Cold dust in the Galactic halo: first detection of dust emission in a high-velocity cloud : Francois Boulanger et Marc-Antoine Miville-Deschênes Miville.

Slides:

Advertisements

Similar presentations

Gas and mm Dust emission François Boulanger et Guilaine Lagache (Institut d Astrophysique Spatiale, Orsay) Tracing diffuse ISM components in te Solar Neighborhood.

Advertisements

Star Formation Why is the sunset red? The stuff between the stars

Gas in the Local Group James Binney & Filippo Fraternali Oxford University.

Molecular Gas and Star Formation in Dwarf Galaxies Alberto Bolatto Research Astronomer UC Berkeley Adam Leroy* Adam Leroy* Josh Simon* Josh Simon* Leo.

H 2 in external galaxies and baryonic dark matter London March 2007 Françoise COMBES.

Molecules in galaxies at all redshifts

High Resolution Observations in B1-IRS: ammonia, CCS and water masers Claire Chandler, NRAO José F. Gómez, LAEFF-INTA Thomas B. Kuiper, JPL José M. Torrelles,

H 2 Formation in the Perseus Molecular Cloud: Observations Meet Theory.

Estimate of physical parameters of molecular clouds Observables: T MB (or F ν ), ν, Ω S Unknowns: V, T K, N X, M H 2, n H 2 –V velocity field –T K kinetic.

Metals at Highish Redshift And Large Scale Structures From DLAs to Underdense Regions Patrick Petitjean Institut d’Astrophysique de Paris B. Aracil R.

Florent Rostagni 1.  Context  Sample  Algorithm for detection and classification  Star formation  X-ray – optical study  Perspectives - Conclusion.

JWST Science 4-chart version follows. End of the dark ages: first light and reionization What are the first galaxies? When did reionization occur? –Once.

The Relation between Atomic and Molecular Gas in the Outer Disks of Galaxies Jonathan Braine Observatoire de Bordeaux with... N. Brouillet, E. Gardan,

DUST AND MOLECULES IN SPIRAL GALAXIES as seen with the JCMT F.P. Israel, Sterrewacht Leiden.

Astronomy and the Electromagnetic Spectrum

A MOPRA CS(1-0) demonstration survey of the Galactic plane G. Fuller, N. Peretto, L. Quinn (University of Manchester UK), J. Green (ATNF ) All dust continuum.

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

Chania, Crete, August 2004 “The environment of galaxies” Pierre-Alain Duc Recycling in the galaxy environment F. Bournaud J. Braine U. Lisenfeld P. Amram.

Heiles meeting, Sep 04 Where is the Atomic Carbon in Ophiuchus Di Li Paul Goldsmith Gary Melnick and SWAS team.

The Interstellar Medium Astronomy 315 Professor Lee Carkner Lecture 19.

Stars science questions Origin of the Elements Mass Loss, Enrichment High Mass Stars Binary Stars.

Stardust in the Early Universe Erik Elfgren Luleå University of Technology Swedish National Graduate School of Space Technology.

The Interstellar Medium ( 星際物質、星際介質 ) Chapter 10.

The Interstellar Medium Astronomy 315 Professor Lee Carkner Lecture 19.

The Mass of the Galaxy We can use the orbital velocity to deduce the mass of the Galaxy (interior to our orbit): v orb 2 =GM/R. This comes out about 10.

1 Origin of Variability of X-ray and γ-ray Spectra on Daily Scale Radovan Milinčić Astrophysics 711 May 3 rd 2005.

The gaseous halos of spiral galaxies

The Interstellar Medium Astronomy 315 Professor Lee Carkner Lecture 18.

Definitive Science with Band 3 adapted from the ALMA Design Reference Science Plan (

Mapping Hydrogen in the Galaxy, Galactic Halo and Local Group with the Galactic Arecibo L-Band Feed Array (GALFA) The GALFA-HI Survey starting with TOGS.

Star and Planet Formation Sommer term 2007 Henrik Beuther & Sebastian Wolf 16.4 Introduction (H.B. & S.W.) 23.4 Physical processes, heating and cooling.

A hot topic: the 21cm line I Benedetta Ciardi MPA.

Black holes: do they exist?

The Canadian Galactic Plane Survey Mapping the Ecology Of the Milky Way Galaxy.

Nebular Astrophysics.

Space Between the Stars: Properties of the Interstellar Medium Steven R. Spangler University of Iowa.

Accurate measurement of interstellar hydrogen as the target of hadronic gamma rays Yasuo Fukui Nagoya University Southern Observatories CTA meeting April.

130 cMpc ~ 1 o z~ = 7.3 Lidz et al ‘Inverse’ views of evolution of large scale structure during reionization Neutral intergalactic medium via HI.

Nov 27th 2008Southwold and Reydon Society FROM SOUTHWOLD SKIES TO THE UNIVERSE - a journey through space astronomy Michael Rowan-Robinson.

Star Formation in our Galaxy Dr Andrew Walsh (James Cook University, Australia) Lecture 1 – Introduction to Star Formation Throughout the Galaxy Lecture.

Note that the following lectures include animations and PowerPoint effects such as fly-ins and transitions that require you to be in PowerPoint's Slide.

The Dark Side of the Universe Sukanya Chakrabarti (FAU)

Interstellar Matter and Star Formation in the Magellanic Clouds François Boulanger (IAS) Collaborators: Caroline Bot (SSC), Emilie Habart (IAS), Monica.

Seeing Stars with Radio Eyes Christopher G. De Pree RARE CATS Green Bank, WV June 2002.

An Investigation of the Molecular-FIR-Radio correlation at small scales in the Galaxy Mónica Ivette Rodríguez Dr. Laurent Loinard (UNAM - México) Dr. Tommy.

The Effect of Escaping Galactic Radiation on the Ionization of High-Velocity Clouds Andrew Fox, UW-Madison STScI, 8 th March 2005.

ASTR112 The Galaxy Lecture 7 Prof. John Hearnshaw 11. The galactic nucleus and central bulge 11.1 Infrared observations (cont.) 11.2 Radio observations.

What we look for when we look for the dark gas * John Dickey Wentworth Falls 26 Nov 2013 *Wordplay on a title by Raymond Carver, "What we talk about, when.

Lecture 30: The Milky Way. topics: structure of our Galaxy structure of our Galaxy components of our Galaxy (stars and gas) components of our Galaxy (stars.

The Interstellar Medium and Star Formation Material between the stars – gas and dust.

Delphine Marcillac Moriond 2005 When UV meets IR... 1 IR properties of distant IR galaxies Delphine Marcillac (PhD student) Supervisor : D. Elbaz In collaboration.

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

AST101 Lecture 20 The Parts of the Galaxy. Shape of the Galaxy.

ASTR112 The Galaxy Lecture 9 Prof. John Hearnshaw 12. The interstellar medium: gas 12.3 H I clouds (and IS absorption lines) 12.4 Dense molecular clouds.

Surveying the Highly Ionized HVCs with FUSE and HST Joe Collins (University of Colorado) Mike Shull (University of Colorado) Mark Giroux (East Tennessee.

Chapter 14 The Interstellar Medium. All of the material other than stars, planets, and degenerate objects Composed of gas and dust ~1% of the mass of.

1 Radio – FIR Spectral Energy Distribution of Young Starbursts Hiroyuki Hirashita 1 and L. K. Hunt 2 ( 1 University of Tsukuba, Japan; 2 Firenze, Italy)

FIRST LIGHT A selection of future facilities relevant to the formation and evolution of galaxies Wavelength Sensitivity Spatial resolution.

First high-resolution 3D inversion of the dust emission in Galactic ISM with Spitzer/Herschel. The case region [l,b]=[30,0] A. Traficante, R. Paladini,

ASTR112 The Galaxy Lecture 12 Prof. John Hearnshaw 16. Evolution of the Galaxy 16.1 Star formation 16.2 Exchange of material between stars and ISM 16.3.

Neutral Atomic Hydrogen Gas at Forbidden Velocities in the Galactic Plane Ji-hyun Kang NAIC Seoul National University Supervisor :Bon-Chul Koo 213 th AAS.

NIR, MIR, & FIR.  Near-infrared observations have been made from ground based observatories since the 1960's  Mid and far-infrared observations can.

“Globular” Clusters: M15: A globular cluster containing about 1 million (old) stars. distance = 10,000 pc radius  25 pc “turn-off age”  12 billion years.

Takashi Hosokawa ( NAOJ ) Daejeon, Korea Shu-ichiro Inutsuka (Kyoto) Hosokawa & Inutsuka, astro-ph/ also see, Hosokawa & Inutsuka,

Ay126: Fine Structure Line Emission from the Galaxy

Galaxy Formation and Evolution: Where we are and where we are going.

An Arecibo HI 21-cm Absorption Survey of Rich Abell Clusters

Atomic gas Molecular clouds

The Interstellar Medium

Presentation transcript:

Cold dust in the Galactic halo: first detection of dust emission in a high-velocity cloud : Francois Boulanger et Marc-Antoine Miville-Deschênes Miville Deschenes, Boulanger, Reach and Noriega-Crespo 2005, Ap. J. 631 L57.

XFLS High Velocity Clouds Observed on 20% of the sky

Widespread interest in HVCs is due to their mystery... > Debatted origin Galactic fountain Tidal debris of local group dwarf galaxies Dark matter halos in the Local Group Physical description, spatial distribution, masses and dynamics

… and their potential for being important > Formation and evolution of galaxies Potential tracers of small dark matter halos Source of gas to fuel star formation Accretion of low metallicity gas for chemical evolution Energy, mass and angular momentum flows within galaxies

Multiphase systems > First detection : Muller, Oort and Raimond 1963 C. R. Acad. Sc. Paris (21cm line, Dwingeloo 25 m dish) > Today: Cold neutral gas (HI) Warm neutral and ionized gas (HI, Halpha) Conductive interfaces (OVI, CIV, NV) Embedded in a Galactic halo of coronal gas (X-rays) Dust and Molecules?

XFLS High Velocity Clouds Observed on 20% of the sky

XFLS Spitzer Extragalactic First-Look Survey

Infrared-HI comparison of the Spitzer Extragalactic First-Look Survey IRAS 100 micron and GBT-HI overlay Draco nebula

HI Spectra HI Maps Lockman and Condon 2005 GBT Observations

IRIS: a new generation of IRAS maps Comparison with Schlegel et al. –Better photometry (scale and brightness correction) –Better angular resolution 4 IRAS bands (Schlegel et al. is only 100 micron) Miville-Deschenes & Lagache, 2005

Spitzer and IRAS Images

Multivariate regression to estimate the infrared emissivity of each HI component. First detection of dust emission in the HVC –HVC Emissivity at 100 m ~ 10 times smaller than local gas, but only a factor 2 smaller at 160 m Colder dust Infrared-HI correlation I (x,y) = i i N HI i (x,y) + C (x,y)

Infrared-HI Correlation

Dust in Complex C Dust Temperatures and emissivities per HI atom

Gas column densities Dust emissivity per H gas metallicity for a fixed fraction of heavy elements in dust (fixed depletion) Z HVC /Z Sun = 0.2 +/- 0.1 (Tripp et al. 2003) Dust emissivity per HI, HVC over Local ISM value > 1.6 (3 ) N H (HVC) > 1.6/0.3 * N HI (HVC) NHII/NH ~ 0.2 (Wakker et al. 1999) Most of the HVC gas is in molecules

FUSE search for H2 in absorption Richter et al. 2001

Conclusions and Perspectives Confirmation of dust detection result on other fields HVC in Spitzer extra-galactic fields: dedicated GBT+DRAO observations scheduled Dedicated Spitzer observing program? HVCs could make part of the sub-mm extra-galactic background! Search for CO emission from molecular clumps IRAM 30m proposal Clumps origin: self gravitating long lived structures or signatures of the dynamical interaction with the Galactic corona New perspective on HVCs and the Galaxy evolution New hunting grounds for molecules ?