Author: "Clive Dickinson" - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Clive Dickinson"' showing total 186 results

Start Over Author "Clive Dickinson"

186 results on '"Clive Dickinson"'

1. Baryon Acoustic Oscillations from Integrated Neutral Gas Observations: an instrument to observe the 21cm hydrogen line in the redshift range 0.13 < z < 0.45 – status update

Author: CARLOS A. WUENSCHE, ELCIO ABDALLA, FILIPE ABDALLA, LUCIANO BAROSI, BIN WANG, RUI AN, JOÃO A. M. BARRETOS, RICHARD BATTYE, FRANCISCO A. BRITO, IAN BROWNE, DANIEL CORREIA, ANDRÉ A. COSTA, JACQUES DELABROUILLE, CLIVE DICKINSON, CHANG FENG, ELISA G. M. FERREIRA, KARIN FORNAZIER, GIANCARLO DE GASPERIS, PRISCILA GUTIERREZ, STUART HARPER, RICARDO G. LANDIM, VINCENZO LICCARDO, YIN-ZHE MA, TELMO MACHADO, BRUNO MAFFEI, ALESSANDRO MARINS, MILENA M. M. MENDES, EDUARDO MERICIA, CHRISTIAN MONSTEIN, PABLO MOTTA, CAMILA NOVAES, CARLOS H. OTOBONE, MICHAEL PEEL, AMILCAR R. QUEIROZ, CHRISTOPHER RADCLIFFE, MATHIEU REMAZEILLES, RAFAEL M. G. RIBEIRO, YU SANG, JULIANA F. R. SANTOS, LARISSA SANTOS, MARCELO. V. SANTOS, CHENXI SHAN, GUSTAVO B. SILVA, FREDERICO VIEIRA, JORDANY VIEIRA, THYRSO VILLELA, LINFENG XIAO, WEIQIANG YANG, JIAJUN ZHANG, XUE ZHANG, and ZENGHAO ZHU
Subjects: 21cm cosmology, radio astronomy, baryon acoustic oscillations, BAO, Science
Abstract: Abstract BINGO (BAO from Integrated Neutral Gas Observations) is a unique radio telescope designed to map the intensity of neutral hydrogen distribution at cosmological distances, making the first detection of Baryon Acoustic Oscillations (BAO) in the frequency band 980 MHz - 1260 MHz, corresponding to a redshift range 0.127 < z < 0.449. BAO is one of the most powerful probes of cosmological parameters and BINGO was designed to detect the BAO signal to a level that makes it possible to put new constraints on the equation of state of dark energy. The telescope will be built in Paraíba, Brazil and consists of two \thicksim 40m mirrors, a feedhorn array of 50 horns, and no moving parts, working as a drift-scan instrument. It will cover a 15 ^{\circ} ∘ declination strip centered at \sim \delta ∼ δ =-15 ^{\circ} ∘, mapping \sim ∼ 5400 square degrees in the sky. The BINGO consortium is led by University of São Paulo with co-leadership at National Institute for Space Research and Campina Grande Federal University (Brazil). Telescope subsystems have already been fabricated and tested, and the dish and structure fabrication are expected to start in late 2020, as well as the road and terrain preparation.
Published: 2021
Full Text: View/download PDF

2. Observations of Anomalous Microwave Emission from HII Regions

Author: Clive Dickinson
Subjects: Astronomy, QB1-991
Abstract: I give a summary of the observations of Anomalous Microwave Emission (AME) from HII regions. AME has been detected in, or in the vicinity of, HII regions. Given the difficulties in measuring accurate SEDs over a wide range of frequencies and in complex environments, many of these detections require more data to confirm them as emitting significant AME. The contribution from optically thick free-free emission from UCHII regions may be also be significant in some cases. The AME emissivity, defined as the ratio of the AME brightness to the 100 μm brightness, is comparable to the value observed in high-latitude diffuse cirrus in some regions, but is significantly lower in others. However, this value is dependent on the dust temperature. More data, both at high frequencies (>~5 GHz) and high resolution (~1′ or better) is required to disentangle the emission processes in such complex regions.
Published: 2013
Full Text: View/download PDF

3. Anomalous Microwave Emission: Theory, Modeling, and Observations

Author: Clive Dickinson, Roberta Paladini, and Laurent Verstraete
Subjects: Astronomy, QB1-991
Published: 2013
Full Text: View/download PDF

4. On the Limitations of the Anomalous Microwave Emission Emissivity

Author: Christopher T. Tibbs, Roberta Paladini, and Clive Dickinson
Subjects: Astronomy, QB1-991
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 cm and the thermal dust emission at 100 μm. However, as studies of Galactic dust emission have shown, the intensity of the thermal dust emission at 100 μm 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 K. We, therefore, conclude that computing the AME emissivity relative to the 100 μm 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.
Published: 2012
Full Text: View/download PDF

5. Modelling the spinning dust emission from LDN 1780

Author: Matias Vidal, Clive Dickinson, S E Harper, Simon Casassus, and A N Witt
Published: 2020
Full Text: View/download PDF

6. COMAP Early Science. VI. A First Look at the COMAP Galactic Plane Survey

Author: Thomas J. Rennie, Stuart E. Harper, Clive Dickinson, Liju Philip, Kieran A. Cleary, Richard J. Bond, Jowita Borowska, Patrick C. Breysse, Morgan Catha, Roke Cepeda-Arroita, Dongwoo T. Chung, Sarah E. Church, Delaney A. Dunne, Hans Kristian Eriksen, Marie Kristine Foss, Todd Gaier, Joshua Ott Gundersen, Andrew I. Harris, Brandon Hensley, Richard Hobbs, Håvard T. Ihle, James W. Lamb, Charles R. Lawrence, Jonas G. S. Lunde, Roberta Paladini, Timothy J. Pearson, Maren Rasmussen, Anthony C. S. Readhead, Nils-Ole Stutzer, Duncan J. Watts, Ingunn Kathrine Wehus, and David P. Woody
Subjects: Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We present early results from the COMAP Galactic Plane Survey conducted between June 2019 and April 2021, spanning $20^\circ, Paper 6 of 7 in series. 28 pages, 10 figures, submitted to ApJ
Published: 2022

7. COMAP Early Science. I. Overview

Author: Kieran A. Cleary, Jowita Borowska, Patrick C. Breysse, Morgan Catha, Dongwoo T. Chung, Sarah E. Church, Clive Dickinson, Hans Kristian Eriksen, Marie Kristine Foss, Joshua Ott Gundersen, Stuart E. Harper, Andrew I. Harris, Richard Hobbs, Håvard T. Ihle, Junhan Kim, Jonathon Kocz, James W. Lamb, Jonas G. S. Lunde, Hamsa Padmanabhan, Timothy J. Pearson, Liju Philip, Travis W. Powell, Maren Rasmussen, Anthony C. S. Readhead, Thomas J. Rennie, Marta B. Silva, Nils-Ole Stutzer, Bade D. Uzgil, Duncan J. Watts, Ingunn Kathrine Wehus, David P. Woody, Lilian Basoalto, J. Richard Bond, Delaney A. Dunne, Todd Gaier, Brandon Hensley, Laura C. Keating, Charles R. Lawrence, Norman Murray, Roberta Paladini, Rodrigo Reeves, Marco P. Viero, and Risa H. Wechsler
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The CO Mapping Array Project (COMAP) aims to use line intensity mapping of carbon monoxide (CO) to trace the distribution and global properties of galaxies over cosmic time, back to the Epoch of Reionization (EoR). To validate the technologies and techniques needed for this goal, a Pathfinder instrument has been constructed and fielded. Sensitive to CO(1-0) emission from $z=2.4$-$3.4$ and a fainter contribution from CO(2-1) at $z=6$-8, the Pathfinder is surveying $12$ deg$^2$ in a 5-year observing campaign to detect the CO signal from $z\sim3$. Using data from the first 13 months of observing, we estimate $P_\mathrm{CO}(k) = -2.7 \pm 1.7 \times 10^4\mu\mathrm{K}^2 \mathrm{Mpc}^3$ on scales $k=0.051-0.62 \mathrm{Mpc}^{-1}$ - the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum. Based on these observations alone, we obtain a constraint on the amplitude of the clustering component (the squared mean CO line temperature-bias product) of $\langle Tb\rangle^2, Comment: Paper 1 of 7 in series. 18 pages, 16 figures, submitted to ApJ
Published: 2022

8. Resolved observations at 31 GHz of spinning dust emissivity variations in ρ Oph

Author: J. Anton Zensus, Miguel Cárcamo, Angela C. Taylor, Simon Casassus, M. Jones, M. Vidal, Anthony C. S. Readhead, J. Richard Bond, Brandon S. Hensley, Carla Arce-Tord, Ricardo Genova-Santos, and Clive Dickinson
Subjects: Physics, 010308 nuclear & particles physics, Spinning dust, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Emissivity, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The $\rho$ Oph 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 arcmin observations with CBI 2 that confirm 31 GHz emission from $\rho$ Oph W, the PDR exposed to B-type star HD 147889, 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 GHz map and proxies for the column density of IR emitters, dust radiance and optical depth templates. We found that the 31 GHz 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$\sigma$ and a variation by a factor of at least 23, at 3$\sigma$, between the peak in $\rho$ Oph W and the location of S1, which means that environmental factors are responsible for boosting spinning dust emissivities locally., Comment: 12 pages, 7 figures, 8 tables. Accepted for publication in MNRAS
Published: 2020
Full Text: View/download PDF

9. Impact of 1/f noise on cosmological parameter constraints for SKA intensity mapping

Author: Clive Dickinson, T Chen, Simon Harper, Richard A. Battye, and André A. Costa
Subjects: Physics, Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Spectral density, Order (ring theory), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Noise (electronics), Redshift, Cosmology, Matrix (mathematics), symbols.namesake, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Dark energy, symbols, Planck, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the impact of $1/f$ noise on cosmology for an intensity mapping survey with SKA1-MID Band\,1 and Band\,2. We use a Fisher matrix approach to forecast constraints on cosmological parameters under the influence of $1/f$ noise, adopting a semi-empirical model from an earlier work, which results from the residual $1/f$ noise spectrum after applying a component separation algorithm to remove smooth spectral components. Without $1/f$ noise, the projected constraints are $4\%$ on $w_0$, $1\%$ on $h$, $2\%$ on $b_{\rm HI}$ using Band\,1+\emph{Planck}, and $3\%$ on $w_0$, $0.5\%$ on $h$, $2\%$ on $b_{\rm HI}$ using Band\,2+\emph{Planck}. A representative baseline $1/f$ noise degrades these constraints by a factor of $\sim1.5$ for Band\,1+\emph{Planck}, and $\sim1.2$ for Band\,2+\emph{Planck}. On the power spectrum measurement, higher redshift and smaller scales are more affected by $1/f$ noise, with minimal contamination comes from $z\lesssim1$ and $\ell\lesssim100$. Subject to the specific scan strategy of the adopted $1/f$ noise model, one prefers a correlated in frequency with minimised spectral slope, a low knee frequency, and a large telescope slew speed in order to reduce its impact., Comment: 15 pages, 8 figures, submitted to MNRAS
Published: 2019
Full Text: View/download PDF

10. Baryon Acoustic Oscillations from Integrated Neutral Gas Observations: an instrument to observe the 21cm hydrogen line in the redshift range 0.13 $<$ z $<$ 0.45 -- status update

Author: CARLOS A. WUENSCHE, ELCIO ABDALLA, FILIPE ABDALLA, LUCIANO BAROSI, BIN WANG, RUI AN, JOÃO A. M. BARRETOS, RICHARD BATTYE, FRANCISCO A. BRITO, IAN BROWNE, DANIEL CORREIA, ANDRÉ A. COSTA, JACQUES DELABROUILLE, CLIVE DICKINSON, CHANG FENG, ELISA G. M. FERREIRA, KARIN FORNAZIER, GIANCARLO DE GASPERIS, PRISCILA GUTIERREZ, STUART HARPER, RICARDO G. LANDIM, VINCENZO LICCARDO, YIN-ZHE MA, TELMO MACHADO, BRUNO MAFFEI, ALESSANDRO MARINS, MILENA M. M. MENDES, EDUARDO MERICIA, CHRISTIAN MONSTEIN, PABLO MOTTA, CAMILA NOVAES, CARLOS H. OTOBONE, MICHAEL PEEL, AMILCAR R. QUEIROZ, CHRISTOPHER RADCLIFFE, MATHIEU REMAZEILLES, RAFAEL M. G. RIBEIRO, YU SANG, JULIANA F. R. SANTOS, LARISSA SANTOS, MARCELO. V. SANTOS, CHENXI SHAN, GUSTAVO B. SILVA, FREDERICO VIEIRA, JORDANY VIEIRA, THYRSO VILLELA, LINFENG XIAO, WEIQIANG YANG, JIAJUN ZHANG, XUE ZHANG, ZENGHAO ZHU, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: Science, media_common.quotation_subject, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, radio astronomy, 01 natural sciences, law.invention, Telescope, Radio telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, media_common, Physics, baryon acoustic oscillations, Multidisciplinary, BAO, 010308 nuclear & particles physics, Equation of state (cosmology), 21cm cosmology, Astrophysics::Instrumentation and Methods for Astrophysics, Redshift, Sky, Dark energy, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Hydrogen line, Baryon acoustic oscillations, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: BINGO (BAO from Integrated Neutral Gas Observations) is a unique radio telescope designed to map the intensity of neutral hydrogen distribution at cosmological distances, making the first detection of Baryon Acoustic Oscillations (BAO) in the frequency band 980 MHz - 1260 MHz, corresponding to a redshift range 0.127 < z < 0.449. BAO is one of the most powerful probes of cosmological parameters and BINGO was designed to detect the BAO signal to a level that makes it possible to put new constraints on the equation of state of dark energy. The telescope will be built in Paraíba, Brazil and consists of two \thicksim 40m mirrors, a feedhorn array of 50 horns, and no moving parts, working as a drift-scan instrument. It will cover a 15^{\circ} declination strip centered at \sim \delta =-15^{\circ}, mapping \sim 5400 square degrees in the sky. The BINGO consortium is led by University of São Paulo with co-leadership at National Institute for Space Research and Campina Grande Federal University (Brazil). Telescope subsystems have already been fabricated and tested, and the dish and structure fabrication are expected to start in late 2020, as well as the road and terrain preparation., Anais da Academia Brasileira de Ciências, 93, ISSN:0001-3765, ISSN:1678-2690
Published: 2021
Full Text: View/download PDF

11. Resolved spectral variations of the centimetre-wavelength continuum from the ρ Oph W photodissociation region

Author: Brandon S. Hensley, Carla Arce-Tord, M. Vidal, Glenn J. White, Michael G. Burton, Clive Dickinson, Balthasar T. Indermuehle, and Simon Casassus
Subjects: Infrared, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Photodissociation region, 01 natural sciences, law.invention, Telescope, Protein filament, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Spinning dust, Molecular cloud, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Wavelength, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract: Cm-wavelength radio continuum emission in excess of free-free, synchrotron and Rayleigh-Jeans dust emission (excess microwave emission, EME), and often called `anomalous microwave emission', is bright in molecular cloud regions exposed to UV radiation, i.e. in photo-dissociation regions (PDRs). The EME correlates with IR dust emission on degree angular scales. Resolved observations of well-studied PDRs are needed to compare the spectral variations of the cm-continuum with tracers of physical conditions and of the dust grain population. The EME is particularly bright in the regions of the rho Ophiuchi molecular cloud (rho Oph) that surround the earliest type star in the complex, HD 147889, where the peak signal stems from the filament known as the rho Oph-W PDR. Here we report on ATCA observations of rho Oph-W that resolve the width of the filament. We recover extended emission using a variant of non-parametric image synthesis performed in the sky plane. The multi-frequency 17 GHz to 39 GHz mosaics reveal spectral variations in the cm-wavelength continuum. At ~30 arcsec resolutions, the 17-20 GHz intensities follow tightly the mid-IR, Icm propto I(8 um), despite the breakdown of this correlation on larger scales. However, while the 33-39 GHz filament is parallel to IRAC 8 mum, it is offset by 15-20 arcsec towards the UV source. Such morphological differences in frequency reflect spectral variations, which we quantify spectroscopically as a sharp and steepening high-frequency cutoff, interpreted in terms of the spinning dust emission mechanism as a minimum grain size a_cutoff ~ 6 +- 1A that increases deeper into the PDR., Comment: accepted for publication in MNRAS
Published: 2021

12. The BINGO project

Author: André A. Costa, Elcio Abdalla, Michael W. Peel, Filipe B. Abdalla, Jiajun Zhang, Vincenzo Liccardo, Thyrso Villela, C. P. Novaes, Luciano Barosi, Francisco A. Brito, Karin S. F. Fornazier, Marcelo Vargas dos Santos, Eduardo J. de Mericia, Larissa Santos, Frederico Vieira, Mathieu Remazeilles, Ricardo G. Landim, Clive Dickinson, Elisa G. M. Ferreira, Stuart Harper, Alessandro Marins, Carlos Alexandre Wuensche, Amilcar R. de Queiroz, and Bin Wang
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, Telescope, Radio telescope, law, 0103 physical sciences, Nuclear Experiment, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Intensity mapping, Astronomy and Astrophysics, Redshift, Cardinal point, Space and Planetary Science, Sky, RADIOTELESCÓPIOS, Radio frequency, Baryon acoustic oscillations, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The large-scale distribution of neutral hydrogen (HI) in the Universe is luminous through its 21 cm emission. The goal of the Baryon Acoustic Oscillations from Integrated Neutral Gas Observations -- BINGO -- radio telescope is to detect baryon acoustic oscillations (BAOs) at radio frequencies through 21 cm intensity mapping (IM). The telescope will span the redshift range 0.127 $< z, 16 pages. Version to appear in A&A
Published: 2022
Full Text: View/download PDF

13. The BINGO project

Author: Carlos A. Wuensche, Thyrso Villela, Elcio Abdalla, Vincenzo Liccardo, Frederico Vieira, Ian Browne, Michael W. Peel, Christopher Radcliffe, Filipe B. Abdalla, Alessandro Marins, Luciano Barosi, Francisco A. Brito, Amilcar R. Queiroz, Bin Wang, Andre A. Costa, Elisa G. M. Ferreira, Karin S.F. Fornazier, Ricardo G. Landim, Camila P. Novaes, Larissa Santos, Marcelo V. dos Santos, Jiajun Zhang, Tianyue Chen, Jacques Delabrouille, Clive Dickinson, Giancarlo de Gasperis, Edmar C. Gurjão, Stuart Harper, Yin-Zhe Ma, Telmo Machado, Bruno Maffei, Eduardo J. de Mericia, Christian Monstein, Pablo Motta, Carlos H. N. Otobone, Luiz A. Reitano, Mathieu Remazeilles, Sambit Roychowdhury, João R. L. Santos, Alexandre J. R. Serres, Andreia P. Souza, Cesar Strauss, Jordany Vieira, Haiguang Xu, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), instrumentation: detectors, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, RADIOTELESCÓPIOS, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The measurement of diffuse 21-cm radiation from the hyperfine transition of neutral hydrogen (HI signal) in different redshifts is an important tool for modern cosmology. However, detecting this faint signal with non-cryogenic receivers in single-dish telescopes is a challenging task. The BINGO (Baryon Acoustic Oscillations from Integrated Neutral Gas Observations) radio telescope is an instrument designed to detect baryonic acoustic oscillations (BAOs) in the cosmological HI signal, in the redshift interval $0.127 \le z \le 0.449$. This paper describes the BINGO radio telescope, including the current status of the optics, receiver, observational strategy, calibration, and the site. BINGO has been carefully designed to minimize systematics, being a transit instrument with no moving dishes and 28 horns operating in the frequency range $980 \le \nu \le 1260$ MHz. Comprehensive laboratory tests were conducted for many of the BINGO subsystems and the prototypes of the receiver chain, horn, polarizer, magic tees, and transitions have been successfully tested between 2018 - 2020. The survey was designed to cover $\sim 13\%$ of the sky, with the primary mirror pointing at declination $\delta=-15^{\circ}$. The telescope will see an instantaneous declination strip of $14.75^{\circ}$. The results of the prototype tests closely meet those obtained during the modeling process, suggesting BINGO will perform according to our expectations. After one year of observations with a $60\%$ duty cycle and 28 horns, BINGO should achieve an expected sensitivity of 102 $\mu K$ per 9.33 MHz frequency channel, one polarization, and be able to measure the HI power spectrum in a competitive time frame., Comment: 13 pages, accepted for publication in A&A
Published: 2022
Full Text: View/download PDF

14. COMAP Early Science. IV. Power Spectrum Methodology and Results

Author: Håvard T. Ihle, Jowita Borowska, Kieran A. Cleary, Hans Kristian Eriksen, Marie K. Foss, Stuart E. Harper, Junhan Kim, Jonas G. S. Lunde, Liju Philip, Maren Rasmussen, Nils-Ole Stutzer, Bade D. Uzgil, Duncan J. Watts, Ingunn Kathrine Wehus, J. Richard Bond, Patrick C. Breysse, Morgan Catha, Sarah E. Church, Dongwoo T. Chung, Clive Dickinson, Delaney A. Dunne, Todd Gaier, Joshua Ott Gundersen, Andrew I. Harris, Richard Hobbs, James W. Lamb, Charles R. Lawrence, Norman Murray, Anthony C. S. Readhead, Hamsa Padmanabhan, Timothy J. Pearson, Thomas J. Rennie, and David P. Woody
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the power spectrum methodology used for the first-season COMAP analysis, and assess the quality of the current data set. The main results are derived through the Feed-feed Pseudo-Cross-Spectrum (FPXS) method, which is a robust estimator with respect to both noise modeling errors and experimental systematics. We use effective transfer functions to take into account the effects of instrumental beam smoothing and various filter operations applied during the low-level data processing. The power spectra estimated in this way have allowed us to identify a systematic error associated with one of our two scanning strategies, believed to be due to residual ground or atmospheric contamination. We omit these data from our analysis and no longer use this scanning technique for observations. We present the power spectra from our first season of observing and demonstrate that the uncertainties are integrating as expected for uncorrelated noise, with any residual systematics suppressed to a level below the noise. Using the FPXS method, and combining data on scales $k=0.051-0.62 \,\mathrm{Mpc}^{-1}$ we estimate $P_\mathrm{CO}(k) = -2.7 \pm 1.7 \times 10^4\mu\textrm{K}^2\mathrm{Mpc}^3$, the first direct 3D constraint on the clustering component of the CO(1-0) power spectrum in the literature., Comment: Paper 4 of 7 in series. 18 pages, 11 figures, as accepted in ApJ
Published: 2022
Full Text: View/download PDF

15. COMAP Early Science: II. Pathfinder Instrument

Author: James W. Lamb, Kieran A. Cleary, David P. Woody, Morgan Catha, Dongwoo T. Chung, Joshua Ott Gundersen, Stuart E. Harper, Andrew I. Harris, Richard Hobbs, Håvard T. Ihle, Jonathon Kocz, Timothy J. Pearson, Liju Philip, Travis W. Powell, Lilian Basoalto, J. Richard Bond, Jowita Borowska, Patrick C. Breysse, Sarah E. Church, Clive Dickinson, Delaney A. Dunne, Hans Kristian Eriksen, Marie Kristine Foss, Todd Gaier, Junhan Kim, Charles R. Lawrence, Jonas G. S. Lunde, Hamsa Padmanabhan, Maren Rasmussen, Anthony C. S. Readhead, Rodrigo Reeves, Thomas J. Rennie, Nils-Ole Stutzer, Marco P. Viero, Duncan J. Watts, and Ingunn Kathrine Wehus
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Line intensity mapping (LIM) is a new technique for tracing the global properties of galaxies over cosmic time. Detection of the very faint signals from redshifted carbon monoxide (CO), a tracer of star formation, pushes the limits of what is feasible with a total-power instrument. The CO Mapping Project (COMAP) Pathfinder is a first-generation instrument aiming to prove the concept and develop the technology for future experiments, as well as delivering early science products. With 19 receiver channels in a hexagonal focal plane arrangement on a 10.4 m antenna, and an instantaneous 26-34 GHz frequency range with 2 MHz resolution, it is ideally suited to measuring CO($J$=1-0) from $z\sim3$. In this paper we discuss strategies for designing and building the Pathfinder and the challenges that were encountered. The design of the instrument prioritized LIM requirements over those of ancillary science. After a couple of years of operation, the instrument is well understood, and the first year of data is already yielding useful science results. Experience with this Pathfinder will drive the design of the next generations of experiments., Comment: Paper 2 of 7 in series. 27 pages, 28 figures, submitted to ApJ
Published: 2021
Full Text: View/download PDF

16. Detection of spectral variations of anomalous microwave emission with QUIJOTE and C-BASS

Author: A. C. S. Readhead, Luke R. P. Jew, Justin L. Jonas, F Guidi, M. Jones, T. J. Pearson, Ricardo Genova-Santos, R. Fernandez-Cobos, Jonathan Sievers, R. Cepeda-Arroita, A. Barr, Angela C. Taylor, B. Casaponsa, R. D. P. Grumitt, J. P. Leahy, B. Ruiz-Granados, Lucio Piccirillo, F. Vansyngel, Enrique Martinez-Gonzalez, Anthony Lasenby, P. Vielva, Frédérick Poidevin, R. B. Barreiro, Robert A. Watson, H M Heilgendorff, H C Chiang, Jose Alberto Rubino-Martin, F. J. Casas, M. Ashdown, Clive Dickinson, Jamie Leech, Rafael Rebolo, Michael W. Peel, D. Herranz, Simon Harper, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), and European Commission
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, 0103 physical sciences, Optical depth (astrophysics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Spinning dust, Resolution (electron density), Spectral density, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, 3. Good health, Interstellar medium, Amplitude, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Intensity (heat transfer), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Anomalous Microwave Emission (AME) is a significant component of Galactic diffuse emission in the frequency range 10–60GHz and a new window into the properties of sub-nanometre-sized grains in the interstellar medium. We investigate the morphology of AME in the ≈10○ diameter λ Orionis ring by combining intensity data from the QUIJOTE experiment at 11, 13, 17, and 19GHz and the C-Band All Sky Survey (C-BASS) at 4.76GHz⁠, together with 19 ancillary data sets between 1.42 and 3000GHz⁠. Maps of physical parameters at 1○ resolution are produced through Markov chain Monte Carlo (MCMC) fits of spectral energy distributions (SEDs), approximating the AME component with a lognormal distribution. AME is detected in excess of 20σ at degree-scales around the entirety of the ring along photodissociation regions (PDRs), with three primary bright regions containing dark clouds. A radial decrease is observed in the AME peak frequency from ≈35GHz near the free–free region to ≈21GHz in the outer regions of the ring, which is the first detection of AME spectral variations across a single region. A strong correlation between AME peak frequency, emission measure and dust temperature is an indication for the dependence of the AME peak frequency on the local radiation field. The AME amplitude normalized by the optical depth is also strongly correlated with the radiation field, giving an overall picture consistent with spinning dust where the local radiation field plays a key role., Partial financial support for QUIJOTE is provided by the Spanish Ministry of Economy and Competitiveness (MINECO) under the projects AYA2007-68058-C03-01, AYA2010-21766-C03-02, AYA2014-60438-P, AYA2017-84185-P, IACA13-3E-2336, IACA15-BE-3707, and EQC2018-004918-P; Agencia Estatal de Investigación (AEI) and Fondo Europeo de Desarrollo Regional (FEDER, UE), under projects ESP2017-83921-C2-1-R and AYA2017-90675-REDC; the European Union’s Horizon 2020 research and innovation programme under grant agreement number 687312 (RADIOFORE; FP acknowledges support from the Spanish Ministerio de Ciencia, Innovación y Universidades (MICINN) under grant numbers ESP2015-65597-C4-4-R, ESP2017-86852-C4-2-R, ESP2015-65597-C4-4-R, and ESP2017-86852-C4-2-R. GROUNDS) and number 658499 (PolAME); Unidad de Excelencia María de Maeztu (MDM-2017-0765)
Published: 2021

17. COMAP Early Science: III. CO Data Processing

Author: Marie K. Foss, Håvard T. Ihle, Jowita Borowska, Kieran A. Cleary, Hans Kristian Eriksen, Stuart E. Harper, Junhan Kim, James W. Lamb, Jonas G. S. Lunde, Liju Philip, Maren Rasmussen, Nils-Ole Stutzer, Bade D. Uzgil, Duncan J. Watts, Ingunn K. Wehus, David P. Woody, J. Richard Bond, Patrick C. Breysse, Morgan Catha, Sarah E. Church, Dongwoo T. Chung, Clive Dickinson, Delaney A. Dunne, Todd Gaier, Joshua Ott Gundersen, Andrew I. Harris, Richard Hobbs, Charles R. Lawrence, Norman Murray, Anthony C. S. Readhead, Hamsa Padmanabhan, Timothy J. Pearson, and Thomas J. Rennie
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We describe the first season COMAP analysis pipeline that converts raw detector readouts to calibrated sky maps. This pipeline implements four main steps: gain calibration, filtering, data selection, and map-making. Absolute gain calibration relies on a combination of instrumental and astrophysical sources, while relative gain calibration exploits real-time total-power variations. High efficiency filtering is achieved through spectroscopic common-mode rejection within and across receivers, resulting in nearly uncorrelated white noise within single-frequency channels. Consequently, near-optimal but biased maps are produced by binning the filtered time stream into pixelized maps; the corresponding signal bias transfer function is estimated through simulations. Data selection is performed automatically through a series of goodness-of-fit statistics, including $\chi^2$ and multi-scale correlation tests. Applying this pipeline to the first-season COMAP data, we produce a dataset with very low levels of correlated noise. We find that one of our two scanning strategies (the Lissajous type) is sensitive to residual instrumental systematics. As a result, we no longer use this type of scan and exclude data taken this way from our Season 1 power spectrum estimates. We perform a careful analysis of our data processing and observing efficiencies and take account of planned improvements to estimate our future performance. Power spectrum results derived from the first-season COMAP maps are presented and discussed in companion papers., Comment: Paper 3 of 7 in series. 26 pages, 23 figures, submitted to ApJ
Published: 2021
Full Text: View/download PDF

18. Overview of the Medium and High Frequency Telescopes of the LiteBIRD satellite mission

Author: Ludovic Montier, Baptiste Mot, Paolo de Bernardis, Bruno Maffei, Giampaolo Pisano, Fabio Columbro, Jon E. Gudmundsson, Sophie Henrot-Versillé, Luca Lamagna, Joshua Montgomery, Thomas Prouvé, Megan Russell, Giorgio Savini, Samantha Stever, Keith L. Thompson, Masahiro Tsujimoto, Carole Tucker, Benjamin Westbrook, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, Ranajoy Banerji, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Masashi Hazumi, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Gianluca Morgante, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Gianluca Polenta, Davide Poletti, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), LiteBIRD, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Lystrup, Makenzie, Montier, L, Mot, B, de Bernardis, P, Maffei, B, Pisano, G, Columbro, F, Gudmundsson, J, Henrot-Versillé, S, Lamagna, L, Montgomery, J, Prouvé, T, Russell, M, Savini, G, Stever, S, Thompson, K, Tsujimoto, M, Tucker, C, Westbrook, B, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Morgante, G, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)
Subjects: cosmological model, experimental methods, detector: satellite, Cosmic microwave background, cosmic background radiation: polarization, detector: noise, magnetic field, 02 engineering and technology, LiteBIRD, cosmic microwave background, polarization measurements, space telescopes, 7. Clean energy, 01 natural sciences, law.invention, law, detector: calibration, media_common, Physics, conductivity: thermal, Settore FIS/05, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, Polarization (waves), inflation: model, experimental equipment, B-mode, cosmic radiation, cryogenics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, cosmic background radiation: detector, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, LiteBIRD, Polarization measurements, Space telescopes, Astrophysics::Cosmology and Extragalactic Astrophysics, bolometer: superconductivity, frequency: high, Radio spectrum, tensor scalar: ratio, 010309 optics, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), detector: angular resolution, Astrophysics::Galaxy Astrophysics, Gravitational wave, synchrotron radiation, gravitational radiation: primordial, Astronomy, Physics::History of Physics, optics, detector: sensitivity, 13. Climate action, Sky, Satellite, temperature: stability, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy. European collaborators acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement Nos. 772253, 819478, and 849169). The European Space Agency (ESA) has led a Concurrent Design Facility study, focused on the MHFT and Sub-Kelvin coolers, and funded Technology Research Programmes for “Large radii Half-Wave Plate (HWP) development” (contract number: 4000123266/18/NL/AF) and for the ‘Development of Large Anti-Reflection Coated Lenses for Passive (Sub)Millimeter-Wave Science Instruments” (contract number: 4000128517/19/NL/AS).
Published: 2020
Full Text: View/download PDF

19. LiteBIRD: JAXA's new strategic L-class mission for all-sky surveys of cosmic microwave background polarization

Author: Masashi Hazumi, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, R. Banjeri, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Paolo de Bernardis, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Fabio Columbro, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Jon E. Gudmundsson, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Sophie Henrot-Versillé, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Luca Lamagna, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Bruno Maffei, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Joshua Montgomery, Ludovic Montier, Gianluca Morgante, Baptiste Mot, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Fabio Noviello, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Giampaolo Pisano, Gianluca Polenta, Davide Poletti, Thomas Prouvé, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Megan Russell, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Giorgio Savini, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Samantha Stever, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Keith L. Thompson, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Masahiro Tsujimoto, Carole Tucker, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Benjamin Westbrook, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LiteBIRD, Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Lystrup, Makenzie, Hazumi, M, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banjeri, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, de Bernardis, P, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Columbro, F, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Henrot-Versillé, S, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Noviello, F, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stever, S, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, and Zonca, A
Subjects: cosmological model, experimental methods, detector: satellite, Physics beyond the Standard Model, Cosmic microwave background, LiteBIRD, cosmic inflation, cosmic microwave background, B-mode polarization, primordial gravi- tational waves, quantum gravity, space telescope, cosmic background radiation: polarization, detector: noise, 02 engineering and technology, 7. Clean energy, 01 natural sciences, expansion: multipole, Cosmology, General Relativity and Quantum Cosmology, B-mode: primordial, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), general relativity, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], B-mode polarization, media_common, Physics, new physics, quantum mechanics, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, BICEP, inflation: model, High Energy Physics - Phenomenology, error: statistical, experimental equipment, cryogenics, power spectrum: angular dependence, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], readout, Astrophysics::Earth and Planetary Astrophysics, dust, control system, 0210 nano-technology, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, cosmic inflation, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, primordial gravi- tational waves, Cosmic background radiation, space telescope, Lagrangian point, FOS: Physical sciences, LiteBIRD, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, polarization: sensitivity, 010309 optics, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ionization, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], cosmic background radiation: power spectrum, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Inflation (cosmology), synchrotron radiation, primordial gravitational waves, gravitational radiation: primordial, Astronomy, calibration, Physics::History of Physics, recombination, detector: sensitivity, angular resolution, Sky, quantum gravity, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Satellite, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], experimental results
Abstract: Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA’s H3 rocket. LiteBIRD plans to map the cosmic microwave background (CMB) polarization over the full sky with unprecedented precision. Its main scientific objective is to carry out a definitive search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with an insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. To this end, LiteBIRD will perform full-sky surveys for three years at the Sun-Earth Lagrangian point L2 for 15 frequency bands between 34 and 448 GHz with three telescopes, to achieve a total sensitivity of 2.16 µK-arcmin with a typical angular resolution of 0.5◦ at 100 GHz. We provide an overview of the LiteBIRD project, including scientific objectives, mission requirements, top-level system requirements, operation concept, and expected scientific outcomes., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy.
Published: 2020
Full Text: View/download PDF

20. Author Correction: Shape of (101955) Bennu indicative of a rubble pile with internal stiffness

Author: M. Lefevre, Aaron S. Burton, Carina Bennett, J. A. Mapel, Renu Malhotra, Peter Fleming, J. McAdams, N. Mogk, R. L. Ballouz, P. H. Smith, V. Nifo, C. K. Maleszewski, Timothy D. Swindle, E. Dotto, Stephen R. Schwartz, C. May, J. Bayron, D. Patterson, D. Guevel, Ellen S. Howell, Humberto Campins, J. Kissell, E. Brown, J. Wood, E. Muhle, John Robert Brucato, J. Small, B. Miller, Oleksiy Golubov, R. Pennington, K. Harshman, J. Nelson, Catherine Elder, M. McGee, R. Burns, J. Contreras, S. Hull, D. Kubitschek, D. Noss, Andrew J. Liounis, J. Backer, B. May, G. Fitzgibbon, J. Donaldson, D. Worden, Bashar Rizk, R. Witherspoon, Catherine L. Johnson, Erica Jawin, G. Shaw, A. Aqueche, Dolores H. Hill, D. Folta, S. Ferrone, M. Lujan, Giovanni Poggiali, B. G. Williams, S. Selznick, Melissa A. Morris, K. Rios, Sara S. Russell, D. Lambert, J. Hong, Jeffrey B. Plescia, H. Bloomenthal, D. Drinnon, Olivier S. Barnouin, Derek S. Nelson, Amanda E. Toland, Michael C. Moreau, J. A. Seabrook, K. Dill, A. Mirfakhrai, K. Hyde, J. D. P. Deshapriya, Hannah Kaplan, Timothy P. McElrath, Juliette I. Brodbeck, N. Ramos, S. Stewart, James B. Garvin, Sei-ichiro Watanabe, M. Arvizu-Jakubicki, Jason P. Dworkin, Matthew A. Siegler, Collin Lewin, Masatoshi Hirabayashi, L. Bloomquist, S. Gardner, Keiko Nakamura-Messenger, A. H. Nair, M. Schmitzer, P. Haas, Julie Bellerose, Dolan E. Highsmith, L. Koelbel, C. C. Lorentson, J. Zareski, E. Queen, S. R. Chesley, Philip A. Bland, A. Cheuvront, V. E. Hamilton, Ronald G. Mink, N. Mastrodemos, H. C. Connolly, K. Bellamy, M. Killgore, A. Gardner, Y. Takahashi, M. Lambert, R. C. Espiritu, Z. Zeszut, E. T. Morton, Kevin J. Walsh, Timothy D. Glotch, M. Skeen, Brian Kennedy, Matthew R.M. Izawa, G. Neumann, F. Teti, D. Doerres, A. Hasten, F. Ciceri, D. Howell, A. Deguzman, J. Nagy, D. Vaughan, H. Ma, C. Lantz, D. N. Brack, David K. Hammond, Erwan Mazarico, Leilah K. McCarthy, L. Rhoads, Kathleen L. Craft, C. Welch, Jay W. McMahon, C. L. Parish, D. C. Reuter, M. Giuntini, N. Castro, Clive Dickinson, J. Kreiner, K. Kingsbury, S. Dickenshied, Joseph A. Nuth, Alan R. Hildebrand, Erik Asphaug, H. Ido, Eric M. Sahr, A. Harbison, Arlin E. Bartels, T. Forrester, D. Eckart, R. Bandrowski, Michael K. Barker, Robert Gaskell, J. Wendel, S. Freund, Marc Bernacki, Ryan S. Park, A. Taylor, E. B. Bierhaus, S. Millington-Veloza, J. Stromberg, L. B. Breitenfeld, K. Stakkestad, D. Ellis, Timothy J. McCoy, M. Susak, Richard G. Cosentino, C. Manzoni, Hisayoshi Yurimoto, C. Drouet d'Aubigny, A. Bjurstrom, Masako Yoshikawa, S. Francis, J. Peachey, J. Geeraert, K. Marchese, O. Billett, M. Rascon, F. Jaen, B. Diallo, Martin Miner, Kris J. Becker, E. Mazzotta Epifani, Florian Thuillet, A. Knight, James H. Roberts, Pasquale Tricarico, Edward A. Cloutis, T. Fisher, Dale Stanbridge, A. Colpo, Osiris-Rex Team, S. Gonzales, Q. Tran, M. K. Crombie, John Marshall, N. Bojorquez-Murphy, David Vokrouhlický, Allen W. Lunsford, H. Bowles, K. L. Edmundson, R. A. Masterson, Peter G. Antreasian, N. Gorius, Benjamin Rozitis, D. Pino Muñoz, S. Carlson-Kelly, C. Thayer, J. Elsila Cook, B. C. Clark, N. Piacentine, José C. Aponte, M. Al Asad, M. A. Barucci, D. Blum, P. Falkenstern, Neil Bowles, Matthew Chojnacki, J. M. Leonard, J. Daly, K. Yetter, M. R. Fisher, Jeffrey N. Grossman, A. Boggs, N. Jayakody, Cristina A. Thomas, C.M. Ernst, Namrah Habib, J. N. Kidd, R. J. Steele, Andrew B. Calloway, Andrew Ryan, Kimberly T. Tait, Paul O. Hayne, J. Y. Li, K. L. Berry, William V. Boynton, Yanga R. Fernandez, D. A. Lorenz, M. Wasser, Daniel J. Scheeres, K. Fortney, A. Scroggins, B. Allen, B. Sutter, T. Ferro, Jonathan Joseph, Derek C. Richardson, D. Hoak, Brian Carcich, W. Chang, P. Wren, C. Boyles, Kaj E. Williams, B. Marty, J. Liang, J. Hoffman, A. Harch, Daniel R. Wibben, Jamie Molaro, S. Rieger, R. Enos, C. W. Hergenrother, Stephen R. Sutton, J. Grindlay, E. J. Lessac-Chenen, E. Huettner, C. Norman, P. Sherman, L. Swanson, M. Coltrin, S. Van wal, B. Buck, A. Fisher, Kevin Righter, Brian Rush, David D. Rowlands, Lauren McGraw, A. Levine, K. Drozd, D. Gaudreau, A. Nguyen, S. Sides, M. Chodas, R. Dubisher, B. Ashman, Michael Caplinger, Amy Simon, W. Moore, S. S. Balram-Knutson, R. Carpenter, S. Fornasier, Shogo Tachibana, Russell Turner, Ian A. Franchi, Trevor Ireland, Chloe B. Beddingfield, D. F. Everett, M. Corvin, Lindsay P. Keller, Tammy L. Becker, S. Carter, J. L. Rizos Garcia, Mark E. Perry, E. Keates, Michael C. Nolan, P. Vasudeva, C. Fellows, K. Herzog, Mark A. Jenkins, J. R. Weirich, J. Swenson, D. R. Golish, Davide Farnocchia, Lydia C. Philpott, Rebecca R. Ghent, Hannah C.M. Susorney, S. W. Squyres, Pedro Hasselmann, J. Hill, Thomas J. Zega, B. Key, Marco Delbo, A. S. French, P. Sánchez, A. Hilbert, J. Y. Pelgrift, R. P. Binzel, L. McNamara, Vishnu Reddy, Michael Daly, Scott Messenger, Daniella DellaGiustina, Maurizio Pajola, Charles Brunet, Joshua L. Bandfield, J. Padilla, A. Janakus, M. Moreau, R. Garcia, R. A. Chicoine, P. Michel, P. Kaotira, K. S. Johnson, J. Forelli, G. Miller, K. Martin, I. Galinsky, S. Desjardins, Naru Hirata, Christine Hartzell, M. L. Jones, S. Hooven, D. Velez, R. Munoz, Carolyn M. Ernst, C. Emr, N. Martinez-Vlasoff, S. Bendall, R. Zellar, E. Church, Theodore Kareta, T. Warren, P. Wolff, V. Morrison, C. Bryan, S. Bhaskaran, N. Jones, D. Hauf, Jeremy Bauman, R. T. Daly, R. Olds, M. M. Westermann, D. K. Hamara, E. Audi, G. Johnston, Eric Palmer, Courtney Mario, Daniel P. Glavin, T. Haltigin, J. Cutts, Javier Licandro, Xiao-Duan Zou, H. L. Roper, Gregory A. Neumann, William M. Owen, S. Sugita, Y. H. Tang, Kevin Burke, H. L. Enos, D. Gallagher, William F. Bottke, K. Getzandanner, Philip R. Christensen, C. W. V. Wolner, K. Fleshman, D. Poland, J. P. Emery, M.M. Riehl, D. Fennell, D. Sallitt, A. D. Rogers, M. Fitzgibbon, John H. Jones, S. Mullen, S. Salazar, S. Oliver, A. T. Polit, J. Cerna, A. Praet, Mark E. Holdridge, E. M. Ibrahim, Coralie D. Adam, J. de León, Christopher J. Miller, M. Ryle, J. Lyzhoft, M. Loveridge, C. Hoekenga, Brent J. Bos, S. Anwar, K. Chaffin, Devin L. Schrader, B. Lovelace, Romy D. Hanna, C. D. Adam, G. L. Mehall, K. L. Donaldson Hanna, F. Merlin, B. Wright, Guy Libourel, L. F. Lim, N. Shultz, Dante S. Lauretta, K. Hanley, Beth E. Clark, L. Le Corre, K. Thomas-Keprta, Moses Milazzo, W. Hagee, B. Page, M. Fisher, E. McDonough, D. Trang, S. Clemett, A. Rubi, A. Ingegneri, Scott A. Sandford, D. Dean, J. Freemantle, Michael D. Smith, Christopher W. Haberle, L. Nguyen, M. Fulchignoni, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), MINES ParisTech - École nationale supérieure des mines de Paris, Université Paris sciences et lettres (PSL), Centre de Mise en Forme des Matériaux (CEMEF), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], 010504 meteorology & atmospheric sciences, Rubble, Stiffness, engineering.material, 010502 geochemistry & geophysics, 01 natural sciences, [SDU]Sciences of the Universe [physics], engineering, medicine, General Earth and Planetary Sciences, Geotechnical engineering, medicine.symptom, Pile, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: International audience
Published: 2020
Full Text: View/download PDF

21. The C-Band All-Sky Survey (C-BASS):Total intensity point source detection over the northern sky

Author: T. J. Pearson, Angela C. Taylor, Simon Harper, Justin L. Jonas, H M Heilgendorff, H C Chiang, Jamie Leech, J. P. Leahy, Jonathan Sievers, M. Jones, R. D. P. Grumitt, A. Barr, Clive Dickinson, R. Cepeda-Arroita, Michael W. Peel, A. C. S. Readhead, and Luke R. P. Jew
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Point source, media_common.quotation_subject, astro-ph.GA, Monte Carlo method, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Declination, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Remote sensing, media_common, Physics, 010308 nuclear & particles physics, Mexican hat wavelet, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a point-source detection algorithm that employs the second order Spherical Mexican Hat wavelet filter (SMHW2), and use it on 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 which 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 $4.76\,\mathrm{GHz}$ northern sky source catalogue in total intensity, containing 1784 sources and covering declinations $\delta\geq-10^{\circ}$. The C-BASS catalogue is matched with the Green Bank 6\,cm (GB6) and Parkes-MIT-NRAO (PMN) catalogues over their areas of common sky coverage. From this we estimate the $90$ per cent completeness level to be approximately $610\,\mathrm{mJy}$, with a corresponding reliability of $98$ per cent, when masking the brightest $30$ per cent 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 cent., Comment: 21 pages, 14 figures
Published: 2020
Full Text: View/download PDF

22. Rodney Deane Davies CBE. 8 January 1930—8 November 2015

Author: Clive Dickinson, Andrew Lyne, and Francis Graham-Smith
Subjects: Research career, History, 010308 nuclear & particles physics, 0103 physical sciences, General Medicine, 010303 astronomy & astrophysics, 01 natural sciences, MERLIN, Early life, Radio astronomy, Management
Abstract: Following early life on a farm in South Australia and a degree in Physics at the University of Adelaide, Rod Davies began his research career at the Radiophysics Laboratory in Sydney in 1951, working on the development of radio interferometers for solar observations. In 1953, he moved to the University of Manchester, Jodrell Bank, working with Bernard Lovell, later becoming the Director of Jodrell Bank from 1988 to 1997 and the President of the Royal Astronomical Society from 1987 to 1989. He is best known for leading observations of the structure of the cosmic microwave background, first carried out at Jodrell Bank and then transferred to Tenerife during the 1980s and 90s. Later, he was instrumental in establishing the European Space Agency's Planck spacecraft mission and continued after retirement to be closely involved in the interpretation of the data from Planck . He was elected a Fellow of the Royal Society in 1992 and awarded a CBE in 1995. During Rod's tenure as Director of Jodrell Bank, he was responsible for the start of a major project to upgrade the Lovell Telescope, recognizing that with increased capability it could play a leading role into the 21st century. He was also Director during a major upgrade to the MERLIN telescope array, completed around 1991, and making MERLIN a modern, useable, open-access instrument. It was transformed into a true national facility, funded by government, and widely used by the national and international radio astronomy community. Rod Davies was always a kind and generous colleague, and a great inspiration to several generations of radio astronomers.
Published: 2018
Full Text: View/download PDF

23. Revisiting the Distance to Radio Loops I and IV Using Gaia and Radio/Optical Polarization Data

Author: A. C. S. Readhead, Michael W. Peel, T. J. Pearson, Georgia Panopoulou, and Clive Dickinson
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Galactic Center, Extinction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Optical polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, CMB cold spot, Synchrotron, Magnetic field, law.invention, symbols.namesake, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), symbols, Planck, Astrophysics::Galaxy Astrophysics
Abstract: Galactic synchrotron emission exhibits large-angular-scale features known as radio spurs and loops. Determining the physical size of these structures is important for understanding the local interstellar structure and for modeling the Galactic magnetic field. However, the distance to these structures is either under debate or entirely unknown. We revisit a classical method of finding the location of radio spurs by comparing optical polarization angles with those of synchrotron emission as a function of distance. We consider three tracers of the magnetic field: stellar polarization, polarized synchrotron radio emission, and polarized thermal dust emission. We employ archival measurements of optical starlight polarization and Gaia distances, and construct a new map of polarized synchrotron emission from WMAP and Planck data. We confirm that synchrotron, dust emission, and stellar polarization angles all show a statistically significant alignment at high Galactic latitude. We obtain distance limits to three regions towards Loop I of 112$\pm$17 pc, 135$\pm$20 pc, and $ 30^\circ$ is local. This is consistent with the conclusions of earlier work based on stellar polarization and extinction, but in stark contrast with the Galactic center origin recently revisited on the basis of X-ray data. We also obtain a distance measurement towards part of Loop IV (180$\pm$15 pc) and find evidence that its synchrotron emission arises from chance overlap of structures located at different distances. Future optical polarization surveys will allow the expansion of this analysis to other radio spurs., Accepted by ApJ, 10 figures, 24 pages
Published: 2021
Full Text: View/download PDF

24. Cosmological parameter forecasts for H i intensity mapping experiments using the angular power spectrum

Author: Lucas C. Olivari, André A. Costa, Mathieu Remazeilles, Clive Dickinson, Simon Harper, Y-Z Ma, and Richard A. Battye
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, symbols.namesake, 0103 physical sciences, Emission spectrum, Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Intensity mapping, Spectral density, Astronomy and Astrophysics, Redshift, Space and Planetary Science, symbols, Dark energy, data analysis, cosmological parameters, dark energy, large-scale structure of Universe, radio continuum: galaxies, radio lines: galaxies [methods], Neutrino, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: HI intensity mapping is a new observational technique to survey the large-scale structure of matter using the 21 cm emission line of atomic hydrogen (HI). In this work, we simulate BINGO (BAO from Integrated Neutral Gas Observations) and SKA (Square Kilometre Array) phase-1 dish array operating in auto-correlation mode. For the optimal case of BINGO with no foregrounds, the combination of the HI angular power spectra with Planck results allows $w$ to be measured with a precision of $4\%$, while the combination of the BAO acoustic scale with Planck gives a precision of $7\%$. We consider a number of potentially complicating effects, including foregrounds and redshift dependent bias, which increase the uncertainty on $w$ but not dramatically; in all cases the final uncertainty is found to be $\Delta w < 8\%$ for BINGO. For the combination of SKA-MID in auto-correlation mode with Planck, we find that, in ideal conditions, $w$ can be measured with a precision of $4\%$ for the redshift range $0.35 < z < 3$ (i.e., for the bandwidth of $\Delta \nu = [350, 1050]$ MHz) and $2\%$ for $0 < z < 0.49$ (i.e., $\Delta \nu = [950, 1421]$ MHz). Extending the model to include the sum of neutrino masses yields a $95\%$ upper limit of $\sum m_\nu < 0.24$ eV for BINGO and $\sum m_\nu < 0.08$ eV for SKA phase 1, competitive with the current best constraints in the case of BINGO and significantly better than them in the case of SKA., Comment: 18 pages, 7 figures, 6 tables. Updated to match version accepted by MNRAS
Published: 2017
Full Text: View/download PDF

25. The OSIRIS-REx Laser Altimeter (OLA) Investigation and Instrument

Author: I. Aslam, Michael C. Nolan, Charles Brunet, Michael Daly, Edward B. Bierhaus, J. A. Seabrook, T. Haltigin, Olivier S. Barnouin, G. Cunningham, Clive Dickinson, D. Gaudreau, William V. Boynton, Catherine L. Johnson, A. Taylor, and Dante S. Lauretta
Subjects: 010504 meteorology & atmospheric sciences, Spacecraft, business.industry, Astronomy and Astrophysics, Terrain, 01 natural sciences, Sample (graphics), Planetary science, Lidar, Space and Planetary Science, Asteroid, 0103 physical sciences, Trajectory, Altimeter, business, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences, Remote sensing
Abstract: The Canadian Space Agency (CSA) has contributed to the Origins Spectral Interpretation Resource Identification Security-Regolith Explorer (OSIRIS-REx) spacecraft the OSIRIS-REx Laser Altimeter (OLA). The OSIRIS-REx mission will sample asteroid 101955 Bennu, the first B-type asteroid to be visited by a spacecraft. Bennu is thought to be primitive, carbonaceous, and spectrally most closely related to CI and/or CM meteorites. As a scanning laser altimeter, the OLA instrument will measure the range between the OSIRIS-REx spacecraft and the surface of Bennu to produce digital terrain maps of unprecedented spatial scales for a planetary mission. The digital terrain maps produced will measure $\sim7~\mbox{cm}$ per pixel globally, and $\sim3~\mbox{cm}$ per pixel at specific sample sites. In addition, OLA data will be used to constrain and refine the spacecraft trajectories. Global maps and highly accurate spacecraft trajectory estimates are critical to infer the internal structure of the asteroid. The global and regional maps also are key to gain new insights into the surface processes acting across Bennu, which inform the selection of the OSIRIS-REx sample site. These, in turn, are essential for understanding the provenance of the regolith sample collected by the OSIRIS-REx spacecraft. The OLA data also are important for quantifying any hazards near the selected OSIRIS-REx sample site and for evaluating the range of tilts at the sampling site for comparison against the capabilities of the sample acquisition device.
Published: 2017
Full Text: View/download PDF

26. Tests of star formation metrics in the low-metallicity galaxy NGC 5253 using ALMA observations of H30α line emission

Author: Kouichiro Nakanishi, D. Espada, Clive Dickinson, Rie E. Miura, George J. Bendo, Michael D'Cruze, Gary A. Fuller, and Robert Beswick
Subjects: dwarf [galaxies], Metallicity, Extinction (astronomy), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Submillimeter Array, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, Spiral galaxy, starburst [galaxies], 010308 nuclear & particles physics, Star formation, Stellar rotation, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, galaxies [radio lines], Galaxy, Space and Planetary Science, individual: NGC 5253 [galaxies], Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies]
Abstract: We use Atacama Large Millimeter/submillimeter Array (ALMA) observations of H30$\alpha$ (231.90 GHz) emission from the low metallicity dwarf galaxy NGC 5253 to measure the star formation rate (SFR) within the galaxy and to test the reliability of SFRs derived from other commonly-used metrics. The H30$\alpha$ emission, which originates mainly from the central starburst, yields a photoionizing photon production rate of (1.9$\pm$0.3)$\times$10$^{52}$ s$^{-1}$ and an SFR of 0.087$\pm$0.013 M$_\odot$ yr$^{-1}$ based on conversions that account for the low metallicity of the galaxy and for stellar rotation. Among the other star formation metrics we examined, the SFR calculated from the total infrared flux was statistically equivalent to the values from the H30$\alpha$ data. The SFR based on previously-published versions of the H$\alpha$ flux that were extinction corrected using Pa$\alpha$ and Pa$\beta$ lines were lower than but also statistically similar to the H30$\alpha$ value. The mid-infrared (22 $\mu$m) flux density and the composite star formation tracer based on H$\alpha$ and mid-infrared emission give SFRs that were significantly higher because the dust emission appears unusually hot compared to typical spiral galaxies. Conversely, the 70 and 160 $\mu$m flux densities yielded SFR lower than the H30$\alpha$ value, although the SFRs from the 70 $\mu$m and H30$\alpha$ data were within 1-2$\sigma$ of each other. While further analysis on a broader range of galaxies are needed, these results are instructive of the best and worst methods to use when measuring SFR in low metallicity dwarf galaxies like NGC 5253., Comment: 14 pages, 5 figures, accepted for publication in MNRAS
Published: 2017
Full Text: View/download PDF

27. Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD

Author: Mario G. Lattanzi, Carlo Baccigalupi, François Levrier, J. M. Duval, J. Austermann, M. Brilenkov, B. Thorne, Eiichiro Komatsu, D. Rambaud, T. Nagasaki, Peter Shirron, H. Imada, Nozomu Kogiso, Jeff Van Lanen, H. Takakura, T. Kawasaki, Lionel Duband, Ingunn Kathrine Wehus, Y. Hoshino, Tadayasu Dotani, Enrique Martinez-Gonzalez, Tucker Elleflot, S. Beckman, T. Kaga, Shogo Nakamura, A. Kato, Giorgio Savini, S. Bounissou, S. Mandelli, Peter Charles Hargrave, Francois Boulanger, Julien Grain, S. Realini, Reijo Keskitalo, Bruno Maffei, Y. Nagano, Davide Maino, D. Herman, Michael R. Vissers, B. Mot, R. Banerji, N. Katayama, James A. Beall, Johannes Hubmayr, Tomotake Matsumura, Shugo Oguri, G. Patanchon, S. Basak, S. Takakura, Créidhe O'Sullivan, Massimo Gervasi, Y. Takase, S. Stever, A. Carones, Raphael Flauger, F. J. Casas, T. de Haan, Yasuhiro Murata, T. Prouvé, Douglas Scott, P. Vielva, Toshiya Namikawa, Mayu Tominaga, Yuki Sakurai, Luca Lamagna, Eric Hivon, S. Nerval, Ken Ebisawa, Noriko Y. Yamasaki, Julian Borrill, Shingo Kashima, Hajime Sugai, M. De Petris, R. Nagata, Ted Kisner, D. W. Curtis, A. Mennella, P. de Bernardis, Alexandre E. Adler, Misao Sasaki, Jiansong Gao, Kam Arnold, K. Ganga, T. Ghigna, Kazunori Kohri, Ben Westbrook, R. Aurlien, T. Toda, Yasuhiro Takeda, U. Fuskeland, Alessandro Gruppuso, Giuseppe Puglisi, A. Ritacco, I. Kreykenbohm, C. Leloup, M. A. Dobbs, Jochen Weller, Joel N. Ullom, Chao-Lin Kuo, M. Migliaccio, Charles A. Hill, E. Allys, Nicola Vittorio, T. Yoshida, R. Takaku, Thomas Essinger-Hileman, Alessandro Paiella, J. Aumont, Berend Winter, Junji Yumoto, Yutaka Terao, Aritoki Suzuki, T. Hasebe, Toshiyuki Nishibori, A. Cukierman, P. Campeti, Y. Hirota, Alan J. Kogut, Josquin Errard, S. Sugiyama, L. P. L. Colombo, Anthony Challinor, Yohei Kobayashi, A. Kushino, Gemma Luzzi, Makoto Nagai, M. Sandri, Christopher Raum, Giuseppe D'Alessandro, Masashi Hazumi, Masaya Hasegawa, Renée Hlozek, Silvia Masi, Joseph Seibert, F. Piacentini, J. A. Murphy, Greg Jaehnig, Jose Alberto Rubino-Martin, Davide Poletti, Michael L. Brown, Blake D. Sherwin, Daniela Paoletti, Joshua Montgomery, F. Columbro, Gianluca Morgante, J. Bermejo, M. Tomasi, Haruki Nishino, P. Diego-Palazuelos, Hirokazu Ishino, T. Iida, Kazuhisa Mitsuda, Haruyuki Sakurai, Keith L. Thompson, Javier Cubas, Neil Trappe, Keisuke Shinozaki, Adrian T. Lee, Hiroyuki Ohsaki, Martina Gerbino, D. Herranz, M. Tsuji, Marco Bersanelli, Nadia Dachlythra, M. Russell, E. Gjerløw, Maresuke Shiraishi, E. de la Hoz, Eric V. Linder, Graeme Smecher, Eric R. Switzer, Erminia Calabrese, G. Roudil, Mario Zannoni, T. Maciaszek, L. Pagano, D. Auguste, Frank Grupp, Kosei Ishimura, Fabrizio Villa, Kuniaki Konishi, I. S. Ohta, G. Signorelli, J. Bonis, A. Tartari, Jun-ichi Suzuki, R. B. Barreiro, J. F. Cliche, M. Maki, Douglas H Beck, Ricardo Genova-Santos, A. J. Banday, M. Galloway, T. L. Svalheim, Fabio Finelli, L. A. Montier, H. K. Eriksen, Nicoletta Krachmalnicoff, Karen C. Cheung, Cristian Franceschet, Matthieu Tristram, V. Chan, G. Polenta, Clive Dickinson, N. W. Halverson, Kiyotomo Ichiki, Yuji Chinone, Mathieu Remazeilles, Giampaolo Pisano, Jon E. Gudmundsson, J. Peloton, M. Reinecke, Shannon M. Duff, Carole Tucker, Y. Minanmi, Gene C. Hilton, Martin Bucher, P. A. R. Ade, G. Vermeulen, K. Komatsu, Norio Okada, Thibaut Louis, Sophie Henrot-Versille, Edward J. Wollack, Paolo Natoli, Hideo Ogawa, Jörn Wilms, E. Taylor, Andrea Zonca, Makoto Hattori, Radek Stompor, Masahiro Tsujimoto, Yutaro Sekimoto, Marcin Gradziel, H. Thommesen, Zmuidzinas, Jonas, Sekimoto, Y, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, de Bernardis, P, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Columbro, F, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versillé, S, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minanmi, Y, Mitsuda, K, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Osaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Tambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stever, S, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique de l'ENS (LPTENS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Hautes Energies (LPTHE), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LiteBIRD, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Laboratoire de Physique Théorique de l'ENS [École Normale Supérieure] (LPTENS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), and Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, FOS: Physical sciences, 7. Clean energy, cryogenic telescope, law.invention, Cosmic microwave background, Entrance pupil, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, millimeter-wave polarization, space program, Settore FIS/05 - Astronomia e Astrofisica, law, Angular resolution, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Stray light, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Lens (optics), Cardinal point, Astrophysics - Instrumentation and Methods for Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: LiteBIRD has been selected as JAXA's strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) $B$-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of $-56$ dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34--161 GHz), one of LiteBIRD's onboard telescopes. It has a wide field-of-view ($18^\circ \times 9^\circ$) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90$^\circ$ are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at $5\,$K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented., Comment: 21 pages, 14 figures
Published: 2020
Full Text: View/download PDF

28. Hemispherical differences in the shape and topography of asteroid (101955) Bennu

Author: James H. Roberts, Benjamin Rozitis, Yun Zhang, E. B. Bierhaus, J. A. Seabrook, K. Getzandanner, Michael Daly, D. N. DellaGuistina, Clive Dickinson, P. Michel, Mark E. Perry, J. R. Weirich, Lydia C. Philpott, R. T. Daly, Robert Gaskell, Hannah C.M. Susorney, J. Geeraert, Andrew Ryan, Eric Palmer, G. Cunningham, Charles Brunet, M. Al Asad, Jason M. Leonard, M. C. Nolan, R. L. Ballouz, H. L. Enos, Olivier S. Barnouin, Dante S. Lauretta, D. Gaudreau, Coralie D. Adam, T. Haltigin, Bashar Rizk, Erwan Mazarico, Gregory A. Neumann, Catherine L. Johnson, Erica Jawin, Kevin J. Walsh, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Southwest Research Institute [Boulder] (SwRI), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), and University of Arizona
Subjects: business.product_category, 010504 meteorology & atmospheric sciences, Longitudinal ridges, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 01 natural sciences, 0103 physical sciences, Asymmetric distribution, Altimeter, Digital elevation model, 010303 astronomy & astrophysics, Geomorphology, Southern Hemisphere, Research Articles, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Northern Hemisphere, SciAdv r-articles, Wedge (mechanical device), Asteroid, [SDU]Sciences of the Universe [physics], business, Space Sciences, Geology, Research Article
Abstract: A lidar model of asteroid (101955) Bennu has a north-south asymmetry in shape and evidence of an early partial disruption., We investigate the shape of near-Earth asteroid (101955) Bennu by constructing a high-resolution (20 cm) global digital terrain model from laser altimeter data. By modeling the northern and southern hemispheres separately, we find that longitudinal ridges previously identified in the north extend into the south but are obscured there by surface material. In the south, more numerous large boulders effectively retain surface materials and imply a higher average strength at depth to support them. The north has fewer large boulders and more evidence of boulder dynamics (toppling and downslope movement) and surface flow. These factors result in Bennu’s southern hemisphere being rounder and smoother, whereas its northern hemisphere has higher slopes and a less regular shape. We infer an originally asymmetric distribution of large boulders followed by a partial disruption, leading to wedge formation in Bennu’s history.
Published: 2020
Full Text: View/download PDF

29. The C-Band All-Sky Survey (C-BASS): Simulated parametric fitting in single pixels in total intensity and polarization

Author: J. P. Leahy, Angela C. Taylor, T. J. Pearson, Jamie Leech, A. C. S. Readhead, Jonathan Sievers, Justin L. Jonas, R. D. P. Grumitt, Luke R. P. Jew, J Hill-Valler, H C Chiang, M. Jones, Michael W. Peel, Clive Dickinson, A. Barr, H M Heilgendorff, and Simon Harper
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Article, 010104 statistics & probability, 0103 physical sciences, 0101 mathematics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Parametric statistics, media_common, Physics, Spectral index, Pixel, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Polarization (waves), Amplitude, Space and Planetary Science, Sky, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The cosmic microwave background (CMB) B-mode signal is potentially weaker than the diffuse Galactic foregrounds over most of the sky at any frequency. A common method of separating the CMB from these foregrounds is via pixel-based parametric-model fitting. There are not currently enough all-sky maps to fit anything more than the most simple models of the sky. By simulating the emission in seven representative pixels, we demonstrate that the inclusion of a 5 GHz data point allows for more complex models of low-frequency foregrounds to be fitted than at present. It is shown that the inclusion of the C-BASS data will significantly reduce the uncertainties in a number of key parameters in the modelling of both the galactic foregrounds and the CMB. The extra data allow estimates of the synchrotron spectral index to be constrained much more strongly than is presently possible, with corresponding improvements in the accuracy of the recovery of the CMB amplitude. However, we show that to place good limits on models of the synchrotron spectral curvature will require additional low-frequency data.
Published: 2019
Full Text: View/download PDF

30. The C-Band All-Sky Survey (C-BASS): constraining diffuse Galactic radio emission in the North Celestial Pole region

Author: Charles Copley, A. Barr, H M Heilgendorff, R. D. P. Grumitt, M. Jones, H C Chiang, A. C. S. Readhead, Jamie Leech, Angela C. Taylor, Michael W. Peel, Clive Dickinson, Jonathan Sievers, Stephen Muchovej, Luke R. P. Jew, Justin L. Jonas, T. J. Pearson, E. M. Leitch, Mark Stevenson, Stuart Harper, and J. P. Leahy
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Synchrotron radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Declination, law.invention, RADIAÇÃO CONTÍNUA, Celestial pole, law, 0103 physical sciences, thermal { diuse radiation { radio continuum, 010303 astronomy & astrophysics, ISM, Astrophysics::Galaxy Astrophysics, media_common, Physics, Spectral index, 010308 nuclear & particles physics, Spinning dust, non-thermal { radiation mechanism, Astrophysics::Instrumentation and Methods for Astrophysics, surveys { radiation mechanism, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Synchrotron, Amplitude, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The C-Band All-Sky Survey C-BASS is a high-sensitivity all-sky radio survey at an angular resolution of 45 arcmin and a frequency of 4.7 GHz. We present a total intensity 4.7 GHz map of the North Celestial Pole (NCP) region of sky, above declination +80 deg, which is limited by source confusion at a level of ~0.6 mK 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 ~20-40 GHz. We quantify the anomalous microwave emission (AME) that is correlated with far-infrared dust emission. The AME amplitude does not change significantly (5 GHz; the best-fitting synchrotron temperature spectral index is $\beta=-2.91\pm0.04$ from 4.7 to 22.8 GHz and $\beta=-2.85\pm0.14$ from 22.8 to 44.1 GHz. Free-free emission is weak, contributing ~$7\,\mu$K rms (~7%) at 22.8 GHz. The best explanation for the AME is still electric dipole emission from small spinning dust grains., Comment: 18 pages, 6 figures, version matches version accepted by MNRAS
Published: 2019
Full Text: View/download PDF

31. The C-Band All-Sky Survey (C-BASS): digital backend for the northern survey

Author: J. J. John, O. G. King, Angela C. Taylor, T. J. Pearson, M. Jones, Stephen Muchovej, Charles Copley, Clive Dickinson, and Mark Stevenson
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), C band, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, polarimeters [instrumentation], 01 natural sciences, symbols.namesake, 0103 physical sciences, data analysis [methods], Demodulation, Planck, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Remote sensing, media_common, Physics, 010308 nuclear & particles physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, CMB cold spot, Bass (sound), Space and Planetary Science, Sky, symbols, general [radio continuum], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The C-Band All-Sky Survey (C-BASS) is an all-sky full-polarization survey at a frequency of 5 GHz, 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., Comment: Accepted for publication in MNRAS
Published: 2019
Full Text: View/download PDF

32. Modelling the spinning dust emission from LDN 1780

Author: Clive Dickinson, Adolf N. Witt, Simon Casassus, Simon Harper, and M. Vidal
Subjects: Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Library science, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We study the anomalous microwave emission (AME) in the Lynds Dark Nebula (LDN) 1780 on two angular scales. Using available ancillary data at an angular resolution of 1 degree, we construct an SED between 0.408 GHz to 2997 GHz. We show that there is a significant amount of AME at these angular scales and the excess is compatible with a physical spinning dust model. We find that LDN 1780 is one of the clearest examples of AME on 1 degree scales. We detected AME with a significance > 20$\sigma$. We also find at these angular scales that the location of the peak of the emission at frequencies between 23-70 GHz differs from the one on the 90-3000 GHz map. In order to investigate the origin of the AME in this cloud, we use data obtained with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) that provides 2 arcmin resolution at 30 GHz. We study the connection between the radio and IR emissions using morphological correlations. The best correlation is found to be with MIPS 70$\mu$m, which traces warm dust (T$\sim$50K). Finally, we study the difference in radio emissivity between two locations within the cloud. We measured a factor $\approx 6$ of difference in 30 GHz emissivity. We show that this variation can be explained, using the spinning dust model, by a variation on the dust grain size distribution across the cloud, particularly changing the carbon fraction and hence the amount of PAHs., Comment: 14 pages, 11 figures, submitted to MNRAS
Published: 2019

33. Hierarchical Bayesian CMB Component Separation with the No-U-Turn Sampler

Author: Clive Dickinson, Luke R. P. Jew, and R. D. P. Grumitt
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Bayesian probability, Pooling, Posterior probability, Sampling (statistics), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Hierarchical database model, symbols.namesake, Space and Planetary Science, 0103 physical sciences, symbols, Mean-shift, Cluster analysis, 010303 astronomy & astrophysics, Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics, Gibbs sampling
Abstract: Key to any cosmic microwave background (CMB) analysis is the separation of the CMB from foreground contaminants. In this paper we present a novel implementation of Bayesian CMB component separation. We sample from the full posterior distribution using the No-U-Turn Sampler (NUTS), a gradient based sampling algorithm. Alongside this, we introduce new foreground modelling approaches. We use the mean-shift algorithm to define regions on the sky, clustering according to naively estimated foreground spectral parameters. Over these regions we adopt a complete pooling model, where we assume constant spectral parameters, and a hierarchical model, where we model individual spectral parameters as being drawn from underlying hyper-distributions. We validate the algorithm against simulations of the LiteBIRD and C-BASS experiments, with an input tensor-to-scalar ratio of $r=5\times 10^{-3}$. Considering multipoles $32\leq\ell\leq 121$, we are able to recover estimates for $r$. With LiteBIRD only observations, and using the complete pooling model, we recover $r=(10\pm 0.6)\times 10^{-3}$. For C-BASS and LiteBIRD observations we find $r=(7.0\pm 0.6)\times 10^{-3}$ using the complete pooling model, and $r=(5.0\pm 0.4)\times 10^{-3}$ using the hierarchical model. By adopting the hierarchical model we are able to eliminate biases in our cosmological parameter estimation, and obtain lower uncertainties due to the smaller Galactic emission mask that can be adopted for power spectrum estimation. Measured by the rate of effective sample generation, NUTS offers performance improvements of $\sim10^3$ over using Metropolis-Hastings to fit the complete pooling model. The efficiency of NUTS allows us to fit the more sophisticated hierarchical foreground model, that would likely be intractable with non-gradient based sampling algorithms., Comment: 19 pages, 9 figures
Published: 2019
Full Text: View/download PDF

34. A first quantification of the effects of absorption for HI intensity mapping experiments

Author: Ian Browne, Clive Dickinson, Sambit Roychowdhury, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Analytical chemistry, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, galaxies: statistics, Physics, radio continuum: galaxies, radio lines: ISM, 010308 nuclear & particles physics, Intensity mapping, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: HI Intensity Mapping (IM) will be used to do precision cosmology using many existing and upcoming radio observatories. The signal will be contaminated due to absorption, the largest component of which will be the flux absorbed by the HI emitting sources themselves from the flux incident on them from background radio continuum sources. We, for the first time, provide a quantitative estimate of the magnitude of the absorbed flux compared to the emitted HI flux for various voxels placed at redshifts between 0.1 and 2.5. We use a cosmological sky simulation of the atomic HI emission line, and sum over the emitted and absorbed fluxes for all sources within voxels at different redshifts. For estimating the absorbed flux we use various relations based on existing observations as well as simulations. We find that for the same co-moving volume of sky, the HI emission falls off quickly with increasing redshift, while the absorption varies much less with redshift and follows the redshift distribution of faint sources that dominate the number counts of radio continuum sources. This results in the fraction of absorption compared to emission to be negligible in the nearby Universe (up to a redshift of ~0.5), increases to about 10% at a redshift of 1, and continues to increase to about 30% up to a redshift of 2.5. These numbers can vary significantly due to the uncertainties on the exact forms of the various relations used, the largest variation being driven by the uncertainty on the number counts of radio continuum sources at sub-mJy flux densities. Absorption of flux incident from background radio continuum sources might become an important contaminant to HI IM signals beyond redshifts of 0.5, and needs to be quantified more accurately using inputs from upcoming deep high resolution surveys of radio continuum sources, HI absorption, and HI emission with the SKA and its precursors., Comment: Accepted for publication in Astronomy & Astrophysics. 12+3 pages, 11 Figures, 2+1 tables. New version includes additional references and corrected numbers in Appendix B
Published: 2019
Full Text: View/download PDF

35. A Two Carrier Families Spectral Profile Model for Anomalous Microwave Emission

Author: Robert M. Shroll, Lawrence S. Bernstein, Clive Dickinson, and J. Quenneville
Subjects: Physics, Microwave emission, Space and Planetary Science, Astronomy and Astrophysics, Computational physics
Published: 2020
Full Text: View/download PDF

36. Baryon Acoustic Oscillations from Integrated Neutral Gas Observations:Radio Frequency Interference Measurements and Telescope Site Selection

Author: Sonia Anton, Christian Monstein, Ian Browne, G. Tancredi, M. Caldas, Luciano Barosi, K. S.F. Fornazier, Thyrso Villela, Carlos Alexandre Wuensche, Cesar Strauss, Elcio Abdalla, Clive Dickinson, and Michael W. Peel
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Site selection, Measure (physics), Radio telescope, FOS: Physical sciences, RFI, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, radio astronomy, 01 natural sciences, Electromagnetic interference, law.invention, Telescope, law, 0103 physical sciences, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Instrumentation, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, site selection, Intensity (physics), Baryon acoustic oscillations, Astrophysics - Instrumentation and Methods for Astrophysics, ADS-B, Radio astronomy
Abstract: The Baryon acoustic oscillations from Integrated Neutral Gas Observations (BINGO) telescope is a new 40-m class radio telescope to measure the large-angular-scale intensity of Hi emission at 980-1260 MHz to constrain dark energy parameters. As it needs to measure faint cosmological signals at the milliKelvin level, it requires a site that has very low radio frequency interference (RFI) at frequencies around 1 GHz. We report on measurement campaigns across Uruguay and Brazil to find a suitable site, which looked at the strength of the mobile phone signals and other radio transmissions, the location of wind turbines, and also included mapping airplane flight paths. The site chosen for the BINGO telescope is a valley at Serra do Urubu, a remote part of Paraiba in North-East Brazil, which has sheltering terrain. During our measurements with a portable receiver we did not detect any RFI in or near the BINGO band, given the sensitivity of the equipment. A radio quiet zone around the selected site has been requested to the Brazilian authorities ahead of the telescope construction., Preprint of an article accepted in the Journal of Astronomical Instrumentation, copyright 2018 World Scientific Publishing Company https://www.worldscientific.com/worldscinet/jai
Published: 2018
Full Text: View/download PDF

37. The C-Band All-Sky Survey (C-BASS):Design and capabilities

Author: Luke R. P. Jew, H M Heilgendorff, Jamie Leech, Angela C. Taylor, Stephen Muchovej, Justin L. Jonas, Clive Dickinson, A. C. S. Readhead, Charles Copley, O. G. King, Mark Stevenson, C. M. Holler, T. J. Pearson, R. D. P. Grumitt, H. Cynthia Chiang, Yaser Hafez, Moumita Aich, E. M. Leitch, J. J. John, R. J. Davis, Jonathan Sievers, M. Jones, J. P. Leahy, Michael W. Peel, Joe Zuntz, M. O. Irfan, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), C-BASS, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Laboratoire AIM, and Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay
Subjects: Planck, Diffuse radiation, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, radio continuum: general, Surveys, 01 natural sciences, 7. Clean energy, rotation, law.invention, law, optical, data analysis [Methods], [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, media_common, Physics, general [Radio continuum], Astrophysics::Instrumentation and Methods for Astrophysics, imaging, Polarization (waves), CMB cold spot, instrumentation: miscellaneous, symbols, astro-ph.CO, miscellaneous [Instrumentation], Astrophysics - Instrumentation and Methods for Astrophysics, performance, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, magnetic field: galaxy, Astrophysics::Cosmology and Extragalactic Astrophysics, frequency: high, Telescope, cosmic background radiation: B-mode, symbols.namesake, polarization: measured, surveys, 0103 physical sciences, synchrotron, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Radiometer, beam: polarization, Astronomy, resolution, Astronomy and Astrophysics, Polarimeter, stability, methods: data analysis, diffuse radiation, 13. Climate action, Space and Planetary Science, Sky, WMAP, correlation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: The C-Band All-Sky Survey (C-BASS) is an all-sky full-polarisation survey at a frequency of 5 GHz, designed to provide complementary data to the all-sky surveys of WMAP and Planck, and future CMB B-mode polarization imaging surveys. The observing frequency has been chosen to provide a signal that is dominated by Galactic synchrotron emission, but suffers little from Faraday rotation, so that the measured polarization directions provide a good template for higher frequency observations, and carry direct information about the Galactic magnetic field. Telescopes in both northern and southern hemispheres with matched optical performance are used to provide all-sky coverage from a ground-based experiment. A continuous-comparison radiometer and a correlation polarimeter on each telescope provide stable imaging properties such that all angular scales from the instrument resolution of 45 arcmin up to full sky are accurately measured. The northern instrument has completed its survey and the southern instrument has started observing. We expect that C-BASS data will significantly improve the component separation analysis of Planck and other CMB data, and will provide important constraints on the properties of anomalous Galactic dust and the Galactic magnetic field., Comment: 21 pages, 9 figures
Published: 2018
Full Text: View/download PDF

38. Potential impact of global navigation satellite services on total power HI intensity mapping surveys

Author: Stuart Harper and Clive Dickinson
Subjects: Physics, Potential impact, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Light pollution, Mode (statistics), Intensity mapping, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Signal, Power (physics), 13. Climate action, Space and Planetary Science, GNSS applications, 0103 physical sciences, Satellite, Astrophysics - Instrumentation and Methods for Astrophysics, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Remote sensing
Abstract: Future total-power single-dish HI intensity mapping (HI IM) surveys have the potential to provide unprecedented insight into late time ($z < 1$) cosmology that are competitive with Stage IV dark energy surveys. However, redshifts between $0 < z < 0.2$ lie within the transmission bands of global navigation satellite services (GNSS), and even at higher redshifts out-of-band leakage from GNSS satellites may be problematic. We estimate the impact of GNSS satellites on future single-dish HI IM surveys using realistic estimates of both the total power and spectral structure of GNSS signals convolved with a model SKA beam. Using a simulated SKA HI IM survey covering 30000 sq. deg. of sky and 200 dishes, we compare the integrated GNSS emission on the sky with the expected HI signal. It is found that for frequencies $> 950$ MHz the emission from GNSS satellites will exceed the expected HI signal for all angular scales to which the SKA is sensitive when operating in single-dish mode., 13 pages, 11 figures, "matches published version"
Published: 2018
Full Text: View/download PDF

39. Exploring Cosmic Origins with CORE:survey requirements and mission design

Author: Karl Young, N. Mandolesi, A. Renzi, D. McCarthy, Andrea Lapi, F. Voisin, F. Oppizzi, Mark Hindmarsh, A. Mennella, Josquin Errard, S. Martin, Jose M. Diego, Enrico Pajer, Douglas Scott, A. Da Silva, Luigi Danese, R. B. Partridge, Subodh P. Patil, Créidhe O'Sullivan, A. M. C. Le Brun, Gianluca Polenta, Deanna C. Hooper, Alessandro Buzzelli, O. Perdereau, Jose Alberto Rubino-Martin, Nicolas Ponthieu, C. J. A. P. Martins, Eric Hivon, M. De Petris, Reijo Keskitalo, Bruno Maffei, Rashid Sunyaev, Michael L. Brown, Elena Giusarma, Marek Biesiada, Joanes Lizarraga, Nicola Bartolo, F. Piacentini, Stephen M. Feeney, G. de Zotti, Neil Trappe, Bin Hu, Cristian Franceschet, Matthieu Tristram, Pasquale Mazzotta, R. Allison, Hannu Kurki-Suonio, Jens Chluba, J. Greenslade, R. Fernandez-Cobos, Alicia Gomez, Stephen Serjeant, A. Catalano, Paolo Natoli, C. S. Carvalho, K. Kiiveri, David L. Clements, Diego Molinari, S. Paradiso, Martina Gerbino, Vincent Vennin, Carole Tucker, Kaustuv Basu, Alexei A. Starobinsky, Sabino Matarrese, Andrea Ravenni, L. Salvati, Eduardo Artal, G. Vermeulen, M. Piat, M. Tucci, F. Noviello, Ingunn Kathrine Wehus, Elia S. Battistelli, Matteo Bonato, R. Banerji, Ted Kisner, Jean-Baptiste Melin, Christophe Ringeval, Christopher G. R. Wallis, Benjamin D. Wandelt, Julian Borrill, Massimiliano Lattanzi, Aurelien Bideaud, Sebastien Clesse, Tiziana Trombetti, Martin Crook, Will Handley, P. de Bernardis, Ruth Durrer, Francois Boulanger, Matthieu Roman, C. Y. Tan, Sébastien Triqueneaux, Silvia Galli, G. Signorelli, A. Tartari, Gianmassimo Tasinato, S. Basak, Nicola Vittorio, D. Tramonte, V. Lindholm, Julien Lesgourgues, J. F. Macías-Pérez, E. Di Valentino, Francesco Forastieri, G. de Gasperis, Thomas Kitching, Vincent Desjacques, François R. Bouchet, Zhen-Yi Cai, Sergio Colafrancesco, Richard A. Battye, Alessandro Monfardini, F.-X. Désert, Alessandro Paiella, Jesús Torrado, Michele Liguori, Anthony Challinor, Carlo Burigana, G. Castellano, Agnieszka Pollo, Daniel Baumann, L. Pagano, Boudewijn F. Roukema, Mathieu Remazeilles, Sophie Henrot-Versille, M. Tomasi, Enrique Martinez-Gonzalez, Giampaolo Pisano, M. Kunz, Joseph J. Mohr, Ricardo Genova-Santos, P. Vielva, Mattia Negrello, Marcella Massardi, Carlo Baccigalupi, Guilaine Lagache, Marco Bersanelli, Anthony Lasenby, S. Hagstotz, Domingos Barbosa, E. Keihänen, D. Prêle, Vivian Poulin, Mario Zannoni, Alain Benoit, Ana Achúcarro, D. T. Hoang, I. Colantoni, U. Fuskeland, D. Contreras, Giovanni Cabass, Jochem J. A. Baselmans, Johannes Goupy, Jochen Weller, I. Charles, Sebastian Grandis, Giuseppe D'Alessandro, M. Ashdown, A. Bonaldi, Frederico Arroja, Guido D'Amico, Gemma Luzzi, M. A. de Avillez, Martino Calvo, Silvia Masi, Daniela Paoletti, Alessandro Coppolecchia, Andrea Caputo, L. Polastri, Alessandro Melchiorri, Jon Urrestilla, Licia Verde, Mario Ballardini, Luisa Toffolatti, Jacques Delabrouille, Alessio Notari, Maciej Bilicki, Fabio Finelli, L. A. Montier, James G. Bartlett, Guillaume Patanchon, Carlos Hernández-Monteagudo, Miguel Quartin, Cora Dvorkin, Simon Doyle, H. K. Eriksen, C. Hervias-Caimapo, R. van de Weygaert, Clive Dickinson, Peter A. R. Ade, Matthew Hills, Luca Lamagna, B. Van Tent, A. J. Banday, Thejs Brinckmann, F. J. Casas, Martin Bucher, Shaul Hanany, Jussi Valiviita, J. González-Nuevo, Diederik Roest, String Theory (ITFA, IoP, FNWI), Universitat de Barcelona, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut Nanosciences et Cryogénie (INAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), CORE, Department of Physics, Helsinki Institute of Physics, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Grenoble Alpes (UGA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Sorbonne Université (SU), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Delabrouille, J, de Bernardis, P, Bouchet, F, Achúcarro, A, Ade, P, Allison, R, Arroja, F, Artal, E, Ashdown, M, Baccigalupi, C, Ballardini, M, Banday, A, Banerji, R, Barbosa, D, Bartlett, J, Bartolo, N, Basak, S, Baselmans, J, Basu, K, Battistelli, E, Battye, R, Baumann, D, Benoít, A, Bersanelli, M, Bideaud, A, Biesiada, M, Bilicki, M, Bonaldi, A, Bonato, M, Borrill, J, Boulanger, F, Brinckmann, T, Brown, M, Bucher, M, Burigana, C, Buzzelli, A, Cabass, G, Cai, Z, Calvo, M, Caputo, A, Carvalho, C, Casas, F, Castellano, G, Catalano, A, Challinor, A, Charles, I, Chluba, J, Clements, D, Clesse, S, Colafrancesco, S, Colantoni, I, Contreras, D, Coppolecchia, A, Crook, M, D'Alessandro, G, D'Amico, G, da Silva, A, de Avillez, M, de Gasperis, G, De Petris, M, de Zotti, G, Danese, L, Désert, F, Desjacques, V, Valentino, E, Dickinson, C, Diego, J, Doyle, S, Durrer, R, Dvorkin, C, Eriksen, H, Errard, J, Feeney, S, Fernández-Cobos, R, Finelli, F, Forastieri, F, Franceschet, C, Fuskeland, U, Galli, S, Génova-Santos, R, Gerbino, M, Giusarma, E, Gomez, A, González-Nuevo, J, Grandis, S, Greenslade, J, Goupy, J, Hagstotz, S, Hanany, S, Handley, W, Henrot-Versillé, S, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Hindmarsh, M, Hivon, E, Hoang, D, Hooper, D, Hu, B, Keihänen, E, Keskitalo, R, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamagna, L, Lapi, A, Lasenby, A, Lattanzi, M, Brun, A, Lesgourgues, J, Liguori, M, Lindholm, V, Lizarraga, J, Luzzi, G, Macìas-Pérez, J, Maffei, B, Mandolesi, N, Martin, S, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Mazzotta, P, Mccarthy, D, Melchiorri, A, Melin, J, Mennella, A, Mohr, J, Molinari, D, Monfardini, A, Montier, L, Natoli, P, Negrello, M, Notari, A, Noviello, F, Oppizzi, F, O'Sullivan, C, Pagano, L, Paiella, A, Pajer, E, Paoletti, D, Paradiso, S, Partridge, R, Patanchon, G, Patil, S, Perdereau, O, Piacentini, F, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Ponthieu, N, Poulin, V, Prêle, D, Quartin, M, Ravenni, A, Remazeilles, M, Renzi, A, Ringeval, C, Roest, D, Roman, M, Roukema, B, Rubiño-Martin, J, Salvati, L, Scott, D, Serjeant, S, Signorelli, G, Starobinsky, A, Sunyaev, R, Tan, C, Tartari, A, Tasinato, G, Toffolatti, L, Tomasi, M, Torrado, J, Tramonte, D, Trappe, N, Triqueneaux, S, Tristram, M, Trombetti, T, Tucci, M, Tucker, C, Urrestilla, J, Väliviita, J, de Weygaert, R, Tent, B, Vennin, V, Verde, L, Vermeulen, G, Vielva, P, Vittorio, N, Voisin, F, Wallis, C, Wandelt, B, Wehus, I, Weller, J, Young, K, and Zannoni, M
Subjects: CMBR experiments, CMBR polarisation, gravitational lensing, physics of the early universe, POLARIZATION, Computer science, Cosmic microwave background, cosmic background radiation: polarization, CMB, 7. Clean energy, 01 natural sciences, Cosmology, Physics, Particles & Fields, cosmic flows, CMBR polarization, astronomy and astrophysics, Cosmic physics, CMBR experiments – CMBR theory – reionization – high redshift galaxies, 010303 astronomy & astrophysics, QC, QB, COSMIC cancer database, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Nuclear & Particles Physics, cryogenics, Physical Sciences, Physics::Space Physics, Systems engineering, astro-ph.CO, proposed experiment, Astrophysics::Earth and Planetary Astrophysics, CMBR experiment, Astrophysics - Instrumentation and Methods for Astrophysics, performance, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), CMBR experiments, CMBR polarisation, gravitational lensing, physics of the early universe, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, NO, HALF-WAVE PLATE, 0202 Atomic, Molecular, Nuclear, Particle And Plasma Physics, Mission design, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), detector: design, activity report, Science & Technology, Cosmologia, 010308 nuclear & particles physics, astro-ph.IM, 115 Astronomy, Space science, sensitivity, Complementarity (physics), 0201 Astronomical And Space Sciences, angular resolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Física còsmica
Abstract: The CORE collaboration thanks CNES, Thales Alenia Space, and Air Liquide Advanced Technologies for advice and technical support during the preparation of the CORE proposal. We also thank the ESA CDF team for the CMB Polarisation CDF study performed in March 2016, the results of which were extensively used to define the mission concept presented in this paper. J.G.N. acknowledges financial support from the Spanish MINECO for a Ramon y Cajal fellowship (RYC-2013-13256) and the I+D 2015 project AYA2015-65887-P (MINECO/FEDER). CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE. F.J.C., R.F.-C., E.M.-G. and P.V. acknowledge support from the Spanish Ministerio de Econom´ıa y Competitividad project ESP2015-70646-C2-1-R (cofinanced with EU FEDER funds), ConsoliderIngenio 2010 project CSD2010-00064 and from the CSIC “Proyecto Intramural Especial” project 201550E091. FA is supported by the National Taiwan University (NTU) under Project No. 103R4000 and by the NTU Leung Center for Cosmology and Particle Astrophysics (LeCosPA) under Project No. FI121. BFR acknowledges support from the National Science Centre, Poland, under grant 2014/13/B/ST9/00845., Macìas-Pérez, J.F., Delabrouille, J., De Bernardis, P., Bouchet, F.R., Achúcarro, A., Ade, P.A.R., Allison, R., Arroja, F., Artal, E., Ashdown, M., Baccigalupi, C., Ballardini, M., Banday, A.J., Banerji, R., Barbosa, D., Bartlett, J., Bartolo, N., Basak, S., Baselmans, J.J.A., Basu, K., Battistelli, E.S., Battye, R., Baumann, D., Benoít, A., Bersanelli, M., Bideaud, A., Biesiada, M., Bilicki, M., Bonaldi, A., Bonato, M., Borrill, J., Boulanger, F., Brinckmann, T., Brown, M.L., Bucher, M., Burigana, C., Buzzelli, A., Cabass, G., Cai, Z.-Y., Calvo, M., Caputo, A., Carvalho, C.-S., Casas, F.J., Castellano, G., Catalano, A., Challinor, A., Charles, I., Chluba, J., Clements, D.L., Clesse, S., Colafrancesco, S., Colantoni, I., Contreras, D., Coppolecchia, A., Crook, M., D'Alessandro, G., D'Amico, G., Silva, A.D., De Avillez, M., De Gasperis, G., Petris, M.D., De Zotti, G., Danese, L., Désert, F.-X., Desjacques, V., Valentino, E.D., Dickinson, C., Diego, J.M., Doyle, S., Durrer, R., Dvorkin, C., Eriksen, H.K., Errard, J., Feeney, S., Fernández-Cobos, R., Finelli, F., Forastieri, F., Franceschet, C., Fuskeland, U., Galli, S., Génova-Santos, R.T., Gerbino, M., Giusarma, E., Gomez, A., González-Nuevo, J., Grandis, S., Greenslade, J., Goupy, J., Hagstotz, S., Hanany, S., Handley, W., Henrot-Versillé, S., Hernández-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Hindmarsh, M., Hivon, E., Hoang, D.T., Hooper, D.C., Hu, B., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lapi, A., Lasenby, A., Lattanzi, M., Brun, A.M.C.L., Lesgourgues, J., Liguori, M., Lindholm, V., Lizarraga, J., Luzzi, G., Macìas-Pérez, J.F., Maffei, B., Mandolesi, N., Martin, S., Martinez-Gonzalez, E., Martins, C.J.A.P., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., McCarthy, D., Melchiorri, A., Melin, J.-B., Mennella, A., Mohr, J., Molinari, D., Monfardini, A., Montier, L., Natoli, P., Negrello, M., Notari, A., Noviello, F., Oppizzi, F., O'Sullivan, C., Pagano, L., Paiella, A., Pajer, E., Paoletti, D., Paradiso, S., Partridge, R.B., Patanchon, G., Patil, S.P., Perdereau, O., Piacentini, F., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Ponthieu, N., Poulin, V., Prêle, D., Quartin, M., Ravenni, A., Remazeilles, M., Renzi, A., Ringeval, C., Roest, D., Roman, M., Roukema, B.F., Rubiño-Martin, J.-A., Salvati, L., Scott, D., Serjeant, S., Signorelli, G., Starobinsky, A.A., Sunyaev, R., Tan, C.Y., Tartari, A., Tasinato, G., Toffolatti, L., Tomasi, M., Torrado, J., Tramonte, D., Trappe, N., Triqueneaux, S., Tristram, M., Trombetti, T., Tucci, M., Tucker, C., Urrestilla, J., Väliviita, J., De Weygaert, R.V., Tent, B.V., Vennin, V., Verde, L., Vermeulen, G., Vielva, P., Vittorio, N., Voisin, F., Wallis, C., Wandelt, B., Wehus, I.K., Weller, J., Young, K., Zannoni, M.
Published: 2018
Full Text: View/download PDF

40. Impact of SZ cluster residuals in CMB maps and CMB-LSS cross-correlations

Author: Tianyue Chen, Mathieu Remazeilles, and Clive Dickinson
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Cosmic background radiation, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Residual, 01 natural sciences, Spectral line, symbols.namesake, 13. Climate action, Space and Planetary Science, 0103 physical sciences, symbols, Cluster (physics), Planck, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Residual foreground contamination in cosmic microwave background (CMB) maps, such as the residual contamination from thermal Sunyaev-Zeldovich (SZ) effect in the direction of galaxy clusters, can bias the cross-correlation measurements between CMB and large-scale structure optical surveys. It is thus essential to quantify those residuals and, if possible, to null out SZ cluster residuals in CMB maps. We quantify for the first time the amount of SZ cluster contamination in the released Planck 2015 CMB maps through (i) the stacking of CMB maps in the direction of the clusters, and (ii) the computation of cross-correlation power spectra between CMB maps and the SDSS-IV large-scale structure data. Our cross-power spectrum analysis yields a $30\sigma$ detection at the cluster scale ($\ell=1500-2500$) and a $39\sigma$ detection on larger scales ($\ell=500-1500$) due to clustering of SZ clusters, giving an overall $54\sigma$ detection of SZ cluster residuals in the Planck CMB maps. The Planck 2015 NILC CMB map is shown to have $44\pm4\%$ of thermal SZ foreground emission left in it. Using the 'Constrained ILC' component separation technique, we construct an alternative Planck CMB map, the 2D-ILC map, which is shown to have negligible SZ contamination, at the cost of being slightly more contaminated by Galactic foregrounds and noise. We also discuss the impact of the SZ residuals in CMB maps on the measurement of the ISW effect, which is shown to be negligible based on our analysis., Comment: 14 pages, 11 figures, 1 table, accepted by MNRAS, close to the published version
Published: 2018
Full Text: View/download PDF

41. Sensitivity and foreground modelling for large-scale cosmic microwave background B-mode polarization satellite missions

Author: Ingunn Kathrine Wehus, H. K. Eriksen, Clive Dickinson, and Mathieu Remazeilles
Subjects: Physics, Spectral index, 010308 nuclear & particles physics, Spinning dust, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic background radiation, Astronomy, Spectral density, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Gravitational lens, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics
Abstract: The measurement of the large-scale B-mode polarization in the cosmic microwave background (CMB) is a fundamental goal of future CMB experiments. However, because of unprecedented sensitivity, future CMB experiments will be much more sensitive to any imperfect modelling of the Galactic foreground polarization in the reconstruction of the primordial B-mode signal. We compare the sensitivity to B-modes of different concepts of CMB satellite missions (LiteBIRD, COrE, COrE+, PRISM, EPIC, PIXIE) in the presence of Galactic foregrounds. In particular, we quantify the impact on the tensor-to-scalar parameter of incorrect foreground modelling in the component separation process. Using Bayesian fitting and Gibbs sampling, we perform the separation of the CMB and Galactic foreground B-modes. The recovered CMB B-mode power spectrum is used to compute the likelihood distribution of the tensor-to-scalar ratio. We focus the analysis to the very large angular scales that can be probed only by CMB space missions, i.e. the reionization bump, where primordial B-modes dominate over spurious B-modes induced by gravitational lensing. We find that fitting a single modified blackbody component for thermal dust where the ‘real’ sky consists of two dust components strongly bias the estimation of the tensor-to-scalar ratio by more than 5σ for the most sensitive experiments. Neglecting in the parametric model the curvature of the synchrotron spectral index may bias the estimated tensor-to-scalar ratio by more than 1σ. For sensitive CMB experiments, omitting in the foreground modelling a 1 per cent polarized spinning dust component may induce a non-negligible bias in the estimated tensor-to-scalar ratio. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Published: 2016
Full Text: View/download PDF

42. Loops and arcs in the radio sky

Author: Clive Dickinson, Michael W. Peel, Matias Vidal, and P. Leahy
Subjects: Physics, symbols.namesake, Sky, media_common.quotation_subject, symbols, General Physics and Astronomy, Astrophysics, Planck, media_common
Abstract: Michael Peel, Matias Vidal, Clive Dickinson and Paddy Leahy explain the discoveries underlying this stunning new map from the Planck Collaboration.
Published: 2016
Full Text: View/download PDF

43. Observations of free–free and anomalous microwave emission from LDN 1622 with the 100 m Green Bank Telescope

Author: Clive Dickinson, K. A. Cleary, and Simon Harper
Subjects: Physics, Infrared, Spinning dust, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Extinction (astronomy), Green Bank Telescope, FOS: Physical sciences, Astronomy, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Photodissociation region, Astrophysics - Astrophysics of Galaxies, Corona, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, media_common
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 WISE. This Paper presents arcminute resolution mapping observations of LDN 1622 at 4.85 GHz and 13.7 GHz using the 100 m Robert C. Byrd Green Bank Telescope. The 4.85 GHz map reveals a corona of free-free emission enclosing LDN 1622 that traces the photo-dissociation region of the cloud. The brightest peaks of the 4.85 GHz map are found to be within 10% agreement with the expected free-free predicted by SHASSA H{\alpha} data of LDN 1622. At 13.7 GHz the AME flux density was found to be 7.0 $\pm$ 1.4 mJy and evidence is presented for a rising spectrum between 13.7 GHz 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., Comment: 12 pages, 7 figures
Published: 2015
Full Text: View/download PDF

44. QUIJOTE scientific results – I. Measurements of the intensity and polarisation of the anomalous microwave emission in the Perseus molecular complex

Author: Keith Grainge, Paul F. Scott, Nima Razavi-Ghods, Anthony Lasenby, Simon J. Melhuish, J. A. Rubiño Martín, Lucio Piccirillo, E. Martínez-González, M. Ashdown, Rafael Rebolo, David Titterington, Ricardo Genova-Santos, Clive Dickinson, Jose M. Diego, Simon Harper, Frédérick Poidevin, R. B. Barreiro, Roger J. Hoyland, Mark McCulloch, Robert A. Watson, D. Herranz, Carlos H. López-Caraballo, A. Peláez-Santos, R. Fernandez-Cobos, P. Vielva, B. Casaponsa, M. López-Caniego, Carlos M. Gutiérrez, D. Tramonte, R. Vignaga, Yvette C. Perrott, Universidad de La Serena (Chile), European Research Council, Ministerio de Economía y Competitividad (España), and Science and Technology Facilities Council (UK)
Subjects: Diffuse radiation, Physics, Radio continuum: ISM, Astronomy and Astrophysics, Astrophysics, Radiation mechanisms: general, ISM. [Radio continuum], Dipole, ISM: individual objects: G159.6-18.5, Microwave emission, individual objects: G159.6-18.5 [ISM], Space and Planetary Science, Angular resolution, Independent data, Intensity (heat transfer), general [Radiation mechanisms]
Abstract: et al., In this paper, we present Q-U-I JOint Tenerife Experiment (QUIJOTE) 10–20 GHz observations (194 h in total over ≈250 deg2) in intensity and polarisation of G159.6-18.5, one of the most widely studied regions harbouring anomalous microwave emission (AME). By combining with other publicly available intensity data, we achieve the most precise spectrum of the AME measured to date in an individual region, with 13 independent data points between 10 and 50 GHz being dominated by this emission. The four QUIJOTE data points provide the first independent confirmation of the downturn of the AME spectrum at low frequencies, initially unveiled by the COSMOlogical Structures On Medium Angular Scales experiment in this region. Our polarisation maps, which have an angular resolution of ≈1° and a sensitivity of ≈ 25 μK beam−1, are consistent with zero polarisation. We obtain upper limits on the polarisation fraction of Π < 6.3 and, This work has been partially funded by the Spanish Ministry of Economy and Competitiveness (MINECO) under the projects AYA2007-68058-C03-01, AYA2010-21766-C03-02, AYA2012-39475-C02-01 and the Consolider-Ingenio project CSD2010-00064 (EPI: Exploring the Physics of Inflation). CD acknowledges support from an ERC Starting (Consolidator) Grant (no. 307209), SH from an STFC-funded studentship, and CHLC from the DIULS (Research Directorship of the University of La Serena).
Published: 2015
Full Text: View/download PDF

45. An improved source-subtracted and destriped 408-MHz all-sky map

Author: M.-A. Bigot-Sazy, Tuhin Ghosh, Mathieu Remazeilles, Clive Dickinson, and A. J. Banday
Subjects: Physics, media_common.quotation_subject, Cosmic microwave background, Spectral density, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, CMB cold spot, Galaxy, Space and Planetary Science, Sky, Scale (map), Reionization, Astrophysics::Galaxy Astrophysics, Noise (radio), media_common
Abstract: The all-sky 408 MHz map of Haslam et al. is one the most important total-power radio surveys. It has been widely used to study diffuse synchrotron radiation from our Galaxy and as a template to remove foregrounds in cosmic microwave background data. However, there are a number of issues associated with it that must be dealt with, including large-scale striations and contamination from extragalactic radio sources. We have re-evaluated and reprocessed the rawest data available to produce a new and improved 408-MHz all-sky map. We first quantify the positional accuracy (?��7 arcmin) and effective beam (56.0 �� 1.0 arcmin) of the four individual surveys from which it was assembled. Large-scale striations associated with 1/f noise in the scan direction are reduced to a level ?�?1 K using a Fourier-based filtering technique. The most important improvement results from the removal of extragalactic sources. We have used an iterative combination of two techniques - two-dimensional Gaussian fitting and minimum curvature spline surface inpainting - to remove the brightest sources (?�?2 Jy), which provides a significant improvement over previous versions of the map. We quantify the impact with power spectra and a template fitting analysis of foregrounds to the WMAP data. The new map is publicly available and is recommended as the template of choice for large-scale diffuse Galactic synchrotron emission. We also provide a higher resolution map with small-scale fluctuations added, assuming a power-law angular power spectrum down to the pixel scale (1.7 arcmin). This should prove useful in simulations used for studying the feasibility of detecting H I fluctuations from the Epoch of Reionization.
Published: 2015
Full Text: View/download PDF

46. ALMA observations of 99 GHz free–free and H40α line emission from star formation in the centre of NGC 253

Author: Clive Dickinson, Michael D'Cruze, Robert Beswick, T. W. B. Muxlow, Gary A. Fuller, and George J. Bendo
Subjects: Physics, Photon, Opacity, Star formation, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Electron, Astrophysics, Astrophysics - Astrophysics of Galaxies, Submillimeter Array, Galaxy, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Millimeter, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: We present Atacama Large Millimeter/submillimeter Array observations of 99.02 GHz free-free and H40$\alpha$ emission from the centre of the nearby starburst galaxy NGC 253. We calculate electron temperatures of 3700-4500 K for the photoionized gas, which agrees with previous measurements. We measure a photoionizing photon production rate of $(3.2\pm0.2)\times10^{53}$ s$^{-1}$ and a star formation rate of $1.73\pm0.12$ M$_\odot$ yr$^{-1}$ within the central 20$\times$10 arcsec, which fall within the broad range of measurements from previous millimetre and radio observations but which are better constrained. We also demonstrate that the dust opacities are ~3 dex higher than inferred from previous near-infrared data, which illustrates the benefits of using millimetre star formation tracers in very dusty sources., Comment: 5 pages, 3 figures, accepted for publication in MNRAS Letters
Published: 2015
Full Text: View/download PDF

47. The State-of-Play of Anomalous Microwave Emission (AME) research

Author: Angela C. Taylor, Jose Alberto Rubino-Martin, J. Hill-Valler, Brandon S. Hensley, Jamie Leech, Thiem Hoang, A. Barr, Roberta Paladini, Ricardo Genova-Santos, Kieran Cleary, J. P. Leahy, Matias Vidal, Bruce T. Draine, Yvette C. Perrott, Luke R. P. Jew, Frank P. Israel, A. C. S. Readhead, Carlos H. López-Caraballo, Stuart Harper, M. Todorović, Simon Casassus, Frédérick Poidevin, Yacine Ali-Haïmoud, Lawrence S. Bernstein, Aaron C. Bell, Takashi Onaka, Iain McDonald, Alex Lazarian, Clive Dickinson, Elia S. Battistelli, Michael W. Peel, Eric J. Murphy, and Christopher Tibbs
Subjects: cosmic microwave background, Opacity, Diffuse radiation, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, 01 natural sciences, 7. Clean energy, radio continuum, Magnetization, Interstellar medium, 0103 physical sciences, Radiation mechanisms, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Spinning dust, interstellar medium, 010308 nuclear & particles physics, spinning dust, Astronomy and Astrophysics, radiation mechanisms, diffuse radiation, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Wavelength, Radio continuum, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Magnetic dipole
Abstract: Anomalous Microwave Emission (AME) is a component of diffuse Galactic radiation observed at frequencies in the range $\approx 10$-60 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-free 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 ($\lesssim 1$%). 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 ($\gtrsim 50$ 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., Comment: Accepted for publication in New Astronomy Reviews. Summary of AME workshop held at ESTEC, The Netherlands, June 2016, 40 pages, 18 figures. Updated to approximately match published version
Published: 2018
Full Text: View/download PDF

48. 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 , 0 )

Author: Sergio Molinari, Sean Carey, Alberto Noriega-Crespo, Clive Dickinson, Alessio Traficante, J. Ingalls, Roberta Paladini, Christopher Tibbs, Paolo Natoli, R. D. Davies, M. I. R. Alves, Gary A. Fuller, L. Cambresy, Mathieu Compiegne, R. J. Davis, and Steven J. Gibson
Subjects: Physics, Line-of-sight, Galactic Center, FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Plasma, Radiation, Galactic plane, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Square degree, 010104 statistics & probability, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Ionization, 0103 physical sciences, 0101 mathematics, Atomic physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Herschel FIR continuum data obtained as part of the Hi-GAL survey have been used, together with the GLIMPSE 8 $\mu$m and MIPSGAL 24 $\mu$m data, to attempt the first 3D-decomposition of dust emission associated with atomic, molecular and ionized gas at 15 arcmin angular resolution. Our initial test case is a 2$\times$2 square degrees region centred on (l,b)=(30$^{\circ}$,0$^{\circ}$), a direction that encompasses the origin point of the Scutum-Crux Arm at the tip of the Galactic Bar. Coupling the IR maps with velocity maps specific for different gas phases (HI 21cm, $^{12}$CO and $^{13}$CO, and RRLs), we estimate the properties of dust blended with each of the gas components and at different Galactocentric distances along the LOS. A statistical Pearson's coefficients analysis is used to study the correlation between the column densities and the intensity of the IR emission. This analysis provides evidence that the 2$\times$2 square degree field under consideration is characterized by the presence of a gas component not accounted for by the standard tracers, possibly associated with warm H$_{2}$ and cold HI. We demonstrate that the IR radiation in the range 8 $\mu$m $, Comment: Accepted for publication in MNRAS. 30 pages, 20 figures, 7 tables
Published: 2014
Full Text: View/download PDF

49. Phoenix LIDAR measurements of Mars atmospheric dust

Author: Clive Dickinson, L. Komguem, Mark T. Lemmon, James A. Whiteway, and Michael Daly
Subjects: Atmosphere, Martian, Daytime, Lidar, Backscatter, Meteorology, Space and Planetary Science, Planetary boundary layer, Mie scattering, Environmental science, Astronomy and Astrophysics, Mars Exploration Program, Atmospheric sciences
Abstract: The LIDAR instrument on the Phoenix mission obtained measurements of atmospheric dust and clouds from the surface in the Arctic region of Mars (68.22°N, 234.25°E) during late spring through the middle of summer. The observed vertical distribution of dust indicated that the planetary boundary layer (PBL) was evenly mixed up to heights of 4 km by daytime convection and turbulence. The values of the dust optical extinction coefficient derived from the LIDAR measurements within the PBL reached a maximum of 0.15 km −1 during the period around summer solstice and then decreased to values approaching 0.03 km −1 over the next 60 martian days (sols). The ratio of the LIDAR backscatter coefficient at wavelength 1064 nm to that at 532 nm for dust was obtained in three cases and found to have values in the range 1.18–1.35, relative to an assumed value of unity for the near surface water ice clouds. Mie scattering calculations were performed to determine that the measured dust 1064/532 backscatter color ratios were consistent with particle size distributions having effective radii in the range of 1.2–1.4 μm.
Published: 2013
Full Text: View/download PDF

50. Joint Bayesian estimation of tensor and lensing B-modes in the power spectrum of CMB polarization data

Author: Mathieu Remazeilles, Ingunn Kathrine Wehus, H. K. Eriksen, and Clive Dickinson
Subjects: Physics, weak, polarization, methods: analytical, cosmic background radiation, early Universe, inflation [gravitational lensing], Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Cosmic background radiation, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Cosmic variance, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, 01 natural sciences, Gravitational lens, South Pole Telescope, Space and Planetary Science, 0103 physical sciences, Probability distribution, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the performance of a simple Bayesian fitting approach to correct the cosmic microwave background (CMB) B-mode polarization for gravitational lensing effects in the recovered probability distribution of the tensor-to-scalar ratio. We perform a two-dimensional power spectrum fit of the amplitude of the primordial B-modes (tensor-to-scalar ratio, $r$) and the amplitude of the lensing B-modes (parameter $A_{lens}$), jointly with the estimation of the astrophysical foregrounds including both synchrotron and thermal dust emissions. Using this Bayesian framework, we forecast the ability of the proposed CMB space mission LiteBIRD to constrain $r$ in the presence of realistic lensing and foreground contributions. We compute the joint posterior distribution of $r$ and $A_{lens}$, which we improve by adopting a prior on $A_{lens}$ taken from the South Pole Telescope (SPT) measurement. As it applies to the power spectrum, this approach cannot mitigate the uncertainty on $r$ that is due to E-mode cosmic variance transferred to B-modes by lensing, unlike standard delensing techniques that are performed on maps. However, the method allows to correct for the bias on $r$ induced by lensing, at the expense of a larger uncertainty due to the increased volume of the parameter space. We quantify, for different values of the tensor-to-scalar ratio, the trade-off between bias correction and increase of uncertainty on $r$. For LiteBIRD simulations, which include foregrounds and lensing contamination, we find that correcting the foreground-cleaned CMB B-mode power spectrum for the lensing bias, not the lensing cosmic variance, still guarantees a $3\sigma$ detection of $r=5\times 10^{-3}$. The significance of the detection is increased to $6\sigma$ when the current SPT prior on $A_{lens}$ is adopted., Comment: 10 pages, 4 figures, 2 tables. Added discussion about non-Gaussianity of lensing B-modes. Updated to match version accepted by MNRAS
Published: 2017
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Database

Publisher

186 results on '"Clive Dickinson"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources