Mapping the HI Neighborhood Around Starburst Dwarf Galaxies Megan Johnson NRAO, Green Bank Tully-Fisher Workshop, April 2012.

Slides:



Advertisements
Similar presentations
Formation of intergroup and intragroup objects Kenji Bekki (UNSW) Origin of isolated massive clouds, intergalactic HII regions, intragroup GCs etc….
Advertisements

H 2 Formation in the Perseus Molecular Cloud: Observations Meet Theory.
Observations of the evolution of HI in galaxies across different environments. D.J. Pisano (West Virginia University)
Dwarf Galaxies in Group Environments Marla Geha Carnegie Observatories (OCIW)
ESO Workshop – Jun 10, 2008 Ángel R. López-Sánchez The Local Volume H I Survey Ángel R. López-Sánchez Ángel R. López-Sánchez Bärbel S. Koribalski & the.
Supermassive Black Holes Course 689 Presentation by Yan Shi Nov 5, 2009.
Ionized and neutral gas in the starburst galaxy NGC 5253 Australia Telescope National Facility (ATNF, Australia) Galaxies in the Local Volume – Sydney.
Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2.
Chania, Crete, August 2004 “The environment of galaxies” Pierre-Alain Duc Recycling in the galaxy environment F. Bournaud J. Braine U. Lisenfeld P. Amram.
The M-81 Group of Galaxies Brian Fleming Stephanie LaMassa Seamus Riley (The Chunky Ponies)
The Milky Way Galaxy part 2
Astro-2: History of the Universe Lecture 4; April
Particle Astrophysics & Cosmology SS Chapter 7 Dark Matter.
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.
Galaxies. First spiral nebulae found in 1845 by the Earl of Rosse. Speculated it was beyond our Galaxy "Great Debate" between Shapley and Curtis.
Primeval Starbursting Galaxies: Presentation of “Lyman-Break Galaxies” by Mauro Giavalisco Jean P. Walker Rutgers University.
ULTRALUMINOUS INFRARED GALAXIES: 2D KINEMATICS AND STAR FORMATION L. COLINA, IEM/CSIC S. ARRIBAS, STSCI & CSIC D. CLEMENTS, IMPERIAL COLLEGE A. MONREAL,
Rand (2000) NGC 5775 Hα map. D = 24.8 Mpc It is an interacting galaxy.
The Complex Star Formation History of NGC 1569 L. Angeretti 1, M. Tosi 2, L. Greggio 3, E. Sabbi 1, A. Aloisi 4, C. Leitherer 4 The object The observations.
CDM cusps in LSB galaxies by means of stellar kinematics A.Pizzella, E.M.Corsini, F. Bertola Università di Padova And J. Magorrian, M. Sarzi University.
HI in galaxies from z = to z = 0.2 Thijs van der Hulst
Krakow 2010 Galactic magnetic fields: MRI or SN-driven dynamo? Detlef Elstner Oliver Gressel Natali Dziourkevich Alfio Bonanno Günther Rüdiger.
90% of Matter in Milky Way is Dark Matter Gives off no detectable radiation. Evidence is from rotation curve: Rotation Velocity (AU/yr) Solar System Rotation.
THE STRUCTURE OF COLD DARK MATTER HALOS J. Navarro, C. Frenk, S. White 2097 citations to NFW paper to date.
Galaxies. ● When we look at the night sky: – Moon and planets- relatively close ~ AU’s – Stars in the Milky Way and its halo, still close ~ kpc ~ 1000’s.
The Milky Way Center, Shape Globular cluster system
Galaxies How big is the Universe? Types of galaxies Elliptical Spiral
Galaxies Chapter Twenty-Six. Guiding Questions How did astronomers first discover other galaxies? How did astronomers first determine the distances to.
A.Kravtsov (U.Chicago) D. Ceverino (NMSU) O. Valenzuela (U.Washington) G. Rhee (UNLV) F. Governato, T.Quinn, G.Stinson (U.Washington) J.Wadsley (McMaster,
M 51. M 51 Galaxy merger simulation.
Chapter 24 Normal and Active Galaxies. The light we receive tonight from the most distant galaxies was emitted long before Earth existed.
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.
Galaxies Chapter 16. Galaxies Star systems like our Milky Way Contain a few thousand to tens of billions of stars. Large variety of shapes and sizes.
Galaxies Chapter 13:. Galaxies Contain a few thousand to tens of billions of stars, Large variety of shapes and sizes Star systems like our Milky Way.
TURBULENCE AND HEATING OF MOLECULAR CLOUDS IN THE GALACTIC CENTER: Natalie Butterfield (UIowa) Cornelia Lang (UIowa) Betsy Mills (NRAO) Dominic Ludovici.
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.
Compact Groups: kinematics and star formation Claudia Mendes de Oliveira U. Sao Paulo, Brazil Collaborators: P. Amram, C. Balkowski, H. Plana, E. Cypriano,
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.
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,
Components of the Milky Way The light from galaxies is centrally concentrated. But is the mass also centrally concentrated? Does Mass follow Light in Galaxies?
The Milky Way Appears as a band of light stretching across the sky There are dark regions along the band, giving the appearance of a lack of stars This.
Galaxy Morphology The Tuning Fork that Blossomed into a Lemon Lance Simms MASS Talk 9/8/08.
Galaxies Please press “1” to test your transmitter.
Gas Properties of Dwarf Galaxies Gas Properties of Dwarf Galaxies Ayesha Begum (IOA, Cambridge) Faint (M B >-14.5) Irregular Galaxies GMRT Survey Results.
Interaction in the NGC 3079 group Nebiha Shafi University of Witwatersrand and HartRAO Supervisors: Prof. Roy Booth (HartRAO) Dr. Raffaella Morganti Dr.
27-Sept. 2001ATNF Synthesis Workshop Spectral Line Image Analysis and Visualization Bärbel Koribalski (ATNF, CSIRO)
The Nature of Galaxies Chapter 17. Other Galaxies External to Milky Way –established by Edwin Hubble –used Cepheid variables to measure distance M31 (Andromeda.
After decoupling, overdense regions collapse IF Collapse timefor all sizes. More small ripples than large waves. --> Universe dominated by globular clusters.
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.
Masses of Galaxy Groups Brent Tully University of Hawaii.
10A Galaxies Island Universes. 10A Copyright – Adam Block, KPNO.
David R. Law Hubble Fellow, UCLA The Physical Structure of Galaxies at z ~ John McDonald, CFHT Galaxies in the Distant Universe: Ringberg Castle.
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.
Astronomy 1143 – Spring 2014 Lecture 21: The Evidence for Dark Matter.
Big Bang f(HI) ~ 0 f(HI) ~ 1 f(HI) ~ History of Baryons (mostly hydrogen) Redshift Recombination Reionization z = 1000 (0.4Myr) z = 0 (13.6Gyr) z.
Universe Tenth Edition Chapter 23 Galaxies Roger Freedman Robert Geller William Kaufmann III.
Introduction to Galaxies Robert Minchin. What is a galaxy?
Competitive Science with the WHT for Nearby Unresolved Galaxies Reynier Peletier Kapteyn Astronomical Institute Groningen.
Caught in the act Caught in the act - witnessing the transformation of a spiral galaxy Jesper Rasmussen + Trevor Ponman, John Mulchaey.
“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.
GALAXIES & BEYOND. What is a galaxy? A galaxy is a very large group of stars held together by gravity. Size: 100,000 ly+ Contain Billions of stars separated.
Galaxies Star systems like our Milky Way
Kinematics of ionized gas outflows caused by star formation
Galaxy Formation and Evolution: Where we are and where we are going.
The “Milky Way”.
Galaxies.
Galaxies.
Dark matter and anomalous gas in the spiral galaxy NGC 4559
Presentation transcript:

Mapping the HI Neighborhood Around Starburst Dwarf Galaxies Megan Johnson NRAO, Green Bank Tully-Fisher Workshop, April 2012

Outline Introduction NGC 1569 –Review of stellar and gas kinematics from LITTLE THINGS –GBT map NGC 4163/NGC 4214 Future Work Summary April 2, 20122Megan Johnson - TF 35

Introduction Starburst = short-lived intense period of star formation that is unsustainable over the Hubble time due to the limited supply of gas within a galaxy (McQuinn ); generally, interactions/mergers are triggers Dwarf Galaxy = low luminosity, low mass system, contained in a dark matter halo; believed to be the “Building Blocks” of larger galaxies Starburst Dwarf Galaxy = possibly a “Building Block” in action? What is the role of interactions/mergers between dwarf galaxies? April 2, 20123Megan Johnson - TF 35

April 2, 20124Megan Johnson - TF 35 Introduction Can HI environment around starburst dwarf galaxies provide clues to their interaction/merger history?

5 A B NGC 1569 – What is its shape? Member of IC 342 Galaxy Group D = 3.36 Mpc (Grocholski ) M V = SFR = 0.24 M  /yr HI mass = 2.5 x 10 8 M  Stellar mass = 2.8 x 10 8 M  Megan Johnson - TF 35April 2, 2012 Stellar and Gas Kinematics  V max /σ z

April 2, 2012Megan Johnson - TF 356 “HI Companion,” “HI Bridge,” Stil & Israel (1998) and “NCM HI Cloud” – Stil & Israel (2002) - HV3 “Chimney” - Hunter et al. (1993); Mühle et al. (2005); Westmoquette et al. (2008) Previous Work:

Stellar Kinematics April 2, 2012Megan Johnson - TF 357

April 2, 2012Megan Johnson - TF 358 Position-Velocity Diagrams – Stars and Gas

Ionized Gas in NGC 1569 B A April 2, 20129Megan Johnson - TF 35

Stellar Velocity Dispersions April 2, 2012Megan Johnson - TF 3510 = 21 ± 4 km/s SSC B SSC A Constant

April 2, 2012Megan Johnson - TF 3511 Bulk Motion Extraction

V max = 50 ± 10 km/s Bulk Motion Extraction April 2, 2012Megan Johnson - TF 3512 Bulk VF Strong NCM Weak NCM Strong + Weak

April 2, Megan Johnson - TF 35 Rotation Curve of NGC 1569 V max = 50 ± 10 km/s

April 2, Megan Johnson - TF 35 Baryonic TF Relation – Trachternach ★ NGC 1569 Total Baryonic Mass = 6.8 x 10 8 M 

April 2, 2012Megan Johnson - TF 3515 GBT Map around NGC km/s UGCA 92 NGC 1569 Southern HI Extension

GBT Map around NGC km/s Intergalactic Filaments MW Cloud UGCA 92 NGC 1569 April 2, 2012Megan Johnson - TF 3516

NGC 4163 Member of Canes Venatici Cloud D = 2.8 Mpc M V = SFR = 9.1 x M  /yr HI mass = 1.4 x 10 7 M  Stellar mass = 2.7 x 10 7 M  April 2, Megan Johnson - TF 35

NGC 4163 – IWM Velocity Field April 2, Megan Johnson - TF 35

NGC 4214 D = 2.9 Mpc M V = SFR = 0.13 M  /yr HI mass = 5.8 x 10 8 M  Stellar mass = 4.8 x 10 8 M  Member of Canes Venatici Cloud April 2, Megan Johnson - TF 35

NGC 4214 – IWM Velocity Field April 2, Megan Johnson - TF 35

UGCA 7605 UGCA 7559 UGCA 7599 NGC 4244 NGC 4214 NGC 4163 NGC 4190 Integrated HI GBT Map April 2, Megan Johnson - TF 35 RMS = 25 mK, (at 1σ in a 1 km/s channel)

April 2, Megan Johnson - TF 35 What about field dwarfs? Are nearby dwarf irregular galaxies still assembling? GBT proposal to map all LITTLE THINGS dwarfs

April 2, Megan Johnson - TF 35 IC 1613 – Local Group Member

April 2, Megan Johnson - TF 35 DDO 165 – M81 Group Member

April 2, Megan Johnson - TF 35 DDO 46 – No Known Group

Summary NGC 1569 is a thick disk –V max / σ z = 2.4 ± 0.7 –Stars and gas kinematically follow each other –Extended HI emission to south and northeast of NGC 1569 in VLA map stretching in the direction of UGCA 92 and confirmed with GBT NGC 4163/4214 –“Unsettled” HI in VLA maps –Possible extended emission detected in GBT map … stay tuned … LITTLE THINGS - ?? April 2, Megan Johnson - TF 35

April 2, Megan Johnson - TF 35

Ultra-dense HI Cloud (UDHIC) Hα tail – Velocity ~ -90 km/s (Tomita et al. 1994)

Integrated HI Intensity Contour Map April 2, 2012Megan Johnson - TF 3529