183 research outputs found
Relic neutrino masses and the highest energy cosmic rays
We consider the possibility that a large fraction of the ultrahigh energy
cosmic rays are decay products of Z bosons which were produced in the
scattering of ultrahigh energy cosmic neutrinos on cosmological relic
neutrinos. We compare the observed ultrahigh energy cosmic ray spectrum with
the one predicted in the above Z-burst scenario and determine the required mass
of the heaviest relic neutrino as well as the necessary ultrahigh energy cosmic
neutrino flux via a maximum likelihood analysis. We show that the value of the
neutrino mass obtained in this way is fairly robust against variations in
presently unknown quantities, like the amount of neutrino clustering, the
universal radio background, and the extragalactic magnetic field, within their
anticipated uncertainties. Much stronger systematics arises from different
possible assumptions about the diffuse background of ordinary cosmic rays from
unresolved astrophysical sources. In the most plausible case that these
ordinary cosmic rays are protons of extragalactic origin, one is lead to a
required neutrino mass in the range 0.08 eV - 1.3 eV at the 68 % confidence
level. This range narrows down considerably if a particular universal radio
background is assumed, e.g. to 0.08 eV - 0.40 eV for a large one. The required
flux of ultrahigh energy cosmic neutrinos near the resonant energy should be
detected in the near future by AMANDA, RICE, and the Pierre Auger Observatory,
otherwise the Z-burst scenario will be ruled out.Comment: 19 pages, 22 figures, REVTeX
Measurement of telescope transmission using a Collimated Beam Projector
With the increasingly large number of type Ia supernova being detected by
current-generation survey telescopes, and even more expected with the upcoming
Rubin Observatory Legacy Survey of Space and Time, the precision of
cosmological measurements will become limited by systematic uncertainties in
flux calibration rather than statistical noise. One major source of systematic
error in determining SNe Ia color evolution (needed for distance estimation) is
uncertainty in telescope transmission, both within and between surveys. We
introduce here the Collimated Beam Projector (CBP), which is meant to measure a
telescope transmission with collimated light. The collimated beam more closely
mimics a stellar wavefront as compared to flat-field based instruments,
allowing for more precise handling of systematic errors such as those from
ghosting and filter angle-of-incidence dependence. As a proof of concept, we
present CBP measurements of the StarDICE prototype telescope, achieving a
standard (1 sigma) uncertainty of 3 % on average over the full wavelength range
measured with a single beam illumination
A measurement of the millimetre emission and the Sunyaev-Zel'dovich effect associated with low-frequency radio sources
We present a statistical analysis of the millimetre-wavelength properties of 1.4GHz-selected sources and a detection of the Sunyaev–Zel’dovich (SZ) effect associated with the haloes that host them. We stack data at 148, 218 and 277GHz from the Atacama Cosmology Telescope at the positions of a large sample of radio AGN selected at 1.4GHz. The thermal SZ effect associated with the haloes that host the AGN is detected at the 5σ level through its spectral signature, representing a statistical detection of the SZ effect in some of the lowest mass haloes (average M 200 ≈ 10 13 M. h −1 70 ) studied to date. The relation between the SZ effect and mass (based on weak lensing measurements of radio galaxies) is consistent with that measured by Planck for local bright galaxies. In the context of galaxy evolution models, this study confirms that galaxies with radio AGN also typically support hot gaseous haloes. Adding Herschel observations allows us to show that the SZ signal is not significantly contaminated by dust emission. Finally, we analyse the contribution of radio sources to the angular power spectrum of the cosmic microwave background
Constraining Type Ia Supernovae progenitors from three years of SNLS data
While it is generally accepted that Type Ia supernovae are the result of the
explosion of a carbon-oxygen White Dwarf accreting mass in a binary system, the
details of their genesis still elude us, and the nature of the binary companion
is uncertain. Kasen (2010) points out that the presence of a non-degenerate
companion in the progenitor system could leave an observable trace: a flux
excess in the early rise portion of the lightcurve caused by the ejecta impact
with the companion itself. This excess would be observable only under favorable
viewing angles, and its intensity depends on the nature of the companion. We
searched for the signature of a non-degenerate companion in three years of
Supernova Legacy Survey data by generating synthetic lightcurves accounting for
the effects of shocking and comparing true and synthetic time series with
Kolmogorov-Smirnov tests. Our most constraining result comes from noting that
the shocking effect is more prominent in rest-frame B than V band: we rule out
a contribution from white dwarf-red giant binary systems to Type Ia supernova
explosions greater than 10% at 2 sigma, and than 20% at 3 sigma level.Comment: 14 pages, 15 figures, resubmitted to ApJ, figure 15 modifie
Total Absorption Spectroscopy Study of Rb Decay: A Major Contributor to Reactor Antineutrino Spectrum Shape
The antineutrino spectra measured in recent experiments at reactors are
inconsistent with calculations based on the conversion of integral beta spectra
recorded at the ILL reactor. Rb makes the dominant contribution to the
reactor spectrum in the 5-8 MeV range but its decay properties are in question.
We have studied Rb decay with total absorption spectroscopy. Previously
unobserved beta feeding was seen in the 4.5-5.5 region and the GS to GS feeding
was found to be 87.5(25)%. The impact on the reactor antineutrino spectra
calculated with the summation method is shown and discussed.Comment: 6 pages, 3 figure
AB Aurigae::Possible evidence of planet formation through the gravitational instability
Recent observations of the protoplanetary disc surrounding AB Aurigae have
revealed the possible presence of two giant planets in the process of forming.
The young measured age of Myr for this system allows us to place strict
time constraints on the formation histories of the observed planets. Hence we
may be able to make a crucial distinction between formation through core
accretion (CA) or the gravitational instability (GI), as CA formation
timescales are typically Myrs whilst formation through GI will occur within the
first yrs of disc evolution. We focus our analysis on the
M planet observed at AU. We find CA formation
timescales for such a massive planet typically exceed the system's age. The
planet's high mass and wide orbit may instead be indicative of formation
through GI. We use smoothed particle hydrodynamic simulations to determine the
system's critical disc mass for fragmentation, finding M. Viscous evolution models of the disc's mass history
indicate that it was likely massive enough to exceed in the
recent past, thus it is possible that a young AB Aurigae disc may have
fragmented to form multiple giant gaseous protoplanets. Calculations of the
Jeans mass in an AB Aurigae-like disc find that fragments may initially form
with masses M, consistent with the planets which have
been observed. We therefore propose that the inferred planets in the disc
surrounding AB Aurigae may be evidence of planet formation through GI.Comment: 12 pages, 5 figure
Trends and inequalities in short-term acute myocardial infarction case fatality in Scotland, 1988-2004
<p>Abstract</p> <p>Background</p> <p>There have been substantial declines in ischemic heart disease in Scotland, partly due to decreases in acute myocardial infarction (AMI) incidence and case fatality (CF). Despite this, Scotland's IHD mortality rates are among the worst in Europe. We examine trends in socioeconomic inequalities in short-term CF after a first AMI event and their associations with age, sex, and geography.</p> <p>Methods</p> <p>We used linked hospital discharge and death records covering the Scottish population (5.1 million). Between 1988 and 2004, 178,781 of 372,349 patients with a first AMI died on the day of the event (Day0 CF) and 34,198 died within 28 days after surviving the day of their AMI (Day1-27 CF).</p> <p>Results</p> <p>Age-standardized Day0 CF at 30+ years decreased from 51% in 1988-90 to 41% in 2003-04. Day1-27 CF decreased from 29% to 18% over that period. Socioeconomic inequalities in Day0 CF existed for both sexes and persisted over time. The odds of case fatality for men aged 30-59 living in the most deprived areas in 2000-04 were 1.7 (95%CI: 1.3-2.2) times as high as in the least deprived areas and 1.9 (1.1-3.2) times as high for women. There was little evidence of socioeconomic inequality in Day1-27 CF in men or women. After adjustment for socioeconomic deprivation, significant geographic variation still remained for both CF definitions.</p> <p>Conclusions</p> <p>A high proportion of AMI incidents in Scotland result in death on the day of the first event; many of these are sudden cardiac deaths. Short-term CF has improved, perhaps reflecting treatment advances and reductions in first AMI severity. However, persistent socioeconomic and geographic inequalities suggest these improvements are not uniform across all population groups, emphasizing the need for population-wide primary prevention.</p
High-energy Neutrino Astronomy: The Cosmic Ray Connection
This is a review of neutrino astronomy anchored to the observational fact
that Nature accelerates protons and photons to energies in excess of
and eV, respectively.
Although the discovery of cosmic rays dates back close to a century, we do
not know how and where they are accelerated. Basic elementary-particle physics
dictates a universal upper limit on their energy of eV, the
so-called Greisen-Kuzmin-Zatsepin cutoff; however, particles in excess of this
energy have been observed by all experiments, adding one more puzzle to the
cosmic ray mystery. Mystery is fertile ground for progress: we will review the
facts as well as the speculations about the sources including gamma ray bursts,
blazars and top-down scenarios.
The important conclusion is that, independently of the specific blueprint of
the source, it takes a kilometer-scale neutrino observatory to detect the
neutrino beam associated with the highest energy cosmic rays and gamma rays. We
also briefly review the ongoing efforts to commission such instrumentation.Comment: 83 pages, 18 figures, submitted to Reports on Progress in Physic
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