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1. Search for new physics in high pT like-sign dilepton events at CDF II.

Author: Aaltonen T, Álvarez González B, Amerio S, Amidei D, Anastassov A, Annovi A, Antos J, Apollinari G, Appel JA, Apresyan A, Arisawa T, Artikov A, Asaadi J, Ashmanskas W, Auerbach B, Aurisano A, Azfar F, Badgett W, Barbaro-Galtieri A, Barnes VE, Barnett BA, Barria P, Bartos P, Bauce M, Bauer G, Bedeschi F, Beecher D, Behari S, Bellettini G, Bellinger J, Benjamin D, Beretvas A, Bhatti A, Binkley M, Bisello D, Bizjak I, Bland KR, Blumenfeld B, Bocci A, Bodek A, Bortoletto D, Boudreau J, Boveia A, Brigliadori L, Brisuda A, Bromberg C, Brucken E, Bucciantonio M, Budagov J, Budd HS, Budd S, Burkett K, Busetto G, Bussey P, Buzatu A, Calancha C, Camarda S, Campanelli M, Campbell M, Canelli F, Carls B, Carlsmith D, Carosi R, Carrillo S, Carron S, Casal B, Casarsa M, Castro A, Catastini P, Cauz D, Cavaliere V, Cavalli-Sforza M, Cerri A, Cerrito L, Chen YC, Chertok M, Chiarelli G, Chlachidze G, Chlebana F, Cho K, Chokheli D, Chou JP, Chung WH, Chung YS, Ciobanu CI, Ciocci MA, Clark A, Clarke C, Compostella G, Convery ME, Conway J, Corbo M, Cordelli M, Cox CA, Cox DJ, Crescioli F, Cuenca Almenar C, Cuevas J, Culbertson R, Dagenhart D, d'Ascenzo N, Datta M, de Barbaro P, De Cecco S, De Lorenzo G, Dell'Orso M, Deluca C, Demortier L, Deng J, Deninno M, Devoto F, d'Errico M, Di Canto A, Di Ruzza B, Dittmann JR, D'Onofrio M, Donati S, Dong P, Dorigo M, Dorigo T, Ebina K, Elagin A, Eppig A, Erbacher R, Errede D, Errede S, Ershaidat N, Eusebi R, Fang HC, Farrington S, Feindt M, Fernandez JP, Ferrazza C, Field R, Flanagan G, Forrest R, Frank MJ, Franklin M, Freeman JC, Funakoshi Y, Furic I, Gallinaro M, Galyardt J, Garcia JE, Garfinkel AF, Garosi P, Gerberich H, Gerchtein E, Giagu S, Giakoumopoulou V, Giannetti P, Gibson K, Ginsburg CM, Giokaris N, Giromini P, Giunta M, Giurgiu G, Glagolev V, Glenzinski D, Gold M, Goldin D, Goldschmidt N, Golossanov A, Gomez G, Gomez-Ceballos G, Goncharov M, González O, Gorelov I, Goshaw AT, Goulianos K, Grinstein S, Grosso-Pilcher C, Group RC, Guimaraes da Costa J, Gunay-Unalan Z, Haber C, Hahn SR, Halkiadakis E, Hamaguchi A, Han JY, Happacher F, Hara K, Hare D, Hare M, Harr RF, Hatakeyama K, Hays C, Heck M, Heinrich J, Herndon M, Hewamanage S, Hidas D, Hocker A, Hopkins W, Horn D, Hou S, Hughes RE, Hurwitz M, Husemann U, Hussain N, Hussein M, Huston J, Introzzi G, Iori M, Ivanov A, James E, Jang D, Jayatilaka B, Jeon EJ, Jha MK, Jindariani S, Johnson W, Jones M, Joo KK, Jun SY, Junk TR, Kamon T, Karchin PE, Kasmi A, Kato Y, Ketchum W, Keung J, Khotilovich V, Kilminster B, Kim DH, Kim HS, Kim HW, Kim JE, Kim MJ, Kim SB, Kim SH, Kim YK, Kimura N, Kirby M, Kittiwisit P, Klimenko S, Kondo K, Kong DJ, Konigsberg J, Kotwal AV, Kreps M, Kroll J, Krop D, Krumnack N, Kruse M, Krutelyov V, Kuhr T, Kurata M, Kwang S, Laasanen AT, Lami S, Lammel S, Lancaster M, Lander RL, Lannon K, Lath A, Latino G, Lecompte T, Lee E, Lee HS, Lee JS, Lee SW, Leo S, Leone S, Lewis JD, Limosani A, Lin CJ, Linacre J, Lindgren M, Lipeles E, Lister A, Litvintsev DO, Liu C, Liu Q, Liu T, Lockwitz S, Loginov A, Lucchesi D, Lueck J, Lujan P, Lukens P, Lungu G, Lys J, Lysak R, Madrak R, Maeshima K, Makhoul K, Malik S, Manca G, Manousakis-Katsikakis A, Margaroli F, Marino C, Martínez M, Martínez-Ballarín R, Mastrandrea P, Mattson ME, Mazzanti P, McFarland KS, McIntyre P, McNulty R, Mehta A, Mehtala P, Menzione A, Mesropian C, Miao T, Mietlicki D, Mitra A, Miyake H, Moed S, Moggi N, Mondragon MN, Moon CS, Moore R, Morello MJ, Morlock J, Movilla Fernandez P, Mukherjee A, Muller T, Murat P, Mussini M, Nachtman J, Nagai Y, Naganoma J, Nakano I, Napier A, Nett J, Neu C, Neubauer MS, Nielsen J, Nodulman L, Norniella O, Nurse E, Oakes L, Oh SH, Oh YD, Oksuzian I, Okusawa T, Orava R, Ortolan L, Pagan Griso S, Pagliarone C, Palencia E, Papadimitriou V, Paramonov AA, Patrick J, Pauletta G, Paulini M, Paus C, Pellett DE, Penzo A, Phillips TJ, Piacentino G, Pianori E, Pilot J, Pitts K, Plager C, Pondrom L, Porter R, Potamianos K, Poukhov O, Prokoshin F, Pronko A, Ptohos F, Pueschel E, Punzi G, Pursley J, Rahaman A, Ramakrishnan V, Ranjan N, Redondo I, Renton P, Rescigno M, Riddick T, Rimondi F, Ristori L, Robson A, Rodrigo T, Rodriguez T, Rogers E, Rolli S, Roser R, Rossi M, Rubbo F, Ruffini F, Ruiz A, Russ J, Rusu V, Safonov A, Sakumoto WK, Sakurai Y, Santi L, Sartori L, Sato K, Saveliev V, Savoy-Navarro A, Schlabach P, Schmidt A, Schmidt EE, Schmidt MP, Schmitt M, Schwarz T, Scodellaro L, Scribano A, Scuri F, Sedov A, Seidel S, Seiya Y, Semenov A, Sforza F, Sfyrla A, Shalhout SZ, Shears T, Shepard PF, Shimojima M, Shiraishi S, Shochet M, Shreyber I, Simonenko A, Sinervo P, Sissakian A, Sliwa K, Smith JR, Snider FD, Soha A, Somalwar S, Sorin V, Squillacioti P, Stancari M, Stanitzki M, St Denis R, Stelzer B, Stelzer-Chilton O, Stentz D, Strologas J, Strycker GL, Sudo Y, Sukhanov A, Suslov I, Takemasa K, Takeuchi Y, Tang J, Tecchio M, Teng PK, Thom J, Thome J, Thompson GA, Thomson E, Ttito-Guzmán P, Tkaczyk S, Toback D, Tokar S, Tollefson K, Tomura T, Tonelli D, Torre S, Torretta D, Totaro P, Trovato M, Tu Y, Ukegawa F, Uozumi S, Varganov A, Vázquez F, Velev G, Vellidis C, Vidal M, Vila I, Vilar R, Vizán J, Vogel M, Volpi G, Wagner P, Wagner RL, Wakisaka T, Wallny R, Wang SM, Warburton A, Waters D, Weinberger M, Wester WC 3rd, Whitehouse B, Whiteson D, Wicklund AB, Wicklund E, Wilbur S, Wick F, Williams HH, Wilson JS, Wilson P, Winer BL, Wittich P, Wolbers S, Wolfe H, Wright T, Wu X, Wu Z, Yamamoto K, Yamaoka J, Yang T, Yang UK, Yang YC, Yao WM, Yeh GP, Yi K, Yoh J, Yorita K, Yoshida T, Yu GB, Yu I, Yu SS, Yun JC, Zanetti A, Zeng Y, and Zucchelli S
Subjects: Models, Theoretical, Uncertainty, Elementary Particles, Physics instrumentation
Abstract: We present a search for new physics in events with two high pT leptons of the same electric charge, using data with an integrated luminosity of 6.1 fb(-1). The observed data are consistent with standard model predictions. We set 95% C.L. lower limits on the mass of doubly charged scalars decaying to like-sign dileptons, m(H±±) > 190-245 GeV/c(2), assuming 100% BR to ee, μμ or eμ.
Published: 2011
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2. Corrigendum: 'Measurement of 73Ge(n,γ) cross sections and implications for stellar nucleosynthesis' [Phys. Lett. B 790 (2019) 458–465]

Author: C. Lederer-Woods, U. Battino, P. Ferreira, A. Gawlik, C. Guerrero, F. Gunsing, S. Heinitz, J. Lerendegui-Marco, A. Mengoni, R. Reifarth, A. Tattersall, S. Valenta, C. Weiss, O. Aberle, J. Andrzejewski, L. Audouin, V. Bécares, M. Bacak, J. Balibrea, M. Barbagallo, S. Barros, F. Bečvář, C. Beinrucker, F. Belloni, E. Berthoumieux, J. Billowes, D. Bosnar, M. Brugger, M. Caamaño, F. Calviño, M. Calviani, D. Cano-Ott, F. Cerutti, E. Chiaveri, N. Colonna, G. Cortés, M.A. Cortés-Giraldo, L. Cosentino, L.A. Damone, K. Deo, M. Diakaki, M. Dietz, C. Domingo-Pardo, R. Dressler, E. Dupont, I. Durán, B. Fernández-Domínguez, A. Ferrari, P. Finocchiaro, R.J.W. Frost, V. Furman, K. Göbel, A.R. García, I. Gheorghe, T. Glodariu, I.F. Gonçalves, E. González-Romero, A. Goverdovski, E. Griesmayer, H. Harada, T. Heftrich, A. Hernández-Prieto, J. Heyse, D.G. Jenkins, E. Jericha, F. Käppeler, Y. Kadi, T. Katabuchi, P. Kavrigin, V. Ketlerov, V. Khryachkov, A. Kimura, N. Kivel, I. Knapova, M. Kokkoris, M. Krtička, E. Leal-Cidoncha, H. Leeb, M. Licata, S. Lo Meo, R. Losito, D. Macina, J. Marganiec, T. Martínez, C. Massimi, P. Mastinu, M. Mastromarco, F. Matteucci, E. Mendoza, P.M. Milazzo, F. Mingrone, M. Mirea, S. Montesano, A. Musumarra, R. Nolte, F.R. Palomo-Pinto, C. Paradela, N. Patronis, A. Pavlik, J. Perkowski, J.I. Porras, J. Praena, J.M. Quesada, T. Rauscher, A. Riego-Perez, M. Robles, C. Rubbia, J.A. Ryan, M. Sabaté-Gilarte, A. Saxena, P. Schillebeeckx, S. Schmidt, D. Schumann, P. Sedyshev, A.G. Smith, A. Stamatopoulos, S.V. Suryanarayana, G. Tagliente, J.L. Tain, A. Tarifeño-Saldivia, L. Tassan-Got, A. Tsinganis, G. Vannini, V. Variale, P. Vaz, A. Ventura, V. Vlachoudis, R. Vlastou, A. Wallner, S. Warren, M. Weigand, T. Wright, and P. Žugec
Subjects: Physics, QC1-999
Published: 2023
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3. Measurement of 73Ge(n,γ) cross sections and implications for stellar nucleosynthesis

Author: C. Lederer-Woods, U. Battino, P. Ferreira, A. Gawlik, C. Guerrero, F. Gunsing, S. Heinitz, J. Lerendegui-Marco, A. Mengoni, R. Reifarth, A. Tattersall, S. Valenta, C. Weiss, O. Aberle, J. Andrzejewski, L. Audouin, V. Bécares, M. Bacak, J. Balibrea, M. Barbagallo, S. Barros, F. Bečvář, C. Beinrucker, F. Belloni, E. Berthoumieux, J. Billowes, D. Bosnar, M. Brugger, M. Caamaño, F. Calviño, M. Calviani, D. Cano-Ott, F. Cerutti, E. Chiaveri, N. Colonna, G. Cortés, M.A. Cortés-Giraldo, L. Cosentino, L.A. Damone, K. Deo, M. Diakaki, M. Dietz, C. Domingo-Pardo, R. Dressler, E. Dupont, I. Durán, B. Fernández-Domínguez, A. Ferrari, P. Finocchiaro, R.J.W. Frost, V. Furman, K. Göbel, A.R. García, I. Gheorghe, T. Glodariu, I.F. Gonçalves, E. González-Romero, A. Goverdovski, E. Griesmayer, H. Harada, T. Heftrich, A. Hernández-Prieto, J. Heyse, D.G. Jenkins, E. Jericha, F. Käppeler, Y. Kadi, T. Katabuchi, P. Kavrigin, V. Ketlerov, V. Khryachkov, A. Kimura, N. Kivel, I. Knapova, M. Kokkoris, M. Krtička, E. Leal-Cidoncha, H. Leeb, M. Licata, S. Lo Meo, R. Losito, D. Macina, J. Marganiec, T. Martínez, C. Massimi, P. Mastinu, M. Mastromarco, F. Matteucci, E. Mendoza, P.M. Milazzo, F. Mingrone, M. Mirea, S. Montesano, A. Musumarra, R. Nolte, F.R. Palomo-Pinto, C. Paradela, N. Patronis, A. Pavlik, J. Perkowski, J.I. Porras, J. Praena, J.M. Quesada, T. Rauscher, A. Riego-Perez, M. Robles, C. Rubbia, J.A. Ryan, M. Sabaté-Gilarte, A. Saxena, P. Schillebeeckx, S. Schmidt, D. Schumann, P. Sedyshev, A.G. Smith, A. Stamatopoulos, S.V. Suryanarayana, G. Tagliente, J.L. Tain, A. Tarifeño-Saldivia, L. Tassan-Got, A. Tsinganis, G. Vannini, V. Variale, P. Vaz, A. Ventura, V. Vlachoudis, R. Vlastou, A. Wallner, S. Warren, M. Weigand, T. Wright, and P. Žugec
Subjects: Physics, QC1-999
Abstract: 73Ge(n,γ) cross sections were measured at the neutron time-of-flight facility n_TOF at CERN up to neutron energies of 300 keV, providing for the first time experimental data above 8 keV. Results indicate that the stellar cross section at kT=30 keV 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. Keywords: Nucleosynthesis, Neutron capture, s process, Germanium, n_TOF
Published: 2019
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4. Neutron spectroscopy of 26Mg states: Constraining the stellar neutron source 22Ne(α,n)25Mg

Author: C. Massimi, S. Altstadt, J. Andrzejewski, L. Audouin, M. Barbagallo, V. Bécares, F. Bečvář, F. Belloni, E. Berthoumieux, J. Billowes, S. Bisterzo, D. Bosnar, M. Brugger, M. Calviani, F. Calviño, D. Cano-Ott, C. Carrapiço, D.M. Castelluccio, F. Cerutti, E. Chiaveri, L. Cosentino, M. Chin, G. Clai, N. Colonna, G. Cortés, M.A. Cortés-Giraldo, S. Cristallo, M. Diakaki, C. Domingo-Pardo, I. Duran, R. Dressler, C. Eleftheriadis, A. Ferrari, P. Finocchiaro, K. Fraval, S. Ganesan, A.R. García, G. Giubrone, I.F. Gonçalves, E. González-Romero, E. Griesmayer, C. Guerrero, F. Gunsing, A. Hernández-Prieto, D.G. Jenkins, E. Jericha, Y. Kadi, F. Käppeler, D. Karadimos, N. Kivel, P. Koehler, M. Kokkoris, S. Kopecky, M. Krtička, J. Kroll, C. Lampoudis, C. Langer, E. Leal-Cidoncha, C. Lederer, H. Leeb, L.S. Leong, S. Lo Meo, R. Losito, A. Mallick, A. Manousos, J. Marganiec, T. Martínez, P.F. Mastinu, M. Mastromarco, E. Mendoza, A. Mengoni, P.M. Milazzo, F. Mingrone, M. Mirea, W. Mondelaers, A. Musumarra, C. Paradela, A. Pavlik, J. Perkowski, M. Pignatari, L. Piersanti, A. Plompen, J. Praena, J.M. Quesada, T. Rauscher, R. Reifarth, A. Riego, M.S. Robles, C. Rubbia, M. Sabaté-Gilarte, R. Sarmento, A. Saxena, P. Schillebeeckx, S. Schmidt, D. Schumann, G. Tagliente, J.L. Tain, D. Tarrío, L. Tassan-Got, A. Tsinganis, S. Valenta, G. Vannini, I. Van Rijs, V. Variale, P. Vaz, A. Ventura, M.J. Vermeulen, V. Vlachoudis, R. Vlastou, A. Wallner, T. Ware, M. Weigand, C. Weiß, R. Wynants, T. Wright, and P. Žugec
Subjects: s Process, α+22Ne, Neutron spectroscopy, Physics, QC1-999
Abstract: This work reports on accurate, high-resolution measurements of the 25Mg(n,γ)26Mg and 25Mg(n,tot) cross sections in the neutron energy range from thermal to about 300 keV, leading to a significantly improved 25Mg(n,γ)26Mg parametrization. The relevant resonances for n+25Mg were characterized from a combined R-matrix analysis of the experimental data. This resulted in an unambiguous spin/parity assignment of the corresponding excited states in 26Mg. With this information experimental upper limits of the reaction rates for 22Ne(α,n)25Mg and 22Ne(α,γ)26Mg were established, potentially leading to a significantly higher (α,n)/(α,γ) ratio than previously evaluated. The impact of these results has been studied for stellar models in the mass range 2 to 25 M⊙.
Published: 2017
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5. Planck frequencies as Schelling points in SETI – Erratum

Author: Jason T. Wright
Subjects: Physics, symbols.namesake, Physics and Astronomy (miscellaneous), Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), symbols, Planck, Ecology, Evolution, Behavior and Systematics, Search for extraterrestrial intelligence, Astrobiology
Published: 2020

6. 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

7. Dyson spheres

Author: Jason T. Wright
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Coupling, Physics, lcsh:Astronomy, Computation, astrobiology, FOS: Physical sciences, Astronomy and Astrophysics, Star (graph theory), Luminosity, lcsh:QB1-991, Theoretical physics, Astrophysics - Solar and Stellar Astrophysics, Radiation pressure, Dissipative system, Radiative transfer, Dyson sphere, stars: general, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: I review the origins and development of the idea of Dyson spheres, their purpose, their engineering, and their detectability. I explicate the ways in which the popular imagining of them as monolithic objects would make them dynamically unstable under gravity and radiation pressure, and mechanically unstable to buckling. I develop a model for the radiative coupling between a star and large amounts of material orbiting it, and connect the observational features of a star plus Dyson sphere system to the gross radiative properties of the sphere itself. I discuss the still-unexplored problem of the effects of radiative feedback on the central star's structure and luminosity. Finally, I discuss the optimal sizes of Dyson spheres under various assumptions about their purpose as sources of low-entropy emission, dissipative work, or computation., Invited review. 21pp, 1 figure. v.3 contains a correction to the definition of s and to the units of Eq. 23
Published: 2020

8. 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

9. Stellar Gravitational Lens Engineering for Interstellar Communication and Artifact SETI

Author: Stephen Kerby and Jason T. Wright
Subjects: Physics, Extraterrestrial intelligence, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Popular Physics (physics.pop-ph), Astrophysics::Cosmology and Extragalactic Astrophysics, Planetary system, Physics - Popular Physics, law.invention, Telescope, Gravitation, Gravitational lens, Space and Planetary Science, law, Planet, Interstellar communication, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Search for extraterrestrial intelligence, Astrophysics::Galaxy Astrophysics, Computer Science::Information Theory
Abstract: Several recent works have proposed "stellar relay" transmission systems in which a spacecraft at the focus of a star's gravitational lens achieves dramatic boosts in the gain of an outgoing or incoming interstellar transmission. We examine some of the engineering requirements of a stellar relay system, evaluate the long-term sustainability of a gravitational relay, and describe the perturbations and drifts that must be actively countered to maintain a relay-star-target alignment. The major perturbations on a relay-Sun-target alignment are the inwards gravity of the Sun and the reflex motion of the Sun imparted by the planets. These approx. m/s/yr accelerations can be countered with modern propulsion systems over century-long timescales. This examination is also relevant for telescope designs aiming to use the Sun as a focusing element. We additionally examine prospects for an artifact SETI search to observe stellar relays placed around the Sun by an extraterrestrial intelligence and suggest certain nearby stars that are relatively unperturbed by planetary systems as favorable nodes for a stellar relay communications system., 13 pages, 1 figure, 2 tables; updated with proofing edits
Published: 2021

10. 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

11. 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

12. 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

13. 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

14. 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

15. Nutritional markers and proteome in patients undergoing treatment for pulmonary tuberculosis differ by geographic region

Author: Komal Kedia, Marc H Weiner, Joseph Keane, Jason P. Wendler, Payam Nahid, Aaron T. Wright, David M. Lewinsohn, Leah G. Jarsberg, Jon M. Jacobs, George Sigal, Marina A. Gritsenko, Richard D. Smith, Tujin Shi, Paul D. Piehowski, and Subbian, Selvakumar
Subjects: Bacterial Diseases, 0301 basic medicine, Proteomics, Male, Proteome, Proteomes, Organic chemistry, Biochemistry, South Africa, Medical Conditions, 0302 clinical medicine, Medicine and Health Sciences, Ethnicities, 2.1 Biological and endogenous factors, Uganda, Nutritional Physiological Phenomena, 030212 general & internal medicine, Aetiology, Vitamin A, Immune Response, Lung, Fluids, screening and diagnosis, Multidisciplinary, Physics, Acute-phase protein, Vitamins, Pulmonary, Middle Aged, Physical sciences, Chemistry, Detection, Treatment Outcome, Infectious Diseases, 6.1 Pharmaceuticals, Geographic regions, Medicine, Female, Infection, Research Article, 4.2 Evaluation of markers and technologies, Adult, States of Matter, medicine.medical_specialty, Treatment response, Tuberculosis, General Science & Technology, Science, Immunology, Clinical Trials and Supportive Activities, Chemical compounds, 03 medical and health sciences, Young Adult, Signs and Symptoms, Rare Diseases, Pulmonary tuberculosis, Clinical Research, Internal medicine, Organic compounds, medicine, Humans, In patient, Tuberculosis, Pulmonary, Nutrition, African People, Inflammation, business.industry, Prevention, Biology and Life Sciences, Proteins, Evaluation of treatments and therapeutic interventions, Acute Phase Proteins, Liquids, Mycobacterium tuberculosis, Tropical Diseases, medicine.disease, Lipid Metabolism, Clinical trial, 030104 developmental biology, Good Health and Well Being, Spain, People and Places, North America, Population Groupings, Clinical Medicine, business, Biomarkers
Abstract: Introduction Contemporary phase 2 TB disease treatment clinical trials have found that microbiologic treatment responses differ between African versus non-African regions, the reasons for which remain unclear. Understanding host and disease phenotypes that may vary by region is important for optimizing curative treatments. Methods We characterized clinical features and the serum proteome of phase 2 TB clinical trial participants undergoing treatment for smear positive, culture-confirmed TB, comparing host serum protein expression in clinical trial participants enrolled in African and Non-African regions. Serum samples were collected from 289 participants enrolled in the Centers for Disease Control and Prevention TBTC Study 29 (NCT00694629) at time of enrollment and at the end of the intensive phase (after 40 doses of TB treatment). Results After a peptide level proteome analysis utilizing a unique liquid chromatography IM-MS platform (LC-IM-MS) and subsequent statistical analysis, a total of 183 core proteins demonstrated significant differences at both baseline and at week 8 timepoints between participants enrolled from African and non-African regions. The majority of the differentially expressed proteins were upregulated in participants from the African region, and included acute phase proteins, mediators of inflammation, as well as coagulation and complement pathways. Downregulated proteins in the African population were primarily linked to nutritional status and lipid metabolism pathways. Conclusions We have identified differentially expressed nutrition and lipid pathway proteins by geographic region in TB patients undergoing treatment for pulmonary tuberculosis, which appear to be associated with differential treatment responses. Future TB clinical trials should collect expanded measures of nutritional status and further evaluate the relationship between nutrition and microbiologic treatment response.
Published: 2021

16. A solar feed for NEID

Author: Joe P. Ninan, Michael W. McElwain, Arpita Roy, Shubham Kanodia, Andrea S. J. Lin, Zhao Guo, Andrew J. Monson, Emily Hunting, Jayadev Rajagopal, Kyle Kaplan, Eric B. Ford, Paul Robertson, Fred Hearty, G. Stefansson, Samuel Halverson, Suvrath Mahadevan, Christian Schwab, Jason T. Wright, Chad F. Bender, Daniel J. Stevens, Colin Nitroy, Ryan Terrien, Lawrence W. Ramsey, Evans, Christopher J., Bryant, Julia J., and Motohara, Kentaro
Subjects: Sunlight, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Exoplanet, law.invention, Telescope, Radial velocity, Early results, law, Observatory, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract: NEID is a radial velocity (RV) instrument including an ultra-stabilized fiber-fed spectrograph, installed in 2019 at the 3.5m WIYN telescope at Kitt Peak National Observatory. Accompanying it is a solar feed system built to supply the spectrograph with disk-integrated sunlight. Observing the Sun “as a star” is essential for developing and validating mitigation strategies for RV variations due to stellar activity and instrument systematics, thus enabling more-effective detections of lower-mass exoplanets. In this paper, we will detail the design of the NEID solar feed system and showcase early results addressing NEID systematics and solar RV variability.
Published: 2020

17. A Mini-Neptune and a Radius Valley Planet Orbiting the Nearby M2 Dwarf TOI-1266 in Its Venus Zone: Validation with the Habitable-zone Planet Finder

Author: Arpita Roy, Chad F. Bender, Joe P. Ninan, Marissa Maney, Jason T. Wright, Caleb I. Cañas, Arvind F. Gupta, Andrew J. Metcalf, Connor Fredrick, William D. Cochran, Eric B. Ford, Andrew J. Monson, Paul Robertson, Samuel Halverson, Lawrence W. Ramsey, Mark E. Everett, Christian Schwab, Scott A. Diddams, Eric Levi, John P. Wisniewski, Ryan Terrien, Fred Hearty, G. Stefansson, Suvrath Mahadevan, Ravi Kumar Kopparapu, Andrea S. J. Lin, Michael Endl, Shubham Kanodia, and Leslie Hebb
Subjects: Physics, biology, Astronomy and Astrophysics, Venus, Radius, Astrophysics::Cosmology and Extragalactic Astrophysics, biology.organism_classification, Exoplanet, Astrobiology, Space and Planetary Science, Planet, Mini-Neptune, Astrophysics::Earth and Planetary Astrophysics, Circumstellar habitable zone, Astrophysics::Galaxy Astrophysics
Abstract: We report on the validation of two planets orbiting the nearby (36 pc) M2 dwarf TOI-1266 observed by the TESS mission. This system is one of a few M dwarf multiplanet systems with close-in planets where the inner planet is substantially larger than the outer planet. The inner planet is sub-Neptune-sized (R = 2.46 ± 0.08 R_⊕) with an orbital period of 10.9 days, while the outer planet has a radius of 1.67_(-0.11)^(+0.09) R_⊕ and resides in the exoplanet radius valley—the transition region between rocky and gaseous planets. With an orbital period of 18.8 days, the outer planet receives an insolation flux of 2.4 times that of Earth, similar to the insolation of Venus. Using precision near-infrared radial velocities with the Habitable-zone Planet Finder Spectrograph, we place upper mass limits of 15.9 and 6.4 M_⊕ at 95% confidence for the inner and outer planet, respectively. A more precise mass constraint of both planets, achievable with current radial velocity instruments given the host star brightness (V = 12.9, J = 9.7), will yield further insights into the dominant processes sculpting the exoplanet radius valley.
Published: 2020

18. 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

19. Searching for Dyson spheres using Gaia and WISE

Author: Jason T. Wright, Erik Zackrisson, Matías Suazo, and Andreas Korn
Subjects: Physics, Theoretical physics, Dyson sphere, Starlight, Thermodynamic process
Abstract: Dyson spheres are hypothetical structures that high-level civilizations may build to harvest energy in the form of starlight. As in any thermodynamic process, the conversion of stellar energy would...
Published: 2020

20. Barycentric Corrections for Precise Radial Velocity Measurements of Sunlight

Author: Shubham Kanodia and Jason T. Wright
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Solar System, FOS: Physical sciences, Astronomy and Astrophysics, Ephemeris, Computational physics, Starlight, Radial velocity, Jupiter, symbols.namesake, Geophysics, Space and Planetary Science, Planet, Asteroid, Physics::Space Physics, Earth and Planetary Sciences (miscellaneous), symbols, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Doppler effect, Astrophysics - Earth and Planetary Astrophysics
Abstract: We provide formulae for the calculation of precise Doppler velocities of sunlight, in both the case of direct observations of the Sun and in reflection from the surfaces of solar system objects such as the Moon or asteroids. We discuss the meaning of a "barycentric correction" of measurements of these Doppler velocities, which is a different procedure from the analogous correction for starlight, and provide a formula for reducing such measurements to the component of the Sun's motion in the direction of the Earth or other Solar System object. We have implemented this procedure in the public barycorrpy Python package, and use it to explore the properties of the barycentric-corrected Doppler velocity of sunlight over 30 years. When measured directly, we show it is dominated by the non-periodic motion due to Jupiter, and that the signals of the other planets, including Venus, are not discernible in Fourier space. We show that "detecting" Venus in the Doppler velocities of sunlight will require either observing sunlight in reflection from an asteroid, or modeling the their individual contributions to the motion of the Sun in counterfactual kinematic or dynamical simulations of the Solar System with and without them., 12 pages, 4 figures, accepted to the Planetary Science Journal. v2 includes minor corrections to the text and references
Published: 2020

21. 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

22. Analysis of nonideality: insights from high concentration simulations of sedimentation velocity data

Author: Walter F. Stafford, R. T. Wright, Peter J. Sherwood, and John J. Correia
Subjects: 0301 basic medicine, 030103 biophysics, Concentration dependence, Diffusion, Biophysics, Thermodynamics, 03 medical and health sciences, Thermodynamic nonideality, Physics, High concentration, Sedimentation velocity, Global fitting, Antibodies, Monoclonal, General Medicine, Sedimentation, Models, Theoretical, Software package, 2nd Virial coefficient, Kinetics, 030104 developmental biology, Spectrometry, Fluorescence, Weak association, Hydrodynamic nonideality, Original Article, Ultracentrifugation
Abstract: The Aviv fluorescence detection system (Aviv-FDS) has allowed the performance of sedimentation velocity experiments on therapeutic antibodies in highly concentrated environments like formulation buffers and serum. Methods were implemented in the software package SEDANAL for the analysis of nonideal, weakly associating AUC data acquired on therapeutic antibodies and proteins (Wright et al. Eur Biophys J 47:709–722, 2018, Anal Biochem 550:72–83, 2018). This involved fitting both hydrodynamic, ks, and thermodynamic, BM1, nonideality where concentration dependence is expressed as s = so/(1 + ksc) and D = Do(1 + 2BM1c)/(1 + ksc) and so and Do are values extrapolated to c = 0 (mg/ml). To gain insight into the consequences of these phenomenological parameters, we performed simulations with SEDANAL of a monoclonal antibody as a function of ks (0–100 ml/g) and BM1 (0–100 ml/g). This provides a visual understanding of the separate and joint impact of ks and BM1 on the shape of high-concentration sedimentation velocity boundaries and the challenge of their unique determination by finite element methods. In addition, mAbs undergo weak self- and hetero-association (Yang et al. Prot Sci 27:1334–1348, 2018) and thus we have simulated examples of nonideal weak association over a wide range of concentrations (1–120 mg/ml). Here we demonstrate these data are best analyzed by direct boundary global fitting to models that account for ks, BM1 and weak association. Because a typical clinical dose of mAb is 50–200 mg/ml, these results have relevance for biophysical understanding of concentrated therapeutic proteins.
Published: 2020

23. 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

24. 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

25. 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

26. 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

27. 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

28. 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

29. 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

30. 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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31. 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

32. 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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33. 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

34. 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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A., Strauss, M., Strologas, J., Sudo, Y., Sukhanov, A., Suslov, I., Suter, L., Svoisky, P., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thomson, E., Thukral, V., Titov, M., Toback, D., Tokar, S., Tokmenin, V. V., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tsai, Y. -T., Tsybychev, D., Tuchming, B., Tully, C., Ukegawa, F., Uozumi, S., Uvarov, L., Uvarov, S., Uzunyan, S., Van Kooten, R., van Leeuwen, W. M., Varelas, N., Varnes, E. W., Vasilyev, I. A., Vazquez, F., Velev, G., Vellidis, C., Verkheev, A. Y., Vernieri, C., Vertogradov, L. S., Verzocchi, M., Vesterinen, M., Vidal, M., Vilanova, D., Vilar, R., Vizan, J., Vogel, M., Vokac, P., Volpi, G., Wagner, P., Wahl, H. D., Wallny, R., Wang, M. H. L. S., Wang, S. M., Warchol, J., Waters, D., Watts, G., Wayne, M., Weichert, J., Welty-Rieger, L., Wester, W. C., Iii, Whiteson, D., Wicklund, A. B., Wilbur, S., Williams, H. H., Williams, M. R. J., Wilson, G. 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
Full Text: View/download PDF

35. TOI-532b: The Habitable-zone Planet Finder confirms a Large Super Neptune in the Neptune Desert orbiting a metal-rich M-dwarf host

Author: Arvind F. Gupta, Maria Schutte, Fred Hearty, Christian Schwab, Joe P. Ninan, Sinclaire Jones, Andrew J. Metcalf, Paul Robertson, Jason Rothenberg, Samuel Halverson, Gudmundur Stefansson, Andrew J. Monson, Jason T. Wright, Arpita Roy, Scott A. Diddams, Suzanne L. Hawley, Lawrence W. Ramsey, Jack Lubin, Ravi Kumar Kopparapu, Shubham Kanodia, Brock A. Parker, John Wisniewski, Andrea S. J. Lin, Corey Beard, Marissa Maney, William D. Cochran, Leslie Hebb, Ryan Terrien, Henry A. Kobulnicky, Chad F. Bender, Caleb I. Cañas, Connor Fredrick, and Suvrath Mahadevan
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Gas giant, Metallicity, Dwarf planet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, Radial velocity, Space and Planetary Science, Neptune, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Circumstellar habitable zone, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We confirm the planetary nature of TOI-532b, using a combination of precise near-infrared radial velocities with the Habitable-zone Planet Finder, TESS light curves, ground based photometric follow-up, and high-contrast imaging. TOI-532 is a faint (J$\sim 11.5$) metal-rich M dwarf with Teff = $3957\pm69$ K and [Fe/H] = $0.38\pm0.04$; it hosts a transiting gaseous planet with a period of $\sim 2.3$ days. Joint fitting of the radial velocities with the TESS and ground-based transits reveal a planet with radius of $5.82\pm0.19$ R$_{\oplus}$, and a mass of $61.5_{-9.3}^{+9.7}$ M$_{\oplus}$. TOI-532b is the largest and most massive super Neptune detected around an M dwarf with both mass and radius measurements, and it bridges the gap between the Neptune-sized planets and the heavier Jovian planets known to orbit M dwarfs. It also follows the previously noted trend between gas giants and host star metallicity for M dwarf planets. In addition, it is situated at the edge of the Neptune desert in the Radius--Insolation plane, helping place constraints on the mechanisms responsible for sculpting this region of planetary parameter space., 19 pages, 9 figures, 4 tables. arXiv admin note: text overlap with arXiv:2006.14546
Published: 2021

36. Stellar Activity Manifesting at a One-year Alias Explains Barnard b as a False Positive

Author: Eric B. Ford, Scott A. Diddams, Paul Robertson, Chad F. Bender, Samuel Halverson, Jason T. Wright, Joe P. Ninan, Arpita Roy, Christian Schwab, William D. Cochran, Ryan Terrien, Andrew J. Metcalf, Suvrath Mahadevan, Lawrence W. Ramsey, Corey Beard, Jack Lubin, Michael Endl, Shubham Kanodia, Gudmundur Stefansson, and Connor Fredrick
Subjects: Physics, Rotation period, Alias, Astronomy and Astrophysics, Astrophysics, Orbital period, Declination, Radial velocity, Stars, symbols.namesake, Space and Planetary Science, Planet, symbols, Doppler effect
Abstract: Barnard’s star is among the most studied stars given its proximity to the Sun. It is often considered the radial velocity (RV) standard for fully convective stars due to its RV stability and equatorial decl. Recently, an M sin i = 3.3 M ⊕ super-Earth planet candidate with a 233 day orbital period was announced by Ribas et al. New observations from the near-infrared Habitable-zone Planet Finder (HPF) Doppler spectrometer do not show this planetary signal. We ran a suite of experiments on both the original data and a combined original + HPF data set. These experiments include model comparisons, periodogram analyses, and sampling sensitivity, all of which show the signal at the proposed period of 233 days is transitory in nature. The power in the signal is largely contained within 211 RVs that were taken within a 1000 day span of observing. Our preferred model of the system is one that features stellar activity without a planet. We propose that the candidate planetary signal is an alias of the 145 day rotation period. This result highlights the challenge of analyzing long-term, quasi-periodic activity signals over multiyear and multi-instrument observing campaigns.
Published: 2021

37. The Dynamics of the Transition from Kardashev Type II to Type III Galaxies Favor Technosignature Searches in the Central Regions of Galaxies

Author: Jonathan Carroll-Nellenback, Adam Frank, Caleb Scharf, and Jason T. Wright
Subjects: Physics, Dynamics (mechanics), Technosignature, General Medicine, Astrophysics, Type (model theory), Galaxy
Abstract: We present a video of a simulation showing the expansion front of a technological species settling a Milky Way-like galaxy, created using the model described in Carroll-Nellenback et al. It illustrates how even very conservative rates of settlement ship launches and ship ranges can quickly lead to a galaxy endemic with technology, and how the rotational and peculiar motions of stars contributes to the expansion. This video confirms and validates previous work showing that the centers of galaxies are promising search directions for SETI.
Published: 2021

38. 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

39. Commentary: High journal acceptance rates are good for science

Author: Jason T. Wright
Subjects: Physics, General Physics and Astronomy
Published: 2020

40. 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

41. 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

42. 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

43. $^{80}$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

44. Choosing a Maximum Drift Rate: Astrophysical Considerations

Author: Emilio Enriquez, Sofia Z. Sheikh, Jason T. Wright, and Andrew Siemion
Subjects: Physics, Acoustics, Component (UML), Transmitter, Stochastic drift, sense organs, skin and connective tissue diseases, Signal, Computer Science::Information Theory
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 in frequency over time. This effect, commonly prod...
Published: 2019

45. Stellar Spectroscopy in the Near-infrared with a Laser Frequency Comb

Author: Steinn Sigurdsson, Fred Hearty, Kartik Srinivasan, Kyle Kaplan, Steve Osterman, Gabriel Ycas, Emily Lubar, Joe P. Ninan, Jeff Jennings, Eric Levi, Larry Ramsey, Jason T. Wright, Gudmundur Stefansson, Samuel Halverson, Andrew J. Monson, Franklyn Quinlan, Wesley Brand, Christian Schwab, Colin Nitroy, Tyler Anderson, Andrew J. Metcalf, David A. Sterner, Arpita Roy, Scott A. Diddams, Scott B. Papp, David R. Carlson, William D. Cochran, Ryan Terrien, Connor Fredrick, Daniel D. Hickstein, Chad F. Bender, Michael Endl, Shubham Kanodia, Alex Wolszczan, Scott Blakeslee, Paul Robertson, and Suvrath Mahadevan
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Solar System, Doppler spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Atomic and Molecular Physics, and Optics, Exoplanet, Galaxy, Electronic, Optical and Magnetic Materials, Radial velocity, Stars, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Circumstellar habitable zone, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Physics - Optics, Optics (physics.optics)
Abstract: The discovery and characterization of exoplanets around nearby stars are driven by profound scientific questions about the uniqueness of Earth and our solar system, and the conditions under which life could exist elsewhere in our galaxy. Doppler spectroscopy, or the radial velocity (RV) technique, has been used extensively to identify hundreds of exoplanets, but with notable challenges in detecting terrestrial mass planets orbiting within habitable zones. We describe infrared RV spectroscopy at the 10 m Hobby–Eberly Telescope that leverages a 30 GHz electro-optic laser frequency comb with a nanophotonic supercontinuum to calibrate the Habitable Zone Planet Finder spectrograph. Demonstrated instrument precision
Published: 2019
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46. 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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47. 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

48. 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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49. 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

50. 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

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