Calendar

Oct
26
Mon
Pizza Lunch: Kyle Uckert and Nancy Chanover
Oct 26 @ 12:30 pm – 1:30 pm
Pizza Lunch: Kyle Uckert and Nancy Chanover

Integration of an IR spectrometer with a rock climbing robot

Mar
13
Mon
Pizza Lunch: Jean McKeever
Mar 13 @ 12:30 pm – 1:30 pm
Pizza Lunch: Jean McKeever @ AY 119

Red Giants in Eclipsing Binary Systems

Jean McKeever

 

Mar
5
Tue
Public Talk: Janna Levin: Black Hole Blues
Mar 5 @ 7:30 pm – 8:45 pm
Sep
6
Fri
Colloquium: Brian Svoboda (Host: Moire Prescott)
Sep 6 @ 3:15 pm – 4:15 pm
Colloquium: Brian Svoboda (Host: Moire Prescott) @ BX102

Starless clumps and the earliest phases of high-mass star formation in the Milky Way

Brian Svoboda, NRAO Jansky Fellow

High-mass stars are key to regulating the interstellar medium, star formation activity, and overall evolution of galaxies, but their formation remains an open problem in astrophysics. In order to understand the physical conditions during the earliest phases of high-mass star formation, I will present observational studies we have carried out on dense starless clump candidates (SCCs) that show no signatures of star formation activity. We identify 2223 SCCs from the 1.1 mm Bolocam Galactic Plane Survey, systematically analyse their physical properties, and show that the starless phase is not represented by a single timescale, but evolves more rapidly with increasing clump mass. To investigate the sub-structure in SCCs at high spatial resolution, we investigate the 12 most high-mass SCCs within 5 kpc using ALMA. We find previously undetected low-luminosity protostars in 11 out of 12 SCCs, fragmentation equal to the thermal Jeans length of the clump, and no starless cores exceeding 30 solar masses. While uncertainties remain concerning the star formation efficiency in this sample, these observational facts are consistent with models where high-mass stars form from initially low- to intermediate-mass protostars that accrete most of their mass from the surrounding clump. I will also present on-going research studying gas inflow signatures with GBT/Argus and ALMA, and the dense core mass function with the JVLA.

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