Author: "Palmer D." - Searchworks@Jio Institute Digital Library Search Results

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4,917 results on '"Palmer D."'

1. Step forward towards treat-to-target management of giant cell arteritis: patients stratification aiming to targeted remission – updated guidelines

Author: El Miedany, Y, El Gaafary, M, Toth, M, Abdel Azim, A, Palmer, D, Dolbear, G, Affam, D, Hassan, W, Tabra, SA, Saber, S, and Abu-zaid, MH
Published: 2024
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2. Swift/UVOT discovery of Swift J221951-484240: a UV luminous ambiguous nuclear transient

Author: Oates, S. R., Kuin, N. P. M., Nicholl, M., Marshall, F., Ridley, E., Boutsia, K., Breeveld, A. A., Buckley, D. A. H., Cenko, S. B., De Pasquale, M., Edwards, P. G., Gromadzki, M., Gupta, R., Laha, S., Morrell, N., Orio, M., Pandey, S. B., Page, M. J., Page, K. L., Parsotan, T., Rau, A., Schady, P., Stevens, J., Brown, P. J., Evans, P. A., Gronwall, C., Kennea, J. A., Klingler, N. J., Siegel, M. H., Tohuvavohu, A., Ambrosi, E., Barthelmy, S. D., Beardmore, A. P., Bernardini, M. G., Bonnerot, C., Campana, S., Caputo, R., Ciroi, S., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V., Giommi, P., Hartmann, D. H., Krimm, H. A., Malesani, D. B., Melandri, A., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Palmer, D. M., Perri, M., Racusin, J. L., Sakamoto, T., Sbarufatti, B., Schlieder, J. E., Tagliaferri, G., Troja, E., and Xu, D.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery of Swift J221951-484240 (hereafter: J221951), a luminous slow-evolving blue transient that was detected by the Neil Gehrels Swift Observatory Ultra-violet/Optical Telescope (Swift/UVOT) during the follow-up of Gravitational Wave alert S190930t, to which it is unrelated. Swift/UVOT photometry shows the UV spectral energy distribution of the transient to be well modelled by a slowly shrinking black body with an approximately constant temperature of T~2.5x10^4 K. At a redshift z=0.5205, J221951 had a peak absolute magnitude of M_u,AB = -23 mag, peak bolometric luminosity L_max=1.1x10^45 erg s^-1 and a total radiated energy of E>2.6x10^52 erg. The archival WISE IR photometry shows a slow rise prior to a peak near the discovery date. Spectroscopic UV observations display broad absorption lines in N V and O VI, pointing toward an outflow at coronal temperatures. The lack of emission in the higher H~Lyman lines, N I and other neutral lines is consistent with a viewing angle close to the plane of the accretion or debris disc. The origin of J221951 can not be determined with certainty but has properties consistent with a tidal disruption event and the turn-on of an active galactic nucleus., Comment: 37 pages (25 main + 12 supplementary), submitted to MNRAS
Published: 2023

3. The 100-month Swift catalogue of supergiant fast X-ray transients II. SFXT diagnostics from outburst properties

Author: P., Romano, A., Evans P., E., Bozzo, V., Mangano, S., Vercellone, C., Guidorzi, L., Ducci, A., Kennea J., D., Barthelmy S., M., Palmer D., A., Krimm H., and B., Cenko
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Supergiant Fast X-ray Transients (SFXT) are High Mass X-ray Binaries displaying X-ray outbursts reaching peak luminosities of 10$^{38}$ erg/s and spend most of their life in more quiescent states with luminosities as low as 10$^{32}$-10$^{33}$ erg/s. The main goal of our comprehensive and uniform analysis of the SFXT Swift triggers is to provide tools to predict whether a transient which has no known X-ray counterpart may be an SFXT candidate. These tools can be exploited for the development of future missions exploring the variable X-ray sky through large FoV instruments. We examined all available data on outbursts of SFXTs that triggered the Swift/BAT collected between 2005-08-30 and 2014-12-31, in particular those for which broad-band data, including the Swift/XRT ones, are also available. We processed all BAT and XRT data uniformly with the Swift Burst Analyser to produce spectral evolution dependent flux light curves for each outburst. The BAT data allowed us to infer useful diagnostics to set SFXT triggers apart from the general GRB population, showing that SFXTs give rise uniquely to image triggers and are simultaneously very long, faint, and `soft' hard-X-ray transients. The BAT data alone can discriminate very well the SFXTs from other fast transients such as anomalous X-ray pulsars and soft gamma repeaters. However, to distinguish SFXTs from, for instance, accreting millisecond X-ray pulsars and jetted tidal disruption events, the XRT data collected around the time of the BAT triggers are decisive. The XRT observations of 35/52 SFXT BAT triggers show that in the soft X-ray energy band, SFXTs display a decay in flux from the peak of the outburst of at least 3 orders of magnitude within a day and rarely undergo large re-brightening episodes, favouring in most cases a rapid decay down to the quiescent level within 3-5 days (at most). [Abridged], Comment: Accepted for publication in Astronomy and Astrophysics. 18 pages, 11 figures
Published: 2022
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4. Treatment with PB125® Increases Femoral Long Bone Strength in 15-Month-Old Female Hartley Guinea Pigs

Author: Andrie, K. M., Palmer, D. R., Wahl, O., Bork, S., Campbell, M., Walsh, M. A., Sanford, J., Musci, R. V., Hamilton, Karyn L., Santangelo, Kelly S., and Puttlitz, Christian M.
Published: 2024
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5. ATHENA Detector Proposal -- A Totally Hermetic Electron Nucleus Apparatus proposed for IP6 at the Electron-Ion Collider

Author: ATHENA Collaboration, Adam, J., Adamczyk, L., Agrawal, N., Aidala, C., Akers, W., Alekseev, M., Allen, M. M., Ameli, F., Angerami, A., Antonioli, P., Apadula, N. J., Aprahamian, A., Armstrong, W., Arratia, M., Arrington, J. R., Asaturyan, A., Aschenauer, E. C., Augsten, K., Aune, S., Bailey, K., Baldanza, C., Bansal, M., Barbosa, F., Barion, L., Barish, K., Battaglieri, M., Bazilevsky, A., Behera, N. K., Berdnikov, V., Bernauer, J., Berriaud, C., Bhasin, A., Bhattacharya, D. S., Bielcik, J., Bielcikova, J., Bissolotti, C., Boeglin, W., Bondì, M., Borri, M., Bossu, F., Bouyjou, F., Brandenburg, J. D., Bressan, A., Brooks, M., Bueltmann, S. L., Byer, D., Caines, H., Sanchez, M. Calderon de la Barca, Calvelli, V., Camsonne, A., Cappelli, L., Capua, M., Castro, M., Cavazza, D., Cebra, D., Celentano, A., Chakaberia, I., Chan, B., Chang, W., Chartier, M., Chatterjee, C., Chen, D., Chen, J., Chen, K., Chen, Z., Chetri, H., Chiarusi, T., Chiosso, M., Chu, X., Chwastowski, J. J., Cicala, G., Cisbani, E., Cline, E., Cloet, I., Colella, D., Contalbrigo, M., Contin, G., Corliss, R., Corrales-Morales, Y., Crafts, J., Crawford, C., Cruz-Torres, R., D'Ago, D., D'Angelo, A., D'Hose, N., Dainton, J., Torre, S. Dalla, Dasgupta, S. S., Dash, S., Dashyan, N., Datta, J., Daugherity, M., De Vita, R., Deconinck, W., Defurne, M., Dehmelt, K., Del Dotto, A., Delcarro, F., Dellacasa, G., Demiroglu, Z. S., Deptuch, G. W., Desai, V., Deshpande, A., Devereaux, K., Dhillon, R., Di Salvo, R., Dilks, C., Dixit, D., Dobbs, S., Dong, X., Drachenberg, J., Drees, A., Dupre, R., Durham, M., Dzhygadlo, R., Fassi, L. El, Elia, D., Epple, E., Esha, R., Evdokimov, O., Eyser, O., Falchieri, D., Fan, W., Fantini, A., Fatemi, R., Fazio, S., Fegan, S., Filippi, A., Fox, H., Francisco, A., Freeze, A., Furletov, S., Furletova, Y., Gal, C., Gardner, S., Garg, P., Gaskell, D., Gates, K., Gericke, M. T. W., Geurts, F., Ghosh, C., Giacalone, M., Giacomini, F., Gilchrist, S., Glazier, D., Gnanvo, K., Gonella, L., Greiner, L. C., Guerrini, N., Guo, L., Gupta, A., Gupta, R., Guryn, W., He, X., Hemmick, T., Heppelmann, S., Higinbotham, D., Hoballah, M., Hoghmrtsyan, A., Hohlmann, M., Horn, T., Hornidge, D., Huang, H. Z., Hyde, C. E., Iapozzuto, P., Idzik, M., Jacak, B. V., Jadhav, M., Jain, S., Jena, C., Jentsch, A., Ji, Y., Ji, Z., Jia, J., Jones, P. G., Jones, R. W. I., Joosten, S., Joshi, S., Kabir, L., Kalicy, G., Karyan, G., Kashyap, V. K. S., Kawall, D., Ke, H., Kelsey, M., Kim, J., Kiryluk, J., Kiselev, A., Klein, S. R., Klest, H., Kochar, V., Korsch, W., Kosarzewski, L., Kotzinian, A., Krizek, F., Kumar, A., Kumar, K. S., Kumar, L., Kumar, R., Kumar, S., Kunnath, A., Kushawaha, N., Lacey, R., Lai, Y. S., Lalwani, K., Landgraf, J., Lanza, L., Lattuada, D., Lavinsky, M., Lee, J. H., Lee, S. H., Lemmon, R., Lestone, A., Lewis, N., Li, H., Li, S., Li, W., Li, X., Liang, X., Ligonzo, T., Lin, T., Liu, J., Liu, K., Liu, M., Livingston, K., Liyanage, N., Ljubicic, T., Long, O., Lukow, N., Ma, Y., Mammei, J., Mammoliti, F., Mamo, K., Mandjavidze, I., Maple, S., Marchand, D., Margotti, A., Markert, C., Markowitz, P., Marshall, T., Martin, A., Marukyan, H., Mastroserio, A., Mathew, S., Mayilyan, S., Mayri, C., McEneaney, M., Mei, Y., Meng, L., Meot, F., Metcalfe, J., Meziani, Z. -E., Mihir, P., Milton, R., Mirabella, A., Mirazita, M., Mkrtchyan, A., Mkrtchyan, H., Mohanty, B., Mondal, M., Morreale, A., Movsisyan, A., Muenstermann, D., Mukherjee, A., Camacho, C. Munoz, Murray, M. J., Mustafa, H., Myska, M., Nachman, B. P., Nagai, K., Naik, R., Naim, J. P., Nam, J., Nandi, B., Nappi, E., Nasim, Md., Neff, D., Neiret, D., Newman, P. R., Nguyen, M., Niccolai, S., Nie, M., Noferini, F., Norman, J., Noto, F., Nunes, A. S., O'Connor, T., Odyniec, G., Okorokov, V. A., Osipenko, M., Page, B., Palatchi, C., Palmer, D., Palni, P., Pandey, S., Panzieri, D., Park, S., Paschke, K., Pastore, C., Patra, R. N., Paul, A., Paul, S., Pecar, C., Peck, A., Pegg, I., Pellegrino, C., Peng, C., Pentchev, L., Perrino, R., Piotrzkowski, K., Polakovic, T., Ploskon, M., Posik, M., Prasad, S., Preghenella, R., Priens, S., Prifti, E., Przybycien, M., Pujahari, P., Quintero, A., Radici, M., Radhakrishnan, S. K., Rahman, S., Rathi, S., Raue, B., Reed, R., Reimer, P., Reinhold, J., Renner, E., Rignanese, L., Ripani, M., Rizzo, A., Romanov, D., Roy, A., Rubini, N., Ruspa, M., Ruan, L., Sabatie, F., Sadhukhan, S., Sahoo, N., Sahu, P., Samuel, D., Sarkar, A., Sarsour, M., Schmidke, W., Schmookler, B., Schwarz, C., Schwiening, J., Scott, M., Sedgwick, I., Segreti, M., Sekula, S., Seto, R., Shah, N., Shahinyan, A., Sharma, D., Sharma, N., Sichtermann, E. P., Signori, A., Singh, A., Singh, B. K., Singh, S. N., Smirnov, N., Sokhan, D., Soltz, R., Sondheim, W., Spinali, S., Stacchi, F., Staszewski, R., Stepanov, P., Strazzi, S., Stroe, I. R., Sun, X., Surrow, B., Sweger, Z., Symons, T. J., Tadevosyan, V., Tang, A., Tassi, E., Teodorescu, L., Tessarotto, F., Thomas, D., Thomas, J. H., Toll, T., Tomasek, L., Torales-Acosta, F., Tribedy, P., Triloki, Tripathi, V., Trotta, R., Trzebiński, M., Trzeciak, B. A., Tsai, O., Tu, Z., Turrisi, R., Tuve, C., Ullrich, T., Urciuoli, G. M., Valentini, A., Vallarino, S., Vandenbroucke, M., Vanek, J., Vino, G., Volpe, G., Voskanyan, H., Vossen, A., Voutier, E., Wang, G., Wang, Y., Watts, D., Wickramaarachchi, N., Wilson, F., Wong, C. -P., Wu, X., Wu, Y., Xie, J., Xu, Q. -H., Xu, Z., Xu, Z. W., Yang, C., Yang, Q., Yang, Y., Ye, Z., Yi, L., Yin, Z., Yurov, M., Zachariou, N., Zhang, J., Zhang, Y., Zhang, Z., Zhao, Y., Zhao, Y. X., Zhao, Z., Zheng, L., and Zurek, M.
Subjects: Physics - Instrumentation and Detectors, High Energy Physics - Experiment, Nuclear Experiment
Abstract: ATHENA has been designed as a general purpose detector capable of delivering the full scientific scope of the Electron-Ion Collider. Careful technology choices provide fine tracking and momentum resolution, high performance electromagnetic and hadronic calorimetry, hadron identification over a wide kinematic range, and near-complete hermeticity. This article describes the detector design and its expected performance in the most relevant physics channels. It includes an evaluation of detector technology choices, the technical challenges to realizing the detector and the R&D required to meet those challenges.
Published: 2022

6. The Second Catalog of Interplanetary Network Localizations of Konus Short Duration Gamma-Ray Bursts

Author: Svinkin, D., Hurley, K., Ridnaia, A., Lysenko, A., Frederiks, D., Golenetskii, S., Tsvetkova, A., Ulanov, M., Kokomov, A., Cline, T. L., Mitrofanov, I., Golovin, D., Kozyrev, A., Litvak, M., Sanin, A., Goldstein, A., Briggs, M. S., Wilson-Hodge, C., Burns, E., von Kienlin, A., Zhang, X. -L., Rau, A., Savchenko, V., Bozzo, E., Ferrigno, C., Barthelmy, S., Cummings, J., Krimm, H., Palmer, D. M., Tohuvavohu, A., Yamaoka, K., Ohno, M., Fukazawa, Y., Hanabata, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Boynton, W., Fellows, C. W., Harshman, K. P., Enos, H., Starr, R., Goldsten, J., Gold, R., Ursi, A., Tavani, M., Bulgarelli, A., Casentini, C., Del Monte, E., Evangelista, Y., Galli, M., Longo, F., Marisaldi, M., Parmiggiani, N., Pittori, C., Romani, M., Verrecchia, F., Smith, D. M., Hajdas, W., Xiao, S., Cai, C., Yi, Q. B., Zhang, Y. Q., Xiong, S. L., Li, X. B., Huang, Y., Li, C. K., Zhang, S. N., Song, L. M., Liu, C. Z., Li, X. Q., Peng, W. X., and Martinez-Castellanos, I.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the catalog of Interplanetary Network (IPN) localizations for 199 short-duration gamma-ray bursts (sGRBs) detected by the Konus-Wind (KW) experiment between 2011 January 1 and 2021 August 31, which extends the initial sample of IPN localized KW sGRBs (arXiv:1301.3740) to 495 events. We present the most comprehensive IPN localization data on these events, including probability sky maps in HEALPix format., Comment: Published in ApJS
Published: 2022
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7. The Gamow Explorer: A gamma-ray burst observatory to study the high redshift universe and enable multi-messenger astrophysics

Author: White, N. E., Bauer, F. E., Baumgartner, W., Bautz, M., Berger, E., Cenko, S. B., Chang, T. -C., Falcone, A., Fausey, H., Feldman, C., Fox, D., Fox, O., Fruchter, A., Fryer, C., Ghirlanda, G., Gorski, K., Grant, K., Guiriec, S., Hart, M., Hartmann, D., Hennawi, J., Kann, D. A., Kaplan, D., Kennea, A., Kocevski, D., Kouveliotou, C., Lawrence, C., Levan, A. J., Lidz, A., Lien, A., Littenberg, T. B., Mas-Ribas, L., Moss, M., O'Brien, P., O'Meara, J., Palmer, D. M., Pasham, D., Racusin, J., Remillard, R., Roberts, O. J., Roming, P., Rud, M., Salvaterra, R., Sambruna, R., Seiffert, M., Sun, G., Tanvir, N. R., Terrile, R., Thomas, N., van der Horst, A., Verstrand, W. T., Willems, P., Wilson-Hodge, C., Young, E. T., Amati, L., Bozzo, E., Karczewski, O. Ł., Hernandez-Monteagudo, C., Lopez, R. Rebolo, Genova-Santos, R., Rubino-Martin, J. A., Granot, J., Bemiamini, P., Gill, R., and Burns, E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Gamow Explorer will use Gamma Ray Bursts (GRBs) to: 1) probe the high redshift universe (z > 6) when the first stars were born, galaxies formed and Hydrogen was reionized; and 2) enable multi-messenger astrophysics by rapidly identifying Electro-Magnetic (IR/Optical/X-ray) counterparts to Gravitational Wave (GW) events. GRBs have been detected out to z ~ 9 and their afterglows are a bright beacon lasting a few days that can be used to observe the spectral fingerprints of the host galaxy and intergalactic medium to map the period of reionization and early metal enrichment. Gamow Explorer is optimized to quickly identify high-z events to trigger follow-up observations with JWST and large ground-based telescopes. A wide field of view Lobster Eye X-ray Telescope (LEXT) will search for GRBs and locate them with arc-minute precision. When a GRB is detected, the rapidly slewing spacecraft will point the 5 photometric channel Photo-z Infra-Red Telescope (PIRT) to identify high redshift (z > 6) long GRBs within 100s and send an alert within 1000s of the GRB trigger. An L2 orbit provides > 95% observing efficiency with pointing optimized for follow up by the James Webb Space Telescope (JWST) and ground observatories. The predicted Gamow Explorer high-z rate is >10 times that of the Neil Gehrels Swift Observatory. The instrument and mission capabilities also enable rapid identification of short GRBs and their afterglows associated with GW events. The Gamow Explorer will be proposed to the 2021 NASA MIDEX call and if approved, launched in 2028., Comment: 14 pages, 8 Figures
Published: 2021
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8. Swift/UVOT follow-up of Gravitational Wave Alerts in the O3 era

Author: Oates, S. R., Marshall, F. E., Breeveld, A. A., Kuin, N. P. M., Brown, P. J., De Pasquale, M., Evans, P. A., Fenney, A. J., Gronwall, C., Kennea, J. A., Klingler, N. J., Page, M. J., Siegel, M. H., Tohuvavohu, A., Ambrosi, E., Barthelmy, S. D., Beardmore, A. P., Bernardini, M. G., Campana, S., Caputo, R., Cenko, S. B., Cusumano, G., D'Aì, A., D'Avanzo, P., D'Elia, V., Giommi, P., Hartmann, D. H., Krimm, H. A., Laha, S., Malesani, D. B., Melandri, A., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Page, K. L., Palmer, D. M., Perri, M., Racusin, J. L., Sakamoto, T., Sbarufatti, B., Schlieder, J. E., Tagliaferri, G., and Troja, E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In this paper, we report on the observational performance of the Swift Ultra-violet/Optical Telescope (UVOT) in response to the Gravitational Wave alerts announced by the Advanced Laser Interferometer Gravitational Wave Observatory and the Advanced Virgo detector during the O3 period. We provide the observational strategy for follow-up of GW alerts and provide an overview of the processing and analysis of candidate optical/UV sources. For the O3 period, we also provide a statistical overview and report on serendipitous sources discovered by Swift/UVOT. Swift followed 18 gravitational-wave candidate alerts, with UVOT observing a total of 424 deg^2. We found 27 sources that changed in magnitude at the 3 sigma level compared with archival u or g-band catalogued values. Swift/UVOT also followed up a further 13 sources reported by other facilities during the O3 period. Using catalogue information, we divided these 40 sources into five initial classifications: 11 candidate active galactic nuclei (AGN)/quasars, 3 Cataclysmic Variables (CVs), 9 supernovae, 11 unidentified sources that had archival photometry and 6 uncatalogued sources for which no archival photometry was available. We have no strong evidence to identify any of these transients as counterparts to the GW events. The 17 unclassified sources are likely a mix of AGN and a class of fast-evolving transient, and one source may be a CV., Comment: 25 pages, 6 figures and 5 tables. Submitted to MNRAS. Supplementary contains 23 pages with 8 figures and 1 table
Published: 2021
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9. A bright gamma-ray flare interpreted as a giant magnetar flare in NGC 253

Author: Svinkin, D., Frederiks, D., Hurley, K., Aptekar, R., Golenetskii, S., Lysenko, A., Ridnaia, A. V., Tsvetkova, A., Ulanov, M., Cline, T. L., Mitrofanov, I., Golovin, D., Kozyrev, A., Litvak, M., Sanin, A., Goldstein, A., Briggs, M. S., Wilson-Hodge, C., von Kienlin, A., Zhang, X. -L., Rau, A., Savchenko, V., Bozzo, E., Ferrigno, C., Ubertini, P., Bazzano, A., Rodi, J. C., Barthelmy, S., Cummings, J., Krimm, H., Palmer, D. M., Boynton, W., Fellows, C. W., Harshman, K. P., Enos, H., and Starr, R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Magnetars are young, highly magnetized neutron stars that produce extremely rare giant flares of gamma-rays, the most luminous astrophysical phenomena in our Galaxy. The detection of these flares from outside the Local Group of galaxies has been predicted, with just two candidates so far. Here we report on the extremely bright gamma-ray flare GRB 200415A of April 15, 2020, which we localize, using the Interplanetary Network, to a tiny (20 sq. arcmin) area on the celestial sphere, that overlaps the central region of the Sculptor galaxy at 3.5 Mpc from the Milky Way. From the Konus-Wind detections, we find a striking similarity between GRB 200415A and GRB 051103, the even more energetic flare that presumably originated from the M81/M82 group of galaxies at nearly the same distance (3.6 Mpc). Both bursts display a sharp, millisecond-scale, hard-spectrum initial pulse, followed by an approximately 0.2 s long steadily fading and softening tail. Apart from the huge initial pulses of magnetar giant flares, no astrophysical signal with this combination of temporal and spectral properties and implied energy has been reported previously. At the inferred distances, the energy released in both flares is on par with that of the December 27, 2004 superflare from the Galactic magnetar SGR 1806-20, but with a higher peak luminosity. Taken all together, this makes GRB 200415A and its twin GRB 051103 the most significant candidates for extragalactic magnetar giant flares, both a factor of five more luminous than the brightest Galactic magnetar flare observed previously, thus providing an important step towards a better understanding of this fascinating phenomenon., Comment: Preprint version of Nature paper
Published: 2021
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10. Swift Multiwavelength Follow-up of LVC S200224ca and the Implications for Binary Black Hole Mergers

Author: Klingler, N. J., Lien, A., Oates, S. R., Kennea, J. A., Evans, P. A., Tohuvavohu, A., Zhang, B., Page, K. L., Cenko, S. B., Barthelmy, S. D., Beardmore, A. P., Bernardini, M. G., Breeveld, A. A., Brown, P. J., Burrows, D. N., Campana, S., Cusumano, G., D'Aì, A., D'Avanzo, P., D'Elia, V., de Pasquale, M., Emery, S. W. K., Garcia, J., Giommi, P., Gronwall, C., Hartmann, D. H., Krimm, H. A., Kuin, N. P. M., Malesani, D. B., Marshall, F. E., Melandri, A., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Palmer, D. M., Page, M. J., Perri, M., Racusin, J. L., Sakamoto, T., Sbarufatti, B., Schlieder, J. E., Siegel, M. H., Tagliaferri, G., and Troja, E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: On 2020 February 24, during their third observing run ("O3"), the Laser Interferometer Gravitational-wave Observatory and Virgo Collaboration (LVC) detected S200224ca: a candidate gravitational wave (GW) event produced by a binary black hole (BBH) merger. This event was one of the best-localized compact binary coalescences detected in O3 (with 50%/90% error regions of 13/72 deg$^2$), and so the Neil Gehrels Swift Observatory performed rapid near-UV/X-ray follow-up observations. Swift-XRT and UVOT covered approximately 79.2% and 62.4% (respectively) of the GW error region, making S200224ca the BBH event most thoroughly followed-up in near-UV (u-band) and X-ray to date. No likely EM counterparts to the GW event were found by the Swift BAT, XRT, or UVOT, nor by other observatories. Here we report on the results of our searches for an EM counterpart, both in the BAT data near the time of the merger, and in follow-up UVOT/XRT observations. We also discuss the upper limits we can place on EM radiation from S200224ca, and the implications these limits have on the physics of BBH mergers. Namely, we place a shallow upper limit on the dimensionless BH charge, $\hat{q} < 1.4 \times10^{-4}$, and an upper limit on the isotropic-equivalent energy of a blast wave $E < 4.1\times10^{51}$ erg (assuming typical GRB parameters)., Comment: 14 pages, 6 figures, accepted for publication in ApJ
Published: 2020
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11. Gemini Planet Imager Spectroscopy of the Dusty Substellar Companion HD 206893 B

Author: Ward-Duong, K., Patience, J., Follette, K., De Rosa, R. J., Rameau, J., Marley, M., Saumon, D., Nielsen, E. L., Rajan, A., Greenbaum, A. Z., Lee, J., Wang, J. J., Czekala, I., Duchêne, G., Macintosh, B., Ammons, S. Mark, Bailey, V. P., Barman, T., Bulger, J., Chen, C., Chilcote, J., Cotten, T., Doyon, R., Esposito, T. M., Fitzgerald, M. P., Gerard, B. L., Goodsell, S. J., Graham, J. R., Hibon, P., Hom, J., Hung, L. -W., Ingraham, P., Kalas, P., Konopacky, Q., Larkin, J. E., Maire, J., Marchis, F., Marois, C., Metchev, S., Millar-Blanchaer, M. A., Oppenheimer, R., Palmer, D., Perrin, M., Poyneer, L., Pueyo, L., Rantakyrö, F. T., Ren, B., Ruffio, J. -B., Savransky, D., Schneider, A. C., Sivaramakrishnan, A., Song, I., Soummer, R., Tallis, M., Thomas, S., Wallace, J. Kent, Wiktorowicz, S., and Wolff, S.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present new near-infrared Gemini Planet Imager (GPI) spectroscopy of HD 206893 B, a substellar companion orbiting within the debris disk of its F5V star. The $J$, $H$, $K1$, and $K2$ spectra from GPI demonstrate the extraordinarily red colors of the object, confirming it as the reddest substellar object observed to date. The significant flux increase throughout the infrared presents a challenging atmosphere to model with existing grids. Best-fit values vary from 1200 K to 1800 K for effective temperature and from 3.0 to 5.0 for log($g$), depending on which individual wavelength band is fit and which model suite is applied. The extreme redness of the companion can be partially reconciled by invoking a high-altitude layer of sub-micron dust particles, similar to dereddening approaches applied to the peculiar red field L-dwarf population. However, reconciling the HD 206893 B spectra with even those of the reddest low-gravity L-dwarf spectra still requires the contribution of additional atmospheric dust, potentially due to the debris disk environment in which the companion resides. Orbit fitting from four years of astrometric monitoring is consistent with a $\sim$30-year period, orbital inclination of 147$^{\circ}$, and semimajor axis of 10 au, well within the estimated disk inner radius of $\sim$50 au. As one of very few substellar companions imaged interior to a circumstellar disk, the properties of this system offer important dynamical constraints on companion-disk interaction and provide a benchmark for substellar and planetary atmospheric study., Comment: Accepted for publication in AJ (October 15, 2020). 35 pages, 20 figures, with tables and appendices presented in their entirety
Published: 2020
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12. Swift-XRT follow-up of gravitational wave triggers during the third aLIGO/Virgo observing run

Author: Page, K. L., Evans, P. A., Tohuvavohu, A., Kennea, J. A., Klingler, N. J., Cenko, S. B., Oates, S. R., Ambrosi, E., Barthelmy, S. D., Beardmore, A. P., Bernardini, M. G., Breeveld, A. A., Brown, P. J., Burrows, D. N., Campana, S., Caputo, R., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V., De Pasquale, M., Emery, S. W. K., Giommi, P., Gronwall, C., Hartmann, D. H., Krimm, H. A., Kuin, N. P. M., Malesani, D. B., Marshall, F. E., Melandri, A., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Page, M. J., Palmer, D. M., Perri, M., Racusin, J. L., Sakamoto, T., Sbarufatti, B., Schlieder, J. E., Siegel, M. H., Tagliaferri, G., and Troja, E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Neil Gehrels Swift Observatory followed up 18 gravitational wave (GW) triggers from the LIGO/Virgo collaboration during the O3 observing run in 2019/2020, performing approximately 6500 pointings in total. Of these events, four were finally classified (if real) as binary black hole (BH) triggers, six as binary neutron star (NS) events, two each of NSBH and Mass Gap triggers, one an unmodelled (Burst) trigger, and the remaining three were subsequently retracted. Thus far, four of these O3 triggers have been formally confirmed as real gravitational wave events. While no likely electromagnetic counterparts to any of these GW events have been identified in the X-ray data (to an average upper limit of 3.60 x 10^{-12} erg cm^{-2} s^{-1} over 0.3-10 keV), or at other wavelengths, we present a summary of all the Swift-XRT observations performed during O3, together with typical upper limits for each trigger observed. The majority of X-ray sources detected during O3 were previously uncatalogued; while some of these will be new (transient) sources, others are simply too faint to have been detected by earlier survey missions such as ROSAT. The all-sky survey currently being performed by eROSITA will be a very useful comparison for future observing runs, reducing the number of apparent candidate X-ray counterparts by up to 95 per cent., Comment: 23 pages (including 4 pages of references, and a 4 page table in the appendix), 5 figures (4 in colour), accepted for publication in MNRAS. (Replaced due to annoying spelling typo in the abstract.)
Published: 2020
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13. Beyond the symptoms: Personalizing giant cell arteritis care through multidimensional patient reported outcome measure

Author: El Miedany, Y, El Gaafary, M, Toth, M, Palmer, D, Ali, Ayman, Bahlas, S, Mahran, S, Hassan, W, Abu-zaid, MH, Saber, S, and Elwakil, W.
Published: 2023
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14. Imaging the 44 AU Kuiper Belt-analogue debris ring around HD 141569A with GPI polarimetry

Author: Bruzzone, J. S., Metchev, S., Duchene, G., Millar-Blanchaer, M. A., Dong, R., Wang, J. J., Graham, J. R., Mazoyer, J., Wolff, S., Ammons, S. M., Schneider, A. C., Greenbaum, A. Z., Matthews, B. C., Arriaga, P., Bailey, V. P., Barman, T., Bulger, J., Chilcote, J., Cotten, T., De Rosa, R. J., Doyon, R., Fitzgerald, M. P., Follette, K. B., Gerard, B. L., Goodsell, S. J., Hibon, P., Hom, J., Hung, L. -W., Ingraham, P., Kalas, P., Konopacky, Q., Larkin, J. E., Macintosh, B., Maire, J., Marchis, F., Marois, C., Morzinski, K. M., Nielsen, E. L., Oppenheimer, R., Palmer, D., Patel, R., Patience, J., Perrin, M., Poyneer, L., Pueyo, L., Rajan, A., Rameau, J., Rantakyro, F. T., Savransky, D., Sivaramakrishnan, A., Song, I., Soummer, R., Thomas, S., Wallace, J. K., Ward-Duong, K., and Wiktorowicz, S.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first polarimetric detection of the inner disk component around the pre-main sequence B9.5 star HD 141569A. Gemini Planet Imager H-band (1.65 micron) polarimetric differential imaging reveals the highest signal-to-noise ratio detection of this ring yet attained and traces structure inwards to 0.25" (28 AU at a distance of 111 pc). The radial polarized intensity image shows the east side of the disk, peaking in intensity at 0.40" (44 AU) and extending out to 0.9" (100 AU). There is a spiral arm-like enhancement to the south, reminiscent of the known spiral structures on the outer rings of the disk. The location of the spiral arm is coincident with 12CO J=3-2 emission detected by ALMA, and hints at a dynamically active inner circumstellar region. Our observations also show a portion of the middle dusty ring at ~220 AU known from previous observations of this system. We fit the polarized H-band emission with a continuum radiative transfer Mie model. Our best-fit model favors an optically thin disk with a minimum dust grain size close to the blow-out size for this system: evidence of on-going dust production in the inner reaches of the disk. The thermal emission from this model accounts for virtually all of the far-infrared and millimeter flux from the entire HD 141569A disk, in agreement with the lack of ALMA continuum and CO emission beyond ~100 AU. A remaining 8-30 micron thermal excess a factor of ~2 above our model argues for a yet-unresolved warm innermost 5-15 AU component of the disk., Comment: 16 pages, 8 figures, accepted at AJ
Published: 2019
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15. Swift-XRT Follow-up of Gravitational Wave Triggers in the Second Advanced LIGO/Virgo Observing Run

Author: Klingler, N. J., Kennea, J. A., Evans, P. A., Tohuvavohu, A., Cenko, S. B., Barthelmy, S. D., Beardmore, A. P., Breeveld, A. A., Brown, P. J., Burrows, D. N., Campana, S., Cusumano, G., D'Aì, A., D'Avanzo, P., D'Elia, V., de Pasquale, M., Emery, S. W. K., Garcia, J., Giommi, P., Gronwall, C., Hartmann, D. H., Krimm, H. A., Kuin, N. P. M., Lien, A., Malesani, D. B., Marshall, F. E., Melandri, A., Nousek, J. A., Oates, S. R., O'Brien, P. T., Osborne, J. P., Page, K. L., Palmer, D. M., Perri, M., Racusin, J. L., Siegel, M. H., Sakamoto, T., Sbarufatti, B., Tagliaferri, G., and Troja, E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Neil Gehrels Swift Observatory carried out prompt searches for gravitational wave (GW) events detected by the LIGO/Virgo Collaboration (LVC) during the second observing run ("O2"). Swift performed extensive tiling of eight LVC triggers, two of which had very low false-alarm rates (GW 170814 and the epochal GW 170817), indicating a high confidence of being astrophysical in origin; the latter was the first GW event to have an electromagnetic counterpart detected. In this paper we describe the follow-up performed during O2 and the results of our searches. No GW electromagnetic counterparts were detected; this result is expected, as GW 170817 remained the only astrophysical event containing at least one neutron star after LVC's later retraction of some events. A number of X-ray sources were detected, with the majority of identified sources being active galactic nuclei. We discuss the detection rate of transient X-ray sources and their implications in the O2 tiling searches. Finally, we describe the lessons learned during O2, and how these are being used to improve the \swift\ follow-up of GW events. In particular, we simulate a population of GRB afterglows to evaluate our source ranking system's ability to differentiate them from unrelated and uncatalogued X-ray sources. We find that $\approx$60-70% of afterglows whose jets are oriented towards Earth will be given high rank (i.e., "interesting" designation) by the completion of our second follow-up phase (assuming their location in the sky was observed), but that this fraction can be increased to nearly 100% by performing a third follow-up observation of sources exhibiting fading behavior., Comment: 18 pages, 4 figures, 2 tables, accepted for publication in ApJS
Published: 2019
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16. SN 2016coi (ASASSN-16fp): an energetic H-stripped core-collapse supernova from a massive stellar progenitor with large mass loss

Author: Terreran, G., Margutti, R., Bersier, D., Brimacombe, J., Caprioli, D., Challis, P., Chornock, R., Coppejans, D. L., Dong, Subo, Guidorzi, C., Hurley, K., Kirshner, R., Migliori, G., Milisavljevic, D., Palmer, D. M., Prieto, J. L., Tomasella, L., Marchant, P., Pastorello, A., Shappee, B. J., Stanek, K. Z., Stritzinger, M. D., Benetti, S., Demarchi, L., Elias-rosa, N., Gall, C., Harmanen, J., and Mattila, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present comprehensive observations and analysis of the energetic H-stripped SN 2016coi (a.k.a. ASASSN-16fp), spanning the $\gamma$-ray through optical and radio wavelengths, acquired within the first hours to $\sim$420 days post explosion. Our campaign confirms the identification of He in the SN ejecta, which we interpret to be caused by a larger mixing of Ni into the outer ejecta layers. From the modeling of the broad bolometric light curve we derive a large ejecta mass to kinetic energy ratio ($M_{\rm{ej}}\sim 4-7\,\rm{M_{\odot}}$, $E_{\rm{k}}\sim 7-8\times 10^{51}\,\rm{erg}$). The small [\ion{Ca}{ii}] \lam\lam7291,7324 to [\ion{O}{i}] \lam\lam6300,6364 ratio ($\sim$0.2) observed in our late-time optical spectra is suggestive of a large progenitor core mass at the time of collapse. We find that SN 2016coi is a luminous source of X-rays ($L_{X}>10^{39}\,\rm{erg\,s^{-1}}$ in the first $\sim100$ days post explosion) and radio emission ($L_{8.5\,GHz}\sim7\times 10^{27}\,\rm{erg\,s^{-1}Hz^{-1}}$ at peak). These values are in line with those of relativistic SNe (2009bb, 2012ap). However, for SN 2016coi we infer substantial pre-explosion progenitor mass-loss with rate $\dot M \sim (1-2)\times 10^{-4}\,\rm{M_{\odot}yr^{-1}}$ and a sub-relativistic shock velocity $v_{sh}\sim0.15c$, in stark contrast with relativistic SNe and similar to normal SNe. Finally, we find no evidence for a SN-associated shock breakout $\gamma$-ray pulse with energy $E_{\gamma}>2\times 10^{46}\,\rm{erg}$. While we cannot exclude the presence of a companion in a binary system, taken together, our findings are consistent with a massive single star progenitor that experienced large mass loss in the years leading up to core-collapse, but was unable to achieve complete stripping of its outer layers before explosion., Comment: Submitted to ApJ. Main text: 21 pages; Appendix: 15 pages; 12 figures
Published: 2019
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17. Risk of Bowel Obstruction in Patients Undergoing Neoadjuvant Chemotherapy for High-risk Colon Cancer: A Nested Case-control Matched Analysis of an International, Multi-centre, Randomised Controlled Trial (FOxTROT)

Author: Glasbey, James, Glasbey, James, Beggs, Andrew, Glimelius, Bengt, Gray, Richard, Handley, Kelly, Laurberg, Søren, Magill, Laura, Murakami, Keigo, Palmer, Andy, Quirke, Philip, Seligman, Jenny, Seymour, Matt, Sinha, Yash, West, Nick, Morton, Dion, Glasbey, James, Handley, Kelly, Palmer, Andy, Morton, Dion, Crosby, T., Olliff, J., Peto (Chair), R., Brown, Gina, Ferry, David, Glimelius, Bengt, Gray, Richard, Handley, Kelly, Ismail, Tariq, Laurberg, Søren, Magill, Laura, Morton, Dion, Oliver, Alf, Quirke, Phil, Seymour, Matt, Scott, Nigel, Seligman, Jenny, Swift, Ian, Warren, Bryan, West, Nick, Northover, J., Parmar (Chair), M., Slevin, M., Magill, Laura, Gray, Richard, Handley, Kelly, Wilcockson, Adrian, Gray, Zoe, Lancaster, Dominic, Brown, James, Palmer, Andrew, Adie, Ladan, Kennedy, Georgia, Eld, M., Holt, G., Yilmaz, M., Spendler, K. Garm, Hansen, F., Laurberg, S., Rosenkilde, M., Ahlstrom, H., Glimelius, B., Abgamu, D., Day, N., Walsh, C., Bannister, J., Furniss, D., Morgan, S., Walkington, L., Yates, S., Branagan, G., Mustajab, A., O’Neil, H., Rees, C., Geh, I., Hendrickse, C., Langman, G., Pallan, A., Conn, A., Lowe, A., Ostrowski, J., Steward, M., Callaway, M., Falk, S., Thomas, M., Wong, N., Cast, J., Hartley, J., Roy, R., Tiam, R., Blunt, D., Cleator, S., Dawson, P., Goldin, R., Gujral, D., Lowdell, C., Ziprin, P., Clenton, S., Dewdney, A., Euinton, H., Furniss, D., Gupta, R., Tarapowewalla, D., Wilshaw, V., Braun, M., Chakrabarty, B., Hill, J., Laasch, H., Saunders, M., Cruickshank, N., Davies, M., Muzaffar, S., Orme, A., Punia, P., Rea, D., Campbell, F., Hughes, M., Palmer, D., Rooney, P., Abbott, G., Hamid, B., Vimalachandran, D., Berry, J., Hinson, F., Maarouf, Z., Nicoll, J., Adams, C., Denson, J., Jackson, S., Sherriff, D., Kweka, E., McAdam, G., Peters, M., Roy, R., Khaira, M., Kurien, G., Robinson, J., Wadsley, J., White, D., Young, R., Dega, R., Lamparelli, M., Orbell, J., Osborne, R., Taylor, P., Thomas, T., Gopalakrishnan, K., Jadhav, V., Scott-Brown, M., Baijal, S., Chapman, M., Glaholm, J., Nelson, C., Singh, R., Harrison, J., Last, K., Scott, D., Scullion, D., Lind, P., Milosavljevic, Z., Dent, J., Ilsley, D., Littleford, S., Roberts, C., Crabtree, M., Orrell, J., Sherwin, E., Smith, S., Soomal, R., Braun, M., De, A., Khan, A., Khan, U., Lavin, V., McBain, C., Radharkrishna, G., Sil, R., Weerasinghe, S., Hill, J., Lee, S., Wright, P., Church, R., Holland, C., Kunene, V., Thompson, A., Glynne-Jones, R., Goh, V., Livingstone, J., Richman, P., Barlow, C., Burn, P., Geraghty, J., Walther, J., Grumett, S., Mangalika, S., Qaiyum, M., Williams, G., Borgstein, R., Bridgewater, J., Melville, D., Rees, J., Coxon, F., Hainsworth, P., Needham, S., Scott, J., Asmussen, J., Hansen, T., Jensen, K., Pfeiffer, P., Alkhaldi, A., Brittenden, J., Jackson, A., Kamposioras, K., Kumaran, G., Macklin, C., Alexander, J., Harle, A., Hickish, T., Talbot, R., Tarver, D., Bridgewater, J., Partridge, W., Sundaresan, V., Vivekanandan, S., Agrawal, N., Higginson, A., Muthuramalingam, S., O’Leary, D., Devarajan, G., Gulati, M., Kerwat, R., Maisey, N., Mikhaeel, G., Ismail, T., Middleton, G., Page, A., Steven, N., Taniere, P., Gutmann, J., Huang, J., Raouf, S., Dunn, W., Escola, C. Lopez, Potter, V., Scholefield, J., Walker, G., Zaitoun, A., Eason, D., McPhail, N., Mmeka, W., Stenhouse, G., Watson, A., Fozard, B., Hickish, T., Snape, S., Ellis, R., Faux, W., Jenkins, R., Maskell, G., Kulkarni, R., Lund, J., Menon, S., Singh, R., Chandler, I., Daniels, I., Harries, S., Osborne, M., Bell, J., Krell, D., Mayer, A., Ogunbiyi, O., Watkins, J., Bronder, C., Eaton, D., Taylor, A., Brown, G., Cunningham, D., Tekkis, P., Wotherspoon, A., Dobson, M., Mitchell, P., Pitt, M., Scott, N., Susnerwala, S., Adab, F., Britton, I., Ghiridaran, S., Howitt, C., Kirby, R., Biddlestone, L., Dalton, S., De Winton, E., Phillips, A., Ferry, D., Grumett, S., Kawesha, A., Maleki, K., Momtahan, N., Burnett, H., Hayes, S., Soop, M., Branagan, G., Cook, I., Cook, S., Iveson, T., Shablak, A., Coup, A., Hamid, A., Moore, P., O’Toole, L., Pai, D., Bateman, A., Bateman, A., Blaquiere, R., Nichols, P., Chappell, M., Dworkin, M., Jain, S., Tsang, D., Hopkins, K., Loveday, E., Lyons, A., Rooney, N., Ali, N., Chatterjee, M., Chiphang, A., Dundas, S., Myint, A. Sun, Zeiderman, M., Beharry, N., Chong, H., Lofts, F., Melville, D., Finan, P., Seymour, M., Tolan, D., West, N., Anyamene, N., Burling, D., Kennedy, R., Moorghen, M., Agrawal, S., Hasan, J., Mehta, S., Saeed, M., Burgess, P., John, L., Lowndes, S., Planner, A., Campbell, F., Hughes, M., Rooney, P., Smith, D., Hochhauser, D., Obichere, A., Rodriguez-Justo, M., Shiu, K., Taylor, S., Correa, P., James, S., Shatwell, W., Williams, N., Brady, J., Lanaspre, E., Mikhaeel, G., Ahmad, M., Gill, T., Wilson, D., Adams, R., Beehen, R., Morgan, M., Lindh, B., Adams, R., Morgan, M., Ford, A., Gopal, K., Pranesh, N., Shareef, D., Tighe, M., Busby, K., Correa, P., Sanders, S., Sinha, R., Ahmad, R., Desai, S., Ramesh, S., Hilman, S., Lott, M., O’Brien, J., Radstone, D., West, D., Amin, S., Hampton, J., Hornbuckle, J., Kitsanta, P., Ali, M., Desai, A., Hadaki, M., Hall, M., Arul, D., Hochhauser, D., Leonard, P., Mukhtar, H., Murray, D., Baxter, A., Churn, M., Farrugia, D., Lake, S., Smith, G., Bansal, A., Chandran, P., Corr, C., Gollins, S., Davenport, A., Saunders, M., Sukumar, S., Bathurst, N., Beaumont, E., Cooper, E., Francis, N., Sephton, M., Sparrow, G., Clarke, A., Haselden, J., Last, K., Woodcock, N., Atkinson, M., Gollins, S., Gupta, M., Maw, A., Abdullah, N., Bale, C., and Lord, M.
Published: 2023
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18. Searching for the most powerful thermonuclear X-ray bursts with the Neil Gehrels Swift Observatory

Author: Zand, J. J. M. in 't, Kries, M. J. W., Palmer, D. M., and Degenaar, N.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We searched for thermonuclear X-ray bursts from Galactic neutron stars in all event mode data of the Neil Gehrels Swift Observatory collected until March 31, 2018. In particular, we are interested in the intermediate-duration bursts (shell flashes fueled by thick helium piles) with the ill-understood phenomenon of strong flux fluctuations. Nine such bursts have been discussed in the literature to date. Swift is particularly suitable for finding additional examples. We find and list a total of 134 X-ray bursts; 44 are detected with BAT only, 41 with XRT only, and 49 with both. Twenty-eight bursts involve automatic slews. We find 12 intermediate-duration bursts, all detected in observations involving automatic slews. Five show remarkably long Eddington-limited phases in excess of 200 s. Five show fluctuations during the decay phase; four of which are first discussed in the present study. We discuss the general properties of the fluctuations, considering also 7 literature cases. In general two types of fluctuations are observed: fast ones, with a typical timescale of 1 s and up and downward fluctuations of up to 70%, and slow ones, with a typical timescale of 1 min and only downward fluctuations of up to 90%. The latter look like partial eclipses because the burst decay remains visible in the residual emission. We revisit the interpretation of this phenomenon in the context of the new data set and find that it has not changed fundamentally despite the expanded data set. It is thought to be due to a disturbance of the accretion disk by outflowing matter and photons, causing obscuration and reflection due to Thompson scattering in an orbiting highly ionized cloud or structure above or below the disk. We discuss in detail the most pronounced burster SAX J1712.6-3739. One of the bursts from this source is unusual in that it lasts longer than 5600 s, but does not appear to be a superburst., Comment: Accepted for publication in Astronomy & Astrophysics, 29 pages, 12 figures. Version 2 has 3 bursts from IGR J17480-2446 re-identified to 2 from Swift J174805.3-244637 and 1 from EXO 1745-248
Published: 2018
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19. 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, S., Siegel, M. H., Sakamoto, T., Sbarufatti, B., Tagliaferri, G., Tanvir, N. R., and Tohuvavohu, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
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 (NuSTAR) of the EM counterpart of the binary neutron star merger GW170817. The bright, rapidly fading ultraviolet emission indicates a high mass ($\approx0.03$ solar masses) wind-driven outflow with moderate electron fraction ($Y_{e}\approx0.27$). Combined with the X-ray limits, we favor an observer viewing angle of $\approx 30^{\circ}$ away from the orbital rotation axis, which avoids both obscuration from the heaviest elements in the orbital plane and a direct view of any ultra-relativistic, highly collimated ejecta (a gamma-ray burst afterglow)., Comment: Science, in press; 56 pages, 12 figures
Published: 2017
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20. The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au

Author: Nielsen, EL, De Rosa, RJ, Macintosh, B, Wang, JJ, Ruffio, JB, Chiang, E, Marley, MS, Saumon, D, Savransky, D, Mark Ammons, S, Bailey, VP, Barman, T, Blain, C, Bulger, J, Burrows, A, Chilcote, J, Cotten, T, Czekala, I, Doyon, R, Duchene, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, BL, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hibon, P, Hinkley, S, Hirsch, LA, Hom, J, Hung, LW, Ilene Dawson, R, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Lee, EJ, Lin, JW, Maire, J, Marchis, F, Marois, C, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Pueyo, L, Rafikov, RR, Rajan, A, Rameau, J, Rantakyrö, FT, Ren, B, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Tallis, M, Thomas, S, Ward-Duong, K, and Wolff, S
Subjects: instrumentation: adaptive optics, planetary systems, planets and satellites: detection, astro-ph.EP, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey. This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semimajor axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M ∗ >1.5 M o more likely to host planets with masses between 2 and 13M Jup and semimajor axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semimajor axis (a) for planet populations around high-mass stars (M ∗ >1.5 M o) of the form , finding α = -2.4 +0.8 and β = -2.0 +0.5, and an integrated occurrence rate of % between 5-13M Jup and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with % of stars hosting a brown dwarf companion between 13-80M Jup and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semimajor axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semimajor axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the radial velocity method, our results are consistent with a peak in occurrence of giant planets between ∼1 and 10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability.
Published: 2019

21. Direct Imaging of the HD 35841 Debris Disk: A Polarized Dust Ring from Gemini Planet Imager and an Outer Halo from HST/STIS

Author: Esposito, TM, Duchne, G, Kalas, P, Rice, M, Choquet, I, Ren, B, Perrin, MD, Chen, CH, Arriaga, P, Chiang, E, Nielsen, EL, Graham, JR, Wang, JJ, Rosa, RJD, Follette, KB, Ammons, SM, Ansdell, M, Bailey, VP, Barman, T, Bruzzone, JS, Bulger, J, Chilcote, J, Cotten, T, Doyon, R, Fitzgerald, MP, Goodsell, SJ, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Konopacky, Q, Larkin, JE, Macintosh, B, Maire, J, Marchis, F, Marois, C, Mazoyer, J, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, D, Patience, J, Poyneer, L, Pueyo, L, Rajan, A, Rameau, J, Rantakyrö, FT, Ryan, D, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
Subjects: circumstellar matter, infrared: planetary systems, stars: individual, techniques: high angular resolution, astro-ph.EP, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present new high resolution imaging of a light-scattering dust ring and halo around the young star HD 35841. Using spectroscopic and polarimetric data from the Gemini Planet Imager in H-band (1.6 μm), we detect the highly inclined (i = 85°) ring of debris down to a projected separation of ∼12 au (∼0.″12) for the first time. Optical imaging from HST/STIS shows a smooth dust halo extending outward from the ring to >140 au (>1.″4). We measure the ring's scattering phase function and polarization fraction over scattering angles of 22°-125°, showing a preference for forward scattering and a polarization fraction that peaks at ∼30% near the ansae. Modeling of the scattered-light disk indicates that the ring spans radii of ∼60-220 au, has a vertical thickness similar to that of other resolved dust rings, and contains grains as small as 1.5 μm in diameter. These models also suggest the grains have a low porosity, are more likely to consist of carbon than astrosilicates, and contain significant water ice. The halo has a surface brightness profile consistent with that expected from grains pushed by radiation pressure from the main ring onto highly eccentric but still bound orbits. We also briefly investigate arrangements of a possible inner disk component implied by our spectral energy distribution models, and speculate about the limitations of Mie theory for doing detailed analyses of debris disk dust populations.
Published: 2018

22. GPI Spectra of HR 8799 c, d, and e from 1.5 to 2.4 μm with KLIP Forward Modeling

Author: Greenbaum, AZ, Pueyo, L, Ruffio, JB, Wang, JJ, Rosa, RJD, Aguilar, J, Rameau, J, Barman, T, Marois, C, Marley, MS, Konopacky, Q, Rajan, A, Macintosh, B, Ansdell, M, Arriaga, P, Bailey, VP, Bulger, J, Burrows, AS, Chilcote, J, Cotten, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Gerard, B, Goodsell, SJ, Graham, JR, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Larkin, JE, Maire, J, Marchis, F, Metchev, S, Millar-Blanchaer, MA, Nielsen, EL, Norton, A, Oppenheimer, R, Palmer, D, Patience, J, Perrin, MD, Poyneer, L, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
Subjects: planets and satellites: gaseous planets, stars: individual, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We explore KLIP forward modeling spectral extraction on Gemini Planet Imager coronagraphic data of HR 8799, using PyKLIP, and show algorithm stability with varying KLIP parameters. We report new and re-reduced spectrophotometry of HR 8799 c, d, and e in the H and K bands. We discuss a strategy for choosing optimal KLIP PSF subtraction parameters by injecting simulated sources and recovering them over a range of parameters. The K1/K2 spectra for HR 8799 c and d are similar to previously published results from the same data set. We also present a K-band spectrum of HR 8799 e for the first time and show that our H-band spectra agree well with previously published spectra from the VLT/SPHERE instrument. We show that HR 8799 c and d show significant differences in their H and K spectra, but do not find any conclusive differences between d and e, nor between c and e, likely due to large error bars in the recovered spectrum of e. Compared to M-, L-, and T-type field brown dwarfs, all three planets are most consistent with mid- and late-L spectral types. All objects are consistent with low gravity, but a lack of standard spectra for low gravity limit the ability to fit the best spectral type. We discuss how dedicated modeling efforts can better fit HR 8799 planets' near-IR flux, as well as how differences between the properties of these planets can be further explored.
Published: 2018

23. Evidence for the magnetar nature of 1E 161348-5055 in RCW 103

Author: D'Aì, A., Evans, P. A., Burrows, D. N., Kuin, N. P. M., Kann, D. A., Campana, S., Maselli, A., Romano, P., Cusumano, G., La Parola, V., Barthelmy, S. D., Beardmore, A. P., Cenko, S. B., De Pasquale, M., Gehrels, N., Greiner, J., Kennea, J. A., Klose, S., Melandri, A., Nousek, J. A., Osborne, J. P., Palmer, D. M., Sbarufatti, B., Schady, P., Siegel, M. H., Tagliaferri, G., Yates, R., and Zane, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the detection of a bright, short, structured X-ray burst coming from the supernova remnant RCW 103 on 2016 June 22 caught by the Swift/BAT monitor, and on the follow-up campaign made with Swift/XRT, Swift/UVOT and the optical/NIR GROND detector. The characteristics of this flash, such as duration, and spectral shape, are consistent with typical short bursts observed from soft gamma repeaters. The BAT error circle at 68 per cent confidence range encloses the point-like X-ray source at the centre of the nebula, 1E161348-5055. Its nature has been long debated due to a periodicity of 6.67 hr in X-rays, which could indicate either an extremely slow pulsating neutron star, or the orbital period of a very compact X-ray binary system. We found that 20 min before the BAT trigger, the soft X-ray emission of 1E161348-5055 was a factor of ~100 higher than measured 2 yr earlier, indicating that an outburst had already started. By comparing the spectral and timing characteristics of the source in the two years before the outburst and after the BAT event, we find that, besides a change in luminosity and spectral shape, also the 6.67 hr pulsed profile has significantly changed with a clear phase shift with respect to its low-flux profile. The UV/optical/NIR observations did not reveal any counterpart at the position of 1E161348-5055. Based on these findings, we associate the BAT burst with 1E161348-5055, we classify it as a magnetar, and pinpoint the 6.67 hr periodicity as the magnetar spin period., Comment: 12 pages, accepted for publication in MNRAS on 2016 August 08
Published: 2016
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24. Swift follow-up of gravitational wave triggers: results from the first aLIGO run and optimisation for the future

Author: Evans, P. A., Kennea, J. A., Palmer, D. M., Bilicki, M., Osborne, J. P., O'Brien, P. T., Tanvir, N. R., Lien, A. Y., Barthelmy, S. D., Burrows, D. N., Campana, S., Cenko, S. B., D'Elia, V., Gehrels, N., Marshall, F. E., Page, K. L., Perri, M., Sbarufatti, B., Siegel, M. H., Tagliaferri, G., and Troja, E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: During its first observing run, in late 2015, the advanced LIGO facility announced 3 gravitational wave (GW) triggers to electromagnetic follow-up partners. Two of these have since been confirmed as being of astrophysical origin: both are binary black hole mergers at ~500 Mpc; the other trigger was later found not to be astrophysical. In this paper we report on the Swift follow up observations of the second and third triggers, including details of 21 X-ray sources detected; none of which can be associated with the GW event. We also consider the challenges that the next GW observing run will bring as the sensitivity and hence typical distance of GW events will increase. We discuss how to effectively use galaxy catalogues to prioritise areas for follow up, especially in the presence of distance estimates from the GW data. We also consider two galaxy catalogues and suggest that the high completeness at larger distances of the 2MASS Photometric Redshift Catalogue (2MPZ) makes it very well suited to optimise Swift follow-up observations., Comment: Modified 2018 December, to correct a normalisation error in equation (7). Corresponding erratum has been submitted to MNRAS
Published: 2016
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25. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., De Rosa, R., DeSalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., MacDonald, T., Machenschalk, B., MacInnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., McCarthy, R., McClelland, D. E., McCormick, S., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McWilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palliyaguru, N., Palomba, C., Pal-Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. -P., Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey-Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., McConnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Castro-Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. R., Hu, Y. -D., Kubánek, P., Guziy, S., Castellón, A., García-Cerezo, A., Muñoz, V. F., del Pulgar, C. Pérez, Castillo-Carrión, S., Cerón, J. M. Castro, Hudec, R., Caballero-García, M. D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Sanguino, T. de J. Mateo, Fernández-Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, Ch., Fan, Y., Wang, Ch., Hiriart, D., Lee, W. H., Claret, A., Sánchez-Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau-Graziati, L., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit-Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica-Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. -F., Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares-Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Zhang, B. -B., Hui, C. M., Jenke, P., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., von Kienlin, A., Kippen, R. M., McBreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. -F., Blackburn, L., Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez-Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., McEnery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. -L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Van Sistine, A., Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, D. K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra-Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston-Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., E., F. Olivares, Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. -W., Valle, M. D., Elias-Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal-Yam, A., Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O'Brien, P., Osborne, J. P., Palmer, D., Perri, M., Siegel, M., Tagliaferri, G., Klotz, A., Turpin, D., Laugier, R., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., DePoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang-Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., McMahon, R. G., Banerji, M., Gonzalez-Solares, E., Schulze, S., Postigo, A. de U., Thoene, C. C., Cano, Z., and Rosswog, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492
Published: 2016
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26. Developing an indicator of productive potential to assess land use suitability in New Zealand

Author: Harris, S., McDowell, R.W., Lilburne, L., Laurenson, S., Dowling, L., Guo, Jing, Pletnyakov, P., Beare, M., and Palmer, D.
Published: 2021
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27. Kinetics of the formation and destruction of PCDD/Fs in a laboratory tubular furnace

Author: Palmer, D., Pou, J.O., Díaz-Ferrero, J., Conesa, Juan A., and Ortuño, N.
Published: 2021
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28. Evidence that the directly imaged planet HD 131399 Ab Is a Background Star

Author: Nielsen, EL, Rosa, RJD, Rameau, J, Wang, JJ, Esposito, TM, Millar-Blanchaer, MA, Marois, C, Vigan, A, Ammons, SM, Artigau, E, Bailey, VP, Blunt, S, Bulger, J, Chilcote, J, Cotten, T, Doyon, R, Duchêne, G, Fabrycky, D, Fitzgerald, MP, Follette, KB, Gerard, BL, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hibon, P, Hinkley, S, Hung, LW, Ingraham, P, Jensen-Clem, R, Kalas, P, Konopacky, Q, Larkin, JE, MacIntosh, B, Maire, J, Marchis, F, Metchev, S, Morzinski, KM, Murray-Clay, RA, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Pueyo, L, Rafikov, RR, Rajan, A, Rantakyrö, FT, Ruffio, JB, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
Subjects: astrometry, instrumentation: adaptive optics, planets and satellites: detection, stars: individual, techniques: image processing, techniques: spectroscopic, astro-ph.EP, astro-ph.SR, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present evidence that the recently discovered, directly imaged planet HD 131399 Ab is a background star with nonzero proper motion. From new JHK1L′ photometry and spectroscopy obtained with the Gemini Planet Imager, VLT/SPHERE, and Keck/NIRC2, and a reanalysis of the discovery data obtained with VLT/SPHERE, we derive colors, spectra, and astrometry for HD 131399 Ab. The broader wavelength coverage and higher data quality allow us to reinvestigate its status. Its near-infrared spectral energy distribution excludes spectral types later than L0 and is consistent with a K or M dwarf, which are the most likely candidates for a background object in this direction at the apparent magnitude observed. If it were a physically associated object, the projected velocity of HD 131399 Ab would exceed escape velocity given the mass and distance to HD 131399 A. We show that HD 131399 Ab is also not following the expected track for a stationary background star at infinite distance. Solving for the proper motion and parallax required to explain the relative motion of HD 131399 Ab, we find a proper motion of 12.3 mas yr-1. When compared to predicted background objects drawn from a galactic model, we find this proper motion to be high but consistent with the top 4% fastest-moving background stars. From our analysis, we conclude that HD 131399 Ab is a background K or M dwarf.
Published: 2017

29. Characterizing 51 Eri b from 1 to 5 μm: A Partly Cloudy Exoplanet

Author: Rajan, A, Rameau, J, Rosa, RJD, Marley, MS, Graham, JR, Macintosh, B, Marois, C, Morley, C, Patience, J, Pueyo, L, Saumon, D, Ward-Duong, K, Ammons, SM, Arriaga, P, Bailey, VP, Barman, T, Bulger, J, Burrows, AS, Chilcote, J, Cotten, T, Czekala, I, Doyon, R, Duchêne, G, Esposito, TM, Fitzgerald, MP, Follette, KB, Fortney, JJ, Goodsell, SJ, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Johnson-Groh, M, Kalas, P, Konopacky, Q, Lafrenière, D, Larkin, JE, Maire, J, Marchis, F, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Nielsen, EL, Oppenheimer, R, Palmer, D, Patel, RI, Perrin, M, Poyneer, L, Rantakyrö, FT, Ruffio, JB, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vasisht, G, Wallace, JK, Wang, JJ, Wiktorowicz, S, and Wolff, S
Subjects: instrumentation: adaptive optics, planets and satellites: atmospheres, planets and satellites: composition, planets and satellites: gaseous planets, stars: individual, astro-ph.EP, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present spectrophotometry spanning 1-5 μm of 51 Eridani b, a 2-10 planet discovered by the Gemini Planet Imager Exoplanet Survey. In this study, we present new K1 (1.90-2.19 μm) and K2 (2.10-2.40 μm) spectra taken with the Gemini Planet Imager as well as an updated L P (3.76 μm) and new M S (4.67 μm) photometry from the NIRC2 Narrow camera. The new data were combined with J (1.13-1.35 μm) and H (1.50-1.80 μm) spectra from the discovery epoch with the goal of better characterizing the planet properties. The 51 Eri b photometry is redder than field brown dwarfs as well as known young T-dwarfs with similar spectral type (between T4 and T8), and we propose that 51 Eri b might be in the process of undergoing the transition from L-type to T-type. We used two complementary atmosphere model grids including either deep iron/silicate clouds or sulfide/salt clouds in the photosphere, spanning a range of cloud properties, including fully cloudy, cloud-free, and patchy/intermediate-opacity clouds. The model fits suggest that 51 Eri b has an effective temperature ranging between 605 and 737 K, a solar metallicity, and a surface gravity of log(g) = 3.5-4.0 dex, and the atmosphere requires a patchy cloud atmosphere to model the spectral energy distribution (SED). From the model atmospheres, we infer a luminosity for the planet of -5.83 to -5.93 (logL/L⊙), leaving 51 Eri b in the unique position of being one of the only directly imaged planets consistent with having formed via a cold-start scenario. Comparisons of the planet SED against warm-start models indicate that the planet luminosity is best reproduced by a planet formed via core accretion with a core mass between 15 and 127 M⊕.
Published: 2017

30. Improving and Assessing Planet Sensitivity of the GPI Exoplanet Survey with a Forward Model Matched Filter

Author: Ruffio, JB, Macintosh, B, Wang, JJ, Pueyo, L, Nielsen, EL, Rosa, RJD, Czekala, I, Marley, MS, Arriaga, P, Bailey, VP, Barman, T, Bulger, J, Chilcote, J, Cotten, T, Doyon, R, Duchene, G, Fitzgerald, MP, Follette, KB, Gerard, BL, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Maire, J, Marchis, F, Marois, C, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Rajan, A, Rameau, J, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
Subjects: instrumentation: adaptive optics, methods: statistical, planetary systems, surveys, techniques: high angular resolution, techniques: image processing, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: We present a new matched-filter algorithm for direct detection of point sources in the immediate vicinity of bright stars. The stellar point-spread function (PSF) is first subtracted using a Karhunen-Loéve image processing (KLIP) algorithm with angular and spectral differential imaging (ADI and SDI). The KLIP-induced distortion of the astrophysical signal is included in the matched-filter template by computing a forward model of the PSF at every position in the image. To optimize the performance of the algorithm, we conduct extensive planet injection and recovery tests and tune the exoplanet spectra template and KLIP reduction aggressiveness to maximize the signal-to-noise ratio (S/N) of the recovered planets. We show that only two spectral templates are necessary to recover any young Jovian exoplanets with minimal S/N loss. We also developed a complete pipeline for the automated detection of point-source candidates, the calculation of receiver operating characteristics (ROC), contrast curves based on false positives, and completeness contours. We process in a uniform manner more than 330 data sets from the Gemini Planet Imager Exoplanet Survey and assess GPI typical sensitivity as a function of the star and the hypothetical companion spectral type. This work allows for the first time a comparison of different detection algorithms at a survey scale accounting for both planet completeness and false-positive rate. We show that the new forward model matched filter allows the detection of 50% fainter objects than a conventional cross-correlation technique with a Gaussian PSF template for the same false-positive rate.
Published: 2017

31. An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO

Author: Rameau, J, Follette, KB, Pueyo, L, Marois, C, MacIntosh, B, Millar-Blanchaer, M, Wang, JJ, Vega, D, Doyon, R, Lafrenire, D, Nielsen, EL, Bailey, V, Chilcote, JK, Close, LM, Esposito, TM, Males, JR, Metchev, S, Morzinski, KM, Ruffio, JB, Wolff, SG, Ammons, SM, Barman, TS, Bulger, J, Cotten, T, Rosa, RJD, Duchene, G, Fitzgerald, MP, Goodsell, S, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Maire, J, Marchis, F, Oppenheimer, R, Palmer, D, Patience, J, Perrin, MD, Poyneer, L, Rajan, A, Rantakyrö, FT, Marley, MS, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, and Wiktorowicz, S
Subjects: instrumentation: adaptive optics, planet-disk interactions, planetary systems, stars: individual, astro-ph.EP, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present H band spectroscopic and Hμ photometric observations of HD 100546 obtained with the Gemini Planet Imager and the Magellan Visible AO camera. We detect H band emission at the location of the protoplanet HD 100546 b, but show that the choice of data processing parameters strongly affects the morphology of this source. It appears point-like in some aggressive reductions, but rejoins an extended disk structure in the majority of the others. Furthermore, we demonstrate that this emission appears stationary on a timescale of 4.6 years, inconsistent at the 2σ level with a Keplerian clockwise orbit at 59 au in the disk plane. The H band spectrum of the emission is inconsistent with any type of low effective temperature object or accreting protoplanetary disk. It strongly suggests a scattered-light origin, as this is consistent with the spectrum of the star and the spectra extracted at other locations in the disk. A non-detection at the 5σ level of HD 100546 b in differential Hμ imaging places an upper limit, assuming the protoplanet lies in a gap free of extinction, on the accretion luminosity of 1.7 ? 10-4 L o and for 1 R Jup. These limits are comparable to the accretion luminosity and accretion rate of T-Tauri stars or LkCa 15 b. Taken together, these lines of evidence suggest that the H band source at the location of HD 100546 b is not emitted by a planetary photosphere or an accreting circumplanetary disk but is a disk feature enhanced by the point-spread function subtraction process. This non-detection is consistent with the non-detection in the K band reported in an earlier study but does not exclude the possibility that HD 100546 b is deeply embedded.
Published: 2017

32. Complex Spiral Structure in the HD 100546 Transitional Disk as Revealed by GPI and MagAO

Author: Follette, KB, Rameau, J, Dong, R, Pueyo, L, Close, LM, Duchêne, G, Fung, J, Leonard, C, MacIntosh, B, Males, JR, Marois, C, Millar-Blanchaer, MA, Morzinski, KM, Mullen, W, Perrin, M, Spiro, E, Wang, J, Ammons, SM, Bailey, VP, Barman, T, Bulger, J, Chilcote, J, Cotten, T, De Rosa, RJ, Doyon, R, Fitzgerald, MP, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Maire, J, Marchis, F, Metchev, S, Nielsen, EL, Oppenheimer, R, Palmer, D, Patience, J, Poyneer, L, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vega, D, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
Subjects: instrumentation: adaptive optics, planet-disk interaction, protoplanetary disk, stars: individual, astro-ph.EP, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present optical and near-infrared high-contrast images of the transitional disk HD 100546 taken with the Magellan Adaptive Optics system (MagAO) and the Gemini Planet Imager (GPI). GPI data include both polarized intensity and total intensity imagery, and MagAO data are taken in Simultaneous Differential Imaging mode at Hα. The new GPI H-band total intensity data represent a significant enhancement in sensitivity and field rotation compared to previous data sets and enable a detailed exploration of substructure in the disk. The data are processed with a variety of differential imaging techniques (polarized, angular, reference, and simultaneous differential imaging) in an attempt to identify the disk structures that are most consistent across wavelengths, processing techniques, and algorithmic parameters. The inner disk cavity at 15 au is clearly resolved in multiple data sets, as are a variety of spiral features. While the cavity and spiral structures are identified at levels significantly distinct from the neighboring regions of the disk under several algorithms and with a range of algorithmic parameters, emission at the location of HD 100546 "c" varies from point-like under aggressive algorithmic parameters to a smooth continuous structure with conservative parameters, and is consistent with disk emission. Features identified in the HD 100546 disk bear qualitative similarity to computational models of a moderately inclined two-armed spiral disk, where projection effects and wrapping of the spiral arms around the star result in a number of truncated spiral features in forward-modeled images.
Published: 2017

33. 1-2.4 μm Near-IR Spectrum of the Giant Planet β Pictoris b Obtained with the Gemini Planet Imager

Author: Chilcote, J, Pueyo, L, Rosa, RJD, Vargas, J, Macintosh, B, Bailey, VP, Barman, T, Bauman, B, Bruzzone, S, Bulger, J, Burrows, AS, Cardwell, A, Chen, CH, Cotten, T, Dillon, D, Doyon, R, Draper, ZH, Duchêne, G, Dunn, J, Erikson, D, Fitzgerald, MP, Follette, KB, Gavel, D, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hartung, M, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Maire, J, Marchis, F, Marley, MS, Marois, C, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Nielsen, EL, Norton, A, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Rajan, A, Rameau, J, Rantakyrö, FT, Sadakuni, N, Saddlemyer, L, Savransky, D, Schneider, AC, Serio, A, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Wang, JJ, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
Subjects: instrumentation: adaptive optics, planetary systems, stars: individual, techniques:spectroscopic, astro-ph.EP, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: Using the Gemini Planet Imager located at Gemini South, we measured the near-infrared (1.0-2.4 μm) spectrum of the planetary companion to the nearby, young star β Pictoris. We compare the spectrum obtained with currently published model grids and with known substellar objects and present the best matching models as well as the best matching observed objects. Comparing the empirical measurement of the bolometric luminosity to evolutionary models, we find a mass of 12.9 ±0.2 , an effective temperature of 1724 ±15 K, a radius of 1.46 ±0.01 , and a surface gravity of [dex] (cgs). The stated uncertainties are statistical errors only, and do not incorporate any uncertainty on the evolutionary models. Using atmospheric models, we find an effective temperature of 1700-1800 K and a surface gravity of -4.0 [dex] depending upon the model. These values agree well with other publications and with "hot-start" predictions from planetary evolution models. Further, we find that the spectrum of β Pic b best matches a low surface gravity L2 ±1 brown dwarf. Finally, comparing the spectrum to field brown dwarfs, we find the the spectrum best matches 2MASS J04062677-381210 and 2MASS J03552337+1133437.
Published: 2017

34. Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., De Rosa, R., DeSalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., MacDonald, T., Machenschalk, B., MacInnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., McCarthy, R., McClelland, D. E., McCormick, S., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McWilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palliyaguru, N., Palomba, C., Pal-Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. -P., Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey-Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., McConnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Castro-Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. R., Hu, Y. -D., Kubánek, P., Guziy, S., Castellón, A., García-Cerezo, A., Muñoz, V. F., del Pulgar, C. Pérez, Castillo-Carrión, S., Cerón, J. M. Castro, Hudec, R., Caballero-García, M. D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Sanguino, T. de J. Mateo, Fernández-Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, Ch., Fan, Y., Wang, Ch., Hiriart, D., Lee, W. H., Claret, A., Sánchez-Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau-Graziati, L., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit-Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica-Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. -F., Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares-Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Zhang, B. -B., Hui, C. M., Jenke, P., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., von Kienlin, A., Kippen, R. M., McBreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. -F., Blackburn, L., Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez-Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., McEnery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. -L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Van Sistine, A., Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, D. K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra-Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston-Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., E., F. Olivares, Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. -W., Valle, M. D., Elias-Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal-Yam, A., Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O'Brien, P., Osborne, J. P., Palmer, D., Perri, M., Siegel, M., Tagliaferri, G., Klotz, A., Turpin, D., Laugier, R., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., DePoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang-Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., McMahon, R. G., Banerji, M., Gonzalez-Solares, E., Schulze, S., Postigo, A. de U., Thoene, C. C., Cano, Z., and Rosswog, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams., Comment: For Supplement, see https://arxiv.org/abs/1604.07864
Published: 2016
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35. Swift follow-up of the Gravitational Wave source GW150914

Author: Evans, P. A., Kennea, J. A., Barthelmy, S. D., Beardmore, A. P., Burrows, D. N., Campana, S., Cenko, S. B., Gehrels, N., Giommi, P., Gronwall, C., Marshall, F. E., Malesani, D., Markwardt, C. B., Mingo, B., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Page, K. L., Palmer, D. M., Perri, M., Racusin, J. L., Siegel, M. H., Sbarufatti, B., and Tagliaferri, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Advanced LIGO observatory recently reported the first direct detection of gravitational waves (GW) which triggered ALIGO on 2015 September 14. We report on observations taken with the Swift satellite two days after the trigger. No new X-ray, optical, UV or hard X-ray sources were detected in our observations, which were focussed on nearby galaxies in the GW error region and covered 4.7 square degrees (~2% of the probability in the rapidly-available GW error region; 0.3% of the probability from the final GW error region, which was produced several months after the trigger). We describe the rapid Swift response and automated analysis of the X-ray telescope and UV/Optical Telescope data, and note the importance to electromagnetic follow up of early notification of the progenitor details inferred from GW analysis., Comment: 5 pages, 2 figures, 2 tables; accepted by MNRAS Letters. Modified to improve the location and shape of the BAT field of view in Fig. 1
Published: 2016
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36. Discovery and spectroscopy of the young Jovian planet 51 Eri b with the Gemini Planet Imager

Author: Macintosh, B., Graham, J. R., Barman, T., De Rosa, R. J., Konopacky, Q., Marley, M. S., Marois, C., Nielsen, E. L., Pueyo, L., Rajan, A., Rameau, J., Saumon, D., Wang, J. J., Patience, J., Ammons, M., Arriaga, P., Artigau, E., Beckwith, S., Brewster, J., Bruzzone, S., Bulger, J., Burningham, B., Burrows, A. S., Chen, C., Chiang, E., Chilcote, J. K., Dawson, R. I., Dong, R., Doyon, R., Draper, Z. H., Duchêne, G., Esposito, T. M., Fabrycky, D., Fitzgerald, M. P., Follette, K. B., Fortney, J. J., Gerard, B., Goodsell, S., Greenbaum, A. Z., Hibon, P., Hinkley, S., Cotten, T. H., Hung, L. -W., Ingraham, P., Johnson-Groh, M., Kalas, P., Lafreniere, D., Larkin, J. E., Lee, J., Line, M., Long, D., Maire, J., Marchis, F., Matthews, B. C., Max, C. E., Metchev, S., Millar-Blanchaer, M. A., Mittal, T., Morley, C. V., Morzinski, K. M., Murray-Clay, R., Oppenheimer, R., Palmer, D. W., Patel, R., Perrin, M. D., Poyneer, L. A., Rafikov, R. R., Rantakyrö, F. T., Rice, E. L., Rojo, P., Rudy, A. R., Ruffio, J. -B., Ruiz, M. T., Sadakuni, N., Saddlemyer, L., Salama, M., Savransky, D., Schneider, A. C., Sivaramakrishnan, A., Song, I., Soummer, R., Thomas, S., Vasisht, G., Wallace, J. K., Ward-Duong, K., Wiktorowicz, S. J., Wolff, S. G., and Zuckerman, B.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric composition and luminosity, which is influenced by their formation mechanism. Using the Gemini Planet Imager, we discovered a planet orbiting the \$sim$20 Myr-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water vapor absorption. Modeling of the spectra and photometry yields a luminosity of L/LS=1.6-4.0 x 10-6 and an effective temperature of 600-750 K. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold- start" core accretion process that may have formed Jupiter., Comment: 29 pages, 3 figures, 2 tables, and Supplementary Materials. published in Science Express on Aug 13 2015. List of authors and the magnitudes of the star were correted
Published: 2015
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37. Longitudinal characterisation of haematological and biochemical parameters in cancer patients prior to and during COVID-19 reveals features associated with outcome

Author: Lee, R.J., Wysocki, O., Bhogal, T., Shotton, R., Tivey, A., Angelakas, A., Aung, T., Banfill, K., Baxter, M., Boyce, H., Brearton, G., Copson, E., Dickens, E., Eastlake, L., Gomes, F., Hague, C., Harrison, M., Horsley, L., Huddar, P., Hudson, Z., Khan, S., Khan, U.T., Maynard, A., McKenzie, H., Palmer, D., Robinson, T., Rowe, M., Thomas, A., Tweedy, J., Sheehan, R., Stockdale, A., Weaver, J., Williams, S., Wilson, C., Zhou, C., Dive, C., Cooksley, T., Palmieri, C., Freitas, A., and Armstrong, A.C.
Published: 2021
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38. Some observations on the geological history of the holoplanktonic gastropods

Author: Hart, M.B., Wall-Palmer, D., Janssen, A.W., and Smart, C.W.
Published: 2020
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39. Swift follow-up of IceCube triggers, and implications for the Advanced-LIGO era

Author: Evans, P. A., Osborne, J. P., Kennea, J. A., Smith, M., Palmer, D. M., Gehrels, N., Gelbord, J. M., Homeier, A., Voge, M., Strotjohann, N. L., Cowen, D. F., Boeser, S., Kowalski, M., and Stasik, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Between 2011 March and 2014 August Swift responded to 20 triggers from the IceCube neutrino observatory, observing the IceCube 50% confidence error circle in X-rays, typically within 5 hours of the trigger. No confirmed counterpart has been detected. We describe the Swift follow up strategy and data analysis and present the results of the campaign. We discuss the challenges of distinguishing the X-ray counterpart to a neutrino trigger from serendipitous uncatalogued X-ray sources in the error circle, and consider the implications of our results for future strategies for multi-messenger astronomy, with particular reference to the follow up of gravitational wave triggers from the advanced-era detectors., Comment: Accepted for publication in MNRAS. 18 pages, including 8 figures and 4 tables; two of which are landscape-oriented
Published: 2015
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40. Imaging an 80 au radius dust ring around the F5V star HD 157587

Author: Millar-Blanchaer, MA, Wang, JJ, Kalas, P, Graham, JR, Duchêne, G, Nielsen, EL, Perrin, M, Moon, DS, Padgett, D, Metchev, S, Ammons, SM, Bailey, VP, Barman, T, Bruzzone, S, Bulger, J, Chen, CH, Chilcote, J, Cotten, T, Rosa, RJD, Doyon, R, Draper, ZH, Esposito, TM, Fitzgerald, MP, Follette, KB, Gerard, BL, Greenbaum, AZ, Hibon, P, Hinkley, S, Hung, LW, Ingraham, P, Johnson-Groh, M, Konopacky, Q, Larkin, JE, MacIntosh, B, Maire, J, Marchis, F, Marley, MS, Marois, C, Matthews, BC, Oppenheimer, R, Palmer, D, Patience, J, Poyneer, L, Pueyo, L, Rajan, A, Rameau, J, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vega, D, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
Subjects: planet-disk interactions, stars: individual, techniques: polarimetric, astro-ph.EP, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present H-band near-infrared polarimetric imaging observations of the F5V star HD 157587 obtained with the Gemini Planet Imager (GPI) that reveal the debris disk as a bright ring structure at a separation of ∼80-100 au. The new GPI data complement recent Hubble Space Telescope/STIS observations that show the disk extending out to over 500 au. The GPI image displays a strong asymmetry along the projected minor axis as well as a fainter asymmetry along the projected major axis. We associate the minor and major axis asymmetries with polarized forward scattering and a possible stellocentric offset, respectively. To constrain the disk geometry, we fit two separate disk models to the polarized image, each using a different scattering phase function. Both models favor a disk inclination of ∼70° and a 1.5 ± 0.6 au stellar offset in the plane of the sky along the projected major axis of the disk. We find that the stellar offset in the disk plane, perpendicular to the projected major axis is degenerate with the form of the scattering phase function and remains poorly constrained. The disk is not recovered in total intensity due in part to strong adaptive optics residuals, but we recover three point sources. Considering the system's proximity to the galactic plane and the point sources' positions relative to the disk, we consider it likely that they are background objects and unrelated to the disk's offset from the star.
Published: 2016

41. The relationship between eruptive activity, flank collapse, and sea level at volcanic islands: A long-term (>1 Ma) record offshore Montserrat, Lesser Antilles

Author: Coussens, M, Wall-Palmer, D, Talling, PJ, Watt, SFL, Cassidy, M, Jutzeler, M, Clare, MA, Hunt, JE, Manga, M, Gernon, TM, Palmer, MR, Hatter, SJ, Boudon, G, Endo, D, Fujinawa, A, Hatfield, R, Hornbach, MJ, Ishizuka, O, Kataoka, K, Le Friant, A, Maeno, F, McCanta, M, and Stinton, AJ
Subjects: landslide, volcanism, sea level, IODP, Expedition 340, Geochemistry & Geophysics, Earth Sciences, Physical Sciences
Abstract: Hole U1395B, drilled southeast of Montserrat during Integrated Ocean Drilling Program Expedition 340, provides a long (>1 Ma) and detailed record of eruptive and mass-wasting events (>130 discrete events). This record can be used to explore the temporal evolution in volcanic activity and landslides at an arc volcano. Analysis of tephra fall and volcaniclastic turbidite deposits in the drill cores reveals three heightened periods of volcanic activity on the island of Montserrat (∼930 to ∼900 ka, ∼810 to ∼760 ka, and ∼190 to ∼120 ka) that coincide with periods of increased volcano instability and mass-wasting. The youngest of these periods marks the peak in activity at the Soufrière Hills volcano. The largest flank collapse of this volcano (∼130 ka) occurred toward the end of this period, and two younger landslides also occurred during a period of relatively elevated volcanism. These three landslides represent the only large (>0.3 km3) flank collapses of the Soufrière Hills edifice, and their timing also coincides with periods of rapid sea level rise (>5 m/ka). Available age data from other island arc volcanoes suggest a general correlation between the timing of large landslides and periods of rapid sea level rise, but this is not observed for volcanoes in intraplate ocean settings. We thus infer that rapid sea level rise may modulate the timing of collapse at island arc volcanoes, but not in larger ocean-island settings.
Published: 2016

42. Technical Design Report EuroGammaS proposal for the ELI-NP Gamma beam System

Author: Adriani, O., Albergo, S., Alesini, D., Anania, M., Angal-Kalinin, D., Antici, P., Bacci, A., Bedogni, R., Bellaveglia, M., Biscari, C., Bliss, N., Boni, R., Boscolo, M., Broggi, F., Cardarelli, P., Cassou, K., Castellano, M., Catani, L., Chaikovska, I., Chiadroni, E., Chiche, R., Cianchi, A., Clarke, J., Clozza, A., Coppola, M., Courjaud, A., Curatolo, C., Dadoun, O., Delerue, N., De Martinis, C., Di Domenico, G., Di Pasquale, E., Di Pirro, G., Drago, A., Druon, F., Dupraz, K., Egal, F., Esposito, A., Falcoz, F., Fell, B., Ferrario, M., Ficcadenti, L., Fichot, P., Gallo, A., Gambaccini, M., Gatti, G., Georges, P., Ghigo, A., Goulden, A., Graziani, G., Guibout, D., Guilbaud, O., Hanna, M., Herbert, J., Hovsepian, T., Iarocci, E., Iorio, P., Jamison, S., Kazamias, S., Labaye, F., Lancia, L., Marcellini, F., Martens, A., Maroli, C., Martlew, B., Marziani, M., Mazzitelli, G., McIntosh, P., Migliorati, M., Mostacci, A., Mueller, A., Nardone, V., Pace, E., Palmer, D. T., Palumbo, L., Pelorosso, A., Perin, F. X., Passaleva, G., Pellegrino, L., Petrillo, V., Pittman, M., Riboulet, G., Ricci, R., Ronsivalle, C., Ros, D., Rossi, A., Serafini, L., Serio, M., Sgamma, F., Smith, R., Smith, S., Soskov, V., Spataro, B., Statera, M., Stecchi, A., Stella, A., Stocchi, A., Tocci, S., Tomassini, P., Tomassini, S., Tricomi, A., Vaccarezza, C., Variola, A., Veltri, M., Vescovi, S., Villa, F., Wang, F., Yildiz, E., and Zomer, F.
Subjects: Physics - Accelerator Physics
Abstract: The machine described in this document is an advanced Source of up to 20 MeV Gamma Rays based on Compton back-scattering, i.e. collision of an intense high power laser beam and a high brightness electron beam with maximum kinetic energy of about 720 MeV. Fully equipped with collimation and characterization systems, in order to generate, form and fully measure the physical characteristics of the produced Gamma Ray beam. The quality, i.e. phase space density, of the two colliding beams will be such that the emitted Gamma ray beam is characterized by energy tunability, spectral density, bandwidth, polarization, divergence and brilliance compatible with the requested performances of the ELI-NP user facility, to be built in Romania as the Nuclear Physics oriented Pillar of the European Extreme Light Infrastructure. This document illustrates the Technical Design finally produced by the EuroGammaS Collaboration, after a thorough investigation of the machine expected performances within the constraints imposed by the ELI-NP tender for the Gamma Beam System (ELI-NP-GBS), in terms of available budget, deadlines for machine completion and performance achievement, compatibility with lay-out and characteristics of the planned civil engineering.
Published: 2014

43. Search for gravitational waves associated with gamma-ray bursts detected by the InterPlanetary Network

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Aasi, J., Abbott, B. P., Abbott, R., Abbott, T., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Affeldt, C., Agathos, M., Aggarwal, N., Aguiar, O. D., Ajith, P., Alemic, A., Allen, B., Allocca, A., Amariutei, D., Andersen, M., Anderson, R. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C., Areeda, J. S., Ast, S., Aston, S. M., Astone, P., Aufmuth, P., Augustus, H., Aulbert, C., Aylott, B. E., Babak, S., Baker, P. T., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barbet, M., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bauchrowitz, J., Bauer, Th. S., Baune, C., Bavigadda, V., Behnke, B., Bejger, M., Beker, M. G., Belczynski, C., Bell, A. S., Bell, C., Bergmann, G., Bersanetti, D., Bertolini, A., Betzwieser, J., Bilenko, I. A., Billingsley, G., Birch, J., Biscans, S., Bitossi, M., Biwer, C., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bond, C., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Bose, Sukanta, Bosi, L., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Brooks, A. F., Brown, D. A., Brown, D. D., Brückner, F., Buchman, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Burman, R., Buskulic, D., Buy, C., Cadonati, L., Cagnoli, G., Bustillo, J. Calderón, Calloni, E., Camp, J. B., Campsie, P., Cannon, K. C., Canuel, B., Cao, J., Capano, C. D., Carbognani, F., Carbone, L., Caride, S., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Celerier, C., Cella, G., Cepeda, C., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, X., Chen, Y., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S. S. Y., Chung, S., Ciani, G., Clara, F., Clark, D. E., Clark, J. A., Clayton, J. H., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C., Colombini, M., Cominsky, L., Constancio Jr., M., Conte, A., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Costa, C. A., Coughlin, M. W., Coulon, J. -P., Countryman, S., Couvares, P., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Croce, R. P., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Cutler, C., Dahl, K., Canton, T. Dal, Damjanic, M., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dattilo, V., Daveloza, H., Davier, M., Davies, G. S., Daw, E. J., Day, R., Dayanga, T., DeBra, D., Debreczeni, G., Degallaix, J., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., De Rosa, R., DeRosa, R. T., DeSalvo, R., Dhurandhar, S., Díaz, M., Dickson, J., Di Fiore, L., Di Lieto, A., Di Palma, I., Di Virgilio, A., Dolique, V., Dominguez, E., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S., Eberle, T., Edo, T., Edwards, M., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Endrőczi, G., Essick, R., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fazi, D., Fehrmann, H., Fejer, M. M., Feldbaum, D., Feroz, F., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finn, L. S., Fiori, I., Fisher, R. P., Flaminio, R., Fournier, J. -D., Franco, S., Frasca, S., Frasconi, F., Frede, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gair, J. R., Gammaitoni, L., Gaonkar, S., Garufi, F., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gleason, J., Goetz, E., Goetz, R., Gondan, L., González, G., Gordon, N., Gorodetsky, M. L., Gossan, S., Goßler, S., Gouaty, R., Gräf, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Groot, P., Grote, H., Grover, K., Grunewald, S., Guidi, G. M., Guido, C. J., Gushwa, K., Gustafson, E. K., Gustafson, R., Ha, J., Hall, E. D., Hamilton, W., Hammer, D., Hammond, G., Hanke, M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hart, M., Hartman, M. T., Haster, C. -J., Haughian, K., Heidmann, A., Heintze, M., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Heptonstall, A. W., Heurs, M., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Holt, K., Hopkins, P., Horrom, T., Hoske, D., Hosken, D. J., Hough, J., Howell, E. J., Hu, Y., Huerta, E., Hughey, B., Husa, S., Huttner, S. H., Huynh, M., Huynh-Dinh, T., Idrisy, A., Ingram, D. R., Inta, R., Islas, G., Isogai, T., Ivanov, A., Iyer, B. R., Izumi, K., Jacobson, M., Jang, H., Jaranowski, P., Ji, Y., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., K, Haris, Kalmus, P., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karlen, J., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, H., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Keiser, G. M., Keitel, D., Kelley, D. B., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, C., Kim, K., Kim, N. G., Kim, N., Kim, S., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kline, J., Koehlenbeck, S., Kokeyama, K., Kondrashov, V., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kumar, A., Kumar, D. Nanda, Kumar, P., Kumar, R., Kuo, L., Kutynia, A., Lam, P. K., Landry, M., Lantz, B., Larson, S., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, J., Lee, P. J., Leonardi, M., Leong, J. R., Roux, A. Le, Leroy, N., Letendre, N., Levin, Y., Levine, B., Lewis, J., Li, T. G. F., Libbrecht, K., Libson, A., Lin, A. C., Littenberg, T. B., Lockerbie, N. A., Lockett, V., Lodhia, D., Loew, K., Logue, J., Lombardi, A. L., Lopez, E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Lubinski, M. J., Lück, H., Lundgren, A. P., Ma, Y., Macdonald, E. P., MacDonald, T., Machenschalk, B., MacInnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R., Mageswaran, M., Maglione, C., Mailand, K., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Manca, G. M., Mandel, I., Mandic, V., Mangano, V., Mangini, N. M., Mansell, G., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Martinelli, L., Martynov, D., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Matichard, F., Matone, L., Mavalvala, N., May, G., Mazumder, N., Mazzolo, G., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McIver, J., McLin, K., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Meinders, M., Melatos, A., Mendell, G., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Mikhailov, E. E., Milano, L., Miller, J., Minenkov, Y., Mingarelli, C. M. F., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moe, B., Moggi, A., Mohan, M., Mohapatra, S. R. P., Moraru, D., Moreno, G., Morgado, N., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, C. L., Mueller, G., Mukherjee, S., Mullavey, A., Munch, J., Murphy, D., Murray, P. G., Mytidis, A., Nagy, M. F., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nelemans, G., Neri, I., Neri, M., Newton, G., Nguyen, T., Nielsen, A. B., Nissanke, S., Nitz, A. H., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Ochsner, E., O'Dell, J., Oelker, E., Oh, J. J., Oh, S. H., Ohme, F., Omar, S., Oppermann, P., Oram, R., O'Reilly, B., Ortega, W., O'Shaughnessy, R., Osthelder, C., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Padilla, C., Pai, A., Palashov, O., Palomba, C., Pan, H., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Paris, H., Pasqualetti, A., Passaquieti, R., Passuello, D., Pedraza, M., Pele, A., Penn, S., Perreca, A., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pierro, V., Pinard, L., Pinto, I. M., Pitkin, M., Poeld, J., Poggiani, R., Poteomkin, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S., Prestegard, T., Price, L. R., Prijatelj, M., Privitera, S., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qin, J., Quetschke, V., Quintero, E., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Rácz, I., Radkins, H., Raffai, P., Raja, S., Rajalakshmi, G., Rakhmanov, M., Ramet, C., Ramirez, K., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Recchia, S., Reed, C. M., Regimbau, T., Reid, S., Reitze, D. H., Reula, O., Rhoades, E., Ricci, F., Riesen, R., Riles, K., Robertson, N. A., Robinet, F., Rocchi, A., Roddy, S. B., Rolland, L., Rollins, J. G., Romano, J. D., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Salemi, F., Sammut, L., Sandberg, V., Sanders, J. R., Sankar, S., Sannibale, V., Santiago-Prieto, I., Saracco, E., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Savage, R., Scheuer, J., Schilling, R., Schilman, M., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sidery, T. L., Siellez, K., Siemens, X., Sigg, D., Simakov, D., Singer, A., Singer, L., Singh, R., Sintes, A. M., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, R. J. E., Smith-Lefebvre, N. D., Son, E. J., Sorazu, B., Souradeep, T., Staley, A., Stebbins, J., Steinke, M., Steinlechner, J., Steinlechner, S., Stephens, B. C., Steplewski, S., Stevenson, S., Stone, R., Stops, D., Strain, K. A., Straniero, N., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Susmithan, S., Sutton, P. J., Swinkels, B., Tacca, M., Talukder, D., Tanner, D. B., Tao, J., Tarabrin, S. P., Taylor, R., Tellez, G., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Travasso, F., Traylor, G., Tse, M., Tshilumba, D., Tuennermann, H., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Vallisneri, M., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, van der Sluys, M. V., van Heijningen, J., van Veggel, A. A., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vincent-Finley, R., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vousden, W. D., Vyachanin, S. P., Wade, A. R., Wade, L., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, M., Wang, X., Ward, R. L., Was, M., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D. J., Whiting, B. F., Wiesner, K., Wilkinson, C., Williams, K., Williams, L., Williams, R., Williams, T. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M., Winkler, W., Wipf, C. C., Wiseman, A. G., Wittel, H., Woan, G., Wolovick, N., Worden, J., Wu, Y., Yablon, J., Yakushin, I., Yam, W., Yamamoto, H., Yancey, C. C., Yang, H., Yoshida, S., Yvert, M., Zadrożny, A., Zanolin, M., Zendri, J. -P., Zhang, Fan, Zhang, L., Zhao, C., Zhu, H., Zhu, X. J., Zucker, M. E., Zuraw, S., Zweizig, J., Aptekar, R. L., Atteia, J. L., Cline, T., Connaughton, V., Frederiks, D. D., Golenetskii, S. V., Hurley, K., Krimm, H. A., Marisaldi, M., Pal'shin, V. D., Palmer, D., Svinkin, D. S., Terada, Y., and von Kienlin, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: We present the results of a search for gravitational waves associated with 223 gamma-ray bursts (GRBs) detected by the InterPlanetary Network (IPN) in 2005-2010 during LIGO's fifth and sixth science runs and Virgo's first, second and third science runs. The IPN satellites provide accurate times of the bursts and sky localizations that vary significantly from degree scale to hundreds of square degrees. We search for both a well-modeled binary coalescence signal, the favored progenitor model for short GRBs, and for generic, unmodeled gravitational wave bursts. Both searches use the event time and sky localization to improve the gravitational-wave search sensitivity as compared to corresponding all-time, all-sky searches. We find no evidence of a gravitational-wave signal associated with any of the IPN GRBs in the sample, nor do we find evidence for a population of weak gravitational-wave signals associated with the GRBs. For all IPN-detected GRBs, for which a sufficient duration of quality gravitational-wave data is available, we place lower bounds on the distance to the source in accordance with an optimistic assumption of gravitational-wave emission energy of $10^{-2}M_{\odot}c^2$ at 150 Hz, and find a median of 13 Mpc. For the 27 short-hard GRBs we place 90% confidence exclusion distances to two source models: a binary neutron star coalescence, with a median distance of 12Mpc, or the coalescence of a neutron star and black hole, with a median distance of 22 Mpc. Finally, we combine this search with previously published results to provide a population statement for GRB searches in first-generation LIGO and Virgo gravitational-wave detectors, and a resulting examination of prospects for the advanced gravitational-wave detectors., Comment: 15 pages, 8 figures, 2 tables; for the science summary, see http://www.ligo.org/science/Publication-IPNS56VSR123grb/index.php
Published: 2014
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44. Non-destructive evaluation of ductile-porous versus brittle 3D printed vascular networks in self-healing concrete

Author: Shields, Y., Tsangouri, E., Riordan, C., Nardi, C., (0000-0003-0848-0662) Da Assuncao Godinho, J. R., Antonaci, P., Palmer, D., Al-Tabbaa, A., Jefferson, T., Belie, N., Tittelboom, K., Shields, Y., Tsangouri, E., Riordan, C., Nardi, C., (0000-0003-0848-0662) Da Assuncao Godinho, J. R., Antonaci, P., Palmer, D., Al-Tabbaa, A., Jefferson, T., Belie, N., and Tittelboom, K.
Abstract: Additive manufacturing (AM) can produce complex vascular network configurations, yet limited testing has been done to characterize the damage and healing behavior of concrete with embedded networks for self-healing. In this study, different AM methods and network wall materials were used to produce vascular networks for self-healing concrete prisms, where their load-response behavior, healing efficiency and microstructure were evaluated using non-destructive techniques: acoustic emission (AE), ultrasonic pulse velocity (UPV), digital image correlation (DIC), and X -ray computed tomography (CT). The types of healing agent release mechanisms that were studied include a ductile-porous network that supplies fluid from its pores and a brittle network that fractures under load to release fluid. DIC coupled with AE verified debonding of ductile-porous networks from the cementitious matrix, and was able to track damage progression as well as healing for all networks with load regains up to 56% and stiffness regains up to 91% using polyurethane.
Published: 2024

45. Swift/UVOT discovery of Swift J221951-484240:a UV luminous ambiguous nuclear transient

Author: Oates, S R, Kuin, N P M, Nicholl, M, Marshall, F, Ridley, E, Boutsia, K, Breeveld, A A, Buckley, D A H, Cenko, S B, De pasquale, M, Edwards, P G, Gromadzki, M, Gupta, R, Laha, S, Morrell, N, Orio, M, Pandey, S B, Page, M J, Page, K L, Parsotan, T, Rau, A, Schady, P, Stevens, J, Brown, P J, Evans, P A, Gronwall, C, Kennea, J A, Klingler, N J, Siegel, M H, Tohuvavohu, A, Ambrosi, E, Barthelmy, S D, Beardmore, A P, Bernardini, M G, Bonnerot, C, Campana, S, Caputo, R, Ciroi, S, Cusumano, G, D’aì, A, D’avanzo, P, D’elia, V, Giommi, P, Hartmann, D H, Krimm, H A, Malesani, D B, Melandri, A, Nousek, J A, O’brien, P T, Osborne, J P, Pagani, C, Palmer, D M, Perri, M, Racusin, J L, Sakamoto, T, Sbarufatti, B, Schlieder, J E, Tagliaferri, G, Troja, E, Xu, D, Oates, S R, Kuin, N P M, Nicholl, M, Marshall, F, Ridley, E, Boutsia, K, Breeveld, A A, Buckley, D A H, Cenko, S B, De pasquale, M, Edwards, P G, Gromadzki, M, Gupta, R, Laha, S, Morrell, N, Orio, M, Pandey, S B, Page, M J, Page, K L, Parsotan, T, Rau, A, Schady, P, Stevens, J, Brown, P J, Evans, P A, Gronwall, C, Kennea, J A, Klingler, N J, Siegel, M H, Tohuvavohu, A, Ambrosi, E, Barthelmy, S D, Beardmore, A P, Bernardini, M G, Bonnerot, C, Campana, S, Caputo, R, Ciroi, S, Cusumano, G, D’aì, A, D’avanzo, P, D’elia, V, Giommi, P, Hartmann, D H, Krimm, H A, Malesani, D B, Melandri, A, Nousek, J A, O’brien, P T, Osborne, J P, Pagani, C, Palmer, D M, Perri, M, Racusin, J L, Sakamoto, T, Sbarufatti, B, Schlieder, J E, Tagliaferri, G, Troja, E, and Xu, D
Published: 2024

46. A Missing-Link in the Supernova-GRB Connection: The Case of SN 2012ap

Author: Chakraborti, Sayan, Soderberg, Alicia, Chomiuk, Laura, Kamble, Atish, Yadav, Naveen, Ray, Alak, Hurley, Kevin, Margutti, Raffaella, Milisavljevic, Dan, Bietenholz, Michael, Brunthaler, Andreas, Pignata, Giuliano, Pian, Elena, Mazzali, Paolo, Fransson, Claes, Bartel, Norbert, Hamuy, Mario, Levesque, Emily, MacFadyen, Andrew, Dittmann, Jason, Krauss, Miriam, Briggs, M. S., Connaughton, V., Yamaoka, K., Takahashi, T., Ohno, M., Fukazawa, Y., Tashiro, M., Terada, Y., Murakami, T., Goldsten, J., Barthelmy, S., Gehrels, N., Cummings, J., Krimm, H., Palmer, D., Golenetskii, S., Aptekar, R., Frederiks, D., Svinkin, D., Cline, T., Mitrofanov, I. G., Golovin, D., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Enos, H., von Kienlin, A., Rau, A., Zhang, X., and Savchenko, V.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Gamma Ray Bursts (GRBs) are characterized by ultra-relativistic outflows, while supernovae are generally characterized by non-relativistic ejecta. GRB afterglows decelerate rapidly usually within days, because their low-mass ejecta rapidly sweep up a comparatively larger mass of circumstellar material. However supernovae, with heavy ejecta, can be in nearly free expansion for centuries. Supernovae were thought to have non-relativistic outflows except for few relativistic ones accompanied by GRBs. This clear division was blurred by SN 2009bb, the first supernova with a relativistic outflow without an observed GRB. Yet the ejecta from SN 2009bb was baryon loaded, and in nearly-free expansion for a year, unlike GRBs. We report the first supernova discovered without a GRB, but with rapidly decelerating mildly relativistic ejecta, SN 2012ap. We discovered a bright and rapidly evolving radio counterpart driven by the circumstellar interaction of the relativistic ejecta. However, we did not find any coincident GRB with an isotropic fluence of more than a sixth of the fluence from GRB 980425. This shows for the first time that central engines in type Ic supernovae, even without an observed GRB, can produce both relativistic and rapidly decelerating outflows like GRBs., Comment: 8 pages, 5 figures, 1 table, accepted for publication in ApJ
Published: 2014
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47. Sub-nanometer flattening of a 45-cm long, 45-actuator x-ray deformable mirror

Author: Poyneer, L. A., McCarville, T., Pardini, T., Palmer, D., Brooks, A., Pivovaroff, M. J., and Macintosh, B.
Subjects: Physics - Instrumentation and Detectors, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We have built a 45-cm long x-ray deformable mirror of super-polished single-crystal silicon that has 45 actuators along the tangential axis. After assembly the surface height error was 19 nm rms. With use of high-precision visible-light metrology and precise control algorithms, we have actuated the x-ray deformable mirror and flattened its entire surface to 0.7 nm rms controllable figure error. This is, to our knowledge, the first sub-nanometer active flattening of a substrate longer than 15 cm., Comment: Revised version accepted by Applied Optics 24 Apr 2014
Published: 2014
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48. Scheduling nab-paclitaxel combined with gemcitabine as first-line treatment for metastatic pancreatic adenocarcinoma

Author: Corrie, P. G., Qian, W., Basu, B., Valle, J. W., Falk, S., lwuji, C., Wasan, H., Palmer, D., Scott-Brown, M., Wadsley, J., Arif, S., Bridgewater, J., Propper, D., Gillmore, R., Gopinathan, A., Skells, R., Bundi, P., Brais, R., Dalchau, K., Bax, L., Chhabra, A., Machin, A., Dayim, A., McAdam, K., Cummins, S., Wall, L., Ellis, R., Anthoney, A., Evans, J., Ma, Y. T., Isherwood, C., Neesse, A., Tuveson, D., and Jodrell, D. I.
Published: 2020
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49. Permeability and pressure measurements in Lesser Antilles submarine slides: Evidence for pressure-driven slow-slip failure

Author: Hornbach, MJ, Manga, M, Genecov, M, Valdez, R, Miller, P, Saffer, D, Adelstein, E, Lafuerza, S, Adachi, T, Breitkreuz, C, Jutzeler, M, Le Friant, A, Ishizuka, O, Morgan, S, Slagle, A, Talling, PJ, Fraass, A, Watt, SFL, Stroncik, NA, Aljahdali, M, Boudon, G, Fujinawa, A, Hatfield, R, Kataoka, K, Maeno, F, Martinez-Colon, M, McCanta, M, Palmer, M, Stinton, A, Subramanyam, KSV, Tamura, Y, Villemant, B, Wall-Palmer, D, and Wang, F
Subjects: Geochemistry, Geology, Geophysics
Abstract: Recent studies hypothesize that some submarine slides fail via pressure-driven slow-slip deformation. To test this hypothesis, this study derives pore pressures in failed and adjacent unfailed deep marine sediments by integrating rock physics models, physical property measurements on recovered sediment core, and wireline logs. Two drill sites (U1394 and U1399) drilled through interpreted slide debris; a third (U1395) drilled into normal marine sediment. Near-hydrostatic fluid pressure exists in sediments at site U1395. In contrast, results at both sites U1394 and U1399 indicate elevated pore fluid pressures in some sediment. We suggest that high pore pressure at the base of a submarine slide deposit at site U1394 results from slide shearing. High pore pressure exists throughout much of site U1399, and Mohr circle analysis suggests that only slight changes in the stress regime will trigger motion. Consolidation tests and permeability measurements indicate moderately low (~10-16-10-17 m2) permeability and overconsolidation in fine-grained slide debris, implying that these sediments act as seals. Three mechanisms, in isolation or in combination, may produce the observed elevated pore fluid pressures at site U1399: (1) rapid sedimentation, (2) lateral fluid flow, and (3) shearing that causes sediments to contract, increasing pore pressure. Our preferred hypothesis is this third mechanism because it explains both elevated fluid pressure and sediment overconsolidation without requiring high sedimentation rates. Our combined analysis of subsurface pore pressures, drilling data, and regional seismic images indicates that slope failure offshore Martinique is perhaps an ongoing, creep-like process where small stress changes trigger motion.
Published: 2015

50. Rapid onset of mafic magmatism facilitated by volcanic edifice collapse

Author: Cassidy, M, Watt, SFL, Talling, PJ, Palmer, MR, Edmonds, M, Jutzeler, M, Wall‐Palmer, D, Manga, M, Coussens, M, Gernon, T, Taylor, RN, Michalik, A, Inglis, E, Breitkreuz, C, Le Friant, A, Ishizuka, O, Boudon, G, McCanta, MC, Adachi, T, Hornbach, MJ, Colas, SL, Endo, D, Fujinawa, A, Kataoka, KS, Maeno, F, Tamura, Y, and Wang, F
Subjects: sector collapse, clinopyroxene, petrology, magma ascent, Meteorology & Atmospheric Sciences
Abstract: ©2015. The Authors. Volcanic edifice collapses generate some of Earth's largest landslides. How such unloading affects the magma storage systems is important for both hazard assessment and for determining long-term controls on volcano growth and decay. Here we present a detailed stratigraphic and petrological analyses of volcanic landslide and eruption deposits offshore Montserrat, in a subduction zone setting, sampled during Integrated Ocean Drilling Program Expedition 340. A large (6-10km3) collapse of the Soufrière Hills Volcano at ~130ka was followed by explosive basaltic volcanism and the formation of a new basaltic volcanic center, the South Soufrière Hills, estimated to have initiated
Published: 2015

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