Astrochemistry with the Upgraded Combined Array for Research in Millimeter-wave Astronomy D. N. Friedel Department of Astronomy University of Illinois.

Slides:

Advertisements

Similar presentations

1 National Radio Astronomy Observatory The EVLA -- Status, Future Rick Perley National Radio Astronomy Observatory.

Advertisements

Arecibo 40th Anniversary Workshop--R. L. Brown The Arecibo Astrometric/Timing Array Robert L. Brown.

ALMA Cycle 2 Capability Jongsoo Kim ALMA EA Korea node.

Dale E. Gary Professor, Physics, Center for Solar-Terrestrial Research New Jersey Institute of Technology 1 9/25/2012Prototype Review Meeting.

Baseband Processing and SKA Simulations using Supercomputers: Enhancing Australia‘s radio astronomy facilities and its bid for the SKA Steven Tingay Swinburne.

Atacama Large Millimeter/ submillimeter Array - ALMA Charge 2 Al Wootten JAO Interim Project Scientist.

CARMA in the ALMA era CARMA is well-suited for mapping large fields, extended objects; unique capabilities at 30 GHz testbed for new instrumentation and.

The Future of the Past Harvard University Astronomy 218 Concluding Lecture, May 4, 2000.

Front end design Front end like SEQUOIA, except that both signal polarizations combined with ortho-mode transition. Entire signal band down-converted.

Project status and specifications Douglas Bock Project Manager 1.

Current mm interferometers Sébastien Muller Nordic ARC Onsala Space Observatory Sweden Turku Summer School – June 2009.

Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array EVLA Observations of.

Star Formation Research Now & With ALMA Debra Shepherd National Radio Astronomy Observatory ALMA Specifications: Today’s (sub)millimeter interferometers.

ALMA During Early Science

J.M. Wrobel - 25 June 2002 PROPOSALS 1 PROPOSAL WRITING TUTORIAL Outline 30 minutes: Lecture on Generic Issues 60 minutes: Small Groups Write Proposals.

C. ChandlerEVLA Advisory Committee Meeting September 6-7, Scientific Commissioning Plan Claire Chandler.

Multiwavelength Continuum Survey of Protostellar Disks in Ophiuchus Left: Submillimeter Array (SMA) aperture synthesis images of 870 μm (350 GHz) continuum.

Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Observing the Pluto.

EVLA Early Science: Shared Risk Observing EVLA Advisory Committee Meeting, March 19-20, 2009 Claire Chandler Deputy AD for Science, NM Ops.

Wideband Imaging and Measurements ASTRONOMY AND SPACE SCIENCE Jamie Stevens | ATCA Senior Systems Scientist / ATCA Lead Scientist 2 October 2014.

Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array The ALMA Observing.

Combined Array for Research in Millimeter-Wave Astronomy Astronomy with CARMA Raising our Sites.

Cycle-3 Capabilities and the OT Andy Biggs ALMA Regional Centre, ESO.

Molecular Gas and Dust in SMGs in COSMOS Left panel is the COSMOS field with overlays of single-dish mm surveys. Right panel is a 0.3 sq degree map at.

Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array The Expanded Very Large.

Polarization at IRAM Status and Plans S.Guilloteau Laboratoire d’Astrophysique de Bordeaux.

8/12/201514th RHESSI Workshop 1 Dale E. Gary, Center for Solar-Terrestrial Research, Physics Department, NJIT.

The Expanded Very Large Array: Phase I Science and Technical Requirements Rick Perley NRAO - Socorro.

Making MOPRA go! Lucyna Kedziora-Chudczer Friend of the telescope (UNSW)

Designing Experiments T. Venturi Istituto di Radioastronomia, Bologna, INAF ERIS, Manchester, 9 September 2005.

Glen Langston: OSU 08 1 Improved Tools for Astrochemistry Glen Langston Methods for detection of families of molecules Example: HC 7 N collaboration with.

Correlator Growth Path EVLA Advisory Committee Meeting, March 19-20, 2009 Michael P. Rupen Project Scientist for WIDAR.

C. ChandlerEVLA Advisory Committee Meeting September 6-7, Transition Operations Claire Chandler.

JVLA capabilities to be offered for semester 2013A Claire Chandler.

K band History Science workshop determined efficiency improvements necessary for K Band: weather, observing requests, mapping programs. Only enough funds.

1 ANASAC Meeting – May 20, 2015 P. Jewell, J. Hibbard, C. Lonsdale Cycle 1 & 2 Status & Cycle 3 results.

1 mm Polarization Science with CARMA Chat Hull UC Berkeley, Radio Astronomy Laboratory Collaborators: Dick Plambeck, Greg Engargiola, & all the CARMA staff.

Moscow presentation, Sept, 2007 L. Kogan National Radio Astronomy Observatory, Socorro, NM, USA EVLA, ALMA –the most important NRAO projects.

URSI January 5, 2009 Science at the ARO with ALMA-Style Frontends Lucy M. Ziurys R.W. Freund And the Staff of ARO.

1wnb Synthesis Imaging Workshop ALMA The Atacama Large Millimeter Array.

Basic Concepts An interferometer measures coherence in the electric field between pairs of points (baselines). Direction to source Because of the geometric.

The North American ALMA Science Center North America’s ALMA Regional Center The North American ALMA Science Center acts as the gateway to ALMA for North.

ALMA Science WorkshopMay 14, 2004 Present and Future Thomas W. Folkers Arizona Radio Observatory.

Molecular Clouds in in the LMC at High Resolution: The Importance of Short ALMA Baselines T. Wong 1,2,4, J. B. Whiteoak 1, M. Hunt 2, J. Ott 1, Y.-N. Chin.

Water Vapor In The Atmosphere: An Examination For CARMA Phase Correction Y.-S. Shiao, L. W. Looney and L. E. Snyder Department of Astronomy University.

Observing Modes from a Software viewpoint Robert Lucas and Philippe Salomé (SSR)

Observing Strategies at cm wavelengths Making good decisions Jessica Chapman Synthesis Workshop May 2003.

Large Area Surveys - I Large area surveys can answer fundamental questions about the distribution of gas in galaxy clusters, how gas cycles in and out.

A Modular K-Band Focal Plane Array for the Green Bank Telescope Matt Morgan National Radio Astronomy Observatory 9/28/2007.

Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array The ALMA Observing.

THE CHEMICAL INVENTORY OF INTERSTELLAR CLOUDS J. M. Hollis (NASA/GSFC), Anthony Remijan (NRAO), P.R. Jewell (NRAO), and F. J. Lovas (NIST) Propose GBT.

1 mm Polarization Science with CARMA

The Allen Telescope Array Douglas Bock Radio Astronomy Laboratory University of California, Berkeley Socorro, August 23, 2001.

A real-time software backend for the GMRT : towards hybrid backends CASPER meeting Capetown 30th September 2009 Collaborators : Jayanta Roy (NCRA) Yashwant.

K-Band Focal Plane Array Project Engineering Overview Matt Morgan National Radio Astronomy Observatory 2/27/2008.

Interferometry at Millimeter and Submillimeter Wavelengths Interacademiaal College 1 maart 2006 Interferometry at Millimeter and Submillimeter Wavelengths.

Transition Observing and Science EVLA Advisory Committee Meeting, March 19-20, 2009 Claire Chandler Deputy AD for Science, NM Ops.

Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array The Very Long Baseline.

NRAO VLA Archive Survey

EVLA Availability - or - When Can I Use It?

EVLA Project Peter Napier

Oxford Algorithms Workshop

Atacama Large Millimeter Array

Observational Astronomy

Observational Astronomy

Shared Risk Observing Claire Chandler EVLA SSS Review, June 5, 2009

Shared Risk Science with the EVLA

Correlator Growth Path

EVLA Advisory Panel Mtg. System Overview

KFPA CDR R. Norrod Feb 27, 2008.

Presentation transcript:

Astrochemistry with the Upgraded Combined Array for Research in Millimeter-wave Astronomy D. N. Friedel Department of Astronomy University of Illinois

CARMA has been operating for several years 3mm and 1mm continuum and spectral line multipoint mosaics Present highlights of upgrades to the array (current and near future) Upgrades to: Antennas Receivers Correlator System

Antennas Incorporation of 8 x 3.5m antennas 23 total antennas – 6 x 10 m, 9 x 6.1 m, 8 x 3.5 m Observations at 1 cm, 3 mm, & 1 mm 253 baselines give large instantaneous u-v coverage Array configurations give resolutions of: 11” - 3mm 5” - 1mm 1cm Paired Antenna Calibration System (PACS) uses 3.5 m antennas as “buddy” for larger antennas

New block downconverters – double the IF bandwidth 8 Ghz IF (each sideband) Large frequency coverage in 1 track Dual 1 mm Circular polarization receivers Increased sensitivity (by √2) Allow observations of polarized continuum and spectral lines Receivers

Correlator New boards giving a total of 8 bands (16 windows) Bandwidths and resolutions: Any combination of bandwidths and LO frequencies (within IF) is possible Some projects are observing 90+ transitions from 16 molecular species at one time Minimizes calibration uncertainties between transitions

System Dual Science Subarrays Allows for 2 simultaneously operating subarrays 1 for spectral line or continuum, 1 for continuum only Antennas can be switched between subarrays via software Online passband calibration Automated data reduction pipeline All data from CARMA will be reduced by an automated system Applies all calibration and creates images

Upgrades and additions to the antennas are mostly complete Correlator is fully upgraded Receiver upgrades are to be complete by the end of the year System upgrades nearly complete The many upgrades to CARMA will allow more and varied science to be accomplished Next proposal call will be in September 2010 Summary