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<!DOCTYPE html>
<html lang="en">
<head>
<meta charset="utf-8">
<meta http-equiv="X-UA-Compatible" content="IE=edge">
<meta name="viewport" content="width=device-width, initial-scale=1">
<meta name="description" content="">
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<title>TRAPUM</title>
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<span class="sr-only">Toggle navigation</span>
<span class="icon-bar"></span>
<span class="icon-bar"></span>
<span class="icon-bar"></span>
</button><a class="navbar-brand page-scroll" href="#page-top">TRAPUM</a>
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<div class="collapse navbar-collapse navbar-ex1-collapse">
<ul class="nav navbar-nav">
<!-- Hidden li included to remove active class from about link when scrolled up past about section -->
<li class="hidden">
<a class="page-scroll" href="#page-top"></a>
</li>
<li>
<a class="page-scroll" href="#goals">Goals</a>
</li>
<li>
<a class="page-scroll" href="#plan">Plan</a>
</li>
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<a class="page-scroll" href="#news">News</a>
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<a class="page-scroll" href="#team">Team</a>
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<a class="page-scroll" href="#organisation">Organisation</a>
</li>
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<a class="page-scroll" href="#publication">Publications</a>
</li>
<li>
<a class="page-scroll" href="#public-engagement">Engagement</a>
</li>
<li>
<a class="page-scroll" href="#data">Data</a>
</li>
<!--
<li>
<a class="page-scroll" href="#policy">Policy Docs</a>
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<li>
<a class="page-scroll" href="/discoveries/"><b>DISCOVERIES</b></a>
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<!-- Intro Section -->
<section id="intro" class="intro-section bgeven">
<div class="container">
<div class="row">
<div class="col-lg-12">
<h1>
<figure>
<img alt="logo1" src="images/TRAPUM_logo_colour_CMYK_reversed_A_lock-up_04.png"
style="width:100%">
<br>
</figure>
</h1>
<em>Image provided by <a href='http://www.ska.ac.za/'>SKA South Africa</a></em>
</p><a class="btn btn-default page-scroll" href="#goals">
<!--Our goal is to discover and understand pulsars and fast transients using MeerKAT.-->
<span class="glyphicon glyphicon-menu-down"></span> Scroll down to discover more <span
class="glyphicon glyphicon-menu-down"></span>
</a>
<p style="padding-top: 1em;" ]>
<a href='#news' class="page-scroll">
<span class="glyphicon glyphicon-chevron-right"></span>
<span class="glyphicon glyphicon-chevron-right"></span>
<span class="glyphicon glyphicon-chevron-right"></span>Latest TRAPUM news<span
class="glyphicon glyphicon-chevron-left"></span>
<span class="glyphicon glyphicon-chevron-left"></span>
<span class="glyphicon glyphicon-chevron-left"></span>
</a>
</p>
</div>
</div>
</div>
</section>
<!-- About Section -->
<section id="goals" class="goals-section bgodd">
<div class="container">
<div class="row">
<div class="col-lg-12">
<h1>TRAPUM Survey Goals</h1>
<p>
Utilising the power of MeerKAT, TRAPUM will discover numerous new pulsars and transient events
in order to expand our knowledge of the populations of sources which emit at radio wavelengths
on timescales ranging from microseconds to seconds. The discovery and continued study of these
objects provides a powerful tool to improve our understanding of physics in extreme
environments.
</p>
</div>
</div>
<div class="row">
<div class="col-lg-8">
<h2>Science Themes</h2>
<p>The science case for TRAPUM covers a broad range of neutron-star, galactic and extra-galactic
astrophysics as well as gravitational and high-energy physics. The primary science objectives
are:
<ul>
<li>
<strong>Increasing the sample size of all types of radio pulsars</strong>, constraining the
birth rates and distribution of neutron stars in the Galaxy.
</li>
<li>
<strong>Exploring the properties and evolution of globular clusters</strong> by discovering
and timing many new pulsars and transients associated with them.
</li>
<li>
<strong>Investigate the dependence of the pulsar and fast transient populations on host
galaxy properties</strong>, by searching for them in external galaxies.
</li>
<li>
<strong>Improve our understanding of gravity</strong>, by discovering relativistic binaries
and millisecond pulsars suitable for gravitational wave experiments.
</li>
<li>
<strong>Working with <a href='http://www.meertrap.org/'>MeerTRAP</a> Expand the searchable
parameter space for fast transient radio sources</strong>, enabling study of the most
energy-dense events in the Universe, and potentially identify electromagnetic counterparts
to gravitational radiation events and <strong>Search for high red-shift radio
bursts</strong> and use them to refine cosmology.
</li>
</ul>
</p>
</div>
<div class="col-lg-4">
<figure>
<img alt="supernova" src="images/CasA.png">
<br>
<figcaption>The Cassiopeia A supernova remnant.<br>(Chandra/NASA)</figcaption>
</figure>
</div>
</div>
<div class="row">
<div class="col-lg-12">
<p>This science-impact driven project plays to the strengths of the MeerKAT telescope in time-domain
astrophysics, the excellent sensitivity allows for the detection of these very faint radio
sources, and the high instantaneous spatial resolution enables localisation of events that last
for a fraction of a second. This capability for localisation of radio transients is critical to
the using and understanding the exotic and currently unknown origins of many of these events.
</p>
<p>These science goals will be achieved through a series of targeted searches, capitalising on the
sensitivity of MeerKAT to make significant new discoveries.</p><a
class="btn btn-default page-scroll" href="#plan">
<span class="glyphicon glyphicon-menu-down"></span> Read more about the survey plan below <span
class="glyphicon glyphicon-menu-down"></span>
</a>
</div>
</div>
</div>
</section>
<section id="plan" class="plan-section bgeven">
<div class="container">
<div class="row">
<div class="col-lg-12">
<h1>Survey Plan</h1>
</div>
</div>
<div class="row">
<div class="col-lg-8">
<p>
<strong>Targeted pulsar searches of SNRs, PWNe, and unidentified Fermi gamma-ray
sources</strong>
<br>Supernova remnants (SNRs), pulsar wind nebulae (PWNe) and Fermi gamma-ray sources host,
arguably, some of the most interesting radio pulsars. The discovery of a radio pulsar coincident
with a SNR/PWN/gamma-ray source is crucial for understanding the energy budget of such systems
and, vice-versa, multi-wavelength counterparts provide substantially more context for
understanding the nature of the radio pulsar itself. Discovering young pulsars associated with
SNRs or PWNe is important for understanding the Galactic neutron star formation rate, the nature
of the supernova explosion, and the injection of high-energy particles into the interstellar
medium. Unidentified Fermi gamma-ray sources provide a treasure map for deep pulsar searches
and, for example: the millisecond pulsars (MSPs) found can probe accretion physics (e.g.
"transitional" MSPs), provide new precision timers for the International Pulsar Timing Array, as
well as identify exotic binaries capable of testing gravity and/or constraining the neutron star
equation of state.
</p>
<p>
<strong>Globular Cluster Searches</strong>
<br>Globular clusters (GCs) harbor a very large number of MSPs per unit stellar mass compared
with the Galactic plane. This is because the dense stellar environments in the cores
(10<sup>4</sup> − 10<sup>3</sup> M<sub>⊙</sub> pc<sup>−3</sup>) promote collisions and exchange
interactions that create binaries capable of recycling old neutron stars to become MSPs. A total
of 146 pulsars have been discovered in globular clusters to date, the majority of them MSPs.
Some clusters are spectacularly prolific: Terzan 5 and 47 Tuc host 34 and 25 pulsars
respectively. Surveying them with MeerKAT therefore has the potential for rich and rapid reward.
</p>
</div>
<div class="col-lg-4">
<table>
<caption>Approximate fraction of observation time spent on each survey component as granted in
2016.</caption>
<tr>
<th>Target</th>
<th>Fraction</th>
</tr>
<tr>
<td>
<acronym title="Supernova Remnants">SNRs</acronym>,<acronym
title="Pulsar Wind Nebulae">PWNe</acronym>,<acronym
title="Tera-electron-Volt emission sources">TeV</acronym> & <acronym
title="Fermi gamma-ray sources">γ-ray</acronym>
</td>
<td>44%</td>
</tr>
<tr>
<td>Globular Clusters</td>
<td>33%</td>
</tr>
<tr>
<td>Nearby Galaxies</td>
<td>22%</td>
</tr>
</table>
</div>
</div>
<div class="row">
<div class="col-lg-12">
<p>
<strong>Extragalactic pulsar and transient searches</strong>
<br>
MeerKAT has the sensitivity to reveal new pulsars and fast transients beyond the Milky Way.
Studying extragalactic pulsars we can help us understand the relationship between the formation
of neutron stars and their environement. Only 29 such extragalactic pulsars are known, and all
are located in the Magellanic Clouds. Using MeerKAT we will reach a survey sensitivity beyond
anything other survey performed before to study not only the Magellanic Clouds but also other
galaxies of the local group and beyond. Detecting pulsars and fast transients outside the local
group, and determining how much their signal was dispersed by the intergalactic medium will
begin to provide us with the tools needed to probe the structure of the intergalact medium.
Moreover, understanding the nearby population of giant pulse emitting, or radio-emitting
magnetars, has gained even more importance given that they are proposed models for at least some
of the fast radio bursts (FRBs) and this is further highlighted by the recent discovery of a
repeating FRB.
</p>
<p>
<strong>Towards a Galactic census</strong>
<br>
The known pulsar population has increased by nearly 50% sources, since 2010 when TRAPUM was
first envisioned.
This increase has been achieved by improving techniques and methods on existing telescopes, and
new telescopes like LOFAR.
Still, the task of finding even more pulsars could not be more timely.
With new pulsars, new science is enabled, resulting from the bulk properties of the discovered
population, from discovered pulsars being probes of the surrounding medium, or by being
exceptional laboratories for testing theories of gravity. With MeerKAT being many times more
sensitive than Parkes, the previous largest dish used for pulsar searches in the South, the
search for pulsars in the
Galactic plane - the birth place of pulsars - provides a significant and rare sharp increase in
sensitivity for exploring the dynamic radio sky. The hundreds of beams combined with much
increased sensitivity mean a significant increase in search capability, making a large-scale
survey with MeerKAT not only possible, but in fact mandatory. With time provided by MPIfR’s
“S-Band Project”, TRAPUM will conduct a L-Band survey along parts of the inner Galaxy. This
TRAPUM survey will be the most sensitive survey of the inner Galactic plane ever conducted,
being the benchmark and testbed for the later SKA surveys.
</p>
<p>
<strong>Using pulsars to probe gravity, dark matter & stellar populations in the Galactic
Centre</strong>
<br>The discovery of a pulsar closely orbiting the super-massive black hole at the centre of our
Galaxy, Sgr A*, would not only supersede all previous tests of General Relativity (GR) in\
the strong-field regime, it would also enable the space-time around a rotating black hole to be
probed with high precision and in a model independent fashion; for example, allowing tests of
the cosmic censorship conjecture and the no hair theorem. Such a "laboratory" for precision
tests of GR and black hole physics would be unrivalled by any future astrometric measurements of
the S-Stars. Furthermore, mass-segregation
in the central parsec may also lead to the presence of additional gravitational testbeds in the
form of stellar-mass pulsar black hole binaries. As part of the MPIfR “S-Band Project”, the
Max-Planck receivers will be used to conduct a sensitive survey of the innermost region of the
Galaxy in the vicinity of the black hole. The MPIfR will share the results with TRAPUM as input
for further studies.
</p>
<p>
<strong>Fast transients – working with <a href='http://www.meertrap.org/'>MeerTRAP</a> to
discovering and understand source populations</strong>
<br>The fast transient landscape has changed dramatically since 2010 with the discovery of the
population of FRBs, including the revelation that some repeat, which are exciting in themselves
but also highlighted that the dynamic radio sky is still largely unexplored and with potentially
more rich rewards. MeerKAT’s unique combination of wide FoV, high sensitivity, and wide
bandwidth will provide supreme sensitivity per unit time and frequency making it a prime
instrument to study the transient sky. We will carry out <em>commensal observing for fast
transients on all of the TRAPUM observations</em> proposed here: High energy point sources
and SNRs, globular clusters and external galaxies. </br>
<!--
<br> Although not yet granted observing time we also consider here the exciting possibility of
the detectability of Lorimer-burst brightness (30 Jy and >400-σ) FRBs with a <strong>MeerKAT
Fly’s Eye experiment</strong> (i.e. single-dish observing). In Fly’s Eye mode, MeerKAT will
instantaneously cover 0.8 × 64 = 51.2 deg<sup>2</sup>, and will therefore be able to detect
rare, bright transient events. Finally, alongside the sheer increase in the number of FRBs
detected the other major development is that FRB 121102 has exhibited repeated bursts seen both
at Arecibo and with the GBT (Scholz et al. 2016). These bursts are characterised by a range of
flux density and strongly varying spectral indices and a wide range of modulation indices that
have so far prevented the detection of any possible underlying periodicity. The repeating nature
indicates that they are not from a cataclysmic event and suggest that at least some FRBs are
possibly associated with neutron star origins, like magnetars or giant pulses from radio
pulsars. Crucial to understanding what this means for the FRB population as a whole is
<em>determining if all FRBs repeat</em> or whether there are multiple classes.
</p>
-->
<p>
<strong>Follow Up Timing </strong>
<br>After the initial discovery of a pulsar, we want to extract as much science as possible by
follow-up timing. Therefore, it is an absolutely crucial aspect of characterising the new TRAPUM
pulsars to get a timing solution. In its most basic form this means getting an accurate
position, period and period derivative so that one can compare the pulsar properties with the
known pulsar population, and in particular for those sources that are found in our targeted
searches we are interested in knowing their characteristic ages and their spin-down energies to
compare with the SNRs and high energy emission, for example. We are also interested in
determining whether or not the sources are potentially high precision timers and so useful for
gravitational wave searches, and/or members of binary systems and so potentially useful for mass
determinations or tests of gravity.
</p>
</div>
</div>
</section>
<section id="news" class="news-section bgodd">
<div class="container">
<div class="row">
<div class="col-lg-12">
<h1>TRAPUM News</h1>
<h3>Globular cluster pulsar population doubles in 5 years</h3>
<span class='date'> <span class="glyphicon glyphicon-time"></span>Oct 2023</span>
<p>
With the most recent discoveries by the MeerKAT and FAST radio telescopes, the <a
href="https://www3.mpifr-bonn.mpg.de/staff/pfreire/GCpsr.html">number of pulsars
known in globular clusters has grown to 302</a>, up from around 150 at the end of 2018. This
doubling of the population in 5
years is a testament to the immense sensitivity of MeerKAT and FAST, with the TRAPUM project
alone now accounting for 28% of all globular cluster pulsar discoveries!
</p>
<h3>Einstein@Home joins the TRAPUM effort to search for pulsars</h3>
<span class='date'> <span class="glyphicon glyphicon-time"></span>Jan 2023</span>
<p>
We have recently initiated a project to search for exotic binary pulsars in TRAPUM globular cluster data
using spare compute cycles of computers from volunteers all around the world. This is part of the already
running Einstein@Home project, which has been running successfully for nearly two decades and has discovered
more than 80 pulsars. Anyone with a personal computer can freely sign up as a volunteer following the instructions
on the <a href="https://einsteinathome.org/">Einstein@Home website</a> and join our large-scale effort for
discovering unique pulsars.
</p>
<h3>First Nearby Galaxies publication and first LMC observations!</h3>
<span class='date'> <span class="glyphicon glyphicon-time"></span>Oct 2022</span>
<p>
The Nearby Galaxies working group has now published its first paper! It can be found in the
"Publications" section of this website. Remarkably, the first two observations of the Large
Magellanic Cloud already revealed 6 new pulsars! The Small Magellanic Cloud survey is also well
under way with 7 pulsar discoveries, doubling the currently known population. In addition,
nearby galaxies Sextans A and B have been surveyed and a Fast Radio Burst has been found
serendipitously. A survey of NGC 253 is currently being processed. Details of our discoveries
can be found on the <a href="/discoveries/"> DISCOVERIES </a> page.
</p>
<h3>TRAPUM/MMGPS Reaches 100 Discoveries!</h3>
<span class='date'> <span class="glyphicon glyphicon-time"></span>Jan 2022</span>
<p>
We are proud to announce that TRAPUM together with its sister project the MPIfR MeerKAT Galactic Plane
Survey (MMGPS) have surpassed 100 pulsar discovieries. Given the source classes that TRAPUM has
targeted, more than 60 of these new pulsars have periods below 30 milliseconds with 37 confirmed
to be in binary systems. This represents more than a 10% increase in the total number of
millisecond pulsars known. With the majority of the discovieres coming since the start of 2021
we are optimistic that we can continue our fantastic discovery rate into 2022 and beyond.
Details of our discoveries can be found on the <a href="/discoveries/"> DISCOVERIES </a> page.
</p>
<h3>TRAPUM First Year Review</h3>
<span class='date'> <span class="glyphicon glyphicon-time"></span>Jan 2022</span>
<p>
Towards the end of 2021 the TRAPUM collaboration submitted its first report on operations to
SARAO. The report detailed how the addition of instrumentation from TRAPUM has enabled MeerKAT
to become a premium pulsar and fast transient discovery machine, with TRAPUM discovering 36
pulsars in 11 globulsar clusters, 3 pulsars in the Small Magellanic Cloud and 15 pulsars (of
which 14 are millisecond pulsars) in Fermi-LAT sources. The collaboration received positive
feedback from the review committee with the reviewers noting that "The TRAPUM team has
demonstrated, through their hard work in collaboration with SARAO teams, that MeerKAT (and by
extension SKA1-MID) can be a prolific pulsar search instrument. This required the development of
novel instrumentation, and they are to be commended for their achievements. Their transparency
in making discovery details public is also welcome. Given their activities and results so far,
it would appear that the team is well poised to make major impacts in pulsar astrophysics."
</p>
<h3>First Extragalactic Pulsar Discoveries!</h3>
<span class='date'><span class="glyphicon glyphicon-time"></span> 2021</span>
<p>
We have started our observations of the Small Magellanic Cloud with TRAPUM in 2021. We have
nearly completed four out of eight pointings in this L-band survey, which uses 769 coherent
beams and the core dishes of MeerKAT. The survey is partially targeted to supernova remnants and
pulsar wind nebulae. We have discovered several new extragalactic pulsars in the SMC, which you
can read about on the <a href="/discoveries/"> DISCOVERIES </a> webpage. We are also observing
other nearby galaxies with the full array.
</p>
<h3>First Fermi Unidentified Sources Search Observations!</h3>
<span class='date'><span class="glyphicon glyphicon-time"></span> 20 June 2020</span>
<p>
We have made our first observations of a set of Fermi Unidentified Sources with TRAPUM. We
observed about a dozen sources using all the available telescopes and about 250 beams arranged
to sample the entire gamma-ray error circle of the sources. This forms the first set of sources
in our sample prepared for our initial shallow survey which is using the L-band receiver and
will include a two-pass approach. News on <a href="/discoveries/"> DISCOVERIES </a> soon.
</p>
<h3>First Globular Cluster Observations!</h3>
<span class='date'><span class="glyphicon glyphicon-time"></span> April & May 2020</span>
<p>
TRAPUM has made its first observations! Using all the available telescopes 288 beams were formed
and used to observe the clusters Terzan 5, 47 Tucanae and NGC 6624 for about 4 hours each. Data
analysis is ongoing. Stand by for announcements of discoveries which will appear on our <a
href="/discoveries/"> DISCOVERIES </a> webpage.
</p>
<h3>Globular Cluster Pulsars Discovered</h3>
<span class='date'><span class="glyphicon glyphicon-time"></span> Update May 2020 </span>
<p>
Working with the <a href="http://www.meertime.org/"> MeerTIME </a> team we have searched 10
Globular clusters using search mode data recorded using the PTUSE backends for a beam pointed at
one of the known pulsars in the cluster. So far we have discovered 10 new pulsars and you can
find a summary of the details of these pulsars at our <a href="/discoveries/"> DISCOVERIES </a>
webpage. The TRAPUM surveys will use between 250 and 400 beams to allow for covering the entire
cluster and will be able to use all 64 dishes to give greater sensitivity.
</p>
<h3>Proposal Submitted</h3>
<span class='date'><span class="glyphicon glyphicon-time"></span> 2016-06-19</span>
<p>
A proposal describing the updated science case and observing request for TRAPUM has been
submitted.
</p>
<h3>Website created</h3>
<span class='date'><span class="glyphicon glyphicon-time"></span> 2016-06-16</span>
<p>
The TRAPUM website, <a href='http://trapum.org'>trapum.org</a>, has been launched. Publications,
data releases and survey status updates will appear here once the survey is underway.
</p>
</div>
</div>
</div>
</section>
<section id="team" class="team-section bgeven">
<div class="container">
<div class="row">
<div class="col-lg-12">
<h1>Team members</h1>
<h3>PIs</h3>
<ul>
<li>Ben Stappers (UK)</li>
<li>Michael Kramer (DE)</li>
</ul>
<h3>Project Scientist</h3>
<ul>
<li>Ewan Barr (DE)</li>
</ul>
<h3>Working Group Chairs</h3>
<ul>
<li>Lina Levin-Preston (UK, Nearby Galaxies)</li>
<li>Ben Stappers (UK, PWNe/SNR/TeV WG)</li>
<li>Rene Breton (UK, Fermi WG Co-chair)</li>
<li>Colin Clark (DE, Fermi WG Co-chair)</li>
<li>Alessandro Ridolfi (IT, Globular Clusters WG)</li>
<li>Marta Burgay (IT, Follow-up WG)</li>
</ul>
<h3>Co-Is</h3>
</div>
</div>
<div class="row">
<div class="col-lg-4">
<ul>
<li>Federico Abbate (IT)</li>
<li>Anjana Ashok (DE)*</li>
<li>Matthew Bailes (AU)</li>
<li>Vishnu Balakrishnan (DE)</li>
<li>Werner Becker (DE)</li>
<li>Miquel Colom I Bernadich (DE)*</li>
<li>Joanna Berteaud (FR)</li>
<li>Mechiel Bezuidenhout (UK)*</li>
<li>Markus Böttcher (SA)</li>
<li>Sarah Buchner (SA)</li>
<li>Francesca Calore (NL)</li>
<li>Emma Carli (UK)*</li>
<li>David Champion (DE)</li>
<li>Weiwei Chen (DE)</li>
<li>Ismaël Cognard (FR)</li>
<li>Sergio Belmonte Diaz (UK)*</li>
<li>Oliver Dodge (UK)*</li>
<li>Andrew Douglas (USA)*</li>
</ul>
</div>
<div class="col-lg-4">
<ul>
<li>Liam Dunn (AUS)*</li>
<li>Arunima Dutta (DE)*</li>
<li>Ralph Eatough (CH)</li>
<li>Elisabeth Ferrara (USA)</li>
<li>Paulo Freire (DE)</li>
<li>Tasha Gautam (DE)*</li>
<li>Lucía Gebauer Werner(DE)*</li>
<li>Marisa Geyer (SA)</li>
<li>Marisa Geyer (SA)</li>
<li>Heinrich Hurter (SA)*</li>
<li>Jean-Mathias Griessmeier (FR)</li>
<li>Jedrzej Jawor (DE)*</li>
<li>Tana Joseph (NL)</li>
<li>Ramesh Karuppusamy (DE)</li>
<li>Evan Keane (IRL)</li>
<li>Lars Künkel (DE)*</li>
<li>Yunpeng Men (DE)</li>
<li>Vanessa McBride (SA)</li>
<li>Rouhin Nag (IT)*</li>
<li>Lars Nieder (DE)</li>
<li>Prajwal Voraganti Padmanabh (DE)</li>
<li>Adipol Phosrisom (UK)*</li>
<li>Viviana Piga (IT)*</li>
</ul>
</div>
<div class="col-lg-4">
<ul>
<li>Denisha Pillay (DE)*</li>
<li>Andrea Possenti (IT)</li>
<li>Venu Prayag (SA)*</li>
<li>Harry Qui (UK)</li>
<li>Isabella Rammala (DE)</li>
<li>Shilpa Ranchod (DE)*</li>
<li>Scott Ransom (US)</li>
<li>Shalini Sengupta (DE)*</li>
<li>Maciej Serylak (UK)</li>
<li>Tinn Thongmeearkom (UK)*</li>
<li>Naomi Titus (SA)</li>
<li>James Turner (UK)*</li>
<li>Vivek Venkatraman Krishnan (DE)</li>
<li>Christo Venter(SA)</li>
<li>Laila Vleeschower Calas (UK)*</li>
<li>Stefan Wagner (DE)</li>
<li>Patrick Weltevrede (UK)</li>
<li>Christoph Weniger (NL)</li>
<li>Norbert Wex (DE)</li>
</ul>
</div>
</div>
<p>* Student</p>
</div>
</div>
</section>
<section id="organisation" class="organisation-section bgodd">
<div class="container">
<div class="row">
<div class="col-lg-12">
<h1>Project Organisation:</h1>
<p>The management of the TRAPUM project will
build upon experience gained from our membership
in other large international collaborations such
as LOFAR, the EPTA and SUPERB. An executive
committee composed of the two PIs (Stappers and
Kramer) and a further five members will be the
decision making body responsible for
organisation, membership, resolution, funding
and planning. These five additional members
correspond to approximately 10% of the total
membership and will be drawn from each of the
science working groups (see below), respecting
diversity in nationality and gender, and will
serve a limited term of no more than two
years. The PIs will have the casting vote if
required. While the science working groups will
have significant overlap in membership and
science topics they will have clear and distinct
goals. In addition there will be two technology
working groups which will work with and across
all the science groups to provide the hardware,
software and practical development necessary to
meet the scientific goals. It is expected that
the technology group members will have strong
overlap with all the scientific groups, with at
least one member from each present.</p>
<h2>The working groups are broken down into the following:</h2>
<ul>
<li><strong>Galactic plane survey:</strong> Planning and executing the Galactic plane and Fermi
excess survey. This is the largest single observing project and will require strong
coordination of resources to ensure the most ecient observing. It will liase strongly with
the targeted surveys group to ensure no overlap of targets.</li>
<li><strong>Targeted surveys:</strong> Planning and executing the surveys of the Galactic
centre, globular clusters, exter- nal galaxies and high-energy sources. These surveys are
grouped together as they all require similar approaches, but they will be broken down
further into specific teams which may not include all members.</li>
<li><strong>Pulsar follow-up:</strong> Extracting maximum information from newly discovered
pulsars eciently. Liaise with MeerKAT and worldwide pulsar timing projects for follow up
radio timing. Organise observations at high energies, optical and perhaps non-photonic
windows.</li>
<li><strong>Transient survey and follow-up:</strong> Detection of transient signals and
triggering of multi-wavelength follow- up observations. Have agreements in place with a
variety observatories to follow-up transients at short notice. Liase with ThunderKAT for
follow up as well.</li>
<li><strong>Commensal observing survey:</strong> This task will involve liaising with
the different working groups to determine what
resources can be used and when and also to
optimise the observing strategies of the
targeted surveys described above to ensure optimal transient detection capabilities. Overlap
with the follow up component of the Transients working group.</li>
<li><strong>Beamforming:</strong> Development of scheme for phasing up array and polarisation
and flux calibration. Includes experts who have performed similar work with other arrays
like WSRT,VLA and LOFAR. Majority of the work will be in the initial phases of roll out of
beamforming, but then will have a continuing reduced role to assess problems if/when they
arise with calibration and related issues.</li>
<li><strong>Processing:</strong> Particular focus on searching multiple data streams for
periodic and transient signals. Also responsible for the organisation of data types, storage
and transfer. Includes experts in machine learning approaches to transient and pulsar
candidate identification.</li>
<li><strong>Outreach working group:</strong> This is an important aspect of the proposal which
all members will contribute to. It will be led by people with significant experience in
professional and public outreach and educators.</li>
</ul>
</div>
</div>
</div>
</section>
<section id="publication" class="publication-section bgeven">
<div class="container">
<div class="row">
<div class="col-lg-12">
<h1>Publications</h1>
<br>
<h3>1) Wide field beamformed observation with MeerKAT</h3>
<p>(Chen et al. 2021): <a
href="https://ui.adsabs.harvard.edu/abs/2021JAI....1050013C/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2110.01667">ArXiv</a>, <a
href="https://doi.org/10.1142/S2251171721500136">DOI</a> </p>
<p>We describe a wide-field beamformer for the MeerKAT radio telescope and outline strategies to
optimally design pulsar and fast transient surveys.</p>
<br>
<h3>2) Eight new millisecond pulsars from the first MeerKAT globular cluster census</h3>
<p>(Ridolfi et al. 2021): <a
href="https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.1407R/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2103.04800">ArXiv</a>, <a
href="https://doi.org/10.1093/mnras/stab790">DOI</a> </p>
<p>We present the first eight pulsar discoveries made by MeerKAT. The eight pulsars are found in six
different globular clusters and are all millisecond pulsars.</p>
<p><b>Pulsars:</b> J1748-2446an, J1701-3006G, J1803-3002D, J1823-3021G, J0024-7204ac, J0024-7204ad,
J1910-5959F, J1823-3021H </p>
<br>
<h3>3) Two New Black Widow Millisecond Pulsars In M28</h3>
<p>(Douglas et al. 2022): <a
href="https://ui.adsabs.harvard.edu/abs/2022ApJ...927..126D/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2201.11238">ArXiv</a>, <a
href="https://doi.org/10.3847/1538-4357/ac4744">DOI</a> </p>
<p>We report the discovery of two Black Widow millisecond pulsars in the globular cluster M28 with
the MeerKAT telescope.</p>
<p><b>Pulsars:</b> J1824−2452M, J1824−2452N</p>
<br>
<h3>4) TRAPUM discovery of 13 new pulsars in NGC 1851 using MeerKAT</h3>
<p>(Ridolfi et al. 2022): <a
href="https://ui.adsabs.harvard.edu/abs/2022arXiv220312302R/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2203.12302">ArXiv</a>, <a
href="https://doi.org/10.1051/0004-6361/202143006">DOI</a> </p>
<p>We report the discovery of 13 new pulsars in the globular cluster NGC 1851 with the MeerKAT
telescope.</p>
<p><b>Pulsars:</b> J0514-4002B, J0514-4002C, J0514-4002D, J0514-4002E, J0514-4002F, J0514-4002G,
J0514-4002H, J0514-4002I, J0514-4002J, J0514-4002K, J0514-4002L, J0514-4002M, J0514-4002N</p>
<br>
<h3>5) Discoveries and Timing of Pulsars in NGC 6440</h3>
<p>(Vleeschower et al. 2022): <a
href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.tmp..889V/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2204.00086">ArXiv</a>, <a
href="https://doi.org/10.1093/mnras/stac921">DOI</a> </p>
<p>We report the MeerKAT discovery of two pulsars in the globular cluster NGC 6440, as well as
long-term timing solutions of the previously known pulsars NGC 6440C and NGC 6440D from
multi-telescope data.</p>
<p><b>Pulsars:</b> J1748−2021G, J1748−2021H</p>
<br>
<h3>6) Four pulsar discoveries in NGC 6624 by TRAPUM using MeerKAT
</h3>
<p>(Abbate et al. 2022): <a
href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.tmp.1002A/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2204.05334">ArXiv</a>, <a
href="https://doi.org/10.1093/mnras/stac1041">DOI</a> </p>
<p>We report the discovery of four new pulsars in the globular cluster NGC 6624 with the MeerKAT
telescope. One of these (J1823-3022) shows a large offset in its position and dispersion measure
when compared to all the other pulsars in NGC 6624, making its association with the cluster
uncertain.</p>
<p><b>Pulsars:</b> J1823-3021I, J1823-3021J, J1823-3021K, J1823-3022</p>
<br>
<h3>7) Radio Detection of an Elusive Millisecond Pulsar in the Globular Cluster NGC 6397
</h3>
<p>(Zhang et al. 2022): <a
href="https://ui.adsabs.harvard.edu/abs/2022ApJ...934L..21Z/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2207.07880">ArXiv</a>, <a
href="https://doi.org/10.3847/2041-8213/ac81c3">DOI</a> </p>
<p>We report the discovery of a new pulsars (PSR J1740-5340B) in the globular cluster NGC 6397. The
pulsar was found with the Parkes radio telecope and confirmed with the MeerKAT telescope in two
TRAPUM observations. PSR J1740-5340B is an eclipsing redback in a 1.97-day orbit, the longest
among all redbacks known.</p>
<p><b>Pulsars:</b> PSR J1740-5340B</p>
<br>
<h3>8) TRAPUM upper limits on pulsed radio emission for SMC X-ray pulsar J0058−7218
</h3>
<p>(Carli et al. 2022): <a
href="https://ui.adsabs.harvard.edu/abs/2022arXiv221004785C/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2210.04785">ArXiv</a>, <a
href="https://dx.doi.org/10.1093/mnras/stac2883">DOI</a> </p>
<p>As part of our survey of the Small Magellanic Cloud, we have published an upper limit on radio
pulsations from X-ray pulsar J0058−7218. This limit is 7 times deeper than previous radio
searches. This suggests that the radio emission of PSR J0058−7218 is not beamed towards Earth or
that PSR J0058−7218 is similar to a handful of Pulsar Wind Nebulae systems that have a very low
radio efficiency, such as PSR B0540−6919, the Large Magellanic Cloud Crab pulsar analogue.</p>
<p><b>Pulsar:</b> PSR J0058-7218</p>
<br>
<h3>9) The TRAPUM L-band survey for pulsars in Fermi-LAT gamma-ray sources
</h3>
<p>(Clark et al. 2023): <a
href="https://ui.adsabs.harvard.edu/abs/2023MNRAS.519.5590C/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2212.08528">ArXiv</a>, <a
href="https://dx.doi.org/10.1093/mnras/stac3742">DOI</a> </p>
<p>We present the discovery of 9 new millisecond pulsars, the first results from our targeted survey
of unidentified Fermi-LAT gamma-ray sources. All but one of these new pulsars are in binary
systems, of which two are eclipsing redbacks with optical counterparts.</p>
<p><b>Pulsars:</b> J1036-4353, J1526-2744, J1623-6936, J1709-0333, J1757-6032, J1803-6707,
J1823-3543, J1858-5422, J1906-1754 </p>
<br>
<h3>10) Missing for 20 yr: MeerKAT Redetects the Elusive Binary Pulsar M30B
</h3>
<p>(Balakrishnan et al. 2023): <a
href="https://ui.adsabs.harvard.edu/abs/2023ApJ...942L..35B/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2308.16802">ArXiv</a>, <a
href="https://doi.org/10.3847/2041-8213/acae99">DOI</a> </p>
<p>We report the re-discovery of PSR J2140−2311B located in the globular cluster M30 and detected
using the MeerKAT telescope. This pulsar has eluded detections for the past 20 years and its
orbital parameters have been a mystery until now. PSR J2140−2311B has an orbital period of 6.2
days and is in a highly eccentric orbit (e = 0.879) around either a WD/NS. We also measured wdot
from pulsar timing and assuming GR, we present here the total mass of the system. This pulsar is
located 1.2(1)' from the cluster center and likely formed as a result of a secondary exchange
encounter.</p>
<p><b>Pulsars:</b> PSR J2140−2311B</p>
<br>
<h3>11) The MPIfR–MeerKAT Galactic Plane Survey – I. System set-up and early results
</h3>
<p>(Padmanabh et al. 2023): <a
href="https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.1291P/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2303.09231">ArXiv</a>, <a
href="https://doi.org/10.1093/mnras/stad1900">DOI</a> </p>
<p> We present here the overview and setup for the 3000 hour Max-Planck-Institut fuer
Radioastronomie (MPIfR) MeerKAT Galactic Plane survey (MMGPS). The survey is unique by operating
in a commensal mode, addressing key science objectives of the survey including the discovery of
new pulsars and transients as well as studies of Galactic magnetism, the interstellar medium and
star formation rates. We have so far discovered 78 new pulsars including 17 confirmed binary
systems of which two are potential double neutron star systems. We have also developed an
imaging pipeline sensitive to the order of a few tens of micro-Jansky with a spatial resolution
of a few arcseconds. Further science operations with an in-house built S-Band receiver operating
between 1.7-3.5 GHz are about to commence.</p>
<p><b>Pulsars:</b> J0853−4648, J0916−5243, J0917−4413, J0922−4534, J0927−5242, J0933−4604,
J0936−4750, J0948−5549, J0954−5754, J1001−5603, J1015−5359, J1020−5510, J1020−6158, J1030−6008,
J1034−5817, J1034−5934, J1039−6108, J1039−6208, J1051−6214, J1108−6329, J1134−6207, J1138−6154,
J1148−6546, J1155−6529, J1208−5936, J1212−5838, J1231−5929, J1232−5843, J1244−6437, J1306−6043,
J1316−6147, J1328−6605, J1338−6425, J1352−6141, J1353−6341, J1359−6242, J1408−6009, J1409−6011,
J1413−5936, J1426−6136, J1436−6405, J1449−6339, J1452−5549, J1454−5416, J1500−6054, J1510−5254,
J1512−6029, J1520−5402, J1526−5652, J1529−5102, J1529−5609, J1530−5724, J1536−6142, J1536−6149,
J1540−5821, J1543−5439, J1547−5056, J1554−4854, J1554−5906, J1604−4832, J1610−4938, J1614−4608,
J1615−5609, J1623−4608, J1623−4931, J1633−4859, J1636−4217, J1645−4836, J1649−3752, J1649−4230,
J1650−5025, J1652−5154, J1702−4145, J1704−3549, J1706−4020, J1708−4843, J1716−3811, J1806−2125
</p>
<br>
<h3>12) The MPIfR-MeerKAT Galactic Plane Survey - II. The eccentric double neutron star system PSR
J1208−5936 and a neutron star merger rate update
</h3>
<p>(Bernadich et al. 2023): <a
href="https://ui.adsabs.harvard.edu/abs/2023arXiv230816802B/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2308.16802">ArXiv</a>, <a
href="https://doi.org/10.1051/0004-6361/202346953">DOI</a> </p>
<p>We present follow-up study of PSR J1208-5936, a 28.71-ms recycled pulsar in a double neutron star
system with an orbital period of 0.632 days and an orbital eccentricity of 0.348, merging within
the Hubble time. From one year of timing we detected the relativistic advance of periastron of
0.918(1) deg/yr, resulting in a total system mass of 2.586(5) solar masses. Using the
sensitivity of the MMGPS-L survey and the fact of PSR J1208-5936 discovery, we provide updated
estimates of the neutron star merger rate.</p>
<p><b>Pulsars:</b> J1208-5936</p>
<br>
<h3>13) MeerKAT discovery of 13 new pulsars in Omega Centauri
</h3>
<p>(Chen et al. 2023): <a
href="https://ui.adsabs.harvard.edu/abs/2023MNRAS.520.3847C/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2301.03864">ArXiv</a>, <a
href="https://doi.org/10.1093/mnras/stad0293">DOI</a> </p>
<p>We report the discovery of 13 new pulsars in globular cluster Omega Centauri. With this discovery
and the known pulsars, we discuss the ratio between isolated and binaries pulsars and how they
were formed in this cluster.</p>
<p><b>Pulsars:</b> J1326-4728F, J1326-4728G, J1326-4728H, J1326-4728I, J1326-4728J, J1326-4728K,
J1326-4728L, J1326-4728M, J1326-4728N, J1326-4728O, J1326-4728P, J1326-4728Q, J1326-4728R</p>
<br>
<h3>14) PulsarX: a new pulsar searching package -I. A high performance folding program for pulsar
surveys
</h3>
<p>(Men et al. 2023): <a
href="https://ui.adsabs.harvard.edu/abs/2023arXiv230902544M/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2309.02544">ArXiv</a>, <a
href="https://doi.org/10.48550/arXiv.2309.02544">DOI</a> </p>
<p>We describe a novel, efficient approach to candidate folding for large-scale pulsar surveys. The
approach is implemented in the PulsarX software package and is tested on the MMGPS and TRAPUM
surveys where we show that the cost of dedipsersion can be reduced by upto a factor of 50 when
compared to traditional approaches. </p>
<br>
<h3>15) Neutron star mass estimates from gamma-ray eclipses in spider millisecond pulsar binaries
</h3>
<p>(Clark et al. 2023): <a
href="https://ui.adsabs.harvard.edu/abs/2023NatAs...7..451C/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2301.10995">ArXiv</a>, <a
href="https://doi.org/10.1038/s41550-022-01874-x">DOI</a> </p>
<p>We present the detection of eclipses in the gamma-ray pulsations from 7 binary millisecond
pulsars. These eclipses allow us to better constrain the masses of the pulsars in these systems,
by providing us with information on the angles from which we view these binaries. TRAPUM
observations contributed to the timing solution for one of the pulsars included in this search.
</p>
<p><b>Pulsars:</b> J0838−2827, J0955−3949, J2333−5526</p>
<br>
<h3>16) MeerKAT caught a Mini Mouse: serendipitous detection of a young radio pulsar escaping its
birth site
</h3>
<p>(Motta et al. 2023): <a
href="https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.2850M/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2305.06130">ArXiv</a>, <a
href="https://doi.org/10.1093/mnras/stad1438">DOI</a> </p>
<p>We report on the serendipitous discovery of a radio nebula with cometary-like morphology. The
feature, which we named ‘the Mini Mouse’ based on its similarity to the previously
discovered ‘Mouse’ nebula, was observed with MeerKAT and we localisted the known
young pulsar J1914+1054g to the head of the nebula.</p>
<p><b>Pulsars:</b> J1914+1054g</p>
<br>
<h3>17) A MeerKAT view of the pulsars in the globular cluster NGC 6522
</h3>
<p>(Abbate et al. 2023): <a href="https://arxiv.org/abs/2310.03800">ArXiv</a>, <a
href="https://doi.org/10.48550/arXiv.2310.03800">DOI</a> </p>
<p>We present the discovery of two isolated pulsars in the globular cluster NGC 6522. The
discoveries confirm predictions of previous theories for the pulsar populations in late-stage
core-collapsed globular clusters.</p>
<p><b>Pulsars:</b> J1803−3002E, J1803−3002F, J1803−3002C</p>
<br>
<br>
<h3>18) The TRAPUM Small Magellanic Cloud pulsar survey with MeerKAT - I. Discovery of seven new pulsars and two Pulsar Wind Nebula associations
</h3>
<p>(Carli et al. 2024): <a
href="https://ui.adsabs.harvard.edu/abs/2024MNRAS.tmp.1306C/abstract">ADS</a>, <a
href="https://arxiv.org/abs/2405.12029">ArXiv</a>, <a
href="https://doi.org/10.1093/mnras/stae1310">DOI</a> </p>
<p>We report the discovery of seven new SMC pulsars, doubling this galaxy’s radio pulsar population and increasing the total extragalactic
population by nearly a quarter. Our discoveries reveal the first two radio pulsar-PWN systems in the SMC, with only one such system previously
known outside our galaxy.</p>
<p><b>Pulsars:</b> J0040−7326, J0040−7335, J0040−7337, J0043−73, J0044−7314, J0048−7317, J0052−72, J0054−7228, J0105−7208</p>
<br>
</div>
</div>
</div>
</section>
<section id="public-engagement" class="public-engagement-section bgodd">
<div class="container">
<div class="row">
<h1>Public Engagement</h1>
<div class="col-lg-6">
<p>
Our public engagement program is focused on two primary areas: reaching the general public and
engaging with school children, particularly in South Africa and other countries associated with the
SKA project.
</p>
<p>Below are the main components of our public engagement program for TRAPUM:</p>
<ul>
<li>
Produce a monthly newsletter featured in select South African print media and online news
portals. We are also fostering relationships with independent science writers.
</li>
<li>
Conduct hands-on observing and data analysis sessions with schools, tailored to their specific
needs.
</li>
<li>
Collaborate with the IAU’s OAD office and the SKA Communication and Outreach Team to develop
mutually beneficial programs.
</li>
<li>
Establish a TRAPUM citizen science initiative based on the Zooniverse project Pulsar Hunters,
promoting public engagement and enabling scientific contributions.
</li>
<li>
Maintain a well-structured webpage, along with Twitter and Facebook profiles.
</li>
<li>
Develop pulsar-related educational materials suitable for various school environments.
</li>
<li>
Deliver presentations at local schools by TRAPUM members during visits to South Africa.
</li>
<li>
Engage current SKA bursary holders at universities to participate in and contribute to the
program.
</li>
</ul>
</div>
<div class="col-lg-6">
<p>
Introduce young astronomers to the fascinating science behind the TRAPUM project and the power of
the MeerKAT radio telescope with this kid-friendly booklet.
</p>
<a href="images/TRAPUM_for_kids.pdf">
<img src="images/TRAPUM_booklet_front_page.png" alt="TRAPUM Booklet" width="40%">
</a>
<p style="margin-top: 20px;">Stay up-to-date with the latest TRAPUM news on social media:</p>
<a href="https://twitter.com/TRAPUM_News">
<img src="images/x-logo-black.png" alt="Twitter/X Logo" width="50" height="50">
</a>
<a href="https://www.linkedin.com/showcase/trapum">
<img src="images/linkedin-logo-linkedin-icon-transparent-free-png.webp" alt="LinkedIn Logo" width="100" height="100">
</a>
</div>
</div>
</div>
</section>
<section id="data" class="data-section bgeven">
<div class="container">
<div class="row">
<div class="col-lg-12">
<h1>Data Releases</h1>
<p>TRAPUM data are generally large with only specific data sets being retained for future use (e.g.
candidate sets and beams of particular scientific interest, such as those on the cores of
globular clusters). We are
working with SARAO to provide open access to some of these data and will update here when
download links are available. In the meantime available TRAPUM data may be released upon
reasonable request.</p>
<br>
<p></p>
</br>
</div>
</div>
</div>
</section>
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