Schuh, Sonja

[["dc.bibliographiccitation.firstpage","231"],["dc.bibliographiccitation.issue","1-2"],["dc.bibliographiccitation.journal","Astrophysics and Space Science"],["dc.bibliographiccitation.lastpage","242"],["dc.bibliographiccitation.volume","329"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Lutz, Ronny"],["dc.contributor.author","Loeptien, Bjoern"],["dc.contributor.author","Green, Elizabeth M."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Leccia, Silvio"],["dc.contributor.author","Kim, Seung-Lee"],["dc.contributor.author","Fontaine, Gilles"],["dc.contributor.author","Charpinet, Stephane"],["dc.contributor.author","Francoeur, Myriam"],["dc.contributor.author","Randall, Suzanna"],["dc.contributor.author","Rodriguez-Lopez, Cristina"],["dc.contributor.author","van Grootel, Valerie"],["dc.contributor.author","Odell, Andrew P."],["dc.contributor.author","Paparo, Margit"],["dc.contributor.author","Bognar, Zsofia"],["dc.contributor.author","Papics, Peter"],["dc.contributor.author","Nagel, Thorsten"],["dc.contributor.author","Beeck, Benjamin"],["dc.contributor.author","Hundertmark, Markus"],["dc.contributor.author","Stahn, Thorsten"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Hessman, Frederic V."],["dc.contributor.author","Dall'Ora, Massimo"],["dc.contributor.author","Mancini, Dario"],["dc.contributor.author","Cortecchia, Fausto"],["dc.contributor.author","Benatti, Serena"],["dc.contributor.author","Claudi, Riccardo"],["dc.contributor.author","Janulis, Rimvydas"],["dc.date.accessioned","2018-11-07T08:38:16Z"],["dc.date.available","2018-11-07T08:38:16Z"],["dc.date.issued","2010"],["dc.description.abstract","In 2007, a companion with planetary mass was found around the pulsating subdwarf B star V391 Pegasi with the timing method, indicating that a previously undiscovered population of substellar companions to apparently single subdwarf B stars might exist. Following this serendipitous discovery, the EXOTIME (http://www.na.astro.it/similar to silvotti/exotime/)) monitoring program has been set up to follow the pulsations of a number of selected rapidly pulsating subdwarf B stars on time scales of several years with two immediate observational goals: (1) determine (P)over dot of the pulsational periods P (2) search for signatures of substellar companions in O-C residuals due to periodic light travel time variations, which would be tracking the central star's companion-induced wobble around the centre of mass These sets of data should therefore, at the same time, on the one hand be useful to provide extra constraints for classical asteroseismological exercises from the P. ( comparison with \"local\" evolutionary models), and on the other hand allow one to investigate the preceding evolution of a target in terms of possible \"binary\" evolution by extending the otherwise unsuccessful search for companions to potentially very low masses. While timing pulsations may be an observationally expensive method to search for companions, it samples a different range of orbital parameters, inaccessible through orbital photometric effects or the radial velocity method: the latter favours massive close-in companions, whereas the timing method becomes increasingly more sensitive toward wider separations. In this paper we report on the status of the on-going observations and coherence analysis for two of the currently five targets, revealing very well-behaved pulsational characteristics in HS 0444+0458, while showing HS 0702+6043 to be more complex than previously thought."],["dc.identifier.doi","10.1007/s10509-010-0356-4"],["dc.identifier.isi","000282823200038"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/7631"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/18728"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Springer"],["dc.relation.issn","0004-640X"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","EXOTIME: searching for planets around pulsating subdwarf B stars"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A130"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","570"],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Charpinet, Stephane"],["dc.contributor.author","Green, E."],["dc.contributor.author","Fontaine, Gilles"],["dc.contributor.author","Telting, J. H."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","van Grootel, V."],["dc.contributor.author","Baran, A. S."],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Machado, L. Fox"],["dc.date.accessioned","2018-11-07T09:34:04Z"],["dc.date.available","2018-11-07T09:34:04Z"],["dc.date.issued","2014"],["dc.description.abstract","KIC 10001893 is one out of 19 subdwarf-B (sdB) pulsators observed by the Kepler spacecraft in its primary mission. In addition to tens of pulsation frequencies in the g-mode domain, its Fourier spectrum shows three weak peaks at very low frequencies, which is too low to be explained in terms of g modes. The most convincing explanation is that we are seeing the orbital modulation of three Earth-size planets (or planetary remnants) in very tight orbits, which are illuminated by the strong stellar radiation. The orbital periods are P-1 = 5.273, P-2 = 7.807, and P-3 = 19.48 h, and the period ratios P-2/P-1 = 1.481 and P-3/P-2 = 2.495 are very close to the 3.2 and 5:2 resonances, respectively. One of the main pulsation modes of the star at 210.68 mu Hz corresponds to the third harmonic of the orbital frequency of the inner planet, suggesting that we see, for the first time in an sdB star, g -mode pulsations tidally excited by a planetary companion. The extreme planetary system that emerges from the Kepler data is very similar to the recent discovery of two Earth-size planets orbiting the sdB pulsator KIC 05807616 (Charpinet et al. 2011a)."],["dc.identifier.doi","10.1051/0004-6361/201424509"],["dc.identifier.fs","609721"],["dc.identifier.isi","000344158500124"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/11403"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/32100"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Kepler detection of a new extreme planetary system orbiting the subdwarf-B pulsator KIC 10001893"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","189"],["dc.bibliographiccitation.issue","7159"],["dc.bibliographiccitation.journal","Nature"],["dc.bibliographiccitation.lastpage","191"],["dc.bibliographiccitation.volume","449"],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Janulis, Rimvydas"],["dc.contributor.author","Solheim, J.-E."],["dc.contributor.author","Bernabei, S."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Oswalt, T. D."],["dc.contributor.author","Bruni, I."],["dc.contributor.author","Gualandi, R."],["dc.contributor.author","Bonanno, A."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Reed, M."],["dc.contributor.author","Chen, C.-W."],["dc.contributor.author","Leibowitz, E. M."],["dc.contributor.author","Paparo, Margit"],["dc.contributor.author","Baran, A."],["dc.contributor.author","Charpinet, Stephane"],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Kawaler, Steven D."],["dc.contributor.author","Kurtz, D. W."],["dc.contributor.author","Moskalik, P."],["dc.contributor.author","Riddle, R."],["dc.contributor.author","Zola, S."],["dc.date.accessioned","2018-11-07T10:58:37Z"],["dc.date.available","2018-11-07T10:58:37Z"],["dc.date.issued","2007"],["dc.description.abstract","After the initial discoveries fifteen years ago(1,2), over 200 extrasolar planets have now been detected. Most of them orbit main-sequence stars similar to our Sun, although a few planets orbiting red giant stars have been recently found(3). When the hydrogen in their cores runs out, main-sequence stars undergo an expansion into red-giant stars. This expansion can modify the orbits of planets and can easily reach and engulf the inner planets. The same will happen to the planets of our Solar System in about five billion years and the fate of the Earth is matter of debate(4,5). Here we report the discovery of a planetary-mass body (Msini = 3.2M(Jupiter)) orbiting the star V 391 Pegasi at a distance of about 1.7 astronomical units (AU), with a period of 3.2 years. This star is on the extreme horizontal branch of the Hertzsprung-Russell diagram, burning helium in its core and pulsating. The maximum radius of the red-giant precursor of V 391 Pegasi may have reached 0.7 AU, while the orbital distance of the planet during the stellar main-sequence phase is estimated to be about 1 AU. This detection of a planet orbiting a post-red-giant star demonstrates that planets with orbital distances of less than 2 AU can survive the red-giant expansion of their parent stars."],["dc.identifier.doi","10.1038/nature06143"],["dc.identifier.isi","000249394500042"],["dc.identifier.pmid","17851517"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/50505"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Nature Publishing Group"],["dc.relation.issn","0028-0836"],["dc.title","A giant planet orbiting the 'extreme horizontal branch' star V391 Pegasi"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1164"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","1174"],["dc.bibliographiccitation.volume","348"],["dc.contributor.author","Reed, M. D."],["dc.contributor.author","Kawaler, Steven D."],["dc.contributor.author","Zola, S."],["dc.contributor.author","Jiang, X. J."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Schuh, S. L."],["dc.contributor.author","Deetjen, J. L."],["dc.contributor.author","Kalytis, R."],["dc.contributor.author","Meistas, E."],["dc.contributor.author","Janulis, Rimvydas"],["dc.contributor.author","Alisauskas, D."],["dc.contributor.author","Krzesinski, J."],["dc.contributor.author","Vuckovic, M."],["dc.contributor.author","Moskalik, P."],["dc.contributor.author","Ogloza, W."],["dc.contributor.author","Baran, A."],["dc.contributor.author","Stachowski, G."],["dc.contributor.author","Kurtz, D. W."],["dc.contributor.author","Perez, JMG"],["dc.contributor.author","Mukadam, A. S."],["dc.contributor.author","Watson, T. K."],["dc.contributor.author","Koen, C."],["dc.contributor.author","Bradley, P. A."],["dc.contributor.author","Cunha, M. S."],["dc.contributor.author","Kilic, M."],["dc.contributor.author","Klumpe, E. W."],["dc.contributor.author","Carlton, R. F."],["dc.contributor.author","Handler, G."],["dc.contributor.author","Kilkenny, D."],["dc.contributor.author","Riddle, R."],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Chevreton, M."],["dc.contributor.author","Wood, M. A."],["dc.contributor.author","Grauer, A."],["dc.contributor.author","Bromage, G."],["dc.contributor.author","Solheim, J. E."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Ulla, A."],["dc.contributor.author","Burleigh, M."],["dc.contributor.author","Good, S."],["dc.contributor.author","Hurkal, O."],["dc.contributor.author","Anderson, R."],["dc.contributor.author","Pakstiene, E."],["dc.date.accessioned","2018-11-07T10:50:20Z"],["dc.date.available","2018-11-07T10:50:20Z"],["dc.date.issued","2004"],["dc.description.abstract","Since pulsating subdwarf B (sdBV or EC14026) stars were first discovered, observational efforts have tried to realize their potential for constraining the interior physics of extreme horizontal branch stars. Difficulties encountered along the way include uncertain mode identifications and a lack of stable pulsation mode properties. Here we report on Feige 48, an sdBV star for which follow- up observations have been obtained spanning more than four years. These observations show some stable pulsation modes. We resolve the temporal spectrum into five stable pulsation periods in the range 340- 380 s with amplitudes less than 1 per cent, and two additional periods that appear in one data set each. The three largest amplitude periodicities are nearly equally spaced, and we explore the consequences of identifying them as a rotationally split l = 1 triplet by consulting a representative stellar model. The general stability of the pulsation amplitudes and phases allows us to use the pulsation phases to constrain the time- scale of evolution for this sdBV star. Additionally, we are able to place interesting limits on any stellar or planetary companion to Feige 48."],["dc.identifier.doi","10.1111/j.1365-2966.2004.07438.x"],["dc.identifier.isi","000220088100006"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/48630"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0035-8711"],["dc.title","Observations of the pulsating subdwarf B star Feige 48: Constraints on evolution and companions"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","219"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","228"],["dc.bibliographiccitation.volume","473"],["dc.contributor.author","Tillich, A."],["dc.contributor.author","Heber, Ulrich"],["dc.contributor.author","O'Toole, S. J."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Schuh, Sonja"],["dc.date.accessioned","2018-11-07T10:57:55Z"],["dc.date.available","2018-11-07T10:57:55Z"],["dc.date.issued","2007"],["dc.description.abstract","Context. Stellar oscillations are an important tool to probe the interior of a star. Subdwarf B stars are core helium burning objects, but their formation is poorly understood as neither single star nor binary evolution can fully explain their observed properties. Since 1997, an increasing number of sdB stars has been found to pulsate forming two classes of stars, the V361 Hya and V1093 Her stars. Aims. We focus on the bright V 361 Hya star PG 1605+ 072 to characterise its frequency spectrum. While most previous studies relied on light variations, we have measured radial velocity variations for as many as 20 modes. In this paper, we aim at characterising the modes from atmospheric parameter and radial velocity variations. Methods. Time resolved spectroscopy (approximate to 9000 spectra) has been carried out to detect line profile variations from which variations of the effective temperature and gravity are extracted by means of a quantitative spectral analysis. Results. We measured variations of effective temperatures and gravities for eight modes with semi- amplitudes ranging from Delta T-eff = 880 K to as small as 88 K, and. log g of 0.08 dex to as low as 0.008 dex. Gravity and temperature vary almost in phase, whereas phase lags are found between temperature and radial velocity. Conclusions. This profound analysis of a unique data set serves as a sound basis for the next step towards an identification of pulsation modes. As rotation may play an important role, the modelling of pulsation modes is challenging but feasible."],["dc.identifier.doi","10.1051/0004-6361:20077949"],["dc.identifier.isi","000249957800024"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9075"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/50363"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.rights","Goescholar"],["dc.rights.access","openAccess"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","The multi-site spectroscopic telescope campaign - II. effective temperature and gravity variations in the multi-periodic pulsating subdwarf B star PG 1605+072"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","submitted_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","219"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","224"],["dc.bibliographiccitation.volume","432"],["dc.contributor.author","Kanaan, A."],["dc.contributor.author","Nitta, A."],["dc.contributor.author","Winget, D. E."],["dc.contributor.author","Kepler, S. O."],["dc.contributor.author","Montgomery, M. H."],["dc.contributor.author","Metcalfe, T. S."],["dc.contributor.author","Oliveira, H."],["dc.contributor.author","Fraga, L."],["dc.contributor.author","da Costa, AFM"],["dc.contributor.author","Costa, JES"],["dc.contributor.author","Castanheira, B. G."],["dc.contributor.author","Giovannini, O."],["dc.contributor.author","Nather, R. E."],["dc.contributor.author","Mukadam, A. S."],["dc.contributor.author","Kawaler, Steven D."],["dc.contributor.author","O'Brien, M. S."],["dc.contributor.author","Reed, M. D."],["dc.contributor.author","Kleinman, S. J."],["dc.contributor.author","Provencal, J. L."],["dc.contributor.author","Watson, T. K."],["dc.contributor.author","Kilkenny, D."],["dc.contributor.author","Sullivan, D. J."],["dc.contributor.author","Sullivan, T."],["dc.contributor.author","Shobbrook, B."],["dc.contributor.author","Jiang, X. J."],["dc.contributor.author","Ashoka, B. N."],["dc.contributor.author","Seetha, S."],["dc.contributor.author","Leibowitz, E. M."],["dc.contributor.author","Ibbetson, P."],["dc.contributor.author","Mendelson, H."],["dc.contributor.author","Meistas, E. G."],["dc.contributor.author","Kalytis, R."],["dc.contributor.author","Alisauskas, D."],["dc.contributor.author","O'Donoghue, D."],["dc.contributor.author","Buckley, D."],["dc.contributor.author","Martinez, P."],["dc.contributor.author","van Wyk, F."],["dc.contributor.author","Stobie, R."],["dc.contributor.author","Marang, F."],["dc.contributor.author","van Zyl, L."],["dc.contributor.author","Ogloza, W."],["dc.contributor.author","Krzesinski, J."],["dc.contributor.author","Zola, S."],["dc.contributor.author","Moskalik, P."],["dc.contributor.author","Breger, M."],["dc.contributor.author","Stankov, A."],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Piccioni, A."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Chevreton, M."],["dc.contributor.author","Deetjen, J."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Perez, JMG"],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Ulla, A."],["dc.contributor.author","Manteiga, M."],["dc.contributor.author","Suarez, O."],["dc.contributor.author","Burleigh, M. R."],["dc.contributor.author","Barstow, M. A."],["dc.date.accessioned","2018-11-07T11:18:05Z"],["dc.date.available","2018-11-07T11:18:05Z"],["dc.date.issued","2005"],["dc.description.abstract","BPM 37093 is the only hydrogen-atmosphere white dwarf currently known which has sufficient mass (similar to 1.1 M-.) to theoretically crystallize while still inside the ZZ Ceti instability strip (T-eff similar to 12 000 K). As a consequence, this star represents our first opportunity to test crystallization theory directly. If the core is substantially crystallized, then the inner boundary for each pulsation mode will be located at the top of the solid core rather than at the center of the star, affecting mainly the average period spacing. This is distinct from the \"mode trapping\" caused by the stratified surface layers, which modifies the pulsation periods more selectively. In this paper we report on Whole Earth Telescope observations of BPM 37093 obtained in 1998 and 1999. Based on a simple analysis of the average period spacing we conclude that a large fraction of the total stellar mass is likely to be crystallized."],["dc.identifier.doi","10.1051/0004-6361:20041125"],["dc.identifier.fs","38252"],["dc.identifier.isi","227493100024"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9872"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/54959"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","E D P Sciences"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Whole Earth Telescope observations of BPM 37093: A seismological test of crystallization theory in white dwarfs"],["dc.title.original","9872"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","445"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.lastpage","450"],["dc.bibliographiccitation.volume","607"],["dc.contributor.author","Reed, M. D."],["dc.contributor.author","Green, Elizabeth M."],["dc.contributor.author","Callerame, K."],["dc.contributor.author","Seitenzahl, I. R."],["dc.contributor.author","White, B. A."],["dc.contributor.author","Hyde, E. A."],["dc.contributor.author","Giovanni, M. K."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Bronowska, A."],["dc.contributor.author","Jeffery, E. J."],["dc.contributor.author","Cordes, O."],["dc.contributor.author","Falter, S."],["dc.contributor.author","Edelmann, H."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Schuh, S. L."],["dc.date.accessioned","2018-11-07T10:48:53Z"],["dc.date.available","2018-11-07T10:48:53Z"],["dc.date.issued","2004"],["dc.description.abstract","A new class of pulsating subdwarf B stars has recently been announced by Green and coworkers. Here we present a follow-up paper describing our observations and the pulsation structure of the class prototype PG 1716+426. The oscillations are multiperiodic with periods between 0.8 and 1.4 hr (180-340 muHz) and semiamplitudes less than 0.2%. We also observe that the periods and amplitudes appear variable, making the pulsation structure of PG 1716 complicated. The periods are an order of magnitude longer than those seen in EC 14026 (sdBV) stars, implying that they are gravity modes rather than pressure modes. As such, they represent a new class of variable star."],["dc.identifier.doi","10.1086/383260"],["dc.identifier.isi","000221523900038"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/48308"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0004-637X"],["dc.title","Discovery of gravity-mode pulsators among subdwarf B stars: PG 1716+426, the class prototype"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]