Topic: Virgo/Fornax CO Survey Line: 12CO(1-0,2-1,

Slides:

Advertisements

Similar presentations

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

Advertisements

Dark Matter in Dwarf Galaxies

Inner Halo Shapes of Dwarf Galaxies: Reconciling the Cusp/Core Problem Kristine Spekkens, Riccardo Giovanelli (Cornell) 203 rd AAS, Session 105: Wednesday,

DARK MATTER IN GALAXIES

Particle Astrophysics & Cosmology SS Chapter 7 Dark Matter.

Star & Planet Formation Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics.

HST ACSCO on ACS in EGS at z=1.12 Molecular Gas in Star Forming Galaxies at z=1-3 Linda Tacconi, MPE Garching & Santa Cruz Galaxy Evolution Workshop.

18 Dark Matter Join me on the Dark Side. 18 Goals The Universe is expanding. Will it expand forever? Depends on mass? How do we know the mass of the universe?

Levels of organization: Stellar Systems Stellar Clusters Galaxies Galaxy Clusters Galaxy Superclusters The Universe Everyone should know where they live:

The Milky Way and Other Galaxies Science A-36 12/4/2007.

A1143 Quiz 4 Distribution of Grades: No Curve. Milky Way: Bright Band Across Sky (Resolved by Galileo)

TURBULENCE AND HEATING OF MOLECULAR CLOUDS IN THE GALACTIC CENTER: Natalie Butterfield (UIowa) Cornelia Lang (UIowa) Betsy Mills (NRAO) Dominic Ludovici.

Latest impacts of observational (radio) astronomy Hiroshi Imai Department of Physics and Astronomy Graduate School of Science and Engineering Introducing.

Physics 231: Section 6 Galaxies 1Phys 231, Topic 6: Galaxies.

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

ALMA DOES GALAXIES! A User’s Perspective on Early Science Jean Turner UCLA.

Understanding the Physics of the Bulge/Black-Hole Connection with GSMT Stephen Eikenberry University of Florida 3 November 2007.

Stellar Populations Science Knut Olsen. The Star Formation Histories of Disk Galaxies Context – Hierarchical structure formation does an excellent job.

Dynamical formation of LMXBs in the inner bulge of M31 by Rasmus Voss with Marat Gilfanov X-rays from nearby galaxies ESAC September 2007.

Molecular Gas (Excitation) at High Redshift Fabian Walter Max Planck Institute for Astronomy Heidelberg Fabian Walter Max Planck Institute for Astronomy.

PX269 Galaxies Part 2: Our Galaxy, the Milky Way 2.1 Components and Structure PX269 Galaxies.

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

次世代位置天文衛星による銀河系ポテンシャル測定 T. Sumi (Nagoya STE) T. Sumi (Nagoya STE) K.V. Johnston (Columbia) K.V. Johnston (Columbia) S. Tremaine (IAS) S. Tremaine (IAS)

The Milky Way Galaxy. Sky Maps in Different Bands.

Title Galaxy Structure and Dark Matter Michael Merrifield University of Nottingham.

14 Dark Matter Join me on the Dark Side. 14 Goals Why do we think there is dark matter? Where do we think it is? How much is there?

CO Rotation Curves High-velocity Rotation, Deep Potential, & Dense Molecular Cores in Spiral Centers Sofue, Y., Koda, J., Nakanishi, H., Onodera, S., Egusa,

Galaxies: Our Galaxy: the Milky Way. . The Structure of the Milky Way Galactic Plane Galactic Center The actual structure of our Milky Way is very hard.

Brigthest Cluster Galaxies Unique class of objects  most luminous  most massive  extended source  some BCG shows multiple nuclei → galaxy merger →

What is EVLA? Giant steps to the SKA-high ParameterVLAEVLAFactor Point Source Sensitivity (1- , 12 hr.)10  Jy1  Jy 10 Maximum BW in each polarization0.1.

PI Total time #CoIs, team Silvia Leurini 24h (ALMA, extended and compact configurations, APEX?) Menten, Schilke, Stanke, Wyrowski Disk dynamics in very.

“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.

ASTR112 The Galaxy Lecture 5 Prof. John Hearnshaw 8. Galactic rotation 8.3 Rotation from HI and CO clouds 8.4 Best rotation curve from combined data 9.

Stellar Populations Science Knut Olsen. The Star Formation Histories of Disk Galaxies Context – Hierarchical structure formation does an excellent job.

Simulated black hole picture

News flash ALMA observes a protoplanetary disk around the young star HL Tauri. This is the first time we can DIRECTLY actually observe a planetary system.

Galaxies! Galactic Types/Shapes (“Morphologies”).

Eyes on the Polarized Sky, Feet on the Ground

The Milky Way Nucleus Bulge Bar Disk Halo.

Lecture 32- Properties of the Milky Way (cont)

Milky Way (-like) Galaxy

RR Lyrae variable stars

The Milky Way Our home galaxy, full of stars, gas and mysterious dark matter We decompose it into a disk and a halo and a few other parts.

Resolving the black hole - nuclear cluster - spheroid connection

Part 2: The Milky Way 2.1 Components and Structure

Grand Rotation Curveｓ　& Galactic Roche Lobes in the Galaxy and M31 Yoshiaki Sofue (Meisei Uni.) at Meisei University.

ARECIBO ASTRONOMY SURVEYS

Dark Matter Join me on the Dark Side.

AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics

Molecular Gas Distribution of our Galaxy: NANTEN Galactic Plane Survey

The “Milky Way”.

HERSCHEL and Galaxies/AGN “dust and gas”

‘3D’ Data Sets are ABSOLUTELY Crucial to Answer the Important Questions of Galaxy Formation and Evolution Galaxy dynamical masses, gas masses Spatially.

Chapter 14 Spiral Galaxy.

When Giovanni Riccioli used a telescope like this one to observe a star in the handle of the Big Dipper, he discovered two stars that orbit each other.

Dark Matter Join me on the Dark Side.

Dark Matter on Galactic Scales (and the Lack Thereof)

(National Astronomical Observatory of Japan)

Dense gas history of the Universe  Tracing the fuel for galaxy formation over cosmic time SF Law SFR Millennium Simulations, Obreschkow & Rawlings 2009;

Kinemetry of High-Redshift Galaxies

Jeopardy Final Jeopardy $100 $100 $100 $100 $100 $200 $200 $200 $200

Topic: Virgo/Fornax CO Survey Line: 12CO(1-0,2-1,

Galaxies How big is the Universe? Types of galaxies Groups of galaxies

3D Galactic Shock Wave at W43 in the 4-kpc Arm

Galactic Center Rotation Curve and Mass Yoshiaki Sofue (Meisei Uni

Dark Halos of M31 and the Milky Way -- Their Dynamical Similarity – Yoshiaki Sofue (U. Tokyo) MW2015, U.Tokyo.

Essential Question: What is a galaxy and how are they classified?

Gerald-rhemann-4apr-02.

The Local Dark Matter Density Yoshiaki Sofue (U-Tokyo & Meisei-U)

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

Presentation transcript:

Virgo/Fornax Clusters CO Survey Yoshiaki Sofue 2013 /2/17 ALMA mini WS, mtk.

Topic: Virgo/Fornax CO Survey Line: 12CO(1-0,2-1, Topic: Virgo/Fornax CO Survey Line: 12CO(1-0,2-1,...) FoV: 20 disks, 100 centers, ca 1000 detection Beamsize: 10-30pc No. of targets: All cluster galaxies (ca 1000) Use of ACA: yes International CoI: Japan (Virgo team), UK (M. Bureau), US (Jin Koda) (TBD)

1. Objects Virgo/Fornax clusters of galaxies CO survey; ~20 disks, ~100 centers, ~1000 detection/per cluster Virgo= Extended NobeCO S, best studied cluster; Fornax= Martin's suggestion, best nearest cluster for ALMA)

2. Science CO database, Rot curve, dynamics, BH to Disk ISM, SF, HI + Environment (SKA-ALMA) Fundamental Plane, CO Tully-Fisher => 3D Vir/For structure)

3. Teams Interntl collabo (recomm 3. Teams Interntl collabo (recomm. for Large Program) Japan(Virgo team), UK (Martin Bureau), US (Koda) SKA (HI team) 4. Relation to other subjects

Topic 1. Rotation Curve and Mass Distribution

1. Log Rotation Curve 2. Mass models 3. BH - Bulge – Disk -DH

In comparison with the Milky Way

MW: Log RC; Inner bulge-BH

Log RC

MW: Surf. Mass Density

Comparison with BH by Genzel et al. 1994