ALMA Science Verification Program. Martin Zwaan ALMA Regional Centre ESO, Garching
|
|
|
- Merryl Potter
- 5 years ago
- Views:
Transcription
1 ALMA Science Verification Program Martin Zwaan ALMA Regional Centre ESO, Garching
2 Science Verification The process by which ALMA demonstrates that it is capable of producing data of the required quality So far focused on reproducing results already obtained with other telescopes The reduced and calibrated datasets will be available to the community for download raw data data reduction scripts and CASA guides data products: images, cubes
3 SV data available TW Hya: Band 3, 6, 7, high spectral resolution. Band 7 CASA guide NGC 3256: Band 3, low spectral resolution. Band 3 CASA guide Antennae galaxies: Band 6, 7, high spectral resolution. Band 7 CASA guide M100 Band 3, low spectral resolution. SgrA* Band 6, recombination lines. BR Band 7: low spectral resolution. IRAS16293 Band 6 and 9 : high spectral resolution. Band 9 CASA guide Centaurus A Band 6: high spectral resolution mosaic. Orion KL Band 6: high resolution spectral survey.
4 ALMA Science Verification: NGC 3256 Band 3 observations of the CO(1-0) line in NGC antennas were used, total integration time ~4hours NGC3256 is a very bright infrared galaxy. This is a nice data set to test your data reduction skills. The full calibration and imaging can be done on a regular desktop or laptop computer CO(1-0) map CO(1-0) velocity field
5 ALMA Science Verification: NGC 3256 CN (high) map CN (high) velocity field CN (low) map CN (low) velocity field
6 ALMA Science Verification: TWHya TW Hya: classical T Tauri star Age of 10 Myr, Distance 51 ± 4 pc, Actively accreting Images at various wavelengths reveal an optically thick dust disk Band 7, total time 4.5 hours, 8 antennas Intensity Velocity Field Velocity dispersion CO(3-2) HCO+(4-3)
7 TWHya Band 6 Öberg et al Deuterium fractionation in TWHya: Evidence for multiple pathways to Deuterium enhancements in protoplanetary disks Caution in interpreting range of deuterium fractions observed in solar system bodies
8 ALMA Science Verification: Antennae galaxies Colors: ALMA SV CO (3-2) data Contours: SMA CO (3-2) data (Ueda, Iono, Petitpas et al.)
9 ALMA Science verification: M100 Grand design spiral in Virgo CO(1-0) line (band 3) observed with 13 antennas - 47 pointing mosaic A very good target to test combination of ACA and single dish data with main array BIMA + 12m OTF map from Helfer et al 2002
10 IRAS16293 band 6 and 9 IRAS (d=160) is a well studied nearby proto-binary system Detailed structure and kinematics in the circumbinary envelope for each component Strong emission from complex organic molecules and other species associated with hot cores in massive star-forming regions Observed in Band 6 and 9 Casaguide available for band 9 data reduction Band 9 mosaic
11 A first ALMA look at IRAS Direct detection of infall onto source B & high-resolution kinematics of source A Pineda, Maury, Fuller et al. (arxiv: ) also Jorgensen et al. (sub.) T MB (K) T MB (K) Dec (J2000) a) b) AU CH 3 OCHO-E 17 (4,13) -16 (4,12) at IRAS16293 B Source B Source A CH 3 OCHO-A 17 (4,13) -16 (4,12) at IRAS16293 B 16 h 32 m 23.5 s 23.0 s 22.5 s RA (J2000) Intensity (Jy beam -1 ) Intensity (Jy beam -1 ) IRAS16293 B IRAS16293 A Frequency (GHz) a) c) CH 3 OCHO-E H 17 (4,13) CCO 11 (1,11) -10 (4,12) (1,10) at at IRAS16293 B 8 6 b) CH 3 OCHO-A 17 (4,13) -16 (4,12) at IRAS16293 B 15 c) H 2 CCO 11 (1,11) -10 (1,10) at IRAS16293 B T MB (K) MB (K) T MB (K) 4 2 T MB (K) V lsr -V 0 (km s -1 ) At 80 AU radius: V lsr -V 0 (km s -1 ) V lsr -V 0 (km s -1 ) Supersonic infall velocity: 0.50±0.05km s 1 Infall rate : M yr 1
12 IRAS16293 Band 9 - first Band 9 data! H13CN (J=8-7) moment GHz continuum H13CN (J=8-7) moment 1
13 Centaurus A - band 6
14 Sgr A* - Band 6 Band 3 data will be released soon!
15 galaxies at z = 4.7: BR Pair of gas-rich galaxies at z = 4.7, BR Extreme merger event? Quasar host galaxy, a bright submillimeter galaxy (SMG) and a fainter star-forming galaxy observed at 335 GHz (Band 7) with seventeen 12 m diameter antennas SMA: Iono 2006 outflow? Wagg et al. 2012
16 Science Verification continues Now: demonstrate the full range of Cycle 1 capabilities Large mosaics Mixed correlator modes ACA and zero spacing Also, commissioning and science verification of: Longer baselines Polarization Solar observing On-the-fly mosaics
17 New SV Targets Mars 3,6,7 (CH4, CO) 12m+ACA +SD mixed, 1spw/ BB multi-field calibration to exclude telluric lines comet C/2009 P1 Garradd 3 (CO, HCN) 12m mixed, 1spw/ BB external ephemeris files, transients VV114 9 (CO) 12m+ACA low spectral res SHADES 7 (contin) 12m low spectral res astrometry and multi-field interferometry Fornax Cluster 3 (CO) 12m+ACA low spectral res multi-field and multivelocity interferometry NGC1512/10 3 (CO) 12m+ACA +SD mixed, 1spw/ BB large mosaic Lamdba Orionis 3 (contin) 12m+ACA +SD low spectral res large mosaic, continuum SD CB54 7 (CO(3-2), HCO+(4-3),... 12m mixed, multiple spw/bb large mosaic
18 New SV Targets (continued) HR 3126/IC (CO, CN) 12m+ACA+SD mixed, 1spw/ BB large mosaic Chameleon 6 (CO, SiO) 12m mixed, 1spw/ BB multi-field interferometry, long baselines M83 7 (CO) 12m+ACA mixed, 1spw/ BB On The Fly mosaic RXCJ (contin) 12m+ACA low spectral res M16 6 (CO) 12m+ACA+SD mixed, 1 spw/ BB 12m+ACA+SD mixed, multiple spw/bb 12m mixed, 1spw/ BB G , 325, 658 GHz water masers 9 (H21a, CH3CN, 34SO2, SO2, CH3CN, 13CO) 7,9 (H2O) large mosaic spectral averaging, high angular res, survey mode (non-multi-field)
19
20
Formation, Detection and the Distribution of Complex Organic Molecules with the Atacama Large Millimeter/submillimeter Array (ALMA)
Formation, Detection and the Distribution of Complex Organic Molecules with the Atacama Large Millimeter/submillimeter Array (ALMA) Anthony J. Remijan, ALMA Program Scientist Joint ALMA Observatory National
Setting the stage for solar system formation
Setting the stage for solar system formation ALMA insights into the early years of young stars Jes Jørgensen! Niels Bohr Institute & Centre for Star and Planet Formation University of Copenhagen http://youngstars.nbi.dk
The ALMA SKA Synergy For Star and Stellar Cluster Formation
The ALMA SKA Synergy For Star and Stellar Cluster Formation Gary Fuller Jodrell Bank Centre for Astrophysics & UK ALMA Regional Centre Node University of Manchester What is ALMA? Atacama Large Millimetre/Sub-millimetre
Millimetre Science with the AT
Millimetre Science with the AT Astrochemistry with mm-wave Arrays G.A. Blake, Caltech 29Nov 2001 mm-arrays: Important Features - Spatial Filtering - Transform to image plane - Cross Correlation (Sub)Millimeter
Extragalactic SMA. Sergio Martín Ruiz. European Southern Observatory
Extragalactic SMA Sergio Martín Ruiz European Southern Observatory Submillimeter Array Advisory Committee Meeting Wednesday 13 th, October 2010 NEARBY GALAXIES: CO 2-1 Mapping BODEGA: Below 0 DEgree Galaxies
Challenges for the Study of Hot Cores with ALMA: NGC 6334I
Challenges for the Study of Hot Cores with ALMA: NGC 6334I Crystal Brogan (NRAO/North American ALMA Science Center) Collaborators: Todd Hunter (NRAO) Remy Indebetouw (UVa/NRAO), Ken (Taco) Young (CfA),
Spectroscopy Exploring Shock Chemistry in Star Forming Regions with the EVLA. January 15-17, 2011 Victoria BC Canada
Spectroscopy 2011 January 15-17, 2011 Victoria BC Canada Exploring Shock Chemistry in Star Forming Regions with the EVLA Joseph P. McMullin, Claire Chandler, Steve Myers, Miller Goss, Goran Sandell Atacama
Spatially Resolved Observations of Protoplanetary Disk Chemistry
Spatially Resolved Observations of Protoplanetary Disk Chemistry Karin Öberg University of Virginia Collaborators: Chunhua Qi (CfA), David Wilner (CfA), Sean Andrews (CfA), Ted Bergin (Michigan), Michiel
ALMA as a Scientific Instrument. Robert Laing
ALMA as a Scientific Instrument Outline What is ALMA? ALMA as it will be ALMA Operations Early Science Planning an ALMA observation Current status Atacama Large Millimetre/ Sub-Millimetre Array Aperture
Tricks of Resolution and Dynamics
Tricks of Resolution and Dynamics A disk-like object that isn t: IRAS 23033+5951 Brenda Matthews (HIA/NRC, Canada) Michael Reid (CfA/McMaster) Reid & Matthews, 2007, submitted to ApJ Motivation: Understanding
Astrochemistry In the Era of Broadband single dish and Interferometric observations
Astrochemistry In the Era of Broadband single dish and Interferometric observations Anthony J. Remijan NA ARC Manager 1 2014 ANASAC Meeting National Radio Astronomy Observatory Overview Why imaging? What
Density. Red. Low high. Blue. Cluster galaxy population: passive and red Hogg et al. 2004
Red Density Blue Low high Cluster galaxy population: passive and red Hogg et al. 2004 Normal spiral galaxy Red S0 galaxy Cluster spiral Field spiral Chung et al. 2009 Walter et al. 2008 Yellow contours:
SCIENTIFIC CASES FOR RECEIVERS UNDER DEVELOPMENT (OR UNDER EVALUATION)
SCIENTIFIC CASES FOR RECEIVERS UNDER DEVELOPMENT (OR UNDER EVALUATION) C.STANGHELLINI (INAF-IRA) Part I Infrastructure 1 Main characteristics and status of the Italian radio telescopes 2 Back-ends, opacity
ALMA Science Cases with our Galaxy. SNU Town hall meeting for ALMA Cycle March 23 Woojin Kwon
ALMA Science Cases with our Galaxy SNU Town hall meeting for ALMA Cycle 5 2016 March 23 Woojin Kwon 1201 refereed articles (ADS) with ALMA in abstracts, as of 3/21/2016 618 publications at www.almascience.org
Robert Laing European Instrument Scientist
Kilometre Array Bonn, April 15 2008 Overview What is? Main performance numbers Sensitivity Resolution Spatial scales Spectral-line modes Synergy between and SKA Science Wavelengths, resolutions, surveys
Probing the embedded phase of star formation with JWST spectroscopy
Probing the embedded phase of star formation with JWST spectroscopy NIRSPEC Spitzer NGC 1333 Low mass Herschel Cygnus X High mass Jorgensen et al. Gutermuth et al. 10 10 Motte, Henneman et al. E.F. van
Accretion-Disk-outflow System in High Mass Star Formation. Yuefang Wu Astronomy Department Peking University, China
Accretion-Disk-outflow System in High Mass Star Formation Yuefang Wu Astronomy Department Peking University, China Outline 1. A debate two models of high mass star formation 2. Our related work- observational
Next Generation VLA Memo. 41 Initial Imaging Tests of the Spiral Configuration. C.L. Carilli, A. Erickson March 21, 2018
Next Generation VLA Memo. 41 Initial Imaging Tests of the Spiral Configuration C.L. Carilli, A. Erickson March 21, 2018 Abstract We investigate the imaging performance of the Spiral214 array in the context
Astrochemistry from a Sub-pc Scale to a kpc Scale. Satoshi Yamamoto Department of Physics and RESCUE The University of Tokyo
Astrochemistry from a Sub-pc Scale to a kpc Scale Satoshi Yamamoto Department of Physics and RESCUE The University of Tokyo Contents Physical and Chemical Processes in Disk Formation around Solar-type
Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of ngvla Working Group 2
Next Generation Very Large Array Working Group 2 HI in M74: Walter+ 08 CO in M51: Schinnerer+ 13 Continuum in M82: Marvil & Owen Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of
Black Holes and Active Galactic Nuclei
Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently
From the VLT to ALMA and to the E-ELT
From the VLT to ALMA and to the E-ELT Mission Develop and operate world-class observing facilities for astronomical research Organize collaborations in astronomy Intergovernmental treaty-level organization
NEARBY GALAXIES AND ALMA
NEARBY GALAXIES AND ALMA Jean Turner, UCLA nearby galaxies close-up views of star formation & nuclear fueling on scales of GMCs and star clusters - where & how do galaxies form stars? - where does gas
NRAO Instruments Provide Unique Windows On Star Formation
NRAO Instruments Provide Unique Windows On Star Formation Crystal Brogan North American ALMA Science Center Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank
The Unbearable Lightness of Chemistry
Z H IG C G N I OM H T A P U The Unbearable Lightness of Chemistry The Unbearable Lightness of Chemistry ~ 0.5 % Molecular (H 2 ) ~ 0.002 % CO ~ 0.000002 % any other molecule A total of 46 molecular species
Can we do this science with SKA1-mid?
Can we do this science with SKA1-mid? Let s start with the baseline design SKA1-mid expected to go up to 3.05 GHz Proposed array configuration: 133 dishes in ~1km core, +64 dishes out to 4 km, +57 antennas
Galaxies of Many Colours: Star Formation Across Cosmic Time. z=0, t= /-0.037x10 9 years (Now)
Galaxies of Many Colours: Star Formation Across Cosmic Time z=0, t=13.798+/-0.037x10 9 years (Now) And if you want to study the initial conditions for star formation the colour is black Dense Gas SDC335:
Deep Impact :! Molecular Gas Properties under Strong ICM Pressure
Deep Impact : Molecular Gas Properties under Strong ICM Pressure Bumhyun Lee & Aeree Chung Department of Astronomy, Yonsei University (Korea) The 3rd workshop on Large Aperture Mm/Submm Telescopes in the
Deflection of a Protostellar Outflow: The Bent Story of NGC 1333 IRAS 4A. NGC 1333 Cluster Forming Region. Driving Source. IRAS 4A Protobinary System
Deflection of a Protostellar Outflow: The Bent Story of NGC 1333 IRAS 4A SNU Colloquium 2006. 3. 22. Minho Choi Evolutionary Scenario of Low-Mass Young Stellar Objects Classification Spectral Energy Distribution
Cinthya Herrera (NAOJ)
Cinthya Herrera (NAOJ) ASTE/ALMA Development Workshop 2014, June 18th, 2014 Galaxies interactions... Key in hierarchical model of galaxy formation and evolution (e.g., Kauffmann et al. 1993) Most massive
An Introduction to Radio Astronomy
An Introduction to Radio Astronomy Second edition Bernard F. Burke and Francis Graham-Smith CAMBRIDGE UNIVERSITY PRESS Contents Preface to the second edition page x 1 Introduction 1 1.1 The role of radio
Advanced Topics in Astrophysics, Lecture 5. Radio Astronomy VLBI Science Phil Diamond, University of Manchester
Advanced Topics in Astrophysics, Lecture 5 Radio Astronomy VLBI Science Phil Diamond, University of Manchester Up to 25 antennas 8000 km baselines Frequency range: 327 MHz 43 GHz Disk-based recording:
The HDO/H2O and D2O/HDO ratios in solar-type protostars
The HD/H and D/HD ratios in solar-type protostars Audrey CUTENS University College London M. V. Persson, J. K. Jørgensen, E. F. van Dishoeck, C. Vastel, V. Taquet, S. Bottinelli, E. Caux, D. Harsono, J.
Radio Interferometry and ALMA
Radio Interferometry and ALMA T. L. Wilson ESO 1 PLAN Basics of radio astronomy, especially interferometry ALMA technical details ALMA Science More details in Interferometry Schools such as the one at
Journal Club Presentation on The BIMA Survey of Nearby Galaxies. I. The Radial Distribution of CO Emission in Spiral Galaxies by Regan et al.
Journal Club Presentation on The BIMA Survey of Nearby Galaxies. I. The Radial Distribution of CO Emission in Spiral Galaxies by Regan et al. ApJ, 561:218-237, 2001 Nov 1 1 Fun With Acronyms BIMA Berkely
Galaxy Collisions & the Origin of Starburst Galaxies & Quasars. February 24, 2003 Hayden Planetarium
Galaxy Collisions & the Origin of Starburst Galaxies & Quasars February 24, 2003 Hayden Planetarium Normal massive galaxy types elliptical & spiral galaxies Spiral Bulge of old stars Large black hole Very
Circumstellar disks The MIDI view. Sebastian Wolf Kiel University, Germany
Circumstellar disks The MIDI view Sebastian Wolf Kiel University, Germany MPIA MIDI SG concluding meeting May 5, 2014 Overview Circumstellar disks: Potential of IR long-baseline interferometry MIDI: Exemplary
10x Effective area JVLA, ALMA 10x Resolution w. 50% to few km + 50% to 300km Frequency range: 1 50, GHz
10x Effective area JVLA, ALMA 10x Resolution w. 50% to few km + 50% to 300km Frequency range: 1 50, 70 115 GHz JVLA: Good 3mm site, elev. ~ 2200m Residual phase rms after calibration 90% coherence 550km
Science Prospects with the wsma
Science Prospects with the wsma SMA: the key mm interferometry facility the SMA has genuinely transformed fields, from planet formation to the high-redshift universe 700 publications; 21000 citations (>1
Unbiased line surveys of protostellar envelopes A study of the physics and chemistry of the youngest protostars in Corona Australis
Unbiased line surveys of protostellar envelopes A study of the physics and chemistry of the youngest protostars in Corona Australis Johan E. Lindberg Astrochemistry Laboratory NASA Goddard Space Flight
Protoplanetary disk demographics. Jonathan Williams! Institute for Astronomy, University of Hawaii
Protoplanetary disk demographics Jonathan Williams! Institute for Astronomy, University of Hawaii Characterizing Planetary Systems Across the HR Diagram Cambridge, July 31, 2014 Disk demographics provide
An Introduction to Radio Astronomy
An Introduction to Radio Astronomy Bernard F. Burke Massachusetts Institute of Technology and Francis Graham-Smith Jodrell Bank, University of Manchester CAMBRIDGE UNIVERSITY PRESS Contents Preface Acknowledgements
Feeding and Feedback in nearby AGN:
Feeding and Feedback in nearby AGN: From Cycle 0 to Cycle 2 Viviana Casasola INAF-Istituto di Radioastronomia Italian ALMA Regional Centre (ARC) Terzo Workshop sull Astronomia millimetrica in Italia Bologna,
Recent VLTI results on stellar winds and perspectives with second generation instruments. Xavier Haubois
Recent VLTI results on stellar winds and perspectives with second generation instruments Xavier Haubois Outline - The VLTI and its instruments - Massive stars - HMXBs - AGBs - Planetary Nebulae - Perspectives
The influence of cosmic rays on the chemistry in Sagittarius B2(N)
The influence of cosmic rays on the chemistry in Sagittarius B2(N) Mélisse Bonfand A. Belloche, K. M. Menten, R. Garrod Sagittarius B2 APEX Telescope Large Area Survey of the Galaxy Sgr B2 Sgr B2(N) Galactic
Driving hot and cold gas flows with AGN feedback in galaxy clusters Credit: ESO
Driving hot and cold gas flows with AGN feedback in galaxy clusters Credit: ESO Helen Russell (Cambridge) Brian McNamara (Waterloo), Andy Fabian (Cambridge), Paul Nulsen (CfA), Michael McDonald (MIT),
Galaxies with Active Nuclei. Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes
Galaxies with Active Nuclei Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes Active Galactic Nuclei About 20 25% of galaxies do not fit well into Hubble categories
Compact Obscured Nuclei in the ALMA era
Compact Obscured Nuclei in the ALMA era Francesco Costagliola Chalmers University of Technology- Onsala Space Observatory Istituto de Astrofísica de Andalucía (IAA-CSIC) S.Aalto, S. Muller, K. Sakamoto,
- Strong extinction due to dust
The Galactic Centre - Strong extinction due to dust At optical wavelemgth the absorption is almost total Information from the 21 line, IR and radio 10 Region between and cm 14 10 22 1 arcsec at the distance
Transition Observing and Science
Transition Observing and Science EVLA Advisory Committee Meeting, March 19-20, 2009 Claire Chandler Deputy AD for Science, NM Ops Transition Observing A primary requirement of the EVLA Project is to continue
Black Holes in Hibernation
Black Holes in Hibernation Black Holes in Hibernation Only about 1 in 100 galaxies contains an active nucleus. This however does not mean that most galaxies do no have SMBHs since activity also requires
Outline. Mm-Wave Interferometry. Why do we care about mm/submm? Star-forming galaxies in the early universe. Dust emission in our Galaxy
Outline 2 Mm-Wave Interferometry Debra Shepherd & Claire Chandler Why a special lecture on mm interferometry? Everything about interferometry is more difficult at high frequencies Some problems are unique
ESO Colloquium um (Santiago de Chile) An E-ELT DRM science case: in deeply embedded dense massive protoclusters
ESO Colloquium um (Santiago de Chile) An E-ELT DRM science case: stellar population and stellar dynamics in deeply embedded dense massive protoclusters Hans Zinnecker (AIP and ESO visiting scientist) OR
The Class 0 Source Barnard 1c (most recent results ) Brenda Matthews Herzberg Institute of Astrophysics National Research Council of Canada
The Class 0 Source Barnard 1c (most recent results ) Brenda Matthews Herzberg Institute of Astrophysics National Research Council of Canada Edwin Bergin (University of Michigan) Antonio Crapsi & Michiel
Resolved studies of gas in high-z galaxies
Resolved studies of gas in high-z galaxies Jacqueline Hodge Jansky Fellow (NRAO) With Fabian Walter (MPIA), Chris Carilli (NRAO), Erwin de Blok (ASTRON), Dominik Riechers (Cornell), Emanuele Daddi (CEA)
Some recent work I. Cosmic microwave background, seeds of large scale structure (Planck) Formation and evolution of galaxies (Figure: Simpson et al.
Radio astronomy Radio astronomy studies celestial objects at wavelengths longward of λ 100 µm (frequencies below ν 3 THz) A radio telecope can see cold gas and dust (Wien s displacement law of BB emision,
Water released in a protostellar accretion burst
CENTRE FOR STAR AND PLANET FORMATION Water released in a protostellar accretion burst Per Bjerkeli J. K. Jørgensen, E. A. Bergin, S. Frimann, D. Harsono, S. K. Jacobsen, M. Persson, J. Lindberg, N. Sakai,
Feeding and Feedback in U/LIRGs: ALMA Case Studies
Feeding and Feedback in U/LIRGs: ALMA Case Studies Kazushi Sakamoto 2015-06-01, "Galaxies of many colours" @Marstrand, Sweden Feedback in U/LIRGs: ALMA Studies on NGC 3256 and Arp 220 NGC 3256 Dual molecular
ALMA Development Program
ALMA Development Program Jeff Kern CASA Team Lead Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Opportunities for Software
Unraveling the Envelope and Disk: The ALMA Perspective
Unraveling the Envelope and Disk: The ALMA Perspective Leslie Looney (UIUC) Lee Mundy (UMd), Hsin-Fang Chiang (UIUC), Kostas Tassis (UChicago), Woojin Kwon (UIUC) The Early Disk Disks are probable generic
Lecture 23 Internal Structure of Molecular Clouds
Lecture 23 Internal Structure of Molecular Clouds 1. Location of the Molecular Gas 2. The Atomic Hydrogen Content 3. Formation of Clouds 4. Clouds, Clumps and Cores 5. Observing Molecular Cloud Cores References
Disk+outflow system in G
EAVW 2018 @ PyeongChang Disk+outflow system in G25.82-0.17 Jungha Kim (D2/SOKENDAI/NAOJ) Tomoya Hirota, Kee-Tae Kim, KaVA SWG for star formation CONTENTS Introduction Observations Results - KaVA imaging
arxiv: v1 [astro-ph.ga] 11 Oct 2018
![arxiv: v1 [astro-ph.ga] 11 Oct 2018](/thumbs/93/114367241.jpg "arxiv: v1 [astro-ph.ga] 11 Oct 2018")
**Volume Title** ASP Conference Series, Vol. **Volume Number** **Author** c **Copyright Year** Astronomical Society of the Pacific Imaging Molecular Gas at High Redshift arxiv:1810.05053v1 [astro-ph.ga]
ALMA 2030: The ALMA development vision and road map
ALMA 2030: The ALMA development vision and road map Chris Wilson, McMaster University (with material from presentations by J. Carpenter, P. Cox, M. McKinnon, E. Murphy) Complementary and overlapping science
Transition Disk Chemistry in the Eye of ALMA
COURTESY NASA/JPL-CALTECH Spectroscopy2011 January 16, 2011 Transition Disk Chemistry in the Eye of ALMA Ilse Cleeves Univ. of Michigan ADVISOR: Edwin Bergin Outline I. Transition Disks: Introduction II.
In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes
In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes Stellar velocity fields MW Distant galaxies Gas motions gas disks around nearby black holes
The kinematics of NGC1333-IRAS2A a true Class 0 protostar
Chapter 6 The kinematics of NGC1333-IRASA a true Class protostar Abstract Low-mass star formation is described by gravitational collapse of dense cores of gas and dust. At some point during the collapse,
Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies. Amy Reines Einstein Fellow NRAO Charlottesville
Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies Amy Reines Einstein Fellow NRAO Charlottesville Motivation: The origin of supermassive BH seeds Motivation: The origin of
wsma for Nearby Galaxies
wsma for Nearby Galaxies Kazushi Sakamoto (ASIAA) The overview talks should focus future discussion on what the upgrade will better enable in their particular area of expertise, rather than summarizing
Microwave emissions, critical tools for probing massive star formation
Microwave emissions, critical tools for probing massive star formation Function of NH 3 molecule Yuefang Wu Astronomy Department Peking University Outline 1. Star formation regions and their probing Stars
arxiv: v3 [astro-ph.ga] 20 Mar 2018
![arxiv: v3 [astro-ph.ga] 20 Mar 2018](/thumbs/78/78216905.jpg "arxiv: v3 [astro-ph.ga] 20 Mar 2018")
Dragan SALAK, Yuto TOMIYASU, Naomasa NAKAI, and Yusuke MIYAMOTO d.salak@kwansei.ac.jp Department of Physics, Kwansei Gakuin University, 2-1 Gakuen, Sanda, 669-1337 Hyogo, Japan arxiv:1612.06488v3 [astro-ph.ga]
Wagg ea. [CII] in ALMA SV 20min, 16 ants. 334GHz. SMA 20hrs
![Wagg ea. [CII] in ALMA SV 20min, 16 ants. 334GHz. SMA 20hrs](/thumbs/80/81969639.jpg "Wagg ea. [CII] in ALMA SV 20min, 16 ants. 334GHz. SMA 20hrs")
BRI1202-0725 z=4.7 HyLIRG (10 13 L o ) pair SFR ~ few 10 3 M o yr -1 4 + SMG + Salome ea. CO 5-4 + M H2 ~ 10 11 M o QSO + HST 814 Hu ea 96 SMA [CII] 158um 334GHz, 20hrs Iono ea 2007 [CII] in 1202-0725
Astrochemistry Lecture 7 Chemistry in star-forming regions
Astrochemistry Lecture 7 Chemistry in star-forming regions Ewine F. van Dishoeck Leiden Observatory Spring 2008 Outline Introduction Observational techniques Chemical scenario Cold outer envelopes around
Astronomy 422! Lecture 7: The Milky Way Galaxy III!
Astronomy 422 Lecture 7: The Milky Way Galaxy III Key concepts: The supermassive black hole at the center of the Milky Way Radio and X-ray sources Announcements: Test next Tuesday, February 16 Chapters
Non-axisymmetric structure in million-year-old discs around intermediate-mass stars
Non-axisymmetric structure in million-year-old discs around intermediate-mass stars Misato Fukagawa (NAOJ) C. A. Grady, J. P. Wisniewski, Y. Ohta, M. Momose, Y. Matura, T. Kotani, Y. Okamoto, J. Hashimoto,
RAMPS: The Radio Ammonia Mid-Plane Survey. James Jackson Institute for Astrophysical Research Boston University
RAMPS: The Radio Ammonia Mid-Plane Survey James Jackson Institute for Astrophysical Research Boston University High Frequency Workshop, Green Bank, 21 September 2015 Collaborators (partial list) Taylor
A Supermassive Black Hole in the Dwarf Starburst Galaxy Henize Amy Reines Einstein Fellow National Radio Astronomy Observatory
A Supermassive Black Hole in the Dwarf Starburst Galaxy Henize 2-10 Amy Reines Einstein Fellow National Radio Astronomy Observatory Supermassive black holes and galaxy evolution Supermassive black holes
ESO in the 2020s: Astrobiology
ESO in the 2020s: Astrobiology Izaskun Jimenez-Serra (IIF Marie Curie Fellow, ESO) Leonardo Testi (ESO), Paola Caselli (MPE) & Serena Viti (UCL) 1 From the ISM to the Origin of Life Molecular clouds (Pre-stellar
Stellar Life Cycle in Giant Galactic Nebula NGC edited by David L. Alles Western Washington University
Stellar Life Cycle in Giant Galactic Nebula NGC 3603 edited by David L. Alles Western Washington University e-mail: alles@biol.wwu.edu Introduction NGC 3603 is a giant HII region in the Carina spiral arm
SMA observations of Magnetic fields in Star Forming Regions. Josep Miquel Girart Institut de Ciències de l Espai (CSIC-IEEC)
SMA observations of Magnetic fields in Star Forming Regions Josep Miquel Girart Institut de Ciències de l Espai (CSIC-IEEC) SMA Community Day, July 11, 2011 Simultaneous process of infall and outflow"
Where do Stars Form?
Where do Stars Form? Coldest spots in the galaxy: T ~ 10 K Composition: Mainly molecular hydrogen 1% dust EGGs = Evaporating Gaseous Globules ftp://ftp.hq.nasa.gov/pub/pao/pressrel/1995/95-190.txt Slide
4. Galaxies in the Local Universe
4. Galaxies in the Local Universe 4.1 Introduction The local universe provides a vital link between our Milky Way Galaxy and the early universe. In particular, the study of nearby galaxies provides crucial
Molecular line survey observations toward nearby galaxies with IRAM 30 m
Molecular line survey observations toward nearby galaxies with IRAM 30 m Yuri Nishimura IoA/The University of Tokyo, NAOJ IRAM 30 m: 32 GHz in only two tunings FTS 200 khz resolution: simultaneously observing
MOLECULES IN THE CIRCUMNUCLEAR DISK OF THE GALACTIC CENTER
MOLECULES IN THE CIRCUMNUCLEAR DISK OF THE GALACTIC CENTER Implications from Chemical Modeling Nanase Harada 1, Denise Riquelme 1, Serena Viti 2, Karl Menten 1, Miguel Requena-Torres 1, Rolf Güsten 1,
Nuclear Star Formation, The Torus, & Gas Inflow in Seyfert Galaxies
Nuclear Star Formation, The Torus, & Gas Inflow in Seyfert Galaxies Richard Davies 1, H. Engel 1, M. Schartmann 1, G. Orban de Xivry 1, E. Sani 2, E. Hicks 3, A. Sternberg 4, R. Genzel 1, L. Tacconi 1,
Star Formation. Spitzer Key Contributions to Date
Star Formation Answering Fundamental Questions During the Spitzer Warm Mission Phase Lori Allen CfA John Carpenter, Caltech Lee Hartmann, University of Michigan Michael Liu, University of Hawaii Tom Megeath,
Zooming into high-mass star-forming regions
Zooming into high-mass star-forming regions Henrik Beuther SMA ATCA PdBI VLA Important questions - What are the characteristics of accretion disks/large toroid in high-mass star formation? - Can we constrain
Understanding the tracers of star formation
Understanding the tracers of star formation Kazi Rygl (ESA-ESTEC) Cygnus X region, HOBYS (F. Motte, M. Hennemann)/Herschel/ESA 22 Jan 2015, Bologna Overview Evolutionary phases of star formation Age determinations:
Short-Spacings Correction From the Single-Dish Perspective
Short-Spacings Correction From the Single-Dish Perspective Snezana Stanimirovic & Tam Helfer (UC Berkeley) Breath and depth of combining interferometer and single-dish data A recipe for observing extended
Observational studies of intermediate-mass protostars with PdBI, 30m and Herschel
Observational studies of intermediate-mass protostars with PdBI, 30m and Herschel Asunción Fuente, Roberto Neri, Aina Palau, José Cernicharo and many excellent collaborators Low-mass star formation Pre-stellar
Chapter 17. Active Galaxies and Supermassive Black Holes
Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study
ALMA Science Ex am ples
ALMA Science Ex am ples Min S. Yun (UMass/ ANASAC) ALMA Science Requirements High Fidelity Imaging Precise Imaging at 0.1 Resolution Routine Sub- mjy Continuum Sensitivity Routine mk Spectral Sensitivity
ALMA's Window on Molecular Emission: Small Ions to Complex Prebiotics
ALMA's Window on Molecular Emission: Small Ions to Complex Prebiotics Al Wootten Complex Molecules in Space Boom Time for IS Spectroscopy 1000 year anniversary of SN1006 this week! Correlator technology:
Astronomy across the spectrum: telescopes and where we put them. Martha Haynes Discovering Dusty Galaxies July 7, 2016
Astronomy across the spectrum: telescopes and where we put them Martha Haynes Discovering Dusty Galaxies July 7, 2016 CCAT-prime: next generation telescope CCAT Site on C. Chajnantor Me, at 18,400 feet
The VLA Nascent Disk and Multiplicity (VANDAM) Survey of Perseus
The VLA Nascent Disk and Multiplicity (VANDAM) Survey of Perseus John Tobin NWO Veni Fellow Leiden Observatory Leiden, The Netherlands VANDAM Team: John Tobin (PI), Leslie Looney (Illinois), Zhi-Yun Li
What's in the brew? A study of the molecular environment of methanol masers and UCHII regions
What's in the brew? A study of the molecular environment of methanol masers and UCHII regions Outline of talk Low vs high -mass star formation (SF) The SF menagerie UCHII regions, hot and cold cores, methanol
The high angular resolution component of the SKA
The high angular resolution component of the SKA Tingay, S. 1, Bignall, H. 1, Colegate, T. 1, Aben, G. 2, Nicolls, J. 2 & Weston, S. 3 Prof. Steven Tingay SKA2010 Deputy Director, ICRAR March 22 25, 2010
Stellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
Intense Star Formation in Nearby Merger Galaxies
Intense Star Formation in Nearby Merger Galaxies 13 February 2009 Authors: Kelsey Johnson (University of Virginia), Sara Beck (Tel Aviv University), Aaron Evans (University of Virginia), Miller Goss (NRAO),
CARMA: Specifications & Status
CARMA: Specifications & Status Anthony J. Beasley a & Stuart N. Vogel b a Combined Array for Research in Millimeter-wave Astronomy Caltech Owens Valley Radio Observatory PO Box 968 Big Pine, CA 93513 tbeasley@ovro.caltech.edu