Spectroscopy in Stellar Astrophysics Alberto Rebassa Mansergas.
Spectroscopy of Resolved Stellar Populations Beyond the Local Group
description
Transcript of Spectroscopy of Resolved Stellar Populations Beyond the Local Group
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Spectroscopy of Resolved Stellar Populations Beyond the Local Group
Chris Evans (UKATC)
Yanbin Yang, Mathieu Puech, Matt Lehnert (GEPI); Annette Ferguson, Mike Barker (Edinburgh);
Jean-Gabriel Cuby (LAM); Simon Morris (Durham)
AO4ELT – Paris – June 2009
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• Resolved stellar populations in the 8-10m and ELT eras
• EAGLE Phase A study
• Science simulations
Overview
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Resolved Stellar Populations in the Local Group
Belokurov et al. (2006)
Richardson et al. (2008)
Battaglia et al. (2006)
M31MW Halo
Dwarf Sphs (e.g. Fornax)
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Resolved Stellar Populations in the Local Group
Belokurov et al. (2006)
Richardson et al. (2008)
Battaglia et al. (2006)
M31MW Halo
Bullock, Johnston et al.
Dwarf Sphs (e.g. Fornax)
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Moderate-resolution spectroscopy of the Ca Triplet @860nm
Tolstoy et al (2001)
Spectroscopy of Resolved Stellar Populations
Abundances & kinematics
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Moderate-resolution spectroscopy of the Ca Triplet @860nm
Tolstoy et al (2001)
Spectroscopy of Resolved Stellar Populations
Abundances & kinematics
Richardson et al. (2008)
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Spectroscopy of Resolved Stellar Populations
Abundances & kinematics
Richardson et al. (2008)
KECK-DEIMOS in M31 Chapman et al. (2006)
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ELTs will unlock a huge range of new targets, including:
• NGC 3109 & Sextans A (1.3 Mpc)
• Spiral-dominated Sculptor Group (2-4 Mpc)
• M83/NGC5128 grouping (4-5 Mpc)
• NGC3379 (11 Mpc)
• Virgo Cluster galaxies (16-17 Mpc)
The ELT era
Resolved Stellar Populations in the Local Volume
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Image Credit: Richard Powell
The (near) Local Volume
1.5 3 4.5 6 Mpc
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Image Credit: Richard Powell
The (near) Local Volume
1.5 3 4.5 6 Mpc
TMT (if in HI)
E-ELT (if in Sth. America)
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• A multi-IFU, near-IR spectrometer for the E-ELT
• French-UK consortium
• PI: Jean-Gabriel Cuby (Marseille)
• 2 year study (09/07-09/09)
• Phase 1 review (07/08), Midterm review (02/09)
EAGLE Phase A study
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Science areas that drive the EAGLE requirements:
• Physics & evolution of high-z galaxies• See talk by Mathieu Puech
• Detection and characterisation of “first-light” galaxies
• Galaxy assembly/evolution from stellar archaeology
• Star-formation, stellar clusters and the IMF
• Co-ordinated growth of black holes and galaxies/AGN
EAGLE Science
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Parameter Specification
Patrol Field 5 arcmin (unobstructed)
eqv. >7 arcmin (vignetted)
Science subfield (IFU FOV)
1.65 x 1.65 arcsec
Multiplex 20
Spatial Resolution 30% EE in 75mas (H-band)
Spectral resolving power 4,000 & 10,000
Wavelength range 0.8-2.5 µm
EAGLE Baseline Design
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EAGLE Baseline Design
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EAGLE Baseline Design
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EAGLE AO
CANARY: 2010-2012:• Demonstrate MOAO in EAGLE config.• Improve real-time control techniques • Develop calibration techniques
Multi-Object Adaptive Optics (MOAO)
See talk by Tim Morris
See talk by Gerard Rousset
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Science Simulations: MOAO performances
• MOAO PSFs from Francois Assemat et al. (ONERA)
• Seeing: 0.65” and 0.8”
• 84x84 DM; 2 x NGS configurations
7.3’ FoV
Selected NGS
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Science Simulations: MOAO performances
• MOAO PSFs from Francois Assemat et al. (ONERA)
• Seeing: 0.65” and 0.8”
• 84x84 DM; 2 x NGS configurations
42m primary
10 hr integration (20x1800s)Δλ = 8400-8750Å @ R =
10,00037.5 mas spaxels1x1 arcsec IFUTotal th’put = 0.19Ulisse Munari’s spectral libraryRON = 5e/pix, dark =
0.01e/pix/sPuech et al. (2008)
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Science Simulations: MOAO performances
• MOAO PSFs from Francois Assemat et al. (ONERA)
• Seeing: 0.65” and 0.8” (@ zenith, eqv. 0.71” & 0.90” @30º)
• 84x84 DM; 2 x NGS configurations42m primary10 hr integration (20x1800s)Δλ = 8400-8750Å @ R = 10,000
37.5 mas spaxels1x1 arcsec IFUTotal th’put = 0.19Ulisse Munari’s spectral libraryRON = 5e/pix, dark = 0.01e/pix/s
I = 23.5 S/N = 24
Puech et al. (2008)
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EAGLE CaT performance• Seeing = 0.8”, 84x84 DM
• texp = 20x1800s
• R = 10,000
I (Vega)
S/N
22.5 42
23.5 24
24.5 11
I (Vega)
S/N
22.5 25
23.5 12
24.5 6
NGS config 10 NGS config 1
cf. E-ELT ETC: LTAO/50mas/R=10,000/I=24.5/M2V S/N=14
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EAGLE CaT performance• Seeing = 0.8”, 84x84 DM
• texp = 20x1800s
• R = 10,000
I (Vega)
S/N
22.5 42
23.5 24
24.5 11
I (Vega)
S/N
22.5 25
23.5 12
24.5 6
NGS config 10 NGS config 1
cf. E-ELT ETC: LTAO/50mas/R=10,000/I=24.5/M2V S/N=14
Want ~15-20% EE in 75 mas at 0.85µm
4 mags deeper than FLAMES LR08 observations
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HST GHOSTS SurveyDe Jong, Radburn-Smith et al., see: www.stsci.edu/~djrs/ghosts
27 target galaxies out to ~17 Mpc
3.6 Mpc1.9 Mpc
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ACS: F814W [~3x3 arcmin]
ACS image
EAGLE Observations in the Sculptor Group
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9 arcsec
ACS image
ACS image
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9 arcsec
ACS image
ACS image
Simulated EAGLE cube
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9 arcsec
ACS image I = 22.8 S/N=28
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9 arcsec
ACS image
I = 23.1 S/N=23
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9 arcsec
ACS image
I = 22.5 S/N=43 & 36
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Image Credits: David Radburn-Smith
Formation & evolution of galaxies in the Sculptor Group
10 hrs/pointing
x20 pointings: > 1,000 stars in
~250 hrs
15 hrs/pointing
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• R=10,000 CaT spectroscopy, S/N > 10 at I ~24.5 in 10 hrs
• Multiple stars per IFU –> much larger effective multiplex
• Large patrol field enables efficient surveys
• Sculptor is just one conceivable EAGLE “Large Programme”
Summary