Processing SMA Data
1.2 m Telescopes

Submillimeter Array Science Archive

Help Page

Search Form


You may enter a single source name or multiple source names. Multiple source names should each be on a new line. This performs an OR search on the given names.

The source names are the archive are those set by the PIs in the observing script. They will not contain any spaces, and are unlikely to match official catalog names.

The search is case-insensitive.

A sub-string of the source name can be given. If this box is left blank all sources will be searched.

A source name search cannot be combined with a coordinates based search.

You can search by source name OR coordinates, but not both. If both are given, a source name search will take priority.


You may enter a single set of coordinates or multiple sets of coordinates. These should be in J2000 format. Multiple coordinates should be on newlines.

Acceptable formats are:
05 35 17.3 -05 23 28
05 35 17.3-05 23 28
05:35:17.3 -05:23:28

A search radius in arcseconds must be provided. To apply a single radius to all listed sources enter this in the Radius box.

For more flexibility when searching multiple positions, an individual radius can be provided for each set of coordinates. Append this to the end of each line following a comma. In this case the Radius box can be left empty.

05 35 17.3 -05 23 28, 300
13 29 52.7 +47 11 42.9, 1000

A coordinate search cannot be combined with a source name based search.

Object Pairs

This will only search for data where both targets are included in the same file. E.g. a science target with a particular calibrator. The inputs are source names. This search is case insensitive and substrings are acceptable.


The user can provide a specific frequency which must be covered by the spectral window of the data. This is a sky frequency in GHz.

Band (GHz)

The tuning range in which LO frequency falls. The default is "Any"; other possibilities are "185-270" (230+240 GHz RXs), "250-410" (345+400 GHz RXs), "600-696" (600 GHz RX). This can be used to narrow down data to a given window.

Remember that the LO frequency itself is not included in the observed spectral window. The routine setup with the SWARM correlator often tunes two receivers to the same frequency and aligns them spectrally so this gap is filled. This ensures an unbroken coverage of 8GHz.

Date Range (yymmdd-yymmdd)

Default is all dates. Note that the switch over from ASIC to SWARM happened mid-2016. See here for a detailed breakdown of the dates of the correlator switch-over.

Minimum Integration Time

In units of minutes. This is useful for weeding out short observations.

Polarization state

Default is "Any". Be aware that polarization data require special calibration steps. They can be used as non-polarization data but only after the cross-terms have been flagged.

PI (Last name only)

The last name of the Principal Investigator. This search is case insensitive and sub-strings are acceptable.

Project Code

The SMA project code, e.g. 2014A-S043. This search is case insensitive.

Results Page

  • Proprietary data is listed but is not available for download through the public archive. The proprietary period for the SMA is 15 months for regular PI projects.
  • Large datasets have been rechunked by 4 using the SMA program SMARechunker. If you require the full resolution data please email
  • If the data are non-proprietary you will see links to the RAW (and, if available, CAL & IMG) files.
  • If the data have been imaged, the page will display the reduced images and spectra for that source. This only applies to tiny percentage of data.
  • Raw (RAW) files are tar and gzipped MIR/IDL format. Calibrated (CAL) files are tar gzipped MIRIAD format. Imaged (IMG) files are tar/gzipped FITS format.
  • Observing reports are available for nearly all observations since 2007. Comments contained within these reports provide useful feedback to the PI regarding quality of the data and any baseline correction that is needed.
  • Supplemental plots show the weather conditions, phase stability and system temperature for a given night. The phase data is provided for a limited number of baselines depending on which phase monitors are not being covered by an antenna.
  • Users are reminded that raw interferometry data files (actually directories) contain data from multiple sources observed over the course of an observation. This typically includes all the calibration sources you will require for data processing.
  • Your browser may have trouble loading multiple-thousand search results. In this case you should go back and increase the filtering.