First optical images of circumstellar dust surrounding the debris disk candidate HD 32297

Near-infrared imaging with the Hubble Space Telescope recently revealed a circumstellar dust disk around the A star HD 32297. Dust scattered light is detected as far as 400 AU radius and the linear morphology is consistent with a disk ~10 degrees away from an edge-on orientation. Here we present the first optical images that show the dust scattered light morphology from 560 to 1680 AU radius. The position angle of the putative disk midplane diverges by 31 degrees and the color of dust scattering is most likely blue. We associate HD 32297 with a wall of interstellar gas and the enigmatic region south of the Taurus molecular cloud. We propose that the extreme asymmetries and blue disk color originate from a collision with a clump of interstellar material as HD 32297 moves southward, and discuss evidence consistent with an age of 30 Myr or younger.Comment: 5 pages; Accepted for publication in ApJ Letter

Surprisingly Little O VI Emission Arises in the Local Bubble

This paper reports the first study of the O VI resonance line emission (1032, 1038 Angstroms) originating in the Local Bubble (or Local Hot Bubble) surrounding the solar neighborhood. In spite of the fact that O VI absorption within the Local Bubble has been observed, no resonance line emission was detected during our 230 ksec Far Ultraviolet Spectroscopic Explorer observation toward a ``shadowing'' filament in the southern Galactic hemisphere. As a result, tight 2 sigma upper limits are set on the intensities in the 1032 and 1038 Angstrom emission lines: 500 and 530 photons cm^{-2} s^{-1} sr^{-1}, respectively. These values place strict constraints on models and simulations. They suggest that the O VI-bearing plasma and the X-ray emissive plasma reside in distinct regions of the Local Bubble and are not mixed in a single plasma, whether in equilibrium with T ~ 10^6 K or highly overionized with T ~ 4 to 6 x 10^4 K. If the line of sight intersects multiple cool clouds within the Local Bubble, then the results also suggest that hot/cool transition zones differ from those in current simulations. With these intensity upper limits, we establish limits on the electron density, thermal pressure, pathlength, and cooling timescale of the O VI-bearing plasma in the Local Bubble. Furthermore, the intensity of O VI resonance line doublet photons originating in the Galactic thick disk and halo is determined (3500 to 4300 photons cm^{-2} s^{-1} sr^{-1}), and the electron density, thermal pressure, pathlength, and cooling timescale of its O VI-bearing plasma are calculated. The pressure in the Galactic halo's O VI-bearing plasma (3100 to 3800 K cm^{-3}) agrees with model predictions for the total pressure in the thick disk/lower halo. We also report the results of searches for other emission lines.Comment: accepted by ApJ, scheduled for May 2003, replacement astro-ph submission corrects typos and grammatical errors in original versio

Optimizing the sensitivity of high repetition rate broadband transient optical spectroscopy with modified shot-to-shot detection

A major limitation of transient optical spectroscopy is that relatively high laser fluences are required to enable broadband, multichannel detection with acceptable signal-to-noise levels. Under typical experimental conditions, many condensed phase and nanoscale materials exhibit fluence dependent dynamics, including higher order effects such as carrier-carrier annihilation. With the proliferation of commercial laser systems, offering both high repetition rates and high pulse energies, has come new opportunities for high sensitivity pump-probe measurements at low pump fluences. However, experimental considerations needed to fully leverage the statistical advantage of these laser systems has not been fully described. Here we demonstrate a high repetition rate, broadband transient spectrometer capable of multichannel shot-to-shot detection at 90 kHz. Importantly, we find that several high-speed cameras exhibit a time-domain fixed pattern noise resulting from interleaved analog-to-digital converters that is particularly detrimental to the conventional "ON/OFF" modulation scheme used in pump-probe spectroscopy. Using a modified modulation and data processing scheme, we achieve a noise level of $10^{-5}$ OD for an integration time of four seconds, an order of magnitude lower than for commercial 1 kHz transient spectrometers. We leverage the high sensitivity of this system to measure the differential transmission of monolayer graphene at low pump fluence. We show that signals on the order of $10^{-6}$ OD can be measured, enabling a new data acquisition regime for low dimensional materials

The Millennium Arecibo 21-CM Absorption Line Survey. II. Properties of the Warm and Cold Neutral Media

We use the Gaussian-fit results of Paper I to investigate the properties of interstellar HI in the Solar neighborhood. The Warm and Cold Neutral Media (WNM and CNM) are physically distinct components. The CNM spin temperature histogram peaks at about 40 K. About 60% of all HI is WNM. At z=0, we derive a volume filling fraction of about 0.50 for the WNM; this value is very rough. The upper-limit WNM temperatures determined from line width range upward from about 500 K; a minimum of about 48% of the WNM lies in the thermally unstable region 500 to 5000 K. The WNM is a prominent constituent of the interstellar medium and its properties depend on many factors, requiring global models that include all relevant energy sources, of which there are many. We use Principal Components Analysis, together with a form of least squares fitting that accounts for errors in both the independent and dependent parameters, to discuss the relationships among the four CNM Gaussian parameters. The spin temperature T_s and column density N(HI) are, approximately, the two most important eigenvectors; as such, they are sufficient, convenient, and physically meaningful primary parameters for describing CNM clouds. The Mach number of internal macroscopic motions for CNM clouds is typically 2.5, but there are wide variations. We discuss the historical tau-T_s relationship in some detail and show that it has little physical meaning. We discuss CNM morphology using the CNM pressure known from UV stellar absorption lines. Knowing the pressure allows us to show that CNM structures cannot be isotropic but instead are sheetlike, with length-to-thickness aspect ratios ranging up to about 280. We present large-scale maps of two regions where CNM lies in very large ``blobby sheets''.Comment: Revised submission to Ap.J. Changes include: (1) correction of turbulent Mach number in equation 16 and figure 12; the new typical value is 1.3 versus the old, incorrect value 2.5. (2) smaller typeface for the astro-ph version to conserve paper. 60 pages, 16 figure

Effect of tillage and cover on runoff and soil losses in the central region of Buenos Aires province

El objetivo de este trabajo fue evaluar a campo la efectividad de diferentes tipos de labranzas junto con distintos grados de cobertura vegetal (CV) del suelo sobre el escurrimiento (E) y la pérdida de suelo (Ps). Se seleccionaron 34 sitios experimentales bajo labranza tradicional (LT) y siembra directa (SD), con diferentes niveles de CV (C1- < 49, C2- 50-79% y C3- > 80%). Se utilizó un diseño experimental completamente aleatorizado con 4 tratamientos y desigual número de repeticiones: 1) SD-C3, 2) LT-C3, 3) LT-C2, y 4) LT-C1, resultante de combinar el tipo de labranza con CV. Se realizó un ANOVA (p ≤ 0,05) y un análisis de contrastes ortogonales: 1) SD-C3 vs LT-C3, 2) LT-C1 vs LT-C2, y 3) C3 vs LT-C2+C1. Al cabo de cada simulación de lluvia se obtuvo el E y Ps. Se determinó: contenido de materia orgánica (CMO), contenido hídrico (CH) y densidad aparente del suelo (DA) en los 10 cm superficiales, y la pendiente (P) del terreno. La LT presentó mayor E y Ps en todos tratamientos evaluados respecto de SD. El mayor E (26,8 mm) se registró en LT-C2, y el menor (0,5 mm) en SD-C3. La Ps mostró igual tendencia que el E con 11,6 y 0,1 g respectivamente. Los contrastes mostraron E estadísticamente diferentes para los tres contrastes, mientras la Ps fue estadísticamente diferente en los contrastes Nº 2 y 3. Escurrimiento y Ps se correlacionaron entre sí (R2 = 0,98) y con P (R2 = 0,83 y 0,72 respectivamente). Los resultados obtenidos demuestran la importancia del efecto protector de la CV del suelo. Sin embargo, el CMO y CH, y la P y DA deben ser considerados también en el proceso de E - erosión del suelo.The objective of this work was evaluate on field the effectiveness of tillage and different grades of soil cover (CV) on runoff (E) and soil losses (Ps). Thirty four experimental sites on conventional tillage (LT) and no-till (SD) with CV levels (C1- < 49, C2- 50-79% y C3- > 80%) were selected. A randomized completely experimental design was used, with 4 treatments and unequal repetition numbers: 1) SD-C3, 2) LT-C3, 3) LT-C2, y 4) LT-C1, which resulted of combination of tillage and CV. An ANVA (p ≤ 0.05) and orthogonal contrast analysis were carried out: 1) SD-C3 vs LT-C3, 2) LT-C1 vs LT-C2, y 3) C3 vs LT-C2+C1. Runoff and Ps were obtained when each simulate event finished. Soil organic matter (CMO), water content (CH) and soil bulk density (DA) on 10 cm top soil, and land slope were determined. Runoff and Ps always were higher on CT than SD. LT-C2 had the highest R (26.8 mm) and SD-C3 had the smallest R (0.5 mm). Soil loss showed the same tend than E with 11.6 y 0.1 g respectively. The three orthogonal contrast show E statistically different and Ps was in the contrasts Nº 2 and 3. Runoff and Ps were correlated between the two of them (R2 = 0.98), and with P (R2 = 0.83 y 0.72 respectively). Results show the important protective effect of soil CV. However, CMO, CH, P y DA should be considered in the E - soil erosion process.Fil: Crespo, Roberto J.. Universidad Nacional del Centro de la Provincia de Buenos Aires. Facultad de AgronomíaFil: Ares, Guadalupe. Universidad Nacional del Centro de la Provincia de Buenos Aires. Facultad de AgronomíaFil: Sfeir, Alberto. Universidad Nacional del Centro de la Provincia de Buenos Aires. Facultad de AgronomíaFil: Wingeyer, Ana B.. University of Nebraska-Lincoln. Department of Agronomy and Horticulture.Fil: Usunoff, Eduardo

Variations in D/H and D/O from New FUSE Observations

We use data obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) to determine the interstellar abundances of DI, NI, OI, FeII, and H2 along the sigh tlines to WD1034+001, BD+393226, and TD132709. Our main focus is on determining the D/H, N/H, O/H, and D/O ratios along these sightlines, with log N(H) > 20.0, that probe gas well outside of the Local Bubble. Hubble Space Telescope (HST) and International Ultraviolet Explorer (IUE) archival data are used to determine the HI column densities along the WD1034+001 and TD132709 sightlines, respectively. For BD+393226, a previously published N(HI) is used. We find (D/H)x10^5 = 2.14 + 0.53 - 0.45, 1.17 + 0.31 - 0.25, and 1.86 + 0.53 - 0.43, and (D/O)x10^2 = 6.31 + 1.79 - 1.38, 5.62 + 1.61 - 1.31, and 7.59 + 2.17 - 1.76, for the WD1034+001, BD+393226, and TD132709 sightlines, respectively (all 1 si gma). The scatter in these three D/H ratios exemplifies the scatter that has been found by other authors for sightlines with column densities in the range 19.2 < log N(H) < 20.7. The D/H ratio toward WD1034+001 and all the D/O ratios derived here are inconsistent with the Local Bubble value and are some of the highest in the literature. We discuss the implications of our measurements for the determination of the present-epoch abundance of deuterium, and for the different scenarios that try to explain the D/H variations. We present a study of D/H as a function of the average sightline gas density, using the ratios derived in this work as well as ratios from the literature, which suggests that D/H decreases with increasing gas volume density. Similar behaviors by other elements such Fe and Si have been interpreted as the result of depletion into dust grains.Comment: Accepted for publication in the Ap

Intérêt des huiles essentielles dans les angines à Streptococcus pyogenes

Pharmacists are increasingly being asked for advice in the area of aromatherapy. Their role consists in judging the relevance of this alternative therapy according to the pathological context and the patient. They must also assess which essential oils offer the best risk-benefit ratio. However, there are still insufficient scientific data relating to their properties

Discovery of Reflection Nebulosity Around Five Vega-like Stars

Coronagraphic optical observations of six Vega-like stars reveal reflection nebulosities, five of which were previously unknown. The nebulosities illuminated by HD 4881, HD 23362, HD 23680, HD 26676, and HD 49662 resemble that of the Pleiades, indicating an interstellar origin for dust grains. The reflection nebulosity around HD 123160 has a double-arm morphology, but no disk-like feature is seen as close as 2.5 arcsec from the star in K-band adaptive optics data. We demonstrate that uniform density dust clouds surrounding HD 23362, HD 23680 and HD 123160 can account for the observed 12-100 micron spectral energy distributions. For HD 4881, HD 26676, and HD 49662 an additional emission source, such as from a circumstellar disk or non-equilibrium grain heating, is required to fit the 12-25 micron data. These results indicate that in some cases, particularly for Vega-like stars located beyond the Local Bubble (>100 pc), the dust responsible for excess thermal emission may originate from the interstellar medium rather than from a planetary debris system.Comment: The Astrophysical Journal, in press for March, 2002 (32 pages, 13 figures

The D/H Ratio in the Interstellar Medium toward the White Dwarf PG0038+199

We determine the D/H ratio in the interstellar medium toward the DO white dwarf PG0038+199 using spectra from the Far Ultraviolet Spectroscopic Explorer (FUSE), with ground-based support from Keck HIRES. We employ curve of growth, apparent optical depth and profile fitting techniques to measure column densities and limits of many other species (H2, NaI, CI, CII, CIII, NI, NII, OI, SiII, PII, SIII, ArI and FeII) which allow us to determine related ratios such as D/O, D/N and the H2 fraction. Our efforts are concentrated on measuring gas-phase D/H, which is key to understanding Galactic chemical evolution and comparing it to predictions from Big Bang nucleosynthesis. We find column densities log N(HI) = 20.41+-0.08, log N(DI)=15.75+-0.08 and log N(H2) = 19.33+-0.04, yielding a molecular hydrogen fraction of 0.14+-0.02 (2 sigma errors), with an excitation temperature of 143+-5K. The high HI column density implies that PG0038+199 lies outside of the Local Bubble; we estimate its distance to be 297 (+164,-104)pc (1 sigma). D/[HI+2H2] toward PG0038+199 is 1.91(+0.52,-0.42) e-5 (2 sigma). There is no evidence of component structure on the scale of Delta v > 8 km/s based on NaI, but there is marginal evidence for structure on smaller scales. The D/H value is high compared to the majority of recent D/H measurements, but consistent with the values for two other measurements at similar distances. D/O is in agreement with other distant measurements. The scatter in D/H values beyond ~100pc remains a challenge for Galactic chemical evolution.Comment: 59 pages, 7 tables, 18 figures (1 standalone), accepted by ApJ v2 minor typos correcte

The Local Leo Cold Cloud and New Limits on a Local Hot Bubble

We present a multi-wavelength study of the local Leo cold cloud (LLCC), a very nearby, very cold cloud in the interstellar medium. Through stellar absorption studies we find that the LLCC is between 11.3 pc and 24.3 pc away, making it the closest known cold neutral medium cloud and well within the boundaries of the local cavity. Observations of the cloud in the 21-cm HI line reveal that the LLCC is very cold, with temperatures ranging from 15 K to 30 K, and is best fit with a model composed of two colliding components. The cloud has associated 100 micron thermal dust emission, pointing to a somewhat low dust-to-gas ratio of 48 x 10^-22 MJy sr^-1 cm^2. We find that the LLCC is too far away to be generated by the collision among the nearby complex of local interstellar clouds, but that the small relative velocities indicate that the LLCC is somehow related to these clouds. We use the LLCC to conduct a shadowing experiment in 1/4 keV X-rays, allowing us to differentiate between different possible origins for the observed soft X-ray background. We find that a local hot bubble model alone cannot account for the low-latitude soft X-ray background, but that isotropic emission from solar wind charge exchange does reproduce our data. In a combined local hot bubble and solar wind charge exchange scenario, we rule out emission from a local hot bubble with an 1/4 keV emissivity greater than 1.1 Snowdens / pc at 3 sigma, 4 times lower than previous estimates. This result dramatically changes our perspective on our local interstellar medium.Comment: 13 pages, 12 figures. Accepted for publication in the Astrophysical Journal. Vector figure version available at http://www.astro.columbia.edu/~jpeek