https://vmcoolwiki.ipac.caltech.edu/api.php?action=feedcontributions&user=Piper&feedformat=atom CoolWiki - User contributions [en] 2024-03-29T05:41:47Z User contributions MediaWiki 1.34.2 https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12224 ProtostarsInNGC281 2013-11-11T21:52:03Z <p>Piper: /* Two Scenarios for Star Formation */</p> <hr /> <div><br /> The idea is to start gathering two items:<br /> # Relevant figures<br /> # Text and references.<br /> <br /> <br /> ===Abstract===<br /> * Carol.<br /> <br /> <br /> ===Introduction to NGC 281===<br /> * Melissa<br /> <br /> <br /> ===Protostar basics===<br /> * Lynn<br /> <br /> <br /> ===Two Scenarios for Star Formation===<br /> * Peggy<br /> <br /> ====Spontaneous vs. Triggered Star Formation====<br /> • Most star formation begins due to spontaneous processes on a galactic scale, given sufficient time and material free fall will result in star formation.&lt;br&gt;<br /> • An outside source of energy can trigger the formation of a star before conditions become sufficient for free fall, leaving sequentially younger stars in its path while clouds broken into filaments by magnetic fields will show a filamentary pattern of protostars.<br /> <br /> ====Star formation in a “controlled” environment====<br /> • small regions where the formation conditions except for the trigger are the same&lt;br&gt;<br /> • physical and geographical characteristics of protostars created can therefore be related to triggering mechanism. <br /> <br /> ====NGC 281====<br /> • HII emission containing the young galactic cluster IC 1590, OB star trapezium system HD5005 with what appears to be two distinct start forming regions around it;&lt;br&gt;<br /> • Triggered East side with “pillars of creation”, newborn stars as a result of triggering from the nearby OB star trapezium system. &lt;br&gt;<br /> • Crowded West side with three distinct clumps (NE, NW and S) of star formation.&lt;br&gt;<br /> <br /> ===Herschel data===<br /> * Carol<br /> <br /> <br /> ===Spitzer data===<br /> * Melissa<br /> <br /> <br /> ===Source Identification===<br /> * Carol<br /> <br /> <br /> ===Photometry Using APT===<br /> * Lynn<br /> <br /> <br /> ===Final Source Selection===<br /> * Melissa<br /> * Peggy<br /> <br /> <br /> ===Analysis &amp; Results===<br /> * TBD<br /> <br /> <br /> ===Discussion &amp; Conclusions===<br /> * TBD<br /> <br /> <br /> ===List of References===<br /> * TBD<br /> <br /> <br /> ===List of Authors &amp; Affiliations===<br /> * Carol</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPsDataTableRules.txt&diff=12126 File:SHIPsDataTableRules.txt 2013-08-15T17:12:54Z <p>Piper: uploaded a new version of &amp;quot;File:SHIPsDataTableRules.txt&amp;quot;</p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SummerVisit&diff=11869 SummerVisit 2013-06-09T00:29:30Z <p>Piper: /* Evening excursions from the past */</p> <hr /> <div><br /> At the moment, this is just a bulletized list of items we wish to cover. An actual agenda (with times and durations) as well as when these items occur will follow.<br /> <br /> ==Sunday, 23 June==<br /> * Arrivals.<br /> ** Lynn 1 adult 3 students pick up van 12:07 p.m. hang around airport or nearby beach to pick up Carol at 3:05 p.m. unless Carol arranges shuttle?<br /> ** Peggy 1 adult 1:40 p.m. find Melissa's group for ride.<br /> ** Melissa 1 adult 4 students pick up van 1:50 p.m.<br /> ** Carol 1 adult 2 students 3:05 p.m., Lynn pick up or take SuperShuttle to Pasadena?<br /> * Hotel - please double check your check out date is Friday, June 28 with Saga front desk.<br /> * Evening. (Possibly) dinner or BBQ.<br /> <br /> ==Monday, 24 June==<br /> * Introductions.<br /> * Tour of KS and meet Wanetta<br /> * Infrared portraits<br /> * Goals, Agenda discussion.<br /> * NGC 281 photometry<br /> ** Presentations by individual groups.<br /> ** Discussion and consolidation<br /> * Pick 14 protostar candidates (1 per person) to follow during the summer visit.<br /> <br /> <br /> ==Tuesday, 25 June==<br /> * Photometry (continued).<br /> * Plans for finalizing data.<br /> * Division of final photometry list for subsequent analysis.<br /> * SEDs<br /> ** How to generate SEDs<br /> ** How to interpret SEDs<br /> ** Plots of 14 protostars.<br /> ** SED fitting by models.<br /> <br /> <br /> ==Wednesday, 26 June==<br /> * Morning: SEDs and protostar discussion.<br /> * Afternoon: Break.<br /> <br /> <br /> ==Thursday, 27 June==<br /> * JPL tour<br /> * Science goals results for 14 protostars.<br /> <br /> <br /> ==Friday, 28 June==<br /> * Departures.<br /> ** Carol extended stay, 2 students 6:30 a.m. flight, shuttle?<br /> ** Peggy extended stay.<br /> ** Lynn 1 adult 3 students return van 6:10 p.m. flight.<br /> ** Melissa 1 adult 4 students return van 10:35 pm. flight.<br /> <br /> ==Evening excursions from the past==<br /> Our day time schedule is very structured, tends to be stressful/mindblowing and there is a hierarchy; Babar, teachers, students. My past groups have left the evenings to the design of the students. As a group they need to come up with where we are going, what we are going to do (wander is perfectly acceptable) and navigate us to these places (we drive, but they find and give directions). As much as possible we let them agree/disagree and come to a solution, we are just along for the ride (and a little supervision). The more these three separate groups of young people come together as a team, the more satisfying this experience will be for both adults and students. <br /> <br /> Please add other ideas your group comes up with to these possible ideas are:<br /> * First (Sunday) night, trip to nearby Target to pick up munchies/drinks for hotel and Caltech. Consider asking each person to contribute one object to munch (bag of chips, box of cookies, twizzlers, etc) for Caltech stash that we will leave in closet of our work room.<br /> * Griffith Observatory<br /> * Hike the Hollywood sign<br /> * Santa Monica Pier, kids roam, adults sit and have meal<br /> * Venice Beach = culture shock (in a good way)<br /> * Walk the Universal City Walk<br /> * One night, nice sit down dinner<br /> * In and Out Burger seems to have some fascinated<br /> * Mount Wilson (I haven't done, but other groups have)<br /> * Sporting event (one group had big fan and those interested went to game, no idea what team, rest of group wandered the beach)<br /> * Lunches - fast, need to get back to work!<br /> ** At least one meal in the Caltech cafeteria with time to stop at book store<br /> ** Walk to near by fast food, let kids scatter as long as no one goes alone, adults may choose to separate or use time to regroup w/o students<br /> ** Use travel from JPL back to Caltech to hit In and Out Burger or other interesting chain.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SummerVisit&diff=11868 SummerVisit 2013-06-09T00:28:23Z <p>Piper: </p> <hr /> <div><br /> At the moment, this is just a bulletized list of items we wish to cover. An actual agenda (with times and durations) as well as when these items occur will follow.<br /> <br /> ==Sunday, 23 June==<br /> * Arrivals.<br /> ** Lynn 1 adult 3 students pick up van 12:07 p.m. hang around airport or nearby beach to pick up Carol at 3:05 p.m. unless Carol arranges shuttle?<br /> ** Peggy 1 adult 1:40 p.m. find Melissa's group for ride.<br /> ** Melissa 1 adult 4 students pick up van 1:50 p.m.<br /> ** Carol 1 adult 2 students 3:05 p.m., Lynn pick up or take SuperShuttle to Pasadena?<br /> * Hotel - please double check your check out date is Friday, June 28 with Saga front desk.<br /> * Evening. (Possibly) dinner or BBQ.<br /> <br /> ==Monday, 24 June==<br /> * Introductions.<br /> * Tour of KS and meet Wanetta<br /> * Infrared portraits<br /> * Goals, Agenda discussion.<br /> * NGC 281 photometry<br /> ** Presentations by individual groups.<br /> ** Discussion and consolidation<br /> * Pick 14 protostar candidates (1 per person) to follow during the summer visit.<br /> <br /> <br /> ==Tuesday, 25 June==<br /> * Photometry (continued).<br /> * Plans for finalizing data.<br /> * Division of final photometry list for subsequent analysis.<br /> * SEDs<br /> ** How to generate SEDs<br /> ** How to interpret SEDs<br /> ** Plots of 14 protostars.<br /> ** SED fitting by models.<br /> <br /> <br /> ==Wednesday, 26 June==<br /> * Morning: SEDs and protostar discussion.<br /> * Afternoon: Break.<br /> <br /> <br /> ==Thursday, 27 June==<br /> * JPL tour<br /> * Science goals results for 14 protostars.<br /> <br /> <br /> ==Friday, 28 June==<br /> * Departures.<br /> ** Carol extended stay, 2 students 6:30 a.m. flight, shuttle?<br /> ** Peggy extended stay.<br /> ** Lynn 1 adult 3 students return van 6:10 p.m. flight.<br /> ** Melissa 1 adult 4 students return van 10:35 pm. flight.<br /> <br /> ==Evening excursions from the past==<br /> Our day time schedule is very structured, tends to be stressful/mindblowing and there is a hierarchy; Babar, teachers, students. My past groups have left the evenings to the design of the students. As a group they need to come up with where we are going, what we are going to do (wander is perfectly acceptable) and navigate us to these places (we drive, but they find and give directions). As much as possible we let them agree/disagree and come to a solution, we are just along for the ride (and a little supervision). The more these three separate groups of young people come together as a team, the more satisfying this experience will be for both adults and students. <br /> <br /> Please add other ideas your group comes up with to these possible ideas are:<br /> * First night, trip to nearby Target to pick up munchies/drinks for hotel and Caltech. Consider asking each person to contribute one object to munch (bag of chips, box of cookies, twizzlers, etc) for Caltech stash that we will leave in closet of our work room.<br /> * Griffith Observatory<br /> * Hike the Hollywood sign<br /> * Santa Monica Pier, kids roam, adults sit and have meal<br /> * Venice Beach = culture shock (in a good way)<br /> * Walk the Universal City Walk<br /> * One night, nice sit down dinner<br /> * In and Out Burger seems to have some fascinated<br /> * Mount Wilson (I haven't done, but other groups have)<br /> * Sporting event (one group had big fan and those interested went to game, no idea what team, rest of group wandered the beach)<br /> * Lunches - fast, need to get back to work!<br /> ** At least one meal in the Caltech cafeteria with time to stop at book store<br /> ** Walk to near by fast food, let kids scatter as long as no one goes alone, adults may choose to separate or use time to regroup w/o students<br /> ** Use travel from JPL back to Caltech to hit In and Out Burger or other interesting chain.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SummerVisit&diff=11867 SummerVisit 2013-06-09T00:01:59Z <p>Piper: /* Friday, 28 June */</p> <hr /> <div><br /> At the moment, this is just a bulletized list of items we wish to cover. An actual agenda (with times and durations) as well as when these items occur will follow.<br /> <br /> ==Sunday, 23 June==<br /> * Arrivals.<br /> ** Lynn 1 adult 3 students pick up van 12:07 p.m. hang around airport or nearby beach to pick up Carol at 3:05 p.m. unless Carol arranges shuttle?<br /> ** Peggy 1 adult 1:40 p.m. find Melissa's group for ride.<br /> ** Melissa 1 adult 4 students pick up van 1:50 p.m.<br /> ** Carol 1 adult 2 students 3:05 p.m., Lynn pick up or take SuperShuttle to Pasadena?<br /> * Hotel - please double check your check out date is Friday, June 28 with Saga front desk.<br /> * Evening. (Possibly) dinner or BBQ.<br /> <br /> ==Monday, 24 June==<br /> * Introductions.<br /> * Tour of KS and meet Wanetta<br /> * Infrared portraits<br /> * Goals, Agenda discussion.<br /> * NGC 281 photometry<br /> ** Presentations by individual groups.<br /> ** Discussion and consolidation<br /> * Pick 14 protostar candidates (1 per person) to follow during the summer visit.<br /> <br /> <br /> ==Tuesday, 25 June==<br /> * Photometry (continued).<br /> * Plans for finalizing data.<br /> * Division of final photometry list for subsequent analysis.<br /> * SEDs<br /> ** How to generate SEDs<br /> ** How to interpret SEDs<br /> ** Plots of 14 protostars.<br /> ** SED fitting by models.<br /> <br /> <br /> ==Wednesday, 26 June==<br /> * Morning: SEDs and protostar discussion.<br /> * Afternoon: Break.<br /> <br /> <br /> ==Thursday, 27 June==<br /> * JPL tour<br /> * Science goals results for 14 protostars.<br /> <br /> <br /> ==Friday, 28 June==<br /> * Departures.<br /> ** Carol extended stay, 2 students 6:30 a.m. flight, shuttle?<br /> ** Peggy extended stay.<br /> ** Lynn 1 adult 3 students return van 6:10 p.m. flight.<br /> ** Melissa 1 adult 4 students return van 10:35 pm. flight.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SummerVisit&diff=11866 SummerVisit 2013-06-08T23:54:32Z <p>Piper: /* Sunday, 23 June */</p> <hr /> <div><br /> At the moment, this is just a bulletized list of items we wish to cover. An actual agenda (with times and durations) as well as when these items occur will follow.<br /> <br /> ==Sunday, 23 June==<br /> * Arrivals.<br /> ** Lynn 1 adult 3 students pick up van 12:07 p.m. hang around airport or nearby beach to pick up Carol at 3:05 p.m. unless Carol arranges shuttle?<br /> ** Peggy 1 adult 1:40 p.m. find Melissa's group for ride.<br /> ** Melissa 1 adult 4 students pick up van 1:50 p.m.<br /> ** Carol 1 adult 2 students 3:05 p.m., Lynn pick up or take SuperShuttle to Pasadena?<br /> * Hotel - please double check your check out date is Friday, June 28 with Saga front desk.<br /> * Evening. (Possibly) dinner or BBQ.<br /> <br /> ==Monday, 24 June==<br /> * Introductions.<br /> * Tour of KS and meet Wanetta<br /> * Infrared portraits<br /> * Goals, Agenda discussion.<br /> * NGC 281 photometry<br /> ** Presentations by individual groups.<br /> ** Discussion and consolidation<br /> * Pick 14 protostar candidates (1 per person) to follow during the summer visit.<br /> <br /> <br /> ==Tuesday, 25 June==<br /> * Photometry (continued).<br /> * Plans for finalizing data.<br /> * Division of final photometry list for subsequent analysis.<br /> * SEDs<br /> ** How to generate SEDs<br /> ** How to interpret SEDs<br /> ** Plots of 14 protostars.<br /> ** SED fitting by models.<br /> <br /> <br /> ==Wednesday, 26 June==<br /> * Morning: SEDs and protostar discussion.<br /> * Afternoon: Break.<br /> <br /> <br /> ==Thursday, 27 June==<br /> * JPL tour<br /> * Science goals results for 14 protostars.<br /> <br /> <br /> ==Friday, 28 June==<br /> * Departures.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=5_APT_Practice_Sources&diff=11699 5 APT Practice Sources 2013-05-06T03:38:38Z <p>Piper: </p> <hr /> <div>Here's what I got for the 5 practice sources, let me know if you are getting something different. &lt;BR&gt;<br /> <br /> [[File:APT Practice image.png|500px]]<br /> <br /> &lt;BR&gt; (results without aperture correction)&lt;BR&gt;<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+5 APT Practice Sources - Peggy's Results<br /> |-<br /> ! scope=&quot;col&quot;| Source #<br /> ! scope=&quot;col&quot;| RA<br /> ! scope=&quot;col&quot;| Dec<br /> ! scope=&quot;col&quot;| Intensity (Jy)<br /> |-<br /> |1 <br /> |00h52m55.935s <br /> |56d37m33.34s <br /> |0.32138 <br /> |-<br /> |2 <br /> |00h52m29.964s <br /> |56d33m28.27s <br /> |1.4025<br /> |-<br /> |3 <br /> |00h52m11.006s <br /> |56d30m57.86s <br /> |10.128<br /> |-<br /> |4 <br /> |00h54m26.111s <br /> |56d33m50.84s <br /> |0.41759<br /> |-<br /> |5 <br /> |00h54m46.474s <br /> |56d34m39.10s <br /> |0.09216<br /> |}</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=5_APT_Practice_Sources&diff=11698 5 APT Practice Sources 2013-05-04T03:34:47Z <p>Piper: </p> <hr /> <div>Here's what I got for the 5 practice sources, let me know if you are getting something different. &lt;BR&gt;<br /> <br /> [[File:APT Practice image.png|500px]]<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+5 APT Practice Sources - Peggy's Results<br /> |-<br /> ! scope=&quot;col&quot;| Source #<br /> ! scope=&quot;col&quot;| RA<br /> ! scope=&quot;col&quot;| Dec<br /> ! scope=&quot;col&quot;| Intensity (Jy)<br /> |-<br /> |1 <br /> |00h52m55.935s <br /> |56d37m33.34s <br /> |0.32138 <br /> |-<br /> |2 <br /> |00h52m29.964s <br /> |56d33m28.27s <br /> |1.4025<br /> |-<br /> |3 <br /> |00h52m11.006s <br /> |56d30m57.86s <br /> |10.128<br /> |-<br /> |4 <br /> |00h54m26.111s <br /> |56d33m50.84s <br /> |0.41759<br /> |-<br /> |5 <br /> |00h54m46.474s <br /> |56d34m39.10s <br /> |0.09216<br /> |}</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=5_APT_Practice_Sources&diff=11697 5 APT Practice Sources 2013-05-04T03:29:18Z <p>Piper: </p> <hr /> <div>[[File:APT Practice image.png]]<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+5 APT Practice Sources - Peggy's Results<br /> |-<br /> ! scope=&quot;col&quot;| Source #<br /> ! scope=&quot;col&quot;| RA<br /> ! scope=&quot;col&quot;| Dec<br /> ! scope=&quot;col&quot;| Intensity (Jy)<br /> |-<br /> |1 <br /> |00h52m55.935s <br /> |56d37m33.34s <br /> |0.32138 <br /> |-<br /> |2 <br /> |00h52m29.964s <br /> |56d33m28.27s <br /> |1.4025<br /> |-<br /> |3 <br /> |00h52m11.006s <br /> |56d30m57.86s <br /> |10.128<br /> |-<br /> |4 <br /> |00h54m26.111s <br /> |56d33m50.84s <br /> |0.41759<br /> |-<br /> |5 <br /> |00h54m46.474s <br /> |56d34m39.10s <br /> |0.09216<br /> |}</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:APT_Practice_image.png&diff=11696 File:APT Practice image.png 2013-05-04T03:28:47Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=5_APT_Practice_Sources&diff=11695 5 APT Practice Sources 2013-05-04T03:27:34Z <p>Piper: </p> <hr /> <div>[[File:APT Practice image.jpg]]<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+5 APT Practice Sources - Peggy's Results<br /> |-<br /> ! scope=&quot;col&quot;| Source #<br /> ! scope=&quot;col&quot;| RA<br /> ! scope=&quot;col&quot;| Dec<br /> ! scope=&quot;col&quot;| Intensity (Jy)<br /> |-<br /> |1 <br /> |00h52m55.935s <br /> |56d37m33.34s <br /> |0.32138 <br /> |-<br /> |2 <br /> |00h52m29.964s <br /> |56d33m28.27s <br /> |1.4025<br /> |-<br /> |3 <br /> |00h52m11.006s <br /> |56d30m57.86s <br /> |10.128<br /> |-<br /> |4 <br /> |00h54m26.111s <br /> |56d33m50.84s <br /> |0.41759<br /> |-<br /> |5 <br /> |00h54m46.474s <br /> |56d34m39.10s <br /> |0.09216<br /> |}</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=5_APT_Practice_Sources&diff=11694 5 APT Practice Sources 2013-05-04T03:26:43Z <p>Piper: Created page with &quot; {| class=&quot;wikitable&quot; |+5 APT Practice Sources - Peggy's Results |- ! scope=&quot;col&quot;| Source # ! scope=&quot;col&quot;| RA ! scope=&quot;col&quot;| Dec ! scope=&quot;col&quot;| Intensity (Jy) |- |1 |00h52m...&quot;</p> <hr /> <div><br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+5 APT Practice Sources - Peggy's Results<br /> |-<br /> ! scope=&quot;col&quot;| Source #<br /> ! scope=&quot;col&quot;| RA<br /> ! scope=&quot;col&quot;| Dec<br /> ! scope=&quot;col&quot;| Intensity (Jy)<br /> |-<br /> |1 <br /> |00h52m55.935s <br /> |56d37m33.34s <br /> |0.32138 <br /> |-<br /> |2 <br /> |00h52m29.964s <br /> |56d33m28.27s <br /> |1.4025<br /> |-<br /> |3 <br /> |00h52m11.006s <br /> |56d30m57.86s <br /> |10.128<br /> |-<br /> |4 <br /> |00h54m26.111s <br /> |56d33m50.84s <br /> |0.41759<br /> |-<br /> |5 <br /> |00h54m46.474s <br /> |56d34m39.10s <br /> |0.09216<br /> |}</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsPhot&diff=11693 SHIPsPhot 2013-05-04T03:15:52Z <p>Piper: /* Photometry Assignment */</p> <hr /> <div>Purpose of this page:<br /> * Provide photometry references for Herschel specific photometry<br /> <br /> <br /> ==Aperture Photometry Parameters==<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Recommended Values for NGC 281<br /> |-<br /> ! scope=&quot;col&quot;| Filter<br /> ! scope=&quot;col&quot;| Aperture Radius (&quot;)<br /> ! scope=&quot;col&quot;| Inner Sky Radius (&quot;)<br /> ! scope=&quot;col&quot;| Outer Sky Radius (&quot;)<br /> ! scope=&quot;coI&quot;| Aperture Correction <br /> |-<br /> |70 microns <br /> |9.6<br /> |9.6<br /> |19.2<br /> |0.7331<br /> |-<br /> |100 microns<br /> |9.6<br /> |9.6<br /> |19.2<br /> |0.6944<br /> |-<br /> |160 microns<br /> |12.8<br /> |12.8<br /> |25.6<br /> |0.6602<br /> |}<br /> <br /> <br /> <br /> ==APT parameters==<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Values to use for APT photometry<br /> |-<br /> ! scope=&quot;col&quot;| Parameter/Setting<br /> ! scope=&quot;col&quot;| SHIPs value<br /> ! scope=&quot;col&quot;| Comments<br /> |-<br /> |Aperture Values<br /> |As in above table recomputed to pixels.<br /> |<br /> |-<br /> |Select source algorithm <br /> |Model 0<br /> |<br /> |-<br /> |Select sky algorithm<br /> |Model B<br /> |<br /> |-<br /> |Use centroid in photometry calculation?<br /> |Yes. Box is checked.<br /> |<br /> |-<br /> |Automatically snap aperture to centroid?<br /> |Yes. Box is checked.<br /> |<br /> |}<br /> <br /> [[File:APT-parameterss.png|300px|Screen capture of APT parameter settings.]]<br /> <br /> <br /> <br /> ==Photometry Assignment==<br /> <br /> [[5 APT Practice Sources]]<br /> <br /> ==The Big Picture==<br /> * Gather relevant and previously available photometry on NGC 281 (DONE, except Spitzer)<br /> * Gather images from previous surveys (DONE)<br /> * Herschel Images (DONE, but may be reprocessed)<br /> * Aperture Photometry<br /> * PSF photometry (Preliminary version, calibration missing).<br /> * Check Aperture photometry for bad sources, missed sources.<br /> * Create flags for all sources.<br /> * Check Aperture vs. PSF photometry. Select one or the other for each protostar.<br /> * Finalize Herschel photometry<br /> * Merge all photometry.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPs_Log&diff=11533 SHIPs Log 2013-03-28T22:13:21Z <p>Piper: /* Log */</p> <hr /> <div><br /> <br /> ==Telecons==<br /> <br /> ===Time===<br /> <br /> Weekly on Thursday, 3:30pm PST = 4:30pm MST = 5:30pm CST = 6:30pm EST<br /> <br /> ===Instructions===<br /> :Everyone calls the number<br /> ::'''866-524-3365'''<br /> ::then enter code (sent separately, check your e-mails).<br /> <br /> ===Log===<br /> :'''January'''<br /> ::[[Telecon011713 | Telecon 17-January-2013]]<br /> ::[[Telecon012413 | Telecon 24-January-2013]]<br /> ::[[Telecon013113 | Telecon 31-January-2013]]<br /> :'''February'''<br /> ::[[Telecon020713 | Telecon 07-February-2013]]<br /> ::[[Telecon021413 | Telecon 14-February-2013]]<br /> ::[[Telecon022113 | Telecon 21-February-2013]]<br /> :'''March'''<br /> ::[[Telecon030713 | Telecon 07-March-2013]]<br /> ::[[Telecon031413 | Telecon 14-March-2013]]<br /> ::[[Telecon031420 | Telecon 20-March-2013]]<br /> ::[[Telecon031428 | Telecon 28-March-2013]]<br /> <br /> ==Join.me==<br /> <br /> <br /> ==Skype==<br /> <br /> <br /> ==Polycom==</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPs_Log&diff=11532 SHIPs Log 2013-03-28T22:11:41Z <p>Piper: /* Log */</p> <hr /> <div><br /> <br /> ==Telecons==<br /> <br /> ===Time===<br /> <br /> Weekly on Thursday, 3:30pm PST = 4:30pm MST = 5:30pm CST = 6:30pm EST<br /> <br /> ===Instructions===<br /> :Everyone calls the number<br /> ::'''866-524-3365'''<br /> ::then enter code (sent separately, check your e-mails).<br /> <br /> ===Log===<br /> :'''January'''<br /> ::[[Telecon011713 | Telecon 17-January-2013]]<br /> ::[[Telecon012413 | Telecon 24-January-2013]]<br /> ::[[Telecon013113 | Telecon 31-January-2013]]<br /> :'''February'''<br /> ::[[Telecon020713 | Telecon 07-February-2013]]<br /> ::[[Telecon021413 | Telecon 14-February-2013]]<br /> ::[[Telecon022113 | Telecon 21-February-2013]]<br /> :'''March'''<br /> ::[[Telecon030713 | Telecon 07-March-2013]]<br /> ::[[Telecon031413 | Telecon 14-March-2013]]<br /> ::[[Telecon031420 | Telecon 20-March-2013]]<br /> ::[[Telecon031420 | Telecon 28-March-2013]]<br /> <br /> ==Join.me==<br /> <br /> <br /> ==Skype==<br /> <br /> <br /> ==Polycom==</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsCalendar&diff=11461 SHIPsCalendar 2013-03-13T23:09:09Z <p>Piper: </p> <hr /> <div>{| class=&quot;wikitable&quot;<br /> |-<br /> ! scope=&quot;col&quot;| Date(s)<br /> ! scope=&quot;col&quot;| Event and description.<br /> ! scope=&quot;col&quot;| Additional comments.<br /> |-<br /> |&lt;span style=&quot;color: Green;&quot;&gt;'''March'''&lt;/span&gt;<br /> |<br /> |<br /> |-<br /> |8<br /> |Proposal due date.<br /> |<br /> |-<br /> |11-15<br /> |Lynn Spring Break<br /> |<br /> |-<br /> |21<br /> |Peggy Out<br /> | may be able to pop in<br /> |-<br /> |23-31 <br /> |Melissa Spring Break<br /> |<br /> |-<br /> |&lt;span style=&quot;color: Green;&quot;&gt;'''March/April'''&lt;/span&gt;<br /> |<br /> |<br /> |-<br /> |28-7<br /> |Peggy Spring Break<br /> |<br /> |-<br /> |&lt;span style=&quot;color: Green;&quot;&gt;'''June'''&lt;/span&gt;<br /> |<br /> |<br /> |-<br /> |23-28<br /> |Summer Meeting of students, teacher, scientist and all other parties involved in SHIPs. Venue is Caltech campus.<br /> |Dedicated linked here.<br /> |}</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_07d.docx&diff=11444 File:SHIPS Proposal v03 07d.docx 2013-03-08T03:55:54Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11443 SHIPsProposal 2013-03-08T03:55:07Z <p>Piper: /* Current Version of the Proposal */</p> <hr /> <div><br /> ==Abstract==<br /> A short, one or two paragraph, summary of the main points:<br /> * Scientific goals of the proposal<br /> * Proposed observations<br /> <br /> <br /> ==Science Introduction and Context==<br /> <br /> Topics to consider when writing this section.<br /> *Background -- The broad picture.<br /> ** Why is star-formation important? (LYNN)<br /> ** What do we know about star-formation. We will likely trim this to suit our goals as the proposal matures? (LYNN)<br /> ** What are the big unknowns? (LYNN)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |NITARP pages<br /> |Our internal NITARP pages from Luisa, me and others. These are okay because they are one of your source of knowledge on the subject.<br /> |<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2007ARA%26A..45..565M McKee &amp; Osteriker (2007)]<br /> |Theory of Star Formation<br /> |Review article<br /> |Available for free via the arXiv link.<br /> |<br /> |-<br /> |[http://arxiv.org/pdf/astro-ph/0306595v2.pdf Larson (2003)]<br /> |The physics of star formation.<br /> |Another review with useful points to refer to.<br /> |<br /> |<br /> |}<br /> <br /> <br /> * This work<br /> ** What aspect of star formation will we address in this work? (PEGGY)<br /> ** What is star formation rate? (PEGGY)<br /> ** How does triggered star formation work? (PEGGY)<br /> ** How is triggered star formation and star formation rates useful in understanding star formation process? (PEGGY)<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1998ASPC..148..150E Elmegreen (1998)]<br /> |Observations and Theory of Dynamical Triggers for Star Formation<br /> |The paper by The author on triggered star-formation.<br /> |<br /> |[[File:Piper Proposal 20130303.docx | Piper Proposal 20130303]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |Discussion of efficiencies, rates and lifetimes.<br /> |<br /> |[[File:Piper Evans.docx | Piper Evan's braindump]]<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What target did we pick? (MELISSA)<br /> ** What do we know about NGC 281? (MELISSA)<br /> ** What is the evidence for triggered star formation in NGC 281? (MELISSA)<br /> ** What is the evidence for young stars in NGC 281? (MELISSA)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....114.1106M Megeath &amp; Wilson (1997)]<br /> |The NGC 281 west cluster. I. Star formation in photoevaporating clumps.<br /> |Establishes NGC 281 as a site of triggered SF.<br /> |[[File:Megeath97.pdf | PDF version]]<br /> |[[File:NITARP Proposal Booker.docx | Melissa's attempt at her section of the proposal]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....113.2116G Guetter &amp; Turner (1997)]<br /> |IC 1590, A Young Cluster Embedded in the Nebulosity of NGC 281<br /> |The seminal paper on NGC 281.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K Koenig et al (2012)]<br /> |Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions<br /> |Good use of WISE<br /> |Possibly picked up by Babar for our review<br /> |<br /> |-<br /> |[http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2012PASJ...64..107S&amp;db_key=AST&amp;nosetcookie=1 Sharma et al. (2012)]<br /> |Multiwavelength Study of the NGC 281 Region<br /> |<br /> |Picked up by Babar<br /> |<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What Observations do we propose to do? (CAROL)<br /> ** What/which properties of NGC 281 do we wish to study? (CAROL)<br /> ** What diagnostics will we use? (CAROL)<br /> ** How will these diagnostics tell us about our proposed goals/question to study? (CAROL)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012arXiv1212.1160F Fischer et al. (2012)]<br /> |Results from HOPS: A Multiwavelength Census of Orion Protostars<br /> |Studying protostars with Herschel<br /> |<br /> |[[File:Carol's Proposal Section.docx | ]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |How do we determine efficiencies and rates.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2008ApJS..179..249D Dunham et al. (2008)]<br /> |Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores<br /> |Why do we need data at Herschel wavelengths.<br /> |<br /> |<br /> |}<br /> <br /> ==Analysis plan== <br /> Specifics about data and what to do with the data.<br /> * How will the data be readied for this study? (Technical term: reduced, or processed).<br /> * Ancillary data<br /> ** Where will we get our data?<br /> ** How will we supplement our data? <br /> ** How will we combine data? <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> * What tools will we use?<br /> ** To work with the data<br /> ** To produce the diagnostic plots.<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> ==Educational/Outreach plan== <br /> * The education angle for the general public.<br /> * Implication for public education?<br /> * Press release?<br /> * Image release?<br /> <br /> ==Current Version of the Proposal==<br /> <br /> [[File:SHIPS_Proposal_v03_03b.docx| ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04.docx| ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04b.docx | Version 9:22pm PST 4-March ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04C.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_04C1.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05a.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05b.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05c.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05d.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_06a.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_06b.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_06C.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_06d.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_06d1.docx|Version with Lynn's Education Outreach]]<br /> <br /> [[File:SHIPS_Proposal_v03_07a.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_07b.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_07c.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_07d.docx]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_06C.docx&diff=11384 File:SHIPS Proposal v03 06C.docx 2013-03-06T18:03:02Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11383 SHIPsProposal 2013-03-06T18:02:30Z <p>Piper: /* Current Version of the Proposal */</p> <hr /> <div><br /> ==Abstract==<br /> A short, one or two paragraph, summary of the main points:<br /> * Scientific goals of the proposal<br /> * Proposed observations<br /> <br /> <br /> ==Science Introduction and Context==<br /> <br /> Topics to consider when writing this section.<br /> *Background -- The broad picture.<br /> ** Why is star-formation important? (LYNN)<br /> ** What do we know about star-formation. We will likely trim this to suit our goals as the proposal matures? (LYNN)<br /> ** What are the big unknowns? (LYNN)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |NITARP pages<br /> |Our internal NITARP pages from Luisa, me and others. These are okay because they are one of your source of knowledge on the subject.<br /> |<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2007ARA%26A..45..565M McKee &amp; Osteriker (2007)]<br /> |Theory of Star Formation<br /> |Review article<br /> |Available for free via the arXiv link.<br /> |<br /> |-<br /> |[http://arxiv.org/pdf/astro-ph/0306595v2.pdf Larson (2003)]<br /> |The physics of star formation.<br /> |Another review with useful points to refer to.<br /> |<br /> |<br /> |}<br /> <br /> <br /> * This work<br /> ** What aspect of star formation will we address in this work? (PEGGY)<br /> ** What is star formation rate? (PEGGY)<br /> ** How does triggered star formation work? (PEGGY)<br /> ** How is triggered star formation and star formation rates useful in understanding star formation process? (PEGGY)<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1998ASPC..148..150E Elmegreen (1998)]<br /> |Observations and Theory of Dynamical Triggers for Star Formation<br /> |The paper by The author on triggered star-formation.<br /> |<br /> |[[File:Piper Proposal 20130303.docx | Piper Proposal 20130303]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |Discussion of efficiencies, rates and lifetimes.<br /> |<br /> |[[File:Piper Evans.docx | Piper Evan's braindump]]<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What target did we pick? (MELISSA)<br /> ** What do we know about NGC 281? (MELISSA)<br /> ** What is the evidence for triggered star formation in NGC 281? (MELISSA)<br /> ** What is the evidence for young stars in NGC 281? (MELISSA)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....114.1106M Megeath &amp; Wilson (1997)]<br /> |The NGC 281 west cluster. I. Star formation in photoevaporating clumps.<br /> |Establishes NGC 281 as a site of triggered SF.<br /> |[[File:Megeath97.pdf | PDF version]]<br /> |[[File:NITARP Proposal Booker.docx | Melissa's attempt at her section of the proposal]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....113.2116G Guetter &amp; Turner (1997)]<br /> |IC 1590, A Young Cluster Embedded in the Nebulosity of NGC 281<br /> |The seminal paper on NGC 281.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K Koenig et al (2012)]<br /> |Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions<br /> |Good use of WISE<br /> |Possibly picked up by Babar for our review<br /> |<br /> |-<br /> |[http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2012PASJ...64..107S&amp;db_key=AST&amp;nosetcookie=1 Sharma et al. (2012)]<br /> |Multiwavelength Study of the NGC 281 Region<br /> |<br /> |Picked up by Babar<br /> |<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What Observations do we propose to do? (CAROL)<br /> ** What/which properties of NGC 281 do we wish to study? (CAROL)<br /> ** What diagnostics will we use? (CAROL)<br /> ** How will these diagnostics tell us about our proposed goals/question to study? (CAROL)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012arXiv1212.1160F Fischer et al. (2012)]<br /> |Results from HOPS: A Multiwavelength Census of Orion Protostars<br /> |Studying protostars with Herschel<br /> |<br /> |[[File:Carol's Proposal Section.docx | ]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |How do we determine efficiencies and rates.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2008ApJS..179..249D Dunham et al. (2008)]<br /> |Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores<br /> |Why do we need data at Herschel wavelengths.<br /> |<br /> |<br /> |}<br /> <br /> ==Analysis plan== <br /> Specifics about data and what to do with the data.<br /> * How will the data be readied for this study? (Technical term: reduced, or processed).<br /> * Ancillary data<br /> ** Where will we get our data?<br /> ** How will we supplement our data? <br /> ** How will we combine data? <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> * What tools will we use?<br /> ** To work with the data<br /> ** To produce the diagnostic plots.<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> ==Educational/Outreach plan== <br /> * The education angle for the general public.<br /> * Implication for public education?<br /> * Press release?<br /> * Image release?<br /> <br /> ==Current Version of the Proposal==<br /> <br /> [[File:SHIPS_Proposal_v03_03b.docx| ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04.docx| ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04b.docx | Version 9:22pm PST 4-March ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04C.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_04C1.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05a.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05b.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05c.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05d.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_06a.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_06b.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_06C.docx]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_05b.docx&diff=11372 File:SHIPS Proposal v03 05b.docx 2013-03-06T02:57:50Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11371 SHIPsProposal 2013-03-06T02:56:10Z <p>Piper: /* Current Version of the Proposal */</p> <hr /> <div><br /> ==Abstract==<br /> A short, one or two paragraph, summary of the main points:<br /> * Scientific goals of the proposal<br /> * Proposed observations<br /> <br /> <br /> ==Science Introduction and Context==<br /> <br /> Topics to consider when writing this section.<br /> *Background -- The broad picture.<br /> ** Why is star-formation important? (LYNN)<br /> ** What do we know about star-formation. We will likely trim this to suit our goals as the proposal matures? (LYNN)<br /> ** What are the big unknowns? (LYNN)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |NITARP pages<br /> |Our internal NITARP pages from Luisa, me and others. These are okay because they are one of your source of knowledge on the subject.<br /> |<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2007ARA%26A..45..565M McKee &amp; Osteriker (2007)]<br /> |Theory of Star Formation<br /> |Review article<br /> |Available for free via the arXiv link.<br /> |<br /> |-<br /> |[http://arxiv.org/pdf/astro-ph/0306595v2.pdf Larson (2003)]<br /> |The physics of star formation.<br /> |Another review with useful points to refer to.<br /> |<br /> |<br /> |}<br /> <br /> <br /> * This work<br /> ** What aspect of star formation will we address in this work? (PEGGY)<br /> ** What is star formation rate? (PEGGY)<br /> ** How does triggered star formation work? (PEGGY)<br /> ** How is triggered star formation and star formation rates useful in understanding star formation process? (PEGGY)<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1998ASPC..148..150E Elmegreen (1998)]<br /> |Observations and Theory of Dynamical Triggers for Star Formation<br /> |The paper by The author on triggered star-formation.<br /> |<br /> |[[File:Piper Proposal 20130303.docx | Piper Proposal 20130303]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |Discussion of efficiencies, rates and lifetimes.<br /> |<br /> |[[File:Piper Evans.docx | Piper Evan's braindump]]<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What target did we pick? (MELISSA)<br /> ** What do we know about NGC 281? (MELISSA)<br /> ** What is the evidence for triggered star formation in NGC 281? (MELISSA)<br /> ** What is the evidence for young stars in NGC 281? (MELISSA)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....114.1106M Megeath &amp; Wilson (1997)]<br /> |The NGC 281 west cluster. I. Star formation in photoevaporating clumps.<br /> |Establishes NGC 281 as a site of triggered SF.<br /> |[[File:Megeath97.pdf | PDF version]]<br /> |[[File:NITARP Proposal Booker.docx | Melissa's attempt at her section of the proposal]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....113.2116G Guetter &amp; Turner (1997)]<br /> |IC 1590, A Young Cluster Embedded in the Nebulosity of NGC 281<br /> |The seminal paper on NGC 281.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K Koenig et al (2012)]<br /> |Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions<br /> |Good use of WISE<br /> |Possibly picked up by Babar for our review<br /> |<br /> |-<br /> |[http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2012PASJ...64..107S&amp;db_key=AST&amp;nosetcookie=1 Sharma et al. (2012)]<br /> |Multiwavelength Study of the NGC 281 Region<br /> |<br /> |Picked up by Babar<br /> |<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What Observations do we propose to do? (CAROL)<br /> ** What/which properties of NGC 281 do we wish to study? (CAROL)<br /> ** What diagnostics will we use? (CAROL)<br /> ** How will these diagnostics tell us about our proposed goals/question to study? (CAROL)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012arXiv1212.1160F Fischer et al. (2012)]<br /> |Results from HOPS: A Multiwavelength Census of Orion Protostars<br /> |Studying protostars with Herschel<br /> |<br /> |[[File:Carol's Proposal Section.docx | ]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |How do we determine efficiencies and rates.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2008ApJS..179..249D Dunham et al. (2008)]<br /> |Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores<br /> |Why do we need data at Herschel wavelengths.<br /> |<br /> |<br /> |}<br /> <br /> ==Analysis plan== <br /> Specifics about data and what to do with the data.<br /> * How will the data be readied for this study? (Technical term: reduced, or processed).<br /> * Ancillary data<br /> ** Where will we get our data?<br /> ** How will we supplement our data? <br /> ** How will we combine data? <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> * What tools will we use?<br /> ** To work with the data<br /> ** To produce the diagnostic plots.<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> ==Educational/Outreach plan== <br /> * The education angle for the general public.<br /> * Implication for public education?<br /> * Press release?<br /> * Image release?<br /> <br /> ==Current Version of the Proposal==<br /> <br /> [[File:SHIPS_Proposal_v03_03b.docx| ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04.docx| ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04b.docx | Version 9:22pm PST 4-March ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04C.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_04C1.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05a.docx]]<br /> <br /> [[File:SHIPS_Proposal_v03_05b.docx]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_04C.docx&diff=11363 File:SHIPS Proposal v03 04C.docx 2013-03-05T07:10:12Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11362 SHIPsProposal 2013-03-05T07:09:25Z <p>Piper: /* Current Version of the Proposal */</p> <hr /> <div><br /> ==Abstract==<br /> A short, one or two paragraph, summary of the main points:<br /> * Scientific goals of the proposal<br /> * Proposed observations<br /> <br /> <br /> ==Science Introduction and Context==<br /> <br /> Topics to consider when writing this section.<br /> *Background -- The broad picture.<br /> ** Why is star-formation important? (LYNN)<br /> ** What do we know about star-formation. We will likely trim this to suit our goals as the proposal matures? (LYNN)<br /> ** What are the big unknowns? (LYNN)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |NITARP pages<br /> |Our internal NITARP pages from Luisa, me and others. These are okay because they are one of your source of knowledge on the subject.<br /> |<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2007ARA%26A..45..565M McKee &amp; Osteriker (2007)]<br /> |Theory of Star Formation<br /> |Review article<br /> |Available for free via the arXiv link.<br /> |<br /> |-<br /> |[http://arxiv.org/pdf/astro-ph/0306595v2.pdf Larson (2003)]<br /> |The physics of star formation.<br /> |Another review with useful points to refer to.<br /> |<br /> |<br /> |}<br /> <br /> <br /> * This work<br /> ** What aspect of star formation will we address in this work? (PEGGY)<br /> ** What is star formation rate? (PEGGY)<br /> ** How does triggered star formation work? (PEGGY)<br /> ** How is triggered star formation and star formation rates useful in understanding star formation process? (PEGGY)<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1998ASPC..148..150E Elmegreen (1998)]<br /> |Observations and Theory of Dynamical Triggers for Star Formation<br /> |The paper by The author on triggered star-formation.<br /> |<br /> |[[File:Piper Proposal 20130303.docx | Piper Proposal 20130303]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |Discussion of efficiencies, rates and lifetimes.<br /> |<br /> |[[File:Piper Evans.docx | Piper Evan's braindump]]<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What target did we pick? (MELISSA)<br /> ** What do we know about NGC 281? (MELISSA)<br /> ** What is the evidence for triggered star formation in NGC 281? (MELISSA)<br /> ** What is the evidence for young stars in NGC 281? (MELISSA)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....114.1106M Megeath &amp; Wilson (1997)]<br /> |The NGC 281 west cluster. I. Star formation in photoevaporating clumps.<br /> |Establishes NGC 281 as a site of triggered SF.<br /> |[[File:Megeath97.pdf | PDF version]]<br /> |[[File:NITARP Proposal Booker.docx | Melissa's attempt at her section of the proposal]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....113.2116G Guetter &amp; Turner (1997)]<br /> |IC 1590, A Young Cluster Embedded in the Nebulosity of NGC 281<br /> |The seminal paper on NGC 281.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K Koenig et al (2012)]<br /> |Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions<br /> |Good use of WISE<br /> |Possibly picked up by Babar for our review<br /> |<br /> |-<br /> |[http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2012PASJ...64..107S&amp;db_key=AST&amp;nosetcookie=1 Sharma et al. (2012)]<br /> |Multiwavelength Study of the NGC 281 Region<br /> |<br /> |Picked up by Babar<br /> |<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What Observations do we propose to do? (CAROL)<br /> ** What/which properties of NGC 281 do we wish to study? (CAROL)<br /> ** What diagnostics will we use? (CAROL)<br /> ** How will these diagnostics tell us about our proposed goals/question to study? (CAROL)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012arXiv1212.1160F Fischer et al. (2012)]<br /> |Results from HOPS: A Multiwavelength Census of Orion Protostars<br /> |Studying protostars with Herschel<br /> |<br /> |[[File:Carol's Proposal Section.docx | ]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |How do we determine efficiencies and rates.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2008ApJS..179..249D Dunham et al. (2008)]<br /> |Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores<br /> |Why do we need data at Herschel wavelengths.<br /> |<br /> |<br /> |}<br /> <br /> ==Analysis plan== <br /> Specifics about data and what to do with the data.<br /> * How will the data be readied for this study? (Technical term: reduced, or processed).<br /> * Ancillary data<br /> ** Where will we get our data?<br /> ** How will we supplement our data? <br /> ** How will we combine data? <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> * What tools will we use?<br /> ** To work with the data<br /> ** To produce the diagnostic plots.<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> ==Educational/Outreach plan== <br /> * The education angle for the general public.<br /> * Implication for public education?<br /> * Press release?<br /> * Image release?<br /> <br /> ==Current Version of the Proposal==<br /> <br /> [[File:SHIPS_Proposal_v03_03b.docx| ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04.docx| ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04b.docx | Version 9:22pm PST 4-March ]]<br /> <br /> [[File:SHIPS_Proposal_v03_04C.docx]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Piper_Proposal_20130303.docx&diff=11349 File:Piper Proposal 20130303.docx 2013-03-04T01:15:01Z <p>Piper: uploaded a new version of &amp;quot;File:Piper Proposal 20130303.docx&amp;quot;</p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Piper_Proposal_20130303.docx&diff=11348 File:Piper Proposal 20130303.docx 2013-03-04T01:09:00Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11347 SHIPsProposal 2013-03-04T01:07:55Z <p>Piper: /* Science Introduction and Context */</p> <hr /> <div><br /> ==Abstract==<br /> A short, one or two paragraph, summary of the main points:<br /> * Scientific goals of the proposal<br /> * Proposed observations<br /> <br /> <br /> ==Science Introduction and Context==<br /> <br /> Topics to consider when writing this section.<br /> *Background -- The broad picture.<br /> ** Why is star-formation important? (LYNN)<br /> ** What do we know about star-formation. We will likely trim this to suit our goals as the proposal matures? (LYNN)<br /> ** What are the big unknowns? (LYNN)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |NITARP pages<br /> |Our internal NITARP pages from Luisa, me and others. These are okay because they are one of your source of knowledge on the subject.<br /> |<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2007ARA%26A..45..565M McKee &amp; Osteriker (2007)]<br /> |Theory of Star Formation<br /> |Review article<br /> |Available for free via the arXiv link.<br /> |<br /> |-<br /> |[http://arxiv.org/pdf/astro-ph/0306595v2.pdf Larson (2003)]<br /> |The physics of star formation.<br /> |Another review with useful points to refer to.<br /> |<br /> |<br /> |}<br /> <br /> <br /> * This work<br /> ** What aspect of star formation will we address in this work? (PEGGY)<br /> ** What is star formation rate? (PEGGY)<br /> ** How does triggered star formation work? (PEGGY)<br /> ** How is triggered star formation and star formation rates useful in understanding star formation process? (PEGGY)<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1998ASPC..148..150E Elmegreen (1998)]<br /> |Observations and Theory of Dynamical Triggers for Star Formation<br /> |The paper by The author on triggered star-formation.<br /> |<br /> |[[File:Piper Proposal 20130303.docx | Piper Proposal 20130303]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |Discussion of efficiencies, rates and lifetimes.<br /> |<br /> |[[File:Piper Evans.docx | Piper Evan's braindump]]<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What target did we pick? (MELISSA)<br /> ** What do we know about NGC 281? (MELISSA)<br /> ** What is the evidence for triggered star formation in NGC 281? (MELISSA)<br /> ** What is the evidence for young stars in NGC 281? (MELISSA)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....114.1106M Megeath &amp; Wilson (1997)]<br /> |The NGC 281 west cluster. I. Star formation in photoevaporating clumps.<br /> |Establishes NGC 281 as a site of triggered SF.<br /> |[[File:Megeath97.pdf | PDF version]]<br /> |[[File:NITARP Proposal Booker.docx | Melissa's attempt at her section of the proposal]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....113.2116G Guetter &amp; Turner (1997)]<br /> |IC 1590, A Young Cluster Embedded in the Nebulosity of NGC 281<br /> |The seminal paper on NGC 281.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K Koenig et al (2012)]<br /> |Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions<br /> |Good use of WISE<br /> |Possibly picked up by Babar for our review<br /> |<br /> |-<br /> |[http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2012PASJ...64..107S&amp;db_key=AST&amp;nosetcookie=1 Sharma et al. (2012)]<br /> |Multiwavelength Study of the NGC 281 Region<br /> |<br /> |Picked up by Babar<br /> |<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What Observations do we propose to do? (CAROL)<br /> ** What/which properties of NGC 281 do we wish to study? (CAROL)<br /> ** What diagnostics will we use? (CAROL)<br /> ** How will these diagnostics tell us about our proposed goals/question to study? (CAROL)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012arXiv1212.1160F Fischer et al. (2012)]<br /> |Results from HOPS: A Multiwavelength Census of Orion Protostars<br /> |Studying protostars with Herschel<br /> |<br /> |[[File:Carol's Proposal Section.docx | ]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |How do we determine efficiencies and rates.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2008ApJS..179..249D Dunham et al. (2008)]<br /> |Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores<br /> |Why do we need data at Herschel wavelengths.<br /> |<br /> |<br /> |}<br /> <br /> ==Analysis plan== <br /> Specifics about data and what to do with the data.<br /> * How will the data be readied for this study? (Technical term: reduced, or processed).<br /> * Ancillary data<br /> ** Where will we get our data?<br /> ** How will we supplement our data? <br /> ** How will we combine data? <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> * What tools will we use?<br /> ** To work with the data<br /> ** To produce the diagnostic plots.<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> ==Educational/Outreach plan== <br /> * The education angle for the general public.<br /> * Implication for public education?<br /> * Press release?<br /> * Image release?<br /> <br /> ==Current Version of the Proposal==<br /> <br /> [[File:SHIPS_Proposal_v03_03b.docx| ]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Piper_Proposal_20130302.docx&diff=11336 File:Piper Proposal 20130302.docx 2013-03-03T07:48:47Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11335 SHIPsProposal 2013-03-03T07:47:07Z <p>Piper: /* Science Introduction and Context */</p> <hr /> <div><br /> ==Abstract==<br /> A short, one or two paragraph, summary of the main points:<br /> * Scientific goals of the proposal<br /> * Proposed observations<br /> <br /> <br /> ==Science Introduction and Context==<br /> <br /> Topics to consider when writing this section.<br /> *Background -- The broad picture.<br /> ** Why is star-formation important? (LYNN)<br /> ** What do we know about star-formation. We will likely trim this to suit our goals as the proposal matures? (LYNN)<br /> ** What are the big unknowns? (LYNN)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |NITARP pages<br /> |Our internal NITARP pages from Luisa, me and others. These are okay because they are one of your source of knowledge on the subject.<br /> |<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2007ARA%26A..45..565M McKee &amp; Osteriker (2007)]<br /> |Theory of Star Formation<br /> |Review article<br /> |Available for free via the arXiv link.<br /> |<br /> |-<br /> |[http://arxiv.org/pdf/astro-ph/0306595v2.pdf Larson (2003)]<br /> |The physics of star formation.<br /> |Another review with useful points to refer to.<br /> |<br /> |<br /> |}<br /> <br /> <br /> * This work<br /> ** What aspect of star formation will we address in this work? (PEGGY)<br /> ** What is star formation rate? (PEGGY)<br /> ** How does triggered star formation work? (PEGGY)<br /> ** How is triggered star formation and star formation rates useful in understanding star formation process? (PEGGY)<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1998ASPC..148..150E Elmegreen (1998)]<br /> |Observations and Theory of Dynamical Triggers for Star Formation<br /> |The paper by The author on triggered star-formation.<br /> |<br /> |[[File:Piper Proposal 20130302.docx | Piper Proposal 20130302]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |Discussion of efficiencies, rates and lifetimes.<br /> |<br /> |[[File:Piper Evans.docx | Piper Evan's braindump]]<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What target did we pick? (MELISSA)<br /> ** What do we know about NGC 281? (MELISSA)<br /> ** What is the evidence for triggered star formation in NGC 281? (MELISSA)<br /> ** What is the evidence for young stars in NGC 281? (MELISSA)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....114.1106M Megeath &amp; Wilson (1997)]<br /> |The NGC 281 west cluster. I. Star formation in photoevaporating clumps.<br /> |Establishes NGC 281 as a site of triggered SF.<br /> |[[File:Megeath97.pdf | PDF version]]<br /> |[[File:NITARP Proposal Booker.docx | Melissa's attempt at her section of the proposal]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....113.2116G Guetter &amp; Turner (1997)]<br /> |IC 1590, A Young Cluster Embedded in the Nebulosity of NGC 281<br /> |The seminal paper on NGC 281.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K Koenig et al (2012)]<br /> |Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions<br /> |Good use of WISE<br /> |Possibly picked up by Babar for our review<br /> |<br /> |-<br /> |[http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2012PASJ...64..107S&amp;db_key=AST&amp;nosetcookie=1 Sharma et al. (2012)]<br /> |Multiwavelength Study of the NGC 281 Region<br /> |<br /> |Picked up by Babar<br /> |<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What Observations do we propose to do? (CAROL)<br /> ** What/which properties of NGC 281 do we wish to study? (CAROL)<br /> ** What diagnostics will we use? (CAROL)<br /> ** How will these diagnostics tell us about our proposed goals/question to study? (CAROL)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012arXiv1212.1160F Fischer et al. (2012)]<br /> |Results from HOPS: A Multiwavelength Census of Orion Protostars<br /> |Studying protostars with Herschel<br /> |<br /> |[[File:Carol's Proposal Section.docx | ]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |How do we determine efficiencies and rates.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2008ApJS..179..249D Dunham et al. (2008)]<br /> |Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores<br /> |Why do we need data at Herschel wavelengths.<br /> |<br /> |<br /> |}<br /> <br /> ==Analysis plan== <br /> Specifics about data and what to do with the data.<br /> * How will the data be readied for this study? (Technical term: reduced, or processed).<br /> * Ancillary data<br /> ** Where will we get our data?<br /> ** How will we supplement our data? <br /> ** How will we combine data? <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> * What tools will we use?<br /> ** To work with the data<br /> ** To produce the diagnostic plots.<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> ==Educational/Outreach plan== <br /> * The education angle for the general public.<br /> * Implication for public education?<br /> * Press release?<br /> * Image release?</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Piper_Elmegreen_Evans.docx&diff=11287 File:Piper Elmegreen Evans.docx 2013-02-25T02:54:05Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11286 SHIPsProposal 2013-02-25T02:53:39Z <p>Piper: </p> <hr /> <div><br /> ==Abstract==<br /> A short, one or two paragraph, summary of the main points:<br /> * Scientific goals of the proposal<br /> * Proposed observations<br /> <br /> <br /> ==Science Introduction and Context==<br /> <br /> Topics to consider when writing this section.<br /> *Background -- The broad picture.<br /> ** Why is star-formation important? (LYNN)<br /> ** What do we know about star-formation. We will likely trim this to suit our goals as the proposal matures? (LYNN)<br /> ** What are the big unknowns? (LYNN)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |NITARP pages<br /> |Our internal NITARP pages from Luisa, me and others. These are okay because they are one of your source of knowledge on the subject.<br /> |<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2007ARA%26A..45..565M McKee &amp; Osteriker (2007)]<br /> |Theory of Star Formation<br /> |Review article<br /> |Available for free via the arXiv link.<br /> |<br /> |-<br /> |[http://arxiv.org/pdf/astro-ph/0306595v2.pdf Larson (2003)]<br /> |The physics of star formation.<br /> |Another review with useful points to refer to.<br /> |<br /> |<br /> |}<br /> <br /> <br /> * This work<br /> ** What aspect of star formation will we address in this work? (PEGGY)<br /> ** What is star formation rate? (PEGGY)<br /> ** How does triggered star formation work? (PEGGY)<br /> ** How is triggered star formation and star formation rates useful in understanding star formation process? (PEGGY)<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1998ASPC..148..150E Elmegreen (1998)]<br /> |Observations and Theory of Dynamical Triggers for Star Formation<br /> |The paper by The author on triggered star-formation.<br /> |<br /> |[[File:Piper Elmegreen Evans.docx | Piper braindump both papers]]<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |Discussion of efficiencies, rates and lifetimes.<br /> |<br /> |[[File:Piper Evans.docx | Piper Evan's braindump]]<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What target did we pick? (MELISSA)<br /> ** What do we know about NGC 281? (MELISSA)<br /> ** What is the evidence for triggered star formation in NGC 281? (MELISSA)<br /> ** What is the evidence for young stars in NGC 281? (MELISSA)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....114.1106M Megeath &amp; Wilson (1997)]<br /> |The NGC 281 west cluster. I. Star formation in photoevaporating clumps.<br /> |Establishes NGC 281 as a site of triggered SF.<br /> |[[File:Megeath97.pdf | PDF version]]<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....113.2116G Guetter &amp; Turner (1997)]<br /> |IC 1590, A Young Cluster Embedded in the Nebulosity of NGC 281<br /> |The seminal paper on NGC 281.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K Koenig et al (2012)]<br /> |Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions<br /> |Good use of WISE<br /> |Possibly picked up by Babar for our review<br /> |<br /> |-<br /> |[http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2012PASJ...64..107S&amp;db_key=AST&amp;nosetcookie=1 Sharma et al. (2012)]<br /> |Multiwavelength Study of the NGC 281 Region<br /> |<br /> |Picked up by Babar<br /> |<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What Observations do we propose to do? (CAROL)<br /> ** What/which properties of NGC 281 do we wish to study? (CAROL)<br /> ** What diagnostics will we use? (CAROL)<br /> ** How will these diagnostics tell us about our proposed goals/question to study? (CAROL)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012arXiv1212.1160F Fischer et al. (2012)]<br /> |Results from HOPS: A Multiwavelength Census of Orion Protostars<br /> |Studying protostars with Herschel<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |How do we determine efficiencies and rates.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2008ApJS..179..249D Dunham et al. (2008)]<br /> |Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores<br /> |Why do we need data at Herschel wavelengths.<br /> |<br /> |<br /> |}<br /> <br /> ==Analysis plan== <br /> Specifics about data and what to do with the data.<br /> * How will the data be readied for this study? (Technical term: reduced, or processed).<br /> * Ancillary data<br /> ** Where will we get our data?<br /> ** How will we supplement our data? <br /> ** How will we combine data? <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> * What tools will we use?<br /> ** To work with the data<br /> ** To produce the diagnostic plots.<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> ==Educational/Outreach plan== <br /> * The education angle for the general public.<br /> * Implication for public education?<br /> * Press release?<br /> * Image release?</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Piper_Evans.docx&diff=11181 File:Piper Evans.docx 2013-02-18T18:10:25Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11180 SHIPsProposal 2013-02-18T18:10:04Z <p>Piper: /* Science Introduction and Context */</p> <hr /> <div><br /> ==Abstract==<br /> A short, one or two paragraph, summary of the main points:<br /> * Scientific goals of the proposal<br /> * Proposed observations<br /> <br /> <br /> ==Science Introduction and Context==<br /> <br /> Topics to consider when writing this section.<br /> *Background -- The broad picture.<br /> ** Why is star-formation important? (LYNN)<br /> ** What do we know about star-formation. We will likely trim this to suit our goals as the proposal matures? (LYNN)<br /> ** What are the big unknowns? (LYNN)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |NITARP pages<br /> |Our internal NITARP pages from Luisa, me and others. These are okay because they are one of your source of knowledge on the subject.<br /> |<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2007ARA%26A..45..565M McKee &amp; Osteriker (2007)]<br /> |Theory of Star Formation<br /> |Review article<br /> |Available for free via the arXiv link.<br /> |<br /> |-<br /> |[http://arxiv.org/pdf/astro-ph/0306595v2.pdf Larson (2003)]<br /> |The physics of star formation.<br /> |Another review with useful points to refer to.<br /> |<br /> |<br /> |}<br /> <br /> <br /> * This work<br /> ** What aspect of star formation will we address in this work? (PEGGY)<br /> ** What is star formation rate? (PEGGY)<br /> ** How does triggered star formation work? (PEGGY)<br /> ** How is triggered star formation and star formation rates useful in understanding star formation process? (PEGGY)<br /> <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1998ASPC..148..150E Elmegreen (1998)]<br /> |Observations and Theory of Dynamical Triggers for Star Formation<br /> |The paper by The author on triggered star-formation.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |Discussion of efficiencies, rates and lifetimes.<br /> |<br /> |[[File:Piper Evans.docx | Piper Evan's braindump]]<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What target did we pick? (MELISSA)<br /> ** What do we know about NGC 281? (MELISSA)<br /> ** What is the evidence for triggered star formation in NGC 281? (MELISSA)<br /> ** What is the evidence for young stars in NGC 281? (MELISSA)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....114.1106M Megeath &amp; Wilson (1997)]<br /> |The NGC 281 west cluster. I. Star formation in photoevaporating clumps.<br /> |Establishes NGC 281 as a site of triggered SF.<br /> |[[File:Megeath97.pdf | PDF version]]<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/1997AJ....113.2116G Guetter &amp; Turner (1997)]<br /> |IC 1590, A Young Cluster Embedded in the Nebulosity of NGC 281<br /> |The seminal paper on NGC 281.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012ApJ...744..130K Koenig et al (2012)]<br /> |Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions<br /> |Good use of WISE<br /> |Possibly picked up by Babar for our review<br /> |<br /> |-<br /> |[http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2012PASJ...64..107S&amp;db_key=AST&amp;nosetcookie=1 Sharma et al. (2012)]<br /> |Multiwavelength Study of the NGC 281 Region<br /> |<br /> |Picked up by Babar<br /> |<br /> |}<br /> <br /> <br /> * This work (cont.)<br /> ** What Observations do we propose to do? (CAROL)<br /> ** What/which properties of NGC 281 do we wish to study? (CAROL)<br /> ** What diagnostics will we use? (CAROL)<br /> ** How will these diagnostics tell us about our proposed goals/question to study? (CAROL)<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2012arXiv1212.1160F Fischer et al. (2012)]<br /> |Results from HOPS: A Multiwavelength Census of Orion Protostars<br /> |Studying protostars with Herschel<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2009ApJS..181..321E Evans et al. (2009)]<br /> |The Spitzer c2d Legacy Results: Star-Formation Rates and Efficiencies; Evolution and Lifetimes<br /> |How do we determine efficiencies and rates.<br /> |<br /> |<br /> |-<br /> |[http://adsabs.harvard.edu/abs/2008ApJS..179..249D Dunham et al. (2008)]<br /> |Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores<br /> |Why do we need data at Herschel wavelengths.<br /> |<br /> |<br /> |}<br /> <br /> ==Analysis plan== <br /> Specifics about data and what to do with the data.<br /> * How will the data be readied for this study? (Technical term: reduced, or processed).<br /> * Ancillary data<br /> ** Where will we get our data?<br /> ** How will we supplement our data? <br /> ** How will we combine data? <br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> * What tools will we use?<br /> ** To work with the data<br /> ** To produce the diagnostic plots.<br /> <br /> {| class=&quot;wikitable&quot;<br /> |+Reading List<br /> |-<br /> ! scope=&quot;col&quot;| Paper<br /> ! scope=&quot;col&quot;| Title<br /> ! scope=&quot;col&quot;| Description<br /> ! scope=&quot;col&quot;| Comments<br /> ! scope=&quot;coI&quot;| Assignment<br /> |-<br /> |<br /> |<br /> |<br /> |<br /> |<br /> |}<br /> <br /> <br /> ==Educational/Outreach plan== <br /> * The education angle for the general public.<br /> * Implication for public education?<br /> * Press release?<br /> * Image release?</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10780 2 Micron All Sky Survey - 2MASS 2013-01-18T00:17:11Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky Survey''' is an all sky survey in the 2 micron range that used both northern and southern hemisphere 1.3 meter telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog which were resolved<br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html 2MASS Picture of the Week]'''<br /> <br /> [[File:2 Mass POW Orion.jpg|400px|thumb|center| Orion - Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]<br /> <br /> There is a really nice image out there somewhere that shows where 2MASS falls on the spectrum that I will try to find.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10779 2 Micron All Sky Survey - 2MASS 2013-01-18T00:14:58Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky Survey''' is an all sky survey in the 2 micron range that used both northern and southern hemisphere 1.3 meter telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog, which are within our galaxy<br /> *1.6 million sources in the extended source catalog which means there are an additional 1.6 million things out there but couldn't be resolved with 2MASS <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html 2MASS Picture of the Week]'''<br /> <br /> [[File:2 Mass POW Orion.jpg|400px|thumb|center| Orion - Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]<br /> <br /> There is a really nice image out there somewhere that shows where 2MASS falls on the spectrum that I will try to find.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10778 2 Micron All Sky Survey - 2MASS 2013-01-18T00:13:56Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky Survey''' is an all sky survey in the 2 micron range that used both northern and southern hemisphere 1.3 meter telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog which means there are an additional 1.6 million things out there but couldn't be resolved with 2MASS <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html 2MASS Picture of the Week]'''<br /> <br /> [[File:2 Mass POW Orion.jpg|400px|thumb|center| Orion - Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]<br /> <br /> There is a really nice image out there somewhere that shows where 2MASS falls on the spectrum that I will try to find.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10776 2 Micron All Sky Survey - 2MASS 2013-01-18T00:06:54Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky Survey''' is an all sky survey in the 2 micron range that used both northern and southern hemisphere 1.3 meter telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog (I don't know what this means yet:) <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html/ There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html 2MASS Picture of the Week]'''<br /> <br /> [[File:2 Mass POW Orion.jpg|400px|thumb|center| Orion - Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]<br /> <br /> There is a really nice image out there somewhere that shows where 2MASS falls on the spectrum that I will try to find.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10739 2 Micron All Sky Survey - 2MASS 2013-01-17T04:27:52Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky Survey''' is an all sky survey in the 2 micron range that used both northern and southern hemisphere 1.3 meter telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog (I don't know what this means yet:) <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html/ There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html/ 2MASS Picture of the Week]'''<br /> <br /> [[File:2 Mass POW Orion.jpg|400px|thumb|center| Orion - Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]<br /> <br /> There is a really nice image out there somewhere that shows where 2MASS falls on the spectrum that I will try to find.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10738 2 Micron All Sky Survey - 2MASS 2013-01-17T04:22:55Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky''' survey is an all sky survey in the 2 micron range that used both northern and southern hemisphere 1.3 meter telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog (I don't know what this means yet:) <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html/ There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html/ 2MASS Picture of the Week]'''<br /> <br /> [[File:2 Mass POW Orion.jpg|400px|thumb|center| Orion - Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]<br /> <br /> There is a really nice image out there somewhere that shows where 2MASS falls on the spectrum that I will try to find.</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:2_Mass_POW_Orion.jpg&diff=10737 File:2 Mass POW Orion.jpg 2013-01-17T04:19:13Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10736 2 Micron All Sky Survey - 2MASS 2013-01-17T04:18:57Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky''' survey is an all sky survey in the 2 micron range that used both northern and southern hemisphere telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog (I don't know what this means yet:) <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html/ There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html/ 2MASS Picture of the Week]'''<br /> <br /> [[File:2 Mass POW Orion.jpg|400px|thumb|center| Orion - Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10735 2 Micron All Sky Survey - 2MASS 2013-01-17T04:17:43Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky''' survey is an all sky survey in the 2 micron range that used both northern and southern hemisphere telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog (I don't know what this means yet:) <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html/ There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html/ 2MASS Picture of the Week]'''<br /> [[File:2 Mass POW Orion.jpg|400px|thumb|right| Orion - Atlas Image courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10734 2 Micron All Sky Survey - 2MASS 2013-01-17T04:17:06Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky''' survey is an all sky survey in the 2 micron range that used both northern and southern hemisphere telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog (I don't know what this means yet:) <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html/ There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[[http://www.ipac.caltech.edu/2mass/gallery/pow.html/ 2MASS Picture of the Week]]'''<br /> [[File:2 Mass POW Orion.jpg|400px|thumb|right| Orion - Atlas Image [or Atlas Image mosaic] courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10733 2 Micron All Sky Survey - 2MASS 2013-01-17T04:16:43Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky''' survey is an all sky survey in the 2 micron range that used both northern and southern hemisphere telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|300px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|400px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' &lt;BR&gt;&lt;BR&gt;<br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog (I don't know what this means yet:) <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/overview/about2mass.html/ There is a lot more info here at the IPAC 2MASS page]'''<br /> <br /> But I have not read through it all and I '''still''' don't know why its '''J, H, K''' which is '''not''' the order of the alphabet and it really bugs me!<br /> <br /> <br /> '''[http://www.ipac.caltech.edu/2mass/gallery/pow.html/ 2MASS Picture of the Week]'''<br /> [[File:2 Mass POW Orion.jpg|400px|thumb|right| Orion - Atlas Image [or Atlas Image mosaic] courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF]]</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10731 2 Micron All Sky Survey - 2MASS 2013-01-17T03:40:33Z <p>Piper: </p> <hr /> <div>'''2MASS''' the '''2 Micron All Sky''' survey is an all sky survey in the 2 micron range that used both northern and southern hemisphere telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> According to wikipedia, the goals of 2MASS were to look into the areas of the Milky way hidden in visible light, to look for brown dwarfs and low mass stars and to create a catalog of all of the galaxies and stars 2MASS could detect.<br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|200px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|200px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' <br /> <br /> *wavelengths J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR)<br /> *over 500 million sources in the point source catalog<br /> *1.6 million sources in the extended source catalog (I don't know what this means yet:) <br /> *catalogs publicly available.<br /> <br /> <br /> <br /> <br /> <br /> Add where it fits with other scopes and what it is typically used for???</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:2_Mass_south.jpg&diff=10727 File:2 Mass south.jpg 2013-01-17T03:22:25Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:2_Mass_north.jpg&diff=10725 File:2 Mass north.jpg 2013-01-17T03:20:35Z <p>Piper: </p> <hr /> <div></div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10724 2 Micron All Sky Survey - 2MASS 2013-01-17T03:20:14Z <p>Piper: </p> <hr /> <div>2MASS is an all sky survey that used both northern and southern hemisphere telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> <br /> <br /> [[File:2 Mass north.jpg|200px|thumb|left|2MASS North Mt. Hopkins and M57 from IPAC image gallery]][[File:2 Mass south.jpg|200px|thumb|right|2MASS South Cerro Tololo CTIO Chili from IPAC image gallery]]<br /> <br /> '''[http://skynet.unc.edu/promptcam/ Click here to see a live webcam pointed at 2MASS south via SKYNET remote network.]''' <br /> <br /> <br /> Wavelengths around 2 microns, J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR) were used in this survey which produced over 500 million sources in the point source catalog and 1.6 million sources in the extended source catalog (I don't know what this means yet:) These catalogs are publicly available.<br /> <br /> Probabley better in bullet form.<br /> <br /> Add pics of actual scopes.<br /> <br /> Add where it fits with other scopes and what it is typically used for???</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10723 2 Micron All Sky Survey - 2MASS 2013-01-17T03:13:12Z <p>Piper: </p> <hr /> <div>2MASS is an all sky survey that used both northern and southern hemisphere telescopes to cover the whole sky from 1997 through 2001 with a final post processing release in 2003. <br /> <br /> <br /> <br /> 2MASS used telescopes in both the northern and southern hemisphers to cover the whole sky. Here is a composite photo of the the Northern 2MASS telescope at Mt. Hopkins and southern hemisphere (Cerro Tololo/CTIO, Chile) ground based telescopes to obtain data from the whole sky. You can actually see a live webcam pointed at the Chile site using [http://skynet.unc.edu/promptcam/ this link to the Skynet remote telescope network.] Wavelengths around 2 microns, J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR) were used in this survey which produced over 500 million sources in the point source catalog and 1.6 million sources in the extended source catalog (I don't know what this means yet:) These catalogs are publicly available.<br /> <br /> Probabley better in bullet form.<br /> <br /> Add pics of actual scopes.<br /> <br /> Add where it fits with other scopes and what it is typically used for???</div> Piper https://vmcoolwiki.ipac.caltech.edu/index.php?title=2_Micron_All_Sky_Survey_-_2MASS&diff=10722 2 Micron All Sky Survey - 2MASS 2013-01-17T03:04:04Z <p>Piper: </p> <hr /> <div>2MASS is an all sky survey that was started in 1997 and completed in 2001 with a final post processing release in 2003. 2MASS used northern (Mt. Hopkins, Arizona) and southern hemisphere (Cerro Tololo/CTIO, Chile) ground based telescopes to obtain data from the whole sky. You can actually see a live webcam pointed at the Chile site using [http://skynet.unc.edu/promptcam/ this link to the Skynet remote telescope network.] Wavelengths around 2 microns, J (1.25 um), H (1.65 um), and Ks (2.17 um) in the Near Infrared (NIR) were used in this survey which produced over 500 million sources in the point source catalog and 1.6 million sources in the extended source catalog (I don't know what this means yet:) These catalogs are publicly available.<br /> <br /> Probabley better in bullet form.<br /> <br /> Add pics of actual scopes.<br /> <br /> Add where it fits with other scopes and what it is typically used for???</div> Piper