Alexandre Beelen
(Institut d'Astrophysique Spatiale / Laboratoire d'Astrophysique de Marseille)
6/7/19, 9:30 AM
More than half of the photons emitted by stars across cosmic times have been absorbed by cosmic dust and re-emitted in the far-infrared and millimeter wavelength domain. Herschel and ALMA revealed that very massive and very dusty galaxies already exist in the early Universe (up to z~7). These objects are one of the keys to understand the formation of the most massive galaxies. However, these...
Mr
Maximilien FRANCO
(DAp CEA-Saclay)
6/7/19, 10:00 AM
We will present the latest results of a 69 arcmin2 ALMA survey at 1.1mm, GOODS-ALMA, matching the deepest HST-WFC3 H-band observed region of the GOODS-South field. We have extracted two catalogs, one of galaxies purely selected by ALMA, from which we have identified sources both with and without HST counterparts, and another catalog based on priors. Our wide contiguous survey allows us to push...
Dr
Nicolas Peretto
(Cardiff University)
6/7/19, 11:00 AM
Over the last decade, Herschel observations of the Galactic interstellar medium have transformed our understanding of the early stages of star formation. At the low-mass end of the stellar initial mass function (IMF), a paradigm has emerged in which low-mass cores – the progenitors of stars with masses from ~0.1 to a couple of solar masses – are thought to form as the result of gravitational...
Dr
Bilal Ladjelate
(IRAM Granada)
6/7/19, 11:30 AM
From molecular clouds to young stellar objects, every step in the evolution of young stars can be observed in the millimetric range.
As part of the NIKA2 (Adam et al. 2018) Large Program GASTON (PI: Nicolas Peretto), we observed at 1.2mm and 2mm the Ophiuchus Molecular Cloud. The dual band capabilities of NIKA2 allow us to understand the properties of dust in star-forming regions, and their...
Dr
Charlène LEFEVRE
(Institut de RadioAstronomie Millimétrique)
6/7/19, 12:00 PM
Dust is the only tracer that is present from the edge of the interstellar cloud to the densest part, inside which stars and planets will form, named pre-stellar cores. It allows to trace the density structure of the cloud, of the core(s), and of the subsequent protoplanetary disk where it becomes a major actor of the planet formation. Dust grains evolve from bare simple elongated shape in the...
