ALMA simulation library
Molecular line emission model for a proto-planetary disk
Observing mode: C17O(3-2) line emission at 337 GHz
Author: Itziar de Gregorio-Monsalvo (ALMA Fellow in Santiago)
corresponding DRSP project Nb 2.4.13 "Protoplanetary disks in Orion"
description from the authors:
These are a set of molecular line emission models calculated for various mass accretion rates, radius, viscosity and maximum dust grain distributions.
We tried to reproduce a real interferometric observation of a protoplanetary disk with different physical parameters, we integrated the radiative transfer equation and convolved each model with a beam of 0."4.
The line selected was C17O(3-2) transition at 337 GHz (high excitation transition of a CO isotope with very low abundance, less susceptible to be affected by absorption and emission from the surrounding cloud material).
Some assumptions:
- we assume disk in steady state, with constant mass accretion rate and viscosity parameter alpha
- we assume gas and dust thermally coupled and vertical hydrostatic equilibrium.
Input parameters:
We considered typical parameters of a TTauri star (Mstar=0.5 Msun, Rstar=2Rsun, Tstar=4000 K) for all the models. We assume the disks are at 140 pc of distance (the distance to the Taurus molecular cloud), and with a disk inclination angle of 60degrees.
We have considered the next set of input physical parameters:
Rd (maximum disk radius) = 50, 100, 150 AU
a_max (maximum radius of dust grains)= 1,10,100,1000,10000,100000 microns
M_p (mass accretion rate)= 10e-09, 3x10e-08, 10e-07 M_sun/year
alpha (viscosity parameter)= 0.001, 0.005, 0.01, 0.02, 0.05
And we have built models for all the combinations (physically possible) of these physical parameters.
References:
de Gregorio-Monsalvo, D'Alessio & Gomez (2007), Rev. Mex. de A y A, 43, 271
Gomez & D'Alessio (2000), ApJ, 535, 943
CO(4-3) imaging of Lyman-break galaxies at z=3
Observing mode: CO(4-3) maps
Author: Thomas Greve (MPIA Heidelberg)
corresponding DRSP Nb 1.1.5 "Molecular line studies of submm galaxies"
or DRSP Nb 1.1.9 "Dust in normal Lyman Break galaxies"
description from the authors:
CO(4-3) maps (velocity-cubes)
The intensity units are simply Jy (I've multiplied with the solid angle of each pixel, so the units are Jy).
The velocity units are km/s
The pixel scale is 0.1kpc/px while the velocity resolution is 5km/s
Reference:
Greve & Sommer-Larsen (2008), A&A, 480, 335
CO imaging of comet Hale-Bobb
Observing mode: CO J2-1 map
Author: Jeremie Boissier (IRAM)
related to DRSP Nb 4.3.1 "A complete picture of Earth-grazing comet 103P/Hartley 2"
or DRSP Nb 4.3.5 "Is Hale-Bobb still alive ?"
description from the authors:
a model of the CO emission of comet Hale-Bopp computed on the basis of hydrodynamical simulations. The model assumes the presence of a CO jet creating a spiral structure.
256x256 pixels (0.5x0.5'' each)
RA: 22:31:17.798, DEC: 40:49:18.55
Units: Jy
reference frequency 230538.0 in channel 20 (CO J2-1)
40 channels of 0.1 km/s
Comet geocentric distance ~1.5 AU
Comet heliocentric distance ~1 AU
Production rate of water : 1.5e31 molecules/s
Production rate of water : 1.3e30 molecules/s
Sensitivity:
The sensitivity is not a limitation by itself in the case of a comet as bright as Hale-Bopp. The spectrum peak in the brightest pixel of the map is close to 1Jy. The important point is to make an image in a short integration time (<1h) in order to have successive snapshots of the coma and study the chinematics of the gas.
Ultradeep continuum survey
Observing mode: continuum band 7
Author: Eelco van Kampen (ESO)
description from the authors:
small area, deep pencil-beam surveys taken from cosmological simulations and phenomenological galaxy formation models. Many fields, including some containing overdensities (proto-clusters).
MISSING PROJECTS:
- spectral line survey (either galactic or extragalactic)
- proto-stars
- star forming regions
- AGN
- gamma-ray bursts
- SZ
- extra-solar planets
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