Super CO survey with NANTEN2

Hiroaki Yamamoto (Nagoya U.)on behalf of “NASCO” projects

CMB workshop in Tokyo 2011/2/17

Contents

• CMB• Goal of study• Why are CO observations needed ? • Foreground sources of CMB obs.• NANTEN GPS ver.1 (NGPS)• Comparison of PLANCK results with NGPS• NASCO Projects

Research Group• Y. Fukui 　 Leader ・ Global Analysis including NASCO 　• T. Okuda 　 Development of NASCO receiver system, Observations• T. T. Takeuchi 　 Modeling of foreground radiation, Development of component separation by statistical methods • K. Ichiki 　 Theoretical study in terms of cosmology• S. Inutsuka 　 Research for magnetic field and turbulence in ISM by MHD. • H. Maesawa 　 Support of receiver developments

• Collaborators （ PLANCK members in IAS France)– J.-L. Puget: PI of HFI in Planck– F. Boulanger: PI of ERC Advanced Research Grants– J.-P. Bernard: Partner of Boulanger

|Cosmic Microwave BackgroundWMAP; Subtracted map of foreground sources

Main Results ・ Age ~ 13.7 billion years・ Composition : baryon ~ 4%, dark matter ~ 23%, dark energy ~ 73%・ Corresponding to an inflation scenario with the results ・ Non detection of B mode polarization due to poor sensitivity

Freq. (dF) [GHz]23 (5.5),33 (7.0),41 (8.3),61 (14.0),94 (20.5)

Goal of StudyDetection of B mode polarization in CMBGiving Strong Constraint from observations to proposed inflation models.

Some foreground sources are higher fractional polarization than expected for the CMB signalsProblem is poor knowledge about the amplitude and scale of the polarization of foreground emissionImportant thing is understanding nature of the foreground sources

B mode polarization is so weak that it has been never detected so far.

Planck can identify large angular scale B mode amplitude.

Why are CO observations needed ? Key component to subtract at microwave　・ Synchrotron　・ Free-free emission　・ Dust radiation

WMAP: Maximum Frequency ~ 104GHz Contribution of CO is not included

PLANCK:

Gold et al. 2011, ApJS, 192,15

In case of WMAP

CO(J=1-0) 109,110,115 GHzCO(J=2-1) 219,220,230 GHzCO(J=3-2) 329,330,345 GHzStrongest line emission in MCs.Contaminated in observed bands.

Component maps by Maximum Entropy Method (MEM) analysis

LFI HFICF 30 44 70 100 143 217 353 545 857

SF 27 39.6 63 83.5 119.

4181.2

294.8

455.1

715.6

EF 33 48.4 77 116.

5166.5

252.8

411.2

634.9

998.4

Galactic center

VLSR (km/s)

12CO(J=1-0) 200MHz

One year all sky survey by Planck

Planck all-sky foreground maps

The Galactic Cold Core Population

the density of cold cores in the Milky Way through its three highest frequency channels.

Planck Early Results: The Galactic Cold Core Population Revealed by the First All-Sky SurveyAde et al. (2011)

Cold clumps vs CO cloudsPlanck Early Results: The Galactic Cold Core Population Revealed by the First All-Sky SurveyAde et al. (2011)

CO: Dame et al. (2001)7.5’ – 30’ grid at HPBW of 8.8’

Resolution of CO survey by Dame et al. is not enoughto compare with Planck data. New CO data is …

NANTEN 　 12CO(J=1-0) Integrated Intensity map

NANTEN GPS ver.1 (NGPS)

600 km s-1

HFI 100GHz vs NGPS

Planck results with NGPS 30GHz 353GHz 857GHz

Composite image of above 3 images NANTEN 12CO (J=1-0)

Orion

NANTEN 12CO (J=1-0)

Composite image of 557GHz, 857GHzand IRAS 100 um

Planck results with NGPS

Ophiuchus to Aquila

NAnten Super CO survey (NASCO)

SurveyName

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<|10| 2.6 4-8 ±300 1.0 ~0.35 1.1

NASCO 70% of sky 2.6 1 ±1300 0.16 ~0.2 20

• New Survey with OTF by NANTEN2 at Atacama (Alt. 4865m) in 12CO and 13CO(J=1-0) simultaneously.• Survey beyond NGPS• Covering 70% area of whole sky

Expected resultsNASCO: Large Scale mapping in CO never done before• Covering 70% of whole sky• Enabling us comparative study with PLANCK• Implementation of an estimation of CMB B mode component by

progressing the study of foreground sources

Breakthrough for ISM study etc.• Comparative study with sub-mm, infrared (Herschel, AKARI) to

gamma-ray (Fermi etc.) in large scale• Spreading effect as historical common property in Astronomy

NAnten Super CO survey (NASCO)

• Collaboration with Planck satellite– 1991 ： start collaboration with IAS in France (Fukui)– 2007 ： Launch WG7 group (Planck consortium) and conclude a

MoU with the WG7 group on the use of NGPS in order to estimate foreground components.

– 2010 ： Proposal of NASCO

• Development of NASCO test receiver

– 2010/4 ： Start to develop– 2011/1 ： Installing in NANTEN2 and checking system NASCO test receiver system

NAnten Super CO survey (NASCO)Current status

○ Carrying out Super large scale mapping in CO (NASCO)○ Total Analysis

Estimation of density and velocity structures in ISM using NASCO and HI datasetEstablish of 3D magnetic field model in the Milky Way from polarization from PLANCKCMB dataset ： Planck, BICEP, EBEX, SPIDER etc.ISM dataset ： NASCO, PILOT, BLAST, EoR, CGPS, SGPS, GASS

• 2011 ：– Observation by a test receiver, Development of NASCO receivers– Comparative study / modeling of the ISM by using NGPS and PLANCK

• 2012-2015 ：– Observations by NASCO receivers– Establishing Higher accurate ISM model– Estimation of CMB B mode polarization, constraint to inflation models

Schedule 2011-2015

NAnten Super CO survey (NASCO)

Summary

• PLANCK dataset includes CO components as well as synchrotron, free-free emission and dust radiation in microwave.

• It is important to remove the contribution of CO gas and related foreground sources to detect weak CMB B mode polarization

• NASCO Project is now on going to compare the Planck data with MCs.