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

Our Galaxy `. Interstellar dust obscures our view at visible wavelengths along lines of sight that lie in the plane of the galactic disk.

Dark Matter in Dwarf Galaxies

DARK MATTER IN GALAXIES

The Distribution of DM in Galaxies Paolo Salucci (SISSA) TeVPa Paris,2010.

Particle Astrophysics & Cosmology SS Chapter 7 Dark Matter.

SIZE OF MILKY WAY Kapteyn all visible stars – 30,000 parsecs sun close to center Shapley globular clusters – 100,000 parsecs sun 2/3.

The Milky Way. Structure of the Milky Way The Milky Way.

Chapter 14 Our Galaxy The Milky Way Revealed Our Goals for Learning What does our galaxy look like? How do stars orbit in our galaxy?

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)

Σπειροειδείς γαλαξίες

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,

THE MILKY WAY Our Home Galaxy GALAXIES 3 Main Types Spiral/Barre d Elliptical Irregular.

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

Clusters Small collection of stars… thousands to millions 2 Types: 1. Open 2. Globular.

Masses of Galaxy Groups Brent Tully University of Hawaii.

Γαλαξίες – 3 Υπερμαζικές Μαύρες Τρύπες στα κέντρα γαλαξιών 15 Ιανουαρίου 2013.

Galactic structure and star counts Du cuihua BATC meeting, NAOC.

The Milky Way Galaxy. Sky Maps in Different Bands.

“OUR GALAXY” Definition of a Galaxy: a huge group of individual stars, star clusters, dust, and gas bound together by gravity.

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

With measurements of true Distance, plus recessional velocity, can infer mass concentration within a given volume [us to GA] M/L ≈ M O /L O Can.

Dark Matter and Rotational Motion e.t. revised feb 09.

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.

Milky Way: Galactic Structure and Dynamics Milky Way has spiral structure Galactic Bulge surrounds the Center Powerful radio source Sagittarius A at Center.

AST101 Lecture 20 Our Galaxy Dissected. Shape of the Galaxy.

Galaxy Formation Collapse of an over-dense region of space (containing more gas and dark matter than average) under gravity Disks are produced as the cloud.

“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.

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

© 2017 Pearson Education, Inc.

Structure of the Milky Way

The Milky Way Nucleus Bulge Bar Disk Halo.

Lecture 32- Properties of the Milky Way (cont)

The Milky Way Galaxy 1/30/03.

Milky Way (-like) Galaxy

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.

Journey to the Galactic Center

AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics

HUBBLE DEEP FIELD:.

Molecular Gas Distribution of our Galaxy: NANTEN Galactic Plane Survey

The “Milky Way”.

‘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.

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.

Title: 30.1 Galaxies and The Universe

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

Lecture 33- What’s the Milky Way made of?

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

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

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)

Presentation transcript:

C4-Large Project Virgo/Fornax Clusters CO Survey Yoshiaki Sofue 2015/2/17 @ 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

MW: Surf. Mass Density

Comparison with BH by Genzel et al. 1994

Decomposition of Rotation Curves of Spiral Galaxies for Correlation Analysis of Sizes and Masses of Bulge, Disk and Dark Halo