Weibin Shi, Xiaohui Sun, Wolfgang Reich Jinlin Han, Patricia Reich, Richard Wielebinski

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Weibin Shi, Xiaohui Sun, Wolfgang Reich nlin Han, Patricia Reich, Richard Wielebins Partner Group of MPIfR at NAOC imary results for 6cm polarizat Survey of the Galactic Plane

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Primary results for 6cm polarization Survey of the Galactic Plane. Weibin Shi, Xiaohui Sun, Wolfgang Reich Jinlin Han, Patricia Reich, Richard Wielebinski Partner Group of MPIfR at NAOC. Outlines. Motivation Observation Status Observation Strategy Data Reduction Initial results. - PowerPoint PPT Presentation

Transcript of Weibin Shi, Xiaohui Sun, Wolfgang Reich Jinlin Han, Patricia Reich, Richard Wielebinski

Weibin Shi, Xiaohui Sun, Wolfgang Reich Jinlin Han, Patricia Reich, Richard Wielebinski

Partner Group of MPIfR at NAOC

Primary results for 6cm polarization Survey of the Galactic Plane

Outlines●Motivation●Observation Status ●Observation Strategy●Data Reduction●Initial results

Motivation: Go to higher frequency ( previously 11cm, 21cm )

little affected by foreground Faraday depolarization

The same HPBW with Effelsberg 21 cm data

Survey products and scientific contribution: Absolute calibrated TP & PI maps of the Galactic plane:

construct foreground template for CMB polarizationunderstand magnetic field structure of our Galaxydisentangle ISM structure of the Galaxy combined

other database

D=25mLongitude: 87d 10’ 40.44”E Latitude: 43d 28’ 16.14”N Altitude: 2029 m

Need to observe : longitude about 10deg to 240deg, latitude -5deg to 5deg, about 2300 square degree.

Observation Status

Good part 46.1deg: 95.9deg to 142deg,Have reduced 33.1deg: 95.9deg to 129deg,No reduction 13deg: 129deg to 142deg.

B direction: every part is 2deg x 10deg (3h25m) or 2.2deg x 10deg (3h45m)

L direction: The width: 2.6deg The length: consider Galactic structure

Observation Strategy

Map Observation

Receive telescope position once every secondscan velocity 2' / sscan spacing 3' integration time 1.5sone night can observe two regions

Data Reduction● Set baselines● Correct parallactic angles● Edit spikes, jumps and scanning

effects● Calibration● Weave● Combination● Absolute Calibration

HII Regions

Supernova Remnants

G106.3+2.7

G109.1-1.0 CTB109

G111.7-2.1 Cas A

G114.3+0.3G116.5+1.1

G116.9+0.2 CTB1

G120.1+1.4

G126.2+1.6

G127.1+0.5 R5

Intensity(image)+B(bars)

Intensity(image)+E(bars)

Polarization Intensity(image) +Intensity(contour)

Polarization Intensity(image) )+B(bars)

Next we will do

•more observation•more reduction•compare 6cm, 11cm, 21cm to obtain Spectral index•confirm sources (Supernova Remnants, HII regions)• Get flux intensity•try to find some new sources•Analyze absolute calibrated TP & PI maps

construct foreground template for CMB polarizationunderstand magnetic field structure of our Galaxydisentangle ISM structure of the Galaxy combined other database

Thank you !