Wine and Cheese Spring 2024 - Revision history

https://caswiki.johnshopkins.edu/index.php?action=history&feed=atom&title=Wine_and_Cheese_Spring_2024 Wine and Cheese Spring 2024 - Revision history 2026-06-04T21:17:17Z Revision history for this page on the wiki MediaWiki 1.40.0 https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1677&oldid=prev Kdkuntz: /* Won-Ju Kim (Köln) */ 2024-05-03T01:39:58Z

<p><span dir="auto"><span class="autocomment">Won-Ju Kim (Köln)</span></span></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 01:39, 3 May 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l87">Line 87:</td> <td colspan="2" class="diff-lineno">Line 87:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Won-Ju Kim (Köln)==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Won-Ju Kim (Köln)==</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''HyGAL and CASCADE Surveys Characterizing the Galactic Interstellar Medium'''<br></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''HyGAL and CASCADE Surveys Characterizing the Galactic Interstellar Medium'''<br></div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><del style="font-weight: bold; text-decoration: none;"> </del>Understanding the interstellar medium (ISM) is the first step to understanding star formation/evolution and, ultimately, planet formation. The formation of molecular gas occurs in diffuse clouds. These clouds are also closely associated with the progenitors of molecular clouds and clumps, which are the potential birthplace of stars. In addition, the initial chemical inventory of molecular clouds is set by the composition of diffuse clouds. These initial chemical conditions are crucial to explain the observed molecular species toward star-forming molecular clouds and their chemical history. I will present some works from two atomic/molecular line surveys (SOFIA legacy program, HyGAL, and a Max Planck-IRAM observatory program (MIOP), CASCADE) to characterize the properties of Galactic ISM in diffuse and dense molecular clouds. </div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Understanding the interstellar medium (ISM) is the first step to understanding star formation/evolution and, ultimately, planet formation. The formation of molecular gas occurs in diffuse clouds. These clouds are also closely associated with the progenitors of molecular clouds and clumps, which are the potential birthplace of stars. In addition, the initial chemical inventory of molecular clouds is set by the composition of diffuse clouds. These initial chemical conditions are crucial to explain the observed molecular species toward star-forming molecular clouds and their chemical history. I will present some works from two atomic/molecular line surveys (SOFIA legacy program, HyGAL, and a Max Planck-IRAM observatory program (MIOP), CASCADE) to characterize the properties of Galactic ISM in diffuse and dense molecular clouds.</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Peter Quinn (SKA)==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Peter Quinn (SKA)==</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''How to Build an Institute'''<br></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''How to Build an Institute'''<br></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Defining, building and running Institutes, Centres and Organizations for astronomy can be a complex and rewarding business. I will review my experiences and highlight some lessons learned with a particular focus on optical and radio astronomy (including an update on the SKA).</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Defining, building and running Institutes, Centres and Organizations for astronomy can be a complex and rewarding business. I will review my experiences and highlight some lessons learned with a particular focus on optical and radio astronomy (including an update on the SKA).</div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1676&oldid=prev Kdkuntz at 01:39, 3 May 2024 2024-05-03T01:39:28Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 01:39, 3 May 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l86">Line 86:</td> <td colspan="2" class="diff-lineno">Line 86:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>=06 May=</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>=06 May=</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Won-Ju Kim (Köln)==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Won-Ju Kim (Köln)==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>''' '''<br></div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>'''<ins style="font-weight: bold; text-decoration: none;">HyGAL and CASCADE Surveys Characterizing the Galactic Interstellar Medium</ins>'''<br></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"> Understanding the interstellar medium (ISM) is the first step to understanding star formation/evolution and, ultimately, planet formation. The formation of molecular gas occurs in diffuse clouds. These clouds are also closely associated with the progenitors of molecular clouds and clumps, which are the potential birthplace of stars. In addition, the initial chemical inventory of molecular clouds is set by the composition of diffuse clouds. These initial chemical conditions are crucial to explain the observed molecular species toward star-forming molecular clouds and their chemical history. I will present some works from two atomic/molecular line surveys (SOFIA legacy program, HyGAL, and a Max Planck-IRAM observatory program (MIOP), CASCADE) to characterize the properties of Galactic ISM in diffuse and dense molecular clouds. </ins></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Peter Quinn (SKA)==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Peter Quinn (SKA)==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>''' '''<br></div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>'''<ins style="font-weight: bold; text-decoration: none;">How to Build an Institute</ins>'''<br></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Defining, building and running Institutes, Centres and Organizations for astronomy can be a complex and rewarding business. I will review my experiences and highlight some lessons learned with a particular focus on optical and radio astronomy (including an update on the SKA).</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1674&oldid=prev Kdkuntz at 13:50, 26 April 2024 2024-04-26T13:50:26Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 13:50, 26 April 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l83">Line 83:</td> <td colspan="2" class="diff-lineno">Line 83:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Illuminating the Chemistry of Planet Formation: Toward Understanding the Role of Radiation Fields in Shaping Planetary Systems'''<br></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Illuminating the Chemistry of Planet Formation: Toward Understanding the Role of Radiation Fields in Shaping Planetary Systems'''<br></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>A fundamental question in planet-formation is at what point and at what location the compositions of future planets are set. The star plays an important role in shaping the disk chemical environment, through emitting high energy radiation as well as energetic particles. Likewise, the environment - background stars as well as interstellar cosmic rays - can alter the composition of the outer, potentially comet forming radii of the disk. I will present an overview of the on-going work in the group to try and understand the role(s) of each of these forces that "stir the pot" of the chemistry of planet formation, and how we are searching for their influence using observations from ALMA of disks in both low and high mass star forming regions.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>A fundamental question in planet-formation is at what point and at what location the compositions of future planets are set. The star plays an important role in shaping the disk chemical environment, through emitting high energy radiation as well as energetic particles. Likewise, the environment - background stars as well as interstellar cosmic rays - can alter the composition of the outer, potentially comet forming radii of the disk. I will present an overview of the on-going work in the group to try and understand the role(s) of each of these forces that "stir the pot" of the chemistry of planet formation, and how we are searching for their influence using observations from ALMA of disks in both low and high mass star forming regions.</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">=06 May=</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Won-Ju Kim (Köln)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">''' '''<br></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Peter Quinn (SKA)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">''' '''<br></ins></div></td></tr> </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1673&oldid=prev Kdkuntz at 13:49, 26 April 2024 2024-04-26T13:49:15Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 13:49, 26 April 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l74">Line 74:</td> <td colspan="2" class="diff-lineno">Line 74:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Challenging our Understanding of High-Redshift Galaxy Formation with JWST Observations'''<br></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Challenging our Understanding of High-Redshift Galaxy Formation with JWST Observations'''<br></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The insights gained from JWST observations at high-redshift has transformed our understanding of early galaxy formation. For example, various surveys have identified substantially more bright galaxies at z > 9 than predicted from many semi-analytic models and simulations, while galaxies are showing metal abundance ratios that have never been observed in the gas-phase. In this talk, I will discuss the physics that may be driving some of this anomalous behaviour, and highlight the successes and failures of our current models.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The insights gained from JWST observations at high-redshift has transformed our understanding of early galaxy formation. For example, various surveys have identified substantially more bright galaxies at z > 9 than predicted from many semi-analytic models and simulations, while galaxies are showing metal abundance ratios that have never been observed in the gas-phase. In this talk, I will discuss the physics that may be driving some of this anomalous behaviour, and highlight the successes and failures of our current models.</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">=22 April=</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==F. Scott Porter (GSFC)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''XRISM First Results'''<br></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">=29 April=</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Ilse Cleeves (UVa)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''Illuminating the Chemistry of Planet Formation: Toward Understanding the Role of Radiation Fields in Shaping Planetary Systems'''<br></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">A fundamental question in planet-formation is at what point and at what location the compositions of future planets are set. The star plays an important role in shaping the disk chemical environment, through emitting high energy radiation as well as energetic particles. Likewise, the environment - background stars as well as interstellar cosmic rays - can alter the composition of the outer, potentially comet forming radii of the disk. I will present an overview of the on-going work in the group to try and understand the role(s) of each of these forces that "stir the pot" of the chemistry of planet formation, and how we are searching for their influence using observations from ALMA of disks in both low and high mass star forming regions.</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1670&oldid=prev Kdkuntz at 18:40, 28 March 2024 2024-03-28T18:40:43Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 18:40, 28 March 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l69">Line 69:</td> <td colspan="2" class="diff-lineno">Line 69:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Lensing of Gravitational Waves: New Opportunities for Fundamental Physics'''<br></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Lensing of Gravitational Waves: New Opportunities for Fundamental Physics'''<br></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Just like light, gravitational waves (GWs) are deflected and magnified by massive objects in the Universe, a phenomenon known as gravitational lensing. In addition, their low frequency, phase coherence and lack of absorption make GWs complementary to lensed electromagnetic sources. Hence, in addition to well known effects (such as the formation of multiple images), lensed GWs allow for new wave-propagation phenomena like diffraction, the bending of the signal's wavefront. Lensing diffraction causes a frequency-dependent modulation of the signal, which encodes information about lens’ mass and distribution. I will describe the rich phenomenology of lensing diffraction, its observational prospects and its potential to probe the dark matter distribution.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Just like light, gravitational waves (GWs) are deflected and magnified by massive objects in the Universe, a phenomenon known as gravitational lensing. In addition, their low frequency, phase coherence and lack of absorption make GWs complementary to lensed electromagnetic sources. Hence, in addition to well known effects (such as the formation of multiple images), lensed GWs allow for new wave-propagation phenomena like diffraction, the bending of the signal's wavefront. Lensing diffraction causes a frequency-dependent modulation of the signal, which encodes information about lens’ mass and distribution. I will describe the rich phenomenology of lensing diffraction, its observational prospects and its potential to probe the dark matter distribution.</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">=08 April=</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Harley Katz (Chicago)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''Challenging our Understanding of High-Redshift Galaxy Formation with JWST Observations'''<br></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">The insights gained from JWST observations at high-redshift has transformed our understanding of early galaxy formation. For example, various surveys have identified substantially more bright galaxies at z > 9 than predicted from many semi-analytic models and simulations, while galaxies are showing metal abundance ratios that have never been observed in the gas-phase. In this talk, I will discuss the physics that may be driving some of this anomalous behaviour, and highlight the successes and failures of our current models.</ins></div></td></tr> </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1668&oldid=prev Kdkuntz at 14:42, 19 March 2024 2024-03-19T14:42:12Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 14:42, 19 March 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l64">Line 64:</td> <td colspan="2" class="diff-lineno">Line 64:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''The Outflow Method of Measuring Black Hole Spin with an Application to Sagittarius A*'''<br></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''The Outflow Method of Measuring Black Hole Spin with an Application to Sagittarius A*'''<br></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The outflow method of measuring black hole spin will be described and applied to various source samples including supermassive and stellar-mass black holes. Excellent agreement is indicated by the comparison of spin values obtained with independent methods for individual black holes. Spin values allow a determination of the different mass components that comprise the total black hole mass. These components, including the rotational mass-energy, the irreducible mass-energy, and the spin mass-energy available for extraction from the black hole, will be described. The outflow method developed and presented by Daly (2019) to determine black hole spin functions, and the use of the spin function to study the mass components that comprise a black hole developed and presented by Daly (2022), will be applied to Sagittarius A* to determine the spin properties and mass components of this supermassive black hole, as described by Daly et al. (2024).</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The outflow method of measuring black hole spin will be described and applied to various source samples including supermassive and stellar-mass black holes. Excellent agreement is indicated by the comparison of spin values obtained with independent methods for individual black holes. Spin values allow a determination of the different mass components that comprise the total black hole mass. These components, including the rotational mass-energy, the irreducible mass-energy, and the spin mass-energy available for extraction from the black hole, will be described. The outflow method developed and presented by Daly (2019) to determine black hole spin functions, and the use of the spin function to study the mass components that comprise a black hole developed and presented by Daly (2022), will be applied to Sagittarius A* to determine the spin properties and mass components of this supermassive black hole, as described by Daly et al. (2024).</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">=01 April=</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Miguel Zumalacarregui (AEI)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''Lensing of Gravitational Waves: New Opportunities for Fundamental Physics'''<br></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Just like light, gravitational waves (GWs) are deflected and magnified by massive objects in the Universe, a phenomenon known as gravitational lensing. In addition, their low frequency, phase coherence and lack of absorption make GWs complementary to lensed electromagnetic sources. Hence, in addition to well known effects (such as the formation of multiple images), lensed GWs allow for new wave-propagation phenomena like diffraction, the bending of the signal's wavefront. Lensing diffraction causes a frequency-dependent modulation of the signal, which encodes information about lens’ mass and distribution. I will describe the rich phenomenology of lensing diffraction, its observational prospects and its potential to probe the dark matter distribution.</ins></div></td></tr> </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1666&oldid=prev Kdkuntz at 18:29, 18 March 2024 2024-03-18T18:29:42Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 18:29, 18 March 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l59">Line 59:</td> <td colspan="2" class="diff-lineno">Line 59:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Cosmology Constraints from Cluster Abundances with Galaxy Clusters Discovered by the South Pole Telescope'''</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Cosmology Constraints from Cluster Abundances with Galaxy Clusters Discovered by the South Pole Telescope'''</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Over the past decade wide-area high-resolution cosmic microwave background (CMB) surveys conducted by the South Pole Telescope (SPT), Atacama Cosmology Telescope, and Planck have enabled the discovery of thousands of clusters via the Sunyaev-Zel'dovich (SZ) effect. The abundance of such clusters is a powerful cosmological probe as it depends sensitively upon both the expansion history of the universe and the growth of density fluctuations. In this talk I will overview recent progress in the field, particularly highlighting results from the SPT cluster cosmology program. This work, combining SPT-selected clusters with external galaxy lensing data from the Dark Energy Survey and Hubble Space Telescope, has led to tight constraints on LCDM cosmological model parameters. Looking to the future, SZ cluster cosmology will be significantly improved with data from the ongoing SPT-3G and future Simons Observatory and CMB-S4 experiments. These experiments, beyond identifying over an order of magnitude more clusters than previous generation projects, will also provide internal mass calibration for cluster samples via weak lensing of the CMB.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Over the past decade wide-area high-resolution cosmic microwave background (CMB) surveys conducted by the South Pole Telescope (SPT), Atacama Cosmology Telescope, and Planck have enabled the discovery of thousands of clusters via the Sunyaev-Zel'dovich (SZ) effect. The abundance of such clusters is a powerful cosmological probe as it depends sensitively upon both the expansion history of the universe and the growth of density fluctuations. In this talk I will overview recent progress in the field, particularly highlighting results from the SPT cluster cosmology program. This work, combining SPT-selected clusters with external galaxy lensing data from the Dark Energy Survey and Hubble Space Telescope, has led to tight constraints on LCDM cosmological model parameters. Looking to the future, SZ cluster cosmology will be significantly improved with data from the ongoing SPT-3G and future Simons Observatory and CMB-S4 experiments. These experiments, beyond identifying over an order of magnitude more clusters than previous generation projects, will also provide internal mass calibration for cluster samples via weak lensing of the CMB.</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">=25 March=</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Ruth Daly (PSU)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''The Outflow Method of Measuring Black Hole Spin with an Application to Sagittarius A*'''<br></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">The outflow method of measuring black hole spin will be described and applied to various source samples including supermassive and stellar-mass black holes. Excellent agreement is indicated by the comparison of spin values obtained with independent methods for individual black holes. Spin values allow a determination of the different mass components that comprise the total black hole mass. These components, including the rotational mass-energy, the irreducible mass-energy, and the spin mass-energy available for extraction from the black hole, will be described. The outflow method developed and presented by Daly (2019) to determine black hole spin functions, and the use of the spin function to study the mass components that comprise a black hole developed and presented by Daly (2022), will be applied to Sagittarius A* to determine the spin properties and mass components of this supermassive black hole, as described by Daly et al. (2024).</ins></div></td></tr> </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1663&oldid=prev Kdkuntz at 15:45, 8 March 2024 2024-03-08T15:45:48Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 15:45, 8 March 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l54">Line 54:</td> <td colspan="2" class="diff-lineno">Line 54:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Tracing Feedback from X-ray Binaries Across Cosmic Time'''<br></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''Tracing Feedback from X-ray Binaries Across Cosmic Time'''<br></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Feedback from X-ray binaries is a key ingredient in regulating how reionization proceeded in the early Universe. I will provide an overview of the importance of feedback from X-ray binaries in star-forming environments, and summarize our current understanding of this component of feedback based on resolved population studies in nearby galaxies, recent measurements of the cosmic 21-cm signal, and binary population synthesis models. Finally, I will present prospects for future X-ray missions to directly trace the evolution of X-ray binary emission across key cosmic epochs, and discuss the importance of X-ray binaries to the ionizing photon budget in star-forming galaxies.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Feedback from X-ray binaries is a key ingredient in regulating how reionization proceeded in the early Universe. I will provide an overview of the importance of feedback from X-ray binaries in star-forming environments, and summarize our current understanding of this component of feedback based on resolved population studies in nearby galaxies, recent measurements of the cosmic 21-cm signal, and binary population synthesis models. Finally, I will present prospects for future X-ray missions to directly trace the evolution of X-ray binary emission across key cosmic epochs, and discuss the importance of X-ray binaries to the ionizing photon budget in star-forming galaxies.</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">=11 March=</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Lindsey Bleem (Argonne)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''Cosmology Constraints from Cluster Abundances with Galaxy Clusters Discovered by the South Pole Telescope'''</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Over the past decade wide-area high-resolution cosmic microwave background (CMB) surveys conducted by the South Pole Telescope (SPT), Atacama Cosmology Telescope, and Planck have enabled the discovery of thousands of clusters via the Sunyaev-Zel'dovich (SZ) effect. The abundance of such clusters is a powerful cosmological probe as it depends sensitively upon both the expansion history of the universe and the growth of density fluctuations. In this talk I will overview recent progress in the field, particularly highlighting results from the SPT cluster cosmology program. This work, combining SPT-selected clusters with external galaxy lensing data from the Dark Energy Survey and Hubble Space Telescope, has led to tight constraints on LCDM cosmological model parameters. Looking to the future, SZ cluster cosmology will be significantly improved with data from the ongoing SPT-3G and future Simons Observatory and CMB-S4 experiments. These experiments, beyond identifying over an order of magnitude more clusters than previous generation projects, will also provide internal mass calibration for cluster samples via weak lensing of the CMB.</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1662&oldid=prev Kdkuntz at 15:12, 1 March 2024 2024-03-01T15:12:08Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 15:12, 1 March 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l45">Line 45:</td> <td colspan="2" class="diff-lineno">Line 45:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>SPHEREx, an upcoming NASA medium-class Explorer Mission, will perform the first all-sky near infrared spectral survey. With a targeted launch date in early 2025, SPHEREx will map the entire sky at 6.2 arcsec from 0.75 to 5μm with a spectral resolution R>35 and 5σ sensitivity AB>19 over the nominal two-year mission. We will use this data set to 1) study the cosmic inflation by mapping the large-scale distribution of galaxies; 2) measure the light produced by stars and galaxies over cosmic history; and 3) determine the abundance of interstellar water and organic ices available to proto-planetary systems.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>SPHEREx, an upcoming NASA medium-class Explorer Mission, will perform the first all-sky near infrared spectral survey. With a targeted launch date in early 2025, SPHEREx will map the entire sky at 6.2 arcsec from 0.75 to 5μm with a spectral resolution R>35 and 5σ sensitivity AB>19 over the nominal two-year mission. We will use this data set to 1) study the cosmic inflation by mapping the large-scale distribution of galaxies; 2) measure the light produced by stars and galaxies over cosmic history; and 3) determine the abundance of interstellar water and organic ices available to proto-planetary systems.</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>In this talk, I will give a summary of the SPHEREx instrument design, survey plan and the expected data product, and highlight the potential science cases that can be done with this full-sky legacy archive available to the community.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>In this talk, I will give a summary of the SPHEREx instrument design, survey plan and the expected data product, and highlight the potential science cases that can be done with this full-sky legacy archive available to the community.</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">=4 March=</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Grecco Oyarzun Martinez (JHU)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''The HI Gas Reservoirs of Galaxies at z~2'''<br></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Neutral hydrogen gas (HI) is fundamental for galaxy formation. The accretion of HI gas from the intergalactic medium fuels star-formation, while the removal of HI gas explains why some galaxies quench. In this talk, I will focus on how we study the HI gas reservoirs around galaxies at z~2. First, I will discuss the major difficulty in carrying out these studies at this redshift: the faintness of HI gas in emission. Because of this limitation, to probe HI gas at z~2 we must instead turn to absorption signatures (DLAs) in the spectra of background quasars. Then, I will present a search for the galaxies associated with 14 DLAs at z~2 in Lyman-alpha emission. We detect a total of 6 Ly-alpha emitters, all of which are associated with intermediate metallicity DLAs (-1.5 < [M/H] < -0.3). This result hints that moderately enriched HI gas is typically associated with Lyman-alpha emitting, low stellar mass galaxies. Metal-rich DLAs, on the other hand, often feature massive galaxies that are bright in the sub-millimeter. This correspondence between the properties of galaxies and DLAs suggests that galaxies and HI gas reservoirs are already intertwined at z~2.</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==Kristen Garofoli (JHU/GSFC)==</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''Tracing Feedback from X-ray Binaries Across Cosmic Time'''<br></ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Feedback from X-ray binaries is a key ingredient in regulating how reionization proceeded in the early Universe. I will provide an overview of the importance of feedback from X-ray binaries in star-forming environments, and summarize our current understanding of this component of feedback based on resolved population studies in nearby galaxies, recent measurements of the cosmic 21-cm signal, and binary population synthesis models. Finally, I will present prospects for future X-ray missions to directly trace the evolution of X-ray binary emission across key cosmic epochs, and discuss the importance of X-ray binaries to the ionizing photon budget in star-forming galaxies.</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2024&diff=1657&oldid=prev Kdkuntz: /* 19 February */ 2024-02-16T16:07:23Z

<p><span dir="auto"><span class="autocomment">19 February</span></span></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 16:07, 16 February 2024</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l32">Line 32:</td> <td colspan="2" class="diff-lineno">Line 32:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>=19 February=</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>=19 February=</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>==<del style="font-weight: bold; text-decoration: none;">TBD </del>(<del style="font-weight: bold; text-decoration: none;">TBD</del>)==</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>==<ins style="font-weight: bold; text-decoration: none;">Kristen Garofoli </ins>(<ins style="font-weight: bold; text-decoration: none;">JHU/GSFC</ins>)==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>'''<del style="font-weight: bold; text-decoration: none;">TBD</del>'''<br></div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>'''<ins style="font-weight: bold; text-decoration: none;">Tracing Feedback from X-ray Binaries Across Cosmic Time</ins>'''<br></div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><del style="font-weight: bold; text-decoration: none;">Abstract</del></div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Feedback from X-ray binaries is a key ingredient in regulating how reionization proceeded in the early Universe. I will provide an overview of the importance of feedback from X-ray binaries in star-forming environments, and summarize our current understanding of this component of feedback based on resolved population studies in nearby galaxies, recent measurements of the cosmic 21-cm signal, and binary population synthesis models. Finally, I will present prospects for future X-ray missions to directly trace the evolution of X-ray binary emission across key cosmic epochs, and discuss the importance of X-ray binaries to the ionizing photon budget in star-forming galaxies.</ins></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>==<del style="font-weight: bold; text-decoration: none;">TBD </del>(<del style="font-weight: bold; text-decoration: none;">TBD</del>)==</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>==<ins style="font-weight: bold; text-decoration: none;">Pallavi Patil </ins>(<ins style="font-weight: bold; text-decoration: none;">JHU</ins>)==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>'''<del style="font-weight: bold; text-decoration: none;">TBD</del>'''<br></div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>'''<ins style="font-weight: bold; text-decoration: none;">WISE-NVSS Selected Heavily Obscured, Jetted Quasars: Probing the Peak of Black Hole Growth at Cosmic Noon</ins>'''<br></div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><del style="font-weight: bold; text-decoration: none;">Abstract</del></div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Active Galactic Nuclei (AGN) feedback at z ~ 1-3 is believed to occur in the presence of thick columns of gas and dust, leading to heavily obscured systems that are challenging to detect at optical/X-rays but are transparent at radio and MIR wavelengths. By combining MIR and radio diagnostics, we have identified a sample of 155 ultra-luminous and obscured quasars (0.4 < z < 3) selected to have extremely red MIR colors in WISE and compact, bright radio emission in the NVSS/FIRST. In this talk, I will provide updates on our ongoing multiwavelength efforts to understand the nature of this unique sample in the context of jet-ISM feedback. High-resolution studies with VLA and VLBA confirm that most of the sample is compact with angular scales <0.2” (1.7 kpc at z~2). A radio spectral analysis reveals many sources show peaked/curved spectra consistent with being young radio AGN. A snapshot imaging survey with the VLBA at 5 GHz of 90 sample sources reveals a range of small jet structures and also unresolved sources. I will also discuss our follow-up study that includes deep multi-frequency VLA imaging and 870μm ALMA continuum and line (CO and HCN) observations, LBT imaging and spectroscopy, and NuSTAR data revealing a Compton-thick AGN. Overall, our sample is consistent with a population of recently triggered, young radio jets caught in a unique evolutionary stage in which they reside in a dense ISM. Finally, I discuss the implications of our study for understanding the impact of young jets on the ISM and star formation rates in powerful young AGNs.</ins></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>=26 February=</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>=26 February=</div></td></tr>  </table>

Kdkuntz