SIRTF LegacySIRTF Legacy

From Molecular Cores to Planet-forming Disks

Infrared Great Observatory– 3 -- m wavelength range

– Background Limited Performance

– 85 cm f/12 Beryllium Telescope, T < 5.5K

– 6.m Diffraction Limit

– Instrumental Capabilities• Imaging/Photometry, 3-180 m

• Spectroscopy, 5-40 m

• Spectrophotometry, 50-m

– Planetary Tracking, 1 arcsec/sec

– >75% of observing time for the

General Scientific Community

– 2.5 yr Lifetime/5 yr Goal

– Launched in August 2003 (Delta 7920H)

– Solar Orbit

Space Infrared Telescope FacilitySpace Infrared Telescope Facility

The LaunchThe Launch

August 25, 2003, Kennedy Space Center

First LightFirst Light

SIRTF Instrumentation OverviewSIRTF Instrumentation Overview Infrared Array Camera (IRAC), G.G.Fazio, SAO, PI.

Wide-field (5x5 arcmin) imaging. Simultaneous viewing at 3.6, 4.5, 5.8, m

InSb and Si:As IBC arrays, 256x256 pixel format Infrared Spectrograph (IRS), J.R.Houck, Cornell, PI.

R=600 echelle spectrographs, 10-20 and 20-40 m

R=50 long-slit spectrographs, 5-15 m and 15-44 m

Imaging/Photometry, 15 m

Si:As and Si:Sb IBC arrays, 128x128 pixel format Multi-band Imaging Photometer for SIRTF (MIPS), G.Rieke, Arizona, PI.

Imaging and photometry: 24, 70, 160 m; optimized for efficient large area surveys and superresolution; R~15 spectrophotometry, 50-100 m

Si:As IBC and Ge:Ga arrays, 128x128 and 32x32 format

Stressed Ge:Ga array, 2x20 format

SIRTF Legacy ScienceSIRTF Legacy Science

Requirements– Large, coherent scientific investigations - not realizable as

series of smaller GO Programs– Programs whose data are of general and lasting importance

to the broad community and also stimulate SIRTF follow-on– Data are non-proprietary, enabling timely and effective

opportunities for both SIRTF follow-on and archival research Possible Scope

– Legacy Programs typically have hundreds of hours of observing time

– Legacy science may utilize up to 50% of the first year of SIRTF observing time

Extra-galactic Legacy ProgramsExtra-galactic Legacy Programs

Great Observatories Origins Deep Survey (GOODS)– M. Dickinson (STScI) and 40 co-Is at 14 institutions– Deep 300 square arcmin IRAC and MIPS (24 microns) survey

overlapping HST and CXO deep fields– Galaxy formation and Evolution, z = 1 to 6

The SIRTF Wide-area Infrared Extragalactic Survey (SWIRE)– C. Lonsdale (IPAC/CIT ) and 19 co-Is at 9 institutions– ~100 sq. deg., high latitudes, reaching z ~ 2.5– Evolution of dusty, star-forming galaxies, AGN

The SIRTF Nearby Galaxies Survey (SINGS): Physics of the star-forming ISM and Galaxy Evolution– R. Kennicutt (Arizona) and 14 co-Is at 7 institutions– Imaging and spectroscopy of 75 nearby galaxies– Connections between ISM and star formation, templates for high z

Space Infrared Telescope Facility

Extragalactic Science in the Legacy Program

Sky Coverage Area

• SINGS

75 galaxies

• SWIRE

~100 sq. deg.

• GOODS

~0.1 sq. deg.

GOODS

SINGS

SWIRE

Galactic Legacy ProgramsGalactic Legacy Programs

The SIRTF Galactic Plane Survey (GLIMPSE)– E. Churchwell (Wisconsin) and 13 co-Is at 6 institutions

– 240 square deg. IRAC survey of inner Galactic plane

– Galaxy structure and star formation From Molecular Cores to Planet-forming Disks (c2d)

– N. Evans (Texas) and 10 co-Is at 8 institutions

– Imaging (IRAC and MIPS) and spectroscopy of star forming regions

– Evolution of molecular cores to stars, disks, sub-stellar objects The Formation and Evolution of Planetary Systems: Placing our

Solar System in Context (FEPS)– M. Meyer (Arizona) and 18 co-Is at 12 institutions

– Imaging and spectroscopy of 300 young stars with disks

– Evolution from accretion disks to planet formation

What will GLIMPSE see?

MSX point srcs 61321 (107) Dark Clouds 210 (?) Open Clusters 76 (104)

IRAS point srcs 15501 Galaxies 157 (?) Planetary Nebulae 65 (?)

HII/SFR regions 1174 (104) ASCA pt srcs 144 Wolf-Rayet stars 50 (103)

ROSAT pt srcs 459 SNR 100 Globular Clusters 1 (?)

Radio pulsars 264 O/B stars 76 (10 4 ?)

Known Objects in the GLIMPSE Survey Region

l=300o to 320o, |b| <1o MSX 8 micron band (Price et al 2001)

, b

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The Formation & Evolution of Planetary

Systems: Placing Our Solar System

in Context Michael R. Meyer (Steward Observatory, The University of Arizona, P.I.) D. Backman (Franklin & Marshall College, D.P.I.) , S.V.W. Beckwith (STScI), J.M. Carpenter

(Caltech), M. Cohen (UC-Berkeley), U. Gorti (NASA-Ames), T. Henning (MPIA), L. Hillenbrand (Caltech, D.P.I.), D. Hines (Steward), D. Hollenbach (NASA-Ames), J. Lunine (LPL), J.S. Kim (Steward), R. Malhotra (LPL), E. Mamajek (Steward), A. Moro-Martin (Steward), P. Morris (SSC), J. Najita (NOAO), D. Padgett (SSC), J. Rodmann (MPIA), M. Silverstone (Steward), D. Soderblom (STScI), J.R. Stauffer (SSC), B. Stobie (Steward), S. Strom (NOAO), D. Watson (Rochester), S. Weidenschilling (PSI), S. Wolf (Caltech), and E. Young (Steward).

A SIRTF Legacy Science Program

For more information please visit http://feps.as.arizona.edu

The c2d TeamThe c2d Team Co-investigators

– Neal J. Evans II (Texas)– Lori E. Allen (SAO)– Geoffrey A. Blake (Caltech)– Paul M. Harvey (Texas)– David W. Koerner (Northern Arizona)– Lee G. Mundy (Maryland)– Philip C. Myers (SAO)– Deborah L. Padgett (SSC)– Anneila I. Sargent (Caltech)– Karl Stapelfeldt (JPL)– Ewine F. van Dishoeck (Leiden)

34 Associates 20 Affiliates

Science GoalsScience Goals

Complete database for nearby (< 350 pc), Low mass (solar type) star formation

Follow evolution from starless cores to planet-forming disks

Coordinate with FEPS team to ensure complete coverage of 0 to 1 Gyr

Cover range of other variables (mass, rotation, turbulence, environment, …) to separate from evolution.

ObservationsObservations

(275 hr) Map ~5 large clouds, ~135 smaller cores with IRAC and MIPS (~20 sq. deg.)

(50 hr) Photometry of ~190 stars (IRAC and MIPS) (75 hr) Spectroscopy of disk material (IRS) for

about 200 targets

Target Large CloudsTarget Large Clouds

PerseusSerpensOphiuchusLupusChamaeleon

Ophiuchus (Overall view)Ophiuchus (Overall view)

Extinction Map (Cambresy 1999, Astr. Ap. 345)Extinction Map (Cambresy 1999, Astr. Ap. 345)

Antares artifact

Ophiuchus AOphiuchus AVV = 3 and AORs = 3 and AORs

Outline of AOutline of AVV = 3 = 3

IRAC IRAC AORSAORS

MIPS MIPS AORsAORs

11oo

Isolated CoresIsolated Cores

Large sample selected based on– Extinction on sky survey– Molecular emission– Reasonably compact– Some isolated, single– Some in small groups

Group of Cores (Mapping)Group of Cores (Mapping)

Mapping mode, step = 280”Mapping mode, step = 280”IRACIRAC MIPSMIPS

Questions : Clouds and CoresQuestions : Clouds and Cores

Spatial Structure of star formation How do molecular cores become

protostars and disks?– Very early evolution (sensitive to L ~ 10-3 Lsun).– Large sample finds rare objects

• First hydrostatic core• Other transitional objects

– Very deeply embedded protostars.

An Evolutionary Sequence An Evolutionary Sequence

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Shu collapseM = 0.29 Msun

ro = 4396 AUAccretion rate= 1.1 x 10–6 Msun/yr

Envelope gone at 270,000 yrFinal star mass =0.24 Msun

Final disk mass = 0.05 Msun

D = 320 pcYoung & Evans, in prep.

Questions: Brown DwarfsQuestions: Brown Dwarfs

Early Evolution of Brown Dwarfs 100’s of candidates down to 5 Mjup at 1 Myr Detect circum-BD envelopes down to 1 Mjup

Detect circum-BD disks (4.5 Mjup to 70 m)– Recent detections in NIR (Muench et al.)– MIR with ISO (Comeron et al.)– High fraction with excesses at 3.8 m (Liu et al.)

Formation of Brown DwarfsFormation of Brown Dwarfs

Young BD, L=0.003 LYoung BD, L=0.003 Lsunsun, ,

1 M1 Mjupjup Envelope Envelope

10 Myr old BD, L=0.007 L10 Myr old BD, L=0.007 Lsunsun, ,

4.5 M4.5 Mjupjup Disk (Chiang et al.) Disk (Chiang et al.)

Scientific Questions: DisksScientific Questions: Disks

Do all solar-mass stars have disks?– Do weak-line T Tauri stars have debris disks?– Are there variables besides time?

What are the timescales for disk evolution?– How does the transition from accretion disks to

debris disks depend on time and other factors?

Evolution of Planet Forming disksEvolution of Planet Forming disks

SIRTF studies will constrain disk masses– Early, through AV ~ 100 mag, can see

• r = 5 AU, M = Mearth disks

– Middle (~ 1 Myr to 1 Gyr) around sun-like stars• 0.1 Mmoon from 30–60 AU at 150 pc

MIR complementary to NIR, mm studies

Detect Debris Disks to 0.1 MDetect Debris Disks to 0.1 Mmoonmoon

Model has 0.1 Mmoon of30 m size dust grainsin a disk from 30–60 AUBars are 3 Model based on disksaround A stars

Protostellar Disks to Planetary SystemsProtostellar Disks to Planetary Systems

FEPS TeamFEPS Team

Cores to DisksCores to Disks

NIR (< 0.1 AU) Excess vs. Cluster Age

Hillenbrand, Meyer, and Carpenter (2002); see alsoHaisch et al. 2001.

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Spectral Evolution QuestionsSpectral Evolution Questions

How do the dust, ice, gas in disks evolve?– Amorphous to crystalline silicates?– How does the icy component evolve?

– How long does gas (H2) persist?

What is the spectral evolution of BDs?– If they form with disks, how does the dust

evolve in those disks?

Spectral EvolutionSpectral Evolution

10 My10 My

100 My100 My

5 Gy5 Gy

Few MyFew My

Data ProductsData ProductsFirst Delivery late May 2004Mosaics of IRAC and MIPS maps

– Over very large areas (~20 sq. deg.) – Cleaned versions of mosaics

Catalogs of all sources, cross references

Spectral atlas of template disk spectraAncillary Data

– submillimeter maps (Bolocam) – optical spectra (NOAO)

Example of Bolocam DataExample of Bolocam Data

Bolocam map of PerseusAbout half the data,Not fully reduced.RMS ~45 mJy 1 x 4 degrees

Enoch et al. in prep.

Perseus Map in Perseus Map in 1212COCO

from the COMPLETE team

Additional ProductsAdditional Products

Analytical Tools for Modeling Disks and Envelopes– K. Dullemond: Disk codes– M. Wolfire : Envelope models

Enhanced data analysis tools– Contributing to IRS data reduction tool

Separating SourcesSeparating Sources

DIRT for SIRTFDIRT for SIRTF

DIRT is being tailored to SIRTF – Wolfire (c2d and GLIMPSE)– IRAC and MIPS bandpasses– Lower luminosity models– Include heating by ISRF– Indicate wavelengths of absorption

against ISRF

http://dustem.astro.umd.edu/wits/dirt/index.html

A Sample of DIRT

Complementary DataComplementary Data Complementary: not part of original prop. Projects initiated by us, with others

– JCMT SCUBA and IRAM MAMBO• Map isolated cores at 850/450 m or 1300 m

– ESO time • SIMBA on SEST, submm mapping of far-south cores• SEST molecular line mapping of far-south cores• TIMMI-2 8–13 m spectra, R~200 of cTTs• ISAAC 2.9–4 m spectra of embedded objects• ADONIS images of wTTs• WFI maps in red, H of Cha and Lupus

Complementary Data (cont.)Complementary Data (cont.)

Other projects initiated by us– BIMA Key project

• 360 hours

Projects initiated by others– CFHT optical imaging of clouds (Menard)

• Time allocated for mapping of Perseus• snapshots of isolated cores approved

– COMPLETE (Goodman et al.)• Molecular line, extinction, submm cont.• Key project to match Legacy survey

– Others?

LegaciesLegacies

Molecular cloud extinction structure Spectroscopic binary candidates Shocks and outflows Brown Dwarf candidates Diffuse Emission– Dust properties Web site: http://peggysue.as.utexas.edu/SIRTF/ PASP paper (2003, 115, 965; preprint available on website)

SIRTF and YouSIRTF and You

General Observer CFP: Nov. 2002 First deadline Feb. 2004

– Includes archival studies– Eventually theory

Subsequent calls each year until 2007 Note also SIRTF Fellows Program

– Like Hubble Fellows– See http://sirtf.caltech.edu/SSC/– Deadline is typically Nov.

Thanks for the invitation…