Detection of Spectral Variations of Anomalous Microwave Emission with QUIJOTE and C-BASS. (arXiv:2001.07159v2 [astro-ph.GA] UPDATED)

Detection of Spectral Variations of Anomalous Microwave Emission with QUIJOTE and C-BASS. (arXiv:2001.07159v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Cepeda_Arroita_R/0/1/0/all/0/1">R. Cepeda-Arroita</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Harper_S/0/1/0/all/0/1">S. Harper</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Dickinson_C/0/1/0/all/0/1">C. Dickinson</a> (1, 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Rubino_Martin_J/0/1/0/all/0/1">J. A. Rubiño-Martín</a> (3, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Genova_Santos_R/0/1/0/all/0/1">R. T. Génova-Santos</a> (3, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_A/0/1/0/all/0/1">Angela C. Taylor</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Pearson_T/0/1/0/all/0/1">T. J. Pearson</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Ashdown_M/0/1/0/all/0/1">M. Ashdown</a> (6, 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Barr_A/0/1/0/all/0/1">A. Barr</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Barreiro_R/0/1/0/all/0/1">R. B. Barreiro</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Casaponsa_B/0/1/0/all/0/1">B. Casaponsa</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Casas_F/0/1/0/all/0/1">F. J. Casas</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Chiang_H/0/1/0/all/0/1">H. C. Chiang</a> (9, 10), <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Cobos_R/0/1/0/all/0/1">R. Fernandez-Cobos</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Grumitt_R/0/1/0/all/0/1">R. D. P. Grumitt</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Guidi_F/0/1/0/all/0/1">F. Guidi</a> (3, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Heilgendorff_H/0/1/0/all/0/1">H. M. Heilgendorff</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Herranz_D/0/1/0/all/0/1">D. Herranz</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Jew_L/0/1/0/all/0/1">L. R. P. Jew</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Jonas_J/0/1/0/all/0/1">J. L. Jonas</a> (11, 12), <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_M/0/1/0/all/0/1">Michael E. Jones</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Lasenby_A/0/1/0/all/0/1">A. Lasenby</a> (6, 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Leech_J/0/1/0/all/0/1">J. Leech</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Leahy_J/0/1/0/all/0/1">J. P. Leahy</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_Gonzalez_E/0/1/0/all/0/1">E. Martínez-González</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Peel_M/0/1/0/all/0/1">M. W. Peel</a> (1, 3, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Poidevin_F/0/1/0/all/0/1">F. Poidevin</a> (3, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Piccirillo_L/0/1/0/all/0/1">L. Piccirillo</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Readhead_A/0/1/0/all/0/1">A. C. S. Readhead</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Rebolo_R/0/1/0/all/0/1">R. Rebolo</a> (3, 4, 13), <a href="http://arxiv.org/find/astro-ph/1/au:+Ruiz_Granados_B/0/1/0/all/0/1">B. Ruiz-Granados</a> (3, 4, 14, 15), <a href="http://arxiv.org/find/astro-ph/1/au:+Sievers_J/0/1/0/all/0/1">J. Sievers</a> (9, 16), <a href="http://arxiv.org/find/astro-ph/1/au:+Vansyngel_F/0/1/0/all/0/1">F. Vansyngel</a> (3, 4), <a href="http://arxiv.org/find/astro-ph/1/au:+Vielva_P/0/1/0/all/0/1">P. Vielva</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Watson_R/0/1/0/all/0/1">R. A. Watson</a> (1) ((1) University of Manchester, (2) California Institute of Technology, (3) Instituto de Astrofísica de Canarias, (4) Universidad de La Laguna, (5) University of Oxford, (6) Cavendish Laboratory, University of Cambridge, (7) Kavli Institute for Cosmology, University of Cambridge, (8) CSIC-Universidad de Cantabria, (9) McGill University (10) School of Mathematics, Statistics & Computer Science, University of KwaZulu-Natal (11) Rhodes University (12) South African Radio Astronomy Observatory (13) Consejo Superior de Investigaciones Científicas (14) Agenzia Spaziale Italiana (15) Istituto Nazionale di Fisica Nucleare (16) School of Chemistry & Physics, University of KwaZulu-Natal)

Anomalous Microwave Emission (AME) is a significant component of Galactic
diffuse emission in the frequency range $10$-$60,$GHz and a new window into
the properties of sub-nanometre-sized grains in the interstellar medium. We
investigate the morphology of AME in the $approx10^{circ}$ diameter $lambda$
Orionis ring by combining intensity data from the QUIJOTE experiment at $11$,
$13$, $17$ and $19,$GHz and the C-Band All Sky Survey (C-BASS) at $4.76,$GHz,
together with 19 ancillary datasets between $1.42$ and $3000,$GHz. Maps of
physical parameters at $1^{circ}$ resolution are produced through Markov Chain
Monte Carlo (MCMC) fits of spectral energy distributions (SEDs), approximating
the AME component with a log-normal distribution. AME is detected in excess of
$20,sigma$ at degree-scales around the entirety of the ring along
photodissociation regions (PDRs), with three primary bright regions containing
dark clouds. A radial decrease is observed in the AME peak frequency from
$approx35,$GHz near the free-free region to $approx21,$GHz in the outer
regions of the ring, which is the first detection of AME spectral variations
across a single region. A strong correlation between AME peak frequency,
emission measure and dust temperature is an indication for the dependence of
the AME peak frequency on the local radiation field. The AME amplitude
normalised by the optical depth is also strongly correlated with the radiation
field, giving an overall picture consistent with spinning dust where the local
radiation field plays a key role.

http://arxiv.org/icons/sfx.gif