https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&feed=atom&action=history Talk:CG4 Proposal - Revision history 2024-03-28T09:37:22Z Revision history for this page on the wiki MediaWiki 1.34.2 https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=4663&oldid=prev Hoette at 18:37, 1 June 2010 2010-06-01T18:37:27Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 18:37, 1 June 2010</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l2" >Line 2:</td> <td colspan="2" class="diff-lineno">Line 2:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>CG4 team page:</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>CG4 team page:</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/CG4_Current_Research_Activities final proposal now linked in from proposal page.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/CG4_Current_Research_Activities final proposal now linked in from proposal page.</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Bigger picture and goals page (agendas for visit, etc)<del class="diffchange diffchange-inline">.</del></div></td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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>Bigger picture and goals page (agendas for visit, etc)<ins class="diffchange diffchange-inline">:</ins></div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/CG4_Bigger_Picture_and_Goals</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/CG4_Bigger_Picture_and_Goals</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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 class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Summer visit logistics page:</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Summer visit logistics page:</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/CG4_Summer_visit</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/CG4_Summer_visit</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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 class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Page with questions specifically for you and our data:</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Page with questions specifically for you and our data:</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/Working_with_CG4%2BSA101  </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/Working_with_CG4%2BSA101  </div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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 class="diffchange diffchange-inline">this </del>is to be used in conjunction with the more generic instructions here:</div></td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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 class="diffchange diffchange-inline">This </ins>is to be used in conjunction with the more generic instructions here:</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/Working_with_L1688</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>http://coolwiki.ipac.caltech.edu/index.php/Working_with_L1688</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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 class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.</div></td></tr> </table> Hoette https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=4662&oldid=prev Hoette at 18:36, 1 June 2010 2010-06-01T18:36:27Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 18:36, 1 June 2010</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l1" >Line 1:</td> <td colspan="2" class="diff-lineno">Line 1:</td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Useful pages: </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">CG4 team page:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Current_Research_Activities final proposal now linked in from proposal page.</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Bigger picture and goals page (agendas for visit, etc).</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Bigger_Picture_and_Goals</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Summer visit logistics page:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Summer_visit</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Page with questions specifically for you and our data:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/Working_with_CG4%2BSA101 </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">this is to be used in conjunction with the more generic instructions here:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/Working_with_L1688</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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 class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>--[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>--[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)</div></td></tr> <tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l54" >Line 54:</td> <td colspan="2" class="diff-lineno">Line 66:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>We propose looking for new young stellar objects (YSOs) in the cometary nebula CG4 in Puppis. We will attempt to answer the following questions: (1) Will stars form here? (2) What triggers star formation? (3) Has a cluster formed? We will use x-ray data from XMM-Newton. We will use astrometry to find proper motion using the Digitized Sky Survey plates and more recent images from CTIO 0.9m telescope. Cometary globule CG4 is approximately 1300 parsecs away. It is one of approximately 30 cometary globules in the Gum Nebula (Choudhury and Bhatt 2008).  These globules are pointed generally radially outward from the center of the Vela OB2 association.  The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. (Reipurth 1993?) CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public. Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine. Our team will use Spitzer IRAC and MIPS data, 2MASS data, and XMM-Newton x-ray data. We expect to find the previously known YSOs (Reipurth and Petersson 1993) and additional YSOs in star-forming regions. We will find other candidate objects using infrared excess across different wavelengths. There will be some non-members in this candidate group. Along with YSOs in the cluster, we expect to find extragalactic sources (i.e., active galactic nuclei). We will use x-ray data, photometric data and astrometry to determine cluster membership and separate YSOs from other objects with infrared excess.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>We propose looking for new young stellar objects (YSOs) in the cometary nebula CG4 in Puppis. We will attempt to answer the following questions: (1) Will stars form here? (2) What triggers star formation? (3) Has a cluster formed? We will use x-ray data from XMM-Newton. We will use astrometry to find proper motion using the Digitized Sky Survey plates and more recent images from CTIO 0.9m telescope. Cometary globule CG4 is approximately 1300 parsecs away. It is one of approximately 30 cometary globules in the Gum Nebula (Choudhury and Bhatt 2008).  These globules are pointed generally radially outward from the center of the Vela OB2 association.  The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. (Reipurth 1993?) CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public. Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine. Our team will use Spitzer IRAC and MIPS data, 2MASS data, and XMM-Newton x-ray data. We expect to find the previously known YSOs (Reipurth and Petersson 1993) and additional YSOs in star-forming regions. We will find other candidate objects using infrared excess across different wavelengths. There will be some non-members in this candidate group. Along with YSOs in the cluster, we expect to find extragalactic sources (i.e., active galactic nuclei). We will use x-ray data, photometric data and astrometry to determine cluster membership and separate YSOs from other objects with infrared excess.</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">CG4 team page:</del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Current_Research_Activities final proposal now linked in from proposal page.</del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">Bigger picture and goals page (agendas for visit, etc).</del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Bigger_Picture_and_Goals</del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">Summer visit logistics page:</del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Summer_visit</del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">Page with questions specifically for you and our data:</del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/Working_with_CG4%2BSA101 </del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">this is to be used in conjunction with the more generic instructions here:</del></div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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;">[http://coolwiki.ipac.caltech.edu/index.php/Working_with_L1688]</del></div></td><td colspan="2"> </td></tr> </table> Hoette https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=4660&oldid=prev Hoette at 18:34, 1 June 2010 2010-06-01T18:34:54Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 18:34, 1 June 2010</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: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>We propose looking for new young stellar objects (YSOs) in the cometary nebula CG4 in Puppis. We will attempt to answer the following questions: (1) Will stars form here? (2) What triggers star formation? (3) Has a cluster formed? We will use x-ray data from XMM-Newton. We will use astrometry to find proper motion using the Digitized Sky Survey plates and more recent images from CTIO 0.9m telescope. Cometary globule CG4 is approximately 1300 parsecs away. It is one of approximately 30 cometary globules in the Gum Nebula (Choudhury and Bhatt 2008).  These globules are pointed generally radially outward from the center of the Vela OB2 association.  The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. (Reipurth 1993?) CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public. Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine. Our team will use Spitzer IRAC and MIPS data, 2MASS data, and XMM-Newton x-ray data. We expect to find the previously known YSOs (Reipurth and Petersson 1993) and additional YSOs in star-forming regions. We will find other candidate objects using infrared excess across different wavelengths. There will be some non-members in this candidate group. Along with YSOs in the cluster, we expect to find extragalactic sources (i.e., active galactic nuclei). We will use x-ray data, photometric data and astrometry to determine cluster membership and separate YSOs from other objects with infrared excess.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>We propose looking for new young stellar objects (YSOs) in the cometary nebula CG4 in Puppis. We will attempt to answer the following questions: (1) Will stars form here? (2) What triggers star formation? (3) Has a cluster formed? We will use x-ray data from XMM-Newton. We will use astrometry to find proper motion using the Digitized Sky Survey plates and more recent images from CTIO 0.9m telescope. Cometary globule CG4 is approximately 1300 parsecs away. It is one of approximately 30 cometary globules in the Gum Nebula (Choudhury and Bhatt 2008).  These globules are pointed generally radially outward from the center of the Vela OB2 association.  The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. (Reipurth 1993?) CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public. Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine. Our team will use Spitzer IRAC and MIPS data, 2MASS data, and XMM-Newton x-ray data. We expect to find the previously known YSOs (Reipurth and Petersson 1993) and additional YSOs in star-forming regions. We will find other candidate objects using infrared excess across different wavelengths. There will be some non-members in this candidate group. Along with YSOs in the cluster, we expect to find extragalactic sources (i.e., active galactic nuclei). We will use x-ray data, photometric data and astrometry to determine cluster membership and separate YSOs from other objects with infrared excess.</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">CG4 team page:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Current_Research_Activities final proposal now linked in from proposal page.</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Bigger picture and goals page (agendas for visit, etc).</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Bigger_Picture_and_Goals</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Summer visit logistics page:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/CG4_Summer_visit</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Page with questions specifically for you and our data:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">http://coolwiki.ipac.caltech.edu/index.php/Working_with_CG4%2BSA101 </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">this is to be used in conjunction with the more generic instructions here:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">[http://coolwiki.ipac.caltech.edu/index.php/Working_with_L1688]</ins></div></td></tr> </table> Hoette https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3997&oldid=prev Mccarron at 16:27, 13 February 2010 2010-02-13T16:27:59Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 16:27, 13 February 2010</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l47" >Line 47:</td> <td colspan="2" class="diff-lineno">Line 47:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>3.  study the distribution of stars, compare the young star population, distribution, and age to other similar sites of star formation.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>3.  study the distribution of stars, compare the young star population, distribution, and age to other similar sites of star formation.</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">DRAFT  CG4 YSO Abstract      DRAFT</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">We propose looking for new young stellar objects (YSOs) in the cometary nebula CG4 in Puppis. We will attempt to answer the following questions: (1) Will stars form here? (2) What triggers star formation? (3) Has a cluster formed? We will use x-ray data from XMM-Newton. We will use astrometry to find proper motion using the Digitized Sky Survey plates and more recent images from CTIO 0.9m telescope. Cometary globule CG4 is approximately 1300 parsecs away. It is one of approximately 30 cometary globules in the Gum Nebula (Choudhury and Bhatt 2008).  These globules are pointed generally radially outward from the center of the Vela OB2 association.  The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. (Reipurth 1993?) CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public. Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine. Our team will use Spitzer IRAC and MIPS data, 2MASS data, and XMM-Newton x-ray data. We expect to find the previously known YSOs (Reipurth and Petersson 1993) and additional YSOs in star-forming regions. We will find other candidate objects using infrared excess across different wavelengths. There will be some non-members in this candidate group. Along with YSOs in the cluster, we expect to find extragalactic sources (i.e., active galactic nuclei). We will use x-ray data, photometric data and astrometry to determine cluster membership and separate YSOs from other objects with infrared excess.</ins></div></td></tr> </table> Mccarron https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3981&oldid=prev Mallory at 05:28, 9 February 2010 2010-02-09T05:28:36Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 05:28, 9 February 2010</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l3" >Line 3:</td> <td colspan="2" class="diff-lineno">Line 3:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited <del class="diffchange diffchange-inline">Superbowl-Sunday </del>7 Feb. 2010<del class="diffchange diffchange-inline">,10:42 p.</del>) <del class="diffchange diffchange-inline">(No, 11:30 p</del>.<del class="diffchange diffchange-inline">)</del></div></td><td class='diff-marker'>+</td><td style="color: #222; 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>Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited 7 Feb. 2010).</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>STAR FORMATION IN CG4</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>STAR FORMATION IN CG4</div></td></tr> </table> Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3977&oldid=prev Mccarron at 23:33, 8 February 2010 2010-02-08T23:33:52Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 23:33, 8 February 2010</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: #222; 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>   </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>   </div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>We propose using IRAC, MIPS and 2MASS data archives along with XMM-Newton satellite data, photometric data (BVRI) from the CTIO 0.9m telescope and astrometric data from the Digitized Sky Survey and more recent images with the CTIO 0.9m telescope to investigate:</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>We propose using IRAC, MIPS and 2MASS data archives along with XMM-Newton satellite data, photometric data (BVRI) from the CTIO 0.9m telescope and astrometric data from the Digitized Sky Survey and more recent images with the CTIO 0.9m telescope to investigate:</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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 class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>1.  Star formation; look for likely cluster member stars with infrared excesses, and  </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>1.  Star formation; look for likely cluster member stars with infrared excesses, and  </div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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 class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>2.  characterize this young star population by obtaining colors and estimates of masses and ages;  </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>2.  characterize this young star population by obtaining colors and estimates of masses and ages;  </div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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 class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>3.  study the distribution of stars, compare the young star population, distribution, and age to other similar sites of star formation.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>3.  study the distribution of stars, compare the young star population, distribution, and age to other similar sites of star formation.</div></td></tr> </table> Mccarron https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3976&oldid=prev Mccarron at 23:33, 8 February 2010 2010-02-08T23:33:29Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 23:33, 8 February 2010</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: #222; 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>Goal:  We are looking for new young stellar objects (YSO) in the cometary nebula CG4 in Puppis.  These objects will tell us about cometary globules and conditions within them.  We will find information about the structures in the globule, their history and possibly their future.   </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Goal:  We are looking for new young stellar objects (YSO) in the cometary nebula CG4 in Puppis.  These objects will tell us about cometary globules and conditions within them.  We will find information about the structures in the globule, their history and possibly their future.   </div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>   </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>   </div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Stars form in regions of dense dust and gas in the interstellar medium (ISM).  The process is....  </div></td><td class='diff-marker'>+</td><td style="color: #222; 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>Stars form in regions of dense dust and gas in the interstellar medium (ISM).  The process is.... <ins class="diffchange diffchange-inline">(See Carolyn's explaination above.)  </ins></div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>   </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>   </div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Cometary globule CG4 is approximately 450 parsec away.  It is a part of a larger structure in the Milky Way.  It is one of a number of cometary globules in the area pointed away from a common center, possibly the Vela supernova remnant.  CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public.  Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine.   </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Cometary globule CG4 is approximately 450 parsec away.  It is a part of a larger structure in the Milky Way.  It is one of a number of cometary globules in the area pointed away from a common center, possibly the Vela supernova remnant.  CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public.  Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine.   </div></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: #222; 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>   </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>   </div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>We propose using IRAC, MIPS and 2MASS data archives along with XMM-Newton satellite data, photometric data (BVRI) from the CTIO 0.9m telescope and astrometric data from the Digitized Sky Survey and more recent images with the CTIO 0.9m telescope to investigate:</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>We propose using IRAC, MIPS and 2MASS data archives along with XMM-Newton satellite data, photometric data (BVRI) from the CTIO 0.9m telescope and astrometric data from the Digitized Sky Survey and more recent images with the CTIO 0.9m telescope to investigate:</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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 class="diffchange diffchange-inline">    </del>1.  Star formation; look for likely cluster member stars with infrared excesses, and  </div></td><td class='diff-marker'>+</td><td style="color: #222; 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>1.  Star formation; look for likely cluster member stars with infrared excesses, and  </div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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 class="diffchange diffchange-inline">    </del>2.  characterize this young star population by obtaining colors and estimates of masses and ages;  </div></td><td class='diff-marker'>+</td><td style="color: #222; 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>2.  characterize this young star population by obtaining colors and estimates of masses and ages;  </div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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 class="diffchange diffchange-inline">    </del>3.  study the distribution of stars, compare the young star population, distribution, and age to other similar sites of star formation.</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>3.  study the distribution of stars, compare the young star population, distribution, and age to other similar sites of star formation.</div></td></tr> </table> Mccarron https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3975&oldid=prev Mccarron at 23:30, 8 February 2010 2010-02-08T23:30:38Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 23:30, 8 February 2010</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l25" >Line 25:</td> <td colspan="2" class="diff-lineno">Line 25:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Spitzer is good at determining these qualities of stars. It is so sensitive that it can see nearly to the 'edge' of the Universe, and integrate data in just a handful of seconds. Further, Spitz, will see the excess IR from the Planatary Disc of a newly formed star, before it gets dissipated, and that will record as a Spare Tire IR Excess. Chandra and XMM data will be helpful in detecting X-ray flares due to large magnetic field, from rapid rotation inducing emission flares in X-ray wavelength.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>Spitzer is good at determining these qualities of stars. It is so sensitive that it can see nearly to the 'edge' of the Universe, and integrate data in just a handful of seconds. Further, Spitz, will see the excess IR from the Planatary Disc of a newly formed star, before it gets dissipated, and that will record as a Spare Tire IR Excess. Chandra and XMM data will be helpful in detecting X-ray flares due to large magnetic field, from rapid rotation inducing emission flares in X-ray wavelength.</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Proposal for CG4 Group</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Goal:  We are looking for new young stellar objects (YSO) in the cometary nebula CG4 in Puppis.  These objects will tell us about cometary globules and conditions within them.  We will find information about the structures in the globule, their history and possibly their future.  </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Stars form in regions of dense dust and gas in the interstellar medium (ISM).  The process is.... </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Cometary globule CG4 is approximately 450 parsec away.  It is a part of a larger structure in the Milky Way.  It is one of a number of cometary globules in the area pointed away from a common center, possibly the Vela supernova remnant.  CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public.  Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine.  </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">Method:  Our team will use Spitzer IRAC and MIPS data (programs 202, 462, 20714), 2MASS data,  and XMM-Newton x-ray data.  We expect to find the previously known YSOs (Reipurth and  Petersson 1993) and additional YSOs in star-forming regions.  We will find other candidate objects using infrared excess across different wavelengths.  There will be some non-members in this candidate group.  Along with YSOs in the cluster, we expect to find extragallactic sources (active galactic nuclei anything else ?).  We will use x-ray data, phtometric data and astrometry to determine cluster membership and separate YSOs from other objects with IR excess.</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">We will use x-ray data from the . We will use astrometry to find proper motion  using the Digitized Sky Survey plates and more recent images from CTIO 0.9m telescope.  </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">We propose using IRAC, MIPS and 2MASS data archives along with XMM-Newton satellite data, photometric data (BVRI) from the CTIO 0.9m telescope and astrometric data from the Digitized Sky Survey and more recent images with the CTIO 0.9m telescope to investigate:</ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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.  Star formation; look for likely cluster member stars with infrared excesses, and </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">    2.  characterize this young star population by obtaining colors and estimates of masses and ages; </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; 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;">    3.  study the distribution of stars, compare the young star population, distribution, and age to other similar sites of star formation.</ins></div></td></tr> </table> Mccarron https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3974&oldid=prev Mallory at 07:29, 8 February 2010 2010-02-08T07:29:41Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 07:29, 8 February 2010</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l3" >Line 3:</td> <td colspan="2" class="diff-lineno">Line 3:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited Superbowl-Sunday 7 Feb. 2010,10:42 p.) (No, 11:<del class="diffchange diffchange-inline">10 </del>p.)</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited Superbowl-Sunday 7 Feb. 2010,10:42 p.) (No, 11:<ins class="diffchange diffchange-inline">30 </ins>p.)</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>STAR FORMATION IN CG4</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>STAR FORMATION IN CG4</div></td></tr> </table> Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3973&oldid=prev Mallory at 07:28, 8 February 2010 2010-02-08T07:28:19Z <p></p> <table class="diff diff-contentalign-left" 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: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 07:28, 8 February 2010</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l3" >Line 3:</td> <td colspan="2" class="diff-lineno">Line 3:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited Superbowl-Sunday 7 Feb. 2010,10:42 p.)  </div></td><td class='diff-marker'>+</td><td style="color: #222; 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>Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited Superbowl-Sunday 7 Feb. 2010,10:42 <ins class="diffchange diffchange-inline">p.) (No, 11:10 </ins>p.)</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>STAR FORMATION IN CG4</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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>STAR FORMATION IN CG4</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their <del class="diffchange diffchange-inline">environment</del>, and form stars?  When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their <ins class="diffchange diffchange-inline">environments</ins>, and form stars?  When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; <del class="diffchange diffchange-inline">Evolution of </del>the structural components of the universe, i.e. <del class="diffchange diffchange-inline">Galaxies</del>, causes evolution of the Universe.  </div></td><td class='diff-marker'>+</td><td style="color: #222; 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>What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; <ins class="diffchange diffchange-inline">which are </ins>the structural components of the universe, i.e. <ins class="diffchange diffchange-inline">Galaxie Changes</ins>, causes evolution of the Universe.  </div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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 Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. Using this Locale, we will attempt to answer three questions: Will Stars Form Here?  If So, Is Their Formation Triggered? and, Has a Whole Cluster Been Formed?</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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 Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. Using this Locale, we will attempt to answer three questions: Will Stars Form Here?  If So, Is Their Formation Triggered? and, Has a Whole Cluster Been Formed?</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude.  Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the <del class="diffchange diffchange-inline">outsides </del>of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude.  Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m. Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the <ins class="diffchange diffchange-inline">surfaces </ins>of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Conditional on the outcome of the first research step; The second step in our research is to determine whether this is Triggered Star Formation.(See “Spitzer Observations of IC 2118.) The outcome of this important research question will help to determine the Rate of Star Formation in the Universe. The presence of both O &amp; B superstars, copious UV and gamma emitters, plus Supernova <del class="diffchange diffchange-inline">Remnats </del>indicating stupendous interstellar explosions, suggest an energetic nebular environment. We verified this using Multiwavelength Photometric Studies, similar to (Kim,S. et al, &quot;Triggered Low Mass Star Formation in the Gum Nebula&quot;, 2003). A similar environment, see Spitzer Observations of IC 2118, confirm this idea. The Skyview Telescope (http://skyview.gsfc.nasa.gov) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. Through our collaborator J.S. Kim (U. AZ)we have access to X-ray data from XMM, Epic and PN images that cover CG4.X-ray + UV presence may have triggered star formation by providing compression pressure onto collapsing nebula gas-knots, or destroyed them by photo-evaporation.</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>Conditional on the outcome of the first research step; The second step in our research is to determine whether this is Triggered Star Formation.(See “Spitzer Observations of IC 2118.) The outcome of this important research question will help to determine the Rate of Star Formation in the Universe. The presence of both O &amp; B superstars, copious UV and gamma emitters, plus Supernova <ins class="diffchange diffchange-inline">Remnants </ins>indicating stupendous interstellar explosions, suggest an energetic nebular environment. We verified this using Multiwavelength Photometric Studies, similar to (Kim,S. et al, &quot;Triggered Low Mass Star Formation in the Gum Nebula&quot;, 2003). A similar environment, see Spitzer Observations of IC 2118, confirm this idea. The Skyview Telescope (http://skyview.gsfc.nasa.gov) shows radiation at all wavelengths and images at all wavelengths<ins class="diffchange diffchange-inline">, </ins>of excited gas/dust in the selected region. Through our collaborator J.S. Kim (U. AZ)we have access to X-ray data from XMM, Epic and PN images that cover CG4. X-ray + UV presence may have triggered star formation by providing compression pressure onto collapsing nebula gas-knots, or destroyed them by photo-evaporation.</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula<del class="diffchange diffchange-inline">. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from  Determining the distance from CG4 to those O &amp; B stars (using              ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.</del></div></td><td class='diff-marker'>+</td><td style="color: #222; 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>Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula.  </div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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 class="diffchange diffchange-inline">When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star</del>.</div></td><td colspan="2"> </td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Our Final Question related to Star Formation in CG4, &quot;Has a Whole Star Cluster Been Formed&quot;, has to be approached carefully, since it is so easy to confuse a foreground/background star with actual Cluster Members. The finest tool to accomplish the identification of Stars Which Are Cluster Members, resides on the IPAC website. What the techniques boils down to, is to determine all YSOs in an area, and be sure they are all the same age. <del class="diffchange diffchange-inline">Likelym </del>they are all members of the same cluster. Some characteristics they should all have/all have in common, are: IR excess<del class="diffchange diffchange-inline">, </del>flaring/in X-rays<del class="diffchange diffchange-inline">, </del>flaring /in radio/stellar active regions, like Sun Spots<del class="diffchange diffchange-inline">, </del>BiPolar outflows (detectable in IR &amp; optical as emitted jets)<del class="diffchange diffchange-inline">, </del>emission lines (from accreting matter)<del class="diffchange diffchange-inline">, </del>variability (not quite in equilibrium yet)<del class="diffchange diffchange-inline">, </del>fast rotation rate (concervation of Angular Momentum)<del class="diffchange diffchange-inline">, </del>UV flaring/mass accretion<del class="diffchange diffchange-inline">, </del>spatial location huddled together<del class="diffchange diffchange-inline">, </del>similar brightness<del class="diffchange diffchange-inline">, </del>common spatial motion as they glide through space <del class="diffchange diffchange-inline">somewhat </del>gravitationally bound together.</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>Our Final Question related to Star Formation in CG4, &quot;Has a Whole Star Cluster Been Formed&quot;, has to be approached carefully, since it is so easy to confuse a foreground/background star with actual Cluster Members. The finest tool to accomplish the identification of Stars Which Are Cluster Members, resides on the IPAC website. What the techniques boils down to, is to determine all YSOs in an area, and be sure they are all the same age. <ins class="diffchange diffchange-inline">If they are the same age, it is likely </ins>they are all members of the same cluster. Some characteristics they should all have/all have in common, are: IR excess<ins class="diffchange diffchange-inline">; </ins>flaring/in X-rays<ins class="diffchange diffchange-inline">; </ins>flaring /in radio/<ins class="diffchange diffchange-inline">emmission from </ins>stellar active regions, like Sun Spots<ins class="diffchange diffchange-inline">; </ins>BiPolar outflows (detectable in IR &amp; optical as emitted jets)<ins class="diffchange diffchange-inline">; </ins>emission lines (from accreting matter)<ins class="diffchange diffchange-inline">; </ins>variability (not quite in equilibrium yet)<ins class="diffchange diffchange-inline">; </ins>fast rotation rate (concervation of Angular Momentum)<ins class="diffchange diffchange-inline">; </ins>UV flaring/mass accretion<ins class="diffchange diffchange-inline">; </ins>spatial location huddled together<ins class="diffchange diffchange-inline">; </ins>similar brightness<ins class="diffchange diffchange-inline">; </ins>common spatial motion as they glide through space <ins class="diffchange diffchange-inline">loosely </ins>gravitationally bound together.</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Spitzer is good at <del class="diffchange diffchange-inline">ddetermining </del>these qualities of stars. It is so sensitive that it can see nearly to the 'edge' of the Universe, and integrate data in just a handful of seconds. Further, Spitz will see the excess IR from the Planatary Disc of a newly formed star, before it gets <del class="diffchange diffchange-inline">disipated</del>, and that will record as a Spare Tire IR Excess. Chandra and XMM data will be helpful in detecting X-ray flares due to large magnetic field from rapid rotation inducing emission flares in X-ray wavelength.</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>Spitzer is good at <ins class="diffchange diffchange-inline">determining </ins>these qualities of stars. It is so sensitive that it can see nearly to the 'edge' of the Universe, and integrate data in just a handful of seconds. Further, Spitz<ins class="diffchange diffchange-inline">, </ins>will see the excess IR from the Planatary Disc of a newly formed star, before it gets <ins class="diffchange diffchange-inline">dissipated</ins>, and that will record as a Spare Tire IR Excess. Chandra and XMM data will be helpful in detecting X-ray flares due to large magnetic field<ins class="diffchange diffchange-inline">, </ins>from rapid rotation inducing emission flares in X-ray wavelength.</div></td></tr> </table> Mallory