3,792 research outputs found
Vortex nucleation in rotating BEC: the role of the boundary condition for the order parameter
We study the process of vortex nucleation in rotating two-dimensional BEC
confined in a harmonic trap. We show that, within the Gross-Pitaevskii theory
with the boundary condition of vanishing of the order parameter at infinity,
topological defects nucleation occurs via the creation of vortex-antivortex
pairs far from the cloud center, where the modulus of the order parameter is
small. Then, vortices move towards the center of the cloud and antivortices
move in the opposite direction but never disappear. We also discuss the role of
surface modes in this process.Comment: 6 pages, 2 figure
Artifacts at 4.5 and 8.0 um in Short Wavelength Spectra from the Infrared Space Observatory
Spectra from the Short Wavelength Spectrometer (SWS) on ISO exhibit artifacts
at 4.5 and 8 um. These artifacts appear in spectra from a recent data release,
OLP 10.0, as spurious broad emission features in the spectra of stars earlier
than ~F0, such as alpha CMa. Comparison of absolutely calibrated spectra of
standard stars to corresponding spectra from the SWS reveals that these
artifacts result from an underestimation of the strength of the CO and SiO
molecular bands in the spectra of sources used as calibrators by the SWS.
Although OLP 10.0 was intended to be the final data release, these findings
have led to an additional release addressing this issue, OLP 10.1, which
corrects the artifacts.Comment: 14 pages, AASTex, including 5 figures. Accepted by ApJ Letter
Physical Conditions in the Narrow-Line Region of Markarian 3. II. Photoionization Modeling Results
We have examined the physical conditions in the narrow-line region (NLR) of
the Seyfert 2 galaxy Markarian 3, using long-slit spectra obtained with the
Hubble Space Telescope/Space Telescope Imaging Spectrograph and photoionization
models. We find three components of photoionized gas in the NLR. Two of these
components, characterized by emission lines such as [NeV] 3426 and [OIII] 5007,
lie within the envelope of the bi-conical region described in our previous
kinematic study. A component of lower ionization gas, in which lines such as
[OII] 3727 arise, is found to lie outside the bi-cone. Each of these components
is irradiated by a power-law continuum which is attenuated by intervening gas,
presumably closer to the central source. The radiation incident upon the low
ionization gas, external to the bi-cone, is much more heavily absorbed. These
absorbers are similar to the intrinsic UV and X-ray absorbers detected in many
Seyfert 1 galaxies, which suggests that the collimation of the ionizing
radiation occurs in a circumnuclear wind, rather than a thick, molecular torus.
We estimate the mass for the observed NLR emitting gas to be 2 million
solar-masses. It is likely that Markarian 3 acquired this gas through an
on-going interaction with the spiral galaxy UGC 3422.Comment: 47 pages, 7 figures; accepted for publication in Ap
The X-ray Emission from the Nucleus of the Dwarf Elliptical Galaxy NGC 3226
We present the first high resolution X-ray image of the dwarf elliptical
galaxy NGC 3226. The data were obtained during an observation of the nearby
Seyfert Galaxy NGC 3227 using the Chandra X-ray Observatory. We detect a point
X-ray source spatially consistent with the optical nucleus of NGC 3226 and a
recently-detected, compact, flat-spectrum, radio source. The X-ray spectrum can
be measured up to ~10 keV and is consistent with a power law with a photon
index 1.7 <~ Gamma <~ 2.2, or thermal bremmstrahlung emission with 4 <~ kT <~
10 keV. In both cases the luminosity in the 2--10 keV band ~10^{40} h_{75}^{-1}
erg/s. We find marginal evidence that the nucleus varies within the
observation. These characteristics support evidence from other wavebands that
NGC 3226 harbors a low-luminosity, active nucleus. We also comment on two
previously-unknown, fainter X-ray sources <~ 15 arcsec from the nucleus of NGC
3226. Their proximity to the nucleus (with projected distances <~ 1.3/h_{75}
kpc) suggests both are within NGC 3226, and thus have luminosities (~few x
10^{38} -- few x 10^{39} erg/s) consistent with black-hole binary systems.Comment: Accepted for publication in ApJ. Figures in colo
New Indicators for AGN Power: The Correlation Between [O IV] lambda 25.89 micron and Hard X-ray Luminosity for Nearby Seyfert Galaxies
We have studied the relationship between the [O IV] lambda 25.89 micron
emission line luminosities, obtained from Spitzer spectra, the X-ray continua
in the 2-10 keV band, primarily from ASCA, and the 14-195 keV band obtained
with the SWIFT/Burst Alert Telescope (BAT), for a sample of nearby (z < 0.08)
Seyfert galaxies. For comparison, we have examined the relationship between the
[O III] 5007, the 2-10 keV and the 14-195 keV luminosities for the same set of
objects. We find that both the [O IV] and [O III] luminosities are
well-correlated with the BAT luminosities. On the other hand, the [O III]
luminosities are better-correlated with 2-10 keV luminosities than are those of
[O IV]. When comparing [O IV] and [O III] luminosities for the different types
of galaxies, we find that the Seyfert 2's have significantly lower [O III] to
[O IV] ratios than the Seyfert 1's. We suggest that this is due to more
reddening of the narrow line region (NLR) of the Seyfert 2's. Assuming Galactic
dust to gas ratios, the average amount of extra reddening corresponds to a
hydrogen column density of ~ few times 10^21 cm^-2, which is a small fraction
of the X-ray absorbing columns in the Seyfert 2's. The combined effects of
reddening and the X-ray absorption are the probable reason why the [O III]
versus 2-10 keV correlation is better than the [O IV] versus 2-10 keV, since
the [O IV] emission line is much less affected by extinction. Overall, we find
the [O IV] to be an accurate and truly isotropic indicator of the power of the
AGN. This suggests that it can be useful in deconvolving the contribution of
the AGN and starburst to the spectrum of Compton-thick and/or X-ray weak
sources.Comment: Accepted for publication in the Astrophysical Journal. 31 pages, 6
figures, 4 table
On the Nature of Intrinsic Absorption in Reddened Seyfert 1 Galaxies
We discuss the origin of the ``dusty lukewarm absorber'', which we previously
identified in the reddened Seyfert 1 galaxies NGC 3227 and Akn 564. This
absorber is characterized by saturated UV absorption lines (C IV, N V) near the
systemic velocity of the host galaxy, and is likely responsible for reddening
both the continuum and the emission lines (including those from the narrow-line
region) from these Seyferts. From a large sample of Seyfert 1 galaxies, we find
that continuum reddening (as measured by UV color) tends to increase with
inclination of the host galaxy. Furthermore, reddened, inclined Seyfert
galaxies observed at moderate to high spectral resolution all show evidence for
dusty lukewarm absorbers. We suggest that these absorbers lie in the plane of
the host galaxy at distances > 100 pc from the nucleus, and are physically
distinct from the majority of intrinsic absorbers that are outflowing from the
nucleus.Comment: 14 pages, including 2 figures, accepted for publication in the
Astrophysical Journal (Letters
Magnetic excitations near the quantum phase transition in the Ising ferromagnet LiHoF_4
Effective-medium theory and inelastic neutron scattering are used to study the magnetic excitations in the Ising ferromagnet LiHoF_4 near its magnetic-field-induced quantum phase transition (QPT). As expected, the dominant mode softens at the QPT, but reaches a finite, rather than vanishing, limit due to the hyperfine interaction. The experimental phase diagram and excitation spectra are well described by an effective-medium theory to first order in the 1/z expansion. There are some differences between theory and experiments, which may be due to domain walls, their dynamics and shape effects, and to magnetoelastic couplings
Radial Velocity Offsets Due to Mass Outflows and Extinction in Active Galactic Nuclei
We present a study of the radial velocity offsets between narrow emission
lines and host galaxy lines (stellar absorption and H I 21-cm emission) in
Seyfert galaxies with observed redshifts less than 0.043. We find that 35% of
the Seyferts in the sample show [O III] emission lines with blueshifts with
respect to their host galaxies exceeding 50 km/s, whereas only 6% show
redshifts this large, in qualitative agreement with most previous studies. We
also find that a greater percentage of Seyfert 1 galaxies show blueshifts than
Seyfert 2 galaxies. Using HST/STIS spatially-resolved spectra of the Seyfert 2
galaxy NGC 1068 and the Seyfert 1 galaxy NGC 4151, we generate geometric models
of their narrow-line regions (NLRs) and inner galactic disks, and show how
these models can explain the blueshifted [O III] emission lines in collapsed
STIS spectra of these two Seyferts. We conclude that the combination of mass
outflow of ionized gas in the NLR and extinction by dust in the inner disk
(primarily in the form of dust spirals) is primarily responsible for the
velocity offsets in Seyfert galaxies. More exotic explanations are not needed.
We discuss the implications of this result for the velocity offsets found in
higher redshift AGN.Comment: 25 pages, 7 figures, accepted for publication in the Astrophysical
Journa
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