New Cool Star Science with Spitzer John Stauffer Spitzer Science Center Caltech CSW13 - Hamburg July 8, 2004

Stauffer-2CSW13, Hamburg July 2004 The Spitzer Observatory A Assembled SIRTF Observatory at Lockheed-Martin, Sunnyvale. Key Characteristics: Aperture – 85 cm Wavelength Range - 3-to-180um Telescope Temperature – 5.5K Mass – 870kg Height – 4m  Launched on 25 August All systems performing well.  Liquid Helium to last ~5 years, with several more years of partial capabilities  1-2 orders of magnitude improvement in sensitivity and performance  Completes NASA’s Great Observatories  Provides corner-stone science for NASA’s Origins Theme, especially JWST

Stauffer-3 SIRTF in the Solar Orbit From Launch to L+62 months

Stauffer-4CSW13, Hamburg July 2004 SIRTF Focal Plane Instruments Integrated at Ball Aerospace Boulder, May, 2001 MIPS Imaging 5’x5’ 24µm: ~0.1 mJy 70 µm:~2 mJy 160µm: ~4 mJy [1σ in 100 sec] Spectroscopy µm R~20 G.Rieke, U Arizona/BATC IRAC Imaging 5’x5’ 3.5 µm: ~2 µJy 4.6 µm : ~2 µJy 5.8 µm : ~10 µJy 8 µm : ~10 µJy [1σ in 100 sec] G. Fazio SAO/GSFC IRS Spectroscopy 5 to 40µm R~100 ~0.1 to 0.3 mJy 10 to 40µm R~600 ~1 to 3 mJy [1σ in 500 sec] J.R. Houck Cornell/BATC

Stauffer-5CSW13, Hamburg July 2004 What Data Have Been Obtained by Spitzer?  First 3 months in orbit – “In Orbit Checkout” and “Science Verification”. Includes Early Release Observations and “First Look Survey”.  Since December ’03, “normal operations” – but targets limited to: –Guaranteed time observers (GTO’s). These are the instrument builders and members of the Science Working Group. Data have a one year proprietary period. –“Legacy Science” Teams – six teams, each awarded hours of time in order to pursue a single science theme. Data are non-proprietary.  See for details.

Spitzer Space Telescope Cool Star Science being done by GTO’s Photometry and spectroscopy of known MLT dwarfs Search for very low mass companions to nearby stars (various samples) Deep IRAC imaging of nearby star forming regions for BD’s IRAC and MIPS imaging of star forming regions for population and structure purposes PMS disk evolution (ages 1 to 15 Myr) – all three instruments Debris disk evolution for A stars (ages 10 Myr to 1 Gyr) – IRAC and MIPS IRAC and MIPS imaging of the Pleiades IRAC and MIPS imaging of Orion Mass loss in globular cluster giants Detailed observations of Vega, Fomalhaut, Beta Pic and Epsilon Eridani

Spitzer Space Telescope The Spitzer Legacy Science Program Mark Dickinson (STScI) & institutions “GOODS: Great Observatories Origins Deep Survey” 647 hours (IRAC, MIPS) Carol Lonsdale (IPAC/Caltech) & 19 9 institutions “ SWIRE: SIRTF Wide-area Infrared Extragalactic Survey” 851 hours (IRAC, MIPS) Robert Kennicutt (U. Arizona) & 14 7 institutions “SINGS: SIRTF Nearby Galaxies Survey” 512 hours (IRAC, MIPS, IRS) Ed Churchwell (U. Wisconsin) & 13 6 institutions “The SIRTF Galactic Plane Survey (GLIMPSE)” 400 hours (IRAC) Neal Evans (U. Texas) & 10 8 institutions “From Molecular Cores to Planets (Cores to Disks)” 400 hours (IRAC, MIPS, IRS) Michael Meyer (U. Arizona) & institutions “The Formation and Evolution of Planetary Systems (FEPS)” 350 hours (IRAC, MIPS, IRS)

Spitzer Space Telescope Recent and Near-Term Future Events Archive opened May 11, 2004 –First Look Survey data sets –Legacy data sets, as they are obtained and as we manage to get the data processed GO-1 Cycle review results announced late May First GO observations were obtained a few days ago. First round of papers to appear in ApJS special issue –Posted to Web in June –Formal publication date in September GO-2 Cycle call to be issued ~November 2004 –Will include medium and large program segments –As always, open to international community

Stauffer-9CSW13, Hamburg July 2004 Spitzer’s Strengths  Peering into regions with large extinction (e.g. GMC cores)  Making maps of large areas of the sky quickly  Dusty things (disks; ISM; outflows)  Very cool objects (brown dwarfs)

Stauffer-10CSW13, Hamburg July 2004

Stauffer-11CSW13, Hamburg July 2004

Stauffer-12CSW13, Hamburg July 2004

Stauffer-13CSW13, Hamburg July 2004 Selected Spitzer “Cool Star” Science  Imaging and spectroscopy of star-forming regions  The Pleiades with IRAC and MIPS  Debris Disk Evolution of A Stars  Brown dwarf colors at IRAC wavelengths

Spitzer Space Telescope IRAC Colors of Young Stellar Objects Protostar models courtesy of Nuria Calvet Disk models from D’Alessio et al (SAO/IRAC YSO team – Megeath,Allen,Hartmann,Calvet etal)

Spitzer Space Telescope IRAC Colors of Young Stellar Objects IRAC colors were generated for models of stars with disks and protostars with infalling envelopes. (Allen et al 2004) Squares: Star/Disk models Lines: Protostar models

Spitzer Space Telescope The Cepheus C Young Stellar Cluster Contours: C 18 O emission (Ridge et al. 2003). Squares: Stars+Disks Circles: Protostars Allen et al – ApJ Supp. Special Issue

Spitzer Space Telescope IRAC Colors of Young Stellar Objects IRAC colors obtained toward four young stellar clusters show a population of sources with very red IRAC colors.

Spitzer Space Telescope IRAC Colors of Young Stellar Objects The colors cannot be the result of reddening, which makes the sources increasingly blue in the [5.8]-[8.0] color. 30 A V vectors The slope of reddening vector is dependent on the reddening law and the spectral shape of the source.

Spitzer Space Telescope IRAC Colors of Young Stellar Objects Squares: Star/Disk models Lines: Protostar models The model colors match well with the observed sources.

Spitzer Space Telescope IRAC Colors of Young Stellar Objects Circles: Protostars Squares: star+disks We have used the models to classify objects as Class II (stars with disks) or Class I (protostars). Megeath et al. 2004

Stauffer-21CSW13, Hamburg July 2004 IC 1396 – Optical Image (Reach et al. 2004, ApJ Supp. Special issue) Elephant’s trunk nebula Dark Globule in IC 1396

Stauffer-22CSW13, Hamburg July 2004 Previously Known young stars in IC 1396 A LkH  349a: T Tauri star Spitzer: detected 3.6 to 8 µm, consistent with photosphere LkH  349c: T Tauri star Spitzer: all wavelengths Strong infrared excess LkH  349 is within a cavity in the head of the globule, possibly blown by 349a wind

Stauffer-23CSW13, Hamburg July 2004 Keven Uchida, IRS/Cornell Hi-Res, 10-20um Lo-Res 5-38um IRS Spectra of Reflection Nebula: Starlight Meets Dust in the Interstellar Medium Most of these Spectral Features are due to Aromatic Hydrocarbon Molecules

Stauffer-24CSW13, Hamburg July 2004         LkH  c  Tr  HD HD  New YSOs & IR Excess

Stauffer-25CSW13, Hamburg July 2004 IRAC+MIPS color-color diagram

Stauffer-26CSW13, Hamburg July 2004 IRAC [3.6] [4.5] [8] AFGL4029 Star Formation in the HII Region W5 – Allen et al 2004

Stauffer-27CSW13, Hamburg July 2004 Class II (T Tauri) Class I (protostars)

Stauffer-28CSW13, Hamburg July 2004 Class II (T Tauri)

Stauffer-29CSW13, Hamburg July 2004 Class I (protostars)

Spitzer Space Telescope Optical Image – HH 46/47 Embedded Protostar (A. Noriega-Crespo et al. 2004)

Spitzer Space Telescope Spitzer Image of HH 46/47: Embedded Protostar + Molecular Outflows 3.6  m blue 4.5  m+5.8  m 8.0  m red 10 x 7 arcmin A. Noriega-Crespo, J. Keene, P. Morris, S. Carey (SSC/Caltech), et. al

Spitzer Space Telescope Spitzer Spectroscopy of HH 46/47: Composition and Chemistry

Spitzer Space Telescope IRS Spectra of Class I PMS stars in Taurus – D. Watson et al. 2004, ApJ Supp. Special Issue

Spitzer Space Telescope IRS spectra of TW Hya CTT’s – Uchida et al. 2004, ApJ Supp…

Stauffer-35CSW13, Hamburg July 2004 Pleiades Data from UA/SAO combined program – E. Young, G. Rieke, J. Muzzerole, J. Stauffer et al.

Stauffer-36CSW13, Hamburg July 2004 Pleiades A stars at 8 Microns Most of the Pleiades A stars do not show extended emission at IRAC wavelengths (i.e. they look like the star at the bottom right). Three of them do show extended emission at 8 microns, however. These may just be the stars that happen to have dust streamers near to them. Or, function of spectral type (UV color)? Or, ? DSS

Stauffer-37CSW13, Hamburg July 2004 Merope Region – IRAS 25micron and MIPS 24 micron images IRAS 25 micron image of 5x5 degree region of the Pleiades. Box is size of MIPS region. MIPS 24 micron - 9’ x 15’ region south of Merope

Stauffer-38CSW13, Hamburg July 2004 Merope Region at 24 Microns

Stauffer-39CSW13, Hamburg July 2004 Merope and region south of Merope IRAC Ch. 4 (8 microns) – PAH emissionMIPS 24 Micron – thermal emission, warm dust

SSC - 40July 04Hamburg CSW13 Small Portion of IRAC 1 Sq. Degree Map of the Pleiades HHJ 8 – lower marked object. Just above HBML. I = 17.1, M(4.5mu) = 13.0 Upper object is field star with M(4.5mu) = 15.2 – indicating that the 24 seconds of integration time for this AOR allows detection of Pleiades brown dwarfs to well below the HBML. IRAC Ch2 (4.5 microns)

SSC - 41July 04Hamburg CSW13 IRAC Ch. 2 (4.5 micron) – 300 second integration The 3 named stars in this field are probable Pleiades late-type members with IRAC Ch. 2 mag ~ The faintest stars in this field (5 sigma detections) have Ch. 2 mag ~ 17.0, or abs. mag ~ BCAH2000 models predict Ch.2 mag = 11.1 for 10 M(Jup) bd at Pleiades age (T ~ 910 K). The IRAC Pleiades deep survey will obtain 800 second integrations for 2400 sq. arcmin (2/3 sq. deg), which should allow identification of Pleiades members to at least 10 M(Jup) – sp. Type ~T5 at Pleiades age. That survey should begin in about six weeks. HCG254 HHJ92 MHO11

Stauffer-42CSW13, Hamburg July 2004 Evolutionary tracks at 1.5, 2, 2.5, 3, 3.5, and 4 M sun. Constant age contours for 0, 100, 200, 300, 400, 600, 800, and 1000 Myr. Gray squares and open circles are known to have ages 200 Myr. Debris disk decay in the planetary zone: the stellar sample G. Rieke et al. A Star Debris Disk Evolution Program

Stauffer-43CSW13, Hamburg July 2004 Pattern of Excesses vs. Age No excess gives 1 in this measure 211

Spitzer Space Telescope IRAC Colors of Brown Dwarfs – SAO BD’s group (B. Patten, J. Stauffer, T. Henry, A. Burrows, J. Liebert, M. Marengo) Brown dwarfs with effective temperatures <1000 K (the T or Methane dwarfs) are predicted to have low 3.6  m fluxes and high 4.5  m fluxes. T-dwarf models courtesy of Adam Burrows

Spitzer Space Telescope IRAC Colors of Brown Dwarfs 42 out of 80 M, L and T dwarfs observed, with spectral types ranging from M5 to T8 Circle: T-dwarf Diamond: L-dwarf Triangle: M-dwarf

Spitzer Space Telescope IRAC Colors of Brown Dwarfs Circle: T-dwarf Diamond: L-dwarf Triangle: M-dwarf A strong dependence of the [3.6]-[4.5] color with spectral type is demonstrated by the IRAC data. Patten et al in prep.

Spitzer Space Telescope The IRAC Galactic Zoo Circa June 1, 2004 Squares: Star/Disks Circles: Protostars Asterisks: Brown Dwarfs Diamonds: Planetary Nebulae Triangles: Outflow Knots

Stauffer-48CSW13, Hamburg July 2004 Slide Title RCW49 – GLIMPSE Image 3.6µm 4.5µm+5.8µm 8.0µm

Stauffer-49CSW13, Hamburg July 2004 G Nebulae

Stauffer-50CSW13, Hamburg July 2004 G Nebula

Stauffer-51CSW13, Hamburg July 2004 G Bubbles

Stauffer-52CSW13, Hamburg July 2004 Spitzer Observations of Brown Dwarf Disks K. L. Luhman (CfA) IC 348 Spitzer IRAC

Stauffer-53CSW13, Hamburg July 2004

Stauffer-54CSW13, Hamburg July 2004 BACKUP SLIDES

Stauffer-55CSW13, Hamburg July 2004  Pleiades at 24 microns

Stauffer-56CSW13, Hamburg July 2004 Class I (envelope) models log  = -14 to g/cm 3 L = 0.1, 1, 10, 100 Lsun inclination = 60 deg Class II (disk) models stellar T eff = 4000 K Mdot = -9 to -6 Msun/yr inclination = 30, 60 deg Allen et al. 2004, ApJS Spitzer Issue (astro-ph ) A v =30 IRAC color-color diagram