Institution
Netherlands Institute for Space Research
Facility•Utrecht, Netherlands•
About: Netherlands Institute for Space Research is a facility organization based out in Utrecht, Netherlands. It is known for research contribution in the topics: Galaxy & Neutron star. The organization has 737 authors who have published 3026 publications receiving 106632 citations. The organization is also known as: SRON & Space Research Organisation Netherlands.
Topics: Galaxy, Neutron star, Stars, Spectral line, Luminosity
Papers published on a yearly basis
Papers
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Sapienza University of Rome1, Cardiff University2, Netherlands Institute for Space Research3, University of Grenoble4, University of Milan5, INAF6, Spanish National Research Council7, Rutherford Appleton Laboratory8, University of Paris9, Université Paris-Saclay10, Maynooth University11, University of Minnesota12, University of the Basque Country13, Leiden University14, University of Cambridge15, University of Cantabria16, University of Bologna17, University of Toulouse18, University of Padua19, Amrita Vishwa Vidyapeetham20, International School for Advanced Studies21, University of Manchester22, Lawrence Berkeley National Laboratory23, Tufts University24, University of California, Berkeley25, Centre national de la recherche scientifique26, RWTH Aachen University27, University of Ferrara28, University of Rome Tor Vergata29, University of Science and Technology of China30, University of Lisbon31, Imperial College London32, University of La Laguna33, Stockholm University34, University of Oviedo35, Ludwig Maximilian University of Munich36, University of Helsinki37, University College London38, University of Geneva39, University of Sussex40, University of Porto41, University of Barcelona42, Jagiellonian University43, University of Savoy44, Federal University of Rio de Janeiro45, Pierre-and-Marie-Curie University46, University of Groningen47, University of Portsmouth48
TL;DR: In this article, a space-borne, multi-band, mult-beam polarimeter aiming at a precise and accurate measurement of the polarization of the Cosmic Microwave Background is presented.
Abstract: We describe a space-borne, multi-band, multi-beam polarimeter aiming at a precise and accurate measurement of the polarization of the Cosmic Microwave Background. The instrument is optimized to be compatible with the strict budget requirements of a medium-size space mission within the Cosmic Vision Programme of the European Space Agency. The instrument has no moving parts, and uses arrays of diffraction-limited Kinetic Inductance Detectors to cover the frequency range from 60 GHz to 600 GHz in 19 wide bands, in the focal plane of a 1.2 m aperture telescope cooled at 40 K, allowing for an accurate extraction of the CMB signal from polarized foreground emission. The projected CMB polarization survey sensitivity of this instrument, after foregrounds removal, is 1.7 μK⋅arcmin. The design is robust enough to allow, if needed, a downscoped version of the instrument covering the 100 GHz to 600 GHz range with a 0.8 m aperture telescope cooled at 85 K, with a projected CMB polarization survey sensitivity of 3.2 μK⋅arcmin.
54 citations
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TL;DR: The RSP retrievals using the MAPP optimal estimation framework represent a key milestone on the path to a combined lidar+polarimeter retrieval using both HSRL and RSP measurements.
Abstract: We present an optimal-estimation-based retrieval framework, the microphysical aerosol properties from polarimetry (MAPP) algorithm, designed for simultaneous retrieval of aerosol microphysical properties and ocean color bio-optical parameters using multi-angular total and polarized radiances. Polarimetric measurements from the airborne NASA Research Scanning Polarimeter (RSP) were inverted by MAPP to produce atmosphere and ocean products. The RSP MAPP results are compared with co-incident lidar measurements made by the NASA High-Spectral-Resolution Lidar HSRL-1 and HSRL-2 instruments. Comparisons are made of the aerosol optical depth (AOD) at 355 and 532 nm, lidar column-averaged measurements of the aerosol lidar ratio and Angstrom exponent, and lidar ocean measurements of the particulate hemispherical backscatter coefficient and the diffuse attenuation coefficient. The measurements were collected during the 2012 Two-Column Aerosol Project (TCAP) campaign and the 2014 Ship-Aircraft Bio-Optical Research (SABOR) campaign. For the SABOR campaign, 73% RSP MAPP retrievals fall within ±0.04 AOD at 532 nm as measured by HSRL-1, with an R value of 0.933 and root-mean-square deviation of 0.0372. For the TCAP campaign, 53% of RSP MAPP retrievals are within 0.04 AOD as measured by HSRL-2, with an R value of 0.927 and root-mean-square deviation of 0.0673. Comparisons with HSRL-2 AOD at 355 nm during TCAP result in an R value of 0.959 and a root-mean-square deviation of 0.0694. The RSP retrievals using the MAPP optimal estimation framework represent a key milestone on the path to a combined lidar+polarimeter retrieval using both HSRL and RSP measurements.
54 citations
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INAF1, University of Cologne2, University of Porto3, Dublin Institute for Advanced Studies4, University of Manchester5, University of Tokushima6, Netherlands Institute for Space Research7, Kapteyn Astronomical Institute8, Indian Institute of Space Science and Technology9, Leiden University10, Academia Sinica Institute of Astronomy and Astrophysics11, Ames Research Center12, California Institute of Technology13
TL;DR: In this article, the authors used ALMA Cycle 0 observations at 870 μm of dust of typical high-density, molecular outflow, and cloud tracers with resolutions of < 0"5.
Abstract: Context. Theoretical scenarios propose that high-mass stars are formed by disk-mediated accretion.
Aims. To test the theoretical predictions on the formation of massive stars, we wish to make a thorough study at high-angular resolution of the structure and kinematics of the dust and gas emission toward the high-mass star-forming region G35.03+0.35, which harbors a disk candidate around a B-type (proto)star.
Methods. We carried out ALMA Cycle 0 observations at 870 μm of dust of typical high-density, molecular outflow, and cloud tracers with resolutions of < 0"5. Complementary Subaru COMICS 25 μm observations were carried out to trace the mid-infrared emission toward this star-forming region.
Results. The submillimeter continuum emission has revealed a filamentary structure fragmented into six cores, called A–F. The filament could be in quasi-equilibrium taking into account that the mass per unit length of the filament, 200–375 M_⊙/pc, is similar to the critical mass of a thermally and turbulently supported infinite cylinder, ~335 M_⊙/pc. The cores, which are on average separated by ~0.02 pc, have deconvolved sizes of 1300–3400 AU, temperatures of 35–240 K, H_2 densities >10^7 cm^(-3), and masses in the range 1–5 M_⊙, and they are subcritical. Core A, which is associated with a hypercompact Hii region and could be the driving source of the molecular outflow observed in the region, is the most chemically rich source in G35.03+0.35 with strong emission of typical hot core tracers such as CH_3CN. Tracers of high density and excitation show a clear velocity gradient along the major axis of the core, which is consistent with a disk rotating about the axis of the associated outflow. The PV plots along the SE–NW direction of the velocity gradient show clear signatures of Keplerian rotation, although infall could also be present, and they are consistent with the pattern of an edge-on Keplerian disk rotating about a star with a mass in the range 5–13 M_⊙. The high t_(ff)/t_(rot) ratio for core A suggests that the structure rotates fast and that the accreting material has time to settle into a centrifugally supported disk.
Conclusions. G35.03+0.35 is one of the most convincing examples of Keplerian disks rotating about high-mass (proto)stars. This supports theoretical scenarios according to which high-mass stars, at least B-type stars, would form through disk-mediated accretion.
54 citations
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University of Nottingham1, Netherlands Institute for Space Research2, University of Texas at Austin3, INAF4, Imperial College London5, University of Vienna6, European Southern Observatory7, Max Planck Society8, Ludwig Maximilian University of Munich9, Commonwealth Scientific and Industrial Research Organisation10
TL;DR: The first results of a far-infrared search for protocluster-associated galaxy overdensities using the Spectral and Photometric Imaging REciever (SPIRE) instrument on-board the Herschel Space Observatory were presented in this paper.
Abstract: This paper presents the first results of a far-infrared search for protocluster-associated galaxy overdensities using the Spectral and Photometric Imaging REciever (SPIRE) instrument on-board the Herschel Space Observatory. Large (∼400 arcmin2) fields surrounding 26 powerful high-redshift radio galaxies (2.0 1028.5 WHz−1) are mapped at 250, 350 and 500 μm to give a unique wide-field sample. On average, the fields have a higher than expected, compared to blank fields, surface density of 500 μm sources within 6 comoving Mpc of the radio galaxy. The analysis is then restricted to potential protocluster members only, which are identified using a far-infrared colour selection; this reveals significant overdensities of galaxies in two fields, neither of which are previously known protoclusters. The probability of finding two overdensities of this size by chance, given the number of fields observed, is 5 × 10−4. Overdensities here exist around radio galaxies with L500 MHz ≳ 1029 WHz−1 and z 1014 M⊙. However, the large uncertainty in the redshift estimation means that it is possible that these far-infrared overdensities consist of several structures across the redshift range searched.
54 citations
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TL;DR: In this paper, the core of the X-ray binary system XTE J1752-223 was located using high-precision optical observations from the Walter Baade Magellan Telescope in conjunction with high-resolution very long baseline interferometric (VLBI) radio imaging with the Very Long Baseline Array (VLBA).
Abstract: Using high-precision astrometric optical observations from the Walter Baade Magellan Telescope in conjunction with high-resolution very long baseline interferometric (VLBI) radio imaging with the Very Long Baseline Array (VLBA), we have located the core of the X-ray binary system XTE J1752-223. Compact radio emission from the core was detected following the state transition from the soft to the hard X-ray state. Its position to the south-east of all previously detected jet components mandated a re-analysis of the existing VLBI data. Our analysis suggests that the outburst comprised at least two ejection events prior to 2010 February 26. No radio-emitting components were detected to the south-east of the core at any epoch, suggesting that the receding jets were Doppler-deboosted below our sensitivity limit. From the ratio of the brightness of the detected components to the measured upper limits for the receding ejecta, we constrain the jet speed beta > 0.66 and the inclination angle to the line of sight theta < 49 degrees. Assuming that the initial ejection event occurred at the transition from the hard intermediate state to the soft intermediate state, an initial period of ballistic motion followed by a Sedov phase (i.e. self-similar adiabatic expansion) appears to fit the motion of the ejecta better than a uniform deceleration model. The accurate core location can provide a long time baseline for a future proper motion determination should the system show a second outburst, providing insights into the formation mechanism of the compact object.
54 citations
Authors
Showing all 756 results
Name | H-index | Papers | Citations |
---|---|---|---|
George Helou | 144 | 662 | 96338 |
Alexander G. G. M. Tielens | 115 | 722 | 51058 |
Gijs Nelemans | 102 | 433 | 83486 |
Jelle Kaastra | 90 | 677 | 28093 |
Christian Frankenberg | 79 | 286 | 19353 |
Jeroen Homan | 72 | 354 | 15499 |
Nanda Rea | 72 | 446 | 19881 |
Mariano Mendez | 70 | 372 | 14475 |
Jorick S. Vink | 70 | 311 | 18826 |
Peter G. Jonker | 67 | 384 | 28363 |
Michael W. Wise | 64 | 271 | 19580 |
George Heald | 64 | 375 | 16261 |
Pieter R. Roelfsema | 64 | 257 | 18759 |
F. F. S. van der Tak | 63 | 314 | 16781 |
Norbert Werner | 63 | 254 | 10741 |