Author: "Kennea, JA" - Searchworks@Jio Institute Digital Library Search Results

23 results on '"Kennea, JA"'

1. Space Telescope and Optical Reverberation Mapping Project. IX. Velocity–Delay Maps for Broad Emission Lines in NGC 5548

Author: Horne, Keith, De Rosa, G, Peterson, BM, Barth, AJ, Ely, J, Fausnaugh, MM, Kriss, GA, Pei, L, Bentz, MC, Cackett, EM, Edelson, R, Eracleous, M, Goad, MR, Grier, CJ, Kaastra, J, Kochanek, CS, Krongold, Y, Mathur, S, Netzer, H, Proga, D, Tejos, N, Vestergaard, M, Villforth, C, Adams, SM, Anderson, MD, Arévalo, P, Beatty, TG, Bennert, VN, Bigley, A, Bisogni, S, Borman, GA, Boroson, TA, Bottorff, MC, Brandt, WN, Breeveld, AA, Brotherton, M, Brown, JE, Brown, JS, Canalizo, G, Carini, MT, Clubb, KI, Comerford, JM, Corsini, EM, Crenshaw, DM, Croft, S, Croxall, KV, Bontà, E Dalla, Deason, AJ, Dehghanian, M, De Lorenzo-Cáceres, A, Denney, KD, Dietrich, M, Done, C, Efimova, NV, Evans, PA, Ferland, GJ, Filippenko, AV, Flatland, K, Fox, OD, Gardner, E, Gates, EL, Gehrels, N, Geier, S, Gelbord, JM, Gonzalez, L, Gorjian, V, Greene, JE, Grupe, D, Gupta, A, Hall, PB, Henderson, CB, Hicks, S, Holmbeck, E, Holoien, TW-S, Hutchison, T, Im, M, Jensen, JJ, Johnson, CA, Joner, MD, Jones, J, Kaspi, S, Kelly, PL, Kennea, JA, Kim, M, Kim, S, Kim, SC, King, A, Klimanov, SA, Korista, KT, Lau, MW, Lee, JC, Leonard, DC, Li, Miao, Lira, P, Lochhaas, C, Ma, Zhiyuan, MacInnis, F, Malkan, MA, Manne-Nicholas, ER, and Mauerhan, JC
Subjects: astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: In this contribution, we achieve the primary goal of the active galactic nucleus (AGN) STORM campaign by recovering velocity-delay maps for the prominent broad emission lines (Lyα, C iv, He ii, and Hβ) in the spectrum of NGC 5548. These are the most detailed velocity-delay maps ever obtained for an AGN, providing unprecedented information on the geometry, ionization structure, and kinematics of the broad-line region. Virial envelopes enclosing the emission-line responses show that the reverberating gas is bound to the black hole. A stratified ionization structure is evident. The He ii response inside 5-10 lt-day has a broad single-peaked velocity profile. The Lyα, C iv, and Hβ responses extend from inside 2 to outside 20 lt-day, with double peaks at ±2500 km s-1 in the 10-20 lt-day delay range. An incomplete ellipse in the velocity-delay plane is evident in Hβ. We interpret the maps in terms of a Keplerian disk with a well-defined outer rim at R = 20 lt-day. The far-side response is weaker than that from the near side. The line-center delay days gives the inclination i ≈ 45°. The inferred black hole mass is M BH ≈ 7 × 107 M o˙. In addition to reverberations, the fit residuals confirm that emission-line fluxes are depressed during the "BLR Holiday"identified in previous work. Moreover, a helical "Barber-Pole"pattern, with stripes moving from red to blue across the C iv and Lyα line profiles, suggests azimuthal structure rotating with a 2 yr period that may represent precession or orbital motion of inner-disk structures casting shadows on the emission-line region farther out.
Published: 2021

2. Space Telescope and Optical Reverberation Mapping Project. XII. Broad-line Region Modeling of NGC 5548

Author: Williams, PR, Pancoast, A, Treu, T, Brewer, BJ, Peterson, BM, Barth, AJ, Malkan, MA, Rosa, GD, Horne, K, Kriss, GA, Arav, N, Bentz, MC, Cackett, EM, Bontà, ED, Dehghanian, M, Done, C, Ferland, GJ, Grier, CJ, Kaastra, J, Kara, E, Kochanek, CS, Mathur, S, Mehdipour, M, Pogge, RW, Proga, D, Vestergaard, M, Waters, T, Adams, SM, Anderson, MD, Arévalo, P, Beatty, TG, Bennert, VN, Bigley, A, Bisogni, S, Borman, GA, Boroson, TA, Bottorff, MC, Brandt, WN, Breeveld, AA, Brotherton, M, Brown, JE, Brown, JS, Canalizo, G, Carini, MT, Clubb, KI, Comerford, JM, Corsini, EM, Crenshaw, DM, Croft, S, Croxall, KV, Deason, AJ, Lorenzo-Cáceres, AD, Denney, KD, Dietrich, M, Edelson, R, Efimova, NV, Ely, J, Evans, PA, Fausnaugh, MM, Filippenko, AV, Flatland, K, Fox, OD, Gardner, E, Gates, EL, Gehrels, N, Geier, S, Gelbord, JM, Gonzalez, L, Gorjian, V, Greene, JE, Grupe, D, Gupta, A, Hall, PB, Henderson, CB, Hicks, S, Holmbeck, E, Holoien, TWS, Hutchison, T, Im, M, Jensen, JJ, Johnson, CA, Joner, MD, Jones, J, Kaspi, S, Kelly, PL, Kennea, JA, Kim, M, Kim, S, Kim, SC, King, A, Klimanov, SA, Knigge, C, Krongold, Y, Lau, MW, Lee, JC, Leonard, DC, Li, M, Lira, P, Lochhaas, C, and Ma, Z
Subjects: Active galaxies, Active galactic nuclei, Reverberation mapping, Seyfert galaxies, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: We present geometric and dynamical modeling of the broad line region (BLR) for the multi-wavelength reverberation mapping campaign focused on NGC 5548 in 2014. The data set includes photometric and spectroscopic monitoring in the optical and ultraviolet, covering the Hβ, C iv, and Ly broad emission lines. We find an extended disk-like Hβ BLR with a mixture of near-circular and outflowing gas trajectories, while the C iv and Ly BLRs are much less extended and resemble shell-like structures. There is clear radial structure in the BLR, with C iv and Ly emission arising at smaller radii than the Hβ emission. Using the three lines, we make three independent black hole mass measurements, all of which are consistent. Combining these results gives a joint inference of . We examine the effect of using the V band instead of the UV continuum light curve on the results and find a size difference that is consistent with the measured UV-optical time lag, but the other structural and kinematic parameters remain unchanged, suggesting that the V band is a suitable proxy for the ionizing continuum when exploring the BLR structure and kinematics. Finally, we compare the Hβ results to similar models of data obtained in 2008 when the active galactic nucleus was at a lower luminosity state. We find that the size of the emitting region increased during this time period, but the geometry and black hole mass remained unchanged, which confirms that the BLR kinematics suitably gauge the gravitational field of the central black hole.
Published: 2020

3. Space Telescope and Optical Reverberation Mapping Project. VIII. Time Variability of Emission and Absorption in NGC 5548 Based on Modeling the Ultraviolet Spectrum

Author: Kriss, GA, De Rosa, G, Ely, J, Peterson, BM, Kaastra, J, Mehdipour, M, Ferland, GJ, Dehghanian, M, Mathur, S, Edelson, R, Korista, KT, Arav, N, Barth, AJ, Bentz, MC, Brandt, WN, Crenshaw, DM, Bontà, E Dalla, Denney, KD, Done, C, Eracleous, M, Fausnaugh, MM, Gardner, E, Goad, MR, Grier, CJ, Horne, Keith, Kochanek, CS, McHardy, IM, Netzer, H, Pancoast, A, Pei, L, Pogge, RW, Proga, D, Silva, C, Tejos, N, Vestergaard, M, Adams, SM, Anderson, MD, Arévalo, P, Beatty, TG, Behar, E, Bennert, VN, Bianchi, S, Bigley, A, Bisogni, S, Boissay-Malaquin, R, Borman, GA, Bottorff, MC, Breeveld, AA, Brotherton, M, Brown, JE, Brown, JS, Cackett, EM, Canalizo, G, Cappi, M, Carini, MT, Clubb, KI, Comerford, JM, Coker, CT, Corsini, EM, Costantini, E, Croft, S, Croxall, KV, Deason, AJ, De Lorenzo-Cáceres, A, De Marco, B, Dietrich, M, Di Gesu, L, Ebrero, J, Evans, PA, Filippenko, AV, Flatland, K, Gates, EL, Gehrels, N, Geier, S, Gelbord, JM, Gonzalez, L, Gorjian, V, Grupe, D, Gupta, A, Hall, PB, Henderson, CB, Hicks, S, Holmbeck, E, Holoien, TW-S, Hutchison, TA, Im, M, Jensen, JJ, Johnson, CA, Joner, MD, Kaspi, S, Kelly, BC, Kelly, PL, Kennea, JA, Kim, M, Kim, SC, Kim, SY, King, A, Klimanov, SA, Krongold, Y, and Lau, MW
Subjects: galaxies: active, galaxies: individual, galaxies: nuclei, galaxies: Seyfert, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: We model the ultraviolet spectra of the Seyfert 1 galaxy NGC 5548 obtained with the Hubble Space Telescope during the 6 month reverberation mapping campaign in 2014. Our model of the emission from NGC 5548 corrects for overlying absorption and deblends the individual emission lines. Using the modeled spectra, we measure the response to continuum variations for the deblended and absorption-corrected individual broad emission lines, the velocity-dependent profiles of Ly and C iv, and the narrow and broad intrinsic absorption features. We find that the time lags for the corrected emission lines are comparable to those for the original data. The velocity-binned lag profiles of Ly and C iv have a double-peaked structure indicative of a truncated Keplerian disk. The narrow absorption lines show a delayed response to continuum variations corresponding to recombination in gas with a density of ∼105 cm-3. The high-ionization narrow absorption lines decorrelate from continuum variations during the same period as the broad emission lines. Analyzing the response of these absorption lines during this period shows that the ionizing flux is diminished in strength relative to the far-ultraviolet continuum. The broad absorption lines associated with the X-ray obscurer decrease in strength during this same time interval. The appearance of X-ray obscuration in ∼2012 corresponds with an increase in the luminosity of NGC 5548 following an extended low state. We suggest that the obscurer is a disk wind triggered by the brightening of NGC 5548 following the decrease in size of the broad-line region during the preceding low-luminosity state.
Published: 2019

4. Space Telescope and Optical Reverberation Mapping Project. VII. Understanding the Ultraviolet Anomaly in NGC 5548 with X-Ray Spectroscopy

Author: Mathur, S, Gupta, A, Page, K, Pogge, RW, Krongold, Y, Goad, MR, Adams, SM, Anderson, MD, Arévalo, P, Barth, AJ, Bazhaw, C, Beatty, TG, Bentz, MC, Bigley, A, Bisogni, S, Borman, GA, Boroson, TA, Bottorff, MC, Brandt, WN, Breeveld, AA, Brown, JE, Brown, JS, Cackett, EM, Canalizo, G, Carini, MT, Clubb, KI, Comerford, JM, Coker, CT, Corsini, EM, Crenshaw, DM, Croft, S, Croxall, KV, Bontà, E Dalla, Deason, AJ, Denney, KD, De Lorenzo-Cáceres, A, De Rosa, G, Dietrich, M, Edelson, R, Ely, J, Eracleous, M, Evans, PA, Fausnaugh, MM, Ferland, GJ, Filippenko, AV, Flatland, K, Fox, OD, Gates, EL, Gehrels, N, Geier, S, Gelbord, JM, Gorjian, V, Greene, JE, Grier, CJ, Grupe, D, Hall, PB, Henderson, CB, Hicks, S, Holmbeck, E, Holoien, TW-S, Horenstein, D, Horne, Keith, Hutchison, T, Im, M, Jensen, JJ, Johnson, CA, Joner, MD, Jones, J, Kaastra, J, Kaspi, S, Kelly, BC, Kelly, PL, Kennea, JA, Kim, M, Kim, S, Kim, SC, King, A, Klimanov, SA, Kochanek, CS, Korista, KT, Kriss, GA, Lau, MW, Lee, JC, Leonard, DC, Li, M, Lira, P, Ma, Z, MacInnis, F, Manne-Nicholas, ER, Malkan, MA, Mauerhan, JC, McGurk, R, McHardy, IM, Montouri, C, Morelli, L, Mosquera, A, Mudd, D, Muller-Sanchez, F, Musso, R, and Nazarov, SV
Subjects: galaxies: active, galaxies: individual, X-rays: galaxies, X-rays: individual, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: During the Space Telescope and Optical Reverberation Mapping Project observations of NGC 5548, the continuum and emission-line variability became decorrelated during the second half of the six-month-long observing campaign. Here we present Swift and Chandra X-ray spectra of NGC 5548 obtained as part of the campaign. The Swift spectra show that excess flux (relative to a power-law continuum) in the soft X-ray band appears before the start of the anomalous emission-line behavior, peaks during the period of the anomaly, and then declines. This is a model-independent result suggesting that the soft excess is related to the anomaly. We divide the Swift data into on- and off-anomaly spectra to characterize the soft excess via spectral fitting. The cause of the spectral differences is likely due to a change in the intrinsic spectrum rather than to variable obscuration or partial covering. The Chandra spectra have lower signal-to-noise ratios, but are consistent with the Swift data. Our preferred model of the soft excess is emission from an optically thick, warm Comptonizing corona, the effective optical depth of which increases during the anomaly. This model simultaneously explains all three observations: the UV emission-line flux decrease, the soft-excess increase, and the emission-line anomaly.
Published: 2017

5. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT.VI. REVERBERATING DISK MODELS FOR NGC 5548

Author: Starkey, D, Horne, Keith, Fausnaugh, MM, Peterson, BM, Bentz, MC, Kochanek, CS, Denney, KD, Edelson, R, Goad, MR, De Rosa, G, Anderson, MD, Arévalo, P, Barth, AJ, Bazhaw, C, Borman, GA, Boroson, TA, Bottorff, MC, Brandt, WN, Breeveld, AA, Cackett, EM, Carini, MT, Croxall, KV, Crenshaw, DM, Bontà, E Dalla, De Lorenzo-Cáceres, A, Dietrich, M, Efimova, NV, Ely, J, Evans, PA, Filippenko, AV, Flatland, K, Gehrels, N, Geier, S, Gelbord, JM, Gonzalez, L, Gorjian, V, Grier, CJ, Grupe, D, Hall, PB, Hicks, S, Horenstein, D, Hutchison, T, Im, M, Jensen, JJ, Joner, MD, Jones, J, Kaastra, J, Kaspi, S, Kelly, BC, Kennea, JA, Kim, SC, Kim, M, Klimanov, SA, Korista, KT, Kriss, GA, Lee, JC, Leonard, DC, Lira, P, MacInnis, F, Manne-Nicholas, ER, Mathur, S, McHardy, IM, Montouri, C, Musso, R, Nazarov, SV, Norris, RP, Nousek, JA, Okhmat, DN, Pancoast, A, Parks, JR, Pei, L, Pogge, RW, Pott, J-U, Rafter, SE, Rix, H-W, Saylor, DA, Schimoia, JS, Schnülle, K, Sergeev, SG, Siegel, MH, Spencer, M, Sung, H-I, Teems, KG, Turner, CS, Uttley, P, Vestergaard, M, Villforth, C, Weiss, Y, Woo, J-H, Yan, H, Young, and S, Zheng, W, and Zu, Y
Subjects: accretion, accretion disks, galaxies: active, galaxies: individual, galaxies: nuclei, galaxies: Seyfert, astro-ph.GA, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: We conduct a multiwavelength continuum variability study of the Seyfert 1 galaxy NGC 5548 to investigate the temperature structure of its accretion disk. The 19 overlapping continuum light curves (1158 A oto 9157 A o) combine simultaneous Hubble Space Telescope, Swift, and ground-based observations over a 180 day period from 2014 January to July. Light-curve variability is interpreted as the reverberation response of the accretion disk to irradiation by a central time-varying point source. Our model yields the disk inclination i = 36° ±10° temperature T1 = 44 ±6 ) × 10 3 K at 1 light day from the black hole, and a temperatureradius slope (T ∞r-a) of a = 0.99 ±0.03. We also infer the driving light curve and find that it correlates poorly with both the hard and soft X-ray light curves, suggesting that the X-rays alone may not drive the ultraviolet and optical variability over the observing period. We also decompose the light curves into bright, faint, and mean accretion-disk spectra. These spectra lie below that expected for a standard blackbody accretion disk accreting at L LEdd = 0.1.
Published: 2017

6. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. IV. ANOMALOUS BEHAVIOR OF THE BROAD ULTRAVIOLET EMISSION LINES IN NGC 5548

Author: Goad, MR, Korista, KT, De Rosa, G, Kriss, GA, Edelson, R, Barth, AJ, Ferland, GJ, Kochanek, CS, Netzer, H, Peterson, BM, Bentz, MC, Bisogni, S, Crenshaw, DM, Denney, KD, Ely, J, Fausnaugh, MM, Grier, CJ, Gupta, A, Horne, KD, Kaastra, J, Pancoast, A, Pei, L, Pogge, RW, Skielboe, A, Starkey, D, Vestergaard, M, Zu, Y, Anderson, MD, Arévalo, P, Bazhaw, C, Borman, GA, Boroson, TA, Bottorff, MC, Brandt, WN, Breeveld, AA, Brewer, BJ, Cackett, EM, Carini, MT, Croxall, KV, Bontà, E Dalla, De Lorenzo-Cáceres, A, Dietrich, M, Efimova, NV, Evans, PA, Filippenko, AV, Flatland, K, Gehrels, N, Geier, S, Gelbord, JM, Gonzalez, L, Gorjian, V, Grupe, D, Hall, PB, Hicks, S, Horenstein, D, Hutchison, T, Im, M, Jensen, JJ, Joner, MD, Jones, J, Kaspi, S, Kelly, BC, Kennea, JA, Kim, M, Kim, SC, Klimanov, SA, Lee, JC, Leonard, DC, Lira, P, MacInnis, F, Manne-Nicholas, ER, Mathur, S, McHardy, IM, Montouri, C, Musso, R, Nazarov, SV, Norris, RP, Nousek, JA, Okhmat, DN, Papadakis, I, Parks, JR, Pott, J-U, Rafter, SE, Rix, H-W, Saylor, DA, Schimoia, JS, Schnülle, K, Sergeev, SG, Siegel, M, Spencer, M, Sung, H-I, Teems, KG, Treu, T, Turner, CS, Uttley, P, Villforth, C, Weiss, Y, Woo, J-H, Yan, H, and Young, S
Subjects: galaxies: active, galaxies: individual, galaxies: nuclei, galaxies: Seyfert, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: During an intensive Hubble Space Telescope (HST) Cosmic Origins Spectrograph (COS) UV monitoring campaign of the Seyfert 1 galaxy NGC 5548 performed from 2014 February to July, the normally highly correlated far UV continuum and broad emission line variations decorrelated for ∼60-70 days, starting ∼75 days after the first HST/COS observation. Following this anomalous state, the flux and variability of the broad emission lines returned to a more normal state. This transient behavior, characterized by significant deficits in flux and equivalent width of the strong broad UV emission lines, is the first of its kind to be unambiguously identified in an active galactic nucleus reverberation mapping campaign. The largest corresponding emission line flux deficits occurred for the high ionization, collisionally excited lines C iv and Si iv(+O iv]), and also He ii(+O iii]), while the anomaly in Lywas substantially smaller. This pattern of behavior indicates a depletion in the flux of photons with relative to those near 13.6 eV. We suggest two plausible mechanisms for the observed behavior: (i) temporary obscuration of the ionizing continuum incident upon broad line region (BLR) clouds by a moving veil of material lying between the inner accretion disk and inner (BLR), perhaps resulting from an episodic ejection of material from the disk, or (ii) a temporary change in the intrinsic ionizing continuum spectral energy distribution resulting in a deficit of ionizing photons with energies >54 eV, possibly due to a transient restructuring of the Comptonizing atmosphere above the disk. Current evidence appears to favor the latter explanation.
Published: 2016

7. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. III. OPTICAL CONTINUUM EMISSION AND BROADBAND TIME DELAYS IN NGC 5548

Author: Fausnaugh, MM, Denney, KD, Barth, AJ, Bentz, MC, Bottorff, MC, Carini, MT, Croxall, KV, De Rosa, G, Goad, MR, Horne, Keith, Joner, MD, Kaspi, S, Kim, M, Klimanov, SA, Kochanek, CS, Leonard, DC, Netzer, H, Peterson, BM, Schnülle, K, Sergeev, SG, Vestergaard, M, Zheng, W-K, Zu, Y, Anderson, MD, Arévalo, P, Bazhaw, C, Borman, GA, Boroson, TA, Brandt, WN, Breeveld, AA, Brewer, BJ, Cackett, EM, Crenshaw, DM, Bontà, E Dalla, De Lorenzo-Cáceres, A, Dietrich, M, Edelson, R, Efimova, NV, Ely, J, Evans, PA, Filippenko, AV, Flatland, K, Gehrels, N, Geier, S, Gelbord, JM, Gonzalez, L, Gorjian, V, Grier, CJ, Grupe, D, Hall, PB, Hicks, S, Horenstein, D, Hutchison, T, Im, M, Jensen, JJ, Jones, J, Kaastra, J, Kelly, BC, Kennea, JA, Kim, SC, Korista, KT, Kriss, GA, Lee, JC, Lira, P, MacInnis, F, Manne-Nicholas, ER, Mathur, S, McHardy, IM, Montouri, C, Musso, R, Nazarov, SV, Norris, RP, Nousek, JA, Okhmat, DN, Pancoast, A, Papadakis, I, Parks, JR, Pei, L, Pogge, RW, Pott, J-U, Rafter, SE, Rix, H-W, Saylor, DA, Schimoia, JS, Siegel, M, Spencer, M, Starkey, D, Sung, H-I, Teems, KG, Treu, T, Turner, CS, Uttley, P, Villforth, C, Weiss, Y, Woo, J-H, Yan, H, and Young, S
Subjects: galaxies: active, galaxies: individual, galaxies: nuclei, galaxies: Seyfert, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: We present ground-based optical photometric monitoring data for NGC 5548, part of an extended multiwavelength reverberation mapping campaign. The light curves have nearly daily cadence from 2014 January to July in nine filters (BVRI and ugriz). Combined with ultraviolet data from the Hubble Space Telescope and Swift, we confirm significant time delays between the continuum bands as a function of wavelength, extending the wavelength coverage from 1158 Å to the z band (∼9160 Å). We find that the lags at wavelengths longer than the V band are equal to or greater than the lags of high-ionization-state emission lines (such as He ii and λ1640 and λ4686), suggesting that the continuum-emitting source is of a physical size comparable to the inner broad-line region (BLR). The trend of lag with wavelength is broadly consistent with the prediction for continuum reprocessing by an accretion disk with τ ∝ λ 4 . However, the lags also imply a disk radius that is 3 times larger than the prediction from standard thin-disk theory, assuming that the bolometric luminosity is 10% of the Eddington luminosity (L = 0.1 L Edd ). Using optical spectra from the Large Binocular Telescope, we estimate the bias of the interband continuum lags due to BLR emission observed in the filters. We find that the bias for filters with high levels of BLR contamination (∼20%) can be important for the shortest continuum lags and likely has a significant impact on the u and U bands owing to Balmer continuum emission.
Published: 2016

8. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. II. SWIFT AND HST REVERBERATION MAPPING OF THE ACCRETION DISK OF NGC 5548

Author: Edelson, R, Gelbord, JM, Horne, K, McHardy, IM, Peterson, BM, Arévalo, P, Breeveld, AA, De Rosa, G, Evans, PA, Goad, MR, Kriss, GA, Brandt, WN, Gehrels, N, Grupe, D, Kennea, JA, Kochanek, CS, Nousek, JA, Papadakis, I, Siegel, M, Starkey, D, Uttley, P, Vaughan, S, Young, S, Barth, AJ, Bentz, MC, Brewer, BJ, Crenshaw, DM, Bontà, E Dalla, De Lorenzo- Cáceres, A, Denney, KD, Dietrich, M, Ely, J, Fausnaugh, MM, Grier, CJ, Hall, PB, Kaastra, J, Kelly, BC, Korista, KT, Lira, P, Mathur, S, Netzer, H, Pancoast, A, Pei, L, Pogge, RW, Schimoia, JS, Treu, T, Vestergaard, M, Villforth, C, Yan, H, and Zu, Y
Subjects: galaxies: active, galaxies: individual, galaxies: nuclei, galaxies: Seyfert, astro-ph.GA, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: Recent intensive Swift monitoring of the Seyfert 1 galaxy NGC 5548 yielded 282 usable epochs over 125 days across six UV/optical bands and the X-rays. This is the densest extended active galactic nucleus (AGN) UV/optical continuum sampling ever obtained, with a mean sampling rate
Published: 2015

9. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. I. ULTRAVIOLET OBSERVATIONS OF THE SEYFERT 1 GALAXY NGC 5548 WITH THE COSMIC ORIGINS SPECTROGRAPH ON HUBBLE SPACE TELESCOPE

Author: De Rosa, G, Peterson, BM, Ely, J, Kriss, GA, Crenshaw, DM, Horne, Keith, Korista, KT, Netzer, H, Pogge, RW, Arévalo, P, Barth, AJ, Bentz, MC, Brandt, WN, Breeveld, AA, Brewer, BJ, Bontà, E Dalla, De Lorenzo-Cáceres, A, Denney, KD, Dietrich, M, Edelson, R, Evans, PA, Fausnaugh, MM, Gehrels, N, Gelbord, JM, Goad, MR, Grier, CJ, Grupe, D, Hall, PB, Kaastra, J, Kelly, BC, Kennea, JA, Kochanek, CS, Lira, P, Mathur, S, McHardy, IM, Nousek, JA, Pancoast, A, Papadakis, I, Pei, L, Schimoia, JS, Siegel, M, Starkey, D, Treu, T, Uttley, P, Vaughan, S, Vestergaard, M, Villforth, C, Yan, H, Young, S, and Zu, Y
Subjects: galaxies: active, galaxies: individual, galaxies: nuclei, galaxies: Seyfert, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: We describe the first results from a six-month long reverberation-mapping experiment in the ultraviolet based on 171 observations of the Seyfert 1 galaxy NGC 5548 with the Cosmic Origins Spectrograph on the Hubble Space Telescope. Significant correlated variability is found in the continuum and broad emission lines, with amplitudes ranging from ∼30% to a factor of two in the emission lines and a factor of three in the continuum. The variations of all the strong emission lines lag behind those of the continuum, with He ii lagging behind the continuum by ∼2.5 days and Ly , C iv , and Si iv lagging by ∼5-6 days. The relationship between the continuum and emission lines is complex. In particular, during the second half of the campaign, all emission-line lags increased by a factor of 1.3-2 and differences appear in the detailed structure of the continuum and emission-line light curves. Velocity-resolved cross-correlation analysis shows coherent structure in lag versus line of sight velocity for the emission lines; the high-velocity wings of C iv respond to continuum variations more rapidly than the line core, probably indicating higher velocity broad-line region clouds at smaller distances from the central engine. The velocity-dependent response of Ly, however, is more complex and will require further analysis.
Published: 2015

10. Swift observations of GRB050904: the most distant cosmic explosion ever observed

Author: Cusumano, G, Mangano, V, Chincarini, G, Panaitescu, A, Burrows, D, La Parola, V, Sakamoto, T, Campana, S, Mineo, T, Tagliaferri, G, Angelini, L, Barthelmy, S, Beardmore, A, Boyd, P, Cominsky, L, Gronwall, C, Fenimore, E, Gehrels, N, Giommi, P, Goad, M, Hurley, K, Immler, S, Kennea, J, Mason, K, Marshal, F, Meszaros, P, Nousek, J, Osborne, J, Palmer, D, Roming, P, Wells, A, White, N, Zhang, B, Burrows, DN, Barthelmy, SD, Beardmore, AP, Boyd, PT, Cominsky, LR, Fenimore, EE, Kennea, JA, Mason, KO, Nousek, JA, Osborne, JP, Palmer, DM, Roming, PWA, White, NE, Zhang, B., CHINCARINI, GUIDO, Cusumano, G, Mangano, V, Chincarini, G, Panaitescu, A, Burrows, D, La Parola, V, Sakamoto, T, Campana, S, Mineo, T, Tagliaferri, G, Angelini, L, Barthelmy, S, Beardmore, A, Boyd, P, Cominsky, L, Gronwall, C, Fenimore, E, Gehrels, N, Giommi, P, Goad, M, Hurley, K, Immler, S, Kennea, J, Mason, K, Marshal, F, Meszaros, P, Nousek, J, Osborne, J, Palmer, D, Roming, P, Wells, A, White, N, Zhang, B, Burrows, DN, Barthelmy, SD, Beardmore, AP, Boyd, PT, Cominsky, LR, Fenimore, EE, Kennea, JA, Mason, KO, Nousek, JA, Osborne, JP, Palmer, DM, Roming, PWA, White, NE, Zhang, B., and CHINCARINI, GUIDO
Abstract: Context. Swift discovered the high redshift (z = 6.29) GRB050904 with the Burst Alert Telescope ( BAT) and began observing with its narrow field instruments 161 s after the burst onset. This gamma-ray burst is the most distant cosmic explosion ever observed. Because of its high redshift, the X-ray Telescope (XRT) and BAT simultaneous observations provide 4 orders of magnitude of spectral coverage (0.2-150 keV; 1.4-1090 keV in the source rest frame) at a very early source-frame time (22 s). The X-ray emission was monitored by the XRT up to 10 days after the burst. Aims. We present the analysis of BAT and XRT observations of GRB050904 and a complete description of its high energy phenomenology. Methods. We performed time resolved spectral analysis and light curve modeling. Results. GRB050904 was a long, multi-peaked, bright GRB with strong variability during its entire evolution. The light curve observed by the XRT is characterized by the presence of a long flaring activity lasting up to 1-2 h after the burst onset in the burst rest frame, with no evidence of a smooth power-law decay following the prompt emission as seen in other GRBs. However, the BAT tail extrapolated to the XRT band joins the XRT early light curve and the overall behavior resembles that of a very long GRB prompt. The spectral energy distribution softens with time, with the photon index decreasing from -1.2 during the BAT observation to -1.9 at the end of the XRT observation. The dips of the late X-ray flares may be consistent with an underlying X-ray emission arising from the forward shock and with the properties of the optical afterglow reported by Tagliaferri et al. (2005b, A& A, 443, L1). Conclusions. We interpret the BAT and XRT data as a single continuous observation of the prompt emission from a very long GRB. The peculiarities observed in GRB050904 could be due to its origin within one of the first star-forming regions in the Universe; very low metallicities of the progenitor at these epochs
Published: 2007

11. Swift X-Ray Telescope and Very Large Telescope Observations of the Afterglow of GRB 041223

Author: Burrows, D, Hill, J, Chincarini, G, Tagliaferri, G, Campana, S, Moretti, A, Romano, P, Malesani, D, Racusin, J, Kobayashi, S, Zhang, B, Mészáros, P, O'Brien, P, Willingale, R, Osborne, J, Cusumano, G, Giommi, P, Angelini, L, Abbey, A, Antonelli, L, Beardmore, A, Capalbi, M, Covino, S, D'Avanzo, P, Goad, M, Kennea, J, Morris, D, Pagani, C, Page, K, Stella, L, Nousek, J, Wells, A, Gehrels, N, Burrows, DN, Hill, JE, Racusin, JL, O'Brien, PT, Osborne, JP, Abbey, AF, Antonelli, LA, Beardmore, AP, Goad, MR, Kennea, JA, Morris, DC, Page, KL, Nousek, JA, Wells, AA, Gehrels, N., CHINCARINI, GUIDO, Burrows, D, Hill, J, Chincarini, G, Tagliaferri, G, Campana, S, Moretti, A, Romano, P, Malesani, D, Racusin, J, Kobayashi, S, Zhang, B, Mészáros, P, O'Brien, P, Willingale, R, Osborne, J, Cusumano, G, Giommi, P, Angelini, L, Abbey, A, Antonelli, L, Beardmore, A, Capalbi, M, Covino, S, D'Avanzo, P, Goad, M, Kennea, J, Morris, D, Pagani, C, Page, K, Stella, L, Nousek, J, Wells, A, Gehrels, N, Burrows, DN, Hill, JE, Racusin, JL, O'Brien, PT, Osborne, JP, Abbey, AF, Antonelli, LA, Beardmore, AP, Goad, MR, Kennea, JA, Morris, DC, Page, KL, Nousek, JA, Wells, AA, Gehrels, N., and CHINCARINI, GUIDO
Abstract: GRB 041223 was the first gamma-ray burst detected by the Swift X-Ray Telescope (XRT), beginning 4.6 hr after the burst. The X-ray detection triggered a VLT observation of the optical/near-infrared (NIR) counterpart, located about 1′′.1 from the XRT position. The X-ray counterpart faded rapidly, with a power-law index of - 1.72 ± 0.20, with an average unabsorbed X-ray flux of 6.5 × 10-12 ergs cm-2 s-1 in the 0.5-10 keV band for a power-law spectrum of photon index 2.02 ± 0.13 with Galactic absorption. The NIR counterpart was observed at three epochs between 16 and 87 hr after the burst and faded with a power-law index of -1.14 ± 0.08 with a reddening-corrected spectral energy distribution power-law slope of -0.40 ± 0.03. We find that the X-ray and NIR data are consistent with a two-component jet in a wind medium. © 2005. The American Astronomical Society. All rights reserved.
Published: 2005

12. SUPPLEMENT: 'lOCALIZATION and BROADBAND FOLLOW-UP of the GRAVITATIONAL-WAVE TRANSIENT GW150914' (2016, ApJL, 826, L13)

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Blackburn, JK, Blair, CD, Blair, DG, Blair, RM, Bloemen, S, Bock, O, Bodiya, TP, Boer, M, Bogaert, G, Bogan, C, Bohe, A, Bojtos, P, Bond, C, Bondu, F, Bonnand, R, Boom, BA, Bork, R, Boschi, V, Bose, S, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, PR, Braginsky, VB, Branchesi, M, Brau, JE, Briant, T, Brillet, A, Brinkmann, M, Brisson, V, Brockill, P, Brooks, AF, Brown, DA, Brown, DD, Brown, NM, Buchanan, CC, Buikema, A, Bulik, T, Bulten, HJ, Buonanno, A, Buskulic, D, Buy, C, Byer, RL, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, JC, Callister, T, Calloni, E, Camp, JB, Cannon, KC, Cao, J, Capano, CD, Capocasa, E, Carbognani, F, Caride, S, Diaz, JC, Casentini, C, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cepeda, CB, Baiardi, LC, Cerretani, G, Cesarini, E, Chakraborty, R, Chalermsongsak, T, Chamberlin, SJ, Chan, M, Chao, S, Charlton, P, Chassande-Mottin, E, Chen, HY, Chen, Y, Cheng, C, Chincarini, A, Chiummo, A, Cho, HS, Cho, M, Chow, JH, Christensen, N, Chu, Q, 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Observ, Inst Astrofis Canarias, Irkutsk State Univ, RAS, Blagoveschensk State Pedag Univ, Tokyo Inst Technol, RIKEN, Nihon Univ, Japan Aerosp Explorat Agcy, Japan Aerosp Explorat Agcy JAXA, Osaka Univ, Eureka Sci Inc, Curtin Univ, Victoria Univ Wellington, Ist Nazl Astrofis, Queens Univ Belfast, Univ Hawaii Manoa, Space Telescope Sci Inst, Harvard Univ, Millennium Inst Astrophys, Univ Andres Bello, European Southern Observ, Univ Turku, Univ Chile, Las Cumbres Observ Global Telescope Network, Univ Calif Santa Barbara, Univ Warsaw, Polish Acad Sci, Univ Leicester, CNRS UMR 5277 UPS, Univ Texas San Antonio, Univ Nacl Cordoba, The LIGO Scientific Collaboration, The Virgo Collaboration, The Australian Square Kilometer Array, Pathfinder (ASKAP) Collaboration, The BOOTES Collaboration, The Dark Energy Survey and the Dark Energy Camera GW-EM Collaborations, The Fermi GBM Collaboration, The Fermi LAT Collaboration, The GRAvitational Wave Inaf TeAm (GRAWITA), The Intermediate Palomar Transient Factory (iPTF) Collaboration, The InterPlanetary Network, The J-GEM Collaboration, The La Silla--QUEST Survey, The Liverpool Telescope Collaboration, The Low Frequency Array (LOFAR) Collaboration, The MASTER Collaboration, The MAXI Collaboration, The Murchison Wide-field Array (MWA) Collaboration, The Pan-STARRS Collaboration, The PESSTO Collaboration, The Pi of the Sky Collaboration, The SkyMapper Collaboration, The Swift Collaboration, The TAROT, Zadko, Algerian National Observatory, C2PU Collaboration, The TOROS Collaboration, The VISTA Collaboration, Abbott BP, Abbott R, Abbott TD, Abernathy MR, Acernese F, Ackley K, Adams C, Adams T, Addesso P, Adhikari RX, Adya VB, Affeldt C, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Allen B, Allocca A, Altin PA, Anderson SB, Anderson WG, Arai K, Araya MC, Arceneaux CC, Areeda JS, Arnaud N, Arun KG, Ascenzi S, Ashton G, Ast M, Aston SM, Astone P, Aufmuth P, Aulbert C, Babak S, Bacon P, Bader MKM, Baker PT, Baldaccini F, Ballardin G, Ballmer SW, Barayoga JC, Barclay SE, Barish BC, Barker D, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Barthelmy S, Bartlett J, Bartos I, Bassiri R, Basti A, Batch JC, Baune C, Bavigadda V, Bazzan M, Behnke B, Bejger M, Bell AS, Bell CJ, Berger BK, Bergman J, Bergmann G, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Bhagwat S, Bhandare R, Bilenko IA, Billingsley G, Birch J, Birney R, Biscans S, Bisht A, Bitossi M, Biwer C, Bizouard MA, Blackburn JK, Blair CD, Blair DG, Blair RM, Bloemen S, Bock O, Bodiya TP, Boer M, Bogaert G, Bogan C, Bohe A, Bojtos P, Bond C, Bondu F, Bonnand R, Boom BA, Bork R, Boschi V, Bose S, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Braginsky VB, Branchesi M, Brau JE, Briant T, Brillet A, Brinkmann M, Brisson V, Brockill P, Brooks AF, Brown DA, Brown DD, Brown NM, Buchanan CC, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buskulic D, Buy C, Byer RL, Cadonati L, Cagnoli G, Cahillane C, Bustillo JC, Callister T, Calloni E, Camp JB, Cannon KC, Cao J, Capano CD, Capocasa E, Carbognani F, Caride S, Diaz JC, Casentini C, Caudill S, Cavaglia M, Cavalier F, Cavalieri R, Cella G, Cepeda CB, Baiardi LC, Cerretani G, Cesarini E, Chakraborty R, Chalermsongsak T, Chamberlin SJ, Chan M, Chao S, Charlton P, Chassande-Mottin E, Chen HY, Chen Y, Cheng C, Chincarini A, Chiummo A, Cho HS, Cho M, Chow JH, Christensen N, Chu Q, Chua S, Chung S, Ciani G, Clara F, Clark JA, Cleva F, Coccia E, Cohadon PF, Colla A, Collette CG, Cominsky L, Constancio M, Conte A, Conti L, Cook D, Corbitt TR, Cornish N, Corsi A, Cortese S, Costa CA, Coughlin MW, Coughlin SB, Coulon JP, Countryman ST, Couvares P, Cowan EE, Coward DM, Cowart MJ, Coyne DC, Coyne R, Craig K, Creighton JDE, Cripe J, Crowder SG, Cumming A, Cunningham L, Cuoco E, Dal Canton T, Danilishin SL, D'Antonio S, Danzmann K, Darman NS, Dattilo V, Dave I, Daveloza HP, Davier M, Davies GS, Daw EJ, Day R, DeBra D, Debreczeni G, Degallaix J, De Laurentis M, Deleglise S, Del Pozzo W, Denker T, Dent T, Dereli H, Dergachev V, DeRosa RT, De Rosa R, DeSalvo R, Dhurandhar S, Diaz MC, 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 KL, Doravari S, Douglas R, Downes TP, Drago M, Drever RWP, Driggers JC, Du Z, Ducrot M, Dwyer SE, Edo TB, Edwards MC, Effler A, Eggenstein HB, Ehrens P, Eichholz J, Eikenberry SS, Engels W, Essick RC, Etzel T, Evans M, Evans TM, Everett R, Factourovich M, Fafone V, Fair H, Fairhurst S, Fan X, Fang Q, Farinon S, Farr B, Farr WM, Favata M, Fays M, Fehrmann H, Fejer MM, Ferrante I, Ferreira EC, Ferrini F, Fidecaro F, Fiori I, Fiorucci D, Fisher RP, Flaminio R, Fletcher M, Fournier JD, Franco S, Frasca S, Frasconi F, Frei Z, Freise A, Frey R, Frey V, Fricke TT, Fritschel P, Frolov VV, Fulda P, Fyffe M, Gabbard HAG, Gair JR, Gammaitoni L, Gaonkar SG, 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 JA, Giardina KD, Giazotto A, Gill K, Glaefke A, Goetz E, Goetz R, Gondan L, Gonzalez G, Castro JMG, Gopakumar A, Gordon NA, Gorodetsky ML, Gossan SE, Gosselin M, Gouaty R, Graef C, Graff PB, Granata M, Grant A, Gras S, Gray C, Greco G, Green AC, Groot P, Grote H, Grunewald S, Guidi GM, Guo X, Gupta A, Gupta MK, Gushwa KE, Gustafson EK, Gustafson R, Hacker JJ, Hall BR, Hall ED, Hammond G, Haney M, Hanke MM, Hanks J, Hanna C, Hannam MD, Hanson J, Hardwick T, Haris K, Harms J, Harry GM, Harry IW, Hart MJ, Hartman MT, Haster CJ, Haughian K, Heidmann A, Heintze MC, Heitmann H, Hello P, Hemming G, Hendry M, Heng IS, Hennig J, Heptonstall AW, Heurs M, Hild S, Hoak D, Hodge KA, Hofman D, Hollitt SE, Holt K, Holz DE, Hopkins P, Hosken DJ, Hough J, Houston EA, Howell EJ, Hu YM, Huang S, Huerta EA, Huet D, Hughey B, Husa S, Huttner SH, Huynh-Dinh T, Idrisy A, Indik N, Ingram DR, Inta R, Isa HN, Isac JM, Isi M, Islas G, Isogai T, Iyer BR, Izumi K, Jacqmin T, Jang H, Jani K, Jaranowski P, Jawahar S, Jimenez-Forteza F, Johnson WW, Jones DI, Jones R, Jonker RJG, Ju L, Kalaghatgi CV, Kalogera V, Kandhasamy S, Kang G, Kanner JB, Karki S, Kasprzack M, Katsavounidis E, Katzman W, Kaufer S, Kaur T, Kawabe K, Kawazoe F, Kefelian F, Kehl MS, Keitel D, Kelley DB, Kells W, Kennedy R, Key JS, Khalaidovski A, Khalili FY, Khan I, Khan S, Khan Z, Khazanov EA, Kijbunchoo N, Kim C, Kim J, Kim K, Kim N, Kim YM, King EJ, King PJ, Kinzel DL, Kissel JS, Kleybolte L, Klimenko S, Koehlenbeck SM, Kokeyama K, Koley S, Kondrashov V, Kontos A, Korobko M, Korth WZ, Kowalska I, Kozak DB, Kringel V, Krolak A, Krueger C, Kuehn G, Kumar P, Kuo L, Kutynia A, Lackey BD, Landry M, Lange J, Lantz B, Lasky PD, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lebigot EO, Lee CH, Lee HK, Lee HM, Lee K, Lenon A, Leonardi M, Leong JR, Leroy N, Letendre N, Levin Y, Levine BM, Li TGF, Libson A, Littenberg TB, Lockerbie NA, Logue J, Lombardi AL, Lord JE, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lough JD, Luck H, Lundgren P, Luo J, Lynch R, Ma Y, MacDonald T, Machenschalk B, MacInnis M, Macleod DM, Magana-Sandoval F, Magee RM, Mageswaran M, Majorana E, Maksimovic I, Malvezzi V, Man N, Mandel I, Mandic V, Mangano V, Mansell GL, Manske M, Mantovani M, Marchesoni F, Marion F, Marka S, Marka Z, Markosyan AS, Maros E, Martelli F, Martellini L, Martin IW, Martin RM, Martynov DV, Marx JN, Mason K, Masserot A, Massinger TJ, Masso-Reid M, Matichard F, Matone L, Mavalvala N, Mazumder N, Mazzolo G, McCarthy R, McClelland DE, McCormick S, McGuire SC, McIntyre G, McIver J, McManus DJ, McWilliams ST, Meacher D, Meadors GD, Meidam J, Melatos A, Mendell G, Mendoza-Gandara D, Mercer RA, Merilh E, Merzougui M, Meshkov S, Messenger C, Messick C, Meyers PM, Mezzani F, Miao H, Michel C, Middleton H, Mikhailov EE, Milano L, Miller J, Millhouse M, Minenkov Y, Ming J, Mirshekari S, Mishra C, Mitra S, Mitrofanov VP, Mitselmakher G, Mittleman R, Moggi A, Mohan M, Mohapatra SRP, Montani M, Moore BC, Moore CJ, Moraru D, Moreno G, Morriss SR, Mossavi K, Mours B, Mow-Lowry CM, Mueller CL, Mueller G, Muir AW, Mukherjee A, Mukherjee D, Mukherjee S, Mukund N, Mullavey A, Munch J, Murphy DJ, Murray PG, Mytidis A, Nardecchia I, Naticchioni L, Nayak RK, Necula V, Nedkova K, Nelemans G, Neri M, Neunzert A, Newton G, Nguyen TT, Nielsen AB, Nissanke S, Nitz A, Nocera F, Nolting D, Normandin MEN, Nuttall LK, Oberling J, Ochsner E, O'Dell J, Oelker E, Ogin GH, Oh JJ, Oh SH, Ohme F, Oliver M, Oppermann P, Oram RJ, O'Reilly B, O'Shaughnessy R, Ottaway DJ, Ottens RS, Overmier H, Owen BJ, Pai A, Pai SA, Palamos JR, Palashov O, Palliyaguru N, Palomba C, Pal-Singh A, Pan H, Pankow C, Pannarale F, Pant BC, Paoletti F, Paoli A, Papa MA, Paris HR, Parker W, Pascucci D, Pasqualetti A, Passaquieti R, Passuello D, Patricelli B, Patrick Z, Pearlstone BL, 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 IM, Pitkin M, Poggiani R, Popolizio P, Post A, Powell J, Prasad J, Predoi V, Premachandra SS, Prestegard T, Price LR, Prijatelj M, Principe M, Privitera S, Prodi GA, Prokhorov L, Puncken O, Punturo M, Puppo P, Purrer M, Qi H, Qin J, Quetschke V, Quintero EA, Quitzow-James R, Raab FJ, Rabeling DS, Radkins H, Raffai P, Raja S, Rakhmanov M, Rapagnani P, Raymond V, Razzano M, Re V, Read J, Reed CM, Regimbau T, Rei L, Reid S, Reitze DH, Rew H, Reyes SD, Ricci F, Riles K, Robertson NA, Robie R, Robinet F, Rocchi A, Rolland L, Rollins JG, Roma VJ, Romano R, Romanov G, Romie JH, Rosinska D, Rowan S, Rudiger A, Ruggi P, Ryan K, Sachdev S, Sadecki T, Sadeghian L, Salconi L, Saleem M, Salemi F, Samajdar A, Sammut L, Sanchez EJ, Sandberg V, Sandeen B, Sanders JR, Sassolas B, Sathyaprakash BS, Saulson PR, Sauter O, Savage RL, Sawadsky A, Schale P, Schilling R, Schmidt J, Schmidt P, Schnabel R, Schofield RMS, Schonbeck A, Schreiber E, Schuette D, Schutz BF, Scott J, Scott SM, Sellers D, Sentenac D, Sequino V, Sergeev A, Serna G, Setyawati Y, Sevigny A, Shaddock DA, Shah S, Shahriar MS, Shaltev M, Shao Z, Shapiro B, Shawhan P, Sheperd A, Shoemaker DH, Shoemaker DM, Siellez K, Siemens X, Sigg D, Silva AD, Simakov D, Singer A, Singh A, Singh R, Singhal A, Sintes AM, Slagmolen BJJ, Smith JR, Smith ND, Smith RJE, Son EJ, Sorazu B, Sorrentino F, Souradeep T, Srivastava AK, Staley A, Steinke M, Steinlechner J, Steinlechner S, Steinmeyer D, Stephens BC, Stone R, Strain KA, Straniero N, Stratta G, Strauss NA, Strigin S, Sturani R, Stuver AL, Summerscales TZ, Sun L, Sutton PJ, Swinkels BL, SzczepaNczyk MJ, Tacca M, Talukder D, Tanner DB, Tpai M, Tarabrin SP, Taracchini A, Taylor R, Theeg T, Thirugnanasambandam P, Thomas EG, Thomas M, Thomas P, Thorne KA, Thorne KS, Thrane E, Tiwari S, Tiwari V, Tokmakov KV, Tomlinson C, Tonelli M, Torres CV, Torrie CI, Tyr D, Travasso F, Traylor G, Trifiro D, Tringali MC, Trozzo L, Tse M, Turconi M, Tuyenbayev D, Ugolini D, Unnikrishnan CS, Urban AL, Usman SA, Vahlbruch H, Vajente G, Valdes G, van Bakel N, van Beuzekom M, van den Brand JFJ, Van den Broeck C, Vander-Hyde DC, van der Schaaf L, van Heijningen JV, van Veggel AA, Vardaro M, Vass S, Vasuth M, Vaulin R, Vecchio A, Vedovato G, Veitch J, Veitch PJ, Venkateswara K, Verkindt D, Vetrano F, Vicere A, Vinciguerra S, Vine DJ, Vinet JY, Vitale S, Vo T, Vocca H, Vorvick C, Voss D, Vousden WD, Vyatchanin SP, Wade AR, Wade LE, Wade M, Walker M, Wallace L, Walsh S, Wang G, Wang H, Wang M, Wang X, Wang Y, Ward RL, Warner J, Was M, Weaver B, Wei LW, Weinert M, Weinstein AJ, Weiss R, Welborn T, Wen L, Wessels P, Westphal T, Wette K, Whelan JT, White DJ, Whiting BF, Williams RD, Williamson AR, Willis JL, Willke B, Wimmer MH, Winkler W, Wipf CC, Wittel H, Woan G, Worden J, Wright JL, Wu G, Yablon J, Yam W, Yamamoto H, Yancey CC, Yap MJ, Yu H, Yvert M, Zadrozny A, Zangrando L, Zanolin M, Zendri JP, Zevin M, Zhang F, Zhang L, Zhang M, Zhang Y, Zhao C, Zhou M, Zhou Z, Zhu XJ, Zucker ME, Zuraw SE, Zweizig J, Allison J, Bannister K, Bell ME, Chatterjee S, Chippendale AP, Edwards PG, Harvey-Smith L, Heywood I, Hotan A, Indermuehle B, Marvil J, McConnell D, Murphy T, Popping A, Reynolds J, Sault RJ, Voronkov MA, Whiting MT, Castro-Tirado AJ, Cunniffe R, Jelinek M, Tello JC, Oates SR, Hu YD, Kubanek P, Guziy S, Castellon A, Garcia-Cerezo A, Munoz VF, del Pulgar CP, Castillo-Carrion S, Ceron JMC, Hudec R, Caballero-Garcia MD, Pata P, Vitek S, Adame JA, Konig S, Rendon F, Sanguino TDM, Fernandez-Munoz R, Yock PC, Rattenbury N, Allen WH, Querel R, Jeong S, Park IH, Bai J, Cui C, Fan Y, Wang C, Hiriart D, Lee WH, Claret A, Sanchez-Ramirez R, Pandey SB, Mediavilla T, Sabau-Graziati L, Abbott TMC, Abdalla FB, Allam S, Annis J, Armstrong R, Benoit-Levy A, Berger E, Bernstein RA, Bertin E, Brout D, Buckley-Geer E, Burke DL, Capozzi D, Carretero J, Castander FJ, Chornock R, Cowperthwaite PS, Crocce M, Cunha CE, D'Andrea CB, da Costa LN, Desai S, Diehl HT, Dietrich JP, Doctor Z, Drlica-Wagner A, Drout MR, Eifler TF, Estrada J, Evrard AE, Fernandez E, Finley DA, Flaugher B, Foley RJ, Fong WF, Fosalba P, Fox DB, Frieman J, Fryer CL, Gaztanaga E, Gerdes DW, Goldstein DA, Gruen D, Gruendl RA, Gutierrez G, Herner K, Honscheid K, James DJ, Johnson MD, Johnson MWG, Karliner I, Kasen D, Kent S, Kessler R, Kim AG, Kind MC, Kuehn K, Kuropatkin N, Lahav O, Li TS, Lima M, Lin H, Maia MAG, Margutti R, Marriner J, Martini P, Matheson T, Melchior P, Metzger BD, Miller CJ, Miquel R, Neilsen E, Nichol RC, Nord B, Nugent P, Ogando R, Petravick D, Plazas AA, Quataert E, Roe N, Romer AK, Roodman A, Rosell AC, Rykoff ES, Sako M, Sanchez E, Scarpine V, Schindler R, Schubnell M, Scolnic D, Sevilla-Noarbe I, Sheldon E, Smith N, Smith RC, Soares-Santos M, Sobreira F, Stebbins A, Suchyta E, Swanson MEC, Tarle G, Thaler J, Thomas D, Thomas RC, Tucker DL, Vikram V, Walker AR, Wechsler RH, Wester W, Yanny B, Zuntz J, Connaughton V, Burns E, Goldstein A, Briggs MS, Zhang BB, Hui CM, Jenke P, Wilson-Hodge CA, Bhat PN, Bissaldi E, Cleveland W, Fitzpatrick G, Giles MM, Gibby MH, Greiner J, von Kienlin A, Kippen RM, McBreen S, Mailyan B, Meegan CA, Paciesas WS, Preece RD, Roberts O, Sparke L, Stanbro M, Toelge K, Veres P, Yu HF, Blackburn L, Ackermann M, Ajello M, Albert A, Anderson B, Atwood WB, Axelsson M, Baldini L, Barbiellini G, Bastieri D, Bellazzini R, Blandford RD, Bloom ED, Bonino R, Bottacini E, Brandt TJ, Bruel P, Buson S, Caliandro GA, Cameron RA, Caragiulo M, Caraveo PA, Cavazzuti E, Charles E, Chekhtman A, Chiang J, Chiaro G, Ciprini S, Cohen-Tanugi J, Cominsky LR, Costanza F, Cuoco A, DAmmando F, de Palma F, Desiante R, Digel SW, Di Lalla N, Di Mauro M, Di Venere L, Dominguez A, Drell PS, Dubois R, Favuzzi C, Ferrara EC, 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 GA, Green D, Grenier IA, Grove JE, Guiriec S, Hadasch D, Harding AK, Hays E, Hewitt JW, Hill AB, Horan D, Jogler T, Johannesson G, Johnson AS, Kensei S, Kocevski D, Kuss M, La Mura G, Larsson S, Latronico L, Li J, Li L, Longo F, Loparco F, Lovellette MN, Lubrano P, Magill J, Maldera S, Manfreda A, Marelli M, Mayer M, Mazziotta MN, McEnery JE, Meyer M, Michelson PF, Mirabal N, Mizuno T, Moiseev AA, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Negro M, Nuss E, Ohsugi T, Omodei N, Orienti M, Orlando E, Ormes JF, Paneque D, Perkins JS, Pesce-Rollins M, Piron F, Pivato G, Porter TA, Racusin JL, Raino S, Rando R, Razzaque S, Reimer A, Reimer O, Salvetti D, Parkinson PMS, Sgro C, Simone D, Siskind EJ, Spada F, Spandre G, Spinelli P, Suson DJ, Tajima H, Thayer JB, Thompson DJ, Tibaldo L, Torres DF, Troja E, Uchiyama Y, Venters TM, Vianello G, Wood KS, Wood M, Zhu S, Zimmer S, Brocato E, Cappellaro E, Covino S, Grado A, Nicastro L, Palazzi E, Pian E, Amati L, Antonelli LA, 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 TJL, Ferrigno C, Hanlon L, Kuulkers E, Laurent P, Mereghetti S, Roques JP, Savchenko V, Ubertini P, Kasliwal MM, Singer LP, Cao Y, Duggan G, Kulkarni SR, Bhalerao V, Miller AA, 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 SV, Aptekar RL, Frederiks DD, Svinkin DS, Rau A, Zhang X, Smith DM, Cline T, Krimm H, Abe F, Doi M, Fujisawa K, Kawabata KS, Morokuma T, Motohara K, Tanaka M, Ohta K, Yanagisawa K, Yoshida M, Baltay C, Rabinowitz D, Ellman N, Rostami S, Bersier DF, Bode MF, Collins CA, Copperwheat CM, Darnley MJ, Galloway DK, Gomboc A, Kobayashi S, Mazzali P, Mundell CG, Piascik AS, Pollacco D, Steele IA, Ulaczyk K, Broderick JW, Fender RP, Jonker PG, Rowlinson A, Stappers BW, Wijers RAMJ, Lipunov V, Gorbovskoy E, Tyurina N, Kornilov V, Balanutsa P, Kuznetsov A, Buckley D, Rebolo R, Serra-Ricart M, Israelian G, Budnev NM, 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 TMO, Gaensler BM, Johnston-Hollitt M, Kaplan DL, Morales MF, Tingay SJ, Wayth RB, Williams A, Smartt SJ, Chambers KC, Smith KW, Huber ME, Young DR, Wright DE, Schultz A, Denneau L, Flewelling H, Magnier EA, Primak N, Rest A, Sherstyuk A, Stalder B, Stubbs CW, Tonry J, Waters C, Willman M, Olivares F, Campbell H, Kotak R, Sollerman J, Smith M, Dennefeld M, Anderson JP, Botticella MT, Chen TW, Valle MD, Elias-Rosa N, Fraser M, Inserra C, Kankare E, Kupfer T, Harmanen J, Galbany L, Le Guillou L, Lyman JD, Maguire K, Mitra A, Nicholl M, Razza A, Terreran G, Valenti S, Gal-Yam A, Cwiek A, Cwiok M, Mankiewicz L, Opiela R, Zaremba M, Zarnecki AF, Onken CA, Scalzo RA, Schmidt BP, Wolf C, Yuan F, Evans PA, Kennea JA, Burrows DN, Campana S, Cenko SB, Marshall FE, Nousek J, O'Brien P, Osborne JP, Palmer D, Perri M, Siegel M, Tagliaferri G, Klotz A, Turpin D, Laugier R, Beroiz M, Penuela T, Macri LM, Oelkers RJ, Lambas DG, Vrech R, Cabral J, Colazo C, Dominguez M, Sanchez B, Gurovich S, Lares M, Marshall JL, Depoy DL, Padilla N, Pereyra NA, Benacquista M, Tanvir NR, Wiersema K, Levan AJ, Steeghs D, Hjorth J, Fynbo JPU, Malesani D, Milvang-Jensen B, Watson D, Irwin M, Fernandez CG, McMahon RG, Banerji M, Gonzalez-Solares E, Schulze S, Postigo AD, Thoene CC, Cano Z, and Rosswog S
Subjects: TELESCOPE, gravitational waves – methods: observational, Astronomy, media_common.quotation_subject, observational [methods], GW150914, ADVANCED LIGO, supplement, 01 natural sciences, localization, SEARCH, Computer Science::Multimedia, 0103 physical sciences, Broadband, EM follow-up, 010303 astronomy & astrophysics, gravitational wave, QC, media_common, QB, Physics, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Gravitational waves, methods: observational, Space and Planetary Science, Astronomy and Astrophysic, Computational physics, GW150914, localization, EM follow-up, supplement, gravitational waves, Sky, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, DARK ENERGY, Transient (oscillation), Current (fluid), SYSTEM
Abstract: Made available in DSpace on 2018-11-26T16:56:32Z (GMT). No. of bitstreams: 0 Previous issue date: 2016-07-01 United States National Science Foundation (NSF) Science and Technology Facilities Council (STFC) of the United Kingdom Max-Planck Society State of Niedersachsen/Germany Australian Research Council Netherlands Organisation for Scientific Research EGO consortium Council of Scientific and Industrial Research of India Department of Science and Technology, India Science & Engineering Research Board (SERB), India Ministry of Human Resource Development, India Spanish Ministerio de Economia y Competitividad Conselleria d'Economia i Competitivitat and Conselleria d'Educacio Cultura i Universitats of the Govern de les Illes Balears National Science Centre of Poland European Commission Royal Society Scottish Funding Council Scottish Universities Physics Alliance Hungarian Scientific Research Fund (OTKA) Lyon Institute of Origins (LIO) National Research Foundation of Korea Industry Canada Province of Ontario through Ministry of Economic Development and Innovation National Science and Engineering Research Council Canada Canadian Institute for Advanced Research Brazilian Ministry of Science, Technology, and Innovation Russian Foundation for Basic Research Leverhulme Trust Research Corporation Ministry of Science and Technology (MOST), Taiwan Kavli Foundation Australian Government National Collaborative Research Infrastructure Strategy Government of Western Australia United States Department of Energy United States National Science Foundation Ministry of Science and Education of Spain Science and Technology Facilities Council of the United Kingdom Higher Education Funding Council for England National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign Kavli Institute of Cosmological Physics at the University of Chicago Center for Cosmology and Astro-Particle Physics at the Ohio State University Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University Financiadora de Estudos e Projetos Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ) Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) Ministerio da Ciencia, Tecnologia e Inovacao Deutsche Forschungsgemeinschaft Collaborating Institutions in the Dark Energy Survey National Science Foundation MINECO Centro de Excelencia Severo Ochoa European Research Council under European Union's Seventh Framework Programme ERC NASA (United States) DOE (United States) IN2P3/CNRS (France) CEA/Irfu (France) ASI (Italy) INFN (Italy) MEXT (Japan) KEK (Japan) JAXA (Japan) Wallenberg Foundation Swedish Research Council National Space Board (Sweden) NASA in the United States DRL in Germany INAF for the project Gravitational Wave Astronomy with the first detections of adLIGO and adVIRGO experiments ESA (Denmark) ESA (France) ESA (Germany) ESA (Italy) ESA (Switzerland) ESA (Spain) German INTEGRAL through DLR grant US under NASA Grant National Science Foundation PIRE program grant Hubble Fellowship KAKENHI of MEXT Japan JSPS Optical and Near-Infrared Astronomy Inter-University Cooperation Program - MEXT UK Science and Technology Facilities Council ERC Advanced Investigator Grant Lomonosov Moscow State University Development programm Moscow Union OPTICA Russian Science Foundation National Research Foundation of South Africa Australian Government Department of Industry and Science and Department of Education (National Collaborative Research Infrastructure Strategy: NCRIS) NVIDIA at Harvard University University of Hawaii National Aeronautics and Space Administration's Planetary Defense Office Queen's University Belfast National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate European Research Council under European Union's Seventh Framework Programme/ERC STFC grants European Union FP7 programme through ERC STFC through an Ernest Rutherford Fellowship FONDECYT Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) NASA in the US This Supplement provides supporting material for Abbott et al. (2016a). 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. UK Space Agency in the UK Agenzia Spaziale Italiana (ASI) in Italy Ministerio de Ciencia y Tecnologia (MinCyT) Consejo Nacional de Investigaciones Cientificas y Tecnologicas (CONICET) from Argentina USA NSF PHYS NSF ICREA Science and Technology Facilities Council UK Space Agency CALTECH, LIGO, Pasadena, CA 91125 USA Louisiana State Univ, Baton Rouge, LA 70803 USA Univ Salerno, I-84084 Salerno, Italy Ist Nazl Fis Nucl, Sez Napoli, Complesso Univ Monte S Angelo, I-80126 Naples, Italy Univ Florida, Gainesville, FL 32611 USA LIGO Livingston Observ, Livingston, LA 70754 USA Univ Savoie Mt Blanc, CNRS IN2P3, Lab Annecy le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany Nikhef, Sci Pk, NL-1098 XG Amsterdam, Netherlands MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bangalore 560012, Karnataka, India Univ Wisconsin Milwaukee, Milwaukee, WI 53201 USA Leibniz Univ Hannover, D-30167 Hannover, Germany Univ Pisa, I-56127 Pisa, Italy Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia Univ Mississippi, University, MS 38677 USA Calif State Univ Fullerton, Fullerton, CA 92831 USA Univ Paris 11, Univ Paris Saclay, CNRS, LAL,IN2P3, Orsay, France Chennai Math Inst, Chennai, Tamil Nadu, India Univ Roma Tor Vergata, I-00133 Rome, Italy Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England Univ Hamburg, D-22761 Hamburg, Germany INFN, Sez Roma, I-00185 Rome, Italy Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS,IN2P3,CEA,Irfu, F-75205 Paris 13, France Montana State Univ, Bozeman, MT 59717 USA Univ Perugia, I-06123 Perugia, Italy Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy EGO, I-56021 Pisa, Italy Syracuse Univ, Syracuse, NY 13244 USA Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland LIGO Hanford Observ, Richland, WA 99352 USA Wigner RCP, RMKI, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA Columbia Univ, New York, NY 10027 USA Stanford Univ, Stanford, CA 94305 USA Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy INFN, Sez Padova, I-35131 Padua, Italy CAMK PAN, PL-00716 Warsaw, Poland Univ Birmingham, Birmingham B15 2TT, W Midlands, England Univ Genoa, I-16146 Genoa, Italy INFN, Sez Genova, I-16146 Genoa, Italy RRCAT, Indore 452013, MP, India Lomonosov Moscow State Univ, Fac Phys, Moscow 119991, Russia Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland Univ Western Australia, Crawley, WA 6009, Australia Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands Univ Cote dAzur, CNRS, Observ Cote dAzur, Artemis, CS 34229, Nice 4, France MTA Eotvos Univ, Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France Washington State Univ, Pullman, WA 99164 USA Univ Urbino Carlo Bo, I-61029 Urbino, Italy INFN, Sez Firenze, I-50019 Florence, Italy Univ Oregon, Eugene, OR 97403 USA UPMC, Sorbonne Univ, PSL Res Univ, CNRS,ENS,Coll France,Lab Kastler Brossel, F-75005 Paris, France Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands Univ Maryland, College Pk, MD 20742 USA Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA Univ Lyon 1, UMR CNRS 5306, Inst Lumiere Mat, F-69622 Villeurbanne, France Univ Lyon, IN2P3 CNRS, LMA, F-69622 Villeurbanne, France Univ Illes Balears, IEEC IAC3, E-07122 Palma De Mallorca, Spain Univ Naples Federico II, Complesso Univ Monte S Angelo, I-80126 Naples, Italy Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada Tsinghua Univ, Beijing 100084, Peoples R China Texas Tech Univ, Lubbock, TX 79409 USA Penn State Univ, University Pk, PA 16802 USA Natl Tsing Hua Univ, Hsinchu 30013, Taiwan Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia Univ Chicago, Chicago, IL 60637 USA Caltech CaRT, Pasadena, CA 91125 USA Korea Inst Sci & Technol Informat, Daejeon 305806, South Korea Carleton Coll, Northfield, MN 55057 USA Univ Roma La Sapienza, I-00185 Rome, Italy Univ Brussels, B-1050 Brussels, Belgium Sonoma State Univ, Rohnert Pk, CA 94928 USA Northwestern Univ, Evanston, IL 60208 USA Univ Minnesota, Minneapolis, MN 55455 USA Univ Melbourne, Parkville, Vic 3010, Australia Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England Univ Sannio Benevento, I-82100 Benevento, Italy Ist Nazl Fis Nucl, Sez Napoli, I-80100 Naples, Italy Montclair State Univ, Montclair, NJ 07043 USA Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy Ist Nazl Fis Nucl, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan Univ Edinburgh, Sch Math, Edinburgh EH9 3FD, Midlothian, Scotland Indian Inst Technol, Ahmadabad 382424, Gujarat, India Inst Plasma Res, Bhat 382428, Gandhinagar, India Univ Szeged, Dom Ter 9, H-6720 Szeged, Hungary Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA Univ Michigan, Ann Arbor, MI 48109 USA Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India Amer Univ, Washington, DC 20016 USA Univ Massachusetts Amherst, Amherst, MA 01003 USA Univ Adelaide, Adelaide, SA 5005, Australia West Virginia Univ, Morgantown, WV 26506 USA Univ Bialystok, PL-15424 Bialystok, Poland Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland IISER TVM, CET Campus, Trivandrum 695016, Kerala, India Inst Appl Phys, Nizhnii Novgorod 603950, Russia Pusan Natl Univ, Busan 609735, South Korea Hanyang Univ, Seoul 133791, South Korea NCBJ, PL-05400 Otwock, Poland IM PAN, PL-00956 Warsaw, Poland Rochester Inst Technol, Rochester, NY 14623 USA Monash Univ, Clayton, Vic 3800, Australia Seoul Natl Univ, Seoul 151742, South Korea Univ Alabama, Huntsville, AL 35899 USA CNRS, ESPCI, F-75005 Paris, France Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy Southern Univ, Baton Rouge, LA 70813 USA A&M Coll, Baton Rouge, LA 70813 USA Coll William & Mary, Williamsburg, VA 23187 USA Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil Univ Cambridge, Cambridge CB2 1TN, England IISER Kolkata, Mohanpur 741252, W Bengal, India Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA Natl Inst Math Sci, Daejeon 305390, South Korea Hobart & 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Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany Clemson Univ, Kinard Lab Phys, Dept Phys & Astron, Clemson, SC 29634 USA Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden Tokyo Metropolitan Univ, Dept Phys, Minami Osawa 1-1, Hachioji, Tokyo 1920397, Japan Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy Ist 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Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA Nagoya Univ, Inst Space Earth Environm Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, Tokyo 1810015, Japan Yamaguchi Univ, Res Inst Time Studies, Yamaguchi, Yamaguchi 7538511, Japan Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan Kyoto Univ, Dept Astron, Kyoto, Kyoto 6068502, Japan Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan Yale Univ, Dept Phys, New Haven, CT 06520 USA Liverpool JMU, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England Monash Univ, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia Univ Nova Gorica, Vipavska 13, Nova Gorica 5000, Slovenia Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000, Slovenia Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands Univ Oxford, Dept Phys, Astrophys, Keble Rd, Oxford OX1 3RH, England SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands Lomonosov Moscow State Univ, Sternberg Astron Inst, 13 Univ Skiy Prospekt, Moscow 119234, Russia South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa Inst Astrofis Canarias, Calle Via Lactea S-N, E-38200 Tenerife, Spain Irkutsk State Univ, Inst Appl Phys, 20 Gagarin Blvd, Irkutsk 664003, Russia RAS, Kislovodsk Solar Stn Main Pulkovo Observ, POB 45,Ul Gagarina 100, Kislovodsk 357700, Russia Blagoveschensk State Pedag Univ, Lenin Str 104, Blagoveshchensk 675000, Amur Region, Russia Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528851, Japan RIKEN, MAXI Team, 2-1 Hirosawa, Wako, Saitama 3510198, Japan Nihon Univ, Dept Phys, Chiyoda Ku, 1-8-14 Kanda Surugadai, Tokyo 1018308, Japan Japan Aerosp Explorat Agcy, Human Spaceflight Technol Directorate, JEM Mission Operat & Integrat Ctr, 2-1-1 Sengen, Tsukuba, Ibaraki 3058505, Japan Japan Aerosp Explorat Agcy JAXA, ISAS, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan Osaka Univ, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan Univ Calif Berkeley, Dept Astron, 501 Campbell Hall 3411, Berkeley, CA 94720 USA Eureka Sci Inc, 2452 Delmer St Suite 100, Oakland, CA 94602 USA MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada Victoria Univ Wellington, Sch Chem & Phys Sci, POB 600, Wellington 6140, New Zealand Ist Nazl Astrofis, Osservatorio Radio Astron, I-40123 Bologna, Italy Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA Harvard Univ, Dept Phys, Cambridge, MA 02138 USA Millennium Inst Astrophys, Casilla 36-D, Santiago, Chile Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France Univ Paris 06, 98 Bis Blvd Arago, F-75014 Paris, France European Southern Observ, Alonso de Cordova 3107, Santiago, Chile Univ Turku, Dept Phys & Astron, Tuorla Observ, Vaialantie 20, FI-21500 Piikkio, Finland Univ Chile, Dept Astron, Camino El Observ 1515, Santiago, Chile Univ Paris 06, Sorbonne Univ, UMR 7585, LPNHE, F-75005 Paris, France CNRS, UMR 7585, Lab Phys Nucl & Hautes Energies, 4 Pl Jussieu, F-75005 Paris, France Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel Univ Warsaw, Fac Phys, PL-02093 Warsaw, Poland Polish Acad Sci, Ctr Theoret Phys, PL-02668 Warsaw, Poland Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA Los Alamos Natl Lab, B244, Los Alamos, NM 87545 USA CNRS UMR 5277 UPS, Inst Rech Astrophys & Planetol, 14 Ave Edouard Belin, F-31400 Toulouse, France Univ Texas San Antonio, San Antonio, TX USA Univ Munich, Fac Phys, Schellingstr 4, D-80799 Munich, Germany Texas A&M Univ, Dept Phys & Astron, Mitchell Inst Fundamental Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA Univ Nacl Cordoba, IATE, Laprida 854, Cordoba, Argentina Pontificia Univ Catolica Chile, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago, Chile CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil National Science Foundation: AST-1138766 National Science Foundation: AST-1238877 MINECO: AYA2012-39559 MINECO: ESP2013-48274 MINECO: FPA2013-47986 Centro de Excelencia Severo Ochoa: SEV-2012-0234 ERC: 240672 ERC: 291329 ERC: 306478 German INTEGRAL through DLR grant: 50 OG 1101 US under NASA Grant: NNX15AU74G National Science Foundation PIRE program grant: 1545949 Hubble Fellowship: HST-HF-51325.01 KAKENHI of MEXT Japan: 24103003 KAKENHI of MEXT Japan: 15H00774 KAKENHI of MEXT Japan: 15H00788 JSPS: 15H02069 JSPS: 15H02075 ERC Advanced Investigator Grant: 267697 Russian Science Foundation: 16-12-00085 Russian Science Foundation: RFBR15-02-07875 National Aeronautics and Space Administration's Planetary Defense Office: NNX14AM74G National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate: NNX08AR22G European Research Council under European Union's Seventh Framework Programme/ERC: 291222 STFC grants: ST/I001123/1 STFC grants: ST/L000709/1 European Union FP7 programme through ERC: 320360 FONDECYT: 3140326 Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO): CE110001020 USA NSF PHYS: 1156600 NSF: 1242090 Science and Technology Facilities Council: Gravitational Waves Science and Technology Facilities Council: ST/L000946/1 Science and Technology Facilities Council: ST/K005014/1 Science and Technology Facilities Council: ST/N000668/1 Science and Technology Facilities Council: ST/M000966/1 Science and Technology Facilities Council: ST/I006269/1 Science and Technology Facilities Council: ST/L000709/1 Science and Technology Facilities Council: ST/J00166X/1 Science and Technology Facilities Council: ST/K000845/1 Science and Technology Facilities Council: ST/K00090X/1 Science and Technology Facilities Council: ST/N000633/1 Science and Technology Facilities Council: ST/H001972/1 Science and Technology Facilities Council: ST/L000733/1 Science and Technology Facilities Council: ST/N000757/1 Science and Technology Facilities Council: ST/M001334/1 Science and Technology Facilities Council: ST/J000019/1 Science and Technology Facilities Council: ST/M003035/1 Science and Technology Facilities Council: ST/I001123/1 Science and Technology Facilities Council: ST/N00003X/1 Science and Technology Facilities Council: ST/I006269/1 Gravitational Waves Science and Technology Facilities Council: ST/N000072/1 Science and Technology Facilities Council: ST/L003465/1 UK Space Agency: ST/P002196/1
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13. Heavy-element production in a compact object merger observed by JWST.

Author: Levan AJ, Gompertz BP, Salafia OS, Bulla M, Burns E, Hotokezaka K, Izzo L, Lamb GP, Malesani DB, Oates SR, Ravasio ME, Rouco Escorial A, Schneider B, Sarin N, Schulze S, Tanvir NR, Ackley K, Anderson G, Brammer GB, Christensen L, Dhillon VS, Evans PA, Fausnaugh M, Fong WF, Fruchter AS, Fryer C, Fynbo JPU, Gaspari N, Heintz KE, Hjorth J, Kennea JA, Kennedy MR, Laskar T, Leloudas G, Mandel I, Martin-Carrillo A, Metzger BD, Nicholl M, Nugent A, Palmerio JT, Pugliese G, Rastinejad J, Rhodes L, Rossi A, Saccardi A, Smartt SJ, Stevance HF, Tohuvavohu A, van der Horst A, Vergani SD, Watson D, Barclay T, Bhirombhakdi K, Breedt E, Breeveld AA, Brown AJ, Campana S, Chrimes AA, D'Avanzo P, D'Elia V, De Pasquale M, Dyer MJ, Galloway DK, Garbutt JA, Green MJ, Hartmann DH, Jakobsson P, Kerry P, Kouveliotou C, Langeroodi D, Le Floc'h E, Leung JK, Littlefair SP, Munday J, O'Brien P, Parsons SG, Pelisoli I, Sahman DI, Salvaterra R, Sbarufatti B, Steeghs D, Tagliaferri G, Thöne CC, de Ugarte Postigo A, and Kann DA
Abstract: The mergers of binary compact objects such as neutron stars and black holes are of central interest to several areas of astrophysics, including as the progenitors of gamma-ray bursts (GRBs) 1 , sources of high-frequency gravitational waves (GWs) 2 and likely production sites for heavy-element nucleosynthesis by means of rapid neutron capture (the r-process) 3 . Here we present observations of the exceptionally bright GRB 230307A. We show that GRB 230307A belongs to the class of long-duration GRBs associated with compact object mergers 4-6 and contains a kilonova similar to AT2017gfo, associated with the GW merger GW170817 (refs. 7-12 ). We obtained James Webb Space Telescope (JWST) mid-infrared imaging and spectroscopy 29 and 61 days after the burst. The spectroscopy shows an emission line at 2.15 microns, which we interpret as tellurium (atomic mass A = 130) and a very red source, emitting most of its light in the mid-infrared owing to the production of lanthanides. These observations demonstrate that nucleosynthesis in GRBs can create r-process elements across a broad atomic mass range and play a central role in heavy-element nucleosynthesis across the Universe., (© 2023. The Author(s).)
Published: 2024
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14. Rapid spectral variability of a giant flare from a magnetar in NGC 253.

Author: Roberts OJ, Veres P, Baring MG, Briggs MS, Kouveliotou C, Bissaldi E, Younes G, Chastain SI, DeLaunay JJ, Huppenkothen D, Tohuvavohu A, Bhat PN, Göğüş E, van der Horst AJ, Kennea JA, Kocevski D, Linford JD, Guiriec S, Hamburg R, Wilson-Hodge CA, and Burns E
Abstract: Magnetars are neutron stars with extremely strong magnetic fields (10 13 to 10 15 gauss) 1,2 , which episodically emit X-ray bursts approximately 100 milliseconds long and with energies of 10 40 to 10 41 erg. Occasionally, they also produce extremely bright and energetic giant flares, which begin with a short (roughly 0.2 seconds), intense flash, followed by fainter, longer-lasting emission that is modulated by the spin period of the magnetar 3,4 (typically 2 to 12 seconds). Over the past 40 years, only three such flares have been observed in our local group of galaxies 3-6 , and in all cases the extreme intensity of the flares caused the detectors to saturate. It has been proposed that extragalactic giant flares are probably a subset 7-11 of short γ-ray bursts, given that the sensitivity of current instrumentation prevents us from detecting the pulsating tail, whereas the initial bright flash is readily observable out to distances of around 10 to 20 million parsecs. Here we report X-ray and γ-ray observations of the γ-ray burst GRB 200415A, which has a rapid onset, very fast time variability, flat spectra and substantial sub-millisecond spectral evolution. These attributes match well with those expected for a giant flare from an extragalactic magnetar 12 , given that GRB 200415A is directionally associated 13 with the galaxy NGC 253 (roughly 3.5 million parsecs away). The detection of three-megaelectronvolt photons provides evidence for the relativistic motion of the emitting plasma. Radiation from such rapidly moving gas around a rotating magnetar may have generated the rapid spectral evolution that we observe.
Published: 2021
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15. Swift and NuSTAR observations of GW170817: Detection of a blue kilonova.

Author: Evans PA, Cenko SB, Kennea JA, Emery SWK, Kuin NPM, Korobkin O, Wollaeger RT, Fryer CL, Madsen KK, Harrison FA, Xu Y, Nakar E, Hotokezaka K, Lien A, Campana S, Oates SR, Troja E, Breeveld AA, Marshall FE, Barthelmy SD, Beardmore AP, Burrows DN, Cusumano G, D'Aì A, D'Avanzo P, D'Elia V, de Pasquale M, Even WP, Fontes CJ, Forster K, Garcia J, Giommi P, Grefenstette B, Gronwall C, Hartmann DH, Heida M, Hungerford AL, Kasliwal MM, Krimm HA, Levan AJ, Malesani D, Melandri A, Miyasaka H, Nousek JA, O'Brien PT, Osborne JP, Pagani C, Page KL, Palmer DM, Perri M, Pike S, Racusin JL, Rosswog S, Siegel MH, Sakamoto T, Sbarufatti B, Tagliaferri G, Tanvir NR, and Tohuvavohu A
Abstract: With the first direct detection of merging black holes in 2015, the era of gravitational wave (GW) astrophysics began. A complete picture of compact object mergers, however, requires the detection of an electromagnetic (EM) counterpart. We report ultraviolet (UV) and x-ray observations by Swift and the Nuclear Spectroscopic Telescope Array of the EM counterpart of the binary neutron star merger GW170817. The bright, rapidly fading UV emission indicates a high mass (≈0.03 solar masses) wind-driven outflow with moderate electron fraction ( Y e ≈ 0.27). Combined with the x-ray limits, we favor an observer viewing angle of ≈30° away from the orbital rotation axis, which avoids both obscuration from the heaviest elements in the orbital plane and a direct view of any ultrarelativistic, highly collimated ejecta (a γ-ray burst afterglow)., (Copyright © 2017, American Association for the Advancement of Science.)
Published: 2017
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16. An anti-glitch in a magnetar.

Author: Archibald RF, Kaspi VM, Ng CY, Gourgouliatos KN, Tsang D, Scholz P, Beardmore AP, Gehrels N, and Kennea JA
Abstract: Magnetars are neutron stars with X-ray and soft γ-ray outbursts thought to be powered by intense internal magnetic fields. Like conventional neutron stars in the form of radio pulsars, magnetars exhibit 'glitches' during which angular momentum is believed to be transferred between the solid outer crust and the superfluid component of the inner crust. The several hundred observed glitches in radio pulsars and magnetars have involved a sudden spin-up (increase in the angular velocity) of the star, presumably because the interior superfluid was rotating faster than the crust. Here we report X-ray timing observations of the magnetar 1E 2259+586 (ref. 8), which exhibited a clear 'anti-glitch'--a sudden spin-down. We show that this event, like some previous magnetar spin-up glitches, was accompanied by multiple X-ray radiative changes and a significant spin-down rate change. Such behaviour is not predicted by models of neutron star spin-down and, if of internal origin, is suggestive of differential rotation in the magnetar, supporting the need for a rethinking of glitch theory for all neutron stars.
Published: 2013
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17. Relativistic jet activity from the tidal disruption of a star by a massive black hole.

Author: Burrows DN, Kennea JA, Ghisellini G, Mangano V, Zhang B, Page KL, Eracleous M, Romano P, Sakamoto T, Falcone AD, Osborne JP, Campana S, Beardmore AP, Breeveld AA, Chester MM, Corbet R, Covino S, Cummings JR, D'Avanzo P, D'Elia V, Esposito P, Evans PA, Fugazza D, Gelbord JM, Hiroi K, Holland ST, Huang KY, Im M, Israel G, Jeon Y, Jeon YB, Jun HD, Kawai N, Kim JH, Krimm HA, Marshall FE, P Mészáros, Negoro H, Omodei N, Park WK, Perkins JS, Sugizaki M, Sung HI, Tagliaferri G, Troja E, Ueda Y, Urata Y, Usui R, Antonelli LA, Barthelmy SD, Cusumano G, Giommi P, Melandri A, Perri M, Racusin JL, Sbarufatti B, Siegel MH, and Gehrels N
Abstract: Supermassive black holes have powerful gravitational fields with strong gradients that can destroy stars that get too close, producing a bright flare in ultraviolet and X-ray spectral regions from stellar debris that forms an accretion disk around the black hole. The aftermath of this process may have been seen several times over the past two decades in the form of sparsely sampled, slowly fading emission from distant galaxies, but the onset of the stellar disruption event has not hitherto been observed. Here we report observations of a bright X-ray flare from the extragalactic transient Swift J164449.3+573451. This source increased in brightness in the X-ray band by a factor of at least 10,000 since 1990 and by a factor of at least 100 since early 2010. We conclude that we have captured the onset of relativistic jet activity from a supermassive black hole. A companion paper comes to similar conclusions on the basis of radio observations. This event is probably due to the tidal disruption of a star falling into a supermassive black hole, but the detailed behaviour differs from current theoretical models of such events.
Published: 2011
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18. The association of GRB 060218 with a supernova and the evolution of the shock wave.

Author: Campana S, Mangano V, Blustin AJ, Brown P, Burrows DN, Chincarini G, Cummings JR, Cusumano G, Della Valle M, Malesani D, Mészáros P, Nousek JA, Page M, Sakamoto T, Waxman E, Zhang B, Dai ZG, Gehrels N, Immler S, Marshall FE, Mason KO, Moretti A, O'Brien PT, Osborne JP, Page KL, Romano P, Roming PW, Tagliaferri G, Cominsky LR, Giommi P, Godet O, Kennea JA, Krimm H, Angelini L, Barthelmy SD, Boyd PT, Palmer DM, Wells AA, and White NE
Abstract: Although the link between long gamma-ray bursts (GRBs) and supernovae has been established, hitherto there have been no observations of the beginning of a supernova explosion and its intimate link to a GRB. In particular, we do not know how the jet that defines a gamma-ray burst emerges from the star's surface, nor how a GRB progenitor explodes. Here we report observations of the relatively nearby GRB 060218 (ref. 5) and its connection to supernova SN 2006aj (ref. 6). In addition to the classical non-thermal emission, GRB 060218 shows a thermal component in its X-ray spectrum, which cools and shifts into the optical/ultraviolet band as time passes. We interpret these features as arising from the break-out of a shock wave driven by a mildly relativistic shell into the dense wind surrounding the progenitor. We have caught a supernova in the act of exploding, directly observing the shock break-out, which indicates that the GRB progenitor was a Wolf-Rayet star.
Published: 2006
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19. Gamma-ray bursts: huge explosion in the early Universe.

Author: Cusumano G, Mangano V, Chincarini G, Panaitescu A, Burrows DN, La Parola V, Sakamoto T, Campana S, Mineo T, Tagliaferri G, Angelini L, Barthelemy SD, Beardmore AP, Boyd PT, Cominsky LR, Gronwall C, Fenimore EE, Gehrels N, Giommi P, Goad M, Hurley K, Kennea JA, Mason KO, Marshall F, Mészáros P, Nousek JA, Osborne JP, Palmer DM, Roming PW, Wells A, White NE, and Zhang B
Abstract: Long gamma-ray bursts (GRBs) are bright flashes of high-energy photons that can last for tens of minutes; they are generally associated with galaxies that have a high rate of star formation and probably arise from the collapsing cores of massive stars, which produce highly relativistic jets (collapsar model). Here we describe gamma- and X-ray observations of the most distant GRB ever observed (GRB 050904): its redshift (z) of 6.29 means that this explosion happened 12.8 billion years ago, corresponding to a time when the Universe was just 890 million years old, close to the reionization era. This means that not only did stars form in this short period of time after the Big Bang, but also that enough time had elapsed for them to evolve and collapse into black holes.
Published: 2006
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20. An origin for short gamma-ray bursts unassociated with current star formation.

Author: Barthelmy SD, Chincarini G, Burrows DN, Gehrels N, Covino S, Moretti A, Romano P, O'Brien PT, Sarazin CL, Kouveliotou C, Goad M, Vaughan S, Tagliaferri G, Zhang B, Antonelli LA, Campana S, Cummings JR, D'Avanzo P, Davies MB, Giommi P, Grupe D, Kaneko Y, Kennea JA, King A, Kobayashi S, Melandri A, Meszaros P, Nousek JA, Patel S, Sakamoto T, and Wijers RA
Abstract: Two short (< 2 s) gamma-ray bursts (GRBs) have recently been localized and fading afterglow counterparts detected. The combination of these two results left unclear the nature of the host galaxies of the bursts, because one was a star-forming dwarf, while the other was probably an elliptical galaxy. Here we report the X-ray localization of a short burst (GRB 050724) with unusual gamma-ray and X-ray properties. The X-ray afterglow lies off the centre of an elliptical galaxy at a redshift of z = 0.258 (ref. 5), coincident with the position determined by ground-based optical and radio observations. The low level of star formation typical for elliptical galaxies makes it unlikely that the burst originated in a supernova explosion. A supernova origin was also ruled out for GRB 050709 (refs 3, 31), even though that burst took place in a galaxy with current star formation. The isotropic energy for the short bursts is 2-3 orders of magnitude lower than that for the long bursts. Our results therefore suggest that an alternative source of bursts--the coalescence of binary systems of neutron stars or a neutron star-black hole pair--are the progenitors of short bursts.
Published: 2005
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21. A short gamma-ray burst apparently associated with an elliptical galaxy at redshift z = 0.225.

Author: Gehrels N, Sarazin CL, O'Brien PT, Zhang B, Barbier L, Barthelmy SD, Blustin A, Burrows DN, Cannizzo J, Cummings JR, Goad M, Holland ST, Hurkett CP, Kennea JA, Levan A, Markwardt CB, Mason KO, Meszaros P, Page M, Palmer DM, Rol E, Sakamoto T, Willingale R, Angelini L, Beardmore A, Boyd PT, Breeveld A, Campana S, Chester MM, Chincarini G, Cominsky LR, Cusumano G, de Pasquale M, Fenimore EE, Giommi P, Gronwall C, Grupe D, Hill JE, Hinshaw D, Hjorth J, Hullinger D, Hurley KC, Klose S, Kobayashi S, Kouveliotou C, Krimm HA, Mangano V, Marshall FE, McGowan K, Moretti A, Mushotzky RF, Nakazawa K, Norris JP, Nousek JA, Osborne JP, Page K, Parsons AM, Patel S, Perri M, Poole T, Romano P, Roming PW, Rosen S, Sato G, Schady P, Smale AP, Sollerman J, Starling R, Still M, Suzuki M, Tagliaferri G, Takahashi T, Tashiro M, Tueller J, Wells AA, White NE, and Wijers RA
Abstract: Gamma-ray bursts (GRBs) come in two classes: long (> 2 s), soft-spectrum bursts and short, hard events. Most progress has been made on understanding the long GRBs, which are typically observed at high redshift (z approximately 1) and found in subluminous star-forming host galaxies. They are likely to be produced in core-collapse explosions of massive stars. In contrast, no short GRB had been accurately (< 10'') and rapidly (minutes) located. Here we report the detection of the X-ray afterglow from--and the localization of--the short burst GRB 050509B. Its position on the sky is near a luminous, non-star-forming elliptical galaxy at a redshift of 0.225, which is the location one would expect if the origin of this GRB is through the merger of neutron-star or black-hole binaries. The X-ray afterglow was weak and faded below the detection limit within a few hours; no optical afterglow was detected to stringent limits, explaining the past difficulty in localizing short GRBs.
Published: 2005
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22. Bright x-ray flares in gamma-ray burst afterglows.

Author: Burrows DN, Romano P, Falcone A, Kobayashi S, Zhang B, Moretti A, O'brien PT, Goad MR, Campana S, Page KL, Angelini L, Barthelmy S, Beardmore AP, Capalbi M, Chincarini G, Cummings J, Cusumano G, Fox D, Giommi P, Hill JE, Kennea JA, Krimm H, Mangano V, Marshall F, Mészáros P, Morris DC, Nousek JA, Osborne JP, Pagani C, Perri M, Tagliaferri G, Wells AA, Woosley S, and Gehrels N
Abstract: Gamma-ray burst (GRB) afterglows have provided important clues to the nature of these massive explosive events, providing direct information on the nearby environment and indirect information on the central engine that powers the burst. We report the discovery of two bright x-ray flares in GRB afterglows, including a giant flare comparable in total energy to the burst itself, each peaking minutes after the burst. These strong, rapid x-ray flares imply that the central engines of the bursts have long periods of activity, with strong internal shocks continuing for hundreds of seconds after the gamma-ray emission has ended.
Published: 2005
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23. An unexpectedly rapid decline in the X-ray afterglow emission of long gamma-ray bursts.

Author: Tagliaferri G, Goad M, Chincarini G, Moretti A, Campana S, Burrows DN, Perri M, Barthelmy SD, Gehrels N, Krimm H, Sakamoto T, Kumar P, Mészáros PI, Kobayashi S, Zhang B, Angelini L, Banat P, Beardmore AP, Capalbi M, Covino S, Cusumano G, Giommi P, Godet O, Hill JE, Kennea JA, Mangano V, Morris DC, Nousek JA, O'Brien PT, Osborne JP, Pagani C, Page KL, Romano P, Stella L, and Wells A
Abstract: 'Long' gamma-ray bursts (GRBs) are commonly accepted to originate in the explosion of particularly massive stars, which give rise to highly relativistic jets. Inhomogeneities in the expanding flow result in internal shock waves that are believed to produce the gamma-rays we see. As the jet travels further outward into the surrounding circumstellar medium, 'external' shocks create the afterglow emission seen in the X-ray, optical and radio bands. Here we report observations of the early phases of the X-ray emission of five GRBs. Their X-ray light curves are characterised by a surprisingly rapid fall-off for the first few hundred seconds, followed by a less rapid decline lasting several hours. This steep decline, together with detailed spectral properties of two particular bursts, shows that violent shock interactions take place in the early jet outflows.
Published: 2005
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23 results on '"Kennea, JA"'

1. Space Telescope and Optical Reverberation Mapping Project. IX. Velocity–Delay Maps for Broad Emission Lines in NGC 5548

2. Space Telescope and Optical Reverberation Mapping Project. XII. Broad-line Region Modeling of NGC 5548

3. Space Telescope and Optical Reverberation Mapping Project. VIII. Time Variability of Emission and Absorption in NGC 5548 Based on Modeling the Ultraviolet Spectrum

4. Space Telescope and Optical Reverberation Mapping Project. VII. Understanding the Ultraviolet Anomaly in NGC 5548 with X-Ray Spectroscopy

5. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT.VI. REVERBERATING DISK MODELS FOR NGC 5548

6. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. IV. ANOMALOUS BEHAVIOR OF THE BROAD ULTRAVIOLET EMISSION LINES IN NGC 5548

7. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. III. OPTICAL CONTINUUM EMISSION AND BROADBAND TIME DELAYS IN NGC 5548

8. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. II. SWIFT AND HST REVERBERATION MAPPING OF THE ACCRETION DISK OF NGC 5548

9. SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. I. ULTRAVIOLET OBSERVATIONS OF THE SEYFERT 1 GALAXY NGC 5548 WITH THE COSMIC ORIGINS SPECTROGRAPH ON HUBBLE SPACE TELESCOPE

10. Swift observations of GRB050904: the most distant cosmic explosion ever observed

11. Swift X-Ray Telescope and Very Large Telescope Observations of the Afterglow of GRB 041223

12. SUPPLEMENT: 'lOCALIZATION and BROADBAND FOLLOW-UP of the GRAVITATIONAL-WAVE TRANSIENT GW150914' (2016, ApJL, 826, L13)

13. Heavy-element production in a compact object merger observed by JWST.

14. Rapid spectral variability of a giant flare from a magnetar in NGC 253.

15. Swift and NuSTAR observations of GW170817: Detection of a blue kilonova.

16. An anti-glitch in a magnetar.

17. Relativistic jet activity from the tidal disruption of a star by a massive black hole.

18. The association of GRB 060218 with a supernova and the evolution of the shock wave.

19. Gamma-ray bursts: huge explosion in the early Universe.

20. An origin for short gamma-ray bursts unassociated with current star formation.

21. A short gamma-ray burst apparently associated with an elliptical galaxy at redshift z = 0.225.

22. Bright x-ray flares in gamma-ray burst afterglows.

23. An unexpectedly rapid decline in the X-ray afterglow emission of long gamma-ray bursts.

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