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Did you know?

by Aaron Evans last modified Mar 07, 2017 by Anthony Remijan
M83

... resolve molecular clouds in a nearby, star-forming galaxy:

in Cycle 5
6 pc clouds of excited CO(J=3-2) gas across the central 400 pc of M83 1.75 hours
30 pc clouds of dense HCN(J=1-0) gas in the central 1.5 kpc of M83 18.75 mins
create an HCN(J=1-0) mosaic of the full M83 bar with 30 pc resolution 2.17 hours
high z

... detect the ISM in high redshift galaxies:

in Cycle 5
dust emission in a “normal” 1011 L galaxy between z=1 and z=6 6 hours
major cooling[CII] line in a lensed Milky Way galaxy at z=4.2 29.5 mins
dust emission in a 1012 L luminous infrared galaxy out to z=10 21 minutes
solar system

... reveal the characteristics of Solar System objects:

in Cycle 5
obtain wind patterns in the atmosphere of Mars with 300 km resolution 27 minutes
trace the atmospheric water content of Venus using HDO lines 8.1 minutes
detect volatiles (HCN, CH3OH, H2CO, CS and HNC) on active comets 4.7 hours
measure Kuiper Belt Object sizes from their thermal emission 50 minutes
Galactic cloud

... survey Galactic clouds and star-forming regions:

in Cycle 5
measure the polarization of dust in 30 protostars in a single star-forming region 1.2 hours
detect thousands of lines over 60 GHz with < 1 km/s resolution toward Orion-KL 42 minutes

... trace the formation of galaxy clusters, cosmic structure:

in Cycle 5
characterize merger shocks in cluster gas with the Sunyaev-­Zel’dovich Effect 1.3 (2.5) hours
survey clustering in a sample of 23 Lyman-α  Blobs (LABs) at z=3.1 < 1 hour

... reveal the nature of planetary disks around nearby stars:

in Cycle 5
resolve the "snow line" in the disk around the T Tauri system HD 163296 14 minutes
measure dense gas flows across gaps in protoplanetary disks 15 minutes
detect a dust disk gap induced by a Jupiter mass planet at 120 pc 2.1 hours
image full debris disk (dense clumps in disk) of ε Eri with 1 AU resolution 18 (3) hours
high resolution imaging of a protoplanetary disk like HL Tau 4.5 hours

... measure stellar activity from low to high mass stars:

in Cycle 5
image molecular ouulows from pre-­planetary nebulae 5 minutes
investigate heating mechanisms of red giant stars 2 minutes
detect z=3 (z=10) GRB afterglow two days after the burst 9 minutes
(2.1 hours)

... study black holes and their environments, near and far:

in Cycle 5
measure black hole mass of NGC 4526 from molecular gas kinematics 47 minutes
infer gas properties in the host galaxy of an obscured z=2.8 quasar 15 minutes
understand the energetics of flares from Sagittarius A* 2 minutes
  • Note: All integration times listed are on source with the main array and assume dual polarization unless otherwise noted. Times are calculated using the online ALMA Sensitivity Calculator available at the time of publication; proposers should re-calculate integration times for themselves. They do not include estimates of overhead or calibration.