IRAS16293Band9 draft: Difference between revisions

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Created page with "Category:ALMA Category:Calibration Category:Spectral line {{checked_6.6.1}} HOW ABOUT SOME LEARNING GOALS? ==Science Target Overview== IRAS 16293-2422 (d=160 pc; Chini 1981) is a well studied nearby Class 0 proto-binary system (consists of sources A and B) located in L1689 (i.e., Ophiuchus star forming cloud). The projected separation between sources A and B is roughly 5" (Mundy et al. 1992; Chandler et al. 2005; Figure 1 left panel). Sub-arcsecond VLA an..."
 
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{{checked_6.6.1}}
{{checked_6.6.1}}


HOW ABOUT SOME LEARNING GOALS?
If you have not used a CASAguide before, you may want to start here: [[ALMA_Tutorials#Introduction]]


==Science Target Overview==
==IRAS16293 Band 9 Data Reduction Tutorial==


IRAS 16293-2422 (d=160 pc; Chini 1981) is a well studied nearby Class 0 proto-binary system (consists of sources A and B) located in L1689 (i.e., Ophiuchus star forming cloud). The projected separation between sources A and B is  roughly 5" (Mundy et al. 1992; Chandler et al. 2005; Figure 1 left panel). Sub-arcsecond VLA and SMA centimeter and  millimeter/submillimeter continuum images have spatially resolved source A as several components associated with protostars and jets (Chandler et al. 2005; Pech et al. 2010).
<pre style="background-color: #ffa07a;">
IRAS 16293-2422 hosts a large-scale quadrupolar outflow (Walker et al. 1988; Mizuno et al. 1990; Castets et al. 2001; Hirano et al. 2001; Garay et al. 2002; Stark et al. 2004; Yeh et al. 2008). The outflow aligned in the east-west direction is currently active and likely originated from source A (Figure 1 right panel). The origin of the other large-scale outflow  aligned in the northeast-southwest direction is not clear.
WARNING: On June 15, 2012 these guides were updated to correct for a 1.2" position error in the  
Previous molecular line studies with the SMA have revealed detailed structure and kinematics in the circumbinary envelope for each component. These imply gas infall and outflow motions (Chandler et al. 2005; Takakuwa et al. 2007; Yeh et al. 2008).
phase calibrator (1625-254). Without correction, the science images will suffer from a similar
In addition, IRAS 16293-2422 exhibits strong emission from a number of complex organic molecules and other species usually associated with hot cores in massive star-forming regions, especially towards source A (e.g., Blake et al. 1994; van Dishoeck et al. 1995; Bottinelli et al. 2004; Kuan et a. 2004; Schoier et al. 2004; Chandler et al. 2005; Huang et al. 2005; Bisschop et al. 2008; Jorgensen et al. 2011; Caux et al. 2011).
offset. The final data products (calibrated science data and images) are available at the science
Finally, source B shows a narrow line width (Bisschop et al. 2008; Jorgensen et al. 2011) and no clear signature of outflow (Chandler et al. 2005). This suggests that the source may be at the very young evolutionary stage; likely even before the mass accretion/loss processes start.
portal as explained below.  
 
</pre>
[[File:intro.jpg|200px|thumb|right|'''Fig. 1.''' Left: Sub-arcsecond continuum image obtained with SMA at 310 GHz by Chandler et al. (2005). Right: Integrated blueshifted and redshifted CO (2-1) image tracing molecular outflow originated from source A. The data were obtained with SMA by Yeh et al. (2008). The emission is integrated over the velocity channels from V_lsr=-7.2 to 3.3 km/s on the blueshifted side and from V_lsr=5.5 to 31.9 km/s on the redshifted side.]]
 
==ALMA Data Overview==


ALMA Science Verification data at Band 9 (602-720 GHz) was taken for IRAS 16293-2422 on April 16 and 17, 2012. The observations have been performed with a seven pointing mosaic centered at RA=16h 32m 22.7s, Dec=-24d28’32.5’’ as shown in Figure 1. The complete 7 pointing mosaic can be seen in Figure 2, superposed on archival SMA data for better visualization.  
The tutorial (called a CASAguide) for reducing these data '''using CASA version 6.6.1''' has been split into calibration and imaging pages. See [[IRAS16293Band9_draft#Obtaining_the_Data]] to download the necessary gzipped tarfiles.


A scheduling block about 2.3 hours long was run four times for a total of about 9.2 hours of observing time. The integration time of each visibility is 6.048 sec, and the total on-source time of of each pointing is between 16 to 20 min. Three data sets were obtained post-transit, while the other one was obtained pre-transit. The name of the four ASDMs are as follows (with the median value
1) '''[[IRAS16293 Band9 - Calibration]]''' : This section of the tutorial steps you through inspection and calibration of the basic visibility (u-v) data. To complete this part, you will need the data in the gzipped tarfile IRAS16293_Band9_UnCalibratedMS.tgz.
of zenithal precipitable water vapor given in parentheses):


*uid___A002_X3d4118_X39b (0.31 mm)
2) '''[[IRAS16293 Band9 - 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 IRAS16293_Band9_CalibratedMS_FIXED.tgz file.
*uid___A002_X3d55cb_X575 (0.65 mm)
*uid___A002_X3d55cb_Xb50 (0.43 mm)
*uid___A002_X3d55cb_X90c (0.41 mm)


Data were obtained with the Double Sideband (DSB) Band 9 receivers. Four basebands were used for obtaining data with Frequency Division Mode (FDM). The baseband centers are located at approximately: 704.249, 691.299, 689.499, and 687.499 GHz. The CO (6-5) line at a rest frequency of 691.473 GHz is strongly detected (though extremely resolved out), along with numerous other weaker (but more compact) organic species throughout all four basebands. Each spectral window is 1.875 GHz in width, and contains 3840 channels. The channel separation is 0.488 MHz (0.2 km/s), but the spectral resolution is factor of 2 poorer (0.4 km/s) due to online Hanning smoothing. The image cubes were made with
We also provide the final continuum and spectral line images in the IRAS16293_Band9_ReferenceImages_FIXED.tgz file.
0.4 km/s channels.
 
These data were obtained using the Cycle 0 Early Science extended configuration which resulted in an angular resolution of about 0.22"
 
[[File:FOVs-2.jpg|200px|thumb|right|'''Fig. 2.'''Pointings (crosses) and field of view (circles with 9”) for the ALMA band 9 SV observations toward IRAS 16293-2422 overlaid on SMA continuum image at 310 GHz obtained with the extended configuration (angular resolution of 0.97”x0.76”). The SMA data were retrieved from archive. The positions of source Aa, Ab, and B reported in Chandler et al. (2005) are denoted by the black dots.]]
 
'''Using the data for publication''': Please use the acknowledgement given at the bottom of the [https://almascience.nrao.edu/alma-data/science-verification Science Verification Data page].


We thank the following people for suggesting IRAS16293 for ALMA Science Verification: Jes Jorgensen, Suzanne Bisschop, Ewine van Dishoeck, Tyler Bourke, Johan Lindberg, Michiel Hogerheijde, Bill Dent, Martin Zwaan, Al Wootten.
If you need these tutorials with an older version of CASA, they are archived at [[IRAS16293Band9_draft#Archived_Casaguide_Versions]]


==Obtaining the Data==
==Obtaining the Data==
Line 68: Line 54:
Please include the following acknowledgement in any papers that result from these data: "This paper makes use of public ALMA Science Verification data.  ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ."
Please include the following acknowledgement in any papers that result from these data: "This paper makes use of public ALMA Science Verification data.  ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ."


==IRAS16293 Band 9 Data Reduction Tutorial==
==Science Target Overview==
 
IRAS 16293-2422 (d=160 pc; Chini 1981) is a well-studied, nearby Class 0 proto-binary system (consisting of sources A and B) located in L1689 (i.e., Ophiuchus star-forming cloud). The projected separation between sources A and B is roughly 5" (Mundy et al. 1992; Chandler et al. 2005; Figure 1 left panel). Sub-arcsecond VLA and SMA centimeter and  millimeter/submillimeter continuum images have spatially resolved source A as several components associated with protostars and jets (Chandler et al. 2005; Pech et al. 2010).
IRAS 16293-2422 hosts a large-scale quadrupolar outflow (Walker et al. 1988; Mizuno et al. 1990; Castets et al. 2001; Hirano et al. 2001; Garay et al. 2002; Stark et al. 2004; Yeh et al. 2008). The outflow aligned in the east-west direction is currently active and likely originated from source A (Figure 1 right panel). The origin of the other large-scale outflow  aligned in the northeast-southwest direction is not clear.
Previous molecular line studies with the SMA have revealed detailed structure and kinematics in the circumbinary envelope for each component. These imply gas infall and outflow motions (Chandler et al. 2005; Takakuwa et al. 2007; Yeh et al. 2008).
In addition, IRAS 16293-2422 exhibits strong emission from a number of complex organic molecules and other species usually associated with hot cores in massive star-forming regions, especially towards source A (e.g., Blake et al. 1994; van Dishoeck et al. 1995; Bottinelli et al. 2004; Kuan et a. 2004; Schoier et al. 2004; Chandler et al. 2005; Huang et al. 2005; Bisschop et al. 2008; Jorgensen et al. 2011; Caux et al. 2011).
Finally, source B shows a narrow line width (Bisschop et al. 2008; Jorgensen et al. 2011) and no clear signature of outflow (Chandler et al. 2005). This suggests that the source may be at the very young evolutionary stage; likely even before the mass accretion/loss processes start.


<pre style="background-color: #ffa07a;">
[[File:intro.jpg|200px|thumb|right|'''Fig. 1.''' Left: Sub-arcsecond continuum image obtained with SMA at 310 GHz by Chandler et al. (2005). Right: Integrated blueshifted and redshifted CO (2-1) image tracing molecular outflow originated from source A. The data were obtained with SMA by Yeh et al. (2008). The emission is integrated over the velocity channels from V_lsr=-7.2 to 3.3 km/s on the blueshifted side and from V_lsr=5.5 to 31.9 km/s on the redshifted side.]]
WARNING: On June 15, 2012 these guides were updated to correct for a 1.2" position error in the
phase calibrator (1625-254). Without correction, the science images will suffer from a similar
offset. The final data products (calibrated science data and images) are available at the science
portal as explained above.  
</pre>


The tutorial (called a casaguide) for reducing these data '''using CASA version 6.6.1''' has been split into calibration and imaging pages:
==ALMA Data Overview==


1) '''[[IRAS16293 Band9 - Calibration]]''' : This section of the tutorial steps you through inspection and calibration of the basic visibility (u-v) data. To complete this part, you will need the data in the first directory: IRAS16293_Band9_UnCalibratedMS.
ALMA Science Verification data at Band 9 (602-720 GHz) was taken for IRAS 16293-2422 on April 16 and 17, 2012. The observations have been performed with a seven pointing mosaic centered at RA=16h 32m 22.7s, Dec=-24d28’32.5’’ as shown in Figure 1. The complete 7 pointing mosaic can be seen in Figure 2, superposed on archival SMA data for better visualization.  


2) '''[[IRAS16293 Band9 - 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 IRAS16293_Band9_CalibratedMS directory.
A scheduling block about 2.3 hours long was run four times for a total of about 9.2 hours of observing time. The integration time of each visibility is 6.048 sec, and the total on-source time of of each pointing is between 16 to 20 min. Three data sets were obtained post-transit, while the other one was obtained pre-transit. The name of the four ASDMs are as follows (with the median value
of zenithal precipitable water vapor given in parentheses):


'''NOTE: CASA 6.1 or later is required to process the data using the guides above''' (see the [https://casa.nrao.edu/casa_obtaining.shtml CASA download page] to obtain the most recent CASA version).
*uid___A002_X3d4118_X39b (0.31 mm)
* The older CASA 6.4 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_6.4]] and [[IRAS16293_Band9_-_Imaging_for_CASA_6.4]]
*uid___A002_X3d55cb_X575 (0.65 mm)
* The older CASA 6.2 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_6.2]] and [[IRAS16293_Band9_-_Imaging_for_CASA_6.2]]
*uid___A002_X3d55cb_Xb50 (0.43 mm)
* The older CASA 6.1 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_6.1]] and [[IRAS16293_Band9_-_Imaging_for_CASA_6.1]]
*uid___A002_X3d55cb_X90c (0.41 mm)
* The older CASA 5.7 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_5.7]] and [[IRAS16293_Band9_-_Imaging_for_CASA_5.7]]
* The older CASA 5.4 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_5.4]] and [[IRAS16293_Band9_-_Imaging_for_CASA_5.4]]
* The older CASA 5.1 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_5.1]] and [[IRAS16293_Band9_-_Imaging_for_CASA_5.1]]
* The older CASA 4.3 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_4.3]] and [[IRAS16293_Band9_-_Imaging_for_CASA_4.3]]
* The older CASA 4.2 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_4.2]] and [[IRAS16293_Band9_-_Imaging_for_CASA_4.2]]
* The older CASA 4.1 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_4.1]] and [[IRAS16293_Band9_-_Imaging_for_CASA_4.1]]
* The older CASA 4.0 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_4.0]] and [[IRAS16293_Band9_-_Imaging_for_CASA_4.0]]
* The older CASA 3.4 versions of the casaguides are still available at:[[IRAS16293_Band9_-_Calibration_for_CASA_3.4]] and [[IRAS16293_Band9_-_Imaging_for_CASA_3.4]]


We also provide the final continuum and spectral line images in the IRAS16293_Band9_ReferenceImages directory.
Data were obtained with the Double Sideband (DSB) Band 9 receivers. Four basebands were used for obtaining data with Frequency Division Mode (FDM). The baseband centers are located at approximately: 704.249, 691.299, 689.499, and 687.499 GHz. The CO (6-5) line at a rest frequency of 691.473 GHz is strongly detected (though extremely resolved out), along with numerous other weaker (but more compact) organic species throughout all four basebands. Each spectral window is 1.875 GHz in width, and contains 3840 channels. The channel separation is 0.488 MHz (0.2 km/s), but the spectral resolution is factor of 2 poorer (0.4 km/s) due to online Hanning smoothing. The image cubes were made with
0.4 km/s channels.  


==How to Use A CASA Guide==
These data were obtained using the Cycle 0 Early Science extended configuration which resulted in an angular resolution of about 0.22"


For tips on using CASA and ways CASA can be run, see [http://casaguides.nrao.edu/index.php?title=EVLA_Spectral_Line_Calibration_IRC%2B10216#How_to_Use_This_casaguide EVLA_Spectral_Line_Calibration_IRC+10216#How_to_Use_This_casaguide] page.
[[File:FOVs-2.jpg|200px|thumb|right|'''Fig. 2.'''Pointings (crosses) and field of view (circles with 9”) for the ALMA band 9 SV observations toward IRAS 16293-2422 overlaid on SMA continuum image at 310 GHz obtained with the extended configuration (angular resolution of 0.97”x0.76”). The SMA data were retrieved from archive. The positions of source Aa, Ab, and B reported in Chandler et al. (2005) are denoted by the black dots.]]


'''To learn how to extract executable Python scripts from the tutorial, see''' [http://casaguides.nrao.edu/index.php?title=Extracting_scripts_from_these_tutorials Extracting_scripts_from_these_tutorials].
'''Using the data for publication''': Please use the acknowledgement given at the bottom of the [https://almascience.nrao.edu/alma-data/science-verification Science Verification Data page].


Within the guides:
We thank the following people for suggesting IRAS16293 for ALMA Science Verification: Jes Jorgensen, Suzanne Bisschop, Ewine van Dishoeck, Tyler Bourke, Johan Lindberg, Michiel Hogerheijde, Bill Dent, Martin Zwaan, Al Wootten.
<source lang="python">
# In CASA
Regions of this color are CASA commands (or definitions) that need to be cut and
pasted in sequence. Wait until one command is finished before pasting another.
Tabs matter in python, make sure that commands that span more than one line and
"for" loops keep their spacing. Sometimes (especially "for" loops) you may need to
explicitly hit enter twice to get the command going.
</source>


<pre style="background-color: #fffacd;">
Information in this color shows excerpts from the CASA Logger output
</pre>


<pre style="background-color: #E0FFFF;">
==Archived Casaguide Versions==
This color shows you background information about the data or other types of reference material
Archived Calibration and Imaging Guides for Older CASA Versions
</pre>
{| class="wikitable" style="margin:left"
|-
| CASA 6.5.4 || [[IRAS16293_Band9_-_Calibration_for_CASA_6.5.4 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_6.5.4 | Imaging]]
|-
| CASA 6.4 || [[IRAS16293_Band9_-_Calibration_for_CASA_6.4 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_6.4 | Imaging]]
|-
| CASA 6.2 || [[IRAS16293_Band9_-_Calibration_for_CASA_6.2 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_6.2 | Imaging]]
|-
| CASA 6.1 || [[IRAS16293_Band9_-_Calibration_for_CASA_6.1 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_6.1 | Imaging]]
|-
| CASA 5.7 || [[IRAS16293_Band9_-_Calibration_for_CASA_5.7 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_5.7 | Imaging]]
|-
| CASA 5.4 || [[IRAS16293_Band9_-_Calibration_for_CASA_5.4 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_5.4 | Imaging]]
|-
| CASA 5.1 || [[IRAS16293_Band9_-_Calibration_for_CASA_5.1 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_5.1 | Imaging]]
|-
| CASA 5.4 || [[IRAS16293_Band9_-_Calibration_for_CASA_5.4 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_5.4 | Imaging]]
|-
| CASA 4.3 || [[IRAS16293_Band9_-_Calibration_for_CASA_4.3 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_4.3 | Imaging]]
|-
| CASA 4.2 || [[IRAS16293_Band9_-_Calibration_for_CASA_4.2 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_4.2 | Imaging]]
|-
| CASA 4.1 || [[IRAS16293_Band9_-_Calibration_for_CASA_4.1 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_4.1 | Imaging]]
|-
| CASA 4.0 || [[IRAS16293_Band9_-_Calibration_for_CASA_4.0 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_4.0 | Imaging]]
|-
| CASA 3.4 || [[IRAS16293_Band9_-_Calibration_for_CASA_3.4 | Calibration]] || [[IRAS16293_Band9_-_Imaging_for_CASA_3.4 | Imaging]]
|}

Latest revision as of 16:31, 25 September 2024

Most recently updated for CASA Version 6.6.1 using Python 3.8

If you have not used a CASAguide before, you may want to start here: ALMA_Tutorials#Introduction

IRAS16293 Band 9 Data Reduction Tutorial

WARNING: On June 15, 2012 these guides were updated to correct for a 1.2" position error in the 
phase calibrator (1625-254). Without correction, the science images will suffer from a similar 
offset. The final data products (calibrated science data and images) are available at the science 
portal as explained below.

The tutorial (called a CASAguide) for reducing these data using CASA version 6.6.1 has been split into calibration and imaging pages. See IRAS16293Band9_draft#Obtaining_the_Data to download the necessary gzipped tarfiles.

1) IRAS16293 Band9 - Calibration : This section of the tutorial steps you through inspection and calibration of the basic visibility (u-v) data. To complete this part, you will need the data in the gzipped tarfile IRAS16293_Band9_UnCalibratedMS.tgz.

2) IRAS16293 Band9 - 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 IRAS16293_Band9_CalibratedMS_FIXED.tgz file.

We also provide the final continuum and spectral line images in the IRAS16293_Band9_ReferenceImages_FIXED.tgz file.

If you need these tutorials with an older version of CASA, they are archived at IRAS16293Band9_draft#Archived_Casaguide_Versions

Obtaining the Data

To download all the data, follow one of the next links:

North America

Europe

East Asia

The links provide you with the option to download the following gzipped tar files:

IRAS16293_Band9_UnCalibratedMS - The file contains the raw data files in ALMA Science Data Model (ASDM) format already converted into CASA Measurement Sets (MS) using importasdm inside CASA.

IRAS16293_Band9_CalibratedMS_FIXED - The fully-calibrated u-v data, ready for imaging.

IRAS16293_Band9_ReferenceImages_FIXED - The final continuum and spectral line images. 

WARNING: On June 15, 2012 the calibration guide and the final data products (calibrated science 
data: IRAS16293_Band9_CalibratedMS_FIXED.tgz and reference images: IRAS16293_Band9_ReferenceImages_FIXED.tgz)) 
were changed to correct for a 1.2" position error in the phase calibrator (1625-254). Without 
correction, the science images will suffer from a similar offset.

You can work with these data products at any of the three stages: the UnCalibratedMS, the Calibrated MS (ready for imaging, or the ReferenceImages. Warning: the UnCalibrated data is large.

Caveat: Before using the ReferenceImages for scientific purposes, please note that only a few of the very strongest lines have been excluded from the continuum subtraction or continuum imaging - you may wish to do a more careful job if your science application is strongly dependent on the flux density or morphology of source B, in particular which shows both strong absorption and emission at the 0.2" resolution of these data. Additionally, there was a glitch in the System Temperature (Tsys) measurements for the absolute flux calibrator, Juno, necessitating the application of Tsys from another source at different elevation. Together with the inherent uncertainties in the Juno flux density model (it has a large crater), the overall absolute flux density uncertainty is at least 20%.

Please include the following acknowledgement in any papers that result from these data: "This paper makes use of public ALMA Science Verification data. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ."

Science Target Overview

IRAS 16293-2422 (d=160 pc; Chini 1981) is a well-studied, nearby Class 0 proto-binary system (consisting of sources A and B) located in L1689 (i.e., Ophiuchus star-forming cloud). The projected separation between sources A and B is roughly 5" (Mundy et al. 1992; Chandler et al. 2005; Figure 1 left panel). Sub-arcsecond VLA and SMA centimeter and millimeter/submillimeter continuum images have spatially resolved source A as several components associated with protostars and jets (Chandler et al. 2005; Pech et al. 2010). IRAS 16293-2422 hosts a large-scale quadrupolar outflow (Walker et al. 1988; Mizuno et al. 1990; Castets et al. 2001; Hirano et al. 2001; Garay et al. 2002; Stark et al. 2004; Yeh et al. 2008). The outflow aligned in the east-west direction is currently active and likely originated from source A (Figure 1 right panel). The origin of the other large-scale outflow aligned in the northeast-southwest direction is not clear. Previous molecular line studies with the SMA have revealed detailed structure and kinematics in the circumbinary envelope for each component. These imply gas infall and outflow motions (Chandler et al. 2005; Takakuwa et al. 2007; Yeh et al. 2008). In addition, IRAS 16293-2422 exhibits strong emission from a number of complex organic molecules and other species usually associated with hot cores in massive star-forming regions, especially towards source A (e.g., Blake et al. 1994; van Dishoeck et al. 1995; Bottinelli et al. 2004; Kuan et a. 2004; Schoier et al. 2004; Chandler et al. 2005; Huang et al. 2005; Bisschop et al. 2008; Jorgensen et al. 2011; Caux et al. 2011). Finally, source B shows a narrow line width (Bisschop et al. 2008; Jorgensen et al. 2011) and no clear signature of outflow (Chandler et al. 2005). This suggests that the source may be at the very young evolutionary stage; likely even before the mass accretion/loss processes start.

Fig. 1. Left: Sub-arcsecond continuum image obtained with SMA at 310 GHz by Chandler et al. (2005). Right: Integrated blueshifted and redshifted CO (2-1) image tracing molecular outflow originated from source A. The data were obtained with SMA by Yeh et al. (2008). The emission is integrated over the velocity channels from V_lsr=-7.2 to 3.3 km/s on the blueshifted side and from V_lsr=5.5 to 31.9 km/s on the redshifted side.

ALMA Data Overview

ALMA Science Verification data at Band 9 (602-720 GHz) was taken for IRAS 16293-2422 on April 16 and 17, 2012. The observations have been performed with a seven pointing mosaic centered at RA=16h 32m 22.7s, Dec=-24d28’32.5’’ as shown in Figure 1. The complete 7 pointing mosaic can be seen in Figure 2, superposed on archival SMA data for better visualization.

A scheduling block about 2.3 hours long was run four times for a total of about 9.2 hours of observing time. The integration time of each visibility is 6.048 sec, and the total on-source time of of each pointing is between 16 to 20 min. Three data sets were obtained post-transit, while the other one was obtained pre-transit. The name of the four ASDMs are as follows (with the median value of zenithal precipitable water vapor given in parentheses):

  • uid___A002_X3d4118_X39b (0.31 mm)
  • uid___A002_X3d55cb_X575 (0.65 mm)
  • uid___A002_X3d55cb_Xb50 (0.43 mm)
  • uid___A002_X3d55cb_X90c (0.41 mm)

Data were obtained with the Double Sideband (DSB) Band 9 receivers. Four basebands were used for obtaining data with Frequency Division Mode (FDM). The baseband centers are located at approximately: 704.249, 691.299, 689.499, and 687.499 GHz. The CO (6-5) line at a rest frequency of 691.473 GHz is strongly detected (though extremely resolved out), along with numerous other weaker (but more compact) organic species throughout all four basebands. Each spectral window is 1.875 GHz in width, and contains 3840 channels. The channel separation is 0.488 MHz (0.2 km/s), but the spectral resolution is factor of 2 poorer (0.4 km/s) due to online Hanning smoothing. The image cubes were made with 0.4 km/s channels.

These data were obtained using the Cycle 0 Early Science extended configuration which resulted in an angular resolution of about 0.22"

Fig. 2.Pointings (crosses) and field of view (circles with 9”) for the ALMA band 9 SV observations toward IRAS 16293-2422 overlaid on SMA continuum image at 310 GHz obtained with the extended configuration (angular resolution of 0.97”x0.76”). The SMA data were retrieved from archive. The positions of source Aa, Ab, and B reported in Chandler et al. (2005) are denoted by the black dots.

Using the data for publication: Please use the acknowledgement given at the bottom of the Science Verification Data page.

We thank the following people for suggesting IRAS16293 for ALMA Science Verification: Jes Jorgensen, Suzanne Bisschop, Ewine van Dishoeck, Tyler Bourke, Johan Lindberg, Michiel Hogerheijde, Bill Dent, Martin Zwaan, Al Wootten.


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