Wine and Cheese Spring 2021 - Revision history

https://caswiki.johnshopkins.edu/index.php?action=history&feed=atom&title=Wine_and_Cheese_Spring_2021 Wine and Cheese Spring 2021 - Revision history 2026-06-04T21:27:07Z Revision history for this page on the wiki MediaWiki 1.40.0 https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1410&oldid=prev Kdkuntz: /* Roberto Cotesta (JHU) */ 2021-04-22T19:44:10Z

<p><span dir="auto"><span class="autocomment">Roberto Cotesta (JHU)</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 19:44, 22 April 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l76">Line 76:</td> <td colspan="2" class="diff-lineno">Line 76:</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>==Roberto Cotesta (JHU)==</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>==Roberto Cotesta (JHU)==</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>'''Enriching the Symphony of Gravitational Waves from Binary Black Holes by Tuning Higher Harmonics'''<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>'''Enriching the Symphony of Gravitational Waves from Binary Black Holes by Tuning Higher Harmonics'''<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>Accurate models of gravitational waveforms are necessary to take full advantage of the increase in sensitivity of current and future gravitational wave detectors. In this talk, I will show the impact of more accurate waveform models for binary black holes</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>Accurate models of gravitational waveforms are necessary to take full advantage of the increase in sensitivity of current and future gravitational wave detectors. In this talk, I will show the impact of more accurate waveform models for binary black holes (BBH), which include the effect of spin-precession and higher harmonics, on the precision and accuracy of the inferred parameters of these sources. I will first focus on the role of these waveform models in the source characterisation of the stellar-mass BBHs detected during the third LIGO and Virgo observing run (O3). I will then explain how the same waveform models can be used for the parameter estimation of massive BBH observable with the space-based interferometer LISA, and describe their impact on the characterisation</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>(BBH), which include the effect of spin-precession and higher harmonics, on the precision and accuracy of the inferred parameters of these sources. I will first focus on the role of these waveform models in the source characterisation of the stellar-mass BBHs</div></td><td colspan="2" class="diff-side-added"></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>detected during the third LIGO and Virgo observing run (O3). I will then explain how the same waveform models can be used for the parameter estimation of massive BBH observable with the space-based interferometer LISA, and describe their impact on the characterisation</div></td><td colspan="2" class="diff-side-added"></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> of these sources.</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> of these sources.</div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1409&oldid=prev Kdkuntz at 19:43, 22 April 2021 2021-04-22T19:43:14Z

<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 19:43, 22 April 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l72">Line 72:</td> <td colspan="2" class="diff-lineno">Line 72:</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>'''Galaxy Formation in Lyman-alpha or: How I Learned to Stop Worrying and Love Scattered Light'''<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>'''Galaxy Formation in Lyman-alpha or: How I Learned to Stop Worrying and Love Scattered Light'''<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>Lyman-alpha emission is produced ubiquitously by excited hydrogen, so it is a powerful tracer of the interactions among gas, stars, and AGN that shape galaxy formation. However, the resonant scattering of this emission line makes its interpretation complex. In this talk, I will describe three spectroscopic surveys of >1000 galaxies at z~2-3 that make use of Lyman-alpha emission: the Keck Baryonic Structure Survey (KBSS), the KBSS-Lya, and the Keck Lyman Continuum Survey (KCLS). By understanding when and where Lya escapes galaxies, we can characterize galaxy feedback, supermassive black hole growth, and the nature of cosmic reionization. In each of these efforts, the scattered nature of Lyman-alpha emission can be a tool as well as a challenge.</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>Lyman-alpha emission is produced ubiquitously by excited hydrogen, so it is a powerful tracer of the interactions among gas, stars, and AGN that shape galaxy formation. However, the resonant scattering of this emission line makes its interpretation complex. In this talk, I will describe three spectroscopic surveys of >1000 galaxies at z~2-3 that make use of Lyman-alpha emission: the Keck Baryonic Structure Survey (KBSS), the KBSS-Lya, and the Keck Lyman Continuum Survey (KCLS). By understanding when and where Lya escapes galaxies, we can characterize galaxy feedback, supermassive black hole growth, and the nature of cosmic reionization. In each of these efforts, the scattered nature of Lyman-alpha emission can be a tool as well as a challenge.</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;">=26 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;">==Roberto Cotesta (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;">'''Enriching the Symphony of Gravitational Waves from Binary Black Holes by Tuning Higher Harmonics'''<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;">Accurate models of gravitational waveforms are necessary to take full advantage of the increase in sensitivity of current and future gravitational wave detectors. In this talk, I will show the impact of more accurate waveform models for binary black holes</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;"> (BBH), which include the effect of spin-precession and higher harmonics, on the precision and accuracy of the inferred parameters of these sources. I will first focus on the role of these waveform models in the source characterisation of the stellar-mass BBHs</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;"> detected during the third LIGO and Virgo observing run (O3). I will then explain how the same waveform models can be used for the parameter estimation of massive BBH observable with the space-based interferometer LISA, and describe their impact on the characterisation</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;"> of these sources.</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1406&oldid=prev Kdkuntz at 17:10, 6 April 2021 2021-04-06T17:10:10Z

<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 17:10, 6 April 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l67">Line 67:</td> <td colspan="2" class="diff-lineno">Line 67:</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 Southern Stellar Stream Spectroscopic Survey (S5)'''<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 Southern Stellar Stream Spectroscopic Survey (S5)'''<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>Over a dozen new stellar streams in the halo of the Milky Way have been discovered in the southern hemisphere with the Dark Energy Survey (DES) in recent years, with other datasets yielding additional stellar substructure. To study these we have embarked on an ongoing spectroscopic program, S5, which has been mapping these southern streams with 2df+AAOmega on the AAT. An international collaboration, S5 is the first systematic program pursuing a complete census of known streams in the southern hemisphere. The radial velocities and stellar metallicities from S5 - together with proper motions from Gaia - provide us with a unique dataset for understanding the stellar populations of the Milky Way's halo, the progenitors and formation processes of the streams, the mass and overall morphology of the Milky Way's gravitational potential, and ultimately potential clues to the nature of dark matter. I will give an overview of the S5 program, including target selection, observation, and data analysis, present early science results from S5 data and follow-up observations, and discuss some of the implications of these results for the study of Milky Way streams and satellites in the context of current and future major astronomical surveys.</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 a dozen new stellar streams in the halo of the Milky Way have been discovered in the southern hemisphere with the Dark Energy Survey (DES) in recent years, with other datasets yielding additional stellar substructure. To study these we have embarked on an ongoing spectroscopic program, S5, which has been mapping these southern streams with 2df+AAOmega on the AAT. An international collaboration, S5 is the first systematic program pursuing a complete census of known streams in the southern hemisphere. The radial velocities and stellar metallicities from S5 - together with proper motions from Gaia - provide us with a unique dataset for understanding the stellar populations of the Milky Way's halo, the progenitors and formation processes of the streams, the mass and overall morphology of the Milky Way's gravitational potential, and ultimately potential clues to the nature of dark matter. I will give an overview of the S5 program, including target selection, observation, and data analysis, present early science results from S5 data and follow-up observations, and discuss some of the implications of these results for the study of Milky Way streams and satellites in the context of current and future major astronomical surveys.</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;">=12 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;">==Ryan Trainor (F&M)==</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;">'''Galaxy Formation in Lyman-alpha or: How I Learned to Stop Worrying and Love Scattered Light'''<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;">Lyman-alpha emission is produced ubiquitously by excited hydrogen, so it is a powerful tracer of the interactions among gas, stars, and AGN that shape galaxy formation. However, the resonant scattering of this emission line makes its interpretation complex. In this talk, I will describe three spectroscopic surveys of >1000 galaxies at z~2-3 that make use of Lyman-alpha emission: the Keck Baryonic Structure Survey (KBSS), the KBSS-Lya, and the Keck Lyman Continuum Survey (KCLS). By understanding when and where Lya escapes galaxies, we can characterize galaxy feedback, supermassive black hole growth, and the nature of cosmic reionization. In each of these efforts, the scattered nature of Lyman-alpha emission can be a tool as well as a challenge.</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1404&oldid=prev Kdkuntz at 00:16, 2 April 2021 2021-04-02T00:16:39Z

<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 00:16, 2 April 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l62">Line 62:</td> <td colspan="2" class="diff-lineno">Line 62:</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>In this live interactive demo session, learn how to access images, spectra, and catalog data from SDSS (including MaNGA/Marvin) and HEASARC, along with catalog parameters and flat files from the Indra and Millennium Simulations. To save time during the demo, please register for a SciServer account beforehand. You will learn about the 20+ sample Jupyter notebooks that you can adapt for your own research and teaching.</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 live interactive demo session, learn how to access images, spectra, and catalog data from SDSS (including MaNGA/Marvin) and HEASARC, along with catalog parameters and flat files from the Indra and Millennium Simulations. To save time during the demo, please register for a SciServer account beforehand. You will learn about the 20+ sample Jupyter notebooks that you can adapt for your own research and teaching.</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;">=05 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;">==Daniel Zucker (Macquarie)==</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 Southern Stellar Stream Spectroscopic Survey (S5)'''<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;">Over a dozen new stellar streams in the halo of the Milky Way have been discovered in the southern hemisphere with the Dark Energy Survey (DES) in recent years, with other datasets yielding additional stellar substructure. To study these we have embarked on an ongoing spectroscopic program, S5, which has been mapping these southern streams with 2df+AAOmega on the AAT. An international collaboration, S5 is the first systematic program pursuing a complete census of known streams in the southern hemisphere. The radial velocities and stellar metallicities from S5 - together with proper motions from Gaia - provide us with a unique dataset for understanding the stellar populations of the Milky Way's halo, the progenitors and formation processes of the streams, the mass and overall morphology of the Milky Way's gravitational potential, and ultimately potential clues to the nature of dark matter. I will give an overview of the S5 program, including target selection, observation, and data analysis, present early science results from S5 data and follow-up observations, and discuss some of the implications of these results for the study of Milky Way streams and satellites in the context of current and future major astronomical surveys.</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1401&oldid=prev Kdkuntz: /* 29 March */ 2021-03-25T19:09:28Z

<p><span dir="auto"><span class="autocomment">29 March</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 19:09, 25 March 2021</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>==Ani Thakar & Jordan Raddick (JHU)==</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>==Ani Thakar & Jordan Raddick (JHU)==</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>'''SciServer - a Science Platform for SDSS and Beyond'''<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>'''SciServer - a Science Platform for SDSS and Beyond'''<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>SciServer (www.sciserver.org) is an online science platform developed by IDIES (idies.jhu.edu) that offers instant browser-based access to Petabytes of scientific data in astronomy and other sciences<del style="font-weight: bold; text-decoration: none;">, including </del>the Sloan Digital Sky Survey (SDSS) datasets. SciServer is the official science platform for the SDSS catalog data, and will continue to host the data for the SDSS V mappers as well. <del style="font-weight: bold; text-decoration: none;"> </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> </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>When you sign up for a free SciServer account, you gain access to our virtual computing resources, including 10 GB of personal storage space and nearly unlimited shared space for temporary data products. In addition to the <del style="font-weight: bold; text-decoration: none;">classic </del>SDSS science portals, SkyServer and CasJobs, SciServer provides many new server-side science capabilities. You can analyze, visualize, and publish all available datasets along with your own<del style="font-weight: bold; text-decoration: none;">. </del>using Python or R scripts in Jupyter notebooks. There is a new spectrum analysis tool that can be used in standalone mode or within a Jupyter notebook. With easy data and resource sharing features and no required setup, SciServer makes an excellent resource for collaborative research and for teaching undergraduate courses. <del style="font-weight: bold; text-decoration: none;"> </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>SciServer (www.sciserver.org) is an online science platform developed by IDIES (idies.jhu.edu) that offers instant browser-based access to Petabytes of scientific data in astronomy and other sciences<ins style="font-weight: bold; text-decoration: none;">. This includes </ins>the Sloan Digital Sky Survey (SDSS) datasets. <ins style="font-weight: bold; text-decoration: none;">In fact </ins>SciServer is the official science platform for the SDSS catalog data, and will continue to host the data for the SDSS<ins style="font-weight: bold; text-decoration: none;">-</ins>V mappers as well. <ins style="font-weight: bold; text-decoration: none;"> </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>In this live interactive demo session, learn how to access images, spectra, and catalog data from SDSS and HEASARC, along with catalog parameters and flat files from the Indra and Millennium Simulations. <del style="font-weight: bold; text-decoration: none;">Bring your laptop</del>, <del style="font-weight: bold; text-decoration: none;">you will leave with </del>a <del style="font-weight: bold; text-decoration: none;">free </del>SciServer account <del style="font-weight: bold; text-decoration: none;">and access to more than </del>20 <del style="font-weight: bold; text-decoration: none;">example </del>notebooks that you can adapt for your own research and teaching.</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> </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>When you sign up for a free SciServer account, you gain access to our virtual computing resources, including 10 GB of personal<ins style="font-weight: bold; text-decoration: none;">, backed-up </ins>storage space and nearly unlimited shared space for temporary data products. In addition to the <ins style="font-weight: bold; text-decoration: none;">stalwart </ins>SDSS science portals, SkyServer and CasJobs, SciServer provides many new server-side science capabilities. You can analyze, visualize, and publish all available datasets along with your own<ins style="font-weight: bold; text-decoration: none;">, </ins>using Python or R scripts in Jupyter notebooks. There is a new spectrum analysis tool that can be used in standalone mode or within a Jupyter notebook. <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> </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>With easy data and resource sharing features and no required setup, SciServer makes an excellent resource for collaborative research and for teaching undergraduate courses.</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> </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>In this live interactive demo session, learn how to access images, spectra, and catalog data from SDSS <ins style="font-weight: bold; text-decoration: none;">(including MaNGA/Marvin) </ins>and HEASARC, along with catalog parameters and flat files from the Indra and Millennium Simulations. <ins style="font-weight: bold; text-decoration: none;">To save time during the demo</ins>, <ins style="font-weight: bold; text-decoration: none;">please register for </ins>a SciServer account <ins style="font-weight: bold; text-decoration: none;">beforehand. You will learn about the </ins>20<ins style="font-weight: bold; text-decoration: none;">+ sample Jupyter </ins>notebooks that you can adapt for your own research and teaching.</div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1400&oldid=prev Kdkuntz: /* 29 March */ 2021-03-17T14:49:06Z

<p><span dir="auto"><span class="autocomment">29 March</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 14:49, 17 March 2021</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>==Ani Thakar & Jordan Raddick (JHU)==</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>==Ani Thakar & Jordan Raddick (JHU)==</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>'''SciServer - a Science Platform for SDSS and Beyond'''<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>'''SciServer - a Science Platform for SDSS and Beyond'''<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>SciServer (www.sciserver.org) is an online science platform developed by IDIES (idies.jhu.edu) that offers instant browser-based access to Petabytes of scientific data in astronomy and other sciences, including the Sloan Digital Sky Survey (SDSS) datasets. SciServer is the official science platform for the SDSS catalog data, and will continue to host the data for the SDSS V mappers as well. </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>SciServer (www.sciserver.org) is an online science platform developed by IDIES (idies.jhu.edu) that offers instant browser-based access to Petabytes of scientific data in astronomy and other sciences, including the Sloan Digital Sky Survey (SDSS) datasets. SciServer is the official science platform for the SDSS catalog data, and will continue to host the data for the SDSS V mappers as well. </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>When you sign up for a free SciServer account, you gain access to our virtual computing resources, including 10 GB of personal storage space and nearly unlimited shared space for temporary data products. In addition to the classic SDSS science portals, SkyServer and CasJobs, SciServer provides many new server-side science capabilities. You can analyze, visualize, and publish all available datasets along with your own. using Python or R scripts in Jupyter notebooks. There is a new spectrum analysis tool that can be used in standalone mode or within a Jupyter notebook. With easy data and resource sharing features and no required setup, SciServer makes an excellent resource for collaborative research and for teaching undergraduate courses. </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>When you sign up for a free SciServer account, you gain access to our virtual computing resources, including 10 GB of personal storage space and nearly unlimited shared space for temporary data products. In addition to the classic SDSS science portals, SkyServer and CasJobs, SciServer provides many new server-side science capabilities. You can analyze, visualize, and publish all available datasets along with your own. using Python or R scripts in Jupyter notebooks. There is a new spectrum analysis tool that can be used in standalone mode or within a Jupyter notebook. With easy data and resource sharing features and no required setup, SciServer makes an excellent resource for collaborative research and for teaching undergraduate courses. </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 live interactive demo session, learn how to access images, spectra, and catalog data from SDSS and HEASARC, along with catalog parameters and flat files from the Indra and Millennium Simulations. Bring your laptop, you will leave with a free SciServer account and access to more than 20 example notebooks that you can adapt for your own research and teaching.</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 live interactive demo session, learn how to access images, spectra, and catalog data from SDSS and HEASARC, along with catalog parameters and flat files from the Indra and Millennium Simulations. Bring your laptop, you will leave with a free SciServer account and access to more than 20 example notebooks that you can adapt for your own research and teaching.</div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1399&oldid=prev Kdkuntz at 14:48, 17 March 2021 2021-03-17T14:48:40Z

<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 14:48, 17 March 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l50">Line 50:</td> <td colspan="2" class="diff-lineno">Line 50:</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 Future of Massively Multiplexed Spectroscopy: the Maunakea Spectroscopic Explorer'''<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 Future of Massively Multiplexed Spectroscopy: the Maunakea Spectroscopic Explorer'''<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 Maunakea Spectroscopic Explorer (MSE) is a planned next generation massively multiplexed spectroscopic facility that is completely dedicated to optical and near-Infrared spectroscopy of samples of thousands to millions of astrophysical objects at resolutions from R~3,000 to R~40,000. With science goals spanning all of astronomy, from detailed chemical abundance studies of nearby stars to investigating the cosmology of the early Universe, MSE will provide key next-generation science capabilities that will revolutionize the field. In this talk I will review the current status of the project and provide an overview of MSE's wide range of scientific capabilities.</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 Maunakea Spectroscopic Explorer (MSE) is a planned next generation massively multiplexed spectroscopic facility that is completely dedicated to optical and near-Infrared spectroscopy of samples of thousands to millions of astrophysical objects at resolutions from R~3,000 to R~40,000. With science goals spanning all of astronomy, from detailed chemical abundance studies of nearby stars to investigating the cosmology of the early Universe, MSE will provide key next-generation science capabilities that will revolutionize the field. In this talk I will review the current status of the project and provide an overview of MSE's wide range of scientific capabilities.</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 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;">==Ani Thakar & Jordan Raddick (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;">'''SciServer - a Science Platform for SDSS and Beyond'''<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;"> SciServer (www.sciserver.org) is an online science platform developed by IDIES (idies.jhu.edu) that offers instant browser-based access to Petabytes of scientific data in astronomy and other sciences, including the Sloan Digital Sky Survey (SDSS) datasets. SciServer is the official science platform for the SDSS catalog data, and will continue to host the data for the SDSS V mappers as well. </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;">When you sign up for a free SciServer account, you gain access to our virtual computing resources, including 10 GB of personal storage space and nearly unlimited shared space for temporary data products. In addition to the classic SDSS science portals, SkyServer and CasJobs, SciServer provides many new server-side science capabilities. You can analyze, visualize, and publish all available datasets along with your own. using Python or R scripts in Jupyter notebooks. There is a new spectrum analysis tool that can be used in standalone mode or within a Jupyter notebook. With easy data and resource sharing features and no required setup, SciServer makes an excellent resource for collaborative research and for teaching undergraduate courses. </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;">In this live interactive demo session, learn how to access images, spectra, and catalog data from SDSS and HEASARC, along with catalog parameters and flat files from the Indra and Millennium Simulations. Bring your laptop, you will leave with a free SciServer account and access to more than 20 example notebooks that you can adapt for your own research and teaching.</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1395&oldid=prev Kdkuntz at 16:24, 26 February 2021 2021-02-26T16:24:14Z

<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 16:24, 26 February 2021</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>'''Using High-Cadence Synthetic Observations to Unlock a New Era in Astrophysics'''<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>'''Using High-Cadence Synthetic Observations to Unlock a New Era in Astrophysics'''<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>As astronomers near the commissioning of the extremely large telescopes, the Rubin Observatory, as well as new space-based observatories like the Roman Space Telescope and JWST to peer more deeply into our Universe, our community is challenged to develop a theoretical and modeling framework to characterize and study what will be humanity's greatest astronomical discoveries. My research addresses this need by generating detailed, state-of-the-art synthetic observations from hydrodynamic cosmological simulations. By calculating all the processes that photons undergo as they travel across the Universe from the surface of a distant star to a telescope’s detector, my collaborators and I have been able to disentangle perplexing trends in observed galactic spectra as well as make predictions for what we might unveil in the near future. Topics we have investigated in prior work include massive black hole formation, the first stars and galaxies, and the intricate interplay between nebular emission lines and the escape fraction of ionizing radiation. Looking forward, I propose to create the largest and most detailed database of synthetic observational tools and predictions at a time that will come to define astronomy for generations.</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>As astronomers near the commissioning of the extremely large telescopes, the Rubin Observatory, as well as new space-based observatories like the Roman Space Telescope and JWST to peer more deeply into our Universe, our community is challenged to develop a theoretical and modeling framework to characterize and study what will be humanity's greatest astronomical discoveries. My research addresses this need by generating detailed, state-of-the-art synthetic observations from hydrodynamic cosmological simulations. By calculating all the processes that photons undergo as they travel across the Universe from the surface of a distant star to a telescope’s detector, my collaborators and I have been able to disentangle perplexing trends in observed galactic spectra as well as make predictions for what we might unveil in the near future. Topics we have investigated in prior work include massive black hole formation, the first stars and galaxies, and the intricate interplay between nebular emission lines and the escape fraction of ionizing radiation. Looking forward, I propose to create the largest and most detailed database of synthetic observational tools and predictions at a time that will come to define astronomy for generations.</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;">=8 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;">==Jennifer Marshall (Texas A&M)==</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 Future of Massively Multiplexed Spectroscopy: the Maunakea Spectroscopic Explorer'''<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 Maunakea Spectroscopic Explorer (MSE) is a planned next generation massively multiplexed spectroscopic facility that is completely dedicated to optical and near-Infrared spectroscopy of samples of thousands to millions of astrophysical objects at resolutions from R~3,000 to R~40,000. With science goals spanning all of astronomy, from detailed chemical abundance studies of nearby stars to investigating the cosmology of the early Universe, MSE will provide key next-generation science capabilities that will revolutionize the field. In this talk I will review the current status of the project and provide an overview of MSE's wide range of scientific capabilities.</ins></div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1386&oldid=prev Kdkuntz: /* 22 February */ 2021-02-18T18:16:14Z

<p><span dir="auto"><span class="autocomment">22 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 18:16, 18 February 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l41">Line 41:</td> <td colspan="2" class="diff-lineno">Line 41:</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>Multiple-planet systems composed of close-in super-Earth/sub-Neptune-sized planets are ubiquitous, representing the dominant outcome of planet formation. This population exhibits predictable hallmarks of architectural regularity and uniformity, such as low eccentricities and inclinations, similar orbital spacings, and intra-system correlations in planetary masses and radii. On top of this first-order structure, however, these systems also exhibit surprising anomalies that require explanation. Examples include (1) ultra-short period planets, whose extremely-irradiated orbits have been separated off from the rest of their systems; (2) planets piled up wide of mean-motion resonances; and (3) a subset of Neptune-sized planets that show signs of radius inflation. In this talk, I will propose that tidal dynamics can account for these specific anomalies and more. Specifically, I will discuss the critical role of enhanced tidal dissipation due to non-zero planetary axial tilts (obliquities), which arise by way of prevalent dynamical resonances. I will highlight strategies for testing these tidal theories and observing obliquities directly in the future.</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>Multiple-planet systems composed of close-in super-Earth/sub-Neptune-sized planets are ubiquitous, representing the dominant outcome of planet formation. This population exhibits predictable hallmarks of architectural regularity and uniformity, such as low eccentricities and inclinations, similar orbital spacings, and intra-system correlations in planetary masses and radii. On top of this first-order structure, however, these systems also exhibit surprising anomalies that require explanation. Examples include (1) ultra-short period planets, whose extremely-irradiated orbits have been separated off from the rest of their systems; (2) planets piled up wide of mean-motion resonances; and (3) a subset of Neptune-sized planets that show signs of radius inflation. In this talk, I will propose that tidal dynamics can account for these specific anomalies and more. Specifically, I will discuss the critical role of enhanced tidal dissipation due to non-zero planetary axial tilts (obliquities), which arise by way of prevalent dynamical resonances. I will highlight strategies for testing these tidal theories and observing obliquities directly in the future.</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;">+</del>1 March=</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;">=</ins>1 March=</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>==Kirk Barrow (KIPAC)==</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>==Kirk Barrow (KIPAC)==</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>'''Using High-Cadence Synthetic Observations to Unlock a New Era in Astrophysics'''<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>'''Using High-Cadence Synthetic Observations to Unlock a New Era in Astrophysics'''<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>As astronomers near the commissioning of the extremely large telescopes, the Rubin Observatory, as well as new space-based observatories like the Roman Space Telescope and JWST to peer more deeply into our Universe, our community is challenged to develop a theoretical and modeling framework to characterize and study what will be humanity's greatest astronomical discoveries. My research addresses this need by generating detailed, state-of-the-art synthetic observations from hydrodynamic cosmological simulations. By calculating all the processes that photons undergo as they travel across the Universe from the surface of a distant star to a telescope’s detector, my collaborators and I have been able to disentangle perplexing trends in observed galactic spectra as well as make predictions for what we might unveil in the near future. Topics we have investigated in prior work include massive black hole formation, the first stars and galaxies, and the intricate interplay between nebular emission lines and the escape fraction of ionizing radiation. Looking forward, I propose to create the largest and most detailed database of synthetic observational tools and predictions at a time that will come to define astronomy for generations.</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>As astronomers near the commissioning of the extremely large telescopes, the Rubin Observatory, as well as new space-based observatories like the Roman Space Telescope and JWST to peer more deeply into our Universe, our community is challenged to develop a theoretical and modeling framework to characterize and study what will be humanity's greatest astronomical discoveries. My research addresses this need by generating detailed, state-of-the-art synthetic observations from hydrodynamic cosmological simulations. By calculating all the processes that photons undergo as they travel across the Universe from the surface of a distant star to a telescope’s detector, my collaborators and I have been able to disentangle perplexing trends in observed galactic spectra as well as make predictions for what we might unveil in the near future. Topics we have investigated in prior work include massive black hole formation, the first stars and galaxies, and the intricate interplay between nebular emission lines and the escape fraction of ionizing radiation. Looking forward, I propose to create the largest and most detailed database of synthetic observational tools and predictions at a time that will come to define astronomy for generations.</div></td></tr>  </table>

Kdkuntz https://caswiki.johnshopkins.edu/index.php?title=Wine_and_Cheese_Spring_2021&diff=1385&oldid=prev Kdkuntz at 18:15, 18 February 2021 2021-02-18T18:15:50Z

<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 18:15, 18 February 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l40">Line 40:</td> <td colspan="2" class="diff-lineno">Line 40:</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>'''Tidal Sculpting of Short-Period Exoplanets'''<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>'''Tidal Sculpting of Short-Period Exoplanets'''<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>Multiple-planet systems composed of close-in super-Earth/sub-Neptune-sized planets are ubiquitous, representing the dominant outcome of planet formation. This population exhibits predictable hallmarks of architectural regularity and uniformity, such as low eccentricities and inclinations, similar orbital spacings, and intra-system correlations in planetary masses and radii. On top of this first-order structure, however, these systems also exhibit surprising anomalies that require explanation. Examples include (1) ultra-short period planets, whose extremely-irradiated orbits have been separated off from the rest of their systems; (2) planets piled up wide of mean-motion resonances; and (3) a subset of Neptune-sized planets that show signs of radius inflation. In this talk, I will propose that tidal dynamics can account for these specific anomalies and more. Specifically, I will discuss the critical role of enhanced tidal dissipation due to non-zero planetary axial tilts (obliquities), which arise by way of prevalent dynamical resonances. I will highlight strategies for testing these tidal theories and observing obliquities directly in the future.</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>Multiple-planet systems composed of close-in super-Earth/sub-Neptune-sized planets are ubiquitous, representing the dominant outcome of planet formation. This population exhibits predictable hallmarks of architectural regularity and uniformity, such as low eccentricities and inclinations, similar orbital spacings, and intra-system correlations in planetary masses and radii. On top of this first-order structure, however, these systems also exhibit surprising anomalies that require explanation. Examples include (1) ultra-short period planets, whose extremely-irradiated orbits have been separated off from the rest of their systems; (2) planets piled up wide of mean-motion resonances; and (3) a subset of Neptune-sized planets that show signs of radius inflation. In this talk, I will propose that tidal dynamics can account for these specific anomalies and more. Specifically, I will discuss the critical role of enhanced tidal dissipation due to non-zero planetary axial tilts (obliquities), which arise by way of prevalent dynamical resonances. I will highlight strategies for testing these tidal theories and observing obliquities directly in the future.</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;">+1 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;">==Kirk Barrow (KIPAC)==</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;">'''Using High-Cadence Synthetic Observations to Unlock a New Era in Astrophysics'''<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;">As astronomers near the commissioning of the extremely large telescopes, the Rubin Observatory, as well as new space-based observatories like the Roman Space Telescope and JWST to peer more deeply into our Universe, our community is challenged to develop a theoretical and modeling framework to characterize and study what will be humanity's greatest astronomical discoveries. My research addresses this need by generating detailed, state-of-the-art synthetic observations from hydrodynamic cosmological simulations. By calculating all the processes that photons undergo as they travel across the Universe from the surface of a distant star to a telescope’s detector, my collaborators and I have been able to disentangle perplexing trends in observed galactic spectra as well as make predictions for what we might unveil in the near future. Topics we have investigated in prior work include massive black hole formation, the first stars and galaxies, and the intricate interplay between nebular emission lines and the escape fraction of ionizing radiation. Looking forward, I propose to create the largest and most detailed database of synthetic observational tools and predictions at a time that will come to define astronomy for generations.</ins></div></td></tr>  </table>

Kdkuntz