Asteroseismology - Meetings (Indico)€¦ · Asteroseismology . Standing sound waves . Observing...
Transcript of Asteroseismology - Meetings (Indico)€¦ · Asteroseismology . Standing sound waves . Observing...
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Asteroseismology
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Asteroseismology
Standing sound waves
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Observing standing waves
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The power spectrum
1
1 1 0
0 2
0
2 2
∆ν
Fourier transform of light curve
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1
1 1 0
0 2
0
2 2
∆ν
Ensemble seismology: M, R, L
mHzTTRR
MM
effeff
1.3/)/(
/
,*2
*
*max ×≅ν
Power location:
HzRRMM µν 135
)/()/(
2/3*
2/1* ×≅∆
Frequency spacing:
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1
1 1 0
0 2
0
2 2
∆ν
Ensemble seismology: M, R, L
mHzTTRR
MM
effeff
1.3/)/(
/
,*2
*
*max ×≅ν
Power location:
R, Teff L
distance
HzRRMM µν 135
)/()/(
2/3*
2/1* ×≅∆
Frequency spacing:
Miglio 2012
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1
1 1 0
0 2
0
2 2
∆ν
Ensemble seismology: M, R, L
mHzTTRR
MM
effeff
1.3/)/(
/
,*2
*
*max ×≅ν
Power location:
R, Teff L
distance
HzRRMM µν 135
)/()/(
2/3*
2/1* ×≅∆
Frequency spacing:
Miglio 2012
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Our Galaxy
Hippoarcos + Copenhagen-Geneva Survey
Bulge
Stellar halo
Stellar disk(s)
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Early results from Kepler and CoRoT
Credit: Miglio
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Model of Milky Way (TRILEGAL)
Kepler data (MS+subgiants)
Chaplin et al. (2011)
Early results from Kepler and CoRoT
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Miglio, Chiappini, Morel et al. 2013
Early results from Kepler and CoRoT
LRa01
LRc01
Observed Red giant stars
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Mathur et al., in prep
New oscillating Kepler giants!
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The Kepler mission 2009-2013
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K2: The concept
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K2: Funded 2 yrs of campaigns Each campaign field: 10-20K stars observed for ~80 days
Campaign 9
Campaign 8
Campaign 7
Campaign 6 Campaign 5
Campaign 4
Campaign 3
Campaign 2
Campaign 1
Campaign 0
2014 Fields 2015 Fields 2016 Fields
“Galactic coordinates”
Campaign 10
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K2: 2014-2016+
RA and Dec coordinates
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K2: 2014-2016+
RA and Dec coordinates
Calibrated pixels delivered
Sep 2014
Dec 2015
Apr 2015
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K2: Instrument performance
• Instrument is performing well. • Spacecraft has fuel for at least 2 years, perhaps 4+ years. • Remaining reaction wheels are behaving. • Initial increase in reaction time for Attitude Control
System (ACS) resulted in noise being motion dominated. • Decrease in ACS reaction time starting in C3 (reduce
motion noise by factor 3-4). • Kepler : 12mag, 6.5hr 30ppm • K2 C0-2: 60ppm (C0 worst!) • K2 C3+ : 40ppm expected
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K2: Instrument performance
• Instrument is performing well. • Spacecraft has fuel for at least 2 years, perhaps 4+ years. • Remaining reaction wheels are behaving. • Initial increase in reaction time for Attitude Control
System (ACS) resulted in noise being motion dominated. • Decrease in ACS reaction time starting in C3 (reduce
motion noise by factor 3-4). • Kepler : 12mag, 6.5hr 30ppm • K2 C0-2: 60ppm (C0 worst!) • K2 C3+ : 40ppm expected
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The K2 Galactic Archaeology Program (GAP)
PI: Dennis Stello, CoIs: Derek Buzasi, Ken Freeman, Savita Mathur, Andrea Miglio, Sanjib Sharma, Marc Pinsonneault, Collaborators: Friedrich Anders, Borja Anguiano, Martin Asplund, Sarbani Basu, Paul Beck, Othman Benomar, Maria Bergemann, Joss Bland-Hawthorn, Tiago Campante, Luca Casagrande, Peter De Cat, Márcio Catelan, Bill Chaplin, Cristina Chiappini, Enrico Corsaro, Orlagh Creevey, Eric Depagne, Patrick Eggenberger, Yvonne Elsworth, Jianning Fu, Rafael A. Garcia, Leo Girardi, Jennifer Johnson, Ulrike Heiter, Saskia Hekker, Paola Marigo, Eric Michel, Annie Robin, Maurizio Salaris, Victor Silva Aguirre, Marica Valentini (+ many more)
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The K2 Galactic Archaeology Program (GAP)
PI: Dennis Stello, CoIs: Derek Buzasi, Ken Freeman, Savita Mathur, Andrea Miglio, Sanjib Sharma, Marc Pinsonneault, Collaborators: Friedrich Anders, Borja Anguiano, Martin Asplund, Sarbani Basu, Paul Beck, Othman Benomar, Maria Bergemann, Joss Bland-Hawthorn, Tiago Campante, Luca Casagrande, Peter De Cat, Márcio Catelan, Bill Chaplin, Cristina Chiappini, Enrico Corsaro, Orlagh Creevey, Eric Depagne, Patrick Eggenberger, Yvonne Elsworth, Jianning Fu, Rafael A. Garcia, Leo Girardi, Jennifer Johnson, Ulrike Heiter, Saskia Hekker, Paola Marigo, Eric Michel, Annie Robin, Maurizio Salaris, Victor Silva Aguirre, Marica Valentini (+ many more)
The thrust: Use seismology of red giants (K2) combined with Teff and [Fe/H] (ground-based) to probe the structure of the Milky Way
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K2 GAP
Campaign-1
• Observational strategy: • Target 5K-10K stars (~5K red giants) at each campaign • Use simple/reproducible section criteria!
J–K > 0.5, V > 9 sorted by V (entire field) or J–K > 0.5, 9 < V < 13.5 random by V (few dense sub-fields)
Credit: Sharma
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K2 GAP
Campaign-1
RA (degrees)
Dec
(deg
rees
)
Credit: Kevin Covey
observed
Campaign-2
RA (degrees)
Dec
(deg
rees
)
Credit: Kevin Covey
observed
• Observational strategy: • Target 5K-10K stars (~5K red giants) at each campaign • Use simple/reproducible section criteria!
J–K > 0.5, V > 9 sorted by V (entire field) or J–K > 0.5, 9 < V < 13.5 random by V (few dense sub-fields)
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K2 GAP • Status of observations: Campaign Ntargets APOGEE-1 APOGEE-2 GALAH Gaia-ESO LAMOST SAGA
0 452 ? 1 8629 ? 2 5138 few 3 3904 ? 4 6357 ? 5 9828 ?
6+ ? ? ~40% of total K2 capacity
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K2 GAP • Status of observations: Campaign Ntargets APOGEE-1 APOGEE-2 GALAH Gaia-ESO LAMOST SAGA
0 452 ? 1 8629 ? 2 5138 ? 3 3904 ? 4 6357 ? 5 ? ?
6+ ? ?
• Don’t forget serendipitous red giants that fall within the pixel stamps of any K2 target => unbiased sample.
~40%
Ground-based coordination: Sanjib Sharma (GALAH) Jennifer Johnson (APOGEE) Sofia Feltzing (Gaia-ESO) Victor Silva Aguirre Dennis Stello
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K2 GAP: C0
Credit: Huber
Credit: Huber
Campaign 0
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K2 GAP: C0
Credit: Huber
Credit: Huber
Campaign 0
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K2 GAP: C1
Campaign 1
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K2 GAP: C1
Campaign 1
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K2 GAP: C1
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K2 GAP: C1
0 0
0 0
2 2 2
2
1
1
1
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K2 GAP: C1
• 117 stars: APOGEE log(g) < 3.8
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K2 GAP: C1
• 117 stars: APOGEE log(g) < 3.8
∆ν too small
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K2 GAP: C1
• 117 stars: APOGEE log(g) < 3.8
∆ν too small
νmax too large
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K2 GAP: C1
• 117 stars: APOGEE log(g) < 3.8 Kepler: APOKASC sample
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K2 GAP: C1
• 67 Stars in total. • 55 Detected (∆ν and νmax). • 7 Marginal (∆ν or νmax not clear). • 5 Non-detected.
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K2 GAP: C1
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K2 GAP: C1
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K2 GAP: C1
No correlation between Kp and logg (corr=0.04)
Luminosity
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K2 GAP: C1
No correlation between Kp and logg (corr=0.04) => Magnitude complete
Luminosity
If a red giant has 1.9 < logg < 3.2 and Kp < 14.5 => We can detect the oscillations!
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Large Area Survey of Bright Stars F, G, K dwarfs: +4 to +12 magnitude M dwarfs known within ~60 parsecs “All sky” observations in 2 years:
• > 200,000 target stars at <2 min cadence • > 20,000,000 stars in full frames at 30 min
cadence
• Primary Goal: Discover Transiting Earths and Super-Earths Orbiting Bright, Nearby Stars
• Rocky Planets & Water Worlds • Habitable planets
• Discover the “Best” ~1000 Small Exoplanets
• “Best” means “Readily characterizable” • Measurable mass & atmospheric
properties
TESS: 2017-2019+
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TESS: 2017-2019+
All-sky observing strategy
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Andrea Miglio
Asteroseismic View of the Milky Way Kepler
CoRoT
K2 TESS!
WFIRST
EUCLID
PLATO
A exciting (space) future for GA