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The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of the Galaxy Princeton, Feb 27, 2009

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Page 1: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

The Apache Point Observatory Galactic

Evolution Experiment

(APOGEE)

Ricardo Schiavon1 (for the team) 1 Gemini Observatory

Construction and Evolution of the GalaxyPrinceton, Feb 27, 2009

Page 2: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

SDSS-IIIAPOGEE: an infrared, high resolution spectroscopic survey of the stellar populations of the Galaxy

BOSS: will measure the cosmic distance scale via clustering in the large-scale galaxy distribution and the Lyman-α forest

SEGUE-2: will map the structure, kinematics, and chemical evolution of the outer Milky Way disk and halo

MARVELS: will probe the population of giant planets via radial velocity monitoring of 11,000 stars

http://www.sdss3.org

Page 3: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

APOGEE People• APOGEE Leadership

S. Majewski (PI, UVa)M. Skrutskie (Instrument Scientist, UVa)J. Wilson (Deputy Instrument Scientist, UVa)R. Schiavon (Survey Scientist, Gemini Observatory)C. Allende-Prieto (Abundances and Stellar Parameters Task Leader, Mullard)M. Shetrone (Spectral Reduction Task Leader, HET)J. Johnson (Field/Target Selection Task Leader, Ohio State)P. Frinchaboy (Field/Calibration Task Leader, U.Wisc., NSF Fellow) D. Bizyaev (Radial Velocities Task Leader, APO)I. Ivans (Princeton), J. Holtzman (NMSU)

• Significant Contributors to DateK. Cunha, V. Smith (NOAO), R. O’Connell (Uva), Neil Reid (STScI),R. Barkhouser, S. Smee (JHU), J. Gunn (Princeton), T. Beers (Michigan State) C. Henderson, B. Blank (Pulseray Machine & Design), D. Spergel (Princeton)G. Fitzgerald, T. Stolberg (NEOS), T. O’Brien (OSU), E. Young (UofA)J. Crane (OCIW), S. Brunner, J. Leisenring (Uva)

Page 4: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

Context: it seems like we live in a -CDM Universe

=> Does the Milky Way fit in that picture?

APOGEE

Page 5: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

APOGEE at a glance

• Bright time 2011 to 2014• 300 fiber, R ~ 24,000, cryogenic spectrograph• H-band: 1.51-1.68• Typical S/N = 100/pixel @ H=12.5 for 3-hr integration• Typical RV uncertainty < 0.5 km/s• 0.1 dex precision abundances for ~15 chemical elements• 105 2MASS-selected giant stars probing all Galactic populations

Page 6: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• Red giants/red clump are bright in NIR.• Complete point source sky catalogue to H > 14 available

from 2MASS, augmented by GLIMPSE andUKIDSS where available.

No need for new photometry!

Advantages of a High Res. H-band Survey

Page 7: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• AH / AV = 0.17 2 flux for AV =1; 100 flux for AH =1• Access to dust-obscured galaxy • Precise velocities and abundances for giant stars across the Galactic plane, bar, bulge, halo => HOMOGENEITY• Low atmospheric extinction makes bulge accessible from North• Avoids thermal background problems of longer

AV = 1 boundary

Advantages of a High Res. H-band Survey

Page 8: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

APOGEE DepthSolar metallicity RGB tip star:

int (hr) Hlim AV d(kpc) 3 12.5 5 27 10 13.4 10 27

[Fe/H]= -1.5 RGB tip star:

int (hr) Hlim AV d(kpc) 3 12.5 0 40 10 13.4 0 60

Page 9: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

APOGEE in Context

Gal.Cen.

AV

10 5

Deeper at high Av than everybody else

Page 10: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

SDSS-III Sloan Review - APOGEE

APOGEE Spectrograph

• The APOGEE Dewar will be housed in the basement of the support building about 40 meters from the base of the telescope.

– The red line approximates the main fiber run. A plug on the cartridge end will insert into a fiber coupling receptacle on the cartridge.

– Slit head is cryogenic and permanently housed in the instrument.

APOGEE

2.5-meter

coupler

cartridge

Page 11: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

75” dia Dewar

Spherical Collimator (Zerodur)

Slit-head (300 fibers)

Fold

VPHRefractive Camera

(2) Teledyne H2RG Detectors

LN2 Tanks

Vibration Isolators

300 fiber pseudo-slit embedded in fold mirror

Collimator

VPH mosaic grating (265 x 450 mm illuminated)

Three HAWAII-2RG arrays(NIRCam-style detector mount)

Fiber feedthroughs

Refractive Camera (Si & Fused Silica)

394 mm

Blanche et al 2004

1.7 m

2.1 m

LN2 cooled Dewar

Page 12: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• A 3-D chemical abundance distribution (many elements), MDFs across Galactic disk, bar, bulge, halo.

• Probe correlations between chemistry and kinematics (noteGaia proper motions eventually as well).

• Constrain SFR and IMF of bulge/disk as function of radius, metallicity/age, chemical evolution of inner Galaxy.

• Determine nature of Galactic bar and spiral arms and theirinfluence on abundances/kinematics of disk/bulge stars.

• Measure Galactic rotation curve (include spec. p., Gaia pm)• Search for and probe chemistry/kinematics of (low-latitude)

halo substructure (e.g., Monoceros Ring).• Combine with existing/expected optical, NIR and MIR data

and map Galactic dust distribution using spec. p’s,constrain variations in extinction law

• Find Pop III stars

Science Goals

Page 13: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• A 3-D chemical abundance distribution (many elements), MDFs across Galactic disk, bar, bulge, halo.

• Probe correlations between chemistry and kinematics (noteGaia proper motions eventually as well).

• Constrain SFR and IMF of bulge/disk as function of radius, metallicity/age, chemical evolution of inner Galaxy.

• Determine nature of Galactic bar and spiral arms and theirinfluence on abundances/kinematics of disk/bulge stars.

• Measure Galactic rotation curve (include spec. p., Gaia pm)• Search for and probe chemistry/kinematics of (low-latitude)

halo substructure (e.g., Monoceros Ring).• Combine with existing/expected optical, NIR and MIR data

and map Galactic dust distribution using spec. p’s,constrain variations in extinction law

• Find Pop III stars?

Science Goals

Page 14: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

Reliable statistics: (level of solar neighborhood) in many (R, , Z) zones

APOGEE seeks to construct similar figures for many elements and for many other discrete Galactic zones.

e.g., GCE models predict variations in these distributions and in radial [X/H] gradients differing at few 0.01 dex level per radial bin

• for gradients requires: ~0.01 dex in <[X/H]> or >100 stars with 0.1 dex per radial bin

• for [X/H]-[Fe/H] distributions requires (100 stars)(~20 [Fe/H] bins)(dozens of zones)

105 starsVenn et al. (2004) 781 compiled stars

Top Level Science Requirements

Page 15: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• order of magnitude leaps: ~1-2 orders more high S/N, high R spectra ever taken

~3 orders larger than any other high R GCE survey

~3 orders more high S/N, high R near-IR spectra than ever taken

First week of observations will exceed all previous work!

Orders of Magnitude

Page 16: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

Simulated APOGEE spectra

• Numerous lines of molecular CN, OH, CO to give LTE-based CNO abundances (most abundant metals in universe)• Plenty of clean lines of Fe, -elements (O, Mg, Si, S, Ca, Ti, Cr), Fe peak (V, Mn, Ni), and some odd-Z (e.g., Na, K, Al)

High-Res. Abundances in H-band

Page 17: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• APOGEE will make possible straightforward tests of Galaxy formation scenarios by verifying how relevant quantities vary with time.

Simple Ideas

Page 18: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• Dias et al. (2003) catalogue of open clusters

Simple Ideas

Page 19: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

Simple Ideas

Age RGC

Vari

ou

s ele

men

tal

ab

un

dan

ces

in o

pen

cl

ust

ersYon

g e

t al. 2

00

5

Page 20: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• APOGEE targets will be seen at large distances even at very large extinction

• 1% of APOGEE sample, ~5 stars/cluster, ~200 clusters!

Simple Ideas

Page 21: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

Galactic Bulge

• We know: star formation in the center, old stars (e.g. Baade window), presence of a bar, high metallicity (Rich 88), probably an abundance gradient (Zoccali et al. 2007), mostly alpha-enhanced (Fullbright et al.).

• Which fraction of the bulge stellar mass was formed in situ, which fraction from mergers, which fraction from secular evolution driven by bar instabilities (e.g., Norman et al. 1996)?

Page 22: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

Galactic Bulge

• Kobayashi (2004): CDM-based 124 SPH simulations of elliptical galaxies, including radiative cooling, star formation, SN and wind feedback, chemical enrichment

• Solid symbols are monolithic collapse, open symbols are systems with a lot of previous merging

• The more merging, the shallower the abundance gradients

Page 23: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

Spectrum Synthesis

Allende Prieto

Ti Mg

Mg Mg

Arcturus Synthesis

Page 24: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

• -calibrated, sky-subtracted, telluric absorption-corrected,

1-D spectra

• RVs to ~0.5 km/s external accuracy

• log(g), [Fe/H], Teff (making use of 2MASS colors)

• elemental abundances to within 0.1 dex accuracy for 15 elements, including CNO, other , Fe-peak, Al, K)

Anticipated Deliverables

Page 25: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

25

SDSS-III High-level Schedule

Page 26: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

Institutional Members• Signed MOUs.

– Univ. of Arizona– Cambridge Univ.– Case Western Univ.– Univ. of Florida– German Participation

Group (AIP, MPE, MPIA, ZAH)

– Johns Hopkins Univ.– Korean Institute for

Advanced Study– Max Planck Astroph.,

Garching – New Mexico St. Univ.– New York Univ.– Ohio State Univ.– Univ. of Pittsburgh– Univ. of Portsmouth

– Princeton Univ.– UC Santa Cruz– Univ. of Utah– Univ. of Washington– Vanderbilt– Univ. Virginia– MSU/ND/JINA– Brazilian PG (ON and four

Univ.)• Near-term possibilities:

– Fermilab– French PG (APC, IAP, CEA,…)– UC Irvine– LBNL– Penn State Univ.– Spanish PG (three CSIC units)– Univ. of Tokyo/IPMU

• Other institutions and individuals are in discussions.

Page 27: The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Ricardo Schiavon 1 (for the team) 1 Gemini Observatory Construction and Evolution of

What We Want to Talk to You About

• Theorists: we need you to produce models for us to rule out.

• All: the survey is being defined. If I were you, I would get involved now. Bring your ideas. Let’s discuss.