Latest results on Anomalous Galactic Microwave Emission from the Cosmosomas Experiment

2. Latest results on Anomalous Galactic Microwave Emission from the Cosmosomas Experiment José Alberto Rubiño Martín (IAC-Tenerife) Orsay, October 27th, 2006 BPOL Workshop

3. Overview • The COSMOSOMAS experiment • Anomalous Microwave Emission in the Galaxy. • Detection in Perseus molecular cloud. • Diffuse emission at high galactic latitudes. • Conclusions

4. The Cosmosomas Experiment (Aimed to measure COSMOlogical Structures On Medium Angular Scales) IAC team: Carlos Gutiérrez Sergi Hildebrandt Roger Hoyland Rafael Rebolo (P.I.) J. Alberto Rubiño-Martín Bob Watson Former collaborators: Silvia Fernández Cerezo Juan Macías Pérez Julio Gallegos Consists of two circular scanning instruments (COSMO11 and COSMO15) operating at four different frequencies in the range 10-17 GHz. (http://www.iac.es/project/cmb/cosmosomas/)

5. COSMOSOMAS receivers layout COSMO11 (one channel @ 10.8 GHz) COSMO15 (3 channels @ 13, 15, 17 GHz)

6. COSMO15 at Teide Observatory. Instrumental setup, showing the 2.5 m flat primary mirror, the 2.4 m parabolic, and the HEMT-based receiver cooled at 20 K.

7. COSMOSOMAS window function

8. COSMOSOMASFirst 18 months of data About 100 useful maps stacked at each frequency. 25% of the whole sky observed 100,000 observed data points (0.3º x 0.3º pixelization) Achieved sensitivity at high Galactic latitude: ~ 40,50, 60, and 115 K/beam at 11, 13, 15 and 17 GHz, respectively. Fernández-Cerezo et al. 2006, MNRAS. (Hildebrandt et al. in prep. with COSMO11)

9. COSMO15: 13GHz band Beam FWHM= 54’ x 66’ Pixelization 20’ x 20’ 25% of the whole sky

10. COSMO15: 15GHz band Beam FWHM= 49’ x 60’ Pixelization 20’ x 20’ 25% of the whole sky

11. COSMO15: 17GHz band Beam FWHM= 46’ x 51’ Pixelization 20’ x 20’ 25% of the whole sky

12. WMAP 23 GHz FILTERED COSMOSOMAS: comparison with WMAP at the galactic plane crossing 13 GHz 15 GHz 17 GHz

13. Perseus Molecular Cloud (Watson et al. 2005)

14. G159.6-18.5 : The Dust Ring • G159.6-18.5 is an IRAS source in Perseus molecular cloud (d=260 pc). • HII region driven by O9.5-B0 V star, found to be in the center of the ring. • Knots appearing around the ring in the IRAS 100 μm map • Knots are bright at 12 μm (suggest transiently heated small dust grains); • Anderson et al. (2000) conclude that the ring is a ruptured blister HII region. IRAS 100 μm

15. Watson, Rebolo, Rubiño-Martín et al. 2005, ApJ 624 L89 G159.6-18.5 There is not enough information to make a detailed model of emission, but the signal can be fitted by a combination of two models of Drained & Lazarian (1998): 0.8WNM (to account for the dense region facing the star) plus 0.3MC (to account for dust warmer further in the cloud) Cleanest detection of anomalous emission

16. VSA-SE Observations in Perseus. Anomalous Emission seen at 33GHz Preliminary results of VSA-SE observations in the Perseus region.

17. Other regions with anomalous spectrum • Recent tentative detections: • Finkbeiner et al. (2002) finds an excess signal from the diffuse HII region LHP201.663+1.643. • Cassanus et al (2004). Excess flux at 31GHz from the Helix planetary nebula. • Finkbeiner, Langston & Minter (2004) using Green Bank GPA (-4o>b>4o) found significant dust correlated emission. • Cassanus et al (2005). Excess at 31GHz from the dark cloud LDN1622

18. Polarization observations of anomalous microwave emission at 11 GHz in the Perseus molecular complex Battistelli, Rebolo, Rubiño-Martín et al. 2006 ApJL. Q: difference between the radiation intensity collected by COSMOSOMAS in the 0º plane (North-South) and the 90º one. Q= - 0.2 ±1.0 % (95% c.l.) U : difference between the orientation –45º and +45º. U=-3.4±2% (95% c.l.) Overall polarization parameter =3.4 ± 2%. The maps are calibrated to the nearby California Nebula (free-free dominated) which is assumed unpolarized (systematic error of less than 1%).

19. Polarization of rotational electric dipole radiation Lazarian and Draine 2000 ApJ Are the molecules aligned and their emission polarized? The energy level splitting arising from grain rotation ensures maximum efficiency of paramagnetic dissipation : time dependent magnetization,energy dissipation and torque causing the molecule to rotate with the axis parallel to the magnetic field COSMOSOMAS

20. Emission at high galactic latitudes with Cosmosomas. Fernández-Cerezo, Gutiérrez, Rebolo, Rubiño-Martín et al. 2006, MNRAS (astro-ph/0601203)

21. Cross correlation method • xCMB : contribution of the fluctuating component of the CMB; • xgal : brightness fluctuations of the Galactic template map.α converts units of the Galactic template into antenna temperature; • ygal : represents any residual Galactic contribution which is uncorrelated with xgal Covariance matrix is sum of covariances of CMB and noise:

22. Cross correlation method (II) Minimizing we obtain The contribution of the galactic template map (xgal) to the observed sky map is given by (so this scaled quantity is in the units of the observed sky map).

23. Templates • WMAP maps (23, 33, 41, 61 & 91 GHz) • DIRBE 100 m, 140 m and 240 m. • Haslam (408 MHz) and Reich & Reich (1420MHz). • Hα maps • Radiosource catalogues (NVSS, GB6) are used to also correlated positions. All maps are degraded to COSMOSOMAS resolution and convolved with the scanning strategy of the instrument

24. Masks • We adopt the Kp0 mask from WMAP team to account for galactic emission and point sources (0.6 deg). • We extend the mask to a radius of 0.9 deg around point sources to account for larger beam size. Mask extended around three most intense sources (3C345, 4C39.25, DA406)

25. Cross-correlation of COSMOSOMAS and WMAP

26. Implied CMB fluctuations in antenna temperature in the combined COSMOSOMAS map TCMB = 29.7± 0.7K (V band) TCMB = 30.0± 0.7K (W band) b > 40° Consistent with the expected level of CMB fluctuations using the best-fit power spectrum to the WMAP data (30K )

27. Correlations with DIRBE 100 m • Correlated signal can not be explained as synchrotron because of the spectral dependence and the amplitude (much larger than the diffuse correlated signal with the Haslam 408 MHz map). • Correlated signal can not be explained as free-free in terms of the Hα correlations. ______COSMOSOMAS______ __________WMAP_________ 13 GHz 15 GHz 17 GHz 23 GHz 33 GHz 41 GHz b>30 deg 7.4  1.1 7.5  1.1 6.5  2.3 2.9  0.2 0.5  0.2 0.0  0.1 b>40 deg 3.7  1.4 5.3  1.4 1.8  2.8 3.7  0.2 2.4  0.2 1.4  0.2

28. Correlations with DIRBE 100 m (|b|>20º) (Banday et al. 2003)

29. Correlations with DIRBE 100 m (|b|>30o)

30. CONCLUSIONS (I) • The anomalous microwave emission is the dominant continuum emission process at 10-40 GHz in the Perseus molecular complex. Becomes comparable with thermal dust at 70-80GHz. • The polarization level of this anomalous emission is less than 5% at 11 GHz. Our best estimate is 3.42 % which would argue in favour of rotational electric dipole radiation of fast spinning small molecules. • But this is the only existing measurement of the polarization of the anomalous emission! Measurements at higher frequencies are requiered.

31. CONCLUSIONS (II) • The DIRBE-correlated signal may turn out to be the dominant Galactic foreground seen by COSMOSOMAS at 1 degree scale and 15 GHz. • It decreases significantly as we go to higher Galactic latitudes and higher frequencies. But there is signal detected up to |b| >40. • The largest correlations are found with the 100 m map. There are significant detections (>2 ) at 140 and 240 m. • The DIRBE-correlated signal is also detected in all the frequencies of WMAP: is about 4% to the total temperature fluctuations in Q band, and progressively less as we increase the frequency. • We find a remarkable agreement with predictions of intensity from spinning dust models. • Measurements of polarized dust-correlated emission needed!

32. Future work • COSMO10 has obtained a map of similar sensitivity to those of COSMO15, and new results will be published soon (Hildebrandt et al. in prep.) • COSMO15 is being re-adapted to be a polarization-sensitive experiment (using a rotating HWP to modulate polarization). First testing of the experiment expected in the next few months.