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<h2>Einstein@Home Gamma-ray Pulsar Discoveries in Fermi-LAT Data</h2>
<h3>Info</h3>
+<p>Einstein@Home searches data from NASA's Fermi Gamma-ray Space Telescope for signals from
+gamma-ray pulsars. Pulsars are very compact stars with extreme physical properties compared to normal matter.
+They are rapidly spinning neutron stars that emit pulses, observable from radio to
+gamma-ray wavelengths.</p>
-Bla
-<h3>Results</h3>
+<p>Searching for new pulsars is an enormous computational challenge, because their spin
+frequencies, sky position and other parameters are unknown. Thus, this requires a blind
+search, where one explicitly searches over a dense grid in parameter space. However, the
+number of discrete grid points to cover such multi-dimensional parameter spaces is
+tremendous and renders "brute forces approaches" computationally unfeasible.</p>
-Bla
-<h3>Einstein@Home new pulsar discoveries</h3>
+<p>We have developed novel and much more efficient data-analysis methods for the volunteer
+supercomputer Einstein@Home, which ranks among the fastest 25 computer systems worldwide.
+Einstein@Home has now discovered four new gamma-ray pulsars that were previously
+inaccessible on computational grounds.</p>
+
+<p>These radio and gamma-ray pulsar discoveries provide important contributions to advance
+our (yet very poor) understanding these stellar objects, their population, and their role
+in our Universe.</p>
+<br>
+
+<h3>New Einstein@Home gamma-ray pulsar discoveries</h3>
+
+<p>This page contains information about the Einstein@Home gamma-ray pulsar discoveries. For
+each pulsar we list the volunteers whose computers discovered the pulsar, and the date at
+which the pulsar was found.</p>
+
+<p>We also provide a list of selected characteristics for each
+of the pulsars. Right ascension is one of the two celestial coordinates that specify the
+sky position of the pulsar. Declination is the second of these. The spin frequency describes
+how many time per second the pulsar is rotating. The first frequency derivative describes
+how much the pulsar is slowing down over time. The energy required to emit electromagnetic
+radiation is drawn from the pulsar rotation. The characteristic age is a rough estimate of
+the pulsar's age, computed from the spin frequency and its derivative. Finally, the
+spin-down power is a measure of the total energy emitted by the pulsar. For comparison, our
+Sun outputs roughly 4 x 10<sup>33</sup> erg per second. All pulsars below have a much higher
+spin-down power.</p>
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- Volunteers (Country):<br>
- Date:<br>
+ <b>Volunteers (Country):</b><br>
+ <a href="http://einstein.phys.uwm.edu/show_user.php?userid=107849">David Z (Canada)</a> and <a href="http://einstein.phys.uwm.edu/show_user.php?userid=557206">Test (France)</a><br><br>
+ <b>Date:</b><br>
+ 06 Jan 2012<br><br>
+ <b>Selected pulsar parameters:</b><br>
+ Right ascension: 05:54:05.01(3)<br>
+ Declination: +31:07:41(4)<br>
+ Spin frequency: 2.15 Hz<br>
+ First frequency derivate: -0.66 x 10<sup>-12</sup> Hz/s<br>
+ Characteristic age: 51.7 kyrs<br>
+ Spin-down power: 5.6 x 10<sup>34</sup> erg/s<br>
</td>
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</tr>
<tr>
<td style="vertical-align: top;">
- Volunteers (Country):<br>
- Date:<br>
+ <b>Volunteers (Country):</b><br>
+ <a href="http://einstein.phys.uwm.edu/show_user.php?userid=63414">Mak-ino (Japan)</a> and <a href="http://einstein.phys.uwm.edu/show_user.php?userid=574023">Thomas M. Jackson (USA)</a><br><br>
+ <b>Date:</b><br>
+ 14 Dec 2011<br><br>
+ <b>Selected pulsar parameters:</b><br>
+ Right ascension: 14:22:27.07(1)<br>
+ Declination: -61:38:28(1)<br>
+ Spin frequency: 2.93 Hz<br>
+ First frequency derivate: -0.83 x 10<sup>-12</sup> Hz/s<br>
+ Characteristic age: 55.8 kyrs<br>
+ Spin-down power: 9.6 x 10<sup>34</sup> erg/s<br>
+ </td>
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<td style="vertical-align: top;">
- Volunteers (Country):<br>
- Date:<br>
+ <b>Volunteers (Country):</b><br>
+ <a href="http://einstein.phys.uwm.edu/show_user.php?userid=337084">The NEMO computing cluster (USA)</a> and --<br><br>
+ <b>Date:</b><br>
+ 30 Sep 2011<br><br>
+ <b>Selected pulsar parameters:</b><br>
+ Right ascension: 15:22:05.3(1)<br>
+ Declination: -57:35:00(1)<br>
+ Spin frequency: 9.79 Hz<br>
+ First frequency derivate: -2.99 x 10<sup>-12</sup> Hz/s<br>
+ Characteristic age: 51.8 kyrs<br>
+ Spin-down power: 115.7 x 10<sup>34</sup> erg/s<br>
</td>
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</tr>
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<td style="vertical-align: top;">
- Volunteers (Country):<br>
- Date:<br>
+ <b>Volunteers (Country):</b><br>
+ <a href="http://einstein.phys.uwm.edu/show_user.php?userid=125291">Doug Lean (Australia)</a> and <a href="http://einstein.phys.uwm.edu/show_user.php?userid=103374">Hans-Peter Tobler (Germany)</a><br><br>
+ <b>Date:</b><br>
+ 19 Sep 2011<br><br>
+ <b>Selected pulsar parameters:</b><br>
+ Right ascension: 19:32:19.70(4)<br>
+ Declination: +19:16:39(1)<br>
+ Spin frequency: 4.80 Hz<br>
+ First frequency derivate: -2.15 x 10<sup>-12</sup> Hz/s<br>
+ Characteristic age: 35.4 kyrs<br>
+ Spin-down power: 40.7 x 10<sup>34</sup> erg/s<br>
</td>
</tr>
</tbody>