254 research outputs found
Calibrant Delivery for Mass Spectrometry
This article describes a means of sampling ions that are created at a location remote from the primary ion source used for mass spectral analysis. Such a source can be used for delivery of calibrant ions on demand. Calibrant ions are sprayed into an atmospheric pressure chamber, at a position substantially removed from the sampling inlet. A gas flow sweeps the calibrants towards the sampling inlet, and a new means for toggling the second ion beam into the instrument can be achieved with the use of a repelling field established by an electrode in front of the sampling inlet. The physical separation of two or more sources of ions eliminates detrimental interactions due to gas flows or fields. When using a nanoflow electrospray tip as the primary ion source, the potential applied to the tip completely repels calibrant ions and there is no compromise in terms of electrospray performance. When calibrant ions are desired, the potential applied to the nanoflow electrospray tip is lowered for a short period of time to allow calibrant ions to be sampled into the instrument, thus providing a means for external calibration that avoids the typical complications and compromises associated with dual spray sources. It is also possible to simultaneously sample ions from multiple ion beams if necessary for internal mass calibration purposes. This method of transporting additional ion beams to a sampling inlet can also be used with different types of atmospheric pressure sources such as AP MALDI, as well as sources configured to deliver ions of different polarity
The Angular Momentum Content and Evolution of Class I and Flat-Spectrum Protostars
We report on the angular momentum content of heavily embedded protostars
based on our analysis of the projected rotation velocities (v sin i s) of 38
Class I/flat spectrum young stellar objects presented by Doppmann et al (2005).
After correcting for projection effects, we find that infrared-selected Class
I/flat spectrum objects rotate significantly more quickly (median equatorial
rotation velocity ~ 38 km/sec) than Classical T Tauri stars (CTTSs; median
equatorial rotation velocity ~ 18 km/sec) in the Rho Ophiuchi and
Taurus-Aurigae regions. The detected difference in rotation speeds between
Class I/flat spectrum sources and CTTSs proves difficult to explain without
some mechanism which transfers angular momentum out of the protostar between
the two phases. Assuming Class I/flat spectrum sources possess physical
characteristics (M_*,R_*,B_*) typical of pre-main sequence stars, fully disk
locked Class I objects should have co-rotation radii within their protostellar
disks that match well (within 30%) with the predicted magnetic coupling radii
of Shu et al (1994). The factor of two difference in rotation rates between
Class I/flat spectrum and CTTS sources, when interpreted in the context of disk
locking models, also imply a factor of 5 or greater difference in mass
accretion rates between the two phases.Comment: 13 pages, 6 figures. Accepted for publication in the Astronomical
Journal (tentatively for June 2005 edition
The Radial Velocity Distribution of Class I and Flat-Spectrum Protostars
We analyze radial velocities for a sample of 31 Class I and flat spectrum
protostars in Taurus-Auriga, rho Ophiuchi and Serpens for evidence of the
global dynamical state of extremely young stellar populations buried within
parental molecular clouds. Comparing the radial velocity of each protostar to
that of the local CO gas, we are able to constrain the one dimensional radial
velocity dispersion of Class I and flat spectrum objects to ~ 2.5 km/sec or
below. This upper limit to the protostellar velocity dispersion is consistent
with the velocity dispersions of surrounding CO gas which we measure to be ~
1.4 km/sec, suggesting that the motions of protostars and local CO gas are
dynamically linked and dominated by the gravitational potential of the
molecular cloud. However, the upper limit on the protostellar velocity
dispersion could still allow for slightly inflated motions of protostars
relative to the local molecular gas. Four of the protostars analyzed appear to
have velocities more than 3 sigma (7.5 km/sec) away from the central local CO
gas velocity while showing spectroscopic indicators of youth and accretion such
as H_2 emission, HI Br Gamma emission, or K band continuum veiling. These
radial velocity outliers may represent protostellar spectroscopic binaries or
ejected cluster members.Comment: 9 pages in emulate ApJ format, accepted for publication in A
Site-specific effects of neurosteroids on GABA(A) receptor activation and desensitization
This study examines how site-specific binding to three identified neurosteroid-binding sites in the
Kepler-503b: An Object at the Hydrogen Burning Mass Limit Orbiting a Subgiant Star
Using spectroscopic radial velocities with the APOGEE instrument and Gaia
distance estimates, we demonstrate that Kepler-503b, currently considered a
validated Kepler planet, is in fact a brown-dwarf/low-mass star in a nearly
circular 7.2-day orbit around a subgiant star. Using a mass estimate for the
primary star derived from stellar models, we derive a companion mass and radius
of () and
(),
respectively. Assuming the system is coeval, the evolutionary state of the
primary indicates the age is Gyr. Kepler-503b sits right at the
hydrogen burning mass limit, straddling the boundary between brown dwarfs and
very low-mass stars. More precise radial velocities and secondary eclipse
spectroscopy with James Webb Space Telescope will provide improved measurements
of the physical parameters and age of this important system to better constrain
and understand the physics of these objects and their spectra. This system
emphasizes the value of radial velocity observations to distinguish a genuine
planet from astrophysical false positives, and is the first result from the
SDSS-IV monitoring of Kepler planet candidates with the multi-object APOGEE
instrument.Comment: Accepted for publication in ApJL, 12 pages, 3 figures, 2 table
Two Rare Magnetic Cataclysmic Variables with Extreme Cyclotron Features Identified in the Sloan Digital Sky Survey
Two newly identified magnetic cataclysmic variables discovered in the Sloan
Digital Sky Survey (SDSS), SDSSJ155331.12+551614.5 and SDSSJ132411.57+032050.5,
have spectra showing highly prominent, narrow, strongly polarized cyclotron
humps with amplitudes that vary on orbital periods of 4.39 and 2.6 hrs,
respectively. In the former, the spacing of the humps indicates the 3rd and 4th
harmonics in a magnetic field of ~60 MG. The narrowness of the cyclotron
features and the lack of strong emission lines imply very low temperature
plasmas and very low accretion rates, so that the accreting area is heated by
particle collisions rather than accretion shocks. The detection of rare systems
like these exemplifies the ability of the SDSS to find the lowest accretion
rate close binaries.Comment: Accepted for publication in the Astrophysical Journal, vol. 583,
February 1, 2003; slight revisions and additions in response to referee's
comments; 17 pages, 6 figures, AASTeX v4.
Stellar and Planetary Characterization of the Ross 128 Exoplanetary System from APOGEE Spectra
The first detailed chemical abundance analysis of the M dwarf (M4.0)
exoplanet-hosting star Ross 128 is presented here, based upon near-infrared
(1.5--1.7 \micron) high-resolution (22,500) spectra from the
SDSS-APOGEE survey. We determined precise atmospheric parameters =3231100K, log=4.960.11 dex and chemical abundances of eight
elements (C, O, Mg, Al, K, Ca, Ti, and Fe), finding Ross 128 to have near solar
metallicity ([Fe/H] = +0.030.09 dex). The derived results were obtained
via spectral synthesis (1-D LTE) adopting both MARCS and PHOENIX model
atmospheres; stellar parameters and chemical abundances derived from the
different adopted models do not show significant offsets. Mass-radius modeling
of Ross 128b indicate that it lies below the pure rock composition curve,
suggesting that it contains a mixture of rock and iron, with the relative
amounts of each set by the ratio of Fe/Mg. If Ross 128b formed with a sub-solar
Si/Mg ratio, and assuming the planet's composition matches that of the
host-star, it likely has a larger core size relative to the Earth. The derived
planetary parameters -- insolation flux (S=1.790.26) and
equilibrium temperature (=29410K) -- support previous findings
that Ross 128b is a temperate exoplanet in the inner edge of the habitable
zone.Comment: Accepted in ApJLetters, 3 figures, 2 tables, 12 page
Fast quantitation of opioid isomers in human plasma by differential mobility spectrometry/mass spectrometry via SPME/open-port probe sampling interface
The final publication is available at Elsevier via https://dx.doi.org/10.1016/j.aca.2017.08.023 © 2017. This manuscript version is made available under the CC-BY-NC-ND 4.0 license https://creativecommons.org/licenses/by-nc-nd/4.0/Mass spectrometry (MS) based quantitative approaches typically require a thorough sample clean-up and a decent chromatographic step in order to achieve needed figures of merit. However, in most cases, such processes are not optimal for urgent assessments and high-throughput determinations. The direct coupling of solid phase microextraction (SPME) to MS has shown great potential to shorten the total sample analysis time of complex matrices, as well as to diminish potential matrix effects and instrument contamination. In this study, we demonstrate the use of the open-port probe (OPP) as a direct and robust sampling interface to couple biocompatible-SPME (Bio-SPME) fibres to MS for the rapid quantitation of opioid isomers (i.e. codeine and hydrocodone) in human plasma. In place of chromatography, a differential mobility spectrometry (DMS) device was implemented to provide the essential selectivity required to quantify these constitutional isomers. Taking advantage of the simplified sample preparation process based on Bio-SPME and the fast separation with DMS-MS coupling via OPP, a high-throughput assay (10–15 s per sample) with limits of detection in the sub-ng/mL range was developed. Succinctly, we demonstrated that by tuning adequate ion mobility separation conditions, SPME-OPP-MS can be employed to quantify non-resolved compounds or those otherwise hindered by co-extracted isobaric interferences without further need of coupling to other separation platforms.SCIEXNatural Sciences and Engineering Research Council (NSERC) of Canad
Sloan Digital Sky Survey Imaging of Low Galactic Latitude Fields: Technical Summary and Data Release
The Sloan Digital Sky Survey (SDSS) mosaic camera and telescope have obtained
five-band optical-wavelength imaging near the Galactic plane outside of the
nominal survey boundaries. These additional data were obtained during
commissioning and subsequent testing of the SDSS observing system, and they
provide unique wide-area imaging data in regions of high obscuration and star
formation, including numerous young stellar objects, Herbig-Haro objects and
young star clusters. Because these data are outside the Survey regions in the
Galactic caps, they are not part of the standard SDSS data releases. This paper
presents imaging data for 832 square degrees of sky (including repeats), in the
star-forming regions of Orion, Taurus, and Cygnus. About 470 square degrees are
now released to the public, with the remainder to follow at the time of SDSS
Data Release 4. The public data in Orion include the star-forming region NGC
2068/NGC 2071/HH24 and a large part of Barnard's loop.Comment: 31 pages, 9 figures (3 missing to save space), accepted by AJ, in
press, see http://photo.astro.princeton.edu/oriondatarelease for data and
paper with all figure
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