1,260 research outputs found
A Narrowband Imaging Survey for High Redshift Galaxies in the Near Infrared
A narrowband imaging survey of 276 square minutes of arc was carried out at
near infrared wavelengths to search for emission line objects at high
redshifts. Most of the fields contained a known quasar or radio galaxy at a
redshift that placed one of the strong, restframe optical emission lines
(H-alpha, [O III], H-beta, or [O II]) in the bandpass of the narrowband filter.
The area weighted line flux limit over the entire survey was 3.4x10e-16
erg/cm2/s (3-sigma), while the most sensitive limits reached 1.4x10e-16
erg/cm2/s. Integrating the volume covered by all four optical emission lines in
each image yields a total comoving volume surveyed of 1.4x10e5 cubic
megaparsecs. Considering only H-alpha emission in the K band (2.05 < z < 2.65),
where the survey is most sensitive, the survey covered a comoving volume of
3.0x10e4 cubic megaparsecs to a volume-weighted average star formation rate of
112 M-solar/yr (for Ho = 50 km/s/Mpc, Omega = 1). This is the most extensive
near-infrared survey which is deep enough to have a reasonable chance at
detecting strong line emission from an actively star-forming population of
galaxies, when d against simple models of galaxy formation. One emission line
candidate was identified in this survey, and subsequently confirmed
spectroscopically.Comment: To appear in the Astronomical Journal, November 1996. 23 pages,
including 2 tables and 7 figure
The Influence of Magnetic Field Geometry on the Evolution of Black Hole Accretion Flows: Similar Disks, Drastically Different Jets
Because the magneto-rotational instability is capable of exponentially
amplifying weak preexisting magnetic fields, it might be hoped that the
character of the magnetic field in accretion disks is independent of the nature
of the seed field. However, the divergence-free nature of magnetic fields in
highly conducting fluids ensures that their large-scale topology is preserved,
no matter how greatly the field intensity is changed. By performing global
two-dimensional and three-dimensional general relativistic magnetohydrodynamic
disk simulations with several different topologies for the initial magnetic
field, we explore the degree to which the character of the flows around black
holes depends on the initial topology. We find that while the qualitative
properties of the accretion flow are nearly independent of field topology,
jet-launching is very sensitive to it: a sense of vertical field consistent for
at least an inner disk inflow time is essential to the support of strong jets.Comment: 42 pages; 17 figures; Accepted for publication in ApJ (some new
discussion and 2 new figures
Symptomatology under storm conditions in the north atlantic in control subjects and in persons with bilateral labyrinthine defects
Motion sickness under conditions of stress and anxiety - role of vestibular apparatu
Exploring the parameter space of MagLIF implosions using similarity scaling. I. Theoretical framework
Magneto-inertial fusion (MIF) concepts, such as the Magnetized Liner Inertial
Fusion (MagLIF) platform [M. R. Gomez et al., Phys. Rev. Lett. 113, 155003
(2014)], constitute a promising path for achieving ignition and significant
fusion yields in the laboratory. The space of experimental input parameters
defining a MagLIF load is highly multi-dimensional, and the implosion itself is
a complex event involving many physical processes. In the first paper of this
series, we develop a simplified analytical model that identifies the main
physical processes at play during a MagLIF implosion. Using non-dimensional
analysis, we determine the most important dimensionless parameters
characterizing MagLIF implosions and provide estimates of such parameters using
typical fielded or experimentally observed quantities for MagLIF. We then show
that MagLIF loads can be "incompletely" similarity scaled, meaning that the
experimental input parameters of MagLIF can be varied such that many (but not
all) of the dimensionless quantities are conserved. Based on similarity-scaling
arguments, we can explore the parameter space of MagLIF loads and estimate the
performance of the scaled loads. In the follow-up papers of this series, we
test the similar scaling theory for MagLIF loads against simulations for two
different scaling "vectors", which include current scaling and rise-time
scaling.Comment: 24 pages, submitted to Physics of Plasma
Communication
Visualizing the functional interactions of biomolecules such as proteins and nucleic acids is key to understanding cellular life on the molecular scale. Spatial proximity is often used as a proxy for the direct interaction of biomolecules. However, current techniques to visualize spatial proximity are either limited by spatial resolution, dynamic range, or lack of single-molecule sensitivity. Here, we introduce Proximity-PAINT (pPAINT), a variation of the super-resolution microscopy technique DNA-PAINT. pPAINT uses a split-docking-site configuration to detect spatial proximity with high sensitivity, low false-positive rates, and tunable detection distances. We benchmark and optimize pPAINT using designer DNA nanostructures and demonstrate its cellular applicability by visualizing the spatial proximity of alpha- and beta-tubulin in microtubules using super-resolution detection. © 2020 Wiley-VCH GmbH
Critical Protoplanetary Core Masses in Protoplanetary Disks and the Formation of Short-Period Giant Planets
We study a solid protoplanetary core of 1-10 earth masses migrating through a
disk. We suppose the core luminosity is generated as a result of planetesimal
accretion and calculate the structure of the gaseous envelope assuming
equilibrium. This is a good approximation when the core mass is less than the
critical value, M_{crit}, above which rapid gas accretion begins. We model the
structure of the protoplanetary nebula as an accretion disk with constant
\alpha. We present analytic fits for the steady state relation between disk
surface density and mass accretion rate as a function of radius r. We calculate
M_{crit} as a function of r, gas accretion rate through the disk, and
planetesimal accretion rate onto the core \dot{M}. For a fixed \dot{M},
M_{crit} increases inwards, and it decreases with \dot{M}. We find that \dot{M}
onto cores migrating inwards in a time 10^3-10^5 yr at 1 AU is sufficient to
prevent the attainment of M_{crit} during the migration process. Only at small
radii where planetesimals no longer exist can M_{crit} be attained. At small
radii, the runaway gas accretion phase may become longer than the disk lifetime
if the core mass is too small. However, massive cores can be built-up through
the merger of additional incoming cores on a timescale shorter than for in situ
formation. Therefore, feeding zone depletion in the neighborhood of a fixed
orbit may be avoided. Accordingly, we suggest that giant planets may begin to
form early in the life of the protostellar disk at small radii, on a timescale
that may be significantly shorter than for in situ formation. (abridged)Comment: 24 pages (including 9 figures), LaTeX, uses emulateapj.sty, to be
published in ApJ, also available at http://www.ucolick.org/~ct/home.htm
An Infrared Emission Line Galaxy at z = 2.43
An object discovered during an infrared survey of the field near the quasar
B2 0149+33 has an emission line at 2.25m that we interpret as H at
a redshift of 2.43. The K-band image shows two compact components 10 kpc apart
surrounded by more extended emission over ~20 kpc. The H emission
appears to be extended over ~15 kpc (2") in a coarsely sampled (0".8/pixel)
image. The star formation rate may be as high as 250 - 1000 M
yr, depending on the extinction. Alternatively, the line may be powered
by an active nucleus, although the probability of serendipitously discovering
an AGN in the survey volume is only ~0.02. The increasing number of similar
objects reported in the literature indicate that they may be an important,
unstudied population in the high redshift universe.Comment: ApJ in press, 21 pages, 2 figures. Also available at
http://www.mpia-hd.mpg.de/MPIA/Projects/STARS/preprints.htm
Formation and structure of the three Neptune-mass planets system around HD69830
Since the discovery of the first giant planet outside the solar system in
1995 (Mayor & Queloz 1995), more than 180 extrasolar planets have been
discovered. With improving detection capabilities, a new class of planets with
masses 5-20 times larger than the Earth, at close distance from their parent
star is rapidly emerging. Recently, the first system of three Neptune-mass
planets has been discovered around the solar type star HD69830 (Lovis et al.
2006). Here, we present and discuss a possible formation scenario for this
planetary system based on a consistent coupling between the extended core
accretion model and evolutionary models (Alibert et al. 2005a, Baraffe et al.
2004,2006). We show that the innermost planet formed from an embryo having
started inside the iceline is composed essentially of a rocky core surrounded
by a tiny gaseous envelope. The two outermost planets started their formation
beyond the iceline and, as a consequence, accrete a substantial amount of water
ice during their formation. We calculate the present day thermodynamical
conditions inside these two latter planets and show that they are made of a
rocky core surrounded by a shell of fluid water and a gaseous envelope.Comment: Accepted in AA Letter
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