669 research outputs found
Reliability History and Improvements to the ANL 50 MEV H- Accelerator
The H- Accelerator consists of a 750 keV Cockcroft Walton preaccelerator and
an Alvarez type 50 MeV linac. The accelerator has been in operation since 1961.
Since 1981, it has been used as the injector for the Intense Pulsed Neutron
Source (IPNS), a national user facility for neutron scattering. The linac
delivers about 3.5x1012 H- ions per pulse, 30 times per second (30 Hz), for
multi-turn injection to a 450 MeV Rapid Cycling Synchrotron (RCS). IPNS
presently operates about 4,000 hours per year, and operating when scheduled is
critical to meeting the needs of the user community. For many years the IPNS
injector/RCS has achieved an average reliability of 95%, helped in large part
by the preaccelerator/linac which has averaged nearly 99%. To maintain and
improve system reliability, records need to show what each subsystem
contributes to the total down time. The history of source and linac subsystem
reliability, and improvements that have been made to improve reliability, will
be described. Plans to maintain or enhance this reliability for at least
another ten years of operation, will also be discussed.Comment: 3 pages, 1 figur
Unveiling a Population of X-ray Non-Detected AGN
We define a sample of 27 radio-excess AGN in the Chandra Deep Field North by
selecting galaxies that do not obey the radio/infrared correlation for
radio-quiet AGN and star-forming galaxies. Approximately 60% of these
radio-excess AGN are X-ray undetected in the 2 Ms Chandra catalog, even at
exposures of > 1 Ms; 25% lack even 2-sigma X-ray detections. The absorbing
columns to the faint X-ray-detected objects are 10^22 cm^-2 < N_H < 10^24
cm^-2, i.e., they are obscured but unlikely to be Compton thick. Using a local
sample of radio-selected AGN, we show that a low ratio of X-ray to radio
emission, as seen in the X-ray weakly- and non-detected samples, is correlated
with the viewing angle of the central engine, and therefore with obscuration.
Our technique can explore the proportion of obscured AGN in the distant
Universe; the results reported here for radio-excess objects are consistent
with but at the low end of the overall theoretical predictions for
Compton-thick objects.Comment: Accepted for publication in the Astrophysical Journal, 15 pages, 10
figures, 4 table
Why Optically--Faint AGN Are Faint: The Spitzer Perspective
Optically--faint X-ray sources (those with f_X/f_R > 10) constitute about 20%
of X-ray sources in deep surveys, and are potentially highly obscured and/or at
high redshift. Their faint optical fluxes are generally beyond the reach of
spectroscopy. For a sample of 20 optically--faint sources in CDFS, we compile
0.4--24 um photometry, relying heavily on Spitzer. We estimate photometric
redshifts for 17 of these 20 sources. We find that these AGN are
optically--faint both because they lie at significantly higher redshifts
(median z ~ 1.6) than most X-ray--selected AGN, and because their spectra are
much redder than standard AGN. They have 2--8 keV X-ray luminosities in the
Seyfert range, unlike the QSO--luminosities of optically--faint AGN found in
shallow, wide--field surveys. Their contribution to the X-ray Seyfert
luminosity function is comparable to that of z>1 optically--bright AGN.Comment: Accepted for publication in the Astrophysical Journa
Spitzer Power-law AGN Candidates in the Chandra Deep Field-North
We define a sample of 62 galaxies in the Chandra Deep Field-North whose
Spitzer IRAC SEDs exhibit the characteristic power-law emission expected of
luminous AGN. We study the multiwavelength properties of this sample, and
compare the AGN selected in this way to those selected via other Spitzer
color-color criteria. Only 55% of the power-law galaxies are detected in the
X-ray catalog at exposures of >0.5 Ms, although a search for faint emission
results in the detection of 85% of the power-law galaxies at the > 2.5 sigma
detection level. Most of the remaining galaxies are likely to host AGN that are
heavily obscured in the X-ray. Because the power-law selection requires the AGN
to be energetically dominant in the near- and mid-infrared, the power-law
galaxies comprise a significant fraction of the Spitzer-detected AGN population
at high luminosities and redshifts. The high 24 micron detection fraction also
points to a luminous population. The power-law galaxies comprise a subset of
color-selected AGN candidates. A comparison with various mid-infrared color
selection criteria demonstrates that while the color-selected samples contain a
larger fraction of the X-ray luminous AGN, there is evidence that these
selection techniques also suffer from a higher degree of contamination by
star-forming galaxies in the deepest exposures. Considering only those
power-law galaxies detected in the X-ray catalog, we derive an obscured
fraction of 68% (2:1). Including all of the power-law galaxies suggests an
obscured fraction of < 81% (4:1).Comment: Accepted for publication in the Astrophysical Journal, 27 pages, 20
figures, 5 tables, version with high-resolution figures and online-only
tables available at: http://frodo.as.arizona.edu/~jdonley/powerlaw
Characterization of AGN and their hosts in the Extended Groth Strip: a multiwavelength analysis
We have employed a reliable technique of classification of Active Galactic
Nuclei (AGN) based on the fit of well-sampled spectral energy distributions
(SEDs) with a complete set of AGN and starburst galaxy templates. We have
compiled ultraviolet, optical, and infrared data for a sample of 116 AGN
originally selected for their X-ray and mid-infrared emissions (96 with single
detections and 20 with double optical counterparts). This is the most complete
compilation of multiwavelength data for such a big sample of AGN in the
Extended Groth Strip (EGS). Through these SEDs, we are able to obtain highly
reliable photometric redshifts and to distinguish between pure and
host-dominated AGN. For the objects with unique detection we find that they can
be separated into five main groups, namely: Starburst-dominated AGN (24 % of
the sample), Starburst-contaminated AGN (7 %), Type-1 AGN (21 %), Type-2 AGN
(24 %), and Normal galaxy hosting AGN (24 %). We find these groups concentrated
at different redshifts: Type-2 AGN and Normal galaxy hosting AGN are
concentrated at low redshifts, whereas Starburst-dominated AGN and Type-1 AGN
show a larger span. Correlations between hard/soft X-ray and ultraviolet,
optical and infrared luminosities, respectively, are reported for the first
time for such a sample of AGN spanning a wide range of redshifts. For the 20
objects with double detection the percentage of Starburst-dominated AGN
increases up to 48%.Comment: 38 pages, 8 figures, 5 tables. Accepted by A
Stability of fermionic Feshbach molecules in a Bose-Fermi mixture
In the wake of successful experiments in Fermi condensates, experimental
attention is broadening to study resonant interactions in degenerate Bose-Fermi
mixtures. Here we consider the properties and stability of the fermionic
molecules that can be created in such a mixture near a Feshbach resonance (FR).
To do this, we consider the two-body scattering matrix in the many-body
environment, and assess its complex poles. The stability properties of these
molecules strongly depend on their centre-of-mass motion, because they must
satisfy Fermi statistics. At low centre-of-mass momenta the molecules are more
stable than in the absence of the environment (due to Pauli-blocking effects),
while at high centre-of-mass momenta nontrivial many body effects render them
somewhat less stable
A Gaseous Group with Unusual Remote Star Formation
We present VLA 21-cm observations of the spiral galaxy ESO 481-G017 to
determine the nature of remote star formation traced by an HII region found 43
kpc and ~800 km s^-1 from the galaxy center (in projection). ESO 481-G017 is
found to have a 120 kpc HI disk with a mass of 1.2x10^10 Msun and UV GALEX
images reveal spiral arms extending into the gaseous disk. Two dwarf galaxies
with HI masses close to 10^8 Msun are detected at distances of ~200 kpc from
ESO 481-G017 and a HI cloud with a mass of 6x10^7 Msun is found near the
position and velocity of the remote HII region. The HII region is somewhat
offset from the HI cloud spatially and there is no link to ESO 481-G017 or the
dwarf galaxies. We consider several scenarios for the origin of the cloud and
HII region and find the most likely is a dwarf galaxy that is undergoing ram
pressure stripping. The HI mass of the cloud and Halpha luminosity of the HII
region (10^38.1 erg s^-1) are consistent with dwarf galaxy properties, and the
stripping can trigger the star formation as well as push the gas away from the
stars.Comment: 19 pages, 4 figures, accepted by PAS
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