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Agenda
for the plenary workshop sessions in Astrophysical Messengers.
All links marked with a⇓ can be used to show/hide the abstracts and presentations.
Click here to show/hide all presentations and abstracts and here for a print version.
You may also download the compact program booklet (PDF, 1.9 MB)
and an abstract booklet (PDF, 0.4 MB).
As long as authors provided us with PDF versions of their slides, the corresponding downloads are available on this page.
Monday – Sep 5, 2011
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11:50 – 12:25 |
Astrophysical Messengers I
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Plenary Session (Festsaal) – Chair:
Takaaki Kajita
11:50
(25' + 10')
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Antimatter in space⇓
slides
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Bruna Bertucci (Università degli Studi di Perugia and INFN)
The search for anti-nuclei, as proof of anti-matter on a cosmological scale,
and the precise measurement of light anti-matter, as smoking gun of Dark
Matter annihilations in the galaxy, have been the driving motivations for a
rich experimental program devoted to the quest of the faint anti-matter
signals in the Cosmic Rays. Along several decades, in fact, this research
has been deeply connected to the understanding of the CR sources, their
acceleration and propagation through the galaxy: light anti-matter is
routinely produced in the interactions of primary CR in the interstellar
medium and a clear signature of exotic primary components must rely on the
correct description of the background coming from ordinary sources. Space is
the ideal environment where to carry these studies due to the lack of
atmospheric backgrounds and long exposure times, the impressive results from
PAMELA and FERMI space experiments have puzzled the scientific community and
triggered a lively debate. PAMELA will soon arrive to the end of its
mission, but a new experiment - AMS-02 - is promising new precision
measurements for the next decade. On May 19, 2011 the AMS-02 experiment
started his operation on board of the International Space Station, following
a 51.7° inclined orbit at 390 km from the earth surface. AMS-02 is a large
acceptance magnetic spectrometer conceived for the search of anti-matter as
well as for the precise measurement of the cosmic ray flux components and
energy spectra in the GV-TV rigidity range. Nine layers of silicon
microstrip detectors constitute the core of the spectrometer, allowing the
simultaneous measurement of the charge magnitude and sign of impinging
particles and reconstructing their rigidity up to the TV. A 3D imaging
calorimeter, with a depth of 17 radiation lengths, and a TRD detector allow
an accurate measurement of the electron and positron components and an
effective rejection of the proton background. Velocity measurement and
redundant measurements of the charge magnitude are performed by the four
scintillator planes constituting the Time of Flight system and a Ring
Imaging Cherenkov detector. During the first three months of data taking, 4x109 triggers have been recorded by AMS-02, for a downlinked data sample of
≈ 35 TB. In this contribution, after a review of the actual measurements of
anti-matter in space, we will report on the flight operations of AMS-02 and
its perspectives for physics measurements.
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Thursday – Sep 8, 2011
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09:00 – 10:45 |
Astrophysical Messengers II
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Plenary Session (Festsaal) – Chair:
David Sinclair
09:00
(25' + 10')
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Novel results on low energy neutrino physics⇓
slides
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Gianpaolo Bellini (Università and INFN Milano)
The study of low energy neutrinos from Sun and Earth have produced recently new insights in the neutrino physics. New measurements of the solar fluxes from 7Be and 8B, the first determination of neutrino flux from pep and the study of the day/night effect at low energy have been provided by Borexino. Their impact on the MSW-LMA model in vacuum and transition regions, and on the global fit with only solar, without antineutrino data, are discussed. Implemented analyses of geoneutrinos are also presented in addition to new results, if any, from SuperK, SNO, Kamland. A campaign of data taking in Borexino with artificial sources has been proposed to check the possible existence of a sterile neutrino.
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09:35
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Diffuse supernova neutrino background (DSNB)⇓
slides
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John Beacom (Ohio State University)
The diffuse supernova neutrino background (DSNB) is the weak glow of MeV neutrinos and antineutrinos from distant core-collapse supernovae. The DSNB has not been detected yet, but the Super-Kamiokande (SK) 2003 upper limit on the electron antineutrino flux is close to predictions, now quite precise, based on astrophysical data. If SK is modified with dissolved gadolinium to reduce detector backgrounds, then it should detect the DSNB at a rate of a few events per year, providing a new probe of supernova neutrino emission and the cosmic core-collapse rate. Neutrino astronomy, while uniquely powerful, has proven extremely difficult—only the Sun and the nearby Supernova 1987A have been detected to date—so the promise of detecting new sources soon is exciting indeed.
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10:10
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Future underground large detectors: Prospects and physics case⇓
slides
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Kate Scholberg (Duke University)
A new generation of large underground detectors is being planned to further investigate neutrino mass and mixing and to search for possible CP violation that may provide a hint to the origin of our asymmetric universe. Such detectors would also investigate neutrinos in nature - from the earth's crust to supernovae. The physics case for such a program is presented and plans for detectors worldwide are summarized.
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11:15 – 13:00 |
Astrophysical Messengers III
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Plenary Session (Festsaal) – Chair:
Christian Spiering
11:15
(25' + 10')
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The sources of highest energy cosmic rays and neutrinos⇓
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Eli Waxman (Weizmann Institute)
The construction of large-volume detectors of high energy, >1 TeV, neutrinos is mainly driven by the search for extra galactic neutrino sources. The existence of such sources is implied by the observations of ultrahigh energy, >1019 eV, cosmic rays (UHECRs), the origin of which is still a mystery. The detection of extra galactic neutrinos will allow one to identify the sources of ultrahigh energy cosmic rays and to resolve open questions related to the underlying physics of models of high energy astrophysical sources. Moreover, such detection may allow one to test for neutrino properties (e.g., flavor oscillations and coupling to gravity) with an accuracy many orders of magnitude better than is currently possible. I will discuss the constraints imposed by current cosmic-ray observations on the properties of the (yet unknown) sources of UHECRs, the implications of AUGER CR observations and of Fermi high energy gamma-ray observations to the expected extra galactic neutrino signal, the open questions that neutrino detection may help addressing, and the current state of the experimental efforts.
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11:50
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Cosmic rays at the highest energies⇓
slides
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Angela Olinto (University of Chicago)
After a century of observations, we still don't know the origin of cosmic
rays. I will review the current state of cosmic ray observations at the highest energies, and their
implications for proposed acceleration models and secondary astroparticle
fluxes. Possible sources have narrowed down with the confirmation of a GZK-like
spectral feature. The anisotropy observed by the Pierre Auger Observatory
may signal the dawn of particle astronomy raising hopes for high energy neutrino observations.
However, composition related measurements point to a different
interpretation. A clear resolution of this mystery calls for much larger statistics than the
reach of current observatories.
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12:25
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High energy neutrino astronomy⇓
slides
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Teresa Montaruli (University of Wisconsin - Madison)
It is an exciting time for neutrino astronomy now that the first cubic-kilometer detector (IceCube) has been completed at the South Pole and the first underwater detector is running in its complete configuration (ANTARES). The discovery of high energy astrophysical neutrinos may come any time now. The status of experimental results and how they constrain models is illustrated. Some of them, for instance the fireball model for gamma-ray bursts, may be severely constrained in a few years unless neutrinos will be revealed. In both case, our view of the highest energy universe will probably change and we will have a more complete picture than what we have now when all information come from photon astronomy. A view of the experimental future of this science will be also provided.
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Friday – Sep 9, 2011
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09:35 – 10:45 |
Astrophysical Messengers IV
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Plenary Session (Festsaal) – Chair:
Barbara De Lotto
09:35
(25' + 10')
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Gamma rays: Review of observations⇓
slides
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David Paneque (MPI für Physik)
Our knowledge of the gamma-ray sky has dramatically changed due to the advent of the new Imaging Atmospheric Cherenkov Telescopes (HESS, MAGIC and VERITAS) and satellite-borne instruments (AGILE and Fermi). These facilities boosted the number of gamma-ray sources by one order of magnitude in the last 6 years, providing us with about 2000 sources detected above 100 MeV (from space) and about 100 sources detected above 100 GeV (from the ground). In this talk I will review some of the most exciting observations from this rapidly evolving field, and I will briefly report about the planned facilities for the coming years.
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10:10
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Gamma-rays: Physics interpretation⇓
slides
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Felix Aharonian (DIAS Dublin)
I will discuss the theoretical implications of the recent gamma-ray
observations in the high and very high energy regimes in the context of origin of cosmic rays, physics and astrophysics of relativistic outflows (pulsar winds and AGN jets), as well as cosmological issues related to the extragalactic radiation and magnetic fields.
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11:15 – 12:25 |
Astrophysical Messengers V
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Plenary Session (Festsaal) – Chair:
Eugenio Coccia
11:15
(25' + 10')
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Gravitational waves: Astronomy and astrophysics with gravitational waves in the advanced detector era⇓
slides
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Alan Weinstein (Caltech)
With the advanced gravitational wave detectors coming on line in the next 5 years, we expect to make the first detections of gravitational waves from astrophysical sources, and study the properties of the waves themselves as tests of General Relativity. In addition, these gravitational waves will be powerful tools for the study of their astrophysical sources and source populations. They carry information that is quite complementary to what can be learned from electromagnetic or neutrino observations, probing the central gravitational engines that power the electromagnetic emissions. Preparations are being made to enable near-simultaneous observations of both gravitational wave and electromagnetic observations of transient sources, using low-latency search pipelines and rapid sky localization. We will review the many opportunities for multi-messenger astronomy and astrophysics with gravitational waves enabled by the advanced detectors, and the preparations that are being made to quickly and fully exploit them.
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11:50
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Gravitational waves: Current and future experimental overview⇓
slides
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Kazuaki Kuroda (ICRR Tokyo)
First generation detectors for gravitational waves, LIGO, Virgo with GEO have recently collected astrophysically interesting data with a sensitivity ranging up to a few tens Mpc for coalescences of compact binary stars. However, no traces of gravitational waves have been detected, yet. This negative result gives the upper limit of occurrence rate of several kinds of gravitational wave events in the Universe. In order to obtain positive result, Advanced LIGO started to be installed utilizing the vacuum facility of the initial LIGO and also the advanced Virgo is ready to be built after the present Virgo. During the observation gap in this construction period, GEO will be operated for targeting higher frequency sources as “AstroWatch”, which is upgraded by introducing vacuum squeezed light with refined mirror suspension system (GEOHF). These advanced detectors of laser interferometer are the so-called second generation ones. There is a broad improvement in sensitivity of about a factor of 10. The limits to sensitivity are quantum noise and thermal noise. Below 100 Hz, the sensitivity is limited by quantum noise arising from the fluctuation of photon recoil pressure, which is the result of higher laser power to reduce photon shot noise at higher frequencies. In the critical mid band, thermal noise limited the sensitivity of the best observation frequencies of the first generation detectors. One method to reduce thermal noise is cooling the temperature of mirror with its suspension system. The other method is to widen the beam size on the mirror. In any case, other thermal noise has to be reduced less than the limit of the quantum noise. Although the Advanced LIGO and Advanced Virgo adopt the widened beam size, the cryogenics is applied to LCGT project that has been recently funded to construct in Japan. These second generation detectors will begin observation in 2015-2017 and certainly detect gravitational wave events. In order to open gravitational wave astronomy, these detectors need to be operated in a network to cover the whole sky. The most important item is the positioning accuracy to make useful the collaboration with optical and electromagnetic wave telescopes. At least three detectors are needed to position on the sky and the longer the baseline, the better accuracy is obtained. In addition to the above second generation detectors, there are two planned projects; LIGO-Australia and LIGO-IndIGO. The former project is primarily pursued at this stage by IndIGO and ACIGA collaborations with LIGO partnership. The planned site is in Western Australia, which would be the first southern hemisphere location to augment the observation network.
These ground-based gravitational wave detectors can detect events in the frequency band around 100 Hz. The main frequency band of black hole coalescence is lower than 10 Hz and there are many sources of frequencies of mHz region apart from black holes. In order to observe these gravitational wave sources, space-based laser interferometers are planned and developed. LISA is the joint project of NASA and ESA to fulfill the requirement to achieve the detection of such lower frequency events with higher sensitivity. However, there are uncertainties about the scope of NASA contributions to several large missions, including LISA. Currently, a redesign of LISA is going on, focusing on the worst case of an ESA-led mission. And by using several ideas on transfer, orbit and mission design, most of the original objectives can be retained, while considerably reducing mass and cost. LISA Pathfinder is almost complete and aims to a launch in 2 years from now. DECIGO is the Japanese space mission to cover the frequency gap (100 mHz - 10 Hz) between the LISA and the second generation detectors. The Path Finder of DECIGO is waiting a fund for launch within a few years.
The effort to realize the detection in frequencies at around 10 Hz is being pursued by European researchers as the Einstein Telescope (ET) project. The working group of ET finished its design study this spring and has been made public. It adopts cryogenics in an underground facility with 10 km scale baseline length of laser interferometer. This third generation detector will drastically expand both the observation volume in the Universe and the observation frequency band.
Finally, the projects for gravitational wave detectors who make up the Gravitational Wave International Committee (GWIC) have chances to prepare and study to realize an international collaboration for observation network considering possible collaboration with wider optical and/or electromagnetic and/or astro-particle observations.
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