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6,215 results on '"Wolf. C."'

1. Radiative neutron capture cross section of $^{242}$Pu measured at n_TOF-EAR1 in the unresolved resonance region up to 600 keV

Author

Lerendegui-Marco, J., Guerrero, C., Mendoza, E., Quesada, J. M., Eberhardt, K., Junghans, A. R., Alcayne, V., Babiano, V., Aberle, O., Andrzejewski, J., Audouin, L., Becares, V., Bacak, M., Balibrea-Correa, J., Barbagallo, M., Barros, S., Becvar, F., Beinrucker, C., Berthoumieux, E., Billowes, J., Bosnar, D., Brugger, M., Caamaño, M., Calviño, F., Calviani, M., Cano-Ott, D., Cardella, R., Casanovas, A., Castelluccio, D. M., Cerutti, F., Chen, Y. H., Chiaveri, E., Colonna, N., Cortés, G., Cortés-Giraldo, M. A., Cosentino, L., Damone, L. A., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Durán, I., Fernández-Domínguez, B., Ferrari, A., Ferreira, P., Finocchiaro, P., Furman, V., Göbel, K., García, A. R., Gawlik, A., Glodariu, T., Goncalves, I. F., González-Romero, E., Goverdovski, A., Griesmayer, E., Gunsing, F., Harada, H., Heftrich, T., Heinitz, S., Heyse, J., Jenkins, D. G., Jericha, E., Käppeler, F., Kadi, Y., Katabuchi, T., Kavrigin, P., Ketlerov, V., Khryachkov, V., Kimura, A., Kivel, N., Kokkoris, M., Krticka, M., Leal-Cidoncha, E., Lederer-Woods, C., Leeb, H., Meo, S. Lo, Lonsdale, S. J., Losito, R., Macina, D., Marganiec, J., Martínez, T., Massimi, C., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mengoni, A., Milazzo, P. M., Mingrone, F., Mirea, M., Montesano, S., Musumarra, A., Nolte, R., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Porras, J. I., Praena, J., Rajeev, K., Rauscher, T., Reifarth, R., Riego-Perez, A., Rout, P. C., Rubbia, C., Ryan, J. A., Sabaté-Gilarte, M., Saxena, A., Schillebeeckx, P., Schmidt, S., Schumann, D., Sedyshev, P., Smith, A. G., Stamatopoulos, A., Tagliente, G., Tain, J. L., Tarifeño-Saldivia, A., Tassan-Got, L., Tsinganis, A., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Wallner, A., Warren, S., Weigand, M., Weiss, C., Wolf, C., Woods, P. J., Wright, T., Zugec, P., and Collaboration, the n_TOF

Subjects
Nuclear Experiment
Abstract

The design of fast reactors burning MOX fuels requires accurate capture and fission cross sections. For the particular case of neutron capture on 242Pu, the NEA recommends that an accuracy of 8-12% should be achieved in the fast energy region (2 keV-500 keV) compared to their estimation of 35% for the current uncertainty. Integral irradiation experiments suggest that the evaluated cross section of the JEFF-3.1 library overestimates the 242Pu(n,{\gamma}) cross section by 14% in the range between 1 keV and 1 MeV. In addition, the last measurement at LANSCE reported a systematic reduction of 20-30% in the 1-40 keV range relative to the evaluated libraries and previous data sets. In the present work this cross section has been determined up to 600 keV in order to solve the mentioned discrepancies. A 242Pu target of 95(4) mg enriched to 99.959% was irradiated at the n TOF-EAR1 facility at CERN. The capture cross section of 242Pu has been obtained between 1 and 600 keV with a systematic uncertainty (dominated by background subtraction) between 8 and 12%, reducing the current uncertainties of 35% and achieving the accuracy requested by the NEA in a large energy range. The shape of the cross section has been analyzed in terms of average resonance parameters using the FITACS code as implemented in SAMMY, yielding results compatible with our recent analysis of the resolved resonance region.The results are in good agreement with the data of Wisshak and K\"appeler and on average 10-14% below JEFF-3.2 from 1 to 250 keV, which helps to achieve consistency between integral experiments and cross section data. At higher energies our results show a reasonable agreement within uncertainties with both ENDF/B-VII.1 and JEFF-3.2. Our results indicate that the last experiment from DANCE underestimates the capture cross section of 242Pu by as much as 40% above a few keV., Comment: 20 pages, 19 figures, submitted to Phys. Rev. C

Published
2024

2. A new way to find symbiotic stars: accretion disc detection with optical survey photometry

Author

Lucy, A. B., Sokoloski, J. L., Luna, G. J. M., Mukai, K., Nuñez, N. E., Buckley, D. A. H., Breytenbach, H., Paul, B., Potter, S. B., Manick, R., Howell, D. A., Wolf, C., and Onken, C. A.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Symbiotic stars are binaries in which a cool and evolved star of luminosity class I-III accretes onto a smaller companion. However, direct accretion signatures like disc flickering and boundary layer X-rays are typically outshone or suppressed by the luminous giant, shell burning on the accreting white dwarf, and the illuminated wind nebula. We present a new way to find symbiotics that is less biased against directly-detectable accretion discs than methods based on narrow-band H$\alpha$ photometry or objective prism plate surveys. We identified outliers in SkyMapper survey photometry, using reconstructed uvg snapshot colours and rapid variability among the three exposures of each 20-minute SkyMapper Main Survey filter sequence, from a sample of 366,721 luminous red objects. We found that SkyMapper catalog colours of large-amplitude pulsating giants must be corrected for variability, and that flickering is detectable with only three data points. Our methods probed a different region of parameter space than a recent search for accreting-only symbiotics in the GALAH survey, while being surprisingly concordant with another survey's infrared detection algorithm. We discovered 12 new symbiotics, including four with optical accretion disc flickering. Two of the optical flickerers exhibited boundary-layer hard X-rays. We also identified 10 symbiotic candidates, and discovered likely optical flickering in the known symbiotic V1044 Cen (CD-36 8436). We conclude that at least 20% of the true population of symbiotics exhibit detectable optical flickering from the inner accretion disc, the majority of which do not meet the H$\alpha$ detection thresholds used to find symbiotics in typical narrow-band surveys., Comment: Submitted to MNRAS. 34 pages, 17 figures (from 20 image files), 5 tables. Centered on A4 paper

Published
2024

3. Timescales of Quasar Accretion Discs from Low to High Black Hole Masses and new Variability Structure Functions at the High Masses

Author

Wolf, C., Lai, S., Tang, J. -J., and Tonry, J.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The UV-optical variability of quasars appears to depend on black-hole mass $M_{\rm BH}$ through physical timescales in the accretion disc. Here, we calculate mean emission radii, $R_{\rm mean}$, and orbital timescales, $t_{\rm orb}$, of thin accretion disc models as a function of emission wavelength from 1000 to 10000 Angstrom, $M_{\rm BH}$ from $10^6$ to $10^{11}$ solar masses, and Eddington ratios from 0.01 to 1. At low $M_{\rm BH}$, we find the textbook behaviour of $t_{\rm orb}\propto M_{\rm BH}^{-1/2}$ alongside $R_{\rm mean} \approx$ const, while towards higher masses the growing event horizon imposes $R_{\rm mean} \propto M_{\rm BH}$ and thus a turnover into $t_{\rm orb}\propto M_{\rm BH}$. We fit smoothly broken power laws to the numerical results and provide analytic convenience functions for $R_{\rm mean}(\lambda,M_{\rm BH},L_{3000})$ and $t_{\rm orb}(\lambda,M_{\rm BH},L_{3000})$ in terms of the observables $\lambda$, $M_{\rm BH}$, and the monochromatic luminosity $L_{3000}$. We then calculate variability structure functions for the ~2200 brightest quasars in the sky with estimates for $M_{\rm BH}$ and $L_{3000}$, using lightcurves from NASA/ATLAS orange passband spanning more than 7 years. The median luminosity of the accretion disc sample is $\log L_{\rm bol}/(\mathrm{erg\,s}^{-1})\approx 47$ and the median $\log M_{\rm BH}/M_\odot\approx 9.35$. At this high mass, the theoretical mass dependence of disc timescales levels off and turns over. The data show a weak dependence of variability on $M_{\rm BH}$ consistent with the turnover and a model where disc timescale drives variability amplitudes in the form $\log A/A_0=1/2\times\Delta t/t_{\rm orb}$, as suggested before. In the future, if the black-hole mass is known, observations of variability might be used as diagnostics of the physical luminosity in accretion discs, and therefore constrain inclination or dust extinction., Comment: 12 pages, 7 figures, submitted to MNRAS

Published
2024

4. Development and Initial Validation of Mindfulness-Based Pain Reduction (MBPR) in Patients With Chronic Low Back Pain

Author

Mehling WE, Brintz CE, Hartogensis W, Wolf C, Rogers K, Adler SR, Strigo IA, and Hecht FM

Subjects
chronic pain, pain management, interoception, interoceptive exposure, mindfulness, attention., Medicine (General), R5-920
Abstract

Wolf E Mehling,1,2 Carrie E Brintz,3,4 Wendy Hartogensis,2 Christiane Wolf,5 Kirsten Rogers,2 Shelley R Adler,1,2 Irina A Strigo,6,7 Frederick M Hecht2,8 1Department of Family and Community Medicine, University of California, San Francisco, San Francisco, CA, USA; 2Osher Center for Integrative Health, University of California, San Francisco, San Francisco, CA, USA; 3Department of Anesthesiology, Center for Musculoskeletal Research, Vanderbilt University Medical Center, Nashville, TN, USA; 4Osher Center for Integrative Health, Vanderbilt University Medical Center, Nashville, TN, USA; 5InsightLA, Los Angeles, CA, USA; 6Emotion and Pain Laboratory and VA Advanced Imaging Research Center San Francisco Veterans Affairs Health Care Center, San Francisco, CA, USA; 7Department of Psychiatry, University of California, San Francisco, San Francisco, CA, USA; 8Department of Medicine, University of California, San Francisco, CA, USACorrespondence: Wolf E Mehling, Osher Center for Integrative Health, Department of Family and Community Medicine, 1545 Divisadero St. 4th Floor, San Francisco, CA, 94115, USA, Tel +1 415 353 9506, Email Wolf.Mehling@ucsf.eduPurpose: Mindfulness-Based Stress Reduction (MBSR) has shown efficacy for alleviating chronic low back pain (cLBP) and is included in current treatment guidelines. However, benefits are moderate. We aimed to optimize MBSR for chronic pain by using recent research to develop Mindfulness-Based Pain Reduction (MBPR) and test it in patients with cLBP.Patients and Methods: Phase 1: We modified the MBSR curriculum with theory-driven components and convened focus groups with local and international mindfulness and clinical pain management experts to refine an 8-week MBPR program. Phase 2: We recruited participants with cLBP from Northern California using outreach in newsletters, social media, and other methods to test and iteratively modify the curriculum. MBPR was delivered in a group format by videoconference. The first three groups received MBPR; a fourth group was randomized to MBSR or MBPR to assess randomization feasibility. We assessed feasibility and acceptability by attendance, practice logs, and exit interviews. We assessed changes in patient-reported outcome measures for low back pain trials using a single arm (treatment group only) approach at 2 and 6 months with linear mixed models (primary: pain intensity and interference (PEG) scores).Results: Phase 1: The MBPR curriculum included: 1) mindful interoceptive exposure to pain, 2) pain neuroscience education, and 3) yoga postures specifically for cLBP. Phase 2: we enrolled 58 patients in 4 cohorts; 49 completed post-intervention and 41 completed 6-month follow-up assessments; 29 of the 41 received MBPR. Participants attended a mean of 80% of sessions and 23 of 24 participants accepted randomization in the 4th cohort. Mean PEG scores improved for 20 of 29 MBPR participants in a clinically meaningful way (PEG scores > 30%).Conclusion: MBPR was feasible and acceptable. Two-thirds of MBPR participants experienced clinically meaningful improvements in pain intensity and interference scores. MBPR warrants further investigation through a randomized, controlled trial.Keywords: chronic pain, pain management, interoception, interoceptive exposure, mindfulness, attention

Published
2025

8. A redshifted excess in the broad emission lines after the flare of the $\gamma$-ray narrow-line Seyfert 1 PKS 2004-447

Author

Hon, W., Berton, M., Sani, E., Webster, R., Wolf, C., Rojas, A. F., Marziani, P., Kotilainen, J., and Congiu, E.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

PKS 2004-447 is a narrow-line Seyfert 1 (NLS1) harbouring a relativistic jet with gamma-ray emission. On 2019-10-25, the Fermi-Large Area Telescope captured a $\gamma$-ray flare from this source, offering a chance to study the broad-line region (BLR) and jet during such violent events. This can provide insights to the BLR structure and jet interactions, which are important for active galactic nuclei and host galaxy coevolution. We report X-Shooter observations of enhancements in the broad line components of Balmer, Paschen and He I lines seen only during the post-flare and vanishing 1.5 years after. These features are biased redward up to $\sim$250 km s$^{-1}$ and are narrower than the pre-existing broad line profiles. This indicates a connection between the relativistic jet and the BLR of a young AGN, and how $\gamma$-ray production can lead to localised addition of broad emission lines., Comment: 19 pages, 14 figures, 3 tables, including appendix. Accepted for publication on A&A Letters

Published
2023
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10. SOP – Fatigue

Author

Cuhls, H., Mochamat, Mücke, M., Jaspers, B., Jentschke, E., Hense, J., Wolf, C., Ostgathe, C., and Radbruch, L.

Published
2024
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14. Multi-filter photometry of Solar System Objects from the SkyMapper Southern Survey

Author

Sergeyev, A. V., Carry, B., Onken, C. A., Devillepoix, H. A. R., Wolf, C., and Chang, S. -W.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. The populations of small bodies of the Solar System (asteroids, comets, Kuiper Belt objects) are used to constrain the origin and evolution of the Solar System. Both their orbital distribution and composition distribution are required to track the dynamical pathway from their regions of formation to their current locations. Aims. We aim at increasing the sample of Solar System objects (SSOs) that have multi-filter photometry and compositional taxonomy. Methods. We search for moving objects in the SkyMapper Southern Survey. We use the predicted SSO positions to extract photometry and astrometry from the SkyMapper frames. We then apply a suite of filters to clean the catalog for false-positive detections. We finally use the near-simultaneous photometry to assign a taxonomic class to objects. Results. We release a catalog of 880,528 individual observations, consisting of 205,515 known and unique SSOs. The catalog completeness is estimated to be about 97% down to V=18 mag and the purity to be above 95% for known SSOs. The near-simultaneous photometry provides either three, two, or a single color that we use to classify 117,356 SSOs with a scheme consistent with the widely used Bus-DeMeo taxonomy. Conclusions. The present catalog contributes significantly to the sample of asteroids with known surface properties (about 40% of main-belt asteroids down to an absolute magnitude of 16). We will release more observations of SSOs with future SkyMapper data releases., Comment: 15 pages, 22 figures, 13 tables

Published
2021
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17. Determination of luminosity for in-ring reactions: A new approach for the low-energy domain

Author

Xing, Y. M., Glorius, J., Varga, L., Bott, L., Bruckner, C. Brandau B., Chen, R. J., Chen, X., Dababneh, S., Davinson, T., Erbacher, P., Fiebiger, S., Gassner, T., Gobel, K., Groothuis, M., Gumberidze, A., Gyurky, G., Heil, M., Hess, R., Hensch, R., Hillmann, P., Hillenbrand, P. -M., Hinrichs, O., Jurado, B., Kausch, T., Khodaparast, A., Kisselbach, T., Klapper, N., Kozhuharov, C., Kurtulgil, D., Lane, G., Langer, C., Lederer-Woods, C., Lestinsky, M., Litvinov, S., Litvinov, Yu. A., Loher, B., Petridis, N., Popp, U., Reed, M., Reifarth, R., Sanjari, M. S., Simon, H., Slavkovska, Z., Spillmann, U., Steck, M., Stohlker, T., Stumm, J., Szucs, T., Nguyen, T. T., Zadeh, A. Taremi, Thomas, B., Torilov, S. Yu., Tornqvist, H., Trageser, C., Trotsenko, S., Volknandt, M., Wang, M., Weigand, M., Wolf, C., Woods, P. J., Zhang, Y. H., and Zhou, X. H.

Subjects
Nuclear Experiment
Abstract

Luminosity is a measure of the colliding frequency between beam and target and it is a crucial parameter for the measurement of absolute values, such as reaction cross sections. In this paper, we make use of experimental data from the ESR storage ring to demonstrate that the luminosity can be precisely determined by modelling the measured Rutherford scattering distribution. The obtained results are in good agreement with an independent measurement based on the x-ray normalization method. Our new method provides an alternative way to precisely measure the luminosity in low-energy stored-beam configurations. This can be of great value in particular in dedicated low-energy storage rings where established methods are difficult or impossible to apply., Comment: 8 pages, 5 figures

Published
2020
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18. Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network

Author

Ackley, K., Adya, V. B., Agrawal, P., Altin, P., Ashton, G., Bailes, M., Baltinas, E., Barbuio, A., Beniwal, D., Blair, C., Blair, D., Bolingbroke, G. N., Bossilkov, V., Boublil, S. Shachar, Brown, D. D., Burridge, B. J., Bustillo, J. Calderon, Cameron, J., Cao, H. Tuong, Carlin, J. B., Chang, S., Charlton, P., Chatterjee, C., Chattopadhyay, D., Chen, X., Chi, J., Chow, J., Chu, Q., Ciobanu, A., Clarke, T., Clearwater, P., Cooke, J., Coward, D., Crisp, H., Dattatri, R. J., Deller, A. T., Dobie, D. A., Dunn, L., Easter, P. J., Eichholz, J., Evans, R., Flynn, C., Foran, G., Forsyth, P., Gai, Y., Galaudage, S., Galloway, D. K., Gendre, B., Goncharov, B., Goode, S., Gozzard, D., Grace, B., Graham, A. W., Heger, A., Vivanco, F. Hernandez, Hirai, R., Holland, N. A., Holmes, Z. J., Howard, E., Howell, E., Howitt, G., Hübner, M. T., Hurley, J., Ingram, C., Hamedan, V. Jaberian, Jenner, K., Ju, L., Kapasi, D. P., Kaur, T., Kijbunchoo, N., Kovalam, M., Choudhary, R. Kumar, Lasky, P. D., Lau, M. Y. M., Leung, J., Liu, J., Loh, K., Mailvagan, A., Mandel, I., McCann, J. J., McClelland, D. E., McKenzie, K., McManus, D., McRae, T., Melatos, A., Meyers, P., Middleton, H., Miles, M. T., Millhouse, M., Mong, Y. Lun, Mueller, B., Munch, J., Musiov, J., Muusse, S., Nathan, R. S., Naveh, Y., Neijssel, C., Neil, B., Ng, S. W. S., Oloworaran, V., Ottaway, D. J., Page, M., Pan, J., Pathak, M., Payne, E., Powell, J., Pritchard, J., Puckridge, E., Raidani, A., Rallabhandi, V., Reardon, D., Riley, J. A., Roberts, L., Romero-Shaw, I. M., Roocke, T. J., Rowell, G., Sahu, N., Sarin, N., Sarre, L., Sattari, H., Schiworski, M., Scott, S. M., Sengar, R., Shaddock, D., Shannon, R., SHI, J., Sibley, P., Slagmolen, B. J. J., Slaven-Blair, T., Smith, R. J. E., Spollard, J., Steed, L., Strang, L., Sun, H., Sunderland, A., Suvorova, S., Talbot, C., Thrane, E., Töyrä, D., Trahanas, P., Vajpeyi, A., van Heijningen, J. V., Vargas, A. F., Veitch, P. J., Vigna-Gomez, A., Wade, A., Walker, K., Wang, Z., Ward, R. L., Ward, K., Webb, S., Wen, L., Wette, K., Willcox, R., Winterflood, J., Wolf, C., Wu, B., Yap, M. Jet, You, Z., Yu, H., Zhang, J., Zhao, C., and Zhu, X.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, General Relativity and Quantum Cosmology
Abstract

Gravitational waves from coalescing neutron stars encode information about nuclear matter at extreme densities, inaccessible by laboratory experiments. The late inspiral is influenced by the presence of tides, which depend on the neutron star equation of state. Neutron star mergers are expected to often produce rapidly-rotating remnant neutron stars that emit gravitational waves. These will provide clues to the extremely hot post-merger environment. This signature of nuclear matter in gravitational waves contains most information in the 2-4 kHz frequency band, which is outside of the most sensitive band of current detectors. We present the design concept and science case for a neutron star extreme matter observatory (NEMO): a gravitational-wave interferometer optimized to study nuclear physics with merging neutron stars. The concept uses high circulating laser power, quantum squeezing and a detector topology specifically designed to achieve the high-frequency sensitivity necessary to probe nuclear matter using gravitational waves. Above one kHz, the proposed strain sensitivity is comparable to full third-generation detectors at a fraction of the cost. Such sensitivity changes expected event rates for detection of post-merger remnants from approximately one per few decades with two A+ detectors to a few per year, and potentially allows for the first gravitational-wave observations of supernovae, isolated neutron stars, and other exotica., Comment: Accepted for publication in PASA

Published
2020
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19. Electron capture of Xe$^{54+}$ in collisions with H${_2}$ molecules in the energy range between 5.5 MeV/u and 30.9 MeV/u

Author

Kröger, F. M., Weber, G., Herdrich, M. O., Glorius, J., Langer, C., Slavkovská, Z., Bott, L., Brandau, C., Brückner, B., Blaum, K., Chen, X., Dababneh, S., Davinson, T., Erbacher, P., Fiebiger, S., Gaßner, T., Göbel, K., Groothuis, M., Gumberidze, A., Gyürky, Gy., Hagmann, S., Hahn, C., Heil, M., Hess, R., Hensch, R., Hillmann, P., Hillenbrand, P. -M., Hinrichs, O., Jurado, B., Kausch, T., Khodaparast, A., Kisselbach, T., Klapper, N., Kozhuharov, C., Kurtulgil, D., Lane, G., Lederer-Woods, C., Lestinsky, M., Litvinov, S., Litvinov, Yu. A., Löher, B., Nolden, F., Petridis, N., Popp, U., Reed, M., Reifarth, R., Sanjari, M. S., Simon, H., Spillmann, U., Steck, M., Stumm, J., Szücs, T., Nguyen, T. T., Zadeh, A. Taremi, Thomas, B., Torilov, S. Yu., Törnqvist, H., Trageser, C., Trotsenko, S., Volknandt, M., Weigand, M., Wolf, C., Woods, P. J., Shevelko, V. P., Tolstikhina, I. Yu., and Stöhlker, Th.

Subjects
Physics - Atomic Physics
Abstract

The electron capture process was studied for Xe$^{54+}$ colliding with H$_2$ molecules at the internal gas target of the ESR storage ring at GSI, Darmstadt. Cross section values for electron capture into excited projectile states were deduced from the observed emission cross section of Lyman radiation, being emitted by the hydrogen-like ions subsequent to the capture of a target electron. The ion beam energy range was varied between 5.5 MeV/u and 30.9 MeV/u by applying the deceleration mode of the ESR. Thus, electron capture data was recorded at the intermediate and in particular the low collision energy regime, well below the beam energy necessary to produce bare xenon ions. The obtained data is found to be in reasonable qualitative agreement with theoretical approaches, while a commonly applied empirical formula significantly overestimates the experimental findings.

Published
2020
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20. Agronomische Perspektive

Author

Migende, Jörg, Sonnen, Johannes, Schauff, Sebastian, Schill, Julian, Mayer-Bosse, Alexa, Leeb, Theo, Stangl, Josef, Stöcklin, Volker, Kiefer, Stefan, Pessl, Gottfried, Blank, Sebastian, Wendling, Ignatz, Terlunen, Sebastian, Zeller, Heike, Herchenbach, Martin, Ziemßen, Fabio, Goertz, Wolf C., Dörr, Jörg, editor, and Nachtmann, Matthias, editor

Published
2023
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21. WALLABY -- An SKA Pathfinder HI Survey

Author

Koribalski, B. S., Staveley-Smith, L., Westmeier, T., Serra, P., Spekkens, K., Wong, O. I., Lagos, C. D. P., Obreschkow, D., Ryan-Weber, E. V., Zwaan, M., Kilborn, V., Bekiaris, G., Bekki, K., Bigiel, F., Boselli, A., Bosma, A., Catinella, B., Chauhan, G., Cluver, M. E., Colless, M., Courtois, H. M., Crain, R. A., de Blok, W. J. G., Dénes, H., Duffy, A. R., Elagali, A., Fluke, C. J., For, B. -Q., Heald, G., Henning, P. A., Hess, K. M., Holwerda, B. W., Howlett, C., Jarrett, T., Jones, D. H., Jones, M. G., Józsa, G. I. G., Jurek, R., Jütte, E., Kamphuis, P., Karachentsev, I., Kerp, J., Keiner, D., Kraan-Korteweg, R. C., Lee-Waddell, K., López-Sánchez, A. R., Madrid, J., Meyer, M., Mould, J., Murugeshan, C., Norris, R. P., Oh, S. -H., Oosterloo, T. A., Popping, A., Putman, M., Reynolds, T. N., Rhee, J., Robotham, A. S. G., Ryder, S., Schröder, A. C., Shao, Li, Stevens, A. R. H., Taylor, E. N., van der Hulst, J. M., Verdes-Montenegro, L., Wakker, B. P., Wang, J., Whiting, M., Winkel, B., and Wolf, C.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (HI) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 x 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radio-quiet zone in Western Australia. WALLABY aims to survey three-quarters of the sky (-90 degr < Dec < +30 degr) to a redshift of z < 0.26, and generate spectral line image cubes at ~30 arcsec resolution and ~1.6 mJy/beam per 4 km/s channel sensitivity. ASKAP's instantaneous field of view at 1.4 GHz, delivered by the PAF's 36 beams, is about 30 sq deg. At an integrated signal-to-noise ratio of five, WALLABY is expected to detect over half a million galaxies with a mean redshift of z ~ 0.05 (~200 Mpc). The scientific goals of WALLABY include: (a) a census of gas-rich galaxies in the vicinity of the Local Group; (b) a study of the HI properties of galaxies, groups and clusters, in particular the influence of the environment on galaxy evolution; and (c) the refinement of cosmological parameters using the spatial and redshift distribution of low-bias gas-rich galaxies. For context we provide an overview of previous large-scale HI surveys. Combined with existing and new multi-wavelength sky surveys, WALLABY will enable an exciting new generation of panchromatic studies of the Local Universe. - First results from the WALLABY pilot survey are revealed, with initial data products publicly available in the CSIRO ASKAP Science Data Archive (CASDA)., Comment: Accepted for publication in ApSS (38 pages, 14 figures), see also https://www.atnf.csiro.au/research/WALLABY/ - Contact email: Baerbel.Koribalski@csiro.au

Published
2020
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23. Expectations of reward and efficacy guide cognitive control allocation.

Author

Frömer, R, Lin, H, Dean Wolf, C, Inzlicht, M, and Shenhav, A

Subjects
Adolescent, Adult, Cognition, Cues, Female, Humans, Male, Motivation, Reward, Self Efficacy, Task Performance and Analysis
Abstract

The amount of mental effort we invest in a task is influenced by the reward we can expect if we perform that task well. However, some of the rewards that have the greatest potential for driving these efforts are partly determined by factors beyond ones control. In such cases, effort has more limited efficacy for obtaining rewards. According to the Expected Value of Control theory, people integrate information about the expected reward and efficacy of task performance to determine the expected value of control, and then adjust their control allocation (i.e., mental effort) accordingly. Here we test this theorys key behavioral and neural predictions. We show that participants invest more cognitive control when this control is more rewarding and more efficacious, and that these incentive components separately modulate EEG signatures of incentive evaluation and proactive control allocation. Our findings support the prediction that people combine expectations of reward and efficacy to determine how much effort to invest.

Published
2021

24. Efficient Ab-initio Multiplet Calculations for Magnetic Adatoms on MgO

Author

Wolf, C., Delgado, F., Reina, J., and Lorente, N.

Subjects
Condensed Matter - Mesoscale and Nanoscale Physics
Abstract

Scanning probe microscopy and spectroscopy, and more recently in combination with electron spin resonance, have allowed the direct observation of electron dynamics on the single-atom limit. The interpretation of data is strongly depending on model Hamiltonians. However, fitting effective spin Hamiltonians to experimental data lacks the ability to explore a vast number of potential systems of interest. By using plane-wave density functional theory (DFT) as starting point, we build a multiplet Hamiltonian making use of maximally-localized Wannier functions. The Hamiltonian contains spin-orbit and electron-electron interactions needed to obtain the relevant spin dynamics. The resulting reduced Hamiltonian is solved by exact diagonalization. We compare three prototypical cases of 3d transition metals Mn (total spin $S=5/2$), Fe ($S=2$) and Co ($S=3/2$) on MgO with experimental data and find that our calculations can accurately predict the spin orientation and anisotropy of the magnetic adatom. Our method does not rely on experimental input and permits us to explore and predict the fundamental magnetic properties of adatoms on surfaces., Comment: 13 figures. It includes Supplementary Material

Published
2019
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25. Constraining the Neutron Star Compactness: Extraction of the $^{23}$Al($p,\gamma$) Reaction Rate for the $rp$-Process

Author

Wolf, C., Langer, C., Montes, F., Pereira, J., Ong, W. -J., Poxon-Pearson, T., Ahn, S., Ayoub, S., Baumann, T., Bazin, D., Bender, P. C., Brown, B. A., Browne, J., Crawford, H., Cyburt, R. H., Deleeuw, E., Elman, B., Fiebiger, S., Gade, A., Gastis, P., Lipschutz, S., Longfellow, B., Meisel, Z., Nunes, F. M., Perdikakis, G., Reifarth, R., Richter, W. A., Schatz, H., Schmidt, K., Schmitt, J., Sullivan, C., Titus, R., Weisshaar, D., Woods, P. J., Zamora, J. C., and Zegers, R. G. T.

Subjects
Nuclear Experiment, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Nuclear Theory
Abstract

The $^{23}$Al($p,\gamma$)$^{24}$Si reaction is among the most important reactions driving the energy generation in Type-I X-ray bursts. However, the present reaction-rate uncertainty limits constraints on neutron star properties that can be achieved with burst model-observation comparisons. Here, we present a novel technique for constraining this important reaction by combining the GRETINA array with the neutron detector LENDA coupled to the S800 spectrograph at the National Superconducting Cyclotron Laboratory. The $^{23}$Al($d,n$) reaction was used to populate the astrophysically important states in $^{24}$Si. This enables a measurement in complete kinematics for extracting all relevant inputs necessary to calculate the reaction rate. For the first time, a predicted close-lying doublet of a 2$_2^+$ and (4$_1^+$,0$_2^+$) state in $^{24}$Si was disentangled, finally resolving conflicting results from two previous measurements. Moreover, it was possible to extract spectroscopic factors using GRETINA and LENDA simultaneously. This new technique may be used to constrain other important reaction rates for various astrophysical scenarios.

Published
2019
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26. Five new real-time detections of Fast Radio Bursts with UTMOST

Author

Farah, W., Flynn, C., Bailes, M., Jameson, A., Bateman, T., Campbell-Wilson, D., Day, C. K., Deller, A. T., Green, A. J., Gupta, V., Hunstead, R., Lower, M. E., Osłowski, S., Parthasarathy, A., Price, D. C., Ravi, V., Shannon, R. M., Sutherland, A., Temby, D., Krishnan, V. Venkatraman, Caleb, M., Chang, S. -W., Cruces, M., Roy, J., Morello, V., Onken, C. A., Stappers, B. W., and Wolf, C.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We detail a new fast radio burst (FRB) survey with the Molonglo Radio Telescope, in which six FRBs were detected between June 2017 and December 2018. By using a real-time FRB detection system, we captured raw voltages for five of the six events, which allowed for coherent dedispersion and very high time resolution (10.24 $\mu$s) studies of the bursts. Five of the FRBs show temporal broadening consistent with interstellar and/or intergalactic scattering, with scattering timescales ranging from 0.16 to 29.1 ms. One burst, FRB181017, shows remarkable temporal structure, with 3 peaks each separated by 1 ms. We searched for phase-coherence between the leading and trailing peaks and found none, ruling out lensing scenarios. Based on this survey, we calculate an all-sky rate at 843 MHz of $98^{+59}_{-39}$ events sky$^{-1}$ day$^{-1}$ to a fluence limit of 8 Jy-ms: a factor of 7 below the rates estimated from the Parkes and ASKAP telescopes at 1.4 GHz assuming the ASKAP-derived spectral index $\alpha=-1.6$ ($F_{\nu}\propto\nu^{\alpha}$). Our results suggest that FRB spectra may turn over below 1 GHz. Optical, radio and X-ray followup has been made for most of the reported bursts, with no associated transients found. No repeat bursts were found in the survey., Comment: 13 pages, 11 figures, submitted to MNRAS

Published
2019
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27. A cotunneling mechanism for all-electrical Electron Spin Resonance of single adsorbed atoms

Author

Gálvez, J. Reina, Wolf, C., Delgado, F., and Lorente, N.

Subjects
Condensed Matter - Mesoscale and Nanoscale Physics
Abstract

The recent development of all-electrical electron spin resonance (ESR) in a scanning tunneling microscope (STM) setup has opened the door to vast applications. Despite the fast growing number of experimental works on STM-ESR, the fundamental principles remains unclear. By using a cotunneling picture, we show that the spin resonance signal can be explained as a time-dependent variation of the tunnel barrier induced by the alternating electric driving field. We demonstrate how this variation translates into the resonant frequency response of the direct current. Our cotunneling theory explains the main experimental findings. Namely, the linear dependence of the Rabi flop rate with the alternating bias amplitude, the absence of resonant response for spin-unpolarized currents, and the weak dependence on the actual atomic species., Comment: 11 pages, 3 figures

Published
2019
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30. Approaching the Gamow window with stored ions: Direct measurement of $^{124}$Xe(p,$\gamma$) in the ESR storage ring

Author

Glorius, J., Langer, C., Slavkovská, Z., Bott, L., Brandau, C., Brückner, B., Blaum, K., Chen, X., Dababneh, S., Davinson, T., Erbacher, P., Fiebiger, S., Gaßner, T., Göbel, K., Groothuis, M., Gumberidze, A., Gyürky, G., Heil, M., Hess, R., Hensch, R., Hillmann, P., Hillenbrand, P. -M., Hinrichs, O., Jurado, B., Kausch, T., Khodaparast, A., Kisselbach, T., Klapper, N., Kozhuharov, C., Kurtulgil, D., Lane, G., Lederer-Woods, C., Lestinsky, M., Litvinov, S., Litvinov, Yu. A., Löher, B., Nolden, F., Petridis, N., Popp, U., Rauscher, T., Reed, M., Reifarth, R., Sanjari, M. S., Savran, D., Simon, H., Spillmann, U., Steck, M., Stöhlker, T., Stumm, J., Surzhykov, A., Szücs, T., Nguyen, T. T., Zadeh, A. Taremi, Thomas, B., Torilov, S. Yu., Törnqvist, H., Träger, M., Trageser, C., Trotsenko, S., Varga, L., Volknandt, M., Weick, H., Weigand, M., Wolf, C., Woods, P. J., and Xing, Y. M.

Subjects
Nuclear Experiment
Abstract

We report the first measurement of low-energy proton-capture cross sections of $^{124}$Xe in a heavy ion storage ring. $^{124}$Xe$^{54+}$ ions of five different beam energies between 5.5 AMeV and 8 AMeV were stored to collide with a windowless hydrogen target. The $^{125}$Cs reaction products were directly detected. The interaction energies are located on the high energy tail of the Gamow window for hot, explosive scenarios such as supernovae and X-ray binaries. The results serve as an important test of predicted astrophysical reaction rates in this mass range. Good agreement in the prediction of the astrophysically important proton width at low energy is found, with only a 30% difference between measurement and theory. Larger deviations are found above the neutron emission threshold, where also neutron- and ${\gamma}$-widths significantly impact the cross sections. The newly established experimental method is a very powerful tool to investigate nuclear reactions on rare ion beams at low center-of-mass energies.

Published
2019
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31. A Fast Radio Burst with frequency-dependent polarization detected during Breakthrough Listen observations

Author

Price, D. C., Foster, G., Geyer, M., van Straten, W., Gajjar, V., Hellbourg, G., Karastergiou, A., Keane, E. F., Siemion, A. P. V., Arcavi, I., Bhat, R., Caleb, M., Chang, S-W., Croft, S., DeBoer, D., de Pater, I., Drew, J., Enriquez, J. E., Farah, W., Gizani, N., Green, J. A., Isaacson, H., Hickish, J., Jameson, A., Lebofsky, M., MacMahon, D. H. E., Möller, A., Onken, C. A., Petroff, E., Werthimer, D., Wolf, C., Worden, S. P., and Zhang, Y. G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Here, we report on the detection and verification of Fast Radio Burst FRB 180301, which occurred on UTC 2018 March 1 during the Breakthrough Listen observations with the Parkes telescope. Full-polarization voltage data of the detection were captured--a first for non-repeating FRBs--allowing for coherent de-dispersion and additional verification tests. The coherently de-dispersed dynamic spectrum of FRB 180301 shows complex, polarized frequency structure over a small fractional bandwidth. As FRB 180301 was detected close to the geosynchronous satellite band during a time of known 1-2 GHz satellite transmissions, we consider whether the burst was due to radio interference emitted or reflected from an orbiting object. Based on the preponderance of our verification tests, we find that FRB 180301 is likely of astrophysical origin, but caution that anthropogenic sources cannot conclusively be ruled out., Comment: Submitted to MNRAS

Published
2019
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32. Milky Way tomography with the SkyMapper Southern Survey: I: Atmospheric parameters and distances of one million red giants

Author

Huang, Y., Chen, B. -Q., Yuan, H. -B., Zhang, H. -W., Xiang, M. -X., Wang, C., Wang, H. -F., Wolf, C., Liu, G. -C., and Liu, X. -W.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Accurate determinations of atmospheric parameters (effective temperature $T_{\rm eff}$, surface gravity log $g$ and metallicity [Fe/H]) and distances for large complete samples are of vital importance for various Galactic studies. We have developed a photometric method to select red giant stars and estimate their atmospheric parameters from the photometric colors provided by the SkyMapper Southern Survey (SMSS) data release (DR) 1.1, using stars in common with the LAMOST Galactic spectroscopic surveys as a training set. Distances are estimated with two different approaches: one based on the Gaia DR2 parallaxes for nearby ($d \leq 4.5$ kpc) bright stars and another based on the absolute magnitudes predicted by intrinsic color $(g-i)_0$ and photometric metallicity [Fe/H] for distant ($d > 4.5$ kpc) faint stars. Various tests show that our method is capable of delivering atmospheric parameters with a precision of $\sim$80 K for $T_{\rm eff}$, $\sim$0.18 dex for [Fe/H] and $\sim$0.35 dex for log $g$, but with a significant systematic error at log $g \sim$ 2.3. For distances delivered from $(g-i)_0$ and photometric [Fe/H], our test with the member stars of globular clusters show a median uncertainty of 16 per cent with a negligible zero-point offset. Using this method, atmospheric parameters and distances of nearly one million red giant stars are derived from SMSS DR1.1. Proper motion measurements from Gaia DR2 are available for almost all of the red giant stars, and radial velocity measurements from several large spectroscopic surveys are available for 44 per cent of these. This sample will be accessible online at https://yanghuang0.wixsite.com/yangh/research ., Comment: Accepted for ApJS, 19 pages, 20 figures, 7 tables; the full catalog now is accessible online at https://yanghuang0.wixsite.com/yangh/research

Published
2019
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33. Agronomy Perspective

Author

Migende, Jörg, Sonnen, Johannes, Schauff, Sebastian, Schill, Julian, Mayer-Bosse, Alexa, Leeb, Theo, Stangl, Josef, Stöcklin, Volker, Kiefer, Stefan, Pessl, Gottfried, Blank, Sebastian, Wendling, Ignatz, Terlunen, Sebastian, Zeller, Heike, Herchenbach, Martin, Ziemßen, Fabio, Goertz, Wolf C., Dörr, Jörg, editor, and Nachtmann, Matthias, editor

Published
2022
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35. SkyMapper stellar parameters for Galactic Archaeology on a grand-scale

Author

Casagrande, L., Wolf, C., Mackey, A. D., Nordlander, T., Yong, D., and Bessell, M.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The SkyMapper photometric surveys provides uvgriz photometry for several millions sources in the Southern sky. We use DR1.1 to explore the quality of its photometry, and develop a formalism to homogenise zero-points across the sky using stellar effective temperatures. Physical flux transformations, and zero-points appropriate for this release are derived, along with relations linking colour indices to stellar parameters. Reddening-free pseudo-colours and pseudo-magnitudes are also introduced. For late-type stars which are best suited for Galactic Archaeology, we show that SkyMapper+2MASS are able to deliver a precision better than 100K in effective temperatures (depending on the filters), ~0.2dex for metallicities above -2, and a reliable distinction between M-dwarfs and -giants. Together with astrometric and asteroseismic space mission, SkyMapper promises to be a treasure trove for stellar and Galactic studies., Comment: MNRAS, accepted. Metallicities and effective temperatures for 9 million Gaia+SkyMapper stars at https://github.com/casaluca/SkyMapper

Published
2018
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36. The ATLAS All-Sky Stellar Reference Catalog

Author

Tonry, J. L., Denneau, L., Flewelling, H., Heinze, A. N., Onken, C. A., Smartt, S. J., Stalder, B., Weiland, H. J., and Wolf, C.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Asteroid Terrestrial-impact Last Alert System (ATLAS) observes most of the sky every night in search of dangerous asteroids. Its data are also used to search for photometric variability, where sensitivity to variability is limited by photometric accuracy. Since each exposure spans 7.6 deg corner to corner, variations in atmospheric transparency in excess of 0.01 mag are common, and 0.01 mag photometry cannot be achieved by using a constant flat field calibration image. We therefore have assembled an all-sky reference catalog of approximately one billion stars to m~19 from a variety of sources to calibrate each exposure's astrometry and photometry. Gaia DR2 is the source of astrometry for this ATLAS Refcat2. The sources of g, r, i, z photometry include Pan-STARRS DR1, the ATLAS Pathfinder photometry project, ATLAS re-flattened APASS data, SkyMapper DR1, APASS DR9, the Tycho-2 catalog, and the Yale Bright Star Catalog. We have attempted to make this catalog at least 99% complete to m<19, including the brightest stars in the sky. We believe that the systematic errors are no larger than 5 millimag RMS, although errors are as large as 20 millimag in small patches near the galactic plane., Comment: 22 pages, 6 figures, ApJ in press

Published
2018
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37. A nearby superluminous supernova with a long pre-maximum 'plateau' and strong CII features

Author

Anderson, J. P., Pessi, P. J., Dessart, L., Inserra, C., Hiramatsu, D., Taggart, K., Smartt, S. J., Leloudas, G., Chen, T. -W., Möller, A., Roy, R., Schulze, S., Perley, D., Selsing, J., Prentice, S. J., Gal-Yam, A., Angus, C. R., Arcavi, I., Ashall, C., Bulla, M., Bray, C., Burke, J., Callis, E., Cartier, R., Chang, S. -W., Chambers, K., Clark, P., Denneau, L., Dennefeld, M., Flewelling, H., Fraser, M., Galbany, L., Gromadzki, M., Gutiérrez, C. P., Heinze, A., Hosseinzadeh, G., Howell, D. A., Hsiao, E. Y., Kankare, E., Kostrzewa-Rutkowska, Z., Magnier, E., Maguire, K., Mazzali, P., McBrien, O., McCully, C., Morrell, N., Lowe, T. B., Onken, C. A., Onori, F., Phillips, M. M., Rest, A., Ridden-Harper, R., Ruiter, A. J., Sand, D. J., Smith, K. W., Smith, M., Stalder, B., Stritzinger, M. D., Sullivan, M., Tonry, J. L., Tucker, B. E., Valenti, S., Wainscoat, R., Waters, C. Z., Wolf, C., and Young, D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Super-luminous supernovae (SLSNe) are rare events defined as being significantly more luminous than normal terminal stellar explosions. The source of the extra powering needed to achieve such luminosities is still unclear. Discoveries in the local Universe (i.e. $z<0.1$) are scarce, but afford dense multi-wavelength observations. Additional low-redshift objects are therefore extremely valuable. We present early-time observations of the type I SLSN ASASSN-18km/SN~2018bsz. These data are used to characterise the event and compare to literature SLSNe and spectral models. Host galaxy properties are also analysed. Optical and near-IR photometry and spectroscopy were analysed. Early-time ATLAS photometry was used to constrain the rising light curve. We identified a number of spectral features in optical-wavelength spectra and tracked their time evolution. Finally, we used archival host galaxy photometry together with HII region spectra to constrain the host environment. ASASSN-18km/SN~2018bsz is found to be a type I SLSN in a galaxy at a redshift of 0.0267 (111 Mpc), making it the lowest-redshift event discovered to date. Strong CII lines are identified in the spectra. Spectral models produced by exploding a Wolf-Rayet progenitor and injecting a magnetar power source are shown to be qualitatively similar to ASASSN-18km/SN~2018bsz, contrary to most SLSNe-I that display weak/non-existent CII lines. ASASSN-18km/SN~2018bsz displays a long, slowly rising, red 'plateau' of $>$26 days, before a steeper, faster rise to maximum. The host has an absolute magnitude of --19.8 mag ($r$), a mass of M$_{*}$ = 1.5$^{+0.08}_{-0.33}$ $\times$10$^{9}$ M$_{\odot}$ , and a star formation rate of = 0.50$^{+2.22}_{-0.19}$ M$_{\odot}$ yr$^{-1}$. A nearby HII region has an oxygen abundance (O3N2) of 8.31$\pm$0.01 dex., Comment: Accepted for publication in A&A after minor corrections to first arXiv version

Published
2018
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38. Deep Extragalactic VIsible Legacy Survey (DEVILS): Motivation, Design and Target Catalogue

Author

Davies, L. J. M., Robotham, A. S. G., Driver, S. P., Lagos, C. P., Cortese, L., Mannering, E., Foster, C., Lidman, C., Hashemizadeh, A., Koushan, S., O'Toole, S., Baldry, I. K., Bilicki, M., Bland-Hawthorn, J., Bremer, M. N., Brown, M. J. I., Bryant, J. J., Catinella, B., Croom, S. M., Grootes, M. W., Holwerda, B. W., Jarvis, M. J., Maddox, N., Meyer, M., Moffett, A. J., Phillipps, S., Taylor, E. N., Windhorst, R. A., and Wolf, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The Deep Extragalactic VIsible Legacy Survey (DEVILS) is a large spectroscopic campaign at the Anglo-Australian Telescope (AAT) aimed at bridging the near and distant Universe by producing the highest completeness survey of galaxies and groups at intermediate redshifts ($0.3

Published
2018
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39. The $^{7}$Be($\boldsymbol{n,p}$)$^{7}$Li reaction and the Cosmological Lithium Problem: measurement of the cross section in a wide energy range at n_TOF (CERN)

Author

Damone, L., Barbagallo, M., Mastromarco, M., Mengoni, A., Cosentino, L., Maugeri, E., Heinitz, S., Schumann, D., Dressler, R., Käppeler, F., Colonna, N., Finocchiaro, P., Andrzejewski, J., Perkowski, J., Gawlik, A., Aberle, O., Altstadt, S., Ayranov, M., Audouin, L., Bacak, M., Balibrea-Correa, J., Ballof, J., Bécares, V., Bečvář, F., Beinrucker, C., Bellia, G., Bernardes, A. P., Berthoumieux, E., Billowes, J., Borge, M. J. G., Bosnar, D., Brown, A., Brugger, M., Busso, M., Caamaño, M., Calviño, F., Calviani, M., Cano-Ott, D., Cardella, R., Casanovas, A., Castelluccio, D. M., Catherall, R., Cerutti, F., Chen, Y. H., Chiaveri, E., Cortés, G., Cortés-Giraldo, M. A., Cristallo, S., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dorsival, A., Dupont, E., Duran, I., Fernandez-Dominguez, B., Ferrari, A., Ferreira, P., Furman, W., Ganesan, S., García-Rio, A., Gilardoni, S., Glodariu, T., Göbel, K., Gonçalves, I. F., González-Romero, E., Goodacre, T. D., Griesmayer, E., Guerrero, C., Gunsing, F., Harada, H., Heftrich, T., Heyse, J., Jenkins, D. G., Jericha, E., Johnston, K., Kadi, Y., Kalamara, A., Katabuchi, T., Kavrigin, P., Kimura, A., Kivel, N., Kohester, U., Kokkoris, M., Krtička, M., Kurtulgil, D., Leal-Cidoncha, E., Lederer-Woods, C., Leeb, H., Lerendegui-Marco, J., Meo, S. Lo, Lonsdale, S. J., Losito, R., Macina, D., Marganiec, J., Marsh, B., Martíne, T., Correia, J. G. Martins, Masi, A., Massimi, C., Mastinu, P., Matteucci, F., Mazzone, A., Mendoza, E., Milazzo, P. M., Mingrone, F., Mirea, M., Musumarra, A., Negret, A., Nolte, R., Oprea, A., Patronis, N., Pavlik, A., Piersanti, L., Piscopo, M., Plompen, A., Porras, I., Praena, J., Quesada, J. M., Radeck, D., Rajeev, K., Rauscher, T., Reifarth, R., Riego-Perez, A., Rothe, S., Rout, P., Rubbia, C., Ryan, J., Sabaté-Gilarte, M., Saxena, A., Schell, J., Schillebeeckx, P., Schmidt, S., Sedyshev, P., Seiffert, C., Smith, A. G., Sosnin, N. V., Stamatopoulos, A., Stora, T., Tagliente, G., Tain, J. L., Tarifeño-Saldivia, A., Tassan-Got, L., Tsinganis, A., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Wallner, A., Warren, S., Weigand, M., Weiß, C., Wolf, C., Woods, P. J., Wright, T., and Žugec, P.

Subjects
Nuclear Experiment
Abstract

We report on the measurement of the $^{7}$Be($n, p$)$^{7}$Li cross section from thermal to approximately 325 keV neutron energy, performed in the high-flux experimental area (EAR2) of the n\_TOF facility at CERN. This reaction plays a key role in the lithium yield of the Big Bang Nucleosynthesis (BBN) for standard cosmology. The only two previous time-of-flight measurements performed on this reaction did not cover the energy window of interest for BBN, and showed a large discrepancy between each other. The measurement was performed with a Si-telescope, and a high-purity sample produced by implantation of a $^{7}$Be ion beam at the ISOLDE facility at CERN. While a significantly higher cross section is found at low-energy, relative to current evaluations, in the region of BBN interest the present results are consistent with the values inferred from the time-reversal $^{7}$Li($p, n$)$^{7}$Be reaction, thus yielding only a relatively minor improvement on the so-called Cosmological Lithium Problem (CLiP). The relevance of these results on the near-threshold neutron production in the p+$^{7}$Li reaction is also discussed.

Published
2018
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40. The first sample of spectroscopically confirmed ultra-compact massive galaxies in the Kilo Degree Survey

Author

Tortora, C., Napolitano, N. R., Spavone, M., La Barbera, F., D'Ago, G., Spiniello, C., Kuijken, K. H., Roy, N., Raj, M. A., Cavuoti, S., Brescia, M., Longo, G., Pota, V., Petrillo, C. E., Radovich, M., Getman, F., Koopmans, L. V. E., Trujillo, I., Kleijn, G. Verdoes, Capaccioli, M., Grado, A., Covone, G., Scognamiglio, D., Blake, C., Glazebrook, K., Joudaki, S., Lidman, C., and Wolf, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present results from an ongoing investigation using the Kilo Degree Survey (KiDS) on the VLT Survey Telescope (VST) to provide a census of ultra-compact massive galaxies (UCMGs), defined as galaxies with stellar masses $M_{\rm \star} > 8 \times 10^{10} \rm M_{\odot}$ and effective radii $R_{\rm e} < 1.5\,\rm kpc$. UCMGs, which are expected to have undergone very few merger events, provide a unique view on the accretion history of the most massive galaxies in the Universe. Over an effective sky area of nearly 330 square degrees, we select UCMG candidates from KiDS multi-colour images, which provide high quality structural parameters, photometric redshifts and stellar masses. Our sample of $\sim 1000$ photometrically selected UCMGs at $z < 0.5$ represents the largest sample of UCMG candidates assembled to date over the largest sky area. In this paper we present the first effort to obtain their redshifts using different facilities, starting with first results for 28 candidates with redshifts $z < 0.5$, obtained at NTT and TNG telescopes. We confirmed, as bona fide UCMGs, 19 out of the 28 candidates with new redshifts. A further 46 UCMG candidates are confirmed with literature spectroscopic redshifts (35 at $z < 0.5$), bringing the final cumulative sample of spectroscopically-confirmed lower-z UCMGs to 54 galaxies, which is the largest sample at redshifts below $0.5$. We use these spectroscopic redshifts to quantify systematic errors in our photometric selection, and use these to correct our UCMG number counts. We finally compare the results to independent datasets and simulations., Comment: Accepted for publication on MNRAS, 27 pages, 13 figures, 7 tables. This revised and improved version presents different updates. In particular, systematics and uncertainties in the measurement of the effective radii are now better discussed, and new plots are added

Published
2018
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41. Radio Galaxy Zoo: Machine learning for radio source host galaxy cross-identification

Author

Alger, M. J., Banfield, J. K., Ong, C. S., Rudnick, L., Wong, O. I., Wolf, C., Andernach, H., Norris, R. P., and Shabala, S. S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We consider the problem of determining the host galaxies of radio sources by cross-identification. This has traditionally been done manually, which will be intractable for wide-area radio surveys like the Evolutionary Map of the Universe (EMU). Automated cross-identification will be critical for these future surveys, and machine learning may provide the tools to develop such methods. We apply a standard approach from computer vision to cross-identification, introducing one possible way of automating this problem, and explore the pros and cons of this approach. We apply our method to the 1.4 GHz Australian Telescope Large Area Survey (ATLAS) observations of the Chandra Deep Field South (CDFS) and the ESO Large Area ISO Survey South 1 (ELAIS-S1) fields by cross-identifying them with the Spitzer Wide-area Infrared Extragalactic (SWIRE) survey. We train our method with two sets of data: expert cross-identifications of CDFS from the initial ATLAS data release and crowdsourced cross-identifications of CDFS from Radio Galaxy Zoo. We found that a simple strategy of cross-identifying a radio component with the nearest galaxy performs comparably to our more complex methods, though our estimated best-case performance is near 100 per cent. ATLAS contains 87 complex radio sources that have been cross-identified by experts, so there are not enough complex examples to learn how to cross-identify them accurately. Much larger datasets are therefore required for training methods like ours. We also show that training our method on Radio Galaxy Zoo cross-identifications gives comparable results to training on expert cross-identifications, demonstrating the value of crowdsourced training data.

Published
2018
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42. Feasibility of ApoC1 serum levels as tumor biomarker in glioblastoma patients: a pilot study

Author

Michelle Hilbert, Peter Kuzman, Wolf C. Mueller, Jürgen Meixensberger, and Ulf Nestler

Subjects
Medicine, Science
Abstract

Abstract Apolipoprotein C1 (ApoC1) has been detected immunohistochemically in glioblastoma tissue, probably expressed by activated monocytes and microglia. The present study was conceived to determine whether the amount of intratumoral ApoC1 expression leads to measurable changes of serum levels after glioblastoma resection or during recurrence. 176 blood samples from 70 glioblastoma patients were collected perioperatively and during subsequent therapy. ApoC1 serum levels were determined using an enzyme linked immunosorbent assay (ELISA). High absorption values due to lipemic or hemolytic serum were removed from the final dataset using a stem and leaf plot. Samples were grouped according to the treatment stage to compare mean ApoC1 serum levels. The number of patients with falling or increasing perioperative values was assessed. 167 ApoC1 serum values from 68 glioblastoma patients were amenable to statistical evaluation. Mean ApoC1 serum level was 91.9 µg/ml (n = 167, sd = 36.0). In samples from patients undergoing first glioblastoma resection, the mean preoperative value was significantly higher (94.8 µg/ml, n = 37, sd = 29.5) than after surgery (77.4 µg/ml, n = 41, sd = 23.2, p = 0.009). Individually, falling ApoC1 levels were detected in 25 and rising levels in 9 patients (p = 0.0061). Single absolute serum levels of ApoC1 do not allow an estimation of glioblastoma activity or tumor response. Although pathophysiologically of interest, ApoC1 serum levels did not qualify as a potential biomarker in glioblastoma management. Our results do not seem to encourage larger, multicenter studies.

Published
2022
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43. A Novel Type of IDH-wildtype Glioma Characterized by Gliomatosis Cerebri-like Growth Pattern, TERT Promoter Mutation, and Distinct Epigenetic Profile

Author

Muench, Amos, Teichmann, Daniel, Spille, Dorothee, Kuzman, Peter, Perez, Eilis, May, Sven-Axel, Mueller, Wolf C., Kombos, Theodoros, Nazari-Dehkordi, Shokufe, Onken, Julia, Vajkoczy, Peter, Ntoulias, Georgios, Bettencourt, Conceição, von Deimling, Andreas, Paulus, Werner, Heppner, Frank L., Koch, Arend, Capper, David, Kaul, David, Thomas, Christian, and Schweizer, Leonille

Published
2023
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44. FRB microstructure revealed by the real-time detection of FRB170827

Author

Farah, W., Flynn, C., Bailes, M., Jameson, A., Bannister, K. W., Barr, E. D., Bateman, T., Bhandari, S., Caleb, M., Campbell-Wilson, D., Chang, S. -W., Deller, A., Green, A. J., Hunstead, R., Jankowski, F., Keane, E., Macquart, J. -P., Möller, A., Onken, C. A., Osłowski, S., Parthasarathy, A., Plant, K., Ravi, V., Shannon, R. M., Tucker, B. E., Krishnan, V. Venkatraman, and Wolf, C.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report a new Fast Radio Burst (FRB) discovered in real-time as part of the UTMOST project at the Molonglo Observatory Synthesis Radio Telescope (MOST). FRB170827 is the first detected with our low-latency ($< 24$ s), machine-learning-based FRB detection system. The FRB discovery was accompanied by the capture of voltage data at the native time and frequency resolution of the observing system, enabling coherent dedispersion and detailed off-line analysis, which have unveiled fine temporal and frequency structure. The dispersion measure (DM) of 176.80 $\pm$ 0.04 pc cm$^{-3}$, is the lowest of the FRB population. The Milky Way contribution along the line of sight is $\sim$ 40 pc cm$^{-3}$, leaving an excess DM of $\sim$ 145 pc cm$^{-3}$. The FRB has a fluence $>$ 20 $\pm$ 7 Jy ms, and is narrow, with a width of $\sim$ 400 $\mu$s at 10$\%$ of its maximum amplitude. However, the burst shows three temporal components, the narrowest of which is $\sim$ 30 $\mu$s, and a scattering timescale of $4.1 \pm 2.7$ $\mu$s. The FRB shows spectral modulations on frequency scales of 1.5 MHz and 0.1 MHz. Both are prominent in the dynamic spectrum, which shows a very bright region of emission between 841 and 843 MHz, and weaker, patchy emission across the entire band. We show the fine spectral structure could arise in the FRB host galaxy, or its immediate vicinity., Comment: 10 pages, 6 figures, accepted for publication in MNRAS

Published
2018
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45. KiDS+2dFLenS+GAMA: Testing the cosmological model with the $E_{\rm G}$ statistic

Author

Amon, A., Blake, C., Heymans, C., Leonard, C. D., Asgari, M., Bilicki, M., Choi, A., Erben, T., Glazebrook, K., Harnois-Deraps, J., Hildebrandt, H., Hoekstra, H., Joachimi, B., Joudaki, S., Kuijken, K., Lidman, C., Loveday, J., Parkinson, D., Valentijn, E. A., and Wolf, C.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a new measurement of $E_{\rm G}$, which combines measurements of weak gravitational lensing, real-space galaxy clustering and redshift space distortions. This statistic was proposed as a consistency test of General Relativity (GR) that is insensitive to linear, deterministic galaxy bias and the matter clustering amplitude. We combine deep imaging data from KiDS with overlapping spectroscopy from 2dFLenS, BOSS DR12 and GAMA and find $E_{\rm G}(\overline{z}=0.267)=0.43 \pm 0.13$ (GAMA), $E_{\rm G}(\overline{z}=0.305)=0.27 \pm 0.08$ (LOWZ+2dFLOZ) and $E_{\rm G}(\overline{z}=0.554)=0.26 \pm 0.07$ (CMASS+2dFHIZ). We demonstrate that the existing tension in the value of the matter density parameter hinders the robustness of this statistic as solely a test of GR. We find that our $E_{\rm G}$ measurements, as well as existing ones in the literature, favour a lower matter density cosmology than the Cosmic Microwave Background. For a flat $\Lambda$CDM Universe and assuming GR, we find $\Omega_{\rm m}(z=0)=0.25\pm0.03$. With this paper we publicly release the 2dFLenS dataset at: \url{http://2dflens.swin.edu.au}., Comment: 17 pages, 8 figures

Published
2017
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46. Follow up of GW170817 and its electromagnetic counterpart by Australian-led observing programs

Author

Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J. R., Anderson, G. E., Ashley, M. C. B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M. S., Bian, F., Bland, P. A., Boer, M., Booler, T., Brandeker, A., Brown, I. S., Buckley, D., Chang, S. -W., Coward, D. M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J. S., Deller, A., Devillepoix, H. A. R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T. J., Franzen, T., Gaensler, B. M., Galloway, D. K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P. J., Hartig, B. A. D., Howell, E. J., Horsley, L., Hotan, A., Howie, R. M., Hu, L., Hu, Y., James, C. W., Johnston, S., Johnston-Hollitt, M., Kaplan, D. L., Kasliwal, M., Keane, E. F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L. C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D. E., McCully, C., Möller, A., Morales, M. F., Morris, D., Murphy, T., Noysena, K., Onken, C. A., Orange, N. B., Oslowski, S., Pallot, D., Paxman, J., Potter, S. B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E. M., Sansom, E. K., Scalzo, R. A., Schmidt, B. P., Scott, S. M., Seghouani, N., Shang, Z., Shannon, R. M., Shao, L., Shara, M. M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N. B., Tao, C., Tingay, S., Towner, M. C., Thierry, P., Trott, C., Tucker, B. E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., and Zovaro, H.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source afterglow cooled from approximately 6400K to 2100K over a 7-day period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (about 2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor., Comment: 26 pages, 9 figures, 15 tables

Published
2017
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47. Photometric redshifts for the Kilo-Degree Survey. Machine-learning analysis with artificial neural networks

Author

Bilicki, M., Hoekstra, H., Brown, M. J. I., Amaro, V., Blake, C., Cavuoti, S., de Jong, J. T. A., Georgiou, C., Hildebrandt, H., Wolf, C., Amon, A., Brescia, M., Brough, S., Costa-Duarte, M. V., Erben, T., Glazebrook, K., Grado, A., Heymans, C., Jarrett, T., Joudaki, S., Kuijken, K., Longo, G., Napolitano, N., Parkinson, D., Vellucci, C., Kleijn, G. A. Verdoes, and Wang, L.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present a machine-learning photometric redshift analysis of the Kilo-Degree Survey Data Release 3, using two neural-network based techniques: ANNz2 and MLPQNA. Despite limited coverage of spectroscopic training sets, these ML codes provide photo-zs of quality comparable to, if not better than, those from the BPZ code, at least up to zphot<0.9 and r<23.5. At the bright end of r<20, where very complete spectroscopic data overlapping with KiDS are available, the performance of the ML photo-zs clearly surpasses that of BPZ, currently the primary photo-z method for KiDS. Using the Galaxy And Mass Assembly (GAMA) spectroscopic survey as calibration, we furthermore study how photo-zs improve for bright sources when photometric parameters additional to magnitudes are included in the photo-z derivation, as well as when VIKING and WISE infrared bands are added. While the fiducial four-band ugri setup gives a photo-z bias $\delta z=-2e-4$ and scatter $\sigma_z<0.022$ at mean z = 0.23, combining magnitudes, colours, and galaxy sizes reduces the scatter by ~7% and the bias by an order of magnitude. Once the ugri and IR magnitudes are joined into 12-band photometry spanning up to 12 $\mu$, the scatter decreases by more than 10% over the fiducial case. Finally, using the 12 bands together with optical colours and linear sizes gives $\delta z<4e-5$ and $\sigma_z<0.019$. This paper also serves as a reference for two public photo-z catalogues accompanying KiDS DR3, both obtained using the ANNz2 code. The first one, of general purpose, includes all the 39 million KiDS sources with four-band ugri measurements in DR3. The second dataset, optimized for low-redshift studies such as galaxy-galaxy lensing, is limited to r<20, and provides photo-zs of much better quality than in the full-depth case thanks to incorporating optical magnitudes, colours, and sizes in the GAMA-calibrated photo-z derivation., Comment: A&A, in press. Data available from the KiDS website http://kids.strw.leidenuniv.nl/DR3/ml-photoz.php#annz2

Published
2017
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48. KiDS-i-800: Comparing weak gravitational lensing measurements in same-sky surveys

Author

Amon, A., Heymans, C., Klaes, D., Erben, T., Blake, C., Hildebrandt, H., Hoekstra, H., Kuijken, K., Miller, L., Morrison, C. B., Choi, A., de Jong, J. T. A., Glazebrook, K., Irissari, N., Joachimi, B., Joudaki, S., Kannawadi, A., Lidman, C., Napolitano, N., Parkinson, D., Schneider, P., van Uitert, E., Viola, M., and Wolf, C.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a weak gravitational lensing analysis of 815 square degree of $i$-band imaging from the Kilo-Degree Survey (KiDS-$i$-800). In contrast to the deep $r$-band observations, which take priority during excellent seeing conditions and form the primary KiDS dataset (KiDS-$r$-450), the complementary yet shallower KiDS-$i$-800 spans a wide range of observing conditions. The overlapping KiDS-$i$-800 and KiDS-$r$-450 imaging therefore provides a unique opportunity to assess the robustness of weak lensing measurements. In our analysis, we introduce two new `null' tests. The `nulled' two-point shear correlation function uses a matched catalogue to show that the calibrated KiDS-$i$-800 and KiDS-$r$-450 shear measurements agree at the level of $1 \pm 4$\%. We use five galaxy lens samples to determine a `nulled' galaxy-galaxy lensing signal from the full KiDS-$i$-800 and KiDS-$r$-450 surveys and find that the measurements agree to $7 \pm 5$\% when the KiDS-$i$-800 source redshift distribution is calibrated using either spectroscopic redshifts, or the 30-band photometric redshifts from the COSMOS survey., Comment: 24 pages, 20 figures. Submitted to MNRAS. Comments welcome

Published
2017
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49. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., De Rosa, R., DeSalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., MacDonald, T., Machenschalk, B., MacInnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., McCarthy, R., McClelland, D. E., McCormick, S., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McWilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. 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Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492

Published
2016
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50. Experimental setup and procedure for the measurement of the 7Be(n,{\alpha}){\alpha} reaction at n_TOF

Author

Cosentino, L., Musumarra, A., Barbagallo, M., Pappalardo, A., Colonna, N., Damone, L., Piscopo, M., Finocchiaro, P., Maugeri, E., Heinitz, S., Schumann, D., Dressler, R., Kivel, N., Aberle, O., Andrzejewski, J., Audouin, L., Ayranov, M., Bacak, M., Barros, S., Balibrea-Correa, J., Beecares, V., Becvar, F., Beinrucker, C., Berthoumieux, E., Billowes, J., Bosnar, D., Brugger, M., Caamano, M., Calviani, M., Calvino, F., Cano-Ott, D., Cardella, R., Casanovas, A., Castelluccio, D. M., Cerutti, F., Chen, Y. H., Chiaveri, E., Cortes, G., Cortes-Giraldo, M. A., Diakaki, M., Domingo-Pardo, C., Dupont, E., Duran, I., Fernandez-Dominguez, B., Ferrari, A., Ferreira, P., Furman, W., Ganesan, S., Garcia-Rios, A., Gawlik, A., Gheorghe, I., Glodariu, T., Goebel, K., Goncalves, I. F., Gonzalez-Romero, E., Griesmayer, E., Guerrero, C., Gunsing, F., Harada, H., Heftrich, T., Heyse, J., Jenkins, D. G., Jericha, E., Kaeppeler, F., Katabuchi, T., Kavrigin, P., Kimura, A., Kokkoris, M., Krticka, M., Leal-Chidonca, E., Lerendegui, J., Lederer, C., Leeb, H., Meo, S. Lo, Lonsdale, S., Losito, R., Macina, D., Marganiec, J., Martinez, T., Massimi, C., Mastinu, P., Mastromarco, M., Matteucci, F., Mazzone, A., Mendoza, E., Mengoni, A., Milazzo, P. M., Mingrone, F., Mirea, M., Montesano, S., Nolte, R., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Praena, J., Quesada, J., Rajeev, K., Rauscher, T., Reifarth, R., Riego-Perez, A., Rout, P., Rubbia, C., Ryan, J., Sabate-Gilarte, M., Saxena, A., Schillebeeckx, P., Schmidt, S., Sedyshev, P., Stamatopoulos, A., Tagliente, G., Tain, J. L., Tarifeno-Saldivia, A., Tassan-Got, L., Tsinganis, A., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Vollaire, J., Wallner, A., Warren, S., Weigand, M., Weiß, C., Wolf, C., Woods, P. J., Wright, T., Zugec, P., and collaboration, n_TOF

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment, Nuclear Experiment
Abstract

The newly built second experimental area EAR2 of the n_TOF spallation neutron source at CERN allows to perform (n, charged particles) experiments on short-lived highly radioactive targets. This paper describes a detection apparatus and the experimental procedure for the determination of the cross-section of the 7Be(n,{\alpha}) reaction, which represents one of the focal points toward the solution of the cosmological Lithium abundance problem, and whose only measurement, at thermal energy, dates back to 1963. The apparently unsurmountable experimental difficulties stemming from the huge 7Be {\gamma}-activity, along with the lack of a suitable neutron beam facility, had so far prevented further measurements. The detection system is subject to considerable radiation damage, but is capable of disentangling the rare reaction signals from the very high background. This newly developed setup could likely be useful also to study other challenging reactions requiring the detectors to be installed directly in the neutron beam., Comment: submitted to Nuclear Instruments and Methods in Physics Research A

Published
2016
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