Star Formation: Interstellar Gas Cloud Mass Distribution

Recently, our blog and the astrological research community have been perplexed  by the discovery of the nearby Segue 1 dwarf galaxy. However, another momentous development by the Max Planck Institute for Astronomy in Heidelberg also has far reaching implications within the field. Jouni Kainulainen and his associates have developed a technique that allows researchers to determine the distribution of mass in interstellar clouds, which are forming stars. According to an interview with Mr. Kainulainen, they are capable of measuring the degree to which these interstellar clouds "dim [the light] of thousands of different stars," whose luminosity we already know. This allows "scientists [to reconstruct] the cloud's 3D structure, helping pinpoint how matter is distributed within the cloud."

3D Mass Distribution Map

Understanding the distribution of matter in galaxies has always been a difficulty, hence the discovery of dark matter, but this new technology allows academics and professionals to better understand the conditions under which stars form in today's universe. We have long known that star formation requires a certain critical density to force the interstellar elements to collapse under their own pressure, eventually igniting nuclear fusion, but this technology has moved us closer to pinpointing these conditions. In fact, the research with the new 3D tech has indicated that a threshold "critical density of 5,000 hydrogen molecules per cubic centimeter" is needed to force a collapse.

Researchers and Mr. Kainulainen have been quick to remind people that this technology and its results are most applicable to today's universe, and may have limited insight regarding early star formation. According to Jouni, "we have to remember that physical conditions during early galaxy formation were quite different from those of galaxies today." Personally, I find this sentiment refreshing, as the Segue 1 discovery seems to be fueling hope of details but also rampant speculation on its relation to early galaxy formation. How do we know what forces affected the Segue 1 galaxy since its inception? Is it fair to attribute all of it's nuances to early galaxy formation, or may later developments been responsible for its peculiar size and lack of heavy metals? 

Segue 1 Dwarf Galaxy

The technology that the Max Planck Institute has developed has real value for research today that does not hinge on speculation of the past, and can help us understand star formation in galaxies that are too distant to directly view. In fact, this new 3D system offers the ability for researchers to gain tangible observational data to support star formation theories. The reliance on light and luminosity obviously means that this forward leap will have little effect on the study of dark matter, as it is not affected by electromagnetic radiation. However, this is a big step towards understanding our current surroundings, and in conjunction with the Segue 1 discover, offers great hope for a more developed model of star and galaxy formation.

Sources:

http://www.scientificamerican.com/article/fossil-galaxy-segue1/

http://www.astronomy.com/news/2014/04/finding-the-recipe-for-star-formation

http://www.mnn.com/earth-matters/space/stories/scientists-unlock-simple-recipe-for-star-formation

http://en.wikipedia.org/wiki/Segue_1