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101. The Role of Primary 16O as a Neutron Poison in AGB stars and Fluorine primary production at Halo Metallicities

Author: Gallino, R., Bisterzo, S., Cristallo, S., and Straniero, O.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: The discovery of a historical bug in the s-post-process AGB code obtained so far by the Torino group forced us to reconsider the role of primary 16O in the 13C-pocket, produced by the 13C(a, n)16O reaction, as important neutron poison for the build up of the s-elements at Halo metallicities. The effect is noticeable only for the highest 13C-pocket efficiencies (cases ST*2 and ST). For Galactic disc metallicities, the bug effect is negligible. A comparative analysis of the neutron poison effect of other primary isotopes (12C, 22Ne and its progenies) is presented. The effect of proton captures, by 14N(n, p)14C, boosts a primary production of Fluorine in Halo AGB stars, with [F/Fe] comparable to [C/Fe], without affecting the s-elements production., Comment: 6 pages, 6 figures, 4 tables
Published: 2010

102. Fluorine Abundances in Galactic AGB Stars

Author: Abia, C., Cunha, K., Cristallo., S., de Laverny, P., Dominguez, I., Eriksson, K., Gialanella, L., Hinkle, K., Imbriani, G., Recio-Blanco, A, Smith, V. V., Straniero, O., and Wahlin, R.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: An analysis of the fluorine abundance in Galactic AGB carbon stars (24 N-type, 5 SC-type and 5 J-type) is presented. This study uses the state- of-the-art carbon rich atmosphere models and improved atomic and molecular line lists in the 2.3 {\mu}m region. F abundances significantly lower are obtained in comparison to previous study in the literature. The main reason of this difference is due to molecular blends. In the case of carbon stars of SC-type, differences in the model atmospheres are also relevant. The new F enhancements are now in agreement with the most recent theoretical nucleosynthesis models in low- mass AGB stars, solving the long standing problem of F in Galactic AGB stars. Nevertheless, some SC-type carbon stars still show larger F abundances than predicted by stellar models. The possibility that these stars are of larger mass is briefly discussed., Comment: 16 pages, 3 figures, Accepted in ApJ Letters
Published: 2010

103. s-Process in Low Metallicity Stars. I. Theoretical Predictions

Author: Bisterzo, S., Gallino, R., Straniero, O., Cristallo, S., and Kaeppeler, F.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: A large sample of carbon enhanced metal-poor stars enriched in s-process elements (CEMP-s) have been observed in the Galactic halo. These stars of low mass (M ~ 0.9 Msun) are located on the main-sequence or the red giant phase, and do not undergo third dredge-up (TDU) episodes. The s-process enhancement is most plausibly due to accretion in a binary system from a more massive companion when on the asymptotic giant branch (AGB) phase (now a white dwarf). In order to interpret the spectroscopic observations, updated AGB models are needed to follow in detail the s-process nucleosynthesis. We present nucleosynthesis calculations based on AGB stellar models obtained with FRANEC (Frascati Raphson-Newton Evolutionary Code) for low initial stellar masses and low metallicities. For a given metallicity, a wide spread in the abundances of the s-process elements is obtained by varying the amount of 13C and its profile in the pocket, where the 13C(a, n)16O reaction is the major neutron source, releasing neutrons in radiative conditions during the interpulse phase. We account also for the second neutron source 22Ne(a, n)25Mg, partially activated during convective thermal pulses. We discuss the surface abundance of elements from carbon to bismuth, for AGB models of initial masses M = 1.3 -- 2 Msun, low metallicities ([Fe/H] from -1 down to -3.6) and for different 13C-pockets efficiencies. In particular we analyse the relative behaviour of the three s-process peaks: light-s (ls at magic neutron number N = 50), heavy-s (hs at N = 82) and lead (N = 126). Two s-process indicators, [hs/ls] and [Pb/hs], are needed in order to characterise the s-process distribution. In the online material, we provide a set of data tables with surface predictions. ..., Comment: 31 pages, 15 figures + 6 online material, 10 tables
Published: 2010
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104. Optical and near infrared coverage of SN 2004et: physical parameters and comparison with other type IIP supernovae

Author: Maguire, K., Di Carlo, E., Smartt, S. J., Pastorello, A., Tsvetkov, D. Yu., Benetti, S., Spiro, S., Arkharov, A. A., Beccari, G., Botticella, M. T., Cappellaro, E., Cristallo, S., Dolci, M., Elias-Rosa, N., Fiaschi, M., D., Gorshanov, Harutyunyan, A., Larionov, V. M., Navasardyan, H., Pietrinferni, A., Raimondo, G., Di Rico, G., Valenti, S., Valentini, G., and Zampieri, L.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present new optical and near infrared (NIR) photometry and spectroscopy of the type IIP supernova, SN 2004et. In combination with already published data, this provides one of the most complete studies of optical and NIR data for any type IIP SN from just after explosion to +500 days. The contribution of the NIR flux to the bolometric light curve is estimated to increase from 15% at explosion to around 50% at the end of the plateau and then declines to 40% at 300 days. SN 2004et is one of the most luminous IIP SNe which has been well studied, and with a luminosity of log L = 42.3 erg/s, it is 2 times brighter than SN 1999em. We provide parametrised bolometric corrections as a function of time for SN 2004et and three other IIP SNe that have extensive optical and NIR data, which can be used as templates for future events. We compare the physical parameters of SN 2004et with those of other IIP SNe and find kinetic energies spanning the range of 10^50-10^51 ergs. We compare the ejected masses calculated from hydrodynamic models with the progenitor masses and limits derived from prediscovery images. Some of the ejected mass estimates are significantly higher than the progenitor mass estimates, with SN 2004et showing perhaps the most serious mass discrepancy. With current models, it appears difficult to reconcile 100 day plateau lengths and high expansion velocities with the low ejected masses of 5-6 Msun implied from 7-8 Msun progenitors. The nebular phase is studied using very late time HST photometry, along with optical and NIR spectroscopy. The light curve shows a clear flattening at 600 days in the optical and the NIR, which is likely due to the ejecta impacting on the CSM. We further show that the [Oi] 6300,6364 Angstrom line strengths of four type IIP SNe imply ejected oxygen masses of 0.5-1.5 Msun., Comment: 25 pages, 27 figures, submitted to MNRAS
Published: 2009
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105. Barium Stars: Theoretical Interpretation

Author: Husti, L., Gallino, R., Bisterzo, S., Straniero, O., and Cristallo, S.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Barium stars are extrinsic Asymptotic Giant Branch (AGB) stars. They present the s-enhancement characteristic for AGB and post-AGB stars, but are in an earlier evolutionary stage (main sequence dwarfs, subgiants, red giants). They are believed to form in binary systems, where a more massive companion evolved faster, produced the s-elements during its AGB phase, polluted the present barium star through stellar winds and became a white dwarf. The samples of barium stars of Allen & Barbuy (2006) and of Smiljanic et al. (2007) are analysed here. Spectra of both samples were obtained at high-resolution and high S/N. We compare these observations with AGB nucleosynthesis models using different initial masses and a spread of 13C-pocket efficiencies. Once a consistent solution is found for the whole elemental distribution of abundances, a proper dilution factor is applied. This dilution is explained by the fact that the s-rich material transferred from the AGB to the nowadays observed stars is mixed with the envelope of the accretor. We also analyse the mass transfer process, and obtain the wind velocity for giants and subgiants with known orbital period. We find evidence that thermohaline mixing is acting inside main sequence dwarfs and we present a method for estimating its depth., Comment: 8 pages, 11 figures, 6 tables
Published: 2009
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106. MONTAGE: AGB nucleosynthesis with full s-process calculations

Author: Church, R. P., Cristallo, S., Lattanzio, J. C., Stancliffe, R. J., Straniero, O., and Cannon, R. C.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present MONTAGE, a post-processing nucleosynthesis code that combines a traditional network for isotopes lighter than calcium with a rapid algorithm for calculating the s-process nucleosynthesis of the heavier isotopes. The separation of those parts of the network where only neutron-capture and beta-decay reactions are significant provides a substantial advantage in computational efficiency. We present the yields for a complete set of s-process isotopes for a 3 Mo, Z = 0.02 stellar model, as a demonstration of the utility of the approach. Future work will include a large grid of models suitable for use in calculations of Galactic chemical evolution., Comment: 9 pages, 4 figures. Accepted by PASA
Published: 2009
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107. Asymptotic Giant Branch models at very low metallicity

Author: Cristallo, S., Piersanti, L., Straniero, O., Gallino, R., Dominguez, I., and Kappeler, F.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: In this paper we present the evolution of a low mass model (initial mass M=1.5 Msun) with a very low metal content (Z=5x10^{-5}, equivalent to [Fe/H]=-2.44). We find that, at the beginning of the AGB phase, protons are ingested from the envelope in the underlying convective shell generated by the first fully developed thermal pulse. This peculiar phase is followed by a deep third dredge up episode, which carries to the surface the freshly synthesized 13C, 14N and 7Li. A standard TP-AGB evolution, then, follows. During the proton ingestion phase, a very high neutron density is attained and the s-process is efficiently activated. We therefore adopt a nuclear network of about 700 isotopes, linked by more than 1200 reactions, and we couple it with the physical evolution of the model. We discuss in detail the evolution of the surface chemical composition, starting from the proton ingestion up to the end of the TP-AGB phase., Comment: Accepted for Publication on PASA
Published: 2009
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108. The 13C Pocket in Low Mass AGB Stars

Author: Straniero, O., Cristallo, S., and Gallino, R.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: It is well known that thermally pulsing Asymptotic Giant Branch stars with low mass play a relevant role in the chemical evolution. They have synthesized about 30% of the galactic carbon and provide an important contribution to the nucleosynthesis of heavy elements (A>80). The relevant nucleosynthesis site is the He-rich intermediate zone (less than 10^{-2} Msun), where alpha(2alpha,gamma)12C reactions and slow neutron captures on seed nuclei essentially iron) take place. A key ingredient is the interplay between nuclear processes and convective mixing. It is the partial overlap of internal and external convective zones that allows the dredge-up of the material enriched in C and heavy elements. We review the progresses made in the last 50 years in the comprehension of the s process in AGB stars, with special attention to the identification of the main neutron sources and to the particular physical conditions allowing this important nucleosynthesis., Comment: Accepted for Publication on PASA
Published: 2009
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109. Evolution, nucleosynthesis and yields of low mass AGB stars

Author: Cristallo, S., Straniero, O., Gallino, R., Piersanti, L., Dominguez, I., and Lederer, M. T.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: The envelope of thermally pulsing AGB stars undergoing periodic third dredge-up episodes is enriched in both light and heavy elements, the ashes of a complex internal nucleosynthesis involving p, alpha and n captures over hundreds of stable and unstable isotopes. In this paper, new models of low-mass AGB stars (2 Msun), with metallicity ranging between Z=0.0138 (the solar one) and Z=0.0001, are presented. Main features are: i) a full nuclear network (from H to Bi) coupled to the stellar evolution code, ii) a mass loss-period-luminosity relation, based on available data for long period variables, and ii) molecular and atomic opacities for C- and/or N-enhanced mixtures, appropriate for the chemical modifications of the envelope caused by the third dredge up. For each model a detailed description of the physical and chemical evolution is presented; moreover, we present a uniform set of yields, comprehensive of all chemical species (from hydrogen to bismuth). The main nucleosynthesis site is the thin 13C pocket, which forms in the core-envelope transition region after each third dredge up episode. The formation of this 13C pockets is the principal by-product of the introduction of a new algorithm, which shapes the velocity profile of convective elements at the inner border of the convective envelope: both the physical grounds and the calibration of the algorithm are discussed in detail. The final surface compositions of the various models reflect the differences in the initial iron-seed content and in the physical structure of AGB stars belonging to different stellar populations. The agreement with the observed [hs/ls] index observed in intrinsic C stars at different [Fe/H] is generally good., Comment: Accepted for publication on ApJ
Published: 2009
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110. Imaging neutron capture cross sections: i-TED proof-of-concept and future prospects based on Machine-Learning techniques

Author: Babiano-Suárez, V., Lerendegui-Marco, J., Balibrea-Correa, J., Caballero, L., Calvo, D., Ladarescu, I., Real, D., Domingo-Pardo, C., Calviño, F., Casanovas, A., Tarifeño-Saldivia, A., Alcayne, V., Guerrero, C., Millán-Callado, M. A., Rodríguez-González, T., Barbagallo, M., Aberle, O., Amaducci, S., Andrzejewski, J., Audouin, L., Bacak, M., Bennett, S., Berthoumieux, E., Billowes, J., Bosnar, D., Brown, A., Busso, M., Caamaño, M., Calviani, M., Cano-Ott, D., Cerutti, F., Chiaveri, E., Colonna, N., Cortés, G., Cortés-Giraldo, M. A., Cosentino, L., Cristallo, S., Damone, L. A., Davies, P. J., Diakaki, M., Dietz, M., Dressler, R., Ducasse, Q., Dupont, E., Durán, I., Eleme, Z., Fernández-Domínguez, B., Ferrari, A., Finocchiaro, P., Furman, V., Göbel, K., Garg, R., Gawlik, A., Gilardoni, S., Gonçalves, I. F., González-Romero, E., Gunsing, F., Harada, H., Heinitz, S., Heyse, J., Jenkins, D. G., Junghans, A., Käppeler, F., Kadi, Y., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krtička, M., Kurtulgil, D., Lederer-Woods, C., Leeb, H., Lonsdale, S. J., Macina, D., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mingrone, F., Moreno-Soto, J., Musumarra, A., Negret, A., Ogállar, F., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Persanti, L., Petrone, C., Pirovano, E., Porras, I., Praena, J., Quesada, J. M., Ramos-Doval, D., Rauscher, T., Reifarth, R., Rochman, D., Rubbia, C., Sabaté-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Sprung, P., Stamatopoulos, A., Tagliente, G., Tain, J. L., Tassan-Got, L., Thomas, Th., Torres-Sánchez, P., Tsinganis, A., Ulrich, J., Urlass, S., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., and Žugec, P.
Published: 2021
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111. Fluorine in AGB Carbon Stars Revisited

Author: Abia, C., Recio-Blanco, A., de Laverny, P., Cristallo, S., Dominguez, I., and Straniero, O.
Subjects: Astrophysics
Abstract: A reanalysis of the fluorine abundance in three Galactic AGB carbon stars (TX Psc, AQ Sgr and R Scl) has been performed from the molecular HF (1-0) R9 line at 2.3358 $\mu$m. High-resolution (R$\sim 50000$) and high signal to noise spectra obtained with the CRIRES spectrograph and the VLT telescope or from the NOAO archive (for TX Psc) have been used. Our abundance analysis uses the latest generation of MARCS model atmospheres for cool carbon rich stars. Using spectral synthesis in LTE we derive for these stars fluorine abundances that are systematically lower by $\sim 0.8$ dex in average with respect to the sole previous estimates by Jorissen, Smith & Lambert (1992). The possible reasons of this discrepancy are explored. We conclude that the difference may rely on the blending with C-bearing molecules (CN and C$_2$) that were not properly taken into account in the former study. The new F abundances are in better agreement with the prediction of full network stellar models of low mass AGB stars. These models also reproduce the $s$-process elements distribution in the sampled stars. This result, if confirmed in a larger sample of AGB stars, might alleviate the current difficulty to explain the largest [F/O] ratios found by Jorissen et al. In particular, it may not be necessary to search for alternative nuclear chains affecting the production of F in AGB stars., Comment: 25 pages, 3 figures. to be appear in The Astrophysical Journal (Jan 2009 issue)
Published: 2008
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112. Evolution and nucleosynthesis in low mass Asymptotic Giant Branch stars

Author: Cristallo, S.
Subjects: Astrophysics
Abstract: People usually smile when astrophysicists assert that we are sons of the stars, but human life confirms this sentence: about 65% of the mass of our body is made up of oxygen, carbon occurs in all organic life and is the basis of organic chemistry, nitrogen is an essential part of amino acids and nucleic acids, calcium is a major component of our bones. Moreover, phosphorus plays a major role in biological molecules such as DNA and RNA (where the chemical codes of life is written) and our blood carries oxygen to tissues by means of the hemoglobin (an iron pigment of red blood cells). All these elements have been created in stars. I just list some examples related to human body, but also common element such as aluminum, nickel, gold, silver and lead come from a pristine generation of stars. The abundances in the Solar System are in fact due to the mixing of material ejected from stars that polluted the Universe in different epochs before the Sun formation, occurred about 5 billion years ago, after the gravitational contraction of the proto-solar cloud. Low mass AGB stars (1
Published: 2008
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113. AGB stars of the intermediate-age LMC cluster NGC 1846 II. Dredge up along the AGB

Author: Lebzelter, T., Lederer, M. T., Cristallo, S., Hinkle, K. H., Straniero, O., and Aringer, B.
Subjects: Astrophysics
Abstract: Aims: We investigate the change in the surface abundance of $^{12}$C during the evolution along the AGB, aiming to constrain third dredge-up models. Methods: High-resolution, near-infrared spectra of a sample of AGB stars in the LMC cluster NGC 1846 were obtained. A cluster sample ensures a high level of homogeneity with respect to age, metallicity, and distance. The C/O ratio and the ratio of $^{12}$C/$^{13}$C were measured and compared with our evolutionary models. Results: For the first time, we show the evolution of the C/O and $^{12}$C/$^{13}$C ratios along a cluster AGB. Our findings allow us to check the reliability of the evolutionary models and, in particular, the efficiency of the third dredge up. The increase in both C/O and $^{12}$C/$^{13}$C in the observed O-rich stars is reproduced by the models well. However, the low carbon isotopic ratios of the two C-stars in our sample indicate the late occurrence of moderate extra mixing. The extra mixing affects the most luminous AGB stars and is capable of increasing the abundance of $^{13}$C, while leaving unchanged the C/O ratio, which has been fixed by the cumulative action of several third dredge-up episodes. We find indications that the F abundance also increases along the AGB, supporting an in situ production of this element., Comment: 11 pages, accepted for publication in A&A
Published: 2008
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114. Fluorine in carbon-enhanced metal-poor stars: a binary scenario

Author: Lugaro, M., de Mink, S. E., Izzard, R. G., Campbell, S. W., Karakas, A. I., Cristallo, S., Pols, O. R., Lattanzio, J. C., Straniero, O., Gallino, R., and Beers, T. C.
Subjects: Astrophysics
Abstract: A super-solar fluorine abundance was observed in the carbon-enhanced metal-poor (CEMP) star HE 1305+0132 ([F/Fe] = +2.90, [Fe/H] = -2.5). We propose that this observation can be explained using a binary model that involve mass transfer from an asymptotic giant branch (AGB) star companion and, based on this model, we predict F abundances in CEMP stars in general. We discuss wether F can be used to discriminate between the formation histories of most CEMP stars: via binary mass transfer or from the ejecta of fast-rotating massive stars. We compute AGB yields using different stellar evolution and nucleosynthesis codes to evaluate stellar model uncertainties. We use a simple dilution model to determine the factor by which the AGB yields should be diluted to match the abundances observed in HE 1305+0132. We further employ a binary population synthesis tool to estimate the probability of F-rich CEMP stars. The abundances observed in HE 1305+0132 can be explained if this star accreted 3-11% of the mass lost by its former AGB companion. The primary AGB star should have dredged-up at least 0.2 Msun of material from its He-rich region into the convective envelope via third dredge-up, which corresponds to AGB models of Z ~ 0.0001 and mass ~ 2 Msun. Many AGB model uncertainties, such as the treatment of convective borders and mass loss, require further investigation. We find that in the binary scenario most CEMP stars should also be FEMP stars, that is, have [F/Fe] > +1, while fast-rotating massive stars do not appear to produce fluorine. We conclude that fluorine is a signature of low-mass AGB pollution in CEMP stars, together with elements associated with the slow neutron-capture process., Comment: accepted for publication on A&A Letters
Published: 2008
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115. Molecular opacities for low-mass metal-poor AGB stars undergoing the Third Dredge Up

Author: Cristallo, S., Straniero, O., Lederer, M. T., and Aringer, B.
Subjects: Astrophysics
Abstract: The concomitant overabundances of C, N and s-process elements are commonly ascribed to the complex interplay of nucleosynthesis, mixing and mass loss taking place in Asymptotic Giant Branch stars. At low metallicity, the enhancement of C and/or N may be up to 1000 times larger than the original iron content and significantly affects the stellar structure and its evolution. For this reason, the interpretation of the already available and still growing amount of data concerning C-rich metal-poor stars belonging to our Galaxy as well as to dwarf spheroidal galaxies would require reliable AGB stellar models for low and very low metallicities. In this paper we address the question of calculation and use of appropriate opacity coefficients, which take into account the C enhancement caused by the third dredge up. A possible N enhancement, caused by the cool bottom process or by the engulfment of protons into the convective zone generated by a thermal pulse and the subsequent huge third dredge up, is also considered. Basing on up-to-date stellar models, we illustrate the changes induced by the use of these opacity on the physical and chemical properties expected for these stars., Comment: 23 pages, 8 figures, accepted for publication in ApJ
Published: 2007
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116. A Method to Derive the Absolute Composition of the Sun, the Solar System and the Stars

Author: Piersanti, L., Straniero, O., and Cristallo, S.
Subjects: Astrophysics
Abstract: The knowledge of isotopic and elemental abundances of the pristine solar system material provides a fundamental test of galactic chemical evolution models, while the composition of the solar photosphere is a reference pattern to understand stellar abundances. However, spectroscopic or meteoritic abundance determinations are only possible for an incomplete sample of the 83 elements detected in the solar system. Therefore, only relative abundances are experimentally determined, with respect to H or to Si for spectroscopic or meteoritic measurements, respectively. For this reason, the available compilations of solar abundances are obtained by combining spectroscopic and meteoritic determinations, a procedure requiring the knowledge of the chemical modification occurred in the solar photosphere. We provide a method to derive the mass fractions of all the 83 elements (and their most abundant isotopes) in the early solar system material and in the present-day solar surface. Calculations are repeated by adopting the most widely adopted compilations of solar abundances. Since for a given [Fe/H], the total metallicity depends on solar (Z/X), a 30% reduction of Z is found when passing from the classical Anders&Grevesse to the most recent Lodders compilation. Some implications are discussed, as, in particular, an increase of about 700 Myr of the estimated age of Globular Clusters. Within the experimental errors, the complete set of relative solar abundances, as obtained by combining meteoritic and photospheric measurements, are consistent with the variations implied by the quoted physical processes. Few deviations can be easily attributed to the decay of long-lived radioactive isotopes. The huge lithium depletion is only partially explained by introducing a rotational-induced mixing in the tachocline., Comment: 22 pages, 8 figures, accepted by A&A
Published: 2006
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117. Short-lived isotopes and 23Na production in low mass AGB Stars

Author: Cristallo, S., Gallino, R., Straniero, O., Piersanti, L., and Dominguez, I.
Subjects: Astrophysics
Abstract: We discuss the synthesis of some short-lived isotopes and of 23Na in thermally pulsing AGB stars with initial mass of 2 Msun and two different metallicities (Z=1.5e-2, corresponding to the metal amount in the Sun, and Z=1e-4), representative of disk and halo stars, respectively. The different nucleosynthesis channels are illustrated in some details. As previously found, the 13C formed after each third dredge up episode is usually completely consumed by alpha captures before the onset of the subsequent thermal pulse, releasing neutrons. This is the most efficient neutron source in low mass AGB stars and the resulting s-process nucleosynthesis is at the origin of the solar main component. However, in the solar metallicity model, we find that the temperature of the first formed 13C pocket remains too low during the interpulse and the 13C is not completely burnt, being partially engulfed in the convective zone generated by the following thermal pulse. Due to the rapid convective mixing in this zone, the 13C is exposed to a larger temperature and a nucleosynthesis characterized by a relatively high neutron density develops. The main effect is the strong enhancement of isotopes located beyond some critical branching in the neutron-capture path, like 60Fe, otherwise only marginally produced during a standard s-process nucleosynthesis., Comment: 6 pages, 3 figures; in the proceedings of the VIII Torino Workshop on Nucleosynthesis in AGB stars; to be published in Mem.SAIt
Published: 2006

118. s Process in low-mass Asymptotic Giant Branch Stars

Author: Straniero, O., Gallino, R., and Cristallo, S.
Subjects: Astrophysics
Abstract: The main component of the s process is produced by low mass stars (between 1.5 and 3 Mo), when they climb for the second time the red giant branch and experience a series of He shell flashes called thermal pulses. During the relatively long period (10^5 yr) that elapses between two subsequent thermal pulses, a slow neutron flux is provided by the 13C(a,n)16O reaction taking place within a thin 13C pocket located in the He-rich and C-rich mantel of these stars. A second, marginal, neutron burst occurs during the thermal pulse and it is powered by the 22Ne(a,n)25Mg reaction. We review the present status of the nucleosynthesis models of low mass AGB stars. The advance in the knowledge of the complex coupling between convective mixing and nuclear process, which allows the surface enrichment of C and s-process elements, is presented, together with the hypotheses concerning the physical mechanism driving the formation of the 13C pocket. In order to illustrate the capabilities and the limits of the theory, an updated computation of a 2 Mo stellar structure with solar chemical composition is reported. This model has been obtained by including a full nuclear network (from H up to Bi, at the termination point of the s-process path) into the stellar evolution code. The predicted modification of the surface composition occurring during the AGB evolution is shown. The new challenge of AGB modeling, namely the study of C-rich and s-rich very metal-poor stars, is discussed., Comment: pages 35
Published: 2005
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119. Experimental setup and procedure for the measurement of the 7Be(n,p)7Li reaction at n_TOF

Author: Barbagallo, M., Andrzejewski, J., Mastromarco, M., Perkowski, J., Damone, L.A., Gawlik, A., Cosentino, L., Finocchiaro, P., Maugeri, E.A., Mazzone, A., Dressler, R., Heinitz, S., Kivel, N., Schumann, D., Colonna, N., Aberle, O., Amaducci, S., Audouin, L., Bacak, M., Balibrea, J., Bečvář, F., Bellia, G., Berthoumieux, E., Billowes, J., Bosnar, D., Brown, A., Caamaño, M., Calviño, F., Calviani, M., Cano-Ott, D., Cardella, R., Casanovas, A., Cerutti, F., Chen, Y.H., Chiaveri, E., Cortés, G., Cortés-Giraldo, M.A., Cristallo, S., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dupont, E., Durán, I., Fernández-Domínguez, B., Ferrari, A., Ferreira, P., Furman, V., Göbel, K., García, A.R., Gilardoni, S., Glodariu, T., Gonçalves, I.F., González-Romero, E., Griesmayer, E., Guerrero, C., Gunsing, F., Harada, H., Heyse, J., Jenkins, D.G., Jericha, E., Johnston, K., Käppeler, F., Kadi, Y., Kalamara, A., Kavrigin, P., Kimura, A., Kokkoris, M., Krtička, M., Kurtulgil, D., Leal-Cidoncha, E., Lederer, C., Leeb, H., Lerendegui-Marco, J., Lo Meo, S., Lonsdale, S.J., Macina, D., Manna, A., Marganiec, J., Martínez, T., Martins-Correia, J.G., Masi, A., Massimi, C., Mastinu, P., Mendoza, E., Mengoni, A., Milazzo, P.M., Mingrone, F., Musumarra, A., Negret, A., Nolte, R., Oprea, A., Pappalardo, A.D., Patronis, N., Pavlik, A., Piscopo, M., Porras, I., Praena, J., Quesada, J.M., Radeck, D., Rauscher, T., Reifarth, R., Robles, M.S., Rubbia, C., Ryan, J.A., Sabaté-Gilarte, M., Saxena, A., Schell, J., Schillebeeckx, P., Sedyshev, P., Smith, A.G., Sosnin, N.V., Stamatopoulos, A., Tagliente, G., Tain, J.L., Tarifeño-Saldivia, A., Tassan-Got, L., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Wallner, A., Warren, S., Weiss, C., Woods, P.J., Wright, T., and Žugec, P.
Published: 2018
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120. Rare earth element abundances in presolar SiC

Author: Ireland, T.R., Ávila, J.N., Lugaro, M., Cristallo, S., Holden, P., Lanc, P., Nittler, L., Alexander, C.M.O'D., Gyngard, F., and Amari, S.
Published: 2018
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121. First detection of a lithium rich carbon star in the Draco dwarf galaxy: evidence for a young stellar population

Author: Dominguez, I., Abia, C., Straniero, O., Cristallo, S., and Pavlenko, Ya. V.
Subjects: Astrophysics
Abstract: We present a spectroscopic study of D461, a giant star belonging to Draco dwarf spheroidal galaxy. From spectral synthesis in LTE we derive a lithium abundance of log e(Li)=3.5+/-0.4 and a C/O ratio between 3 and 5. This is the first detection of a lithium rich C-star in a dwarf spheroidal galaxy. Basing on stellar models of appropriate chemical composition, we show that a similar C enrichment is compatible with that expectedfor a low mass low metallicity thermally pulsing AGB star, undergoing few third dredge up episodes. The position in the log g-log Teff diagram of D461 is also compatible with this theoretical scenario. In particular, the low effective temperature, lower than that expected for a low metallicity giant star, is a consequence of the huge increase of the envelope opacity occurring after the carbon dredge up. The Li enrichment may be explained if a deep circulation would take place during the interpulse period, the so called cool bottom process. In spite of the low resolution of our spectra, we derive a lower limit for the carbon isotopic ratio, namely 12C/13C>40, and a constraint for the Ba abundance, namely 0.5<[Ba/Fe]< 2. The proposed scenario also fits these further constraints. Then, we estimate that the mass of D461 ranges between 1.2 and 2 $M_\odot$, which corresponds to an age ranging between 1 and 3 Gyr. We conclude that this star is more massive and younger than the typical stellar population of Draco., Comment: 10 pages, 5 figues. Accepted for publication in A&A
Published: 2004
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122. Measurement of the $$^{244}$$ 244 Cm and $$^{246}$$ 246 Cm Neutron-Induced Cross Sections at the n_TOF Facility

Author: Alcayne, V., primary, Kimura, A., additional, Mendoza, E., additional, Cano-Ott, D., additional, Aberle, O., additional, Amaducci, S., additional, Andrzejewski, J., additional, Audouin, L., additional, Babiano-Suarez, V., additional, Bacak, M., additional, Barbagallo, M., additional, Bécares, V., additional, Bečvář, F., additional, Bellia, G., additional, Berthoumieux, E., additional, Billowes, J., additional, Bosnar, D., additional, Brown, A. S., additional, Busso, M., additional, Caamaño, M., additional, Caballero, L., additional, Calviani, M., additional, Calviño, F., additional, Casanovas, A., additional, Cerutti, F., additional, Chen, Y. H., additional, Chiaveri, E., additional, Colonna, N., additional, Cortés, G. P., additional, Cortés-Giraldo, M. A., additional, Cosentino, L., additional, Cristallo, S., additional, Damone, L. A., additional, Diakaki, M., additional, Dietz, M., additional, Domingo-Pardo, C., additional, Dressler, R., additional, Dupont, E., additional, Durán, I., additional, Eleme, Z., additional, Fernández-Domíngez, B., additional, Ferrari, A., additional, Ferro-Gon calves, I., additional, Finocchiaro, P., additional, Furman, V., additional, Gawlik, A., additional, Gilardoni, S., additional, Glodariu, T., additional, Göbel, K., additional, González-Romero, E., additional, Guerrero, C., additional, Gunsing, F., additional, Heinitz, S., additional, Heyse, J., additional, Jenkins, D. G., additional, Kadi, Y., additional, Käppeler, F., additional, Kivel, N., additional, Kokkoris, M., additional, Kopatch, Y., additional, Krtička, M., additional, Kurtulgil, D., additional, Ladarescu, I., additional, Lederer-Woods, C., additional, Lerendegui-Marco, J., additional, Meo, S. Lo, additional, Lonsdale, S.-J., additional, Macina, D., additional, Manna, A., additional, Martínez, T., additional, Masi, A., additional, Massimi, C., additional, Mastinu, P. F., additional, Mastromarco, M., additional, Matteucci, F., additional, Maugeri, E., additional, Mazzone, A., additional, Mengoni, A., additional, Michalopoulou, V., additional, Milazzo, P. M., additional, Mingrone, F., additional, Musumarra, A., additional, Negret, A., additional, Nolte, R., additional, Ogállar, F., additional, Oprea, A., additional, Patronis, N., additional, Pavlik, A., additional, Perkowski, J., additional, Piersanti, L., additional, Porras, I., additional, Praena, J., additional, Quesada, J. M., additional, Radeck, D., additional, Doval, D. Ramos, additional, Rausher, T., additional, Reifarth, R., additional, Rochman, D., additional, Rubbia, C., additional, Sabaté-Gilarte, M., additional, Saxena, A., additional, Schillebeeckx, P., additional, Schumann, D., additional, Smith, A. G., additional, Sosnin, N., additional, Stamatopoulos, A., additional, Tagliente, G., additional, Tain, J. L., additional, Talip, Z., additional, Tarifeño-Saldivia, A. E., additional, Tassan-Got, L., additional, Tsinganis, A., additional, Ulrich, J., additional, Urlass, S., additional, Valenta, S., additional, Vannini, G., additional, Variale, V., additional, Vaz, P., additional, Ventura, A., additional, Vlachoudis, V., additional, Vlastou, R., additional, Wallner, A., additional, Woods, P. J., additional, Wright, T. J., additional, and Žugec, P., additional
Published: 2019
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123. The neutron time-of-flight facility n_TOF at CERN Recent facility upgrades and detector developments

Author: Domingo-Pardo, C., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Koster, U., Kokkoris, M., Krtiscka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Perez de Rada, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., Zugec, P., Domingo-Pardo, C., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Koster, U., Kokkoris, M., Krtiscka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Perez de Rada, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., and Zugec, P.
Abstract: Based on an idea by Carlo Rubbia, the n_TOF facility at CERN has been operating for over 20 years. It is a neutron spallation source, driven by the 20 GeV/c proton beam from the CERN PS accelerator. Neutrons in a very wide energy range (from GeV, down to sub-eV kinetic energy) are generated by a massive Lead spallation target feeding two experimental areas. EAR1, horizonal with respect to the proton beam direction is set at 185 meters from the spallation target. EAR2, on the vertical line from the spallation source, is placed at 20 m. Neutron energies for experiments are selected by the time-of-flight technique (hence the name n_TOF), while the long flight paths ensure a very good energy resolution. Over one hundred experiments have been performed by the n_TOF Collaboration at CERN, with applications ranging from nuclear astrophysics (synthesis of the heavy elements in stars, big bang nucleosynthesis, nuclear cosmo-chronology), to advanced nuclear technologies (nuclear data for applications, nuclear safety), as well as for basic nuclear science (reaction mechanisms, structure and decay of highly excited compound states). During the planned shutdown of the CERN accelerator complex between 2019 and 2021, the facility went through a substantial upgrade with a new target-moderator assembly, refurbishing of the neutron beam lines and experimental areas. An additional measuring and irradiation station (the NEAR Station) has been envisaged and its capabilities for performing material test studies and new physics opportunities are presently explored. An overview of the facility and of the activities performed at CERN is presented in this contribution, with a particular emphasis on the most relevant experiments for nuclear astrophysics.
Published: 2023
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124. The Gaia-ESO survey : Placing constraints on the origin of r-process elements

Author: van der Swaelmen, M., Viscasillas Vazquez, C., Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaisiene, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jimenez-Esteban, F., Guiglion, G., Korn, Andreas, Masseron, T., Minkeviiute, R., Smiljanic, R., Spina, L., Stonkute, E., Zaggia, S., van der Swaelmen, M., Viscasillas Vazquez, C., Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaisiene, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jimenez-Esteban, F., Guiglion, G., Korn, Andreas, Masseron, T., Minkeviiute, R., Smiljanic, R., Spina, L., Stonkute, E., and Zaggia, S.
Abstract: Context: A renewed interest in the origin of r-process elements has been stimulated by the multi-messenger observation of the gravitational event GW170817, with the detection of both gravitational waves and electromagnetic waves corresponding to the merger of two neutron stars. Such a phenomenon has been proposed as one of the main sources of the r-process. However, the origin of the r-process elements at different metallicities is still under debate. Aims: We aim at investigate the origin of the r-process elements in the Galactic thin-disc population. Methods: From the sixth internal data release of the Gaia-ESO, we have collected a large sample of Milky Way (MW) thin- and thick-disc stars for which abundances of Eu, O, and Mg are available. The sample consists of members of 62 open clusters (OCs), located at a Galactocentric radius between similar to 5kpc and similar to 20kpc in the disc, in the metallicity range [- 0.5,0.4], and covering an age interval from 0.1 to 7 Gy, and about 1300 Milky Way disc field stars in the metallicity range [- 1.5,0.5]. We compare the observations with the results of a chemical evolution model, in which we varied the nucleosynthesis sources for the three elements considered. Results: Our main result is that Eu in the thin disc is predominantly produced by sources with short lifetimes, such as magneto-rotationally driven SNe. There is no strong evidence for additional sources at delayed times. Conclusions: Our findings do not imply that there cannot be a contribution from mergers of neutron stars in other environments, as in the halo or in dwarf spheroidal galaxies, but such a contribution is not needed to explain Eu abundances at thin-disc metallicities.
Published: 2023
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125. The n_TOF NEAR Station Commissioning and first physics case

Author: Stamati, M. E., Torres-Sanchez, P., Perez-Maroto, P., Cecchetto, M., Goula, S., Mastromarco, M., Chasapoglou, S., Beltrami, C., Chiesa, D., Manna, A., Mucciola, R., Patronis, N., Praena, J., Guerrero, C., Colonna, N., Mengoni, A., Massimi, C., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Camprini, P. C. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticke, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Martinez, T., Masi, A., Mastinu, P., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Michalopoulou, V., Milazzo, P. M., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Oprea, A., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zugec, P., Stamati, M. E., Torres-Sanchez, P., Perez-Maroto, P., Cecchetto, M., Goula, S., Mastromarco, M., Chasapoglou, S., Beltrami, C., Chiesa, D., Manna, A., Mucciola, R., Patronis, N., Praena, J., Guerrero, C., Colonna, N., Mengoni, A., Massimi, C., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Camprini, P. C. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticke, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Martinez, T., Masi, A., Mastinu, P., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Michalopoulou, V., Milazzo, P. M., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Oprea, A., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., and Zugec, P.
Abstract: The NEAR Station is a new experimental area developed at the n_TOF Facility at CERN. The activation station of NEAR underwent a characterization of the beam following the installation of the new n_TOF Spallation Target. The commissioning of the neutron beam comprises a set of simulations made with the FLUKA code and experimental verification. The experimental determination of the neutron spectrum was made using activation techniques with three separate set-ups. Two set-ups were based on the Multi-foil Activation technique (MAM-1 and MAM-2), and the third set-up relied on the process of neutron moderation and activation of a single material (ANTILoPE). The three set-ups are presented. Also the present plans and future perspectives of the activation station of NEAR are discussed.
Published: 2023
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126. Compton imaging for enhanced sensitivity (n,gamma) cross section TOF experiments : Status and prospects

Author: Domingo-Pardo, C., Babiano-Suarez, V., Balibrea-Correa, J., Caballero, L., Ladarescul, I., Lerendegui-Marco, J., Tarifeno-Saldivia, A., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Andrzejewski, J., Bacak, M., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Koster, U., Krticka, M., Kyritsis, N., Lederer-Woods, C., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez-Caballero, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., Zugec, P., Domingo-Pardo, C., Babiano-Suarez, V., Balibrea-Correa, J., Caballero, L., Ladarescul, I., Lerendegui-Marco, J., Tarifeno-Saldivia, A., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Andrzejewski, J., Bacak, M., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Koster, U., Krticka, M., Kyritsis, N., Lederer-Woods, C., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez-Caballero, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., and Zugec, P.
Abstract: Radiative neutron-capture cross sections are of pivotal importance in many fields such as nucle-osynthesis studies or innovative reactor technologies. A large number of isotopes have been measured with high accuracy, but there are still a large number of relevant isotopes whose cross sections could not be experimentally determined yet, at least with sufficient accuracy and completeness, owing to limitations in detection techniques, sample production methods or in the facilities themselves. In the context of the HYMNS (High-sensitivitY Measurements of key stellar Nucleo-Synthesis reactions) project over the last six years we have developed a novel detection technique aimed at background suppression in radiative neutron-capture time-of-flight measurements. This new technique utilizes a complex detection set-up based on position-sensitive radiation-detectors deployed in a Compton-camera array configuration. The latter enables to implement gamma-ray imaging techniques, which help to disentangle true capture events arising from the sample under study and contaminant background events from the surroundings. A summary on the main developments is given in this contribution together with an update on recent experiments at CERN n_TOF and an outlook on future steps.
Published: 2023
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127. First high resolution measurement of neutron capture resonances in Yb-176 at the n_TOF CERN facility.

Author: Garcia-Infantes, F., Praena, J., Casanovas, A., Mastromarco, M., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. C. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Oprea, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Stamati, M. E., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Torres-Sanchez, P., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zugec, P., Garcia-Infantes, F., Praena, J., Casanovas, A., Mastromarco, M., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. C. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Oprea, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Stamati, M. E., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Torres-Sanchez, P., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., and Zugec, P.
Abstract: Several international agencies recommend the study of new routes and new facilities for producing radioisotopes with application to nuclear medicine. Lu-177 is a versatile radioisotope used for therapy and diagnosis (theranostics) of cancer with good success in neuroendocrine tumours that is being studied to be applied to a wider range of tumours. Lu-177 is produced in few nuclear reactors mainly by the neutron capture on Lu-176. However, it could be produced at high -intensity accelerator-based neutron facilities. The energy of the neutrons in accelerator-based neutron facilities is higher than in thermal reactors. Thus, experimental data on the Yb-176(n,(sic)) cross-section in the eV and keV region are mandatory to calculate accurately the production of Yb-177, which beta decays to 177Lu. At present, there are not experimental data available from thermal to 3 keV of the Yb-176(n,(sic)) cross-section. In addition, there is no data in the resolved resonance region (RRR). This contribution shows the first results of the Yb-176 capture measurement performed at the n_TOF facility at CERN.
Published: 2023
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128. Characterisation of the n_TOF 20 m beam line at CERN with the new spallation target

Author: Pavon-Rodriguez, J. A., Alcayne, V., Amaducci, S., Bacak, M., Casanovas, A., Cortes-Giraldo, M. A., Garcia-Infantes, F., Lerendegui-Marco, J., Manna, A., Musacchio-Gonzalez, E., Patronis, N., Sabate-Gilarte, M., Stamati, M. E., Tassan-Got, L., Vlachoudis, V., Aberle, O., Altieri, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Balibrea, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. C. Console, Cortes, G., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guetrero, C., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerner, G., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musumarra, A., Negret, A., Oprea, A., Perez-Maroto, P., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Praena, J., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sanchez, A., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Torres-Sanchez, P., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zugec, P., Pavon-Rodriguez, J. A., Alcayne, V., Amaducci, S., Bacak, M., Casanovas, A., Cortes-Giraldo, M. A., Garcia-Infantes, F., Lerendegui-Marco, J., Manna, A., Musacchio-Gonzalez, E., Patronis, N., Sabate-Gilarte, M., Stamati, M. E., Tassan-Got, L., Vlachoudis, V., Aberle, O., Altieri, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Balibrea, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. C. Console, Cortes, G., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guetrero, C., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerner, G., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musumarra, A., Negret, A., Oprea, A., Perez-Maroto, P., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Praena, J., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sanchez, A., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Torres-Sanchez, P., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., and Zugec, P.
Abstract: The n_TOF facility hosts CERN's pulsed neutron source, comprising two beam lines of different flight paths and one activation station. It is based on a proton beam delivered by the PS accelerator impinging on a lead spallation target. During Long Shutdown 2 (LS2) at CERN (2019-2021), a major upgrade of the spallation target was carried out in order to optimize the performances of the neutron beam. Therefore, the characteristics of n_TOF two experimental areas were investigated in detail. In this work, the focus is on the second experimental area (EAR2), located 20 m above the spallation target. Preliminary results of the neutron energy distribution and beam line energy resolution are presented, compared to previous experimental campaigns and Monte Carlo simulations with the FLUKA code. Moreover, preliminary results of the spatial beam profile measurements are shown.
Published: 2023
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129. Overview of the dissemination of n_TOF experimental data and resonance parameters

Author: Dupont, E., Otuka, N., Rochman, D., Noguere, G., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Romanets, Y., Rubbia, C., Sanchez-Caballero, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., Zugec, P., Dupont, E., Otuka, N., Rochman, D., Noguere, G., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Romanets, Y., Rubbia, C., Sanchez-Caballero, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., and Zugec, P.
Abstract: The n_TOF neutron time-of-flight facility at CERN is used for nuclear data measurements. The n_TOF Collaboration works closely with the Nuclear Reaction Data Centres (NRDC) network to disseminate the experimental data through the international EXFOR library. In addition, the Collaboration helps integrate the results in the evaluated library projects. The present contribution describes the dissemination status of n_TOF results, their impact on evaluated libraries and ongoing efforts to provide n_TOF resonance parameters in ENDF-6 format for further use by evaluation projects.
Published: 2023
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130. New perspectives for neutron capture measurements in the upgraded CERN-n_TOF Facility

Author: Lerendegui-Marco, J., Casanovas, A., Alcayne, V., Aberle, O., Altieri, S., Amaducci, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarrío, Diego, Torres-Sanchez, P., Urlass, S., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, T., Woods, P. J., Wright, T., Zarrella, R., Zugec, P., Lerendegui-Marco, J., Casanovas, A., Alcayne, V., Aberle, O., Altieri, S., Amaducci, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerner, G., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarrío, Diego, Torres-Sanchez, P., Urlass, S., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, T., Woods, P. J., Wright, T., Zarrella, R., and Zugec, P.
Abstract: The n_TOF facility has just undergone in 2021 a major upgrade with the installation of its third generation spallation target that has been designed to optimize the performance of the two n_TOF time-of-flight lines. This contribution describes the key features and limitations for capture measurements in the two beam lines prior to the target upgrade and presents first results of (n,gamma) measurements carried out as part of the commissioning of the upgraded facility. In particular, the energy resolution, a key factor for both increasing the signal-to background ratio and obtaining accurate resonance parameters, has been clearly improved for the 20 m long vertical beam-line with the new target design while keeping the remarkably high resolution of the long beamline n_TOF-EAR1. The improvements in the n_TOF neutron beam-lines need to be accompanied by improvements in the instrumentation. A review is given on recent detector R&D projects aimed at tackling the existing challenges and further improving the capabilities of this facility.
Published: 2023
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131. Neutron capture and total cross-section measurements on Mo-94'95'96 at n_TOF and GELINA

Author: Mucciola, R., Paradela, C., Manna, A., Alaerts, G., Massimi, C., Kopecky, S., Mengoni, A., Moens, A., Schillebeeckx, P., Wynants, R., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. C. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Martinez, T., Masi, A., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Michalopoulou, V., Milazzo, P. M., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Oprea, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Praena, J., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Stamati, M. E., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Torres-Sanchez, P., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zugec, P., Mucciola, R., Paradela, C., Manna, A., Alaerts, G., Massimi, C., Kopecky, S., Mengoni, A., Moens, A., Schillebeeckx, P., Wynants, R., Aberle, O., Alcayne, V., Altieri, S., Amaducci, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. C. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Martinez, T., Masi, A., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Michalopoulou, V., Milazzo, P. M., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Oprea, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Praena, J., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Stamati, M. E., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Torres-Sanchez, P., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., and Zugec, P.
Abstract: Capture and total cross section measurements for 94'95'96 MO have been performed at the neutron time -of-flight facilities, n_TOF at CERN and GELINA at JRC-Geel. The measurements were performed using isotopically enriched samples with an enrichment above 95% for each of the (94'95'96)M0 isotopes. The capture measurements were performed at n_TOF using C6D6 detectors and a new sTED detector. The transmission measurements were performed at a 10 m station of GELINA using a Li-6 glass neutron detector. Preliminary results of these measurements are presented.
Published: 2023
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132. A segmented total energy detector (sTED) for (n, gamma) cross section measurements at n_TOF EAR2

Author: Alcayne, V., Cano-Ott, D., Garcia, J., Gonzalez-Romero, E., Martinez, T., Mendoza, E., Sanchez, A., Plaza, J., Balibrea-Correa, J., Casanovas, A., Domingo-Pardo, C., Lerendegui-Marco, J., Aberle, O., Altieri, S., Amaducci, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibreas, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ottl, D., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. C. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerner, G., Manna, A., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Oprea, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Praena, J., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Stamati, M. E., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Torres-Sanchez, P., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zugec, P., Alcayne, V., Cano-Ott, D., Garcia, J., Gonzalez-Romero, E., Martinez, T., Mendoza, E., Sanchez, A., Plaza, J., Balibrea-Correa, J., Casanovas, A., Domingo-Pardo, C., Lerendegui-Marco, J., Aberle, O., Altieri, S., Amaducci, S., Es-Sghir, H. Amar, Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibreas, J., Bennett, S., Bernardes, A. P., Berthoumieux, E., Bosnar, D., Busso, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ottl, D., Castelluccio, D. M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. C. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Di Castro, M., Diacono, D., Diakaki, M., Dietz, M., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Katabuchi, T., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerner, G., Manna, A., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Oprea, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Pomp, Stephan, Porras, I., Praena, J., Protti, N., Quesada, J. M., Rauscher, T., Reifarth, R., Rochman, D., Romanets, Y., Romano, F., Rubbia, C., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Spelta, M., Stamati, M. E., Tagliente, G., Tarifeno-Saldivia, A., Tarrío, Diego, Terranova, N., Torres-Sanchez, P., Urlass, S., Valenta, S., Variale, V., Vaz, P., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., and Zugec, P.
Abstract: The neutron time-of-flight facility n_TOF is characterised by its high instantaneous neutron intensity, high resolution and broad neutron energy spectra, specially conceived for neutron-induced reaction cross section measurements. Two Time-Of-Flight (TOR) experimental areas are available at the facility: experimental area 1 (EAR1), located at the end of the 185 m horizontal flight path from the spallation target, and experimental area 2 (EAR2), placed at 20 m from the target in the vertical direction. The neutron fluence in EAR2 is similar to 300 times more intense than in EARL in the relevant time-of-flight window. EAR2 was designed to carry out challenging cross-section measurements with low mass samples (approximately 1 mg), reactions with small cross-sections or/and highly radioactive samples. The high instantaneous fluence of EAR2 results in high counting rates that challenge the existing capture systems. Therefore, the sTED detector has been designed to mitigate these effects. In 2021, a dedicated campaign was done validating the performance of the detector up to at least 300 keV neutron energy. After this campaign, the detector has been used to perform various capture cross section measurements at n_TOF EAR2.
Published: 2023
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133. Measurement of the Gd-160(n, gamma) cross section at n_TOF and its medical implications

Author: Mastromarco, M., Manna, A., Garcia-Infantes, F., Amaducci, S., Mengoni, A., Massimi, C., Tagliente, G., Cristallo, S., Aberle, O., Alcayne, V., Altieri, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadil, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Martinez, T., Masi, A., Mastinu, P., Maugeri, E. A., Mazzone, A., Mendoza, E., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Perez de Rada, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tarifeno-Saldivia, A., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., Zugec, P., Mastromarco, M., Manna, A., Garcia-Infantes, F., Amaducci, S., Mengoni, A., Massimi, C., Tagliente, G., Cristallo, S., Aberle, O., Alcayne, V., Altieri, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadil, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lerner, G., Martinez, T., Masi, A., Mastinu, P., Maugeri, E. A., Mazzone, A., Mendoza, E., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., Perez de Rada, A., Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tarifeno-Saldivia, A., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., and Zugec, P.
Abstract: Neutron-capture reactions on gadolinium isotopes play an important role in several fields of physics, in particular in nuclear Astrophysics for the understanding of the nucleosynthesis of heavy elements (beyond iron) in stars via the s- and r-processes [1] and in nuclear technology. Another important application of gadolinium is linked to the production of terbium, that offers a set of clinically interesting isotopes for theranostics, characterized by complementary physical decay characteristics. In particular, the low -energy beta(-) emitter terbium-161 is very similar to lutetium-177 in terms of half-life (6.89 d), beta(-) - energy and chemical properties. Being a significant emitter of conversion/Auger electrons, greater therapeutic effect can therefore be expected in comparison to Lu-177 [2, 3]. For this reason, in the last decade, the study of the neutron capture reaction Gd-160(n,,gamma)(161) Gd and the subsequent beta(-) - decay in terbium-161 is getting particular attention. As the nuclear data on the Gd-160 neutron capture reaction are quite scarce and inconsistent, a new measurement of the capture cross section of Gd-160 at the CERN neutron Time -Of-Flight facilty was performed in order to provide high resolution, high -accuracy data on this important reaction, in the energy range from thermal to hundreds of keV. In this contribution, the preliminary results of the n_TOF measurement are presented.
Published: 2023
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134. The Gaia-ESO survey:Placing constraints on the origin of r-process elements

Author: van der Swaelmen, M., Viscasillas Vazquez, C., Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaisiene, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jimenez-Esteban, F., Guiglion, G., Korn, A., Masseron, T., Minkeviiute, R., Smiljanic, R., Spina, L., Stonkute, E., Zaggia, S., van der Swaelmen, M., Viscasillas Vazquez, C., Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaisiene, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jimenez-Esteban, F., Guiglion, G., Korn, A., Masseron, T., Minkeviiute, R., Smiljanic, R., Spina, L., Stonkute, E., and Zaggia, S.
Abstract: Context. A renewed interest in the origin of r-process elements has been stimulated by the multi-messenger observation of the gravitational event GW170817, with the detection of both gravitational waves and electromagnetic waves corresponding to the merger of two neutron stars. Such a phenomenon has been proposed as one of the main sources of the r-process. However, the origin of the r-process elements at different metallicities is still under debate.Aims. We aim at investigate the origin of the r-process elements in the Galactic thin-disc population.Methods. From the sixth internal data release of the Gaia-ESO, we have collected a large sample of Milky Way (MW) thin- and thick-disc stars for which abundances of Eu, O, and Mg are available. The sample consists of members of 62 open clusters (OCs), located at a Galactocentric radius between similar to 5kpc and similar to 20kpc in the disc, in the metallicity range [- 0.5,0.4], and covering an age interval from 0.1 to 7 Gy, and about 1300 Milky Way disc field stars in the metallicity range [- 1.5,0.5]. We compare the observations with the results of a chemical evolution model, in which we varied the nucleosynthesis sources for the three elements considered.Results. Our main result is that Eu in the thin disc is predominantly produced by sources with short lifetimes, such as magneto-rotationally driven SNe. There is no strong evidence for additional sources at delayed times.Conclusions. Our findings do not imply that there cannot be a contribution from mergers of neutron stars in other environments, as in the halo or in dwarf spheroidal galaxies, but such a contribution is not needed to explain Eu abundances at thin-disc metallicities.
Published: 2023

135. New detection systems for an enhanced sensitivity in key stellar (n,$\gamma$) measurements

Author: Lerendegui-Marco, J., Babiano-Suarez, V., Balibrea-Correa, J., Domingo-Pardo, C., Ladarescu, I., Tarifeno-Saldivia, A., Alcayne, V., Cano-Ott, D., Gonzalez-Romero, E., Martinez, T., Mendoza, E., Guerrero, C., Calvino, F., Casanovas, A., Koster, U., Chiera, N. M., Dressler, R., Maugeri, E. A., Schumann, D., Aberle, O., Altieri, S., Amaducci, S., Andrzejewski, J., Bacak, M., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., Beyer, R., Boromiza, M., Bosnar, D., Caamano, M., Calviani, M., Cerutti, F., Cescutti, G., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Garcia-Infantes, F., Gawlik-Ramiega, A., Gervino, G., Gilardoni, S., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Krticka, M., Kyritsis, N., Lederer-Woods, C., Lerner, G., Manna, A., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Mazzone, A., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Patronis, N., Pavon-Rodriguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, Stephan, Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez-Caballero, A., Sabate-Gilarte, M., Schillebeeckx, P., Sekhar, A., Smith, A. G., Sosnin, N. V., Stamati, M. E., Sturniolo, A., Tagliente, G., Tarrío, Diego, Torres-Sanchez, P., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zarrella, R., Zugec, P., Freeman, S., Lederer-Woods, C., Manna, A., and Mengoni, A.
Subjects: Subatomär fysik, neutron capture, n_TOF, neutron time of flight, Astrophysics and Astronomy, Astronomi, astrofysik och kosmologi, Subatomic Physics, Astronomy, Astrophysics and Cosmology, Nuclear Physics - Experiment, General Medicine, nucl-ex, Astrophysics - Instrumentation and Methods for Astrophysics, Nuclear Experiment, astro-ph.IM
Abstract: Neutron capture cross-section measurements are fundamental in the study of astrophysical phenomena, such as the slow neutron capture (s-) process of nucleosynthesis operating in red-giant and massive stars. However, neutron capture measurements via the time-of-flight (TOF) technique on key s-process nuclei are often challenging. Difficulties arise from the limited mass (∼mg) available and the high sample-related background in the case of the unstable s-process branching points. Measurements on neutron magic nuclei, that act as s-process bottlenecks, are affected by low (n,γ) cross sections and a dominant neutron scattering background. Overcoming these experimental challenges requires the combination of facilities with high instantaneous flux, such as n_TOFEAR2, with detection systems with an enhanced detection sensitivity and high counting rate capabilities. This contribution reviews some of the latest detector developments in detection systems for (n,γ) measurements at n_TOF, such as i-TED, an innovative detection system which exploits the Compton imaging technique to reduce the dominant neutron scattering background and s-TED, a highly segmented total energy detector intended for high flux facilities. The discussion will be illustrated with results of the first measurement of key the s-process branching-point reaction 79Se(n,γ)., European Research Council (ERC), European Union’s Horizon 2020 research and innovation programme (ERC Consolidator Grant project HYMNS, with grant agreement No. 681740), FJC2020-044688-I, ICJ220-045122-I funded by MCIN/AEI/ 10.13039/501100011033, European Union NextGenerationEU/PRTR, Spanish Ministerio de Ciencia e Innovación under grants PID2019- 104714GB-C21, FPA2017-83946-C2-1-P, FIS2015-71688-ERC, PIE-201750I26, CERN policy in matters of scientific publications, the n_TOF Collaboration
Published: 2023

136. The Gaia-ESO survey: Placing constraints on the origin of r-process elements

Author: Van der Swaelmen, M., primary, Viscasillas Vázquez, C., additional, Cescutti, G., additional, Magrini, L., additional, Cristallo, S., additional, Vescovi, D., additional, Randich, S., additional, Tautvaišienė, G., additional, Bagdonas, V., additional, Bensby, T., additional, Bergemann, M., additional, Bragaglia, A., additional, Drazdauskas, A., additional, Jiménez-Esteban, F., additional, Guiglion, G., additional, Korn, A., additional, Masseron, T., additional, Minkeviiūtė, R., additional, Smiljanic, R., additional, Spina, L., additional, Stonkutė, E., additional, and Zaggia, S., additional
Published: 2023
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137. Characterization of a detector setup for the measurement of the 235U(n,f) cross section relative to n-p scattering up to 500 MeV at the n_TOF facility at CERN

Author: Manna, A., primary, Pirovano, E., additional, Colonna, N., additional, Castelluccio, D., additional, Console Camprini, P., additional, Cosentino, L., additional, Dietz, M., additional, Ducasse, Q., additional, Finocchiaro, P., additional, Le Naour, C., additional, Massimi, C., additional, Mengoni, A., additional, Nolte, R., additional, Tassan-Got, L., additional, Terranova, N., additional, Vannini, G., additional, Ventura, A., additional, Aberle, O., additional, Alcayne, V., additional, Amaducci, S., additional, Andrzejewski, J., additional, Audouin, L., additional, Babiano-Suarez, V., additional, Bacak, M., additional, Barbagallo, M., additional, Bennett, S., additional, Berthoumieux, E., additional, Billowes, J., additional, Bosnar, D., additional, Brown, A., additional, Busso, M., additional, Caamaño, M., additional, Caballero-Ontanaya, L., additional, Calviño, F., additional, Calviani, M., additional, Cano-Ott, D., additional, Casanovas, A., additional, Cerutti, F., additional, Chiaveri, E., additional, Cortés, G., additional, Cortés-Giraldo, M. A., additional, Cristallo, S., additional, Damone, L. A., additional, Davies, P. J., additional, Diakaki, M., additional, Domingo-Pardo, C., additional, Dressler, R., additional, Dupont, E., additional, Durán, I., additional, Eleme, Z., additional, Fernández-Domínguez, B., additional, Ferrari, A., additional, Göbel, K., additional, Garg, R., additional, Gawlik-Ramiega, R. A., additional, Gilardoni, S., additional, Gonçalves, I. F., additional, González-Romero, E., additional, Guerrero, C., additional, Gunsing, F., additional, Harada, H., additional, Heinitz, S., additional, Heyse, J., additional, Jenkins, D. G., additional, Junghans, A., additional, Käppeler, F., additional, Kadi, Y., additional, Kimura, A., additional, Knapová, I., additional, Kokkoris, M., additional, Krtička, M., additional, Kurtulgil, D., additional, Ladarescu, I., additional, Lederer-Woods, C., additional, Leeb, H., additional, Lerendegui-Marco, J., additional, Lonsdale, S. J., additional, Macina, D., additional, Martínez, T., additional, Masi, A., additional, Mastinu, P., additional, Mastromarco, M., additional, Maugeri, E. A., additional, Mazzone, A., additional, Mendoza, E., additional, Michalopoulou, V., additional, Milazzo, P. M., additional, Mingrone, F., additional, Moreno-Soto, J., additional, Musumarra, A., additional, Negret, A., additional, Ogállar, F., additional, Oprea, A., additional, Patronis, N., additional, Pavlik, A., additional, Perkowski, J., additional, Piersanti, L., additional, Petrone, C., additional, Porras, I., additional, Praena, J., additional, Quesada, J. M., additional, Ramos-Doval, D., additional, Rauscher, T., additional, Reifarth, R., additional, Rochman, D., additional, Rubbia, C., additional, Sabaté-Gilarte, M., additional, Saxena, A., additional, Schillebeeckx, P., additional, Schumann, D., additional, Sekhar, A., additional, Smith, A. G., additional, Sosnin, N. V., additional, Sprung, P., additional, Stamatopoulos, A., additional, Tagliente, G., additional, Tain, J. L., additional, Tarifeño-Saldivia, A., additional, Thomas, Th., additional, Torres-Sánchez, P., additional, Tsinganis, A., additional, Ulrich, J., additional, Urlass, S., additional, Valenta, S., additional, Variale, V., additional, Vaz, P., additional, Vescovi, D., additional, Vlachoudis, V., additional, Vlastou, R., additional, Wallner, A., additional, Woods, P. J., additional, Wright, T., additional, and Žugec, P., additional
Published: 2023
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138. Detector set up for the measurements of the neutron-induced fission cross section of 235U relative to n-p scattering up to 150 MeV at CERN-n_TOF

Author: Pirovano, E., primary, Manna, A., additional, Colonna, N., additional, Console Camprini, P., additional, Cosentino, L., additional, Dietz, M., additional, Ducasse, Q., additional, Finocchiaro, P., additional, Massimi, C., additional, Mengoni, A., additional, Nolte, R., additional, Radeck, D., additional, Tassan-Got, L., additional, Terranova, N., additional, Ventura, A., additional, Aberle, O., additional, Alcayne, V., additional, Amaducci, S., additional, Andrzejewski, J., additional, Audouin, L., additional, Babiano-Suarez, V., additional, Bacak, M., additional, Barbagallo, M., additional, Bennett, S., additional, Berthoumieux, E., additional, Billowes, J., additional, Bosnar, D., additional, Brown, A., additional, Busso, M., additional, Caamaño, M., additional, Caballero-Ontanaya, L., additional, Calviño, F., additional, Calviani, M., additional, Cano-Ott, D., additional, Casanovas, A., additional, Cerutti, F., additional, Chiaveri, E., additional, Cortés, G., additional, Cortés-Giraldo, M. A., additional, Cristallo, S., additional, Damone, L. A., additional, Davies, P. J., additional, Diakaki, M., additional, Domingo-Pardo, C., additional, Dressler, R., additional, Dupont, E., additional, Durán, I., additional, Eleme, Z., additional, Fernández-Domínguez, B., additional, Ferrari, A., additional, Göbel, K., additional, Garg, R., additional, Gawlik-Ramie˛ga, A., additional, Gilardoni, S., additional, Gonçalves, I. F., additional, González-Romero, E., additional, Guerrero, C., additional, Gunsing, F., additional, Harada, H., additional, Heinitz, S., additional, Heyse, J., additional, Jenkins, D. G., additional, Junghans, A., additional, Käppeler†, F., additional, Kadi, Y., additional, Kimura, A., additional, Knapová, I., additional, Kokkoris, M., additional, Krtička, M., additional, Kurtulgil, D., additional, Ladarescu, I., additional, Lederer-Woods, C., additional, Leeb, H., additional, Lerendegui-Marco, J., additional, Lonsdale, S. J., additional, Macina, D., additional, Martínez, T., additional, Masi, A., additional, Mastinu, P., additional, Mastromarco, M., additional, Maugeri, E. A., additional, Mazzone, A., additional, Mendoza, E., additional, Michalopoulou, V., additional, Milazzo, P. M., additional, Mingrone, F., additional, Moreno-Soto, J., additional, Musumarra, A., additional, Negret, A., additional, Ogállar, F., additional, Oprea, A., additional, Patronis, N., additional, Pavlik, A., additional, Perkowski, J., additional, Piersanti, L., additional, Petrone, C., additional, Porras, I., additional, Praena, J., additional, Quesada, J. M., additional, Ramos-Doval, D., additional, Rauscher, T., additional, Reifarth, R., additional, Rochman, D., additional, Rubbia, C., additional, Sabaté-Gilarte, M., additional, Saxena, A., additional, Schillebeeckx, P., additional, Schumann, D., additional, Sekhar, A., additional, Smith, A. G., additional, Sosnin, N. V., additional, Sprung, P., additional, Stamatopoulos, A., additional, Tagliente, G., additional, Tain, J. L., additional, Tarifeño-Saldivia, A., additional, Thomas, Th., additional, Torres-Sánchez, P., additional, Tsinganis, A., additional, Ulrich, J., additional, Urlass, S., additional, Valenta, S., additional, Vannini, G., additional, Variale, V., additional, Vaz, P., additional, Vescovi, D., additional, Vlachoudis, V., additional, Vlastou, R., additional, Wallner, A., additional, Woods, P. J., additional, Wright, T., additional, and Žugec, P., additional
Published: 2023
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139. Overview of the dissemination of n_TOF experimental data and resonance parameters

Author: Dupont, E., primary, Otuka, N., additional, Rochman, D., additional, Nogèure, G., additional, Aberle, O., additional, Alcayne, V., additional, Altieri, S., additional, Amaducci, S., additional, Andrzejewski, J., additional, Babiano-Suarez, V., additional, Bacak, M., additional, Balibrea, J., additional, Beltrami, C., additional, Bennett, S., additional, Bernardes, A.P., additional, Berthoumieux, E., additional, Beyer, R., additional, Boromiza, M., additional, Bosnar, D., additional, Caamaño, M., additional, Calviño, F., additional, Calviani, M., additional, Cano-Ott, D., additional, Casanovas, A., additional, Cerutti, F., additional, Cescutti, G., additional, Chiaveri, E., additional, Colombetti, P., additional, Colonna, N., additional, Console Camprini, P., additional, Cortés, G., additional, Cortés-Giraldo, M.A., additional, Cosentino, L., additional, Cristallo, S., additional, Dellmann, S., additional, Di Castro, M., additional, Di Maria, S., additional, Diakaki, M., additional, Dietz, M., additional, Domingo-Pardo, C., additional, Dressler, R., additional, Durán, I., additional, Eleme, Z., additional, Fargier, S., additional, Fernández, B., additional, Fernández-Domínguez, B., additional, Finocchiaro, P., additional, Fiore, S., additional, Furman, V., additional, García-Infantes, F., additional, Gawlik-Ramięga, A., additional, Gervino, G., additional, Gilardoni, S., additional, González-Romero, E., additional, Guerrero, C., additional, Gunsing, F., additional, Gustavino, C., additional, Heyse, J., additional, Hillman, W., additional, Jenkins, G.D., additional, Jericha, E., additional, Junghans, A., additional, Kadi, Y., additional, Kaperoni, K., additional, Kaur, G., additional, Kimura, A., additional, Knapová, I., additional, Kokkoris, M., additional, Kopatch, Y., additional, Krtička, M., additional, Kyritsis, N., additional, Ladarescu, I., additional, Lederer-Woods, C., additional, Lerendegui-Marco, J., additional, Lerner, G., additional, Manna, A., additional, Martínez, T., additional, Masi, A., additional, Massimi, C., additional, Mastinu, P., additional, Mastromarco, M., additional, Maugeri, E.A., additional, Mazzone, A., additional, Mendoza, E., additional, Mengoni, A., additional, Michalopoulou, V., additional, Milazzo, P.M., additional, Mucciola, R., additional, Murtas, F., additional, Musacchio-Gonzalez, E., additional, Musumarra, A., additional, Negret, A., additional, Pérez de Rada, A., additional, Pérez-Maroto, P., additional, Patronis, N., additional, Pavón-Rodrgíuez, J.A., additional, Pellegriti, M.G., additional, Perkowski, J., additional, Petrone, C., additional, Pirovano, E., additional, Plaza, J., additional, Pomp, S., additional, Porras, I., additional, Praena, J., additional, Quesada, J.M., additional, Reifarth, R., additional, Romanets, Y., additional, Rubbia, C., additional, Sánchez-Caballero, A., additional, Sabaté-Gilarte, M., additional, Schillebeeckx, P., additional, Schumann, D., additional, Sekhar, A., additional, Smith, A.G., additional, Sosnin, N.V., additional, Stamati, M.E., additional, Sturniolo, A., additional, Tagliente, G., additional, Tarifeño-Saldivia, A., additional, Taríro, D., additional, Torres-Sánchez, P., additional, Vagena, E., additional, Valenta, S., additional, Variale, V., additional, Vaz, P., additional, Vecchio, G., additional, Vescovi, D., additional, Vlachoudis, V., additional, Vlastou, R., additional, Wallner, A., additional, Woods, P.J., additional, Wright, T., additional, Zarrella, R., additional, and Žugec, P., additional
Published: 2023
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140. MINCE

Author: Cescutti, G., primary, Bonifacio, P., additional, Caffau, E., additional, Monaco, L., additional, Franchini, M., additional, Lombardo, L., additional, Matas Pinto, A. M., additional, Lucertini, F., additional, François, P., additional, Spitoni, E., additional, Lallement, R., additional, Sbordone, L., additional, Mucciarelli, A., additional, Spite, M., additional, Hansen, C. J., additional, Di Marcantonio, P., additional, Kučinskas, A., additional, Dobrovolskas, V., additional, Korn, A. J., additional, Valentini, M., additional, Magrini, L., additional, Cristallo, S., additional, and Matteucci, F., additional
Published: 2022
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141. First measurement of the $^{94}$Nb($n$,$\gamma$) cross section at the CERN n\_TOF facility

Author: Balibrea-Correa, J., Babiano-Suarez, V., Lerendegui-Marco, J., Domingo-Pardo, C., Ladarescu, I., Tarifeño-Saldivia, A., Alcayne, V., Cano-Ott, D., González-Romero, E., Martínez, T., Mendoza, E., Plaza, J., Sánchez-Caballero, A., Calviño, F., Casanovas, A., Guerrero, C., Heinitz, S., Köster, U., Maugeri, E.A., Dressler, R., Schumann, D., Mönch, I., Cristallo, S., Lederer-Woods, C., Aberle, O., Altieri, S., Amaducci, S., Andrzejewski, J., Bacak, M., Beltrami, C., Bennett, S., Bernardes, A.P., Berthoumieux, E., Boromiza, M., Bosnar, D., Caamaño, M., Calviani, M., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Colonna, N., Camprini, P. Console, Cortés, G., Cortés-Giraldo, M.A., Cosentino, L., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Dupont, E., Durán, I., Eleme, Z., Fargier, S., Fernández, B., Fernández-Domínguez, B., Finocchiaro, P., Fiore, S., Furman, V., García-Infantes, F., ˛ega, A. Gawlik-Rami, Gawlik-Ramięga, A., Gervino, G., Gilardoni, S., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D.G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapová, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Lerner, G., Manna, A., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Mazzone, A., Mengoni, A., Michalopoulou, V., Milazzo, P.M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Pérez, Pérez-Maroto, P., Patronis, N., Pavón-Rodríguez, J.A., Pellegriti, M.G., Perkowski, J., Petrone, C., Pirovano, E., Pomp, S., Porras, I., Praena, J., Quesada, J.M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sabaté-Gilarte, M., Schillebeeckx, P., Sekhar, A., Smith, A.G., Sosnin, N.V., Stamati, M.E., Sturniolo, A., Tagliente, G., Tarrío, D., Torres-Sánchez, P., Urlass, S., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, T., Woods, P.J., Wright, T., Zarrella, R., Žugec, P., Freeman, S., Lederer-Woods, C., Manna, A., and Mengoni, A.
Subjects: Subatomär fysik, Astronomi, astrofysik och kosmologi, neutron capture, 94Nb, n_TOF, neutron time of flight, Subatomic Physics, Astronomy, Astrophysics and Cosmology, Nuclear Physics - Experiment, General Medicine, Nuclear Experiment
Abstract: One of the crucial ingredients for the improvement of stellar models is the accurate knowledge of neutron capture cross-sections for the different isotopes involved in the s-,r- and i- processes. These measurements can shed light on existing discrepancies between observed and predicted isotopic abundances and help to constrain the physical conditions where these reactions take place along different stages of stellar evolution. In the particular case of the radioactive 94Nb, the 94Nb(n,γ) cross-section could play a role in the determination of the s-process production of 94Mo in AGB stars, which presently cannot be reproduced by state-of-the-art stellar models. There are no previous 94Nb(n,γ) experimental data for the resolved and unresolved resonance regions mainly due to the difficulties in producing highquality samples and also due to limitations in conventional detection systems commonly used in time-of-flight experiments. Motivated by this situation, a first measurement of the 94Nb(n,γ) reaction was carried out at CERN n_TOF, thereby exploiting the high luminosity of the EAR2 area in combination with a new detection system of small-volume C6D6-detectors and a high quality 94Nb-sample. The latter was based on hyper-pure 93Nb material activated at the high-flux reactor of ILL-Grenoble. An innovative ring-configuration detection system in close geometry around the capture sample allowed us to significantly enhance the signal-to-background ratio. This set-up was supplemented with two conventional C6D6-detectors and a highresolution LaCl3(Ce)-detector, which will be employed for addressing reliably systematic effects and uncertainties. At the current status of the data analysis, 18 resonance in 94Nb+n have been observed for the first time in the neutron energy range from thermal up to 10 keV., European Research Council (ERC), European Union’s Horizon 2020 research and innovation programme (ERC Consolidator Grant project HYMNS, with grant agreement No. 681740), ICJ220-045122-I, MCIN/AEI/ 10.13039/501100011033, European Union NextGenerationEU/PRTR, Spanish Ministerio de Ciencia e Innovación under grants PID2019-104714GB-C21, FPA2017-83946-C2-1-P, FIS2015-71688-ERC, CSIC, PIE-201750I26
Published: 2023

142. Measurement of the <math><mrow><mmultiscripts><mi>Se</mi><mprescripts/><none/><mn>77</mn></mmultiscripts><mo>(</mo><mi>n</mi><mo>,</mo><mi>γ</mi><mo>)</mo></mrow></math> cross section up to 200 keV at the n_TOF facility at CERN

Author: Sosnin, N V, Lederer-Woods, C, Krtička, M, Garg, R, Dietz, M, Bacak, M, Barbagallo, M, Battino, U, Cristallo, S, Damone, L A, Diakaki, M, Heinitz, S, Macina, D, Mastromarco, M, Mingrone, F, St J Murphy, A, Tagliente, G, Valenta, S, Vescovi, D, Aberle, O, Alcayne, V, Amaducci, S, Andrzejewski, J, Audouin, L, Bécares, V, Babiano-Suarez, V, Bečvář, F, Bellia, G, Berthoumieux, E, Billowes, J, Bosnar, D, Brown, A, Busso, M, Caamaño, M, Caballero, L, Calviño, F, Calviani, M, Cano-Ott, D, Casanovas, A, Cerutti, F, Chen, Y H, Chiaveri, E, Colonna, N, Cortés, G, Cortés-Giraldo, M A, Cosentino, L, Domingo-Pardo, C, Dressler, R, Dupont, E, Durán, I, Eleme, Z, Fernández-Domínguez, B, Ferrari, A, Finocchiaro, P, Göbel, K, Gawlik-Ramięga, A, Gilardoni, S, Glodariu, T, Gonçalves, I F, González-Romero, E, Guerrero, C, Gunsing, F, Harada, H, Heyse, J, Jenkins, D G, Jericha, E, Käppeler, F, Kadi, Y, Kimura, A, Kivel, N, Kokkoris, M, Kurtulgil, D, Ladarescu, I, Leeb, H, Lerendegui-Marco, J, Meo, S Lo, Lonsdale, S J, Manna, A, Martínez, T, Masi, A, Massimi, C, Mastinu, P, Matteucci, F, Maugeri, E A, Mazzone, A, Mendoza, E, Mengoni, A, Michalopoulou, V, Milazzo, P M, Musumarra, A, Negret, A, Nolte, R, Ogállar, F, Oprea, A, Patronis, N, Pavlik, A, Perkowski, J, Piersanti, L, Porras, I, Praena, J, Quesada, J M, Radeck, D, Ramos-Doval, D, Rauscher, T, Reifarth, R, Rochman, D, Rubbia, C, Sabaté-Gilarte, M, Saxena, A, Schillebeeckx, P, Schumann, D, Smith, A G, Stamatopoulos, A, Tain, J L, Talip, T, Tarifeño-Saldivia, A, Tassan-Got, L, Torres-Sánchez, P, Tsinganis, A, Ulrich, J, Urlass, S, Vannini, G, Variale, V, Vaz, P, Ventura, A, Vlachoudis, V, Vlastou, R, Wallner, A, Woods, P J, Wright, T, Žugec, P, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and n_TOF
Subjects: Nuclear Physics - Experiment, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex]
Abstract: International audience; The Se77(n,γ) reaction is of importance for Se77 abundance during the slow neutron capture process in massive stars. We have performed a new measurement of the Se77 radiative neutron capture cross section at the Neutron Time-of-Flight facility at CERN. Resonance capture kernels were derived up to 51 keV and cross sections up to 200 keV. Maxwellian-averaged cross sections were calculated for stellar temperatures between kT=5keV and kT=100keV, with uncertainties between 4.2% and 5.7%. Our results lead to substantial decreases of 14% and 19% in Se77 abundances produced through the slow neutron capture process in selected stellar models of 15M⊙ and 2M⊙, respectively, compared to using previous recommendation of the cross section.
Published: 2023

143. Measurement of the 160Gd(n, γ) cross section at n_TOF and its medical implications.

Author: Mastromarco, M., Manna, A., García-Infantes, F., Amaducci, S., Mengoni, A., Massimi, C., Tagliente, G., Cristallo, S., Aberle, O., Alcayne, V., Altieri, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Bernardes, A. P., Berthoumieux, E., and Beyer, R.
Subjects: NUCLEAR cross sections, TIME-of-flight measurements, NEUTRON capture, GADOLINIUM isotopes, NUCLEOSYNTHESIS
Abstract: Neutron-capture reactions on gadolinium isotopes play an important role in several fields of physics,in particular in nuclear Astrophysics for the understanding of the nucleosynthesis of heavy elements (beyond iron) in stars via the s- and r-processes [1] and in nuclear technology. Another important application of gadolinium is linked to the production of terbium, that offers a set of clinically interesting isotopes for theranostics, characterized by complementary physical decay characteristics. In particular, the low-energy β −emitter terbium-161 is very similar to lutetium-177 in terms of half-life (6.89 d), β − energy and chemical properties. Being a significant emitter of conversion/Auger electrons, greater therapeutic effect can therefore be expected in comparison to Lu-177 [2, 3]. For this reason, in the last decade, the study of the neutron capture reaction 160Gd(n,γ)161 Gd and the subsequent β − decay in terbium-161 is getting particular attention. As the nuclear data on the Gd-160 neutron capture reaction are quite scarce and inconsistent, a new measurement of the capture cross section of Gd-160 at the CERN neutron Time-Of-Flight facilty was performed in order to provide high resolution, high-accuracy data on this important reaction, in the energy range from thermal to hundreds of keV. In this contribution, the preliminary results of the n_TOF measurement are presented. [ABSTRACT FROM AUTHOR]
Published: 2023
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144. Zr 92 (n,g) and (n,tot) measurements at the GELINA and n_TOF facilities

Author: Tagliente G., Kopecky S., Heyse J., Krticka M., Massimi C., Mengoni A., Milazzo P. M., Plompen A. J. M., Schillebeeckx P., Valenta S., Wynants R., Altstadt S., Andrzejewski J., Audouin L., Becares V., Barbagallo M., Becvar F., Belloni F., Berthoumieux E., Billowes J., Boccone V., Bosnar D., Brugger M., Calvino F., Calviani M., Cano-Ott D., Carrapico C., Cerutti F., Chiaveri E., Chin M., Colonna N., Cortes G., Cortes-Giraldo M. A., Cristallo S., Diakaki M., Domingo-Pardo C., Dressler R., Duran I., Eleftheriadis C., Ferrari A., Fraval K., Furman V., Gobel K., Gomez-Hornillos M. B., Ganesan S., Garcia A. R., Giubrone G., Goncalves I. F., Gonzalez-Romero E., Goverdovski A., Griesmayer E., Guerrero C., Gunsing F., Heftrich T., Hernandez-Prieto A., Jericha E., Kappeler F., Kadi Y., Karadimos D., Katabuchi T., Ketlerov V., Khryachkov V., Kivel N., Kokkoris M., Kroll J., Lampoudis C., Langer C., Leal-Cidoncha E., Lederer C., Leeb H., Leong L. S., Losito R., Lugaro M., Mallick A., Manousos A., Marganiec J., Martinez T., Mastinu P., Mastromarco M., Mendoza E., Mingrone F., Mirea M., Paradela C., Pavlik A., Perkowski J., Praena J., Quesada J. M., Rauscher T., Reifarth R., Riego-Perez A., Robles M., Rubbia C., Ryan J. A., Sabate-Gilarte M., Sarmento R., Saxena A., Schmidt S., Schumann D., Sedyshev P., Tain J. L., Tarifeno-Saldivia A., Tarrio D., Tassan-Got L., Tsinganis A., Vannini G., Variale V., Vaz P., Ventura A., Vermeulen M. J., Vescovi D., Vlachoudis V., Vlastou R., Wallner A., Ware T., Weigand M., Weiss C., Wright T., Zugec P., Tagliente G., Kopecky S., Heyse J., Krticka M., Massimi C., Mengoni A., Milazzo P.M., Plompen A.J.M., Schillebeeckx P., Valenta S., Wynants R., Altstadt S., Andrzejewski J., Audouin L., Becares V., Barbagallo M., Becvar F., Belloni F., Berthoumieux E., Billowes J., Boccone V., Bosnar D., Brugger M., Calvino F., Calviani M., Cano-Ott D., Carrapico C., Cerutti F., Chiaveri E., Chin M., Colonna N., Cortes G., Cortes-Giraldo M.A., Cristallo S., Diakaki M., Domingo-Pardo C., Dressler R., Duran I., Eleftheriadis C., Ferrari A., Fraval K., Furman V., Gobel K., Gomez-Hornillos M.B., Ganesan S., Garcia A.R., Giubrone G., Goncalves I.F., Gonzalez-Romero E., Goverdovski A., Griesmayer E., Guerrero C., Gunsing F., Heftrich T., Hernandez-Prieto A., Jericha E., Kappeler F., Kadi Y., Karadimos D., Katabuchi T., Ketlerov V., Khryachkov V., Kivel N., Kokkoris M., Kroll J., Lampoudis C., Langer C., Leal-Cidoncha E., Lederer C., Leeb H., Leong L.S., Losito R., Lugaro M., Mallick A., Manousos A., Marganiec J., Martinez T., Mastinu P., Mastromarco M., Mendoza E., Mingrone F., Mirea M., Paradela C., Pavlik A., Perkowski J., Praena J., Quesada J.M., Rauscher T., Reifarth R., Riego-Perez A., Robles M., Rubbia C., Ryan J.A., Sabate-Gilarte M., Sarmento R., Saxena A., Schmidt S., Schumann D., Sedyshev P., Tain J.L., Tarifeno-Saldivia A., Tarrio D., Tassan-Got L., Tsinganis A., Vannini G., Variale V., Vaz P., Ventura A., Vermeulen M.J., Vescovi D., Vlachoudis V., Vlastou R., Wallner A., Ware T., Weigand M., Weiss C., Wright T., and Zugec P.
Subjects: n_TOF, s process, Zr
Published: 2022

145. AGB Stars: Nucleosynthesis and Open Problems

Author: Domínguez, I., Abia, C., Cristallo, S., Laverny, P. de, Straniero, O., Figueras, Francesca, editor, Girart, Josep Miquel, editor, Hernanz, Margarita, editor, and Jordi, Carme, editor
Published: 2007
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146. Destruction of the cosmic γ -ray emitter Al 26 in massive stars: Study of the key Al 26 (n,p) reaction

Author: Lederer-Woods, C., Woods, P. J., Davinson, T., Kahl, D., Lonsdale, S. J., Aberle, O., Amaducci, S., Andrzejewski, J., Audouin, L., Bacak, M., Balibrea, J., Barbagallo, M., Bečvář, F., Berthoumieux, E., Billowes, J., Bosnar, D., Brown, A., Caamaño, M., Calviño, F., Calviani, M., Cano-Ott, D., Cardella, R., Casanovas, A., Cerutti, F., Chen, Y. H., Chiaveri, E., Colonna, N., Cortés, G., Cortés-Giraldo, M. A., Cosentino, L., Cristallo, S., Damone, L. A., Diakaki, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Durán, I., Fernández-Domínguez, B., Ferrari, A., Ferreira, P., Ferrer, F. J., Finocchiaro, P., Furman, V., Göbel, K., García, A. R., Gawlik, A., Gilardoni, S., Glodariu, T., Gonçalves, I. F., González-Romero, E., Griesmayer, E., Guerrero, C., Gunsing, F., Harada, H., Heinitz, S., Heyse, J., Jenkins, D. G., Jericha, E., Käppeler, F., Kadi, Y., Kalamara, A., Kavrigin, P., Kimura, A., Kivel, N., Kokkoris, M., Krtička, M., Kurtulgil, D., Leal-Cidoncha, E., Leeb, H., Lerendegui-Marco, J., Lo Meo, S., Macina, D., Manna, A., Marganiec, J., Martínez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Milazzo, P. M., Mingrone, F., Musumarra, A., Negret, A., Nolte, R., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Porras, I., Praena, J., Quesada, J. M., Radeck, D., Rauscher, T., Reifarth, R., Rubbia, C., Ryan, J. A., Sabaté-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Sedyshev, P., Smith, A. G., Sosnin, N. V., Stamatopoulos, A., Tagliente, G., Tain, J. L., Tarifeño-Saldivia, A., Tassan-Got, L., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Wallner, A., Warren, S., Weiss, C., Wright, T., Žugec, P., Lederer-Woods C., Woods P.J., Davinson T., Kahl D., Lonsdale S.J., Aberle O., Amaducci S., Andrzejewski J., Audouin L., Bacak M., Balibrea J., Barbagallo M., Becvar F., Berthoumieux E., Billowes J., Bosnar D., Brown A., Caamano M., Calvino F., Calviani M., Cano-Ott D., Cardella R., Casanovas A., Cerutti F., Chen Y.H., Chiaveri E., Colonna N., Cortes G., Cortes-Giraldo M.A., Cosentino L., Cristallo S., Damone L.A., Diakaki M., Domingo-Pardo C., Dressler R., Dupont E., Duran I., Fernandez-Dominguez B., Ferrari A., Ferreira P., Ferrer F.J., Finocchiaro P., Furman V., Gobel K., Garcia A.R., Gawlik A., Gilardoni S., Glodariu T., Goncalves I.F., Gonzalez-Romero E., Griesmayer E., Guerrero C., Gunsing F., Harada H., Heinitz S., Heyse J., Jenkins D.G., Jericha E., Kappeler F., Kadi Y., Kalamara A., Kavrigin P., Kimura A., Kivel N., Kokkoris M., Krticka M., Kurtulgil D., Leal-Cidoncha E., Leeb H., Lerendegui-Marco J., Lo Meo S., Macina D., Manna A., Marganiec J., Martinez T., Masi A., Massimi C., Mastinu P., Mastromarco M., Maugeri E.A., Mazzone A., Mendoza E., Mengoni A., Milazzo P.M., Mingrone F., Musumarra A., Negret A., Nolte R., Oprea A., Patronis N., Pavlik A., Perkowski J., Porras I., Praena J., Quesada J.M., Radeck D., Rauscher T., Reifarth R., Rubbia C., Ryan J.A., Sabate-Gilarte M., Saxena A., Schillebeeckx P., Schumann D., Sedyshev P., Smith A.G., Sosnin N.V., Stamatopoulos A., Tagliente G., Tain J.L., Tarifeno-Saldivia A., Tassan-Got L., Valenta S., Vannini G., Variale V., Vaz P., Ventura A., Vlachoudis V., Vlastou R., Wallner A., Warren S., Weiss C., Wright T., Zugec P., Lederer-Woods, C., Woods, P. J., Davinson, T., Kahl, D., Lonsdale, S. J., Aberle, O., Amaducci, S., Andrzejewski, J., Audouin, L., Bacak, M., Balibrea, J., Barbagallo, M., Becvar, F., Berthoumieux, E., Billowes, J., Bosnar, D., Brown, A., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Cardella, R., Casanovas, A., Cerutti, F., Chen, Y. H., Chiaveri, E., Colonna, N., Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Damone, L. A., Diakaki, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Fernandez-Dominguez, B., Ferrari, A., Ferreira, P., Ferrer, F. J., Finocchiaro, P., Furman, V., Gobel, K., Garcia, A. R., Gawlik, A., Gilardoni, S., Glodariu, T., Goncalves, I. F., Gonzalez-Romero, E., Griesmayer, E., Guerrero, C., Gunsing, F., Harada, H., Heinitz, S., Heyse, J., Jenkins, D. G., Jericha, E., Kappeler, F., Kadi, Y., Kalamara, A., Kavrigin, P., Kimura, A., Kivel, N., Kokkoris, M., Krticka, M., Kurtulgil, D., Leal-Cidoncha, E., Leeb, H., Lerendegui-Marco, J., Lo Meo, S., Macina, D., Manna, A., Marganiec, J., Martinez, T., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Milazzo, P. M., Mingrone, F., Musumarra, A., Negret, A., Nolte, R., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Porras, I., Praena, J., Quesada, J. M., Radeck, D., Rauscher, T., Reifarth, R., Rubbia, C., Ryan, J. A., Sabate-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Sedyshev, P., Smith, A. G., Sosnin, N. V., Stamatopoulos, A., Tagliente, G., Tain, J. L., Tarifeno-Saldivia, A., Tassan-Got, L., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Wallner, A., Warren, S., Weiss, C., Wright, T., and Zugec, P.
Subjects: al emitter, TOF, nucleosynthesis, ntof,cern,tof, al emitter
Abstract: The Al26(n,p)Mg26 reaction is the key reaction impacting on the abundances of the cosmic γ-ray emitter Al26 produced in massive stars and impacts on the potential pollution of the early solar system with Al26 by asymptotic giant branch stars. We performed a measurement of the Al26(n,p)Mg26 cross section at the high-flux beam line EAR-2 at the n_TOF facility (CERN). We report resonance strengths for eleven resonances, nine being measured for the first time, while there is only one previous measurement for the other two. Our resonance strengths are significantly lower than the only previous values available. Our cross-section data range to 150 keV neutron energy, which is sufficient for a reliable determination of astrophysical reactivities up to 0.5 GK stellar temperature.
Published: 2021

147. MINCE I. Presentation of the project and of the first year sample

Author: Cescutti, G., Bonifacio, P., Caffau, E., Monaco, L., Franchini, M., Lombardo, L., Pinto, A. M. Matas, Lucertini, F., Francois, P., Spitoni, E., Lallement, R., Sbordone, L., Mucciarelli, A., Spite, M., Hansen, C. J., Di Marcantonio, P., Kucinskas, A., Dobrovolskas, V., Korn, Andreas J., Valentini, M., Magrini, L., Cristallo, S., Matteucci, F., Cescutti, G., Bonifacio, P., Caffau, E., Monaco, L., Franchini, M., Lombardo, L., Pinto, A. M. Matas, Lucertini, F., Francois, P., Spitoni, E., Lallement, R., Sbordone, L., Mucciarelli, A., Spite, M., Hansen, C. J., Di Marcantonio, P., Kucinskas, A., Dobrovolskas, V., Korn, Andreas J., Valentini, M., Magrini, L., Cristallo, S., and Matteucci, F.
Abstract: Context. In recent years, Galactic archaeology has become a particularly vibrant field of astronomy, with its main focus set on the oldest stars of our Galaxy. In most cases, these stars have been identified as the most metal-poor. However, the struggle to find these ancient fossils has produced an important bias in the observations - in particular, the intermediate metal-poor stars (-2.5 < [Fe/H] < -1.5) have been frequently overlooked. The missing information has consequences for the precise study of the chemical enrichment of our Galaxy, in particular for what concerns neutron capture elements and it will be only partially covered by future multi object spectroscopic surveys such as WEAVE and 4MOST.Aims. Measuring at Intermediate Metallicity Neutron Capture Elements (MINCE) is gathering the first high-quality spectra (high signal-to-noise ratio, S/N, and high resolution) for several hundreds of bright and metal-poor stars, mainly located in our Galactic halo.Methods. We compiled our selection mainly on the basis of Gaia data and determined the stellar atmospheres of our sample and the chemical abundances of each star.Results. In this paper, we present the first sample of 59 spectra of 46 stars. We measured the radial velocities and computed the Galactic orbits for all stars. We found that 8 stars belong to the thin disc, 15 to disrupted satellites, and the remaining cannot be associated to the mentioned structures, and we call them halo stars. For 33 of these stars, we provide abundances for the elements up to zinc. We also show the chemical evolution results for eleven chemical elements, based on recent models.Conclusions. Our observational strategy of using multiple telescopes and spectrographs to acquire high S/N and high-resolution spectra for intermediate-metallicity stars has proven to be very efficient, since the present sample was acquired over only about one year of observations. Finally, our target selection strategy, after an initial adjustment
Published: 2022
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148. The CERN n TOF NEAR station for astrophysics- and application-related neutron activation measurements

Author: Patronis, N., Mengoni, A., Colonna, N., Cecchetto, M., Domingo-Pardo, C., Aberle, O., Lerendegui-Marco, J., Gervino, G., Stamati, M. E., Goula, S., Bernardes, A. P., Mastromarco, M., Manna, A., Vlastou, R., Massimi, C., Calviani, M., Alcayne, V., Altieri, S., Amaducci, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Berthoumieux, E., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerner, G., Martınez, T., Masi, A., Mastinu, P., Maugeri, E. A., Mazzone, A., Mendoza, E., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Pavon-Rodrıguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, S., Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Sturniolo, A., Tagliente, G., Tarrio, D., Torres-Sanchez, P., Urlass, S., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Wallner, T., Woods, P. J., Wright, T., Zarrella, R., Zugec, P., Patronis, N., Mengoni, A., Colonna, N., Cecchetto, M., Domingo-Pardo, C., Aberle, O., Lerendegui-Marco, J., Gervino, G., Stamati, M. E., Goula, S., Bernardes, A. P., Mastromarco, M., Manna, A., Vlastou, R., Massimi, C., Calviani, M., Alcayne, V., Altieri, S., Amaducci, S., Andrzejewski, J., Babiano-Suarez, V., Bacak, M., Balibrea, J., Beltrami, C., Bennett, S., Berthoumieux, E., Boromiza, M., Bosnar, D., Caamano, M., Calvino, F., Cano-Ott, D., Casanovas, A., Cerutti, F., Cescutti, G., Chasapoglou, S., Chiaveri, E., Colombetti, P., Camprini, P. Console, Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Dellmann, S., Di Castro, M., Di Maria, S., Diakaki, M., Dietz, M., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fargier, S., Fernandez, B., Fernandez-Dominguez, B., Finocchiaro, P., Fiore, S., Furman, V., Garcia-Infantes, F., Gawlik-Ramiega, A., Gilardoni, S., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Gustavino, C., Heyse, J., Hillman, W., Jenkins, D. G., Jericha, E., Junghans, A., Kadi, Y., Kaperoni, K., Kaur, G., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kyritsis, N., Ladarescu, I., Lederer-Woods, C., Lerner, G., Martınez, T., Masi, A., Mastinu, P., Maugeri, E. A., Mazzone, A., Mendoza, E., Milazzo, P. M., Mucciola, R., Murtas, F., Musacchio-Gonzalez, E., Musumarra, A., Negret, A., de Rada, A. Perez, Perez-Maroto, P., Pavon-Rodrıguez, J. A., Pellegriti, M. G., Perkowski, J., Petrone, C., Pirovano, E., Plaza, J., Pomp, S., Porras, I., Praena, J., Quesada, J. M., Reifarth, R., Rochman, D., Romanets, Y., Rubbia, C., Sanchez, A., Sabate-Gilarte, M., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N. V., Sturniolo, A., Tagliente, G., Tarrio, D., Torres-Sanchez, P., Urlass, S., Vagena, E., Valenta, S., Variale, V., Vaz, P., Vecchio, G., Vescovi, D., Vlachoudis, V., Wallner, T., Woods, P. J., Wright, T., Zarrella, R., and Zugec, P.
Abstract: A new experimental area, the NEAR station, has recently been built at the CERN n TOF facility, at a short distance from the spallation target (1.5 m). The new area, characterized by a neutron beam of very high flux, has been designed with the purpose of performing activation measurements of interest for astrophysics and various applications. The beam is transported from the spallation target to the NEAR station through a hole in the shielding wall of the target, inside which a collimator is inserted. The new area is complemented with a {\gamma}-ray spectroscopy laboratory, the GEAR station, equipped with a high efficiency HPGe detector, for the measurement of the activity resulting from irradiation of a sample in the NEAR station. The use of a moderator/filter assembly is envisaged, in order to produce a neutron beam of Maxwellian shape at different thermal energies, necessary for the measurement of Maxwellian Averaged Cross Sections of astrophysical interest. A new fast-cycling activation technique is also being investigated, for measurements of reactions leading to isotopes of very short half life.
Published: 2022

149. The Gaia-ESO survey: placing constraints on the origin of r-process elements

Author: Van der Swaelmen, M., Vázquez, C. Viscasillas, Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaišienė, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jiménez-Esteban, F., Guiglion, G., Korn, A., Masseron, T., Minkevičiūtė, R., Smiljanic, R., Spina, L., Stonkutė, E., Zaggia, S., Van der Swaelmen, M., Vázquez, C. Viscasillas, Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaišienė, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jiménez-Esteban, F., Guiglion, G., Korn, A., Masseron, T., Minkevičiūtė, R., Smiljanic, R., Spina, L., Stonkutė, E., and Zaggia, S.
Abstract: A renewed interest about the origin of \emph{r}-process elements has been stimulated by the multi-messenger observation of the gravitational event GW170817, with the detection of both gravitational waves and electromagnetic waves corresponding to the merger of two neutron stars. Such phenomenon has been proposed as one of the main sources of the \emph{r}-process. However, the origin of the \emph{r}-process elements at different metallicities is still under debate. We aim at investigating the origin of the \emph{r}-process elements in the Galactic thin disc population. From the sixth internal data release of the \emph{Gaia}-ESO we have collected a large sample of Milky Way thin- and thick-disc stars for which abundances of Eu, O, and Mg are available. The sample consists of members of 62 open clusters, located at a Galactocentric radius from $\sim 5$ kpc to $\sim 20$ kpc in the disc, in the metallicity range $[-0.5, 0.4]$ and covering an age interval from 0.1 to 7 Gy, and about 1300 Milky Way disc field stars in the metallicity range $[-1.5, 0.5]$. We compare the observations with the results of a chemical evolution model, in which we varied the nucleosynthesis sources for the three considered elements. Our main result is that Eu in the thin disc is predominantly produced by sources with short lifetimes, such as magneto-rotationally driven SNe. There is no strong evidence for additional sources at delayed times. Our findings do not imply that there cannot be a contribution from mergers of neutron stars in other environments, as in the halo or in dwarf spheroidal galaxies, but such a contribution is not needed to explain Eu abundances at thin disc metallicities., Comment: 20 pages, accepted for publication in A&A
Published: 2022
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150. Bottom-up dust nucleation theory in oxygen-rich evolved stars: I. Aluminum oxide clusters

Author: Gobrecht, D, Plane, JMC, Bromley, ST, Decin, L, Cristallo, S, and Sekaran, S
Abstract: Context. Aluminium oxide (alumina; Al2O3) is a promising candidate as a primary dust condensate in the atmospheres of oxygen-rich evolved stars. Therefore, alumina ‘seed’ particles might trigger the onset of stellar dust formation and of stellar mass loss in the wind. However, the formation of alumina dust grains is not well understood. Aims. We aim to shed light on the initial steps of cosmic dust formation (i.e. nucleation) in oxygen-rich environments via a quantum-chemical bottom-up approach. Methods. Starting with an elemental gas-phase composition, we construct a detailed chemical-kinetic network that describes the formation and destruction of aluminium-bearing molecules and dust-forming (Al2O3)n clusters up to the size of dimers (n = 2) coagulating to tetramers (n = 4). Intermediary species include the prevalent gas-phase molecules AlO and AlOH as well as AlxOy clusters with x = 1–5, y = 1–6. The resulting extensive network is applied to two model stars, which represent a semi-regular variable and a Mira type, and to different circumstellar gas trajectories, including a non-pulsating outflow and a pulsating model. The growth of larger-sized (Al2O3)n clusters with n = 4–10 is described by the temperature-dependent Gibbs free energies of the most favourable structures (i.e. the global minima clusters) as derived from global optimisation techniques and calculated via density functional theory. We provide energies, bond characteristics, electrostatic properties, and vibrational spectra of the clusters as a function of size, n, and compare these to corundum, which corresponds to the crystalline bulk limit (n →∞). Results. The circumstellar aluminium gas-phase chemistry in oxygen-rich giants is primarily controlled by AlOH and AlO, which are tightly coupled by the reactions AlO+H2, AlO+H2O, and their reverse. Models of semi-regular variables show comparatively higher AlO abundances, as well as a later onset and a lower efficiency of alumina cluster formation when compared to Mira-like models. The Mira-like models exhibit an efficient cluster production that accounts for more than 90% of the available aluminium content, which is in agreement with the most recent ALMA observations. Chemical equilibrium calculations fail to predict both the alumina cluster formation and the abundance trends of AlO and AlOH in the asymptotic giant branch dust formation zone. Furthermore, we report the discovery of hitherto unreported global minimum candidates and low-energy isomers for cluster sizes n = 7, 9, and 10. A homogeneous nucleation scenario, where Al2O3 monomers are successively added, is energetically viable. However, the formation of the Al2O3 monomer itself represents an energetic bottleneck. Therefore, we provide a bottom-up interpolation of the cluster characteristics towards the bulk limit by excluding the monomer, approximately following an n−1∕3 dependence.
Published: 2022

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