Talk:CG4 Proposal

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. --Mallory 12:43, 3 February 2010 (PST)

Draft

STAR FORMATION IN CG4

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?

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.

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 & 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.

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 & 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, "Triggered Low Mass Star Formation in the Gum Nebula", 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.

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 & 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 & 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. 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.