[ { "id": "authors:vkn8s-js750", "collection": "authors", "collection_id": "vkn8s-js750", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200903-132014697", "type": "article", "title": "The C-Band All-Sky Survey: total intensity point-source detection over the northern sky", "author": [ { "family_name": "Grumitt", "given_name": "R. D. P.", "orcid": "0000-0001-9578-6111", "clpid": "Grumitt-R-D-P" }, { "family_name": "Taylor", "given_name": "Angela C.", "clpid": "Taylor-A-C" }, { "family_name": "Jew", "given_name": "Luke", "orcid": "0000-0002-1831-4898", "clpid": "Jew-L" }, { "family_name": "Jones", "given_name": "Michael E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Barr", "given_name": "A.", "clpid": "Barr-A-ASTRO" }, { "family_name": "Cepeda-Arroita", "given_name": "R.", "orcid": "0000-0002-9043-2645", "clpid": "Cepeda-Arroita-R" }, { "family_name": "Chiang", "given_name": "H. C.", "clpid": "Chiang-H-C" }, { "family_name": "Harper", "given_name": "S. E.", "clpid": "Harper-S-E" }, { "family_name": "Heilgendorff", "given_name": "H. M.", "clpid": "Heilgendorff-H-M" }, { "family_name": "Jonas", "given_name": "J. L.", "clpid": "Jonas-J-L" }, { "family_name": "Leahy", "given_name": "J. P.", "clpid": "Leahy-J-P" }, { "family_name": "Leech", "given_name": "J.", "clpid": "Leech-J" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Peel", "given_name": "M. W.", "orcid": "0000-0003-3412-2586", "clpid": "Peel-M-W" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Sievers", "given_name": "J.", "orcid": "0000-0001-6903-5074", "clpid": "Sievers-J" } ], "abstract": "We present a point-source detection algorithm that employs the second-order Spherical Mexican Hat wavelet filter (SMHW2), and use it on C-Band All-Sky Survey (C-BASS) northern intensity data to produce a catalogue of point sources. This catalogue allows us to cross-check the C-BASS flux-density scale against existing source surveys, and provides the basis for a source mask that will be used in subsequent C-BASS and cosmic microwave background (CMB) analyses. The SMHW2 allows us to filter the entire sky at once, avoiding complications from edge effects arising when filtering small sky patches. The algorithm is validated against a set of Monte Carlo simulations, consisting of diffuse emission, instrumental noise, and various point-source populations. The simulated source populations are successfully recovered. The SMHW2 detection algorithm is used to produce a 4.76GHz northern sky source catalogue in total intensity, containing 1784 sources and covering declinations \u03b4 \u2265 \u221210\u00b0. The C-BASS catalogue is matched with the Green Bank 6\u2009cm (GB6) and Parkes-MIT-NRAO (PMN) catalogues over their areas of common sky coverage. From this we estimate the 90 per\u2009cent completeness level to be approximately 610mJy\u2060, with a corresponding reliability of 98 per\u2009cent, when masking the brightest 30 per\u2009cent of the diffuse emission in the C-BASS northern sky map. We find the C-BASS and GB6 flux-density scales to be consistent with one another to within approximately 4 per\u2009cent.", "doi": "10.1093/mnras/staa1572", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2020-08", "series_number": "2", "volume": "496", "issue": "2", "pages": "1941-1958" }, { "id": "authors:b6k79-svx14", "collection": "authors", "collection_id": "b6k79-svx14", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200717-103452078", "type": "article", "title": "Resolved observations at 31\u2009GHz of spinning dust emissivity variations in \u03c1\u2009Oph", "author": [ { "family_name": "Arce-Tord", "given_name": "Carla", "orcid": "0000-0002-0176-4331", "clpid": "Arce-Tord-C" }, { "family_name": "Vidal", "given_name": "Matias", "orcid": "0000-0003-2134-1587", "clpid": "Vidal-M" }, { "family_name": "Casassus", "given_name": "Simon", "orcid": "0000-0002-0433-9840", "clpid": "Casassus-S" }, { "family_name": "C\u00e1rcamo", "given_name": "Miguel", "orcid": "0000-0003-0564-8167", "clpid": "C\u00e1rcamo-M" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Hensley", "given_name": "Brandon S.", "orcid": "0000-0001-7449-4638", "clpid": "Hensley-B-S" }, { "family_name": "G\u00e9nova-Santos", "given_name": "Ricardo", "orcid": "0000-0001-5479-0034", "clpid": "G\u00e9nova-Santos-R" }, { "family_name": "Bond", "given_name": "J. Richard", "orcid": "0000-0003-2358-9949", "clpid": "Bond-J-R" }, { "family_name": "Jones", "given_name": "Michael E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Readhead", "given_name": "Anthony C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Taylor", "given_name": "Angela C.", "clpid": "Taylor-A-C" }, { "family_name": "Zensus", "given_name": "J. Anton", "orcid": "0000-0001-7470-3321", "clpid": "Zensus-J-A" } ], "abstract": "The \u03c1\u2009Oph molecular cloud is one of the best examples of spinning dust emission, first detected by the cosmic background imager (CBI). Here, we present 4.5\u2009arcmin observations with CBI\u20092 that confirm 31\u2009GHz emission from \u03c1\u2009Oph\u2009W, the PDR exposed to B-type star HD\u2009147889, and highlight the absence of signal from S1, the brightest IR nebula in the complex. In order to quantify an association with dust-related emission mechanisms, we calculated correlations at different angular resolutions between the 31\u2009GHz map and proxies for the column density of IR emitters, dust radiance, and optical depth templates. We found that the 31\u2009GHz emission correlates best with the PAH column density tracers, while the correlation with the dust radiance improves when considering emission that is more extended (from the shorter baselines), suggesting that the angular resolution of the observations affects the correlation results. A proxy for the spinning dust emissivity reveals large variations within the complex, with a dynamic range of 25 at 3\u03c3 and a variation by a factor of at least 23, at 3\u03c3, between the peak in \u03c1\u2009Oph\u2009W and the location of S1, which means that environmental factors are responsible for boosting spinning dust emissivities locally.", "doi": "10.1093/mnras/staa1422", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2020-07", "series_number": "3", "volume": "495", "issue": "3", "pages": "3482-3493" }, { "id": "authors:gswkz-vyg12", "collection": "authors", "collection_id": "gswkz-vyg12", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190801-103843596", "type": "article", "title": "The C-Band All-Sky Survey (C-BASS): constraining diffuse Galactic radio emission in the North Celestial Pole region", "author": [ { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Barr", "given_name": "A.", "clpid": "Barr-A" }, { "family_name": "Chiang", "given_name": "H. C.", "clpid": "Chiang-H-C" }, { "family_name": "Copley", "given_name": "C.", "clpid": "Copley-C" }, { "family_name": "Grumitt", "given_name": "R. D. P.", "clpid": "Grumitt-R-D-P" }, { "family_name": "Harper", "given_name": "S. E.", "clpid": "Harper-S-E" }, { "family_name": "Heilgendorff", "given_name": "H. M.", "clpid": "Heilgendorff-H-M" }, { "family_name": "Jew", "given_name": "L. R. P.", "clpid": "Jew-L-R-P" }, { "family_name": "Jonas", "given_name": "J. L.", "clpid": "Jonas-J-L" }, { "family_name": "Jones", "given_name": "Michael E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Leahy", "given_name": "J. P.", "clpid": "Leahy-J-P" }, { "family_name": "Leech", "given_name": "J.", "clpid": "Leech-J" }, { "family_name": "Leitch", "given_name": "E. M.", "clpid": "Leitch-E-M" }, { "family_name": "Muchovej", "given_name": "S. J. C.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Peel", "given_name": "M. W.", "orcid": "0000-0003-3412-2586", "clpid": "Peel-M-W" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Sievers", "given_name": "J.", "orcid": "0000-0001-6903-5074", "clpid": "Sievers-J" }, { "family_name": "Stevenson", "given_name": "M. A.", "clpid": "Stevenson-M-A" }, { "family_name": "Taylor", "given_name": "Angela C.", "clpid": "Taylor-A-C" } ], "abstract": "The C-Band All-Sky Survey (C-BASS) is a high sensitivity all-sky radio survey at an angular resolution of 45\u2009arcmin and a frequency of 4.7\u2009GHz. We present a total intensity map of the North Celestial Pole (NCP) region of sky, above declination >+80\u00b0, which is limited by source confusion at a level of \u22480.6\u2009mK rms. We apply the template-fitting (cross-correlation) technique to WMAP and Planck data, using the C-BASS map as the synchrotron template, to investigate the contribution of diffuse foreground emission at frequencies \u223c20\u201340\u2009GHz. We quantify the anomalous microwave emission (AME) that is correlated with far-infrared dust emission. The AME amplitude does not change significantly (\u2060<10 per cent\u2060) when using the higher frequency C-BASS 4.7\u2009GHz template instead of the traditional Haslam 408\u2009MHz map as a tracer of synchrotron radiation. We measure template coefficients of 9.93 \u00b1 0.35 and 9.52 \u00b1 0.34\u2009K per unit \u03c4_(353) when using the Haslam and C-BASS synchrotron templates, respectively. The AME contributes 55 \u00b1 2\u03bcK rms at 22.8\u2009GHz and accounts for \u224860 per cent of the total foreground emission. Our results show that a harder (flatter spectrum) component of synchrotron emission is not dominant at frequencies \u22735\u2009GHz; the best-fitting synchrotron temperature spectral index is \u03b2 = \u22122.91 \u00b1 0.04 from 4.7 to 22.8\u2009GHz and \u03b2 = \u22122.85 \u00b1 0.14 from 22.8 to 44.1\u2009GHz. Free\u2013free emission is weak, contributing \u22487\u03bcK rms (\u2060\u22487 per cent\u2060) at 22.8\u2009GHz. The best explanation for the AME is still electric dipole emission from small spinning dust grains.", "doi": "10.1093/mnras/stz522", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2019-05", "series_number": "2", "volume": "485", "issue": "2", "pages": "2844-2860" }, { "id": "authors:y8ahs-rfn83", "collection": "authors", "collection_id": "y8ahs-rfn83", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190301-092706950", "type": "article", "title": "The C-Band All-Sky Survey (C-BASS): digital backend for the northern survey", "author": [ { "family_name": "Stevenson", "given_name": "M. A.", "clpid": "Stevenson-M-A" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Jones", "given_name": "Michael E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Copley", "given_name": "C. J.", "clpid": "Copley-C-J" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "John", "given_name": "J. J.", "clpid": "John-J-J" }, { "family_name": "King", "given_name": "O. G.", "clpid": "King-O-G" }, { "family_name": "Muchovej", "given_name": "S. J. C.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Taylor", "given_name": "Angela C.", "clpid": "Taylor-A-C" } ], "abstract": "The C-Band All-Sky Survey (C-BASS) is an all-sky full-polarization survey at a frequency of 5\u2009GHz, designed to provide data complementary to the all-sky surveys of WMAP and Planck and future CMB B-mode polarization imaging surveys. We describe the design and performance of the digital backend used for the northern part of the survey. In particular, we describe the features that efficiently implement the demodulation and filtering required to suppress contaminating signals in the time-ordered data, and the capability for real-time correction of detector non-linearity and receiver balance.", "doi": "10.1093/mnras/stz313", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2019-04-21", "series_number": "4", "volume": "484", "issue": "4", "pages": "5377-5388" }, { "id": "authors:06ht1-djn48", "collection": "authors", "collection_id": "06ht1-djn48", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180227-084611974", "type": "article", "title": "The State-of-Play of Anomalous Microwave Emission (AME) Research", "author": [ { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K-A" }, { "family_name": "Hensley", "given_name": "B.", "orcid": "0000-0001-7449-4638", "clpid": "Hensley-B-S" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" } ], "abstract": "Anomalous Microwave Emission (AME) is a component of diffuse Galactic radiation observed at frequencies in the range \u202f\u2248\u202f10\u201360 GHz. AME was first detected in 1996 and recognised as an additional component of emission in 1997. Since then, AME has been observed by a range of experiments and in a variety of environments. AME is spatially correlated with far-IR thermal dust emission but cannot be explained by synchrotron or free\u2013free emission mechanisms, and is far in excess of the emission contributed by thermal dust emission with the power-law opacity consistent with the observed emission at sub-mm wavelengths. Polarization observations have shown that AME is very weakly polarized (\u202f\u2272\u202f1 %). The most natural explanation for AME is rotational emission from ultra-small dust grains (\"spinning dust\"), first postulated in 1957. Magnetic dipole radiation from thermal fluctuations in the magnetization of magnetic grain materials may also be contributing to the AME, particularly at higher frequencies (\u202f\u2273\u202f50 GHz). AME is also an important foreground for Cosmic Microwave Background analyses. This paper presents a review and the current state-of-play in AME research, which was discussed in an AME workshop held at ESTEC, The Netherlands, June 2016.", "doi": "10.1016/j.newar.2018.02.001", "issn": "1387-6473", "publisher": "Elsevier", "publication": "New Astronomy Reviews", "publication_date": "2018-02", "volume": "80", "pages": "1-28" }, { "id": "authors:2gk9v-6xm54", "collection": "authors", "collection_id": "2gk9v-6xm54", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151119-140541600", "type": "article", "title": "Observations of free\u2013free and anomalous microwave emission from LDN 1622 with the 100 m Green Bank Telescope", "author": [ { "family_name": "Harper", "given_name": "S. E.", "clpid": "Harper-S-E" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K" } ], "abstract": "LDN 1622 has previously been identified as a possible strong source of dust-correlated anomalous microwave emission (AME). Previous observations were limited by resolution meaning that the radio emission could not be compared with current generation high-resolution infrared data from Herschel, Spitzer or Wide-field Infrared Sky Explorer. This paper presents arcminute resolution mapping observations of LDN 1622 at 4.85 and 13.7 GHz using the 100 m Robert C. Byrd Green Bank Telescope. The 4.85 GHz map reveals a corona of free\u2013free emission enclosing LDN 1622 that traces the photodissociation region of the cloud. The brightest peaks of the 4.85 GHz map are found to be within \u224810 per cent agreement with the expected free\u2013free predicted by Southern H-Alpha Sky Survey Atlas H\u2009\u03b1 data of LDN 1622. At 13.7 GHz, the AME flux density was found to be 7.0 \u00b1 1.4 mJy and evidence is presented for a rising spectrum between 13.7 and 31 GHz. The spinning dust model of AME is found to naturally account for the flux seen at 13.7 GHz. Correlations between the diffuse 13.7 GHz emission and the diffuse mid-infrared emission are used to further demonstrate that the emission originating from LDN 1622 at 13.7 GHz is described by the spinning dust model.", "doi": "10.1093/mnras/stv1863", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2015-11-11", "series_number": "4", "volume": "453", "issue": "4", "pages": "3375-3385" }, { "id": "authors:z5p7g-e9789", "collection": "authors", "collection_id": "z5p7g-e9789", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151218-105944715", "type": "article", "title": "Anomalous Microwave Emission in HII Regions: Is it Really Anomalous? The Case of RCW 49", "author": [ { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Ingallinera", "given_name": "Adriano", "orcid": "0000-0002-3137-473X", "clpid": "Ingallinera-A" }, { "family_name": "Agliozzo", "given_name": "Claudia", "orcid": "0000-0003-1749-2542", "clpid": "Agliozzo-C" }, { "family_name": "Tibbs", "given_name": "Christopher T.", "clpid": "Tibbs-C-T" }, { "family_name": "Noriega-Crespo", "given_name": "Alberto", "orcid": "0000-0002-6296-8960", "clpid": "Noriega-Crespo-A" }, { "family_name": "Umana", "given_name": "Grazia", "clpid": "Umana-G" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Trigilio", "given_name": "Corrado", "orcid": "0000-0002-1216-7831", "clpid": "Trigilio-C" } ], "abstract": "The detection of an excess of emission at microwave frequencies with respect to the predicted free\u2013free emission has been reported for several Galactic H ii regions. Here, we investigate the case of RCW 49, for which the Cosmic Background Imager tentatively (~3\u03c3) detected Anomalous Microwave Emission (AME) at 31 GHz on angular scales of 7'. Using the Australia Telescope Compact Array, we carried out a multi-frequency (5, 19, and 34 GHz) continuum study of the region, complemented by observations of the H109\u03b1 radio recombination line. The analysis shows that: (1) the spatial correlation between the microwave and IR emission persists on angular scales from 3farcm4 to 0farcs4, although the degree of the correlation slightly decreases at higher frequencies and on smaller angular scales; (2) the spectral indices between 1.4 and 5 GHz are globally in agreement with optically thin free\u2013free emission, however, ~30% of these are positive and much greater than \u22120.1, consistent with a stellar wind scenario; and (3) no major evidence for inverted free\u2013free radiation is found, indicating that this is likely not the cause of the Anomalous Emission in RCW 49. Although our results cannot rule out the spinning dust hypothesis to explain the tentative detection of AME in RCW 49, they emphasize the complexity of astronomical sources that are very well known and studied, such as H ii regions, and suggest that, at least in these objects, the reported excess of emission might be ascribed to alternative mechanisms such as stellar winds and shocks.", "doi": "10.1088/0004-637X/813/1/24", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2015-11-01", "series_number": "1", "volume": "813", "issue": "1", "pages": "Art. No. 24" }, { "id": "authors:mer5v-tz292", "collection": "authors", "collection_id": "mer5v-tz292", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151119-140539394", "type": "article", "title": "Observations of Galactic star-forming regions with the Cosmic Background Imager at 31 GHz", "author": [ { "family_name": "Demetroullas", "given_name": "C.", "clpid": "Demetroullas-C" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Stamadianos", "given_name": "D.", "clpid": "Stamadianos-D" }, { "family_name": "Harper", "given_name": "S. E.", "clpid": "Harper-S-E" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K" }, { "family_name": "Jones", "given_name": "Michael E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Taylor", "given_name": "Angela C.", "clpid": "Taylor-A-C" } ], "abstract": "Studies of the diffuse Galactic radio emission are interesting both for better understanding the physical conditions in our Galaxy and for minimizing the contamination in cosmological measurements. Motivated by this, we present Cosmic Background Imager 31 GHz observations of the Galactic regions NGC 6357, NGC 6334, W51 and W40 at \u223c4.5 arcmin resolution and conduct an investigation of the spectral emission process in the regions at 4.5 arcmin and 1\u00b0 resolution. We find that most of the emission in the regions is due to optically thin free\u2013free. For two sub-regions of NGC 6334 and for a sub-region of W51 though, at 4.5 arcmin resolution and at 31 GHz we detect less emission than expected from extrapolation of radio data at lower frequencies assuming a spectral index of \u22120.12 for optically thin free\u2013free emission, at 3.3\u03c3, 3.7\u03c3 and 6.5\u03c3, respectively. We also detect excess emission in a sub-region of NCG 6334 at 6.4\u03c3, after ruling out any possible contribution from ultra-compact H\u2009II regions. At 1\u00b0 resolution, we detect a spinning dust component in the spectral energy distribution of W40 that accounts for 18 \u00b1 7 per\u2009cent of the total flux density in the region at the peak frequency of 37 GHz. Comparison with 100\u2009\u03bcm data indicates an average dust emissivity for the sub-regions of 0.5 \u00b1 4.4\u2009\u03bcK(MJy sr^(\u22121))^(\u22121). Finally, we translate the excess emission in the regions to an anomalous microwave emission (AME) emissivity relative to the optical depth at 250\u2009\u03bcm. We find that this form of emissivity is independent of the AME significance and has a value somewhere in the order of 10^4 Jy.", "doi": "10.1093/mnras/stv1793", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2015-10-21", "series_number": "2", "volume": "453", "issue": "2", "pages": "2082-2093" }, { "id": "authors:tnad2-0fn24", "collection": "authors", "collection_id": "tnad2-0fn24", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180821-142709022", "type": "book_section", "title": "Studies of Anomalous Microwave Emission (AME) with the SKA", "book_title": "Advancing Astrophysics with the Square Kilometre Array", "author": [ { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Ali-Ha\u00efmoud", "given_name": "Y.", "clpid": "Ali-Ha\u00efmoud-Y" }, { "family_name": "Beswick", "given_name": "R. J.", "clpid": "Beswick-R-J" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K" }, { "family_name": "Draine", "given_name": "B. T.", "orcid": "0000-0002-0846-936X", "clpid": "Draine-B-T" }, { "family_name": "G\u00e9nova-Santos", "given_name": "R.", "clpid": "G\u00e9nova-Santos-R" }, { "family_name": "Grainge", "given_name": "K.", "clpid": "Grainge-K-J-B" }, { "family_name": "Hoang", "given_name": "T. C.", "clpid": "Hoang-T-C" }, { "family_name": "Lazarian", "given_name": "A.", "clpid": "Lazarian-A" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Peel", "given_name": "M. W.", "orcid": "0000-0003-3412-2586", "clpid": "Peel-M-W" }, { "family_name": "Perrott", "given_name": "Y.", "clpid": "Perrott-Y-C" }, { "family_name": "Rubi\u00f1o-Martin", "given_name": "J.-A.", "clpid": "Rubi\u00f1o-Martin-J-A" }, { "family_name": "Scaife", "given_name": "A.", "clpid": "Scaife-A-M-M" }, { "family_name": "Tibbs", "given_name": "C. T.", "clpid": "Tibbs-C-T" }, { "family_name": "Verstraete", "given_name": "L.", "clpid": "Verstraete-L" }, { "family_name": "Vidal", "given_name": "M.", "clpid": "Vidal-M" }, { "family_name": "Watson", "given_name": "R. A.", "clpid": "Watson-R-A" }, { "family_name": "Ysard", "given_name": "N.", "clpid": "Ysard-N" } ], "abstract": "In this chapter, we will outline the scientific motivation for studying Anomalous Microwave Emission\n(AME) with the SKA. AME is thought to be due to electric dipole radiation from small\nspinning dust grains, although thermal fluctuations of magnetic dust grains may also contribute.\nStudies of this mysterious component would shed light on the emission mechanism, which then\nopens up a new window onto the interstellar medium (ISM). AME is emitted mostly in the frequency\nrange ~10\u2013100 GHz, and thus the SKA has the potential of measuring the low frequency\nside of the AME spectrum, particularly in band 5. Science targets include dense molecular clouds\nin the Milky Way, as well as extragalactic sources. We also discuss the possibility of detecting\nrotational line emission from Poly-cyclic Aromatic Hydrocarbons (PAHs), which could be\nthe main carriers of AME. Detecting PAH lines of a given spacing would allow for a definitive\nidentification of specific PAH species.", "doi": "10.22323/1.215.0124", "isbn": "9781909204706", "publisher": "SISSA", "place_of_publication": "Trieste, Italy", "publication_date": "2015-05-29", "pages": "Art. No. 124" }, { "id": "authors:6eqf0-hc013", "collection": "authors", "collection_id": "6eqf0-hc013", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150424-150715438", "type": "article", "title": "C-Band All-Sky Survey: a first look at the Galaxy", "author": [ { "family_name": "Irfan", "given_name": "M. O.", "clpid": "Irfan-M-O" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Copley", "given_name": "C.", "clpid": "Copley-C" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Ferreira", "given_name": "P. G.", "clpid": "Ferreira-P-G" }, { "family_name": "Holler", "given_name": "C. M.", "clpid": "Holler-C-M" }, { "family_name": "Jonas", "given_name": "J. L.", "clpid": "Jonas-J-L" }, { "family_name": "Jones", "given_name": "Michael E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "King", "given_name": "O. G.", "clpid": "King-O-G" }, { "family_name": "Leahy", "given_name": "J. P.", "clpid": "Leahy-J-P" }, { "family_name": "Leech", "given_name": "J.", "clpid": "Leech-J" }, { "family_name": "Leitch", "given_name": "E. M.", "clpid": "Leitch-E-M" }, { "family_name": "Muchovej", "given_name": "S. J. C.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Peel", "given_name": "M. W.", "orcid": "0000-0003-3412-2586", "clpid": "Peel-M-W" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Stevenson", "given_name": "M. A.", "clpid": "Stevenson-M-A" }, { "family_name": "Sutton", "given_name": "D.", "clpid": "Sutton-D" }, { "family_name": "Taylor", "given_name": "Angela C.", "clpid": "Taylor-A-C" }, { "family_name": "Zuntz", "given_name": "J.", "clpid": "Zuntz-J" } ], "abstract": "We present an analysis of the diffuse emission at 5\u2009GHz in the first quadrant of the Galactic plane using two months of preliminary intensity data taken with the C-Band All-Sky Survey (C-BASS) northern instrument at the Owens Valley Radio Observatory, California. Combining C-BASS maps with ancillary data to make temperature\u2013temperature plots, we find synchrotron spectral indices of \u03b2 = \u22122.65 \u00b1 0.05 between 0.408 and 5\u2009GHz and \u03b2 = \u22122.72 \u00b1 0.09 between 1.420 and 5\u2009GHz for \u221210\u00b0 < |b| < \u22124\u00b0, 20\u00b0 < l < 40\u00b0. Through the subtraction of a radio recombination line free\u2013free template, we determine the synchrotron spectral index in the Galactic plane (|b| < 4\u00b0) to be \u03b2 = \u22122.56 \u00b1 0.07 between 0.408 and 5\u2009GHz, with a contribution of 53 \u00b1 8 per cent from free\u2013free emission at 5\u2009GHz. These results are consistent with previous low-frequency measurements in the Galactic plane. By including C-BASS data in spectral fits, we demonstrate the presence of anomalous microwave emission (AME) associated with the H\u2009ii complexes W43, W44 and W47 near 30\u2009GHz, at 4.4\u03c3, 3.1\u03c3 and 2.5\u03c3, respectively. The CORNISH (Co-Ordinated Radio 'N' Infrared Survey for High mass star formation) VLA 5-GHz source catalogue rules out the possibility that the excess emission detected around 30\u2009GHz may be due to ultracompact H\u2009ii regions. Diffuse AME was also identified at a 4\u03c3 level within 30\u00b0 < l < 40\u00b0, \u22122\u00b0 < b < 2\u00b0 between 5 and 22.8\u2009GHz.", "doi": "10.1093/mnras/stv212", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2015-03-11", "series_number": "4", "volume": "448", "issue": "4", "pages": "3572-3586" }, { "id": "authors:m7y21-kda78", "collection": "authors", "collection_id": "m7y21-kda78", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150113-083744623", "type": "book_section", "title": "SKA studies of nearby galaxies: star-formation, accretion processes and molecular gas across all environments", "author": [ { "family_name": "Beswick", "given_name": "R. J.", "clpid": "Beswick-R-J" }, { "family_name": "Brinks", "given_name": "E.", "orcid": "0000-0002-7758-9699", "clpid": "Brinks-E" }, { "family_name": "P\u00e9rez-Torres", "given_name": "M. A.", "clpid": "P\u00e9rez-Torres-M-A" }, { "family_name": "Richards", "given_name": "A. M. S.", "clpid": "Richards-A-M-S" }, { "family_name": "Aalto", "given_name": "S.", "orcid": "0000-0002-5828-7660", "clpid": "Aalto-Susanne" }, { "family_name": "Alberdi", "given_name": "A.", "clpid": "Alberdi-A" }, { "family_name": "Argo", "given_name": "M. K.", "clpid": "Argo-M-K" }, { "family_name": "van Bemmel", "given_name": "I.", "clpid": "van-Bemmel-I" }, { "family_name": "Conway", "given_name": "J. E.", "clpid": "Conway-J-E" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Fenech", "given_name": "C. M.", "clpid": "Fenech-D-M" }, { "family_name": "Gray", "given_name": "M. D.", "clpid": "Gray-M-D" }, { "family_name": "Kl\u00f6ckner", "given_name": "H.-R.", "clpid": "Kl\u00f6ckner-H-R" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Muxlow", "given_name": "T. W. B.", "clpid": "Muxlow-T-W-B" }, { "family_name": "Peel", "given_name": "M.", "clpid": "Peel-M" }, { "family_name": "Rushton", "given_name": "A. P.", "clpid": "Rushton-A-P" }, { "family_name": "Schinnerer", "given_name": "E.", "orcid": "0000-0002-3933-7677", "clpid": "Schinnerer-E" } ], "abstract": "The SKA will be a transformational instrument in the study of our local Universe. In particular, by virtue of its high sensitivity (both to point sources and diffuse low surface brightness emission), angular resolution and the frequency ranges covered, the SKA will undertake a very wide range of astrophysical research in the field of nearby galaxies. By surveying vast numbers of nearby galaxies of all types with mJy sensitivity and sub-arcsecond angular resolutions at radio wavelengths, the SKA will provide the cornerstone of our understanding of star-formation and accretion activity in the local Universe. In this chapter we outline the key continuum and molecular line science areas where the SKA, both during phase-1 and when it becomes the full SKA, will have a significant scientific impact.", "doi": "10.48550/arXiv.1412.5810", "publisher": "Proceedings of Science", "publication_date": "2014-12-18" }, { "id": "authors:3rx8z-k2329", "collection": "authors", "collection_id": "3rx8z-k2329", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170519-140259138", "type": "book_section", "title": "The Astrophysics of Star Formation Across Cosmic Time at \u227310 GHz with the Square Kilometre Array", "author": [ { "family_name": "Murphy", "given_name": "Eric J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Sargent", "given_name": "Mark T.", "orcid": "0000-0003-1033-9684", "clpid": "Sargent-M-T" }, { "family_name": "Beswick", "given_name": "Rob J.", "clpid": "Beswick-R-J" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Heywood", "given_name": "Ian", "clpid": "Heywood-I" }, { "family_name": "Hunt", "given_name": "Leslie K.", "orcid": "0000-0001-9162-2371", "clpid": "Hunt-L-K" }, { "family_name": "Hyunh", "given_name": "Minh T.", "clpid": "Hyunh-Minh-T" }, { "family_name": "Jarvis", "given_name": "Matt", "orcid": "0000-0001-7039-9078", "clpid": "Jarvis-M-J" }, { "family_name": "Karim", "given_name": "Alexander", "orcid": "0000-0002-8414-9579", "clpid": "Karim-A" }, { "family_name": "Krause", "given_name": "Marita", "clpid": "Krause-M" }, { "family_name": "Prandoni", "given_name": "Isabella", "clpid": "Prandoni-I" }, { "family_name": "Seymour", "given_name": "Nicholas", "orcid": "0000-0003-3506-5536", "clpid": "Seymour-N" }, { "family_name": "Schinnerer", "given_name": "Eva", "orcid": "0000-0002-3933-7677", "clpid": "Schinnerer-E" }, { "family_name": "Tabatabaei", "given_name": "Fatemeh S.", "clpid": "Tabatabaei-F-S" }, { "family_name": "Wagg", "given_name": "Jeff", "clpid": "Wagg-J" } ], "abstract": "In this chapter, we highlight a number of science investigations that are enabled by the inclusion of\nBand 5 (4.6-13.8 GHz) for SKA1-MID science operations, while focusing on the astrophysics of star formation over cosmic time. For studying the detailed astrophysics of star formation at highredshift, surveys at frequencies \u227310 GHz have the distinct advantage over traditional ~1.4 GHz\nsurveys as they are able to yield higher angular resolution imaging while probing higher rest frame frequencies of galaxies with increasing redshift, where emission of star-forming galaxies becomes dominated by thermal (free-free) radiation. In doing so, surveys carried out at \u227310 GHz provide a robust, dust-unbiased measurement of the massive star formation rate by being highly sensitive to the number of ionizing photons that are produced. To access this powerful star formation rate diagnostic requires that Band 5 be available for SKA1-MID. We additionally present a detailed science case for frequency coverage extending up to 30 GHz during full SKA2 operations, as this allows for highly diverse science while additionally providing contiguous frequency coverage between the SKA and ALMA, which will likely be the two most powerful interferometers for the coming decades. To enable this synergy, it is crucial that the dish design of the SKA be flexible\nenough to include the possibility of being fit with receivers operating up to 30 GHz.", "doi": "10.48550/arXiv.1412.5677", "publisher": "Proceedings of Science", "publication_date": "2014-12-18" }, { "id": "authors:nfc70-34j74", "collection": "authors", "collection_id": "nfc70-34j74", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140620-102116115", "type": "article", "title": "The pros and cons of the inversion method approach to derive 3D dust emission properties in the ISM: the Hi-GAL field centred on (l, b) = (30\u00b0, 0\u00b0)", "author": [ { "family_name": "Traficante", "given_name": "A.", "orcid": "0000-0003-1665-6402", "clpid": "Traficante-A" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Compiegne", "given_name": "M.", "clpid": "Compiegne-M" }, { "family_name": "Alves", "given_name": "M. I. R.", "clpid": "Alves-M-I-R" }, { "family_name": "Cambr\u00e9sy", "given_name": "L.", "clpid": "Cambr\u00e9sy-L" }, { "family_name": "Gibson", "given_name": "S. J.", "clpid": "Gibson-S-J" }, { "family_name": "Tibbs", "given_name": "C. T.", "clpid": "Tibbs-C-T" }, { "family_name": "Noriega-Crespo", "given_name": "A.", "orcid": "0000-0002-6296-8960", "clpid": "Noriega-Crespo-A" }, { "family_name": "Molinari", "given_name": "S.", "clpid": "Molinari-S" }, { "family_name": "Carey", "given_name": "S. J.", "orcid": "0000-0002-0221-6871", "clpid": "Carey-S-J" }, { "family_name": "Ingalls", "given_name": "J. G.", "orcid": "0000-0003-4714-1364", "clpid": "Ingalls-J-G" }, { "family_name": "Natoli", "given_name": "P.", "clpid": "Natoli-P" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Fuller", "given_name": "G. A.", "orcid": "0000-0001-8509-1818", "clpid": "Fuller-G-A" } ], "abstract": "Herschel far-infrared continuum data obtained as part of the Hi-GAL survey have been used, together with the GLIMPSE 8\u2009\u03bcm and MIPSGAL 24\u2009\u03bcm data, to attempt the first 3D-decomposition of dust emission associated with atomic, molecular and ionized gas at 15\u2009arcmin angular resolution. Our initial test case is a 2 \u00d7 2 square degrees region centred on (l, b) = (30\u00b0, 0\u00b0), a direction that encompasses the origin point of the Scutum\u2013Crux Arm at the tip of the Galactic Bar. Coupling the IR maps with velocity maps specific for different gas phases (H\u2009i 21cm, ^(12)CO and ^(13)CO, and radio recombination lines), we estimate the properties of dust blended with each of the gas components and at different Galactocentric distances along the line of sight (LOS). A statistical Pearson's coefficients analysis is used to study the correlation between the column densities estimated for each gas component and the intensity of the IR emission. This analysis provides evidence that the 2 \u00d7 2 square degree field under consideration is characterized by the presence of a gas component not accounted for by the standard tracers, possibly associated with warm H_2 and cold H\u2009I. We demonstrate that the IR radiation in the range 8 < \u03bb < 500\u2009\u03bcm is systematically dominated by emission originating within the Scutum\u2013Crux Arm. By applying an inversion method, we recover the dust emissivities associated with atomic, molecular and ionized gas. Using the DustEM model, we fit the spectral energy distributions for each gas phase, and find average dust temperatures of T_(d,H I) = 18.82 \u00b1 0.47\u2009K, T_(d,H_2) = 18.84 \u00b1 1.06\u2009K and T_(d,H II) = 22.56 \u00b1 0.64\u2009K, respectively. We also obtain an indication for polycyclic aromatic hydrocarbons depletion in the diffuse ionized gas. We demonstrate the importance of including the ionized component in 3D-decompositions of the total IR emission. However, the main goal of this work is to discuss the impact of the missing column density associated with the dark gas component on the accurate evaluation of the dust properties, and to shed light on the limitations of the inversion method approach when this is applied to a small section of the Galactic plane and when the working resolution allows sufficient de-blending of the gas components along the LOS.", "doi": "10.1093/mnras/stu493", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2014-06-01", "series_number": "4", "volume": "440", "issue": "4", "pages": "3588-3612" }, { "id": "authors:wj7vq-qwn60", "collection": "authors", "collection_id": "wj7vq-qwn60", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180824-100034233", "type": "book_section", "title": "Synchrotron emission from molecular clouds", "author": [ { "family_name": "Strong", "given_name": "A. W.", "orcid": "0000-0003-3799-5489", "clpid": "Strong-A-W" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Murphy", "given_name": "E.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" } ], "abstract": "Observations of the properties of dense molecular clouds are critical in understanding the process of star-formation. One of the most important, but least understood, is the role of the magnetic fields. We discuss the possibility of using high-resolution, high-sensitivity radio observations to measure the in-situ synchrotron radiation from these molecular clouds. If the cosmic-ray (CR) particles penetrate clouds as expected, then we can measure the B-field strength directly using radio data. So far, this signature has never been detected from the collapsing clouds themselves and would be a unique probe of the magnetic field. Dense cores are typically \u223c 0.05 pc in size, corresponding to \u223carcsec at \u223ckpc distances, and flux density estimates are \u223c mJy at 1 GHz. They should be detectable, for example with the Square Kilometre Array.", "doi": "10.22323/1.221.0036", "publisher": "SISSA", "publication_date": "2014-06" }, { "id": "authors:8vacg-swg50", "collection": "authors", "collection_id": "8vacg-swg50", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180910-131320837", "type": "book_section", "title": "SKA studies of in situ synchrotron radiation from molecular clouds", "author": [ { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Beck", "given_name": "R.", "clpid": "Beck-R" }, { "family_name": "Crocker", "given_name": "R.", "clpid": "Crocker-R-M" }, { "family_name": "Crutcher", "given_name": "R. M.", "clpid": "Crutcher-R-M" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Ferri\u00e8re", "given_name": "K.", "clpid": "Ferri\u00e8re-K" }, { "family_name": "Fuller", "given_name": "G.", "orcid": "0000-0001-8509-1818", "clpid": "Fuller-G-A" }, { "family_name": "Jaffe", "given_name": "T.", "clpid": "Jaffe-T-R" }, { "family_name": "Jones", "given_name": "D. I.", "clpid": "Jones-D-I" }, { "family_name": "Leahy", "given_name": "J. P.", "clpid": "Leahy-J-P" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Peel", "given_name": "M. W.", "orcid": "0000-0003-3412-2586", "clpid": "Peel-M-W" }, { "family_name": "Orlando", "given_name": "E.", "clpid": "Orlando-E" }, { "family_name": "Porter", "given_name": "T.", "clpid": "Porter-T" }, { "family_name": "Protheroe", "given_name": "R. J.", "clpid": "Protheroe-R-J" }, { "family_name": "Robishaw", "given_name": "T.", "clpid": "Robishaw-T" }, { "family_name": "Strong", "given_name": "A. W.", "orcid": "0000-0003-3799-5489", "clpid": "Strong-A-W" }, { "family_name": "Watson", "given_name": "R. A.", "clpid": "Watson-R-A" }, { "family_name": "Yusef-Zadeh", "given_name": "F.", "clpid": "Yusef-Zadeh-F" } ], "abstract": "Observations of the properties of dense molecular clouds are critical in understanding the process of star-formation. One of the most important, but least understood, is the role of the magnetic fields. We discuss the possibility of using high-resolution, high-sensitivity radio observations with the SKA to measure for the first time the in-situ synchrotron radiation from these molecular clouds. If the cosmic-ray (CR) particles penetrate clouds as expected, then we can measure the B-field strength directly using radio data. So far, this signature has never been detected from the collapsing clouds themselves and would be a unique probe of the magnetic field. Dense cores are typically \u223c 0.05 pc in size, corresponding to \u223carcsec at \u223ckpc distances, and flux density estimates are \u223c mJy at 1 GHz. The SKA should be able to readily detect directly, for the first time, along lines-of-sight that are not contaminated by thermal emission or complex foreground/background synchrotron emission. Polarised synchrotron may also be detectable providing additional information about the regular/turbulent fields.", "doi": "10.22323/1.215.0102", "publisher": "SISSA", "publication_date": "2014-06" }, { "id": "authors:5zgq0-je861", "collection": "authors", "collection_id": "5zgq0-je861", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140401-101451734", "type": "article", "title": "The C-Band All-Sky Survey (C-BASS): design and implementation of the northern receiver", "author": [ { "family_name": "King", "given_name": "O. G.", "clpid": "King-O-G" }, { "family_name": "Jones", "given_name": "Michael E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Blackhurst", "given_name": "E. J.", "clpid": "Blackhurst-E-J" }, { "family_name": "Copley", "given_name": "C.", "clpid": "Copley-C" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Holler", "given_name": "C. M.", "clpid": "Holler-C-M" }, { "family_name": "Irfan", "given_name": "M. O.", "clpid": "Irfan-M-O" }, { "family_name": "John", "given_name": "J. J.", "clpid": "John-J-J" }, { "family_name": "Leahy", "given_name": "J. P.", "clpid": "Leahy-J-P" }, { "family_name": "Leech", "given_name": "J.", "clpid": "Leech-J" }, { "family_name": "Muchovej", "given_name": "S. J. C.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Stevenson", "given_name": "M. A.", "clpid": "Stevenson-M-A" }, { "family_name": "Taylor", "given_name": "Angela C.", "clpid": "Taylor-A-C" } ], "abstract": "The C-Band All-Sky Survey is a project to map the full sky in total intensity and linear polarization at 5\u2009GHz. The northern component of the survey uses a broad-band single-frequency analogue receiver fitted to a 6.1-m telescope at the Owens Valley Radio Observatory in California, USA. The receiver architecture combines a continuous-comparison radiometer and a correlation polarimeter in a single receiver for stable simultaneous measurement of both total intensity and linear polarization, using custom-designed analogue receiver components. The continuous-comparison radiometer measures the temperature difference between the sky and temperature-stabilized cold electrical reference loads. A cryogenic front-end is used to minimize receiver noise, with a system temperature of \u224830\u2009K in both linear polarization and total intensity. Custom cryogenic notch filters are used to counteract man-made radio frequency interference. The radiometer 1/f noise is dominated by atmospheric fluctuations, while the polarimeter achieves a 1/f noise knee frequency of 10 mHz, similar to the telescope azimuthal scan frequency.", "doi": "10.1093/mnras/stt2359", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2014-03-01", "series_number": "3", "volume": "438", "issue": "3", "pages": "2426-2439" }, { "id": "authors:t5spw-1vg89", "collection": "authors", "collection_id": "t5spw-1vg89", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130717-111400136", "type": "article", "title": "Constraints on Free-Free Emission from Anomalous Microwave Emission Sources in the Perseus Molecular Cloud", "author": [ { "family_name": "Tibbs", "given_name": "C. T.", "clpid": "Tibbs-C-T" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Mason", "given_name": "B. S.", "clpid": "Mason-B-S" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Watson", "given_name": "R. A.", "clpid": "Watson-R-A" } ], "abstract": "We present observations performed with the Green Bank Telescope at 1.4 and 5 GHz of three strips coincident with the anomalous microwave emission features previously identified in the Perseus molecular cloud at 33 GHz with the Very Small Array. With these observations we determine the level of the low frequency (~1-5 GHz) emission. We do not detect any significant extended emission in these regions and we compute conservative 3\u03c3 upper limits on the fraction of free-free emission at 33 GHz of 27%, 12%, and 18% for the three strips, indicating that the level of the emission at 1.4 and 5 GHz cannot account for the emission observed at 33 GHz. Additionally, we find that the low frequency emission is not spatially correlated with the emission observed at 33 GHz. These results indicate that the emission observed in the Perseus molecular cloud at 33 GHz, is indeed in excess over the low frequency emission, hence confirming its anomalous nature.", "doi": "10.1088/0004-637X/770/2/122", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2013-06-20", "series_number": "2", "volume": "770", "issue": "2", "pages": "Art. No. 122" }, { "id": "authors:p0j5y-a6k15", "collection": "authors", "collection_id": "p0j5y-a6k15", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130408-093637967", "type": "article", "title": "AMI Observations of the Anomalous Microwave Emission in the Perseus Molecular Cloud", "author": [ { "family_name": "Tibbs", "given_name": "C. T.", "clpid": "Tibbs-C-T" }, { "family_name": "Scaife", "given_name": "A. M. M.", "clpid": "Scaife-A-M-M" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Grainge", "given_name": "K. J. B.", "clpid": "Grainge-K-J-B" }, { "family_name": "Watson", "given_name": "R. A.", "clpid": "Watson-R-A" } ], "abstract": "We present observations of the known anomalous microwave emission region, G159.6\u201318.5, in the Perseus molecular cloud at 16 GHz performed with the Arcminute Microkelvin Imager Small Array. These are the highest angular resolution observations of G159.6\u201318.5 at microwave wavelengths. By combining these microwave data with infrared observations between 5.8 and 160 \u03bcm from the Spitzer Space Telescope, we investigate the existence of a microwave-infrared correlation on angular scales of ~2'. We find that the overall correlation appears to increase toward shorter infrared wavelengths, which is consistent with the microwave emission being produced by electric dipole radiation from small, spinning dust grains. We also find that the microwave-infrared correlation peaks at 24 \u03bcm (6.7\u03c3), suggesting that the microwave emission is originating from a population of stochastically heated small interstellar dust grains rather than polycyclic aromatic hydrocarbons.", "doi": "10.1088/0004-637X/768/2/98", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2013-05-10", "series_number": "2", "volume": "768", "issue": "2", "pages": "Art. No. 98" }, { "id": "authors:e4wtp-xge14", "collection": "authors", "collection_id": "e4wtp-xge14", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130717-111201896", "type": "article", "title": "Long-term variability of extragalactic radio sources in the Planck Early Release Compact Source Catalogue", "author": [ { "family_name": "Chen", "given_name": "X.", "orcid": "0000-0001-9152-6224", "clpid": "Chen-Xi-Tracy-IPAC" }, { "family_name": "Rachen", "given_name": "J. P.", "clpid": "Rachen-J-P" }, { "family_name": "L\u00f3pez-Caniego", "given_name": "M.", "clpid": "L\u00f3pez-Caniego-M" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Fuhrmann", "given_name": "L.", "clpid": "Fuhrmann-L" }, { "family_name": "Krichbaum", "given_name": "T. P.", "clpid": "Krichbaum-T-P" }, { "family_name": "Partridge", "given_name": "B.", "clpid": "Partridge-B" }, { "family_name": "Chen", "given_name": "X." } ], "abstract": "Combining measurements taken using the Wilkinson Microwave Anisotropy Probe (WMAP) from 2001 to 2008 with measurements taken using Planck from 2009 to 2010, we investigate the long-term flux density variability of extragalactic radio sources selected from the Planck Early Release Compact Source Catalogue. The single-year, single-frequency WMAP maps are used to estimate yearly-averaged flux densities of the sources in the four WMAP bands: Ka (33\u2009GHz), Q (41\u2009GHz), V (61\u2009GHz), and W (94\u2009GHz). We identify 82, 67, 32, and 15 sources respectively as variable at greater than 99% confidence level in these four bands. The amplitudes of variation are comparable between bands, and are not correlated with either the flux densities or the spectral indices of the sources. The number counts of WMAP Ka-band sources are stable from year to year despite the fluctuation caused by individual source variability. Most of our sources show strong correlation in variability between bands. Almost all the sources that show variability are blazars. We have attempted to fit two simple, four-parameter models to the time-series of 32 sources showing correlated variability at multiple frequencies \u2013 a long-term flaring model and a rotating-jet model. We find that 19 sources (60%) can be fit with the simple rotating-jet model, and ten of these also fit the simple long-term flaring model. The remaining 13 sources (40%) show more complex variability behaviour that is not consistent with either model. Extended radio galaxies in our sample show no sign of variability, as expected, with the exception of Pictor A for which we report evidence for a millimetre flare lasting between 2002 and 2010.", "doi": "10.1051/0004-6361/201220517", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2013-05", "volume": "553", "pages": "Art. No. A107" }, { "id": "authors:0tech-p3666", "collection": "authors", "collection_id": "0tech-p3666", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140131-100941995", "type": "article", "title": "Anomalous Microwave Emission: Theory, Modeling, and Observations", "author": [ { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Verstraete", "given_name": "Laurent", "clpid": "Verstraete-L" } ], "abstract": "Anomalous Microwave Emission (AME) was first identified\nin the late 1990s, through sensitive high frequency radio CMB\nobservations. The usual emission mechanisms (e.g., blackbody,\nsynchrotron, and free-free) did not appear to be able\nto account for the excess emission in the frequency range 10\u2013\n60GHz. Since then, a large body of observational evidence\nhas emerged showing that AME appears to be emitted both\nin the diffuse interstellar medium at large, and from specific\nclouds within our galaxy. Detections from star-forming\nregions in an external galaxy have also been made. Nevertheless,\ndetailed measurements have been difficult due to the frequency\nrange (difficult to observe from the ground) and confusion\nwith other emission mechanisms that emit in this frequent\nrange. The most promising candidate for the AME\nis electric dipole radiation from small spinning dust grains\n(spinning dust emission). This was first predicted in the\nlate 50s, with major developments in the theory over the\nlast 15 years. The theory predicts a peaked spectrum which\nemits at frequencies from about 10GHz to over 100GHz,\nbut with a wide range of peak frequencies and emissivities,\nwhich depend on the local environment and dust grain size\ndistribution. There is still significant debate about the true\nnature of the AME, and both observations and theory are still\nrelatively unexplored. An exciting possibility is to use detailed\nradio observations of spinning dust to study the interstellar\nmedium, in a complementary way to the optical, UV, and\ninfrared domains. This special issue is dedicated to the study\nof AME.", "doi": "10.1155/2013/134979", "issn": "1687-7969", "publisher": "Hindawi Publishing Corporation", "publication": "Advances in Astronomy", "publication_date": "2013", "volume": "2013", "pages": "Art. No. 134979" }, { "id": "authors:shwfb-wjq92", "collection": "authors", "collection_id": "shwfb-wjq92", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120604-081346731", "type": "article", "title": "A multi-wavelength investigation of RCW175: an H_II region harboring spinning dust emission", "author": [ { "family_name": "Tibbs", "given_name": "C. T.", "clpid": "Tibbs-C-T" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Compiegne", "given_name": "M.", "clpid": "Compiegne-M" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Alves", "given_name": "M. I. R.", "clpid": "Alves-M-I-R" }, { "family_name": "Flagey", "given_name": "N.", "orcid": "0000-0002-8763-1555", "clpid": "Flagey-N" }, { "family_name": "Shenoy", "given_name": "S.", "clpid": "Shenoy-S" }, { "family_name": "Noriega-Crespo", "given_name": "A.", "orcid": "0000-0002-6296-8960", "clpid": "Noriega-Crespo-A" }, { "family_name": "Carey", "given_name": "S.", "orcid": "0000-0002-0221-6871", "clpid": "Carey-S-J" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Molinari", "given_name": "S.", "clpid": "Molinari-S" }, { "family_name": "Elia", "given_name": "D.", "clpid": "Elia-D" }, { "family_name": "Pestalozzi", "given_name": "M.", "clpid": "Pestalozzi-M" }, { "family_name": "Schisano", "given_name": "E.", "clpid": "Schisano-E" } ], "abstract": "Using infrared, radio continuum and spectral observations, we performed a detailed investigation of\nthe Hii region RCW175. We determined that RCW175, which actually consists of two separate Hii\nregions, G29.1-0.7 and G29.0-0.6, is located at a distance of 3.2 \u00b1 0.2 kpc. Based on the observations\nwe infer that the more compact G29.0-0.6 is less evolved than G29.1-0.7 and was possibly produced as\na result of the expansion of G29.1-0.7 into the surrounding interstellar medium. We compute a star\nformation rate for RCW175 of (12.6 \u00b1 1.9) x 10^(-5) M_\u2299 yr^(-1), and identified 6 possible young stellar\nobject candidates within its vicinity. Additionally, we estimate that RCW175 contains a total dust\nmass of 215 \u00b1 53 M_\u2299.\nRCW175 has previously been identified as a source of anomalous microwave emission (AME), an\nexcess of emission at cm wavelengths often attributed to electric dipole radiation from the smallest\ndust grains. We find that the AME previously detected in RCW175 is not correlated with the smallest\ndust grains (polycyclic aromatic hydrocarbons or small carbonaceous dust grains), but rather with\nthe exciting radiation field within the region. This is a similar result to that found in the Perseus\nmolecular cloud, another region which harbors AME, suggesting that the radiation field may play a\npivotal role in the production of this new Galactic emission mechanism. Finally, we suggest that these\nobservations may hint at the importance of understanding the role played by the major gas ions in\nspinning dust models.", "doi": "10.1088/0004-637X/754/2/94", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-08-01", "series_number": "2", "volume": "754", "issue": "2", "pages": "Art. No. 94" }, { "id": "authors:wtfcw-t1b52", "collection": "authors", "collection_id": "wtfcw-t1b52", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120620-090826781", "type": "article", "title": "Foreground analysis using cross-correlations of external templates on the 7-year Wilkinson Microwave Anisotropy Probe data", "author": [ { "family_name": "Ghosh", "given_name": "Tuhin", "clpid": "Ghosh-T" }, { "family_name": "Banday", "given_name": "A. J.", "clpid": "Banday-A-J" }, { "family_name": "Jaffe", "given_name": "Tess", "clpid": "Jaffe-T-R" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Davies", "given_name": "Rod", "clpid": "Davies-R" }, { "family_name": "Davis", "given_name": "Richard", "clpid": "Davis-R" }, { "family_name": "Gorski", "given_name": "Krzysztof", "clpid": "Gorski-K" } ], "abstract": "Wilkinson Microwave Anisotropy Probe (WMAP) data when combined with ancillary data on free\u2013free, synchrotron and dust allow an improved understanding of the spectrum of emission from each of these components. Here we examine the sky variation at intermediate and high latitudes using a cross-correlation technique. In particular, we compare the observed emission in several global partitions of the sky plus 33 selected sky regions to three 'standard' templates. The regions are selected using a criterion based on the morphology of these template maps.\nThe synchrotron emission shows evidence of steepening between GHz frequencies and the WMAP bands. There are indications of spectral index variations across the sky, but the current data are not precise enough to accurately quantify this from region to region.\nThe H\u03b1 template correlated emission derived from the global fits shows clear evidence of deviation from a free\u2013free spectrum. If this spectrum is decomposed into a contribution from both free\u2013free and spinning dust emission in the warm ionized medium of the Galaxy, the derived free\u2013free emissivity corresponds to a mean electron temperature of \u223c6000 K (a value critically dependent on the impact of dust absorption on the H\u03b1 intensity), and the spinning dust emission has a peak emission in intensity typically in the range 40\u201350 GHz. However, the analysis of the smaller regions is generally unrevealing and the analysis presented here does not unambiguously demonstrate the presence of spinning dust emission in the warm ionized medium, as advocated by Dobler & Finkbeiner.\nThe anomalous microwave emission associated with dust is detected at high significance in most of the 33 fields studied. The anomalous emission correlates well with the Finkbeiner et al. model 8 predictions (FDS8) at 94 GHz, and is well described globally by a power-law emission model with an effective spectral index between 20 and 60 GHz of \u03b2\u2248\u22122.7. It is clear that attempts to explain the emission by spinning dust models require multiple components, which presumably relates to a complex mix of emission regions along a given line of sight. An enhancement of the thermal dust contribution over the FDS8 predictions by a factor \u223c1.2 is required with such models. Furthermore, the emissivity varies by a factor of \u223c50 per cent from cloud to cloud relative to the mean.\nThe significance of these results for the correction of cosmic microwave background data for Galactic foreground emission is discussed.", "doi": "10.1111/j.1365-2966.2012.20875.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2012-06", "series_number": "4", "volume": "422", "issue": "4", "pages": "3617-3642" }, { "id": "authors:s97bv-4r516", "collection": "authors", "collection_id": "s97bv-4r516", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180427-155707605", "type": "article", "title": "On the Limitations of the Anomalous Microwave Emission Emissivity", "author": [ { "family_name": "Tibbs", "given_name": "Christopher T.", "clpid": "Tibbs-C-T" }, { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" } ], "abstract": "Many studies of anomalous microwave emission (AME) have computed an AME emissivity to compare the strength of the AME detected in different regions. Such a value is usually defined as the ratio between the intensity of the AME at 1\u2009cm and the thermal dust emission at 100\u2009\u03bcm. However, as studies of Galactic dust emission have shown, the intensity of the thermal dust emission at 100\u2009\u03bcm is strongly dependent on the dust temperature, which has severe implications for the AME emissivity defined in this way. In this work, we illustrate and quantify this effect and find that the AME emissivity decreases by a factor of 11.1 between dust temperatures of 20 and 30\u2009K. We, therefore, conclude that computing the AME emissivity relative to the 100\u2009\u03bcm emission does not allow for accurate comparisons between the AME observed in different environments. With this in mind, we investigate the use of other tracers of the dust emission with which to compute the AME emissivity and we ultimately conclude that, despite the difficulty in deriving its value, the column density of the dust would be the most suitable quantity with which to compute the AME emissivity.", "doi": "10.1155/2012/124931", "issn": "1687-7969", "publisher": "Hindawi Publishing Corporation", "publication": "Advances in Astronomy", "publication_date": "2012", "volume": "2012", "pages": "Art. No. 124931" }, { "id": "authors:rx1wa-v1769", "collection": "authors", "collection_id": "rx1wa-v1769", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120217-113352431", "type": "article", "title": "Spitzer characterization of dust in an anomalous emission region: the Perseus cloud", "author": [ { "family_name": "Tibbs", "given_name": "C. T.", "clpid": "Tibbs-C-T" }, { "family_name": "Flagey", "given_name": "N.", "orcid": "0000-0002-8763-1555", "clpid": "Flagey-N" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Compi\u00e8gne", "given_name": "M.", "clpid": "Compi\u00e8gne-M" }, { "family_name": "Shenoy", "given_name": "S.", "clpid": "Shenoy-S" }, { "family_name": "Carey", "given_name": "S.", "orcid": "0000-0002-0221-6871", "clpid": "Carey-S-J" }, { "family_name": "Noriega-Crespo", "given_name": "A.", "orcid": "0000-0002-6296-8960", "clpid": "Noriega-Crespo-A" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Ali-Ha\u00efmoud", "given_name": "Y.", "clpid": "Ali-Ha\u00efmoud-Y" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Hirata", "given_name": "C. M.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Watson", "given_name": "R. A.", "clpid": "Watson-R-A" } ], "abstract": "Anomalous microwave emission is known to exist in the Perseus cloud. One of the most promising candidates to explain this excess of emission is electric dipole radiation from rapidly rotating very small dust grains, commonly referred to as spinning dust. Photometric data obtained with the Spitzer Space Telescope have been reprocessed and used in conjunction with the dust emission model dustem to characterize the properties of the dust within the cloud. This analysis has allowed us to constrain spatial variations in the strength of the interstellar radiation field (\u03c7_(ISRF)), the mass abundances of the polycyclic aromatic hydrocarbons (PAHs) and the very small grains (VSGs) relative to the big grains (Y_(PAH) and Y_(VSG)), the column density of hydrogen (N_H) and the equilibrium dust temperature (T_(dust)). The parameter maps of Y_(PAH), Y_(VSG) and \u03c7_(ISRF) are the first of their kind to be produced for the Perseus cloud, and we used these maps to investigate the physical conditions in which anomalous emission is observed. We find that in regions of anomalous emission the strength of the ISRF, and consequently the equilibrium temperature of the dust, is enhanced while there is no significant variation in the abundances of the PAHs and the VSGs or the column density of hydrogen. We interpret these results as an indication that the enhancement in \u03c7_(ISRF) might be affecting the properties of the small stochastically heated dust grains resulting in an increase in the spinning dust emission observed at 33 GHz. This is the first time that such an investigation has been performed, and we believe that this type of analysis creates a new perspective in the field of anomalous emission studies, and represents a powerful new tool for constraining spinning dust models.", "doi": "10.1111/j.1365-2966.2011.19605.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2011-12", "series_number": "3", "volume": "418", "issue": "3", "pages": "1889-1900" }, { "id": "authors:sfjdv-ssn77", "collection": "authors", "collection_id": "sfjdv-ssn77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120217-114701245", "type": "article", "title": "The Cosmic Background Imager 2", "author": [ { "family_name": "Taylor", "given_name": "Angela C.", "clpid": "Taylor-A-C" }, { "family_name": "Jones", "given_name": "Michael E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Allison", "given_name": "James R.", "clpid": "Allison-J-R" }, { "family_name": "Angelakis", "given_name": "Emmanouil", "orcid": "0000-0001-7327-5441", "clpid": "Angelakis-E" }, { "family_name": "Bond", "given_name": "J. Richard", "orcid": "0000-0003-2358-9949", "clpid": "Bond-J-R" }, { "family_name": "Bronfman", "given_name": "Leonardo", "clpid": "Bronfman-L" }, { "family_name": "Bustos", "given_name": "Ricardo", "clpid": "Bustos-R" }, { "family_name": "Davis", "given_name": "Richard J.", "clpid": "Davis-R-J" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Leech", "given_name": "Jamie", "clpid": "Leech-J" }, { "family_name": "Mason", "given_name": "Brian S.", "clpid": "Mason-B-S" }, { "family_name": "Myers", "given_name": "Steven T.", "clpid": "Myers-Steven-Theodore" }, { "family_name": "Pearson", "given_name": "Timothy J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Readhead", "given_name": "Anthony C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Reeves", "given_name": "Rodrigo", "orcid": "0000-0001-5704-271X", "clpid": "Reeves-R-A" }, { "family_name": "Shepherd", "given_name": "Martin C.", "clpid": "Shepherd-Martin-C" }, { "family_name": "Sievers", "given_name": "Jonathan L.", "clpid": "Sievers-J-L" } ], "abstract": "We describe an upgrade to the Cosmic Background Imager instrument to increase its surface brightness sensitivity at small angular scales. The upgrade consisted of replacing the 13 0.9-m antennas with 1.4-m antennas incorporating a novel combination of design features, which provided excellent sidelobe and spillover performance for low manufacturing cost. Off-the-shelf spun primaries were used, and the secondary mirrors were oversized and shaped relative to a standard Cassegrain in order to provide an optimum compromise between aperture efficiency and low spillover lobes. Low-order distortions in the primary mirrors were compensated for by custom machining of the secondary mirrors. The secondaries were supported on a transparent dielectric foam cone to minimize scattering. The antennas were tested in the complete instrument, and the beam shape and spillover noise contributions were as expected. We demonstrate the performance of the telescope and the intercalibration with the previous system using observations of the Sunyaev\u2013Zel'dovich effect in the cluster Abell 1689. The enhanced instrument has been used to study the cosmic microwave background, the Sunyaev\u2013Zel'dovich effect and diffuse Galactic emission.", "doi": "10.1111/j.1365-2966.2011.19661.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2011-12", "series_number": "4", "volume": "418", "issue": "4", "pages": "2720-2729" }, { "id": "authors:w9my7-nk392", "collection": "authors", "collection_id": "w9my7-nk392", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110815-085844658", "type": "article", "title": "Dust-correlated cm wavelength continuum emission from translucent clouds \u03b6 Oph and LDN 1780", "author": [ { "family_name": "Vidal", "given_name": "M.", "clpid": "Vidal-M" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Witt", "given_name": "A. N.", "clpid": "Witt-A-N" }, { "family_name": "Castellanos", "given_name": "P.", "clpid": "Castellanos-P" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Cabrera", "given_name": "G.", "clpid": "Cabrera-G" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K-A" }, { "family_name": "Allison", "given_name": "J. R.", "clpid": "Allison-J-R" }, { "family_name": "Bond", "given_name": "J. R.", "orcid": "0000-0003-2358-9949", "clpid": "Bond-J-R" }, { "family_name": "Bronfman", "given_name": "L.", "clpid": "Bronfman-L" }, { "family_name": "Bustos", "given_name": "R.", "clpid": "Bustos-R" }, { "family_name": "Jones", "given_name": "M. E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Reeves", "given_name": "R.", "orcid": "0000-0001-5704-271X", "clpid": "Reeves-R-A" }, { "family_name": "Sievers", "given_name": "J. L.", "clpid": "Sievers-J-L" }, { "family_name": "Taylor", "given_name": "A. C.", "clpid": "Taylor-A-C" } ], "abstract": "The diffuse cm wave IR-correlated signal, the 'anomalous' CMB foreground, is thought to arise in the dust in cirrus clouds. We present Cosmic Background Imager (CBI) cm wave data of two translucent clouds, \u03b6 Oph and LDN 1780 with the aim of characterizing the anomalous emission in the translucent cloud environment.\n\nIn \u03b6 Oph, the measured brightness at 31 GHz is 2.4\u03c3 higher than an extrapolation from 5-GHz measurements assuming a free\u2013free spectrum on 8 arcmin scales. The SED of this cloud on angular scales of 1\u00b0 is dominated by free\u2013free emission in the cm range. In LDN 1780 we detected a 3\u03c3 excess in the SED on angular scales of 1\u00b0 that can be fitted using a spinning dust model. In this cloud, there is a spatial correlation between the CBI data and IR images, which trace dust. The correlation is better with near-IR templates (IRAS 12 and 25 \u03bcm) than with IRAS 100 \u03bcm, which suggests a very small grain origin for the emission at 31 GHz.\n\nWe calculated the 31-GHz emissivities in both clouds. They are similar and have intermediate values between that of cirrus clouds and dark clouds. Nevertheless, we found an indication of an inverse relationship between emissivity and column density, which further supports the VSGs origin for the cm emission since the proportion of big relative to small grains is smaller in diffuse clouds.", "doi": "10.1111/j.1365-2966.2011.18562.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2011-07", "series_number": "3", "volume": "414", "issue": "3", "pages": "2424-2435" }, { "id": "authors:wtehy-8ft39", "collection": "authors", "collection_id": "wtehy-8ft39", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110322-143934107", "type": "article", "title": "Galactic cold cores. II. Herschel study of the extended dust emission around the first Planck detections", "author": [ { "family_name": "Juvela", "given_name": "M.", "clpid": "Juvela-M" }, { "family_name": "Ristorcelli", "given_name": "I.", "clpid": "Ristorcelli-I" }, { "family_name": "Pelkonen", "given_name": "V.-M.", "orcid": "0000-0002-8898-1047", "clpid": "Pelkonen-Veli-Matti" }, { "family_name": "Marshall", "given_name": "D. J.", "clpid": "Marshall-D-J" }, { "family_name": "Montier", "given_name": "L. A.", "clpid": "Montier-L-A" }, { "family_name": "Bernard", "given_name": "J.-P.", "clpid": "Bernard-J-P" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Lunttila", "given_name": "T.", "clpid": "Lunttila-T" }, { "family_name": "Abergel", "given_name": "A.", "clpid": "Abergel-A" }, { "family_name": "Andr\u00e9", "given_name": "Ph.", "clpid": "Andr\u00e9-P" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Dupac", "given_name": "X.", "clpid": "Dupac-X" }, { "family_name": "Malinen", "given_name": "J.", "clpid": "Malinen-J" }, { "family_name": "Martin", "given_name": "P.", "orcid": "0000-0002-5236-3896", "clpid": "Martin-P-G" }, { "family_name": "McGehee", "given_name": "P.", "orcid": "0000-0003-0948-6716", "clpid": "McGehee-P-M" }, { "family_name": "Pagani", "given_name": "L.", "clpid": "Pagani-L" }, { "family_name": "Ysard", "given_name": "N.", "clpid": "Ysard-N" }, { "family_name": "Zavagno", "given_name": "A.", "clpid": "Zavagno-A" } ], "abstract": "Context. Within the project Galactic cold cores we are carrying out Herschel photometric observations of cold interstellar clouds detected with the Planck satellite. The three fields observed as part of the Herschel science demonstration phase (SDP) provided the first glimpse into the nature of these sources. The aim of the project is to derive the physical properties of the full cold core population revealed by Planck. \nAims. We examine the properties of the dust emission within the three fields observed during the SDP. We determine the dust sub-millimetre opacity, look for signs of spatial variations in the dust spectral index, and estimate how the apparent variations of the parameters could be affected by different sources of uncertainty.\nMethods. We use the Herschel observations where the zero point of the surface brightness scale is set with the help of the Planck satellite data. We derive the colour temperature and column density maps of the regions and determine the dust opacity by a comparison with extinction measurements. By simultaneously fitting the colour temperature and the dust spectral index values we look for spatial variations in the apparent dust properties. With a simple radiative transfer model we estimate to what extent these can be explained by line-of-sight temperature variations, without changes in the dust grain properties. \nResults. The analysis of the dust emission reveals cold and dense clouds that coincide with the Planck sources and confirm those detections. The derived dust opacity varies in the range \u03ba(250 \u2009 \u03bcm) ~ 0.05\u22120.2\u2009cm^2\u2009g^(-1), higher values being observed preferentially in regions of high column density. The average dust spectral index \u03b2 is ~1.9\u22122.2. There are indications that \u03b2 increases towards the coldest regions. The spectral index decreases strongly near internal heating sources but, according to radiative transfer models, this can be explained by the line-of-sight temperature variations without a change in the dust properties.", "doi": "10.1051/0004-6361/201015916", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2011-03", "volume": "527", "pages": "Art. No. A111" }, { "id": "authors:28jjb-j6k81", "collection": "authors", "collection_id": "28jjb-j6k81", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110322-091232450", "type": "article", "title": "Dust-correlated centimetre-wave radiation from the M78 reflection nebula", "author": [ { "family_name": "Castellanos", "given_name": "Pablo", "clpid": "Castellanos-P" }, { "family_name": "Casassus", "given_name": "Simon", "clpid": "Casassus-S" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Vidal", "given_name": "Mat\u00edas", "clpid": "Vidal-M" }, { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Cleary", "given_name": "Kieran", "clpid": "Cleary-K" }, { "family_name": "Davies", "given_name": "Rodney D.", "clpid": "Davies-R-D" }, { "family_name": "Davis", "given_name": "Richard J.", "clpid": "Davis-R-J" }, { "family_name": "White", "given_name": "Glenn J.", "clpid": "White-G-J" }, { "family_name": "Taylor", "given_name": "Angela", "clpid": "Taylor-A" } ], "abstract": "An anomalous radio continuum component at cm-wavelengths has been observed in various sources, including dark clouds. This continuum component represents a new property of the interstellar medium. In this work, we focus on one particular dark cloud, the bright reflection nebula M78. The main goal of this work is to investigate the cm-wave continuum emission in a prominent molecular cloud, nearby and with complementary observational data. We acquired Cosmic Background Imager (CBI) visibility data of M78 at 31 GHz with an angular resolution of ~5.8 arcmin, and CBI2 data at an angular resolution of ~4.2 arcmin. A morphological analysis was undertaken to search for possible correlations with templates that trace different emission mechanisms. Using data from Wilkinson Microwave Anisotropy Probe and the Rhodes/HartRAO 2326-MHz survey, we constructed the spectral energy distribution (SED) of M78 in a 45-arcmin circular aperture. We used results from the literature to constrain the physical conditions and the stellar content. The 5\u201331 GHz spectral index in flux density (\u03b1 = 1.89 \u00b1 0.15) is significantly different from optically thin free\u2013free values. We also find closer morphological agreement with IR dust tracers than with free\u2013free sources. Dust-correlated cm-wave emission that is not due to free\u2013free is significant at small scales (CBI resolutions). However, a free\u2013free background dominates at cm-wavelengths on large scales (~1\u00b0). We correct for this uniform background by differencing against a set of reference fields. The differenced SED of M78 shows excess emission at 10\u201370 GHz over free\u2013free and a modified blackbody, at 3.4\u03c3. The excess is matched by the spinning dust model from Draine & Lazarian.", "doi": "10.1111/j.1365-2966.2010.17743.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2011-02", "series_number": "2", "volume": "411", "issue": "2", "pages": "1137-1150" }, { "id": "authors:x7b4t-wbb15", "collection": "authors", "collection_id": "x7b4t-wbb15", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101029-083848929", "type": "article", "title": "Infrared-correlated 31-GHz radio emission from Orion East", "author": [ { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Allison", "given_name": "J. R.", "clpid": "Allison-J-R" }, { "family_name": "Bustos", "given_name": "R.", "clpid": "Bustos-R" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Jones", "given_name": "M. E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Reeves", "given_name": "R.", "clpid": "Reeves-R" }, { "family_name": "Taylor", "given_name": "A. C.", "clpid": "Taylor-A-C" }, { "family_name": "Tibbs", "given_name": "C. T.", "clpid": "Tibbs-C-T" }, { "family_name": "Watson", "given_name": "R. A.", "clpid": "Watson-R-A" } ], "abstract": "Lynds dark cloud LDN1622 represents one of the best examples of anomalous dust emission, possibly originating from small spinning dust grains. We present Cosmic Background Imager (CBI) 31-GHz data of LDN1621, a diffuse dark cloud to the north of LDN1622 in a region known as Orion East. A broken ring-like structure with diameter \u224820 arcmin of diffuse emission is detected at 31 GHz, at \u224820\u201330 mJy beam^(\u22121) with an angular resolution of \u22485 arcmin. The ring-like structure is highly correlated with far-infrared (FIR) emission at 12\u2013100 \u03bcm with correlation coefficients of r \u2248 0.7\u20130.8, significant at ~10\u03c3. The FIR-correlated\nemission at 31 GHz therefore appears to be mostly due to radiation associated with dust. Multifrequency data are used to place constraints on other components of emission that could be contributing to the 31-GHz flux. An analysis of the GB6 survey maps at 4.85 GHz yields a 3\u03c3 upper limit on free\u2013free emission of 7.2 mJy beam^(\u22121) (\u227e30 per cent of the observed flux) at the CBI resolution. The bulk of the 31-GHz flux therefore appears to be mostly due to dust radiation. Aperture photometry, at an angular resolution of 13 arcmin and with an aperture of diameter 30 arcmin, allowed the use of IRAS maps and the Wilkinson Microwave\nAnisotropy Probe 5-yr W-band map at 93.5 GHz. A single modified blackbody model was fitted to the data to estimate the contribution from thermal dust, which amounts to ~10 per cent at 31 GHz. In this model, an excess of 1.52 \u00b1 0.66 Jy (2.3\u03c3) is seen at 31 GHz. Correlations with the IRAS 100 \u03bcm gave a coupling coefficient of 18.1 \u00b1 4.4 \u03bcK (MJy sr^(\u22121))^(\u22121), consistent with the values found for LDN1622.", "doi": "10.1111/j.1365-2966.2010.17079.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2010-10-01", "series_number": "4", "volume": "407", "issue": "4", "pages": "2223-2229" }, { "id": "authors:36gqh-gfe09", "collection": "authors", "collection_id": "36gqh-gfe09", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160506-163548043", "type": "book_section", "title": "Prospects for polarized foreground removal", "book_title": "CMB Polarization Workshop; Theory and Foregrounds, CMBPol Mission Concept", "author": [ { "family_name": "Dunkley", "given_name": "J.", "clpid": "Dunkley-J" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Rocha", "given_name": "G.", "orcid": "0000-0002-4150-8076", "clpid": "Rocha-G-M" }, { "family_name": "Vaillancourt", "given_name": "J. E.", "clpid": "Vaillancourt-J-E" } ], "contributor": [ { "family_name": "Dodelson", "given_name": "Scott", "clpid": "Dodelson-S" }, { "family_name": "Baumann", "given_name": "Daniel", "clpid": "Baumann-D" }, { "family_name": "Cooray", "given_name": "Asantha", "clpid": "Cooray-A" }, { "family_name": "Dunkley", "given_name": "Joanna", "clpid": "Dunkley-J" }, { "family_name": "Fraisse", "given_name": "Aur\u00e9lien", "clpid": "Fraisse-A-A" }, { "family_name": "Jackson", "given_name": "Mark G.", "clpid": "Jackson-Mark-G" }, { "family_name": "Kogut", "given_name": "Alan", "clpid": "Kogut-A" }, { "family_name": "Krauss", "given_name": "Lawrence", "clpid": "Krauss-L-M" }, { "family_name": "Zaldarriaga", "given_name": "Matias", "clpid": "Zaldarriaga-M" }, { "family_name": "Smith", "given_name": "Kendrick", "clpid": "Smith-K-M" } ], "abstract": "In this report we discuss the impact of polarized foregrounds on a future CMBPol satellite mission. We review our current knowledge of Galactic polarized emission at microwave frequencies, including synchrotron and thermal dust emission. We use existing data and our understanding of the physical behavior of the sources of foreground emission to generate sky templates, and start to assess how well primordial gravitational wave signals can be separated from foreground contaminants for a CMBPol mission. At the estimated foreground minimum of \u223c100 GHz, the polarized foregrounds are expected to be lower than a primordial polarization signal with tensor\u2010to\u2010scalar ratio r = 0.01, in a small patch (\u223c1%) of the sky known to have low Galactic emission. Over 75% of the sky we expect the foreground amplitude to exceed the primordial signal by about a factor of eight at the foreground minimum and on scales of two degrees. Only on the largest scales does the polarized foreground amplitude exceed the primordial signal by a larger factor of about 20. The prospects for detecting an r = 0.01 signal including degree\u2010scale measurements appear promising, with 5\u03c3_r\u223c0.003 forecast from multiple methods. A mission that observes a range of scales offers better prospects from the foregrounds perspective than one targeting only the lowest few multipoles. We begin to explore how optimizing the composition of frequency channels in the focal plane can maximize our ability to perform component separation, with a range of typically 40 \u2272 \u03bd \u2272 300 GHz preferred for ten channels. Foreground cleaning methods are already in place to tackle a CMBPol mission data set, and further investigation of the optimization and detectability of the primordial signal will be useful for mission design.", "doi": "10.1063/1.3160888", "isbn": "978-0-7354-0678-0", "publisher": "American Institute of Physics", "place_of_publication": "Melville, NY", "publication_date": "2009-06-09", "pages": "222-264" }, { "id": "authors:4pjg9-qrp22", "collection": "authors", "collection_id": "4pjg9-qrp22", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090818-152816437", "type": "article", "title": "A Limit on the Polarized Anomalous Microwave Emission of Lynds 1622", "author": [ { "family_name": "Mason", "given_name": "B. S.", "clpid": "Mason-B-S" }, { "family_name": "Robishaw", "given_name": "T.", "clpid": "Robishaw-T" }, { "family_name": "Heiles", "given_name": "C.", "clpid": "Heiles-C" }, { "family_name": "Finkbeiner", "given_name": "D.", "clpid": "Finkbeiner-D" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" } ], "abstract": "The dark cloud Lynds 1622 is one of a few specific sites in the Galaxy where, relative to observed free-free and vibrational dust emission, there is a clear excess of microwave emission. In order to constrain models for this microwave emission, and to better establish the contribution which it might make to ongoing and near-future microwave background polarization experiments, we have used the Green Bank Telescope to search for linear polarization at 9.65 Ghz toward Lynds 1622. We place a 95.4% upper limit of 88 \u03bcK (123 \u03bcK at 99.7% confidence) on the total linear polarization of this source averaged over a 1.'3 FWHM beam. Relative to the observed level of anomalous emission in Stokes I these limits correspond to fractional linear polarizations of 2.7% and 3.5%.", "doi": "10.1088/0004-637X/697/2/1187", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-06-01", "series_number": "2", "volume": "697", "issue": "2", "pages": "1187-1193" }, { "id": "authors:pz2tq-fez09", "collection": "authors", "collection_id": "pz2tq-fez09", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090720-111934514", "type": "article", "title": "A refined model for spinning dust radiation", "author": [ { "family_name": "Ali-Ha\u00efmoud", "given_name": "Yacine", "clpid": "Ali-Ha\u00efmoud-Y" }, { "family_name": "Hirata", "given_name": "Christopher M.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" } ], "abstract": "We present a comprehensive treatment of the spectrum of electric dipole emission from spinning dust grains, updating the commonly used model of Draine & Lazarian. Grain angular velocity distributions are computed using the Fokker\u2013Planck equation; we revisit the drift and diffusion coefficients for the major torques on the grain, including collisions, grain-plasma interactions and infrared emission. We use updated grain optical properties and size distributions. The theoretical formalism is implemented in the companion code, spdust, which is publicly available. The effect of some environmental and grain parameters on the emissivity is shown and analysed.", "doi": "10.1111/j.1365-2966.2009.14599.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2009-05", "series_number": "2", "volume": "395", "issue": "2", "pages": "1055-1078" }, { "id": "authors:225z7-2x297", "collection": "authors", "collection_id": "225z7-2x297", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:DICapj09", "type": "article", "title": "Anomalous Microwave Emission from the H II Region RCW175", "author": [ { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Allison", "given_name": "J. R.", "clpid": "Allison-J-R" }, { "family_name": "Bond", "given_name": "J. R.", "orcid": "0000-0003-2358-9949", "clpid": "Bond-J-R" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Jones", "given_name": "M. E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Mason", "given_name": "B. S.", "clpid": "Mason-B-S" }, { "family_name": "Myers", "given_name": "S. T.", "clpid": "Myers-Steven-Theodore" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Sievers", "given_name": "J. L.", "clpid": "Sievers-J-L" }, { "family_name": "Taylor", "given_name": "A. C.", "clpid": "Taylor-A-C" }, { "family_name": "Todorovi\u0107", "given_name": "M.", "clpid": "Todorovi\u0107-M" }, { "family_name": "White", "given_name": "G. J.", "clpid": "White-G-J" }, { "family_name": "Wilkinson", "given_name": "P. N.", "clpid": "Wilkinson-P-N" } ], "abstract": "We present evidence for anomalous microwave emission in the RCW175 H II region. Motivated by 33 GHz 13' resolution data from the Very Small Array (VSA), we observed RCW175 at 31 GHz with the Cosmic Background Imager (CBI) at a resolution of 4'. The region consists of two distinct components, G29.0-0.6 and G29.1-0.7, which are detected at high signal-to-noise ratio. The integrated flux density is 5.97 \u00b1 0.30 Jy at 31 GHz, in good agreement with the VSA. The 31 GHz flux density is 3.28 \u00b1 0.38 Jy (8.6\u03c3) above the expected value from optically thin free-free emission based on lower frequency radio data and thermal dust constrained by IRAS and WMAP data. Conventional emission mechanisms such as optically thick emission from ultracompact H II regions cannot easily account for this excess. We interpret the excess as evidence for electric dipole emission from small spinning dust grains, which does provide an adequate fit to the data.", "doi": "10.1088/0004-637X/690/2/1585", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-01-10", "series_number": "2", "volume": "690", "issue": "2", "pages": "1585-1589" }, { "id": "authors:2tewb-nvq43", "collection": "authors", "collection_id": "2tewb-nvq43", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:CASmnras08", "type": "article", "title": "Centimetre-wave continuum radiation from the \u03c1 Ophiuchi molecular cloud", "author": [ { "family_name": "Casassus", "given_name": "Simon", "clpid": "Casassus-S" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Cleary", "given_name": "Kieran", "clpid": "Cleary-K" }, { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Etxaluze", "given_name": "Mireya", "clpid": "Etxaluze-M" }, { "family_name": "Lim", "given_name": "Tanya", "clpid": "Lim-Tanya-L" }, { "family_name": "White", "given_name": "Glenn J.", "clpid": "White-G-J" }, { "family_name": "Burton", "given_name": "Michael", "clpid": "Burton-M" }, { "family_name": "Indermuehle", "given_name": "Balt", "clpid": "Indermuehle-B" }, { "family_name": "Stahl", "given_name": "Otmar", "clpid": "Stahl-O" }, { "family_name": "Roche", "given_name": "Patrick", "clpid": "Roche-P" } ], "abstract": "The \u03c1 Oph molecular cloud is undergoing intermediate-mass star formation. Ultraviolet radiation from its hottest young stars heats and dissociates exposed layers, but does not ionize hydrogen. Only faint radiation from the Rayleigh-Jeans tail of \u223c10\u2013100 K dust is expected at wavelengths longwards of \u223c3 mm. Yet cosmic background imager (CBI) observations reveal that the \u03c1 Oph W photodissociation region is surprisingly bright at centimetre wavelengths. We searched for interpretations consistent with the Wilkinson Microwave Anisotropy Probe radio spectrum, new Infrared Space Observatory-Long Wavelength Spectrograph (LWS) parallel mode images and archival Spitzer data. Dust-related emission mechanisms at 1 cm, as proposed by Draine & Lazarian, are a possibility. But a magnetic enhancement of the grain opacity at 1 cm is inconsistent with the morphology of the dust column maps Nd and the lack of detected polarization. Spinning dust, or electric-dipole radiation from spinning very small grains (VSGs), comfortably explains the radio spectrum, although not the conspicuous absence from the CBI data of the infrared circumstellar nebulae around the B-type stars S1 and SR3. Allowing for VSG depletion can marginally reconcile spinning dust with the data. As an alternative interpretation, we consider the continuum from residual charges in \u03c1 Oph W, where most of carbon should be photoionized by the close binary HD 147889 (B2IV, B3IV). Electron densities of \u223c10^2 cm^\u22123 , or H-nucleus densities nH > 10^6 cm^\u22123 , are required to interpret \u03c1 Oph W as the C ii Str\u00f6mgren sphere of HD 147889. However, the observed steep and positive low-frequency spectral index would then imply optically thick emission from an hitherto unobserved ensemble of dense clumps or sheets with a filling factor of \u223c10^\u22124 and nH\u223c 10^7 cm^\u22123 .", "doi": "10.1111/j.1365-2966.2008.13954", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2008-12-11", "series_number": "3", "volume": "391", "issue": "3", "pages": "1075-1090" }, { "id": "authors:3bhxp-37e34", "collection": "authors", "collection_id": "3bhxp-37e34", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090526-094724857", "type": "article", "title": "Component separation methods for the PLANCK mission", "author": [ { "family_name": "Leach", "given_name": "S. M.", "clpid": "Leach-S-M" }, { "family_name": "Cardoso", "given_name": "J.-F.", "clpid": "Cardoso-J-F" }, { "family_name": "Baccigalupi", "given_name": "C.", "clpid": "Baccigalupi-C" }, { "family_name": "Barreiro", "given_name": "R. B.", "orcid": "0000-0002-6139-4272", "clpid": "Barreiro-R-B" }, { "family_name": "Betoule", "given_name": "M.", "clpid": "Betoule-M" }, { "family_name": "Bobin", "given_name": "J.", "clpid": "Bobin-J" }, { "family_name": "Bonaldi", "given_name": "A.", "clpid": "Bonaldi-A" }, { "family_name": "Delabrouille", "given_name": "J.", "clpid": "Delabrouille-J" }, { "family_name": "de Zotti", "given_name": "G.", "orcid": "0000-0003-2868-2595", "clpid": "De-Zotti-G" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Eriksen", "given_name": "H. K.", "clpid": "Eriksen-H-K" }, { "family_name": "Gonz\u00e1lez-Nuevo", "given_name": "J.", "clpid": "Gonz\u00e1lez-Nuevo-J" }, { "family_name": "Hansen", "given_name": "F. K.", "clpid": "Hansen-F-K" }, { "family_name": "Herranz", "given_name": "D.", "clpid": "Herranz-D" }, { "family_name": "Le Jeune", "given_name": "M.", "clpid": "Le-Jeune-M" }, { "family_name": "L\u00f3pez-Caniego", "given_name": "M.", "clpid": "L\u00f3pez-Caniego-M" }, { "family_name": "Mart\u00ednez-Gonz\u00e1lez", "given_name": "E.", "clpid": "Mart\u00ednez-Gonz\u00e1lez-E" }, { "family_name": "Massardi", "given_name": "M.", "clpid": "Massardi-M" }, { "family_name": "Melin", "given_name": "J.-B.", "clpid": "Melin-J-B" }, { "family_name": "Miville-Desch\u00eanes", "given_name": "M.-A.", "clpid": "Miville-Desch\u00eanes-M-A" }, { "family_name": "Patanchon", "given_name": "G.", "clpid": "Patanchon-G" }, { "family_name": "Prunet", "given_name": "S.", "clpid": "Prunet-S" }, { "family_name": "Ricciardi", "given_name": "S.", "clpid": "Ricciardi-S" }, { "family_name": "Salerno", "given_name": "E.", "clpid": "Salerno-E" }, { "family_name": "Sanz", "given_name": "J. L.", "clpid": "Sanz-J-L" }, { "family_name": "Starck", "given_name": "J.-L.", "clpid": "Starck-J-L" }, { "family_name": "Stivoli", "given_name": "F.", "clpid": "Stivoli-F" }, { "family_name": "Stolyarov", "given_name": "V.", "clpid": "Stolyarov-V" }, { "family_name": "Stompor", "given_name": "R.", "clpid": "Stompor-R" }, { "family_name": "Vielva", "given_name": "P.", "clpid": "Vielva-P" } ], "abstract": "Context. The PLANCK satellite will map the full sky at nine frequencies from 30 to 857 GHz. The CMB intensity and polarization that are its prime targets are contaminated by foreground emission.\n\nAims. The goal of this paper is to compare proposed methods for separating CMB from foregrounds based on their different spectral and spatial characteristics, and to separate the foregrounds into \"components\" with different physical origins (Galactic synchrotron, free-free and dust emissions; extra-galactic and far-IR point sources; Sunyaev-Zeldovich effect, etc.) \n\nMethods. A component separation challenge has been organised, based on a set of realistically complex simulations of sky emission. Several methods including those based on internal template subtraction, maximum entropy method, parametric method, spatial and harmonic cross correlation methods, and independent component analysis have been tested.\n\nResults. Different methods proved to be effective in cleaning the CMB maps of foreground contamination, in reconstructing maps of diffuse Galactic emissions, and in detecting point sources and thermal Sunyaev-Zeldovich signals. The power spectrum of the residuals is, on the largest scales, four orders of magnitude lower than the input Galaxy power spectrum at the foreground minimum. The CMB power spectrum was accurately recovered up to the sixth acoustic peak. The point source detection limit reaches 100 mJy, and about 2300 clusters are detected via the thermal SZ effect on two thirds of the sky. We have found that no single method performs best for all scientific objectives.\n\nConclusions. We foresee that the final component separation pipeline for PLANCK will involve a combination of methods and iterations between processing steps targeted at different objectives such as diffuse component separation, spectral estimation, and compact source extraction.", "doi": "10.1051/0004-6361:200810116", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2008-11", "series_number": "2", "volume": "491", "issue": "2", "pages": "597-615" }, { "id": "authors:h24cr-d8049", "collection": "authors", "collection_id": "h24cr-d8049", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:ERIapj08", "type": "article", "title": "Joint Bayesian Component Separation and CMB Power Spectrum Estimation", "author": [ { "family_name": "Eriksen", "given_name": "H. K.", "clpid": "Eriksen-H-K" }, { "family_name": "Jewell", "given_name": "J. B.", "clpid": "Jewell-J-B" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Banday", "given_name": "A. J.", "clpid": "Banday-A-J" }, { "family_name": "G\u00f3rski", "given_name": "K. M.", "clpid": "G\u00f3rski-K-M" }, { "family_name": "Lawrence", "given_name": "C. R.", "clpid": "Lawrence-C-R" } ], "abstract": "We describe and implement an exact, flexible, and computationally efficient algorithm for joint component separation and CMB power spectrum estimation, building on a Gibbs sampling framework. Two essential new features are (1) conditional sampling of foreground spectral parameters and (2) joint sampling of all amplitude-type degrees of freedom (e.g., CMB, foreground pixel amplitudes, and global template amplitudes) given spectral parameters. Given a parametric model of the foreground signals, we estimate efficiently and accurately the exact joint foreground-CMB posterior distribution and, therefore, all marginal distributions such as the CMB power spectrum or foreground spectral index posteriors. The main limitation of the current implementation is the requirement of identical beam responses at all frequencies, which restricts the analysis to the lowest resolution of a given experiment. We outline a future generalization to multiresolution observations. To verify the method, we analyze simple models and compare the results to analytical predictions. We then analyze a realistic simulation with properties similar to the 3 yr WMAP data, downgraded to a common resolution of 3\u00b0 FWHM. The results from the actual 3 yr WMAP temperature analysis are presented in a companion Letter.", "doi": "10.1086/525277", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2008-03-20", "series_number": "1", "volume": "676", "issue": "1", "pages": "10-32" }, { "id": "authors:cw11n-s9e96", "collection": "authors", "collection_id": "cw11n-s9e96", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091028-132353961", "type": "article", "title": "A centimetre-wave excess over free\u2013free emission in planetary nebulae", "author": [ { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Nyman", "given_name": "L.-\u00c5.", "clpid": "Nyman-L-\u00c5" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" } ], "abstract": "We report a centimetre-wave (cm-wave, 5\u201331 GHz) excess over free\u2013free emission in planetary nebulae (PNe). Accurate 31- and 250-GHz measurements show that the 31-GHz flux densities in our sample are systematically higher than the level of optically thin free\u2013free continuum extrapolated from 250-GHz. The 31-GHz excess is observed, within one standard deviation, in all 18 PNe with reliable 31- and 250-GHz data, and is significant in nine PNe. The only exception is the peculiar object M2-9, whose radio spectrum is that of an optically thick stellar wind. On average the fraction of non-free\u2013free emission represents 51 per cent of the total flux density at 31 GHz, with a scatter of 11 per cent. The average 31\u2013250 GHz spectral index of our sample is\u3008\u03b1^(250)_(31)\u3009=\u22120.43 \u00b1 0.03 (in flux density, with a scatter of 0.14). The 31\u2013250 GHz drop is reminiscent of the anomalous foreground observed in the diffuse interstellar medium (ISM) by cosmic microwave background (CMB) anisotropy experiments. The 5\u201331 GHz spectral indices are consistent with both flat spectra and spinning dust emissivities, given the 10 per cent calibration uncertainty of the comparison 5-GHz data. However, a detailed study of the objects with the largest cm-excess, including the low-frequency data available in the literature, shows that present spinning dust models alone cannot explain the cm-wave excess in PNe. Although we have no definitive interpretation of our data, the least implausible explanation involves a synchrotron component absorbed by a cold nebular screen. We give flux densities for 37 objects at 31 GHz, and for 26 objects at 250 GHz.", "doi": "10.1111/j.1365-2966.2007.12366.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2007-12-21", "series_number": "4", "volume": "382", "issue": "4", "pages": "1607-1622" }, { "id": "authors:d7h4c-13q90", "collection": "authors", "collection_id": "d7h4c-13q90", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091028-145009600", "type": "article", "title": "CBI limits on 31 GHz excess emission in southern H II regions", "author": [ { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Bronfman", "given_name": "L.", "clpid": "Bronfman-L" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Wilkinson", "given_name": "P. N.", "clpid": "Wilkinson-P-N" } ], "abstract": "We have mapped four regions of the southern Galactic plane at 31 GHz with the Cosmic Background Imager. From the maps, we have extracted the flux densities for six of the brightest H ii regions in the southern sky and compared them with multifrequency data from the literature. The fitted spectral index for each source was found to be close to the theoretical value expected for optically thin free\u2013free emission, thus confirming that the majority of flux at 31 GHz is due to free\u2013free emission from ionized gas with an electron temperature of \u22487000\u20138000 K.\n\nWe also found that, for all six sources, the 31-GHz flux density was slightly higher than the predicted value from data in the literature. This excess emission could be due to spinning dust or another emission mechanism. Comparisons with 100-\u03bcm data indicate an average dust emissivity of 3.3 \u00b1 1.7 \u03bcK (MJy sr^(\u22121))^(\u22121) , or a 95 per cent confidence limit of <6.1 \u03bcK (MJy sr^(\u22121))^(\u22121) . This is lower than that found in diffuse clouds at high Galactic latitudes by a factor of \u223c3\u20134. The most significant detection (3.3\u03c3) was found in G284.3\u22120.3 (RCW 49) and may account for up to \u224830 per cent of the total flux density observed at 31 GHz. Here, the dust emissivity of the excess emission is 13.6 \u00b1 4.2 \u03bcK (MJy sr^(\u22121))^(\u22121) and is within the range observed at high Galactic latitudes.\n\nLow-level polarized emission was observed in all six sources with polarization fractions in the range 0.3\u20130.6 per cent. This is likely to be mainly due to instrumental leakage and is therefore an upper limit to the free\u2013free polarization. It corresponds to an upper limit of ~1 per cent for the polarization of anomalous emission.", "doi": "10.1111/j.1365-2966.2007.11967.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2007-07-21", "series_number": "1", "volume": "379", "issue": "1", "pages": "297-307" }, { "id": "authors:q6dz0-kgg68", "collection": "authors", "collection_id": "q6dz0-kgg68", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091113-094407290", "type": "article", "title": "Implications of the Cosmic Background Imager Polarization Data", "author": [ { "family_name": "Sievers", "given_name": "J. L.", "clpid": "Sievers-J-L" }, { "family_name": "Achermann", "given_name": "C.", "clpid": "Achermann-C" }, { "family_name": "Bond", "given_name": "J. R.", "orcid": "0000-0003-2358-9949", "clpid": "Bond-J-R" }, { "family_name": "Bronfman", "given_name": "L.", "clpid": "Bronfman-L" }, { "family_name": "Bustos", "given_name": "R.", "clpid": "Bustos-R" }, { "family_name": "Contaldi", "given_name": "C. R.", "clpid": "Contaldi-C-R" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Ferreira", "given_name": "P. G.", "clpid": "Ferreira-P-G" }, { "family_name": "Jones", "given_name": "M. E.", "orcid": "0000-0003-3564-6680", "clpid": "Jones-M-E" }, { "family_name": "Lewis", "given_name": "A. M.", "clpid": "Lewis-A-M" }, { "family_name": "Mason", "given_name": "B. S.", "clpid": "Mason-B-S" }, { "family_name": "May", "given_name": "J.", "clpid": "May-J" }, { "family_name": "Myers", "given_name": "S. T.", "clpid": "Myers-Steven-Theodore" }, { "family_name": "Oyarce", "given_name": "N.", "clpid": "Oyarce-N" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Pospieszalski", "given_name": "M.", "clpid": "Pospieszalski-M" }, { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Reeves", "given_name": "R.", "orcid": "0000-0001-5704-271X", "clpid": "Reeves-R-A" }, { "family_name": "Taylor", "given_name": "A. C.", "clpid": "Taylor-A-C" }, { "family_name": "Torres", "given_name": "S.", "clpid": "Torres-S" } ], "abstract": "We present new measurements of the power spectra of the E mode of cosmic microwave background (CMB) polarization, the temperature T, the cross-correlation of E and T, and upper limits on the B mode from 2.5 yr of dedicated Cosmic Background Imager (CBI) observations. Both raw maps and optimal signal images in the (u, v)-plane and the sky plane show strong detections of the E mode (11.7 \u03c3 for the EE power spectrum overall) and no detection of the B mode. The power spectra are used to constrain parameters of the flat tilted adiabatic \u039bCDM models: those determined from EE and TE bandpowers agree with those from TT, which is a powerful consistency check. There is little tolerance for shifting polarization peaks from the TT-forecast locations, as measured by the angular sound crossing scale \u03b8 = 100/l_s = 1.03 \u00b1 0.02 from EE and TE; compare with 1.044 \u00b1 0.005 with the TT data included. The scope for extra out-of-phase peaks from subdominant isocurvature modes is also curtailed. The EE and TE measurements of CBI, DASI, and BOOMERANG are mutually consistent and, taken together rather than singly, give enhanced leverage for these tests.", "doi": "10.1086/510504", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2007-05-10", "series_number": "2", "volume": "660", "issue": "2", "pages": "976-987" }, { "id": "authors:f8yfx-sj252", "collection": "authors", "collection_id": "f8yfx-sj252", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091113-100849088", "type": "article", "title": "Constraints on spinning dust towards Galactic targets with the Very Small Array: a tentative detection of excess microwave emission towards 3C396", "author": [ { "family_name": "Scaife", "given_name": "Anna", "clpid": "Scaife-A" }, { "family_name": "Green", "given_name": "David A.", "clpid": "Green-D-A" }, { "family_name": "Battye", "given_name": "Richard A.", "clpid": "Battye-R-A" }, { "family_name": "Davies", "given_name": "Rod D.", "clpid": "Davies-R-D" }, { "family_name": "Davis", "given_name": "Richard J.", "clpid": "Davis-R-J" }, { "family_name": "Dickinson", "given_name": "Clive", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Franzen", "given_name": "Thomas", "clpid": "Franzen-T" }, { "family_name": "G\u00e9nova-Santos", "given_name": "Ricardo", "clpid": "G\u00e9nova-Santos-R" }, { "family_name": "Grainge", "given_name": "Keith", "clpid": "Grainge-K" }, { "family_name": "Hafez", "given_name": "Yaser A.", "clpid": "Hafez-Y-A" }, { "family_name": "Hobson", "given_name": "Michael P.", "clpid": "Hobson-M-P" }, { "family_name": "Lasenby", "given_name": "Anthony", "clpid": "Lasenby-A" }, { "family_name": "Pooley", "given_name": "Guy G.", "clpid": "Pooley-G-G" }, { "family_name": "Rajguru", "given_name": "Nutan", "clpid": "Rajguru-N" }, { "family_name": "Rebolo", "given_name": "Rafael", "orcid": "0000-0003-3767-7085", "clpid": "Rebolo-R" }, { "family_name": "Rubi\u00f1o-Martin", "given_name": "Jos\u00e9 Alberto", "clpid": "Rubi\u00f1o-Martin-J-A" }, { "family_name": "Saunders", "given_name": "Richard D. E.", "clpid": "Saunders-R-D-E" }, { "family_name": "Scott", "given_name": "Paul F.", "clpid": "Scott-P-F" }, { "family_name": "Titterington", "given_name": "David", "clpid": "Titterington-D" }, { "family_name": "Waldram", "given_name": "Elizabeth", "clpid": "Waldram-E-M" }, { "family_name": "Watson", "given_name": "Robert A.", "clpid": "Watson-R-A" } ], "abstract": "We present results from observations made at 33 GHz with the Very Small Array (VSA) telescope towards potential candidates in the Galactic plane for spinning dust emission. In the cases of the diffuse H ii regions LPH96 and NRAO591 we find no evidence for anomalous emission and, in combination with Effelsberg data at 1.4 and 2.7 GHz, confirm that their spectra are consistent with optically thin free\u2013free emission. In the case of the infrared bright supernova remnant 3C396 we find emission inconsistent with a purely non-thermal spectrum and discuss the possibility of this excess arising from either a spinning dust component or a shallow spectrum pulsar wind nebula, although we conclude that the second case is unlikely given the strong constraints available from lower-frequency radio images.", "doi": "10.1111/j.1745-3933.2007.00305.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2007-05", "series_number": "1", "volume": "377", "issue": "1", "pages": "L69-L73" }, { "id": "authors:swz90-9pq65", "collection": "authors", "collection_id": "swz90-9pq65", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:DAVmnras06a", "type": "article", "title": "A determination of the spectra of Galactic components observed by the Wilkinson Microwave Anisotropy Probe", "author": [ { "family_name": "Davies", "given_name": "R. D.", "clpid": "Davies-R-D" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Banday", "given_name": "A. J.", "clpid": "Banday-A-J" }, { "family_name": "Jaffe", "given_name": "T. R.", "clpid": "Jaffe-T-R" }, { "family_name": "G\u00f3rski", "given_name": "K. M.", "clpid": "G\u00f3rski-K-M" }, { "family_name": "Davis", "given_name": "R. J.", "clpid": "Davis-R-J" } ], "abstract": "Wilkinson Microwave Anisotropy Probe (WMAP) data when combined with ancillary data on free-free, synchrotron and dust allow an improved understanding of the spectrum of emission from each of these components. Here, we examine the sky variation at intermediate latitudes using a cross-correlation technique. In particular, we compare the observed emission in 15 selected sky regions to three 'standard' templates. \n\nThe free-free emission of the diffuse ionized gas is fitted by a well-known spectrum at K and Ka band, but the derived emissivity corresponds to a mean electron temperature of similar to 4000-5000 K. This is inconsistent with estimates from Galactic H II regions although a variation in the derived ratio of H alpha to free-free intensity by a factor of similar to 2 is also found from region to region. The origin of the discrepancy is unclear. \n\nThe anomalous emission associated with dust is clearly detected in most of the 15 fields studied. The anomalous emission correlates well with the Finkbeiner, Davis & Schlegel model 8 predictions (FDS8) at 94 GHz, with an effective spectral index between 20 and 60 GHz, of beta similar to -2.85. Furthermore, the emissivity varies by a factor of similar to 2 from cloud to cloud. A modestly improved fit to the anomalous dust at K band is provided by modulating the template by an estimate of the dust colour temperature, specifically FDS8 x T^n. We find a preferred value n similar to 1.6, although there is a scatter from region to region. Nevertheless, the preferred index drops to zero at higher frequencies where the thermal dust emission dominates. \n\nThe synchrotron emission steepens between GHz frequencies and the WMAP bands. There are indications of spectral index variations across the sky but the current data are not precise enough to accurately quantify this from region to region. \n\nOur analysis of the WMAP data indicates strongly that the dust-correlated emission at the low WMAP frequencies has a spectrum which is compatible with spinning dust; we find no evidence for a synchrotron component correlated with dust. The importance of these results for the correction of cosmic microwave background data for Galactic foreground emission is discussed.", "doi": "10.1111/j.1365-2966.2006.10572.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2006-08-11", "series_number": "3", "volume": "370", "issue": "3", "pages": "1125-1139" }, { "id": "authors:zn8tc-yrh09", "collection": "authors", "collection_id": "zn8tc-yrh09", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141202-152432483", "type": "article", "title": "Polarization Observations with the Cosmic Background Imager", "author": [ { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Myers", "given_name": "S. T.", "clpid": "Myers-Steven-Theodore" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Sievers", "given_name": "J. L.", "clpid": "Sievers-J-L" }, { "family_name": "Mason", "given_name": "B. S.", "clpid": "Mason-B-S" }, { "family_name": "Contaldi", "given_name": "C. R.", "clpid": "Contaldi-C-R" }, { "family_name": "Bond", "given_name": "J. R.", "orcid": "0000-0003-2358-9949", "clpid": "Bond-J-R" }, { "family_name": "Bustos", "given_name": "R.", "clpid": "Bustos-R" }, { "family_name": "Altamirano", "given_name": "P.", "clpid": "Altamirano-P" }, { "family_name": "Achermann", "given_name": "C.", "clpid": "Achermann-C" }, { "family_name": "Bronfman", "given_name": "L.", "clpid": "Bronfman-L" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Cartwright", "given_name": "J. K.", "clpid": "Cartwright-J-K" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Holzapfel", "given_name": "W. L.", "clpid": "Holzapfel-W-L" }, { "family_name": "Kovac", "given_name": "J. M.", "clpid": "Kovac-J-M" }, { "family_name": "Leitch", "given_name": "E. M.", "clpid": "Leitch-E-M" }, { "family_name": "May", "given_name": "J.", "clpid": "May-J" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Pogosyan", "given_name": "D.", "clpid": "Pogosyan-D" }, { "family_name": "Pospieszalski", "given_name": "M.", "clpid": "Pospieszalski-M" }, { "family_name": "Pryke", "given_name": "C.", "clpid": "Pryke-C" }, { "family_name": "Reeves", "given_name": "R.", "orcid": "0000-0001-5704-271X", "clpid": "Reeves-R-A" }, { "family_name": "Shepherd", "given_name": "M. C.", "clpid": "Shepherd-Martin-C" }, { "family_name": "Torres", "given_name": "S.", "clpid": "Torres-S" } ], "abstract": "Polarization observations of the cosmic microwave background with the Cosmic Background Imager from September 2002 to May 2004 provide a significant detection of the E-mode polarization and reveal an angular power spectrum of polarized emission showing peaks and valleys that are shifted in phase by half a cycle relative to those of the total intensity spectrum. This key agreement between the phase of the observed polarization spectrum and that predicted on the basis of the total intensity spectrum provides support for the standard model of cosmology, in which dark matter and dark energy are the dominant constituents, the geometry is close to flat, and primordial density fluctuations are predominantly adiabatic with a matter power spectrum commensurate with inflationary cosmological models.", "doi": "10.1126/science.1105598", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "2004-10-29", "series_number": "5697", "volume": "306", "issue": "5697", "pages": "836-844" } ]