Protoplanetary Disk Evolution Science goal: A composite picture of gas and dust evolution chemical evolution as a tracer of planet formation Technical.

Slides:

Advertisements

Similar presentations

Oct.10, 2007EAMA7 Japanese Space Activity on Exoplanets (JAXAs prespective) & Pathways to Habitable Planets September 16, 2009 Takao Nakagawa (ISAS/JAXA)

Advertisements

Debris disks with CCAT Jane Greaves: ~2012??

Circumstellar disks: what can we learn from ALMA? March ARC meeting, CSL.

Francesco Trotta YERAC, Manchester Using mm observations to constrain variations of dust properties in circumstellar disks Advised by: Leonardo.

Water In Star-forming regions with Herschel  A 429 hr GT key-program with Herschel to study the physical and chemical structure of star forming regions.

Water In Star-forming regions with Herschel  A 429 hr GT key-program with Herschel to study the physical and chemical structure of star forming regions.

Sarah Kendrew Leiden Instrumentation Group.  One of eight potential instruments for the European ELT, the largest planned optical/IR telescope for the.

SN 1987A spectacular physics Bruno Leibundgut ESO.

Star Formation in AGN hosts Li Shao & PACS Evolutionary Probe (PEP) group Hangzhou, China April 28, 2011 Evidence from Herschel PACS.

Studying circumstellar envelopes with ALMA

Dust/Gas Correlation in the Large Magellanic Cloud: New Insights from the HERITAGE and MAGMA surveys Julia Roman-Duval July 14, 2010 HotScI.

Detecting the signature of planets at millimeter wavelengths F. Ramos-Stierle, D.H. Hughes, E. L. Chapin (INAOE, Mexico ), G.A. Blake ???

1 Debris Disk Studies with CCAT D. Dowell, J. Carpenter, H. Yorke 2005 October 11.

Radio Science and PILOT Tony Wong ATNF/UNSW PILOT Workshop 26 March 2003.

TIGER The TIGER Instrument Overview Phil Hinz - PI July 13, 2010.

Millimeter Spectroscopy Joanna Brown. Why millimeter wavelengths? >1000 interstellar & circumstellar molecular lines Useful for objects at all different.

Herschel HIFI | Jürgen Stutzki for the HIFI team | Universität zu Köln| Pag. 1 Herschel HIFI: the Heterodyn Instrument for the Far-Infrared –PI-Institut:

STAR FORMATION STUDIES with the CORNELL-CALTECH ATACAMA TELESCOPE Star Formation/ISM Working Group Paul F. Goldsmith (Cornell) & Neal. J. Evans II (Univ.

Millimetron mision sensitivities and instrumentation concept

Future of Astronomy Astronomy 315 Professor Lee Carkner Lecture 25.

Line Detection Rates for Next Generation IR/Submm Spectroscopic Surveys Eric J. Murphy BLISS/X-Spec Science teams.

The tools. Hot question of Galileo’s time what’s at the centre: earth or sun?

Exo-planets: ground-based How common are giant planets? What is the distribution of their orbits? –3.6m HARPS: long-term radial velocity monitoring of.

HIFI – The instrument, its capabilities and the proposed science Frank Helmich SRON – National Institute for Space Research.

Multiwavelength Continuum Survey of Protostellar Disks in Ophiuchus Left: Submillimeter Array (SMA) aperture synthesis images of 870 μm (350 GHz) continuum.

Lighting the dark molecular gas using the MIR H 2 rotational lines Aditya Togi Advisor: JD Smith University of Toledo 19 th June

The ALMA Level One Science Goals Al Wootten NRAO; ALMA/NA Project Scientist The highest level document governing the Atacama Large Millimeter Array (ALMA)

→ Herschel data for absolute beginners Herschel Science Centre (ESAC)

Evolution of protoplanetary disks Some new rules for planet- and star-formers, from the bounty of the Spitzer and Herschel missions. Dan Watson University.

MIRHES (Mid-IR high-resolution echelle spectrometer) MIRHES team.

Conclusions some general thoughts  NL strong in submm because of very strong synergy between science and technology  Perfect up to Herschel and ALMA,

1 BDRv3 - November 26, Markus Kissler-Patig E-ELT Programme 1 E-ELT Science Case Markus Kissler-Patig.

Molecular Gas and Dust in SMGs in COSMOS Left panel is the COSMOS field with overlays of single-dish mm surveys. Right panel is a 0.3 sq degree map at.

The Formation of Stars and Planets James De Buizer (SOFIA/USRA) Neal Evans (U. Texas), John Bally (U. Colorado), Ewine van Dishoek (Leiden Obs), Murad.

GMTNIRS (Giant Magellan Telescope Near-IR Spectrograph) Survey Science Group Workshop 3 조 김상혁 김재영 최나현

ESO Seminar, 25 May Science With ALMA T. L. Wilson European ALMA Project Scientist, and Interim JAO Project Scientist.

The Solar System Lancelot L. Kao Updated: Jan 18, 2010.

SPIRE-FTS spectrum of Arp 220, Mrk 231 and NGC Bright CO (J = 4-3 to J = 13-12), water, and atomic fine-structure line transitions are labeled. The.

Star and Planet Formation with SOFIA Neal Evans, John Bally, Jim De Buizer, Murad Hamidouche, Thomas Henning, Goran Sandell, Floris van der Tak, Ewine.

Moscow presentation, Sept, 2007 L. Kogan National Radio Astronomy Observatory, Socorro, NM, USA EVLA, ALMA –the most important NRAO projects.

Technologies for Future Far-IR Telescopes and Interferometers Dave Leisawitz, NASA GSFC SPICA SPIRIT CALISTO.

HIFI Heterodyne Instrument for the Far Infrared

Next Gen VLA Observations of Protoplanetary Disks A. Meredith Hughes Wesleyan University ALMA (NRAO/ESO/NAOJ); C. Brogan, B. Saxton (NRAO/AUI/NSF)

Science with continuum data ALMA continuum observations: Physical, chemical properties and evolution of dust, SFR, SED, circumstellar discs, accretion.

ALMA Timeline  Design and Development Phase Jun Dec 2001  International partnership established 1999  Prototype antenna contract Dec 99  ALMA/NA.

The Local Universe A CCAT perspective Christine Wilson McMaster University, Canada 7 January 20131AAS 221 – Long Beach, CA.

PACS SVR 22/23 June 2006 Scientific/Performance Requirements1 PACS Science and Performance Requirements A. Poglitsch.

The Far-Infrared Universe: from the Universe’s oldest light to the birth of its youngest stars Jeremy P. Scott, on behalf of Locke D. Spencer Physics and.

Deciphering the interplay between starlight and disks: Where is the gas? Gerrit van der Plas From disks to planets: Learning from starlight, March 18 th.

ALMA Observations of proto-planetary disks I HD – P.I. Casassus 2013 Nature 493, 191 Herbig Ae star 140 pc, 2 Myr, 1.9 M , disk mass 0.1 M  Left:

The planet-forming zones of disks around solar- mass stars: a CRIRES evolutionary study VLT Large Program 24 nights.

ALMA Science Examples Min S. Yun (UMass/ANASAC). ALMA Science Requirements  High Fidelity Imaging  Precise Imaging at 0.1” Resolution  Routine Sub-mJy.

Dust cycle through the ISM Francois Boulanger Institut d ’Astrophysique Spatiale Global cycle and interstellar processing Evidence for evolution Sub-mm.

Jet Propulsion Laboratory

Hi. My name is Alexia Lewis

Gaspard Duchêne UC Berkeley & Obs. Grenoble From circumstellar disks to planetary systems – Garching – Nov

Competitive Science with the WHT for Nearby Unresolved Galaxies Reynier Peletier Kapteyn Astronomical Institute Groningen.

High Redshift Galaxies/Galaxy Surveys ALMA Community Day April 18, 2011 Neal A. Miller University of Maryland.

Protoplanetary and Debris Disks A. Meredith Hughes Wesleyan University.

Why is water interesting? Evidence of water in space Water in young disks Water in the terrestrial planet-forming zone Future prospects Water in young.

Grain Growth and Substructure in Protoplanetary Disks David J. Wilner Harvard-Smithsonian Center for Astrophysics S. Corder (NRAO) A. Deller.

SOFIA — The Observatory

ATACAMA CCAT : The Cornell-Caltech Atacama Telescope

Key Inputs / Requirements

Debris Disk Studies with CCAT

Herschel Space Observatory

ALMA does Circumstellar Disks

9-10 Aprile Osservatorio Astronomico di Capodimonte

Cornell-Caltech Atacama Telescope (CCAT)

Presentation transcript:

Protoplanetary Disk Evolution Science goal: A composite picture of gas and dust evolution chemical evolution as a tracer of planet formation Technical requirements: High spectral resolution (R > 10 6 resolve line profile) High sensitivity (better than W/m 2 ) High spatial resolution (< 0.025” for SFR < 400 pc)

Summary TelescopeStartOuter disk Inner disk Line profiles Spatial resolution No. of disks APEXworking+-+-few Herschel PACS + HIFI ---- hundreds few SOFIA GREAT-few CCAT few ALMA2011/ few Millimetron?? SPICA~ all FIRI> ??

Protoplanetary Disk Evolution Science goal: A composite picture of gas and dust evolution chemical evolution as a tracer of planet formation Technical requirements: High spectral resolution (R > 10 6 resolve line profile) High sensitivity (better than W/m 2 ) High spatial resolution (< 0.025” for SFR < 400 pc) Instruments (soon) available: Herschel (PACS hundreds of disks - hr/target, HIFI few disks, no spatial resolution) SOFIA (GREAT few disks - hrs/target -, no spatial resolution, very narrow wavelength range) APEX (few disks - hrs/target -, no spatial resolution, only cold outer gas)

Science goal: A composite picture of gas and dust evolution chemical evolution as a tracer of planet formation Technical requirements: High spectral resolution (R > 10 6 resolve line profile) High sensitivity (better than W/m 2 ) High spatial resolution (< 0.025” for SFR < 400 pc) Future Instruments: ALMA (spatially resolve few disks - hrs/target, only cold outer gas) CCAT (no spatial resolution, only cold outer gas) FIRI (with heterodyne: spatially resolve hundreds of disks, also gas in planet forming regions) Millimetron () SPICA (all disks, only integrated fluxes, very limited spatial resolution) - successor to Herschel/PACS