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This page contains a discussion of what BDPs ADMIT will offer and how they are structured including dependencies.


BDP Definitions

Here are the BDPs we will offer and the data they contain in no particular order

moment maps
moment type
moment method
number of channels
frequency/velocity coverage
the data
line list
line id/quantum numbers etc
PV slice
molecule id
continuum map
number of channels
line cube
molecule ID
overlap integral
molecule ids
feature list
coordinates (x,y,z)
description vector

BDP Dependencies

I see the feature list as the highest level BDP since everything we derive or calculate will depend on where things are. The feature list can be generated by clumpfind, peak spectra, or an other method.

Use Cases

Here out some general use cases (based on a quick read of the DSRP documents). I do not include short term TOO observations (24 hours or less notification) as it is my understanding the ALMA is not capable of this. Also VLBI observation are not included as they do their own thing anyway.

Galaxies and Cosmology

Description Req Δδ Req Δv (km/s) Notes
Continuum and line survey at high z 1" or better <1 Looking at lenses, may be mosaics
Blind molecular survey at z=1-5 .2" 1
Deep comtinuum survey 1" n/a Multi frequency, many fiels 10's - 1000's targets
Line emitting galaxies 300 (entire line)
Dust in Ly break galaxies n/a Continuum detection
SED determination of galaxies n/a Multi-frequency continuum
Weak lensing of CO 0.3-.1" 1-2
Line survey of distant absorbers 1" 1-4 May be multiple sources in small FOV
Galaxy cluster imaging in SZ 1-2 n/a Mosaics over 180" or more
Imgaing molecules in AGNs .06" with sensitivity up to 25" 5
Hot spots in galaxies .2" n/a uses polarization
GMC scale chemistry 1" 5 includes total power measurements
Multi CO survey of galaxies .5" in general 0.05" in cores 3 sensitivity to structures up to 60"

Star and Planet Formation

Description Req Δδ Req Δv (km/s) Notes
Temperatures and densities of YSOs and HMCs .5" Using continuum and molecules to probe conditions, may be huge mosiacs
Infall in starless cores 1" 0.03 derive radial profiles of infall
Magnetic field geometry 1"  ? May use molecular lines as well as polarized continuum
CO survey on outflows 10"
Kinematics of prestellar cores .5" .1 model line profiles, disk/jet interaction
Molecular line surveys .2-3" .25 multiple cores, fractionation, outflows
Interstellar line absorption PS .5
Molecules in disks .2-.4" 0.05 CO, deuteration
Disk properties .1" .2 Use continuum and molecules to look at dust properties, muti wavelength, gaps in disks

Stars and Their Evolution

Description Req Δδ Req Δv (km/s) Notes
Structure of the chromosphere .1" n/a huge amount of structure on many spatial scales
Solar recombination lines .1" .1 huge amount of structure on many spatial scales
Magnetic fields in MS stars PS n/a polarization observation
Thermal emission from stars 0.01" n/a multi wavelength
Proper motion of stars 0.0018" n/a
Molecules around stars 0.006"  ?
Molecules in planetary nebulae .1" .1 could be huge amount of structure on multiple spatial scales
Supernova remnant interactions .15" 1 small structures in large field of view that are related

Solar System

Description Req Δδ Req Δv (km/s) Notes
Planetary atmospheres .5" .05 CO and other molecules, turbulence
Astrometry NEO and TNO 0.001 or better n/a may have to time slice data to get good maps
Comets 1" for molecules 0.05" for nucleus 0.1 may have to time slice to get maps of jets etc.
Detection of Jupiters around other stars .1" n/a

Data Structure

Here I present several different possible data structures.

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