https://vmcoolwiki.ipac.caltech.edu/api.php?action=feedcontributions&feedformat=atom&user=Booker 2026-04-10T01:19:21Z User contributions MediaWiki 1.34.2 https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12265 2013-12-09T22:53:51Z

<p>Booker: </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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula.&quot;&lt;br/&gt;&lt;br/&gt;<br /> NGC 281 contains several distinct regions: <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **NGC 281 East: The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West: (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.<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 /> Completing our analysis of the properties of the protostars in NGC 281 East and NGC 281 West required the analysis of 24 micron data taken from the Spitzer Space Telescope using MIPS. We obtained this data and photometry from the studies conducted by Scott Wolk et al. Using the Spitzer data and the 70, 100, and 160 microns data from the Hershel Observatory, we were able to create color-color diagrams of both the east and west candidate protostars. In addition, the Spitzer data allowed us to compare the SED slopes of the candidate protostars.<br /> <br /> ===Source Identification===<br /> * Carol<br /> <br /> <br /> ===Photometry Using APT===<br /> * Lynn<br /> <br /> <br /> ===Final Source Selection===<br /> NGC 281 East--Identified over 100 possible sources by examining the 70 um FITS file in both DS9 and APT. In APT, we performed aperture photometry at 70, 100, and 160um of all possible sources. Then, in APT and DS9, we examined several features of the flux profile from each candidate protostar: (1) visual shape of the source and the surrounding dust and gas, (2) XY slices of the flux within the aperture, and (3) value of the full width-half maximum (FWHM). We plotted the distribution of the FWHM's to determine acceptable range of FWHMs for the aperture photometry in each band. Taking all of the above into consideration, we then determined 41 possible sources on the east side with 8 of them providing the most confidence given their shape, radial profile, and XY slices. We called these 8 our &quot;yes&quot; sources, and the other 33 our &quot;maybe&quot; sources. These are most likely sources, but do not inspire as much confidence.<br /> <br /> <br /> <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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12264 2013-12-06T13:53:58Z

<p>Booker: /* Introduction to NGC 281 */</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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula.&quot;&lt;br/&gt;&lt;br/&gt;<br /> NGC 281 contains several distinct regions: <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **NGC 281 East: The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West: (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.<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 /> Completing our analysis of the properties of the protostars in NGC 281 East and NGC 281 West required the analysis of 24 micron data taken from the Spitzer Space Telescope using MIPS. We obtained this data and photometry from the studies conducted by Scott Wolk et al. Using the Spitzer data and the 70, 100, and 160 microns data from the Hershel Observatory, we were able to create color-color diagrams of both the east and west candidate protostars. In addition, the Spitzer data allowed us to compare the SED slopes of the candidate protostars.<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12263 2013-12-06T13:53:19Z

<p>Booker: /* Spitzer data */</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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula.&quot;&lt;br/&gt;&lt;br/&gt;<br /> NGC 281 contains several distinct regions: <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **NGC 281 East: The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West: (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.<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 /> Completing our analysis of the properties of the protostars in NGC 281 East and NGC 281 West required the analysis of 24 micron data taken from the Spitzer Space Telescope using MIPS. We obtained this data and photometry from the studies conducted by Scott Wolk et al. Using the Spitzer data and the 70, 100, and 160 microns data from the Hershel Observatory, we were able to create color-color diagrams of both the east and west candidate protostars. In addition, the Spitzer data allowed us to compare the SED slopes of the candidate protostars.<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=CharmingTheSnake&diff=12262 2013-12-06T13:51:28Z

<p>Booker: </p> <hr /> <div><br /> *'''How was Python used in the research process?'''<br /> **Data organization <br /> **Took all our data from APT and converted it into tables<br /> ***All the data gathered from the sources was converted into manageable charts <br /> ***A single table with all the bands of photometry - Cull and Merge data from all bands (Band merging)<br /> **Useful for implementing multiple applications<br /> ***Can do multiple steps/processes in one programs<br /> **Used for making graphs - FWHM<br /> **Used to create regions files&lt;br/&gt;&lt;br/&gt;<br /> *'''Student affective responses to learning Python'''<br /> **It challenged me to be more creative (coming up with ways to organize data) and detail oriented (coding so that the program runs)<br /> **It was easy at first with simple coding for quick results, but then it got a bit more arduous as we had to recall more code and take on larger projects with more steps. That said, it was ultimately achievable and the challenges made for a fun experience.<br /> **I liked the idea of being able to streamline our research process.<br /> **It was great to learn coding by doing as a part of an ongoing project instead of learning through made up examples.&lt;br/&gt;&lt;br/&gt;<br /> *'''Applications for high school-level research'''<br /> **Can create and provide visual examples of experiments<br /> ***Python (Visual Python)<br /> **Organizing large pools of data (perhaps from databases)<br /> ***Using organized data to create visually appealing graphs and charts<br /> **Sorting data so that it is easily accessible and easy to read<br /> **To help check math work<br /> ***Changes to calculations take only seconds to change within a program<br /> **Can make formulas to aid any mathematical needs<br /> **To combine multiple pools of data<br /> **Write a program to do a repetitive task<br /> **Programming can be used in almost any class where I student needs to cull, sort, and analyze a large pool of data&lt;br/&gt;&lt;br/&gt;<br /> *'''Advice &amp; Recommendations for teachers &amp; curriculum specialists'''<br /> **Start small (“Hello World”, Basic Math Operations)<br /> **Code Academy<br /> **Learn libraries specific to what you are doing (SciPy, NumPy, Visual)<br /> **Integration of programming into all STEM-based classes<br /> **Learn Excel programming if nothing else</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12261 2013-12-06T13:49:18Z

<p>Booker: /* Spitzer data */</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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula.&quot;&lt;br/&gt;&lt;br/&gt;<br /> NGC 281 contains several distinct regions: <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **NGC 281 East: The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West: (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.<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 /> Completing our analysis of the properties of the protostars in NGC 281 East and NGC 281 West required the analysis of 24 micron data taken from the Spitzer Space Telescope using MIPS. We obtained this data and photometry from the studies conducted by Scott Wolk et al. Using the Spitzer data and the 70, 100, and 160 microns data from the Hershel Observatory, we were able to create color-color diagrams of both the east and west candidate protostars. In addition, the Spitzer data allowed us to compare the SED slopes between 24um and 70um of the candidate protostars.<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12260 2013-12-06T13:37:32Z

<p>Booker: /* Introduction to NGC 281 */</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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula.&quot;&lt;br/&gt;&lt;br/&gt;<br /> NGC 281 contains several distinct regions: <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **NGC 281 East: The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West: (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12259 2013-12-06T13:36:52Z

<p>Booker: /* Introduction to NGC 281 */</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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula.&quot;&lt;br/&gt;&lt;br/&gt;<br /> '''NGC 281 contains several distinct regions:''' <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **NGC 281 East: The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West: (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12258 2013-12-06T13:36:09Z

<p>Booker: /* Introduction to NGC 281 */</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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula.&quot;&lt;br/&gt;&lt;br/&gt;<br /> '''NGC 281 contains several distinct regions:''' <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **NGC281 East: The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West: (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12257 2013-12-06T13:35:21Z

<p>Booker: /* Introduction to NGC 281 */</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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula.&quot;&lt;br/&gt;&lt;br/&gt;<br /> '''NGC 281 contains several distinct regions:''' <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12256 2013-12-06T13:34:38Z

<p>Booker: </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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. It is often referred to as the &quot;PacMan nebula&quot;&lt;br/&gt;&lt;br/&gt;<br /> '''NGC 281 contains several distinct regions:''' <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders. <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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12255 2013-12-06T13:33:20Z

<p>Booker: </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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. &lt;br/&gt;&lt;br/&gt;<br /> '''NGC 281 contains several distinct regions:''' <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.&lt;br/&gt;<br /> *Two quite distinct CO molecular clouds:<br /> **The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> **NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders. <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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12254 2013-12-06T13:31:26Z

<p>Booker: </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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. &lt;br/&gt;&lt;br/&gt;<br /> '''<br /> NGC 281 contains several distinct regions:''' <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005 (Guetter &amp; Turner 1997). &lt;br/&gt;<br /> *Two quite distinct CO molecular clouds (Elmegreen &amp; Lada 1978):<br /> **The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 kms-1 vs. -26.5 kms-1) (Leisawitz 1988). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> <br /> **NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust (Guetter &amp; Turner 1997) and has a LSR (+44 kms-1) quite different from that of its eastern neighbor and the HII region it borders (Leisawitz 1988). <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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12253 2013-12-06T13:30:09Z

<p>Booker: </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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;\alpha&lt;/math&gt;2000=00h52m, &lt;math&gt;\delta&lt;/math&gt;2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. &lt;br/&gt;&lt;br/&gt;<br /> '''<br /> NGC 281 contains several distinct regions:''' <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005 (Guetter &amp; Turner 1997). &lt;br/&gt;<br /> Two quite distinct CO molecular clouds (Elmegreen &amp; Lada 1978):<br /> *The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 kms-1 vs. -26.5 kms-1) (Leisawitz 1988). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> <br /> *NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust (Guetter &amp; Turner 1997) and has a LSR (+44 kms-1) quite different from that of its eastern neighbor and the HII region it borders (Leisawitz 1988). <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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=ProtostarsInNGC281&diff=12252 2013-12-06T13:23:45Z

<p>Booker: </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 /> NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (&lt;math&gt;a&lt;/math&gt;2000=00h52m, &lt;math&gt;d&lt;/math&gt;2000=+56d34m or l=123.1d, b= -6.3d)in the constellation Cassiopeia. &lt;br/&gt;<br /> '''<br /> NGC 281 contains several distinct regions:''' <br /> *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005 (Guetter &amp; Turner 1997). &lt;br/&gt;<br /> Two quite distinct CO molecular clouds (Elmegreen &amp; Lada 1978):<br /> *The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 kms-1 vs. -26.5 kms-1) (Leisawitz 1988). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. <br /> <br /> *NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath &amp; Wilson 1997). The region is heavily obscured by dust (Guetter &amp; Turner 1997) and has a LSR (+44 kms-1) quite different from that of its eastern neighbor and the HII region it borders (Leisawitz 1988). <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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=CharmingTheSnake&diff=12250 2013-12-03T01:58:27Z

<p>Booker: </p> <hr /> <div><br /> *'''How was Python used in the research process?'''<br /> **Data organization <br /> **Took all our data from APT and converted it into tables<br /> ***All the data gathered from the sources was converted into manageable charts <br /> ***A single table with all the bands of photometry - Cull and Merge data from all bands (Band merging)<br /> **Useful for implementing multiple applications<br /> ***Can do multiple steps/processes in one programs<br /> **Used for making graphs - FWHM<br /> **Used to create regions files<br /> <br /> *'''Student affective responses to learning Python'''<br /> **It challenged me to be more creative (coming up with ways to organize data) and detail oriented (coding so that the program runs)<br /> **It was easy at first with simple coding for quick results, but then it got a bit more arduous as we had to recall more code and take on larger projects with more steps. That said, it was ultimately achievable and the challenges made for a fun experience.<br /> **I liked the idea of being able to streamline our research process.<br /> **It was great to learn coding by doing as a part of an ongoing project instead of learning through made up examples.<br /> <br /> *'''Applications for high school-level research'''<br /> **Can create and provide visual examples of experiments<br /> ***Python (Visual Python)<br /> **Organizing large pools of data (perhaps from databases)<br /> ***Using organized data to create visually appealing graphs and charts<br /> **Sorting data so that it is easily accessible and easy to read<br /> **To help check math work<br /> ***Changes to calculations take only seconds to change within a program<br /> **Can make formulas to aid any mathematical needs<br /> **To combine multiple pools of data<br /> **Write a program to do a repetitive task<br /> **Programming can be used in almost any class where I student needs to cull, sort, and analyze a large pool of data<br /> <br /> *'''Advice &amp; Recommendations for teachers &amp; policy makers'''<br /> **Start small (“Hello World”, Basic Math Operations)<br /> **Code Academy<br /> **Learn libraries specific to what you are doing (SciPy, NumPy, Visual)<br /> **Integration of programming into all STEM-based classes<br /> **Learn Excel programming if nothing else</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=CharmingTheSnake&diff=12249 2013-12-03T01:57:33Z

<p>Booker: </p> <hr /> <div><br /> *'''How was Python used in the research process?'''<br /> **Data organization <br /> **Took all our data from APT and converted it into tables<br /> ***All the data gathered from the sources was converted into manageable charts <br /> ***A single table with all the bands of photometry - Cull and Merge<br /> ***Band merging<br /> **Useful for implementing multiple applications<br /> ***Can do multiple steps/processes in one programs<br /> **Used for making graphs - FWHM<br /> **Used to create regions files<br /> <br /> *'''Student affective responses to learning Python'''<br /> **It challenged me to be more creative (coming up with ways to organize data) and detail oriented (coding so that the program runs)<br /> **It was easy at first with simple coding for quick results, but then it got a bit more arduous as we had to recall more code and take on larger projects with more steps. That said, it was ultimately achievable and the challenges made for a fun experience.<br /> **I liked the idea of being able to streamline our research process.<br /> **It was great to learn coding by doing as a part of an ongoing project instead of learning through made up examples.<br /> <br /> *'''Applications for high school-level research'''<br /> **Can create and provide visual examples of experiments<br /> ***Python (Visual Python)<br /> **Organizing large pools of data (perhaps from databases)<br /> ***Using organized data to create visually appealing graphs and charts<br /> **Sorting data so that it is easily accessible and easy to read<br /> **To help check math work<br /> ***Changes to calculations take only seconds to change within a program<br /> **Can make formulas to aid any mathematical needs<br /> **To combine multiple pools of data<br /> **Write a program to do a repetitive task<br /> **Programming can be used in almost any class where I student needs to cull, sort, and analyze a large pool of data<br /> <br /> *'''Advice &amp; Recommendations for teachers &amp; policy makers'''<br /> **Start small (“Hello World”, Basic Math Operations)<br /> **Code Academy<br /> **Learn libraries specific to what you are doing (SciPy, NumPy, Visual)<br /> **Integration of programming into all STEM-based classes<br /> **Learn Excel programming if nothing else</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=CharmingTheSnake&diff=12248 2013-12-03T01:56:51Z

<p>Booker: </p> <hr /> <div><br /> *'''How was Python used in the research process?'''<br /> **Data organization <br /> **Took all our data from APT and converted it into tables<br /> ***All the data gathered from the sources was converted into manageable charts <br /> ***A single table with all the bands of photometry - Cull and Merge<br /> ***Band merging<br /> **Useful for implementing multiple applications<br /> ***Can do multiple steps/processes in one programs<br /> **Used for making graphs - FWHM<br /> **Used to create regions files<br /> <br /> *'''Student affective responses to learning Python'''<br /> **It challenged me to be more creative (coming up with ways to organize data) and detail oriented (coding so that the program runs)<br /> **It was easy at first with simple coding for quick results, but then it got a bit more arduous as we had to recall more code and take on larger projects with more steps. That said, it was ultimately achievable and the challenges made for a fun experience.<br /> **I liked the idea of being able to streamline our research process.<br /> **It was great to learn coding by doing as a part of an ongoing project instead of learning through made up examples.<br /> <br /> *'''Applications for high school-level research'''<br /> **Can create and provide visual examples of experiments<br /> ***Python (Visual Python)<br /> **Organizing large pools of data (perhaps from databases)<br /> ***Using organized data to create visually appealing graphs and charts<br /> **Sorting data so that it is easily accessible and easy to read<br /> **To help check math work<br /> ***Changes to calculations take only seconds to change within a program<br /> **Can make formulas to aid any mathematical needs<br /> **To combine multiple pools of data<br /> **Write a program to do a repetitive task<br /> **Programming can be used in almost any class where I student needs to cull, sort, and analyze a large pool of data<br /> <br /> *'''Advice &amp; Recommendation for teachers &amp; policy makers'''<br /> **Start small (“Hello World”, Basic Math Operations)<br /> **Code Academy<br /> **Learn libraries specific to what you are doing (SciPy, NumPy, Visual)<br /> **Integration of programming into all STEM-based classes<br /> **Learn Excel programming if nothing else</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=CharmingTheSnake&diff=12247 2013-12-02T20:41:35Z

<p>Booker: </p> <hr /> <div><br /> *'''How was Python used in the research process?'''<br /> **Data organization <br /> **Took all our data from APT and converted it into tables<br /> ***All the data gathered from the sources was converted into manageable charts <br /> ***A single table with all the bands of photometry - Cull and Merge<br /> ***Band merging<br /> **Useful for implementing multiple applications<br /> ***Can do multiple steps/processes in one programs<br /> **Used for making graphs - FWHM<br /> **Used to create regions files<br /> <br /> *'''Student affective responses to learning Python'''<br /> **It challenged me to be more creative (coming up with ways to organize data) and detail oriented (coding so that the program runs)<br /> **It was easy at first with simple coding for quick results, but then it got a bit more arduous as we had to recall more code and take on larger projects with more steps. That said, it was ultimately achievable and the challenges made for a fun experience.<br /> **I liked the idea of being able to streamline our research process.<br /> **It was great to learn coding by doing as a part of an ongoing project instead of learning through made up examples.<br /> <br /> *'''Applications for high school-level research'''<br /> **Can create and provide visual examples of experiments<br /> ***Python (Visual Python)<br /> **Organizing large pools of data (perhaps from databases)<br /> ***Using organized data to create visually appealing graphs and charts<br /> **Sorting data so that it is easily accessible and easy to read<br /> **To help check math work<br /> ***Changes to calculations take only seconds to change within a program<br /> **Can make formulas to aid any mathematical needs<br /> **To combine multiple pools of data<br /> **Write a program to do a repetitive task<br /> **Programming can be used in almost any class where I student needs to cull, sort, and analyze a large pool of data<br /> <br /> *'''Advice for teachers &amp; policy makers'''<br /> **Start small (“Hello World”, Basic Math Operations)<br /> **Code Academy<br /> **Learn libraries specific to what you are doing (SciPy, NumPy, Visual)<br /> **Integration of programming into all STEM-based classes<br /> **Learn Excel programming if nothing else</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=CharmingTheSnake&diff=12246 2013-12-02T20:39:18Z

<p>Booker: </p> <hr /> <div><br /> *How was Python used in the research process?<br /> **Data organization <br /> **Took all our data from APT and converted it into tables<br /> ***All the data gathered from the sources was converted into manageable charts <br /> ***A single table with all the bands of photometry - Cull and Merge<br /> ***Band merging<br /> **Useful for implementing multiple applications<br /> ***Can do multiple steps/processes in one programs<br /> **Used for making graphs - FWHM<br /> **Used to create regions files<br /> <br /> *Student affective responses to learning Python<br /> **It challenged me to be more creative (coming up with ways to organize data) and detail oriented (coding so that the program runs)<br /> **It was easy at first with simple coding for quick results, but then it got a bit more arduous as we had to recall more code and take on larger projects with more steps. That said, it was ultimately achievable and the challenges made for a fun experience.<br /> **I liked the idea of being able to streamline our research process.<br /> **It was great to learn coding by doing as a part of an ongoing project instead of learning through made up examples.<br /> <br /> *Applications for high school-level research<br /> **Can create and provide visual examples of experiments<br /> ***Python (Visual Python)<br /> **Organizing large pools of data (perhaps from databases)<br /> ***Using organized data to create visually appealing graphs and charts<br /> **Sorting data so that it is easily accessible and easy to read<br /> **To help check math work<br /> ***Changes to calculations take only seconds to change within a program<br /> **Can make formulas to aid any mathematical needs<br /> **To combine multiple pools of data<br /> **Write a program to do a repetitive task<br /> **Programming can be used in almost any class where I student needs to cull, sort, and analyze a large pool of data<br /> <br /> *Advice for teachers &amp; policy makers<br /> **Start small (“Hello World”, Basic Math Operations)<br /> **Code Academy<br /> **Learn libraries specific to what you are doing (SciPy, NumPy, Visual)<br /> **Integration of programming into all STEM-based classes<br /> **Learn Excel programming if nothing else</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=CharmingTheSnake&diff=12245 2013-12-02T20:38:28Z

<p>Booker: </p> <hr /> <div><br /> *How was Python used in the research process?<br /> **Data organization <br /> **Took all our data from APT and converted it into tables<br /> ***All the data gathered from the sources was converted into manageable charts <br /> ***A single table with all the bands of photometry - Cull and Merge<br /> ***Band merging<br /> **Useful for implementing multiple applications<br /> ***Can do multiple steps/processes in one programs<br /> **Used for making graphs - FWHM<br /> **Used to create regions files<br /> <br /> *Student affective responses to learning Python<br /> **It challenged me to be more creative (coming up with ways to organize data) and detail oriented (coding so that the program runs)<br /> **It was easy at first with simple coding for quick results, but then it got a bit more arduous as we had to recall more code and take on larger projects with more steps. That said, it was ultimately achievable and the challenges made for a fun experience.<br /> **I liked the idea of being able to streamline our research process.<br /> **It was great to learn coding by doing as a part of an ongoing project instead of learning through made up examples.<br /> <br /> *Applications for high school-level research<br /> **Can create and provide visual examples of experiments<br /> ***Python (Visual Python)<br /> **Organizing large pools of data (perhaps from databases)<br /> ***Using organized data to create visually appealing graphs and charts<br /> **Sorting data so that it is easily accessible and easy to read<br /> **To help check math work<br /> ***Changes to calculations take only seconds to change within a program<br /> **Can make formulas to aid any mathematical needs<br /> **To combine multiple pools of data<br /> **Write a program to do a repetitive task<br /> **Programming can be used in almost any class where I student needs to cull, sort, and analyze a large pool of data<br /> <br /> *Advice for teachers &amp; policy makers (Ms. Booker)<br /> **Start small (“Hello World”, Basic Math Operations)<br /> **Code Academy<br /> **Learn libraries specific to what you are doing (SciPy, NumPy, Visual)<br /> **Integration of programming into all STEM-based classes<br /> **Learn Excel programming if nothing else</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=CharmingTheSnake&diff=12244 2013-12-02T20:38:09Z

<p>Booker: Created page with &quot; *How was Python used in the research process? **Data organization **Took all our data from APT and converted it into tables ***All the data gathered from the sources was con...&quot;</p> <hr /> <div><br /> *How was Python used in the research process?<br /> **Data organization <br /> **Took all our data from APT and converted it into tables<br /> ***All the data gathered from the sources was converted into manageable charts <br /> ***A single table with all the bands of photometry - Cull and Merge<br /> Band merging<br /> **Useful for implementing multiple applications<br /> ***Can do multiple steps/processes in one programs<br /> **Used for making graphs - FWHM<br /> **Used to create regions files<br /> <br /> *Student affective responses to learning Python<br /> **It challenged me to be more creative (coming up with ways to organize data) and detail oriented (coding so that the program runs)<br /> **It was easy at first with simple coding for quick results, but then it got a bit more arduous as we had to recall more code and take on larger projects with more steps. That said, it was ultimately achievable and the challenges made for a fun experience.<br /> **I liked the idea of being able to streamline our research process.<br /> **It was great to learn coding by doing as a part of an ongoing project instead of learning through made up examples.<br /> <br /> *Applications for high school-level research<br /> **Can create and provide visual examples of experiments<br /> ***Python (Visual Python)<br /> **Organizing large pools of data (perhaps from databases)<br /> ***Using organized data to create visually appealing graphs and charts<br /> **Sorting data so that it is easily accessible and easy to read<br /> **To help check math work<br /> ***Changes to calculations take only seconds to change within a program<br /> **Can make formulas to aid any mathematical needs<br /> **To combine multiple pools of data<br /> **Write a program to do a repetitive task<br /> **Programming can be used in almost any class where I student needs to cull, sort, and analyze a large pool of data<br /> <br /> *Advice for teachers &amp; policy makers (Ms. Booker)<br /> **Start small (“Hello World”, Basic Math Operations)<br /> **Code Academy<br /> **Learn libraries specific to what you are doing (SciPy, NumPy, Visual)<br /> **Integration of programming into all STEM-based classes<br /> **Learn Excel programming if nothing else</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_FINAL.docx&diff=11446 2013-03-08T11:20:49Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11445 2013-03-08T11:19:28Z

<p>Booker: </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]]<br /> <br /> [[File:SHIPS_Proposal_FINAL.docx]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_07c.docx&diff=11442 2013-03-08T02:33:14Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11441 2013-03-08T02:32:04Z

<p>Booker: </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]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11440 2013-03-08T02:30:27Z

<p>Booker: </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_07d.docx]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_07a.docx&diff=11432 2013-03-07T23:28:02Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11431 2013-03-07T23:27:22Z

<p>Booker: </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_07a.docx]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_06d.docx&diff=11386 2013-03-06T18:22:32Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11385 2013-03-06T18:21:25Z

<p>Booker: </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]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_06b.docx&diff=11382 2013-03-06T15:46:20Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11381 2013-03-06T15:44:44Z

<p>Booker: </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]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_06a.docx&diff=11380 2013-03-06T13:47:44Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11379 2013-03-06T13:45:24Z

<p>Booker: </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]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_05c.docx&diff=11376 2013-03-06T04:11:28Z

<p>Booker: uploaded a new version of &amp;quot;File:SHIPS Proposal v03 05c.docx&amp;quot;</p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_05c.docx&diff=11375 2013-03-06T03:43:13Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11374 2013-03-06T03:41:40Z

<p>Booker: </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]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_04.docx&diff=11358 2013-03-05T03:51:59Z

<p>Booker: uploaded a new version of &amp;quot;File:SHIPS Proposal v03 04.docx&amp;quot;</p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_04.docx&diff=11357 2013-03-05T03:16:04Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11356 2013-03-05T03:13:42Z

<p>Booker: </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| ]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_03b.docx&diff=11352 2013-03-04T03:52:01Z

<p>Booker: uploaded a new version of &amp;quot;File:SHIPS Proposal v03 03b.docx&amp;quot;: v03_03d</p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_03b.docx&diff=11350 2013-03-04T02:04:13Z

<p>Booker: uploaded a new version of &amp;quot;File:SHIPS Proposal v03 03b.docx&amp;quot;: New file 03_03c</p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:SHIPS_Proposal_v03_03b.docx&diff=11346 2013-03-04T01:02:27Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11345 2013-03-04T01:01:42Z

<p>Booker: </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?<br /> <br /> ==Current Version of the Proposal==<br /> <br /> [[File:SHIPS_Proposal_v03_03b.docx| ]]</div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11296 2013-02-26T03:23:20Z

<p>Booker: </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 /> |[[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 /> |<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:NITARP_Proposal_Booker.docx&diff=11295 2013-02-26T03:22:14Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11294 2013-02-26T03:21:17Z

<p>Booker: </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 /> |[[File:NITARP Proposal Booker.dox | 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 /> |<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11293 2013-02-26T03:20:36Z

<p>Booker: </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 /> |[[File:NITARP Proposal Booker.dox | 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 /> |<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>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Megeath.docx&diff=11289 2013-02-25T03:58:56Z

<p>Booker: </p> <hr /> <div></div>

Booker https://vmcoolwiki.ipac.caltech.edu/index.php?title=SHIPsProposal&diff=11288 2013-02-25T03:58:13Z

<p>Booker: /* 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 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 /> |[[File:Megeath.docx | Booker brain dump on both papers]]<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>

Booker