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    <title>Jeff Carlin on Jeff Carlin</title>
    <link>http://jeffcarlin.github.io/</link>
    <description>Recent content in Jeff Carlin on Jeff Carlin</description>
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    <copyright>&amp;copy; 2018</copyright>
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    <item>
      <title>Tidal destruction in a low mass galaxy environment: the discovery of tidal tails around DDO 44</title>
      <link>http://jeffcarlin.github.io/publication/ddo44_stream/</link>
      <pubDate>Wed, 06 Nov 2019 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/ddo44_stream/</guid>
      <description></description>
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      <title>What do we learn by studying the outer Milky Way halo?</title>
      <link>http://jeffcarlin.github.io/post/dist_rrl_science/</link>
      <pubDate>Wed, 14 Nov 2018 12:34:07 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/post/dist_rrl_science/</guid>
      <description>

&lt;p&gt;&lt;em&gt;In &lt;a href=&#34;http://jeffcarlin.github.io/post/dist_rrl/&#34; target=&#34;_blank&#34;&gt;my previous post&lt;/a&gt; I discussed our project to find some of the most distant stars in the outskirts of our Milky Way galaxy. (The illustration above shows the fields on the sky that we have observed so far as part of our survey.) In this post, I&amp;rsquo;ll explain more about &lt;em&gt;why&lt;/em&gt; we want to find these distant Milky Way halo stars.&lt;/em&gt;&lt;/p&gt;

&lt;h3 id=&#34;mass-of-the-milky-way&#34;&gt;Mass of the Milky Way&lt;/h3&gt;

&lt;p&gt;&lt;em&gt;We don&amp;rsquo;t even know the mass of our Galaxy better than about a factor of two.&lt;/em&gt; That&amp;rsquo;s like if someone asked me how much I weigh, and I said &amp;ldquo;Oh, somewhere between 125 and 250 pounds.&amp;rdquo; (That&amp;rsquo;s about 57-113 kilograms, for those of you not used to pounds, or about 9-18 stone, if you prefer.) That&amp;rsquo;s a true statement, but not very informative. We live inside the Milky Way, so it&amp;rsquo;s hard to get an idea of the entire Galaxy from our perspective. It&amp;rsquo;s like if you were in downtown Chicago, and you and your friends went to the observation deck of your favorite skyscraper. Do you think that by looking out over the city, you could guess how big it is and how many people live there? Sure, you could each come up with a reasonable guess, but maybe at best within a factor of two (for example, ranging between about 4.5 million to 18 million, or a factor of 2 in either direction from the Chicago metro area&amp;rsquo;s population of roughly 9 million). Seems like a pretty uncertain guess, right? Well, that&amp;rsquo;s how well we know the total mass of our Milky Way galaxy.&lt;/p&gt;

&lt;figure&gt;

&lt;img src=&#34;http://jeffcarlin.github.io/img/eadie_juric2018_MW_mass_profile.png&#34; alt=&#34;Various estimates of the mass of the Milky Way. A given study can only estimate the mass that is contained within the distance of the tracers used, so the plot above shows the mass within each radius in the Milky Way. The vertical axis is mass in units of $10^\{12}$ (trillions!) of _Solar masses_ (the mass of the Sun, a typical star). You can see that at $R =100$ kpc (_kiloparsecs_, where 100 kpc is a distance of about 325,000 light years), the estimates for our Galaxy&amp;#39;s mass range from less than half a trillion Solar masses to as much as 1.5 trillion. This highlights just how difficult it is to measure our Galaxy&amp;#39;s mass. (Image from [this recent paper by Eadie &amp;amp; Jurić (2018)](https://arxiv.org/abs/1810.10036); their best estimates for the mass are shown as shaded gray regions.)&#34; width=&#34;80%&#34; /&gt;



&lt;figcaption data-pre=&#34;Figure &#34; data-post=&#34;:&#34; &gt;
  &lt;p&gt;
    Various estimates of the mass of the Milky Way. A given study can only estimate the mass that is contained within the distance of the tracers used, so the plot above shows the mass within each radius in the Milky Way. The vertical axis is mass in units of $10^{12}$ (trillions!) of &lt;em&gt;Solar masses&lt;/em&gt; (the mass of the Sun, a typical star). You can see that at $R =100$ kpc (&lt;em&gt;kiloparsecs&lt;/em&gt;, where 100 kpc is a distance of about 325,000 light years), the estimates for our Galaxy&amp;rsquo;s mass range from less than half a trillion Solar masses to as much as 1.5 trillion. This highlights just how difficult it is to measure our Galaxy&amp;rsquo;s mass. (Image from &lt;a href=&#34;https://arxiv.org/abs/1810.10036&#34; target=&#34;_blank&#34;&gt;this recent paper by Eadie &amp;amp; Jurić (2018)&lt;/a&gt;; their best estimates for the mass are shown as shaded gray regions.)
    
    
    
  &lt;/p&gt; 
&lt;/figcaption&gt;

&lt;/figure&gt;

&lt;p&gt;Fine, but why does it matter whether we know our Galaxy&amp;rsquo;s mass or not? First off, &lt;em&gt;because we live inside of it, the Milky Way is the best-studied galaxy in the Universe.&lt;/em&gt; Because of this, we use it as a benchmark to understand other galaxies and the results of computer simulations of galaxy formation and evolution. To know which simulated galaxies to compare to, we need to know how much &amp;ldquo;stuff&amp;rdquo; (gas, stars, and dark matter &amp;ndash; more on that soon) our Galaxy contains.&lt;/p&gt;

&lt;p&gt;At least half the mass of the Milky Way is in the form of &lt;em&gt;dark matter&lt;/em&gt;. What is dark matter? Well, we don&amp;rsquo;t know for sure, but we &lt;em&gt;do&lt;/em&gt; know that it&amp;rsquo;s there. It was first definitively shown to exist in the mid-1970s by &lt;a href=&#34;https://en.wikipedia.org/wiki/Vera_Rubin&#34; target=&#34;_blank&#34;&gt;Vera Rubin&lt;/a&gt;, who measured the speed at which stars in the outer parts of nearby galaxies are rotating. The orbit of an object is determined by the amount of mass contained inside its orbit (for example, the Earth&amp;rsquo;s orbit is mostly due to the Sun&amp;rsquo;s gravitational influence, since the Sun makes up most of the mass in the Solar system). But when Rubin compared the rotation speeds she was measuring to what was expected due to the mass we can see (gas, dust, and stars) in the galaxies she studied, she found that all of the galaxies were rotating faster than the visible matter could account for. This means that to account for the galaxies&amp;rsquo; faster rotation, there must be some other mass present that we can&amp;rsquo;t directly see &amp;ndash; this unseen mass is what we call &amp;ldquo;dark matter.&amp;rdquo; It turns out that &lt;em&gt;dark matter makes up the majority of the mass in many (or perhaps most) galaxies&lt;/em&gt;. There is a lot of other evidence for the existence of dark matter, and a lot of ongoing study to determine what it is made up of.&lt;/p&gt;

&lt;p&gt;The reason dark matter is relevant to the discussion at hand is because it makes up most of our Galaxy&amp;rsquo;s mass in the outer regions. Only 1% of the Milky Way&amp;rsquo;s stars are in the halo, with most of them concentrated in the pancake-like disk of our Galaxy. Thus one of the ways to understand our Galaxy&amp;rsquo;s size, mass, and shape is to use the few stars that &lt;em&gt;are&lt;/em&gt; present to study its outer parts.&lt;/p&gt;

&lt;figure&gt;

&lt;img src=&#34;http://jeffcarlin.github.io/img/mwdwarfs_map.jpg&#34; width=&#34;80%&#34; /&gt;


&lt;/figure&gt;

&lt;h3 id=&#34;remnants-of-destroyed-dwarf-galaxies&#34;&gt;Remnants of destroyed dwarf galaxies&lt;/h3&gt;

&lt;p&gt;When large galaxies like the Milky Way form, there are also smaller &amp;ldquo;dwarf galaxies&amp;rdquo; that form with them, and continue to orbit around their larger host galaxy. The image above shows an illustration of the dwarf companions of the Milky Way that were known as of about 10 years ago. We have since found many more. Dwarf galaxies are of particular interest because they have few stars, with the vast majority of their mass made up by dark matter. The number and properties of dwarf galaxies that form around each larger galaxy help us to decide between models of galaxy formation, and in particular between predictions of the properties of dark matter that makes up most of the mass. However, the dwarf galaxies that we see today don&amp;rsquo;t represent &lt;em&gt;all&lt;/em&gt; of the dwarfs that the Milky Way has hosted. When these tiny galaxies approach the inner parts of their host galaxy, the stronger gravitational forces they encounter pull them apart. This is illustrated in the video shown below (from Kathryn Johnston and James Bullock), which is a computer simulation of what happens to dwarf galaxies (the colored points) as they orbit in a Milky Way-like galaxy&amp;rsquo;s dark matter halo. You can see that many of them are shredded apart, and their stars become part of an overall &amp;ldquo;halo&amp;rdquo; of stars.&lt;/p&gt;






  

&lt;video autoplay loop &gt;
  &lt;source src=&#34;http://jeffcarlin.github.io/img/timesequence1e2.mp4&#34; type=&#34;video/mp4&#34;&gt;
&lt;/video&gt;

&lt;h3 id=&#34;shape-density-profile-of-the-halo&#34;&gt;Shape, density profile of the halo&lt;/h3&gt;

&lt;p&gt;In fact, it is thought that most of the stars in the Milky Way halo came from destroyed dwarf galaxies, and that the outermost portions of the halo are entirely made up of recently ingested dwarf galaxies. This means that by mapping the outer halo, we can infer something about the history of our galaxy. The number and properties of dwarf galaxies that have been swallowed can affect the shape of the halo (for example, if all the dwarf galaxies were concentrated to one side, the halo may look oblong). Also, the number of stars seen in the outer regions may tell us how many dwarfs fell in, and how large they were. In this way we can piece together how many dwarf galaxies were originally hosted by the Milky Way.&lt;/p&gt;

&lt;h3 id=&#34;tracers-of-mass&#34;&gt;Tracers of mass&lt;/h3&gt;

&lt;p&gt;Finally, as mentioned when we discussed dark matter, the motions of stars are determined by the amount of mass inside their orbit. So if we are able to measure the orbits of stars (or even of dwarf galaxies) in the Milky Way, we can use them as &amp;ldquo;tracers&amp;rdquo; to tell us how much mass is contained inside their location in our Galaxy. In the outermost Milky Way, there are very few stars, so in order to really pin down the total mass within, say, 600,000 light years, we need to find as many possible tracers as we can. This is our goal with the RR Lyrae stars &amp;ndash; we want to find them, then measure their motions through space, so that we can use them to determine the mass of our Galaxy. Right now, the only means we have of tracing the Galaxy&amp;rsquo;s mass in the outer parts is dwarf galaxies and star clusters, of which there are very few. &lt;em&gt;This is why we need lots of RR Lyrae stars &amp;ndash; we don&amp;rsquo;t have many tracers in the outer regions, and they&amp;rsquo;re not spread out over the sky.&lt;/em&gt; As mentioned in my previous post, we&amp;rsquo;ll eventually find a lot of these variable stars in the outer Milky Way via LSST, but that&amp;rsquo;s no reason not to look for them now! With a group of collaborators, I am doing just that &amp;ndash; the map at the top of this post shows the regions of sky we have searched thus far. It&amp;rsquo;s painstaking work, but slowly we&amp;rsquo;re building up a sample of RR Lyrae variables in the outer Galaxy with which we can probe the mass and history of the build-up of our Galaxy.&lt;/p&gt;
</description>
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    <item>
      <title>Studying the outer Milky Way halo with distant RR Lyrae variable stars</title>
      <link>http://jeffcarlin.github.io/post/dist_rrl/</link>
      <pubDate>Sat, 13 Oct 2018 12:34:07 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/post/dist_rrl/</guid>
      <description>

&lt;p&gt;&lt;em&gt;Hi, folks! In this, the first blog post on my site, I&amp;rsquo;ll explain a bit about one of my research projects that I&amp;rsquo;m especially excited about lately. I&amp;rsquo;ll aim to keep it at a level that is understandable for &amp;ldquo;non-experts,&amp;rdquo; but inevitably there will be some astro jargon that creeps in&amp;hellip; -Jeff&lt;/em&gt;&lt;/p&gt;

&lt;p&gt;The sparsely-populated outermost regions of our Milky Way galaxy are poorly studied. In part, this is because stars of a given type become fainter the more distant they are from us &amp;ndash; think about a flashlight: if I stand a few feet away from you, it will look pretty bright (you could read a book by its light), while if I&amp;rsquo;m a block away, it will just look like a small point of light. This is due to what&amp;rsquo;s often called the &amp;ldquo;inverse square law,&amp;rdquo; which says that light from a given source diminishes in intensity proportional to the &lt;em&gt;square&lt;/em&gt; of the distance from the viewer (10 times further away means $10^2$, or 100 times, fainter). This means that the old stars in the most distant parts of the Milky Way&amp;rsquo;s &amp;ldquo;halo&amp;rdquo; are quite faint. Furthermore, it&amp;rsquo;s difficult to estimate the distances to typical stars. So, to study the distant reaches of our Galaxy&amp;rsquo;s stellar halo, we need stars that:&lt;/p&gt;

&lt;ol&gt;
&lt;li&gt;are intrinsically bright (so we can still detect them even at large distances),&lt;/li&gt;
&lt;li&gt;are fairly common in old, metal-poor populations such as the Milky Way halo,&lt;/li&gt;
&lt;li&gt;are easy to pick out from among the other, more numerous, types of stars between us and the outer Galaxy, and&lt;/li&gt;
&lt;li&gt;whose distances can be easily estimated.&lt;/li&gt;
&lt;/ol&gt;

&lt;figure&gt;

&lt;img src=&#34;http://jeffcarlin.github.io/img/mw_halo.jpg&#34; alt=&#34;The halo of the Milky Way is the diffuse outer region surrounding the disk, where we live along with most of the gas, dust, and stars in the Galaxy. Although it contains only about 1% of the stars in our Galaxy, the halo gives us vital clues about how the Milky Way has grown and evolved. (Image from [Hubblesite](http://hubblesite.org/image/3051).)&#34; width=&#34;60%&#34; /&gt;



&lt;figcaption data-pre=&#34;Figure &#34; data-post=&#34;:&#34; &gt;
  &lt;p&gt;
    The halo of the Milky Way is the diffuse outer region surrounding the disk, where we live along with most of the gas, dust, and stars in the Galaxy. Although it contains only about 1% of the stars in our Galaxy, the halo gives us vital clues about how the Milky Way has grown and evolved. (Image from &lt;a href=&#34;http://hubblesite.org/image/3051&#34; target=&#34;_blank&#34;&gt;Hubblesite&lt;/a&gt;.)
    
    
    
  &lt;/p&gt; 
&lt;/figcaption&gt;

&lt;/figure&gt;

&lt;h2 id=&#34;rr-lyrae-pulsating-variable-stars&#34;&gt;RR Lyrae &amp;ndash; pulsating variable Stars&lt;/h2&gt;

&lt;p&gt;For an ongoing project I&amp;rsquo;m working on, the solution we have adopted is to use RR Lyrae stars. These are a type of variable stars named after the first one to be discovered &amp;ndash; the star RR Lyrae. RR Lyrae stars are a type of star whose brightness varies because the &lt;em&gt;entire star&lt;/em&gt; is pulsating (growing larger, then shrinking, then growing larger again&amp;hellip;). As the star expands and contracts, its brightness changes in a characteristic way, which can be seen in repeated observations of the star (some examples are seen in the header image above, on the right side). (For history of RR Lyrae, including details of their discovery by &lt;a href=&#34;https://en.wikipedia.org/wiki/Williamina_Fleming&#34; target=&#34;_blank&#34;&gt;Williamina Fleming&lt;/a&gt;, see &lt;a href=&#34;https://www.aavso.org/vsots_rrlyr&#34; target=&#34;_blank&#34;&gt;this intro at the AAVSO site&lt;/a&gt;.) It turns out that the period of this pulsation (the time it takes to complete one &amp;ldquo;cycle&amp;rdquo; of expansion/contraction) is related to the intrinsic brightness of the star, so once you know the period, you can compare its average measured brightness with the derived intrinsic brightness and determine how far away the RR Lyrae star is.&lt;/p&gt;

&lt;figure&gt;

&lt;img src=&#34;http://jeffcarlin.github.io/img/M3_color3.gif&#34; alt=&#34;Image of the outer regions of the globular cluster M3. This shows an animation of 4 images of the same field taken over the course of the same night. You can see that most of the stars remain the same as it blinks between the 4 images, but some stars change their brightness with time. Most of these are RR Lyrae variables, which can fairly easily be selected by observing the same field of view multiple times. (Image from [this page](https://www.astro.princeton.edu/~jhartman/M3_movies.html).)&#34; width=&#34;60%&#34; /&gt;



&lt;figcaption data-pre=&#34;Figure &#34; data-post=&#34;:&#34; &gt;
  &lt;p&gt;
    Image of the outer regions of the globular cluster M3. This shows an animation of 4 images of the same field taken over the course of the same night. You can see that most of the stars remain the same as it blinks between the 4 images, but some stars change their brightness with time. Most of these are RR Lyrae variables, which can fairly easily be selected by observing the same field of view multiple times. (Image from &lt;a href=&#34;https://www.astro.princeton.edu/~jhartman/M3_movies.html&#34; target=&#34;_blank&#34;&gt;this page&lt;/a&gt;.)
    
    
    
  &lt;/p&gt; 
&lt;/figcaption&gt;

&lt;/figure&gt;

&lt;p&gt;You can see from the figure above that criterion #3 (&amp;ldquo;are easy to pick out from among the other, more numerous, types of stars&amp;rdquo;) is easily satisfied by revisiting the same field repeatedly and determining which stars change in brightness within a few hours. As we mentioned above, the distances to RR Lyrae stars are easily determined once you establish the period of pulsation (#4 above). RR Lyrae stars are indeed fairly bright, and only occur when stars roughly the mass of the Sun (but with much lower abundances of metals) are in the late stages of their lives. Thus they satisfy all of the criteria we laid out above for ideal tracers of the Milky Way halo.&lt;/p&gt;

&lt;p&gt;Now, RR Lyrae stars are well-studied, and are used frequently to map the inner parts of the Milky Way&amp;rsquo;s halo. However, it has only been recently that it has become feasible to observe these pulsating variables in the outermost halo. This is because it requires a large enough telescope to quickly gather enough light from faint, distant stars, that also has a camera with a large enough field of view that we can map large areas of sky in a reasonable time frame. One example is the &lt;a href=&#34;https://www.darkenergysurvey.org/the-des-project/instrument/&#34; target=&#34;_blank&#34;&gt;Dark Energy Camera (DECam)&lt;/a&gt; (built for the &lt;a href=&#34;https://www.darkenergysurvey.org/&#34; target=&#34;_blank&#34;&gt;Dark Energy Survey&lt;/a&gt;) on the &lt;a href=&#34;http://www.ctio.noao.edu/noao/content/Victor-Blanco-4-m-Telescope&#34; target=&#34;_blank&#34;&gt;4-meter Blanco telescope at CTIO&lt;/a&gt;, which we are using for a survey of the outer halo of the Galaxy.&lt;/p&gt;

&lt;figure&gt;

&lt;img src=&#34;http://jeffcarlin.github.io/img/rrlyrae_head2.png&#34; alt=&#34;Figures from a paper by Medina et al. (2017) showing first results from our survey. At the right, we show &amp;#34;light curves&amp;#34; (brightness vs. time within the pulsational period, or &amp;#34;phase&amp;#34;) of the most distant RR Lyrae from our survey, with template RR Lyrae curves overlaid. The lower left figure shows regions on the sky that we have observed thus far, and the upper left illustrates the distances ($d_{H}$) as a function of position in a small wedge of sky. &#34; width=&#34;80%&#34; /&gt;



&lt;figcaption data-pre=&#34;Figure &#34; data-post=&#34;:&#34; &gt;
  &lt;p&gt;
    Figures from a paper by Medina et al. (2017) showing first results from our survey. At the right, we show &amp;ldquo;light curves&amp;rdquo; (brightness vs. time within the pulsational period, or &amp;ldquo;phase&amp;rdquo;) of the most distant RR Lyrae from our survey, with template RR Lyrae curves overlaid. The lower left figure shows regions on the sky that we have observed thus far, and the upper left illustrates the distances ($d_{H}$) as a function of position in a small wedge of sky.
    
    
    
  &lt;/p&gt; 
&lt;/figcaption&gt;

&lt;/figure&gt;

&lt;p&gt;The figure above shows results from &lt;a href=&#34;http://jeffcarlin.github.io/publication/medina_distant_rrl/&#34; target=&#34;_blank&#34;&gt;our first publication&lt;/a&gt; about this project. In that paper, we presented a total of 173 RR Lyrae stars in about 120 square degrees of sky, in 40 DECam fields that were observed 20 times each. About &lt;sup&gt;1&lt;/sup&gt;&amp;frasl;&lt;sub&gt;3&lt;/sub&gt; of these are in the Sextans dwarf spheroidal galaxy, which happens to be within the field of view, another 2 are in the Leo IV dwarf galaxy, and 3 more are newly-discovered variables in the Leo V dwarf galaxy (&lt;a href=&#34;http://jeffcarlin.github.io/publication/medina_leov/&#34; target=&#34;_blank&#34;&gt;see this Medina et al. 2017a paper&lt;/a&gt;). Of the remaining RR Lyrae, we found 18 that are beyond 90 kiloparsecs (abbreviated &lt;em&gt;kpc&lt;/em&gt;; 90 kpc is about 290,000 light years), including the most distant RR Lyrae yet known around the Milky Way at beyond 200 kpc (650,000 light years; we think the &amp;ldquo;edge&amp;rdquo; of our Galaxy should be around 250-300 kpc &amp;ndash; but that&amp;rsquo;s one of the things we&amp;rsquo;re hoping to find out with this study!). We have now obtained DECam observations of 3 times as many fields, and analysis is ongoing. We hope to expand the sample of RR Lyrae stars at the outer limits of the Milky Way to more than 50 (in about 1% of the sky), so that we can begin to infer global properties of the stellar halo of our Galaxy.&lt;/p&gt;

&lt;p&gt;This is precursor science in anticipation of (and to develop tools for) the upcoming &lt;a href=&#34;https://www.lsst.org/&#34; target=&#34;_blank&#34;&gt;Large Synoptic Survey Telescope (LSST)&lt;/a&gt;. LSST will consist of an 8.4-meter optical telescope (currently under construction in Chile), a 3.5-degree diameter field of view, and a 3.2 &lt;em&gt;billion&lt;/em&gt; pixel (that&amp;rsquo;s &lt;em&gt;giga-pixel&lt;/em&gt;) camera. The planned survey (starting in 2023) will observe roughly half the night sky repeatedly for 10 years, ultimately imaging each patch of sky hundreds of times with each of 6 filters. This deep survey will revolutionize our understanding of time-varying astronomical phenomena (including variable stars, but also supernovae, active galactic nuclei, and many other objects). In fact, LSST will find RR Lyrae to distances more than 3 times further than we are reaching in our current DECam survey, over more than 50 times the sky area. Stay tuned!&lt;/p&gt;

&lt;p&gt;&lt;strong&gt;In &lt;a href=&#34;http://jeffcarlin.github.io/post/dist_rrl_science/&#34; target=&#34;_blank&#34;&gt;my next post&lt;/a&gt;&lt;/strong&gt; I&amp;rsquo;ll explain more about &lt;em&gt;why&lt;/em&gt; we want to find these distant Milky Way halo stars.&lt;/p&gt;
</description>
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      <title>ΛCDM predictions for the satellite population of M33</title>
      <link>http://jeffcarlin.github.io/publication/patel_m33/</link>
      <pubDate>Mon, 01 Oct 2018 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/patel_m33/</guid>
      <description></description>
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      <title>Boötes III is a Disrupting Dwarf Galaxy Associated with the Styx Stellar Stream</title>
      <link>http://jeffcarlin.github.io/publication/booiii/</link>
      <pubDate>Sat, 01 Sep 2018 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/booiii/</guid>
      <description></description>
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      <title>A Deeper Look at the New Milky Way Satellites: Sagittarius II, Reticulum II, Phoenix II, and Tucana III</title>
      <link>http://jeffcarlin.github.io/publication/burcin_ufds/</link>
      <pubDate>Wed, 01 Aug 2018 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/burcin_ufds/</guid>
      <description></description>
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      <title>3D Asymmetrical motions of the Galactic outer disc with LAMOST K giant stars</title>
      <link>http://jeffcarlin.github.io/publication/haifeng_asymm_motions/</link>
      <pubDate>Sun, 01 Jul 2018 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/haifeng_asymm_motions/</guid>
      <description></description>
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      <title>Chemical Abundances of Hydrostatic and Explosive Alpha-elements in Sagittarius Stream Stars</title>
      <link>http://jeffcarlin.github.io/publication/sgr_hex/</link>
      <pubDate>Tue, 01 May 2018 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/sgr_hex/</guid>
      <description></description>
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      <title>Discovery of Distant RR Lyrae Stars in the Milky Way Using DECam</title>
      <link>http://jeffcarlin.github.io/publication/medina_distant_rrl/</link>
      <pubDate>Thu, 01 Mar 2018 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/medina_distant_rrl/</guid>
      <description></description>
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    <item>
      <title>Mapping the Milky Way with LAMOST - II. The stellar halo</title>
      <link>http://jeffcarlin.github.io/publication/xuyan_lamost_halo/</link>
      <pubDate>Mon, 01 Jan 2018 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/xuyan_lamost_halo/</guid>
      <description></description>
    </item>
    
    <item>
      <title>Deep Subaru Hyper Suprime-Cam Observations of Milky Way Satellites Columba I and Triangulum II</title>
      <link>http://jeffcarlin.github.io/publication/coli_triii/</link>
      <pubDate>Fri, 01 Dec 2017 00:00:00 -0700</pubDate>
      
      <guid>http://jeffcarlin.github.io/publication/coli_triii/</guid>
      <description></description>
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    <item>
      <title>A Map of the Local Velocity Substructure in the Milky Way Disk</title>
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      <pubDate>Wed, 01 Nov 2017 00:00:00 -0700</pubDate>
      
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      <description></description>
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      <pubDate>Tue, 01 Aug 2017 00:00:00 -0700</pubDate>
      
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      <description></description>
    </item>
    
    <item>
      <title>Red Runaways II: Low-mass Hills Stars in SDSS Stripe 82</title>
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      <pubDate>Tue, 01 Nov 2016 00:00:00 -0700</pubDate>
      
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