1 / 19

Latest report about e-VLBI

Latest report about e-VLBI. Masachika Kijima The Graduate University for Advanced Studies Ph-D student, 2 nd grade. 2007/10/20 Kawaguchi-seminar. Report about e-VLBI. X-ray binary. Other(North-hemisphere) array cannot observe at 8GHz & 22GHz. Ib/c supernova. Post-RSG. Gravitational lens.

liesel
Download Presentation

Latest report about e-VLBI

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Latest report about e-VLBI Masachika Kijima The Graduate University for Advanced Studies Ph-D student, 2nd grade 2007/10/20 Kawaguchi-seminar

  2. Report about e-VLBI X-ray binary • Other(North-hemisphere) array cannot observe at 8GHz & 22GHz Ib/c supernova Post-RSG Gravitational lens

  3. Garrett (2004, eEVN) • Gravitational lens • First real-time eEVN image

  4. Richards et al.(2005, eEVN) • eEVN, OH maser

  5. Paragi et al. (2005, eEVN) • 1.6GHz • eEVN(1024Mbps) +Cambridge(112Mbps) +Arecibo(100Mbps) • Disk base?

  6. Rushton et al. (2007,eEVN) • GRS1915+105(X-ray binary) • 5GHz • +X-ray, 15GHz data • Extended component (PA=140deg) • Large-scale jet which is simillar Fender et al.(1999)

  7. Epoch I Tudose et al. (2007, eEVN) Epoch II • Cyg X-3 • 5GHz (2pol,Phase-ref) • +X-ray, 15GHz • Polarized flux • Jet or Core? • C isn’t Core! • One-sided jet in the sequence C,B,A

  8. Paragi et al. (2007, eEVN) • May be in prepare. (“The Astronomer’s telegram” in 18 Sep 2007) • 4.97GHz, 2pol, 256-128Mbps(4IF*8MHz*2pol),Phase-ref • rms noise = 0.075[mJy]

  9. Phillips et al. (2007,PAMHELA) • Cir X-1(X-ray binary) • 1.6&8.4GHz • rms nois 0.2mJy/beam • Size:λ2.2variation • Scattering model • Flux variation • Be buried error of Tsys • Jet like structure (Fender et al(1998,2004)) • Resolve-out

  10. Progress of eEVN reports PAMHELA X-ray binary eEVN Ib/c supernova Post-RSG Gravitational lens • Recently, report are written by EVN-data only?

  11. Resolution & Sensitivity • OCTAVE is comparable with eEVN PAMHELA eEVN

  12. U07140A • rms noise 5.600mJy/beam :Image ≠0.093mJy :Expect(3740sec) • Using new SEFD(M.Kijima) • Amplitude calibration isn’t enough Peak:0.49[mJy] 0.2[mJy] 0.1[mJy] M.Murgia et al. (2003, 8.1GHz VLBA)

  13. Difference of SEFD between OCTAVE and JVN? JVN SEFD(Doi) • NRAO 512 • Point source for OCTAVE New SEFD(M.Kijima) 1.7[mJy]

  14. Efficiency of TSUKUBA • Efficiency is about 50-60%. Not reliable

  15. If eEVN reached 1024Mbps(256MHz) • OCTAVE will be comparable to eEVN. • fortunately eEVN can’t observe at 8GHz

  16. Data-rate & Band • OCTAVE reached 2Gbps PAMHELA eEVN

  17. Summary • Frequency • OCTAVE has succeeded 8GHz(image) & 22GHz(fringe) • Other array can’t observe at 8GHz(no plan)&22GHz(plan) • Resolution & Sensitivity • Comparable with eEVN(256Mbps) • Polarimetry • Give up yet ?

  18. Future work • Amplitude calibration • Is there difference of DPFU between OCTAVE and JVN? We need statistical analysis. • Improvement of Tsys & 1st amplifier of VERA at 8GHz? • VERA is useful at 22GHz • Try imaging at 22GHz. • Boost-up(blend visibility, cf DIR2K&OCTAVE) • Phase referencing

  19. ~Fin~

More Related