Presentation is loading. Please wait.

Presentation is loading. Please wait.

Observations of SNR G156.2+5.7 at 6cm JianWen Xu, Li Xiao, XiaoHui Sun, Chen Wang, Wolfgang Reich, JinLin Han Partner Group of MPIfR at NAOC.

Published byBethany Doyle Modified over 8 years ago

Similar presentations

Presentation on theme: "Observations of SNR G156.2+5.7 at 6cm JianWen Xu, Li Xiao, XiaoHui Sun, Chen Wang, Wolfgang Reich, JinLin Han Partner Group of MPIfR at NAOC."— Presentation transcript:

1 Observations of SNR G156.2+5.7 at 6cm JianWen Xu, Li Xiao, XiaoHui Sun, Chen Wang, Wolfgang Reich, JinLin Han Partner Group of MPIfR at NAOC

2 System parameters/Calibrators Central frequency: 4.8 GHz Bandwidth: 600 MHz System temperature: 22-25 K HPBW: 9.5 arcmin Aperture efficiency: 62% Beam efficiency: 67% Conversion factor: 0.164 K/Jy r.m.s: 1.5 mK for 1s integration tim Primary Calibrator: 3C138 –Intensity: 3.64 Jy, –Polarization Angle: 169 deg, –Polarization Percent: 11.7%

3 Properties of SNR G156.2+5.7 Identified firstly by the ROSAT observatory in the all- sky survey for X-ray sources Among the 10 brightest X-ray Galactic SNRs The lowest radio surface brightness among all known SNRs Common magnetic field strength & therefore a low electron density

4 Some Parameters of SNR G156.2+5.7 Spectral index  = 0.5  0.15 (Reich et al. 1992) A distance of d  3kpc (Pfeffermann et al. 1991) A diameter of 108’, or  95pc (Pfeffermann et al. 1991) Type I progenitor SN of E 0 = 10 51 erg (Reich et al. 1992) An age of   2.6  10 4 yr (Pfeffermann et al. 1991)

5 r.m.s: 1.0 mK in I Flux density:2.2+/-0.6Jy polarization percentage : Left:<= 40%, Right:<=70% G156.2+5.7 one of the most weak SNRs The red source in the southwest with strongest radio emission is probably an extragalactic one Total intensity (image)

6 r.m.s: 1.0 mK in I Flux density:2.2+/-0.6Jy polarization percentage : Left:<= 40%, Right:<=70% G156.2+5.7 Total intensity (image+contours) one of the most weak SNRs The red source in the southwest with strongest radio emission is probably an extragalactic one

7 r.m.s: 1.0 mK in I Flux density:2.2+/-0.6Jy polarization percentage : Left:<= 40%, Right:<=70% G156.2+5.7 Intensity (image) + B (bars) + Polarization Intensity (contours) one of the most weak SNRs small patchy of polarization in the center ---probably local structure

8 r.m.s: 0.25 K T B in I Flux density:4.2+/-1.0Jy polarization percentage : unavailable G156.2+5.7 Intensity (image+contours) (Reich et al. 1992) one of the most weak SNRs The source in the southwest with strongest radio emission is probably an extragalactic one

9 r.m.s: unavailable Flux density:3.0+/-1.0Jy polarization percentage : Left:<= 75%, Right:<=50% G156.2+5.7 Intensity (image) + B (bars) + Polarization Intensity (contours)(Reich et al. 1992) one of the most weak SNRs small patchy of polarization in the center ---probably local structure

10 r.m.s: 0.5 mK in PI Flux density:2.2+/-0.6Jy Polarization percentage : Left:<= 40%, Right:<=70% G156.2+5.7 Polarization Intensity (contours) one of the most weak SNRs small patchy of polarization in the center ---probably local structure

11 r.m.s: 0.5 mK in PI Flux density:2.2+/-0.6Jy polarization percentage : Left:<= 40%, Right:<=70% G156.2+5.7 Polarization Intensity (contours) + B (bars) one of the most weak SNRs small patchy of polarization in the center ---probably local structure

12 r.m.s: unavailable Flux density:3.0+/-1.0Jy polarization percentage : Left:<= 75%, Right:<=50% G156.2+5.7 Polarization Intensity (contours) + B (bars) (Reich et al. 1992) one of the most weak SNRs small patchy of polarization in the center ---probably local structure

13 r.m.s: 1.0 mK in I, 0.5 mK in PI Flux density:2.2+/-0.6Jy polarization percentage : Left:<= 40%, Right:<=70% G156.2+5.7 Polarization Percentage (contours) one of the most weak SNRs small patchy of polarization in the center ---probably local structure

14 Integrated flux densities --by open circle (derived from our observations) --by filled circle (taken from Reich et al. 1992) G156.2+5.7 Radio spectrum at 4.8 GHz Spectral index  = 0.54  0.06

15 Summary Total flux density is 2.2  0.6 Jy at 4.8GHz Spectral index is  = 0.54  0.06 Surface brightness  = 2.9  10 -22 W m -2 Hz -1 sr -1 a t 4.8GHz

16 Thank You

Download ppt "Observations of SNR G156.2+5.7 at 6cm JianWen Xu, Li Xiao, XiaoHui Sun, Chen Wang, Wolfgang Reich, JinLin Han Partner Group of MPIfR at NAOC."

Similar presentations

A Crash Course in Radio Astronomy and Interferometry: 1. Basic Radio/mm Astronomy James Di Francesco National Research Council of Canada North American.

A Crash Course in Radio Astronomy and Interferometry: 1. Basic Radio/mm Astronomy James Di Francesco National Research Council of Canada North American.
(2) Profile of the Non-Thermal Filaments of SNRs =>High Energy Particle Acceleration =>High Energy Particle Acceleration In all the SNRs & GC Non Thermal.

(2) Profile of the Non-Thermal Filaments of SNRs =>High Energy Particle Acceleration =>High Energy Particle Acceleration In all the SNRs & GC Non Thermal.
Fundamentals of Radio Astronomy Lyle Hoffman, Lafayette College ALFALFA Undergraduate Workshop Arecibo Observatory, 2009 Jan. 12.

Fundamentals of Radio Astronomy Lyle Hoffman, Lafayette College ALFALFA Undergraduate Workshop Arecibo Observatory, 2009 Jan. 12.
OH (1720 MHz) Masers: Tracers of Supernova Remnant / Molecular Cloud Interactions Crystal L. Brogan (NRAO) VLBA 10 th Anniversary Meeting June 8-12, 2003.

OH (1720 MHz) Masers: Tracers of Supernova Remnant / Molecular Cloud Interactions Crystal L. Brogan (NRAO) VLBA 10 th Anniversary Meeting June 8-12, 2003.
S-PASS, a new view of the polarized sky Gianni Bernardi SKA SA On behalf of the S-PASS team CMB2013, Okinawa, June 10-14 th 2013.

S-PASS, a new view of the polarized sky Gianni Bernardi SKA SA On behalf of the S-PASS team CMB2013, Okinawa, June th 2013.
Primary results of polarization survey of large-SNRs at 6cm Li Xiao, XiaoHui Sun, Chen Wang, WeiBin Shi, Wolfgang Reich, JinLin Han Partner Group of MPIfR.

Primary results of polarization survey of large-SNRs at 6cm Li Xiao, XiaoHui Sun, Chen Wang, WeiBin Shi, Wolfgang Reich, JinLin Han Partner Group of MPIfR.
The Sino-German 6cm polarization survey of the Galactic plane Total intensity Polarized intensity Xiaohui Sun NAOC.

The Sino-German 6cm polarization survey of the Galactic plane Total intensity Polarized intensity Xiaohui Sun NAOC.
On the nature of the Long-duration radio transients Eran Ofek CALTECH Collaborators: B. Breslauer, A. Gal-Yam, D. Frail, S.R. Kulkarni, P. Chandra, M.

On the nature of the Long-duration radio transients Eran Ofek CALTECH Collaborators: B. Breslauer, A. Gal-Yam, D. Frail, S.R. Kulkarni, P. Chandra, M.
BDT Radio – 1b – CMV 2009/09/04 Basic Detection Techniques 1b (2009/09/04): Single pixel feeds Theory: Brightness function Beam properties Sensitivity,

BDT Radio – 1b – CMV 2009/09/04 Basic Detection Techniques 1b (2009/09/04): Single pixel feeds Theory: Brightness function Beam properties Sensitivity,
A young pulsar with a long radio trail emerging from SNR G315.9-0.0 F. Camilo, C.-Y. NG et al. arxiv :0908.2421v1.

A young pulsar with a long radio trail emerging from SNR G F. Camilo, C.-Y. NG et al. arxiv : v1.
The Evolution of Extragalactic Radio Sources Greg Taylor (UNM), Steve Allen (KIPAC), Andy Fabian (IoA), Jeremy Sanders (IoA), Robert Dunn (IoA), Gianfranco.

The Evolution of Extragalactic Radio Sources Greg Taylor (UNM), Steve Allen (KIPAC), Andy Fabian (IoA), Jeremy Sanders (IoA), Robert Dunn (IoA), Gianfranco.
Facts about SNe and their remnants Evolution of an SNR sensitively depends on its environment. Observed SNRs are typically produced by SNe in relative.

Facts about SNe and their remnants Evolution of an SNR sensitively depends on its environment. Observed SNRs are typically produced by SNe in relative.
SLAC, 7 October 2004 1 Multifrequency Strategies for the Identification of Gamma-Ray Sources Marcus Ziegler Santa Cruz Institute for Particle Physics Gamma-ray.

SLAC, 7 October Multifrequency Strategies for the Identification of Gamma-Ray Sources Marcus Ziegler Santa Cruz Institute for Particle Physics Gamma-ray.
A Primer on SZ Surveys Gil Holder Institute for Advanced Study.

A Primer on SZ Surveys Gil Holder Institute for Advanced Study.
Galactic Magnetic Field Research with LOFAR Wolfgang Reich Max-Planck-Institut für Radioastronomie Bonn, Germany.

Galactic Magnetic Field Research with LOFAR Wolfgang Reich Max-Planck-Institut für Radioastronomie Bonn, Germany.
Radio Emission from Masuda Sources New Jersey Institute of Technology Sung-Hong Park.

Radio Emission from Masuda Sources New Jersey Institute of Technology Sung-Hong Park.
Panorama of the Universe: Daily all-sky surveys with the SKA John D. Bunton, CSIRO TIP, Ronald D. Ekers, CSIRO ATNF and Elaine M. Sadler, University of.

Panorama of the Universe: Daily all-sky surveys with the SKA John D. Bunton, CSIRO TIP, Ronald D. Ekers, CSIRO ATNF and Elaine M. Sadler, University of.
An X-ray Study of the Bright Supernova Remnant G296.1-0.5 with XMM-Newton SNRs and PWNe in the Chandra Era Boston, MA – July 8 th, 2009 Daniel Castro,

An X-ray Study of the Bright Supernova Remnant G with XMM-Newton SNRs and PWNe in the Chandra Era Boston, MA – July 8 th, 2009 Daniel Castro,
Low frequency sky surveys with the Murchison Widefield Array (MWA) Gianni Bernardi Harvard-Smithsonian Center for Astrophysics SKA SA project/MeerKAT observatory.

Low frequency sky surveys with the Murchison Widefield Array (MWA) Gianni Bernardi Harvard-Smithsonian Center for Astrophysics SKA SA project/MeerKAT observatory.
Star Formation Research Now & With ALMA Debra Shepherd National Radio Astronomy Observatory ALMA Specifications: Today’s (sub)millimeter interferometers.

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

Similar presentations

Ads by Google