https://vmcoolwiki.ipac.caltech.edu/api.php?action=feedcontributions&feedformat=atom&user=Mallory 2026-04-15T22:33:43Z User contributions MediaWiki 1.34.2 https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:My_cg4_image_1000x1500.jpg&diff=4200 2010-05-03T17:16:29Z

<p>Mallory: </p> <hr /> <div></div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3981 2010-02-09T05:28:36Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited 7 Feb. 2010).<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environments, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; which are the structural components of the universe, i.e. Galaxie Changes, causes evolution of the Universe. <br /> <br /> The Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. Using this Locale, we will attempt to answer three questions: Will Stars Form Here? If So, Is Their Formation Triggered? and, Has a Whole Cluster Been Formed?<br /> <br /> The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude. Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m. Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the surfaces of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.<br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether this is Triggered Star Formation.(See “Spitzer Observations of IC 2118.) The outcome of this important research question will help to determine the Rate of Star Formation in the Universe. The presence of both O &amp; B superstars, copious UV and gamma emitters, plus Supernova Remnants indicating stupendous interstellar explosions, suggest an energetic nebular environment. We verified this using Multiwavelength Photometric Studies, similar to (Kim,S. et al, &quot;Triggered Low Mass Star Formation in the Gum Nebula&quot;, 2003). A similar environment, see Spitzer Observations of IC 2118, confirm this idea. The Skyview Telescope (http://skyview.gsfc.nasa.gov) shows radiation at all wavelengths and images at all wavelengths, of excited gas/dust in the selected region. Through our collaborator J.S. Kim (U. AZ)we have access to X-ray data from XMM, Epic and PN images that cover CG4. X-ray + UV presence may have triggered star formation by providing compression pressure onto collapsing nebula gas-knots, or destroyed them by photo-evaporation.<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. <br /> <br /> <br /> Our Final Question related to Star Formation in CG4, &quot;Has a Whole Star Cluster Been Formed&quot;, has to be approached carefully, since it is so easy to confuse a foreground/background star with actual Cluster Members. The finest tool to accomplish the identification of Stars Which Are Cluster Members, resides on the IPAC website. What the techniques boils down to, is to determine all YSOs in an area, and be sure they are all the same age. If they are the same age, it is likely they are all members of the same cluster. Some characteristics they should all have/all have in common, are: IR excess; flaring/in X-rays; flaring /in radio/emmission from stellar active regions, like Sun Spots; BiPolar outflows (detectable in IR &amp; optical as emitted jets); emission lines (from accreting matter); variability (not quite in equilibrium yet); fast rotation rate (concervation of Angular Momentum); UV flaring/mass accretion; spatial location huddled together; similar brightness; common spatial motion as they glide through space loosely gravitationally bound together.<br /> <br /> Spitzer is good at determining these qualities of stars. It is so sensitive that it can see nearly to the 'edge' of the Universe, and integrate data in just a handful of seconds. Further, Spitz, will see the excess IR from the Planatary Disc of a newly formed star, before it gets dissipated, and that will record as a Spare Tire IR Excess. Chandra and XMM data will be helpful in detecting X-ray flares due to large magnetic field, from rapid rotation inducing emission flares in X-ray wavelength.<br /> <br /> <br /> <br /> Proposal for CG4 Group<br /> <br /> Goal: We are looking for new young stellar objects (YSO) in the cometary nebula CG4 in Puppis. These objects will tell us about cometary globules and conditions within them. We will find information about the structures in the globule, their history and possibly their future. <br /> <br /> Stars form in regions of dense dust and gas in the interstellar medium (ISM). The process is.... (See Carolyn's explaination above.) <br /> <br /> Cometary globule CG4 is approximately 450 parsec away. It is a part of a larger structure in the Milky Way. It is one of a number of cometary globules in the area pointed away from a common center, possibly the Vela supernova remnant. CG4 is a nearby and dramatic cometary globule, so it is of interest to scientists and the public. Recent visible and visible/infrared mosaics have been featured in Astronomy Magazine and Science News Magazine. <br /> <br /> Method: Our team will use Spitzer IRAC and MIPS data (programs 202, 462, 20714), 2MASS data, and XMM-Newton x-ray data. We expect to find the previously known YSOs (Reipurth and Petersson 1993) and additional YSOs in star-forming regions. We will find other candidate objects using infrared excess across different wavelengths. There will be some non-members in this candidate group. Along with YSOs in the cluster, we expect to find extragallactic sources (active galactic nuclei anything else ?). We will use x-ray data, phtometric data and astrometry to determine cluster membership and separate YSOs from other objects with IR excess.<br /> <br /> We will use x-ray data from the . We will use astrometry to find proper motion using the Digitized Sky Survey plates and more recent images from CTIO 0.9m telescope. <br /> <br /> We propose using IRAC, MIPS and 2MASS data archives along with XMM-Newton satellite data, photometric data (BVRI) from the CTIO 0.9m telescope and astrometric data from the Digitized Sky Survey and more recent images with the CTIO 0.9m telescope to investigate:<br /> <br /> 1. Star formation; look for likely cluster member stars with infrared excesses, and <br /> <br /> 2. characterize this young star population by obtaining colors and estimates of masses and ages; <br /> <br /> 3. study the distribution of stars, compare the young star population, distribution, and age to other similar sites of star formation.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3974 2010-02-08T07:29:41Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited Superbowl-Sunday 7 Feb. 2010,10:42 p.) (No, 11:30 p.)<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environments, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; which are the structural components of the universe, i.e. Galaxie Changes, causes evolution of the Universe. <br /> <br /> The Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. Using this Locale, we will attempt to answer three questions: Will Stars Form Here? If So, Is Their Formation Triggered? and, Has a Whole Cluster Been Formed?<br /> <br /> The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude. Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m. Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the surfaces of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.<br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether this is Triggered Star Formation.(See “Spitzer Observations of IC 2118.) The outcome of this important research question will help to determine the Rate of Star Formation in the Universe. The presence of both O &amp; B superstars, copious UV and gamma emitters, plus Supernova Remnants indicating stupendous interstellar explosions, suggest an energetic nebular environment. We verified this using Multiwavelength Photometric Studies, similar to (Kim,S. et al, &quot;Triggered Low Mass Star Formation in the Gum Nebula&quot;, 2003). A similar environment, see Spitzer Observations of IC 2118, confirm this idea. The Skyview Telescope (http://skyview.gsfc.nasa.gov) shows radiation at all wavelengths and images at all wavelengths, of excited gas/dust in the selected region. Through our collaborator J.S. Kim (U. AZ)we have access to X-ray data from XMM, Epic and PN images that cover CG4. X-ray + UV presence may have triggered star formation by providing compression pressure onto collapsing nebula gas-knots, or destroyed them by photo-evaporation.<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. <br /> <br /> <br /> Our Final Question related to Star Formation in CG4, &quot;Has a Whole Star Cluster Been Formed&quot;, has to be approached carefully, since it is so easy to confuse a foreground/background star with actual Cluster Members. The finest tool to accomplish the identification of Stars Which Are Cluster Members, resides on the IPAC website. What the techniques boils down to, is to determine all YSOs in an area, and be sure they are all the same age. If they are the same age, it is likely they are all members of the same cluster. Some characteristics they should all have/all have in common, are: IR excess; flaring/in X-rays; flaring /in radio/emmission from stellar active regions, like Sun Spots; BiPolar outflows (detectable in IR &amp; optical as emitted jets); emission lines (from accreting matter); variability (not quite in equilibrium yet); fast rotation rate (concervation of Angular Momentum); UV flaring/mass accretion; spatial location huddled together; similar brightness; common spatial motion as they glide through space loosely gravitationally bound together.<br /> <br /> Spitzer is good at determining these qualities of stars. It is so sensitive that it can see nearly to the 'edge' of the Universe, and integrate data in just a handful of seconds. Further, Spitz, will see the excess IR from the Planatary Disc of a newly formed star, before it gets dissipated, and that will record as a Spare Tire IR Excess. Chandra and XMM data will be helpful in detecting X-ray flares due to large magnetic field, from rapid rotation inducing emission flares in X-ray wavelength.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3973 2010-02-08T07:28:19Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited Superbowl-Sunday 7 Feb. 2010,10:42 p.) (No, 11:10 p.)<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environments, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; which are the structural components of the universe, i.e. Galaxie Changes, causes evolution of the Universe. <br /> <br /> The Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. Using this Locale, we will attempt to answer three questions: Will Stars Form Here? If So, Is Their Formation Triggered? and, Has a Whole Cluster Been Formed?<br /> <br /> The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude. Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m. Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the surfaces of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.<br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether this is Triggered Star Formation.(See “Spitzer Observations of IC 2118.) The outcome of this important research question will help to determine the Rate of Star Formation in the Universe. The presence of both O &amp; B superstars, copious UV and gamma emitters, plus Supernova Remnants indicating stupendous interstellar explosions, suggest an energetic nebular environment. We verified this using Multiwavelength Photometric Studies, similar to (Kim,S. et al, &quot;Triggered Low Mass Star Formation in the Gum Nebula&quot;, 2003). A similar environment, see Spitzer Observations of IC 2118, confirm this idea. The Skyview Telescope (http://skyview.gsfc.nasa.gov) shows radiation at all wavelengths and images at all wavelengths, of excited gas/dust in the selected region. Through our collaborator J.S. Kim (U. AZ)we have access to X-ray data from XMM, Epic and PN images that cover CG4. X-ray + UV presence may have triggered star formation by providing compression pressure onto collapsing nebula gas-knots, or destroyed them by photo-evaporation.<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. <br /> <br /> <br /> Our Final Question related to Star Formation in CG4, &quot;Has a Whole Star Cluster Been Formed&quot;, has to be approached carefully, since it is so easy to confuse a foreground/background star with actual Cluster Members. The finest tool to accomplish the identification of Stars Which Are Cluster Members, resides on the IPAC website. What the techniques boils down to, is to determine all YSOs in an area, and be sure they are all the same age. If they are the same age, it is likely they are all members of the same cluster. Some characteristics they should all have/all have in common, are: IR excess; flaring/in X-rays; flaring /in radio/emmission from stellar active regions, like Sun Spots; BiPolar outflows (detectable in IR &amp; optical as emitted jets); emission lines (from accreting matter); variability (not quite in equilibrium yet); fast rotation rate (concervation of Angular Momentum); UV flaring/mass accretion; spatial location huddled together; similar brightness; common spatial motion as they glide through space loosely gravitationally bound together.<br /> <br /> Spitzer is good at determining these qualities of stars. It is so sensitive that it can see nearly to the 'edge' of the Universe, and integrate data in just a handful of seconds. Further, Spitz, will see the excess IR from the Planatary Disc of a newly formed star, before it gets dissipated, and that will record as a Spare Tire IR Excess. Chandra and XMM data will be helpful in detecting X-ray flares due to large magnetic field, from rapid rotation inducing emission flares in X-ray wavelength.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3972 2010-02-08T07:09:35Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited Superbowl-Sunday 7 Feb. 2010,10:42 p.) <br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe. <br /> <br /> The Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. Using this Locale, we will attempt to answer three questions: Will Stars Form Here? If So, Is Their Formation Triggered? and, Has a Whole Cluster Been Formed?<br /> <br /> The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude. Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the outsides of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.<br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether this is Triggered Star Formation.(See “Spitzer Observations of IC 2118.) The outcome of this important research question will help to determine the Rate of Star Formation in the Universe. The presence of both O &amp; B superstars, copious UV and gamma emitters, plus Supernova Remnats indicating stupendous interstellar explosions, suggest an energetic nebular environment. We verified this using Multiwavelength Photometric Studies, similar to (Kim,S. et al, &quot;Triggered Low Mass Star Formation in the Gum Nebula&quot;, 2003). A similar environment, see Spitzer Observations of IC 2118, confirm this idea. The Skyview Telescope (http://skyview.gsfc.nasa.gov) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. Through our collaborator J.S. Kim (U. AZ)we have access to X-ray data from XMM, Epic and PN images that cover CG4.X-ray + UV presence may have triggered star formation by providing compression pressure onto collapsing nebula gas-knots, or destroyed them by photo-evaporation.<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O &amp; B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.<br /> When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.<br /> <br /> <br /> Our Final Question related to Star Formation in CG4, &quot;Has a Whole Star Cluster Been Formed&quot;, has to be approached carefully, since it is so easy to confuse a foreground/background star with actual Cluster Members. The finest tool to accomplish the identification of Stars Which Are Cluster Members, resides on the IPAC website. What the techniques boils down to, is to determine all YSOs in an area, and be sure they are all the same age. Likelym they are all members of the same cluster. Some characteristics they should all have/all have in common, are: IR excess, flaring/in X-rays, flaring /in radio/stellar active regions, like Sun Spots, BiPolar outflows (detectable in IR &amp; optical as emitted jets), emission lines (from accreting matter), variability (not quite in equilibrium yet), fast rotation rate (concervation of Angular Momentum), UV flaring/mass accretion, spatial location huddled together, similar brightness, common spatial motion as they glide through space somewhat gravitationally bound together.<br /> <br /> Spitzer is good at ddetermining these qualities of stars. It is so sensitive that it can see nearly to the 'edge' of the Universe, and integrate data in just a handful of seconds. Further, Spitz will see the excess IR from the Planatary Disc of a newly formed star, before it gets disipated, and that will record as a Spare Tire IR Excess. Chandra and XMM data will be helpful in detecting X-ray flares due to large magnetic field from rapid rotation inducing emission flares in X-ray wavelength.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3971 2010-02-08T06:45:14Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft (Can't find name &amp; time stamp on this page. Many additions and heavily edited Superbowl-Sunday 7 Feb. 2010,10:42 p.) <br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe. <br /> <br /> The Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. Using this Locale, we will attempt to answer three questions: Will Stars Form Here? If So, Is Their Formation Triggered? and, Has a Whole Cluster Been Formed?<br /> <br /> The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude. Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the outsides of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.<br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether this is Triggered Star Formation.(See “Spitzer Observations of IC 2118.) The outcome of this important research question will help to determine the Rate of Star Formation in the Universe. The presence of both O &amp; B superstars, copious UV and gamma emitters, plus Supernova Remnats indicating stupendous interstellar explosions, suggest an energetic nebular environment. We verified this using Multiwavelength Photometric Studies, similar to (Kim,S. et al, &quot;Triggered Low Mass Star Formation in the Gum Nebula&quot;, 2003). A similar environment, see Spitzer Observations of IC 2118, confirm this idea. The Skyview Telescope (http://skyview.gsfc.nasa.gov) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. Through our collaborator J.S. Kim (U. AZ)we have access to X-ray data from XMM, Epic and PN images that cover CG4.X-ray + UV presence may have triggered star formation by providing compression pressure onto collapsing nebula gas-knots, or destroyed them by photo-evaporation.<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O &amp; B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.<br /> When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3970 2010-02-08T06:37:29Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe. <br /> <br /> The Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude. Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the outsides of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.<br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether this is Triggered Star Formation.(See “Spitzer Observations of IC 2118.) The outcome of this important research question will help to determine the Rate of Star Formation in the Universe. The presence of both O &amp; B superstars, copious UV and gamma emitters, plus Supernova Remnats indicating stupendous interstellar explosions, suggest an energetic nebular environment. We verified this using Multiwavelength Photometric Studies, similar to (Kim,S. et al, &quot;Triggered Low Mass Star Formation in the Gum Nebula&quot;, 2003). A similar environment, see Spitzer Observations of IC 2118, confirm this idea. The Skyview Telescope (http://skyview.gsfc.nasa.gov) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. Through our collaborator J.S. Kim (U. AZ)we have access to X-ray data from XMM, Epic and PN images that cover CG4.X-ray + UV presence may have triggered star formation by providing compression pressure onto collapsing nebula gas-knots, or destroyed them by photo-evaporation.<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O &amp; B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.<br /> When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3969 2010-02-08T06:17:55Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe. <br /> <br /> The Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude. Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm/collapsing gas clouds/protostars. Additional indication of YSOs is available by using POSS 8000 mm data to reveal the near IR signature of excess IR coming from a newly-forming star. Spitzer data is especially well-suited to detect the presence of PAHs on the outsides of collapsing dust/gas clouds, in 6 &amp; 8 mm, and to comfirm YSOs' excess gases BiPolar outflow in 4.6 and 5.5 mm IR. Using Spectral Energy Distribution data, newly formed stars can be both identified and classified. The primary goal of this research: Determination of Star Formation in CG4, can be achieved.<br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether a Cluster of New Stars exists in the area, and that information may to relevant to the study of Triggered Star Formation.(See “Spitzer Observations of IC 2118.)<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O &amp; B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.<br /> When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3968 2010-02-08T06:05:13Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe. <br /> <br /> The Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) is an excellent site to study formation of stars. The CG4- Gum Nebula environment is chosen because the area is visually, photometrically dense with star-forming material. USNO http://www.nofs.navy.mil/data/fchPix used to determine opacity of nebula and optical magnitude. Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether a Cluster of New Stars exists in the area, and that information may to relevant to the study of Triggered Star Formation.(See “Spitzer Observations of IC 2118.)<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O &amp; B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.<br /> When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3967 2010-02-08T05:57:46Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> What is the importance of Young Stars? On the local scale, even small stars usually form discs, which often coalesce into planets; some may be Earth-Like planets. On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe. <br /> <br /> We choose the Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) in which to look for new stars. The following is a summary of info describing the CG4- Gum Nebula environment, chosen because the area is visually and photometrically dense with star-forming material. (Used USNO http://www.nofs.navy.mil/data/fchPix to determine opacity of nebula and optical magnitude.) Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether a Cluster of New Stars exists in the area, and that information may to relevant to the study of Triggered Star Formation.(See “Spitzer Observations of IC 2118.)<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O &amp; B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.<br /> When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3966 2010-02-08T05:48:19Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> And what is the importance of Young Stars, anyway? On the local scale, even small stars usually form discs, which often coalesce into planets. And some may be Earth-Like planets! On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe! <br /> <br /> We choose the Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) in which to look for new stars. The following is a summary of info describing the CG4- Gum Nebula environment, chosen because the area is visually and photometrically dense with star-forming material. (Used USNO http://www.nofs.navy.mil/data/fchPix to determine opacity of nebula and optical magnitude.) Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> Conditional on the outcome of the first research step; The second step in our research is to determine whether a Cluster of New Stars exists in the area, and that information may to relevant to the study of Triggered Star Formation.(See “Spitzer Observations of IC 2118.)<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O &amp; B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.<br /> When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3949 2010-02-03T20:43:07Z

<p>Mallory: </p> <hr /> <div>Please see a very raw first cut at writing the Introduction and Background for The Proposal. You already feel free to edit, right? This gives a place to start, or a decision to start over.<br /> --[[User:Mallory|Mallory]] 12:43, 3 February 2010 (PST)<br /> <br /> <br /> Draft<br /> <br /> STAR FORMATION IN CG4<br /> <br /> What factors can make Nebulae, ordinary clouds of hydrogen and helium and perhaps some tritium gas, plus dust of common silicate compounds, which appear widely throughout the plane of The Milky Way/or any galaxy, overcome the plentiful disruptive forces in their environment, and form stars? When can the classically interpreted Force of Gravity, overwhelm the dispersive effect of radiation, and force collapse into a star, on a cloud of gas and dust?<br /> <br /> And what is the importance of Young Stars, anyway? On the local scale, even small stars usually form discs, which often coalesce into planets. And some may be Earth-Like planets! On a more grand scale, formation and evolution of different types of stars, changes gas and dust and chemical composition of Galaxies; Evolution of the structural components of the universe, i.e. Galaxies, causes evolution of the Universe! <br /> <br /> We choose the Cometary Globules CG4 (R. A. 7 degrees 34’ 9”, Dec -56 degrees, Ecliptic Co-ords.) in which to look for new stars. The following is a summary of info describing the CG4- Gum Nebula environment, chosen because the area is visually and photometrically dense with star-forming material. (Used USNO http://www.nofs.navy.mil/data/fchPix to determine opacity of nebula and optical magnitude.) Through our collaborator J.S. Kim (U. AZ.) we have access to CG4 optical data in BVRI filters from the CTIO 0.9m.Extrapolating from this info may permit us to predict where and why new stars form. Conditional on the outcome of the first research step; The second step in our research is to determine whether a Cluster of New Stars exists in the area, and that information may to relevant to the study of Triggered Star Formation.(See “Spitzer Observations of IC 2118.)<br /> <br /> <br /> Skyview Telescope (http://skyview.gsfc.nasa.gov)) shows radiation at all wavelengths and images at all wavelengths of excited gas/dust in the selected region. In addition, O &amp; B Stars, as well as supernova remnants of their cousin stars, reside in the nearby Vela Nebula. Through our collaborator J.S.Kim (U. AZ) we have access to X-ray data from XMM, Epic and PN images that cover CG4. Their presence may have aided star formation by providing compression pressure onto nebula, or destroyed knots of collapsing dust, by photo evaporation, thus terminating the young stars before they reach The Main Sequence. (UV data source detecting photo evaporation from Determining the distance from CG4 to those O &amp; B stars (using ) will be important to determine what effect that parameter has on star formation. We plan to use Spitzer MIPS data, available in far IR 24, 70, 160 mm wavelengths to detect warm, collapsing gas clouds/protostars.<br /> When candidates have been thus identified, POSS (Palomar Observatory Sky Survey) in 8000 mm will reveal the near IR signature of excess IR coming from a newly formed star.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3948 2010-02-03T20:36:19Z

<p>Mallory: Blanked the page</p> <hr /> <div></div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=CG4_Proposal&diff=3925 2010-01-27T01:35:49Z

<p>Mallory: /* Education */</p> <hr /> <div>=Instructions=<br /> <br /> ==Previous Examples== <br /> All of the previous proposals are online, linked from the teams' Cool Cosmos page. All of the programs are listed here:<br /> http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/allprog.shtml<br /> and if you go to any of the team pages, you'll see lots of things, including a link to the proposal.<br /> <br /> BUT PLEASE NOTE that all of these past proposals were OBSERVING proposals and you are writing an ARCHIVAL proposal.<br /> <br /> ==Recommended Contents==<br /> In general, good proposals should have:<br /> * introduction and context. how you picked the target(s) and why. background on subject and target. educated guesses on what you might find.<br /> * detailed information on what data are available, and what you plan to do with it (e.g. much more than &quot;i'm sure spitzer observed this at some point&quot;). how you are going to reduce the data. kind of analysis planned.<br /> * education/outreach plan. what your team will do, individually or together.<br /> <br /> You don't have page limits, but nor do you want the review committee<br /> annoyed because you made them read a book.... or tiny fonts. A professor<br /> in grad school always used to annoy me with broad essay questions followed<br /> by the instruction &quot;Be brief but specific.&quot; But he's right ...<br /> <br /> <br /> <br /> =Background information=<br /> <br /> example table <br /> <br /> {| border=&quot;1&quot;<br /> |Table example <br /> | example2 <br /> | example3<br /> |-<br /> |line2<br /> |line2<br /> |line2<br /> |}<br /> <br /> <br /> <br /> Identifiers (aliases) for CG 4 ...<br /> ''BHR 21, <br /> Sandqvist 103, <br /> FEST 2-30, <br /> DCld 259.4-12.7''<br /> <br /> I found this by typing ''CG4'' into SIMBAD. The results were in the middle of the page. Scrolling down further, there's a list of 20 articles in which CG 4 is mentioned.<br /> <br /> Talk to you on Wednesday!<br /> --chj<br /> <br /> <br /> My Plan to continue Lit. search--[[User:Mallory|Mallory]] 23:35, 11 January 2010 (PST) is to finish SIMBAD, then go to ADS and to find a way to confirm and quantify lots! of IR present in suspected YSOs in CG4(probably by opacity class) and little UV/max not to exceed a threshold to be determined; don't want the object to be a middle-aged star already.<br /> <br /> Is it the group's intention to consider locations outside of CG4, which could be cluster members? <br /> <br /> --[[User:Mallory|Mallory]] 23:28, 11 January 2010 (PST)Carolyn<br /> <br /> <br /> <br /> In a search through SIMBAD for CG 4 info, some interesting info and unanswered questions have emerged.<br /> <br /> If a gaseous region were collapsing due to a radiation-driven implosion, what's to stop it from rebounding back out, and how would we know the mechanism had occurred? Maybe by the length of tails (also created by outward pressures)? Is this a safe assumption?<br /> There seems to be a conflict between different analyses as to whether tails can be traced by CO(12) spectra. How to resolve? <br /> If collapse/expansion, and rotation can occur all in the same region, are there any tools other than redshift to sort out what is happening?<br /> Interesting that there could be more than one &quot;Center of Influence' in a region, i.e. massive star,--[[User:Mallory|Mallory]] 15:48, 12 January 2010 (PST) whose radiation influences the CG's/YSO's evolution.<br /> <br /> <br /> ''Carolyn, I moved your latest research here to the Background Section, and took it out of the Education section. Nice Job in finding information. - Viv''<br /> <br /> Hey. No Fair. Carolyn is thinking while she reads! Nice work Carolyn. 14 jan 10 <br /> --klm<br /> <br /> <br /> The following is a summary of info describing the CG4 environment, and includes a small amount of info from other areas qualitatively similar to the Gum Nebula area. The environmental characteristics listed will describe the environment needed for star formation, confirmed by the presence of YSOs in the--[[User:Mallory|Mallory]] 22:24, 13 January 2010 (PST) region:<br /> <br /> -cg4 resides in the Gum Nebula, within the constellation Puppis, adjacent to Vela. This area is 1,300 LY distant from Solar System, and even visually, is laced with plentiful clouds of gas and dust.<br /> <br /> -using appropriate wavelengths, should do a search for nearby massive O &amp; B stars (typical neighborhood bullies)to determine the possibility of photoevaporation of coalescing dust and gas taking place in newly formed stars, and if so, switch area being investigated. Cometary Globule tails all coinciding in direction they're pointing is another indication that newly forming stars are being photoevaporated by nearby large star radiation/emissions. There can be a number of Centers of Influence near a newly forming Star Cluster, check this optically, in radio, and in both UV and Xray.<br /> <br /> -Note that radiation driven implosion also occurs, as well as collapse due to gravitational attraction. Do muiltiwavelength study. Radio wavelengths especially.<br /> <br /> -Expect IR excess in area of star formation (Universal Gas Law; volume mass forming star decreases/temp increase) Necessary to determine the average value for IR around a small mass Main Sequence star, so we know what amount defines 'excess IR'.<br /> <br /> - If head of cometary nebula is opaque in visible wavelengths, it can be assumed that sufficient gas and dust exist in the nebula to create new stars. Thus, opacity/Opacity Class, is an indicator of star-forming region BUT needs to be quantified and observed in the appropriate wavelengths/optical photometry/MIPS data probably.<br /> <br /> - Information about contraction/expansion/rotation, can be obtained from red-blue shift observations. This is necessary information! Personal question; could implosion produce an outward rebound?<br /> <br /> -Spectroscopic info can reveal the age/stage of development of baby stars uncovered in this study. Use MIPS data.<br /> <br /> -To determine which stars visible in same area are members of the same CG4 Cluster, see common age/convection % compared to radiation &amp; conduction, speed of rotation (need to know axis of rotation to determine blue-red shift anyway), variability, spatial location, and spatial motion of all the local stars/i.e. do they seem to be moving as a group/cluster. All of these qualities are indicators of the age of a YSO.<br /> <br /> -Excess IR (define 'excess' as variation from average IR emission from a similar mass young Main Sequence star IR average emissions) typifies newly forming stars, such as what we are looking for in CG4. Conflict in literature about UV emissions; forming star should have almost none/core processes do not yet produce, but very young stars can have a lot of UV emission due to rapid rotation. Supposedly, really young stars have low Magnetic Field.<br /> <br /> -Another variable of which to be aware, is the number of YSOs in a given area. Too many, and only those with largest relative mass will grow to be stars, since largest mass baby stars have the gravitational-strength advantage/capture the most infalling gas+dust. (Think nestfull of eagle eggs, which hatch at different times.)<br /> <br /> The sources listed below indicate that these are the qualities in nebulae which affect Star Formation. <br /> <br /> Carolyn Mallory<br /> <br /> Sources Used to Gather This information Include but are Not Limited to:<br /> SIMBAD, ic 2118, ADS, CoolWiki Finding Cluster Members, Spitzer Archives, Infrared Handbook by Wolfe &amp; Zissie.<br /> <br /> here is the paper from serena from 2005<br /> http://adsabs.harvard.edu/abs/2005AJ....129.1564K<br /> --[[User:Rebull|Rebull]] 15:57, 13 January 2010 (PST)<br /> <br /> Title: Low-Mass Star Formation in the Gum Nebula: The CG 30/31/38 Complex<br /> Authors: Kim, Jinyoung Serena; Walter, Frederick M.; Wolk, Scott J.<br /> Affiliation: AA(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.; Visiting Astronomer, Cerro Tololo Inter-American Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under contact with the National Science Foundation.), AB(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.), AC(Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.)<br /> Publication: The Astronomical Journal, Volume 129, Issue 3, pp. 1564-1579. (AJ Homepage)<br /> Publication Date:03/2005<br /> Origin:UCP<br /> AJ Keywords:Stars: Circumstellar Matter, ISM: H II Regions, ISM: Globules, Stars: Formation, Stars: Low-Mass, Brown Dwarfs, Stars: Pre-Main-Sequence<br /> DOI:10.1086/428002<br /> Bibliographic Code:2005AJ....129.1564K<br /> <br /> Abstract<br /> We present photometric and spectroscopic results for the low-mass pre-main-sequence (PMS) stars with spectral types K-M in the cometary globule (CG) 30/31/38 complex. We obtained multiobject high-resolution spectra for the targets selected as possible PMS stars from multiwavelength photometry. We identified 11 PMS stars brighter than V=16.5 with ages &lt;~5 Myr at a distance of approximately 200 pc. The spatial distribution of the PMS stars, CG clouds, and ionizing sources (O stars and supernova remnants) suggests a possible triggered origin of the star formation in this region. We confirm the youth of the photometrically selected PMS stars using the lithium abundances. The radial velocities of the low-mass PMS stars are consistent with those of the cometary globules. Most of the PMS stars show weak Hα emission with Wλ(Hα)&lt;10 Å. Only one out of the 11 PMS stars shows a moderate near-IR excess, which suggests a short survival time (t&lt;5 Myr) of circumstellar disks in this star-forming environment. In addition, we find five young late-type stars and one Ae star that have no obvious relation to the CG 30/31/38 complex. We also discuss a possible scenario of the star formation history in the CG 30/31/38 region. <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> --Some background papers I found:<br /> <br /> <br /> <br /> <br /> <br /> {| border=&quot;1&quot;<br /> |Article <br /> | Comments <br /> | Comments on Comments<br /> |-<br /> |'''Kinematics of the Young Stellar Objects associated with the Cometary Globules in the Gum Nebula''' <br /> Authors: Rumpa Choudhury, H. C. Bhatt<br /> (Submitted on 26 Nov 2008)<br /> <br /> http://arxiv.org/PS_cache/arxiv/pdf/0811/0811.4389v1.pdf<br /> <br /> <br /> |Best I've found so far: Article on motion of YSOs in CGs in Gum Nebula (including CG4). There is a list of YSOs in the Gum Nebula, including 8 in or near CG4. In addition to the list, there's an outside chance it might help us determine if YSOs are members of the cluster or if we kick them off the island. (Note: I didn't say it was good - only the best I'd found so far...)<br /> |Thumbs up<br /> <br /> |-<br /> |'''Star formation in Bok globules and low-mass clouds. V : Hα emission stars near Sa 101, CG13 and CG22''' <br /> Author(s)REIPURTH B. (1) ; PETERSSON B. ;<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1993A%26A...267..439R&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> <br /> |Maybe useful. I think this is an early (or maybe the first) article establishing low-mass star formation in CG4. There is a list of objects, but not many in CG4. It is cited by others. Kind of old. (Reipurth is pretty big into this stuff - editor of The Star Formation Newsletter has publications from 1960s to today)<br /> <br /> |Thumbs up (I think)<br /> <br /> |-<br /> |Low Mass Star Formation in the Gum Nebula<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?2003ASPC..287..275K&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> <br /> |Limited use. This is a paper presentation by Serena Kim for Astronomical Society of the Pacific. It compares another nearby region to CG4. May be useful to as a gague for how many YSOs we might find in CG4????<br /> |Qualified Thumbs up<br /> <br /> |-<br /> |Star formation in Bok globules and low-mass clouds<br /> Author REIPURTH B.<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1987A%26AS...70...69P&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> |Limited use. Older article - cited by Kim about CG4 YSOs, but I don't see anything on CG4 here, just the area. <br /> |Thumbs down<br /> |-<br /> |An Objective-prism Survey of Ha-emmission-line stars of a field in Puppis <br /> Author PETERSSON B.<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1983A%26A...117..183R&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> |Limited use. Another old one, sort of outlines the CG4 area. Cited by others.<br /> |Thumbs down<br /> |-<br /> <br /> |Title: Probing environment and circumstellar disk evolution in triggered star forming regions: IRAC and MIPS imaging of bright-rimmed globules CG4/SA101 and CG30/31 <br /> Authors: Kim, Jinyoung Serena; Sherry, Wiiliam<br /> <br /> http://adsabs.harvard.edu/abs/2005sptz.prop20714K<br /> |Limited use. Spitzer application, but directly related to what we are doing. No paper to read.<br /> |Thumbs down<br /> |-<br /> <br /> |Title: Star Formation in the Gum Nebula: Cometary Globules CG4/6/SA101 <br /> Authors: Kim, Jinyoung S.; Walter, F. M.; Wolk, S. J.; Sherry, W. H.; Foster, M. <br /> <br /> http://adsabs.harvard.edu/abs/2006AAS...20921915K<br /> <br /> |Limited use. Just an abstract. No paper to read. <br /> |Thumbs down<br /> |-<br /> <br /> |}<br /> <br /> <br /> <br /> --Let me know if the first couple are helpful. I feel like I'm finding interesting stuff, but not what we really need. <br /> --klm<br /> <br /> =Existing observations=<br /> <br /> Wiki page on searching Leopard is part of [[How do I download data from the Spitzer Telescope?]]. You probably want specifically [[How can I find any prior observations for an object?]] Visualization instructions: http://coolwiki.ipac.caltech.edu/index.php/How_do_I_download_data_from_the_Spitzer_Telescope%3F#Visualize_AOR_using_Leopard_.28optional_but_useful_if_truly_new_at_this.29<br /> <br /> =Education=<br /> <br /> Viv's assignment in the group was to organize the Education portion of our proposal. What if we make a case for the importance of:<br /> # Teacher/Student/Scientist Scientific Research within the context of today's national and education initiatives. <br /> # NITARP as a Professional Learning Community offering a Center of Strength in Science Teacher Leadership<br /> # Include the variety of expected student populations and levels of participation, considering how we might measure impact across these groups. <br /> <br /> Each team member: Please briefly describe your own science education objectives for your student team, your plan for selecting students, and your expectation for being able to influence a broader community of teachers and/or students through this NITARP proposal. If you have any ideas about assessment or ideas about competencies the students will demonstrate as their knowledge and skills grow throughout the project, please make note of them. It would be nice to be able to track performance as we progress through the project. Also we should probably include items such as taking responsibility as members of a team, mentoring others, etc. <br /> <br /> [http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/r3-lynds/LyndsProposal.pdf] Link to a previous project ''Star Formation in Lynds Dark Nebulae'' in which Chelen was one of the team members. Refer to <br /> this to see how they framed their education section. <br /> <br /> http://www.nagb.org/publications/frameworks/science-09.pdf Science Framework for the 2009 National Assessment of Educational Progress (NAEP) by the National Assessment Governing Board, 800 North Capitol Street, N.W., Suite 825, Washington, DC 20002-4233 [http://www.nagb.org/publications/frameworks/science-09.pdf] U.S. Department of Education <br /> ''<br /> ''''The framework reflects the nature and practice of science. The National Standards<br /> and Benchmarks include standards that address science as inquiry, nature of science, history of science, and the manmade world. The framework should emphasize the importance of these aspects of science education and should include the expectation that students will understand the nature and practice of science.'' page 5<br /> <br /> ''An assessment framework is a subset of the achievement universe from which assessment developers must choose to develop sets of items that can be assessed within time and resource constraints. Hence, the science content to be assessed by NAEP has been identified as that considered central to the Physical, Life, and Earth and Space Sciences. As a result, some important outcomes<br /> of science education that are difficult and time consuming to measure (such as habits of mind, sustained inquiry, and collaborative research), but valued by scientists, science educators, and the business community, will be only partially represented in the framework and in the NAEP Science Assessment. Moreover, the wide range of science standards in the guiding national documents that could be incorporated into the framework had to be reduced in number so as to allow some indepth probing of fundamental science content. As a result, the framework and the specifications represent a careful distillation that is not a complete representation of the original universe of achievement outcomes desirable for science education.'' p8<br /> <br /> ''TIME AND RESOURCE CONSTRAINTS<br /> What NAEP can assess is limited by time and resources. Like most standardized assessments, NAEP is an “on-demand” assessment. It ascertains what students know and can do in a limited amount of time (50 minutes for paper-and-pencil questions and, for a subset<br /> of students sampled, an additional 30 minutes for hands-on performance or interactive computer tasks) and with limited access to resources (e.g., reference materials, feedback from peers and teachers, opportunities for reflection and revision). The national and state standards, however, contain goals that require extended time (days, weeks, or months). Therefore, to assess student achievement in the kinds of extended activities that are a central feature of the national and state standards and many science curricula, it would be necessary to know (for example) the quality of students’:<br /> •<br /> reasoning while framing their research questions;<br /> •<br /> planning for data collection and the execution of the plan<br /> •<br /> abilities to meet unpredictable challenges that arise during an actual, ongoing scientific<br /> investigation;<br /> •<br /> lines of argument in deciding how to alter their experimental approach in the light of new evidence;<br /> •<br /> engagement with fellow students and/or the teacher in interpreting an observation or result and deciding what to do about it; and<br /> •<br /> deliberations and reasoning when settling on the defensible conclusions that might be drawn from their work.<br /> <br /> Like other on-demand assessments, NAEP cannot be used to draw conclusions about student<br /> achievement with respect to the full range of goals of science education. States, districts,<br /> schools, and teachers can supplement NAEP and other standardized assessments to assess the full range of science education standards. In addition to describing the content and format of an examination, assessment frameworks like this one signal to the public and to teachers the elements of a subject that are important. The absence of extended inquiry in NAEP, however, is not intended to signal its relative importance in the curriculum.<br /> Indeed, because of the significance of inquiry in science education, the framework promotes as much consideration of inquiry as can be accomplished within the time and resources available for assessment.'' pages 8-9<br /> ''''<br /> <br /> <br /> <br /> I like these three strands. Great idea, Viv.<br /> --chj 17:19 CST 13-Jan-2010.<br /> <br /> <br /> Nice Topic Breakdown; would be difficult to quantify ed outcome at such diverse ages/locations/populations as exist at Breck-Yerkes-OPRF High-Pierce College, any other way. --[[User:Mallory|Mallory]] 18:41, 18 January 2010 (PST)<br /> '''''Bold text'''''<br /> <br /> <br /> test--[[User:Mallory|Mallory]] 15:27, 26 January 2010 (PST)<br /> <br /> CG4-Spitzer Ed Plan For Pierce College.doc<br /> <br /> Students will be recruited by in-class announcements and through (large, inclusive) Pierce College Astronomy Society. Astron Society semester sched is always distributed throughout campus, and meetings announced on marquee/college newspaper; (26,000 enrollment.) Astron Soc Semester Sched will include on it, “Use live data from NASA space telescopes; use cool software, plus your own analytical skills to make science discoveries! Join Team today!” Notation on your college transcript. <br /> <br /> Application for team inclusion will ask students: how interested are you in the actual process of science-designing activities to accomplish specific purpose + data gathering + analysis + reach conclusions. Are you willing to devote extra time to read, learn some new applications, and plan the work we will do? Are you free to go to Cal Tech for three days, June 14 – 16? Application will also ask: college major, math-computer-lab abilities, analysis and interpretation skills, dependability, ambition!<br /> <br /> Students incorporated into team must know physical science basics in; matter states, spectroscopy, magnitude scale/photometry, Newton’s + Kepler’s + Wien’s + Stefan-Boltzmann Laws, Conservation Laws, nebulae and star formation, inquiry design. Any student who comes from another instructor, can be evaluated by that person.<br /> <br /> Science Ed Objectives and Performance Expectations: One of the major current science ed objectives is for students to be able to take data and extract meaning from it. That is a huge part of why I am glad to be part of NITARP/learn how to do that! Students will have to plan their own data gathering, organization, and analysis, to answer specific questions. They’ll have to be able to revise methods if the selected actions don’t yield answers; use Teamwork in data collection and analysis, and reaching conclusions. Students will have to be able to explain and defend their conclusions.<br /> <br /> There are significant ways in which NITARP can be shared within my institution, and every one of them builds the educational strength of the college! First, I’m strengthened significantly from research/software/process exposure, already. What has gone into my brain will come out in my teaching, and thus be shared. Students who enter the program receive significant boosts in their own scientific skills and processes, then they will share with other students and multiply the effects that way. Team Students will be specifically directed to ask the ‘more modestly endowed’ students for input, and then to consider that input thoughtfully. There is a monthly Faculty Lunch, and guess who will be speakers at that event. My department has periodic meetings and it will be keen to invite students to give presentations to those eager ears. Other instructors can ask for presentations.<br /> <br /> My students are Special! Many are first generation College Students, whose parents don’t speak English. Some have babies; struggle with money, time, and academic proficiency. They need to be reinforced in their desire to obtain an education, and they need education perks. Other students/smaller percentage, are spoiled brats from wealthy surrounding suburbs, who think their instructors should do their work and then give them good grades! Often they’re academically capable, but too ‘entitled’ to reach for proficiency; just as great a loss if they under-achieve.<br /> <br /> <br /> <br /> --[[User:Mallory|Mallory]] 17:35, 26 January 2010 (PST)<br /> <br /> =New questions=<br /> <br /> In continuing CG4/Low Mass Star Formation background research, this issue is of interest,and understanding may lead to further idea development: What do Outflows from regions of increased density really represent? It could have catastrophic influence on star formation? --[[User:Mallory|Mallory]] 12:48, 20 January 2010 (PST)<br /> <br /> http://coolwiki.ipac.caltech.edu/index.php/Studying_Young_Stars</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=CG4_Proposal&diff=3924 2010-01-26T23:27:47Z

<p>Mallory: /* Education */</p> <hr /> <div>=Instructions=<br /> <br /> ==Previous Examples== <br /> All of the previous proposals are online, linked from the teams' Cool Cosmos page. All of the programs are listed here:<br /> http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/allprog.shtml<br /> and if you go to any of the team pages, you'll see lots of things, including a link to the proposal.<br /> <br /> BUT PLEASE NOTE that all of these past proposals were OBSERVING proposals and you are writing an ARCHIVAL proposal.<br /> <br /> ==Recommended Contents==<br /> In general, good proposals should have:<br /> * introduction and context. how you picked the target(s) and why. background on subject and target. educated guesses on what you might find.<br /> * detailed information on what data are available, and what you plan to do with it (e.g. much more than &quot;i'm sure spitzer observed this at some point&quot;). how you are going to reduce the data. kind of analysis planned.<br /> * education/outreach plan. what your team will do, individually or together.<br /> <br /> You don't have page limits, but nor do you want the review committee<br /> annoyed because you made them read a book.... or tiny fonts. A professor<br /> in grad school always used to annoy me with broad essay questions followed<br /> by the instruction &quot;Be brief but specific.&quot; But he's right ...<br /> <br /> <br /> <br /> =Background information=<br /> <br /> example table <br /> <br /> {| border=&quot;1&quot;<br /> |Table example <br /> | example2 <br /> | example3<br /> |-<br /> |line2<br /> |line2<br /> |line2<br /> |}<br /> <br /> <br /> <br /> Identifiers (aliases) for CG 4 ...<br /> ''BHR 21, <br /> Sandqvist 103, <br /> FEST 2-30, <br /> DCld 259.4-12.7''<br /> <br /> I found this by typing ''CG4'' into SIMBAD. The results were in the middle of the page. Scrolling down further, there's a list of 20 articles in which CG 4 is mentioned.<br /> <br /> Talk to you on Wednesday!<br /> --chj<br /> <br /> <br /> My Plan to continue Lit. search--[[User:Mallory|Mallory]] 23:35, 11 January 2010 (PST) is to finish SIMBAD, then go to ADS and to find a way to confirm and quantify lots! of IR present in suspected YSOs in CG4(probably by opacity class) and little UV/max not to exceed a threshold to be determined; don't want the object to be a middle-aged star already.<br /> <br /> Is it the group's intention to consider locations outside of CG4, which could be cluster members? <br /> <br /> --[[User:Mallory|Mallory]] 23:28, 11 January 2010 (PST)Carolyn<br /> <br /> <br /> <br /> In a search through SIMBAD for CG 4 info, some interesting info and unanswered questions have emerged.<br /> <br /> If a gaseous region were collapsing due to a radiation-driven implosion, what's to stop it from rebounding back out, and how would we know the mechanism had occurred? Maybe by the length of tails (also created by outward pressures)? Is this a safe assumption?<br /> There seems to be a conflict between different analyses as to whether tails can be traced by CO(12) spectra. How to resolve? <br /> If collapse/expansion, and rotation can occur all in the same region, are there any tools other than redshift to sort out what is happening?<br /> Interesting that there could be more than one &quot;Center of Influence' in a region, i.e. massive star,--[[User:Mallory|Mallory]] 15:48, 12 January 2010 (PST) whose radiation influences the CG's/YSO's evolution.<br /> <br /> <br /> ''Carolyn, I moved your latest research here to the Background Section, and took it out of the Education section. Nice Job in finding information. - Viv''<br /> <br /> Hey. No Fair. Carolyn is thinking while she reads! Nice work Carolyn. 14 jan 10 <br /> --klm<br /> <br /> <br /> The following is a summary of info describing the CG4 environment, and includes a small amount of info from other areas qualitatively similar to the Gum Nebula area. The environmental characteristics listed will describe the environment needed for star formation, confirmed by the presence of YSOs in the--[[User:Mallory|Mallory]] 22:24, 13 January 2010 (PST) region:<br /> <br /> -cg4 resides in the Gum Nebula, within the constellation Puppis, adjacent to Vela. This area is 1,300 LY distant from Solar System, and even visually, is laced with plentiful clouds of gas and dust.<br /> <br /> -using appropriate wavelengths, should do a search for nearby massive O &amp; B stars (typical neighborhood bullies)to determine the possibility of photoevaporation of coalescing dust and gas taking place in newly formed stars, and if so, switch area being investigated. Cometary Globule tails all coinciding in direction they're pointing is another indication that newly forming stars are being photoevaporated by nearby large star radiation/emissions. There can be a number of Centers of Influence near a newly forming Star Cluster, check this optically, in radio, and in both UV and Xray.<br /> <br /> -Note that radiation driven implosion also occurs, as well as collapse due to gravitational attraction. Do muiltiwavelength study. Radio wavelengths especially.<br /> <br /> -Expect IR excess in area of star formation (Universal Gas Law; volume mass forming star decreases/temp increase) Necessary to determine the average value for IR around a small mass Main Sequence star, so we know what amount defines 'excess IR'.<br /> <br /> - If head of cometary nebula is opaque in visible wavelengths, it can be assumed that sufficient gas and dust exist in the nebula to create new stars. Thus, opacity/Opacity Class, is an indicator of star-forming region BUT needs to be quantified and observed in the appropriate wavelengths/optical photometry/MIPS data probably.<br /> <br /> - Information about contraction/expansion/rotation, can be obtained from red-blue shift observations. This is necessary information! Personal question; could implosion produce an outward rebound?<br /> <br /> -Spectroscopic info can reveal the age/stage of development of baby stars uncovered in this study. Use MIPS data.<br /> <br /> -To determine which stars visible in same area are members of the same CG4 Cluster, see common age/convection % compared to radiation &amp; conduction, speed of rotation (need to know axis of rotation to determine blue-red shift anyway), variability, spatial location, and spatial motion of all the local stars/i.e. do they seem to be moving as a group/cluster. All of these qualities are indicators of the age of a YSO.<br /> <br /> -Excess IR (define 'excess' as variation from average IR emission from a similar mass young Main Sequence star IR average emissions) typifies newly forming stars, such as what we are looking for in CG4. Conflict in literature about UV emissions; forming star should have almost none/core processes do not yet produce, but very young stars can have a lot of UV emission due to rapid rotation. Supposedly, really young stars have low Magnetic Field.<br /> <br /> -Another variable of which to be aware, is the number of YSOs in a given area. Too many, and only those with largest relative mass will grow to be stars, since largest mass baby stars have the gravitational-strength advantage/capture the most infalling gas+dust. (Think nestfull of eagle eggs, which hatch at different times.)<br /> <br /> The sources listed below indicate that these are the qualities in nebulae which affect Star Formation. <br /> <br /> Carolyn Mallory<br /> <br /> Sources Used to Gather This information Include but are Not Limited to:<br /> SIMBAD, ic 2118, ADS, CoolWiki Finding Cluster Members, Spitzer Archives, Infrared Handbook by Wolfe &amp; Zissie.<br /> <br /> here is the paper from serena from 2005<br /> http://adsabs.harvard.edu/abs/2005AJ....129.1564K<br /> --[[User:Rebull|Rebull]] 15:57, 13 January 2010 (PST)<br /> <br /> Title: Low-Mass Star Formation in the Gum Nebula: The CG 30/31/38 Complex<br /> Authors: Kim, Jinyoung Serena; Walter, Frederick M.; Wolk, Scott J.<br /> Affiliation: AA(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.; Visiting Astronomer, Cerro Tololo Inter-American Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under contact with the National Science Foundation.), AB(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.), AC(Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.)<br /> Publication: The Astronomical Journal, Volume 129, Issue 3, pp. 1564-1579. (AJ Homepage)<br /> Publication Date:03/2005<br /> Origin:UCP<br /> AJ Keywords:Stars: Circumstellar Matter, ISM: H II Regions, ISM: Globules, Stars: Formation, Stars: Low-Mass, Brown Dwarfs, Stars: Pre-Main-Sequence<br /> DOI:10.1086/428002<br /> Bibliographic Code:2005AJ....129.1564K<br /> <br /> Abstract<br /> We present photometric and spectroscopic results for the low-mass pre-main-sequence (PMS) stars with spectral types K-M in the cometary globule (CG) 30/31/38 complex. We obtained multiobject high-resolution spectra for the targets selected as possible PMS stars from multiwavelength photometry. We identified 11 PMS stars brighter than V=16.5 with ages &lt;~5 Myr at a distance of approximately 200 pc. The spatial distribution of the PMS stars, CG clouds, and ionizing sources (O stars and supernova remnants) suggests a possible triggered origin of the star formation in this region. We confirm the youth of the photometrically selected PMS stars using the lithium abundances. The radial velocities of the low-mass PMS stars are consistent with those of the cometary globules. Most of the PMS stars show weak Hα emission with Wλ(Hα)&lt;10 Å. Only one out of the 11 PMS stars shows a moderate near-IR excess, which suggests a short survival time (t&lt;5 Myr) of circumstellar disks in this star-forming environment. In addition, we find five young late-type stars and one Ae star that have no obvious relation to the CG 30/31/38 complex. We also discuss a possible scenario of the star formation history in the CG 30/31/38 region. <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> <br /> --Some background papers I found:<br /> <br /> <br /> <br /> <br /> <br /> {| border=&quot;1&quot;<br /> |Article <br /> | Comments <br /> | Comments on Comments<br /> |-<br /> |'''Kinematics of the Young Stellar Objects associated with the Cometary Globules in the Gum Nebula''' <br /> Authors: Rumpa Choudhury, H. C. Bhatt<br /> (Submitted on 26 Nov 2008)<br /> <br /> http://arxiv.org/PS_cache/arxiv/pdf/0811/0811.4389v1.pdf<br /> <br /> <br /> |Best I've found so far: Article on motion of YSOs in CGs in Gum Nebula (including CG4). There is a list of YSOs in the Gum Nebula, including 8 in or near CG4. In addition to the list, there's an outside chance it might help us determine if YSOs are members of the cluster or if we kick them off the island. (Note: I didn't say it was good - only the best I'd found so far...)<br /> |Thumbs up<br /> <br /> |-<br /> |'''Star formation in Bok globules and low-mass clouds. V : Hα emission stars near Sa 101, CG13 and CG22''' <br /> Author(s)REIPURTH B. (1) ; PETERSSON B. ;<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1993A%26A...267..439R&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> <br /> |Maybe useful. I think this is an early (or maybe the first) article establishing low-mass star formation in CG4. There is a list of objects, but not many in CG4. It is cited by others. Kind of old. (Reipurth is pretty big into this stuff - editor of The Star Formation Newsletter has publications from 1960s to today)<br /> <br /> |Thumbs up (I think)<br /> <br /> |-<br /> |Low Mass Star Formation in the Gum Nebula<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?2003ASPC..287..275K&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> <br /> |Limited use. This is a paper presentation by Serena Kim for Astronomical Society of the Pacific. It compares another nearby region to CG4. May be useful to as a gague for how many YSOs we might find in CG4????<br /> |Qualified Thumbs up<br /> <br /> |-<br /> |Star formation in Bok globules and low-mass clouds<br /> Author REIPURTH B.<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1987A%26AS...70...69P&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> |Limited use. Older article - cited by Kim about CG4 YSOs, but I don't see anything on CG4 here, just the area. <br /> |Thumbs down<br /> |-<br /> |An Objective-prism Survey of Ha-emmission-line stars of a field in Puppis <br /> Author PETERSSON B.<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1983A%26A...117..183R&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> |Limited use. Another old one, sort of outlines the CG4 area. Cited by others.<br /> |Thumbs down<br /> |-<br /> <br /> |Title: Probing environment and circumstellar disk evolution in triggered star forming regions: IRAC and MIPS imaging of bright-rimmed globules CG4/SA101 and CG30/31 <br /> Authors: Kim, Jinyoung Serena; Sherry, Wiiliam<br /> <br /> http://adsabs.harvard.edu/abs/2005sptz.prop20714K<br /> |Limited use. Spitzer application, but directly related to what we are doing. No paper to read.<br /> |Thumbs down<br /> |-<br /> <br /> |Title: Star Formation in the Gum Nebula: Cometary Globules CG4/6/SA101 <br /> Authors: Kim, Jinyoung S.; Walter, F. M.; Wolk, S. J.; Sherry, W. H.; Foster, M. <br /> <br /> http://adsabs.harvard.edu/abs/2006AAS...20921915K<br /> <br /> |Limited use. Just an abstract. No paper to read. <br /> |Thumbs down<br /> |-<br /> <br /> |}<br /> <br /> <br /> <br /> --Let me know if the first couple are helpful. I feel like I'm finding interesting stuff, but not what we really need. <br /> --klm<br /> <br /> =Existing observations=<br /> <br /> Wiki page on searching Leopard is part of [[How do I download data from the Spitzer Telescope?]]. You probably want specifically [[How can I find any prior observations for an object?]] Visualization instructions: http://coolwiki.ipac.caltech.edu/index.php/How_do_I_download_data_from_the_Spitzer_Telescope%3F#Visualize_AOR_using_Leopard_.28optional_but_useful_if_truly_new_at_this.29<br /> <br /> =Education=<br /> <br /> Viv's assignment in the group was to organize the Education portion of our proposal. What if we make a case for the importance of:<br /> # Teacher/Student/Scientist Scientific Research within the context of today's national and education initiatives. <br /> # NITARP as a Professional Learning Community offering a Center of Strength in Science Teacher Leadership<br /> # Include the variety of expected student populations and levels of participation, considering how we might measure impact across these groups. <br /> <br /> Each team member: Please briefly describe your own science education objectives for your student team, your plan for selecting students, and your expectation for being able to influence a broader community of teachers and/or students through this NITARP proposal. If you have any ideas about assessment or ideas about competencies the students will demonstrate as their knowledge and skills grow throughout the project, please make note of them. It would be nice to be able to track performance as we progress through the project. Also we should probably include items such as taking responsibility as members of a team, mentoring others, etc. <br /> <br /> <br /> [http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/r3-lynds/LyndsProposal.pdf] Link to a previous project ''Star Formation in Lynds Dark Nebulae'' in which Chelen was one of the team members. Refer to this to see how they framed their education section. <br /> <br /> http://www.nagb.org/publications/frameworks/science-09.pdf Science Framework for the 2009 National Assessment of Educational Progress (NAEP) by the National Assessment Governing Board, 800 North Capitol Street, N.W., Suite 825, Washington, DC 20002-4233 [http://www.nagb.org/publications/frameworks/science-09.pdf] U.S. Department of Education <br /> ''<br /> ''''The framework reflects the nature and practice of science. The National Standards<br /> and Benchmarks include standards that address science as inquiry, nature of science, history of science, and the manmade world. The framework should emphasize the importance of these aspects of science education and should include the expectation that students will understand the nature and practice of science.'' page 5<br /> <br /> ''An assessment framework is a subset of the achievement universe from which assessment developers must choose to develop sets of items that can be assessed within time and resource constraints. Hence, the science content to be assessed by NAEP has been identified as that considered central to the Physical, Life, and Earth and Space Sciences. As a result, some important outcomes<br /> of science education that are difficult and time consuming to measure (such as habits of mind, sustained inquiry, and collaborative research), but valued by scientists, science educators, and the business community, will be only partially represented in the framework and in the NAEP Science Assessment. Moreover, the wide range of science standards in the guiding national documents that could be incorporated into the framework had to be reduced in number so as to allow some indepth probing of fundamental science content. As a result, the framework and the specifications represent a careful distillation that is not a complete representation of the original universe of achievement outcomes desirable for science education.'' p8<br /> <br /> ''TIME AND RESOURCE CONSTRAINTS<br /> What NAEP can assess is limited by time and resources. Like most standardized assessments, NAEP is an “on-demand” assessment. It ascertains what students know and can do in a limited amount of time (50 minutes for paper-and-pencil questions and, for a subset<br /> of students sampled, an additional 30 minutes for hands-on performance or interactive computer tasks) and with limited access to resources (e.g., reference materials, feedback from peers and teachers, opportunities for reflection and revision). The national and state standards, however, contain goals that require extended time (days, weeks, or months). Therefore, to assess student achievement in the kinds of extended activities that are a central feature of the national and state standards and many science curricula, it would be necessary to know (for example) the quality of students’:<br /> •<br /> reasoning while framing their research questions;<br /> •<br /> planning for data collection and the execution of the plan<br /> •<br /> abilities to meet unpredictable challenges that arise during an actual, ongoing scientific<br /> investigation;<br /> •<br /> lines of argument in deciding how to alter their experimental approach in the light of new evidence;<br /> •<br /> engagement with fellow students and/or the teacher in interpreting an observation or result and deciding what to do about it; and<br /> •<br /> deliberations and reasoning when settling on the defensible conclusions that might be drawn from their work.<br /> <br /> Like other on-demand assessments, NAEP cannot be used to draw conclusions about student<br /> achievement with respect to the full range of goals of science education. States, districts,<br /> schools, and teachers can supplement NAEP and other standardized assessments to assess the full range of science education standards. In addition to describing the content and format of an examination, assessment frameworks like this one signal to the public and to teachers the elements of a subject that are important. The absence of extended inquiry in NAEP, however, is not intended to signal its relative importance in the curriculum.<br /> Indeed, because of the significance of inquiry in science education, the framework promotes as much consideration of inquiry as can be accomplished within the time and resources available for assessment.'' pages 8-9<br /> ''''<br /> <br /> <br /> <br /> I like these three strands. Great idea, Viv.<br /> --chj 17:19 CST 13-Jan-2010.<br /> <br /> <br /> Nice Topic Breakdown; would be difficult to quantify ed outcome at such diverse ages/locations/populations as exist at Breck-Yerkes-OPRF High-Pierce College, any other way. --[[User:Mallory|Mallory]] 18:41, 18 January 2010 (PST)<br /> '''''Bold text'''''<br /> <br /> <br /> test--[[User:Mallory|Mallory]] 15:27, 26 January 2010 (PST)<br /> <br /> =New questions=<br /> <br /> In continuing CG4/Low Mass Star Formation background research, this issue is of interest,and understanding may lead to further idea development: What do Outflows from regions of increased density really represent? It could have catastrophic influence on star formation? --[[User:Mallory|Mallory]] 12:48, 20 January 2010 (PST)<br /> <br /> http://coolwiki.ipac.caltech.edu/index.php/Studying_Young_Stars</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3833 2010-01-20T20:48:01Z

<p>Mallory: </p> <hr /> <div>In continuing CG4/Low Mass Star Formation background research, this issue is of interest,and understanding may lead to further idea development: What do Outflows from regions of increased density really represent? It could have catastrophic influence on star formation? --[[User:Mallory|Mallory]] 12:48, 20 January 2010 (PST)</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:CG4_Proposal&diff=3814 2010-01-19T02:41:25Z

<p>Mallory: </p> <hr /> <div>== CG4 Discussion Page ==<br /> <br /> <br /> == Education ==<br /> <br /> Viv's assignment in the group was to organize the Education portion of our proposal. What if we make a case for the importance of:<br /> 1. Teacher/Student/Scientist Scientific Research within the context of today's national and education initiatives. <br /> 2. NITARP as a Professional Learning Community offering a Center of Strength in Science Teacher Leadership<br /> 3. Include the variety of expected student populations and levels of participation, considering how we might measure impact across these groups.<br /> <br /> <br /> I like these three strands. Great idea, Viv.<br /> --chj 17:19 CST 13-Jan-2010.<br /> <br /> Nice Topic Breakdown; would be difficult to quantify ed outcome at such diverse ages/locations/populations as exist at Breck-Yerkes-OPRF High-Pierce College, any other way. --[[User:Mallory|Mallory]] 18:41, 18 January 2010 (PST)</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=CG4_Proposal&diff=3813 2010-01-19T02:26:00Z

<p>Mallory: /* Background information */</p> <hr /> <div>=Instructions=<br /> <br /> ==Previous Examples== <br /> All of the previous proposals are online, linked from the teams' Cool Cosmos page. All of the programs are listed here:<br /> http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/allprog.shtml<br /> and if you go to any of the team pages, you'll see lots of things, including a link to the proposal.<br /> <br /> BUT PLEASE NOTE that all of these past proposals were OBSERVING proposals and you are writing an ARCHIVAL proposal.<br /> <br /> ==Recommended Contents==<br /> In general, good proposals should have:<br /> * introduction and context. how you picked the target(s) and why. background on subject and target. educated guesses on what you might find.<br /> * detailed information on what data are available, and what you plan to do with it (e.g. much more than &quot;i'm sure spitzer observed this at some point&quot;). how you are going to reduce the data. kind of analysis planned.<br /> * education/outreach plan. what your team will do, individually or together.<br /> <br /> You don't have page limits, but nor do you want the review committee<br /> annoyed because you made them read a book.... or tiny fonts. A professor<br /> in grad school always used to annoy me with broad essay questions followed<br /> by the instruction &quot;Be brief but specific.&quot; But he's right ...<br /> <br /> <br /> <br /> =Background information=<br /> <br /> Identifiers (aliases) for CG 4 ...<br /> ''BHR 21, <br /> Sandqvist 103, <br /> FEST 2-30, <br /> DCld 259.4-12.7''<br /> <br /> I found this by typing ''CG4'' into SIMBAD. The results were in the middle of the page. Scrolling down further, there's a list of 20 articles in which CG 4 is mentioned.<br /> <br /> Talk to you on Wednesday!<br /> --chj<br /> <br /> <br /> My Plan to continue Lit. search--[[User:Mallory|Mallory]] 23:35, 11 January 2010 (PST) is to finish SIMBAD, then go to ADS and to find a way to confirm and quantify lots! of IR present in suspected YSOs in CG4(probably by opacity class) and little UV/max not to exceed a threshold to be determined; don't want the object to be a middle-aged star already.<br /> <br /> Is it the group's intention to consider locations outside of CG4, which could be cluster members? <br /> <br /> --[[User:Mallory|Mallory]] 23:28, 11 January 2010 (PST)Carolyn<br /> <br /> <br /> <br /> In a search through SIMBAD for CG 4 info, some interesting info and unanswered questions have emerged.<br /> <br /> If a gaseous region were collapsing due to a radiation-driven implosion, what's to stop it from rebounding back out, and how would we know the mechanism had occurred? Maybe by the length of tails (also created by outward pressures)? Is this a safe assumption?<br /> There seems to be a conflict between different analyses as to whether tails can be traced by CO(12) spectra. How to resolve? <br /> If collapse/expansion, and rotation can occur all in the same region, are there any tools other than redshift to sort out what is happening?<br /> Interesting that there could be more than one &quot;Center of Influence' in a region, i.e. massive star,--[[User:Mallory|Mallory]] 15:48, 12 January 2010 (PST) whose radiation influences the CG's/YSO's evolution.<br /> <br /> <br /> ''Carolyn, I moved your latest research here to the Background Section, and took it out of the Education section. Nice Job in finding information. - Viv''<br /> <br /> Hey. No Fair. Carolyn is thinking while she reads! Nice work Carolyn. 14 jan 10 <br /> --klm<br /> <br /> <br /> The following is a summary of info describing the CG4 environment, and includes a small amount of info from other areas qualitatively similar to the Gum Nebula area. The environmental characteristics listed will describe the environment needed for star formation, confirmed by the presence of YSOs in the--[[User:Mallory|Mallory]] 22:24, 13 January 2010 (PST) region:<br /> <br /> -cg4 resides in the Gum Nebula, within the constellation Puppis, adjacent to Vela. This area is 1,300 LY distant from Solar System, and even visually, is laced with plentiful clouds of gas and dust.<br /> <br /> -using appropriate wavelengths, should do a search for nearby massive O &amp; B stars (typical neighborhood bullies)to determine the possibility of photoevaporation of coalescing dust and gas taking place in newly formed stars, and if so, switch area being investigated. Cometary Globule tails all coinciding in direction they're pointing is another indication that newly forming stars are being photoevaporated by nearby large star radiation/emissions. There can be a number of Centers of Influence near a newly forming Star Cluster, check this optically, in radio, and in both UV and Xray.<br /> <br /> -Note that radiation driven implosion also occurs, as well as collapse due to gravitational attraction. Do muiltiwavelength study. Radio wavelengths especially.<br /> <br /> -Expect IR excess in area of star formation (Universal Gas Law; volume mass forming star decreases/temp increase) Necessary to determine the average value for IR around a small mass Main Sequence star, so we know what amount defines 'excess IR'.<br /> <br /> - If head of cometary nebula is opaque in visible wavelengths, it can be assumed that sufficient gas and dust exist in the nebula to create new stars. Thus, opacity/Opacity Class, is an indicator of star-forming region BUT needs to be quantified and observed in the appropriate wavelengths/optical photometry/MIPS data probably.<br /> <br /> - Information about contraction/expansion/rotation, can be obtained from red-blue shift observations. This is necessary information! Personal question; could implosion produce an outward rebound?<br /> <br /> -Spectroscopic info can reveal the age/stage of development of baby stars uncovered in this study. Use MIPS data.<br /> <br /> -To determine which stars visible in same area are members of the same CG4 Cluster, see common age/convection % compared to radiation &amp; conduction, speed of rotation (need to know axis of rotation to determine blue-red shift anyway), variability, spatial location, and spatial motion of all the local stars/i.e. do they seem to be moving as a group/cluster. All of these qualities are indicators of the age of a YSO.<br /> <br /> -Excess IR (define 'excess' as variation from average IR emission from a similar mass young Main Sequence star IR average emissions) typifies newly forming stars, such as what we are looking for in CG4. Conflict in literature about UV emissions; forming star should have almost none/core processes do not yet produce, but very young stars can have a lot of UV emission due to rapid rotation. Supposedly, really young stars have low Magnetic Field.<br /> <br /> -Another variable of which to be aware, is the number of YSOs in a given area. Too many, and only those with largest relative mass will grow to be stars, since largest mass baby stars have the gravitational-strength advantage/capture the most infalling gas+dust. (Think nestfull of eagle eggs, which hatch at different times.)<br /> <br /> The sources listed below indicate that these are the qualities in nebulae which affect Star Formation. <br /> <br /> Carolyn Mallory<br /> <br /> Sources Used to Gather This information Include but are Not Limited to:<br /> SIMBAD, ic 2118, ADS, CoolWiki Finding Cluster Members, Spitzer Archives, Infrared Handbook by Wolfe &amp; Zissie.<br /> <br /> here is the paper from serena from 2005<br /> http://adsabs.harvard.edu/abs/2005AJ....129.1564K<br /> --[[User:Rebull|Rebull]] 15:57, 13 January 2010 (PST)<br /> <br /> Title: Low-Mass Star Formation in the Gum Nebula: The CG 30/31/38 Complex<br /> Authors: Kim, Jinyoung Serena; Walter, Frederick M.; Wolk, Scott J.<br /> Affiliation: AA(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.; Visiting Astronomer, Cerro Tololo Inter-American Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under contact with the National Science Foundation.), AB(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.), AC(Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.)<br /> Publication: The Astronomical Journal, Volume 129, Issue 3, pp. 1564-1579. (AJ Homepage)<br /> Publication Date:03/2005<br /> Origin:UCP<br /> AJ Keywords:Stars: Circumstellar Matter, ISM: H II Regions, ISM: Globules, Stars: Formation, Stars: Low-Mass, Brown Dwarfs, Stars: Pre-Main-Sequence<br /> DOI:10.1086/428002<br /> Bibliographic Code:2005AJ....129.1564K<br /> <br /> Abstract<br /> We present photometric and spectroscopic results for the low-mass pre-main-sequence (PMS) stars with spectral types K-M in the cometary globule (CG) 30/31/38 complex. We obtained multiobject high-resolution spectra for the targets selected as possible PMS stars from multiwavelength photometry. We identified 11 PMS stars brighter than V=16.5 with ages &lt;~5 Myr at a distance of approximately 200 pc. The spatial distribution of the PMS stars, CG clouds, and ionizing sources (O stars and supernova remnants) suggests a possible triggered origin of the star formation in this region. We confirm the youth of the photometrically selected PMS stars using the lithium abundances. The radial velocities of the low-mass PMS stars are consistent with those of the cometary globules. Most of the PMS stars show weak Hα emission with Wλ(Hα)&lt;10 Å. Only one out of the 11 PMS stars shows a moderate near-IR excess, which suggests a short survival time (t&lt;5 Myr) of circumstellar disks in this star-forming environment. In addition, we find five young late-type stars and one Ae star that have no obvious relation to the CG 30/31/38 complex. We also discuss a possible scenario of the star formation history in the CG 30/31/38 region. <br /> <br /> <br /> http://adsabs.harvard.edu/abs/2006AAS...20921915K<br /> <br /> <br /> Title: Star Formation in the Gum Nebula: Cometary Globules CG4/6/SA101 <br /> Authors: Kim, Jinyoung S.; Walter, F. M.; Wolk, S. J.; Sherry, W. H.; Foster, M. <br /> Affiliation: AA(Univ. of Arizona), AB(Stony Brook University), AC(CfA), AD(NSO/NOAO), AE(Univ. of Arizona) <br /> Publication: 2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #219.15; Bulletin of the American Astronomical Society, Vol. 38, p.1205 <br /> Publication Date: 12/2006 <br /> Origin: AAS <br /> Bibliographic Code: 2006AAS...20921915K <br /> <br /> Abstract<br /> As a part of our on-going program to study star formation under various environments, we present preliminary results from our multi-wavelength study of a bright-rimmed cometary globule complex, CG4/6/SA101 in the Gum Nebula. These cometary clouds are photo-evaporating due to UV radiation from neighboring O stars (10 &lt; d &lt; 100 pc) in the Vela OB2 association. The intermediate and low-mass stars in these cometary clouds form in an environment that differs from both the quiet isolation of young stars in T-associations such as Taurus and the violently energetic environment like that of the Orion Nebula cluster (ONC). The moderate separation between the cometary clouds and the O stars creates a radiation environment that has an intensity intermediate between the Taurus and Orion star forming regions. Circumstellar material and accretion disks may last longer than those in ONC, yet may not survive as long as they would in an isolated region such as Taurus or TW Hya. We compare our results with other star forming regions under different environments. <br /> <br /> <br /> <br /> http://adsabs.harvard.edu/abs/2005sptz.prop20714K<br /> <br /> Title: Probing environment and circumstellar disk evolution in triggered star forming regions: IRAC and MIPS imaging of bright-rimmed globules CG4/SA101 and CG30/31 <br /> Authors: Kim, Jinyoung Serena; Sherry, Wiiliam <br /> Publication: Spitzer Proposal ID #20714 <br /> Publication Date: 06/2005 <br /> Origin: SPITZER <br /> Bibliographic Code: 2005sptz.prop20714K <br /> <br /> Abstract<br /> We propose to obtain IRAC and MIPS images of a newly discovered star forming region, cometary cloud complex CG~4/SA101 (Kim et al. 2005c). We also propose to acquire more complete IRAC and MIPS images of a cometary globule complex CG~30/31, where we found young stars (Kim et al. 2005a,c), but existing program by a Spitzer legacy team (c2d) did not observe. Both star forming complexes reside in the Gum Nebula, where early O stars, Wolf-Rayet star, supernovae remnants, and OB associations produce strong ionizing UV photons. These two star forming regions are in a photoevaporating cometary shaped bright-rimmed clouds, at few tens of parsecs away from the common center of main ionizing sources in the Gum Nebula, placing them in a 'intermediate' UV radiation field between Orion-like Strong radiation field regions and Taurus-like weak radiation field regions. We propose to perform comparative and statistical studies probing circumstellar disk characteristics and evolution in different star forming environments together with existing data of well-known star forming regions. The age range of the young stars in these regions (1-5 Myr old) is also of a great interest, because this is a time when transition from optically thick disks to optically thin debris disks occurs. Therefore, this proposed observations will provide an important dataset to study lifetime of inner disks and optically thick disk evolution in such environments. We probe yet another common mode of star formation, forming in groups in triggered mode or influenced by UV photons from nearby ionizing sources. Our dataset and study will contribute to a better understanding of star formation and circumstellar disk evolution linking well-known star forming regions in weak and strong radiation field environments. We believe that this dataset will also benefit other star formation and disk communities for various other studies in addition to existing dataset of clusters and associations, obtained by GTO, legacy, and GO1.<br /> <br /> <br /> <br /> --Some background papers I found in ADS:<br /> <br /> --Best I've found so far: Article on motion of YSOs in CGs in Gum Nebula (including CG4). There is a list of YSOs in the Gum Nebula, including 8 in or near CG4. In addition to the list, there's an outside chance it might help us determine if YSOs are members of the cluster or if we kick them off the island. (Note: I didn't say it was good - only the best I'd found so far...)<br /> <br /> http://arxiv.org/PS_cache/arxiv/pdf/0811/0811.4389v1.pdf<br /> <br /> '''Kinematics of the Young Stellar Objects associated with the Cometary Globules in the Gum Nebula''' <br /> Authors: Rumpa Choudhury, H. C. Bhatt<br /> (Submitted on 26 Nov 2008)<br /> <br /> --Maybe useful. I think this is an early (or maybe the first) article establishing low-mass star formation in CG4. There is a list of objects, but not many in CG4. It is cited by others. Kind of old. (Reipurth is pretty big into this stuff - editor of The Star Formation Newsletter has publications from 1960s to today)<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1993A%26A...267..439R&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> '''Star formation in Bok globules and low-mass clouds. V : Hα emission stars near Sa 101, CG13 and CG22''' <br /> Author(s)REIPURTH B. (1) ; PETERSSON B. ;<br /> <br /> --Limited use. This is a paper presentation by Serena Kim for Astronomical Society of the Pacific. It compares another nearby region to CG4. May be useful to as a gague for how many YSOs we might find in CG4???? <br /> <br /> Low Mass Star Formation in the Gum Nebula<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?2003ASPC..287..275K&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> --Limited use. Another old one, sort of outlines the CG4 area. Cited by others.<br /> <br /> An Objective-prism Survey of Ha-emmission-line stars of a field in Puppis <br /> Author PETERSSON B.<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1983A%26A...117..183R&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> --Limited use. Older article - cited by Kim about CG4 YSOs, but I don't see anything on CG4 here, just the area. <br /> <br /> Star formation in Bok globules and low-mass clouds<br /> Author REIPURTH B.<br /> <br /> http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1987A%26AS...70...69P&amp;amp;data_type=PDF_HIGH&amp;amp;whole_paper=YES&amp;amp;type=PRINTER&amp;amp;filetype=.pdf<br /> <br /> <br /> --Let me know if the first couple are helpful. I feel like I'm finding interesting stuff, but not what we really need. <br /> --klm<br /> <br /> =Existing observations=<br /> <br /> Wiki page on searching Leopard is part of [[How do I download data from the Spitzer Telescope?]]. You probably want specifically [[How can I find any prior observations for an object?]]<br /> <br /> =Education=<br /> <br /> Viv's assignment in the group was to organize the Education portion of our proposal. What if we make a case for the importance of:<br /> # Teacher/Student/Scientist Scientific Research within the context of today's national and education initiatives. <br /> # NITARP as a Professional Learning Community offering a Center of Strength in Science Teacher Leadership<br /> # Include the variety of expected student populations and levels of participation, considering how we might measure impact across these groups.<br /> <br /> <br /> I like these three strands. Great idea, Viv.<br /> --chj 17:19 CST 13-Jan-2010.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=CG4_Proposal&diff=3787 2010-01-14T06:24:38Z

<p>Mallory: </p> <hr /> <div>=Background information=<br /> <br /> Identifiers (aliases) for CG 4 ...<br /> ''BHR 21, <br /> Sandqvist 103, <br /> FEST 2-30, <br /> DCld 259.4-12.7''<br /> <br /> I found this by typing ''CG4'' into SIMBAD. The results were in the middle of the page. Scrolling down further, there's a list of 20 articles in which CG 4 is mentioned.<br /> <br /> Talk to you on Wednesday!<br /> --chj<br /> <br /> <br /> My Plan to continue Lit. search--[[User:Mallory|Mallory]] 23:35, 11 January 2010 (PST) is to finish SIMBAD, then go to ADS and to find a way to confirm and quantify lots! of IR (probably by opacity class) and little UV/max not to exceed a threshold to be determined; don't want the object to be a middle-aged star already.<br /> <br /> Is it the group's intention to consider locations outside of CG4, which could be cluster members? <br /> <br /> --[[User:Mallory|Mallory]] 23:28, 11 January 2010 (PST)Carolyn<br /> <br /> <br /> <br /> In a search through SIMBAD for CG 4 info, some interesting info and unanswered questions have emerged.<br /> <br /> If a gaseous region were collapsing due to a radiation-driven implosion, what's to stop it from rebounding back out, and how would we know the mechanism had occurred? Maybe by the length of tails (also created by outward pressures)? Is this a safe assumption?<br /> There seems to be a conflict between different analyses as to whether tails can be traced by CO(12) spectra. How to resolve? <br /> If collapse/expansion, and rotation can occur all in the same region, are there any tools other than redshift to sort out what is happening?<br /> Interesting that there could be more than one &quot;Center of Influence' in a region, i.e. massive star,--[[User:Mallory|Mallory]] 15:48, 12 January 2010 (PST) whose radiation influences the CG's evolution.<br /> <br /> chj, I'm not closely enough focused? Your ideas and suggestions?<br /> <br /> I'll continue info-gathering. You know, this is grinding but fun; it's interesting, and I'm figuring that the Laws of Physics are the same throughout the Universe.<br /> -C<br /> <br /> <br /> here is the paper from serena from 2005<br /> http://adsabs.harvard.edu/abs/2005AJ....129.1564K<br /> --[[User:Rebull|Rebull]] 15:57, 13 January 2010 (PST)<br /> <br /> Title: Low-Mass Star Formation in the Gum Nebula: The CG 30/31/38 Complex<br /> Authors: Kim, Jinyoung Serena; Walter, Frederick M.; Wolk, Scott J.<br /> Affiliation: AA(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.; Visiting Astronomer, Cerro Tololo Inter-American Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under contact with the National Science Foundation.), AB(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.), AC(Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.)<br /> Publication: The Astronomical Journal, Volume 129, Issue 3, pp. 1564-1579. (AJ Homepage)<br /> Publication Date:03/2005<br /> Origin:UCP<br /> AJ Keywords:Stars: Circumstellar Matter, ISM: H II Regions, ISM: Globules, Stars: Formation, Stars: Low-Mass, Brown Dwarfs, Stars: Pre-Main-Sequence<br /> DOI:10.1086/428002<br /> Bibliographic Code:2005AJ....129.1564K<br /> <br /> Abstract<br /> We present photometric and spectroscopic results for the low-mass pre-main-sequence (PMS) stars with spectral types K-M in the cometary globule (CG) 30/31/38 complex. We obtained multiobject high-resolution spectra for the targets selected as possible PMS stars from multiwavelength photometry. We identified 11 PMS stars brighter than V=16.5 with ages &lt;~5 Myr at a distance of approximately 200 pc. The spatial distribution of the PMS stars, CG clouds, and ionizing sources (O stars and supernova remnants) suggests a possible triggered origin of the star formation in this region. We confirm the youth of the photometrically selected PMS stars using the lithium abundances. The radial velocities of the low-mass PMS stars are consistent with those of the cometary globules. Most of the PMS stars show weak Hα emission with Wλ(Hα)&lt;10 Å. Only one out of the 11 PMS stars shows a moderate near-IR excess, which suggests a short survival time (t&lt;5 Myr) of circumstellar disks in this star-forming environment. In addition, we find five young late-type stars and one Ae star that have no obvious relation to the CG 30/31/38 complex. We also discuss a possible scenario of the star formation history in the CG 30/31/38 region. <br /> <br /> <br /> http://adsabs.harvard.edu/abs/2006AAS...20921915K<br /> <br /> <br /> Title: Star Formation in the Gum Nebula: Cometary Globules CG4/6/SA101 <br /> Authors: Kim, Jinyoung S.; Walter, F. M.; Wolk, S. J.; Sherry, W. H.; Foster, M. <br /> Affiliation: AA(Univ. of Arizona), AB(Stony Brook University), AC(CfA), AD(NSO/NOAO), AE(Univ. of Arizona) <br /> Publication: 2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #219.15; Bulletin of the American Astronomical Society, Vol. 38, p.1205 <br /> Publication Date: 12/2006 <br /> Origin: AAS <br /> Bibliographic Code: 2006AAS...20921915K <br /> <br /> Abstract<br /> As a part of our on-going program to study star formation under various environments, we present preliminary results from our multi-wavelength study of a bright-rimmed cometary globule complex, CG4/6/SA101 in the Gum Nebula. These cometary clouds are photo-evaporating due to UV radiation from neighboring O stars (10 &lt; d &lt; 100 pc) in the Vela OB2 association. The intermediate and low-mass stars in these cometary clouds form in an environment that differs from both the quiet isolation of young stars in T-associations such as Taurus and the violently energetic environment like that of the Orion Nebula cluster (ONC). The moderate separation between the cometary clouds and the O stars creates a radiation environment that has an intensity intermediate between the Taurus and Orion star forming regions. Circumstellar material and accretion disks may last longer than those in ONC, yet may not survive as long as they would in an isolated region such as Taurus or TW Hya. We compare our results with other star forming regions under different environments. <br /> <br /> <br /> <br /> http://adsabs.harvard.edu/abs/2005sptz.prop20714K<br /> <br /> Title: Probing environment and circumstellar disk evolution in triggered star forming regions: IRAC and MIPS imaging of bright-rimmed globules CG4/SA101 and CG30/31 <br /> Authors: Kim, Jinyoung Serena; Sherry, Wiiliam <br /> Publication: Spitzer Proposal ID #20714 <br /> Publication Date: 06/2005 <br /> Origin: SPITZER <br /> Bibliographic Code: 2005sptz.prop20714K <br /> <br /> Abstract<br /> We propose to obtain IRAC and MIPS images of a newly discovered star forming region, cometary cloud complex CG~4/SA101 (Kim et al. 2005c). We also propose to acquire more complete IRAC and MIPS images of a cometary globule complex CG~30/31, where we found young stars (Kim et al. 2005a,c), but existing program by a Spitzer legacy team (c2d) did not observe. Both star forming complexes reside in the Gum Nebula, where early O stars, Wolf-Rayet star, supernovae remnants, and OB associations produce strong ionizing UV photons. These two star forming regions are in a photoevaporating cometary shaped bright-rimmed clouds, at few tens of parsecs away from the common center of main ionizing sources in the Gum Nebula, placing them in a 'intermediate' UV radiation field between Orion-like Strong radiation field regions and Taurus-like weak radiation field regions. We propose to perform comparative and statistical studies probing circumstellar disk characteristics and evolution in different star forming environments together with existing data of well-known star forming regions. The age range of the young stars in these regions (1-5 Myr old) is also of a great interest, because this is a time when transition from optically thick disks to optically thin debris disks occurs. Therefore, this proposed observations will provide an important dataset to study lifetime of inner disks and optically thick disk evolution in such environments. We probe yet another common mode of star formation, forming in groups in triggered mode or influenced by UV photons from nearby ionizing sources. Our dataset and study will contribute to a better understanding of star formation and circumstellar disk evolution linking well-known star forming regions in weak and strong radiation field environments. We believe that this dataset will also benefit other star formation and disk communities for various other studies in addition to existing dataset of clusters and associations, obtained by GTO, legacy, and GO1.<br /> <br /> =Existing observations=<br /> <br /> Wiki page on searching Leopard is part of [[How do I download data from the Spitzer Telescope?]]<br /> <br /> =Education=<br /> <br /> Viv's assignment in the group was to organize the Education portion of our proposal. What if we make a case for the importance of:<br /> # Teacher/Student/Scientist Scientific Research within the context of today's national and education initiatives. <br /> # NITARP as a Professional Learning Community offering a Center of Strength in Science Teacher Leadership<br /> # Include the variety of expected student populations and levels of participation, considering how we might measure impact across these groups.<br /> <br /> <br /> I like these three strands. Great idea, Viv.<br /> --chj 17:19 CST 13-Jan-2010.<br /> <br /> <br /> test. CRM--[[User:Mallory|Mallory]] 21:02, 13 January 2010 (PST)<br /> <br /> The following is a summary of info describing the CG4 environment, and includes a small amount of info from other areas quantitatively similar to the Gum Nebula area. The environmental characteristics listed will describe the environment needed for star formation, demonstrated by the presence of YSOs in the--[[User:Mallory|Mallory]] 22:24, 13 January 2010 (PST) region:<br /> <br /> -cg4 resides in the Gum Nebula, within the constellation Puppis, adjacent to Vela. This area is 1,300 LY distant, and even visually is laced with plentiful clouds of gas and dust.<br /> <br /> -using appropriate wavelengths, should do a search for nearby massive O &amp; B stars (typical neighborhood bullies)to determine the possibility of photoevaporation of coalescing dust and gas taking place in newly formed stars, and if so, switch area being investigated. Cometary Globule tails all coinciding in direction they're pointing is another indication that newly forming stars are being photoevaporated by nearby large star radiation/emissions. There can be a number of Centers of Influence near a newly forming Star Cluster, check this optically, in radio, and in both UV and Xray.<br /> <br /> -Note that radiation driven implosion also occurs. Do muiltiwavelength study. Radio wavelengths especially.<br /> <br /> -Expect IR excess in area of star formation (Universal Gas Law; volume decrease/temp increase) Necessary to have an average value for IR around a small mass Main Sequence star, so we know what amount 'excess IR' is.<br /> <br /> - If head of cometary nebula is opaque, it can be assumed that sufficient gas and dust exist to create new stars. Thus, this opacity/Opacity Class is an indicator of star-forming region BUT needs to be quantified and observed in the appropriate wavelengths/optical photometry/MIPS probably.<br /> <br /> - Information about contraction/expansion/rotation, can be obtained from red-blue shift observations. This is necessary information! Personal question; could implosion produce an outward rebound?<br /> <br /> -Spectroscopic info can reveal the age/stage of development of baby stars uncovered in this study. MIPS.<br /> <br /> -To determine which stars visible in same area are members of the same CG4 Cluster, see common age/convection % compared to radiation &amp; conduction, speed of rotation (need to know axis of rotation to determine blue-red shift anyway), variability, spatial location, and spatial motion of all the local stars/i.e. do they seem to be moving as a group/cluster.<br /> <br /> -Excess IR (define 'excess' as variation from average IR emission from a similar mass young Main Sequence star IR average emissions) typifies newly forming stars, such as what we are looking for in CG4. Conflict in literature about UV emissions; forming star should have almost none/core processes do not yet produce, but very young stars can have a lot of UV emission due to repid rotation. Supposedly, really young stars have low Magnetic Field.<br /> <br /> -Another variable of which to be aware, is the number of YSOs in a given area. Too many, and only those with largest relative mass will grow to be stars, since they have the gravitational-strength advantage/capture the most infalling gas+dust. (Think nestfull of eagle eggs, which hatch at different times.)<br /> <br /> The sources listed below indicate that these are the qualities in nebulae which affect Star Formation. <br /> <br /> Carolyn Mallory<br /> <br /> Sources Used to Gather This information Include but are Not Limited to:<br /> SIMBAD, ic 2118, ADS, CoolWiki Finding Cluster Members, Spitzer Archives, Infrared Handbook by Wolfe &amp; Zissie.</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=CG4_Proposal&diff=3786 2010-01-14T05:02:34Z

<p>Mallory: </p> <hr /> <div>=Background information=<br /> <br /> Identifiers (aliases) for CG 4 ...<br /> ''BHR 21, <br /> Sandqvist 103, <br /> FEST 2-30, <br /> DCld 259.4-12.7''<br /> <br /> I found this by typing ''CG4'' into SIMBAD. The results were in the middle of the page. Scrolling down further, there's a list of 20 articles in which CG 4 is mentioned.<br /> <br /> Talk to you on Wednesday!<br /> --chj<br /> <br /> <br /> My Plan to continue Lit. search--[[User:Mallory|Mallory]] 23:35, 11 January 2010 (PST) is to finish SIMBAD, then go to ADS and to find a way to confirm and quantify lots! of IR (probably by opacity class) and little UV/max not to exceed a threshold to be determined; don't want the object to be a middle-aged star already.<br /> <br /> Is it the group's intention to consider locations outside of CG4, which could be cluster members? <br /> <br /> --[[User:Mallory|Mallory]] 23:28, 11 January 2010 (PST)Carolyn<br /> <br /> <br /> <br /> In a search through SIMBAD for CG 4 info, some interesting info and unanswered questions have emerged.<br /> <br /> If a gaseous region were collapsing due to a radiation-driven implosion, what's to stop it from rebounding back out, and how would we know the mechanism had occurred? Maybe by the length of tails (also created by outward pressures)? Is this a safe assumption?<br /> There seems to be a conflict between different analyses as to whether tails can be traced by CO(12) spectra. How to resolve? <br /> If collapse/expansion, and rotation can occur all in the same region, are there any tools other than redshift to sort out what is happening?<br /> Interesting that there could be more than one &quot;Center of Influence' in a region, i.e. massive star,--[[User:Mallory|Mallory]] 15:48, 12 January 2010 (PST) whose radiation influences the CG's evolution.<br /> <br /> chj, I'm not closely enough focused? Your ideas and suggestions?<br /> <br /> I'll continue info-gathering. You know, this is grinding but fun; it's interesting, and I'm figuring that the Laws of Physics are the same throughout the Universe.<br /> -C<br /> <br /> <br /> here is the paper from serena from 2005<br /> http://adsabs.harvard.edu/abs/2005AJ....129.1564K<br /> --[[User:Rebull|Rebull]] 15:57, 13 January 2010 (PST)<br /> <br /> Title: Low-Mass Star Formation in the Gum Nebula: The CG 30/31/38 Complex<br /> Authors: Kim, Jinyoung Serena; Walter, Frederick M.; Wolk, Scott J.<br /> Affiliation: AA(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065.; Visiting Astronomer, Cerro Tololo Inter-American Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under contact with the National Science Foundation.), AB(Department of Physics and Astronomy, State University of New York at Stony Brook, NY 11794-3800 serena@as.arizona.edu.), AC(Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.)<br /> Publication: The Astronomical Journal, Volume 129, Issue 3, pp. 1564-1579. (AJ Homepage)<br /> Publication Date:03/2005<br /> Origin:UCP<br /> AJ Keywords:Stars: Circumstellar Matter, ISM: H II Regions, ISM: Globules, Stars: Formation, Stars: Low-Mass, Brown Dwarfs, Stars: Pre-Main-Sequence<br /> DOI:10.1086/428002<br /> Bibliographic Code:2005AJ....129.1564K<br /> <br /> Abstract<br /> We present photometric and spectroscopic results for the low-mass pre-main-sequence (PMS) stars with spectral types K-M in the cometary globule (CG) 30/31/38 complex. We obtained multiobject high-resolution spectra for the targets selected as possible PMS stars from multiwavelength photometry. We identified 11 PMS stars brighter than V=16.5 with ages &lt;~5 Myr at a distance of approximately 200 pc. The spatial distribution of the PMS stars, CG clouds, and ionizing sources (O stars and supernova remnants) suggests a possible triggered origin of the star formation in this region. We confirm the youth of the photometrically selected PMS stars using the lithium abundances. The radial velocities of the low-mass PMS stars are consistent with those of the cometary globules. Most of the PMS stars show weak Hα emission with Wλ(Hα)&lt;10 Å. Only one out of the 11 PMS stars shows a moderate near-IR excess, which suggests a short survival time (t&lt;5 Myr) of circumstellar disks in this star-forming environment. In addition, we find five young late-type stars and one Ae star that have no obvious relation to the CG 30/31/38 complex. We also discuss a possible scenario of the star formation history in the CG 30/31/38 region. <br /> <br /> <br /> http://adsabs.harvard.edu/abs/2006AAS...20921915K<br /> <br /> <br /> Title: Star Formation in the Gum Nebula: Cometary Globules CG4/6/SA101 <br /> Authors: Kim, Jinyoung S.; Walter, F. M.; Wolk, S. J.; Sherry, W. H.; Foster, M. <br /> Affiliation: AA(Univ. of Arizona), AB(Stony Brook University), AC(CfA), AD(NSO/NOAO), AE(Univ. of Arizona) <br /> Publication: 2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #219.15; Bulletin of the American Astronomical Society, Vol. 38, p.1205 <br /> Publication Date: 12/2006 <br /> Origin: AAS <br /> Bibliographic Code: 2006AAS...20921915K <br /> <br /> Abstract<br /> As a part of our on-going program to study star formation under various environments, we present preliminary results from our multi-wavelength study of a bright-rimmed cometary globule complex, CG4/6/SA101 in the Gum Nebula. These cometary clouds are photo-evaporating due to UV radiation from neighboring O stars (10 &lt; d &lt; 100 pc) in the Vela OB2 association. The intermediate and low-mass stars in these cometary clouds form in an environment that differs from both the quiet isolation of young stars in T-associations such as Taurus and the violently energetic environment like that of the Orion Nebula cluster (ONC). The moderate separation between the cometary clouds and the O stars creates a radiation environment that has an intensity intermediate between the Taurus and Orion star forming regions. Circumstellar material and accretion disks may last longer than those in ONC, yet may not survive as long as they would in an isolated region such as Taurus or TW Hya. We compare our results with other star forming regions under different environments. <br /> <br /> <br /> <br /> http://adsabs.harvard.edu/abs/2005sptz.prop20714K<br /> <br /> Title: Probing environment and circumstellar disk evolution in triggered star forming regions: IRAC and MIPS imaging of bright-rimmed globules CG4/SA101 and CG30/31 <br /> Authors: Kim, Jinyoung Serena; Sherry, Wiiliam <br /> Publication: Spitzer Proposal ID #20714 <br /> Publication Date: 06/2005 <br /> Origin: SPITZER <br /> Bibliographic Code: 2005sptz.prop20714K <br /> <br /> Abstract<br /> We propose to obtain IRAC and MIPS images of a newly discovered star forming region, cometary cloud complex CG~4/SA101 (Kim et al. 2005c). We also propose to acquire more complete IRAC and MIPS images of a cometary globule complex CG~30/31, where we found young stars (Kim et al. 2005a,c), but existing program by a Spitzer legacy team (c2d) did not observe. Both star forming complexes reside in the Gum Nebula, where early O stars, Wolf-Rayet star, supernovae remnants, and OB associations produce strong ionizing UV photons. These two star forming regions are in a photoevaporating cometary shaped bright-rimmed clouds, at few tens of parsecs away from the common center of main ionizing sources in the Gum Nebula, placing them in a 'intermediate' UV radiation field between Orion-like Strong radiation field regions and Taurus-like weak radiation field regions. We propose to perform comparative and statistical studies probing circumstellar disk characteristics and evolution in different star forming environments together with existing data of well-known star forming regions. The age range of the young stars in these regions (1-5 Myr old) is also of a great interest, because this is a time when transition from optically thick disks to optically thin debris disks occurs. Therefore, this proposed observations will provide an important dataset to study lifetime of inner disks and optically thick disk evolution in such environments. We probe yet another common mode of star formation, forming in groups in triggered mode or influenced by UV photons from nearby ionizing sources. Our dataset and study will contribute to a better understanding of star formation and circumstellar disk evolution linking well-known star forming regions in weak and strong radiation field environments. We believe that this dataset will also benefit other star formation and disk communities for various other studies in addition to existing dataset of clusters and associations, obtained by GTO, legacy, and GO1.<br /> <br /> =Existing observations=<br /> <br /> Wiki page on searching Leopard is part of [[How do I download data from the Spitzer Telescope?]]<br /> <br /> =Education=<br /> <br /> Viv's assignment in the group was to organize the Education portion of our proposal. What if we make a case for the importance of:<br /> # Teacher/Student/Scientist Scientific Research within the context of today's national and education initiatives. <br /> # NITARP as a Professional Learning Community offering a Center of Strength in Science Teacher Leadership<br /> # Include the variety of expected student populations and levels of participation, considering how we might measure impact across these groups.<br /> <br /> <br /> I like these three strands. Great idea, Viv.<br /> --chj 17:19 CST 13-Jan-2010.<br /> <br /> <br /> test. CRM--[[User:Mallory|Mallory]] 21:02, 13 January 2010 (PST)</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=CG4_Proposal&diff=3770 2010-01-12T23:48:06Z

<p>Mallory: </p> <hr /> <div>Identifiers (aliases) for CG 4 ...<br /> ''BHR 21, <br /> Sandqvist 103, <br /> FEST 2-30, <br /> DCld 259.4-12.7''<br /> <br /> I found this by typing ''CG4'' into SIMBAD. The results were in the middle of the page. Scrolling down further, there's a list of 20 articles in which CG 4 is mentioned.<br /> <br /> Talk to you on Wednesday!<br /> --chj<br /> <br /> <br /> My Plan to continue Lit. search--[[User:Mallory|Mallory]] 23:35, 11 January 2010 (PST) is to finish SIMBAD, then go to ADS and to find a way to confirm and quantify lots! of IR (probably by opacity class) and little UV/max not to exceed a threshold to be determined; don't want the object to be a middle-aged star already.<br /> <br /> Is it the group's intention to consider locations outside of CG4, which could be cluster members? <br /> <br /> --[[User:Mallory|Mallory]] 23:28, 11 January 2010 (PST)Carolyn<br /> <br /> <br /> <br /> In a search through SIMBAD for CG 4 info, some interesting info and unanswered questions have emerged.<br /> <br /> If a gaseous region were collapsing due to a radiation-driven implosion, what's to stop it from rebounding back out, and how would we know the mechanism had occurred? Maybe by the length of tails (also created by outward pressures)? Is this a safe assumption?<br /> There seems to be a conflict between different analyses as to whether tails can be traced by CO(12) spectra. How to resolve? <br /> If collapse/expansion, and rotation can occur all in the same region, are there any tools other than redshift to sort out what is happening?<br /> Interesting that there could be more than one &quot;Center of Influence' in a region, i.e. massive star,--[[User:Mallory|Mallory]] 15:48, 12 January 2010 (PST) whose radiation influences the CG's evolution.<br /> <br /> chj, I'm not closely enough focused? Your ideas and suggestions?<br /> <br /> I'll continue info-gathering. You know, this is grinding but fun; it's interesting, and I'm figuring that the Laws of Physics are the same throughout the Universe.<br /> -C</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=CG4_Proposal&diff=3769 2010-01-12T07:35:27Z

<p>Mallory: </p> <hr /> <div>Identifiers (aliases) for CG 4 ...<br /> ''BHR 21, <br /> Sandqvist 103, <br /> FEST 2-30, <br /> DCld 259.4-12.7''<br /> <br /> I found this by typing ''CG4'' into SIMBAD. The results were in the middle of the page. Scrolling down further, there's a list of 20 articles in which CG 4 is mentioned.<br /> <br /> Talk to you on Wednesday!<br /> --chj<br /> <br /> <br /> My Plan to continue Lit. search--[[User:Mallory|Mallory]] 23:35, 11 January 2010 (PST) is to finish SIMBAD, then go to ADS and to find a way to confirm and quantify lots! of IR (probably by opacity class) and little UV/max not to exceed a threshold to be determined; don't want the object to be a middle-aged star already.<br /> <br /> Is it the group's intention to consider locations outside of CG4, which could be cluster members? <br /> <br /> --[[User:Mallory|Mallory]] 23:28, 11 January 2010 (PST)Carolyn</div>

Mallory https://vmcoolwiki.ipac.caltech.edu/index.php?title=CG4_Proposal&diff=3768 2010-01-12T07:28:49Z

<p>Mallory: </p> <hr /> <div>Identifiers (aliases) for CG 4 ...<br /> ''BHR 21, <br /> Sandqvist 103, <br /> FEST 2-30, <br /> DCld 259.4-12.7''<br /> <br /> I found this by typing ''CG4'' into SIMBAD. The results were in the middle of the page. Scrolling down further, there's a list of 20 articles in which CG 4 is mentioned.<br /> <br /> Talk to you on Wednesday!<br /> --chj<br /> <br /> <br /> My Plan to continue Lit. searchm is to finish SIMBAD, then go to ADS and to find a way to confirm and quantify lots! of IR (probably by opacity class) and little UV/max not to exceed a threshold to be determined; don't want the object to be a middle-aged star already.<br /> <br /> Is it the group's intention to consider locations outside of CG4, which could be cluster members? <br /> <br /> --[[User:Mallory|Mallory]] 23:28, 11 January 2010 (PST)Carolyn</div>

Mallory