DETECTION OF ANOMALOUS MICROWAVE EMISSION IN THE PLEIADES REFLECTION NEBULA WITH WILKINSON MICROWAVE ANISOTROPY PROBE AND THE COSMOSOMAS EXPERIMENT

We present evidence for anomalous microwave emission (AME) in the Pleiades reflection nebula, using data from the seven-year release of the Wilkinson Microwave Anisotropy Probe and from the COSMOSOMAS (Cosmological Structures on Medium Angular Scales) experiment. The flux integrated in a 1° radius around R.A. = 56°.24, decl. = 23°.78 (J2000) is 2.15 ± 0.12 Jy at 22.8 GHz, where AME is dominant. COSMOSOMAS data show no significant emission, but allow one to set upper limits of 0.94 and 1.58 Jy (99.7% confidence level), respectively, at 10.9 and 14.7 GHz, which are crucial to pin down the AME spectrum at these frequencies, and to discard any other emission mechanisms which could have an important contribution to the signal detected at 22.8 GHz. We estimate the expected level of free-free emission from an extinction-corrected Hα template, while the thermal dust emission is characterized from infrared DIRBE data and extrapolated to microwave frequencies. When we deduct the contribution from these two components at 22.8 GHz, the residual flux, associated with AME, is 2.12 ± 0.12 Jy (17.7σ). The spectral energy distribution from 10 to 60 GHz can be accurately fitted with a model of electric dipole emission from small spinning dust grains distributed in two separated phases of molecular and atomic gas, respectively. The dust emissivity, calculated by correlating the 22.8 GHz data with 100 μm data, is found to be 4.36 ± 0.17 μK (MJy sr^(–1))^(–1), a value considerably lower than in typical AME clouds, which present emissivities of ~20 μK (MJy sr^(–1))^(–1), although higher than the 0.2 μK (MJy sr^(–1))^(–1) of the translucent cloud LDN 1780, where AME has recently been claimed. The physical properties of the Pleiades nebula, in particular its low extinction A_V ~ 0.4, indicate that this is indeed a much less opaque object than those where AME has usually been studied. This fact, together with the broad knowledge of the stellar content of this region, provides an excellent testbed for AME characterization in physical conditions different from those generally explored up to now.

[1]  D. Finkbeiner,et al.  A LIMIT ON THE POLARIZED ANOMALOUS MICROWAVE EMISSION OF LYNDS 1622 , 2009, 0901.0133.

[2]  Magnetic Dipole Microwave Emission from Dust Grains , 1998, astro-ph/9807009.

[3]  J. Weingartner,et al.  Dust Grain-Size Distributions and Extinction in the Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud , 2001 .

[5]  D. J. Fixsen,et al.  Calibrator Design for the COBE Far Infrared Absolute Spectrophotometer (FIRAS) , 1998, astro-ph/9810373.

[6]  A. Lazarian,et al.  SPINNING DUST EMISSION: EFFECTS OF IRREGULAR GRAIN SHAPE, TRANSIENT HEATING, AND COMPARISON WITH WILKINSON MICROWAVE ANISOTROPY PROBE RESULTS , 2011, The Astrophysical Journal.

[7]  A. Lazarian,et al.  Electric Dipole Radiation from Spinning Dust Grains , 1998, astro-ph/9802239.

[8]  E. L. Wright,et al.  The COBE Diffuse Infrared Background Experiment Search for the Cosmic Infrared Background. I. Limits and Detections , 1998, astro-ph/9806167.

[9]  Kenneth H. Nordsieck,et al.  The Pleiades Reflection Nebula. II. Simple Model Constraints on Dust Properties and Scattering Geometry , 2003 .

[10]  D. Schlegel,et al.  Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds , 1998 .

[11]  D. Hartmann,et al.  The Milky Way in Molecular Clouds: A New Complete CO Survey , 2000, astro-ph/0009217.

[12]  Morphological Analysis of the Centimeter-Wave Continuum in the Dark Cloud LDN 1622 , 2005, astro-ph/0511283.

[13]  D. Schlegel,et al.  Tentative detection of electric dipole emission from rapidly rotating dust grains , 2001, astro-ph/0109534.

[14]  K. Gorski,et al.  HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere , 2004, astro-ph/0409513.

[15]  D. Finkbeiner Microwave Interstellar Medium Emission Observed by the Wilkinson Microwave Anisotropy Probe , 2004 .

[16]  R. Rebolo,et al.  CONSTRAINTS ON THE POLARIZATION OF THE ANOMALOUS MICROWAVE EMISSION IN THE PERSEUS MOLECULAR COMPLEX FROM SEVEN-YEAR WMAP DATA , 2010, 1011.1242.

[17]  J. Bond,et al.  ANOMALOUS MICROWAVE EMISSION FROM THE H ii REGION RCW175 , 2008, 0807.3985.

[18]  A. Lazarian,et al.  IMPROVING THE MODEL OF EMISSION FROM SPINNING DUST: EFFECTS OF GRAIN WOBBLING AND TRANSIENT SPIN-UP , 2010, The Astrophysical Journal.

[19]  C. B. Netterfield,et al.  Planck early results. XX. New light on anomalous microwave emission from spinning dust grains , 2011, 1101.2031.

[20]  M. Halpern,et al.  Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Polarization , 2007, The Astrophysical Journal.