Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26339
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Moldón, J. | en_US |
dc.contributor.author | Deller, A. T. | en_US |
dc.contributor.author | Wucknitz, O. | en_US |
dc.contributor.author | Jackson, N. | en_US |
dc.contributor.author | Drabent, A. | en_US |
dc.contributor.author | Carozzi, T. | en_US |
dc.contributor.author | Conway, J. | en_US |
dc.contributor.author | Kapińska, A. D. | en_US |
dc.contributor.author | McKean, J. P. | en_US |
dc.contributor.author | Morabito, L. | en_US |
dc.contributor.author | Varenius, E. | en_US |
dc.contributor.author | Zarka, P. | en_US |
dc.contributor.author | Anderson, J. | en_US |
dc.contributor.author | Asgekar, A. | en_US |
dc.contributor.author | Avruch, I. M. | en_US |
dc.contributor.author | Bell, M. E. | en_US |
dc.contributor.author | Bentum, M. J. | en_US |
dc.contributor.author | BERNARDI, GIANNI | en_US |
dc.contributor.author | Best, P. | en_US |
dc.contributor.author | Bîrzan, L. | en_US |
dc.contributor.author | Bregman, J. | en_US |
dc.contributor.author | Breitling, F. | en_US |
dc.contributor.author | Broderick, J. W. | en_US |
dc.contributor.author | Brüggen, M. | en_US |
dc.contributor.author | Butcher, H. R. | en_US |
dc.contributor.author | Carbone, D. | en_US |
dc.contributor.author | Ciardi, B. | en_US |
dc.contributor.author | de Gasperin, F. | en_US |
dc.contributor.author | de Geus, E. | en_US |
dc.contributor.author | Duscha, S. | en_US |
dc.contributor.author | Eislöffel, J. | en_US |
dc.contributor.author | Engels, D. | en_US |
dc.contributor.author | Falcke, H. | en_US |
dc.contributor.author | Fallows, R. A. | en_US |
dc.contributor.author | Fender, R. | en_US |
dc.contributor.author | Ferrari, C. | en_US |
dc.contributor.author | Frieswijk, W. | en_US |
dc.contributor.author | Garrett, M. A. | en_US |
dc.contributor.author | Grießmeier, J. | en_US |
dc.contributor.author | Gunst, A. W. | en_US |
dc.contributor.author | Hamaker, J. P. | en_US |
dc.contributor.author | Hassall, T. E. | en_US |
dc.contributor.author | Heald, G. | en_US |
dc.contributor.author | Hoeft, M. | en_US |
dc.contributor.author | Juette, E. | en_US |
dc.contributor.author | Karastergiou, A. | en_US |
dc.contributor.author | Kondratiev, V. I. | en_US |
dc.contributor.author | Kramer, M. | en_US |
dc.contributor.author | Kuniyoshi, M. | en_US |
dc.contributor.author | Kuper, G. | en_US |
dc.contributor.author | Maat, P. | en_US |
dc.contributor.author | Mann, G. | en_US |
dc.contributor.author | Markoff, S. | en_US |
dc.contributor.author | McFadden, R. | en_US |
dc.contributor.author | McKay-Bukowski, D. | en_US |
dc.contributor.author | Morganti, R. | en_US |
dc.contributor.author | Munk, H. | en_US |
dc.contributor.author | Norden, M. J. | en_US |
dc.contributor.author | Offringa, A. R. | en_US |
dc.contributor.author | Orru, E. | en_US |
dc.contributor.author | Paas, H. | en_US |
dc.contributor.author | Pandey-Pommier, M. | en_US |
dc.contributor.author | Pizzo, R. | en_US |
dc.contributor.author | Polatidis, A. G. | en_US |
dc.contributor.author | Reich, W. | en_US |
dc.contributor.author | Röttgering, H. | en_US |
dc.contributor.author | Rowlinson, A. | en_US |
dc.contributor.author | Scaife, A. M. M. | en_US |
dc.contributor.author | Schwarz, D. | en_US |
dc.contributor.author | Sluman, J. | en_US |
dc.contributor.author | Smirnov, O. | en_US |
dc.contributor.author | Stappers, B. W. | en_US |
dc.contributor.author | Steinmetz, M. | en_US |
dc.contributor.author | Tagger, M. | en_US |
dc.contributor.author | Tang, Y. | en_US |
dc.contributor.author | Tasse, C. | en_US |
dc.contributor.author | Thoudam, S. | en_US |
dc.contributor.author | Toribio, M. C. | en_US |
dc.contributor.author | Vermeulen, R. | en_US |
dc.contributor.author | Vocks, C. | en_US |
dc.contributor.author | van Weeren, R. J. | en_US |
dc.contributor.author | White, S. | en_US |
dc.contributor.author | Wise, M. W. | en_US |
dc.contributor.author | Yatawatta, S. | en_US |
dc.contributor.author | Zensus, A. | en_US |
dc.date.accessioned | 2020-07-06T05:50:45Z | - |
dc.date.available | 2020-07-06T05:50:45Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26339 | - |
dc.description | LOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries that are owned by various parties (each with their own funding sources), and that are collectively operated by the international LOFAR Telescope (ILT) foundation under a joint scientific policy. A.T.D. is supported by a Veni Fellowship from NWO. A.D.K. acknowledges support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. LKM acknowledges financial support from NWO Top LOFAR project, project n. 614.001.006. CF acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. | en_US |
dc.description.abstract | <BR /> Aims: An efficient means of locating calibrator sources for international LOw Frequency ARray (LOFAR) is developed and used to determine the average density of usable calibrator sources on the sky for subarcsecond observations at 140 MHz. <BR /> Methods: We used the multi-beaming capability of LOFAR to conduct a fast and computationally inexpensive survey with the full international LOFAR array. Sources were preselected on the basis of 325 MHz arcminute-scale flux density using existing catalogues. By observing 30 different sources in each of the 12 sets of pointings per hour, we were able to inspect 630 sources in two hours to determine if they possess a sufficiently bright compact component to be usable as LOFAR delay calibrators. <BR /> Results: More than 40% of the observed sources are detected on multiple baselines between international stations and 86 are classified as satisfactory calibrators. We show that a flat low-frequency spectrum (from 74 to 325 MHz) is the best predictor of compactness at 140 MHz. We extrapolate from our sample to show that the sky density of calibrators that are sufficiently bright to calibrate dispersive and non-dispersive delays for the international LOFAR using existing methods is 1.0 per square degree. <BR /> Conclusions: The observed density of satisfactory delay calibrator sources means that observations with international LOFAR should be possible at virtually any point in the sky provided that a fast and efficient search, using the methodology described here, is conducted prior to the observation to identify the best calibrator. <P />Full Table 6 is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/574/A73">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/574/A73</A> | en_US |
dc.language.iso | eng | en_US |
dc.title | The LOFAR long baseline snapshot calibrator survey | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201425042 | en_US |
dc.identifier.scopus | 2-s2.0-85006437595 | en_US |
dc.identifier.isi | 000349467000073 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2015/02/aa25042-14/aa25042-14.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 574 | en_US |
dc.relation.firstpage | A73 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | FRA | en_US |
dc.contributor.country | DEU | en_US |
dc.contributor.country | NLD | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015A&A...574A..73M | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_6 Stars and stellar systems | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.orcid | 0000-0002-0916-7443 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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Moldon2015.pdf | PDF editoriale | 632.08 kB | Adobe PDF | View/Open |
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