Author: "T. Wright" / Topic: 0103 physical sciences - Searchworks@Jio Institute Digital Library Search Results

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1. Concepts for future missions to search for technosignatures

Author: Ravi Kumar Kopparapu, James Benford, Ross Davis, Jason T. Wright, Jacob Haqq-Misra, and Hector Socas-Navarro
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), 020301 aerospace & aeronautics, Computer science, Scale (chemistry), FOS: Physical sciences, Aerospace Engineering, 02 engineering and technology, Space (commercial competition), 01 natural sciences, Data science, Astrophysics - Solar and Stellar Astrophysics, 0203 mechanical engineering, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Set (psychology), Optimal methods, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Search for extraterrestrial intelligence, Astrophysics - Earth and Planetary Astrophysics
Abstract: New and unique opportunities now exist to look for technosignatures (TS) beyond traditional SETI radio searches, motivated by tremendous advances in exoplanet science and observing capabilities in recent years. Space agencies, both public and private, may be particularly interested in learning about the community's views as to the optimal methods for future TS searches with current or forthcoming technology. This report is an effort in that direction. We put forward a set of possible mission concepts designed to search for TS, although the data supplied by such missions would also benefit other areas of astrophysics. We introduce a novel framework to analyze a broad diversity of TS in a quantitative manner. This framework is based on the concept of ichnoscale, which is a new parameter related to the scale of a TS cosmic footprint, together with the number of potential targets where such TS can be searched for, and whether or not it is continuous in time., Accepted for publication in Acta Astronautica
Published: 2021

2. The <scp>HD</scp> 217107 planetary system: Twenty years of radial velocity measurements

Author: Stephen R. Kane, Cullen H. Blake, Robert A. Wittenmyer, Samson A. Johnson, David H. Sliski, Jason T. Wright, Audrey Houghton, Maurice Wilson, Mark R. Giovinazzi, Jonathan Horner, Nate McCrady, Joseph P. Glaser, John Asher Johnson, Peter Plavchan, Jason D. Eastman, and Juliana Garcia-Mejia
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics, Planetary system, 01 natural sciences, Exoplanet, Radial velocity, Orbit, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Precession, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The hot Jupiter HD 217107 b was one of the first exoplanets detected using the radial velocity (RV) method, originally reported in the literature in 1999. Today, precise RV measurements of this system span more than 20 years, and there is clear evidence for a longer-period companion, HD 217107 c. Interestingly, both the short-period planet ($P_\mathrm{b}\sim7.13$ d) and long-period planet ($P_\mathrm{c}\sim5059$ d) have significantly eccentric orbits ($e_\mathrm{b}\sim0.13$ and $e_\mathrm{c}\sim0.40$). We present 42 additional RV measurements of this system obtained with the MINERVA telescope array and carry out a joint analysis with previously published RV measurements from four different facilities. We confirm and refine the previously reported orbit of the long-period companion. HD 217107 b is one of a relatively small number of hot Jupiters with an eccentric orbit, opening up the possibility of detecting precession of the planetary orbit due to General Relativistic effects and perturbations from other planets in the system. In this case, the argument of periastron, $\omega$, is predicted to change at the level of $\sim$0.8$^\circ$ century$^{-1}$. Despite the long time baseline of our observations and the high quality of the RV measurements, we are only able to constrain the precession to be $\dot{\omega}, Comment: 8 pages, 3 figures, accepted for publication in Astronomische Nachrichten
Published: 2020

3. Planck frequencies as Schelling points in SETI

Author: Jason T. Wright
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Planck energy, 010504 meteorology & atmospheric sciences, Physics and Astronomy (miscellaneous), Electromagnetic spectrum, Transmitter, FOS: Physical sciences, Context (language use), 01 natural sciences, symbols.namesake, Theoretical physics, Frequency comb, Space and Planetary Science, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), symbols, Planck, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Game theory, Ecology, Evolution, Behavior and Systematics, Search for extraterrestrial intelligence, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: In SETI, when searching for "beacons" -- transmissions intended for us and meant to get our attention -- one must guess the appropriate frequency to search by considering what frequencies would be universally obvious to other species. This is a well known concept in game theory, where such solutions to a non-communicative cooperative game (such as a mutual search) are called "Schelling points." It is noteworthy, therefore, that when developing his eponymous units, Planck called them "natural" because they "remain meaningful for all times and also for extraterrestrial and non-human cultures." Here, I apply Planck's suggestion in the context of Schelling points in SETI with a "Planck Frequency Comb," constructed by multiplying the Planck energy by integer powers of the fine structure constant. This comb includes a small number of frequencies in regions of the electromagnetic spectrum where laser and radio SETI typically operates. Searches might proceed and individual teeth in the comb, or at many teeth at once, across the electromagnetic spectrum. Indeed, the latter strategy can be additionally justified by the transmitter's desire to signal at many frequencies at once, to improve the chances that the receiver will guess one of them correctly. There are many arbitrary and anthropocentric choices in this comb's construction, and indeed one can construct several different frequency combs with only minor and arbitrary modifications. This suggests that it may be fruitful to search for signals arriving in frequency combs of arbitrary spacing. And even though the frequencies suggested here are only debatably "better" than others proposed, the addition of the Planck Frequency Comb to the list of "magic frequencies" can only help searches for extraterrestrial beacons., Comment: 14 tables, 5 tables, accepted to the International Journal of Astrobiology. v4. Has minor language corrections and a correction to equations 5 and 7, and proper number of significant figures in the tables. v5. adds a relevant reference
Published: 2020

4. Measurement of the charge asymmetry of electrons from the decays of W bosons produced in pp¯ collisions at s=1.96 TeV

Author: M. Kurata, Andrew Ivanov, Daniela Bortoletto, P. E. Karchin, A. Castro, V. Thukral, D. Goldin, G. Piacentino, M. Kambeitz, J. Keung, A. Mukherjee, Pavol Bartos, G. Manca, T. A. Schwarz, Monica D'Onofrio, M. Rescigno, Justin Pilot, Rainer Wallny, Mario Campanelli, V. V. Glagolev, H. Gerberich, G. Chlachidze, B. Auerbach, S. Donati, R. F. Harr, K. R. Bland, Kenichi Hatakeyama, D. Tonelli, T. Yang, Y. C. Yang, C. Paus, M. Franklin, Chris Hays, A. Semenov, Mark Kruse, Alison Lister, C. Plager, J. Nett, Stefano Giagu, J. D. Lewis, Hirokazu Miyake, S. Amerio, Alberto Annovi, T. Tomura, Jian Tang, P. Garosi, I. Redondo Fernández, O. Norniella, R. Vilar, C. M. Ginsburg, J. E. Kim, S. H. Kim, K. K. Joo, Scott Wilbur, Nicola D'Ascenzo, J. A. Appel, M. J. Shochet, A. Hocker, J. S. Conway, M. Iori, C. Pagliarone, T. Rodriguez, Javier Cuevas, Hong Ye Song, A. Simonenko, G. Pauletta, V. A. Giakoumopoulou, Virgil E Barnes, G. Volpi, Gervasio Gomez, D. W. Jang, V. Papadimitriou, J. C. Freeman, P. F. Shepard, S. H. Oh, P. J. Bussey, D. Waters, B. Di Ruzza, A. Ruiz, Adrian Buzatu, Y. Nagai, D. J. Cox, C. Galloni, T. Nigmanov, M. Gold, Koji Yamamoto, Ulrich Husemann, A. Manousakis-Katsikakis, N. Moggi, P. K. Teng, Matthew Jones, D. Yamato, A. Savoy-Navarro, Yuji Sudo, Andrew Beretvas, Giuseppe Latino, D. Mietlicki, Jonathan L. Rosner, T. Miao, D. Chokheli, G. Punzi, Itsuo Nakano, I. Yu, Alan Garfinkel, Marcelo Vogel, Fabrizio Margaroli, J. R. Smith, P. Schlabach, P. Totaro, B. Jayatilaka, Henry J. Frisch, K. Gibson, Matteo Cremonesi, Fumihiko Ukegawa, Xin Wu, Th. Müller, K. Sliwa, J. N. Bellinger, Y. D. Oh, G. Flanagan, D. Torretta, Viviana Cavaliere, T. Wright, T. Aaltonen, L. Ristori, Y. Takeuchi, W.F. Badgett, Peter Wagner, W. Ashmanskas, S. Lockwitz, Sudhir Malik, M. Vidal, Marco Trovato, H. S. Budd, W. Parker, L. Brigliadori, Keunchang Cho, A. Elagin, A. Bocci, Jay Dittmann, Stephan Lammel, E. J. Jeon, T. Kuhr, F. Canelli, K. Takemasa, V. Saveliev, S. Moed, Kiminori Kondo, M. J. Kim, M. M. Deninno, D. H. Kim, A. Loginov, A. B. Wicklund, Erik Brücken, E. E. Schmidt, A. Cerri, D. Stentz, H. S. Kim, W. Ketchum, E. Thomson, J. Antos, Prabhakar Palni, C. Mesropian, S. Y. Noh, Kazuhiko Hara, S. Carrillo, E. Gramellini, Giovanni Bellettini, M. E. Mattson, S. R. Hahn, E. Palencia, F. Vázquez, A. Di Canto, Maxim Goncharov, J. Asaadi, E. James, Naoki Kimura, A. Kasmi, V. Vecchio, L. Demortier, O. Gonzalez Lopez, S. Leo, A. Mazzacane, J. Vizán, Luca Scodellaro, V. Rusu, M. Lancaster, S. Torre, Fedor Prokoshin, Sandra Leone, A. R. Clark, P. Giromini, Koji Sato, Anna Zanetti, Chen Zhou, J. Lueck, Peter Wittich, P. B. Renton, M. Mussini, Stefano Camarda, T. Harrington-Taber, Y. Zeng, K. Matera, T. Okusawa, L. Pondrom, S. Z. Shalhout, A. Mitra, W. C. Wester, R. Forrest, Y. Seiya, R. McNulty, M. Hare, A. Sukhanov, Sally Seidel, Federico Sforza, Manfred Paulini, G.V. Velev, D. Cruz, W. K. Sakumoto, M. H. Kirby, Elisabetta Pianori, Jane Nachtman, S. Wolbers, A. Pranko, Kevin Burkett, M. Tecchio, James Russ, Kohei Yorita, Stefano Zucchelli, Maxwell Chertok, Caterina Vernieri, Kai Yi, J. Huston, Luigi Marchese, H. Wolfmeister, Y. Sakurai, Michal Kreps, C. Grosso-Pilcher, Y. K. Kim, D. Lucchesi, J. Lys, R. Roser, Ryan Christopher Edgar, P. Murat, T. Liu, M. Shimojima, Fabrizio Scuri, A. Driutti, John Strologas, Lucio Cerrito, L. Nodulman, P. Marino, F. Devoto, Ziqing Hong, Roger Moore, Paul Wilson, Duncan Carlsmith, F. Ptohos, H. H. Williams, Q. Liu, L. B. Oakes, M. J. Morello, F. D. Snider, R. St. Denis, K. Ebina, A. Boveia, J. Y. Han, J. Boudreau, G. P. Yeh, G. Introzzi, A. Robson, R. Orava, A. Anastassov, Christopher Clarke, Walter Hopkins, G. Lungu, A. Napier, Rodolfo Carosi, S. M. Wang, A. T. Laasanen, C. A. Cox, T. Bae, R. D. Field, K. Potamianos, A. Artikov, F. Azfar, Tomoko Yoshida, Sergo Jindariani, U. K. Yang, T. J. Phillips, S. B. Kim, J. S. H. Lee, A. Isgrò, J. Kroll, R. Culbertson, F. Happacher, Matthew Herndon, Andrea Di Luca, J. Budagov, A. Bhatti, S. Rolli, Benjamin Kilminster, Barry Blumenfeld, Roman Lysak, I. Suslov, Sinead Farrington, S. Uozumi, K. Goulianos, Manfredi Ronzani, Aristotle Calamba, S. Poprocki, D. J. Kong, C. Vellidis, J. P. Fernández Ramos, P. de Barbaro, B. Carls, V. Sorin, Franco Bedeschi, P. Lukens, A. Bodek, D. Toback, M. Stancari, Yongsun Kim, A. Golossanov, M. Corbo, Y. C. Chen, S. Tokar, L. Santi, Giorgio Chiarelli, Emanuele Michielin, Mahmoud I. Hussein, Patrizia Barria, B. A. Barnett, T. R. Junk, Teruki Kamon, P. Mazzanti, Bruno Casal, D. Cauz, P. Mehtala, E. Gerchtein, J. Yoh, S. Y. Jun, Matteo Bauce, Antonio Limosani, Robin Erbacher, M. Datta, W-M. Yao, A. T. Goshaw, C. S. Moon, M. Cordelli, G. Busetto, Brian L Winer, D. Glenzinski, S. R. Hou, S. Errede, R. Madrak, J. Naganoma, Giorgio Apollinari, F. Rimondi, Tetsuo Arisawa, B. Esham, D. P. Benjamin, Joachim Heinrich, A. K. Mehta, G. B. Yu, S. Behari, Y. Funakoshi, Y. Kato, J. Guimaraes Da Costa, K. T. Pitts, I. V. Gorelov, Zhenbin Wu, K. Tollefson, Pierfrancesco Butti, A. V. Kotwal, I. Shreyber-Tecker, D. Amidei, Jacobo Konigsberg, Elliot Lipeles, R. E. Hughes, Daniel Whiteson, F. Ruffini, A. Aurisano, J. S. Wilson, N. Giokaris, J. Thom, Kevin Lannon, M. D'Errico, M. E. Convery, Guillelmo Gomez-Ceballos, L. Ortolan, Paul Lujan, Massimo Casarsa, M. Dorigo, P. Catastini, C. Bromberg, A. Barbaro-Galtieri, T. G. Shears, H. S. Lee, and Paolo Maestro
Subjects: Physics, Particle physics, Proton, 010308 nuclear & particles physics, media_common.quotation_subject, High Energy Physics::Phenomenology, Tevatron, Parton, 7. Clean energy, 01 natural sciences, Asymmetry, law.invention, law, Pseudorapidity, 0103 physical sciences, Physics::Accelerator Physics, High Energy Physics::Experiment, Fermilab, Nuclear Experiment, 010306 general physics, Collider, Collider Detector at Fermilab, media_common
Abstract: At the Fermilab Tevatron proton-antiproton ($p\bar{p}$) collider, high-mass electron-neutrino ($e\nu$) pairs are produced predominantly in the process $p \bar{p} \rightarrow W(\rightarrow e\nu) + X$. The asymmetry of the electron and positron yield as a function of their pseudorapidity constrain the slope of the ratio of the $u$- to $d$-quark parton distributions versus the fraction of the proton momentum carried by the quarks. This paper reports on the measurement of the electron-charge asymmetry using the full data set recorded by the Collider Detector at Fermilab in 2001--2011 and corresponding to 9.1~fb$^{-1}$ of integrated luminosity. The measurement significantly improves the precision of the Tevatron constraints on the parton-distribution functions of the proton. Numerical tables of the measurement are provided.
Published: 2021

5. The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades

Author: Gregory W. Henry, Lauren M. Weiss, Howard Isaacson, Ryan A. Rubenzahl, Cayla M. Dedrick, Ilya A. Sherstyuk, Heather A. Knutson, Geoffrey W. Marcy, Lea A. Hirsch, Ian J. M. Crossfield, Ashley Chontos, Stephen R. Kane, Lee J. Rosenthal, Paul A. Dalba, Debra A. Fischer, Aida Behmard, Molly R. Kosiarek, Jason T. Wright, Justin R. Crepp, Erik A. Petigura, Sarah Blunt, Benjamin J. Fulton, and Andrew W. Howard
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Orbital elements, 010308 nuclear & particles physics, Gas giant, media_common.quotation_subject, Giant planet, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Exoplanet, Radial velocity, Stars, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Eccentricity (behavior), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present a high-precision radial velocity (RV) survey of 719 FGKM stars, which host 164 known exoplanets and 14 newly discovered or revised exoplanets and substellar companions. This catalog updated the orbital parameters of known exoplanets and long-period candidates, some of which have decades-longer observational baselines than they did upon initial detection. The newly discovered exoplanets range from warm sub-Neptunes and super-Earths to cold gas giants. We present the catalog sample selection criteria, as well as over 100,000 radial velocity measurements, which come from the Keck-HIRES, APF-Levy, and Lick-Hamilton spectrographs. We introduce the new RV search pipeline RVSearch that we used to generate our planet catalog, and we make it available to the public as an open-source Python package. This paper is the first study in a planned series that will measure exoplanet occurrence rates and compare exoplanet populations, including studies of giant planet occurrence beyond the water ice line, and eccentricity distributions to explore giant planet formation pathways. We have made public all radial velocities and associated data that we use in this catalog., Accepted to ApJS
Published: 2021

6. The California Legacy Survey II. Occurrence of Giant Planets Beyond the Ice line

Author: Debra A. Fischer, Stephen R. Kane, Cayla M. Dedrick, Geoffrey W. Marcy, Paul A. Dalba, Lauren M. Weiss, Ian Crossfield, Howard Isaacson, Ilya A. Sherstyuk, Justin R. Crepp, Ashley Chontos, Gregory W. Henry, Andrew W. Howard, Ryan A. Rubenzahl, Erik A. Petigura, Benjamin J. Fulton, Lee J. Rosenthal, Aida Behmard, Heather Knutson, Sarah Blunt, Molly R. Kosiarek, Jason T. Wright, and Lea A. Hirsch
Subjects: Physics, 05 social sciences, 050301 education, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Exoplanet, Radial velocity, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 0503 education, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We used high-precision radial velocity measurements of FGKM stars to determine the occurrence of giant planets as a function of orbital separation spanning 0.03-30 au. Giant planets are more prevalent at orbital distances of 1-10 au compared to orbits interior or exterior of this range. The increase in planet occurrence at $\sim$1 au by a factor of $\sim$4 is highly statistically significant. A fall-off in giant planet occurrence at larger orbital distances is favored over models with flat or increasing occurrence. We measure $14.1^{+2.0}_{-1.8}$ giant planets per 100 stars with semi-major axes of 2-8 au and $8.9^{+3.0}_{-2.4}$ giant planets per 100 stars in the range 8-32 au, a decrease in giant planet occurrence with increasing orbital separation that is significant at the $\sim$2$\sigma$ level. We find that the occurrence rate of sub-Jovian planets (0.1-1 Jupiter masses) is also enhanced for 1-10 au orbits. This suggests that lower mass planets may share the formation or migration mechanisms that drive the increased prevalence near the water-ice line for their Jovian counterparts. Our measurements of cold gas giant occurrence are consistent with the latest results from direct imaging surveys and gravitational lensing surveys despite different stellar samples. We corroborate previous findings that giant planet occurrence increases with stellar mass and metallicity., Comment: accepted to ApJS
Published: 2021

7. High-resolution spectroscopy of Boyajian’s star during optical dimming events

Author: Carlos González-Fernández, Sergio Simón-Díaz, Emilio Molinari, Thomas Masseron, G. Holgado, Tabetha S. Boyajian, Jason T. Wright, A. Collier Cameron, Grant M. Kennedy, J. Saario, Hector Socas-Navarro, M. J. Martínez González, B. Toledo-Padrón, J. I. González Hernández, A. Asensio Ramos, C. Westendorp Plaza, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: Epoch (astronomy), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), 01 natural sciences, circumstellar matter [Stars], 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, observational [Methods], 010303 astronomy & astrophysics, Chromosphere, Solar and Stellar Astrophysics (astro-ph.SR), QC, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, Stellar atmosphere, DAS, Astronomy and Astrophysics, Light curve, findamental parameters [Stars], Interstellar medium, Radial velocity, QC Physics, Radiative equilibrium, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, activity [Stars]
Abstract: Boyajian's star is an apparently normal main sequence F-type star with a very unusual light curve. The dipping activity of the star, discovered during the Kepler mission, presents deep, asymmetric, and aperiodic events. Here we present high resolution spectroscopic follow-up during some dimming events recorded post-Kepler observations, from ground-based telescopes. We analise data from the HERMES, HARPS-N and FIES spectrographs to characterise the stellar atmosphere and to put some constraints on the hypotheses that have appeared in the literature concerning the occulting elements. The star's magnetism, if existing, is not extreme. The spots on the surface, if present, would occupy 0.02% of the area, at most. The chromosphere, irrespective of the epoch of observation, is hotter than the values expected from radiative equilibrium, meaning that the star has some degree of activity. We find no clear evidence of the interstellar medium nor exocoments being responsible for the dimmings of the light curve. However, we detect at 1-2 sigma level, a decrease of the radial velocity of the star during the first dip recorded after the \emph{\emph{Kepler}} observations. We claim the presence of an optically thick object with likely inclined and high impact parameter orbits that produces the observed Rossiter-McLaughlin effect., Comment: submitted to MNRAS
Published: 2019

8. A Harsh Test of Far-Field Scrambling with the Habitable Zone Planet Finder and the Hobby Eberly Telescope

Author: Eric B. Ford, Samuel Halverson, Michael Endl, Chad F. Bender, Suvrath Mahadevan, William D. Cochran, Joe P. Ninan, Ryan Terrien, Steven Janowiecki, Fred Hearty, Christian Schwab, Gudmundur Stefansson, Jason T. Wright, Shubham Kanodia, Niv Drory, Lawrence W. Ramsey, Scott A. Diddams, Andrew J. Monson, Arpita Roy, Andrew J. Metcalf, and Paul Robertson
Subjects: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, 01 natural sciences, Optical telescope, Optics, Planet, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Spectrograph, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, business.industry, Centroid, Astronomy and Astrophysics, Radial velocity, 13. Climate action, Space and Planetary Science, Sky, Hobby–Eberly Telescope, business, Astrophysics - Instrumentation and Methods for Astrophysics, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Habitable zone Planet Finder (HPF) is a fiber fed precise radial velocity spectrograph at the 10 m Hobby Eberly Telescope (HET). Due to its fixed altitude design, the HET pupil changes appreciably across a track, leading to significant changes of the fiber far-field illumination. HPF's fiber scrambler is designed to suppress the impact of these illumination changes on the radial velocities -- but the residual impact on the radial velocity measurements has yet to be probed on sky. We use GJ 411, a bright early type (M2) M dwarf to probe the effects of far-field input trends due to these pupil variations on HPF radial velocities (RVs). These large changes ($\sim$ 2x) in pupil area and centroid present a harsh test of HPF's far-field scrambling. Our results show that the RVs are effectively decoupled from these extreme far-field input changes due to pupil centroid offsets, attesting to the effectiveness of the scrambler design. This experiment allows us to test the impact of these changes with large pupil variation on-sky, something we would not easily be able to do at a conventional optical telescope. While the pupil and illumination changes expected at these other telescopes are small, scaling from our results enables us to estimate and bound these effects, and show that they are controllable even for the new and next generation of RV instruments in their quest to beat down instrumental noise sources towards the goal of a few cm/s., 16 pages. Published in The Astrophysical Journal
Published: 2021

9. Target Prioritization and Observing Strategies for the NEID Earth Twin Survey

Author: Chad F. Bender, Andrew J. Monson, Cullen H. Blake, Michael W. McElwain, Ryan Terrien, Paul Robertson, Samuel Halverson, Sarah E. Logsdon, Suvrath Mahadevan, Arvind F. Gupta, Gudmundur Stefansson, Arpita Roy, Jacob K. Luhn, Shubham Kanodia, Joe P. Ninan, Eric B. Ford, Fred Hearty, Jason T. Wright, and Christian Schwab
Subjects: Prioritization, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, law, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Spectrograph, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Exoplanet, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Astrophysics - Earth and Planetary Astrophysics
Abstract: NEID is a high-resolution optical spectrograph on the WIYN 3.5-m telescope at Kitt Peak National Observatory and will soon join the new generation of extreme precision radial velocity instruments in operation around the world. We plan to use the instrument to conduct the NEID Earth Twin Survey (NETS) over the course of the next 5 years, collecting hundreds of observations of some of the nearest and brightest stars in an effort to probe the regime of Earth-mass exoplanets. Even if we take advantage of the extreme instrumental precision conferred by NEID, it will remain difficult to disentangle the weak (~10 cm s$^{-1}$) signals induced by such low-mass, long-period exoplanets from stellar noise for all but the quietest host stars. In this work, we present a set of quantitative selection metrics which we use to identify an initial NETS target list consisting of stars conducive to the detection of exoplanets in the regime of interest. We also outline a set of observing strategies with which we aim to mitigate uncertainty contributions from intrinsic stellar variability and other sources of noise., 19 pages, 10 figures, 1 table
Published: 2021

10. An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELT

Author: B. Scott Gaudi, S. Villanueva, Joseph E. Rodriguez, Allyson Bieryla, Karen A. Collins, Aaron C. Rizzuto, Michael L. Calkins, Patcharapol Wachiraphan, John F. Kielkopf, Rudolf B. Kuhn, George Zhou, Jason T. Wright, Gilbert A. Esquerdo, Michael B. Lund, P. Berlind, Adam L. Kraus, Thomas G. Beatty, Robert J. Siverd, David W. Latham, Keivan G. Stassun, Mark Manner, Daniel J. Stevens, Marshall C. Johnson, and Joshua Pepper
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Star (game theory), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Mass ratio, Light curve, 01 natural sciences, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Binary star, Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Low Mass, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of \thisstar\ (HD 58730), a very low mass ratio ($q \equiv M_2/M_1 \approx 0.07$) eclipsing binary (EB) identified by the Kilodegree Extremely Little Telescope (KELT) survey. We present the discovery light curve and perform a global analysis of four high-precision ground-based light curves, the Transiting Exoplanets Survey Satellite (TESS) light curve, radial velocity (RV) measurements, Doppler Tomography (DT) measurements, and the broad-band spectral energy distribution (SED). Results from the global analysis are consistent with a fully convective ($M_2 = 0.22 \pm 0.02\ M_{\odot})$ M star transiting a late-B primary ($M_1 = 3.34^{+0.07}_{-0.09}\ M_{\odot};\ T_{\rm eff,1} = 11960^{+430}_{-520}\ {\rm K}$). We infer that the primary star is $183_{-30}^{+33}$ Myr old and that the companion star's radius is inflated by $26 \pm 8\%$ relative to the predicted value from a low-mass isochrone of similar age. We separately and analytically fit for the variability in the out-of-eclipse TESS phase curve, finding good agreement between the resulting stellar parameters and those from the global fit. Such systems are valuable for testing theories of binary star formation and understanding how the environment of a star in a close-but-detached binary affects its physical properties. In particular, we examine how a star's properties in such a binary might differ from the properties it would have in isolation., Comment: 19 pages, 12 figures, accepted to MNRAS
Published: 2020

11. The Habitable-zone Planet Finder Reveals A High Mass and a Low Obliquity for the Young Neptune K2-25b

Author: Jayadev Rajagopal, Flynn Haase, Christian Schwab, Andrew J. Metcalf, Eric B. Ford, Suvrath Mahadevan, Paul Robertson, William D. Cochran, Arpita Roy, Lori Allen, Chad F. Bender, Samuel Halverson, Rebekah I. Dawson, Scott A. Diddams, Gudmundur Stefansson, Joe P. Ninan, Ryan Terrien, Marissa Maney, Angie Wolfgang, Lawrence W. Ramsey, Eric Levi, Andrew J. Monson, Connor Fredrick, Fred Hearty, Shubham Kanodia, Caleb I. Cañas, Joshua N. Winn, John P. Wisniewski, Jason T. Wright, and Leslie Hebb
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Planetary system, Light curve, 01 natural sciences, Radial velocity, Photometry (optics), Space and Planetary Science, Neptune, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Circumstellar habitable zone, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Using radial-velocity data from the Habitable-zone Planet Finder, we have measured the mass of the Neptune-sized planet K2-25b, as well as the obliquity of its M4.5-dwarf host star in the 600-800MYr Hyades cluster. This is one of the youngest planetary systems for which both of these quantities have been measured, and one of the very few M dwarfs with a measured obliquity. Based on a joint analysis of the radial velocity data, time-series photometry from the K2 mission, and new transit light curves obtained with diffuser-assisted photometry, the planet's radius and mass are $3.44\pm 0.12 \mathrm{R_\oplus}$ and $24.5_{-5.2}^{+5.7} \mathrm{M_\oplus}$. These properties are compatible with a rocky core enshrouded by a thin hydrogen-helium atmosphere (5% by mass). We measure an orbital eccentricity of $e=0.43 \pm 0.05$. The sky-projected stellar obliquity is $\lambda=3 \pm 16^{\circ}$, compatible with spin-orbit alignment, in contrast to other "hot Neptunes" that have been studied around older stars., Comment: Accepted for publication in AJ, 31 pages, 14 figures
Published: 2020

12. A warm Jupiter transiting an M dwarf: A TESS single transit event confirmed with the Habitable-zone Planet Finder

Author: Mark E. Everett, Samuel Halverson, Jayadev Rajagopal, Robert F. Wilson, Gudmundur Stefansson, Fred Hearty, Arpita Roy, Hannah M. Lewis, Arvind F. Gupta, Rebekah I. Dawson, Andrew J. Monson, William D. Cochran, Jason T. Wright, Christian Schwab, Mary Brewer, Scott A. Diddams, Ryan Terrien, Lawrence W. Ramsey, Suvrath Mahadevan, Connor Fredrick, Andrew J. Metcalf, Chad F. Bender, Andrea S. J. Lin, Eric B. Ford, Paul Robertson, Caleb I. Cañas, Corey Beard, Leslie Hebb, Steven R. Majewski, Joe P. Ninan, Shubham Kanodia, Michael Endl, and Jack Lubin
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Gas giant, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Exoplanet, Photometry (optics), Orbit, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Circumstellar habitable zone, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We confirm the planetary nature of a warm Jupiter transiting the early M dwarf TOI-1899, using a combination of available TESS photometry; high-precision, near-infrared spectroscopy with the Habitable-zone Planet Finder; and speckle and adaptive optics imaging. The data reveal a transiting companion on an $\sim29$-day orbit with a mass and radius of $0.66\pm0.07\ \mathrm{M_{J}}$ and $1.15_{-0.05}^{+0.04}\ \mathrm{R_{J}}$, respectively. The star TOI-1899 is the lowest-mass star known to host a transiting warm Jupiter, and we discuss the follow-up opportunities afforded by a warm ($\mathrm{T_{eq}}\sim362$ K) gas giant orbiting an M0 star. Our observations reveal that TOI-1899.01 is a puffy warm Jupiter, and we suggest additional transit observations to both refine the orbit and constrain the true dilution observed in TESS., 24 pages, 5 figures, 3 tables, published in AJ
Published: 2020

13. Measurement of the 154Gd(n,γ) cross section and its astrophysical implications

Author: Z. Talip, A. S. Brown, J. Lerendegui-Marco, S. Amaducci, Alexandru Negret, P. Vaz, F. Käppeler, A. Masi, R. Wynants, Alberto Ventura, D. G. Jenkins, M. Sabaté-Gilarte, E. Mendoza, A. Kimura, G. Vannini, O. Aberle, V. Babiano-Suarez, Stefan Kopecky, A. Manna, A. Pavlik, A. Stamatopoulos, M. Diakaki, M. Mastromarco, C. Domingo-Pardo, V. Variale, Dimitri Rochman, S. Heinitz, M. A. Cortés-Giraldo, Z. Eleme, Emilio Andrea Maugeri, M. Kokkoris, Anton Wallner, D. Macina, B. Fernández-Domíngez, E. Jericha, S. Urlass, Mario Barbagallo, Alfredo Ferrari, Paolo Finocchiaro, Maurizio Busso, G. Alaerts, A. Oprea, J. Heyse, D. M. Castelluccio, R. Mucciola, F. Calviño, D. Schumann, Ariel Tarifeño-Saldivia, S. J. Lonsdale, A. Musumarra, G. Cortes, E. Chiaveri, D. Cano-Ott, I. Ferro-Gonçalves, P. M. Milazzo, Ignacio Porras, Rene Reifarth, Giulia Clai, S. Valenta, A. Gawlik, N. Patronis, P. Schillebeeckx, Javier Praena, S. Lo Meo, Carlos Guerrero, J. Perkowski, P. Torres-Sánchez, F. Bečvář, A. Saxena, Marco Calviani, Alberto Mengoni, I. Ladarescu, A. G. Smith, R. Garg, J. Billowes, J. M. Quesada, E. González-Romero, L. Tassan-Got, F. Gunsing, Francesca Matteucci, I. Duran, M. Dietz, Diego Vescovi, Sergio Cristallo, F. Mingrone, J. Andrzejewski, Cristian Massimi, Philip Woods, V. Bécares, L. Caballero, Claudia Lederer-Woods, R. Dressler, V. Vlachoudis, R. Vlastou, Ralf Nolte, M. Caamaño, Deniz Kurtulgil, L. A. Damone, Damir Bosnar, Y. Kadi, K. Göbel, F. Cerutti, V. Alcayne, T. Wright, V. Furman, Y. Kopatch, N. V. Sosnin, Simone Gilardoni, Annamaria Mazzone, Petar Žugec, J. Ulrich, D. Radeck, E. Berthoumieux, J. L. Tain, Niko Kivel, G. Bellia, F. Ogállar, Y. H. Chen, C. Rubbia, G. Tagliente, D. Ramos Doval, A. Casanovas, L. Cosentino, P. F. Mastinu, M. Krtička, T. Martinez, A. Tsinganis, Luciano Piersanti, Nicola Colonna, E. Dupont, M. Bacak, T. Glodariu, L. Audouin, V. Michalopoulou, ITA, GBR, FRA, DEU, ESP, AUT, BEL, HRV, JPN, GRC, IND, POL, CZE, CHE, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, n_TOF, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. Doctorat en Enginyeria Nuclear i de les Radiacions Ionitzants, Universitat Politècnica de Catalunya. Institut de Tècniques Energètiques, Universitat Politècnica de Catalunya. ANT - Advanced Nuclear Technologies Research Group, 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), Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Mazzone, A., Cristallo, S., Aberle, O., Alaerts, G., Alcayne, V., Amaducci, S., Andrzejewski, J., Audouin, L., Babiano-Suarez, V., Bacak, M., Barbagallo, M., Becares, V., Becvar, F., Bellia, G., Berthoumieux, E., Billowes, J., Bosnar, D., Brown, A. S., Busso, M., Caamano, M., Caballero, L., Calviani, M., Calvino, F., Cano-Ott, D., Casanovas, A., Castelluccio, D. M., Cerutti, F., Chen, Y. H., Chiaveri, E., Clai, G., Colonna, N., Cortes, G. P., Cortes-Giraldo, M. A., Cosentino, L., Damone, L. A., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Eleme, Z., Fernandez-Domingez, B., Ferrari, A., Ferro-Goncalves, I., Finocchiaro, P., Furman, V., Garg, R., Gawlik, A., Gilardoni, S., Glodariu, T., Gobel, K., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Heinitz, S., Heyse, J., Jenkins, D. G., Jericha, E., Kadi, Y., Kappeler, F., Kimura, A., Kivel, N., Kokkoris, M., Kopatch, Y., Kopecky, S., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lo Meo, S., Lonsdale, S. -J., Macina, D., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P. F., Mastromarco, M., Matteucci, F., Maugeri, E., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mingrone, F., Mucciola, R., Musumarra, A., Negret, A., Nolte, R., Ogallar, F., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Piersanti, L., Porras, I., Praena, J., Quesada, J. M., Radeck, D., Ramos Doval, D., Reifarth, R., Rochman, D., Rubbia, C., Sabate-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Smith, A. G., Sosnin, N., Stamatopoulos, A., Tagliente, G., Tain, J. L., Talip, Z., Tarifeno-Saldivia, A. E., Tassan-Got, L., Torres-Sanchez, 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., Wynants, R., Wright, T. J., Zugec, P., Mazzone A., Cristallo S., Aberle O., Alaerts G., Alcayne V., Amaducci S., Andrzejewski J., Audouin L., Babiano-Suarez V., Bacak M., Barbagallo M., Becares V., Becvar F., Bellia G., Berthoumieux E., Billowes J., Bosnar D., Brown A.S., Busso M., Caamano M., Caballero L., Calviani M., Calvino F., Cano-Ott D., Casanovas A., Castelluccio D.M., Cerutti F., Chen Y.H., Chiaveri E., Clai G., Colonna N., Cortes G.P., Cortes-Giraldo M.A., Cosentino L., Damone L.A., Diakaki M., Dietz M., Domingo-Pardo C., Dressler R., Dupont E., Duran I., Eleme Z., Fernandez-Domingez B., Ferrari A., Ferro-Goncalves I., Finocchiaro P., Furman V., Garg R., Gawlik A., Gilardoni S., Glodariu T., Gobel K., Gonzalez-Romero E., Guerrero C., Gunsing F., Heinitz S., Heyse J., Jenkins D.G., Jericha E., Kadi Y., Kappeler F., Kimura A., Kivel N., Kokkoris M., Kopatch Y., Kopecky S., Krticka M., Kurtulgil D., Ladarescu I., Lederer-Woods C., Lerendegui-Marco J., Lo Meo S., Lonsdale S.-J., Macina D., Manna A., Martinez T., Masi A., Massimi C., Mastinu P.F., Mastromarco M., Matteucci F., Maugeri E., Mendoza E., Mengoni A., Michalopoulou V., Milazzo P.M., Mingrone F., Mucciola R., Musumarra A., Negret A., Nolte R., Ogallar F., Oprea A., Patronis N., Pavlik A., Perkowski J., Piersanti L., Porras I., Praena J., Quesada J.M., Radeck D., Ramos Doval D., Reifarth R., Rochman D., Rubbia C., Sabate-Gilarte M., Saxena A., Schillebeeckx P., Schumann D., Smith A.G., Sosnin N., Stamatopoulos A., Tagliente G., Tain J.L., Talip Z., Tarifeno-Saldivia A.E., Tassan-Got L., Torres-Sanchez 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., Wynants R., Wright T.J., and Zugec P.
Subjects: Nuclear and High Energy Physics, Gd, Neutron time of flight, Física::Física de partícules [Àrees temàtiques de la UPC], Nuclear physics, Neutrons--Captura, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], nucl-ex, Neutron time of flightn, 01 natural sciences, 7. Clean energy, Neutrons--Capture, Cross section (physics), Nucleosynthesis, ComputingMethodologies_SYMBOLICANDALGEBRAICMANIPULATION, 0103 physical sciences, Neutron cross section, ddc:530, Nuclear Physics - Experiment, Spallation, Neutron, n_TOF, Nuclear Experiment, 010306 general physics, 154Gd, Physics, Scintillation, 154 Gd, Física [Àrees temàtiques de la UPC], 010308 nuclear & particles physics, s process, Atmospheric temperature range, lcsh:QC1-999, NATURAL SCIENCES. Physics, PRIRODNE ZNANOSTI. Fizika, Neutron time-of-flight, Física nuclear, s-process, lcsh:Physics
Abstract: The isotope used in this research was supplied by the United States Department of Energy Office of Science by the Isotope Program in the Office of Nuclear Physics., The neutron capture cross section of 154Gd was measured from 1 eV to 300 keV in the experimental area located 185 m from the CERN n_TOF neutron spallation source, using a metallic sample of gadolinium, enriched to 67% in 154Gd. The capture measurement, performed with four C6D6 scintillation detectors, has been complemented by a transmission measurement performed at the GELINA time-of-flight facility (JRC-Geel), thus minimising the uncertainty related to sample composition. An accurate Maxwellian averaged capture cross section (MACS) was deduced over the temperature range of interest for s process nucleosynthesis modelling. We report a value of 880(50) mb for the MACS at kT = 30 keV, significantly lower compared to values available in literature. The new adopted 154Gd(n,γ ) cross section reduces the discrepancy between observed and calculated solar s-only isotopic abundances predicted by s-process nucleosynthesis models., EUFRAT open access programme of the Joint Research Centre at Geel
Published: 2020

14. Properties of F Stars with Stable Radial Velocity Timeseries: A Useful Metric for Selecting Low-jitter F Stars

Author: Howard Isaacson, Jason T. Wright, and Jacob K. Luhn
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Sequence, Polynomial, 010504 meteorology & atmospheric sciences, Oscillation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Metric (mathematics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Jitter, Astrophysics - Earth and Planetary Astrophysics
Abstract: In a companion paper, we have conducted an in-depth analysis of radial velocity jitter of over 600 stars, examining the astrophysical origins including stellar granulation, oscillation, and magnetic activity. In this paper, we highlight a subsample of those stars, specifically the main sequence and "retired" F stars -- which we refer to as "MSRF" stars -- that show low levels of RV jitter ($, 10 pages, 8 figures, published in The Astronomical Journal
Published: 2020

15. Solar Contamination in Extreme-precision Radial-velocity Measurements: Deleterious Effects and Prospects for Mitigation

Author: Cullen H. Blake, Jason T. Wright, Paul Robertson, Gudmundur Stefansson, Shubham Kanodia, Chad F. Bender, Eli Golub, Joe P. Ninan, Marsha J. Wolf, Kurt P. Jaehnig, Suvrath Mahadevan, Arpita Roy, Jayadev Rajagopal, Ryan Terrien, Kyle Kaplan, Sarah E. Logsdon, Christian Schwab, Michael W. McElwain, Andrew J. Monson, Sharon X. Wang, Arvind F. Gupta, and Samuel Halverson
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, Sky brightness, law, 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Remote sensing, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Observational error, Spectrometer, Diffuse sky radiation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: Solar contamination, due to moonlight and atmospheric scattering of sunlight, can cause systematic errors in stellar radial velocity (RV) measurements that significantly detract from the ~10 cm s−1 sensitivity required for the detection and characterization of terrestrial exoplanets in or near habitable zones of Sun-like stars. The addition of low-level spectral contamination at variable effective velocity offsets introduces systematic noise when measuring velocities using classical mask-based or template-based cross-correlation techniques. Here we present simulations estimating the range of RV measurement error induced by uncorrected scattered sunlight contamination. We explore potential correction techniques, using both simultaneous spectrometer sky fibers and broadband imaging via coherent fiber imaging bundles, that could reliably reduce this source of error to below the photon-noise limit of typical stellar observations. We discuss the limitations of these simulations, the underlying assumptions, and mitigation mechanisms. We also present and discuss the components designed and built into the NEID (NN-EXPLORE Exoplanet Investigations with Doppler spectroscopy) precision RV instrument for the WIYN 3.5 m telescope, to serve as an ongoing resource for the community to explore and evaluate correction techniques. We emphasize that while "bright time" has been traditionally adequate for RV science, the goal of 10 cm s−1 precision on the most interesting exoplanetary systems may necessitate access to darker skies for these next-generation instruments.
Published: 2020

16. A compact fission detector for fission-tagging neutron capture experiments with radioactive fissile isotopes

Author: D. Macina, A. Musumarra, K. Göbel, M. Sabaté-Gilarte, E. Mendoza, A. Oprea, I. Knapova, N. V. Sosnin, T. Wright, J. Heyse, Rene Reifarth, N. Kivel, R. Nolte, L. Cosentino, J. Marganiec, P. F. Mastinu, P. Vaz, F. Bečvář, Annamaria Mazzone, Petar Žugec, M. Aiche, I. Duran, Stefan Kopecky, A. Saxena, A. Kimura, Alberto Ventura, G. Vannini, S. Valenta, Nicola Colonna, M. Kokkoris, M. A. Cortés-Giraldo, P. M. Milazzo, R. Dressler, P. Kavrigin, E. Dupont, Carlos Guerrero, G. Sibbens, M. Mastromarco, Marco Calviani, B. Laurent, E. González-Romero, P. Ferreira, Mario Barbagallo, L. Audouin, M. Krtička, A. Pavlik, A. G. Smith, J. Billowes, D. Schumann, E. Griesmayer, Anton Wallner, Alexandru Negret, G. Cortes, C. Domingo-Pardo, G. Tagliente, M. Bacak, L. A. Damone, F. Käppeler, J. Balibrea, Philip Woods, O. Aberle, D. Vanleeuw, F. Mingrone, J. Andrzejewski, F. Calviño, H. Leeb, E. A. Maugeri, A. Kalamara, T. Martinez, C. Weiss, R. Vlastou, Olivier Serot, Carlo Rubbia, V. Vlachoudis, J. Perkowski, M. Diakaki, D. Radeck, Alfredo Ferrari, E. Berthoumieux, Stephan Richter, P. Schillebeeckx, S. Warren, F. Gunsing, A. Masi, Damir Bosnar, Y. Kadi, A. Manna, Hideo Harada, Deniz Kurtulgil, V. Variale, D. G. Jenkins, Y. H. Chen, Cristian Massimi, P. V. Sedyshev, G. Belier, S. Heinitz, V. Furman, A. Stamatopoulos, E. Chiaveri, D. Cano-Ott, A. S. Brown, A. Casanovas, C. Lederer, E. Jericha, T. Glodariu, Paolo Finocchiaro, J. M. Quesada, L. Tassan-Got, A. Moens, J. A. Ryan, S. Amaducci, Simone Gilardoni, R. Cardella, Javier Praena, S. Lo Meo, M. Caamaño, F. Cerutti, B. Fernández-Domínguez, J. L. Tain, J. Taieb, L. Mathieu, E. Leal-Cidoncha, A. Gawlik, Thomas Rauscher, A. R. García, Ariel Tarifeño-Saldivia, S. J. Lonsdale, Ignacio Porras, J. Lerendegui-Marco, I. F. Gonçalves, N. Patronis, Alberto Mengoni, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Bacak, M., Aiche, M., Belier, G., Berthoumieux, E., Diakaki, M., Dupont, E., Gunsing, F., Heyse, J., Kopecky, S., Laurent, B., Leeb, H., Mathieu, L., Moens, A., Richter, S., Schillebeeckx, P., Serot, O., Sibbens, G., Taieb, J., Vanleeuw, D., Vlachoudis, V., Aberle, O., Amaducci, S., Andrzejewski, J., Audouin, L., Balibrea, J., Barbagallo, M., Becvar, F., 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., Damone, L. A., Domingo-Pardo, C., Dressler, R., Duran, I., Fernandez-Dominguez, B., Ferrari, A., Ferreira, P., 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., Harada, H., Heinitz, S., Jenkins, D. G., Jericha, E., Kappeler, F., Kadi, Y., Kalamara, A., Kavrigin, P., Kimura, A., Kivel, N., Knapova, I., Kokkoris, M., Krticka, M., Kurtulgil, D., Leal-Cidoncha, E., Lederer, C., Lerendegui-Marco, J., Lo Meo, S., Lonsdale, S. J., 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., 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., Vlastou, R., Wallner, A., Warren, S., Weiss, C., Woods, P. J., Wright, T., Zugec, P., Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. Doctorat en Enginyeria Nuclear i de les Radiacions Ionitzants, Universitat Politècnica de Catalunya. Institut de Tècniques Energètiques, Universitat Politècnica de Catalunya. ANT - Advanced Nuclear Technologies Research Group, Bacak M., Aiche M., Belier G., Berthoumieux E., Diakaki M., Dupont E., Gunsing F., Heyse J., Kopecky S., Laurent B., Leeb H., Mathieu L., Moens A., Richter S., Schillebeeckx P., Serot O., Sibbens G., Taieb J., Vanleeuw D., Vlachoudis V., Aberle O., Amaducci S., Andrzejewski J., Audouin L., Balibrea J., Barbagallo M., Becvar F., 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., Damone L.A., Domingo-Pardo C., Dressler R., Duran I., Fernandez-Dominguez B., Ferrari A., Ferreira P., 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., Harada H., Heinitz S., Jenkins D.G., Jericha E., Kappeler F., Kadi Y., Kalamara A., Kavrigin P., Kimura A., Kivel N., Knapova I., Kokkoris M., Krticka M., Kurtulgil D., Leal-Cidoncha E., Lederer C., Lerendegui-Marco J., Lo Meo S., Lonsdale S.J., 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., 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., Vlastou R., Wallner A., Warren S., Weiss C., Woods P.J., Wright T., and Zugec P.
Subjects: Nuclear and High Energy Physics, Fission, Physics::Instrumentation and Detectors, Nuclear Theory, Física::Física de partícules [Àrees temàtiques de la UPC], Nuclear physics, Context (language use), Neutrons--Captura, 01 natural sciences, 7. Clean energy, Neutrons--Capture, 0103 physical sciences, Physics::Atomic and Molecular Clusters, 233 U, ddc:530, n_TOF, 010306 general physics, Nuclear Experiment, Instrumentation, Energies::Energia nuclear [Àrees temàtiques de la UPC], Physics, [PHYS]Physics [physics], Fission detector, 233U, Time-of-flight, Física [Àrees temàtiques de la UPC], Fissile material, 010308 nuclear & particles physics, Detector, Neutron radiation, Fast fission, NATURAL SCIENCES. Physics, Calorimeter, PRIRODNE ZNANOSTI. Fizika, Neutron capture, 13. Climate action, Física nuclear, Other
Abstract: In the measurement of neutron capture cross-sections of fissile isotopes, the fission channel is a source of background which can be removed efficiently using the so-called fission-tagging or fission-veto technique. For this purpose a new compact and fast fission chamber has been developed. The design criteria and technical description of the chamber are given within the context of a measurement of the 233U(n, ��) cross-section at the n_TOF facility at CERN, where it was coupled to the n_TOF Total Absorption Calorimeter. For this measurement the fission detector was optimized for time resolution, minimization of material in the neutron beam and for alpha-fission discrimination. The performance of the fission chamber and its application as a fission tagging detector are discussed., This work was partially supported by the French NEEDS/NACRE Project and by the European Commission within HORIZON2020 via the EURATOM Project EUFRAT.
Published: 2020

17. A Sub-Neptune-sized Planet Transiting the M2.5 Dwarf G 9-40: Validation with the Habitable-zone Planet Finder

Author: Jason T. Wright, Jeff Jennings, Brett M. Morris, Joe P. Ninan, Caleb I. Cañas, Shubham Kanodia, Arpita Roy, Chad F. Bender, Eric B. Ford, Scott A. Diddams, Marissa Maney, Colin Nitroy, Suvrath Mahadevan, William D. Cochran, Andrew J. Monson, Connor Fredrick, Kyle Kaplan, Ryan Terrien, Lawrence W. Ramsey, Eric Levi, Samuel Halverson, Christian Schwab, Andrew J. Metcalf, Gudmundur Stefansson, Steinn Sigurdsson, Joseph Huehnerhoff, Michael Endl, J. Christopher Clemens, Emily Lubar, Leslie Hebb, Paul Robertson, Peter Brunt, Corey Beard, Fred Hearty, and John Wisniewski
Subjects: Rotation period, 010504 meteorology & atmospheric sciences, Metallicity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Photometry (optics), Neptune, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy, Astronomy and Astrophysics, Effective temperature, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: We validate the discovery of a 2 Earth radii sub-Neptune-size planet around the nearby high proper motion M2.5-dwarf G 9-40 (EPIC 212048748), using high-precision near-infrared (NIR) radial velocity (RV) observations with the Habitable-zone Planet Finder (HPF), precision diffuser-assisted ground-based photometry with a custom narrow-band photometric filter, and adaptive optics imaging. At a distance of $d=27.9\mathrm{pc}$, G 9-40b is the second closest transiting planet discovered by K2 to date. The planet's large transit depth ($\sim$3500ppm), combined with the proximity and brightness of the host star at NIR wavelengths (J=10, K=9.2) makes G 9-40b one of the most favorable sub-Neptune-sized planet orbiting an M-dwarf for transmission spectroscopy with JWST, ARIEL, and the upcoming Extremely Large Telescopes. The star is relatively inactive with a rotation period of $\sim$29 days determined from the K2 photometry. To estimate spectroscopic stellar parameters, we describe our implementation of an empirical spectral matching algorithm using the high-resolution NIR HPF spectra. Using this algorithm, we obtain an effective temperature of $T_{\mathrm{eff}}=3404\pm73$K, and metallicity of $\mathrm{[Fe/H]}=-0.08\pm0.13$. Our RVs, when coupled with the orbital parameters derived from the transit photometry, exclude planet masses above $11.7 M_\oplus$ with 99.7% confidence assuming a circular orbit. From its radius, we predict a mass of $M=5.0^{+3.8}_{-1.9} M_\oplus$ and an RV semi-amplitude of $K=4.1^{+3.1}_{-1.6}\mathrm{m\:s^{-1}}$, making its mass measurable with current RV facilities. We urge further RV follow-up observations to precisely measure its mass, to enable precise transmission spectroscopic measurements in the future., Comment: Accepted for publication in AJ, 22 pages, 15 figures
Published: 2020

18. Review and new concepts for neutron-capture measurements of astrophysical interest

Author: M. Sabaté-Gilarte, A. Kimura, A. Segarr, J. Lerendegui-Marco, M. Krtička, T. Martinez, M. Busso, M. Mastromarco, L. Caballero, J. L. Tain, G. Tagliente, Mario Barbagallo, Z. Eleme, D. Schumann, I. Knapova, S. Bennett, B. Fernandez-Domingez, G. Vannini, P. Vaz, P. Sprung, A. Masi, F. Ogallar, A. Saxena, F. Gunsing, V. Michalopoulou, J. Heyse, A. Stamatopoulos, N. Patronis, A. Casanovas, D. G. Jenkins, Alberto Ventura, E. Jericha, E. Berthoumieux, Javier Praena, B. Thomas, A. Negret, Cristian Massimi, Alberto Mengoni, I. Ferro-Goncalves, P. J. Davies, M. A. Cortés-Giraldo, C. Rubbia, P. M. Milazzo, Paolo Finocchiaro, G. Cortes, D. R. Doval, E. Mendoza, S. Urlass, Alfredo Ferrari, J. Balibrea-Correa, J. Moreno-Soto, D. Rochman, L. Cosentino, N. V. Sosnin, A. Mazzone, M. Kokkoris, E. Maugeri, P. F. Mastinua, A. Oprea, Rene Reifarth, C. Petrone, Claudia Lederer-Woods, V. Variale, Arnd R. Junghans, P. Torres-Sanchez, A. Sekhar, M. Diakaki, U. Jiri, F. Mingrone, S. Amaducci, M. Bacak, J. M. Quesada, L. Tassan-Got, Deniz Kurtulgil, J. Andrzejewski, M. Caamaño, E. Chiaveri, V. Babiano-Suarez, D. Cano-Ott, D. Macina, F. Cerutti, V. Vlachoudis, I. Ladarescu, L. Audouin, Carlos Guerrero, L. Piersanti, A. Pavlik, A. S. Brown, R. Garg, C. Domingo-Pardo, E. González-Romero, I. Porras, Ariel Tarifeño-Saldivia, S. J. Lonsdale, M. T. Rodriguez-Gonzalez, O. Aberle, V. Furman, Y. Kopatch, A. Tsinganis, Simone Gilardoni, F. Calviño, E. Pirovano, Nicola Colonna, J. Perkowski, E. Dupont, M. A. Millán-Callado, K. Göbel, S. Cristallo, T. Wright, Diego Vescovi, F. Käppeler, A. Musumarra, R. Vlastou, Damir Bosnar, Y. Kadi, A. Manna, Q. Ducasse, S. Valenta, P. Zugec, Marco Calviani, A. G. Smith, M. Dietz, Philip Woods, Anton Wallner, P. Schillebeeckx, A. Gawlik, L. A. Damone, I. Duran, R. Dressler, V. Alcayne, 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, n_TOF, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Domingo-Pardo, C., Babiano-Suarez, V., Balibrea-Correa, J., Caballero, L., Ladarescu, I., Lerendegui-Marco, J., Tain, J. L., Calvino, F., Casanovas, A., Segarr, A., Tarifeno-Saldivia, A. E., Guerrero, C., Millan-Callado, M. A., Quesada, J. M., Rodriguez-Gonzalez, M. T., Aberle, O., Alcayne, V., Amaducci, S., Andrzejewski, J., Audouin, L., Bacak, M., Barbagallo, M., Bennett, S., Berthoumieux, E., Bosnar, D., Brown, A. S., Busso, M., Caamano, M., Calviani, M., Cano-Ott, D., Cerutti, F., Chiaveri, E., Colonna, N., Cortes, G. P., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Damone, L. A., Davies, P. J., Diakaki, M., Dietz, M., Dressler, R., Ducasse, Q., Dupont, E., Duran, I., Eleme, Z., Fernandez-Domingez, B., Ferrari, A., Ferro-Goncalves, I., Finocchiaro, P., Furman, V., Garg, R., Gawlik, A., Gilardoni, S., Gobel, K., Gonzalez-Romero, E., Gunsing, F., Heyse, J., Jenkins, D. G., Jericha, E., Jiri, U., Junghans, A., Kadi, Y., Kappeler, F., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Lederer-Woods, C., Lonsdale, S. -J., Macina, D., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinua, P. F., Mastromarco, M., Maugeri, E., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mingrone, F., Moreno-Soto, J., Musumarra, A., Negret, A., Ogallar, F., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Porras, I., Praena, J., Doval, D. R., Reifarth, R., Rochman, D., Rubbia, C., Sabate-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N., Sprung, P., Stamatopoulos, A., Tagliente, G., Tassan-Got, L., Thomas, B., Torres-Sanchez, P., Tsinganis, A., 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. J., Zugec, P., Domingo-Pardo C., Babiano-Suarez V., Balibrea-Correa J., Caballero L., Ladarescu I., Lerendegui-Marco J., Tain J.L., Calvino F., Casanovas A., Segarr A., Tarifeno-Saldivia A.E., Guerrero C., Millan-Callado M.A., Quesada J.M., Rodriguez-Gonzalez M.T., Aberle O., Alcayne V., Amaducci S., Andrzejewski J., Audouin L., Bacak M., Barbagallo M., Bennett S., Berthoumieux E., Bosnar D., Brown A.S., Busso M., Caamano M., Calviani M., Cano-Ott D., Cerutti F., Chiaveri E., Colonna N., Cortes G.P., Cortes-Giraldo M.A., Cosentino L., Cristallo S., Damone L.A., Davies P.J., Diakaki M., Dietz M., Dressler R., Ducasse Q., Dupont E., Duran I., Eleme Z., Fernandez-Domingez B., Ferrari A., Ferro-Goncalves I., Finocchiaro P., Furman V., Garg R., Gawlik A., Gilardoni S., Gobel K., Gonzalez-Romero E., Gunsing F., Heyse J., Jenkins D.G., Jericha E., Jiri U., Junghans A., Kadi Y., Kappeler F., Kimura A., Knapova I., Kokkoris M., Kopatch Y., Krticka M., Kurtulgil D., Lederer-Woods C., Lonsdale S.-J., Macina D., Manna A., Martinez T., Masi A., Massimi C., Mastinua P.F., Mastromarco M., Maugeri E., Mazzone A., Mendoza E., Mengoni A., Michalopoulou V., Milazzo P.M., Mingrone F., Moreno-Soto J., Musumarra A., Negret A., Ogallar F., Oprea A., Patronis N., Pavlik A., Perkowski J., Petrone C., Piersanti L., Pirovano E., Porras I., Praena J., Doval D.R., Reifarth R., Rochman D., Rubbia C., Sabate-Gilarte M., Saxena A., Schillebeeckx P., Schumann D., Sekhar A., Smith A.G., Sosnin N., Sprung P., Stamatopoulos A., Tagliente G., Tassan-Got L., Thomas B., Torres-Sanchez P., Tsinganis A., 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.J., and Zugec P.
Subjects: History, Physics - Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Measure (physics), FOS: Physical sciences, General Physics and Astronomy, 7. Clean energy, 01 natural sciences, Education, Nuclear physics, Nucleosynthesis, 0103 physical sciences, Neutron, 14. Life underwater, Instrumentation (computer programming), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Detectors and Experimental Techniques, 010306 general physics, physics.ins-det, 010303 astronomy & astrophysics, Stellar evolution, Physics, neutron capture, detector, TOF, Detector, Instrumentation and Detectors (physics.ins-det), Computer Science Applications, Progressive refinement, Neutron capture, astrophysics, neutron capture, neutron time of flight, n_TOF
Abstract: The idea of slow-neutron capture nucleosynthesis formulated in 1957 triggered a tremendous experimental effort in different laboratories worldwide to measure the relevant nuclear physics input quantities, namely (n, γ) cross sections over the stellar temperature range (from few eV up to several hundred keV) for most of the isotopes involved from Fe up to Bi. A brief historical review focused on total energy detectors will be presented to illustrate how advances in instrumentation have led to the assessment of new aspects of s-process nucleosynthesis and to the progressive refinement of stellar models. A summary will be presented on current efforts to develop new detection concepts, such as the Total-Energy Detector with γ-ray imaging capability (i-TED). The latter is based on the simultaneous combination of Compton imaging with neutron time-of-flight (TOF) techniques, in order to achieve a superior level of sensitivity and selectivity in the measurement of stellar neutron capture rates., European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (ERC Consolidator Grant project HYMNS) 681740, Instituto de Salud Carlos III Spanish Government FPA2014-52823-C2-1-P FPA2017-83946-C2-1-P, Consejo Superior de Investigaciones Cientificas (CSIC) PIE-201750I26, Program Severo Ochoa SEV-2014-0398
Published: 2020

19. Persistent starspot signals on M dwarfs: multi-wavelength Doppler observations with the Habitable-zone Planet Finder and Keck/HIRES

Author: J. Lubin, Shubham Kanodia, Joe P. Ninan, Chad F. Bender, Eric B. Ford, Christian Schwab, Paul Robertson, Andrew J. Monson, Connor Fredrick, Lawrence W. Ramsey, Jonathan Palafoutas, Andrew J. Metcalf, Arpita Roy, William D. Cochran, Lydia Juan, Ryan Terrien, Corey Beard, Michael Endl, Gudmundur Stefansson, Scott A. Diddams, Jason T. Wright, Nicholas Duong, Samuel Halverson, Suvrath Mahadevan, Rae Holcomb, and Fred Hearty
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), symbols.namesake, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Starspot, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Exoplanet, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, symbols, Astrophysics::Earth and Planetary Astrophysics, Doppler effect, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: Young, rapidly-rotating M dwarfs exhibit prominent starspots, which create quasiperiodic signals in their photometric and Doppler spectroscopic measurements. The periodic Doppler signals can mimic radial velocity (RV) changes expected from orbiting exoplanets. Exoplanets can be distinguished from activity-induced false positives by the chromaticity and long-term incoherence of starspot signals, but these qualities are poorly constrained for fully-convective M stars. Coherent photometric starspot signals on M dwarfs may persist for hundreds of rotations, and the wavelength dependence of starspot RV signals may not be consistent between stars due to differences in their magnetic fields and active regions. We obtained precise multi-wavelength RVs of four rapidly-rotating M dwarfs (AD Leo, G 227-22, GJ 1245B, GJ 3959) using the near-infrared (NIR) Habitable-zone Planet Finder, and the optical Keck/HIRES spectrometer. Our RVs are complemented by photometry from Kepler, TESS, and the Las Cumbres Observatory (LCO) network of telescopes. We found that all four stars exhibit large spot-induced Doppler signals at their rotation periods, and investigated the longevity and optical-to-NIR chromaticity for these signals. The phase curves remain coherent much longer than is typical for Sunlike stars. Their chromaticity varies, and one star (GJ 3959) exhibits optical and NIR RV modulation consistent in both phase and amplitude. In general, though, we find that the NIR amplitudes are lower than their optical counterparts. We conclude that starspot modulation for rapidly-rotating M stars frequently remains coherent for hundreds of stellar rotations, and gives rise to Doppler signals that, due to this coherence, may be mistaken for exoplanets., Comment: Accepted for publication in the Astrophysical Journal
Published: 2020
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20. Transits of Known Planets Orbiting a Naked-eye Star

Author: Stephen R. Kane, Tiago L. Campante, Ekrem Murat Esmer, Rodrigo F. Díaz, Özgür Baştürk, Magali Deleuil, Stéphane Udry, Natalie R. Hinkel, Howard Isaacson, Simon J. O'Toole, Brad D. Carter, Maxime Marmier, Damien Ségransan, Margaret C. Turnbull, R. Paul Butler, H. P. Osborn, Jason T. Wright, Francesco Pepe, Christophe Lovis, Andrew W. Howard, Xavier Dumusque, Jon M. Jenkins, François Bouchy, Sara Seager, Jeremy Bailey, Robert A. Wittenmyer, Andrew Vanderburg, Geoffrey W. Marcy, Joshua N. Winn, Duncan J. Wright, Roland Vanderspek, Martti H. Kristiansen, Louise D. Nielsen, Darin Ragozzine, Hugh R. A. Jones, Jacob L. Bean, David Ehrenreich, Tansu Daylan, Selçuk Yalçınkaya, George R. Ricker, C. G. Tinney, Romain Allart, David W. Latham, Jonathan Horner, Colby Ostberg, Tara Fetherolf, Paul A. Dalba, Teo Mocnik, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Radial velocity, 010504 meteorology & atmospheric sciences, Star (game theory), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanets, Astronomy and Astrophysics, Planetary system, Exoplanet, Exoplanet structure, Orbit, Stars, Photometry (astronomy), 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Transit photometry, Exoplanet atmospheres, Astrophysics - Earth and Planetary Astrophysics
Abstract: Some of the most scientifically valuable transiting planets are those that were already known from radial velocity (RV) surveys. This is primarily because their orbits are well characterized and they preferentially orbit bright stars that are the targets of RV surveys. The Transiting Exoplanet Survey Satellite ({\it TESS}) provides an opportunity to survey most of the known exoplanet systems in a systematic fashion to detect possible transits of their planets. HD~136352 (Nu$^2$~Lupi) is a naked-eye ($V = 5.78$) G-type main-sequence star that was discovered to host three planets with orbital periods of 11.6, 27.6, and 108.1 days via RV monitoring with the HARPS spectrograph. We present the detection and characterization of transits for the two inner planets of the HD~136352 system, revealing radii of $1.482^{+0.058}_{-0.056}$~$R_\oplus$ and $2.608^{+0.078}_{-0.077}$~$R_\oplus$ for planets b and c, respectively. We combine new HARPS observations with RV data from Keck/HIRES and the AAT, along with {\it TESS} photometry from Sector 12, to perform a complete analysis of the system parameters. The combined data analysis results in extracted bulk density values of $\rho_b = 7.8^{+1.2}_{-1.1}$~gcm$^{-3}$ and $\rho_c = 3.50^{+0.41}_{-0.36}$~gcm$^{-3}$ for planets b and c, respectively, thus placing them on either side of the radius valley. The combination of the multi-transiting planet system, the bright host star, and the diversity of planetary interiors and atmospheres means this will likely become a cornerstone system for atmospheric and orbital characterization of small worlds., Comment: 13 pages, 4 figures, 3 tables, accepted for publication in the Astronomical Journal
Published: 2020

21. A Framework for Relative Biosignature Yields from Future Direct Imaging Missions

Author: Noah W. Tuchow and Jason T. Wright
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Habitability, FOS: Physical sciences, Astronomy and Astrophysics, Direct imaging, 01 natural sciences, Exoplanet, Astrobiology, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Biosignature, Terrestrial planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Circumstellar habitable zone, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Future exoplanet direct imaging missions, such as HabEx and LUVOIR, will select target stars to maximize the number of Earth-like exoplanets that can have their atmospheric compositions characterized. Because one of these missions’ aims is to detect biosignatures, they should also consider the expected biosignature yield of planets around these stars. In this work, we develop a method of computing relative biosignature yields among potential target stars, given a model of habitability and biosignature genesis, and using a star’s habitability history. As an illustration and first application of this method, we use MESA stellar models to calculate the time evolution of the habitable zone and examine three simple models for biosignature genesis to calculate the relative biosignature yield for different stars. We find that the relative merits of K stars versus F stars depend sensitively on model choice. In particular, use of the present-day habitable zone as a proxy for biosignature detectability favors young, luminous stars lacking the potential for long-term habitability. Biosignature yields are also sensitive to whether life can arise on Cold Start exoplanets that enter the habitable zone after formation, an open question deserving of more attention. Using the case study of biosignature yields calculated for θ Cygni and 55 Cancri, we find that robust mission design and target selection for HabEx and LUVOIR depend on choosing a specific model of biosignature appearance with time, the terrestrial planet occurrence rate as a function of orbital separation, precise knowledge of stellar properties, and accurate stellar evolutionary histories.
Published: 2020
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22. Effects of Telluric Contamination in Iodine-calibrated Precise Radial Velocities

Author: Philip S. Muirhead, Jason T. Wright, Howard Isaacson, Andrew W. Howard, Sharon X. Wang, Chad F. Bender, and Mark Veyette
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Accuracy and precision, 010504 meteorology & atmospheric sciences, Absorption spectroscopy, Telluric contamination, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Astronomical spectroscopy, Spectral line, Radial velocity, Stars, Space and Planetary Science, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Noise (radio), Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: We characterized the effects of telluric absorption lines on the radial velocity (RV) precision of stellar spectra taken through an iodine cell. To isolate the effects induced by telluric contamination from other stellar, instrumental, or numerical systematic RV noise, we extracted RVs from simulated iodine calibrated spectra of three RV standard stars regularly observed by Keck/HIRES. We add in water absorption lines according to measured precipitable water vapor (PWV) contents over a one-year period. We concluded that telluric contamination introduces additional RV noise and spurious periodic signals on the level of 10-20 cm/s, consistent with similar previous studies. Our findings show that forward modeling the telluric lines effectively recovers the RV precision and accuracy, with no prior knowledge of the PWV needed. Such a recovery is less effective when the water absorption lines are relatively deep in the stellar template used in the forward modeling. Overall, telluric contamination plays an insignificant role for typical iodine-calibrated RV programs aiming at ~1-2 m/s, but we recommend adding modeling of telluric lines and taking stellar template observations on nights with low humidity for programs aiming to achieve sub-m/s precision., Comment: 17 pages, 9 figures. AJ accepted
Published: 2019

23. Rio 2.0: revising the Rio scale for SETI detections

Author: Duncan Forgan, Eric J. Korpela, Elisabeth Piotelat, Jill Tarter, Jason T. Wright, Iván Almár, Andrew Siemion, SUPA School of Physics and Astronomy [University of St Andrews], University of St Andrews [Scotland]-Scottish Universities Physics Alliance (SUPA), Center for Exoplanets and Habitable World (CEHW), Pennsylvania State University (Penn State), Penn State System-Penn State System, Breakthrough Listen Laboratory, SETI Institute, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Department of Astronomy [Berkeley], Radboud university [Nijmegen], Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Laboratoire d'Informatique pour la Mécanique et les Sciences de l'Ingénieur (LIMSI), Université Paris Saclay (COmUE)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université - UFR d'Ingénierie (UFR 919), Sorbonne Université (SU)-Sorbonne Université (SU)-Université Paris-Saclay-Université Paris-Sud - Paris 11 (UP11), European Research Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: 010504 meteorology & atmospheric sciences, Physics and Astronomy (miscellaneous), Computer science, T-NDAS, 01 natural sciences, Terminology, [INFO.INFO-NI]Computer Science [cs]/Networking and Internet Architecture [cs.NI], Rio scale, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), QB Astronomy, Science communication, Set (psychology), 010303 astronomy & astrophysics, QC, Ecology, Evolution, Behavior and Systematics, Search for extraterrestrial intelligence, QB, 0105 earth and related environmental sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Suite, Scale (chemistry), Extraterrestrial intelligence, SETI, science communication, T Technology, Data science, QC Physics, Space and Planetary Science, Extraterrestrial life
Abstract: DHF gratefully acknowledges support from the ECOGAL project, grant agreement 291227, funded by the European Research Council under ERC-2011-ADG. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. The Rio scale is a tool for communicating the significance of a signal to the general public. It assigns scores to signals detected in searches for extraterrestrial intelligence (SETI), which characterizes both the consequences of a signal and the probability the signal is truly from ETI, in an easily digestible format for laypeople to interpret. In the 17 years since its construction, the number of groups actively conducting searches for evidence of intelligent life beyond the Earth has increased significantly, and theoretical work has established a new suite of observables that are capable of revealing the presence of ETI in a range of astronomical observations. In this paper, we revise the Rio scale, with the aim of (i) achieving consensus across academic disciplines on a scheme for classifying signals potentially indicating the existence of advanced extraterrestrial life, (ii) supplying a pedagogical tool to help inform the public about the process scientists go through to develop an understanding of a signal and (iii) providing a means of calibrating the expectations of the world at large when signals are discussed in the media. We also present (and encourage the SETI community to adopt) a single set of consistent terminology for discussing signals. Postprint
Published: 2018

24. Preparation and characterization of 33S samples for 33S(n,α)30Si cross-section measurements at the n_TOF facility at CERN

Author: J. Praena, F.J. Ferrer, W. Vollenberg, M. Sabaté-Gilarte, B. Fernández, J. García-López, I. Porras, J.M. Quesada, S. Altstadt, J. Andrzejewski, L. Audouin, V. Bécares, M. Barbagallo, F. Bečvář, F. Belloni, E. Berthoumieux, J. Billowes, V. Boccone, D. Bosnar, M. Brugger, F. Calviño, M. Calviani, D. Cano-Ott, C. Carrapiço, F. Cerutti, E. Chiaveri, M. Chin, N. Colonna, G. Cortés, M.A. Cortés-Giraldo, M. Diakaki, M. Dietz, C. Domingo-Pardo, R. Dressler, I. Durán, C. Eleftheriadis, A. Ferrari, K. Fraval, V. Furman, K. Göbel, M.B. Gómez-Hornillos, S. Ganesan, A.R. García, G. Giubrone, I.F. Gonçalves, E. González-Romero, A. Goverdovski, E. Griesmayer, C. Guerrero, F. Gunsing, T. Heftrich, A. Hernández-Prieto, J. Heyse, D.G. Jenkins, E. Jericha, F. Käppeler, Y. Kadi, D. Karadimos, T. Katabuchi, V. Ketlerov, V. Khryachkov, N. Kivel, P. Koehler, M. Kokkoris, J. Kroll, M. Krtička, C. Lampoudis, C. Langer, E. Leal-Cidoncha, C. Lederer, H. Leeb, L.S. Leong, J. Lerendegui-Marco, R. Losito, A. Mallick, A. Manousos, J. Marganiec, T. Martínez, C. Massimi, P. Mastinu, M. Mastromarco, E. Mendoza, A. Mengoni, P.M. Milazzo, F. Mingrone, M. Mirea, W. Mondelaers, C. Paradela, A. Pavlik, J. Perkowski, A.J.M. Plompen, T. Rauscher, R. Reifarth, A. Riego-Perez, M. Robles, C. Rubbia, J.A. Ryan, R. Sarmento, A. Saxena, P. Schillebeeckx, S. Schmidt, D. Schumann, P. Sedyshev, G. Tagliente, J.L. Tain, A. Tarifeño-Saldivia, D. Tarrío, L. Tassan-Got, A. Tsinganis, S. Valenta, G. Vannini, V. Variale, P. Vaz, A. Ventura, M.J. Vermeulen, V. Vlachoudis, R. Vlastou, A. Wallner, T. Ware, M. Weigand, C. Weiss, T. Wright, and P. Žugec
Subjects: Physics, Nuclear and High Energy Physics, Thin layers, 010308 nuclear & particles physics, Analytical chemistry, chemistry.chemical_element, Rutherford backscattering spectrometry, 7. Clean energy, 01 natural sciences, Copper, Kapton, Chromium, chemistry, 0103 physical sciences, Sublimation (phase transition), Neutron, 010306 general physics, Instrumentation, Titanium
Abstract: Thin 33S samples for the study of the 33S(n, α)30Si cross-section at the n_TOF facility at CERN were made by thermal evaporation of 33S powder onto a dedicated substrate made of kapton covered with thin layers of copper, chromium and titanium. This method has provided for the first time bare sulfur samples a few centimeters in diameter. The samples have shown an excellent adherence with no mass loss after few years and no sublimation in vacuum at room temperature. The determination of the mass thickness of 33S has been performed by means of Rutherford backscattering spectrometry. The samples have been successfully tested under neutron irradiation.
Published: 2018

25. Combined Forward-Backward Asymmetry Measurements in Top-Antitop Quark Production at the Tevatron

Author: M. Franklin, Gavin Davies, Lorenzo Santi, Y. Scheglov, A. Ruiz, K. Yi, Ping-Kun Teng, Jan Stark, S. Carrillo, Martin Grunewald, Milos Lokajicek, Darien Wood, S. Blessing, P. F. Ding, Scott Snyder, Jonathan Wilson, M. Herndon, Cecilia Elena Gerber, Luigi Marchese, Cecile Deterre, M. Lancaster, Tiehui Ted Liu, Prabhakar Palni, R. St. Denis, A. Fauré, Nikos Varelas, Sally Seidel, C. L. McGivern, Bing Zhou, P. Barria, D. A. Stoyanova, G. Piacentino, L. Brigliadori, Sergey Burdin, Chen Zhou, S. Bhatia, C. Royon, G. Ginther, M. H.L.S. Wang, Taegil Bae, M. C. Cousinou, Pierfrancesco Butti, Y. Seiya, G. Gomez, Christoph Paus, M. Cooke, S. Cihangir, Robert Hirosky, I. Howley, Fumihiko Ukegawa, Kristian Harder, A. Anastassov, Don Lincoln, Erich Varnes, Y. N. Kharzheev, Suyong Choi, P. H. Garbincius, A. Das, P. Svoisky, L. Oakes, S. Fuess, L. Pondrom, Jianming Qian, B. Kilminster, B. Casal, Pietro Marino, Giorgio Bellettini, R. Wallny, Hui Li, M. J. Shochet, Ron Lipton, Y. Sakurai, Virgil E Barnes, John Christian Freeman, K. Devaughan, Andreas Werner Jung, F. Ptohos, A. Elagin, Peter Wagner, Gueorgui Velev, Elliot Lipeles, K. Potamianos, DongHee Kim, S. Rolli, A. Di Canto, Marcelo Vogel, Hugh Williams, M. Iori, Robert Kehoe, Graham Wilson, Massimo Casarsa, W. H. Hopkins, Jongmin Lee, Lidija Zivkovic, Y. D. Oh, A. Kumar, Howard Scott Budd, Christopher Clarke, W. Ketchum, Philip Baringer, Hyun-Chul Kim, T. Kurca, A. Evdokimov, J. Kraus, Matthias Schott, K. Herner, J. Budagov, V. Gavrilov, S. Banerjee, T. Wright, Matthew T Jones, Aliaksandr Pranko, Gordon Watts, Romain Madar, D. Jang, N. Moggi, B. Di Ruzza, Ashutosh Kotwal, N. K. Mondal, Ting Miao, D. Boline, H. T. Diehl, M. Vesterinen, Jieun Kim, Andrew Askew, S. W. Lee, M. M. Deninno, Markus Wobisch, G. Latino, J. Zennamo, A. Dubey, Michael Mulhearn, A. Loginov, L. Feng, G. Golovanov, T. Kamon, Jay Dittmann, S. Amerio, T. Kuhr, A. Simonenko, L. S. Vertogradov, W. Geng, P. Lukens, Boris Tuchming, V. Glagolev, D. Stentz, A. S. Ito, T. Aaltonen, B. Hoeneisen, D. J. Cox, Q. Liu, D. Cruz, C. Bromberg, J. Clutter, Maxim Perfilov, R. McNulty, M. Hare, A. Drutskoy, J. K. Lim, A. Lucà, K. Pitts, Y. T. Tsai, C. Pagliarone, A. Boehnlein, Mark Raymond Adams, D. Karmanov, H. Hegab, V. Parihar, E. De La Cruz-Burelo, Stefano Giagu, John Hobbs, M. Hohlfeld, Antonio Boveia, Gregorio Bernardi, B. Carls, V. Sorin, A. Mazzacane, A. V. Popov, R. D. Schamberger, J. T. Linnemann, U. K. Yang, J. Nachtman, A. S. Santos, E. Brucken, Phillip Gutierrez, Frederic Deliot, G. P. Yeh, Douglas Benjamin, C. S. Moon, D. Menezes, Stanislav Tokár, Kohei Yorita, D. Glenzinski, Hal Evans, T. Head, D.P. Brown, Seo-Young Noh, P. Mazzanti, J. R. Smith, G. B. Yu, J. Ellison, Emanuela Barberis, Yuji Enari, K. Soustruznik, Elemer Nagy, S. Y. Jun, G. Savage, T. G. Zhao, W. Ye, V. Aushev, J. Conway, Thomas Ferbel, M. Prewitt, Nazar Stefaniuk, Yuji Takeuchi, J. Weichert, Song-Ming Wang, Y. Aushev, G. Grenier, F. Miconi, E. Kajfasz, A. P. Heinson, J. Boudreau, Jose Andres Garcia-Gonzalez, Kazuhiro Yamamoto, M. Savitskyi, Andrew Brandt, L. Bellantoni, A. Ivanov, S. Dutt, S. Caughron, C. Galloni, J. Nett, J. Warchol, J. Konigsberg, A. Kasmi, Pavol Bartos, L. Bagby, Oleg Brandt, Bjoern Penning, Franco Rimondi, Maria Rescigno, H. E. Fisk, D. Lucchesi, W. Ashmanskas, Sudhir Malik, L. Ristori, Ia Iashvili, Adrian Buzatu, J. Keung, G. C. Blazey, D. Torretta, L. Nodulman, A. Sukhanov, Andrew Beretvas, Brajesh C Choudhary, V. V. Lipaev, J. Lellouch, M. A. Pleier, A. Alton, T. Nigmanov, A. Mukherjee, R. Forrest, Giovanni Busetto, Y. Sudo, I. Suslov, Maxim Goncharov, Kunitaka Kondo, Richard D Field, V. E. Bazterra, N. Khalatyan, R. Ruchti, Thibault Guillemin, P. D. Grannis, P. Jiang, R. Yamada, P. Mehtala, Sandra Leone, P. Totaro, I. Ripp-Baudot, Hao Song, L. Scodellaro, J. Orduna, T. Yoshida, Manfredi Ronzani, Sinead Farrington, Andrea Bocci, D. Li, V. L. Malyshev, A. Y. Verkheev, Jeffrey A. Appel, S. Lammel, Giovanni Punzi, O. Norniella, Manfred Paulini, Manuela Campanelli, V. A. Kuzmin, H. Wolfmeister, Fabrice Couderc, F. Badaud, F. Happacher, B. Baldin, N. d’Ascenzo, M. Borysova, Sung Keun Park, Guillelmo Gomez-Ceballos, M. Titov, Christopher George Tully, Aran Garcia-Bellido, K. Hatakeyama, Young-Jin Kim, R. Illingworth, D. Mietlicki, Mitchell Wayne, H. Schellman, S. Torre, J. M. Kohli, L. Ortolan, D. Cauz, W. E. Cooper, A. Jayasinghe, P. Slattery, V. Giakoumopoulou, A. Sánchez-Hernández, S. Poprocki, E. Gramellini, William Wester, Adam Aurisano, S. J. De Jong, C. Hensel, P. Skubic, Joey Huston, P. Wittich, Ziqing Hong, Katsufumi Sato, O. Gogota, B. Jayatilaka, Daniel R Claes, R. Vilar, B. Auerbach, Liang Li, M. Corbo, Jean-Arcady Meyer, Davit Chokheli, J. Y. Han, F. Margaroli, O. Gonzalez Lopez, A. Bhatti, D. Hedin, F. Devoto, S. Leo, M. Mussini, V. Rusu, L. Welty-Rieger, Marc Besancon, Stefan Grünendahl, Elizaveta Shabalina, M. J. Morello, S. R. Hou, P. E. Karchin, A. Chapelain, S. Errede, Eugene E. Schmidt, Emily Johnson, D. Yamato, A. Golossanov, Vaia Papadimitriou, Alessandro Cerri, A. Mitra, Marco Verzocchi, G. Flanagan, J. P. Agnew, Dmitri Tsybychev, P. Lebrun, Yongsun Kim, Lev Dudko, Nikos Giokaris, A. Grohsjean, Y. C. Chen, V. Saveliev, Dmitri Denisov, J. Russ, Stephen R. Hahn, M. Kurata, R. Madrak, M. Buehler, J. Naganoma, L. Sonnenschein, L. Demortier, Chris Hays, Seog Oh, J. Sekaric, Michael A. Strauss, Maxwell Chertok, A. Patwa, H. Gerberich, J. Joshi, J. Martínez-Ortega, Yang Yang, Zdenek Hubacek, E. Palencia, Giorgio Chiarelli, R. E. Hughes, J. Antos, B. A. Barnett, Giorgio Apollinari, Pedro G Mercadante, S. Atkins, G. Pauletta, Adam L. Lyon, J. P. Negret, Victor Daniel Elvira, K. R. Bland, K. Takemasa, V. M. Podstavkov, P. F. Shepard, Arnaud Duperrin, Carlos Avila, K. Lannon, Eric B James, E. J. Jeon, F. Vázquez, D. Waters, Kazuhiko Hara, M. Fortner, A. Chandra, Satoru Uozumi, U. Bassler, S. Kim, Mark Edward Mattson, Alberto Annovi, S. Zucchelli, Ulrich Heintz, S. Söldner-Rembold, M. Eads, Kenneth Johns, J. Vizán, Marcia Begalli, M. Jaffré, C. A. Cox, Joseph Haley, H. Miyake, J. L. Holzbauer, Kihyeon Cho, Yoshikazu Nagai, P. N. Ratoff, Y. Peters, J. Franc, R. Luna-Garcia, Mousumi Datta, J. Lueck, Lucio Cerrito, R. Roser, Frank Filthaut, Regina Demina, Meenakshi Narain, J. Yoh, F. Bedeschi, T. Harrington-Taber, Y. Zeng, N. Prokopenko, M. Kambeitz, Mark Richard James Williams, Michael Hildreth, W. M. Lee, H. Greenlee, Claus P. Buszello, Ph Gris, T. Hoang, Yujiro Funakoshi, M. Diesburg, Darren Price, Hang Yin, A. Bross, R. Magaña-Villalba, G. Chen, J. Snow, A. A. Shchukin, E. Gerchtein, Fedor Prokoshin, H. T. Nguyen, M. Hussein, S. Z. Shalhout, R. Nayyar, S. Uzunyan, V. Bhatnagar, Alexander Kupco, Emilien Chapon, V. Simak, P. de Barbaro, T. Okusawa, T. Scanlon, T. Yang, Guennadi Borissov, J. Strologas, Y. A. Yatsunenko, Arnd Meyer, T. Rodriguez, James Nugent Bellinger, M. Cordelli, S. Kermiche, Anthony Ross, Shabnam Jabeen, Savanna Marie Shaw, Suman Bala Beri, Barry Blumenfeld, B. L. Winer, T. Tomura, Frank Fiedler, J. Asaadi, M. Merkin, Pierluigi Catastini, S. Chakrabarti, I. Katsanos, M. Dorigo, I. Heredia-De La Cruz, E. E. Boos, N. Parua, M. Tecchio, D. Toback, Arnulf Quadt, Alexander Khanov, R. Carosi, Alfred Goshaw, V. Hynek, A. Hocker, R. Bernhard, Amnon Harel, C. Schwanenberger, U. Husemann, Heriberto Castilla-Valdez, W. C. Fisher, W. Parker, M. Kaur, V. V. Tokmenin, G. Alkhazov, Charles Plager, Roman Lysak, S. Donati, K. Matera, D. Amidei, J. M. Yu, Karen Ruth Gibson, Antonio Limosani, P. Rubinov, M. Vidal, D. Vilanova, M. Cremonesi, Q. Z. Li, Lev Uvarov, V. M. Abazov, P. Wilson, Naoki Kimura, Mark Kruse, Alison Lister, I. Kiselevich, Bobby Samir Acharya, H. A. Neal, V. Shary, Daniela Bortoletto, S. Wilbur, C.M. Ginsburg, Pushpalatha C Bhat, Raymond Brock, K. Yip, S. H. Kim, D. V. Bandurin, Raymond Lloyd Culbertson, Jeremy Lys, R. Van Kooten, Neeti Parashar, J. Hogan, A. Juste, K. Petridis, T. Nunnemann, R. Beuselinck, W-M. Yao, Todd Adams, Javier Cuevas, V. Thukral, Jason Dhia Mansour, S. Greder, Iain Alexander Bertram, G. Chlachidze, Yanwen Liu, H. Frisch, A. K.A. Maciel, Lee Sawyer, C. Vellidis, S. Moed, K. Goulianos, Y. Xie, Fabrizio Scuri, J. P. Fernández Ramos, P. Giromini, Michal Kreps, A. Artikov, I. Razumov, M. Zielinski, A. Barbaro-Galtieri, M. D. Corcoran, Gianluca Introzzi, W. Badgett, M. Stancari, Arie Bodek, J. Hays, G. Gutierrez, P. Renton, Evelyn Thomson, V. N. Evdokimov, Th. Müller, M. Rominsky, M. Shimojima, K. Sliwa, P. Neustroev, Sabine Lammers, N. Osman, Liyuan Han, Jakub Cúth, A. Driutti, G. Lungu, R. Jesik, Kyung Kwang Joo, D. Edmunds, R. Lopes De Sá, M. J. Kim, Duncan Carlsmith, Thomas J. Phillips, Andrew Mehta, Zhenyu Ye, Yuri Gershtein, S. Lockwitz, Andrea Castro, A. T. Laasanen, G. D. Alexeev, Flera Rizatdinova, E. Camacho-Pérez, I. Yu, Reinhard Schwienhorst, A. M. Zanetti, Stefano Camarda, Jean-Francois Grivaz, G. Manca, J. Pilot, Arthur Barry Wicklund, Michael S. Gold, Kwok Ming Chan, Yuriy Ilchenko, X. Lei, Daniel Whiteson, Paolo Maestro, Michael H Kirby, A. Jonckheere, A. Semenov, F. Ruffini, A. Lobodenko, M. P. Sanders, B. Esham, M. Brochmann, Aidan Robson, A. Melnitchouk, S. Behari, Daria Zieminska, M. D'Errico, Y. Kato, J. Guimaraes Da Costa, D. Tonelli, A. Napier, T. R. Wyatt, I. V. Gorelov, Zhenbin Wu, R. Erbacher, P. Jonsson, Kamil Augsten, A. Pal, S. W. Youn, Thomas Hebbeker, J. M. Hauptman, A. Kharchilava, Siqi Yang, Elisabetta Pianori, I. Shreyber-Tecker, O. Shkola, Federico Sforza, Brad Abbott, Pierre Petroff, Gregory R Snow, Sergey Denisov, Viviana Cavaliere, G. Sajot, Horst Severini, Hakjae Lee, W. M. Van Leeuwen, Junjie Zhu, Joe Kroll, B. C.K. Casey, S. Wolbers, P. Lujan, Monica D'Onofrio, T. R. Junk, G. Petrillo, J. Tang, Jonathan Lewis, S. Uvarov, Marvin Johnson, Philip Schlabach, M. Trovato, A. V. Kozelov, Jonathan L. Rosner, B. Quinn, C. Mesropian, X. B. Bu, K. Ebina, Alice Bean, Willis Kazuo Sakumoto, Ryan Christopher Edgar, Xin Wu, T. A. Schwarz, C. Grosso-Pilcher, Viacheslav Bunichev, Volker Buescher, Peter Bussey, H. D. Wahl, Florencia Canelli, Matteo Bauce, Tara Shears, D. J. Kong, S. Desai, D. Goldin, Petr Vokac, Kirsten Tollefson, J. Thom, Risto Orava, M. M. Meijer, Kevin Burkett, T. Yasuda, P. Garosi, Aaron Dominguez, Jochen Jens Heinrich, I. Redondo Fernández, H. Liu, F. D. Snider, C. Vernieri, Guido Volpi, Itsuo Nakano, Harald Fox, Aurore Savoy-Navarro, S. W. Cho, A. Manousakis-Katsikakis, Allan G Clark, Roger Moore, F. Azfar, David Cutts, M. E. Convery, T. Arisawa, Alan Garfinkel, James G. Bartlett, L. Suter, S. Jindariani, P. Murat, I. A. Vasilyev, A. Calamba, R. Partridge, Kenneth Bloom, R. McCarthy, M. S. Jeong, Gavin Grant Hesketh, R. F. Harr, Aaltonen, T., Abazov, V. M., Abbott, B., Acharya, B. S., Adams, M., Adams, T., Agnew, J. P., Alexeev, G. D., Alkhazov, G., Alton, A., Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Askew, A., Atkins, S., Auerbach, B., Augsten, K., Aurisano, A., Aushev, V., Aushev, Y., Avila, C., Azfar, F., Badaud, F., Badgett, W., Bae, T., Bagby, L., Baldin, B., Bandurin, D. V., Banerjee, S., Barbaro-Galtieri, A., Barberis, E., Baringer, P., Barnes, V. E., Barnett, B. A., Barria, P., Bartlett, J. F., Bartos, P., Bassler, U., Bauce, M., Bazterra, V., Bean, A., Bedeschi, F., Begalli, M., Behari, S., Bellantoni, L., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Beri, S. B., Bernardi, G., Bernhard, R., Bertram, I., Besancon, M., Beuselinck, R., Bhat, P. C., Bhatia, S., Bhatnagar, V., Bhatti, A., Bland, K. R., Blazey, G., Blessing, S., Bloom, K., Blumenfeld, B., Bocci, A., Bodek, A., Boehnlein, A., Boline, D., Boos, E. E., Borissov, G., Bortoletto, D., Borysova, M., Boudreau, J., Boveia, A., Brandt, A., Brandt, O., Brigliadori, L., Brochmann, M., Brock, R., Bromberg, C., Bross, A., Brown, D., Brucken, E., Bu, X. B., Budagov, J., Budd, H. S., Buehler, M., Buescher, V., Bunichev, V., Burdin, S., Burkett, K., Busetto, G., Bussey, P., Buszello, C. P., Butti, P., Buzatu, A., Calamba, A., Camacho-Perez, E., Camarda, S., Campanelli, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Casal, B., Casarsa, M., Casey, B. C. K., Castilla-Valdez, H., Castro, A., Catastini, P., Caughron, S., Cauz, D., Cavaliere, V., Cerri, A., Cerrito, L., Chakrabarti, S., Chan, K. M., Chandra, A., Chapelain, A., Chapon, E., Chen, G., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Cho, K., Cho, S. W., Choi, S., Chokheli, D., Choudhary, B., Cihangir, S., Claes, D., Clark, A., Clarke, C., Clutter, J., Convery, M. E., Conway, J., Cooke, M., Cooper, W. E., Corbo, M., Corcoran, M., Cordelli, M., Couderc, F., Cousinou, M. -C., Cox, C. A., Cox, D. J., Cremonesi, M., Cruz, D., Cuevas, J., Culbertson, R., Cuth, J., Cutts, D., Das, A., D'Ascenzo, N., Datta, M., Davies, G., de Barbaro, P., de Jong, S. J., De La Cruz-Burelo, E., Deliot, F., Demina, R., Demortier, L., Deninno, M., Denisov, D., Denisov, S. P., D'Errico, M., Desai, S., Deterre, C., Devaughan, K., Devoto, F., Di Canto, A., Di Ruzza, B., Diehl, H. T., Diesburg, M., Ding, P. F., Dittmann, J. R., Dominguez, A., Donati, S., D'Onofrio, M., Dorigo, M., Driutti, A., Drutskoy, A., Dubey, A., Dudko, L. V., Duperrin, A., Dutt, S., Eads, M., Ebina, K., Edgar, R., Edmunds, D., Elagin, A., Ellison, J., Elvira, V. D., Enari, Y., Erbacher, R., Errede, S., Esham, B., Evans, H., Evdokimov, A., Evdokimov, V. N., Farrington, S., Faure, A., Feng, L., Ferbel, T., Fernandez Ramos, J. P., Fiedler, F., Field, R., Filthaut, F., Fisher, W., Fisk, H. E., Flanagan, G., Forrest, R., Fortner, M., Fox, H., Franc, J., Franklin, M., Freeman, J. C., Frisch, H., Fuess, S., Funakoshi, Y., Galloni, C., Garbincius, P. H., Garcia-Bellido, A., Garcia-Gonzalez, J. A., Garfinkel, A. F., Garosi, P., Gavrilov, V., Geng, W., Gerber, C. E., Gerberich, H., Gerchtein, E., Gershtein, Y., Giagu, S., Giakoumopoulou, V., Gibson, K., Ginsburg, C. M., Ginther, G., Giokaris, N., Giromini, P., Glagolev, V., Glenzinski, D., Gogota, O., Gold, M., Goldin, D., Golossanov, A., Golovanov, G., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez Lopez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Gramellini, E., Grannis, P. D., Greder, S., Greenlee, H., Grenier, G., Gris, Ph., Grivaz, J. -F., Grohsjean, A., Grosso-Pilcher, C., Grunendahl, S., Grunewald, M. W., Guillemin, T., da Costa, J. Guimarae, Gutierrez, G., Gutierrez, P., Hahn, S. R., Haley, J., Han, J. Y., Han, L., Happacher, F., Hara, K., Harder, K., Hare, M., Harel, A., Harr, R. F., Harrington-Taber, T., Hatakeyama, K., Hauptman, J. M., Hays, C., Hays, J., Head, T., Hebbeker, T., Hedin, D., Hegab, H., Heinrich, J., Heinson, A. P., Heintz, U., Hensel, C., Heredia-De La Cruz, I., Herndon, M., Herner, K., Hesketh, G., Hildreth, M. D., Hirosky, R., Hoang, T., Hobbs, J. D., Hocker, A., Hoeneisen, B., Hogan, J., Hohlfeld, M., Holzbauer, J. L., Hong, Z., Hopkins, W., Hou, S., Howley, I., Hubacek, Z., Hughes, R. E., Husemann, U., Hussein, M., Huston, J., Hynek, V., Iashvili, I., Ilchenko, Y., Illingworth, R., Introzzi, G., Iori, M., Ito, A. S., Ivanov, A., Jabeen, S., Jaffre, M., James, E., Jang, D., Jayasinghe, A., Jayatilaka, B., Jeon, E. J., Jeong, M. S., Jesik, R., Jiang, P., Jindariani, S., Johns, K., Johnson, E., Johnson, M., Jonckheere, A., Jones, M., Jonsson, P., Joo, K. K., Joshi, J., Jun, S. Y., Jung, A. W., Junk, T. R., Juste, A., Kajfasz, E., Kambeitz, M., Kamon, T., Karchin, P. E., Karmanov, D., Kasmi, A., Kato, Y., Katsanos, I., Kaur, M., Kehoe, R., Kermiche, S., Ketchum, W., Keung, J., Khalatyan, N., Khanov, A., Kharchilava, A., Kharzheev, Y. N., Kilminster, B., Kim, D. H., Kim, H. S., Kim, J. E., Kim, M. J., Kim, S. H., Kim, S. B., Kim, Y. J., Kim, Y. K., Kimura, N., Kirby, M., Kiselevich, I., Kohli, J. M., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kozelov, A. V., Kraus, J., Kreps, M., Kroll, J., Kruse, M., Kuhr, T., Kumar, A., Kupco, A., Kurata, M., Kurca, T., Kuzmin, V. A., Laasanen, A. T., Lammel, S., Lammers, S., Lancaster, M., Lannon, K., Latino, G., Lebrun, P., Lee, H. S., Lee, J. S., Lee, S. W., Lee, W. M., Lei, X., Lellouch, J., Leo, S., Leone, S., Lewis, J. D., Li, D., Li, H., Li, L., Li, Q. Z., Lim, J. K., Limosani, A., Lincoln, D., Linnemann, J., Lipaev, V. V., Lipeles, E., Lipton, R., Lister, A., Liu, H., Liu, Q., Liu, T., Liu, Y., Lobodenko, A., Lockwitz, S., Loginov, A., Lokajicek, M., de Sa, R. 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W., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wobisch, M., Wolbers, S., Wolfmeister, H., Wood, D. R., Wright, T., Wu, X., Wu, Z., Wyatt, T. R., Xie, Y., Yamada, R., Yamamoto, K., Yamato, D., Yang, S., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yasuda, T., Yatsunenko, Y. A., Ye, W., Ye, Z., Yeh, G. P., Yi, K., Yin, H., Yip, K., Yoh, J., Yorita, K., Yoshida, T., Youn, S. W., Yu, G. B., Yu, I., Yu, J. M., Zanetti, A. M., Zeng, Y., Zennamo, J., Zhao, T. 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Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Department of Physics, Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Laboratory for Nuclear Science, Gomez-Ceballos, Guillelmo, Goncharov, Maxim, Paus, Christoph M. E., Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de Physique de Clermont ( LPC ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Clermont Auvergne ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Institut Pluridisciplinaire Hubert Curien ( IPHC ), Centre National de la Recherche Scientifique ( CNRS ) -Université de Strasbourg ( UNISTRA ), Institut de Physique Nucléaire de Lyon ( IPNL ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), 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 ), Laboratoire de Physique Subatomique et de Cosmologie ( LPSC ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Abazov, V.M., Acharya, B.S., Agnew, J.P., Alexeev, G.D., Appel, J.A., Bandurin, D.V., Barnes, V.E., Barnett, B.A., Bartlett, J.F., Beri, S.B., Besançon, M., Bhat, P.C., Bland, K.R., Boos, E.E., Bu, X.B., Budd, H.S., Buszello, C.P., Camacho-Pérez, E., Casey, B.C.K., Chan, K.M., Chen, Y.C., Cho, S.W., Convery, M.E., Cooper, W.E., Cousinou, M.-C., Cox, C.A., Cox, D.J., De Barbaro, P., De Jong, S.J., Déliot, F., Denisov, S.P., Diehl, H.T., Ding, P.F., Dittmann, J.R., Dudko, L.V., Elvira, V.D., Evdokimov, V.N., Fauré, A., Fernández Ramos, J.P., Fisk, H.E., Freeman, J.C., Garbincius, P.H., García-González, J.A., Garfinkel, A.F., Gerber, C.E., Ginsburg, C.M., González López, O., Goshaw, A.T., Grannis, P.D., Grivaz, J.-F., Grünendahl, S., Grünewald, M.W., Guimaraes Da Costa, J., Hahn, S.R., Han, J.Y., Harr, R.F., Hauptman, J.M., Heinson, A.P., Hildreth, M.D., Hobbs, J.D., Holzbauer, J.L., Hughes, R.E., Ito, A.S., Jaffré, M., Jeon, E.J., Jeong, M.S., Joo, K.K., Jun, S.Y., Jung, A.W., Junk, T.R., Karchin, P.E., Kharzheev, Y.N., Kim, D.H., Kim, H.S., Kim, J.E., Kim, M.J., Kim, S.H., Kim, S.B., Kim, Y.J., Kim, Y.K., Kohli, J.M., Kong, D.J., Kotwal, A.V., Kozelov, A.V., Kurča, T., Kuzmin, V.A., Laasanen, A.T., Lee, H.S., Lee, J.S., Lee, S.W., Lee, W.M., Lewis, J.D., Li, Q.Z., Lim, J.K., Lipaev, V.V., Lopes De Sa, R., Lucà, A., Lyon, A.L., Maciel, A.K.A., Magaña-Villalba, R., Malyshev, V.L., Martínez-Ortega, J., Mattson, M.E., McCarthy, R., McGivern, C.L., McNulty, R., Meijer, M.M., Mercadante, P.G., Mondal, N.K., Moon, C.S., Morello, M.J., Neal, H.A., Negret, J.P., Nguyen, H.T., Noh, S.Y., Oh, S.H., Oh, Y.D., Park, S.K., Pétroff, P., Phillips, T.J., Pleier, M.-A., Podstavkov, V.M., Popov, A.V., Ratoff, P.N., Redondo Fernández, I., Rosner, J.L., Sakumoto, W.K., Sánchez-Hernández, A., Sanders, M.P., Santos, A.S., Schamberger, R.D., Schmidt, E.E., Shalhout, S.Z., Shchukin, A.A., Shepard, P.F., Smith, J.R., Snider, F.D., Snow, G.R., Söldner-Rembold, S., St Denis, R., Stoyanova, D.A., Teng, P.K., Tokmenin, V.V., Tsai, Y.-T., Van Leeuwen, W.M., Varnes, E.W., Vasilyev, I.A., Vázquez, F., Verkheev, A.Y., Vertogradov, L.S., Vizán, J., Wahl, H.D., Wang, M.H.L.S., Wang, S.M., Wester, W.C., Wicklund, A.B., Williams, H.H., Williams, M.R.J., Wilson, G.W., Wilson, J.S., Winer, B.L., Wood, D.R., Wyatt, T.R., Yang, U.K., Yang, Y.C., Yao, W.-M., Yatsunenko, Y.A., Yeh, G.P., Youn, S.W., Yu, G.B., Yu, J.M., Zanetti, A.M., Zhao, T.G., Clark, Allan Geoffrey, Lister, Alison, Wu, Xin, and Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)
Subjects: Top quark, Tevatron, General Physics and Astronomy, pair production [top], 01 natural sciences, 7. Clean energy, High Energy Physics - Experiment, Subatomär fysik, High Energy Physics - Experiment (hep-ex), DZERO, Subatomic Physics, ddc:550, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Quantum Chromodynamics, Batavia TEVATRON Coll, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), media_common, Physics, scattering [anti-p p], Particle properties, 02 Physical Sciences, rapidity: difference, CDF, top-quark, difference [rapidity], asymmetry [angular distribution], kinematics, Physical Sciences, top: pair production, Quark, Particle physics, General Physics, angular distribution: asymmetry, Tevatron Collider, media_common.quotation_subject, Physics, Multidisciplinary, FOS: Physical sciences, Forward backward, ddc:500.2, Hadron-hadron interactions, Asymmetry, Computer Science::Digital Libraries, 114 Physical sciences, Marie curie, CDF Collaboration, anti-p p: colliding beams, Physics and Astronomy (all), [ PHYS.HEXP ] Physics [physics]/High Energy Physics - Experiment [hep-ex], 0103 physical sciences, anti-p p: scattering, media_common.cataloged_instance, ddc:530, High Energy Physics, European union, 010306 general physics, Science & Technology, 1960 GeV-cms, 010308 nuclear & particles physics, hep-ex, High Energy Physics::Phenomenology, Q007TFB, Research council, Experimental High Energy Physics, High Energy Physics::Experiment, colliding beams [anti-p p], High Energy Physics, Top quark, Hadron-hadron interactions, Quantum Chromodynamics, Particle properties, Tevatron Collider, D0 Collaboration, experimental results
Abstract: The CDF and D0 experiments at the Fermilab Tevatron have measured the asymmetry between yields of forward- and backward-produced top and antitop quarks based on their rapidity difference and the asymmetry between their decay leptons. These measurements use the full data sets collected in proton-antiproton collisions at a center-of-mass energy of √s=1.96 TeV. We report the results of combinations of the inclusive asymmetries and their differential dependencies on relevant kinematic quantities. The combined inclusive asymmetry is At¯tFB=0.128±0.025. The combined inclusive and differential asymmetries are consistent with recent standard model predictions., Physical Review Letters, 120 (4), ISSN:0031-9007, ISSN:1079-7114
Published: 2018
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26. Breakthrough Listen – A new search for life in the universe

Author: S. Pete Worden, Matt Lebofsky, Jason T. Wright, Dan Werthimer, David DeBoer, David MacMahon, Danny C. Price, Jack Hickish, Steve Croft, Jamie Drew, Vishal Gajjar, Howard Isaacson, and Andrew Siemion
Subjects: Physics, Theoretical physics, 010308 nuclear & particles physics, Extraterrestrial life, 0103 physical sciences, Aerospace Engineering, 010303 astronomy & astrophysics, 01 natural sciences, Epistemology
Published: 2017

27. Negative tone photolithography with photo-sensitised polymethyl methacrylate (PMMA)

Author: Faiz Rahman, Jason T. Wright, and Daniel J. Carbaugh
Subjects: 010302 applied physics, Materials science, Polymethyl methacrylate, technology, industry, and agriculture, Nanotechnology, 02 engineering and technology, 021001 nanoscience & nanotechnology, Condensed Matter Physics, 01 natural sciences, Atomic and Molecular Physics, and Optics, Surfaces, Coatings and Films, Electronic, Optical and Magnetic Materials, law.invention, Tone (musical instrument), Resist, law, 0103 physical sciences, Dry etching, Electrical and Electronic Engineering, Photolithography, 0210 nano-technology, Science, technology and society, Photoinitiator, Lithography
Abstract: We describe the science and technology of negative tone photolithography using polymethyl methacrylate (PMMA), photo-sensitised with the addition of the commercial photoinitiator Irgacure 651. This versatile two-active-ingredient resist system is shown to enable negative tone photolithography which can be customised to application requirements by adjusting the ratio of the two ingredients. This study describes the complete lithographic process from resist preparation to pattern transfer in considerable detail. Furthermore, we also elucidate the mechanism of resist action through exploration of the effects of such parameters as the molecular weight of PMMA, exposure wavelength, post-exposure bake conditions and resist development temperature, among others. This work also demonstrates that photo-cross-linkable resists can be made resistant to dry etching by a post-development blanket UV exposure step. Finally, we also show example structures fabricated using both additive and subtractive techniques, with the use of this resist system. Display Omitted A technique for performing optical lithography with PMMA is described.PMMA is cross-linked by using Irgacure 651.A post-exposure bake greatly improves this process.Cross-linking also improves dry-etch resistance of patterned PMMA.
Published: 2017

28. Measurement of the Ge70(n,γ) cross section up to 300 keV at the CERN n_TOF facility

Author: E. A. Maugeri, G. Cortes, A. Musumarra, Claudia Lederer-Woods, A. R. García, S. Warren, V. Variale, V. Bécares, C. Weiss, R. Vlastou, A. Tattersall, P. C. Rout, M. Brugger, F. Gunsing, Tanja Heftrich, P. V. Sedyshev, Cristian Massimi, P. Ferreira, Damir Bosnar, Y. Kadi, I. Knapova, M. Krtička, N. Patronis, M. A. Cortés-Giraldo, A. Riego-Perez, C. Beinrucker, D. M. Castelluccio, Alfredo Ferrari, Petar Žugec, P. Vaz, K. Göbel, M. Mirea, G. Tagliente, T. Martinez, K. Rajeev, B. Fernández-Domínguez, F. Calviño, H. Leeb, M. Bacak, G. Vannini, E. Leal-Cidoncha, Javier Praena, S. Lo Meo, I. Duran, Alberto Ventura, A. Kimura, T. Wright, Francesca Matteucci, V. Khryachkov, D. Macina, J. Perkowski, A. Gawlik, U. Battino, F. Mingrone, J. Andrzejewski, Thomas Rauscher, F. Käppeler, A. Pavlik, J. Marganiec, C. Domingo-Pardo, J. I. Porras, J. L. Tain, F. Bečvář, A. Saxena, Roberto Losito, S. Valenta, Carlos Guerrero, M. Kokkoris, Tatsuya Katabuchi, O. Aberle, C. Wolf, Mario Weigand, Mario Barbagallo, A. Casanovas, P. F. Mastinu, Marco Calviani, Carlo Rubbia, A. G. Smith, R. Dressler, E. Mendoza, S. Barros, L. Cosentino, D. Schumann, Philip Woods, Rene Reifarth, P. Kavrigin, E. Berthoumieux, N. Kivel, A. Tsinganis, Stefan Schmidt, L. Audouin, Nicola Colonna, V. Vlachoudis, E. González-Romero, J. M. Quesada, E. Chiaveri, L. Tassan-Got, E. Dupont, D. Cano-Ott, E. Griesmayer, Y. H. Chen, L. A. Damone, M. Caamaño, S. Heinitz, V. Furman, E. Jericha, V. Ketlerov, Alberto Mengoni, T. Glodariu, Paolo Finocchiaro, F. Cerutti, J. A. Ryan, D. G. Jenkins, Ariel Tarifeño-Saldivia, S. J. Lonsdale, J. Lerendegui-Marco, R. Cardella, I. F. Gonçalves, S. Montesano, A. Stamatopoulos, A. Oprea, J. Heyse, M. Mastromarco, Anton Wallner, J. Billowes, J. Balibrea, P. Schillebeeckx, Hideo Harada, M. Sabaté-Gilarte, M. Diakaki, R. Nolte, P. M. Milazzo, M. Dietz, and A. Goverdovski
Subjects: Physics, Standard solar model, Solar mass, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, 01 natural sciences, 7. Clean energy, Neutron temperature, Nuclear physics, Neutron capture, 13. Climate action, Nucleosynthesis, 0103 physical sciences, Neutron cross section, Astrophysics::Solar and Stellar Astrophysics, Neutron, Nuclear Experiment, 010306 general physics, s-process
Abstract: Neutron capture data on intermediate mass nuclei are of key importance to nucleosynthesis in the weak component of the slow neutron capture processes, which occurs in massive stars. The $(n,\gamma)$ cross section on $^{70}Ge$, which is mainly produced in the s process, was measured at the neutron time-of-flight facility n_TOF at CERN. Resonance capture kernels were determined up to 40 keV neutron energy and average cross sections up to 300 keV. Stellar cross sections were calculated from $kT=5 keV$ to $kT=100 keV$ and are in very good agreement with a previous measurement by Walter and Beer (1985) and recent evaluations. Average cross sections are in agreement with Walter and Beer (1985) over most of the neutron energy range covered, while they are systematically smaller for neutron energies above 150 keV. We have calculated isotopic abundances produced in s-process environments in a 25 solar mass star for two initial metallicities (below solar and close to solar). While the low metallicity model reproduces best the solar system germanium isotopic abundances, the close to solar model shows a good global match to solar system abundances in the range of mass numbers A=60–80.
Published: 2019

29. Choosing a Maximum Drift Rate in a SETI Search: Astrophysical Considerations

Author: Andrew P. V. Siemion, Sofia Z. Sheikh, J. Emilio Enriquez, and Jason T. Wright
Subjects: Physics, 010504 meteorology & atmospheric sciences, Astronomy, Transmitter, Extraterrestrial intelligence, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Signal, Computational physics, Acceleration, Narrowband, Space and Planetary Science, 0103 physical sciences, Range (statistics), Stochastic drift, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Search for extraterrestrial intelligence, 0105 earth and related environmental sciences
Abstract: A radio transmitter which is accelerating with a non-zero radial component with respect to a receiver will produce a signal that appears to change its frequency over time. This effect, commonly produced in astrophysical situations where orbital and rotational motions are ubiquitous, is called a drift rate. In radio SETI (Search for Extraterrestrial Intelligence) research, it is unknown a priori which frequency a signal is being sent at, or even if there will be any drift rate at all besides motions within the solar system. Therefore a range of potential drift rates need to be individually searched, and a maximum drift rate needs to be chosen. The middle of this range is zero, indicating no acceleration, but the absolute value for the limits remains unconstrained. A balance must be struck between computational time and the possibility of excluding a signal from an ETI. In this work, we examine physical considerations that constrain a maximum drift rate and highlight the importance of this problem in any narrowband SETI search. We determine that a normalized drift rate of 200 nHz (eg. 200 Hz/s at 1 GHz) is a generous, physically motivated guideline for the maximum drift rate that should be applied to future narrowband SETI projects if computational capabilities permit., Published in the Astrophysical Journal, 16 pages, 2 figures
Published: 2019

30. $^{80}$Se(n,$\gamma$) cross-section measurement at CERN n_TOF

Author: I. Knapova, P. Vaz, F. Mingrone, E. Jericha, J. Andrzejewski, Luis Caballero, Paolo Finocchiaro, A. Gawlik, F. Ogállar, V. Vlachoudis, G. Tagliente, D. Ramos Doval, G. Vannini, F. Gunsing, Javier Praena, J. L. Tain, Cristian Massimi, F. Calviño, J. Perkowski, Alberto Ventura, M. Sabaté-Gilarte, Z. Eleme, A. Casanovas, Emilio Andrea Maugeri, E. Mendoza, V. Variale, Dimitri Rochman, Arnd R. Junghans, Rene Reifarth, M. Kokkoris, Y. Kopatch, Carlos Guerrero, L. Cosentino, S. Heinitz, A. Tsinganis, J. Lerendegui-Marco, S. Amaducci, R. Garg, J. M. Quesada, L. Tassan-Got, P. J. Davies, A. Kimura, Diego Vescovi, C. Petrone, Luciano Piersanti, Sergio Cristallo, E. González-Romero, Alfredo Ferrari, Nicola Colonna, E. Chiaveri, G. Cortes, M. A. Cortés-Giraldo, D. Cano-Ott, M. Caamaño, O. Aberle, I. Ferro-Gonçalves, P. J. Woods, E. Dupont, J. Balibrea-Correa, D. Macina, S. Valenta, F. Cerutti, A. Sekhar, M. Diakaki, P. M. Milazzo, Pierfrancesco Mastinu, A. S. Brown, A. Pavlik, N. Patronis, C. Domingo-Pardo, M. Bacak, A. Musumarra, M. A. Millán-Callado, Marco Calviani, P. Schillebeeckx, Mario Barbagallo, B. Fernández-Domíngez, A. G. Smith, D. Schumann, Ignacio Porras, C. Rubbia, Simone Gilardoni, S. Urlass, P. Torres-Sánchez, Alberto Mengoni, I. Ladarescu, A. Oprea, J. Heyse, M. Dietz, M. Mastromarco, U. Jiri, Q. Ducasse, A. Saxena, V. Michalopoulou, K. Göbel, Anton Wallner, S. Bennett, A. Masi, A. Stamatopoulos, T. Wright, J. Moreno-Soto, D. G. Jenkins, I. Duran, Maurizio Busso, R. Vlastou, R. Dressler, Damir Bosnar, Y. Kadi, Ariel Tarifeño-Saldivia, S. J. Lonsdale, L. A. Damone, M. Krtička, T. Martinez, E. Berthoumieux, N. V. Sosnin, Annamaria Mazzone, Petar Žugec, P. Sprung, Alexandru Negret, F. Käppeler, E. Pirovano, V. Babiano-Suarez, A. Manna, V. Furman, B. Thomas, V. Alcayne, L. Audouin, Claudia Lederer-Woods, Deniz Kurtulgil, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, European Research Council (ERC) 681740, Babiano-Suarez V., Aberle O., Alcayne V., Amaducci S., Andrzejewski J., Audouin L., Bacak M., Balibrea-Correa J., Barbagallo M., Bennett S., Berthoumieux E., Bosnar D., Brown A.S., Busso M., Caamao M., Caballero L., Calviani M., Calvio F., Cano-Ott D., Casanovas A., Cerutti F., Chiaveri E., Colonna N., Cortes G.P., Cortes-Giraldo M.A., Cosentino L., Cristallo S., Damone L.A., Davies P.J., Diakaki M., Dietz M., Domingo-Pardo C., Dressler R., Ducasse Q., Dupont E., Durn I., Eleme Z., Fernndez-Domingez B., Ferrari A., Ferro-Goncalves I., Finocchiaro P., Furman V., Garg R., Gawlik A., Gilardoni S., Gobel K., Gonzlez-Romero E., Guerrero C., Gunsing F., Heinitz S., Heyse J., Jenkins D.G., Jericha E., Jiri U., Junghans A., Kadi Y., Kappeler F., Kimura A., Knapov I., Kokkoris M., Kopatch Y., Krticka M., Kurtulgil D., Ladarescu I., Lederer-Woods C., Lerendegui-Marco J., Lonsdale S.-J., Macina D., Manna A., Martinez T., Masi A., Massimi C., Mastinu P.F., Mastromarco M., Maugeri E., Mazzone A., Mendoza E., Mengoni A., Michalopoulou V., Milazzo P.M., Milln-Callado M.A., Mingrone F., Moreno-Soto J., Musumarra A., Negret A., Ogllar F., Oprea A., Patronis N., Pavlik A., Perkowski J., Petrone C., Piersanti L., Pirovano E., Porras I., Praena J., Quesada J.M., Ramos Doval D., Reifarth R., Rochman D., Rubbia C., Sabate-Gilarte M., Saxena A., Schillebeeckx P., Schumann D., Sekhar A., Smith A.G., Sosnin N., Sprung P., Stamatopoulos A., Tagliente G., Tain J.L., Tarifeo-Saldivia A.E., Tassan-Got L., Thomas B., Torres-Snchez P., Tsinganis A., 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.J., Zugec P., Babiano-Suarez, V., Aberle, O., Alcayne, V., Amaducci, S., Andrzejewski, J., Audouin, L., Bacak, M., Balibrea-Correa, J., Barbagallo, M., Bennett, S., Berthoumieux, E., Bosnar, D., Brown, A. S., Busso, M., Caamao, M., Caballero, L., Calviani, M., Calvio, F., Cano-Ott, D., Casanovas, A., Cerutti, F., Chiaveri, E., Colonna, N., Cortes, G. P., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Damone, L. A., Davies, P. J., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Ducasse, Q., Dupont, E., Durn, I., Eleme, Z., Fernndez-Domingez, B., Ferrari, A., Ferro-Goncalves, I., Finocchiaro, P., Furman, V., Garg, R., Gawlik, A., Gilardoni, S., Gobel, K., Gonzlez-Romero, E., Guerrero, C., Gunsing, F., Heinitz, S., Heyse, J., Jenkins, D. G., Jericha, E., Jiri, U., Junghans, A., Kadi, Y., Kappeler, F., Kimura, A., Knapov, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Lonsdale, S. -J., Macina, D., Manna, A., Martinez, T., Masi, A., Massimi, C., Mastinu, P. F., Mastromarco, M., Maugeri, E., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Milln-Callado, M. A., Mingrone, F., Moreno-Soto, J., Musumarra, A., Negret, A., Ogllar, F., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Petrone, C., Piersanti, L., Pirovano, E., Porras, I., Praena, J., Quesada, J. M., Ramos Doval, D., Reifarth, R., Rochman, D., Rubbia, C., Sabate-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Sekhar, A., Smith, A. G., Sosnin, N., Sprung, P., Stamatopoulos, A., Tagliente, G., Tain, J. L., Tarifeo-Saldivia, A. E., Tassan-Got, L., Thomas, B., Torres-Snchez, P., Tsinganis, A., 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. J., and Zugec, P.
Subjects: Physics, History, Large Hadron Collider, Isotope, General Physics and Astronomy, 80Se, neutron capture, neutron time of flight, n_TOF, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Computer Science Applications, Education, Nuclear physics, s process, neutron physics, Time of flight, Nucleosynthesis, 0103 physical sciences, Neutron cross section, Radiative transfer, Nuclear Physics - Experiment, Slow neutron, 010306 general physics, s-process, 010303 astronomy & astrophysics
Abstract: Radiative neutron capture cross section measurements are of fundamental importance for the study of the slow neutron capture (s-) process of nucleosynthesis. This mechanism is responsible for the formation of most elements heavier than iron in the Universe. Particularly relevant are branching nuclei along the s-process path, which are sensitive to the physical conditions of the stellar environment. One such example is the branching at 79Se (3.27 × 105 y), which shows a thermally dependent β-decay rate. However, an astrophysically consistent interpretation requires also the knowledge of the closest neighbour isotopes involved. In particular, the 80Se(n,γ) cross section directly affects the stellar yield of the “cold” branch leading to the formation of the s-only 82Kr. Experimentally, there exists only one previous measurement on 80Se using the time of flight (TOF) technique. However, the latter suffers from some limitations that are described in this presentation. These drawbacks have been significantly improved in a recent measurement at CERN n TOF. This contribution presents a summary of the latter measurement and the status of the data analysis.
Published: 2019

31. Calibrating Iodine Cells for Precise Radial Velocities

Author: Sharon X. Wang, Phillip J. MacQueen, Joseph R. Schmitt, Jason T. Wright, Coyne A. Gibson, David R. Doss, and William D. Cochran
Subjects: Materials science, 010504 meteorology & atmospheric sciences, Absorption spectroscopy, FOS: Physical sciences, 01 natural sciences, Spectral line, law.invention, Telescope, Optics, Operating temperature, law, 0103 physical sciences, Calibration, 010303 astronomy & astrophysics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), business.industry, Resolution (electron density), Astronomy and Astrophysics, Wavelength, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: High fidelity iodine spectra provide the wavelength and instrument calibration needed to extract precise radial velocities (RVs) from stellar spectral observations taken through iodine cells. Such iodine spectra are usually taken by a Fourier Transform Spectrometer (FTS). In this work, we investigated the reason behind the discrepancy between two FTS spectra of the iodine cell used for precise RV work with the High Resolution Spectrograph (HRS) at the Hobby-Eberly Telescope. We concluded that the discrepancy between the two HRS FTS spectra was due to temperature changes of the iodine cell. Our work demonstrated that the ultra-high resolution spectra taken by the TS12 arm of the Tull Spectrograph One at McDonald Observatory are of similar quality to the FTS spectra and thus can be used to validate the FTS spectra. Using the software IodineSpec5, which computes the iodine absorption lines at different temperatures, we concluded that the HET/HRS cell was most likely not at its nominal operating temperature of 70 degree Celsius during its FTS scan at NIST or at the TS12 measurement. We found that extremely high resolution echelle spectra (R>200,000) can validate and diagnose deficiencies in FTS spectra. We also recommend best practices for temperature control and nightly calibration of iodine cells., 28 pages, 11 figures, PASP accepted
Published: 2019
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32. Measurement of 73Ge(n,g) cross sections and implications for stellar nucleosynthesis

Author: S. Montesano, V. Khryachkov, A. Tsinganis, Alfredo Ferrari, F. R. Palomo-Pinto, Nicola Colonna, E. Dupont, A. Goverdovski, G. Tagliente, J. Heyse, A. Musumarra, Claudia Lederer-Woods, M. Mastromarco, F. Gunsing, Cristian Massimi, Pedro G. Ferreira, Mario Weigand, I. Duran, E. Mendoza, Anton Wallner, M. Bacak, P. V. Sedyshev, M. Mirea, J. Balibrea, V. Furman, F. Calviño, H. Leeb, Ioana Gheorghe, J. Perkowski, Tanja Heftrich, S. Heinitz, J. Billowes, M. Sabaté-Gilarte, A. Kimura, Francesca Matteucci, A. Riego-Perez, T. Glodariu, M. Krtička, A. Hernández-Prieto, S. Warren, V. Bécares, L. Cosentino, N. Patronis, R. Dressler, Roberto Losito, M. S. Robles, T. Martinez, E. Jericha, C. Weiss, D. Macina, R. Vlastou, V. Variale, Paolo Finocchiaro, A. Stamatopoulos, P. M. Milazzo, O. Aberle, J. A. Ryan, D. G. Jenkins, E. Berthoumieux, Mario Barbagallo, M. Diakaki, Alberto Mengoni, J. Marganiec, Carlos Guerrero, F. Bečvář, A. Saxena, S. V. Suryanarayana, D. Schumann, Damir Bosnar, Y. Kadi, E. González-Romero, P. F. Mastinu, A. Tattersall, P. Schillebeeckx, Hideo Harada, M. A. Cortés-Giraldo, P. Kavrigin, F. Mingrone, S. Valenta, J. Andrzejewski, Ralf Nolte, Marco Calviani, V. Vlachoudis, M. Kokkoris, Rene Reifarth, E. Griesmayer, A. G. Smith, Petar Žugec, C. Paradela, M. Dietz, Stefan Schmidt, L. A. Damone, L. Audouin, J. M. Quesada, L. Tassan-Got, K. Göbel, B. Fernández-Domínguez, F. Käppeler, T. Wright, Tatsuya Katabuchi, S. Barros, U. Battino, A. Pavlik, C. Domingo-Pardo, E. Chiaveri, D. Cano-Ott, J. I. Porras, I. Knapova, P. Vaz, Alberto Ventura, C. Rubbia, J. L. Tain, Niko Kivel, G. Cortes, J. Lerendegui-Marco, A. R. García, M. Brugger, I. F. Gonçalves, R. J. W. Frost, C. Beinrucker, E. Leal-Cidoncha, Javier Praena, S. Lo Meo, Fabio Belloni, G. Vannini, A. Gawlik, Thomas Rauscher, Ariel Tarifeño-Saldivia, M. Licata, K. Deo, M. Caamaño, V. Ketlerov, F. Cerutti, Lederer-Woods, C., Battino, U., Ferreira, P., Gawlik, A., Guerrero, C., Gunsing, F., Heinitz, S., Lerendegui-Marco, J., Mengoni, A., Reifarth, R., Tattersall, A., Valenta, S., Weiss, C., Aberle, O., Andrzejewski, J., Audouin, L., Becares, V., Bacak, M., Balibrea, J., Barbagallo, M., Barros, S., Becvar, F., Beinrucker, C., Belloni, F., Berthoumieux, E., Billowes, J., Bosnar, D., Brugger, M., Caamano, M., Calvino, F., Calviani, M., Cano-Ott, D., Cerutti, F., Chiaveri, E., Colonna, N., Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Damone, L. A., Deo, K., Diakaki, M., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Duran, I., Fernandez-Dominguez, B., Ferrari, A., Finocchiaro, P., Frost, R. J. W., Furman, V., Gobel, K., Garcia, A. R., Gheorghe, I., Glodariu, T., Goncalves, I. F., Gonzalez-Romero, E., Goverdovski, A., Griesmayer, E., Harada, H., Heftrich, T., Hernandez-Prieto, A., Heyse, J., Jenkins, D. G., Jericha, E., Kappeler, F., Kadi, Y., Katabuchi, T., Kavrigin, P., Ketlerov, V., Khryachkov, V., Kimura, A., Kivel, N., Knapova, I., Kokkoris, M., Krticka, M., Leal-Cidoncha, E., Leeb, H., Licata, M., Lo Meo, S., Losito, R., Macina, D., Marganiec, J., Martinez, T., Massimi, C., Mastinu, P., Mastromarco, M., Matteucci, F., Mendoza, E., Milazzo, P. M., Mingrone, F., Mirea, M., Montesano, S., Musumarra, A., Nolte, R., Palomo-Pinto, F. R., Paradela, C., Patronis, N., Pavlik, A., Perkowski, J., Porras, J. I., Praena, J., Quesada, J. M., Rauscher, T., Riego-Perez, A., Robles, M., Rubbia, C., Ryan, J. A., Sabate-Gilarte, M., Saxena, A., Schillebeeckx, P., Schmidt, S., Schumann, D., Sedyshev, P., Smith, A. G., Stamatopoulos, A., Suryanarayana, S. V., Tagliente, G., Tain, J. L., Tarifeno-Saldivia, A., Tassan-Got, L., Tsinganis, A., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Wallner, A., Warren, S., Weigand, M., Wright, T., Zugec, 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), n_TOF, Ministerio de Economía y Competitividad (España), Bécares, V., Bečvář, F., Caamaño, M., Calviño, F., Cortés, G., Cortés-Giraldo, M.A., Damone, L.A., Durán, I., Fernández-Domínguez, B., Frost, R.J.W., Göbel, K., García, A.R., Gonçalves, I.F., González-Romero, E., Hernández-Prieto, A., Jenkins, D.G., Käppeler, F., Krtička, M., Martínez, T., Milazzo, P.M., Palomo-Pinto, F.R., Porras, J.I., Quesada, J.M., Ryan, J.A., Sabaté-Gilarte, M., Smith, A.G., Suryanarayana, S.V., Tain, J.L., Tarifeño-Saldivia, A., Žugec, P., Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. ANT - Advanced Nuclear Technologies Research Group, and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Nucleosynthesis, Neutron capture, s process, Germanium, n_TOF, s proce, Nuclear reaction, Natural abundance, nucl-ex, 01 natural sciences, 7. Clean energy, Stellar nucleosynthesis, CERN, Astrophysics::Solar and Stellar Astrophysics, n_TOF, Nuclear Experiment (nucl-ex), Nuclear Experiment, Physics, Cross section, Germanium, lcsh:QC1-999, PRIRODNE ZNANOSTI. Fizika, Neutron capture, Nucleosynthesis, s process, Nucleosíntesi, Nuclear and High Energy Physics, nTOF, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Neutron, Neutrons--Captura, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Neutrons--Capture, Nuclear physics, 0103 physical sciences, Nuclear Physics - Experiment, 010306 general physics, Nucleosynthesi, Energies::Energia nuclear [Àrees temàtiques de la UPC], Física [Àrees temàtiques de la UPC], 010308 nuclear & particles physics, Capture cross section, NATURAL SCIENCES. Physics, Stars, 13. Climate action, s-process, lcsh:Physics
Abstract: 73Ge(n, γ) cross sections were measured at the neutron time-of-flight facility n_TOF at CERN up to neutron energies of 300keV, providing for the first time experimental data above 8keV. Results indicate that the stellar cross section at kT=30keV is 1.5 to 1.7 times higher than most theoretical predictions. The new cross sections result in a substantial decrease of 73Ge produced in stars, which would explain the low isotopic abundance of 73Ge in the solar system., This work was supported by the Austrian Science Fund FWF (J3503), the Adolf Messer Foundation (Germany), the UK Science and Facilities Council (ST/M006085/1), and the European Research Council ERC-2015-StG Nr.677497.
Published: 2019
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33. Measurement of the 244Cm and 246Cm neutron-induced capture cross sections at the n_TOF facility

Author: A. Oprea, J. Heyse, F. Gunsing, E. Chiaveri, G. Vannini, D. Cano-Ott, Paolo Finocchiaro, M. Bacak, F. Ogállar, V. Bécares, A. Kimura, Y. H. Chen, A. Musumarra, Cristian Massimi, G. Tagliente, J. Ulrich, L. Audouin, V. Michalopoulou, J. Lerendegui-Marco, I. Duran, A. Masi, Francesca Matteucci, A. Gawlik, Mario Barbagallo, G. Cortes, T. Glodariu, Thomas Rauscher, D. G. Jenkins, I. Knapova, D. Schumann, Alfredo Ferrari, D. Radeck, F. Becčvář, I. F. Gonçalves, P. Vaz, F. Mingrone, J. Andrzejewski, R. Dressler, Ralf Nolte, E. Mendoza, Simone Gilardoni, Carlos Guerrero, A. Casanovas, E. Berthoumieux, Alberto Ventura, V. Vlachoudis, L. A. Damone, E. González-Romero, F. Calviño, S. Heinitz, A. S. Brown, A. Tsinganis, M. Diakaki, O. Aberle, L. Cosentino, Nicola Colonna, M. Krtička, J. Perkowski, E. Dupont, G. Bellia, A. Pavlik, P. Schillebeeckx, Maurizio Busso, C. Domingo-Pardo, Diego Vescovi, T. Martinez, V. Variale, A. Saxena, A. Stamatopoulos, Dimitri Rochman, V. Alcayne, Z. Eleme, Hideo Harada, Ariel Tarifeño-Saldivia, S. J. Lonsdale, D. Macina, Javier Praena, S. Lo Meo, L. Persanti, Y. Kopatch, Ignacio Porras, A. Manna, Rene Reifarth, S. Urlass, P. M. Milazzo, M. Mastromarco, P. F. Mastinu, L. Caballero-Ontanaya, Alexandru Negret, Claudia Lederer-Woods, J. L. Tain, T. Talip, J. M. Quesada, N. Patronis, L. Tassan-Got, B. Fernández-Domínguez, Anton Wallner, F. Käppeler, M. Caamaño, Sergio Cristallo, Deniz Kurtulgil, Niko Kivel, F. Cerutti, V. Furman, M. Sabaté-Gilarte, Alberto Mengoni, I. Ladarescu, N. V. Sosnin, Tatsuya Katabuchi, Annamaria Mazzone, Petar Žugec, J. Billowes, D. Ramos-Doval, Emilio Andrea Maugeri, M. Kokkoris, M. A. Cortés-Giraldo, R. Vlastou, Damir Bosnar, Y. Kadi, S. Simone, K. Göbel, T. Wright, S. Valenta, Marco Calviani, A. G. Smith, M. Dietz, Philip Woods, Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. Doctorat en Enginyeria Nuclear i de les Radiacions Ionitzants, Universitat Politècnica de Catalunya. ANT - Advanced Nuclear Technologies Research Group, 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre National de la Recherche Scientifique (CNRS), Université Paris-Saclay, Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Alcayne, V., Kimura, A., Mendoza, E., Cano-Ott, D., Martínez, T., Aberle, O., Andrzejewski, J., Audouin, L., Bécares, V., Bacak, M., Barbagallo, M., Becčvář, F., Bellia, G., Berthoumieux, E., Billowes, J., Bosnar, D., Brown, A., Busso, M., Caamaño, M., Caballero-Ontanaya, L., Calviño, F., Calviani, M., 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., Dietz, M., Domingo-Pardo, C., Dressler, R., Dupont, E., Durán, I., Eleme, Z., Fernández-Domínguez, B., Ferrari, A., Finocchiaro, P., Furman, V., Göbel, K., Gawlik, A., Gilardoni, S., Glodariu, T., Gonçalves, I. F., González-Romero, E., Guerrero, C., Gunsing, F., Harada, H., Heinitz, S., Heyse, J., Jenkins, D. G., Käppeler, F., Kadi, Y., Katabuchi, T., Kivel, N., Knapova, I., Kokkoris, M., Kopatch, Y., Krtička, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lerendegui-Marco, J., Meo, S. Lo, Lonsdale, S. J., Macina, D., Manna, A., Masi, A., Massimi, C., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mingrone, F., Musumarra, A., Negret, A., Nolte, R., Ogállar, F., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Persanti, L., Porras, I., Praena, J., Quesada, J. M., Radeck, D., Ramos-Doval, D., Rauscher, T., Reifarth, R., Rochman, D., Sabaté-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Simone, S., Smith, A. G., Sosnin, N. V., Stamatopoulos, A., Tagliente, G., Tain, J. L., Talip, T., Tarifeño-Saldivia, A., Tassan-Got, L., 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.
Subjects: Nuclear reaction, Neutron emission, QC1-999, Nuclear physics, 01 natural sciences, 7. Clean energy, law.invention, law, 0103 physical sciences, CERN, Neutron, n_TOF, 010306 general physics, [PHYS]Physics [physics], Physics, Energies::Energia nuclear [Àrees temàtiques de la UPC], Neutrons, Isotope, Física [Àrees temàtiques de la UPC], Cross section, 010308 nuclear & particles physics, r-process, Actinide, Nuclear reactor, Neutron capture, n_TOF, 244Cm, 246Cm, neutron capture, 13. Climate action, neutron capture, n_TOF, r-process, Física nuclear, Other, n_TOF, neutron reaction, Cm, neutron capture
Abstract: The neutron capture reactions of the 244Cm and 246Cm isotopes open the path for the formation of heavier Cm isotopes and heavier elements such asThe neutron capture reactions of the 244Cm and 246Cm isotopes open the path for the formation of heavier Cm isotopes and heavier elements such as Bk and Cf in a nuclear reactor. In addition, both isotopes belong to the minor actinides with a large contribution to the decay heat and to the neutron emission in irradiated fuels. There are only two previous 244Cm and 246Cm capture cross section measurements: one in 1969 using a nuclear explosion and the most recent data measured at J-PARC in 2010. The data for both isotopes are very scarce due to the difficulties in performing the measurements: high intrinsic activity of the samples and limited facilities capable of providing isotopically enriched samples. We have measured both neutron capture cross sections at the n_TOF Experimental Area 2 (EAR-2) with three C6D6 detectors and also at Area 1 (EAR-1) with the TAC. Preliminary results assessing the quality and limitations (background subtraction, measurement technique and counting statistics) of this new experimental datasets are presented and discussed. Bk and Cf in a nuclear reactor. In addition, both isotopes belong to the minor actinides with a large contribution to the decay heat and to the neutron emission in irradiated fuels. There are only two previous 244Cm and 246Cm capture cross section measurements: one in 1969 using a nuclear explosion and the most recent data measured at J-PARC in 2010. The data for both isotopes are very scarce due to the difficulties in performing the measurements: high intrinsic activity of the samples and limited facilities capable of providing isotopically enriched samples. We have measured both neutron capture cross sections at the n_TOF Experimental Area 2 (EAR-2) with three C6D6 detectors and also at Area 1 (EAR-1) with the TAC. Preliminary results assessing the quality and limitations (background subtraction, measurement technique and counting statistics) of this new experimental datasets are presented and discussed.
Published: 2019

34. TESS reveals that the nearby Pisces-Eridanus stellar stream is only 120 Myr old

Author: Jeffrey D. Cummings, Marcel A. Agüeros, Jason T. Wright, Jason L. Curtis, and Eric E. Mamajek
Subjects: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Eridanus, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, media_common, Physics, Astronomy and Astrophysics, Exoplanet, Photometry (astronomy), Stars, Star cluster, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Sky, Astrophysics::Earth and Planetary Astrophysics, Pleiades, Open cluster
Abstract: Pisces-Eridanus (Psc-Eri), a nearby ($d$ $\simeq$ 80-226 pc) stellar stream stretching across $\approx$120 degrees of the sky, was recently discovered with Gaia data. The stream was claimed to be $\approx$1 Gyr old, which would make it an exceptional discovery for stellar astrophysics, as star clusters of that age are rare and tend to be distant, limiting their utility as benchmark samples. We test this old age for Psc-Eri in two ways. First, we compare the rotation periods for 101 low-mass members (measured using time series photometry from the Transiting Exoplanet Survey Satellite, TESS) to those of well-studied open clusters. Second, we identify 34 new high-mass candidate members, including the notable stars $\lambda$ Tauri (an Algol-type eclipsing binary) and HD 1160 (host to a directly imaged object near the hydrogen-burning limit). We conduct an isochronal analysis of the color--magnitude data for these highest-mass members, again comparing our results to those for open clusters. Both analyses show that the stream has an age consistent with that of the Pleiades, i.e., $\approx$120 Myr. This makes the Psc-Eri stream an exciting source of young benchmarkable stars and, potentially, exoplanets located in a more diffuse environment that is distinct from that of the Pleiades and of other dense star clusters., Comment: 15 pages, 5 figures, 3 tables. The figure set (101 images) for Figure 2 will be available on AJ upon publication
Published: 2019
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35. Photon-weighted barycentric correction and its importance for precise radial velocities

Author: Ryan T. Blackman, René Tronsgaard, Jason T. Wright, Lars A. Buchhave, and Jason D. Eastman
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], Mathematical analysis, Flux, Magnitude (mathematics), FOS: Physical sciences, Astronomy and Astrophysics, Barycentric coordinate system, 01 natural sciences, Measure (mathematics), Term (time), 010309 optics, Radial velocity, Space and Planetary Science, Position (vector), 0103 physical sciences, spectrographs [Instrumentation], Constant (mathematics), Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract: When applying the barycentric correction to a precise radial velocity measurement, it is common practice to calculate its value only at the photon-weighted midpoint time of the observation instead of integrating over the entire exposure. However, since the barycentric correction does not change linearly with time, this leads to systematic errors in the derived radial velocities. The typical magnitude of this second-order effect is of order 10 cm s$^{-1}$, but it depends on several parameters, e.g. the latitude of the observatory, the position of the target on the sky, and the exposure time. We show that there are realistic observing scenarios, where the errors can amount to more than 1 ms$^{-1}$. We therefore recommend that instruments operating in this regime always record and store the exposure meter flux curve (or a similar measure) to be used as photon-weights for the barycentric correction. In existing data, if the flux curve is no longer available, we argue that second-order errors in the barycentric correction can be mitigated by adding a correction term assuming constant flux., 9 pages, 7 figures, accepted to MNRAS
Published: 2019

36. KELT-22Ab: A Massive, Short-Period Hot Jupiter Transiting a Near-solar Twin

Author: Marshall C. Johnson, Joshua Pepper, David Kasper, Michael L. Calkins, Denise C. Stephens, Nate McCrady, Eric L. N. Jensen, Ivan A. Curtis, Perry Berlind, Jason D. Eastman, Dax L. Feliz, Valerio Bozza, Kim K. McLeod, David H. Cohen, Xinyu Yao, Thomas G. Beatty, Steven Villanueva, Thomas E. Oberst, David J. James, Thiam-Guan Tan, George Zhou, Rudolf B. Kuhn, Keivan G. Stassun, Amber Malpas, Phillip A. Reed, Benjamin J. Fulton, Phil Evans, John Asher Johnson, Robert J. Siverd, Joseph E. Rodriguez, Jonathan Labadie-Bartz, Samson A. Johnson, Matthew T. Penny, David H. Sliski, B. Scott Gaudi, Daniel Bayliss, Jason T. Wright, Michael D. Albrow, Howard M. Relles, Joao Bento, David R. Ciardi, Gilbert A. Esquerdo, Michael D. Joner, David W. Latham, John F. Kielkopf, Knicole D. Colón, Mark Manner, Roberto Zambelli, Daniel J. Stevens, Allyson Bieryla, Karen A. Collins, Kaloyan Penev, Joao Gregorio, Robert A. Wittenmyer, Michael B. Lund, and Chris Stockdale
Subjects: Physics, planets and satellites: detection, 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Methods observational, planets and satellites: gaseous planets, techniques: photometric, Space and Planetary Science, techniques: radial velocities, 0103 physical sciences, Hot Jupiter, methods: observational, techniques: spectroscopic, Period (geology), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: We present the discovery of KELT-22Ab, a hot Jupiter from the KELT-South survey. KELT-22Ab transits the moderately bright (V∼11.1) Sun-like G2V star TYC 7518-468-1. The planet has an orbital period of P = 1.3866529±0.0000027 days, a radius of R_P = 1.285^(+0.12)_(−0.071) R_J, and a relatively large mass of M_P = 3.47^(+0.15)_(−0.14) M_J. The star has R⋆ = 1.099^(+0.079)_(−0.046) R⊙, M⋆ = 1.092^(+0.045)_(−0.041) M⊙, T_(eff) = 5767^(+50)_(−49) K, log g⋆ = 4.393^(+0.039)_(−0.060) (cgs), and [m/H] = +0.259^(+0.085)_(−0.083), and thus, other than its slightly super-solar metallicity, appears to be a near solar twin. Surprisingly, KELT-22A exhibits kinematics and a Galactic orbit that are somewhat atypical for thin disk stars. Nevertheless, the star is rotating quite rapidly for its estimated age, shows evidence of chromospheric activity, and is somewhat metal rich. Imaging reveals a slightly fainter companion to KELT-22A that is likely bound, with a projected separation of 6” (∼1400 AU). In addition to the orbital motion caused by the transiting planet, we detect a possible linear trend in the radial velocity of KELT-22A suggesting the presence of another relatively nearby body that is perhaps non-stellar. KELT-22Ab is highly irradiated (as a consequence of the small semi-major axis of a/R⋆ = 4.97), and is mildly inflated. At such small separations, tidal forces become significant. The configuration of this system is optimal for measuring the rate of tidal dissipation within the host star. Our models predict that, due to tidal forces, the semi-major axis of KELT-22Ab is decreasing rapidly, and is thus predicted to spiral into the star within the next Gyr.
Published: 2019

37. First radial velocity results from the MINiature Exoplanet Radial Velocity Array (MINERVA)

Author: Timothy D. Morton, Ana Colon, Philip S. Muirhead, Jon de Vera, Peter Plavchan, Connor Robinson, Emilio E. Falco, Adam S. Bolton, Samson A. Johnson, Gilbert A. Esquerdo, John Hamlin, William J. Schap, Sharon X. Wang, Gabriel Grell, Jason D. Eastman, Anthony Sergi, Kevin O. Rivera-García, Juliana Garcia-Mejia, Audrey Houghton, George Lawrence, Eric Blackhurst, Matthew A. Cornachione, Jonathan Horner, Annie Kirby, Justin Myles, Claire Geneser, Robert A. Wittenmyer, Michael Bottom, David H. Sliski, Tony Reed, Samuel Halverson, Nate McCrady, Ashley D. Baker, Jason T. Wright, John Asher Johnson, Chantanelle Nava, Howard M. Relles, Julien Andrew Luebbers, S. Janssens, Cullen H. Blake, Bryson Cale, Graeme Jonas, Perry Berlind, Forest Chaput de Saintonge, Ted Groner, Steven R. Gibson, Michael L. Calkins, Reed Riddle, Jonathan J. Swift, Maurice Wilson, Damien Jones, Pascal Fortin, M. Henderson, Thomas G. Beatty, and Stuart I. Barnes
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, 01 natural sciences, symbols.namesake, Optics, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Dispersion (water waves), 010303 astronomy & astrophysics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Exoplanet, Radial velocity, Stars, Space and Planetary Science, symbols, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Doppler effect, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: The MINiature Exoplanet Radial Velocity Array (MINERVA) is a dedicated observatory of four 0.7m robotic telescopes fiber-fed to a KiwiSpec spectrograph. The MINERVA mission is to discover super-Earths in the habitable zones of nearby stars. This can be accomplished with MINERVA's unique combination of high precision and high cadence over long time periods. In this work, we detail changes to the MINERVA facility that have occurred since our previous paper. We then describe MINERVA's robotic control software, the process by which we perform 1D spectral extraction, and our forward modeling Doppler pipeline. In the process of improving our forward modeling procedure, we found that our spectrograph's intrinsic instrumental profile is stable for at least nine months. Because of that, we characterized our instrumental profile with a time-independent, cubic spline function based on the profile in the cross dispersion direction, with which we achieved a radial velocity precision similar to using a conventional "sum-of-Gaussians" instrumental profile: 1.8 m s$^{-1}$ over 1.5 months on the RV standard star HD 122064. Therefore, we conclude that the instrumental profile need not be perfectly accurate as long as it is stable. In addition, we observed 51 Peg and our results are consistent with the literature, confirming our spectrograph and Doppler pipeline are producing accurate and precise radial velocities., Comment: 22 pages, 9 figures, submitted to PASP, Peer-Reviewed and Accepted
Published: 2019
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38. Measurement of the differential cross sections for W -boson production in association with jets in pp¯ collisions at s=1.96 TeV

Author: M. Jones, Julia Thom, Elliot Lipeles, A. Aurisano, Yuji Takeuchi, Kevin Lannon, Guillelmo Gomez-Ceballos, J. Antos, L. Ortolan, M. Mussini, Massimo Casarsa, S. Torre, Stephan Lammel, Roman Lysak, K. Matera, D. Waters, A. Mitra, M. Gold, Lucio Cerrito, A. Artikov, D. Amidei, C. Pagliarone, G. Velev, E. J. Jeon, Maxwell Chertok, H. Gerberich, M. Dorigo, M. Vidal, B. Esham, P. Wilson, Aidan Robson, D. P. Benjamin, Virgil E Barnes, W. Ketchum, Jochen Jens Heinrich, A. Mukherjee, S. Behari, Luigi Marchese, Stanislav Tokár, Adrian Buzatu, S. Carrillo, P. Totaro, G. Lungu, M. E. Mattson, T. Tomura, Andrea Bocci, D. Tonelli, V. Saveliev, Jian Tang, Matthew Herndon, G. Volpi, Gervasio Gomez, T. Wright, Luca Scodellaro, J. Vizán, H. H. Williams, T. Nigmanov, Aristotle Calamba, Jonathan L. Rosner, D. Chokheli, T. Kuhr, Y. Kato, W. Hopkins, J. Guimaraes Da Costa, W. Badgett, T. Aaltonen, Michal Kreps, Giovanni Bellettini, Intae Yu, M. J. Kim, D. H. Kim, K. Gibson, Matteo Cremonesi, M. Hussein, S. Rolli, Benjamin Kilminster, C. Vellidis, Aurore Savoy-Navarro, I. V. Gorelov, Zhenbin Wu, R. D. Field, Risto Orava, I. Redondo Fernández, R. Culbertson, O. Norniella, R. Vilar, S. H. Kim, Javier Cuevas, J. Strologas, J. P. Fernández Ramos, Xin Wu, G. Chlachidze, M. Shimojima, T. Yang, F. Canelli, C. M. Ginsburg, P. F. Shepard, S. H. Oh, B. Auerbach, P. Giromini, Koji Sato, E. Palencia, Sergo Jindariani, L. Santi, Mario Campanelli, Christoph Paus, Barry Blumenfeld, Peter Wagner, E. Thomson, Roger Moore, B. Jayatilaka, Fabrizio Scuri, A. Driutti, Sooran Kim, Anna Zanetti, J. Budagov, B. Di Ruzza, C. A. Cox, K. Kondo, Matteo Bauce, R. Wallny, Tara Shears, D. J. Cox, Y. C. Yang, T. Harrington-Taber, U. K. Yang, D. Yamato, Ting Miao, D. Goldin, K. Takemasa, A. Di Canto, B. A. Barnett, Giorgio Apollinari, W. C. Wester, Itsuo Nakano, K. Tollefson, F. Vázquez, M. M. Deninno, D. Lucchesi, M. E. Convery, Henry J. Frisch, P. Schlabach, Teruki Kamon, P. Mazzanti, Bruno Casal, Elisabetta Pianori, A. V. Kotwal, Duncan Carlsmith, P. Barria, E. James, F. Rimondi, Naoki Kimura, L. Pondrom, D. Cauz, Th. Müller, I. Shreyber-Tecker, P. Marino, K. Sliwa, Federico Sforza, R. McNulty, M. Hare, L. Oakes, A. Barbaro-Galtieri, Jane Nachtman, Seo-Young Noh, J. R. Smith, D. Mietlicki, Caterina Vernieri, Fumihiko Ukegawa, A. Pranko, M. Tecchio, R. Forrest, Sally Seidel, Y. D. Oh, E. Michielin, Ryan Christopher Edgar, T. Yoshida, Gianluca Introzzi, U. Husemann, Joe Kroll, M. Kambeitz, A. Loginov, A. B. Wicklund, C. Bromberg, P. Mehtala, Hao Song, L. Demortier, Jacobo Konigsberg, Hyun-Chul Kim, A. T. Laasanen, Monica D'Onofrio, G. P. Yeh, I. Suslov, James Russ, Kohei Yorita, D. Glenzinski, E. Gerchtein, H. Wolfmeister, T. A. Schwarz, P. Garosi, N. Moggi, G. Manca, Sinead Farrington, T. R. Junk, Nicola D'Ascenzo, A. Napier, J. A. Appel, Pavol Bartos, A. Simonenko, K. T. Pitts, A. Boveia, Stefano Camarda, E. E. Schmidt, G. Pauletta, K. R. Bland, J. Yoh, Mousumi Datta, D. W. Jang, Q. Liu, Christopher Clarke, Y. Funakoshi, C. Galloni, D. Stentz, S. Poprocki, E. Gramellini, A. Bodek, T. J. Phillips, E. Brucken, M. Trovato, V. Papadimitriou, A. Lucà, G. Punzi, Daniel Whiteson, G. B. Yu, F. Ruffini, M. Stancari, Ziqing Hong, Y. K. Kim, A. Golossanov, Alessandro Cerri, V. V. Glagolev, Andrew Beretvas, Song-Ming Wang, D. J. Kong, A. Anastassov, Luciano Ristori, Paolo Maestro, Tiehui Liu, Michael H Kirby, K. K. Joo, J. N. Bellinger, B. Carls, V. Sorin, Azeddine Kasmi, H. S. Budd, W. Parker, S. R. Hahn, Rodolfo Carosi, P. Lukens, K. Ebina, F. Azfar, Kazuhiko Hara, Chen Zhou, K. Potamianos, Kai Yi, D. Cruz, Fedor Prokoshin, Y. Sudo, Manfred Paulini, T. Okusawa, Satoru Uozumi, N. Giokaris, J. Lys, R. F. Harr, J. Huston, H. Miyake, M. D'Errico, Kevin Burkett, K. Goulianos, F. Happacher, R. Roser, A. Bhatti, P. J. Bussey, Ankita Mehta, J. S. H. Lee, Yongsun Kim, A. T. Goshaw, Paul Lujan, J. E. Kim, M. Corbo, Y. C. Chen, P. de Barbaro, Giorgio Chiarelli, M. J. Morello, Franco Bedeschi, Prabhakar Palni, P. Catastini, J. D. Lewis, S. R. Hou, S. Errede, Yasuyoshi Nagai, D. Toback, Alberto Annovi, R. Madrak, Y. Seiya, Kyung-Suk Cho, R. E. Hughes, T. Rodriguez, R. St. Denis, S. Donati, Kenichi Hatakeyama, J. Naganoma, M. Franklin, J. C. Freeman, A. Ruiz, Giuseppe Latino, V. A. Giakoumopoulou, Chris Hays, Marcelo Vogel, Fabrizio Margaroli, G. Piacentino, L. Brigliadori, F. Ptohos, A. Elagin, C. S. Moon, C. Plager, J. Nett, Stefano Giagu, Jay Dittmann, M. Cordelli, G. Busetto, Brian L Winer, O. Gonzalez Lopez, F. Devoto, S. Leo, Scott Wilbur, M. Iori, S. Amerio, P. B. Renton, Y. Zeng, Hyun Lee, S. Zucchelli, Mauro Ronzani, Peter Wittich, S. Y. Jun, M. Rescigno, Justin Pilot, J. Asaadi, A. G. Clark, Alan Garfinkel, Antonio Limosani, Y. Sakurai, Robin Erbacher, A. Hocker, W-M. Yao, Mark Kruse, Alison Lister, M. Kurata, Sandra Leone, Andrew Ivanov, P. Murat, Daniela Bortoletto, L. Nodulman, W. K. Sakumoto, P. E. Karchin, A. Castro, F. D. Snider, Taegil Bae, V. Thukral, J. Y. Han, S. Wolbers, J. Keung, D. Torretta, Pierfrancesco Butti, A. Sukhanov, C. Mesropian, A. Semenov, M. J. Shochet, G. Flanagan, J. Conway, Viviana Cavaliere, J. S. Wilson, Koji Yamamoto, A. Manousakis-Katsikakis, P. K. Teng, S. Moed, W. Ashmanskas, Sudhir Malik, S. Lockwitz, A. Mazzacane, J. Lueck, V. Rusu, M. Lancaster, Shalhout Shalhout, J. Boudreau, Maxim Goncharov, C. Grosso-Pilcher, and Tetsuo Arisawa
Subjects: Physics, Jet (fluid), Muon, Luminosity (scattering theory), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, Tevatron, Multiplicity (mathematics), Electron, 01 natural sciences, 7. Clean energy, Nuclear physics, 0103 physical sciences, Physics::Accelerator Physics, High Energy Physics::Experiment, 010306 general physics, Collider Detector at Fermilab, Lepton
Abstract: This paper presents a study of the production of a single W boson in association with one or more jets in proton-antiproton collisions at √ s = 1.96 TeV , using the entire data set collected in 2001–2011 by the Collider Detector at Fermilab at the Tevatron, which corresponds to an integrated luminosity of 9.0 fb − 1 . The W boson is identified through its leptonic decays into electron and muon. The production cross sections are measured for each leptonic decay mode and combined after testing that the ratio of the W ( → μ ν ) + jets cross section to the W ( → e ν ) + jets cross section agrees with the hypothesis of e - μ lepton universality. The combination of measured cross sections, differential in the inclusive jet multiplicity ( W + ≥ N jets with N = 1 , 2, 3, or 4) and in the transverse energy of the leading jet, are compared with theoretical predictions.
Published: 2018

39. Retired A Stars and Their Companions VIII: 15 New Planetary Signals Around Subgiants and Transit Parameters for California Planet Search Planets with Subgiant Hosts

Author: Howard Isaacson, Fabienne A. Bastien, Jason T. Wright, Jacob K. Luhn, John Asher Johnson, and Andrew W. Howard
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Subgiant, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Transit time, 01 natural sciences, Stars, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of 7 new planets and 8 planet candidates around subgiant stars, as additions to the known sample of planets around "retired A stars" (Johnson et al. 2006). Among these are the possible first 3-planet systems around subgiant stars, HD 163607 and HD 4917. Additionally, we present calculations of possible transit times, durations, depths, and probabilities for all known planets around subgiant (3 < log g < 4) stars, focused on possible transits during the TESS mission. While most have transit probabilities of 1-2%, we find that there are 3 planets with transit probabilities > 9%., 30 pages, 24 figures, accepted for publication in The Astrophysical Journal. Machine-readable tables included in source download. A coauthor was accidentally omitted in version 1. Version 2 also includes clarification on the calculated transit probabilities. Version 3 fixes small errors in Tables 3 and 5
Published: 2018

40. First measurement of the W-boson mass in run II of the Tevatron

Author: T. AALTONEN, A. ABULENCIA, HELSINKI I.N.S.T. OF PHYS, J. ADELMAN, ILLINOIS U, URBANA, ANTHONY ALLEN AFFOLDER, CHICAGO U, EFI, T. AKIMOTO, SANTA BARBARA, MICHAEL G. ALBROW, TSUKUBA U, S. AMERIO, FERMILAB, DANTE E. AMIDEI, PADUA U, A. ANASTASSOV, MICHIGAN U, K. ANIKEEV, RUTGERS U, PISCATAWAY, A. ANNOVI, J. ANTOS, FRASCATI, M. AOKI, COMENIUS U, G. APOLLINARI, T. ARISAWA, A. ARTIKOV, WASEDA U, WILLIAM JOSEPH ASHMANSKAS, DUBNA, JINR, A. ATTAL, ADAM AURISANO, BARCELONA, IFAE, F. AZFAR, TEXAS A. M, P. AZZI BACCHETTA, OXFORD U, PAOLO AZZURRI, NICOLA BACCHETTA, PISA U, W. BADGETT, ANGELA BARBARO GALTIERI, V. E. BARNES, LBL, BERKELEY, BRUCE A. BARNETT, PURDUE U, S. BAROIANT, JOHNS HOPKINS U, V. BARTSCH, UC, DAVIS, G. BAUER, UNIVERSITY C.O.L.L. LONDON, P. H. BEAUCHEMIN, MIT, LNS, FRANCO BEDESCHI, MCGILL U, S. BEHARI, GIORGIO BELLETTINI, JAMES NUGENT BELLINGER, A. BELLONI, WISCONSIN U, MADISON, DOUGLAS P. BENJAMIN, ANDREW F. BERETVAS, DUKE U, JUERG BERINGER, T. BERRY, ANWAR AHMAD BHATTI, LIVERPOOL U, MORRIS BINKLEY, ROCKEFELLER U, DARIO BISELLO, ILIJA BIZJAK, ROBERT EUGENE BLAIR, CRAIG ALAN BLOCKER, ARGONNE, BARRY J. BLUMENFELD, BRANDEIS U, ANDREA BOCCI, ARIE BODEK, VERONIQUE BOISVERT, G. BOLLA, ROCHESTER U, A. BOLSHOV, D. BORTOLETTO, J. BOUDREAU, A. BOVEIA, PITTSBURGH U, BENJAMIN P. BRAU, LUCA BRIGLIADORI, CARL MICHAEL BROMBERG, BOLOGNA U, ERIK MATTHEWS BRUBAKER, MICHIGAN STATE U, J. BUDAGOV, H. S. BUDD, SARAH REBECCA BUDD, K. BURKETT, GIOVANNI BUSETTO, P. BUSSEY, A. BUZATU, GLASGOW U, K. L. BYRUM, S. CABRERA, M. CAMPANELLI, M. CAMPBELL, GENEVA U, MARIA FLORENCIA CANELLI, A. CANEPA, S. CARRILLO, PENNSYLVANIA U, DUNCAN L. CARLSMITH, FLORIDA U, R. CAROSI, S. CARRON, BRUNO CASAL, M. CASARSA, CANTABRIA U, SANTANDER, A. CASTRO, INFN, UDINE, PIERLUIGI CATASTINI, D. CAUZ, MATTEO CAVALLI SFORZA, ALESSANDRO CERRI, LUCIO CERRITO, SANGHYEON CHANG, Y. C. CHEN, KYUNGPOOK N.A.T.L. U, MAXWELL BENJAMIN CHERTOK, TAIWAN, I.N.S.T. PHYS, GIORGIO CHIARELLI, G. CHLACHIDZE, F. CHLEBANA, I. CHO, K. CHO, D. CHOKHELI, J. P. CHOU, GEORGIOS CHOUDALAKIS, HARVARD U, S. H. CHUANG, K. CHUNG, W. H. CHUNG, CARNEGIE MELLON U, YEON SEI CHUNG, M. CILIJAK, CATALIN IRINEL CIOBANU, M. A. CIOCCI, A. CLARK, D. CLARK, MIRCEA NOROCEL COCA, G. COMPOSTELLA, M. E. CONVERY, JOHN S. CONWAY, B. COOPER, KATHERINE COPIC, M. CORDELLI, G. CORTIANA, F. CRESCIOLI, C. CUENCA ALMENAR, J. CUEVAS, RAY L. CULBERTSON, J. C. CULLY, S. DARONCO, M. DATTA, SAVERIO D'AURIA, T. DAVIES, WILLIAM DAVID DAGENHART, P. DE BARBARO, S. DE CECCO, A. DEISHER, ROME U, G. DE LENTDECKER, G. DE LORENZO, MAURO DELL'ORSO, F. DELLI PAOLI, LUC DEMORTIER, J. DENG, M. DENINNO, D. DE PEDIS, P. F. DERWENT, G. P. DI GIOVANNI, C. DIONISI, PARIS U, VI VII, JAY R. DITTMANN, M. D'ONOFRIO, BAYLOR U, M.A.T.H. DEPT, CHRISTIAN DOERR, S. DONATI, KARLSRUHE U, EKP, P. DONG, J. DONINI, UCLA, T. DORIGO, S. DUBE, JONATHAN ZVI EFRON, ROBIN D. ERBACHER, OHIO STATE U, D. ERREDE, STEVEN MICHAEL ERREDE, RICARDO EUSEBI, H. C. FANG, SINEAD MARIE FARRINGTON, I. FEDORKO, W. T. FEDORKO, R. G. FEILD, MICHAEL FEINDT, YALE U, J. P. FERNANDEZ, R. FIELD, MADRID, CIEMAT, G. FLANAGAN, R. FORREST, S. FORRESTER, M. FRANKLIN, J. C. FREEMAN, I. FURIC, MICHELE GALLINARO, J. GALYARDT, J. E. GARCIA, F. GARBERSON, A. F. GARFINKEL, C. GAY, H. GERBERICH, DAVID W. GERDES, STEFANO GIAGU, P. GIANNETTI, K. GIBSON, JENNIFER LINDSAY GIMMELL, CAMILLE M. GINSBURG, N. GIOKARIS, MARIO PAOLO GIORDANI, P. GIROMINI, M. GIUNTA, GAVRIL A. GIURGIU, V. GLAGOLEV, DOUGLAS A. GLENZINSKI, M. GOLD, NATHAN JOEL GOLDSCHMIDT, NEW MEXICO U, JOEL GOLDSTEIN, ALEXANDER GOLOSSANOV, G. GOMEZ, G. GOMEZ CEBALLOS, MAXIM T. GONCHAROV, O. GONZALEZ, IGOR V. GORELOV, ALFRED T. GOSHAW, KONSTANTIN GOULIANOS, A. GRESELE, SEBASTIAN GRINSTEIN, C. GROSSO PILCHER, ROBERT CRAIG GROUP, ULYSSES GRUNDLER, JOAO PEDRO BARREIRO GUIMARAES DA COSTA, Z. GUNAY UNALAN, CARL H. HABER, K. HAHN, STEPHEN R. HAHN, E. HALKIADAKIS, A. HAMILTON, B. Y. HAN, J. Y. HAN, R. HANDLER, F. HAPPACHER, K. HARA, D. HARE, M. HARE, S. HARPER, TUFTS U, ROBERT FRANCIS HARR, R. M. HARRIS, WAYNE STATE U, M. HARTZ, KENICHI HATAKEYAMA, J. HAUSER, CHRISTOPHER PAUL HAYS, M. HECK, A. HEIJBOER, B. HEINEMANN, JOEL HEINRICH, C. HENDERSON, M. HERNDON, J. HEUSER, DEAN ANDREW HIDAS, CHRISTOPHER S. HILL, D. HIRSCHBUEHL, JAMES ANDREW HOCKER, A. HOLLOWAY, S. HOU, MICHAEL A. HOULDEN, S. C. HSU, BRIAN T. HUFFMAN, SAN DIEGO, R. E. HUGHES, ULRICH HUSEMANN, J. HUSTON, JOSEPH R. INCANDELA, G. INTROZZI, M. IORI, A. IVANOV, B. IYUTIN, ERIC B. JAMES, D. JANG, BODHITHA ANJALIKE JAYATILAKA, D. JEANS, E. J. JEON, SERGO JINDARIANI, W. JOHNSON, M. JONES, K. K. JOO, S. Y. JUN, J. E. JUNG, THOMAS R. JUNK, TERUKI KAMON, PAUL E. KARCHIN, Y. KATO, Y. KEMP, OSAKA CITY U, R. KEPHART, U. KERZEL, V. KHOTILOVICH, B. KILMINSTER, D. H. KIM, H. S. KIM, J. E. KIM, M. J. KIM, S. B. KIM, S. H. KIM, YOUNG KEE KIM, N. KIMURA, LAWRENCE E. KIRSCH, SERGEY KLIMENKO, MARKUS KLUTE, BRUCE OWEN KNUTESON, BYEONGROK KO, K. KONDO, DAE JUNG KONG, JACOBO KONIGSBERG, A. KORYTOV, ASHUTOSH VIJAY KOTWAL, AAFKE CHRISTINE KRAAN, J. KRAUS, M. KREPS, J. KROLL, N. KRUMNACK, MARK CHARLES KRUSE, VYACHESLAV E. KRUTELYOV, T. KUBO, S. E. KUHLMANN, T. KUHR, N. P. KULKARNI, Y. KUSAKABE, S. KWANG, ALVIN TOIVO LAASANEN, S. LAI, STEFANO LAMI, S. LAMMEL, M. LANCASTER, R. L. LANDER, K. LANNON, A. LATH, G. LATINO, I. LAZZIZZERA, THOMAS JOSEPH LECOMPTE, J. LEE, Y. J. LEE, SUNG WON LEE, R. LEFEVRE, NUNO T. LEONARDO, SANDRA LEONE, S. LEVY, JONATHAN D. LEWIS, C. LIN, CHENG JU STEPHEN LIN, MICHAEL ALLEN LINDGREN, E. LIPELES, TONY M. LISS, A. LISTER, D. O. LITVINTSEV, T. LIU, NIGEL S. LOCKYER, A. LOGINOV, MAURIZIO LORETI, R. S. LU, D. LUCCHESI, P. LUJAN, P. LUKENS, G. LUNGU, LOUIS LYONS, J. LYS, R. LYSAK, ELSE LYTKEN, P. MACK, D. MACQUEEN, ROBYN LEIGH MADRAK, KAORI MAESHIMA, KHALDOUN MAKHOUL, T. MAKI, PETAR MAKSIMOVIC, S. MALDE, S. MALIK, G. MANCA, A. MANOUSAKIS, F. MARGAROLI, RADU MARGINEAN, C. MARINO, C. P. MARINO, A. MARTIN, M. MARTIN, V. MARTIN, M. MARTINEZ, R. MARTINEZ BALLARIN, T. MARUYAMA, P. MASTRANDREA, TATSUYA MASUBUCHI, H. MATSUNAGA, M. E. MATTSON, R. MAZINI, PAOLO MAZZANTI, KEVIN S. MCFARLAND, PETER M. MCINTYRE, R. MCNULTY, A. MEHTA, P. MEHTALA, S. MENZEMER, A. MENZIONE, P. MERKEL, CHRISTINA MESROPIAN, A. MESSINA, TING MIAO, N. MILADINOVIC, J. MILES, R. MILLER, C. MILLS, MICHAEL MILNIK, A. MITRA, GUENAKH MITSELMAKHER, A. MIYAMOTO, S. MOED, KEK, TSUKUBA, N. MOGGI, B. MOHR, C. S. MOON, R. MOORE, M. MORELLO, PEDRO A. MOVILLA FERNANDEZ, J. MULMENSTADT, A. MUKHERJEE, T.H. MULLER, R. MUMFORD, P. MURAT, M. MUSSINI, JANE MARIE NACHTMAN, A. NAGANO, JUNJI NAGANOMA, K. NAKAMURA, I. NAKANO, AUSTIN NAPIER, OKAYAMA U, V. NECULA, CHRISTOPHER C. NEU, MARK STEPHEN NEUBAUER, JASON A. NIELSEN, L. NODULMAN, OLGA NORNIELLA, E. NURSE, S. H. OH, Y. D. OH, I. OKSUZIAN, T. OKUSAWA, RUDOLF OLDEMAN, RISTO ORAVA, K. OSTERBERG, C. PAGLIARONE, E. PALENCIA, VAIA PAPADIMITRIOU, A. PAPAIKONOMOU, A. A. PARAMONOV, B. PARKS, SHABNAZ PASHAPOUR ALAMDARI, J. PATRICK, G. PAULETTA, M. PAULINI, CHRISTOPH M. E. PAUS, D. E. PELLETT, A. PENZO, THOMAS J. PHILLIPS, G. PIACENTINO, JONATAN PIEDRA, L. PINERA, K. PITTS, CHARLES PLAGER, LEE PONDROM, X. PORTELL, O. POUKHOV, N. POUNDER, F. PRAKOSHYN, A. PRONKO, JAMES PROUDFOOT, F. PTOHOS, G. PUNZI, JENNIFER M. PURSLEY, J. RADEMACKER, A. RAHAMAN, V. RAMAKRISHNAN, N. RANJAN, I. REDONDO, B. REISERT, V. REKOVIC, PETER RENTON, MARCO RESCIGNO, S. RICHTER, F. RIMONDI, L. RISTORI, A. ROBSON, T. RODRIGO, E. ROGERS, SIMONA ROLLI, ROBERT M. ROSER, M. ROSSI, R. ROSSIN, P. ROY, A. RUIZ, J. RUSS, V. RUSU, H. SAARIKKO, ALEXEI NIKOLAYEVICH SAFONOV, W. K. SAKUMOTO, G. SALAMANNA, O. SALTO, L. SANTI, S. SARKAR, L. SARTORI, K. SATO, P. SAVARD, A. SAVOY NAVARRO, T. SCHEIDLE, P. SCHLABACH, EUGENE E. SCHMIDT, M. P. SCHMIDT, M. SCHMITT, T. SCHWARZ, NORTHWESTERN U, L. SCODELLARO, ADAM LIDDLE SCOTT, A. SCRIBANO, F. SCURI, A. SEDOV, SALLY CAROL SEIDEL, YOSHIHIRO SEIYA, A. 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Gunay-Unalan, C. Haber, K. Hahn, S. R. Hahn, E. Halkiadaki, A. Hamilton, B.-Y. Han, J. Y. Han, R. Handler, F. Happacher, K. Hara, D. Hare, M. Hare, S. Harper, R. F. Harr, R. M. Harri, M. Hartz, K. Hatakeyama, J. Hauser, C. Hay, M. Heck, A. Heijboer, B. Heinemann, J. Heinrich, C. Henderson, M. Herndon, J. Heuser, D. Hida, C. S. Hill, D. Hirschbuehl, A. Hocker, A. Holloway, S. Hou, M. Houlden, S.-C. Hsu, B. T. Huffman, R. E. Hughe, U. Husemann, J. Huston, J. Incandela, G. Introzzi, M. Iori, A. Ivanov, B. Iyutin, E. Jame, D. Jang, B. Jayatilaka, D. Jean, E. J. Jeon, S. Jindariani, W. Johnson, M. Jone, K. K. Joo, S. Y. Jun, J. E. Jung, T. R. Junk, T. Kamon, P. E. Karchin, Y. Kato, Y. Kemp, R. Kephart, U. Kerzel, V. Khotilovich, B. Kilminster, D. H. Kim, H. S. Kim, J. E. Kim, M. J. Kim, S. B. Kim, S. H. Kim, Y. K. Kim, N. Kimura, L. Kirsch, S. Klimenko, M. Klute, B. Knuteson, B. R. Ko, K. Kondo, D. J. Kong, J. Konigsberg, A. Korytov, A. V. Kotwal, A. C. Kraan, J. Krau, M. Krep, J. Kroll, N. Krumnack, M. Kruse, V. Krutelyov, T. Kubo, S. E. Kuhlmann, T. Kuhr, N. P. Kulkarni, Y. Kusakabe, S. Kwang, A. T. Laasanen, S. Lai, S. Lami, S. Lammel, M. Lancaster, R. L. Lander, K. Lannon, A. Lath, G. Latino, I. Lazzizzera, T. LeCompte, J. Lee, Y. J. Lee, S. W. Lee, R. Lefèvre, N. Leonardo, S. Leone, S. Levy, J. D. Lewi, C. Lin, C. S. Lin, M. Lindgren, E. Lipele, T. M. Li, A. Lister, D. O. Litvintsev, T. Liu, N. S. Lockyer, A. Loginov, M. Loreti, R.-S. Lu, D. Lucchesi, P. Lujan, P. Luken, G. Lungu, L. Lyon, J. Ly, R. Lysak, E. Lytken, P. Mack, D. MacQueen, R. Madrak, K. Maeshima, K. Makhoul, T. Maki, P. Maksimovic, S. Malde, S. Malik, G. Manca, A. Manousaki, F. Margaroli, R. Marginean, C. Marino, C. P. Marino, A. Martin, M. Martin, V. Martin, M. Martínez, R. Martínez-Ballarín, T. Maruyama, P. Mastrandrea, T. Masubuchi, H. Matsunaga, M. E. Mattson, R. Mazini, P. Mazzanti, K. S. McFarland, P. McIntyre, R. McNulty, A. Mehta, P. Mehtala, S. Menzemer, A. Menzione, P. Merkel, C. Mesropian, A. Messina, T. Miao, N. Miladinovic, J. Mile, R. Miller, C. Mill, M. Milnik, A. Mitra, G. Mitselmakher, A. Miyamoto, S. Moed, N. Moggi, B. Mohr, C. S. Moon, R. Moore, M. Morello, P. Movilla Fernandez, J. Mülmenstädt, A. Mukherjee, Th. Muller, R. Mumford, P. Murat, M. Mussini, J. Nachtman, A. Nagano, J. Naganoma, K. Nakamura, I. Nakano, A. Napier, V. Necula, C. Neu, M. S. Neubauer, J. Nielsen, L. Nodulman, O. Norniella, E. Nurse, S. H. Oh, Y. D. Oh, I. Oksuzian, T. Okusawa, R. Oldeman, R. Orava, K. Osterberg, C. Pagliarone, E. Palencia, V. Papadimitriou, A. Papaikonomou, A. A. Paramonov, B. Park, S. Pashapour, J. Patrick, G. Pauletta, M. Paulini, C. Pau, D. E. Pellett, A. Penzo, T. J. Phillip, G. Piacentino, J. Piedra, L. Pinera, K. Pitt, C. Plager, L. Pondrom, X. Portell, O. Poukhov, N. Pounder, F. Prakoshyn, A. Pronko, J. Proudfoot, F. Ptoho, G. Punzi, J. Pursley, J. Rademacker, A. Rahaman, V. Ramakrishnan, N. Ranjan, I. Redondo, B. Reisert, V. Rekovic, P. Renton, M. 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Suzuki, A. Taffard, R. Takashima, Y. Takeuchi, R. Tanaka, M. Tecchio, P. K. Teng, K. Terashi, J. Thom, A. S. Thompson, E. Thomson, P. Tipton, V. Tiwari, S. Tkaczyk, D. Toback, S. Tokar, K. Tollefson, T. Tomura, D. Tonelli, S. Torre, D. Torretta, S. Tourneur, W. Trischuk, S. Tsuno, Y. Tu, N. Turini, F. Ukegawa, S. Uozumi, S. Vallecorsa, N. van Remortel, A. Varganov, E. Vataga, F. Vazquez, G. Velev, C. Vellidi, G. Veramendi, V. Veszpremi, M. Vidal, R. Vidal, I. Vila, R. Vilar, T. Vine, M. Vogel, I. Vollrath, I. Volobouev, G. Volpi, F. Würthwein, P. Wagner, R. G. Wagner, R. L. Wagner, J. Wagner, W. Wagner, R. Wallny, S. M. Wang, A. Warburton, D. Water, M. Weinberger, W. C. Wester, III, B. Whitehouse, D. Whiteson, A. B. Wicklund, E. Wicklund, G. William, H. H. William, P. Wilson, B. L. Winer, P. Wittich, S. Wolber, C. Wolfe, T. Wright, X. Wu, S. M. Wynne, A. Yagil, K. Yamamoto, J. Yamaoka, T. Yamashita, C. Yang, U. K. Yang, Y. C. Yang, W. M. Yao, G. P. Yeh, J. Yoh, K. Yorita, T. Yoshida, G. B. Yu, I. Yu, S. S. Yu, J. C. Yun, L. Zanello, A. Zanetti, I. Zaw, X. Zhang, J. Zhou, S. Zucchelli, and Ptohos, Fotios [0000-0002-3432-3452]
Subjects: 13.38.Be, 14.70.Fm, 12.15.Ji, 13.85.Qk, Particle physics, Single measurement, Physics, Multidisciplinary, Tevatron, FOS: Physical sciences, General Physics and Astronomy, Elementary particle, Data recording, ddc:500.2, 01 natural sciences, Particle detector, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), [PACS] Decays of W bosons, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], W-boson mass, Fermilab, Measurement theory, 010306 general physics, Nuclear Experiment, +10+GeV%29%22">[PACS] Hadron-induced inclusive production with identified leptons, photons, or other nonhadronic particles (energy > 10 GeV), Bosons, Boson, Physics, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Detectors, [PACS] W bosons, High Energy Physics::Experiment, Bar (unit)
Abstract: 7 pages, 4 figures.-- PACS nrs.: 14.70.Fm; 13.38.Be; 13.85.Qk.-- ISI Article Identifier: 000250140600014.-- ArXiv pre-print available at: http://arxiv.org/abs/0707.0085.-- et al., We present a measurement of the W-boson mass using 200 pb(-1) of data collected in p(p)over-bar collisions at sqrt{s}=1.96 TeV by the CDF II detector at run II of the Fermilab Tevatron. With a sample of 63 964 W --> e(nu) candidates and 51 128 W --> μ(nu) candidates, we measure M(W) = 80413 ± 34(stat) ± 34(syst) = 80 413 ± 48 MeV/c^2. This is the most precise single measurement of the W-boson mass to date., This work was supported by the U.S. Department of Energy and National Science Foundation; the Italian Istituto Nazionale di Fisica Nucleare; the Ministry of Education, Culture, Sports, Science and Technology of Japan; the Natural Sciences and Engineering Research Council of Canada; the National Science Council of the Republic of China; the Swiss National Science Foundation; the A.P. Sloan Foundation; the Bundesministerium für Bildung und Forschung, Germany; the Korean Science and Engineering Foundation and the Korean Research Foundation; the Science and Technology Facilities Council and the Royal Society, U.K.; the Institut National de Physique Nucleaire et Physique des Particules/CNRS; the Russian Foundation for Basic Research; the Comisión Interministerial de Ciencia y Tecnología, Spain; the European Community’s Human Potential Programme; the European Commission under the Marie Curie Programme; the Slovak R&D Agency; and the Academy of Finland.
Published: 2016

41. Search for Higgs bosons produced in association with b quarks

Author: Jongmin Lee, C. Calancha, R. Culbertson, O. Norniella, G. Giurgiu, C. A. Cox, Mario Campanelli, S. De Cecco, S. Amerio, A. Barbaro-Galtieri, D. Horn, D. Krop, Christoph Paus, M. N. Mondragon, J. Lueck, M. Gold, Fumihiko Ukegawa, L. Sartori, J. D. Lewis, G. Manca, M. D'Errico, S. Budd, G. Latino, Paul Lujan, M. P. Schmidt, V. Rusu, M. Dorigo, F. Wick, P. Catastini, C. Bromberg, D. J. Cox, A. Di Canto, V. Saveliev, A. Anastassov, A. T. Goshaw, Jian Tang, S. H. Kim, C. Pagliarone, Javier Cuevas, D. E. Pellett, Stanislav Tokár, B. Jayatilaka, Kai Yi, A. Loginov, A. B. Wicklund, Adrian Buzatu, Ivan-Kresimir Furic, M. Lancaster, Z. Gunay-Unalan, G. Chlachidze, Erik Brücken, G. L. Strycker, E. E. Schmidt, D. Stentz, D. Dagenhart, Katsufumi Sato, W. Johnson, A. Simonenko, J. Keung, T. Miao, Markus Frank, Roman Lysak, D. Amidei, S. Wilbur, M. Heck, D. Beecher, Peter Wagner, S. R. Hou, S. Errede, Yasuyoshi Nagai, Francesco Crescioli, A. Mukherjee, T. Riddick, H. Gerberich, Vyacheslav Krutelyov, J. Vizán, M. J. Shochet, D. Chokheli, K. Gibson, V. Papadimitriou, R. Madrak, Andrew Beretvas, B. Whitehouse, S. Y. Jun, A. Scribano, S. Torre, H. Wolfe, J. Pursley, Jochen Jens Heinrich, G. A. Thompson, D. Torretta, C. Mesropian, Jason Nielsen, B. Casal, S. W. Lee, P. Ttito-Guzmán, Xin Wu, F. Canelli, J. Naganoma, M. Binkley, S. B. Kim, E. Rogers, Alberto Annovi, V. Khotilovich, Y. Seiya, K. Ebina, M. M. Deninno, D. Lucchesi, Bernd Stelzer, Mark Neubauer, Emily Nurse, J. E. Kim, R. E. Hughes, A. Brisuda, T. Rodriguez, Y. Takeuchi, M. Rossi, T. Wakisaka, A. Mitra, Maxwell Chertok, Matteo Bauce, Eva Halkiadakis, A. Semenov, K. Takemasa, R. Orava, Koji Yamamoto, A. Manousakis-Katsikakis, Thomas LeCompte, P. K. Teng, C. Cuenca Almenar, Andrea Bocci, I. Oksuzian, M. Giunta, Tara Shears, D. Goldin, Th. Müller, K. Sliwa, S. Klimenko, Chris Hays, Michael Schmitt, Y. D. Oh, I. Bizjak, Tommaso Dorigo, W. Ketchum, Yang Yang, A. Hamaguchi, Shalhout Shalhout, I. Shreyber, W. Ashmanskas, S. Lockwitz, Sudhir Malik, G. Flanagan, M. Vidal, G. Lungu, F. Vázquez, H. W. Kim, P. Squillacioti, Kazuhiko Hara, J. Conway, E. Lee, M. Stanitzki, G. Piacentino, Viviana Cavaliere, Andrea Castro, Michal Kreps, A. Kasmi, Andrew Mehta, Jacobo Konigsberg, S. Behari, J. Boudreau, R. McNulty, M. Hare, J. Asaadi, P. Barria, E. James, P. Movilla Fernandez, R. D. Field, Evelyn Thomson, A. Pronko, Arie Bodek, R. Vilar, M. Tecchio, C. P. Marino, Sunil Somalwar, Naoki Kimura, S. Moed, Maxim Goncharov, U. Husemann, C. Deluca, Fabrizio Scuri, L. Brigliadori, B. Álvarez González, N. Hussain, A. Varganov, A. Sedov, M. Kurata, M. Corbo, Fedor Prokoshin, O. Poukhov, V. A. Giakoumopoulou, W. C. Wester, B. Di Ruzza, Andrew Ivanov, F. Devoto, S. Carron, C. M. Ginsburg, T. Okusawa, S. Tkaczyk, J. Strologas, P. Sinervo, Pavol Bartos, Keunchang Cho, M. Feindt, Allan G Clark, Roger Moore, Duncan Carlsmith, M. Kirby, P. F. Shepard, S. H. Oh, J. Patrick, P. Schlabach, D. O. Litvintsev, Daniela Bortoletto, R. Forrest, D. Hare, Dean Hidas, Kevin Lannon, Marcelo Vogel, P. E. Karchin, G. De Lorenzo, J. Huston, F. Ptohos, A. Elagin, Rainer Wallny, V. V. Glagolev, Chi Lin, Virgil E Barnes, G. P. Yeh, Jay Dittmann, M. Campbell, N. Ranjan, Guido Volpi, C. Plager, Stefano Camarda, A. Napier, C. Ferrazza, J. R. Smith, G. B. Yu, P. Murat, O. González, Itsuo Nakano, J. Nett, Stefano Giagu, Teresa Rodrigo, Joe Kroll, Mauro Dell'Orso, Y. S. Chung, L. Nodulman, A. Penzo, Alan Garfinkel, R. F. Harr, E. Pueschel, C. Haber, Y. Funakoshi, T. J. Phillips, T. A. Schwarz, Monica D'Onofrio, Michele Gallinaro, W. Badgett, Alexei Safonov, A. T. Laasanen, M. Trovato, N. Krumnack, Stephan Lammel, Lucio Cerrito, G. Bauer, K. Kondo, T. Wright, T. Aaltonen, K. S. McFarland, M. Shimojima, Peter Wittich, K. R. Bland, I. Suslov, F. D. Snider, J. Y. Han, A. Apresyan, S. Hewamanage, Sinead Farrington, Daniel Whiteson, Sandra Leone, P. Garosi, F. Ruffini, T. Yang, Andreas Warburton, E. J. Jeon, S. Wolbers, J. A. Appel, N. Moggi, Peter McIntyre, A. Sukhanov, J. Linacre, M. J. Kim, Justin Pilot, A. Menzione, G. Pauletta, M. Stancari, M. E. Mattson, T. Tomura, Chuan-Ming Liu, V. Ramakrishnan, K. K. Joo, D. W. Jang, A. Golossanov, Alessandro Cerri, S. Pagan Griso, W. K. Sakumoto, G. Punzi, P. B. Renton, S. S. Yu, M. Iori, M. E. Convery, E. Palencia, James Russ, N. Ershaidat, Y. Zeng, Aidan Robson, D. P. Benjamin, A. Hocker, Kohei Yorita, D. Glenzinski, C. Grosso-Pilcher, J. N. Bellinger, D. Errede, J. Thome, S. Leo, H. S. Budd, Hyun Lee, S. Lami, I. Yu, W. H. Chung, N. Goldschmidt, Peter Bussey, Aron Soha, Mark Kruse, Alison Lister, Y. Kato, W. Hopkins, Kevin Burkett, J. Guimaraes Da Costa, Y. Sakurai, A. Rahaman, D. Tonelli, Guillelmo Gomez-Ceballos, H. C. Fang, R. Martínez-Ballarín, Sebastian Grinstein, J. Galyardt, I. V. Gorelov, Zhenbin Wu, K. Tollefson, M. Lindgren, Elisabetta Pianori, M. J. Morello, A. V. Kotwal, Federico Sforza, Luciano Ristori, L. Ortolan, Tiehui Liu, Rodolfo Carosi, U. K. Yang, S. Shiraishi, H. Miyake, S. Kwang, D. H. Kim, M. Hurwitz, F. Happacher, Dario Bisello, A. Bhatti, S. R. Hahn, M. Mussini, J. Antos, Frank Chlebana, P. Mehtala, E. Gerchtein, T. Yoshida, C. I. Ciobanu, T. R. Junk, A. Artikov, J. Yoh, Matthew Herndon, M. K. Jha, M. Hussein, S. Rolli, Benjamin Kilminster, Barry Blumenfeld, Ricardo Eusebi, Gervasio Gomez, Elliot Lipeles, K. Makhoul, Manfred Paulini, M. Weinberger, S. Uozumi, J. C. Yun, Oliver Stelzer-Chilton, Yongsun Kim, Y. C. Chen, J. Deng, Giorgio Chiarelli, D. Waters, Amitabh Lath, Anna Sfyrla, Paola Giannetti, B. A. Barnett, Giorgio Apollinari, Luca Scodellaro, J. P. Fernandez, Teruki Kamon, P. Mazzanti, Francesco Rubbo, P. Giromini, D. Cauz, Anna Zanetti, Kaori Maeshima, L. Oakes, Jane Nachtman, Paolo Mastrandrea, J. Lys, R. Roser, Ivan Vila, P. Wilson, J. E. Garcia, Matteo Cavalli-Sforza, Ignacio Redondo, Hyun-Chul Kim, R. St. Denis, B. Auerbach, S. Carrillo, K. T. Pitts, C. Vellidis, L. Pondrom, E. Wicklund, Q. Liu, G. Velev, S. Donati, Kenichi Hatakeyama, Alexander Paramonov, M. Franklin, P. Totaro, A. Eppig, Song-Ming Wang, J. C. Freeman, N. D'ascenzo, T. Kuhr, A. Ruiz, Giovanni Bellettini, F. Azfar, A. N. Sissakian, John Paul Chou, Fabrizio Margaroli, J. Morlock, A. Aurisano, Sally Seidel, J. S. Wilson, M. Bucciantonio, A. Boveia, Christopher Clarke, R. L. Wagner, K. Goulianos, P. de Barbaro, Franco Bedeschi, D. Toback, N. Giokaris, A. Schmidt, G. Compostella, Antonio Limosani, Robin Erbacher, M. Datta, W-M. Yao, J. Yamaoka, C. S. Moon, M. Cordelli, G. Busetto, Brian L Winer, S. Zucchelli, F. Rimondi, Maria Agnese Ciocci, Tetsuo Arisawa, C. Neu, M. Jones, D. Mietlicki, L. Demortier, P. N. Dong, Julia Thom, D. J. Kong, B. Carls, V. Sorin, P. Lukens, A. Savoy-Navarro, M. Martinez, Y. Sudo, H. H. Williams, G. Introzzi, Y. Tu, K. Potamianos, Sergo Jindariani, L. Santi, J. Budagov, R. L. Lander, Massimo Casarsa, Universidad de Cantabria, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), CDF, T. AALTONEN, B. ÁLVAREZ GONZÁLEZ, S. AMERIO, D. AMIDEI, A. ANASTASSOV, A. ANNOVI, J. ANTOS, G. APOLLINARI, J. APPEL, T. ARISAWA, A. ARTIKOV, J. ASAADI, W. ASHMANSKAS, B.AUERBACH, A. AURISANO, F. AZFAR, W. BADGETT, T. BAE, A. BARBARO-GALTIERI, V. E. BARNES, B. A. BARNETT, P. BARRIA, P. BARTOS, M. BAUCE, F. BEDESCHI, S. BEHARI, G. BELLETTINI, J. BELLINGER, D. BENJAMIN, A. BERETVAS, A. BHATTI, M. BINKLEY, D. BISELLO, I. BIZJAK, K.R. BLAND, B. BLUMENFELD, A. BOCCI, A. BODEK, D. BORTOLETTO, J. BOUDREAU, A. BOVEIA, L. BRIGLIADORI, C. BROMBERG, E. BRUCKEN, J. BUDAGOV, H. S. BUDD, K. BURKETT, G. BUSETTO, P. BUSSEY, A. BUZATU, A. CALAMBA, C. CALANCHA, S. CAMARDA, M. CAMPANELLI, M. CAMPBELL, F. CANELLI, B. CARLS, D. CARLSMITH, R. CAROSI, S. CARRILLO, S. CARRON, B. CASAL, M. CASARSA, A. CASTRO, P. CATASTINI, D. CAUZ, V. CAVALIERE, M. CAVALLI-SFORZA, A. CERRI, L. CERRITO, Y. C. CHEN, M. CHERTOK, G. CHIARELLI, G. CHLACHIDZE, F. CHLEBANA, K. CHO, D. CHOKHELI, W. H. CHUNG, Y. S. CHUNG, M. A. CIOCCI, A. CLARK, C. CLARKE, G. COMPOSTELLA, M. E. CONVERY, J. CONWAY, M. CORBO, M. CORDELLI, C. A. COX, D. J. COX, F. CRESCIOLI, J. CUEVAS, R. CULBERTSON, D. DAGENHART, N. D’ASCENZO, M. DATTA, P. DE BARBARO, M. DELL’ORSO, L. DEMORTIER, M. DENINNO, F. DEVOTO, M. D’ERRICO, A. DI CANTO, B. DI RUZZA, J. R. DITTMANN, S. DONATI, P. DONG, M. D’ONOFRIO, M. DORIGO, T. DORIGO, K. EBINA, A. ELAGIN, A. EPPIG, R. ERBACHER, S. ERREDE, N. ERSHAIDAT, R. EUSEBI, S. FARRINGTON, M. FEINDT, J. P. FERNANDEZ, R. FIELD, G. FLANAGAN, R. FORREST, M. J. FRANK, M. FRANKLIN, J. C. FREEMAN, Y. FUNAKOSHI, I. FURIC, M. GALLINARO, J. E. GARCIA, A. F. GARFINKEL, P. GAROSI, H. GERBERICH, E. GERCHTEIN, S. GIAGU, V. GIAKOUMOPOULOU, P. GIANNETTI, K. GIBSON, C. M. GINSBURG, N. GIOKARIS, P. GIROMINI, G. GIURGIU, V. GLAGOLEV, D. GLENZINSKI, M. GOLD, D. GOLDIN, N. GOLDSCHMIDT, A. GOLOSSANOV, G. GOMEZ, G. GOMEZ-CEBALLOS, M. GONCHAROV, O. GONZÁLEZ, I. GORELOV, A. T. GOSHAW, K. GOULIANOS, S. GRINSTEIN, C. GROSSO-PILCHER, R. C. GROUP, J. 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C., Yun, A., Zanetti, Y., Zeng, S., Zucchelli, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Clark, Allan Geoffrey, Garcia Navarro, Jose Enrique, Lister, Alison, and Wu, Xin
Subjects: Quark, Nuclear and High Energy Physics, Particle physics, Higgs Physics, Tevatron, FOS: Physical sciences, ddc:500.2, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Fermilab, High Energy Physics, 010306 general physics, TEVATRON, Boson, Physics, HIGGS BOSON, Collider Physics, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Observable, Scalar boson, 14.80.Da, 12.60.Fr, 13.85.Rm, Higgs boson, CDF, High Energy Physics::Experiment, Minimal Supersymmetric Standard Model
Abstract: We present a search for neutral Higgs bosons decaying into bb̄, produced in association with b quarks in pp̄ collisions. This process could be observable in supersymmetric models with high values of tanβ. The event sample corresponds to 2.6fb -1 of integrated luminosity collected with the CDF II detector at the Fermilab Tevatron collider. We search for an enhancement in the mass of the two leading jets in events with three jets identified as coming from b quarks using a displaced vertex algorithm. A data-driven procedure is used to estimate the dijet mass spectrum of the nonresonant multijet background. The contributions of backgrounds and a possible Higgs boson signal are determined by a two-dimensional fit of the data, using the dijet mass together with an additional variable which is sensitive to the flavor composition of the three tagged jets. We set mass-dependent limits on σ(pp̄→)×B(→bb̄) which are applicable for a narrow scalar particle produced in association with b quarks. We also set limits on tanβ in supersymmetric Higgs models including the effects of the Higgs boson width. © 2012 American Physical Society., Department of Energy (US); National Science Foundation (US); Istituto Nazionale di Fisica Nucleare (Italia); Ministry of Education, Culture, Sports, Science and Technology (Japan); National Research Council of Canada; Swiss National Science Foundation; Alfred P. Sloan Foundation; Bundesministerium für Bildung und Forschung (Deutschland); National Research Foundation of Korea; Science and Technology Facilities Council (UK); The Royal Society (UK); Russian Foundation for Basic Research; Ministerio de Ciencia e Innovación (España); Slovak Research and Development Agency; Academy of Finland; Australian Research Council.
Published: 2016

42. Dry photolithography through ultraviolet radiation-induced photo-etching of polymethyl methacrylate

Author: Daniel J. Carbaugh, Jason T. Wright, Faiz Rahman, Savas Kaya, and Parthiban Rajan
Subjects: Materials science, 02 engineering and technology, 01 natural sciences, law.invention, law, 0103 physical sciences, Polymer chemistry, Materials Chemistry, Irradiation, Lithography, 010302 applied physics, Gas-discharge lamp, business.industry, Metals and Alloys, Surfaces and Interfaces, Photoelectric effect, 021001 nanoscience & nanotechnology, Surfaces, Coatings and Films, Electronic, Optical and Magnetic Materials, Resist, Optoelectronics, Dry etching, Photolithography, 0210 nano-technology, business, Electron-beam lithography
Abstract: We describe a technique for photo-patterning polymethyl methacrylate (PMMA) resist films that does not use a wet development step. 254 nm deep ultraviolet radiation from an ordinary mercury discharge lamp was used to both chain scission and remove PMMA in a single step lithographic process. PMMA films several microns thick can be patterned through this technique. The patterned film can also be directly used as a structure, by itself, for applications in microfluidics etc. Our process relies on a synergistic effect that greatly accelerates the loss of PMMA when it is simultaneously heated close to its glass transition temperature and irradiated with 254 nm radiation. Furthermore, we also describe a secondary exposure effect in this process that originates from electrons that are generated through a photoelectric effect at the PMMA-substrate interface. This gives rise to a proximity effect analogous to that encountered in conventional electron beam lithography.
Published: 2016

43. MBE Grown In x Ga1−x N Thin Films with Bright Visible Emission Centered at 550 nm

Author: Jason T. Wright, Savas Kaya, Bibek Thapa, Ratnakar Palai, K. Dasari, Wojciech M. Jadwisienczak, and J. Wang
Subjects: 010302 applied physics, Photoluminescence, Reflection high-energy electron diffraction, Materials science, Scanning electron microscope, Analytical chemistry, chemistry.chemical_element, 02 engineering and technology, 021001 nanoscience & nanotechnology, Condensed Matter Physics, 01 natural sciences, Electronic, Optical and Magnetic Materials, Crystallography, chemistry, Electron diffraction, X-ray photoelectron spectroscopy, 0103 physical sciences, Materials Chemistry, Electrical and Electronic Engineering, Thin film, 0210 nano-technology, Indium, Molecular beam epitaxy
Abstract: The In x Ga1−x N thin films with indium content of x = 14–18 at.% were successfully grown by using molecular beam epitaxy (MBE) at high growth temperatures from 650°C to 800°C. In situ reflection high-energy electron diffraction (RHEED) of the In x Ga1−x N films confirmed the Stranski–Krastanov growth mode. X-ray diffraction (XRD) of the films confirmed their highly crystalline nature having c-axis orientation with a small fraction of secondary InN phase admixture. High-resolution cross-sectional scanning electron microscopy images showed two-dimensional epilayers growth with thickness of about ∼260 nm. The high growth temperature of In x Ga1−x N epilayers is found to be favorable to facilitate more GaN phase than InN phase. All the fundamental electronic states of In, Ga, and N were identified by x-ray photoelectron spectroscopy (XPS) and the indium composition has been calculated from the obtained XPS spectra with CASAXPS software. The composition calculations from XRD, XPS and photoluminescence closely match each other. The biaxial strain has been calculated and found to be increasing with the In content. Growing In x Ga1−x N at high temperatures resulted in the reduction in stress/strain which affects the radiative electron–hole pair recombination. The In x Ga1−x N film with lesser strain showed a brighter and stronger green emission than films with the larger built-in strain. A weak S-shaped near band edge emission profile confirms the relatively homogeneous distribution of indium.
Published: 2016

44. Laser excitation of red, green, blue and trichromatic white rare-earth phosphors for solid-state lighting applications

Author: Sara Al-waisawy, David Pendrill, Faiz Rahman, Wojciech M. Jadwisienczak, and Jason T. Wright
Subjects: Materials science, Biophysics, Phosphor, 02 engineering and technology, Color temperature, 01 natural sciences, Biochemistry, law.invention, 010309 optics, Optics, law, 0103 physical sciences, Activator (phosphor), Chromaticity, business.industry, General Chemistry, 021001 nanoscience & nanotechnology, Condensed Matter Physics, Laser, Ray, Atomic and Molecular Physics, and Optics, Solid-state lighting, Optoelectronics, 0210 nano-technology, business, Light-emitting diode
Abstract: Phosphors for solid-state lighting, based on a number of different compositional schemes and driven by light from blue light-emitting diodes (LEDs) are widely used for lighting applications. The low efficiency of pump LEDs at high drive currents (droop effect) limits the amount of light produced by conventional LED and phosphor combination. Pumping with laser diodes (LDs) can circumvent this limitation. In this paper we report on the characterisation of individual and a mixture of KEu(WO 4 ) 2 (red), BaMg 2 Al 16 O 27 :Eu, Mn (green) and (Sr,Mg) 2 SiO 4 :Eu (blue) phosphors, excited by a CW-driven LD operating at 404 nm. The activator ion in each of these phosphors is, respectively, Eu 3+ , Mn 2+ and Eu 2+ . Characteristics of light produced with each phosphor, variations with incident light power and phosphor temperature as well as effects from phosphor ageing are described. Results of comparison between pumping with coherent and incoherent light at the same wavelength are also described.
Published: 2016

45. An empirically derived three-dimensional Laplace resonance in the Gliese 876 planetary system

Author: Howard Isaacson, Matthew J. Payne, Eric B. Ford, Seth Pritchard, Paul Robertson, Katherine M. Deck, Jason T. Wright, and Benjamin E. Nelson
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Laplace transform, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, Planetary system, Space (mathematics), 01 natural sciences, Radial velocity, Orbit, Amplitude, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Libration, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report constraints on the three-dimensional orbital architecture for all four planets known to orbit the nearby M dwarf Gliese 876 based solely on Doppler measurements and demanding long-term orbital stability. Our dataset incorporates publicly available radial velocities taken with the ELODIE and CORALIE spectrographs, HARPS, and Keck HIRES as well as previously unpublished HIRES velocities. We first quantitatively assess the validity of the planets thought to orbit GJ 876 by computing the Bayes factors for a variety of different coplanar models using an importance sampling algorithm. We find that a four-planet model is preferred over a three-planet model. Next, we apply a Newtonian MCMC algorithm to perform a Bayesian analysis of the planet masses and orbits using an n-body model in three-dimensional space. Based on the radial velocities alone, we find that a 99% credible interval provides upper limits on the mutual inclinations for the three resonant planets ($��_{cb}, 19 pages, 11 figures, 8 tables. Accepted to MNRAS. Posterior samples available at https://github.com/benelson/GJ876
Published: 2015

46. Toward a Direct Measure of the Galactic Acceleration

Author: Eric L. Nielsen, Daniel Huber, Philip Chang, Elena D'Onghia, Robert J. De Rosa, Sukanya Chakrabarti, Jason T. Wright, Peter Craig, Kathryn V. Johnston, Alice C. Quillen, Katherine L. Rhode, and Joey Territo
Subjects: Physics, Dark matter, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Acceleration (differential geometry), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Exoplanet, Direct measure, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: High precision spectrographs can enable not only the discovery of exoplanets, but can also provide a fundamental measurement in Galactic dynamics. Over about ten year baselines, the expected change in the line-of-sight velocity due to the Galaxy's gravitational field for stars at $\sim$ kpc scale distances above the Galactic mid-plane is $\sim$ few - 10 cm/s, and may be detectable by the current generation of high precision spectrographs. Here, we provide theoretical expectations for this measurement based on both static models of the Milky Way and isolated Milky Way simulations, as well from controlled dynamical simulations of the Milky Way interacting with dwarf galaxies. We simulate a population synthesis model to analyze the contribution of planets and binaries to the Galactic acceleration signal. We find that while low-mass, long-period planetary companions are a contaminant to the Galactic acceleration signal, their contribution is very small. Our analysis of $\sim$ ten years of data from the LCES HIRES/Keck precision radial velocity (RV) survey shows that slopes of the RV curves of standard RV stars agree with expectations of the local Galactic acceleration near the Sun within the errors, and that the error in the slope scales inversely as the square root of the number of observations. Thus, we demonstrate that a survey of stars with low intrinsic stellar jitter at kpc distances above the Galactic mid-plane for realistic sample sizes can enable a direct determination of the dark matter density., accepted to ApJ Letters
Published: 2020

47. TOI-1728b: The Habitable-zone Planet Finder Confirms a Warm Super-Neptune Orbiting an M-dwarf Host

Author: Caleb I. Cañas, Helen Baran, Andrea S. J. Lin, Arpita Roy, Chad F. Bender, Marissa Maney, Jiayin Dong, Gudmundur Stefansson, Lawrence W. Ramsey, Samuel Halverson, Joe P. Ninan, William D. Cochran, Andrew J. Monson, Jason T. Wright, Ryan Terrien, Fred Hearty, Connor Fredrick, Eric B. Ford, Paul Robertson, Leslie Hebb, Michael Endl, Shubham Kanodia, Christian Schwab, Scott A. Diddams, Andrew J. Metcalf, and Suvrath Mahadevan
Subjects: 010504 meteorology & atmospheric sciences, Gas giant, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Planet, Neptune, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, Orbital period, Exoplanet, Radial velocity, Orbit, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: We confirm the planetary nature of TOI-1728b using a combination of ground-based photometry, near-infrared Doppler velocimetry and spectroscopy with the Habitable-zone Planet Finder.TOI-1728 is an old, inactive M0 star with \teff{} $= 3980^{+31}_{-32}$ K, which hosts a transiting super Neptune at an orbital period of $\sim$ 3.49 days. Joint fitting of the radial velocities and TESS and ground-based transits yields a planetary radius of $5.05_{-0.17}^{+0.16}$ R$_{\oplus}$, mass $26.78_{-5.13}^{+5.43}$ M$_{\oplus}$ and eccentricity $0.057_{-0.039}^{+0.054}$. We estimate the stellar properties, and perform a search for He 10830 \AA absorption during the transit of this planet and claim a null detection with an upper limit of 1.1$\%$ with 90\% confidence. A deeper level of He 10830 \AA ~ absorption has been detected in the planet atmosphere of GJ 3470b, a comparable gaseous planet. TOI-1728b is the largest super Neptune -- the intermediate subclass of planets between Neptune and the more massive gas-giant planets -- discovered around an M dwarf. With its relatively large mass and radius, TOI-1728 represents a valuable datapoint in the M-dwarf exoplanet mass-radius diagram, bridging the gap between the lighter Neptune-sized planets and the heavier Jovian planets known to orbit M-dwarfs. With a low bulk density of $1.14_{-0.24}^{+0.26}$ g/cm$^3$, and orbiting a bright host star (J $\sim 9.6$, V $\sim 12.4$), TOI-1728b is also a promising candidate for transmission spectroscopy both from the ground and from space, which can be used to constrain planet formation and evolutionary models., Comment: 21 pages, 12 figures, 4 tables: Accepted for publication
Published: 2020

48. Dynamic hydroelastic response of a surface-piercing strut in waves and ventilated flows

Author: Hyunse Yoon, Yin Lu Young, T. Wright, and Casey M. Harwood
Subjects: Coalescence (physics), Physics, Mechanical Engineering, Modal analysis, 02 engineering and technology, Mechanics, Simple harmonic motion, Vortex shedding, 01 natural sciences, Dynamic load testing, 010305 fluids & plasmas, Physics::Fluid Dynamics, Vibration, 020303 mechanical engineering & transports, Modal, 0203 mechanical engineering, 0103 physical sciences, Trailing edge
Abstract: The objective of this work is to study the effects of waves and ventilation on the dynamic hydroelastic response of a surface-piercing strut via towing tank studies. The experimental studies are especially designed to test the hypothesis that flow conditions affect the modal response and hence structural dynamics, which in turn affect the hydrodynamic response through fluid–structure interaction, particularly near regions of mode localization such as frequency coalescence. The results showed that the modal frequencies decrease with increasing submergence, and are higher in fully ventilated flow compared to fully wetted flow. Regular, non-breaking waves lead to simple harmonic oscillations about the mean values at the encountered wave frequency for the slowly varying component of the hydrodynamic loads and tip deformations. The spectral response of the fast fluctuating component of the hydrodynamic loads and tip deformations showed peaks at the modal frequencies and vortex shedding frequencies (off the blunt trailing edge of the strut). Significant dynamic load amplifications and flow-induced vibrations were observed when the second and third modal frequencies coalesced at a submerged aspect ratio of two in fully wetted flow. In fully ventilated flow, the second and third modes separated enough to result in drastically reduced dynamic load fluctuations and flow-induced vibrations. When the submergence decreased, the separation between the modal frequencies increased, which avoided frequency coalescence in both fully wetted and fully ventilated flows. The results suggest that for cases where the wave encountered frequency is well separated from the modal frequencies, the spectral response of the fast fluctuating component of the hydrodynamic loads and tip deformations are governed by the structural response, and not by wave conditions.
Published: 2020

49. A review of polymethyl methacrylate (PMMA) as a versatile lithographic resist – With emphasis on UV exposure

Author: Daniel J. Carbaugh, Parthiban Rajan, Faiz Rahman, Sneha G. Pandya, Jason T. Wright, and Savas Kaya
Subjects: 010302 applied physics, Fabrication, Materials science, Polymethyl methacrylate, business.industry, 02 engineering and technology, 021001 nanoscience & nanotechnology, Condensed Matter Physics, 01 natural sciences, Atomic and Molecular Physics, and Optics, Surfaces, Coatings and Films, Electronic, Optical and Magnetic Materials, Resist, 0103 physical sciences, Optoelectronics, Electrical and Electronic Engineering, 0210 nano-technology, business, Electron beam resist, Lithography, Acrylic polymer
Abstract: This review describes the utility of polymethyl methacrylate (PMMA) as a resist for several types of lithographic processes. Ordinarily, PMMA is only considered an electron beam resist but in fact it can be used as a resist material with exposure systems based on both particle beams and electromagnetic radiations. In each case, both positive tone and negative tone resist action can be realized with appropriate process design. We first describe and review the mechanisms that bring about lithographic pattern formation in this acrylic polymer. This is followed by descriptions of processes for using PMMA in different ways as a lithographic resist. Use of PMMA at both long and short UV wavelengths is treated in more detail as this aspect is less well-known for lithography with PMMA. We also describe several new findings from own work here, such as cross-linking PMMA with Michler's ketone (MK), use of resist reflow for three-dimensional structure fabrication and lithographic tone switching with change in UV exposure dose. The aim of this exposition is to emphasize the great versatility of PMMA as a resist for micro- and nano-electronic device fabrication.
Published: 2020

50. Diffuser-assisted Infrared Transit Photometry for Four Dynamically Interacting Kepler Systems

Author: Daniel Thorngren, Jason T. Wright, Leo Y. Liu, Gautam Vasisht, Heather Knutson, Shreyas Vissapragada, Maxwell A. Millar-Blanchaer, Dimitri Mawet, Daniel Jontof-Hutter, Avi Shporer, Eve J. Lee, Yayaati Chachan, Samaporn Tinyanont, and Ricky Nilsson
Subjects: 010504 meteorology & atmospheric sciences, Infrared, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Kepler, law.invention, Telescope, Photometry (optics), Spitzer Space Telescope, law, Observatory, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Exoplanet, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present ground-based infrared transit observations for four dynamically interacting \textit{Kepler} planets, including Kepler-29b, Kepler-36c, KOI-1783.01, and Kepler-177c, obtained using the Wide-field Infrared Camera on the Hale 200" telescope at Palomar Observatory. By utilizing an engineered diffuser and custom guiding software, we mitigate time-correlated telluric and instrumental noise sources in these observations. We achieve an infrared photometric precision comparable to or better than that of space-based observatories such as the \textit{Spitzer Space Telescope}, and detect transits with greater than 3$\sigma$ significance for all planets. For Kepler-177c ($J=13.9$) our measurement uncertainties are only $1.2\times$ the photon noise limit and 1.9 times better than the predicted photometric precision for \textit{Spitzer} IRAC photometry of this same target. We find that a single transit observation obtained $4-5$ years after the end of the original \textit{Kepler} mission can reduce dynamical mass uncertainties by as much as a factor of three for these systems. Additionally, we combine our new observations of KOI-1783.01 with information from the literature to confirm the planetary nature of this system. We discuss the implications of our new mass and radius constraints in the context of known exoplanets with low incident fluxes, and we note that Kepler-177c may be a more massive analog to the currently known super-puffs given its core mass (3.8$\pm0.9M_\Earth$) and large gas-to-core ratio (2.8$\pm0.7$). Our demonstrated infrared photometric performance opens up new avenues for ground-based observations of transiting exoplanets previously thought to be restricted to space-based investigation., Comment: 33 pages, 18 figures, accepted by AJ
Published: 2020

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