1. The Very Large Array Sky Survey
Description and Survey Science
Mark Lacy, for the VLASS Science Survey Group.
Galactic Center (Survey) Multiwavelength Image
Credit: X-ray: NASA/UMass/D.Wang et al., Radio: N
RAO/AUI/NSF/NRL/N.Kassim, Mid-Infrared: MSX

2. Survey parameters “All-sky” (above declination -40 deg).
Resolution: 2.5”
Frequency: 3GHz (2-4GHz less RFI affected regions)
Cadence: 3 epochs separated by 32 months, starting Oct 2017 pending reviews (pilot survey summer 2016).
RMS per epoch: 120muJy
Co-added RMS: 69muJy
I,Q,U polarization.

3. Science drivers “Hidden explosions” and other radio transients.
Faraday tomography of the magnetic sky.
AGN and galaxy evolution in concert with new optical/IR surveys.
Peering through our dusty Galaxy.
“Missing physics”

4. Hidden explosions VLASS will open new parameter space for finding
dusty/unbeamed GRBs, SNe, compact object mergers

5. Faraday tomography
The properties of the magneto-ionic medium in AGNs and galaxies: wide bandwidth (2-4GHz less some RFI affected regions) will allow rotation measure estimates for ~105 sources. Essential for studies of AGN feedback.
Faraday rotation map of Milky Way will increase in resolution by a factor of ~10.
Oppermann et al (NVSS)

6. AGN and galaxy evolution
New generations of wide area optical/IR surveys will benefit from a high resolution radio survey for cross-identifications.
PanSTARRs, DES, LSST – need radio data of comparable resolution to make reliable identifications as source density is so high (~50-100/square arcminute).
In conjunction with photo-zs from these surveys (+WISE), will be able to determine accurate demographics of radio-loud/intermediate population, important for constraining AGN feedback theories.
VLASS will provide a baseline for follow-up of AGN flares and candidate black hole merger events from gravitational wave detectors.

7. Galactic Science – peering through our dusty galaxy
Extreme pulsars – identify candidate double neutron stars, millisecond pulsars for follow-up
Potential for finding exotic systems e.g. pulsar-BH binary with which to refine tests of GR.
Cools stars with active coronae
Cross-correlate variable objects in VLASS with LSST and vice-versa.
Planetary nebulae
Refine evolutionary models
HII regions
Improve census of massive star formation and galactic structure models.

8. Education and Outreach
EPO activities have been built into the survey from the start.
Will use social media to explain the survey and report on its progress. #VLASS
“Picture of the week”
Citizen Science (e.g. Radio Galaxy Zoo, transient searches).
Science stories and blogs.
Educational activities (in partnership with NRAO and other institutions).
Science community updates.

9. How to get involved
We are actively seeking scientists who are interested in helping with the survey and data products. Please with a brief description of your interests and I will put you in touch with the appropriate science or technical working group.
“All-sky” (above declination -40 deg).
Resolution: 2.5”
Frequency: 3GHz (2-4GHz less RFI affected regions)
Cadence: 3 epochs separated by 32 months, starting Oct 2017 (pilot survey summer 2016).
RMS per epoch: 120muJy
Co-added RMS: 69muJy
I,Q,U polarization.