Tracing the disk-halo interaction in late type galaxies by X-ray observations Ralf-Jürgen Dettmar Astronomical Institute Ruhr-University Bochum with Jörn.

Slides:

Advertisements

Similar presentations

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

Advertisements

Feedback: in the form of outflow. AGN driven outflow.

X Y i M82 Blue: Chandra Red: Spitzer Green & Orange: Hubble Face-on i = 0 Edge-on i = 90 Absorption-line probes of the prevalence and properties of outflows.

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

Front X-ray Studies of Galaxies and Galaxy Systems Jesper Rasmussen Ph.D. Defence Astronomical Observatory, Univ. of Copenhagen 17th March 2004.

Galaxies-I. By the 1700’s the old notion that the Earth was the center of the Universe was overthrown by the success of Newton’s theory of universal gravitation,

X-ray Properties of Five Galactic SNRs arXiv: Thomas G. Pannuti et al.

Gaseous galactic halos and the interstellar disk-halo connection Ralf-Jürgen Dettmar Astronomical Institute Ruhr-University Bochum.

CLUES TO THE FORMATION AND EVOLUTION OF THE MILKY WAY

ASKAP Continuum Surveys of Local Galaxies Michael Brown ARC Future Fellow Monash University.

The 6 th KIAS Workshop on Cosmology & Structure Formation Nov. 4, 2014 Effects of hot halo gas during distant galaxy-galaxy encounters Jeong-Sun Hwang.

3-D Simulations of Magnetized Super Bubbles J. M. Stil N. D. Wityk R. Ouyed A. R. Taylor Department of Physics and Astronomy, The University of Calgary,

June 4, 2015Dusty2004 Spitzer Space TelescopeCen A Elliptical and (other) early-type galaxies T. Wiklind ESA/STScI.

Figure 8. Input parameters for a tilted-ring model of the HI in NGC We used 40 rings of width 29”, corresponding to a width of ~1.2 kpc at a distance.

Searching for the large-scale hot gaseous Galactic halo --Observations confront theories Yangsen Yao in collaboration with Michael A. Nowak Q. Daniel Wang.

Katarzyna Otmianowska-Mazur (OA UJ Kraków)‏ Grzegorz Kowal (Uniw. Sao Paulo, Brazylia/OA UJ Kraków)‏ Katarzyna Kulpa-Dybeł (OA UJ Kraków) Hubert Siejkowski,

Although there are regions of the galaxy M33 which show both high density neutral hydrogen gas and 24 micron emission, high density gas does not always.

Malaysia09:Galaxy evolution and Environment Compact Groups’ Group: S. Borthakur, T. Ponman, J. Ramussen, M. S. Yun, D. Espada, U. Lisenfeld Malaysia09:Galaxy.

Q. Daniel Wang and Cornelia Lang (U. of Massachusetts) Eric Gotthelf (Columbia U.) Chandra X-ray Survey of the Galactic Center: On the Nature of the X-ray.

The gaseous halos of spiral galaxies

Rand (2000) NGC 5775 Hα map. D = 24.8 Mpc It is an interacting galaxy.

T.G.Arshakian MPI für Radioastronomie (Bonn) Exploring the weak magnetic fields with LOFAR.

Multi-long-slit Spectroscopy for Kinematic Studies II. Initial Results for Edge-on Galaxies NGC891 and NGC4244 Jiehae Choi, Sophia Cisneros, Cat Wu, Maria.

IRAC 8 micro K-band keV X-ray Emission Line Spectroscopy of Diffuse Hot Plasma XMM-Newton RGS Liu, Wang, Li, & Peterson 2010 Li & Wan 2007 T ~ 3.

1.Extraplanar diffuse X-ray emission – a survey of highly inclined disk galaxies –How is the emission correlated with galaxy properties? –How are observations.

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

Figure 2: H  emission from NGC 1569 (Hunter et al. 1993). Note the numerous filaments extending far into the halo and the prominent H  arm in the west.

Cosmic magnetism ( KSP of the SKA) understand the origin and evolution of magnetism in the Galaxy, extragalactic objects, clusters and inter-galactic/-cluster.

8th Sino-German Workshop Kunming, Feb 23-28, 2009 Milky Way vs. M31: a Tale of Two Disks Jinliang HOU In collaboration with : Ruixiang CHANG, Shiyin SHEN,

Chris Wilson McMaster University - C. Wilson, F. Israel, S. Serjeant (coordinators) - B. Warren, E. Sinukoff, D. Attewell; C. Baker, J. Newton, T. Parkin,

Matthias Ehle The Environments of Galaxies Crete, 9-13 August XMM-Newton SOC, ESAC Hot gaseous Halos & their Dependence on Activity in the underlying.

Unravelling the formation and evolutionary histories of the most massive galaxies Ilani Loubser (Univ. of the Western Cape)

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.

Gas Dynamics, AGN, Star Formation and ISM in Nearby Galaxies Eva Schinnerer (MPIA) S. Haan, F. Combes, S. Garcia-Burillo, C.G. Mundell, T. Böker, D.S.

Hot gas in galaxy pairs Olga Melnyk. It is known that the dark matter is concentrated in individual haloes of galaxies and is located in the volume of.

The shapes of the THINGS HI profiles Presented by : Ianjamasimanana Roger Supervisor : Erwin de Blok UNIVERSITY OF CAPE TOWN.

The J Group: Evolution and Interaction Virginia Kilborn Swinburne University of Technology Sarah Sweet (Australian National University) Gerhardt.

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

Extreme soft X-ray emission from the broad-line quasar REJ R.L.C. Starling 1*, E.M. Puchnarewicz 1, K.O. Mason 1 & E. Romero- Colmenero 2 1 Mullard.

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

Kashi1 Radio continuum observations of the Sombrero galaxy NGC4594 (M104) and other edge-on spirals Marita Krause MPIfR, Bonn Michael Dumke ESO,

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.

Radio Waves Interaction With Interstellar Matter

MNRAS, submitted. Galaxy evolution Evolution in global properties reasonably well established What drives this evolution? How does it depend on environment?

ICM-ISM Stripping in Virgo Cluster Spiral Galaxies Jeff Kenney (Yale University) with: J. Van Gorkom B. Vollmer H. Crowl * A. Abramson A. Chung J. Cortes.

Introduction KU-4/2007 The ISM K.D.Kuntz The Henry A. Rowland Department of Physics and Astronomy The Johns Hopkins University (Diffuse Emission in Galaxies)

X-ray study of a nearby nuclear X-ray study of a nearby nuclear starburst and a nearby AGN starburst and a nearby AGN Roberto Soria (UCL) Mat Page, Kinwah.

Distant Galaxies Hubble Space Telescope Ultra Deep Field.

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

Quiz #10 What would really happen to you if you were to fall all the way into the Event Horizon of a black hole? We know the gravity is unbelievably strong.

ASTR112 The Galaxy Lecture 2 Prof. John Hearnshaw 2. Constituents of the Galaxy 3. Structure of the Galaxy 4. The system of galactic coordinates 5. Stellar.

ISM X-ray Astrophysics Randall K. Smith Chandra X-ray Center.

Peter-Christian Zinn | AGN feedback works both ways | The Modern Radio Universe | 22 APR 2013 AGN feedback works both ways Positive AGN feedback through.

Our Changing View of the Galaxy NGC 2915 Ed Elson Department of Astronomy, UCT Supervised by: Prof. R. C. Kraan-Korteweg Prof W. J. G. de Blok 3 rd Annual.

Cornelia C. Lang University of Iowa collaborators:

XMM-Newton 1 Matthias Ehle - RSSD XMM-Newton Observations of nearby edge-on Starburst Galaxies Matthias Ehle XMM-Newton Science Operations Centre VilSpa,

Universe Tenth Edition

Introduction to Galaxies Robert Minchin. What is a galaxy?

Imaging Dust in Starburst Outflows with GALEX Charles Hoopes Tim Heckman Dave Strickland and the GALEX Science Team March 7, 2005 Galactic Flows: The Galaxy/IGM.

Ewan O’Sullivan (SAO) thanks to: J. Vrtilek, L. David, S. Giacintucci, S. Raychaudhury, A. Zezas, and others.

“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.

On the initial conditions and evolution of isolated galaxy models 2012 Workshop on Computational Sciences and Research Hub Induck Hall at Pusan Nat'l University.

Lecture 9: Wind-Blown Bubbles September 21, 2011.

The Milky Way Announcements Assigned reading: Chapter 15.1 Assigned reading: Chapter 15.1 Please, follow this final part of the course with great care.

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

The X-ray Morphology and Spectra of Galactic Disks

Dark matter and anomalous gas in the spiral galaxy NGC 4559

Cornelia C. Lang University of Iowa collaborators:

SKADS Polarization Simulations The MPIfR team (Milky Way & star-forming galaxies): Tigran Arshakian, Rainer Beck, Marita Krause, Wolfgang Reich, XiaoHui.

Presentation transcript:

Tracing the disk-halo interaction in late type galaxies by X-ray observations Ralf-Jürgen Dettmar Astronomical Institute Ruhr-University Bochum with Jörn Rossa, Ralph Tüllmann, Volker Heesen, Dieter Breitschwerdt, Michael Dahlem, Matthias Ehle, Wolfgang Piech, Rainer Beck, Marita Krause, Marian Soida, Marek Urbanik, Peter Kamphuis et al.

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC our paradigm… from Reynolds in Scientific American

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC Ferrara & McLow

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC NGC 4631 Chandra Wang et al. NGC 4631NGC 4631

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC What controls the interstellar disk-halo 1 connection ? we want to look at… energy required mass transfered metals provided 1) Sometimes now also called ISM/IGM connection

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC example: N891 total HI Halos have a multiphase medium: neutral (perhaps even molecular?)

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC gaseous galactic halos of diffuse ionized gas (DIG) are easily observable in H  NGC4700 (Rossa&Dettmar 2001)

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC Larger sample of edge-on galaxies including objects with lower FIR luminosity

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC Rossa & Dettmar (2003)

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC NGC 7090 Dahlem & Ehle ATCA Rossa et al. ACS/HST

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC a small survey of disk galaxies with XMM: (Tüllmann et al A&A)

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC NGC 4631 seen with XMM-Newton (Tüllmann, Dettmar et. al. 2006)

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC X-ray luminosity – SFR correlation Tüllmann et al. A&A 2006 a,b from XMM-Newton

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC numerical models of the ISM: de Avillez & Breitschwerdt

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC DIG halo of NGC 5775 VLT / FORS1 slit positions (Tüllmann et al 2000)

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC NGC 5775 rotation drops to systemic

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC NGC 891 WIYN Howk et al.

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC NGC 891 H  velocity field from Fabry-Perot observations Kamphuis, Peletier, Dettmar et al. A&A 2007

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC Kamphuis, Peletier, Dettmar, et al. 2007

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC Summary: gas halo ISM is „multiphase“ the presence of ionized gas and CRs in halos is correlated with the star formation in the underlying disk observed „X-ray hot halos“ fit into this general picture (temp. gradients) a strong poloidal component of the magnetic field is associated with the presence of gaseous halos the warm ionized gaseous halos rotate differentially showing decreasing rotation with increasing hight above the plane

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC VLA 6cm mosaic (15 pointings) Heesen, PhD thesis, in prep.

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC Red: Halpha Green: VLA 6.2 cm total power Blue: ROSAT (soft X-ray)‏ B-vectors VLA 6.2 cm

X-rays from the disk-halo interface in spirals Ralf-Jürgen from Nearby Galaxies ESAC