astrometry with ska: case of oh maser sources hiroshi imai graduate school of science and...
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Astrometry with SKA: case of OH maser sources
Hiroshi ImaiGraduate School of Science and
Engineering, Kagoshima UniversityGASKAP collaboration
Workshop on East-Asian Collaboration for
SKA in Daejeon, Korea on 2011
December 2
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ContentsContentsSKA and Australian SKA Pathfinder (ASKAP)
High sensitivity, wide-band, wide-field astrometry Stellar and interstellar OH masers as a probe of
stellar mass loss flows and the Milky Way dynamics Galactic ASKAP Spectral Line Survey (GASKAP)
Survey specification: HI—OH mapping and OH maser survey
Activities in the Survey Study PhaseToward SKA astrometry
Possible future collaboration in the Pacific region Current progress in VERA+KVN/ EAVN
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Aperture (dish)=50 VLAs Baseline SEFD=2.4 Jy (with core-remote station),
enabling to use fainter phase-reference sources
Image dynamic range=106 High angular resolution
θSKA~θVLA/80 (3000 km), 2.4 mas @ 3cm Baseline extension with distant remote stations
High sensitivity astrometry with SKA High sensitivity astrometry with SKA (mid-band)(mid-band)
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Wide-field astrometry with SKA (mid-band)Wide-field astrometry with SKA (mid-band)Permitted phase coherence angle within atmospheric fluctuation for 10-μas level astrometry
(e.g. Asaki et al. 2007)Δθ(target – reference) < 2 deg @22 GHzΔθ(target – reference) < 6 deg @6 GHz
~30,000 reference sources with S8GHz > 1 mJy
Δθ(reference – reference) ~0.7 deg Multi-reference, in-beam astrometry is possible.Wide-angle astrometry is still necessary and possible for estimation/ correction of zenith delay residuals.
ASKAP focal plane phased array FoV=30 deg2 @1.5GHz
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Wide band astrometry with SKA (mid band)Wide band astrometry with SKA (mid band)λ= 3 – 60 cm (0.5-10 GHz) Pulsar astrometry (main target? Tingay’s and
Kameya’s talks) Thermal source astrometry (OB stars, YSOs)
Recombination line and thermal continuum sources Proper motion measurement
Non-thermal sources: annual parallaxes Maser source astrometry (in MHz)
OH: 1612, 1665, 1667, 1720, 4751, 4766, 6031, 6035, 13441 CH3OH: 6669, 12179 H2O: 22235, NH3: 23694, 23723, 23870 (high-band) OH maser survey in GASKAP and OH maser astrometry (this talk) Galactic kinematics of CH3OH maser sources (Matsumoto’s talk) Internal motions and kinematics H2O masers (Chibueze’s talk)
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Why OH maser astrometry?Why OH maser astrometry? Major maser lines in SKA mid-band Targets of wide-field VLBI astrometry Nearby HI 21-cm line Wide variety of populations of OH maser sources
star forming regions (high-mass, intermediate mass YSOs) in the Galactic thin disk
evolved stars (long period variables, OH/infrared stars) in Galactic thick disk, bulge, halo (including globular clusters)
Unique property of 1612 MHz OH maser sources Light curve phase-lag technique for distance
determination sites of present mass release from dying stars in the
Milky Way
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Stellar OH maser sources distributedStellar OH maser sources distributed in the whole Milky Way in the whole Milky Way
Mira variables, OH/IR starspost-AGB stars, supergiants,
http://www.hs.uni-hamburg.de/~st2b102/maserdb
From targeted (VLA/Parkes/ATCA) to unbiased sky survey (ASKAP)
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OH maser distributionOH maser distribution Tracing Galactic rotation and arms (|b|<1 deg)
Credit: Daniel Tafoya
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Rotation curve derived with OH masersRotation curve derived with OH masers Using tangential point method in each longitude bin
R0=8kpcθ0= 200 km/s
Credit: Daniel Tafoya
Stellar OH maser sources= collision-less system transparent toward Galactic plane
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Light curve phase-lag technique for distance determinationLight curve phase-lag technique for distance determination
van Langevelde et al. (1990) Herman & Habing (1985)
W43A OH masers(Imai et al. 2002)
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ASKAPASKAPAustralian Australian
Square Kilometer ArraySquare Kilometer ArrayPathfinderPathfinder
(Norris’s talk)(Norris’s talk) 36 12-m dish antennas Radio Quiet Zone in western
Australia Focal Plane Phased-Array
Antenna (FPA) covering 30 deg2
300 MHz band width, 16384 spectral channels
Operation from 2013
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GASKAP: GASKAP: Galactic ASKAP Spectral Line SurveyGalactic ASKAP Spectral Line Survey One of the Survey Science Programs (SSPs) defined in
ASKAP. A program integrated since the Expression of Interests in
2009. The fastest surveys of HI / OH thermal and OH maser
emission in the Milky Way, Magellanic Clouds, Stream, and Bridge.
Simultaneous mapping of HI (1.4 GHz) and OH (1.6 GHz). ~7,000 hours in total, 0.15—2.40 hr/deg2
Exploration of HI gas circulation between the disk and low latitude halo/MCs.
Galactic dynamics probed by OH maser sources Sites of present stellar mass loss in the Miky Way
star forming regions (1665/1667 MHz) circumstellar envelopes (16120 MHz)
GASKAP logo designed by Josh Peek
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GASKAP international teamGASKAP international teamP.I. John Dickey (Univ. Tasmania)Steering committee
Steven Gibson (Western Kentucky Univ. USA) José F. Gómez (CSIC, Spain) Hiroshi Imai (Kagoshima Univ., Japan) Paul Jones (Univ. New South Wales,
Australia) Naomi McClure-Griffiths (ATNF, Australia) Snězana Stanimirović (Univ. Wisconsin) Jacco van Loon (Keele Univ., United
Kingdom)~80 team members Now working in “Design Study Phase”.
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GASKAP Working Groups in Design Study PhaseGASKAP Working Groups in Design Study Phase
WG1: Simulations Calibration and imaging (de-convolution for diffuse
source) Multiple gridding (30”, 60”, 90”, 180”) Simulated source catalogs of OH masers
WG2: Source finding from image cubes CLUMPFIND, DUCHAMP, Selavy, etc. for a huge
image cube WG3: Survey strategy
Management of field rotation in Phased Array Feed WG4: ASKAP hardware commitment
Correlation in zoom mode, band-pass stability WG5: Data management
Output data format for a virtual observat0ry
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Survey areasSurvey areas Galactic plane (|b|<10°, δ<40°) Magellanic Clouds, Stream, Bridge Galactic bulge, center and lower halo (GASKAP+ ?)
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Approved Approved
possible possible
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What we want to see in HI?What we want to see in HI?
Comparison of HI sky surveys (McClure-Griffiths et al. 2009)
Magellanic leading arm high-velocity cloud interacting with the Galactic plane (McClure-Griffiths et al. 2008)
1 kpc @D=21 kpc
Dynamic atomic hydrogen motions on 0.1—1000 pc scale
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Bubbles, arcs, and loopsBubbles, arcs, and loopsin the whole Milky Wayin the whole Milky Way
“2° UV tail” of Mira (Martin et al. 2007)
Magellanic leading arm high-velocity cloud interacting with the Galactic plane (McClure-Griffiths et al. 2008)
Any gas structure traced by HI emission
“CO gas loops” (Fukui et al. 2006)
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Predicted 1612 MHz OH maser detectionPredicted 1612 MHz OH maser detection
Detecting typical (O-rich) OH/IR stars in MW.
Red supergiants in LMC and SMC.
Slower expansion velocity envelope in LMC/SMC due to lower metalicity?
J. van Loon (from GASKAP proposal)
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More realistic OH maser catalog for More realistic OH maser catalog for GASKAP source finding simulationGASKAP source finding simulation
Based on existing 1612 MHz OH maser catalogs A complete unbiased deepy survey with VLA
towards the Galactic Center (Sjouwerman et al. 1998)
Incomplete catalog towards the whole Galaxy (Engels 2007) … GASKAP can double OH
maser sources.
Candidates for OH maser sources MSX (MIR) sources
(~80% coincidence within 20”) SiO maser sources
(~20% coincidence within 20”)
Simulated OH maser histogram within 3 deg from GC (J.F. Gómez)
Log (Flux density [mJy])
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Simulation of HI map reproductionSimulation of HI map reproduction Input: HI map from previous observations (right) Output: Map reproduction in ASKAP configuration (left)
Good recovery in 180” resolution
ASKAP+Parkes
Credit: P. Jones
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From imaging to source From imaging to source identificationidentification
Input single channel map 90” resolution synthesized image
CLUMPFIND identification clump distribution
Next goal: removing artifactsthrough finding multi-channel correlation (will be tested with VERA data)
Credit: J.F. Gomez
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Technical challenging in GASKAPTechnical challenging in GASKAP Visibility calibration schemes in wide-field imaging.
With/without using calibrators in the same scan field Uniform sensitivity in the whole scan field and frequency
band Real-time processing of calibration
Automatic and reliable visibility calibration through “the pipeline”.
Emission identification in the complicated structures. Including absorption
Outputs in the “virtual observatory”. HI Image cubes …. huge file size! Fitting parameters for OH maser sources.
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Current collaborations in East-Asian VLBI NetworkCurrent collaborations in East-Asian VLBI Networkrelated to SKArelated to SKA
SKA-JP sub-WG on AstrometryY. Asaki (ISAS/JAXA), H. Imai, D. Tafoya (Kagoshima Univ.), K. Ohnishi
(Nagano Nat’l. College of Technology), T. Hirota, Y. Hagiwara, N. Matsumoto (NAOJ/Mizusawa VLBI), Niimura (Yamaguchi Univ.), N. Goda, T. Tsujimoto, T. Yano (NAOJ/JASMINE), Mitsumi Fujishita (Tokai Univ.)
VLBI demonstrations for 6.7 GHz CH3OH maser sources in JVN and SHAO since 2010 Autumn (See Matsumoto’s talk)
Planning KVN+VERA Key Science since 2011 June (star formation, AGN, evolved stars, astrometry sub-WGs)
International team collaboration for development of multi-frequency band, phase-referencing technique (lead by U. Western Australia /ICRAR)
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Possible GASKAP/SKA/EAVN collaborationPossible GASKAP/SKA/EAVN collaborationin maser source astrometryin maser source astrometry