crossing the reverse shock front, in
the velocity intervals (7,500~~~~2,800 km s) and
(1,000~~~~7,500 km s), =
1.2~~10 M yr. We also present the first
Lyman- imaging of the whole remnant and new X-ray
observations. Comparing the spatial distribution of the Lyman- and
X-ray emission, we observe that the majority of the high-velocity
Lyman- emission originates interior to the equatorial ring. The
observed Lyman-/H- photon ratio, ~17, is significantly higher than the theoretically
predicted ratio of 5 for neutral atoms crossing the reverse shock
front. We attribute this excess to Lyman- emission produced by X-ray
heating of the outer debris. The spatial orientation of the Lyman- and
X-ray emission suggests that X-ray heating of the outer debris is the dominant
Lyman- production mechanism in SN 1987A at this phase in its evolution.Comment: 6 pages, 5 figures. ApJL - accepte
Analytic Inversion of Emission Lines of Arbitrary Optical Depth for the Structure of Supernova Ejecta
We derive a method for inverting emission line profiles formed in supernova
ejecta. The derivation assumes spherical symmetry and homologous expansion
(i.e., ), is analytic, and even takes account of occultation by
a pseudo-photosphere. Previous inversion methods have been developed which are
restricted to optically thin lines, but the particular case of homologous
expansion permits an analytic result for lines of {\it arbitrary} optical
depth. In fact, we show that the quantity that is generically retrieved is the
run of line intensity with radius in the ejecta. This result is
quite general, and so could be applied to resonance lines, recombination lines,
etc. As a specific example, we show how to derive the run of (Sobolev) optical
depth with radius in the case of a pure resonance scattering
emission line.Comment: 6 pages, no figures, to appear in Astrophysical Journal Letters,
requires aaspp4.sty to late
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