34,012 research outputs found
Fully automatic telemetry data processor
Satellite Telemetry Automatic Reduction System /STARS 2/, a fully automatic computer-controlled telemetry data processor, maximizes data recovery, reduces turnaround time, increases flexibility, and improves operational efficiency. The system incorporates a CDC 3200 computer as its central element
A Kiloparsec-Scale Hyper-Starburst in a Quasar Host Less than 1 Gigayear after the Big Bang
The host galaxy of the quasar SDSS J114816.64+525150.3 (at redshift z=6.42,
when the Universe was <1 billion years old) has an infrared luminosity of
2.2x10^13 L_sun, presumably significantly powered by a massive burst of star
formation. In local examples of extremely luminous galaxies such as Arp220, the
burst of star formation is concentrated in the relatively small central region
of <100pc radius. It is unknown on which scales stars are forming in active
galaxies in the early Universe, which are likely undergoing their initial burst
of star formation. We do know that at some early point structures comparable to
the spheroidal bulge of the Milky Way must have formed. Here we report a
spatially resolved image of [CII] emission of the host galaxy of
J114816.64+525150.3 that demonstrates that its star forming gas is distributed
over a radius of ~750pc around the centre. The surface density of the star
formation rate averaged over this region is ~1000 M_sun/yr/kpc^2. This surface
density is comparable to the peak in Arp220, though ~2 orders of magnitudes
larger in area. This vigorous star forming event will likely give rise to a
massive spheroidal component in this system.Comment: Nature, in press, Feb 5 issue, p. 699-70
Ionized Nitrogen at High Redshift
We present secure [N II]_(205 μm) detections in two millimeter-bright, strongly lensed objects at high redshift, APM 08279+5255 (z = 3.911) and MM 18423+5938 (z = 3.930), using the IRAM Plateau de Bure Interferometer. Due to its ionization energy [N II]_(205 μm) is a good tracer of the ionized gas phase in the interstellar medium. The measured fluxes are S([N II]_(205 μm)) = (4.8 ± 0.8) Jy km s^(–1) and (7.4 ± 0.5) Jy km s^(–1), respectively, yielding line luminosities of L([N II]_(205 μm)) = (1.8 ± 0.3) × 10^9 μ^(–1) L_⊙ for APM 08279+5255 and L([N II]_(205 μm)) = (2.8 ± 0.2) × 10(^9) μ^(–1) L_⊙ for MM 18423+5938. Our high-resolution map of the [N II]_(205 μm) and 1 mm continuum emission in MM 18423+5938 clearly resolves an Einstein ring in this source and reveals a velocity gradient in the dynamics of the ionized gas. A comparison of these maps with high-resolution EVLA CO observations enables us to perform the first spatially resolved study of the dust continuum-to-molecular gas surface brightness (Σ_(FIR)α Σ^N_CO, which can be interpreted as the star formation law) in a high-redshift object. We find a steep relation (N = 1.4 ± 0.2), consistent with a starbursting environment. We measure a [N II]_(205 μm)/FIR luminosity ratio in APM 08279+5255 and MM 18423+5938 of 9.0 × 10^(–6) and 5.8 × 10^(–6), respectively. This is in agreement with the decrease of the [N II]_(205 μm)/FIR ratio at high FIR luminosities observed in local galaxies
Molecular gas in QSO host galaxies at z>5
We present observations with the IRAM Plateau de Bure Interferometer of three
QSOs at z>5 aimed at detecting molecular gas in their host galaxies as traced
by CO transitions. CO (5-4) is detected in SDSSJ033829.31+002156.3 at z=5.0267,
placing it amongst the most distant sources detected in CO. The CO emission is
unresolved with a beam size of ~1", implying that the molecular gas is
contained within a compact region, less than ~3kpc in radius. We infer an upper
limit on the dynamical mass of the CO emitting region of ~3x10^10
Msun/sin(i)^2. The comparison with the Black Hole mass inferred from near-IR
data suggests that the BH-to-bulge mass ratio in this galaxy is significantly
higher than in local galaxies. From the CO luminosity we infer a mass reservoir
of molecular gas as high as M(H2)=2.4x10^10 Msun, implying that the molecular
gas accounts for a significant fraction of the dynamical mass. When compared to
the star formation rate derived from the far-IR luminosity, we infer a very
short gas exhaustion timescale (~10^7 yrs), comparable to the dynamical
timescale. CO is not detected in the other two QSOs (SDSSJ083643.85+005453.3
and SDSSJ163033.90+401209.6) and upper limits are given for their molecular gas
content. When combined with CO observations of other type 1 AGNs, spanning a
wide redshift range (0<z<6.4), we find that the host galaxy CO luminosity
(hence molecular gas content) and the AGN optical luminosity (hence BH
accretion rate) are correlated, but the relation is not linear: L(CO) ~
[lambda*L_lambda(4400A)]^0.72. Moreover, at high redshifts (and especially at
z>5) the CO luminosity appears to saturate. We discuss the implications of
these findings in terms of black hole-galaxy co-evolution.Comment: Accepted for publication in A&A Letters, 6 pages, 3 figure
Interferometric Observations of Powerful CO Emission from the three Submillimeter Galaxies at z=2.30, 2.51 and 3.35
We report IRAM Plateau de Bure, millimeter interferometry of three z=~2.4 to
3.4, SCUBA deep field galaxies. Our CO line observations confirm the rest-frame
UV/optical redshifts, thus more than doubling the number of confirmed,
published redshifts of the faint submillimeter population and proving their
high-z nature. In all three sources our measurements of the intrinsic gas and
dynamical mass are large (1e10 to 1e11 Msun). In at least two cases the data
show that the submillimeter sources are part of an interacting system. Together
with recent information gathered in the X-ray, optical and radio bands our
observations support the interpretation that the submm-population consists of
gas rich (gas to dynamical mass ratio ~0.5) and massive, composite
starburst/AGN systems, which are undergoing a major burst of star formation and
are evolving into m*-galaxies.Comment: only minor modifications to comply with the ApJL edition rule
Small Energy Scale for Mixed-Valent Uranium Materials
We investigate a two-channel Anderson impurity model with a magnetic
and a quadrupolar ground doublet, and a excited triplet. Using
the numerical renormalization group method, we find a crossover to a non-Fermi
liquid state below a temperature varying as the triplet-doublet
splitting to the 7/2 power. To within numerical accuracy, the non-linear
magnetic susceptibility and the contribution to the linear
susceptibility are given by universal one-parameter scaling functions. These
results may explain UBe as mixed valent with a small crossover scale
.Comment: 4 pages, 3 figures, REVTeX, to appear in Phys. Rev. Let
Simulating non-Markovian stochastic processes
We present a simple and general framework to simulate statistically correct
realizations of a system of non-Markovian discrete stochastic processes. We
give the exact analytical solution and a practical an efficient algorithm alike
the Gillespie algorithm for Markovian processes, with the difference that now
the occurrence rates of the events depend on the time elapsed since the event
last took place. We use our non-Markovian generalized Gillespie stochastic
simulation methodology to investigate the effects of non-exponential
inter-event time distributions in the susceptible-infected-susceptible model of
epidemic spreading. Strikingly, our results unveil the drastic effects that
very subtle differences in the modeling of non-Markovian processes have on the
global behavior of complex systems, with important implications for their
understanding and prediction. We also assess our generalized Gillespie
algorithm on a system of biochemical reactions with time delays. As compared to
other existing methods, we find that the generalized Gillespie algorithm is the
most general as it can be implemented very easily in cases, like for delays
coupled to the evolution of the system, where other algorithms do not work or
need adapted versions, less efficient in computational terms.Comment: Improvement of the algorithm, new results, and a major reorganization
of the paper thanks to our coauthors L. Lafuerza and R. Tora
Detection of M of molecular gas in the host galaxy of the SDSS quasar J0927+2001
We have detected emission by the CO 5-4 and 6-5 rotational transitions at from the host galaxy of the SDSS quasar J0927+2001 using
the Plateau de Bure interferometer. The peak line flux density for the CO 5-4
line is mJy, with a line FWHM = km s. The
implied molecular gas mass is M. We also
detect the 90 GHz continuum at mJy, consistent with a 47K dust
spectrum extrapolated from higher frequencies. J0927+2001 is the second example
of a huge molecular gas reservoir within the host galaxy of a quasar within 1
Gyr of the big bang. Observations of J0927+2001 are consistent with a massive
starburst coeval with a bright quasar phase in the galaxy, suggesting the rapid
formation of both a super-massive black hole through accretion, and the stellar
host spheroid, at a time close to the end of cosmic reionization.Comment: 12 pages, 2 figures, to appear in ApJ Letter
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