358 research outputs found
Production of linalool, cis- and trans-nerolidol, and trans,trans-farnesol by Saccharomyces fermentati growing as a film on simulated wine
Linalool, cis-nerolidol, trans-nerolidol, and trans,trans-farnesol are produced in low concentrations by the wine yeast Saccharomyces fermentati growing as a film for 10 weeks on the surface of a simulated fino sherry containing ethanol as the only volatile carbon containing compound. lt is not known whether Saccharomyces cerevisiae also produces terpenes while fermenting grape juice to wine. However, caution seems advisable in differentiating among Vitis vinifera cultivars on the basis of terpenes found in the wines.Die Bildung von Linalool, cis- und trans-Nerolidol sowie trans,trans-Farnesol durch eine Decke von Saccharomyces fermentati auf einem ModellweinDie deckenbildende Form von Saccharomyces fermentati erzeugte im Verlauf von 10 Wochen auf einem simulierten Fino-Sherry, der als einzige flĂŒchtige Kohlenstoffverbindung Ăthanol enthielt, geringe Mengen von Linalool, cis-Nerolidol, trans-Nerolidol und trans,trans-Farnesol. Es ist zwar nicht bekannt, ob Saccharomyces cerevisiae bei der VergĂ€rung von Traubensaft ebenfalls Terpene bildet; trotzdem scheint Vorsicht geboten zu sein, wenn Vitis-vinifera-Sorten aufgrund der in den Weinen gefundenen Terpene charakterisiert werden
Highly-Ionized High-Velocity Gas in the Vicinity of the Galaxy
We report the results of an extensive FUSE study of high velocity OVI
absorption along 102 complete sight lines through the Galactic halo. The high
velocity OVI traces a variety of phenomena, including tidal interactions with
the Magellanic Clouds, accretion of gas, outflow from the Galactic disk,
warm/hot gas interactions in a highly extended Galactic corona, and
intergalactic gas in the Local Group. We identify 85 high velocity OVI features
at velocities of -500 < v(LSR) < +500 km/s along 59 of the 102 sight lines.
Approximately 60% of the sky (and perhaps as much as 85%) is covered by high
velocity H+ associated with the high velocity OVI. Some of the OVI is
associated with known high velocity HI structures (e.g., the Magellanic Stream,
Complexes A and C), while some OVI features have no counterpart in HI 21cm
emission. The smaller dispersion in the OVI velocities in the GSR and LGSR
reference frames compared to the LSR is necessary (but not conclusive) evidence
that some of the clouds are extragalactic. Most of the OVI cannot be produced
by photoionization, even if the gas is irradiated by extragalactic background
radiation. Collisions in hot gas are the primary OVI ionization mechanism. We
favor production of some of the OVI at the boundaries between warm clouds and a
highly extended [R > 70 kpc], hot [T > 10^6 K], low-density [n < 10^-4 cm^-3]
Galactic corona or Local Group medium. A hot Galactic corona or Local Group
medium and the prevalence of high velocity OVI are consistent with predictions
of galaxy formation scenarios. Distinguishing between the various phenomena
producing high velocity OVI will require continuing studies of the distances,
kinematics, elemental abundances, and physical states of the different types of
high velocity OVI features found in this study. (abbreviated)Comment: 78 pages of text/tables + 31 figures, AASTeX preprint format. All
figures are in PNG format due to astro-ph space restrictions. Bound copies of
manuscript and two accompanying articles are available upon request.
Submitted to ApJ
A Catalogue of Field Horizontal Branch Stars Aligned with High Velocity Clouds
We present a catalogue of 430 Field Horizontal Branch (FHB) stars, selected
from the Hamburg/ESO Survey (HES), which fortuitously align with high column
density neutral hydrogen (HI) High-Velocity Cloud (HVC) gas. These stars are
ideal candidates for absorption-line studies of HVCs, attempts at which have
been made for almost 40 years with little success. A parent sample of 8321 HES
FHB stars was used to extract HI spectra along each line-of-sight, using the HI
Parkes All-Sky Survey. All lines-of-sight aligned with high velocity HI
emission with peak brightness temperatures greater than 120mK were examined.
The HI spectra of these 430 probes were visually screened and cross-referenced
with several HVC catalogues. In a forthcoming paper, we report on the results
of high-resolution spectroscopic observations of a sample of stars drawn from
this catalogue.Comment: 7 pages, 4 figures. ApJS accepted. Full catalogue and all online-only
images available at
http://astronomy.swin.edu.au/staff/cthom/catalogue/index.htm
Photometric validation of a model independent procedure to extract galaxy clusters
By means of CCD photometry in three bands (Gunn g, r, i) we investigate the
existence of 12 candidate clusters extracted via a model independent peak
finding algorithm (\cite{memsait}) from DPOSS data. The derived color-magnitude
diagrams allow us to confirm the physical nature of 9 of the cluster
candidates, and to estimate their photometric redshifts. Of the other
candidates, one is a fortuitous detection of a true cluster at z~0.4, one is a
false detection and the last is undecidable on the basis of the available data.
The accuracy of the photometric redshifts is tested on an additional sample of
8 clusters with known spectroscopic redshifts. Photometric redshifts turn out
to be accurate within z~0.01 (interquartile range).Comment: A&A in pres
An Optical Catalog of Galaxy Clusters Obtained from an Adaptive Matched Filter Finder Applied to SDSS DR6
We present a new cluster catalog extracted from the Sloan Digital Sky Survey
Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster
finder. We identify 69,173 galaxy clusters in the redshift range 0.045 0.78 in 8420 sq. deg. of the sky. We provide angular position, redshift,
richness, core and virial radii estimates for these clusters, as well as an
error analysis for each of these quantities. We also provide a catalog of more
than 205,000 galaxies representing the three brightest galaxies in the band
which are possible BCG candidates. We show basic properties of the BCG
candidates and study how their luminosity scales in redshift and cluster
richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as
with that of Wen, Han, and Liu. We match between 30% and 50% of clusters
between catalogs over all overlapping redshift ranges. We find that the
percentage of matches increases with the richness for all catalogs. We cross
match the AMF catalog with available X-ray data in the same area of the sky and
find 539 matches, 119 of which with temperature measurements. We present
scaling relations between optical and X-ray properties and cluster center
comparison. We find that both and correlate well with
both and , with no significant difference in trend if we restrict
the matches to flux-limited X-ray samples.Comment: 59 pages, 28 figures; accepted for publication in The Astrophysical
Journa
The Impact of Bisphenol A and Triclosan on Immune Parameters in the U.S. Population, NHANES 2003â2006
Background: Exposure to environmental toxicants is associated with numerous disease outcomes, many of which involve underlying immune and inflammatory dysfunction.
Objectives: To address the gap between environmental exposures and immune dysfunction, we investigated the association of two endocrine-disrupting compounds (EDCs) with markers of immune function.
Methods: Using data from the 2003â2006 National Health and Nutrition Examination Survey, we compared urinary bisphenol A (BPA) and triclosan levels with serum cytomegalovirus (CMV) antibody levels and diagnosis of allergies or hay fever in U.S. adults and children â„ 6 years of age. We used multivariate ordinary least squares linear regression models to examine the association of BPA and triclosan with CMV antibody titers, and multivariate logistic regression models to investigate the association of these chemicals with allergy or hay fever diagnosis. Statistical models were stratified by age (\u3c 18 years and â„ 18 years).
Results: In analyses adjusted for age, sex, race, body mass index, creatinine levels, family income, and educational attainment, in the â„ 18-year age group, higher urinary BPA levels were associated with higher CMV antibody titers (p \u3c 0.001). In the \u3c 18-year age group, lower levels of BPA were associated with higher CMV antibody titers (p \u3c 0.05). However, triclosan, but not BPA, showed a positive association with allergy or hay fever diagnosis. In the \u3c 18-year age group, higher levels of triclosan were associated with greater odds of having been diagnosed with allergies or hay fever (p \u3c 0.01).
Conclusions: EDCs such as BPA and triclosan may negatively affect human immune function as measured by CMV antibody levels and allergy or hay fever diagnosis, respectively, with differential consequences based on age. Additional studies should be done to investigate these findings
The ACS LCID project. VI. The SFH of the Tucana dSph and the relative ages of the isolated dSph galaxies
We present a detailed study of the star formation history (SFH) of the Tucana
dwarf spheroidal galaxy. High quality, deep HST/ACS data, allowed us to obtain
the deepest color-magnitude diagram to date, reaching the old main sequence
turnoff (F814 ~ 29) with good photometric accuracy. Our analysis, based on
three different SFH codes, shows that Tucana is an old and metal-poor stellar
system, which experienced a strong initial burst of star formation at a very
early epoch (~ 13 Gyr ago) which lasted a maximum of 1 Gyr (sigma value). We
are not able to unambiguously answer the question of whether most star
formation in Tucana occurred before or after the end of the reionization era,
and we analyze alternative scenarios that may explain the transformation of
Tucana from a gas-rich galaxy into a dSph. Current measurements of its radial
velocity do not preclude that Tucana may have crossed the inner regions of the
Local Group once, and so gas stripping by ram pressure and tides due to a close
interaction cannot be ruled out. On the other hand, the high star formation
rate measured at early times may have injected enough energy into the
interstellar medium to blow out a significant fraction of the initial gas
content. Gas that is heated but not blown out would also be more easily
stripped via ram pressure. We compare the SFH inferred for Tucana with that of
Cetus, the other isolated LG dSph galaxy in the LCID sample. We show that the
formation time of the bulk of star formation in Cetus is clearly delayed with
respect to that of Tucana. This reinforces the conclusion of Monelli et al.
(2010) that Cetus formed the vast majority of its stars after the end of the
reionization era implying, therefore, that small dwarf galaxies are not
necessarily strongly affected by reionization, in agreement with many
state-of-the-art cosmological models. [abridged]Comment: Accepted for publication on ApJ, 19 pages, 10 figures, 2 tables. A
version with full resolution figures is available at
http://www.iac.es/project/LCID/?p=publication
- âŠ