DOCSLIB.ORG

Theory of Debris Disks Modeling

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Theory of Debris Disks Modeling THEORY OF DEBRIS DISKS MODELING Jean-Charles Augereau, IPAG – Grenoble, France 2 What is a debris disk? Star Fomalhaut : composite HST+ALMA image Kalas et al. 2005, Boley et al. 2012 • Extrasolar planetary systems have planets, but also comets and asteroids ! • Extrasolar comets/asteroids manifest themselves when they release dust : collisions, evaporation ! • Debris disks • cold (~20-100K), extra-solar analogs to the Kuiper Belt • warm/hot (up to ~1500/2000K), extra-solar analogs to the asteroid belt and zodiacal dust 3 Why modeling debris disks? What do we want to know? • Grain properties: • Spatial distribution: • composition of • interaction with the unseen planets population of • history of the planetesimals formation and • size distribution evolution of planetesimals Toward a complete census of the constituents of extrasolar planetary systems, and a detailed understanding of their overall dynamics. 4 Theory of debris disk modeling Spectral Energy Distributions. Blackbody fitting, and limitations 10.0 1.0 Flux in Jy 0.1 • Hundreds of debris disks detected • Only ~40-50 have been spatially 1 10 100 1000 resolved [µm] 5 • Fractional luminosity: Spectral energy f = LIR / Lstar distribution ! ! 10.0 ! ! 1.0 !Flux in Jy Lstar ! 0.1 LIR ! 1 10 100 1000 ! [µm] • f ~ optical thickness ≪ 1 u the disk is optically thin In this example: f = 3x10-4 6 • Fit of a blackbody to the disk emission Spectral energy u disk mean temperature Tdust distribution ! • Spherical blackbody grains in thermal equilibrium: Tdust u disk radius Labsorbed = Lemitted L (⇡a2) ? =(4⇡a2)σT 4 4⇡r2 dust 10.0 L? rbb = 4 1.0 16⇡T Flux in Jy s dust 0.1 1 10 100 1000 [µm] 7 • Blackbody vs observed disk Spectral energy radii distribution Spectral L Star T r robserved Type (Lsun) Fomalhaut A3 16.6 65 K 75 AU HR 4796 A0 21 110 K 30 AU HD 181327 F6 3.3 75 K 25 AU q1 Eri F8 1.6 60 K 27 AU HD 15115 F2 3.1 65 K 32 AU HD 207129 G2 1.3 50 K 35 AU 8 • Blackbody vs observed disk Spectral energy radii distribution Spectral L Star T r robserved Type (Lsun) Fomalhaut A3 16.6 65 K 75 AU ~140 AU HR 4796 A0 21 110 K 30 AU HD 181327 F6 3.3 75 K 25 AU q1 Eri F8 1.6 60 K 27 AU HD 15115 F2 3.1 65 K 32 AU HD 207129 G2 1.3 50 K 35 AU 9 • Blackbody vs observed disk Spectral energy radii distribution Spectral L Star T r robserved Type (Lsun) Fomalhaut A3 16.6 65 K 75 AU ~140 AU HR 4796 A0 21 110 K 30 AU ~70 AU HD 181327 F6 3.3 75 K 25 AU q1 Eri F8 1.6 60 K 27 AU HD 15115 F2 3.1 65 K 32 AU HD 207129 G2 1.3 50 K 35 AU VLT/SPHERE press release image Beuzit et al. 2014 10 • Blackbody vs observed disk Spectral energy radii distribution Spectral L Star T r robserved Type (Lsun) Fomalhaut A3 16.6 65 K 75 AU ~140 AU HR 4796 A0 21 110 K 30 AU ~70 AU HD 181327 F6 3.3 75 K 25 AU ~90 AU q1 Eri F8 1.6 60 K 27 AU HD 15115 F2 3.1 65 K 32 AU HST/STIS, Schneider et al. 2014 HD 207129 G2 1.3 50 K 35 AU Figure 5. Comparison of PSF-subtraction methods revealing the HD 181327 debris ring in HST coronagraphic images with (A–D) derived from the same raw data (NICMOS 1.1 µm imagery) and (E) STIS 6 roll (6R) contemporaneous observationally matched-PSF template subtracted coronagraphy (PSFTSC). A: NICMOS discovery image using two (of ten) non-contemporaneously observed PSF template stars (Schneider et al, 2006; HST GO program 10177). B: “LAPLACE” (HST AR program 11279) re-processing and globally optimized re-reduction with PSF-matching from a down-selected 53 template ensemble (Schneider et al., 2010). C: LOCI re-processing (without regularization) with a 232 LAPLACE recalibrated PSF template library. D: KLIP re-processing (35 coefficients) using same PSF template library as (C) with regularization. C and D from Soummer, Pueyo, and Larkin 2012 (HST AR program 12652). E: STIS 6R-PSFTSC (result from this program discussed in this paper). Gray circle indicates the location and size of the NICMOS r = 0.3" coronagraphic circular obscuration. 6.2. Comparison with HST/ACS Observations While the large angular extent of the ACS coronagraphic masks (r = 0.9" and r = 1.8") preclude CS observations at small IWA’s the instrument (unlike NICMOS) does provide a coronagraphic FOV comparable to STIS. This has been used advantageously for (angularly) large CS debris systems, but is significantly less efficient than STIS. For example, the full extent of the HD 181327 debris system (unseen with NICMOS) is revealed with STIS six-roll PSFTCS and compared in Fig. 6, over the full dynamic range of imaging sensitivity, to a discovery epoch PSF-subtracted ACS image at very similar central wavelength (from Schneider et al 2006). Nebulosity in the STIS image is traced to stellocentric distances of 9.5" with more complete sampling about the star, better image fidelity, and higher sensitivity to low surface-brightness light-scattering material in the outermost, photon-limited, portions of the HD 181327 debris system. The STIS instrument’s near full-throughput pupil (compared to ~ 50% for ACS in its coronagraphic mode), and unfiltered spectral sensitivity (∆λ/λ = 75%, compared to 25% for ACS/F606W) together provide an ≈ 6x gain in exposure depth per unit integration time. For these STIS observations, with the additional investment in exposure time of a factor ≈ 4.5x over the ACS images, an improvement in exposure depth by a factor of ≈ x27 and photon-limited S/N 11 • Blackbody vs observed disk Spectral energy radii distribution Spectral L Star T r robserved −1.6 Type (Lsun) −1.7 log −1.8 10 (Flux) in Jy / arcsec Fomalhaut A3 16.6 65 K 75 AU ~140 AU −1.9 −2.0 HR 4796 A0 21 110 K 30 AU ~70 AU −2.1 HD 181327 F6 3.3 75 K 25 AU ~90 AU −2.2 −2.3 2 q1 Eri F8 1.6 60 K 27 AU ~75 AU −2.4 −2.5 HD 15115 F2 3.1 65 K 32 AU Herschel/PACS deconvoled image, HD 207129 G2 1.3 50 K 35 AU DUNES consortium Gemini/NICI, Mazoyeral.subm. et distribution Spectral energy Mazoyer et al.: Is the HD15115 inner disk really asymmetrical? -2.10-7 -1.10-7 0 1.10-7 2.10-7 Figure 2. Final KLIP image of the disk around HD 15115 in H band on the November 7, 2011. We pointed out the zones of interest. The color scale indicates the contrast with respect to the maximum intensity in the PSF image. • Blackbodyobserved vs disk But more importantly, these NICI data, of better quality than the previous ones, are radii the first to suggest a ring-like inner disk (labelled (3) in Fig. 2), which directly implies a strong dust depletion within a radius of about 2”. On the Nov. 7th, 2011 data (Fig. 2), the edges of this ring are visible in the two sides, while the Nov. 22th, 2011 data (Fig. 1, bottom, left) shows this feature in the east side only. Finally, on the west part of the disk, the bottom part of the ring below the midplane is also barely suspected in Fig. 2. A simple ellipse fitting of the suspected ring, directly in a KLIP image from Nov 7th, 2011, yields a first rough estimation of the disk parameter. We found PA 98.5◦, i 86.2◦, ⇡ ⇡ radius 2.0”. Noticeably, the ring appears almost symmetrical in size, which contrasts with ⇡ the brightness asymmetry. In addition, we didn’t measure any significant o↵set along the major axis neither along the minor axis, with respect to the star position. 3.2. Signal to noise ratio 0 2 4 6 8 10 12 0 2 4 6 8 10 12 Spectral L Star T r robserved Type (Lsun) N N 1" 1" E FomalhautE A3 16.6 65 K 75 AU ~140 AU Figure 3. Signal to noise ratio maps, calculated for the H (left)HR and Ks4796 (right) bands in A0 21 110 K 30 AU ~70 AU the Nov. 7th, 2011 data. Color scales indicate the S/N per resolution element. HD 181327 F6 3.3 75 K 25 AU ~90 AU We calculated the signal to noise ratio (S/N) in the H (Fig. 3, left) and Ks (Fig. 3, right) bands in the Nov. 7th, 2011 data. The noise is estimated in theq1 upper Eri part of the image F8 1.6 60 K 27 AU ~75 AU (PA=30 to 180◦) and per resolution element. The disk is detected as close as a separation of 1” in both sides. In the Ks band the disk has a lower S/N thanHD in the 15115 H band as we can F2 3.1 65 K 32 AU ~90 AU expect from its blue color (Debes et al. 2008). Finally, the S/N map confirms the brightness 12 asymmetry, and the rather symmetrical ring-like pattern of theHD inner disk.207129 G2 1.3 50 K 35 AU 6 13 T. Löhne et al.: Modelling the huge, Herschel-resolved debris ring around HD 207129 • Blackbody vs observed disk Spectral energy radii distribution Spectral L Star T r robserved Type (Lsun) Fomalhaut A3 16.6 65 K 75 AU ~140 AU HR 4796 A0 21 110 K 30 AU ~70 AU HD 181327 F6 3.3 75 K 25 AU ~90 AU q1 Eri F8 1.6 60 K 27 AU ~75 AU HD 15115 F2 3.1 65 K 32 AU ~90 AU Herchel/PACS, Löhne et al.
Load more

Recommended publications
  • Astrophysics Division Astrophysics Douglas Hudgins Program Scientist, Exoplanet Exploration Program Key NASA/SMD Science Themes
    National Aeronautics and Space Administration NASA and the Search for Life on Planets around Other Stars A presentation to the National Academies Committee on Exoplanet Science Strategy 6 March 2018 Paul Hertz Director, Astrophysics Division Astrophysics Douglas Hudgins Program Scientist, Exoplanet Exploration Program Key NASA/SMD Science Themes Protect and Improve Life on Earth Search for Life Elsewhere Discover the Secrets of the Universe 2 Talk summary 3 NASA’s Exoplanet Exploration Program Space Missions and Mission Studies Public Communications Kepler, WFIRST Decadal Studies K2 Starshade Coronagraph Supporting Research & Technology Key Sustaining Research NASA Exoplanet Science Institute Technology Development Coronagraph Masks Large Binocular Keck Single Aperture Telescope Interferometer Imaging and RV High-Contrast Deployable Archives, Tools, Sagan Fellowships, Imaging Starshades Professional Engagement NN-EXPLORE https://exoplanets.nasa.gov 4 Foundational Documents for the NASA’s Astrophysics Division 5 NASA’s cross-divisional Search for Life Elsewhere ASTROPHYSICS • Exoplanet detection and Planetary SCIENCE/ characterization ASTROBIOLOGY • Stellar characterization • Comparative planetology • Mission data analysis • Planetary atmospheres Hubble, Spitzer, Kepler, • Assessment of observable TESS, JWST, WFIRST, biosignatures etc. • Habitability EARTH SCIENCES • GCM • Planets as systems PLANETARY SCIENCE RESEARCH HELIOPHYSICS • Exoplanet characterization • Stellar characterization • Protoplanetary disks • Stellar winds • Planet formation • Detection of planetary • Comparative planetology magnetospheres 6 Exoplanet Exploration at NASA 2007 - present 7 The Spitzer Space Telescope For the last decade, the Spitzer Space Telescope has used both spectroscopic and photometric measurements in the mid-IR to probe exoplanets and exoplanetary systems. • Spitzer follow up observations of known transiting systems have revealed additional, new planets and helped refine measurements of the size and orbital dynamics of known planets as small as the Earth.
    [Show full text]
  • Discovery of Extreme Asymmetry in the Debris Disk Surrounding HD 15115
    Submitted to ApJ Letters December 18, 2006; Accepted April 04, 2007 A Preprint typeset using LTEX style emulateapj v. 08/22/09 DISCOVERY OF EXTREME ASYMMETRY IN THE DEBRIS DISK SURROUNDING HD 15115 Paul Kalas1,2, Michael P. Fitzgerald1,2, James R. Graham1,2 Submitted to ApJ Letters December 18, 2006; Accepted April 04, 2007 ABSTRACT We report the first scattered light detection of a dusty debris disk surrounding the F2V star HD 15115 using the Hubble Space Telescope in the optical, and Keck adaptive optics in the near-infrared. The most remarkable property of the HD 15115 disk relative to other debris disks is its extreme length asymmetry. The east side of the disk is detected to ∼315 AU radius, whereas the west side of the disk has radius >550 AU. We find a blue optical to near-infrared scattered light color relative to the star that indicates grain scattering properties similar to the AU Mic debris disk. The existence of a large debris disk surrounding HD 15115 adds further evidence for membership in the β Pic moving group, which was previously argued based on kinematics alone. Here we hypothesize that the extreme disk asymmetry is due to dynamical perturbations from HIP 12545, an M star 0.5◦ (0.38 pc) east of HD 15115 that shares a common proper motion vector, heliocentric distance, galactic space velocity, and age. Subject headings: stars: individual(HD 15115) - circumstellar matter 1. INTRODUCTION is consistent with a single temperature dust belt at ∼35 Volume-limited, far-infrared surveys of the solar neigh- AU radius with an estimated dust mass of 0.047 M⊕ borhood suggest that ∼15% of main sequence stars have (Zuckerman & Song 2004; Williams & Andrews 2006).
    [Show full text]
  • Disks in Nearby Planetary Systems with JWST and ALMA
    Disks in Nearby Planetary Systems with JWST and ALMA Meredith A. MacGregor NSF Postdoctoral Fellow Carnegie Department of Terrestrial Magnetism 233rd AAS Meeting ExoPAG 19 January 6, 2019 MacGregor Circumstellar Disk Evolution molecular cloud 0 Myr main sequence star + planets (?) + debris disk (?) Star Formation > 10 Myr pre-main sequence star + protoplanetary disk Planet Formation 1-10 Myr MacGregor Debris Disks: Observables First extrasolar debris disk detected as “excess” infrared emission by IRAS (Aumann et al. 1984) SPHERE/VLT Herschel ALMA VLA Boccaletti et al (2015), Matthews et al. (2015), MacGregor et al. (2013), MacGregor et al. (2016a) Now, resolved at wavelengthsfrom from Herschel optical DUNES (scattered light) to millimeter and radio (thermal emission) MacGregor Planet-Disk Interactions Planets orbiting a star can gravitationally perturb an outer debris disk Expect to see a variety of structures: warps, clumps, eccentricities, central offsets, sharp edges, etc. Goal: Probe for wide separation planets using debris disk structure HD 15115 β Pictoris Kuiper Belt Asymmetry Warp Resonance Kalas et al. (2007) Lagrange et al. (2010) Jewitt et al. (2009) MacGregor Debris Disks Before ALMA Epsilon Eridani HD 95086 Tau Ceti Beta PictorisHR 4796A HD 107146 AU Mic Greaves+ (2014) Su+ (2015) Lawler+ (2014) Vandenbussche+ (2010) Koerner+ (1998) Hughes+ (2011) Matthews+ (2015) 49 Ceti HD 181327 HD 21997 Fomalhaut HD 10647 (q1 Eri) Eta Corvi HR 8799 Roberge+ (2013) Lebreton+ (2012) Moor+ (2015) Acke+ (2012) Liseau+ (2010) Lebreton+ (2016)
    [Show full text]
  • Abstracts for “Extreme Solar Systems”
    Abstracts for \Extreme Solar Systems" Talk Abstracts \Pulsar Planets" Wolszczan, A. I will review the history and current status of our understanding of the PSR B1257+12 planetary system. I will also discuss neutron star planet formation scenarios and their relevance to formation and evolution of planetary systems around other stars. 1 \Extrasolar Planets: The Golden Age of Radial Velocities" Udry, S. Twelve years after the discovery of 51Pegb more than 220 planets have been detected with the radial-velocity technique. The information gathered on the orbital-element distributions, as well as on the characteristics of the planet-host stars, have largely contributed to improve our understanding of planet formation. In this presentation I will review these results with a special focus on the recent efforts of the past few years to improve the parameter space of stellar and planetary properties. The complementary and fundamental role of radial velocities in the planetary transit cases and the additional information they bring on the planet structure and on the geometry of the systems will be discussed as well. 2 \From Hot Jupiters to Hot Super-Earths" Mayor, M. In the last twelve years, more than 200 exoplanets have been detected. These discoveries have revealed the impressive diversity of exoplanet orbital properties. The past twelve years have also witnessed a remarkable improvement of the precision of radial velocity measurements with a gain of about a factor 100. Thanks to the HARPS spectro- graph installed in 2003 at la Silla Observatory ,numerous planets with masses as small as a few earth-masses have been detected.
    [Show full text]
  • Abstract Ems
    abstracts.md A table containing the talk and poster abstracts is posted below, in alphabetical order of last name. The posters themselves can be viewed on ZENODO (click for link), as well as during the gather.town live viewing sessions. Poster identifiers are in a topic.idnumber schema. Categories are as follows: 1. Atmospheres and Interiors . Detection: Transits, RVs, Microlensing, Astrometry, Imaging . Planet Formation (+ Disk) + Evolution . Know Your Star . Population Statistics & Occurrence . Dynamics 3. Instrumentation / Future 4. Habitability & Astrobiology 5. Machine Learning / Techniques / Methods Name (Affiliation). Title. Abstract Where. We present the optical transmission spectrum of the highly inflated Saturn-mass exoplanet WASP- 21b, using three transits obtained with the ACAM instrument on the William Herschel Telescope through the LRG-BEASTS survey (Low Resolution Ground-Based Exoplanet Atmosphere Survey Lili Alderson (University of using Transmission Spectroscopy). Our transmission spectrum covers a wavelength range of 4635- Bristol). LRG-BEASTS: 9000Å, achieving an average transit depth precision of 197ppm compared to one atmospheric scale Ground-bAsed Detection height at 246ppm. Whilst we detect sodium absorption in a bin width of 30Å, at >4 sigma of Sodium And A Steep confidence, we see no evidence of absorption from potassium. Atmospheric retrieval analysis of the OpticAl Slope in the scattering slope indicates that it is too steep for Rayleigh scattering from H2, but is very similar to Atmosphere of the Highly that of HD189733b. The features observed in our transmission spectrum cannot be caused by stellar InflAted Hot-SAturn activity alone, with photometric monitoring and Ca H&K analysis of WASP-21 showing it to be an WASP-21b.
    [Show full text]
  • Multiple Rings of Millimeter Dust Emission in the Hd 15115 Debris Disk
    Accepted to ApJL: May 15, 2019 Preprint typeset using LATEX style AASTeX6 v. 1.0 MULTIPLE RINGS OF MILLIMETER DUST EMISSION IN THE HD 15115 DEBRIS DISK Meredith A. MacGregor1,2, Alycia J. Weinberger1, Erika R. Nesvold1, A. Meredith Hughes3, D. J. Wilner4, Thayne Currie5, John H. Debes6, Jessica K. Donaldson1, Seth Redfield3, Aki Roberge7, Glenn Schneider8 1Department of Terrestrial Magnetism, Carnegie Institution for Science, 5241 Broad Branch Road NW, Washington, DC 20015, USA 2NSF Astronomy and Astrophysics Postdoctoral Fellow 3Astronomy Department and Van Vleck Observatory, Wesleyan University, 96 Foss Hill Drive, Middletown, CT 06459, USA 4Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA 5National Astronomical Observatory of Japan, Subaru Telescope, National Institutes of Natural Sciences, Hilo, HI 96720, USA 6Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21218, USA 7Exoplanets and Stellar Astrophysics Lab, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 8Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA ABSTRACT We present observations of the HD 15115 debris disk from ALMA at 1.3 mm that capture this intriguing system with the highest resolution (000: 6 or 29 AU) at millimeter wavelengths to date. This new ALMA image shows evidence for two rings in the disk separated by a cleared gap. By fitting models directly to the observed visibilities within a MCMC framework, we are able to characterize the millimeter continuum emission and place robust constraints on the disk structure and geometry. In the best-fit model of a power law disk with a Gaussian gap, the disk inner and outer edges are at 43:9 5:8 AU (000: 89 000: 12) and 92:2 2:4 AU (100: 88 000: 49), respectively, with a gap located ± ± ± ± at 58:9 4:5 AU (100: 2 000: 10) with a fractional depth of 0:88 0:10 and a width of 13:8 5:6 AU ± ± ± ± (000: 28 000: 11).
    [Show full text]
  • The Blue Gray Needle: LBT AO Imaging of the HD 15115 Debris Disk
    The Blue Gray Needle: LBT AO Imaging of the HD 15115 Debris Disk Timothy J. Rodigas + Phil Hinz, Andy Skemer, Kate Su, Glenn Schneider, Laird Close, Vanessa Bailey, Thayne Currie & 48 Co-authors… University of Arizona/LBTO/INAF Rodigas et al. 2012 (ApJ) L86 KALAS, FITZGERALD, & GRAHAM Vol. 661 TABLE 1 to the edge of the field, no nebulosity is detected 9.0Љ–14.9Љ Stellar Properties radius. The appearance of the disk is more symmetric in the Parameter HD 15115 HIP 12545 Reference 2006 October Keck data, which show the disk between 0.7Љ (31 AU) and 2.5Љ (112 AU). Spectral type ...... F2 M0 Hipparcos Optical surface brightness contours (Fig. 2) reveal a sharp mV (mag) .......... 6.79 10.28 Hipparcos Mass (M, ) ........ 1.6 0.5 Cox (2006) midplane morphology for the west extension that indicates an ϩ2.22 ϩ4.38 Distance (pc) ...... 44.78Ϫ2.01 40.54Ϫ3.61 Hipparcos edge-on orientation to the line of sight. The west midplane is R.A. (ICRS) ....... 02 26 16.2447 02 41 25.89 Hipparcos qualitatively similar to that of b Pic’s northeast midplane, in- Decl. (ICRS) ...... ϩ06 17 33.188 ϩ05 59 18.41 Hipparcos Ϫ1 cluding a characteristic width asymmetry (Kalas & Jewitt 1995; Hipparcos 4.46 ע 82.32 1.09 ע ma(mas yr )....... 86.09 Ϫ1 Hipparcos Golimowski et al. 2006). The northern side of the west midplane 2.45 ע Ϫ55.13 0.71 ע md (mas yr )...... Ϫ50.13 Ϫ1 ,Tycho-2 is more vertically extended than the southern side. For example 4.3 ע 82.3 1.2 ע ma(mas yr )......
    [Show full text]
  • Publication List Josh Eisner
    Publication List Josh Eisner 92. \ELT Imaging of MWC 297 from the 23-m LBTI: Complex Disk Structure and a Companion Candidate", S. Sallum, J.A. Eisner, J. Stone, et al. 2021, Astronomical Journal, 161, 28 91. \Betelgeuse scope: Single-mode-fibers-assisted optical interferometer design for dedicated stellar activity monitoring", N. Anugu, K.M Morzinski, J.A. Eisner, et al. 2020, Proc. SPIE, 11490 90. \Protoplanetary disk masses in NGC 2024: evidence for two populations", S.E. van Ter- wisga, et al., 2020, Astronomy & Astrophysics, 640, 27 89. \Protoplanetary Disks in the Orion Nebula Cluster: Gas Disk Morphologies and Kinematics as seen with ALMA", R.D. Boyden & J.A. Eisner, 2020, Astrophysical Journal, 894, 74 88. \New Spatially Resolved Imaging of the SR 21 Transition Disk and Constraints on the Small-Grain Disk Geometry", S. Sallum, A. Skemer, J.A. Eisner, et al., 2019, Astrophysical Journal, 883, 100 87. \Dusty disk winds at the sublimation rim of the highly inclined, low mass YSO SU Aurigae", A. Labdon, et al., 2019, Astronomy & Astrophysics, 627, 36 86. \High Precision Dynamical Masses of Pre-Main Sequence Stars with ALMA and Gaia", P.D. Sheehan, Y.-L. Wu, J.A. Eisner, & J. Tobin, 2019, Astrophysical Journal, 874, 136 85. \Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus", N.P. Ballering & J.A. Eisner, 2019, Astronomical Journal, 157, 144 84. \The LEECH Exoplanet Imaging Survey: Limits on Planet Occurrence Rates Under Con- servative Assumptions", J. M. Stone, et al., 2018, Astronomical Journal, 156, 286 83. \The wide integral field infrared spectrograph: commissioning results and on-sky perfor- mance", S.
    [Show full text]
  • DEBRIS DISKS in the SCORPIUS-CENTAURUS OB ASSOCIATION RESOLVED by ALMA Jesse Lieman-Sifry1, A
    Accepted for publication in ApJ: June 20, 2016 Preprint typeset using LATEX style emulateapj v. 04/20/08 DEBRIS DISKS IN THE SCORPIUS-CENTAURUS OB ASSOCIATION RESOLVED BY ALMA Jesse Lieman-Sifry1, A. Meredith Hughes1, John M. Carpenter2,3, Uma Gorti4, Antonio Hales3,5, Kevin M. Flaherty1 Accepted for publication in ApJ: June 20, 2016 ABSTRACT We present a CO(2-1) and 1240 µm continuum survey of 23 debris disks with spectral types B9-G1, observed at an angular resolution of 000: 5-1" with the Atacama Large Millimeter/Submillimeter Array (ALMA). The sample was selected for large infrared excess and age ∼10 Myr, to characterize the prevalence of molecular gas emission in young debris disks. We identify three CO-rich debris disks, plus two additional tentative (3σ) CO detections. Twenty disks were detected in the continuum at the > 3σ level. For the 12 disks in the sample that are spatially resolved by our observations, we perform an independent analysis of the interferometric continuum visibilities to constrain the basic dust disk geometry, as well as a simultaneous analysis of the visibilities and broad-band spectral energy distribution to constrain the characteristic grain size and disk mass. The gas-rich debris disks exhibit preferentially larger outer radii in their dust disks, and a higher prevalence of characteristic grain sizes smaller than the blowout size. The gas-rich disks do not exhibit preferentially larger dust masses, contrary to expectations for a scenario in which a higher cometary destruction rate would be expected to result in a larger mass of both CO and dust.
    [Show full text]
  • Dimitri Mawet
    DIMITRI MAWET [email protected] http://www.astro.caltech.edu/~dmawet/ (+1)626-395-1452 California Institute of Technology, Astronomy Department MC 249-17 1200 E. California Blvd., Pasadena, CA 91125 RESEARCH INTERESTS Extrasolar planetary systems formation and evolution: • Exoplanet detection, imaging and spectroscopic remote sensing. • Proto-planetary, transitional and debris circumstellar disk studies. Optical/infrared astronomy instrumentation: • Imaging, spectroscopy, (spectro-)polarimetry. • High contrast imaging/coronagraphy from optical to mid-infrared wavelengths. • Optical vortex, and vector vortex coronagraphy. • Adaptive optics/wavefront control techniques for ground and space-based telescopes. • Micro/nano-optics, diffractive optics, optical design/modeling, polarization. EDUCATION Ph.D. in Science, University of Li`ege Sep 2006 • Thesis: Subwavelength gratings for extrasolar planetary system detection and characterization. • Advisor: Prof. J. Surdej M.Phil. in Science, University of Li`ege Jun 2004 • Thesis:Applications des r´eseaux sub-lambda en interf´erom`etrieet coronographie. • Advisor: Prof. J. Surdej M.Phil. in Physical Engineering, University of Li`ege Sep 2002 • Thesis:Etude d'un coronographe `a4 quadrants au moyen de l'optique diffractive. • Advisor: Prof. J. Surdej B.S. in Civil Engineering, University of Li`ege Sep 1999 APPOINTMENTS & EXPERIENCE California Institute of Technology Feb 2015 - Present Associate Professor of Astronomy Pasadena, CA · Teaching: Ay105, Ay122a, Ay/Ge198, Ay141, Ay142, Ay30. · Astronomy Colloquium committee. · Graduate student admission committee. · Postdoctoral Prize fellowships in experimental physics or astrophysics selection committee. · Caltech Optical Observatories Time Allocation Committee. · PI of the Exoplanet Technology Laboratory. · PI of the High Contrast Spectroscopy Testbed for Segmented Telescopes. · PI of the Keck Planet Imager and Characterizer (KPIC).
    [Show full text]
  • Dr. Meredith A. Macgregor
    Dr. Meredith A. MacGregor Contact Carnegie DTM (720) 989-5691 Information 5241 Broad Branch Road [email protected] Washington, D.C. 20015 https://www.cfa.harvard.edu/∼mmacgreg Research Circumstellar disk structure and evolution Planetary system formation Interests Planet{disk interactions Stellar activity and impact on habitability Radio interferometry Aperture synthesis techniques Education Harvard University, Cambridge, MA Ph.D., Astronomy and Astrophysics, May 2017 • Thesis Title: `Millimeter Studies of Nearby Debris Disks' • Advisor: Dr. David J. Wilner M.A., Astronomy and Astrophysics, May 2013 Harvard University, Cambridge, MA B.A., Astronomy and Astrophysics, Physics, June 2011 • Cum Laude • Thesis Title: `A Search for Fast Optical Transients' • Advisor: Prof. Edo Berger Academic NSF Postdoctoral Fellow, Carnegie Fellow Sept. 2017 { present Positions Carnegie Department of Terrestrial Magnetism Supervisor: Dr. Alycia J. Weinberger Postdoctoral Researcher May 2017 { Sept. 2017 Harvard-Smithsonian Center for Astrophysics Supervisor: Dr. David J. Wilner Graduate Research Assistant Sept. 2011 { May 2017 Dept. of Astronomy, Harvard University Advisor: Dr. David J. Wilner Undergraduate Research Assistant Dec. 2009 { June 2011 Dept. of Astronomy, Harvard University Advisor: Prof. Edo Berger NSF REU May 2010 { Aug. 2010 National Radio Astronomy Observatory Advisor: Dr. Jeffery G. Mangum NSF REU May 2009 { Aug. 2009 Maria Mitchell Observatory Advisor: Dr. Vladimir Strelnitski Publications 30 publications in total (10 first author, 3 second author, 10 co-author, 7 unrefereed) with 438 citations and h-index of 14 (from ADS). A complete listing is at the end. Awards Fellowships and Scholarships • NSF Astronomy and Astrophysics Postdoctoral Fellowship 2017 • Carnegie Postdoctoral Fellowship, Carnegie DTM 2017 • Jansky Postdoctoral Fellowship (declined) 2017 • John P.
    [Show full text]
  • A. Meredith Hughes Curriculum Vitae – May 29, 2019 Van Vleck Observatory [email protected] 96 Foss Hill Dr
    A. Meredith Hughes Curriculum Vitae – May 29, 2019 Van Vleck Observatory [email protected] 96 Foss Hill Dr. http://amhughes.web.wesleyan.edu/ Middletown, CT 06459 Phone: (860) 685-3667 Office: VVO109 EDUCATION Harvard University, Cambridge, Massachusetts Ph.D., Astronomy (Advisor: Dr. David Wilner) May 2010 Thesis title: Circumstellar Disk Structure through Resolved Submillimeter Observations Yale University, New Haven, Connecticut B.S., Astronomy and Physics (with distinction), summa cum laude 2005 PROFESSIONAL EXPERIENCE Associate Professor, Wesleyan University Department of Astronomy 2019-present Assistant Professor, Wesleyan University Department of Astronomy 2013-2019 Miller Fellow, UC Berkeley Department of Astronomy 2010-2012 Graduate Student Researcher, Harvard University Department of Astronomy 2005-2010 RESEARCH INTERESTS Planet formation. Circumstellar disk structure and dynamics: gas and dust. Disk evolution: viscous transport and clearing processes. Radio astronomy. Aperture synthesis techniques. HONORS AND AWARDS Cottrell Scholar, Research Corporation for Science Advancement (for outstanding teacher-scholars) 2018 Bok Prize, Harvard University Dept of Astronomy (research excellence by PhD graduate under age 35) 2015 Miller Fellowship, Miller Institute for Basic Research in Science, UC Berkeley 2010-2012 Fireman Fellowship, Harvard University Dept of Astronomy (outstanding PhD thesis) 2010 National Science Foundation Graduate Research Fellowship 2007-2010 Certificate of Distinction in Teaching, Derek Bok Center at Harvard University 2009 George Beckwith Prize in Astronomy, Yale University 2005 Phi Beta Kappa, Yale University (top 1% of Junior class) 2003 TEACHING & ADVISING Postdoctoral Collaborators Supervised Kevin Flaherty, 2013-2018 à Williams College Lecturer and Observatory Supervisor MA Theses Supervised 2013-present 6. Jonas Powell ’19 à Systems & Technology Research, Woburn, MA Exploring the Role of Environment in the Composition of ONC Proplyds.
    [Show full text]