Coordinated High |b| Drift Survey Basics: Combination of 12 s/beam and 60 s/beam surveys High latitude sky (wait for low latitude for commensal) 100 MHz.

Slides:



Advertisements
Similar presentations
Future Directions and Initiatives in the Use of Remote Sensing for Water Quality.
Advertisements

Arecibo 40th Anniversary Workshop--R. L. Brown The Arecibo Astrometric/Timing Array Robert L. Brown.
Jeroen Stil Department of Physics & Astronomy University of Calgary Stacking of Radio Surveys.
Beta Testing: The Contractor’s Perspective Trns·port User Group Meeting October 2005.
Managing Data from Avian Radar Systems Edwin Herricks, PhD Siddhartha Majumdar.
Deep Neutral Hydrogen Surveys with the Arecibo 305-m Telescope – the Arecibo Galaxy Environment Survey Robert Minchin NAIC Arecibo Observatory.
Extragalactic ALFA Survey Plans Arecibo Legacy Fast ALFA (ALFALFA) Team leader: Giovanelli (Cornell) Arecibo Galaxy Environments Survey (AGES) Team leader:
HI from z ~ 0 – 1 with FAST D.J. Pisano West Virginia University NRAO.
RFI in the alpha band pass Murray Lewis N A T I O N A L A S T R O N O M Y A N D I O N O S P H E R E C E N T E R Senior Research Associate Radio Astronomy.
SKAMP - the Molonglo SKA Demonstrator M.J. Kesteven CSIRO ATNF, T. J. Adams, D. Campbell-Wilson, A.J. Green E.M. Sadler University of Sydney, J.D. Bunton,
Calibration of the SDSS Spectroscopic Line Width Scaling Relations Calibration of the SDSS Spectroscopic Line Width Scaling Relations Barbara Catinella.
A Web service for Distributed Covariance Computation on Astronomy Catalogs Presented by Haimonti Dutta CMSC 691D.
Using ALFA for ALFALFA Martha Haynes, Cornell University 2005 ALFALFA Undergraduate Workshop.
Computer Security: Principles and Practice
Business Intelligence Dr. Mahdi Esmaeili 1. Technical Infrastructure Evaluation Hardware Network Middleware Database Management Systems Tools and Standards.
Dec 2010 AAVP Cambridge workshop AAVP AAVS1/2-low demonstrators Jan Geralt Bij de Vaate.
Release & Deployment ITIL Version 3
SE-02 CONFIGURATION MANAGEMENT Today we talk about Software Configuration Management (SCM for short): - What? - Why? - How?
Commissioning the NOAO Data Management System Howard H. Lanning, Rob Seaman, Chris Smith (National Optical Astronomy Observatory, Data Products Program)
Tower SystemsJanuary AMS Short Course on Instrumentation 1 Installation and Use of Meteorological Tower Systems Melanie A. Wetzel Desert Research.
Common PDR Problems ACES Presentation T. Gregory Guzik March 6, 2003.
EVLA Early Science: Shared Risk Observing EVLA Advisory Committee Meeting, March 19-20, 2009 Claire Chandler Deputy AD for Science, NM Ops.
Bill Reach 2009 May 14 Greater IPAC Technology Symposium.
Science with the Virtual Observatory Brian R. Kent NRAO.
Software for Deep Survey How useful are tools developed for HIPASS for ALFA surveys? HIPASS members in DEEP working group Software not specific to DEEP.
Which dipoles to use to optimize survey speed? –What tapering? –Trade-off between sensitivity, FOV and low side-lobe levels –Station beam stability, pointing.
EOVSA Data and Database System Gordon Hurford and Jim McTiernan EOVSA Prototype Readiness Review 24-Sept-2012.
Georgia Institute of Technology CS 4320 Fall 2003.
Correlator Growth Path EVLA Advisory Committee Meeting, March 19-20, 2009 Michael P. Rupen Project Scientist for WIDAR.
Software Engineering 2003 Jyrki Nummenmaa 1 CONFIGURATION MANAGEMENT Today we talk about Software Configuration Management (SCM for short): -
PDS Geosciences Node Page 1 Archiving Mars Mission Data Sets with the Planetary Data System Report to MEPAG Edward A. Guinness Dept. of Earth and Planetary.
PACS NHSC Data Processing Workshop – Pasadena 10 th - 14 th Sep 2012 SPIRE AOTs, Products and Quick Look Tools Bernhard Schulz NHSC/IPAC on behalf of the.
The Arecibo Legacy Fast ALFA Drift Survey (ALFALFA/VAVA) and E-ALFA Data Processing Overview Overview Riccardo Giovanelli GALFA/Aug 2004.
EVLA Software Bryan Butler. 2007May22EVLA SAGE Meeting2 Requirements and Goals of EVLA Software Maximize scientific throughput of the instrument At a.
Swift HUG April Swift data archive Lorella Angelini HEASARC.
NAIC’s 2009 Program Plan & Budget Presentation December 2008 Radio Astronomy & Future Plans (Continued) Chris Salter (NAIC, Arecibo Observatory)
GALFA Software Group GALFA-HI –Narrow-band spectral line data cubes of HI emission GALFA-RRL –Narrow-bad spectral line data cubes of recombination lines.
Software Phase V Testing and Improvements to Test Procedures S. Corder and L.-A. Nyman April 18, 20131ICT Planning Meeting, Santiago.
Pulsar surveys at Arecibo and Green Bank David Champion Gravity Wave Meeting, Marsfield, Dec 2007.
2007Sep06 EAC Butler - Software Overview 1 Software Overview Bryan Butler.
Murchison Widefield Array (MWA) : Design and Status Divya Oberoi, Lenoid Benkevitch MIT Haystack Observatory doberoi, On behalf.
1 KFPA Critical Design Review – Fri., Jan. 30, 2009 KFPA Data Pipeline Bob Garwood- NRAO-CV.
Observing Strategies at cm wavelengths Making good decisions Jessica Chapman Synthesis Workshop May 2003.
Data Archives: Migration and Maintenance Douglas J. Mink Telescope Data Center Smithsonian Astrophysical Observatory NSF
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.
ALFA Ultra-Deep Survey Team: Elias Brinks, Noah Brosch, Barbara Catinella, Christopher Conselice, Jonathan Davies, Erwin de Blok, Virginia Kilborn, Suzanne.
A real-time software backend for the GMRT : towards hybrid backends CASPER meeting Capetown 30th September 2009 Collaborators : Jayanta Roy (NCRA) Yashwant.
A Sample IHY 2007 Instrumentation Proposal J. Kasper, B. Thompson, N. Fox.
Plan of the Talk What is AGES The AGES volume High density environments –Groups and clusters Low density environments –Galaxy pairs, isolated galaxies.
GALFA Test Observations & Plans (A1943)  Testing GALFA Spectrometer  Mapping modes: Basketweave scanning (JOSH’s TALK) & drift/driven mapping.  Observing.
GBT Future Instrumentation Workshop Fixing the frequency coverage hole in C-Band Jagadheep D. Pandian Cornell University.
ALFA Installation & Status Steve Torchinsky GALFA Meet3, Arecibo August 29, 2004.
First Exploration of MWA Deep Field Point Source Population C. Williams - PhD Thesis J. Hewitt – reporting some analysis.
E-ALFA Medium-Deep Survey Jessica L. Rosenberg. Can we design a medium-deep survey that will allow us to explore new parameter space for galaxy detection.
1 SUZAKU HUG 12-13April, 2006 Suzaku archive Lorella Angelini/HEASARC.
Frazer OwenNSF EVLA Mid-Project Review May 11-12, Transition to EVLA
1 1 CORNISH WORKSHOP Leeds, 13 th April 2007 James Green The Methanol Multibeam Project Project MMB.
Achieving a Quantum Leap in Observation Density Bill Petrachenko, NRCan.
THE ALMA ORION BAND 6 SCIENCE VERIFICATION DATA SPECTRAL LINE SURVEY - CONTENT AND DISCOVERY AVAILABLE FOR ALL SCIENCE Anthony J. Remijan ALMA Program.
Computer Security: Principles and Practice First Edition by William Stallings and Lawrie Brown Lecture slides by Lawrie Brown Chapter 17 – IT Security.
GLAST LAT ProjectNovember 18, 2004 I&T Two Tower IRR 1 GLAST Large Area Telescope: Integration and Test Two Tower Integration Readiness Review SVAC Elliott.
Early Continuum Science with ASKAP
Computing Architecture
Proposal for LAT Year 1 Data Release Plan
2006 ALFALFA Undergraduate Workshop
EVLA Advisory Committee Meeting
Gustaaf van Moorsel September 9, 2003
Formic Acid or 18OH Absorption?
Correlator Growth Path
Presentation transcript:

Coordinated High |b| Drift Survey Basics: Combination of 12 s/beam and 60 s/beam surveys High latitude sky (wait for low latitude for commensal) 100 MHz adequate (WAPPs ok) Limited-azimuth drift scan technique (simplest) Lays groundwork for deeper surveys Involves 30+ astronomers with wide range of interests Precursor proposal A1946 highly ranked (“A”) Early science potential: M33 region NGC 784 group of dwarfs Leo I group region Swath across heart of Virgo, perpendicular to Supergalactic plane (Possible) blind HI absorption Surprises

Anti-Virgo Direction

Virgo Direction

Coordinated High |b| Drift Survey Science objectives What science goals will the proposed survey address? How will the proposed survey improve on previous surveys? What science goals will the proposed survey NOT address? What are our "early science" goals (2 year timeframe)? Possible PhD theses?

Science goals, follow-up Strategy/planning of Arecibo follow-up observations Detection verification New discoveries...? Deeper sampling of selected regions? Coordination with small ALFA projects How will this work? What is our position? Should we make suggestion to NAIC on guidelines? Coordination/verification of complementarity; How can we insure that small datasets can be incorporated into our larger one to increase solid angle coverage? Coordination of complementary observations Definition of objectives Existing datasets (SDSS, GALEX, etc) what do we need? who? Acquisition of new datasets: what do we need? who? Non-Arecibo observations of new discoveries

Instrument/Backends ALFA characteristics System specifications: updates System performance at AO: reality sets in… Is AO staff performing all calibration/testing we need? System optimization for our needs? How do we communicate with NAIC on this? What WAPP configuration should be adopted and what are the tradeoffs in terms of spectral resolution, bit sampling, bandwidth? Is 100 MHz required? Why or why not? (The digitizers see 100 MHz anyway.) Is 50 MHz enough? Why or why not? There is rfi below 1375 MHz (airport radars and Puntas Salinas hopping radar). Is 5.5 km/s resolution enough? Why or why not? Should we conduct entire survey with WAPPS or move to new spectrometer when it's ready? (We don't need to answer this yet) What are NAIC plans for the 2nd generation spectrometer? Availability date?

Drift scan technique/tiling the sky We propose to conduct drift scans at very limited azimuth orientations of "tiles" 20 min in RA by 4 deg in Dec. Is this the right approach? Should the fall VAVA' strip be shifted east by one tile; two tiles? Best configuration: rotate arm or rotate array? The +18d strip will be conducted at a different orientation than the other strips. How do we verify/validate that this differences introduces no biases/systematics? Precursor/share-risk observations A 1946 Will be scheduled in Jul-Aug Any modifications to strategy? Who will observe (on site)? Data processing? Assessment of results?

Observing who, when, where Observing issues Scheduling: Who decides on schedule on short timescales (<~1-2 days)? Observing logs: Who keeps records daily? Access? Observing: On-site? Remote? Absentee? Backup plan (in case of net failure)? What are our expectations of how this will work and what the responsibilities are? Certainly at the beginning, someone will have to be on site. It may be that later on, observing can be done remotely. But someone does need to take the responsibility to keep track. Data quality verification: Standards? Timescale? Who? How ?

Bandpass/continuum calibration Bandpass calibration Regular observation of selected continuum sources? Firing the cal? How often? How long? NAIC needs to provide software for this; it almost worked in Jan 04 In-scan cross calibration with NVSS? Bandpass/standing wave removal best technique: 1-d or 2-d? galactic HI/low velocities software development for this task? Continuum sources Continuum catalog Continuum subtraction Transient detection? Coordination with others? Absorption lines?

RFI identification/excision RFI expectations and effects What RFI can we expect in the 50 or 100 MHz bands? FAA radars plus hopping Puntas Salinas radar. They will be there; unless we want to use the radar blanker (slows things too much?) we have to live with them. What are its characteristics? Limitations on science goals or not? RFI-related techniques Beam-to-beam correlation Sub-beam sampling (time domain) Cross-polarization Excision techniques: options, algorithm development? When should they be applied?

Software issues Gridding best algorithms weighting schemes platform? what options to allow, what to save, etc? Signal detection algorithms Algorithm development: Fourier domain? Peak flux? Other? Platform? Verification? HI catalog: parameter extraction, astrometry Data reduction process Distributed ("assembly line") or shared process ("pipeline")? Coordination/management? Verification/validation? General software issues Platform: IDL? Data format: SDFITS? What standard? Algorithm development responsibility?

Data products/EPO Public data products Objectives Data product definition Data product development responsibility Data access; release schedule Data product standards/validation Delivery mechanism Education and public outreach Development of display for AOVEF: what, who? Display materials for our own use (PPT slides, etc): what, who? Development of course-related materials (undergrad, grad): what, who?

Resources/Management Manpower needs Task list and manpower requirements Expectations for commitment at different levels Task assignment Reporting/tracking Hardware needs Disk storage location Data transfer modes/medium Data access policies Raw compute power needs and resources? Locations? Project management Resource identification/management Communications Documentation development/maintenance Conflict resolution: what if problems (such as non-delivery of promised task) arise?

Software Issues: Steve Torchinsky NAIC responsibilities and plans Karen O’Neil Platforms and options Wolfram Freudling Software plans for UltraDeep Precursor Riccardo Giovanelli Software plans for Drift Precursor Brian Kent Possible VO portal Martha Haynes Software Issues from the Whitepaper

Questions for NAIC Does NAIC intend to deliver all the Level I data products as proposed in the E-ALFA whitepaper? If not, what items will/will not NAIC provide? What platform will form the basis of NAIC-provided monitoring and quick-look software? How much archiving capability will NAIC provide? Where will data be archived? What protocol? How will access be granted? Will NAIC provide access tools?