Time Domain, Cosmology, Fundamental Physics...Metzger & Berger 2012 Jetted Stellar Tidal Disruption...
Transcript of Time Domain, Cosmology, Fundamental Physics...Metzger & Berger 2012 Jetted Stellar Tidal Disruption...
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Time Domain,
Cosmology, &
Fundamental Physics
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Participants • External Chair: Geoff Bower
(ASIAA) * slides compliments of • Internal Chair: Paul Demorest
(NRAO) • Jim Braatz • Avery Broderick • Sarah Burke-Spolaor • Bryan Butler • Tzu-Ching Chang • Laura Chomiuk • Jim Cordes • Jeremy Darling • Jean Eilek • Dale Frail
• Gregg Hallinan • Nissim Kanekar • Michael Kramer • Dan Marrone • Walter Max-Moerbeck • Brian Metzger • Miguel Morales • Steve Myers • Rachel Osten • Frazer Owen • Michael Rupen • Andrew Siemion • Ashley Zauderer
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Important
• Wide frequency coverage
• Large field of view/fast survey speed
• Balance: – High resolution (localization)
– Faithful imaging (diffuse plasma structures)
• A case for long baselines?
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Headliners
Image credits: R. Eatough/MPIfR; NASA;
Galactic Center Pulsars Astrometric Cosmology
Multi-messenger Astronomy
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Time Domain
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Advanced LIGO and GW Detection Major Increase in Sensitivity in 2016+
But source localization is poor
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Radio Counterparts of LIGO Gravitational Wave Sources
Nakar & Piran (2011) Metzger & Berger 2012
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Jetted Stellar Tidal Disruption Events
Berger et al. 2012
Bloom et al. 2011
Synchrotron Radio Emission from Shocked ISM Around Black Hole (Giannios & Metzger 2011)
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Under the Hood of Nature’s Particle Accelerators
Gamma-Ray Novae (Chomiuk et al. 2014, Nature)
Synchrotron knots
embedded in thermal ejecta
Simulated image of X-ray binary GRS 1915+105
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Peeling the Onion: Frequency agility Radio tomography
Yields density profiles, total masses, 3D geometry
1 GHz
10 GHz photosphere
100 GHz
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Fundamental Physics
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Using Pulsars to Measure Spacetime Around Sgr A*
χ = 0.9997 ± 0.0010
Liu et al 2012
Shapiro delay
Einstein delay
Precession of periastron
Black Hole Mass Black Hole Spin
acceleration
100 µas timing
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GC Radio Pulsars
Deneva et al 2009 Bower et al 2014
Kramer Talk!
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Fundamental Constant Evolution
• 22 free parameters in Standard Model of particle physics and General Relativity
• Fine structure constant, α = e2/ℏc; proton-electron mass ratio, μ = mp/me. Changes in μ likely larger than those in α.
• Astronomical spectroscopy in different atomic/molecular lines from high-z absorbers allows us to probe cosmological evolution in μ , α.
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[∆α/α] = (−5.4 ± 1.1) × 10−6 (0 < z < 1.8)
“EVIDENCE” FOR A CHANGING α ?
(Murphy et al. 2004, Lect. Notes Phys.)
Many-multiplet method
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Fundamental Constants Radio Wave Results
• Many molecular transitions sensitive to changes in , . Few systematics if all lines from single molecule.
• Best constraints on changes in μ ! – [∆µ/µ] < few × 10−7 (NH3, CH3OH: Effelsberg, GBT,
VLA) • Sensitivity to changes in , increases non-
linearly with telescope sensitivity, due to multiple absorbers and multiple techniques. – 10 × VLA: [∆µ/µ] ~ few × 10−10 from z ~ 2.
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Plasma Physics
Arendt et al 2011 M87 Cotton et al 2009
• Particle acceleration • Magnetic reconnection Requirements • Surface brightness sensitivity • Broad, continuous frequency
coverage
Solar Flares Crab Nebula Abell 2256
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Revealing the Plasma Physics of Star-Planet Interactions
• Cool stellar mass loss characterized by an ionized stellar wind ➜ favors higher radio frequencies for detection
• Star-exoplanet interactions: evaporation of atmosphere from close-in planetary companion • Particle flux interaction with exoplanet magnetic field can affect planetary dynamo • NGVLA can provide the most sensitive direct detection of the stellar wind
artist’s conception of evaporating exoplanet atmosphere
Earth-Sun interaction is complex, composed of radiation, particles and magnetic field interactions
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Cosmology
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Progress with Megamaser Surveys
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• 162 galaxies detected
out of > 3000 observed
• ~ 37 have evidence of being in a disk and are suitable for MBH measurement
• ~ 10 suitable for distance measurement
• Primary sample for
surveys: Type 2 AGNs at z < 0.05
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A Sample of VLBI Maps of H2O Megamaser Disks
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NGC 6323 Mrk 1419 NGC 2273 J0437+2456
UGC 3789 NGC 6264 NGC 1194 NGC 5765b
IC 2560
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The H2O Megamaser in UGC 3789
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Summary of Results for Megamaser Science
• MCP measurement of H0 is one-step, geometric measurement that provides a critical complement to measures using standard candles.
• Megamasers determine H0 = 70.4 ± 3.6 km s-1 Mpc-1. The measurement can be improved by measuring additional galaxies, and increasing sensitivity.
• Megamasers have determined gold standard masses of SMBH in ~20 galaxies. These measurements demonstrate departures from M-σ relation at the low-mass end and provide a more realistic view of galaxy/BH evolution than a universal M-σ relation.
• Megamasers provide the only means of direct imaging gas in AGN on sub-pc scales. Thin megamaser disks present a puzzle for AGN unification models
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Requirements for a Next Gen Radio Telescope for Megamaser Science and Astrometry
• With the NG instrument, we would aim to measure H0 to ~1% to constrain models of dark energy and fundamental physics, and we aim to measure BH masses in >> 100 galaxies.
• Sensitivity and resolution are key. To optimize science, a new telescope should have at least ~20% of its collecting area in long baselines (~ 5000 km).
• UV coverage requirements are modest. The long baselines could be achieved with ~ 5 100-m class apertures.
• Frequency coverage for the long baselines must include up to 22 GHz to get the H2O line. Higher frequencies may prove useful for imaging other maser lines (e.g. SiO at 46 GHz) but are currently lower priority.
• The recording and correlator requirements for spectral line work are in line with current capabilities. It should permit imaging ~ 1 GHz contiguously with spectral resolution of at least ~ 25 kHz.
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Intensity Mapping the Cosmic Web
Neutral Hydrogen
Massive Galaxies Ionized Gas
The Multitude of Galaxies: Milky Way Building Blocks
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Even NG VLA Is Limited in the Galaxy Population it Can See
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Same approach as taken for microwave background and HI EoR
time
x y
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HI Intensity Mapping
• GBT HI @ 600 MHz
• DEEP2 Galaxies @ Z~1
• Statistical detection of angular correlation between HI noise and galaxies
• Chang et al. 2010 • Masui et al 2012
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The Era of Wide Area OIR Surveys
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Technical Requirements of Intensity Mapping
• Wide field of view • Dense (u,v) coverage • Broad frequency
coverage • Coarse frequency
resolution
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Technical Requirements Technical Requirement Science Case
Long Baselines Megamasers, astrometry, resolved galactic transients
Compact Configuration Plasma physics, intensity mapping, GC pulsars, megamasers, fundamental constants
Wide Field of View/Survey Speed Intensity mapping, EM GW sources
High Frequencies (> 50 GHz) Fundamental constants, intensity mapping, plasma physics
High Time Resolution (imaging, beamforming)
GC Pulsars
Real time processing Transients
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More information
• Wiki – https://safe.nrao.edu/wiki/bin/view/NGVLA/Time
CosmologyPhysicsSWG
• Whitepaper – arXiv:1510.06432
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To Consider
• Compact Configurations and Field of View – What fraction of the collecting area should be packed
into a dense configuration? • Long Baselines
– Astrometric science requires an integrated long baseline array
• Synoptic Surveys – Do the science cases favor a model of individual
targets or large area surveys? • Experiment or Facility?