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<!DOCTYPE HTML>
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<title>New LA: Alexander S. Binks</title>
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<h1><a href="index.html">Alexander S. Binks</a></h1>
<p>Astronomer, Stargazer and consumer of music</p>
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<li><a href="www.astro.keele.ac.uk">Keele Astrophysics</a></li>
<li><a href="www.nasa.gov">NASA</a></li>
<li><a href="#">GAIA</a></li>
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<div class="title">A new Local Association?</div>
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<p>In a series of publications in the 1960s, Olin Eggen hypothesised the existence of a "Local Association" of co-moving, young early-type
stars in the solar vicinity, consisting of objects in the Pleiades, α Persei and IC 2602 open clusters. In the 1990s follow-up spectroscopic
observations of many X-ray active solar-type and low-mass stars were able to identify hundreds of counterparts to the Local Association,
leading to the discovery to dozens of kinematically-coherent, but spatially-dispersed, approximately coeval moving groups throughout the
2000s.</p>
<p>Many subsequent searches for nearby, young stars have attempted to expand the number of objects belonging to the various groups that
constitute the Local Association by identifying stars that are potentially co-moving, and confirming their youth and kinematics with follow-up
spectroscopy. Whilst thousands of new, young nearby stars have been identified through this techique, there is a significant drawback in the
sense that the search mechanisms are "kinematically biased" and cannot uncover new kinematic grouping outside the velocity domain encapsulated
by the Local Association.</p>
<p>In order to search for entirely new kinematic groupings of young stars I developed a novel technique to identify young stars across the
entire sky by selecting X-ray active stars from the ROSAT all-sky survey that also have short rotation periods as measured in the SuperWASP
all-sky survey. I was then able to win telescope time to spectroscopically observe hundreds of these potentially young stars, and used the
presence of lithium to confirm the youth status (< 100 Myr) for several dozens of young stars, which revealed a curious kinematic sub-grouping
of 7 stars in a unique part of the Galactic velocity space diagram, approximately near to the Octans moving group, but 10s of km/s from the
"classic" Local Association.</p>
<p>This prompted me to investigate this region of velocity space further and we acquired more spectroscopic observing time focused on
identifying stars from the all-sky survey that are most likely to be co-moving with this potentially new kinematic ensemble. Our findings
doubled the number of young stars in this kinematic subgrouping, which I labelled as the Pisces moving group (since the majority of these
stars are in the direction of the Pisces constellation).</p>
<p>It is possible that these young kinematically-coherent stars in a unique section of the velocity space diagram may be the tip-of-the-iceberg
of a much larger kinematic entity, akin to a new Local Association consisting of objects in Octans and Pisces and other yet to be identified
groups. I am currently working alongside Simon Murphy (Australian National University) to spectroscopically observe more objects from this
list on the ANU 2.3m telescope. Our catalogue of almost 500 stars represents a large dedicated campaign to search for young stars near the
Sun and work is ongoing to investigate the nature of this potential new Local Association.</p>
<div class="col-6 col-12-medium">
<section class="highlight">
<img src="images/New_LA.png" alt="" style="width:800px;height:800px;"/>
<h3>Galactic space velocities for dozens of spectroscopically-confirmed young, nearby stars from my kinematically unbiased target catalogue.
There are two distinct kinematic entities: the first is the classic Local Association, the second, with a similar "U" velocity, but much slower
"V" velocity may be representative of a new Local Association</h3>
</section>
</div>
</div>
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<div class="title">Research Highlights</div>
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<img src="images/lightcurve_example.png" alt="" style="width:500px;height:400px;"/>
<h3>Testing how well evolutionary models simultaneous fit both the
CMD and Li-depletion </h3>
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<li><a href="CMD_Li.html" class="button style1">Learn More</a></li>
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<img src="images/uvw.png" alt="" style="width:500px;height:400px;"/>
<h3>Half the young G/K stars within 100 pc are not kinematically
linked with any known moving groups</h3>
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<li><a href="kinematics.html" class="button style1">Learn More</a></li>
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<section class="highlight">
<img src="images/New_LA.png" alt="" style="width:500px;height:400px;"/>
<h3>Is there another kinematic "local association" of
young, nearby stars?</h3>
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<li><a href="New_LA.html" class="button style1">Learn More</a></li>
</ul>
</section>
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<img src="images/SEDs.png" alt="" style="width:500px;height:400px;"/>
<h3>What fraction of low-mass M-stars in young moving groups
have debris disks?</h3>
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<img src="images/Xray_VKs.png" alt="" style="width:500px;height:400px;"/>
<h3>Searching for new, nearby young stars in the Northern Hemisphere:
About 1/3 of fast rotating stars are genuinely young based on Li content.</h3>
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<li><a href="kinunbiased.html" class="button style1">Learn More</a></li>
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<img src="images/LDB_BPMG.png" alt="" style="width:500px;height:400px;"/>
<h3>A Lithium Depletion Boundary age of 24+/-4 Myr for the Beta
Pictoris Moving Group: twice the age estimate from isochronal fitting.</h3>
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<li><a href="LDB.html" class="button style1">Learn More</a></li>
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<input type="text" name="name" id="contact-name" placeholder="Name" />
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<h3 class="icon solid fa-home">Office Address</h3>
<p>
School of Chemical and Physical Sciences<br />
Lennard-Jones Building<br />
Keele University<br />
Staffordshire<bf />
ST5 5BG, UK
</p>
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<a href="http://orcid.org/0000-0001-5976-4644"
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<img src="images/orcid_logo.png"
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style="width:30px;height:30px;"/>
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style="width:30px;height:30px;"/>
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<p>
<a href="#">alex.s.binks@gmail.com</a>
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+44 (0)1782-732000
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