PPT-1 On star-formation compactness & bulges: the ALMA view

S IR z2 S IR z0 x 6 S IR z4 S IR z0 x 12 S IR z S IR z0 x 1z 25 vs S UV z S UV z0 x 1z SFR M t lt1Gyr R SB sSFRsSFR. on subsets of means and are apart In metric space Apartness complement 8801 brPage 3br De64257nitions Compactness Our Criteria Conclusion Apartness Axioms B0 B1 B2 B3 B4 B5 brPage 4br De64257nitions Compactness Our Criteria Conclusion Lo Holes. Alister. Graham. Swinburne University. Australia. Overview. Galaxy bulge light profiles, and model fitting. The resultant structural properties of bulges. Bulge-(black hole). . scaling . relations. ALMA detected C. 2. H. 5. CN in 27 rotational lines at 1.3mm. HC. 3. N, CH. 3. CN and CH. 3. CCH simultaneously detected. Emission from these species peak in the northern (spring) hemisphere. Emission from . 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. elliptical galaxies – II. Monsters at Heart. Dimitri Gadotti (ESO). Outline – Lecture Two. Composite bulges. Host galaxies and environment. Elliptical galaxies and two dichotomies. core. -depleted vs. extra-. 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 . Roberto Maiolino. Feedback is the key:. - reducing SF efficiency . . (gas . heating+turbulence. ). - removing baryons. Discrepancy . between halo . mass . functions . and stellar/baryons mass function. use it?. Dr. Lizette Guzman-Ramirez. ESO Fellow for ALMA. What is ALMA?. Atacama Large Millimeter and sub-millimeter Array.. ALMA as an Interferometer. 66 antennas working as one . radiotelescope. .. , ALMA. 10x . Resolution w. . 50% to few km + . 50. % to . 300km . Frequency . range: 1. . – 50, 70 – 115 . GHz. JVLA: . Good 3mm site, elev. .. ~ 2200m. 550km. 9. 0% coherence. Residual phase . Universe. . Epoch of galaxy assembly (z~1 to 5). Massive galaxy formation: imaging hyper-starbursts . . Main sequence galaxies: gas dominated disks. . Pushing toward first light: the role of [CII] observations. Imaging a galaxy-scale molecular outflow. ALMA has imaged expanding molecular shells in the starburst nucleus of NGC 253 at 50-parsec resolution. . T. he . extraplanar. molecular gas closely tracks the Hα filaments, and connects to expanding molecular shells located in the starburst region. The molecular outflow rate is 9 M. 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.