AntennaeBand7 for CASA 3.3

Science Target Overview

Fig. 1. HST image of Antennae. White contours correspond to the CO(1-0) intensity map in Wilson et al. (2000) (see also Fig. 2). (Credit: NASA, ESA, and the Hubble Heritage Team STScI/AURA)-ESA/Hubble Collaboration. Acknowledgement: B. Whitmore ( Space Telescope Science Institute) and James Long (ESA/Hubble)

Fig. 2. Caltech millimeter array CO(1-0) integrated intensity map from Wilson et al. (2000).

The Antennae are a nearby (22 Mpc) pair of merging galaxies, NGC 4038 (RA 12h 01m 53.0s, Dec −18° 52′ 10″) in the north and NGC 4039 (RA 12h 01m 53.6s, Dec −18° 53′ 11″) in the south. These two spiral galaxies started to interact only a few hundred million years ago, making the Antennae one of the nearest and youngest examples of a major galaxy merger. The yellow bright components to the south and north of the image center of Figure 1 correspond to the nuclei of the original galaxies and are composed mostly of old stars. Dust filaments, which appear brown in the image, pervade the region between the two nuclei and a (blue) star-forming regions surrounded by HII regions can be seen throughout the system. Wilson et al. (2000) used OVRO to map CO(1-0) emission, a tracer of the bulk molecular gas distribution, with a resolution of 3.15″ x 4.91″ (Figures 1 and 2). Molecular emission is throughout the system and is particularly bright in the the "interaction region" between the nuclei, where it appears concentrated in five supergiant molecular complexes (see Figure 2).

ALMA Data Overview

Coverage of the "Northern Mosaic" carried out for ALMA Science Verification overlaid on an HST image. Circles show individual pointings, which were observed in rapid succession during each of the "Northern" observations.

Coverage of the "Southern Mosaic" carried out for ALMA Science Verification overlaid on an HST image. Circles show individual pointings, which were observed in rapid succession during each of the "Southern" observations.

This CASA Guide steps through reduction and imaging of ALMA Science Verification data targeting the CO 3-2 line in the Antennae galaxy. These data were obtained using the ALMA Band 7 receiver and observed in 10 separate blocks, each typically a few hours long, during May and June 2011. Each block observed one of two mosaic patterns, which we will refer to as the "Northern" and "Southern" mosaics. Figures 3 and 4 show the coverage of these two mosaics on an optical image of the Antennae. Within an individual observing block, observations rotated rapidly among the individual fields of the mosaic being observed. One field was offset from the main body of the galaxy in each mosaic for calibration purposes.

The ten individual data sets are broken down by mosaic as follows...

Northern mosaic (covering the nucleus of NGC 4038):

• uid://A002/X1ff7b0/Xb
• uid://A002/X207fe4/X3a
• uid://A002/X207fe4/X3b9
• uid://A002/X2181fb/X49

Southern mosaic (covering the nucleus of NGC 4039 and some of the interaction region):

• uid://A002/X1ff7b0/X1c8
• uid://A002/X207fe4/X1f7
• uid://A002/X207fe4/X4d7
• uid://A002/X215db8/X1d5
• uid://A002/X215db8/X392
• uid://A002/X215db8/X18

The observations observed two basebands, each associated with one spectral window (see the ALMA Technical Handbook for a discussion of the distinction between basebands and spectral windows). The baseband in the lower sideband (LSB) is centered on CO (3-2) and the baseband in the upper sideband (USB) containing mainly continuum emission. This guide will focus on the reduction of the LSB CO (3-2) data. Each sideband was observed in both a high spectral resolution "Frequency Domain Mode" (FDM) and a lower spectral resolution "Time Domain Mode" (TDM). We will focus on reducing the FDM data, which have an effective total bandwidth of 1.875 GHz (1634 km/s) divided over 3840 channels. The channel width in FDM mode is 488.28 MHz (0.426 km/s), because the data are Hanning smoothing automatically the actual spectral resolution is twice this. The TDM mode data were observed and used mainly for calibration purposes, we will not directly analyze them in this CASA Guide, though we will use calibration products (system temperature measurements) derived from these data.

When these observations were taken, the ALMA antennas were in a configuration that is intermediate between the Cycle 0 "Extended" and "Compact" configurations. We expect this configuration to yield an angular resolution of about 1 arcsecond near 345 GHz.

We thank Junko Ueda for suggesting CO 3-2 observations of the Antennae as an ALMA Science Verification target and providing their SMA CO(3-2) data for verification purposes (Ueda, Iono, Petitpas et al., in preparation, to be submitted to ApJ).

Obtaining the Data

To download the data, click on the region closest to your location:

North America Europe East Asia

Here you will find three gzipped tar files which, after unpacking, will create three directories:

• Antennae_Band7_UnCalibratedMSandTablesForReduction - Here we provide you with "starter" datasets, where we have taken the raw data in ALMA Science Data Model (ASDM) format and converted them to CASA Measurement Sets (MS). We did this using the importasdm task in CASA. Along with the raw data, we also provide some tables that you will need for the calibration. This functionality will be available in CASA for Early Science, but it is still under development.

• Antennae_Band7_CalibratedData - The fully-calibrated uvdata, ready for imaging

• Antennae_Band7_ReferenceImages - The final continuum and spectral line images

To see which files you will need, read on below. The downloads to your local computer will take some time, so you may wish to begin them now.

NOTE: CASA 3.2.1 or later is required to follow this guide. For more information on obtaining the latest version of CASA, see http://casa.nrao.edu.

Antennae Band 7 Data Reduction Tutorial

In this tutorial, or "casaguide", we will guide you step-by-step through the reduction of the ALMA science verification data on the Antennae galaxies and its subsequent imaging. This casaguide consists of two parts:

1) Antennae Band7 - Calibration

2) Antennae Band7 - Imaging

To complete the Calibration section of the tutorial, you will need the data in the first directory: Antennae_Band7_UnCalibratedMSandTablesForReduction. For those wishing to skip the calibration section and proceed to Imaging, we also provide the fully-calibrated data in the Antennae_Band7_CalibratedData directory. Finally, we provide the final continuum and spectral line images in the Antennae_Band7_ReferenceImages directory.

NOTE: These guides are dynamic and will evolve as our understanding of how best to reduce ALMA data improves. Check back for updates periodically.

For a similar tutorial on the reduction of ALMA Band 7 data on TW Hydra, and Band 3 on NGC 3256, see the casaguides TWHydraBand7 and NGC3256Band3.

How to use this casaguide

For both portions of the guide, we will provide you with the full CASA commands needed to carry out each step.

# In CASA
The commands you need to execute 
will be displayed in regions 
like this.

Simply copy and paste the commands in order into your CASA terminal. Be careful with the tabs in the 'for' loops, as this is part of the python format. You may also type the commands in by hand if desired, but be mindful of typos. In loops, note that you may need to hit Enter twice in order for the process to start running. Also note that copying and pasting multiple commands at a time may not work, so only copy and paste the contents of one region at a time.

To learn how to extract the CASA commands into an executable python script, click here.

Occasionally we will also show output to the CASA logger:

This output will be displayed 
in regions like this.

Other relevant information will be presented in the following format:

This color shows you background information about the data or other types of reference material

For a brief introduction to the different ways CASA can be run, see the EVLA_Spectral_Line_Calibration_IRC+10216#How_to_Use_This_casaguide page. For further help getting started with CASA, see Getting_Started_in_CASA.

Daniel Espada 12:00 UT, 27 July 2011