1. Placing our Solar System in Context Latest Results from the FEPS Spitzer Legacy Science Program http://feps.as.arizona.edu/ D. Soderblom (STScI), & FEPS collaboration: M.R. Meyer (U. of Arizona, PI), L.A. Hillenbrand (Caltech, D.PI.), D. Backman (SETI) S.V.W. Beckwith (STScI), J. Bouwman (MPIA), J.M. Carpenter (CalTech), M. Cohen (UC-Berkeley), S. Cortes (Steward), U. Gorti (NASA-Ames), T. Henning (MPIA), D.C. Hines (Space Science Institute), D. Hollenbach (NASA-Ames), J. Serena Kim (Steward), J. Lunine (LPL), R. Malhotra (LPL), E. Mamajek (CfA), A. Moro-Martin (Steward), P. Morris (SSC), J. Najita (NOAO), D. Padgett (SSC),I. Pascucci (Steward), J. Rodmann (MPIA), Wayne M. Schlingman (U. of Arizona), M.D. Silverstone (Steward), J.R. Stauffer (SSC), E. Stobie (Steward), S. Strom (NOAO), D. Watson (Rochester), S. Weidenschilling (PSI), S. Wolf (MPIA), and E. Young (Steward) Summary We present results from the Formation and Evolution of Planetary Systems (FEPS) Spitzer Legacy Science Program. FEPS utilizes Spitzer observations of 336 sun-like stars with ages from 3 Myr to 3 Gyr in order to construct spectral energy distributions (SEDs) from 3-160 microns, as well as obtain high resolution mid- infrared spectra. The SEDs yield constraints on the geometric distribution and mass of dust while the spectra enable a search for emission from gas in circumstellar disks as a function of stellar age. Our main goals are to study the transition from primordial to debris disks at ages < 100 Myr, determine the lifetimes of gas-rich disks in order to constrain theories of Jupiter-mass planet formation, and explore the diversity of planetary architectures through studies of the range of observed debris disk systems. We summarize recent results including: 1) the lifetime of inner disks emitting in the IRAC bands from 3-8 microns from 3-30 Myr (Silverstone et al. 2006); 2) limits on the lifetime of gas-rich disks from analysis of a IRS high resolution spectral survey (Pascucci et al. 2006), 3) detection of warm debris disks using MIPS 24 and the IRS (Hines et al. 2006; Meyer et al. in prep); 4) physical properties of old, cold debris disk systems detected with MIPS 70 (Hillenbrand et al. in prep); and 5) exploration of the connection between debris and the presence of radial velocity planets (Moro-Martin et al., submitted). A full program description can be found in Meyer et al. (2006, PASP, in press). Cold Kuiper Belt-like disks (Hillenbrand et al. in prep; Moro-Martin et al. submitted) Age range: 300 Myr – 3 Gyr a dust : ~10 micron with P-R drag time scales of 10um silicate grains: 2 – 30 Myr. Radiation blowout sizes (a MIN, silicate ): ~0.3 – 0.7 micron L dust /L * : ~10 -4 with M dust : from blackbody models: 10 -10 – 10 -11 M sun R IN : ~20 - >30 AU ( > R SUBLIMATION, icy grains ) We find Kuiper-Belt like debris disks in 13 new objects for a total of 31 sources with 70 micron excess in the FEPS sample. Some sources appear to have extended debris disks with multi-temperature dust models required. Figure 7: Warm Dust Radii vs. Cool Dust Radii Rinner determined from blackbody grain fit to 24-33 um color temperature and limit on Router from 70 um constraints. AgeN*/NtotDistance (pc)Targets 3-10 Myr50/~14080 - 60Tau, Oph, Cha, Lup, Upper Sco 10-30 Myr60/~16060 - 160Tau, Oph, Cha, Lup, Cen Crux 30-100 Myr65/~13040 - 180IC2602, a Per 100-300 Myr65/~10020 - 120Ursa Major, Castor, Pleiades 0.3-1 Gyr65/~10020 - 60Field stars, Hyades 1-3 Gyr50/~100020 - 60Field stars From Protostellar Disks to Mature Planetary Systems Primordial Disks: - gas rich - opacity is dominated by primordial grains. Transition Disks: - very short time scale - planetesimals grow Debris disks: - no detection of gas - Poynting-Robertson (P-R) drag time scale is shorter than the age of system, therefore pristine grains in a disk had been spiraled into the star. Therefore, we expect no residual ISM dust left over from formation. - opacity is dominated by 2 nd generation grains produced by collisions of planetesimals. See recent review by Meyer et al. (2006). Spitzer Observations IRAC (imaging at 3.6um, 4.8um, 8.0um) IRS (spectroscopy at 5um - 35um) - both Low and high resolution MIPS (imaging at 24um, 70um, 160um) Overall FEPS Goals Characterize transition from primordial to debris disks Constrain timescale of gas disk dissipation Examine the diversity of planetary systems Is our Solar System common or rare? Sample Dissipation of Gas-Rich Disks (Silverstone et al. 2006; Pascucci et al. 2006) Age range: 3 - 300 Myr Among the 74 sources 3-30 Myr analyzed for continuum excess emission: -- 5 excesses are detected in IRAC bands -- 4 / 29 are in 3 – 10 Myr age bin -- 1 / 45 in the 10 – 30 Myr age bin Optically-thick disks typically dissipate in < 3 Myr from 0.3-3 AU. Lack of gas emission-line detections in 15 stars 3-300 Myr old limit the timescale for gas giant and ice giant planet formation as well migration scenarios for the evolution of protoplanetary orbits. References Backman, D. E. & Paresce, F. 1993, Protostars and Planets III. 1253 Beichman et al. 2005, ApJ, 622, 1160. Bryden et al. 2006, ApJ, 636, 1098. Gorlova et al. 2006, ApJ, 649, 1028. Gorti and Hollenbach, 2004, ApJ, 613, 424. Greaves et al. 2006, MNRAS, 366, 283. Hollenbach et al. 2005, ApJ, 631, 1180 Hines et al. 2006, ApJ, 638, 1070. Kenyon and Bromley, 2006, AJ, 131, 1837 Kim et al. 2005, ApJ, 632, 659-669 Meyer, M. R. et al. 2004. ApJS, 154, 422. Meyer, Backman, Weinberger, and Wyatt, 2006, PPV, in press ( astro-ph/0606399). Pascucci et al. 2006, ApJ, 651, 1177. Rieke et al. 2005, ApJ, 620, 1010. Silverstone et al. 2006, ApJ, 639, 1138. Stauffer et al. 2005, AJ, 130, 1834 Warm Disks (Hines et al. 2006; Meyer et al. in prep) 24 micron excess emission: Initially identified through [8] – [24] micron colors. Dispersion in locus of colors for non-disked sources sets 3-sigma limits. Limits for detection in dust mass: ~10 -4 – 10 -6 M earth HD 12039: A warm disk dominated by grains larger than 7 microns at T~110K around R = 4-6 AU, similar to the properties of our own asteroid belt. The star is 30Myr old. The P-R drag time is < 2 Myrs. Dust mass is about 2 x 10 -6 M earth. Hines et al. (2006). Figure 2: Gas Surface Density Upper Limits From Non-detections of Gas Emission Lines We searched for emission lines of H2, [FeII], [SI], and [SiII] using the high resolution mode of the Spitzer IRS, as well as sub-mm lines of CO with the SMT in Arizona. No emission lines were detected. Applying the models of Gorti and Hollenbach (2004) and following Hollenbach et al. (2005) we placed upper limits to the gas surface density for 15 FEPS targets with optically-thin (or lacking) dust disk signatures. The ages of the targets ranged from 3-300 Myr. Our results suggest that there is not enough gas in these systems to form gas giants (Jupiter mass), nor ice giants (Neptune mass). Furthermore, it is unlikely there is enough gas left in the terrestrial planet zone (0.3-3 AU) to damp eccemtricities of forming proto-planets as requred in some models (Pascucci et al. 2006). Blackbody Debris Disk Models Preliminary models are based on color temperatures of excess flux measured in IRS and MIPS bands fluxes. The relation between grain temperature, position, and primary stellar luminosity (Backman & Paresce 1993) is for blackbody grains larger than the longest wavelength of observation. Grain albedo is assumed to be zero. Lack of data beyond the peak of emission prevents useful characterization of outer boundary (R OUT ). Information from mineralogical features can be used to help characterizing grain size (Bouwman et al. in prep). The total radiating masses can be considered lower limits, calculated for single particle size and fixed grain density (e.g., 10 um radius and density 2.5 g/cm 3 ). Note that the Poynting-Robertson drag lifetime of a 100 um-radius grain of density 2.5 g/ cm 3 at r = 20AU around 1 L SUN star is ~ 7 x 10 7 yrs. Figure 5: Evolution of 24 Micron Excess Selected as 3-sigma Excess in [8]-[24] color: The fraction of FEPS stars with 24 micron excess selected from a sub-sample of the data for stars within 100 parsecs [light green squares] is compared to recent results from the literature as a function of age. The red squares are from Gorlova et al. (2006; see also Stauffer et al. 2005), Siegler et al. (in press), and Bryden et al. (2006). The light [dark] blue circles are from Rieke et al. (2005) [Hernandez et al. (in press)] respectively. The dark green square is a compilation of Padgett et al., Bouwman et al., and Carpenter et al. (all in press). Also indicated at the top of the chart are major epochs in the formation and evolution of our solar system. While the excess fractions for the FGK stars track below the early type stars (though they are sensitive to SMALLER amounts of dust as detected as a fraction of the photosphere), the open cluster data (red squares < 100 Myr) are consistent with the field star data (light green squares). The ensemble of the data is broadly consistent with models for terrestrial planet formation (e.g. Kenyon and Bromley 2006) and the history of our solar system (Meyer et al. in preparation). A full analysis of the distribution of dust as a function of temperature and stellar age will appear in Carpenter et al. (in preparation). Figure 1: [2Mass Ks] - IRAC [3.6um] vs. IRAC [4.5um] - [8.0um] color-color diagram 74 young targets from the FEPS sample Five apparent excess targets appear above and to the right of the locus of photospheres in this diagram are optically-thick disks. The typical error is plotted as a cross in the upper- left of this figure (Silverstone et al. 2006). The lack of sources with optically-thin excess places constraints on the during of the transition time between thick and thin from 0.3-3 AU. Figure 6: Excess emission distributions for a sub-set of the debris disk sources. Residual Spitzer emission after removal of stellar contribution. The blue lines are fits to the 33-70 um excess, the red lines are fits to the 24-33 um emission, and the green lines are composite fits when excess emission is detected at three or more wavelengths (Hillenbrand et al. in prep). Figure 3: Observed 24 micron flux divided by the expected 24 micron photospheric flux as a function of star age for all FEPS targets within 100 pc. Figure 4: SED of HD 12039 Upper limits represent the measured on source flux density + 3 times the uncertainty including calibration uncertainty. Blackbody dust model is the best fit emission model for blackbody grains. Model_11AU allows for grains to exist to 11 AU and violates the 3sigma upper limit at 70 microns. Lower spectrum is everything divided by the Kurucz model, showing departure from the photosphere at 12-14 microns (Hines et al. 2006). Figure 8: 70 Micron Dust excess as a function of age for stars with and without planets: While there was a preliminary suggestion of a correlation between the presence of a planet and the frequency and magnitude of detected debris dust from Beichman et al. (2005), we are unable to confirm a correlation based on statistical analysis of both the Bryden et al. (2006) and FEPS samples. The frequency of massive debris disks (> x100 soloar system levels) in both samples is 10-15 % regardless of the presence of known radial velocity planets. This is consistent with the notion that the conditions to generate debris (presence of planetesimal belts with at least one large oligarch) are less stringent than those required to form gas giant planets (cf. Greaves et al. 2006; Najita et al. in prep). Solid line model in left panel from Kenyon and Bromley. One planet host star in the FEPS sample, HD 38528, shown at right, has a debris disk at 70 microns. Modelling of the planet and dust disk dynamics is underway (Moro-Martin et al. in preparation).