the very large array sky survey
DESCRIPTION
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.TRANSCRIPT
VLA SKY SURVEY
January 2016 AAS meeting 1
THE VERY LARGE ARRAY SKY SURVEYDescription and Survey ScienceMark Lacy, for the VLASS Science Survey Group.
Galactic Center (Survey) Multiwavelength ImageCredit: X-ray: NASA/UMass/D.Wang et al., Radio: NRAO/AUI/NSF/NRL/N.Kassim, Mid-Infrared: MSX
VLA SKY SURVEY
January 2016 AAS meeting 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.
VLA SKY SURVEY
January 2016 AAS meeting 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”
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Hidden explosionsVLASS will open new parameter space for finding dusty/unbeamed GRBs, SNe, compact object mergers
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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. 2012 (NVSS)
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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.
VLA SKY SURVEY
January 2016 AAS meeting 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.
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January 2016 AAS meeting 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 email updates.
VLA SKY SURVEY
January 2016 AAS meeting 9
How to get involved
• “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.
We are actively seeking scientists who are interested in helping with the survey and data products. Please email [email protected] with a brief description of your interests and I will put you in touch with the appropriate science or technical working group.