Synthesis of Compounds Related to Fluoranthene

Part 1a. The known 4-methylfluoranthene and 4-phenylfluoranthene have been synthesised by condensation of methyl and phenyl vinyl ketones, or the corresponding Mannich bases, methyl 2-morpholinoethyl ketone and 2-diethylaminoethyl phenyl ketone respectively, with methyl fluorene-9-carboxylate, followed by hydrolysis and decarboxylation, reduction, cyclisation, and dehydrogenation. Unsuccessful attempts to evolve a new synthesis of methyl fluorene-9-carboxylate were made. Part lb. 1:2:5:6-Dibenzpyracylene was synthesised by a crossed Ullmann reaction between 4-iodofluoranthene and 2-bromonitrobenzene, followed by reduction, diazotisation, and ring-closure. An attempt at synthesis by the method described in Part la failed. The ultra-violet absorption spectrum is reported and discussed, especially in relation to Clar's Anellation Theory. Part 2. 2:3-Benzfluoranthene has been synthesised from o-diphenylenephthalide by Clar's zinc dust-zinc chloride fusion method. An attempt to synthesise 2:3-benzfluoranthene by cyclisation of 9-bromo-9-o-bromo-o-tolylfluorene gave a compound believed, in the light of spectrographic and analytical evidence, to be 1:9-diphenylanthracene. The spectrum of 2:3-benzfluoranthene is reported and discussed, especially in relation to the Anellation Theory. Part 3. 3:4-Dimethylfluoranthene was obtained by the Grignard reaction on 4-keto-3-methyl-1:2:3:4-tetra-hydrofluoranthene, followed by dehydration-dehydrogenation. 2-Methoxyfluoranthene was synthesised by a crossed Ullmann reaction between 1-iodo-2-methoxynaphthalene and o-bromonitrobenzene, followed by reduction, diazotisation, and ring-closure. Part 4. The ultra-violet absorption spectra of several mono-, di-, and trimethylfluoranthenes, methoxy-fluoranthenes, and 4-phenylfluoranthene, not previously recorded, have been measured. They are shown to be of value in characterisation of the pure compounds. Distortion due to overlapping of the substituent methyl- or methoxyl- group with a hydrogen atom in the 2- or 10- substituted derivatives appears to produce corresponding distortions in the ultraviolet absorption curve

Earthshine as an Illumination Source at the Moon

Earthshine is the dominant source of natural illumination on the surface of the Moon during lunar night, and at locations within permanently shadowed regions that never receive direct sunlight. As such, earthshine may enable the exploration of areas of the Moon that are hidden from solar illumination. The heat flux from earthshine may also influence the transport and cold trapping of volatiles present in the very coldest areas. In this study, Earth's spectral radiance at the Moon is examined using a suite of Earth spectral models created using the Virtual Planetary Laboratory (VPL) three dimensional modeling capability. At the Moon, the broadband, hemispherical irradiance from Earth near 0 phase is approximately 0.15 watts per square meter, with comparable contributions from solar reflectance and thermal emission. Over the simulation timeframe, spanning two lunations, Earth's thermal irradiance changes less than a few mW per square meter as a result of cloud variability and the south-to-north motion of sub-observer position. In solar band, Earth's diurnally averaged light curve at phase angles < 60 degrees is well fit using a Henyey Greenstein integral phase function. At wavelengths > 0.7 microns, near the well known vegetation "red edge", Earth's reflected solar radiance shows significant diurnal modulation as a result of the longitudinal asymmetry in projected landmass, as well as from the distribution of clouds. A simple formulation with adjustable coefficients is presented for estimating Earth's hemispherical irradiance at the Moon as a function of wavelength, phase angle and sub-observer coordinates. It is demonstrated that earthshine is sufficiently bright to serve as a natural illumination source for optical measurements from the lunar surface.Comment: 27 pages, 15 figures, 1 tabl

Predictive Power of Strong Coupling in Theories with Large Distance Modified Gravity

We consider theories that modify gravity at cosmological distances, and show that any such theory must exhibit a strong coupling phenomenon, or else it is either inconsistent or is already ruled out by the solar system observations. We show that all the ghost-free theories that modify dynamics of spin-2 graviton on asymptotically flat backgrounds, automatically have this property. Due to the strong coupling effect, modification of the gravitational force is source-dependent, and for lighter sources sets in at shorter distances. This universal feature makes modified gravity theories predictive and potentially testable not only by cosmological observations, but also by precision gravitational measurements at scales much shorter than the current cosmological horizon. We give a simple parametrization of consistent large distance modified gravity theories and their predicted deviations from the Einsteinian metric near the gravitating sources.Comment: 12 pages, Latex, to be published in New Journal of Physic

Discovery and Characterization of a Caustic Crossing Microlensing Event in the SMC

We present photometric observations and analysis of the second microlensing event detected towards the Small Magellanic Cloud (SMC), MACHO Alert 98-SMC-1. This event was detected early enough to allow intensive observation of the lightcurve. These observations revealed 98-SMC-1 to be the first caustic crossing, binary microlensing event towards the Magellanic Clouds to be discovered in progress. Frequent coverage of the evolving lightcurve allowed an accurate prediction for the date of the source crossing out of the lens caustic structure. The caustic crossing temporal width, along with the angular size of the source star, measures the proper motion of the lens with respect to the source, and thus allows an estimate of the location of the lens. Lenses located in the Galactic halo would have a velocity projected to the SMC of v^hat ~1500 km/s, while an SMC lens would typically have v^hat ~60 km/s. We have performed a joint fit to the MACHO/GMAN data presented here, including recent EROS data of this event. These joint data are sufficient to constrain the time for the lens to move an angle equal to the source angular radius; 0.116 +/- 0.010 days. We estimate a radius for the lensed source of 1.4 +/- 0.1 R_sun. This yields a projected velocity of v^hat = 84 +/- 9 km/s. Only 0.15% of halo lenses would be expected to have a v^hat value at least as small as this, while 31% of SMC lenses would be expected to have v^hat as large as this. This implies that the lensing system is more likely to reside in the SMC than in the Galactic halo.Comment: 16 pages, including 3 tables and 3 figures; submitted to The Astrophysical Journa

Hole doping dependences of the magnetic penetration depth and vortex core size in YBa2Cu3Oy: Evidence for stripe correlations near 1/8 hole doping

We report on muon spin rotation measurements of the internal magnetic field distribution n(B) in the vortex solid phase of YBa2Cu3Oy (YBCO) single crystals, from which we have simultaneously determined the hole doping dependences of the in-plane Ginzburg-Landau (GL) length scales in the underdoped regime. We find that Tc has a sublinear dependence on 1/lambda_{ab}^2, where lambda_{ab} is the in-plane magnetic penetration depth in the extrapolated limits T -> 0 and H -> 0. The power coefficient of the sublinear dependence is close to that determined in severely underdoped YBCO thin films, indicating that the same relationship between Tc and the superfluid density is maintained throughout the underdoped regime. The in-plane GL coherence length (vortex core size) is found to increase with decreasing hole doping concentration, and exhibit a field dependence that is explained by proximity-induced superconductivity on the CuO chains. Both the magnetic penetration depth and the vortex core size are enhanced near 1/8 hole doping, supporting the belief by some that stripe correlations are a universal property of high-Tc cuprates.Comment: 12 pages, 13 figure

APOLLO: the Apache Point Observatory Lunar Laser-ranging Operation: Instrument Description and First Detections

A next-generation lunar laser ranging apparatus using the 3.5 m telescope at the Apache Point Observatory in southern New Mexico has begun science operation. APOLLO (the Apache Point Observatory Lunar Laser-ranging Operation) has achieved one-millimeter range precision to the moon which should lead to approximately one-order-of-magnitude improvements in the precision of several tests of fundamental properties of gravity. We briefly motivate the scientific goals, and then give a detailed discussion of the APOLLO instrumentation.Comment: 37 pages; 10 figures; 1 table: accepted for publication in PAS