Demonstration Science

EVLA Demonstration Science

 A number of observations demonstrating new EVLA and WIDAR capabilities are being undertaken, and are described in the table below. Both raw and calibrated demonstration science data will be public. Raw data can be downloaded through the archive by selecting the project code listed. Processed data will be provided through links from this page, as they become available.

EVLA Demonstration Science Observations

Project Code Overview Observations Notes/status
TDEM0001 5 GHz continuum polarimetry mosaic of the SNR 3C391 for the synthesis imaging summer school data reduction tutorials 7 pointings in D-configuration, two widely separated 128 MHz sub-bands using the 4-8 GHz EVLA receivers Data and casa reduction scripts are available at the casaguides web pageYour browser may not support display of this image.
TDEM0003 (Summer School)
 36 GHz imaging of SiS and HC3N line emission from the AGB star IRC+10216 for the synthesis imaging summer school data reduction tutorials Single pointing with two 8 MHz sub-bands in D-configuration, full polarization, each centered on one of the spectral lines Data and casa reduction scripts are available at the casaguides web pageYour browser may not support display of this image.
TDEM0003 Spectral sweep of the AGB star IRC+10216 from 18 to 26.5 GHz with coarse spectral resolution, plus targetted imaging of several lines between 18 and 40 GHz with higher spectral resolution Single pointing in D and DnC-configurations, 128 MHz sub-bands (2 MHz channels) for spectral sweep, 8 MHz sub-bands (125 kHz channels) for detailed imaging Reduced data are posted here Your browser may not support display of this image.
cassiniF10171412 Tracking of Cassini/Saturn transit and occultation Observation of the June 18, 2010, transit of Saturn, tracking the Ka-band downlink beacon A movie of the Cassini satellite transiting, and being occulted by, Saturn and its rings will be posted here when available
TDEM0006 L and Ka-band imaging of the jet and lobes of M87 Multi-configuration (D/C/B/A) imaging at L and Ka-bands, 2 GHz total bandwidth Awaiting observations in A configurationYour browser may not support display of this image.
TDEM0007 The Crab Nebula Multi-configuration, multi-frequency imaging Awaiting observations in A configuration
TDEM0008 Continuum and spectroscopic imaging of M51 at L-band Multi-configuration, multi-frequency imaging Observations completed; data will be posted here when reduction is complete
TDEM0010 Continuum imaging of M82 Multi-configuration, multi-frequency imaging Awaiting observations in A configuration
TDEM0011 Continuum imaging of Hercules A Multi-configuration, multi-frequency imaging Awaiting observations in A configurationYour browser may not support display of this image.
TDEM0012 Continuum imaging of W50 L-band imaging in the D and C configurations Observations completed; data will be posted here when reduction is complete
TDEM0013 5 GHz and 22 GHz movies of SS433 C-band and K-band imaging in A-configuration: 6 epochs separated by 1 week Awaiting observations in A configuration

WIDAR-0 2009 Demonstration Science

 A 12-station subset of the final EVLA correlator underwent extensive testing and system integration prior to the final shutdown of the VLA correlator. To illustrate the future power of the EVLA we used this 12-station correlator in December 2009 to observe the Orion Hot Core at a wavelength of 1.2 cm, covering a total bandwidth of 3 GHz with 24,000 channels (a spectral resolution of ~1.5 km/s). The resulting cube contains emission from many transitions of ammonia, methanol, and sulphur dioxide, each of which shows a different spatial distribution within the Hot Core. The data are publicly available at this ftp site.

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Figure 2: EVLA WIDAR-0 spectra in the Orion K-L region. Results from 1.5hr integrations with 12 antennas in three 1 GHz wide observations. The spectral image cubes have 24000 channels over 3 GHz, and 96x96 image planes. You can see different species at different places in the image (e.g. Methanol maser lines predominant in NW and SE). Slide taken from presentation at January 2010 meeting of the American Astronomical Society, courtesy Steven Myers (NRAO).

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