Overview of ADMIT

The ALMA Data-Mining Toolkit (ADMIT) is an execution environment and set of tools for analyzing image data cubes. ADMIT is based on python and designed to be fully compliant with CASA and to utilize CASA routines where possible. ADMIT has a flow-oriented approach, executing a series of ADMIT Tasks (ATs) in a sequence to produce a sequence of outputs. For the beginner, ADMIT can be driven by simple scripts that can be run at the unix level or from inside of CASA. ADMIT provides a simple browser interface for looking at the data products, and all major data products are on disk as CASA images and graphics files. For the advanced user, ADMIT is a python environment for data analysis and for creating new tools for analyzing data.

The primary operations supported by ADMIT are focused on analysis of images commonly produced by ALMA and similar radio telescopes. ADMIT has three primary functionalities:

  1. An automatic pipeline flow which produces a fixed set of science data products which are ingested into the ALMA Archive and available to the requester from the ALMA Archive. These ADMIT products are created from the ALMA image cubes after they are accepted as valid by the observatory. ADMIT products are not currently available from the ALMA Archive – they should become available later in 2016.
  2. A desktop environment where the astronomer can quickly create flows to produce and inspect ADMIT data products via a web or graphic file browser and access information in the form of XML table, PNG files, and FITS files. Because ADMIT is a Python environment, the user can choose to examine the data using the Python capabilities.
  3. A capability for astronomers to rerun pipeline flows with hand-tuned parameters and to modify flows based on existing ADMIT Tasks. Additionally, the advanced user may create new ADMIT tasks to suit the needs of their scientific goals.

Typically an astronomer will interact with ADMIT in one of two ways:

  • By retrieving the ADMIT products from the ALMA Archive. These products will be in a gzipped tar file of size a few to a few tens of megabytes. Once untar’ed on the disk, these products can be viewed with a browser utilizing the index.html file provided or inspected directly with unix or xml tools. Archive products available later in 2016.
  • By creating a local ADMIT flow to do the user requested analysis, inspect the results, and then modify and improve the flow parameters to achieve the desired final data products.

ADMIT does not interact with u,v data or create images from u,v data; CASA should be used to create images. ADMIT provides a number of ways to inspect your image cubes. The astronomer can then decide whether the ALMA image cubes need to be improved, which requires running standard CASA routines to re-image the u,v data. If new images are made, the ADMIT flow can be run on these new image cubes to produce new set of ADMIT products.

ADMIT requires that you have the image cubes local to the execution machine to create new data products. You do not need to have the image cubes local to view pre-existing ADMIT products. The tarball from the ALMA archive will contain ADMIT products without the image cubes. If you wish to modify parameters and make new ADMIT products, you need to download the appropriate data cubes from the ALMA archive and then re-run the ADMIT flow.

A Short Summary of the Technical Side of ADMIT

ADMIT is Python-based software which utilizes CASA routines where possible and reads CASA image format or FITS. ADMIT is an add-on package to CASA and designed to be compatable with the CASA Python environment. Currently, compatability with CASA forces incompatability with some commonly used Python packages (e.g., APLpy, astropy). CASA must be installed on your computer and instantiated in your working shell in order to use ADMIT. ADMIT software must be installed on your system (see Install Guide).

The basic components of ADMIT are:

  • ADMIT Task (AT): An ADMIT task is a Python script that accomplishes a specfic job. Each task has a specific set of keywords and a set of outputs. Most tasks follow a load-and-execute model so that they can be run automatically based on set inputs.
  • Basic Data Product (BDP): A Basic Data Product is an output from an AT and often the input to another AT. The content of the BDP is defined by the AT that produces it. It can consist of XML, PNG images, and image data in CASA or FITS format. BDPs are written to disk.
  • Flow: ADMIT Tasks are generally run sequentially to create a set of BDPs. Tasks are created and added to the Flow, and once the flow is set up, the user runs the flow which runs each task in turn. Tasks are connected to each other via BDPs – the output BDP of an AT is used as the input BDP to another AT downstream. ADMIT has a Flow Manager which maintains information about the sequence of ATs and the input and output BDPs. The Flow Manager allows the astronomer to re-run any sequence and only execute tasks whose input parameters have changed. Furthermore, if an input BDP or keyword value for one AT in a flow is altered, the Flow Manager knows to execute not only that AT, but any ATs further along in the flow that depend on the output of altered AT.

ADMIT operates on individual ALMA data cubes. The output BDPs are written to a directory named input-cube-name.admit, where the originating FITS file would be input-cube-name.fits. (As ALMA FITS file names can be rather long, the the user has the option to give an alias for the basename). Each data cube is associated with its own input-cube-name.admit directory. Within that directory, the admit.xml file contains metadata about the BDPs and the summary information that that is used to create the index.html file for displaying the BDPs in the browser. Each BDP created by an AT has a xml file (file extension .bdp) in this directory which contains information about the BDP and pointers to any PNG or image files associated with the BDP. Most users will never examine admit.xml or a BDP file directly, rather they will use the web browser interface or Python methods.

ADMIT expects to be in control the contents of its BDPs so users should not delete files in the input-cube-name.admit directory. Furthermore, if the input-cube-name.admit directory is deleted at the unix level, all information about the flow and all data products are deleted.

Getting Started with ADMIT (for Linux users)

You should have already installed ADMIT on your local machine (see Install Guide).

In the shell that you want to work, there must be a path to casa.

which casa

on your unix command line and you should see the path to casa. If not, you need to either install casa or invoke your local script that defines your path to casa. Similarly, admit should be in your path

     which admit
or   echo $ADMIT

on your unix command line and you should see the path to ADMIT. If you do not, go to the directory where ADMIT was installed and source the admit start-up script:

source admit_start.csh

You can type “echo $ADMIT” again and now you should see the path.

Now you are ready. If you have downloaded an ADMIT products tarball from the ALMA archive and just want to look at the products, you can skip down to the ADMIT in Your Web Browser section on viewing data products. Right now, since ADMIT products are not yet in the archive, you should proceed to the next section to create simple ADMIT data products from an ALMA image in FITS or casa format.

Getting Started with ADMIT (for OS X users)

You should have already installed ADMIT on your local machine (see Install Guide).

In the shell that you want to work, there must be a path to casa.

which casa

on your OS X command line and you should see the path to casa. If not, you need to either install casa or invoke your local script that defines your path to casa. Similarly, admit should be in your path

       which admit
or     echo $ADMIT

on your OS X command line and you should see the path to ADMIT. If you do not, go to the directory where ADMIT was installed and source the admit start-up script:

source admit_start.csh

You can type “echo $ADMIT” again and now you should see the path.

There are now two more steps. First, casa must be able to “see” where ADMIT is. The mac executable ‘casa’ or ‘casapy’ overwrites the system supplied path. To fix this, edit (in your home directory) the ~/.casa/init.py file to reflect both the ADMIT path and the ADMIT/bin path.

import os
import sys


try:
   admit_path = os.environ['ADMIT']
   sys.path.append(admit_path)
       os.environ["PATH"] += os.pathsep + admit_path + '/bin/'  + os.pathsep + '/usr/local/bin/'
except KeyError:
       print("ADMIT path not defined. If you wish to use ADMIT, source the admit_start.[c]sh file.")

(you can find a template of this script in $ADMIT/scripts/casa.init.py) The second thing that must be done is that calls to the ADMIT-supplied script ‘casarun’ must be replaced with calls to the casa-supplied command ‘casa-config.’ As an explicit example, one test that is run to establish the Python-path as seen by casa is performed by running

make python1

This command in the Makefile reads ‘casarun bin/python-env’, and it will hang on OS X. Instead, this should be edited to read ‘casa-config –exec bin/python-env’.

Now you are ready. If you have downloaded an ADMIT products tarball from the ALMA archive and just want to look at the products, you can skip down to the ADMIT in Your Web Browser section on viewing data products. Right now, since ADMIT products are not yet in the ALMA archive, you should proceed to the next section to create simple ADMIT data products from an ALMA image FITS file or casa image.

Prepared ADMIT Recipes

ADMIT will provide standard recipe scripts for common flows. These can be invoked in CASA or at the shell command line. For example, to invoke the recipe Line_Moment in CASA:

CASA<1>: import admit
CASA<2>: admit.recipe("Line_Moment","myimage.fits")

and at the shell command line:

admit_recipe Line_Moment myimage.fits

To see the list of available recipes, type admit_recipe with no arguments. There are some advanced Unix scripts to run ADMIT flows, but these are discussed below. See runa1 and admit1.py.

Making an ADMIT Data Product

ADMIT Tasks – which do the work – can be run directly within casa from the command line, or from scripts in either the unix or casa environment. The goal of ADMIT is to produce, reproduce, and simply modify the production of data products of scientific interest to you so ADMIT must internally keep track of what you are doing. To do this, ADMIT will create a “your-name-choice”.admit directory and store information there. This tracking capability also means that simple ADMIT usage will involve a couple of administrative steps.

Let’s start in the casa environment. At the casa prompt, type:

CASA <1>: import admit
CASA <2>: p  = admit.Project('your-name-choice.admit',dataserver=True)
CASA <3>: t0 = p.addtask(admit.Ingest_AT(file='your-image-cube-name.fits', vlsr=10.0))

The admit.Project command initiates the project, opens the directory with the name that you gave and creates an Python ‘Admit object’ in memory named “p”. The “p” can be anything that you choose; it will become the first piece of every ADMIT task command so chose a short name. The dataserver=True flag causes ADMIT to start up a webpage for showing the results, more on that later (in ADMIT in Your Web Browser). The webpage will be blank until you actually perform calculations.

The addtask command puts an ADMIT task into your flow: in this case, the Ingest_AT. The Ingest_AT brings an image cube into ADMIT. If it is a FITS file, the image cube will be read into a casa image on disk. If it is a casa image, Ingest_AT will just create an ADMIT information file. “t0” is the ADMIT task number. In the ADMIT world, “t0” (or whatever you chose for a name) is the way to refer to your first Basic Data Product (BDP). Since casa images generally do not have information about your source Vlsr, Ingest_AT is typically a good place to input it – in km/sec.

To make a moment map, or zero, first, and second moment maps, from the image cube, you would then type

CASA <4>: t1  = p.addtask(admit.CubeStats_AT(ppp=True), [t0])
CASA <5>: t2  = p.addtask(admit.Moment_AT(mom0clip=2.0, numsigma=[3.0]), [t0, t1])

The CubeStats_AT will produce a series of statistics about your data (t0) which will be stored in BDP “t1”. The Moment_AT produces the requested moment maps for the image cube (“t0”) that your digested. In this case, for the entire cube (all spectral channels) with a S/N cutoff of 3 times the RMS noise determined by CubeStats (the “t1” input), and with the higher moment maps (1,2,3...) clipped to be valid only where the moment zero map is greater then 2 time the RMS.

Up to this point, you have just been creating a flow but the data products have not been calculated. You should have seen an “INFO” message as you entered each of the above lines. To execute your flow, you now type:

CASA <6>: p.run()

p.run causes ADMIT to calculate your data products. The data products can be viewed in your local browser window – there should be one now crested by ADMIT. If not, you can start one up by typing

CASA <7>: p.startDataServer()

If you already have a data server running, the above command, will inform you

A data server for this Admit object is already running on localhost:NNNNN,

where NNNNN is a port number. If so, look through the webpages in your browser to see if it is hiding among your tabs, or copy and paste the localhost:NNNNNN to a new tab. You should now have a browser page with bars for Ingest, CubeStats, and Moment. Click on the bars to see the products. In this case, the most interesting one is probably the moment map which is the integrated emisson over frequency in your cube – the moment zero map.

Great. Now let’s say that you want a spectrum at the highest peak in your moment map. ADMIT can do that because one of the products in the Moment_AT is the pixel location of the peak. To make the spectrum, you use the CubeSpectrum_AT.

CASA <8>: t3 = p.addtask(admit.CubeSpectrum_AT(), [t0, t2])
CASA <9>: p.run()

The p.run() command is needed again. The add-task puts the task into the flow, and p.run() execute it. Your browser page should now have a new line at the bottom which is labeled CubeSpectrum. Click on the bar and you will see your spectrum.

The ADMIT Tasks, as they execute, create a python structure in memory containing all of the task information, and they write out information, images, and files to the “your-name-choice”.admit directory. As long as you remain in your casa session, you have access to the contents of the structure and you can add to the flow, and your browser page will continue to update as you add to and run the flow.

Using ADMIT Scripts

ADMIT can also be run from script files using either the unix command line or the casa command line. The direct connection to the browser page and the ability to add to flows from the command line is only available from within casa because the casa session keeps your python structures persistent in memory. When a script is run from the unix command line, all memory-based products die when the script ends; fortunately, ADMIT writes all of the products to disk so you can view your ADMIT products using the browser as described in the next section.

An ADMIT script looks very much like what you would type on the casa command line. For example, the script below will create all of the same products in the casa session in the last section.

#!/usr/bin/env casarun
# set up admit in the casa environment
import admit
# define project name
p = admit.Project('your-name-choice.admit',dataserver=True )
# Flow tasks.
t0  = p.addtask(admit.Ingest_AT(file='your-image-cube-name.fits'))
t1  = p.addtask(admit.CubeStats_AT(ppp=True), [t0])
t2  = p.addtask(admit.Moment_AT(mom0clip=2.0, numsigma=[3.0]), [t0, t1])
t3  = p.addtask(admit.CubeSpectrum_AT(), [t0, t2])
p.run()

The script can be run in casa using the “execfile” command, or from the unix command line by making the script file executable (chmod +x) and them executing it. The file containing your script should be named ‘anything-you-want.py’

The ‘your-name-choice.admit’ directory includes a file (which is currently called admit0.py) containg a script that will re-run exactly the flow that created ‘your-name-choice.admit’.

Molecular Line Identification

ADMIT is very useful for finding spectral lines in your data, identifying the molecular species and transition of the line, and cutting out a sub-cube which contains only the channels with line emission. The primary tasks for this purpose are LineID_AT and LineCube_AT. LineID_AT find the channel intervals with emission above a user-selected noise level and then tries to identify the lines in the Splatalog database. LineCube_AT cuts out sub-cubes for each identified line emission region and writes out a separate casa image file for each.

Information about the Vlsr of your object is not passed down the ALMA imaging pipeline to your ALMA image cubes. Hence, ADMIT does not have access to the Vlsr or spectral line information that you input in your observing set up and correlator setting in the ALMA OT. The proper identification of lines is greatly aided by having the approximately correct Vlsr of your target source. You are allowed to put this value into ADMIT when you ingest your image cube, and/or when you run LineID_AT. If you use the Vlsr keyword in LineID_AT it overrides the value used in Ingest_AT.

A typical use of LineID_AT would look like this in a script:

#!/usr/bin/env casarun
# set up admit in the casa environment
import admit
# Master project.
p = admit.Project('you-name-choice.admit', Dataserver=True)
# Flow tasks.
t0  = p.addtask(admit.Ingest_AT(file='your-image-cube-name.fits'))
t1  = p.addtask(admit.CubeStats_AT(ppp=True), [t0])
t2  = p.addtask(admit.Moment_AT(mom0clip=2.0, numsigma=[3.0]), [t0, t1])
t3  = p.addtask(admit.CubeSpectrum_AT(), [t0, t2])
t4  = p.addtask(admit.LineID_AT(csub=[0, 0], minchan=4, maxgap=6, numsigma=5.0), [t1, t3])
t5 = p.addtask(admit.LineCube_AT(pad=40), [t0, t4])
t6 = p.addtask(admit.Moment_AT(mom0clip=2.0, moments=[0, 1, 2]), [t5, t1])
t7 = p.addtask(admit.CubeSpectrum_AT(), [t5, t6])
p.run()

The CubeStats_AT is done to get the RMS noise in the cube and to generate two spectra: one consisting of the maximum flux density in each channel and the other the minimum. The CubeSpectrum_AT is run to get the spectrum at the position of the peak total integrated emission. Both of these BDPs are input to LineID_AT to estimate the emission segments and do the line identification. LineCube_AT, Moment_AT, and CubeSpectrum_AT are then repeated for each emission segment identified.

At the present time, some (perhaps many) ALMA total power line cubes have baselines that are not “average” zero in the non-line channels. There are infrequently cases where the 7-m or 12-m interferometric maps have incorrect continuum subtractions but you are best off to correct that by remaking the maps in casa based on a new continuum subtracted u,v dataset. For the total power data, the sequence would be similar to the above with the insertion of two new tasks: LineSegment_AT and ContinuumSub_AT. LineSegment_AT finds the channel segments with emission above your set noise level; ContinuumSub_AT does a spatial pixel by spatial pixel baseline removal in the spectral direction with the emission segments ignored in determining the baseline fit. The output of ContinuumSub_AT is a new image cube with the baseline removed – and that is then fed forward to the rest of the script.

#!/usr/bin/env casarun
# set up admit in the casa environment
import admit
# Master project.
p = admit.Project('you-name-choice.admit', dataserver=True)
# Flow tasks.
t0  = p.addtask(admit.Ingest_AT(file='your-image-cube-name.fits'))
t1  = p.addtask(admit.CubeStats_AT(ppp=True), [t0])
t2  = p.addtask(admit.CubeSum_AT(numsigma=5.0, sigma=99.0), [t0, t1])
t3  = p.addtask(admit.CubeSpectrum_AT(), [t0, t2])
t4  = p.addtask(admit.LineSegment_AT(csub=[0, 0], minchan=4, maxgap=6, numsigma=5.0), [t1, t3])
t5 = p.addtask(admit.ContinuumSub_AT(fitorder=1, pad=60),[t0, t4])
t6 = p.addtask(admit.CubeStats_AT(ppp=True), [t5])
t7 = p.addtask(admit.CubeSpectrum_AT(), [t5, t6])
t8 = p.addtask(admit.Moment_AT(mom0clip=2.0, numsigma=[3.0]), [t5, t6])
t9 = p.addtask(admit.LineID_AT(csub=[0, 0], minchan=4, maxgap=6, numsigma=5.0), [t6, t7])
t10 = p.addtask(admit.LineCube_AT(pad=40), [t5, t9])
t11 = p.addtask(admit.Moment_AT(mom0clip=2.0, moments=[0, 1, 2]), [t10, t6])
t11 = p.addtask(admit.CubeSpectrum_AT(), [t10, t11])
p.run()

Interacting with Line ID

The identification of emission/absorption from specific molecular species and transitions is important to the scientific analysis of ALMA data. The general case of species/transition identification is a difficult problem due to the possibilities of complex line shapes and line blending, and the high density of potential matching lines in the Splatalog database. Add to this the range of physical conditions giving rise to molecular emission in the Universe (cold cores, hot cores, evolved stars, galaxies diffuse ISM) and the perfect identification of species/transition is not practical without significant a priori information, which is not available from the ALMA archive data at present.

LineID_AT attempts to identify lines based first on the most commonly observed species and transitions. CO, CS, HCN, CN, H2CO, and other such common species are given preference in a first search for indentification. The Tier 1 Database contains a list of these molecules along with their transitions. See the following section for a more detailed description of the database. After that a deeper search is done with either the CASA slsearch task or the online splatalogue database. There are several keywords in LineID_AT for controlling aspects of the search and identification. The following are the keywords that may be of the most use to the user.

Keyword Description
vlsr The vlsr of the source in km/s. The closer this is to the source’s average vlsr, the more accurate the results will be.
numsigma Minimum intensity, in terms of the rms noise of the individual sepctra, to consider a given channel to not be noise. Default is 5.0, but lower values may be more appropriate in the cases of lower overall S/N.
minchan Minimum number of consecutive channels above numsigma to consider them part of a line. The default is 4, but smaller or larger values may give better results depending on the typical width of lines in the spectra.
smooth Smooth the input spectra with one of the several available soothing algorithms. The default is to not smooth, but in cases of noisy spectra it is advisable to smooth the data.
force If there is a transition that you want to mark specifically, use the force keyword to pass the information to LineID_AT. Any other transitions will be forbidden from the specified channel region.
reject If there are specific molecules or transitions that you do not want to be considered for identifications, the reject keyword can be used to pass this to LineID_AT.
csub LineID_AT works best when there is no continuum in the input spectra. If the spectra are not continuum free then the csub keyword can be used to remove the continua from the spectra. By definition the spectra from CubeStats_AT have a continuum that needs to be removed. The default ([1, None]) removes this continuum, but leaves all other spectra as they are.

The output of LineID_AT in the browser page includes a table of emission segments found, and identification for each segment if found. The LineId Editor mode in the browser (see tabs along the second line from the top of the ADMIT page for your data prducts). Click on that button and you initiate the capability to edit the results from LineID_AT. You can: change the frequency, id, and channel range of an emission region. You can reject an emission segment; then you can write out your estimate of the best line identification as a replacement for the original LineID_AT BDP, which can be fed into LineCube_AT to cut line cubes. You can also use the force and reject buttons as input advise to a second run of LineID_AT.

The interaction mode with LineID Editor can only be used if your ADMIT file is created or opened from within your current casa session. The editing mode requires that your ADMIT flow be present as an active python memory structure. The interactive edits that you make within LineID Editor are not saved to the flow so, at present, you cannot automatically recreated your final data products by re-running the flow from the scratch.

Tier 1 Database

The Tier 1 Database (DB) contains the transitions of molecules that if present, are expected to be a dominant emission peak in the spectrum. The allowed frequency/velocity ranges for these transitions are relaxed compared to those of others. In gneneral any peak detected within 30 km/s (galactic source) and 200 km/s (extragalactic source) of a Tier 1 rest frequency will be assigned the identification of that transition. Additionally, the identified peak is traced down to the cutoff level and any additional peaks found along the way are also labeled the Tier 1 transition. Tier 1 molecules are:

Molecule Constraints
CO 31.0 - 950.0 GHz
13CO 31.0 - 950.0 GHz
C17O 31.0 - 950.0 GHz
HCO+ 31.0 - 950.0 GHz
HDO 31.0 - 950.0 GHz
CCH 31.0 - 950.0 GHz, HFL
CN 31.0 - 950.0 GHz, HFL, weakest lines eliminated
HCN 31.0 - 950.0 GHz, HFL
HNC 31.0 - 950.0 GHz
13CN 31.0 - 950.0 GHz, HFL, weakest lines eliminated
H13CN 31.0 - 950.0 GHz, HFL
HN13C 31.0 - 950.0 GHz
N2H+ 31.0 - 950.0 GHz, HFL
C18O” 31.0 - 950.0 GHz
H13CO+ 31.0 - 950.0 GHz
DCO+ 31.0 - 950.0 GHz
H2CO 31.0 - 950.0 GHz, weakest lines eliminated, limited to Eu < 200 K
DCN 31.0 - 950.0 GHz, HFL
CS 31.0 - 950.0 GHz
SiO 31.0 - 950.0 GHz
SO 31.0 - 950.0 GHz, weakest lines eliminated
HC3N 31.0 - 950.0 GHz, HFL, weakest lines eliminated
13CS 31.0 - 950.0 GHz
C34S 31.0 - 950.0 GHz

HFL indicates hyperfine lines, these transitions are treated specially in that only the strongest hyperfine line is searched for initially. If that line is found then the rest of the hyperfine components are searched for. There are currently 962 transitions in the DB (542 primary transitions and 420 hyperfine transitions).

You can query the DB directly through python as follows:

from admit.util.Tier1DB import Tier1DB
# connect to the DB
t1db = Tier1DB()
# query for all primary transitions between 90.0 and 90.1 GHz
t1db.searchtransitions(freq=[90.0, 90.1])
# get the results as LineData objects
results = t1db.getall()
# look for any with hyperfine transitions (hfnum > 0) and get them
for line in results:
  if line.getkey("hfnum") > 0:
    t1db.searchhfs(line.getkey("hfnum"))
    hfsresults = t1db.getall()

ADMIT in Your Web Browser

ADMIT Data Products are most easily viewed from your favorite web browser utilizing the index.html file that is present within the input-cube-name.admit (default, or your-alias-name.admit) directory.

You can do this To do so, start up CASA and instantiate an ADMIT object of the output data:

CASA <1>: import admit
CASA <2>: a = admit.Project('/path/to/input-cube-name.admit',dataserver=True)

This will open a new page in your default browser (or new browser window if none was open) and load the ADMIT products web page view of the specified directory. The page is divided into 4 separate tabs: Flow View, Form View, ADMIT Log, LineID Editor, and ADMIT Documentation.

Flow View
This view shows the tasks in the order in which they were executed. At the top is the directed acyclic graph of the entire ADMIT Flow. Each task has a bar giving the task name and arguments. If you click on the bar, that section will expand to show all the output from that task. Clicking on a thumbnail of an image will display a larger version of the image.
Form View
This view allows you to edit task parameters and re-run the ADMIT flow. Similar to Flow View, the tasks are show in execution order and clicking on each bar will expand to give an editable form of the task keywords. Once you are done editting keywords, click on Re-run ADMIT Flow” button at the bottom of the page. This will communicate your changes back to your CASA session and re-run the tasks that you changed (and any that depended on them).
ADMIT Log
This is the full log file of the ADMIT process/script that created your ADMIT data.
LineID Editor
This allows you do modify the results of LineID_AT. Currently in prototype stage.
ADMIT Documentation
Link to the on-line ADMIT documentation webpages.

ADMIT output for multiple projects can be loaded one at a time into separate browser pages. The browser pages do not interact.

For simply viewing the products without a CASA session, you can enter the full directory path into an open browser (file:///full-directory-path as the url) or by using the ADMIT aopen.

aopen index.html or aopen sub-directory-name/index.html

However, note you do not get the Form or LineID Editor functionality with this mode.