664 research outputs found
An infrared jet in Centaurus A (NGC 5128): Evidence for interaction between the active nucleus and the interstellar medium
In the present study, higher resolution near infrared images of the visually-obscured central region of Centaurus A were obtained in order to investigate the effects of the active nucleus on the surrounding galaxy. Researchers present J(1.25 microns), H(1.65 microns), and K(2.2 microns) images of the central 40 seconds of the galaxy, taken with the Univ. of Texas InSb array camera on the Anglo Australian 3.9 meter telescope. These images reveal a jet extending approx. 10 arcseconds to the northeast of the nucleus at the same position angle as the x ray and radio jets. The infrared jet is most prominent at the shortest wavelength (1.25 microns), where its brightness surpasses that of the nucleus. The blue appearance of the infrared jet is remarkable considering the heavy obscuration that is evident at visual wavelengths. The amount of reddening in the vicinity of the jet is determined from the measured colors of the stellar core of the galaxy, and this value is used to generate an extinction-corrected energy distribution. In contrast to previously studied optical and infrared jets in active nuclei, the short-wavelength prominence of the Cen A jet indicates that it cannot be attributed to synchrotron emission from a beam of relativistic electrons. The remaining viable mechanisms involve an interaction between the interstellar medium and the active nucleus: the infrared radiation from the jet may be due to emission from interstellar gas that has been entrained and heated by the flow of relativistic particles from the nucleus; alternatively, luminous blue stars may have been created by compression of interstellar material by the relativistic plasma. To investigate these proposed mechanisms, near-infrared spectroscopic studies of Cen A are in progress to look for collisionally excited molecular hydrogen emission lines and recombination lines from ionized gas
Trends in early childhood obesity in a large, urban school district in the Southwest from 2007 to 2014.
Presented at: Experimental Biology 2016; April 2-6, 2016; San Diego, CA.https://digitalrepository.unm.edu/prc-posters-presentations/1022/thumbnail.jp
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The design of a liquid lithium lens for a muon collider
The last stage of ionization cooling for the muon collider requires a multistage liquid lithium lens. This system uses a large ({approximately}0.5 MA) pulsed current through liquid lithium to focus the beam while energy loss in the lithium removes momentum which is replaced by linacs. The beam optics are designed to maximize the 6 dimensional transmission from one lens to the next while minimizing emittance growth. The mechanical design of the lithium vessel is constrained by a pressure pulse due to the sudden ohmic heating, and the stress on the Be window. The authors describe beam optics, the liquid lithium pressure vessel, pumping, power supplies, as well as the overall optimization of the system
Infrared L Band Observations of the Trapezium Cluster: A Census of Circumstellar Disks and Candidate Protostars
We report the results of a sensitive near-infrared JHKL imaging survey of the
Trapezium cluster in Orion. We use the JHKL colors to obtain a census of
infrared excess stars in the cluster. Of (391) stars brighter than 12th
magnitude in the K and L bands, 80 +/- 7% are found to exhibit detectable
infrared excess on the J-H, K-L color-color diagram. Examination of a subsample
of 285 of these stars with published spectral types yields a slightly higher
infrared excess fraction of 85%. We find that 97% of the optical proplyds in
the cluster exhibit excess in the JHKL color-color diagram indicating that the
most likely origin of the observed infrared excesses is from circumstellar
disks. We interpret these results to indicate that the fraction of stars in the
cluster with circumstellar disks is between 80-85%. Moreover, we find that the
probability of finding an infrared excess/protoplanetary disk around a star is
independent of stellar mass over essentially the entire range of the stellar
mass function down to the hydrogen burning limit. We identify 78 stars in our
sample characterized by K-L colors suggestive of deeply embedded protostellar
objects. If even a modest fraction fraction (i.e., ~ 50%) of these objects are
protostars, then star formation could be continuing in the molecular ridge at a
rate comparable to that which produced the foreground Trapezium cluster.Comment: 33 pages plus 3 separate color figures. For higher resolution color
figures and a single file containing the entire paper, figures and tables see
http://cfa-www.harvard.edu/~gmuench/thesis/clusters/TRAP/traplband.html Used
AASTEX macros v 5.0. Paper will appear in December A
Muon Colliders
Muon Colliders have unique technical and physics advantages and disadvantages
when compared with both hadron and electron machines. They should thus be
regarded as complementary. Parameters are given of 4 TeV and 0.5 TeV high
luminosity \mumu colliders, and of a 0.5 TeV lower luminosity demonstration
machine. We discuss the various systems in such muon colliders, starting from
the proton accelerator needed to generate the muons and proceeding through muon
cooling, acceleration and storage in a collider ring. Problems of detector
background are also discussed.Comment: 28 pages, with 12 postscript figures. To be published Proceedings of
the 9th Advanced ICFA Beam Dynamics Workshop, AIP Pres
Synchronous Optical and Radio Polarization Variability in the Blazar OJ287
We explore the variability and cross-frequency correlation of the flux
density and polarization of the blazar OJ287, using imaging at 43 GHz with the
Very Long Baseline Array, as well as optical and near-infrared polarimetry. The
polarization and flux density in both the optical waveband and the 43 GHz
compact core increased by a small amount in late 2005, and increased
significantly along with the near-IR polarization and flux density over the
course of 10 days in early 2006. Furthermore, the values of the electric vector
position angle (EVPA) at the three wavebands are similar. At 43 GHz, the EVPA
of the blazar core is perpendicular to the flow of the jet, while the EVPAs of
emerging superluminal knots are aligned parallel to the jet axis. The core
polarization is that expected if shear aligns the magnetic field at the
boundary between flows of disparate velocities within the jet. Using variations
in flux density, percentage polarization, and EVPA, we model the inner jet as a
spine-sheath system. The model jet contains a turbulent spine of half-width 1.2
degrees and maximum Lorentz factor of 16.5, a turbulent sheath with Lorentz
factor of 5, and a boundary region of sheared field between the spine and
sheath. Transverse shocks propagating along the fast, turbulent spine can
explain the superluminal knots. The observed flux density and polarization
variations are then compatible with changes in the direction of the inner jet
caused by a temporary change in the position of the core if the spine contains
wiggles owing to an instability. In addition, we can explain a stable offset of
optical and near-IR percentage polarization by a steepening of spectral index
with frequency, as supported by the data.Comment: 34 pages, 12 figures; To be published in Astrophysical Journal,
accepted 03/200
Pressurized H-2 rf Cavities in Ionizing Beams and Magnetic Fields
A major technological challenge in building a muon cooling channel is operating rf cavities in multitesla external magnetic fields. We report the first proof-of-principle experiment of a high pressure gas-filled rf cavity for use with intense ionizing beams and strong external magnetic fields. rf power consumption by beam-induced plasma is investigated with hydrogen and deuterium gases with pressures between 20 and 100 atm and peak rf gradients between 5 and 50 MV/m. The low pressure case agrees well with an analytical model based on electron and ion mobilities. Varying concentrations of oxygen gas are investigated to remove free electrons from the cavity and reduce the rf power consumption. Measurements of the electron attachment time to oxygen and rate of ion-ion recombination are also made. Additionally, we demonstrate the operation of the gas-filled rf cavity in a solenoidal field of up to 3 T, finding no major magnetic field dependence. All these results indicate that a high pressure gas-filled cavity is a viable technology for muon ionization cooling.open1
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