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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California Institute of Technology1, Johns Hopkins University2, Ohio State University3, Max Planck Society4, University of Cologne5, University of Michigan6, École Normale Supérieure7, Centre national de la recherche scientifique8, Chalmers University of Technology9, Institute for Advanced Study10, Spanish National Research Council11, Pierre-and-Marie-Curie University12, Nicolaus Copernicus University in Toruń13, National Research Council14, University of Toronto15, Smithsonian Institution16, Tata Institute of Fundamental Research17, National University of Ireland18, University of Calgary19, ASTRON20, University of Massachusetts Amherst21, Netherlands Institute for Space Research22
TL;DR: In this article, the fundamental rotational transitions of ortho- and para-H 16 Oa nd H 18 O in absorption towards Sagittarius B2(M) and W31C were observed and a low ortho/para ratio of 2.35± 0.35 was derived.
Abstract: We present Herschel/HIFI observations of the fundamental rotational transitions of ortho- and para-H 16 Oa nd H 18 O in absorption towards Sagittarius B2(M) and W31C. The ortho/para ratio in water in the foreground clouds on the line of sight towards these bright continuum sources is generally consistent with the statistical high-temperature ratio of 3, within the observational uncertainties. However, somewhat unexpectedly, we derive a low ortho/para ratio of 2.35± 0.35, corresponding to a spin temperature of ∼27 K, towards Sagittarius B2(M) at velocities of the expanding molecular ring. Water molecules in this region appear to have formed with, or relaxed to, an ortho/para ratio close to the value corresponding to the local temperature of the gas and dust.
73 citations
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TL;DR: In this paper, the authors detect a gradual, long-term change in the shape of the X-ray spectrum of the isolated neutron star RX J0720.4-3125, such that the spectrum can no longer be described as a blackbody spectrum.
Abstract: We detect a gradual, long-term change in the shape of the X-ray spectrum of the isolated neutron star RX J0720.4-3125, such that the spectrum of the source can no longer be described as a blackbody spectrum. The change is accompanied by an energy-dependent change in the pulse profile. If the X-ray emission is influenced by the magnetic field of the pulsar, these changes in spectral shape may point to precession of the neutron star.
73 citations
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Netherlands Institute for Space Research1, Leiden University2, Space Telescope Science Institute3, Virginia Tech4, Technion – Israel Institute of Technology5, Roma Tre University6, University College London7, INAF8, University of Geneva9, Polish Academy of Sciences10, Ohio State University11, Centre national de la recherche scientifique12, University of Grenoble13, University of Cambridge14, Max Planck Society15
TL;DR: In this article, a Swift monitoring program was carried out to track the X-ray hardness variability of eight type-I AGN over a year, and the purpose of this monitoring was to find intense obscuration events in AGN, and thereby study them by triggering joint XMM-Newton, NuSTAR, and HST observations.
Abstract: In 2016 we carried out a Swift monitoring programme to track the X-ray hardness variability of eight type-I AGN over a year. The purpose of this monitoring was to find intense obscuration events in AGN, and thereby study them by triggering joint XMM-Newton, NuSTAR, and HST observations. We successfully accomplished this for NGC 3783 in December 2016. We found heavy X-ray absorption produced by an obscuring outflow in this AGN. As a result of this obscuration, interesting absorption features appear in the UV and X-ray spectra, which are not present in the previous epochs. Namely, the obscuration produces broad and blue-shifted UV absorption lines of Lyα, C iv, and N v, together with a new high-ionisation component producing Fe xxv and Fe xxvi absorption lines. In soft X-rays, only narrow emission lines stand out above the diminished continuum as they are not absorbed by the obscurer. Our analysis shows that the obscurer partially covers the central source with a column density of few 1023 cm-2, outflowing with a velocity of few thousand km s-1. The obscuration in NGC 3783 is variable and lasts for about a month. Unlike the commonly seen warm-absorber winds at pc-scale distances from the black hole, the eclipsing wind in NGC 3783 is located at about 10 light days. Our results suggest that the obscuration is produced by an inhomogeneous and clumpy medium, consistent with clouds in the base of a radiatively driven disk wind at the outer broad-line region of the AGN.
73 citations
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Virginia Tech1, University of La Laguna2, Spanish National Research Council3, California Institute of Technology4, European Southern Observatory5, Stanford University6, Dalhousie University7, Imperial College London8, University of California, Irvine9, European University Cyprus10, Institut d'Astrophysique de Paris11, University of Sussex12, Valparaiso University13, National Radio Astronomy Observatory14, University College London15, University of Oxford16, University of British Columbia17, University of Illinois at Urbana–Champaign18, Netherlands Institute for Space Research19, Durham University20
TL;DR: In this article, the authors investigated the relation between star formation rates and AGN properties in optically selected type 1 quasars at 2 < z < 3 using data from Herschel and the SDSS.
Abstract: We investigate the relation between star formation rates (M_s) and AGN properties in optically selected type 1 quasars at 2 < z < 3 using data from Herschel and the SDSS. We find that M_s remains approximately constant with redshift, at 300 ± 100 M⊙ yr^(−1). Conversely, M_s increases with AGN luminosity, up to a maximum of ∼ 600 M⊙ yr^(−1), and with C IV FWHM. In context with previous results, this is consistent with a relation between M_s and black hole accretion rate (M_(bh)) existing in only parts of the z−M_s–M_(bh) plane, dependent on the free gas fraction, the trigger for activity, and the processes that may quench star formation. The relations between M_s and both AGN luminosity and C IV FWHM are consistent with star formation rates in quasars scaling with black hole mass, though we cannot rule out a separate relation with black hole accretion rate. Star formation rates are observed to decline with increasing C IV equivalent width. This decline can be partially explained via the Baldwin effect, but may have an additional contribution from one or more of three factors; M_i is not a linear tracer of L_(2500), the Baldwin effect changes form at high AGN luminosities, and high C IV EW values signpost a change in the relation between M_s and M_(bh). Finally, there is no strong relation between M_s and Eddington ratio, or the asymmetry of the C IV line. The former suggests that star formation rates do not scale with how efficiently the black hole is accreting, while the latter is consistent with C IV asymmetries arising from orientation effects.
73 citations
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TL;DR: Abbott et al. as mentioned in this paper compared the four probability sky maps produced for the gravitational-wave transient GW150914, and provided additional details of the EM follow-up observations that were performed in the different bands.
Abstract: This Supplement provides supporting material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands.
73 citations
Authors
Showing all 756 results
Name | H-index | Papers | Citations |
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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 |