asteroseismology and the time domain revolution in astronomy marc pinsonneault ohio state university...
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Asteroseismology and the Time Domain Revolution in
Astronomy
Marc Pinsonneault
Ohio State UniversityCollaborators:The APOKASC teamMelissa NessMarie Martig
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The Need for Precision Stellar Astrophysics
Stars are important across a wide range of astrophysics
Origins Questions– Planet Formation– Structure Formation
Complex Observational Patterns: Things Move!Þ Precise Data NeededÞ Need Better Stellar Physics
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Kepler mission:160,000 stars
monitored
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Waves are Generated by Turbulence in Stars
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Two Major Impacts of AsteroseismologyWe can measure fundamental properties (mass, radius, age, rotation) in bulk stellar populations
Extremely precise surface gravities are a natural product
We have entirely new categories of stellar observables– Surface CZ depth– He ionization– Core rotation– Core mass and density
Spectroscopy + Asteroseismology 2Gether 4Ever
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Solar-like Oscillations in Kepler16 Cyg AMetcalfe et al. 2012
Pure p-mode pattern
nmaxRotational Splittings
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The observed oscillation
pattern is a strong
function of log g
From Chaplin & Miglio 2013
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Giants and Kepler
Giants are high-amplitude pulsators– Periods of days to months
Long period is a huge advantageÞ Accessible with 30 minute cadenceÞ 16,000 stars monitored, essentially all detected
(Mosser et al. 2009; Hekker et al. 2010)
Observed frequency pattern is complex!
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Giant and Dwarf Frequency Patterns Compared
CM13
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The Complex Giant Pattern is Explained by Mixed Modes
Mixed modes propagate as p-modes in the convective envelope and g-modes in the deep core; especially strong impact on l=1
l=0 modes are pure p-modes
Seen in red giants (Bedding et al. 2010) because the p and g mode frequencies become commensurate
Comparing the two yields distinct diagnostics of core and envelope properties
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Distinct Patterns in Different Evolutionary States
Dwarf Subgiant
RGB RCCM13
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Scaling Relations for Bulk Populations
Two most basic observables: – Frequency of maximum
power– Mean frequency spacing
Hekker et al. 2010data for Kepler giants
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Radius and Mass Scaling in ClustersDiscrepancy for clump giant radii relative to RGB radii (~0.05) tied to structural properties
Small but real mass difference 0.06-0.08 Msun, RGB vs. that expected from EB constraints on the MS (Brogaard et al. 2012)
Miglio et al. (2012)
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Epstein et al. (2014)
Trouble In Halo-Land
Halo Star Masses From SR Are WellAbove Expected Values….
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Beyond Scaling Relations:Towards Reliable Masses
Boutique Modeling:Reasonable Mass!
Parallax+ Dn:Reasonable Mass!
Gaia will have a huge impact
Calibrate…Correct…OR
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Two Paths ForwardBoutique Modeling
Use the full information in the frequency spectrum
Use absolute frequencies for evolutionary state
Replace nu(max) with g-mode spacings
Add in proper modeling of mean density
Parallax Über Alles
P + Fluxes+ Teff = R
Add in proper modeling of mean density
Profit!
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APOGEE at a GlanceThe Apache Point Observatory Galactic Evolution ExperimentOperates in the near-infrared (H band): 1.51-1.68 mmTargeted ~105 RG stars sampling the bulge, disk(s), and halo(es)DR10 (Ahn et al. 2014): [M/H], [a/Fe] DR11-12 (Alam et al. 2015) 15 Element Mix (C, N, O, Na, Mg, Al, Si, S, K, Ca, Ti, V, Mn, Fe, Ni)
More numbers!• S/N = 100+/pixel• R ~ 22,500• ~230 science fibers, 7 deg2
FOV• RV precision: ~ 100 m/s• Abundance precision: <0.1
dexS. R. Majewski
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APOKASC SummarizedORIGINAL KEPLER FIELD
Dwarfs: Kepler Field Control– ~2,000 (AU 2015)– ~7,000 (SU 2016)
Giants: Population Asteroseismology– DR10: 1,916 (Pinsonneault et al. 2014)– DR11+12: ~8,000 (AU 2015)– DR13: ~16,000 (SU 2016)
Targeting Criterion:H<11 (1 hour exposure)Teff < 5500 K
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Automated Pipeline Analysis
Boutique analysis of 100,000 targets…NO.
Automated fitting algorithm (FERRE) for the entire H band spectrum
Ex post facto calibration of results against independent measurements– Star cluster members– Asteroseismic log g
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Calibrating the Pipeline: Temperatures
Meszaros et al. (2013)Star Cluster Data
Holtzman et al. (2015)Low Reddening Photometric Temperatures
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Calibrating the Pipeline:Surface Gravity
Meszaros et al. (2013):Cluster Star + asteroseismic log g
Holtzman et al. (2015)Pure asteroseismic log g
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Calibrating the Pipeline:Metallicities
Meszaros et al. (2013)
Holtzman et al. (2015)
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New: 15 Element Mixture
Individual Elements fit with a limited line list calibrated vs. cluster stars
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APOGEE: 100,000 Red Giant Spectra
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The APOKASC ApproachAPOGEE sample: 1916 stars that pass quality control checks
Extract mean asteroseismic properties (Dn, nmax)
Scaling relations + grid-based modeling
Pinsonneault et al. 2014
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Results: Snapping Into Focus
Photometry Spectroscopy Asteroseismology +SpectroscopyPinsonneault et al. 2014
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Mass Trends, Fixed [Fe/H]
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Metallicity Trends, Fixed Mass
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A Test of Atmospheres
The difference between asteroseismic and spectroscopic log g is different for RC, RGB
Is this an atmospheres or asteroseismic systematic?
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One Size Does Not Fit All
Macroturbulence is very different in the clump and RGB
Þ Different line broadening
Þ Impacts gravities
Massarotti et al. 2008
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Testing the Assumptions of Chemical Tagging
Martig et al. 2015 4% of high [a/Fe] stars are young (or mergers)
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…Invisible to Traditional Surveys
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On the Way:Much larger a-rich, metal-poor samples
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New in 2015: Richer Phase Space Coverage
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Much Larger Sample Size
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The Future of Large Spectroscopic Surveys?
Ness et al. 2015a
“Cannon”
Compare Spectra toEmpirical Calibrators,Not Directly to Models
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From Spectra to Mass and Age
Surface C/N, C12/C13 are strongly related to mass through 1st dredge-up
=> Spectroscopic Mass labelling of red giants!
Martig et al. 2015b
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An Age Map of the Red Clump…
Asteroseismic Masses Inferred From Spectra (Ness et al. 2015b)
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…Across the Galaxy
Ness et al. 2015b
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Kepler Rebooted: K2
The New Kepler Mission: Step and Stare in the Ecliptic PlaneStrong overlap with APOGEE fields; opportunity for samplinga wide range of stellar populations-TESS; PLATO;…..
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Future: SDSS-4 + K2
SDSS-4: Two spectrographs (north and south)
K2 – numerous APOGEE targets already in fields, used for targeting.
10,000+ fibers reserved for K2 targets