NANTEN2: the low Frequency Receivers and the CO Survey

Transcription

1 NANTEN2: the low Frequency Receivers and the CO Survey Hidetoshi SANO Nagoya Univ., PhD student The 2012 Nanten2 Work UNSW

2 Contents What is NANTEN2 project? Recent status of NANETN2 ScienJfic Results 230GHz New project NASCO ScienJfic Results 100GHz History of NASCO & Future Plans

3 What is NANTEN2 project? etc. Current observing frequencies la Bola

4 Interna'onal Universi'es collabora'ons Nagoya University Osaka Prefecture University Universität zu Köln Universität Bonn Universidad de Chile Seoul National University The University of New South Wales The University of Sydney Macquarie University Swiss Federal Institute of Technology Zurich

5 From the planet measurements, Current surface accuracy is EsJmated to σ ~ 15 microns. Simon et al. 2007

6 Site Infrastructures sky with good transmission at sub- mm membrane containers; rest room, experimental room, observing room, ware house etc. generator house Telescope with an astronomical dome keeping a good surface accuracy in dayjme keeping a good poinjng accuracy in strong wind condijon

7 NANTEN2(2011/07/11)

8 NANTEN2(2011/07/11)

9 NANTEN2(2011/07/11)

10 NANTEN2(2011/07/11)

11 NANTEN2(2011/07/11)

12 Receivers NANTEN2 Instrumentation 115 or 230 GHz: 1 pixel, DSB DSB (8 beam for 460GHz, 8 beam for 800GHz) Spectrometers DFS 1GHz band, 61kHz resolution for 115 or 230GHz AOS for SMART 1 GHz width and 500kHz resolution for All pixel in future, change to DFT.

13 Receivers NANTEN2 Instrumentation 115 or 230 GHz: 1 pixel, DSB DSB (8 beam for 460GHz, 8 beam for 800GHz) Spectrometers DFS 1GHz band, 61kHz resolution for 115 or 230GHz AOS for SMART 1 GHz width and 500kHz resolution for All pixel in future, change to DFT.

14 Sub-ref Nagoya RX Main dish Tertiary mirror SMART Fourth mirror Fifth mirror with wire grid Nagoya Sixth mirror Cabin Cold load SMART 230GHz receiver SMART

15 Receivers NANTEN2 Instrumentation 115 or 230 GHz: 1 pixel, DSB DSB (8 beam for 460GHz, 8 beam for 800GHz) Spectrometers DFS 1GHz band, 61kHz resolution for 115 or 230GHz AOS for SMART 1 GHz width and 500kHz resolution for All pixel in future, change to DFT.

16 Receivers NANTEN2 Instrumentation 115 or 230 GHz: 1 pixel, DSB - Jan DSB (8 beam for 460GHz, 8 beam for 800GHz) Spectrometers DFS 1GHz band, 61kHz resolution for 115 or 230GHz AOS for SMART 1 GHz width and 500kHz resolution for All pixel in future, change to DFT.

17 GalacJc Center (230GHz) HPBW=90, OTF, Grid=30 12 CO(J=2-1) Enokiya et al in prep.

18 W44(230GHz) Color Images: 12CO(J=1-0) I.I. (Vlsr: km/s) White contours: (lek) Fermi GeV γ- rays, (right) ATCA&Parkes 1.4 GHz ConJnuum Yoshiike et al in prep.

19 Replace 230GHz system to 115GHz one (Jan ) 230 GHz system * 1 DSB receiver * 4-8 GHz IF * only 1 line, 12 CO(J=2-1) or 13 CO(J=2-1) * 1 DFS for 1 line. Vc 1300 km/s, Vr 0.08 km/s 115 GHz system (Currently test receiver) * 1 DSB receiver * 4-12 GHz IF * 12 CO(J=1-0) and 13 CO(J=1-0) simultaneously * 2 DFSs for 12 CO and 13 CO. Vc 2600 km/s, Vr 0.16 km/s Goal: 4beam 2SB receivers with 2 polarizajon 100GHz test Nagoya Univ.

20 NAnten Super CO survey as Legacy (NASCO) New Survey by NANTEN2 in 12 CO and 13 CO(J=1-0) simultaneously. Survey beyond NGPS Covering 70% area of whole sky CollaboraJve study with Planck team!! Obs. area Unobservable from NANTEN2 Image: Planck 1 year result, Black shade: MCs by NGPS Survey Name Coverage (deg) HPBW ( ) Grid ( ) Vel cov. (km/s) Vel reso. (km/s) RMS[K]@ 1km/s reso. Total points (million) NGPS 200<l<60, b < ± ~ NASCO 70% of sky ± ~0.2 20

21 Goal of NASCO NASCO will provide the most comprehensive and detailed dataset of the morphology and velocity distribujon of the dense ISM within the Galaxy. The foreground GalacJc polarizajon can be derived from dust and ISM MHD models developed by Planck team. The resuljng GalacJc polarizajon model will be compared with the Planck polarizajon data. This process will produce the most accurate descripjon of the polarized CMB emission, and will reveal the morphological structure of the B- mode polarizajon. Detec'on of CMB B- mode polariza'on provide strong constraint from observa'ons to proposed infla'on models. Fig. SchemaJc image of the anisotropy in the CMB. ExtracJng the B- mode polarizajon induced by the primordial gravitajonal waves requires a precise separajon of complicajng processes.

22 About ObservaJon Tareas: GUI of NANTEN2 operajon sys. ( tareas is Spanish for duty ) We can observe remotely from Nagoya Univ. Tareas console (connected by VNC) X- Scan 1deg Y- Scan 1deg = 60 grid RMS Calculate procedure Standard of NASCO observing parameter - Observing footprint: 1 deg 1deg - On- the- Fly mode (X and Y- scan) - IntegraJon Jme: 0.6 s/grid - Observing Time: 1.5 h / 1 scan

23 Observing Target in 2011 Season GalacJc Plane Survey MBM High LaJtude Molecular Clouds Extra Galaxy Survey SNR IC443 Musca Dark Lane etc Observed Area in 2011 season SNR IC443 GalacJc Plane Survey Musca Dark Lane

24 GalacJc Center 100GHz L= MBM53-55

25 Musca Dark Lane Mizuno et al. 2001

26 <Planck Commander Map> Planck LFI and HFI freq. maps (30 to 353 GHz) were used. <Planck LinSys 100GHz Map> Planck HFI freq. maps (100 to 353 GHz) smoothed to a com- mon 10arcmin resolujon. Credit: "ASTROPHYSICS FROM THE RADIO TO THE SUB- MILLIMETRE PLANCK AND OTHER EXPERIMENTS IN TEMPERATURE AND POLARIZATION"

27 Musca Dark Lane NANTEN2 12CO + 13CO vs Planck Lynsis 100GHz CorrelaJon Plot between NANTEN2 and Planck data. NANTEN2 12CO + 13CO vs Planck Commander Map Credit: "ASTROPHYSICS FROM THE RADIO TO THE SUB- MILLIMETRE PLANCK AND OTHER EXPERIMENTS IN TEMPERATURE AND POLARIZATION"

28 History of NASCO & Future Plans Start of NASCO Project NASCO test receiver installed Test observajons of 12 CO(J=1-0) CO, 13 CO simultaneous recepjon system installed CO, 13 CO simultaneously observajons Future Plans 2012 DSB with 2 polarizajon receiver install beam 2SB with 2 polarizajon construcjon Now designing. This Year Update from Jme to Jme (ex, GUNN osc.- >VDI Lo chain) To conjnue NASCO observajon with 100GHz receiver

29 115GHz MulJ beam receiver MulJ beam OpJcal System Now designing 6.8 LHCP OMT RHCP Model of Pyramid mirror Design by quasi- opjcs and GRASP

30