S. Casassus - University de Chile

S. Casassus
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Name
S. Casassus
Affiliation
University de Chile
City
Santiago
Country
Chile

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Solar and Stellar Astrophysics (24)
 
Earth and Planetary Astrophysics (22)
 
Astrophysics of Galaxies (19)
 
Instrumentation and Methods for Astrophysics (5)
 
Cosmology and Nongalactic Astrophysics (2)
 
Computer Science - Distributed; Parallel; and Cluster Computing (1)
 
Physics - Space Physics (1)

Publications Authored By S. Casassus

The maximum entropy method (MEM) is a well known deconvolution technique in radio-interferometry. This method solves a non-linear optimization problem with an entropy regularization term. Other heuristics such as CLEAN are faster but highly user dependent. Read More

We present Atacama Large Millimeter/sub-millimeter Array (ALMA) Cycle-2 observations of the HBC 494 molecular outflow and envelope. HBC 494 is an FU Ori-like object embedded in the Orion A cloud and is associated with the reflection nebulae Re50 and Re50N. We use $^{12}$CO, $^{13}$CO and C$^{18}$O spectral line data to independently describe the outflow and envelope structures associated with HBC 494. Read More

We have conducted a search for optical circumstellar absorption lines in the spectra of 16 debris disc host stars. None of the stars in our sample showed signs of emission line activity in either H$_{\alpha}$, Ca II or Na I, confirming their more evolved nature. Four stars were found to exhibit narrow absorption features near the cores of the photospheric Ca II and Na I D lines (when Na I D data were available). Read More

As part of an ALMA survey to study the origin of episodic accretion in young eruptive variables, we have observed the circumstellar environment of the star V2775 Ori. This object is a very young, pre-main sequence object which displays a large amplitude outburst characteristic of the FUor class. We present Cycle-2 band 6 observations of V2775 Ori with a continuum and CO (2-1) isotopologue resolution of 0. Read More

Context: Gaps, cavities and rings in circumstellar disks are signposts of disk evolution and planet-disk interactions. We follow the recent suggestion that Herbig Ae/Be disks with a flared disk harbour a cavity, and investigate the disk around HD~97048. Aims: We aim to resolve the 34$\pm$ 4 au central cavity predicted by Maaskant et al. Read More

A snow-line is the region of a protoplanetary disk at which a major volatile, such as water or carbon monoxide, reaches its condensation temperature. Snow-lines play a crucial role in disk evolution by promoting the rapid growth of ice-covered grains. Signatures of the carbon monoxide snow-line (at temperatures of around 20 kelvin) have recently been imaged in the disks surrounding the pre-main-sequence stars TW Hydra and HD163296, at distances of about 30 astronomical units (au) from the star. Read More

An increasing number of observations have shown that gaseous debris discs are not an exception. However, until now we only knew of cases around A stars. Here we present the first detection of 12CO (2-1) disc emission around an F star, HD 181327, obtained with ALMA observations at 1. Read More

Transition disks correspond to a short stage between the young protoplanetary phase and older debris phase. Along this evolutionary sequence, the gas component disappears leaving room for a dust-dominated environment where already-formed planets signpost their gravitational perturbations. We endeavor to study the very inner region of the well-known and complex debris, but still gas-rich disk, around HD 141569A using the exquisite high-contrast capability of SPHERE at the VLT. Read More

The star HR 8799 hosts one of the largest known debris discs and at least four giant planets. Previous observations have found evidence for a warm belt within the orbits of the planets, a cold planetesimal belt beyond their orbits and a halo of small grains. With the infrared data, it is hard to distinguish the planetesimal belt emission from that of the grains in the halo. Read More

Resolved observations are bringing new constraints on the origin of radial gaps in protoplanetary disks. The kinematics, sampled in detail in one case-study, are indicative of non-Keplerian flows, corresponding to warped structures and accretion which may both play a role in the development of cavities. Disk asymmetries seen in the radio continuum are being interpreted in the context of dust segregation via aerodynamic trapping. Read More

We present the results of ALMA band 7 observations of dust and CO gas in the disks around 7 objects with spectral types ranging between M5.5 and M7.5 in Upper Scorpius OB1, and one M3 star in Ophiuchus. Read More

Debris disks offer valuable insights into the latest stages of circumstellar disk evolution, and can possibly help us to trace the outcomes of planetary formation processes. In the age range 10 to 100\,Myr, most of the gas is expected to have been removed from the system, giant planets (if any) must have already been formed, and the formation of terrestrial planets may be on-going. Pluto-sized planetesimals, and their debris released in a collisional cascade, are under their mutual gravitational influence, which may result into non-axisymmetric structures in the debris disk. Read More

Circumstellar asymmetries such as central warps have recently been shown to cast shadows on outer disks. We investigate the hydrodynamical consequences of such variable illumination on the outer regions of a transition disk, and the development of spiral arms. Using 2D simulations, we follow the evolution of a gaseous disk passively heated by the central star, under the periodic forcing of shadows with an opening angle of $\sim$28$^\circ$. Read More

The finding of residual gas in the large central cavity of the HD142527 disk motivates questions on the origin of its non-Keplerian kinematics, and possible connections with planet formation. We aim to understand the physical structure that underlies the intra-cavity gaseous flows, guided by new molecular-line data in CO(6-5) with unprecedented angular resolutions. Given the warped structure inferred from the identification of scattered-light shadows cast on the outer disk, the kinematics are consistent, to first order, with axisymmetric accretion onto the inner disk occurring at all azimuth. Read More

A pathway to the formation of planetesimals, and eventually giant planets, may occur in concentrations of dust grains trapped in pressure maxima. Dramatic crescent-shaped dust concentrations have been seen in recent radio images at sub-mm wavelengths. These disk asymmetries could represent the initial phases of planet formation in the dust trap scenario, provided that grain sizes are spatially segregated. Read More

The identification of on-going planet formation requires the finest angular resolutions and deepest sensitivities in observations inspired by state-of-the-art numerical simulations. Hydrodynamic simulations of planet-disk interactions predict the formation of circumplanetary disks (CPDs) around accreting planetary cores. These CPDs have eluded unequivocal detection -their identification requires predictions in CPD tracers. Read More

The formation of planetesimals requires that primordial dust grains grow from micron- to km-sized bodies. Dust traps caused by gas pressure maxima have been proposed as regions where grains can concentrate and grow fast enough to form planetesimals, before radially migrating onto the star. We report new VLA Ka & Ku observations of the protoplanetary disk around the Herbig Ae/Be star MWC 758. Read More

While recent observational progress is converging on the detection of compact regions of thermal emission due to embedded protoplanets, further theoretical predictions are needed to understand the response of a protoplanetary disk to the planet formation radiative feedback. This is particularly important to make predictions for the observability of circumplanetary regions. In this work we use 2D hydrodynamical simulations to examine the evolution of a viscous protoplanetary disk in which a luminous Jupiter-mass planet is embedded. Read More

We present 850 micron observations of the 2-3 Myr cluster IC 348 in the Perseus molecular cloud using the SCUBA-2 camera on the James Clerk Maxwell Telescope. Our SCUBA-2 map has a diameter of 30 arcmin and contains ~370 cluster members, including ~200 objects with IR excesses. We detect a total of 13 discs. Read More

Context. Z\,CMa is a binary composed of an embedded Herbig Be and an FU Ori class star separated by $\sim100$ au. Observational evidence indicate a complex environment in which each star has a circumstellar disk and drives a jet, and the whole system is embedded in a large dusty envelope. Read More

We present ALMA (Cycle 0) band-6 and band-3 observations of the transition disk Sz\,91. The disk inclination and position angle are determined to be $i=49.5\degr\pm3. Read More

We present a new algorithm designed to improve the signal to noise ratio (SNR) of point and extended source detections in direct imaging data. The novel part of our method is that it finds the linear combination of the science images that best match counterpart images with signal removed from suspected source regions. The algorithm, based on the Locally Optimized Combination of Images (LOCI) method, is called Matched LOCI or MLOCI. Read More

In this chapter, we will outline the scientific motivation for studying Anomalous Microwave Emission (AME) with the SKA. AME is thought to be due to electric dipole radiation from small spinning dust grains, although thermal fluctuations of magnetic dust grains may also contribute. Studies of this mysterious component would shed light on the emission mechanism, which then opens up a new window onto the interstellar medium (ISM). Read More

2014Dec
Affiliations: 1MAD Universidad de Chile, 2MAD Universidad de Chile, 3MAD Universidad de Chile

Detailed observations of gaps in protoplanetary disks have revealed structures that drive current research on circumstellar disks. One such feature is the two intensity nulls seen along the outer disk of the HD 142527 system, which are particularly well traced in polarized differential imaging. Here we propose that these are shadows cast by the inner disk. Read More

Context : The properties of the inner disks of bright Herbig AeBe stars have been studied with near infrared (NIR) interferometry and high resolution spectroscopy. The continuum and a few molecular gas species have been studied close to the central star; however, sensitivity problems limit direct information about the inner disks of the fainter T Tauri stars. Aims : Our aim is to measure some of the properties of the inner regions of disks surrounding southern T Tauri stars. Read More

Inner cavities and annular gaps in circumstellar disks are possible signposts of giant planet formation. The young star HD 142527 hosts a massive protoplanetary disk with a large cavity that extends up to 140 au from the central star, as seen in continuum images at infrared and millimeter wavelengths. Estimates of the survival of gas inside disk cavities are needed to discriminate between clearing scenarios. Read More

The disk around HD 142527 attracts a lot of attention, amongst others because of its resolved (sub) mm dust continuum that is concentrated into a horseshoe-shape towards the north of the star. In this manuscript we present spatially resolved ALMA detections of the HCN J=4-3 and CS J=7-6 emission lines. These lines give us a view deeper into the disk compared to the (optically thicker) CO isotopes. Read More

We carried out a 12CO(3-2) survey of 52 southern stars with a wide range of IR excesses (LIR/L*) using the single dish telescopes APEX and ASTE. The main aims were (1) to characterize the evolution of molecular gas in circumstellar disks using LIR/L* values as a proxy of disk dust evolution, and (2) to identify new gas-rich disk systems suitable for detailed study with ALMA. About 60% of the sample (31 systems) have LIR/L* > 0. Read More

Many stars are surrounded by disks of dusty debris formed in the collisions of asteroids, comets and dwarf planets. But is gas also released in such events? Observations at submm wavelengths of the archetypal debris disk around $\beta$ Pictoris show that 0.3% of a Moon mass of carbon monoxide orbits in its debris belt. Read More

2014Mar
Authors: Planck Collaboration, M. Arnaud, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, K. Benabed, A. Benoit-Lévy, J. -P. Bernard, M. Bersanelli, P. Bielewicz, A. Bonaldi, J. R. Bond, J. Borrill, F. R. Bouchet, C. S. Buemi, C. Burigana, J. -F. Cardoso, S. Casassus, A. Catalano, L. Cerrigone, A. Chamballu, H. C. Chiang, S. Colombi, L. P. L. Colombo, F. Couchot, B. P. Crill, A. Curto, F. Cuttaia, R. D. Davies, R. J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, C. Dickinson, J. M. Diego, S. Donzelli, O. Doré, X. Dupac, T. A. Enßlin, H. K. Eriksen, F. Finelli, M. Frailis, E. Franceschi, S. Galeotta, K. Ganga, M. Giard, J. González-Nuevo, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. L. Harrison, S. R. Hildebrandt, E. Hivon, W. A. Holmes, J. L. Hora, A. Hornstrup, W. Hovest, K. M. Huffenberger, T. R. Jaffe, W. C. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T. S. Kisner, J. Knoche, M. Kunz, H. Kurki-Suonio, A. Lähteenmäki, J. -M. Lamarre, A. Lasenby, C. R. Lawrence, R. Leonardi, P. Leto, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, J. F. Macías-Pérez, B. Maffei, D. Maino, N. Mandolesi, P. G. Martin, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, L. Mendes, A. Mennella, M. Migliaccio, M. -A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, F. Noviello, D. Novikov, I. Novikov, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, M. Peel, O. Perdereau, F. Perrotta, F. Piacentini, M. Piat, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, L. Popa, G. W. Pratt, P. Procopio, S. Prunet, J. -L. Puget, J. P. Rachen, M. Reinecke, M. Remazeilles, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, L. D. Spencer, V. Stolyarov, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, C. Trigilio, M. Tristram, T. Trombetti, M. Tucci, G. Umana, J. Valiviita, B. Van Tent, P. Vielva, F. Villa, L. A. Wade, B. D. Wandelt, A. Zacchei, A. Zijlstra, A. Zonca

Late stages of stellar evolution are characterized by copious mass-loss events whose signature is the formation of circumstellar envelopes (CSE). Planck multi-frequency measurements have provided relevant information on a sample of Galactic planetary nebulae (PNe) in the important and relatively unexplored observational band between 30 and 857GHz. Planck enables the assembly of comprehensive PNe spectral energy distributions (SEDs) from radio {\bf to} far-infrared frequencies. Read More

2014Mar
Affiliations: 1Universidad de Chile, 2Universidad de Chile, 3Universidad de Chile, 4Universidad de Chile, 5UMI-FCA, CNRS/INSU and Universidad de Chile

In view of both the size of its gap and the previously reported asymmetries and near-infrared spiral arms, the transition disk of the Herbig Fe star HD 142527 constitutes a remarkable case study. This paper focuses on the morphology of the outer disk through ALMA observations of $^{12}$CO J=2-1, $^{12}$CO J=3-2 and $^{13}$CO J=2-1. Both $^{12}$CO J=2-1 and $^{12}$CO J=3-2 show spiral features of different sizes. Read More

We present the various science cases for building Band 1 receivers as part of ALMA's ongoing Development Program. We describe the new frequency range for Band 1 of 35-52 GHz, a range chosen to maximize the receiver suite's scientific impact. We first describe two key science drivers: 1) the evolution of grains in protoplanetary disks and debris disks, and 2) molecular gas in galaxies during the era of re-ionization. Read More

2013Sep
Authors: Planck Collaboration, P. A. R. Ade, N. Aghanim, M. I. R. Alves, M. Arnaud, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, K. Benabed, A. Benoit-Lévy, J. -P. Bernard, M. Bersanelli, P. Bielewicz, J. Bobin, A. Bonaldi, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, C. Burigana, J. -F. Cardoso, S. Casassus, A. Catalano, A. Chamballu, X. Chen, H. C. Chiang, L. -Y Chiang, P. R. Christensen, D. L. Clements, S. Colombi, L. P. L. Colombo, F. Couchot, B. P. Crill, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, F. -X. Désert, C. Dickinson, J. M. Diego, S. Donzelli, O. Doré, X. Dupac, T. A. Enßlin, H. K. Eriksen, F. Finelli, O. Forni, E. Franceschi, S. Galeotta, K. Ganga, R. T. Génova-Santos, T. Ghosh, M. Giard, J. González-Nuevo, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, G. Helou, C. Hernández-Monteagudo, S. R. Hildebrandt, E. Hivon, A. Hornstrup, A. H. Jaffe, T. R. Jaffe, W. C. Jones, E. Keihänen, R. Keskitalo, R. Kneissl, J. Knoche, M. Kunz, H. Kurki-Suonio, A. Lähteenmäki, J. -M. Lamarre, A. Lasenby, C. R. Lawrence, R. Leonardi, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, J. F. Macías-Pérez, B. Maffei, D. Maino, N. Mandolesi, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, M. -A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, P. Naselsky, F. Nati, P. Natoli, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, C. A. Oxborrow, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, G. Patanchon, T. J. Pearson, M. Peel, O. Perdereau, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, G. W. Pratt, S. Prunet, J. -L. Puget, J. P. Rachen, R. Rebolo, W. Reich, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, L. D. Spencer, V. Stolyarov, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. Tauber, D. Tavagnacco, L. Terenzi, C. T. Tibbs, L. Toffolatti, M. Tomasi, M. Tristram, M. Tucci, L. Valenziano, J. Valiviita, B. Van Tent, J. Varis, P. Vielva, F. Villa, B. D. Wandelt, R. Watson, A. Wilkinson, N. Ysard, D. Yvon, A. Zacchei, A. Zonca

Anomalous microwave emission (AME) is believed to be due to electric dipole radiation from small spinning dust grains. The aim of this paper is a statistical study of the basic properties of AME regions and the environment in which they emit. We used WMAP and Planck maps, combined with ancillary radio and IR data, to construct a sample of 98 candidate AME sources, assembling SEDs for each source using aperture photometry on 1deg-smoothed maps from 0. Read More

HD 142527 is a pre-transition disk with strong evidence for on-going planet formation. Recent observations show a disrupted disk with spiral arms, a dust-depleted inner cavity and the possible presence of gas streams driving gas from the outer disk towards the central star. We aim to derive the morphology of the disk, as well as the distribution and properties of the dust at its surface. Read More

2013May
Affiliations: 11. Departamento de Astronomia, Universidad de Chile 2. Joint ALMA Observatory 3. European Southern Observatory 4. National Radio Astronomy Observatory, USA 5. Observatoire de Geneve 6. Departamento de Astronomia, Pontificia Universidad Catolica de Chile 7. UMI-FCA, CNRS / INSU France, 21. Departamento de Astronomia, Universidad de Chile 2. Joint ALMA Observatory 3. European Southern Observatory 4. National Radio Astronomy Observatory, USA 5. Observatoire de Geneve 6. Departamento de Astronomia, Pontificia Universidad Catolica de Chile 7. UMI-FCA, CNRS / INSU France, 31. Departamento de Astronomia, Universidad de Chile 2. Joint ALMA Observatory 3. European Southern Observatory 4. National Radio Astronomy Observatory, USA 5. Observatoire de Geneve 6. Departamento de Astronomia, Pontificia Universidad Catolica de Chile 7. UMI-FCA, CNRS / INSU France

Gaseous giant planet formation is thought to occur in the first few million years following stellar birth. Models predict that giant planet formation carves a deep gap in the dust component (shallower in the gas). Infrared observations of the disk around the young star HD142527, at ~140pc, found an inner disk ~10AU in radius, surrounded by a particularly large gap, with a disrupted outer disk beyond 140AU, indicative of a perturbing planetary-mass body at ~90 AU. Read More

We present observations performed with the Green Bank Telescope at 1.4 and 5 GHz of three strips coincident with the anomalous microwave emission features previously identified in the Perseus molecular cloud at 33 GHz with the Very Small Array. With these observations we determine the level of the low frequency (~1 - 5 GHz) emission. Read More

We present deep Sparse Aperture Masking (SAM) observations obtained with the ESO Very Large Telescope of the pre-transitional disk object FL Cha (SpT=K8, d=160 pc), the disk of which is known to have a wide optically thin gap separating optically thick inner and outer disk components. We find non-zero closure phases, indicating a significant flux asymmetry in the K-band emission (e.g. Read More

2012Jul
Affiliations: 1Universidad de Chile, 2Universidad de Chile, 3Universidad Católica de Chile, 4UMI-FCA 3386, CNRS / INSU at Universidad de Chile, 5Universidad Católica de Chile, 6Universidad Valparaiso, 7Joint ALMA Observatory, 8Ludwig-Maximillians University, Munich

The vestiges of planet formation have been observed in debris disks harboring young and massive gaseous giants. The process of giant planet formation is terminated by the dissipation of gas in the protoplanetary disk. The gas-rich disk around HD142527 features a small inner disk, a large gap from \sim10 to \sim140AU, and a massive outer disk extending out to \sim300AU. Read More

Using infrared, radio continuum and spectral observations, we performed a detailed investigation of the HII region RCW175. We determined that RCW175, which actually consists of two separate HII regions, G29.1-0. Read More

High angular resolution radio continuum images of NGC 1976 (M42, Orion A) at frequency=330 MHz (wavelength=91 cm), 1.5 GHz (20 cm) and 10.6 GHz (2. Read More

High angular resolution radio continuum images of NGC 1976 (M42, Orion A) at frequency=330 MHz (wavelength=91 cm), 1.5 GHz (20 cm) and 10.6 GHz (2. Read More

A preliminary VLT-UVES spectrum of NGC 6302 (Casassus et al. 2002, MN), which hosts one of the hottest PN nuclei known (Teff ~ 220000 K; Wright et al. 2011, MN), has been recently analysed by means of X-SSN, a spectrum synthesis code for nebulae (Morisset and P\'equignot). Read More

2011Aug
Affiliations: 1Jodrell Bank Centre for Astrophysics, The University of Manchester, 2Spitzer Science Center, Caltech, 3Spitzer Science Center, Caltech, 4Spitzer Science Center, Caltech, 5Space Science Division, NASA Ames Research Center, 6Spitzer Science Center, Caltech, 7Spitzer Science Center, Caltech, 8Jodrell Bank Centre for Astrophysics, The University of Manchester, 9Cahill Center for Astronomy and Astrophysics, Caltech, 10Departamento de Astronomía, Universidad de Chile, 11Cahill Center for Astronomy and Astrophysics, Caltech, 12Jodrell Bank Centre for Astrophysics, The University of Manchester, 13Jodrell Bank Centre for Astrophysics, The University of Manchester, 14Cahill Center for Astronomy and Astrophysics, Caltech, 15Jodrell Bank Centre for Astrophysics, The University of Manchester

Anomalous microwave emission is known to exist in the Perseus cloud. One of the most promising candidates to explain this excess of emission is electric dipole radiation from rapidly rotating very small dust grains, commonly referred to as spinning dust. Photometric data obtained with the Spitzer Space Telescope have been reprocessed and used in conjunction with the dust emission model DUSTEM to characterise the properties of the dust within the cloud. Read More

The diffuse cm-wave IR-correlated signal, the "anomalous" CMB foreground, is thought to arise in the dust in cirrus clouds. We present Cosmic Background Imager (CBI) cm-wave data of two translucent clouds, {\zeta} Oph and LDN 1780 with the aim of characterising the anomalous emission in the translucent cloud environment. In {\zeta} Oph, the measured brightness at 31 GHz is 2. Read More

2011Jan
Authors: Planck Collaboration, P. A. R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, J. Aumont, C. Baccigalupi, A. Balbi, A. J. Banday, R. B. Barreiro, J. G. Bartlett, E. Battaner, K. Benabed, A. Benoît, J. -P. Bernard, M. Bersanelli, R. Bhatia, J. J. Bock, A. Bonaldi, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, M. Bucher, C. Burigana, P. Cabella, B. Cappellini, J. -F. Cardoso, S. Casassus, A. Catalano, L. Cayón, A. Challinor, A. Chamballu, R. -R. Chary, X. Chen, L. -Y Chiang, C. Chiang, P. R. Christensen, D. L. Clements, S. Colombi, F. Couchot, A. Coulais, B. P. Crill, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, G. de Gasperis, A. de Rosa, G. de Zotti, J. Delabrouille, J. -M. Delouis, C. Dickinson, S. Donzelli, O. Doré, U. Dörl, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, O. Forni, M. Frailis, E. Franceschi, S. Galeotta, K. Ganga, R. T. Génova-Santos, M. Giard, G. Giardino, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, G. Helou, S. Henrot-Versillé, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, W. Hovest, R. J. Hoyland, K. M. Huffenberger, T. R. Jaffe, A. H. Jaffe, W. C. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, L. Knox, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J. -M. Lamarre, A. Lasenby, R. J. Laureijs, C. R. Lawrence, S. Leach, R. Leonardi, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. Macías-Pérez, C. J. MacTavish, B. Maffei, D. Maino, N. Mandolesi, R. Mann, M. Maris, D. J. Marshall, E. Martínez-González, S. Masi, S. Matarrese, F. Matthai, P. Mazzotta, P. McGehee, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, S. Mitra, M. -A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, A. Murphy, P. Naselsky, P. Natoli, C. B. Netterfield, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, I. J. O'Dwyer, S. Osborne, F. Pajot, R. Paladini, B. Partridge, F. Pasian, G. Patanchon, T. J. Pearson, M. Peel, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, S. Plaszczynski, P. Platania, E. Pointecouteau, G. Polenta, N. Ponthieu, T. Poutanen, G. Prézeau, P. Procopio, S. Prunet, J. -L. Puget, W. T. Reach, R. Rebolo, W. Reich, M. Reinecke, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, M. Rowan-Robinson, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, D. Santos, G. Savini, D. Scott, M. D. Seiffert, P. Shellard, G. F. Smoot, J. -L. Starck, F. Stivoli, V. Stolyarov, R. Stompor, R. Sudiwala, J. -F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, J. -P. Torre, M. Tristram, J. Tuovinen, G. Umana, L. Valenziano, J. Varis, L. Verstraete, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, R. Watson, A. Wilkinson, N. Ysard, D. Yvon, A. Zacchei, A. Zonca

Anomalous microwave emission (AME) has been observed by numerous experiments in the frequency range ~10-60 GHz. Using Planck maps and multi-frequency ancillary data, we have constructed spectra for two known AME regions: the Perseus and Rho Ophiuchi molecular clouds. The spectra are well fitted by a combination of free-free radiation, cosmic microwave background, thermal dust, and electric dipole radiation from small spinning dust grains. Read More

An anomalous radio continuum component at cm-wavelengths has been observed in various sources, including dark clouds. This continuum component represents a new property of the ISM. In this work we focus on one particular dark cloud, the bright reflection nebula M 78. Read More

2010Jul
Affiliations: 1CfA, 2CfA, 3CfA, 4ETH Zurich, 5Caltech, 6CfA, 7NRAO, 8U. Chile, 9Leiden, 10Rochester, 11Kiel, 12MPIfA, 13Eureka Scientific

The late stages of evolution of the primordial circumstellar disks surrounding young stars are poorly understood, yet vital to constrain theories of planet formation. We consider basic structural models for the disks around two ~10 Myr-old members of the nearby RCrA association, RX J1842.9-3532 and RX J1852. Read More

2010Mar
Affiliations: 1Jodrell Bank Centre for Astrophysics, University of Manchester, 2Universidad de Chile, 3Jodrell Bank Centre for Astrophysics, University of Manchester, 4University of Oxford, 5Universidad de Chile, 6Caltech, 7Jodrell Bank Centre for Astrophysics, University of Manchester, 8University of Oxford, 9Caltech, 10Caltech, 11Caltech, 12University of Oxford, 13Jodrell Bank Centre for Astrophysics, University of Manchester, 14Jodrell Bank Centre for Astrophysics, University of Manchester

Lynds dark cloud LDN1622 represents one of the best examples of anomalous dust emission, possibly originating from small spinning dust grains. We present Cosmic Background Imager (CBI) 31 GHz data of LDN1621, a diffuse dark cloud to the north of LDN1622 in a region known as Orion East. A broken ring with diameter g\approx 20 arcmin of diffuse emission is detected at 31 GHz, at \approx 20-30 mJy beam$^{-1}$ with an angular resolution of \approx 5 arcmin. Read More

We present a set of compelling science cases for the ALMA Band 1 receiver suite. For these cases, we assume in tandem the updated nominal Band 1 frequency range of 35-50 GHz with a likely extension up to 52 GHz; together these frequencies optimize the Band 1 science return. The scope of the science cases ranges from nearby stars to the re-ionization edge of the Universe. Read More