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In order to enable an iCal export link, your account needs to have a key created. This key enables other applications to access data from within Indico even when you are neither using nor logged into the Indico system yourself with the link provided. Once created, you can manage your key at any time by going to 'My Profile' and looking under the tab entitled 'HTTP API'. Further information about HTTP API keys can be found in the Indico documentation.
I have read and understood the above.
In conjunction with a having a key associated with your account, to have the possibility of exporting private event information necessitates the creation of a persistent key. This new key is also associated with your account and whilst it is active the data which can be obtained through using this key can be obtained by anyone in possession of the link provided. Due to this reason, it is extremely important that you keep links generated with this key private and for your use only. If you think someone else may have acquired access to a link using this key in the future, you must immediately remove it from 'My Profile' under the 'HTTP API' tab and generate a new key before regenerating iCalendar links.
I have read and understood the above.
Permanent link for public information only:
Permanent link for all public and protected information:
The Cygnus arm of the galaxy contains a large number of
energetic astrophysical sources, including numerous
supernova remnants (SNRs), pulsar wind nebulae (PWN) and
X-ray binary systems. Indeed, in terms of potential
galactic sources needed to explain the origin of the
high energy cosmic rays, Cygnus is the promising region
accessible to northern hemisphere observatories using
the air s
... More
The H.E.S.S. telescope has detected a new very high energy gamma-ray point-like
source, HESS J0632+058. It is the first point-like source detected by H.E.S.S.
without any obvious counterpart. The excess lies in a region where interaction
between the Monoceros supernova remnant and the Rosette Nebula may occur. The energy
spectrum of the observed gamma-rays is well described by a power law of i
... More
Presented by Mr. Armand FIASSON
on
4/7/2007
at
16:30
The TeV source J2032+4130 is the first unidentified detection in very high
energy astrophysics and remains so. There have been contradictory claims
regarding its extension, flux level and variability in gamma-rays, although
the longest and most sensitive observation up to now favor a steady, extended
source. MAGIC has devoted more than 80 hours on J2032+4130 observations during
2005 and 2006.
... More
Presented by Dr. Emma OÑA-WILHELMI
on
4/7/2007
at
16:06
The South Pole Air Shower Experiment (SPASE-2) began operation in 1996 and took data
until it was decommissioned in December, 2006. We are currently analyzing some 200
million reconstructed events taken between 1997 and the end of 2006. In this paper we
report on a search for 100 TeV gamma-rays from three specific Southern hemisphere
point sources discovered by H.E.S.S. to have gamma-ray spect
... More
Presented by Dr. Xinhua BAI (*!)
on
4/7/2007
at
16:18
Many of the unidentified Egret sources are believed to be young pulsars.
Such young not-identified pulsars should be surrounded by pulsar wind
nebulae which are at present well established TeV gamma-ray sources
(like Vela X, MSH 15-52 and G0.9+0.1). Moreover, other type of
gamma-ray sources are likely, i.e. binary systems, molecular clouds,
supernovae
remnants, massive stars. The Milagro exp
... More
Presented by Mr. Hendrik BARTKO
on
4/7/2007
at
15:30
The Tibet air shower array experiment has been conducted at Yangbajing
(90.522°E, 30.102°N; 4300m above sea level) in Tibet, China, Since 1990. A
search for extended emission from Cygnus region was carried out using data
taken from the Tibet III (1999 November -2005 November) arrays. Spreading
across -3° to ~3° in Galactic latitude and 65°to ~85°in Galactic
longitude, an excess tha
... More
The gamma-quantum spectra produced by the electronic and hadronic components of
cosmic rays have similar shapes at the energies from 1GeV to 1 TeV due to the
synchrotron losses of the electrons. So, the only observational possibility to
discriminate between leptonic and hadronic contributions is to measure the
gamma-quantum spectrum at energies higher than 1 TeV, where these two spectra are
e
... More
Presented by Vera Yurievna SINITSYNA
on
4/7/2007
at
16:42
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