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1,025 results on '"Fryer, C"'

152. Transient Puzzles

Author

Kouveliotou, Chryssa, Granot, J, Racusin, J. L, Bellm, E, Vianello, G, Oates, S, Fryer, C. L, Boggs, S. E, Christensen, F. E, Craig, W. W, Dermer, C. D, Gehrels, N, Hailey, C. J, Harrison, F. A, Melandri, A, McEnery, J. E, Mundell, C. G, Stern, D. K, Tagliaferri, G, and Zhang, W. W

Subjects
Astronomy, Astrophysics
Published
2014

153. Experimental observation of elevated heating in dynamically compressed CHfoam

Author

Falk, K., Fontes, C. J., Fryer, C. L., Greeff, C. W., Holec, M., Johns, H. M., Montgomery, D. S., Schmidt, D. W., and Smid, M.

Abstract

We present an experimental result of significantly increased heating in a laser-driven blastwaveexperiment carried out at the OMEGA laser facility. Abnormally high temperatures wereobserved in warm dense CH compared to older experiments and theoretical predictions. Thehigher temperatures in compressed CH were linked to an improved smoothness of the laserintensity profile, which resulted in better efficiency of the drive and coupling of more energyinto the system compared to previous similar experiments. Fifteen beams with combinedintensity of∼7×1014W cm−2and a square intensity profile with 2 ns duration were used todrive a strong shock, which subsequently developed to a blastwave travelling through lowdensity CH foam creating warm dense matter. Multiple diagnostics were used to examine thethermodynamic conditions in the warm dense CH foam. Velocity interferometry (VISAR) andstreaked pyrometry (SOP) observed increased blastwave velocities, while x-ray Thomsonscattering (XRTS) measured elevated temperatures of 17.5−35 eV in compressed CH foam.The experimental results were compared to hydrodynamic simulations and a potentialcontribution from x-rays to the elevated temperatures in the dense material was considered.

Published
2020

154. Experimental observation of elevated heating in dynamically compressed CHfoam

Author

(0000-0001-5975-776X) Falk, K., Fontes, C. J., Fryer, C. L., Greeff, C. W., Holec, M., Johns, H. M., Montgomery, D. S., Schmidt, D. W., (0000-0002-7162-7500) Smid, M., (0000-0001-5975-776X) Falk, K., Fontes, C. J., Fryer, C. L., Greeff, C. W., Holec, M., Johns, H. M., Montgomery, D. S., Schmidt, D. W., and (0000-0002-7162-7500) Smid, M.

Abstract

We present an experimental result of significantly increased heating in a laser-driven blastwaveexperiment carried out at the OMEGA laser facility. Abnormally high temperatures wereobserved in warm dense CH compared to older experiments and theoretical predictions. Thehigher temperatures in compressed CH were linked to an improved smoothness of the laserintensity profile, which resulted in better efficiency of the drive and coupling of more energyinto the system compared to previous similar experiments. Fifteen beams with combinedintensity of∼7×1014W cm−2and a square intensity profile with 2 ns duration were used todrive a strong shock, which subsequently developed to a blastwave travelling through lowdensity CH foam creating warm dense matter. Multiple diagnostics were used to examine thethermodynamic conditions in the warm dense CH foam. Velocity interferometry (VISAR) andstreaked pyrometry (SOP) observed increased blastwave velocities, while x-ray Thomsonscattering (XRTS) measured elevated temperatures of 17.5−35 eV in compressed CH foam.The experimental results were compared to hydrodynamic simulations and a potentialcontribution from x-rays to the elevated temperatures in the dense material was considered.

Published
2020

155. The Broadband Counterpart of the Short GRB 200522A atz= 0.5536: A Luminous Kilonova or a Collimated Outflow with a Reverse Shock?

Author

Fong, W., primary, Laskar, T., additional, Rastinejad, J., additional, Escorial, A. Rouco, additional, Schroeder, G., additional, Barnes, J., additional, Kilpatrick, C. D., additional, Paterson, K., additional, Berger, E., additional, Metzger, B. D., additional, Dong, Y., additional, Nugent, A. E., additional, Strausbaugh, R., additional, Blanchard, P. K., additional, Goyal, A., additional, Cucchiara, A., additional, Terreran, G., additional, Alexander, K. D., additional, Eftekhari, T., additional, Fryer, C., additional, Margalit, B., additional, Margutti, R., additional, and Nicholl, M., additional

Published
2021
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158. The unusual γ-ray burst GRB 101225A from a helium star/neutron star merger at redshift 0.33

Author

Thöne, C. C., de Ugarte Postigo, A., Fryer, C. L., Page, K. L., Gorosabel, J., Aloy, M. A., Perley, D. A., Kouveliotou, C., Janka, H. T., Mimica, P., Racusin, J. L., Krimm, H., Cummings, J., Oates, S. R., Holland, S. T., Siegel, M. H., De Pasquale, M., Sonbas, E., Im, M., Park, W.-K., Kann, D. A., Guziy, S., García, L. Hernández, Llorente, A., Bundy, K., Choi, C., Jeong, H., Korhonen, H., Kubànek, P., Lim, J., Moskvitin, A., Muñoz-Darias, T., Pak, S., and Parrish, I.

Published
2011
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163. Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes

Author

Belczynski, K., primary, Klencki, J., additional, Fields, C. E., additional, Olejak, A., additional, Berti, E., additional, Meynet, G., additional, Fryer, C. L., additional, Holz, D. E., additional, O’Shaughnessy, R., additional, Brown, D. A., additional, Bulik, T., additional, Leung, S. C., additional, Nomoto, K., additional, Madau, P., additional, Hirschi, R., additional, Kaiser, E., additional, Jones, S., additional, Mondal, S., additional, Chruslinska, M., additional, Drozda, P., additional, Gerosa, D., additional, Doctor, Z., additional, Giersz, M., additional, Ekstrom, S., additional, Georgy, C., additional, Askar, A., additional, Baibhav, V., additional, Wysocki, D., additional, Natan, T., additional, Farr, W. M., additional, Wiktorowicz, G., additional, Coleman Miller, M., additional, Farr, B., additional, and Lasota, J.-P., additional

Published
2020
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166. NuSTAR Observations of G11.2–0.3

Author

Madsen, K. K., primary, Fryer, C. L., additional, Grefenstette, B. W., additional, Lopez, L. A., additional, Reynolds, S., additional, and Zoglauer, A., additional

Published
2020
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168. An Unusual Stellar Death on Christmas Day

Author

Thone, C. C, de Ugarte Postigo, A, Fryer, C. L, Page, K. L, Gorosabel, J, Aloy, M. A, Perley, D. A, Kouveliotou, C, Janka, H. T, Mimica, P, Racusin, J. L, Krimm, H, Cummings, J, Oates, S. R, Holland, S. T, Siegel, M. H, De Pasquale, M, Sonbas, E, Im, M, Park, W. K, Kann, D. A, Guziy, S, Hernandez Garcia, L, Llorente, A, and Bundy, K

Subjects
Astronomy
Abstract

Long Gamma-Ray Bursts (GRBs) are the most dramatic examples of massive stellar deaths, usually associated with supernovae. They release ultra-relativistic jets producing non-thermal emission through synchrotron radiation as they interact with the surrounding medium. Here we report observations of the peculiar GRB 101225A (the "Christmas burst"). Its gamma-ray emission was exceptionally long and followed by a bright X-ray transient with a hot thermal component and an unusual optical couuterpart. During the first 10 days, the optical emission evolved as an expanding, cooling blackbody after which an additional component, consistent with a faint supernova, emerged. We determine its distance to 1.6 Gpc by fitting the spectral-energy distribution and light curve of the optical emission with a GRB-supernova template. Deep optical observations may have revealed a faint, unresolved host galaxy. Our proposed progenitor is a helium star-neutron star merger that underwent a common envelope phase expelling its hydrogen envelope. The resulting explosion created a GRB-like jet which gets thermalized by interacting with the dense, previously ejected material and thus creating the observed black-body, until finally the emission from the supernova dominated. An alternative explanation is a minor body falling onto a neutron star io the Galaxy

Published
2011

169. Ex Luna, Scientia: The Lunar Occultation eXplorer (LOX)

Author

Miller, Richard S., Ajello, M., John Beacom, Bloser, P. F., Burrows, A., Fryer, C. L., Goldsten, J. O., Hartmann, D. H., Hoeflich, P., Hungerford, A., Lawrence, D. J., Leising, M. D., Milne, P., Peplowski, P. N., Shirazi, F., Sukhbold, T., The, L. -S, Yokley, Z., and Young, C. A.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

LOX is a lunar-orbiting astrophysics mission that will probe the cosmos at MeV energies. It is guided by open questions regarding thermonuclear, or Type-Ia, supernovae (SNeIa) and will characterize these inherently radioactive objects by enabling a systematic survey of SNeIa at gamma-ray energies for the first time. Astronomical investigations from lunar orbit afford new opportunities to advance our understanding of the cosmos. The foundation of LOX is an observational approach well suited to the all-sky monitoring demands of supernova investigations and time-domain astronomy. Its inherently wide field-of-view and continuous all-sky monitoring provides an innovative way of addressing decadal survey questions at MeV energies (0.1-10 MeV). The LOX approach achieves high sensitivity with a simple, high-heritage instrument design that eliminates the need for complex, position-sensitive detectors, kinematic event reconstruction, masks, or other insensitive detector mass, while also mitigating technology development, implementation complexity, and their associated costs. LOX can be realized within existing programs, like Explorer., Comment: Astro2020 APC White Paper, Submitted to the National Academy of Sciences Decadal Survey on Astronomy and Astrophysics (Astro2020); 15 pages

Published
2019
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173. Predictors of self-perceived cultural responsiveness in entry-level physiotherapy students in Australia and Aotearoa New Zealand

Author

Te, M., Blackstock, F., Fryer, C., Gardner, Peter, Geary, L., Kuys, S., McPherson, K., Nahon, I., Tang, C., Taylor, L., Van Kessel, G., van der Zwan, K., Chipchase, L., Te, M., Blackstock, F., Fryer, C., Gardner, Peter, Geary, L., Kuys, S., McPherson, K., Nahon, I., Tang, C., Taylor, L., Van Kessel, G., van der Zwan, K., and Chipchase, L.

Abstract

Background: Ensuring physiotherapy students are well prepared to work safely and effectively in culturally diverse societies upon graduation is vital. Therefore, determining whether physiotherapy programs are effectively developing the cultural responsiveness of students is essential. This study aimed to evaluate the level of self-perceived cultural responsiveness of entry level physiotherapy students during their training, and explore the factors that might be associated with these levels. Methods: A cross sectional study of physiotherapy students from nine universities across Australia and Aotearoa New Zealand was conducted using an online self-administered questionnaire containing three parts: The Cultural Competence Assessment tool, Altemeyer’s Dogmatism scale, and the Marlowe-Crowne social desirability scale- short form. Demographic data relating to university, program, and level of study were also collected. Data was analysed using one-way ANOVA, t-tests and multiple regression analysis. Results: A total of 817 (19% response rate) students participated in this study. Overall, students had a moderate level of self-perceived cultural responsiveness (Mean (SD) = 5.15 (0.67)). Fewer number of weeks of clinical placement attended, lower levels of dogmatism, and greater social desirability were related to greater self-perceived cultural responsiveness. Additionally, fourth year undergraduate students perceived themselves to be less culturally responsive than first and second year students (p < 0.05). Conclusions: These results provide educators with knowledge about the level of self-perceived cultural responsiveness in physiotherapy students, and the factors that may need to be assessed and addressed to support the development of culturally responsive practice.

Published
2019

174. How Massive Single Stars End Their Life

Author

Heger, A, Fryer, C. L, Woosley, S. E, Langer, N, and Hartmann, D. H

Subjects
Astrophysics
Abstract

How massive stars die-what sort of explosion and remnant each produces-depends chiefly on the masses of their helium cores and hydrogen envelopes at death. For single stars, stellar winds are the only means of mass loss, and these are a function of the metallicity of the star. We discuss how metallicity, and a simplified prescription for its effect on mass loss, affects the evolution and final fate of massive stars. We map, as a function of mass and metallicity, where black holes and neutron stars are likely to form and where different types of supernovae are produced. Integrating over an initial mass function, we derive the relative populations as a function of metallicity. Provided that single stars rotate rapidly enough at death, we speculate on stellar populations that might produce gamma-ray bursts and jet-driven supernovae.

Published
2003

181. The Broadband Counterpart of the Short GRB 200522A at z = 0.5536: A Luminous Kilonova or a Collimated Outflow with a Reverse Shock?

Author

Fong, W., Laskar, T., Rastinejad, J., Escorial, A. Rouco, Schroeder, G., Barnes, J., Kilpatrick, C. D., Paterson, K., Berger, E., Metzger, B. D., Dong, Y., Nugent, A. E., Strausbaugh, R., Blanchard, P. K., Goyal, A., Cucchiara, A., Terreran, G., Alexander, K. D., Eftekhari, T., and Fryer, C.

Subjects
GAMMA ray bursts, GRAVITATIONAL waves, SPACE telescopes, LUMINOSITY
Abstract

We present the discovery of the radio afterglow and near-infrared (NIR) counterpart of the Swift short gamma-ray burst (GRB) GRB 200522A, located at a small projected offset of ≈1 kpc from the center of a young, star-forming host galaxy at z = 0.5536. The radio and X-ray luminosities of the afterglow are consistent with those of on-axis cosmological short GRBs. The NIR counterpart, revealed by our Hubble Space Telescope observations at a rest-frame time of ≈2.3 days, has a luminosity of ≈(1.3–1.7) × 1042 erg s−1. This is substantially lower than on-axis short GRB afterglow detections but is a factor of ≈8–17 more luminous than the kilonova of GW170817 and significantly more luminous than any kilonova candidate for which comparable observations exist. The combination of the counterpart's color (i − y = −0.08 ± 0.21; rest frame) and luminosity cannot be explained by standard radioactive heating alone. We present two scenarios to interpret the broadband behavior of GRB 200522A: a synchrotron forward shock with a luminous kilonova (potentially boosted by magnetar energy deposition), or forward and reverse shocks from a ≈14°, relativistic (Γ0 ≳ 10) jet. Models that include a combination of enhanced radioactive heating rates, low-lanthanide mass fractions, or additional sources of heating from late-time central engine activity may provide viable alternate explanations. If a stable magnetar was indeed produced in GRB 200522A, we predict that late-time radio emission will be detectable starting ≈0.3–6 yr after the burst for a deposited energy of ≈1053 erg. Counterparts of similar luminosity to GRB 200522A associated with gravitational wave events will be detectable with current optical searches to ≈250 Mpc. [ABSTRACT FROM AUTHOR]

Published
2021
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182. A search for optical and near-infrared counterparts of the compact binary merger GW190814.

Author

Thakur, A L, Dichiara, S, Troja, E, Chase, E A, Sánchez-Ramírez, R, Piro, L, Fryer, C L, Butler, N R, Watson, A M, Wollaeger, R T, Ambrosi, E, Becerra González, J, Becerra, R L, Bruni, G, Cenko, S B, Cusumano, G, D'Aì, A, Durbak, J, Fontes, C J, and Gatkine, P

Subjects
GAMMA ray bursts, OPTICAL limiting, GRAVITATIONAL waves, BLACK holes, STELLAR mergers, PHOTOMETRY
Abstract

We report on our observing campaign of the compact binary merger GW190814, detected by the Advanced LIGO and Advanced Virgo detectors on 2019 August 14. This signal has the best localization of any observed gravitational wave (GW) source, with a 90 per cent probability area of 18.5 deg2, and an estimated distance of ≈240 Mpc. We obtained wide-field observations with the Deca-Degree Optical Transient Imager (DDOTI) covering 88 per cent of the probability area down to a limiting magnitude of w = 19.9 AB. Nearby galaxies within the high probability region were targeted with the Lowell Discovery Telescope (LDT), whereas promising candidate counterparts were characterized through multicolour photometry with the Reionization and Transients InfraRed (RATIR) and spectroscopy with the Gran Telescopio de Canarias (GTC). We use our optical and near-infrared limits in conjunction with the upper limits obtained by the community to constrain the possible electromagnetic counterparts associated with the merger. A gamma-ray burst seen along its jet's axis is disfavoured by the multiwavelength data set, whereas the presence of a burst seen at larger viewing angles is not well constrained. Although our observations are not sensitive to a kilonova similar to AT2017gfo, we can rule out high-mass (>0.1 M⊙) fast-moving (mean velocity ≥0.3 c) wind ejecta for a possible kilonova associated with this merger. [ABSTRACT FROM AUTHOR]

Published
2020
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183. Multi-messenger Observations of a Binary Neutron Star Merger

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, Markus, Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calder, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, Ximeng, Chen, Y., Cheng, H. P., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, A. K. W., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. F., Cohen, D., Colla, A., Collette, C. G., Cominsky, L. R., Jr., M. Constancio, Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Dálya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C. F., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., De, S., DeBra, D., Degallaix, J., De Laurentis, M., Deléglise, S., Pozzo, W. Del, Demos, N., Denker, T., Dent, T., De Pietri, R., Dergachev, V., De Rosa, R., DeRosa, R. T., De Rossi, C., DeSalvo, R., De Varona, O., Devenson, J., Dhurandhar, S., Díaz, M. C., Fiore, L. Di, Giovanni, M. Di, Girolamo, T. Di, Lieto, A. Di, Pace, S. Di, Palma, I. Di, Renzo, F. Di, Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Álvarez, M. Dovale, Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Ducrot, M., Dupej, P., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J. D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Gretarsson, E. M., Griswold, B., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C. J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H. N., Isac, J. M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. 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A., Hampel-Arias, Z., Harding, J. P., Hernandez, S., Hernandez-Almada, A., Hona, B., Hüntemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Kieda, D., Lara, A., Lauer, R. J., Lennarz, D., Linnemann, J. T., Longinotti, A. L., Luna-García, R., López-Coto, R., Malone, K., Marinelli, S. S., Martinez, O., Martinez-Castellanos, I., Martínez-Castro, J., Martínez-Huerta, H., Matthews, J. A., Miranda-Romagnoli, P., Moreno, E., Mostafá, M., Nellen, L., Newbold, M., Nisa, M. U., Noriega-Papaqui, R., Pelayo, R., Pretz, J., Pérez-Pérez, E. G., Ren, Z., Rho, C. D., Rivière, C., Rosa-González, D., Rosenberg, M., Ruiz-Velasco, E., Salazar, H., Sandoval, A., Schneider, M., Schoorlemmer, H., Sinnis, G., Smith, A. J., Springer, R. W., Surajbali, P., Tibolla, O., Tollefson, K., Torres, I., Ukwatta, T. N., Weisgarber, T., Westerhoff, S., Wisher, I. G., Wood, J., Yapici, T., Yodh, G. B., Younk, P. W., Zhou, H., Álvarez, J. D., Aab, A., Abreu, P., Aglietta, M., Albuquerque, I. F. 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G., Jandt, I., Johnsen, J. A., Josebachuili, M., Jurysek, J., Kääpä, A., Kampert, K. H., Keilhauer, B., Kemmerich, N., Kemp, Julian, Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, Rafael, Krohm, N., Kuempel, D., Kunka, N., Lago, B. L., LaHurd, D., Lang, R. G., Lauscher, Markus, Legumina, R., Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lopes, L., López, R., Lorek, R., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Marsella, G., Martello, D., Martinez, H., Mathes, H. J., Mathys, S., Matthews, J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K. D., Michal, S., Micheletti, M. I., Middendorf, Lukas, Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Morlino, G., Müller, A. L., Müller, Gero, Muller, M. A., Müller, S., Mussa, R., Naranjo, I., Nguyen, P. H., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, Tim, Nitz, D., Nosek, D., Novotny, V., Nožka, L., Núñez, L. A., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pȩkala, J., Peña-Rodriguez, J., Pereira, L. A. S., Perlin, M., Perrone, L., Peters, Christine Jutta, Petrera, S., Phuntsok, J., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Plum, Matthias, Poh, J., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos-Pollan, Raúl, Rautenberg, J., Ravignani, D., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Saleh, A., Salina, G., Sánchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schröder, S., Schumacher, Johannes Christian, Sciutto, S. J., Segreto, A., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Soriano, J. F., Squartini, R., Stanca, D., Stasielak, J., Stassi, P., Stolpovskiy, M., Strafella, F., Streich, A., Suarez, F., Suarez-Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Šupík, J., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Timmermans, C., Tomankova, L., Tomé, B., Travnicek, P., Trini, M., Tueros, M., Ulrich, R., Unger, M., Urban, Martin, Valiño, I., Valore, L., Van Aar, G., Van Bodegom, Patrick, Van Den Berg, A. M., Van Vliet, A., Varela, E., Vargas Cárdenas, Bernardo, Vázquez, R. A., Ventura, C., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, David Simon, Watson, A. A., Weber, M., Weindl, A., Wiedeński, M., Wiencke, L., Wilczyński, H., Wirtz, Marcus, Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Kim, S., Schulze, S., Corral-Santana, J. M., González-López, J., Hartmann, D. H., Ishwara-Chandra, C. H., Martín, S., Mehner, A., Misra, K., Michałowski, M. J., Resmi, L., Paragi, Z., Agudo, I., An, T., Beswick, R., Casadio, C., Frey, S., Jonker, P., Kettenis, M., Marcote, B., Moldon, J., Szomoru, A., Langevelde, H. J., Cwiek, A., Cwiok, M., Czyrkowski, H., Dabrowski, R., Kasprowicz, G., Mankiewicz, L., Nawrocki, K., Opiela, R., Piotrowski, L. W., Wrochna, G., Zaremba, M., Żarnecki, A. F., Haggard, D., Nynka, M., Ruan, J. J., Bland, P. A., Booler, T., Devillepoix, H. A. R., De Gois, J. S., Hancock, P. J., Howie, R. M., Paxman, J., Sansom, E. K., Towner, M. C., Tonry, J., Coughlin, M., Stubbs, C. W., Denneau, L., Heinze, A., Stalder, B., Weiland, H., Eatough, R. P., Kramer, M., Kraus, A., Piro, L., González, J. Becerra, Butler, N. R., Khandrika, H. G., Kutyrev, A., Lee, W. H., Ricci, R., Sanchez-Ramirez, R., Veilleux, S., Watson, A. M., Wieringa, M. H., Burgess, J. M., Van Eerten, H., Fontes, C. J., Korobkin, O., Wollaeger, R. T., Camilo, F., Foley, A. R., Goedhart, S., Makhathini, S., Oozeer, N., Smirnov, O. M., and Woudt, P. A.

Abstract

59 Seiten : Illustrationen, Tabellen, Diagramme (2017).

Published
2017
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184. The intergroup study of Hodgkin's disease in children: a study of stages I and II

Author

Gehan, Edmund A., Sullivan, M.P., Fuller, L.M., Johnston, J., Kennedy, P., Fryer, C., Gilchrist, G.S., Hays, D.M., Hanson, W., Heller, R., Jenkin, R.D.T., Kung, F., Sheehan, W., Tefft, M., Ternberg, J., and Wharam, M.

Subjects
Hodgkin's disease -- Care and treatment, Chemotherapy, Radiotherapy, Hodgkin's disease in children -- Care and treatment, Health
Abstract

A total of 228 previously untreated children with Hodgkin's disease were treated at two cancer centers. At one, the patients were randomly assigned to receive either radiotherapy of the involved field alone, or radiotherapy of the involved field with chemotherapy. At the second center, patients received either extended-field radiotherapy alone or involved-field radiotherapy with chemotherapy. In both cases the chemotherapy consisted of six courses of mechlorethamine, vincristine, prednisone, and procarbazine. Five years after treatment, the groups which received adjuvant chemotherapy in addition to involved-field radiotherapy had significantly better relapse-free survival, at 97 percent and 93 percent at the two centers. However, despite having more relapses, the two groups receiving radiotherapy alone had a comparable overall five-year survival to those receiving adjuvant chemotherapy. In this study the extended-field radiation alone was superior to the involved-field radiotherapy for relapse-free survival at 67 and 41 percent respectively, but the patients were not randomized between the two centers conducting the study. Since the overall survival was not significantly changed by the chemotherapy, the benefits of remaining relapse-free must be weighed against the disadvantages of chemotherapy, including sterility and infection, in deciding on the appropriate course of treatment for Hodgkin's disease in children. (Consumer Summary produced by Reliance Medical Information, Inc.)

Published
1990

186. Californium-254 and Kilonova Light Curves

Author

Zhu, Y., primary, Wollaeger, R. T., additional, Vassh, N., additional, Surman, R., additional, Sprouse, T. M., additional, Mumpower, M. R., additional, Möller, P., additional, McLaughlin, G. C., additional, Korobkin, O., additional, Kawano, T., additional, Jaffke, P. J., additional, Holmbeck, E. M., additional, Fryer, C. L., additional, Even, W. P., additional, Couture, A. J., additional, and Barnes, J., additional

Published
2018
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190. Swift and NuSTAR observations of GW170817: Detection of a blue kilonova

Author

Evans, P. A., primary, Cenko, S. B., additional, Kennea, J. A., additional, Emery, S. W. K., additional, Kuin, N. P. M., additional, Korobkin, O., additional, Wollaeger, R. T., additional, Fryer, C. L., additional, Madsen, K. K., additional, Harrison, F. A., additional, Xu, Y., additional, Nakar, E., additional, Hotokezaka, K., additional, Lien, A., additional, Campana, S., additional, Oates, S. R., additional, Troja, E., additional, Breeveld, A. A., additional, Marshall, F. E., additional, Barthelmy, S. D., additional, Beardmore, A. P., additional, Burrows, D. N., additional, Cusumano, G., additional, D’Aì, A., additional, D’Avanzo, P., additional, D’Elia, V., additional, de Pasquale, M., additional, Even, W. P., additional, Fontes, C. J., additional, Forster, K., additional, Garcia, J., additional, Giommi, P., additional, Grefenstette, B., additional, Gronwall, C., additional, Hartmann, D. H., additional, Heida, M., additional, Hungerford, A. L., additional, Kasliwal, M. M., additional, Krimm, H. A., additional, Levan, A. J., additional, Malesani, D., additional, Melandri, A., additional, Miyasaka, H., additional, Nousek, J. A., additional, O’Brien, P. T., additional, Osborne, J. P., additional, Pagani, C., additional, Page, K. L., additional, Palmer, D. M., additional, Perri, M., additional, Pike, S., additional, Racusin, J. L., additional, Rosswog, S., additional, Siegel, M. H., additional, Sakamoto, T., additional, Sbarufatti, B., additional, Tagliaferri, G., additional, Tanvir, N. R., additional, and Tohuvavohu, A., additional

Published
2017
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191. Swift and NuSTAR observations of GW170817 : Detection of a blue kilonova

Author

Evans, P. A., Cenko, S. B., Kennea, J. A., Emery, S. W. K., Kuin, N. P. M., Korobkin, O., Wollaeger, R. T., Fryer, C. L., Madsen, K. K., Harrison, F. A., Xu, Y., Nakar, E., Hotokezaka, K., Lien, A., Campana, S., Oates, S. R., Troja, E., Breeveld, A. A., Marshall, F. E., Barthelmy, S. D., Beardmore, A. P., Burrows, D. N., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V., De Pasquale, M., Even, W. P., Fontes, C. J., Forster, K., Garcia, J., Giommi, P., Grefenstette, B., Gronwall, C., Hartmann, D. H., Heida, M., Hungerford, A. L., Kasliwal, M. M., Krimm, H. A., Levan, A. J., Malesani, D., Melandri, A., Miyasaka, H., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Page, K. L., Palmer, D. M., Perri, M., Pike, S., Racusin, J. L., Rosswog, Stephan, Siegel, M. H., Sakamoto, T., Sbarufatti, B., Tagliaferri, G., Tanvir, N. R., Tohuvavohu, A., Evans, P. A., Cenko, S. B., Kennea, J. A., Emery, S. W. K., Kuin, N. P. M., Korobkin, O., Wollaeger, R. T., Fryer, C. L., Madsen, K. K., Harrison, F. A., Xu, Y., Nakar, E., Hotokezaka, K., Lien, A., Campana, S., Oates, S. R., Troja, E., Breeveld, A. A., Marshall, F. E., Barthelmy, S. D., Beardmore, A. P., Burrows, D. N., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V., De Pasquale, M., Even, W. P., Fontes, C. J., Forster, K., Garcia, J., Giommi, P., Grefenstette, B., Gronwall, C., Hartmann, D. H., Heida, M., Hungerford, A. L., Kasliwal, M. M., Krimm, H. A., Levan, A. J., Malesani, D., Melandri, A., Miyasaka, H., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Page, K. L., Palmer, D. M., Perri, M., Pike, S., Racusin, J. L., Rosswog, Stephan, Siegel, M. H., Sakamoto, T., Sbarufatti, B., Tagliaferri, G., Tanvir, N. R., and Tohuvavohu, A.

Abstract

With the first direct detection of merging black holes in 2015, the era of gravitational wave (GW) astrophysics began. A complete picture of compact object mergers, however, requires the detection of an electromagnetic (EM) counterpart. We report ultraviolet (UV) and x-ray observations by Swift and the Nuclear Spectroscopic Telescope Array of the EM counter part of the binary neutron star merger GW170817. The bright, rapidly fading UV emission indicates a high mass (approximate to 0.03 solar masses) wind-driven outflow with moderate electron fraction (Y-e approximate to 0.27). Combined with the x-ray limits, we favor an observer viewing angle of approximate to 30 degrees away from the orbital rotation axis, which avoids both obscuration from the heaviest elements in the orbital plane and a direct view of any ultrarelativistic, highly collimated ejecta (a gamma-ray burst afterglow).

Published
2017
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192. The Emergence of a Lanthanide-rich Kilonova Following the Merger of Two Neutron Stars

Author

Tanvir, N. R., Levan, A. J., Gonzalez-Fernandez, C., Korobkin, O., Mandel, I., Rosswog, Stephan, Hjorth, J., D'Avanzo, P., Fruchter, A. S., Fryer, C. L., Kangas, T., Milvang-Jensen, B., Rosetti, S., Steeghs, D., Wollaeger, R. T., Cano, Z., Copperwheat, C. M., Covino, S., D'Elia, V., de Ugarte Postigo, A., Evans, P. A., Even, W. P., Fairhurst, S., Jaimes, R. Figuera, Fontes, C. J., Fujii, Y. I., Fynbo, J. P. U., Gompertz, B. P., Greiner, J., Hodosan, G., Irwin, M. J., Jakobsson, P., Jorgensen, U. G., Kann, D. A., Lyman, J. D., Malesani, D., McMahon, R. G., Melandri, A., O'Brien, P. T., Osborne, J. P., Palazzi, E., Perley, D. A., Pian, E., Piranomonte, S., Rabus, M., Rol, E., Rowlinson, A., Schulze, S., Sutton, P., Thone, C. C., Ulaczyk, K., Watson, D., Wiersema, K., Wijers, R. A. M. J., Tanvir, N. R., Levan, A. J., Gonzalez-Fernandez, C., Korobkin, O., Mandel, I., Rosswog, Stephan, Hjorth, J., D'Avanzo, P., Fruchter, A. S., Fryer, C. L., Kangas, T., Milvang-Jensen, B., Rosetti, S., Steeghs, D., Wollaeger, R. T., Cano, Z., Copperwheat, C. M., Covino, S., D'Elia, V., de Ugarte Postigo, A., Evans, P. A., Even, W. P., Fairhurst, S., Jaimes, R. Figuera, Fontes, C. J., Fujii, Y. I., Fynbo, J. P. U., Gompertz, B. P., Greiner, J., Hodosan, G., Irwin, M. J., Jakobsson, P., Jorgensen, U. G., Kann, D. A., Lyman, J. D., Malesani, D., McMahon, R. G., Melandri, A., O'Brien, P. T., Osborne, J. P., Palazzi, E., Perley, D. A., Pian, E., Piranomonte, S., Rabus, M., Rol, E., Rowlinson, A., Schulze, S., Sutton, P., Thone, C. C., Ulaczyk, K., Watson, D., Wiersema, K., and Wijers, R. A. M. J.

Abstract

We report the discovery and monitoring of the near-infrared counterpart (AT2017gfo) of a binary neutron-star merger event detected as a gravitational wave source by Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo (GW170817) and as a short gamma-ray burst by Fermi Gamma-ray Burst Monitor (GBM) and Integral SPI-ACS (GRB 170817A). The evolution of the transient light is consistent with predictions for the behavior of a kilonova/ macronova powered by the radioactive decay of massive neutron-rich nuclides created via r-process nucleosynthesis in the neutron-star ejecta. In particular, evidence for this scenario is found from broad features seen in Hubble Space Telescope infrared spectroscopy, similar to those predicted for lanthanide-dominated ejecta, and the much slower evolution in the near-infrared K-s-band compared to the optical. This indicates that the late-time light is dominated by high-opacity lanthanide-rich ejecta, suggesting nucleosynthesis to the third r-process peak (atomic masses A approximate to 195). This discovery confirms that neutron-star mergers produce kilo-/macronovae and that they are at least a major-if not the dominant-site of rapid neutron capture nucleosynthesis in the universe.

Published
2017
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193. The X-ray counterpart to the gravitational wave event GW 170817

Author

Troja, E., Piro, L., van Eerten, H., Wollaeger, R. T., Im, M., Fox, O. D., Butler, N. R., Cenko, S. B., Sakamoto, T., Fryer, C. L., Ricci, R., Lien, A., Ryan Jr., R. E., Korobkin, O., Lee, S. -K., Burgess, J. M., Lee, W. H., Watson, A. M., Choi, C., Covino, S., Avanzo, P. D', Fontes, C. J., Gonzalez, J. Becerra, Khandrika, H. G., Kim, J., Kim, S. -L., Lee, C. -U., Lee, H. M., Kutyrev, A., Lim, G., Ramirez, R. Sanchez, Veilleux, S., Wieringa, M. H., Yoon, Y., Troja, E., Piro, L., van Eerten, H., Wollaeger, R. T., Im, M., Fox, O. D., Butler, N. R., Cenko, S. B., Sakamoto, T., Fryer, C. L., Ricci, R., Lien, A., Ryan Jr., R. E., Korobkin, O., Lee, S. -K., Burgess, J. M., Lee, W. H., Watson, A. M., Choi, C., Covino, S., Avanzo, P. D', Fontes, C. J., Gonzalez, J. Becerra, Khandrika, H. G., Kim, J., Kim, S. -L., Lee, C. -U., Lee, H. M., Kutyrev, A., Lim, G., Ramirez, R. Sanchez, Veilleux, S., Wieringa, M. H., and Yoon, Y.

Abstract

A long-standing paradigm in astrophysics is that collisions- or mergers- of two neutron stars (NSs) form highly relativistic and collimated outflows (jets) powering gamma-ray bursts (GRBs) of short (< 2 s) duration. However, the observational support for this model is only indirect. A hitherto outstanding prediction is that gravitational wave (GW) events from such mergers should be associated with GRBs, and that a majority of these GRBs should be off-axis, that is, they should point away from the Earth. Here we report the discovery of the X-ray counterpart associated with the GW event GW170817. While the electromagnetic counterpart at optical and infrared frequencies is dominated by the radioactive glow from freshly synthesized r-process material in the merger ejecta, known as kilonova, observations at X-ray and, later, radio frequencies exhibit the behavior of a short GRB viewed off-axis. Our detection of X-ray emission at a location coincident with the kilonova transient provides the missing observational link between short GRBs and GWs from NS mergers, and gives independent confirmation of the collimated nature of the GRB emission., Comment: 38 pages, 10 figures, Nature, in press

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2017
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194. A gravitational-wave standard siren measurement of the Hubble constant

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Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. 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Abstract

The detection of GW170817 in both gravitational waves and electromagnetic waves heralds the age of gravitational-wave multi-messenger astronomy. On 17 August 2017 the Advanced LIGO and Virgo detectors observed GW170817, a strong signal from the merger of a binary neutron-star system. Less than 2 seconds after the merger, a gamma-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source. This sky region was subsequently observed by optical astronomy facilities, resulting in the identification of an optical transient signal within $\sim 10$ arcsec of the galaxy NGC 4993. These multi-messenger observations allow us to use GW170817 as a standard siren, the gravitational-wave analog of an astronomical standard candle, to measure the Hubble constant. This quantity, which represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Our measurement combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using electromagnetic data. This approach does not require any form of cosmic "distance ladder;" the gravitational wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be $70.0^{+12.0}_{-8.0} \, \mathrm{km} \, \mathrm{s}^{-1} \, \mathrm{Mpc}^{-1}$ (maximum a posteriori and 68% credible interval). This is consistent with existing measurements, while being completely independent of them. Additional standard-siren measurements from future gravitational-wave sources will provide precision constraints of this important cosmological parameter., Comment: 26 pages, 5 figures, Nature in press. For more information see https://dcc.ligo.org/LIGO-P1700296/public

Published
2017
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195. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. I. Dark Energy Camera Discovery of the Optical Counterpart

Author

Soares-Santos, M., Holz, D. E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H., Kessler, R., Sako, M., Allam, S., Tucker, D. L., Butler, R. E., Palmese, A., Doctor, Z., Diehl, H. T., Frieman, J., Yanny, B., Lin, H., Scolnic, D., Cowperthwaite, P., Neilsen, E., Marriner, J., Kuropatkin, N., Hartley, W. G., Paz-Chinchón, F., Alexander, K. D., Balbinot, E., Blanchard, P., Brown, D. A., Carlin, J. L., Conselice, C., Cook, E. R., Drlica-Wagner, A., Drout, M. R., Durret, F., Eftekhari, T., Farr, B., Finley, D. A., Foley, R. J., Fong, W., Fryer, C. L., García-Bellido, J., Gill, M. S . S., Gruendl, R. A., Hanna, C., Kasen, D., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Margutti, R., Marshall, J. L., Matheson, T., Medina, G. E., Metzger, B. D., Muñoz, R. R., Muir, J., Nicholl, M., Quataert, E., Rest, A., Sauseda, M., Schlegel, D. J., Secco, L. F., Sobreira, F., Stebbins, A., Villar, V. A., Walker, A. R., Wester, W., Williams, P. K. G., Zenteno, A., Zhang, Y., Abbott, T. M. C., Abdalla, F. B., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Lahav, O., Lima, M., Maia, M. A. G., March, M., McMahon, R. G., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R. L. C., Petravick, D., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Wechsler, R. H., Weller, J., Soares-Santos, M., Holz, D. E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H., Kessler, R., Sako, M., Allam, S., Tucker, D. L., Butler, R. E., Palmese, A., Doctor, Z., Diehl, H. T., Frieman, J., Yanny, B., Lin, H., Scolnic, D., Cowperthwaite, P., Neilsen, E., Marriner, J., Kuropatkin, N., Hartley, W. G., Paz-Chinchón, F., Alexander, K. D., Balbinot, E., Blanchard, P., Brown, D. A., Carlin, J. L., Conselice, C., Cook, E. R., Drlica-Wagner, A., Drout, M. R., Durret, F., Eftekhari, T., Farr, B., Finley, D. A., Foley, R. J., Fong, W., Fryer, C. L., García-Bellido, J., Gill, M. S . S., Gruendl, R. A., Hanna, C., Kasen, D., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Margutti, R., Marshall, J. L., Matheson, T., Medina, G. E., Metzger, B. D., Muñoz, R. R., Muir, J., Nicholl, M., Quataert, E., Rest, A., Sauseda, M., Schlegel, D. J., Secco, L. F., Sobreira, F., Stebbins, A., Villar, V. A., Walker, A. R., Wester, W., Williams, P. K. G., Zenteno, A., Zhang, Y., Abbott, T. M. C., Abdalla, F. B., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Lahav, O., Lima, M., Maia, M. A. G., March, M., McMahon, R. G., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R. L. C., Petravick, D., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Wechsler, R. H., and Weller, J.

Abstract

We present the Dark Energy Camera (DECam) discovery of the optical counterpart of the first binary neutron star merger detected through gravitational wave emission, GW170817. Our observations commenced 10.5 hours post-merger, as soon as the localization region became accessible from Chile. We imaged 70 deg$^2$ in the $i$ and $z$ bands, covering 93\% of the initial integrated localization probability, to a depth necessary to identify likely optical counterparts (e.g., a kilonova). At 11.4 hours post-merger we detected a bright optical transient located $10.6''$ from the nucleus of NGC\,4993 at redshift $z=0.0098$, consistent (for $H_0 = 70$\, km s$^{-1}$ Mpc$^{-1}$) with the distance of $40 \pm 8$\, Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes $i\approx 17.30$ and $z\approx 17.45$, and thus an absolute magnitude of $M_i = -15.7$, in the luminosity range expected for a kilonova. We identified 1,500 potential transient candidates. Applying simple selection criteria aimed at rejecting background events such as supernovae, we find the transient associated with NGC\,4993 as the only remaining plausible counterpart, and reject chance coincidence at the 99.5\% confidence level. We therefore conclude that the optical counterpart we have identified near NGC\,4993 is associated with GW170817. This discovery ushers in the era of multi-messenger astronomy with gravitational waves, and demonstrates the power of DECam to identify the optical counterparts of gravitational-wave sources., Comment: 9 Pages, 3 Figures, 2 Tables. ApJL, In Press. Keywords: GW170817, LVC

Published
2017
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196. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. IV. Detection of Near-infrared Signatures of r-process Nucleosynthesis with Gemini-South

Author

Chornock, R., Berger, E., Kasen, D., Cowperthwaite, P. S., Nicholl, M., Villar, V. A., Alexander, K. D., Blanchard, P. K., Eftekhari, T., Fong, W., Margutti, R., Williams, P. K. G., Annis, J., Brout, D., Brown, D. A., Chen, H. -Y., Drout, M. R., Foley, R. J., Frieman, J. A., Fryer, C. L., Holz, D. E., Matheson, T., Metzger, B. D., Quataert, E., Rest, A., Sako, M., Scolnic, D. M., Smith, N., Soares-Santos, M., Chornock, R., Berger, E., Kasen, D., Cowperthwaite, P. S., Nicholl, M., Villar, V. A., Alexander, K. D., Blanchard, P. K., Eftekhari, T., Fong, W., Margutti, R., Williams, P. K. G., Annis, J., Brout, D., Brown, D. A., Chen, H. -Y., Drout, M. R., Foley, R. J., Frieman, J. A., Fryer, C. L., Holz, D. E., Matheson, T., Metzger, B. D., Quataert, E., Rest, A., Sako, M., Scolnic, D. M., Smith, N., and Soares-Santos, M.

Abstract

We present a near-infrared spectral sequence of the electromagnetic counterpart to the binary neutron star merger GW170817 detected by Advanced LIGO/Virgo. Our dataset comprises seven epochs of J+H spectra taken with FLAMINGOS-2 on Gemini-South between 1.5 and 10.5 days after the merger. In the initial epoch, the spectrum is dominated by a smooth blue continuum due to a high-velocity, lanthanide-poor blue kilonova component. Starting the following night, all subsequent spectra instead show features that are similar to those predicted in model spectra of material with a high concentration of lanthanides, including spectral peaks near 1.07 and 1.55 microns. Our fiducial model with 0.04 M_sun of ejecta, an ejection velocity of v=0.1c, and a lanthanide concentration of X_lan=1e-2 provides a good match to the spectra taken in the first five days, although it over-predicts the late-time fluxes. We also explore models with multiple fitting components, in each case finding that a significant abundance of lanthanide elements is necessary to match the broad spectral peaks that we observe starting at 2.5 d after the merger. These data provide direct evidence that binary neutron star mergers are significant production sites of even the heaviest r-process elements., Comment: 9 pages, 4 figures, 1 table, ApJL, in press

Published
2017
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197. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. II. UV, Optical, and Near-IR Light Curves and Comparison to Kilonova Models

Author

Cowperthwaite, P. S., Berger, E., Villar, V. A., Metzger, B. D., Nicholl, M., Chornock, R., Blanchard, P. K., Fong, W., Margutti, R., Soares-Santos, M., Alexander, K. D., Allam, S., Annis, J., Brout, D., Brown, D. A., Butler, R. E., Chen, H. -Y., Diehl, H. T., Doctor, Z., Drout, M. R., Eftekhari, T., Farr, B., Finley, D. A., Foley, R. J., Frieman, J. A., Fryer, C. L., García-Bellido, J., Gill, M. S. S., Guillochon, J., Herner, K., Holz, D. E., Kasen, D., Kessler, R., Marriner, J., Matheson, T., Neilsen, Jr., E. H., Quataert, E., Palmese, A., Rest, A., Sako, M., Scolnic, D. M., Smith, N., Tucker, D. L., Williams, P. K. G., Balbinot, E., Carlin, J. L., Cook, E. R., Durret, F., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Marshall, J. L., Medina, G. E., Muir, J., Muñoz, R. R., Sauseda, M., Schlegel, D. J., Secco, L. F., Vivas, A. K., Wester, W., Zenteno, A., Zhang, Y., Abbott, T. M. C., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., March, M., Martini, P., McMahon, R. G., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Ogando, R. L. C., Plazas, A. A., Roe, N., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Yanny, B., Zuntz, J., Cowperthwaite, P. S., Berger, E., Villar, V. A., Metzger, B. D., Nicholl, M., Chornock, R., Blanchard, P. K., Fong, W., Margutti, R., Soares-Santos, M., Alexander, K. D., Allam, S., Annis, J., Brout, D., Brown, D. A., Butler, R. E., Chen, H. -Y., Diehl, H. T., Doctor, Z., Drout, M. R., Eftekhari, T., Farr, B., Finley, D. A., Foley, R. J., Frieman, J. A., Fryer, C. L., García-Bellido, J., Gill, M. S. S., Guillochon, J., Herner, K., Holz, D. E., Kasen, D., Kessler, R., Marriner, J., Matheson, T., Neilsen, Jr., E. H., Quataert, E., Palmese, A., Rest, A., Sako, M., Scolnic, D. M., Smith, N., Tucker, D. L., Williams, P. K. G., Balbinot, E., Carlin, J. L., Cook, E. R., Durret, F., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Marshall, J. L., Medina, G. E., Muir, J., Muñoz, R. R., Sauseda, M., Schlegel, D. J., Secco, L. F., Vivas, A. K., Wester, W., Zenteno, A., Zhang, Y., Abbott, T. M. C., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., March, M., Martini, P., McMahon, R. G., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Ogando, R. L. C., Plazas, A. A., Roe, N., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Yanny, B., and Zuntz, J.

Abstract

We present UV, optical, and NIR photometry of the first electromagnetic counterpart to a gravitational wave source from Advanced LIGO/Virgo, the binary neutron star merger GW170817. Our data set extends from the discovery of the optical counterpart at $0.47$ days to $18.5$ days post-merger, and includes observations with the Dark Energy Camera (DECam), Gemini-South/FLAMINGOS-2 (GS/F2), and the {\it Hubble Space Telescope} ({\it HST}). The spectral energy distribution (SED) inferred from this photometry at $0.6$ days is well described by a blackbody model with $T\approx 8300$ K, a radius of $R\approx 4.5\times 10^{14}$ cm (corresponding to an expansion velocity of $v\approx 0.3c$), and a bolometric luminosity of $L_{\rm bol}\approx 5\times10^{41}$ erg s$^{-1}$. At $1.5$ days we find a multi-component SED across the optical and NIR, and subsequently we observe rapid fading in the UV and blue optical bands and significant reddening of the optical/NIR colors. Modeling the entire data set we find that models with heating from radioactive decay of $^{56}$Ni, or those with only a single component of opacity from $r$-process elements, fail to capture the rapid optical decline and red optical/NIR colors. Instead, models with two components consistent with lanthanide-poor and lanthanide-rich ejecta provide a good fit to the data, the resulting "blue" component has $M_\mathrm{ej}^\mathrm{blue}\approx 0.01$ M$_\odot$ and $v_\mathrm{ej}^\mathrm{blue}\approx 0.3$c, and the "red" component has $M_\mathrm{ej}^\mathrm{red}\approx 0.04$ M$_\odot$ and $v_\mathrm{ej}^\mathrm{red}\approx 0.1$c. These ejecta masses are broadly consistent with the estimated $r$-process production rate required to explain the Milky Way $r$-process abundances, providing the first evidence that BNS mergers can be a dominant site of $r$-process enrichment., Comment: 13 Pages, 3 Figures, 2 Tables. ApJL, In Press. Keywords: GW170817, LVC

Published
2017
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198. NuGrid Stellar Data Set. II. Stellar Yields from H to Bi for Stellar Models with Mzams = 1 to 25Msun and Z = 0.0001 to 0.02

Author

Ritter, C., Herwig, F., Jones, S., Pignatari, M., Fryer, C., Hirschi, R., Ritter, C., Herwig, F., Jones, S., Pignatari, M., Fryer, C., and Hirschi, R.

Abstract

We provide here a significant extension of the NuGrid Set 1 models in mass coverage and toward lower metallicity, adopting the same physics assumptions. The combined data set now includes the initial masses M/Msun = 1, 1.65, 2, 3, 4, 5, 6, 7, 12, 15, 20, 25 for Z = 0.02, 0.01, 0.006, 0.001, 0.0001 with alpha-enhanced composition for the lowest three metallicities. These models are computed with the MESA stellar evolution code and are evolved up to the AGB, the white dwarf stage, or until core collapse. The nucleosynthesis was calculated for all isotopes in post-processing with the NuGrid mppnp code. Explosive nucleosynthesis is based on semi-analytic 1D shock models. Metallicity-dependent mass loss, convective boundary mixing in low- and intermediate mass models and H and He core burning massive star models is included. Convective O-C shell mergers in some stellar models lead to the strong production of odd-Z elements P, Cl, K and Sc. In AGB models with hot dredge-up the convective boundary mixing efficiency is reduced to accommodate for its energetic feedback. In both low-mass and massive star models at the lowest metallicity H-ingestion events are observed and lead to i-process nucleosynthesis and substantial N-15 production. Complete yield data tables, derived data products and online analytic data access are provided., Comment: Published. Detailed online data available at Canadian Astronomical Data Center, DOI:10.11570/18.0002 (http://www.canfar.phys.uvic.ca/vospace/nodes/AstroDataCitationDOI/CISTI.CANFAR/18.0002/18.0002.html?view=data). See Appendix for details

Published
2017
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199. The evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates of LIGO/Virgo binary black holes

Author

Belczynski, K., Klencki, J., Fields, C. E., Olejak, A., Berti, E., Meynet, G., Fryer, C. L., Holz, D. E., O'Shaughnessy, R., Brown, D. A., Bulik, T., Leung, S. C., Nomoto, K., Madau, P., Hirschi, R., Kaiser, E., Jones, S., Mondal, S., Chruslinska, M., Drozda, P., Gerosa, D., Doctor, Z., Giersz, M., Ekstrom, S., Georgy, C., Askar, A., Baibhav, V., Wysocki, D., Natan, T., Farr, W. M., Wiktorowicz, G., Miller, M. Coleman, Farr, B., Lasota, J. -P., Belczynski, K., Klencki, J., Fields, C. E., Olejak, A., Berti, E., Meynet, G., Fryer, C. L., Holz, D. E., O'Shaughnessy, R., Brown, D. A., Bulik, T., Leung, S. C., Nomoto, K., Madau, P., Hirschi, R., Kaiser, E., Jones, S., Mondal, S., Chruslinska, M., Drozda, P., Gerosa, D., Doctor, Z., Giersz, M., Ekstrom, S., Georgy, C., Askar, A., Baibhav, V., Wysocki, D., Natan, T., Farr, W. M., Wiktorowicz, G., Miller, M. Coleman, Farr, B., and Lasota, J. -P.

Abstract

All ten LIGO/Virgo binary black hole (BH-BH) coalescences reported from the O1/O2 runs have near zero effective spins. There are only three potential explanations of this fact. If the BH spin magnitudes are large then (i) either both BH spin vectors must be nearly in the orbital plane or (ii) the spin angular momenta of the BHs must be oppositely directed and similar in magnitude. Or, (iii) the BH spin magnitudes are small. We test the third hypothesis within the framework of the classical isolated binary evolution scenario of the BH-BH merger formation. We test three models of angular momentum transport in massive stars: a mildly efficient transport by meridional currents (as employed in the Geneva code), an efficient transport by the Tayler-Spruit magnetic dynamo (as implemented in the MESA code), and a very-efficient transport (as proposed by Fuller et al.) to calculate natal BH spins. We allow for binary evolution to increase the BH spins through accretion and account for the potential spin-up of stars through tidal interactions. Additionally, we update the calculations of the stellar-origin BH masses, include revisions to the history of star formation and to the chemical evolution across cosmic time. We find that we can match simultaneously the observed BH-BH merger rate density, BH masses, and effective spins. Models with efficient angular momentum transport are favored. The updated stellar-mass weighted gas-phase metallicity evolution now used in our models appears to be a key in better reproducing the LIGO/Virgo merger rate estimate. Mass losses during the pair-instability pulsation supernova phase are likely overestimated if the merger GW170729 hosts a BH more massive than 50 Msun. We also estimate rate of BH-NS mergers from recent LIGO/Virgo observations. Our updated models of BH-BH, BH-NS and NS-NS mergers are now publicly available at www.syntheticuniverse.org., Comment: A&A accepted: revised comparison with LIGO/Virgo (41 pages)

Published
2017
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200. Microlensing constraints on the mass of single stars from HST astrometric measurements

Author

Kains, Noé, Calamida, A., Sahu, K. C., Casertano, S., Anderson, J., Udalski, A., Zoccali, M., Bond, H., Albrow, M., Bond, I., Brown, T., Dominik, M., Fryer, C., Livio, M., Mao, S., Rejkuba, M., Kains, Noé, Calamida, A., Sahu, K. C., Casertano, S., Anderson, J., Udalski, A., Zoccali, M., Bond, H., Albrow, M., Bond, I., Brown, T., Dominik, M., Fryer, C., Livio, M., Mao, S., and Rejkuba, M.

Abstract

We report on the first results from a large-scale observing campaign aiming to use astrometric microlensing to detect and place limits on the mass of single objects, including stellar remnants. We used the Hubble Space Telescope to monitor stars near the Galactic Center for 3 years, and we measured the brightness and positions of $\sim$2 million stars at each observing epoch. In addition to this, we monitored the same pointings using the VIMOS imager on the Very Large Telescope. The stars we monitored include several bright microlensing events observed from the ground by the OGLE collaboration. In this paper, we present the analysis of our photometric and astrometric measurements for 6 of these events, and derive mass constraints for the lens in each of these. Although these constraints are limited by the photometric precision of ground-based data, and our ability to determine the lens distance, we were able to constrain the size of the Einstein ring radius thanks to our precise astrometric measurements, the first routine measurements of this type from a large-scale observing program. This demonstrates the power of astrometric microlensing as a tool to constrain the masses of stars, stellar remnants, and, in the future, of extrasolar planets, using precise ground- and space-based observations., Comment: ApJ, in press; 16 pages, 10 figures

Published
2017
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