Transcript AAS_Jan2016_VLASS_Lacyx

January 2016 AAS meeting
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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
VLA SKY SURVEY
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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
VLA SKY SURVEY
• I,Q,U polarization.
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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”
VLA SKY SURVEY
January 2016 AAS meeting
Hidden explosions
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VLASS 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 crossidentifications.
• 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 radioloud/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.
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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 viceversa.
• Planetary nebulae
• Refine evolutionary models
• HII regions
• Improve census of massive star formation and galactic structure
models.
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Education and Outreach
• EPO activities have been built into the survey from the
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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.
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How to get involved
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.
“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.
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VLA SKY SURVEY