3C286 Polarization

Last checked on CASA Version 6.5.4

Data Reduction and Imaging Tutorials

This tutorial has been split into calibration and imaging pages:

1. Calibration

   This section of the tutorial steps you through inspection and calibration of the visibility (u-v) data. To complete this part, you will need the data in the 3C286_Band6_UncalibratedData directory.

2. Imaging

   This part of the tutorial focuses on constructing images from the fully calibrated visibility data. If you wish to skip calibration and proceed directly to this part of the tutorial, you will need the fully-calibrated visibility data in the 3C286_Band6_CalibratedData directory.

For information on obtaining the latest version of CASA, see the CASA home page.

For help getting started with CASA, see Getting_Started_in_CASA.

To learn how to extract the CASA commands into an executable python script, see Extracting_scripts_from_these_tutorials.

Guide history for past CASA versions:

• Calibration: [5.4] [5.1] [4.3]
• Imaging: [5.4] [5.1] [4.3]

Obtaining the Data

Calibrated data is provided if you wish to skip the Calibration section and start with Imaging. To download the most recent calibrated data and image products for this guide here:

• https://bulk.cv.nrao.edu/almadata/public/casaguides/3C286_Band6_6.6.1

  3C286_Band6_CalibratedData [~3 GB]

  The fully calibrated u-v data in CASA Measurement Set (MS) format, ready for imaging.

  3C286_Band6_ReferenceImages [~5 MB]

  The final total intensity and polarization images.

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

• North America
• Europe
• East Asia

Here you will find:

3C286_Band6_UncalibratedData [~6 GB]

The raw data files in ALMA Science Data Model (ASDM) format.

Science Target Overview

Figure 1 Maps of 3C286 at 1.4 and 4.8 GHz. (Akujor & Garrington 1995)

Figure 2 3C286 map at 8.4 GHz. The jet to the W of the core is highly polarized with E-vectors parallel to the jet axis at 8.4 GHz. (Akujor & Garrington 1995)

These SV observations have been taken with the aim of testing ALMA polarization capabilities at Band 6 (233 GHz, 1 mm).

The target observed is 3C286: a bright, compact, steep-spectrum radio quasar at a redshift of 0.849 (e.g. Hewett & Wild et al. 2010). Radio imaging with the Very Large Array (VLA) at subarcsecond resolution has revealed an extended structure composed of three misaligned bright features. The linear polarization emission is dominated by the two brightest features (see Figure 1), and the electric vector position angle is oriented nearly parallel to the axis of the jet like structure between them (Akujor & Garringon 1995).

This source has been widely used as calibrator for linear polarization observations at centimeter wavelengths because of its extremely stable polarization angle (33º at frequencies < 10 GHz). At higher frequencies, however, the polarization angle slowly increases from 33º below 10 GHz to 36º at 45 GHz (VLA results from Perley & Butler 2012). Recent results from IRAM, CARMA, and now ALMA are characterizing the polarization of 3C286 at the much higher frequencies of the millimeter regime.

Details of the ALMA results can be found in the Imaging portion of this guide at the end of the Image Visualization and Analysis section, where we also compare the results with available measurements from IRAM and CARMA.

ALMA Data Overview

This CASA Guide shows the calibration and imaging steps for the ALMA Science Verification data in full polarization targeting the quasar 3C286.

The ALMA Science Verification observations consist of three Executions over 1 observing session on July 1st, 2014. The data from each Execution is saved in ASDM format, as follows:

1. uid___A002_X85c183_X10a
2. uid___A002_X85c183_X51a
3. uid___A002_X85c183_X822

All four cross correlation (XX, XY, YX, and YY) measurements were observed using a spectral setup with four 2 GHz spectral windows of 64 channels each (TDM mode with 31.25 MHz resolution per channel). To calibrate the instrumental polarization, we sampled a polarized source (J1337-1257) as a function of paralactic angle every 30 minutes for 5 minutes per sample. The strongly polarized source 3C279 was also observed as a bandpass calibrator; however, it can also be used to check the instrumental polarization calibration.

Using the data for publication

The following statement should be included in the acknowledgment of papers using the datasets listed above:

"This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00017.SV. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ."