PPT-Q1: Quenching and the cessation of star-formation

1 The Q word and its meaning Is quenching a good word to describe the end of starformation in galaxies What are the timescales for quenching Pablo Jarle Is quenching due to starvation or gas expulsion . What force makes stars? . Gravity!. Out of what? Interstellar gas and dust. But this stuff is VERY low density… a dense area may have ~100 atoms / cm. 3. . Compare that the air you’re breathing… ~10. Smolcic. . ea. ). Compilation based on different star formation estimators (UV, IR, radio, Hα..). Large scatter: Dust obscuration is major problem. Hopkins & . Beacom. (2006) compilation. redshift. Rich Dwarf Galaxies. . Sambit. . Roychowdhury. (NCRA), . Jayaram. . N. . Chengalur. . (. NCRA. ), . . Igor . D. . Karachentsev. (SAO. ), Margarita . Sharina. (SAO). Ayesha Begum . . (. Peng. et al 2010, 2012). f. rom . Peng. et al (2012). centrals. satellites. Two “separable effects”. Mass-quenching: Depends on mass but not environment. Satellite quenching: Depends on environment but not on mass. Christopher W. Ashcraft M.S., M.Ed.. Big Bang vs. Creation. Origin of Stars. Solar System: Evidence of Design. Age of the Cosmos. Are we being told all the evidence or just selected information to support a particular idea?. Sections 39.1-39.5. Reminders. Don. ’. t forget about weekly reflections. …. Should I drop the 2 lowest weekly reflections?. Should I drop the 3 lowest reading quizzes?. Final . exam. . Thursday. D. Calzetti (Univ. of Massachusetts). a. nd the LEGUS . Team. https://. legus.stsci.edu. /. HUBBLE2020: Hubble’s 25. th. Anniversary Symposium. STScI. , Baltimore, April 20-24, 2015. NGC3344. NGC1566. Greg Goldstein. PhD student, . Dept. of Physics and Astronomy, Macquarie University. Supervisors:. Dr. Richard . McDermid. Dr Matt Owers. Galaxy Evolution:. star-forming spirals decrease - quiescent ellipticals increase over time. Oleg . Gnedin. (University of Michigan. ). g. raduate student . Hui. Li. Star clusters are dominant components of active star formation:. they connect small-scale SF (local) and global processes in galaxies. with Marco Lombardi, . Joao Alves, . Jan Forbrich, . Gus Munch. Kevin Covey. & Carlos Roman . z = 1 - 10. Bouwens et al. 2010. z = 0.000. S. Guisard ESO. Pipe Nebula. Guidepost. In this chapter, you will consider how the interstellar medium condenses into stars and what the conditions inside stars must be like. How do stars form?. What is the evidence that stars are forming now?. Zooming in on Star Formation. , Nafplio, June 14. , 2019. Galactic Scale Star Formation. What we know for sure now:. Feedback, and vertical pressure (. im. -)balance is crucial. The role of radial and vertical net mass transport is poorly understood. Jeff Mangum. NRAO. 2. Extragalactic Star Formation. 3. Multi-transition analysis of molecular excitation within high spatial. . density (n(H2) > 10^5 cm^-3) and high kinetic temperature (. Tk. > 100 K) environments. How Galaxies form Stars – August 24 2016 . Robbert. Verbeke. 1. Bert . Vandenbroucke. Sven De . Rijcke. Ghent University. 1. Robbert.verbeke@ugent.be. @. Rbhfd. Λ. CDM. Standard model for cosmology.